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\begin{document}

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\begin{center}
{\Large
{\bf Notes on Individual HH Objects}
}
\vspace*{0.5cm}

\end{center}


\baselineskip0.5cm

{\bf HH 1/2} {\em (5 33, -06 48)}.  Original papers: Herbig (1951),
Haro (1952,1953).  These are among the brightest HH objects in the
sky, and form bow shocks in a highly collimated bipolar outflow with
dimension 2.5 arcmin (0.34 pc projected). A small jet originates from
the embedded central source.  
{\em Optical Spectroscopic Studies:}
Herbig (1951), B\"{o}hm (1956), Osterbrock (1958), Haro \& Minkowski
(1960), B\"{o}hm, Perry, Schwartz (1973), B\"{o}hm, Siegmund, Schwartz
(1976a), Dopita (1978a), Schwartz (1978), B\"ohm \& Brugel (1979),
Brugel, B\"ohm, Mannery (1981a), Schwartz (1981), Dopita, Binette,
Schwartz (1982), Hartmann \& Raymond (1984), B\"ohm \& Solf (1985),
Cant\'o \& Rodr\'\i guez (1986), Solf, B\"ohm, Raga (1988),
Noriega-Crespo, B\"ohm, Raga (1989), Solf \& B\"ohm (1991), Solf et
al. (1991), B\"ohm \& Solf (1992), Beck-Winchatz \& B\"ohm (1994),
Beck-Winchatz, B\"ohm, Noriega-Crespo (1996).  
{\em Studies of Blue Continua:} 
B\"ohm, Schwartz, Siegmund (1974), Brugel, B\"ohm, Mannery
(1981b), Dopita, Binette, Schwartz (1982), Solf, B\"ohm, Raga (1988).
{\em Ultraviolet Spectroscopy:} 
Ortolani \& D'Odorico (1980), B\"ohm,
B\"ohm-Vitense, Brugel (1981), Brugel, Shull, Seab (1982),
B\"ohm-Vitense et al. (1982), Brugel et al. (1985), B\"ohm et
al. (1987), Lee et al. (1988), B\"ohm, Raga, Binette (1991), B\"ohm,
Noriega-Crespo, Solf (1993), Moro-Martin et al. (1996), Raymond,
Blair, Long (1997).  
{\em Structure and CCD Imaging:} 
Strom et al. (1985a, 1986), Mundt, Brugel, B\"uhrke (1987), Raga \& Mateo
(1988a), Raga et al. (1988), Schwartz et al. (1993), Reipurth et
al. (1993b), Eisl\"offel, Mundt, B\"ohm (1994), Ogura (1995), Ray et
al. (1996), Hester, Stapelfeldt, Scowen (1998).  
{\em Variability of Knots:} 
Herbig (1969, 1973), Schwartz (1976), Herbig \& Jones (1981),
Brugel et al. (1985), Raga, Barnes, Mateo (1990).  
{\em Infrared observations:} 
Elias (1980), Harvey et al. (1986), Zinnecker et
al. (1989), Zealey et al. (1992), Davis, Eisl\"offel, Ray (1994),
Kelly, Rieke, Campbell (1994), Noriega-Crespo \& Garnavich (1994a,b),
Schwartz et al. (1995), Gredel (1996).  
{\em Radio continuum studies:}
Pravdo et al. (1985), Curiel, Cant\'o, Rodr\'\i guez (1987), Rodr\'\i
guez et al. (1990b).  {\em Search for X-rays:} Pravdo \& Marshall
(1981), Strom et al. (1990), Pravdo \& Angelini (1993).  
{\em Polarization studies}: 
Strom, Strom, Kinman (1974), Schmidt \& Vrba (1975).  
{\em Energy Source:} 
Pravdo et al. (1985), Rodr\'\i guez,
Roth, Tapia (1985), Strom et al. (1985a), Harvey et al. (1986), Pravdo
\& Chester (1987), Tapia et al.  (1987), Reipurth (1989b), Rodr\'\i
guez et al. (1990b), Reipurth et al.  (1993a), Chini et al. (1997b),
Zavagno et al. (1997), Dent, Matthew, Ward-Thompson (1998).
{\em Studies of Jet:} 
Strom et al. (1985a), Bohigas et al. (1985),
Cohen \& Fuller (1985), Schwartz, Cohen, Williams (1987), Mundt,
Brugel, B\"uhrke (1987), Roth et al. (1989), Reipurth et al. (1993b).
{\em Proper Motions:} 
Herbig \& Jones (1981), Reipurth et al. (1993b),
Eisl\"offel, Mundt, B\"ohm (1994), Noriega-Crespo et al. (1997).
{\em Dust scattered emission:} 
Solf \& B\"ohm (1991), Noriega-Crespo,
Calvet, B\"ohm (1991), Henney, Raga, Axon (1994).
{\em Mm Studies:} 
Loren, Evans, Knapp (1979), Edwards \& Snell (1984),
Torrelles et al. (1985b),
Levreault (1988), Marcaide et al. (1988), Davis, Dent, Burnell (1990),
Cernicharo (1990), Morgan et al. (1991),
Torrelles et al. (1992b, 1993c, 1994), Chernin \& Masson (1995),
Choi \& Zhou (1997), Correia, Griffin, Saraceno (1997), Choi \& Lee (1998).
{\em Various model calculations:} 
Hartmann \& Raymond (1984), Choe,
B\"ohm, Solf (1985), Hartigan, Raymond, Hartmann (1987), Raga et al.
(1988), Hartigan (1989), Noriega-Crespo, B\"ohm, Raga (1989,1990),
Indebetouw \& Noriega-Crespo (1995).
See also notes for HH 144 and HH 145, and for HH~401/402.

\vspace*{0.3cm}

{\bf HH 3} {\em (5 33, -06 44)}.
Original papers: Herbig (1951), Haro (1952,1953). Bright HH
object with a jet-like protrusion (Ray 1987) and associated with a
group of faint HH knots (Reipurth 1989b). Associated with faint
near-infrared object (Roth et al. 1989). No molecular outflow detected
by Edwards \& Snell (1984). Optical spectroscopy: Dopita (1978a),
Brugel, B\"ohm, Mannery (1981a).

\vspace*{0.3cm}

{\bf HH 4} {\em (3 26, +31 09)}.
Herbig (1974) notes that this is ``a faint nebulosity 7-8 arcsec in
diameter with a sharp condensation or faint star on the west edge''.
It is seen in the infrared images of Aspin, Sandell, Russell (1994),
and the optical images of Bally, Devine, Reipurth (1996).

\vspace*{0.3cm}

{\bf HH 5} {\em (3 26, +31 02)}.
Originally found by Herbig (1974). H$_2$ detection by Lane \& Bally
(1986). CCD image presented by Ray (1987). Astrometry and proper
motion by Herbig \& Jones (1983). Detailed optical/infrared imaging
and spectroscopic study by Cohen, Jones, Hereld (1991). Low excitation
object. It is seen in the infrared images of Aspin, Sandell, Russell
(1994), and the optical images of Bally, Devine, Reipurth
(1996). Schwartz et al. (1995) present near-infrared spectroscopy.

\vspace*{0.3cm}

{\bf HH 6} {\em (3 26, +31 08)}.  
Originally found by Herbig (1974). H$_2$ detection by Lane \& Bally
(1986), Lightfoot \& Glencross (1986), and Schwartz, Cohen, Williams
(1987). Detailed optical/infrared imaging and spectroscopic study by
Cohen, Jones, Hereld (1991).  CCD images are also presented by Bally,
Devine, Reipurth (1996).  This is a low excitation object. A weak VLA
6 cm continuum source is found nearby (Snell \& Bally 1986) as well as
an H$_2$O maser source (Henkel, Haschick, G\"usten 1986). Energy
source of 33 L$_\odot$ detected at 50 and 100 $\mu$m in IRAS CPC
observations (Jennings et al. 1987). The HH object is seen in the
infrared images of Aspin, Sandell, Russell (1994).  Schwartz et
al. (1995) present near-infrared spectroscopy. Liseau, Sandell, Knee
(1988) found a very weak molecular outflow.


\vspace*{0.3cm}

{\bf HH 7/8/9/10/11} {\em (3 26, +31 05)}.  This is a chain of bright HH
knots about 1 arcmin long, first discussed by Herbig (1974) and Strom,
Grasdalen, Strom (1974). {\em CCD Imaging:} Strom et al. (1986), Solf
\& B\"ohm (1987), Raga \& Mateo (1988a), Hartigan, Curiel, Raymond
(1989), Aspin, Sandell, Russell (1994), Davis et al. (1995), Bally,
Devine, Reipurth (1996).  {\em Optical Spectroscopy:} Strom, Grasdalen
Strom (1974), B\"ohm, Brugel, Mannery (1980), Cohen \& Schmidt (1981),
B\"ohm, Brugel, Olmsted (1983), Goodrich (1986a), Solf \& B\"ohm
(1987), B\"ohm \& Solf (1990), Beck-Winchatz \& B\"ohm (1994),
Beck-Winchatz, B\"ohm, Noriega-Crespo (1996).  {\em Infrared
Observations:} Simon \& Joyce (1983), Zealey, Williams, Sandell
(1984), Lightfoot \& Glencross (1986), Cohen et al. (1988), Zinnecker
et al. (1989), Burton et al. (1989), Hartigan, Curiel, Raymond (1989),
Garden, Russell, Burton (1990), Stapelfeldt et al. (1991), Carr
(1993), Aspin, Sandell, Russell (1994), Fernandes \& Brand (1995),
Gredel (1996), Lada, Alves, Lada (1996), Everett (1997).  {\em
Ultraviolet Observations:} Cameron \& Liseau (1990).  {\em Proper
Motions:} Herbig \& Jones (1983).  {\em Radio Observations:} Lada et
al. (1974), Ho \& Barrett (1980), Snell \& Edwards (1981), Liseau \&
Sandell (1986), Mirabel et al. (1987), Liseau et al. (1988), Rudolph
\& Welch (1988), Lizano et al. (1988), Koo (1990), Masson, Mundy,
Keene (1990), Rodr\'\i guez et al. (1990a), Bachiller \& Cernicharo
(1990), Phillips \& Mampaso (1991), Giovanardi et al. (1992), Dent et
al. (1993), Mehringer (1996), Cernicharo, Bachiller, Gonzalez-Alfonso
(1996), Warin et al. (1996), Lefloch et
al. (1998a,b), Bachiller et al. (1998b), Codella, Bachiller, Reipurth (1999).
{\em Source:} Strom, Vrba, Strom (1976a), Cohen \&
Schwartz (1983), Cohen et al. (1984a), Hodapp (1984), Snell \& Bally
(1986), Goodrich (1986), Cohen \& Schwartz (1987), Grossman et
al. (1987), Jennings et al. (1987), Sandell et al. (1990), Eisl\"offel
et al. (1991), Carr \& Tokunaga (1992), Liseau, Lorenzetti, Molinari
(1992), Molinari, Liseau, Lorenzetti (1993), Reipurth et al. (1993a),
Aspin \& Sandell (1994), Chandler, Carlstrom, Scoville (1995), Najita,
Carr, Tokunaga (1996), Rodriguez, Anglada, Curiel (1997), Chini et
al. (1997b), Biscaya et al. (1997).  {\em Magnetic Field Direction:}
Heyer, Strom, Strom (1987).  {\em H$_2$O Masers:} Dickinson, Kojoian,
Strom (1974), Lo et al.  (1976), Haschick et al. (1980), Haschick,
Moran, Rodr\'\i guez (1980), Claussen et al. (1996), Lefloch et
al. (1998a).  {\em Distance:} Herbig \& Jones (1983), C\u{e}rnis
(1990) and references therein; a distance of 220 pc is adopted here.

\vspace*{0.3cm}

{\bf HH 12} {\em (3 25, +31 09)}.  Originally found by Herbig (1974).
{\em CCD Imaging:} Strom, Strom, Stocke (1983), Strom et al. (1986),
Stapelfeldt et al. (1991), Aspin, Sandell, Russell (1994), Bally,
Devine, Reipurth (1996).  {\em Spectroscopy:} Strom, Grasdalen, Strom
(1974), Strom, Strom, Stocke (1983), Cohen \& Jones (1987).  {\em IR
Observations:} Simon \& Joyce (1983), Lane \& Bally (1986), Schwartz,
Cohen, Williams (1987), Garden, Russell, Burton (1990), Stapelfeldt et
al. (1991), Aspin, Sandell, Russell (1994).  {\em Proper motions:}
Herbig \& Jones (1983).  {\em Mm Observations:} Ho \& Barrett (1980),
Edwards \& Snell (1983), Liseau et al. (1988), Bachiller et al. (1998b).
{\em Magnetic Field Direction:} Heyer, Strom, Strom (1987).  {\em
Source:} The source has not been unequivocally identified, but there
are several candidates, star 107 proposed by Strom, Strom, Stocke
(1983), and SVS 12 (Strom, Vrba, Strom 1976a, Cohen \& Schwartz 1987,
Jennings et al. (1987), Stapelfeldt et al. 1991, Molinari, Liseau,
Lorenzetti 1993); Bachiller et al. (1998b) suggest that HH~12 is the
working surface of a molecular jet driven by the submillimeter source
SVS~13b.

\vspace*{0.3cm}

{\bf HH 13} {\em (3 25, +30 56)}. 
Original paper: Herbig (1974). CCD images by Bally, Devine, Reipurth
(1996) show this to be an about 1 arcminute large cluster of mostly
[SII] bright knots.


\vspace*{0.3cm}

{\bf HH 14} {\em (3 25, +30 50)}.  
Original paper: Herbig (1974), who notes that this is ``a group of
about 6 nebulous spots distributed over an area of about 20 $\times$
60 arcsec.''  CCD images are presented by Bally, Devine, Reipurth
(1996).  Cohen \& Schwartz (1987) draw attention to the nearby IRAS
source 03254+3050 as a candidate energy source.

\vspace*{0.3cm}

{\bf HH 15} {\em (3 25, +30 57)}.
Original paper: Herbig (1974). Cohen \& Schwartz (1987) suggest IRAS
03256+3055 could be a possible energy source.  Bally, Devine, Reipurth
(1996) show a CCD image, and note that HH~15 lies on a line through
IRAS 03255+3103 (IRAS~1) together with HH~338 and HH~339, which are on
the opposite side of this IRAS source. The morphology of HH~15 is
consistent with it being a bow shock originating in the IRAS~1
source. Phillips et al. (1988) detected a molecular outflow from
IRAS~1 along the HH~15-341-338-339 axis.

\vspace*{0.3cm}

{\bf HH 16} {\em (3 26, +30 58)}.  Herbig (1974) describes this as ``a
faint elongated smudge about 3 $\times$ 7 arcsec.'' Cohen \& Schwartz
(1987) suggest IRAS 03256+3055 could be a possible energy source. CCD
images are shown by Bally, Devine, Reipurth (1996). Bachiller et
al. (1998b) note that HH 16 is lying on the axis of a molecular jet
from SVS~13b.

\vspace*{0.3cm}

{\bf HH 17} {\em (3 26, +31 08)}.
Herbig (1974) writes that this is ``a very faint nebulosity 5 to 10
arcsec across, with a sharp condensation or star at the northern
edge''. Bally, Devine, Reipurth (1996) show CCD images. Jennings et
al. (1987) found an IRAS source (IRAS~f) very close to HH~17.  A
near-infrared source (SVS 5 = ASR 112) was detected by Strom, Vrba,
Strom (1976a) and Aspin, Sandell, Russell (1994).

\vspace*{0.3cm}

{\bf HH 18} {\em (3 26, +30 57)}.
Herbig (1974) notes that this is ``a group of at least 5 faint
nebulous spots distributed over an area of about 20 $\times$ 35
arcsec.'' CCD images are shown by Bally, Devine, Reipurth (1996).

\vspace*{0.3cm}

{\bf HH 19} {\em (5 43, $-$00 06)}.  Original paper: Herbig (1974). CCD
images presented by Mundt et al.  (1984), Strom et al. (1986) and
Eisl\"offel \& Mundt (1997). Spectroscopy by Jones et al. (1987) and Mundt,
Brugel, B\"uhrke (1987). Proper motions by Jones et al.  (1987) suggest an
origin near SSV~63 and HH~24.  Specifically, Eisl\"offel \& Mundt (1997)
argue that HH 19 is a bow shock from the HH 24J jet, which has a
counter-flow in the HH 24K jet and the HH 27 bow shock, with a total
projected extent of 1.6 pc.  Infrared H$_2$ spectroscopy by Zinnecker et
al. (1989). Infrared imaging by Zealey et al. (1992).

\vspace*{0.3cm}

{\bf HH 20/21} {\em (5 43, $-$00 05)}.  Original paper: Herbig
(1974). These objects form a loose group of HH knots together with HH~70
(Reipurth \& Graham 1988) and HH~37 of Strom et al. (1986); both papers
present CCD images. Located near HH 19. The proper motion study by Jones et
al. (1987) suggests HH~20 originates near SSV~63 and HH~24.  Based on
wide-field CCD images, Eisl\"offel \& Mundt (1997) suggest that HH 20/21,
HH 37 and HH 70 may form a single giant bow shock from a flow originating
in HH 24.  HH~20 was observed spectroscopically by Jones et al. (1987).

\vspace*{0.3cm}

{\bf HH 22} {\em (5 43, $-$00 06)}.  Original paper: Herbig (1974). CCD
images by Eisl\"offel \& Mundt (1997) show that this is a 3 arcmin long
finely collimated jet. No source has been identified.

\vspace{0.3cm}

{\bf HH 23} {\em (5 43, $-$00 04)}. Original paper: Herbig (1974). CCD
images by Eisl\"offel \& Mundt (1997) show that this is a collimated flow
from the IRAS 05436$-$0007 source, which displays a faint reflection
nebula. Jones et al. (1987) attempted to measure the proper motions of HH
23.

\vspace*{0.3cm}

{\bf HH 24} {\em (5 43, $-$00 11)}.  Originally discovered by Herbig
\& Kuhi (1963). This is a very complex region with at least three and
perhaps more outflows. For an overview of the region, source locations
and nomenclature of knots see Figs. 17 and 19 of Mundt, Ray, Raga
(1991), and Fig. 8 of Eisl\"offel \& Mundt (1997).  {\em Structure and
CCD Images:} Strom et al. (1986), Jones et al. (1987), Mundt, Ray,
Raga (1991), Eisl\"offel \& Mundt (1997).  {\em Optical Spectroscopy:}
Strom, Grasdalen, Strom (1974), Dopita (1978a), Schmidt \& Miller
(1979), Brugel, B\"ohm, Mannery (1981a,b), Solf (1987), Bacciotti \&
Eisl\"offel (1999).  {\em Ultraviolet Spectroscopy:} Lee et
al. (1988), B\"ohm et al. (1992), Moro-Martin et al. (1996).  {\em
Infrared Observations:} Zealey et al. (1992), Hodapp (1994), Moneti \&
Reipurth (1995), Davis et al. (1997a).  {\em Proper Motions:} Jones et
al. (1987).  {\em Polarization Measurements:} Strom, Grasdalen, Strom
(1974), Strom, Strom, Kinman (1974), Schmidt \& Miller (1979),
Scarrott, Gledhill, Warren-Smith (1987).  {\em Source(s):} Strom,
Grasdalen, Strom (1974), Strom, Strom, Vrba (1976a), Cohen \& Schwartz
(1983, 1987), Cohen et al. (1984a), Bieging, Cohen, Schwartz (1984),
Cohen, Dopita, Schwartz (1986b), Lane (1989), Zealey et al. (1989,
1992), Reipurth et al.  (1993a), Molinari, Liseau, Lorenzetti (1993),
Chini et al. (1993), Kr\"ugel \& Chini (1994), Ward-Thompson et
al. (1995), Chandler et al. (1995), Bontemps, Andr\'e, Ward-Thompson
(1995), Bontemps, Ward-Thompson, Andr\'e (1996), Greaves, Holland,
Ward-Thompson (1997), Anglada et al (1998), Dent, Matthew,
Ward-Thompson (1998),  Gibb (1999).  {\em Radio Observations:} Lada et
al. (1974), Snell \& Edwards (1982), Wootten et al. (1982), Matthews
\& Little (1983), Torrelles et al. (1983a), Edwards \& Snell (1984),
Little et al. (1985), Torrelles et al. (1989), Pastor et al. (1991),
Lada et al.  (1991), Gibb \& Heaton (1993), Harju, Walmsley,
Wouterloot (1993), Gibb et al.  (1995), Gibb \& Little (1998), Gibb
(1999).

\vspace*{0.3cm}

{\bf HH 25/26} {\em (5 43, $-$00 15)}.  Original paper: Herbig
(1974). The comment by Cohen \& Schwartz (1987) that HH 25 is not an
emission nebula is incorrect (e.g. Jones et al.  1987). Structure and
CCD images discussed by Strom et al. (1986) and Jones et
al. (1987). Optical spectroscopy presented by Jones et al.  (1987). A
2.0 - 2.5 $\mu$m spectrum of HH~26 is given by Schwartz, Cohen,
Williams (1987), and further near-infrared spectroscopy of both
objects is presented by Schwartz et al. (1995). Infrared imaging is
discussed by Schwartz, Burton, Herrmann (1997).  An embedded
near-infrared source, SSV~59 (= IRAS 05435--0015), is located between
HH~25 and 26, and is a candidate energy source (Strom, Strom, Vrba
1976a, Cohen \& Schwartz 1983, Cohen et al. 1984a). Another deeply
embedded source, HH~25~IRS, is more recently discovered in the region
(see e.g. Gibb \& Davis 1998).  Centimeter radio continuum
observations are discussed by Bontemps, Andr\'e, Ward-Thompson (1995),
Anglada et al. (1998) and Gibb (1999).  Hodapp (1994) presents a large-field K'
band image and Davis et al. (1997a) discuss narrow-band infrared
images.  The region is very complex at mm wavelengths (see Gibb \&
Heaton 1993 for a summary, and references to radio observations under
HH~24). Verdes-Montenegro \& Ho (1996) have mapped the molecular core
around the IR source in NH$_3$.

\vspace*{0.3cm}

{\bf HH 27} {\em (5 43, $-$00 14)}.  Original paper: Herbig
(1974). Structure and CCD images are discussed by Strom et al. (1986),
Jones et al. (1987) and Eisl\"offel \& Mundt (1997).  It is suggested by
Eisl\"offel \& Mundt (1997) that HH 27 is a bow shock from the HH 24K jet,
which has a counterflow in the HH 24J jet and the HH 19 bow shock.  Optical
spectroscopy is presented by Jones et al. (1987). H$_2$ is detected by
Schwartz, Cohen, Williams (1987). Mm observations are summarized by Gibb \&
Heaton (1993), see also notes under HH~24.

\vspace*{0.3cm}

{\bf HH 28/29} {\em (4 28, +17 58)}.  Original paper: Herbig
(1974). These are two rather bright objects, which form bow shocks in
the large outflow from L1551 IRS 5 starting in the HH~154 jet. CCD
images are presented by Snell et al. (1985), Strom et al. (1986),
Stocke et al. (1988), Graham \& Heyer (1990), Garnavich,
Noriega-Crespo, Green (1992), Fridlund, Liseau, Perryman (1993), Davis
et al. (1995) and Devine, Reipurth, Bally (1999). Infrared images are
presented by Davis et al. (1995).  Optical spectroscopy is discussed
by Strom, Grasdalen, Strom (1974) and Stocke et al. (1988).  Detailed
spectroscopy of HH~29 is analyzed by Fridlund, Liseau, Gullbring
(1998). Ultraviolet spectroscopy of HH 29 is presented by Cameron \&
Liseau (1990) and Liseau et al. (1996a).  The objects have large
proper motions in a direction away from IRS~5 (Cudworth \& Herbig
1979). More recent data suggest that HH~28/29 may instead originate in
the neighboring source L1551NE (Devine, Reipurth, Bally 1998).  The
molecular outflow from IRS~5 has an abrupt velocity change at HH~29
(Fridlund et al. 1984).  For references on the molecular outflow and
the source, see notes on the HH~154 jet.

\vspace*{0.3cm}

{\bf HH 30} {\em (4 28, +18 06)}.
Original paper: Herbig (1974). {\em Structure and CCD Images:} Mundt
\& Fried (1983), Cohen \& Jones (1987), Mundt, Ray, B\"uhrke (1988),
Mundt et al. (1990), Graham \& Heyer (1990), Mundt, Ray, Raga (1991),
L\'opez et al. (1995). {\em HST observations:} 
Burrows et al. (1996), Ray et al. (1996), Stapelfeldt et al. (1999a).
{\em Optical Spectroscopy:} Brugel, B\"ohm, Mannery (1981a), Cohen \&
Schmidt (1981), Mundt, Brugel, B\"uhrke (1987), Cohen \& Jones (1987),
Mundt et al. (1990), Raga et al. (1997).  
{\em Proper Motions:} Cudworth \& Herbig (1979),
Mundt et al. (1990), L\'opez et al. (1996), Burrows et al. (1996).  
{\em Source:} Cohen \&
Schwartz (1980), Vrba, Rydgren, Zak (1985), Cohen \& Schwartz (1987).
{\em Mm Data:} Calvet, Cant\'o, Rodr\'\i guez (1983).

\vspace*{0.3cm}

{\bf HH 31} {\em (4 25, +26 11)}.  Original paper: Herbig (1974). CCD
images are discussed by Strom et al. (1986). A likely energy source,
HH~31~IRS~2 (IRAS 04248+2612) was found by Cohen \& Schwartz (1983),
and further studied by Cohen et al.  (1984a), Cohen, Harvey, Schwartz
(1985) and Cohen \& Schwartz (1987).  A spectrum of a little nebula at
the location of the source (identified as knot D by Herbig 1974) by
Cohen \& Fuller (1985) showed little emission, but Strom et al. (1986)
found a southern emission line extension. G\'omez, Whitney, Kenyon
(1997) present deep [SII] images which reveal further faint HH knots
in the flow. Lucas \& Roche (1997) present near-infrared images of the
source and associated nebula, and Padgett et al. (1999) used
HST/NICMOS to image the nebula at high resolution and show that the
source is a binary with a separation of 0.16 arcsec. Kenyon et
al. (1998) suggest a spectral type of the source of M2.  Whitney,
Kenyon, G\'omez (1997) present near-infrared polarimetry of the
source. Moriarty-Schieven et al. (1994) measured the source at 1300
$\mu$m, and Dent, Matthews, Ward-Thompson (1998) at other sub-mm
wavelengths .  Limited $^{12}$CO data of Edwards \& Snell (1983)
revealed no high-velocity gas.

\vspace*{0.3cm}

{\bf HH 32} {\em (19 18, +10 56)}.
Original paper: Herbig (1974). {\em CCD Images:} Mundt, Stocke,
Stockman (1983), Hartigan, Mundt, Stocke (1986), Curiel et al. (1997).  
{\em Optical
Spectroscopy:} Dopita (1978a), Brugel, B\"ohm, Mannery (1981a,b),
Herbig \& Jones (1983), Solf, B\"ohm, Raga (1986), Hartigan, Mundt,
Stocke (1986).  {\em UV Spectroscopy:} B\"ohm \& B\"ohm-Vitense
(1984), Lee et al. (1988), Moro-Martin et al. (1996).
{\em IR Observations:} Zealey et
al. (1986), Zinnecker et al. (1989), Hodapp (1994), Davis,
Eisl\"offel, Smith (1996).  {\em Radio Continuum Emission:} Anglada et
al. (1992, 1998).  {\em Proper Motions:} Herbig \& Jones (1983).  {\em
Source:} AS353A (=V1352 Aql) was discovered by Merrill \& Burwell
(1950).  The optical spectrum of the star has been extensively
discussed by Cohen \& Kuhi (1979), Herbig \& Jones (1983), Mundt,
Stocke, Stockman (1983), Hartigan, Mundt, Stocke (1986), B\"ohm \&
Raga (1987) and Eisl\"offel, Solf, B\"ohm (1990).  Near-infrared
spectroscopy of AS 353A is discussed by Najita, Carr, Tokunaga (1996),
and Biscaya et al. (1997).
IR and sub-mm photometry is given by Cohen \& Schwartz (1983, 1987),
and Reipurth et al. (1993a). Edwards \& Snell (1982) report
high-velocity CO emission. {\em Various model calculations:} Raga,
B\"ohm, Solf (1986), Hartigan, Raymond, Hartmann (1987). See also HH
332.

\vspace*{0.3cm}

{\bf HH 33/40} {\em (5 32, $-$06 19)}.  HH~40 was discovered by Haro
(1953), who also later found HH~33 (see Herbig 1974).  HH 33 and 40
are physically connected with an emission-line filament.  Mundt et
al. (1984) suggest the HH objects form a jet, but Bally \& Devine
(1994) propose they are really a distant bow shock in the HH~34
flow. This is confirmed in a kinematic study based on radial
velocities and proper motions by Devine et al. (1997).  CCD images are
presented by Mundt et al.  (1984), Strom et al. (1986), Bally \&
Devine (1994), Eisl\"offel \& Mundt (1997) and Devine et al. (1997).
Optical spectroscopy is discussed by Dopita (1978a), Brugel, B\"ohm,
Mannery (1981a), Goodrich (1986a), Mundt, Brugel, B\"uhrke (1987) and
Devine et al. (1997). Infrared H$_2$ observations are discussed by
Elias (1980), Schwartz, Cohen, Williams (1987), Zinnecker et
al. (1989), and Zealey et al. (1992).  Heyer, Strom, Strom (1987)
suggest an alignment with magnetic field lines. No convincing energy
source has been found near HH~33/40 (Cohen \& Schwartz 1983, 1987), in
further support of the idea that the complex is driven by HH~34~IRS
(Bally \& Devine 1994). Edwards \& Snell (1983) found no high-velocity
gas in the region.

\vspace*{0.3cm}

{\bf HH 34} {\em (5 33, $-$06 29)}.  Discovered by Haro, see Herbig
(1974). HH 34, located in L1641 in Orion, is a large bright bow shock
in the approaching lobe of a major bipolar HH complex which includes a
very fine jet. This jet, the discovery of which was announced by
Reipurth (1985b), was studied in detail by Reipurth et al. (1986), who
present CCD images and low-dispersion spectrocopy. Further CCD images
were made by Raga \& Mateo (1988b), who resolved the width of the jet
knots. B\"uhrke, Mundt, Ray (1988) used CCD images and
medium-dispersion spectroscopy for their study, in which they also
pointed out a counter-bow shock, HH 34-North, placed symmetrically to
HH~34 on the other side of the source. Very high resolution images
were discussed by Raga, Mundt, Ray (1991). Further CCD images are
discussed by Eisl\"offel \& Mundt (1997) and Devine et al. (1997).
Ray et al. (1996) discuss brief HST exposures.  The existence of
multiple bow shocks in the blue lobe of the HH~34 flow was discussed
by Reipurth \& Heathcote (1992), pointing to eruptive events in the
driving source. Cohen \& Jones (1987) drew attention to the extremely
low H$\alpha$/[SII] ratio of the jet. High-resolution long-slit
spectroscopy was presented of the entire approaching lobe of the HH 34
system by Heathcote \& Reipurth (1992), and Fabry-Perot observations
of the HH~34 bow shock and jet were analyzed by Morse et al. (1992,
1993b). Further long-slit spectroscopy of the HH 34 jet is analyzed by
Bacciotti \& Eisl\"offel (1999).  Proper motion studies were discussed
by Heathcote \& Reipurth (1992), and Eisl\"offel \& Mundt (1992). The
optical polarization study of Scarrott (1988b) showed the reflection
nebulae in the blue lobe to be illuminated by the source. Stapelfeldt
et al.  (1991) noted that neither the HH 34 bow shocks nor the HH 34
jet emit in the infrared molecular hydrogen lines, but the jet was
mapped in the 1.644 $\mu$m line of [FeII].  With deeper H$_2$ images,
Stanke, McCaughrean, Zinnecker (1998) detected a few knots in the jet
plus a new infrared counter bow shock.  Zealey, Suters, Randall (1993)
and Moneti \& Reipurth (1995) present broadband infrared images of the
region. The driving source of the HH~34 complex was identified by
Reipurth et al. (1986), who gave optical/infrared photometry and
showed a red spectrum. Cohen et al. (1984) detected the source at 100
$\mu$m, Cohen \& Schwartz (1987) derived a luminosity of 45 L$_\odot$
from IRAS data, and Reipurth et al. (1993a) detected the cold dust
around the source at 1300 $\mu$m.  Further sub-millimeter photometry
is given by Dent, Matthew, Ward-Thompson (1998).  The source was also
detected with the VLA at 3.6 cm by Rodr\'\i guez \& Reipurth (1996).
Mm-observations of various molecular species are discussed by Reipurth
et al. (1986), Anglada et al. (1989), Cernicharo (1990), Rudolph \&
Welch (1992), Stapelfeldt \& Scoville (1993) and Davis \& Dent (1993).
VLA observations of ammonia are discussed by Anglada et al. (1995).  A
weak molecular outflow is detected by Chernin \& Masson (1995).  The
mass loss rate in the jet is estimated by Hartigan, Morse, Raymond
(1994), and Bacciotti, Chiuderi, Oliva (1995) interpret available
observations. Raga \& Noriega-Crespo (1998) present a variable
velocity jet model that is fitted to observations of the jet.  From a
large-field CCD imaging study, Bally \& Devine (1994) have suggested
that the HH~34 complex is much larger than previously thought,
including HH~173 and HH~86/87/88 in the blue lobe, and HH~126, HH~85
and HH~33/40 in the red lobe. Devine et al. (1997) confirmed this with
a detailed radial velocity and proper motion study. Also, Eisl\"offel
\& Mundt (1997) present CCD images that support the Bally \& Devine
(1994) scenario.

\vspace*{0.3cm}

{\bf HH 35} {\em (5 33, $-$06 43)}.
Herbig (1974) found this small elongated object and suggested it
originates in V380 Ori. CCD images are presented by Strom et al.
(1986) and Corcoran \& Ray (1995); the latter study also includes
spectroscopy. The Herbig Ae/Be star V380 Ori is discussed in detail by
Herbig (1960); see also Cohen \& Kuhi (1979), Finkenzeller \& Mundt
(1984) and Shevchenko (1994). The star is surrounded by a large
reflection nebula (e.g. Br\"uck 1974).  Edwards \& Snell (1984),
Levreault (1988) and Morgan et al. (1991) discuss high velocity gas
around the star. A companion to V380 Ori was found with a separation
of 0.17 arcsec by Leinert et al. (1994). 
The mass loss rate from infrared lines is derived by Nisini et al. (1995).
For further references to
V380 Ori see Herbig (1960) and Herbig \& Bell (1988).  See also notes
on HH~130 and HH~148.

\vspace*{0.3cm}

{\bf HH 36} {\em (5 34, $-$06 46)}.
Original paper: Herbig (1974). A small chain of HH knots south-east of
the HH 1/2 and V380 region. Corcoran \& Ray (1995) present CCD images,
and suggest that V851 Ori may be the driving source.

\vspace*{0.3cm}

{\bf HH 37} {\em (5 43, $-$00 06)}.  Original paper: Strom et al. (1986),
who present CCD images. This is a single HH object in the little group of
HH objects HH 20, 21 and 70 in the NGC~2068 region. It is no.37 of the list
of Strom et al. (1986), their Table~18. The nature of the nearby objects
18-42 and 18-43 of Strom et al. (1986) is unclear. All objects are seen on
the CCD images of Reipurth \& Graham (1988). Based on wide-field CCD
images, Eisl\"offel \& Mundt (1997) suggest that HH 37 may be part of a
giant bow shock (including HH 20/21 and HH 70) which originates in HH 24.

\vspace*{0.3cm}

{\bf HH 38} {\em (5 35, $-$07 13)}.  Originally found by Haro (see Herbig
1974). Also see notes for HH~43, which together with HH 38 forms a large HH
flow driven by HH 43 IRS1 = IRAS 05357$-$0710.

\vspace*{0.3cm}

{\bf HH 39} {\em (6 36, +08 54)}.  Original papers: Herbig
(1968,1974).  This is a small cluster of knots forming a bow shock in
a flow from R~Mon.  {\em Structure and CCD Imaging:} Jones \& Herbig
(1982), Brugel, Mundt, B\"uhrke (1984), Walsh \& Malin (1985), Mundt,
Brugel, B\"uhrke (1987), Schwartz \& Schultz (1992).  {\em
Spectroscopy:} Brugel, Mundt, B\"uhrke (1984), Walsh \& Malin (1985).
{\em Proper Motions:} Jones \& Herbig (1982).  {\em Source:} R~Mon and
its reflection nebula NGC~2261 has been extensively studied by many
authors, and the following is only a partial list of the literature:
Hubble (1916), Knox-Shaw (1916), Herbig (1960, 1968), Br\"uck (1974),
Stockton, Chesley, Chesley (1975), B\"ohm, Siegmund, Schwartz (1976b),
Greenstein et al. (1976,1979), Harvey, Thronson, Gatley (1979),
Bellingham \& Rossano (1980), Gething et al.  (1982), Cohen \&
Schwartz (1983), Persson et al. (1984), Aspin, McLean, Coyne (1985),
Cohen, Harvey, Schwartz (1985), Edwards et al. (1987), Warren-Smith,
Draper, Scarrott (1987), Menard, Bastien, Robert (1988), Lightfoot
(1989), Scarrott, Draper, Warren-Smith (1989), Yamashita et
al. (1989b), Hodapp (1990), Natta et al. (1993), Kelly, Rieke,
Campbell (1994), Hodapp (1994), Mannings (1994), Hamann et al. (1994),
Nisini et al. (1995), Close et al. (1997b), Corcoran \& Ray (1997),
Matsumura, Seki, Kawabata (1999).  {\em Mm Data:} Cant\'o et
al. (1981), Beckwith et al. (1984,1986), Sargent \& Beckwith (1987).

\vspace*{0.3cm}

{\bf HH 40} {\em (5 32, -06 20)}.
See notes for HH 33.

\vspace*{0.3cm}

{\bf HH 41/42} {\em (5 33, $-$05 05)}.
Original paper: Haro (1953). The little-studied objects, HH~41 and 42,
form, together with HH~128 and 129, a small cluster of HH objects in
the NGC 1976/77 region. Photographic plates of the region are
presented by Schwartz (1977a), Reipurth (1985a) and Ogura \& Walsh
(1991).  Reipurth, Bally, Devine (1997) present CCD images. Optical
spectroscopy of HH 42 is given by Schwartz et al. (1995).  Infrared
observations are discussed by Schwartz, Cohen, Williams (1987), Cohen
et al. (1988), Schwartz et al. (1995) and Schwartz, Burton, Herrman
(1997). It is suggested by Reipurth, Bally, Devine (1997) that HH
41/42 together with HH 128/129 forms the eastern lobe of a giant
bipolar outflow driven by IRAS 05329--0505; this source drives the HH
294 jet, and the western lobe contains HH 295.

\vspace*{0.3cm}

{\bf HH 43} {\em (5 35, $-$07 11)}.  Original paper: Haro (1953). {\em
Structure and CCD Images:} Herbig (1974), Strom et al. (1986),
Schwartz et al. (1988), Eisl\"offel \& Mundt (1997).  {\em Optical
Spectra:} Herbig (1957), Strom, Grasdalen, Strom (1974), Dopita
(1978a), Cohen \& Schmidt (1981), Dopita, Binette, Schwartz (1982),
B\"ohm, Brugel, Olmsted (1983), Schwartz, Dopita, Cohen (1985), B\"ohm
\& Solf (1990), Beck-Winchatz \& B\"ohm (1994), Beck-Winchatz, B\"ohm,
Noriega-Crespo (1996), Schwartz \& Greene (1999).  {\em Infrared
Observations:} Schwartz, Cohen, Williams (1987), Schwartz et
al. (1988), Cohen et al. (1988), Zinnecker et al. (1989), Gredel
(1994), Schwartz et al. (1995), Schwartz \& Greene (1999).  {\em
Ultraviolet Observations:} Schwartz (1983a), Schwartz, Dopita, Cohen
(1985), Lee et al. (1988), B\"ohm, Scott, Solf (1991), Moro-Martin et
al. (1996).  {\em Polarization:} Cohen \& Schmidt (1981).  {\em
Source:} Cohen \& Schwartz (1980, 1983, 1987), Cohen et al.  (1984a),
Cohen, Harvey, Schwartz (1985), Schwartz et al. (1988), Strom et
al. (1989), Reipurth et al. (1993a), Molinari, Liseau, Lorenzetti
(1993), Dent, Matthew, Ward-Thompson (1998).  The source is a binary
star (Gredel 1994, Moneti \& Reipurth 1995).  {\em Model
calculations:} Indebetouw \& Noriega-Crespo (1995) calculate various
shock parameters.  {\em Mm Data:} Loren, Evans, Knapp (1979), and
Anglada et al. (1989).

\vspace*{0.3cm}

{\bf HH 44} {\em (5 32, $-$05 12)}.
Discovered by Schwartz (1977a). Located close to the OMC-2 region.

\vspace*{0.3cm}

{\bf HH 45} {\em (5 33, $-$04 52)}.  Discovered by Schwartz (1977a). CCD
images and spectroscopy by Reipurth (1989b). It has a strong morphological
resemblance to a bow shock facing away from the OMC 3 region, where a
number of class 0/I sources are located (Chini et al. 1997a).

\vspace*{0.3cm}

{\bf HH 46/47} {\em (8 24, $-$50 50)}.  Discovered by Schwartz
(1977a,b). This is a major bipolar highly collimated Herbig-Haro jet
with several bow shocks and emanating from an infrared source embedded
in the Bok globule ESO 210-6A (= Sa~111 = DC~267.4-7.5). The globule
is part of the system of cometary globules in the Gum Nebula (Reipurth
1983).  {\em Structure and CCD imaging:} Bok (1978), Dopita (1978b),
Dopita, Schwartz, Evans (1982), Graham \& Elias (1983), Raga \& Mateo
(1987, 1988a), Hartigan, Raymond, Meaburn (1990), Reipurth \&
Heathcote (1991), Hartigan et al. (1993), Eisl\"offel \& Mundt (1994),
Heathcote et al. (1996).  {\em Optical spectroscopy:} Dopita
(1978a,b), Dopita, Schwartz, Evans (1982), Dopita, Binette, Schwartz
(1982), Graham \& Elias (1983), Meaburn \& Dyson (1987), Hartigan,
Raymond, Meaburn (1990), Reipurth \& Heathcote (1992), Hartigan et
al. (1993), Bacciotti \& Eisl\"offel (1999), Hartigan et al. (1999).
{\em Ultraviolet spectroscopy:} Schwartz (1983), Lee et al. (1988),
B\"ohm, Scott, Solf (1991), Moro-Martin et al. (1996), Hartigan et
al. (1999).  {\em Infrared observations:} Elias (1980), Graham \&
Elias (1983), Graham \& Heyer (1989), Wilking et al. (1990), Zealey,
Suters, Randall (1993), Eisl\"offel et al.  (1994), Curiel et
al. (1995), Micono et al. (1998).  {\em Proper motions:} Schwartz,
Jones, Sirk (1984), Eisl\"offel \& Mundt (1994), Micono et al. (1998).
{\em Reflection nebula:} Graham (1987), Scarrott \& Warren-Smith
(1988).  {\em Molecular outflow:} Chernin \& Masson (1991), Olberg,
Reipurth, Booth (1989, 1992), Codella, Bachiller, Reipurth (1999).
{\em Source:} Elias et al. (1982), Graham \& Elias (1983), Cohen et
al. (1984b), Emerson et al. (1984), Cohen, Dopita, Schwartz (1986b),
Graham \& Heyer(1989), Sahu, Sahu, Pottasch (1989), Reipurth \&
Heathcote (1991), Reipurth et al. (1993a), Molinari, Liseau,
Lorenzetti (1993), Dent, Matthew, Ward-Thompson (1998).  {\em
Globule:} Kuiper et al. (1987), Hodapp (1987), Sahu, Sahu, Pottasch
(1989), Olberg, Reipurth, Booth (1992).  {\em Shock structure and
modelling:} Hartigan (1989), Raga et al. (1990), Hartigan, Raymond,
Meaburn (1990), Morse et al. (1994), Raymond et al. (1994), Hartigan,
Morse, Raymond (1994).

\vspace*{0.3cm}

{\bf HH 48} {\em (11 03, $-$77 01)}.
Discovered by Schwartz (1977a). The object, which consists of two
knots, coincides with an infrared source (Elias 1980) and a weak IRAS
source 11030-7702 (Cohen \& Schwartz 1987). The source may be a faint
T Tauri star (Cohen, Dopita, Schwartz 1986b). No proper motion was
found by Schwartz, Jones, Sirk (1984).

\vspace*{0.3cm}

{\bf HH 49/50} {\em (11 04, $-$77 17)}.
Discovered by Schwartz (1977a). The two closely associated objects are
located in a high extinction region of the Cha I clouds, and are
illustrated by Schwartz, Jones, Sirk (1984), who find a very large and
similar proper motion for the two objects. Schwartz \& Dopita (1980)
have obtained spectrophotometric data. Combining radial velocities and
proper motions show a space motion close to the plane of the sky.
Cohen \& Schwartz (1987) suggest a low-luminosity far-infrared source
IRAS 11054--7706C, on the axis of the proper motion vectors, as the
energy source. Prusti et al. (1991) show this source to be multiple,
and identifies one of them, Ced~110-IRS4, as the energy source. It was
detected at 1300 $\mu$m by Reipurth et al. (1993a), and has a weak
molecular outflow (Mattila, Liljestr\"om, Toriseva 1989). A 1300
$\mu$m map by Reipurth, Nyman, Chini (1996) reveals a compact mm
continuum source just south of the sources detected by IRAS, and this
new object is a plausible driving source. Whittet et al. (1997) determine a
distance for Cha~I of 160 pc.

\vspace*{0.3cm}

{\bf HH 51} {\em (11 08, -76 08)}.
Discovered by Schwartz (1977a). Very faint object north of the Cha I
clouds. Schwartz, Jones, Sirk (1984) speculate that it is a
counterflow to HH 49/50.

\vspace*{0.3cm}

{\bf HH 52/53/54} {\em (12 52, $-$76 41)}.  Discovered by Schwartz
(1977a). The objects may form a giant fractured bow shock driven by an
embedded source IRAS 12496--7650 located fourteen arcmin to the
south-west. The source has a faint optical counterpart with the small
HH~274 object on the side towards the HH objects (Reipurth,
unpublished).  {\em Structure and CCD images:} Schwartz (1977a),
Schwartz, Jones, Sirk (1984), Sandell et al. (1987), Graham and Heyer
(1988).  {\em Optical spectroscopy:} Schwartz \& Dopita (1980), Graham
\& Hartigan (1988).  {\em Infrared observations:} Elias (1980),
Sandell et al. (1987), Zealey, Suters, Randall (1993), Gredel
(1994). {\em ISO observations:} Liseau et al. (1996b), Nisini et
al. (1996), Neufeld, Melnick, Harwit (1998).  {\em Source:} Cohen \&
Schwartz (1987), Hughes et al. (1989, 1991), Reipurth et al. (1993a),
Molinari, Liseau, Lorenzetti (1993), Henning et al. (1998).  {\em Mm
observations:} Knee (1992). Whittet et al. (1997) determine a distance
for Cha~II of 178 pc.

\vspace*{0.3cm}

{\bf HH 55} {\em (15 53, $-$37 42)}.
Discovered by Schwartz (1977a). The object consists of a compact knot
surrounded by a faint envelope (Heyer \& Graham 1990) centered in a 90
arcsec long very faint bipolar jet (Graham \& Chen 1994).
Spectra are
presented by Krautter, Reipurth, Eichendorf (1984), Cohen, Dopita,
Schwartz (1986b), and Heyer \& Graham (1990). The HH object is
coincident with a faint IRAS source 15533--3742 (Cohen \& Schwartz
1987), which appears to be a T~Tauri star (Cohen, Dopita, Schwartz
1986b, Heyer \& Graham 1990).

\vspace*{0.3cm}

{\bf HH 56} {\em (16 28, $-$44 48)}.  Discovered by Schwartz
(1977a). It is a bright bow shock in a bipolar collimated outflow
(Reipurth et al. 1997a). Optical spectra are presented by Schwartz \&
Dopita (1980), Wilking et al. (1990) detected it in molecular hydrogen
emission, and Gredel (1994) obtained infrared spectra.  Schwartz,
Jones, Sirk (1984) attempted a proper motion determination. A little
reflection nebula, Re~13, is illuminated by the energy source
(Reipurth 1981), which is detected in the infrared (Prusti et
al. 1993) and at 1.3 mm (Reipurth et al. 1993a). Spectra of Re~13 show
H$\alpha$ emission (Alvarez et al.  1986), Cohen, Dopita, Schwartz
1986a). Mm observations are presented by Alvarez et al. (1986), and a
molecular outflow has been mapped by Evans et al. (1994) and Reipurth
et al. (1997a). SiO emission has been detected by Codella, Bachiller,
Reipurth (1999).

\vspace*{0.3cm}

{\bf HH 57} {\em (16 28, $-$44 49)}.
Discovered by Schwartz (1977a). This is a small Herbig-Haro knot,
studied spectroscopically by Schwartz \& Dopita (1980). CCD images are
shown by Graham \& Frogel (1985), Reipurth (1985c), and Reipurth et
al. (1997a). A proper motion
determination was attempted by Schwartz, Jones, Sirk (1984). The energy
source is a bright near- and far-infrared (IRAS 16289--4449) source
(Elias 1980, Reipurth \& Wamsteker 1983, Cohen et al. 1984b, 1985,
Cohen \& Schwartz 1987, Prusti et al. 1993). Near-infrared photometry
is summarized by Molinari, Liseau, Lorenzetti (1993) and Reipurth et
al. (1997a). Graham (1983)
announced that a visible star had appeared at the source, which was
identified as an FU Orionis object by Graham \& Frogel (1985) and
Reipurth (1985c). A weak stellar absorption spectrum was seen by
Cohen, Dopita, Schwartz (1986a). The star is partly embedded and
surrounded by a reflection nebula (Graham \& Frogel 1985, Reipurth
1985c, Scarrott, Gledhill, Warren-Smith 1987). Circumstellar dust has
been detected at sub-mm wavelengths by Weintraub, Sandell, Duncan
(1991) and Reipurth et al. (1993a). The 3 $\mu$m water ice band was
detected by Graham \& Chen (1991), and further studied by Graham (1998).
Mm observations are presented by
Alvarez et al. (1986), and a molecular outflow has been mapped by
Evans et al. (1994) and Reipurth et al. (1997a). 
SiO emission has been detected by Codella, Bachiller,
Reipurth (1999).

\vspace*{0.3cm}

{\bf HH 58} {\em (5 28, $-$04 11)}.
Original paper: Reipurth \& Graham (1988), where a CCD image is shown.
The object consists of a northern and a southern group of knots. Cohen
(1990) suggests that IRAS 05283--0412 could be a possible energy
source.

\vspace*{0.3cm}

{\bf HH 59} {\em (5 29, $-$06 31)}.
Original paper: Reipurth \& Graham (1988), where a CCD image is shown.
The object is large and amorphous and located in the eastern outskirts
of the L1641 complex.

\vspace*{0.3cm}

{\bf HH 60} {\em (5 30, $-$06 28)}.
Original paper: Reipurth \& Graham (1988), where a CCD image is shown.
The object is a curved diffuse emission nebula only 5 arcmin NE of
HH~59, and they may be related.

\vspace*{0.3cm}

{\bf HH 61/62} {\em (5 33, $-$07 10)}.  Original paper: Reipurth \&
Graham (1988), where CCD images are presented. The two objects are
situated on a north-south line with a separation of 4 arcmin, and are
most likely related. HH 61 has a diffuse bow shape, while HH 62
consists of a little cluster of knots.  Ogura \& Walsh (1991) show a
photographic plate of the region (note that their knot D is
incorrectly identified), and present spectroscopy of HH 61. Cohen
(1990) suggests that IRAS 05339--0708C could be a possible energy
source for HH 61, but Reipurth, Devine, Bally (1998) believe the
object is part of a giant HH flow from the L1641-N region.

\vspace*{0.3cm}

{\bf HH 63} {\em (5 34, $-$04 27)}.
Original paper: Reipurth \& Graham (1988), where a CCD image is given.
It is a small group of moderately bright HH knots embedded in a faint
bow shaped nebula. Located next to the emission line binary star P2441.


\vspace*{0.3cm}

{\bf HH 64} {\em (5 35, $-$07 07)}.
Original paper: Reipurth \& Graham (1988), where a CCD image is
shown. It consists of two faint closely attached knots, and is located
in the same region of L1641 as HH 38 and HH 43. Cohen (1990) suggests
that IRAS 05355--0709C could be a possible energy source. Anglada et
al. (1989) has detected a dense ammonia condensation, which they
suggest may contain an energy source.

\vspace*{0.3cm}

{\bf HH 65} {\em (5 37, $-$07 26)}.  Original paper: Reipurth \&
Graham (1988), where a CCD image is shown.  It is a small faint
nebula, located in the red lobe of the molecular outflow driven by
Re50 IRS = IRAS 05380--0728 (Reipurth \& Bally 1986). The outflow was
also found by Fukui et al. (1986) and further studied by Morgan et
al. (1991). The source illuminates the large variable reflection
nebula Re50 (Reipurth 1985a).  An optical polarization study of the
Re50 nebula has been done by Scarrott \& Wolstencroft (1988), and
infrared observations of the source and nebula are presented by Heyer
et al. (1990), Casali (1991) and Hodapp (1994).  Near-infrared
polarimetry is discussed by Colom\'e, Di Francesco, Harvey (1996).
Far-infrared maps are presented by Di~Francesco et al. (1998).  Strom
\& Strom (1993) suggest that Re50 IRS is an FU Orionis star. It was
detected at 6 cm at the VLA (Morgan, Snell, Strom 1990), at 1300
$\mu$m by Reipurth et al. (1993a), and at several sub-mm wavelengths
by Zavagno et al. (1997) and Dent, Matthew, Ward-Thompson (1998).

\vspace*{0.3cm}

{\bf HH 66} {\em (5 37, $-$02 04)}.
Original paper: Reipurth \& Graham (1988), where a CCD image is
presented. The object consists of two knots, and is located in the HII
region IC434 in the western low extinction region of the L1630 cloud.

\vspace*{0.3cm}

{\bf HH 67} {\em (5 38, $-$01 48)}.
Original paper: Reipurth \& Graham (1988), where a CCD image is
presented. The object consists of a little chain of compact knots,
located in a very opaque area of L1630 at the northwestern edge of NGC
2024. There are several nearby IRAS sources, including IRAS
05386--0149C (Cohen 1990).

\vspace*{0.3cm}

{\bf HH 68/69} {\em (5 39, $-$06 29)}.
Original paper: Reipurth \& Graham (1988), where CCD images are shown.
This is a chain of three groups of knots, located with equidistant
spacing on a well defined straight line. A faint red star is found
underneath the HH 68b knot. HH 68c and HH 69 resemble small bow
shocks. The energy source is most probably located on the flow axis
somewhere to the NNW of HH 68c and HH 69. Cohen (1990) suggests
separate driving sources for HH 68 and HH 69.

\vspace*{0.3cm}

{\bf HH 70} {\em (5 43, $-$00 06)}.  Original paper: Reipurth \& Graham
(1988), who show H$\alpha$ and [SII] CCD images. The object is a small knot
among a group of other HH knots, including HH~20 and 21. The region is also
discussed by Strom et al. (1986). Based on wide-field CCD images,
Eisl\"offel \& Mundt (1997) suggest that HH 70 is part of a giant bow
shock, which includes HH 20/21 and HH 37, and originates in HH 24.

\vspace*{0.3cm}

{\bf HH 71} {\em (5 44, +00 39)}.  Original paper: Reipurth \& Graham
(1988), who show a CCD image. It consists of two closely spaced knots
and a faint diffuse tail, and is located in a region active in
low-mass star formation. Cohen (1990) discusses several nearby young
stars as potential driving sources.  See also notes for HH~471-474.

\vspace*{0.3cm}

{\bf HH 72} {\em (7 18, $-$23 56)}.
Original paper: Reipurth \& Graham (1988), who present a large-field
Schmidt plate, an H$\alpha$ CCD image and a low-dispersion spectrum.
This is a small chain of HH knots emanating from a bright-rimmed Bok
globule, which is illuminated by the young OB cluster NGC~2362. The
energy source is the nearby bright class I IRAS source 07180--2356
embedded in the globule. It was detected at 1300 $\mu$m by Reipurth et
al. (1993a). Cohen (1990) estimates a luminosity of 280 L$_\odot$.
The source drives a molecular outflow (Schwartz, Gee, Huang 1988).  An
H$_2$O maser was detected by Wouterloot, Brand, Fiegle (1993).  Hodapp
(1994) presents a wide field K' band image of the region.  In a
detailed H$_2$ imaging study, Davis et al. (1997a) found a long,
winding and bipolar chain of H$_2$ knots centered on the IRAS source,
of which the three easternmost knots correspond to the optically
visible HH objects.

\vspace*{0.3cm}

{\bf HH 73} {\em (9 00, $-$44 39)}.
Original paper: Reipurth \& Graham (1988), who present CCD images.
This is a 29 arcsec long, finely collimated HH flow located one arcmin
south of a PMS binary illuminating the reflection nebula Re6. It
probably belongs to the Vela star forming complex at a distance of
about 700 pc (Liseau et al. 1992).

\vspace*{0.3cm}


{\bf HH 74} {\em (9 00, $-$44 37)}.
Original paper: Reipurth \& Graham (1988), who show CCD images. This
is a single HH knot located about 20 arcsec north of a PMS binary
illuminating the reflection nebula Re6, which could be the energy
source.

\vspace*{0.3cm}

{\bf HH 75} {\em (9 09, $-$45 30)}.
Original paper: Reipurth \& Graham (1988), who present a CCD image and
a low-dispersion spectrum. This is a large complex of many rather
bright HH knots. It probably is part of the Vela star forming complex
(Liseau et al. 1992). Cohen (1990) suggests that IRAS 09094--4522 could
be the energy source.

\vspace*{0.3cm}

{\bf HH 76} {\em (14 56, $-$62 52)}.  Original paper: Reipurth \&
Graham (1988), who show a CCD image. This object consists of two
compact HH knots with sub-structure. They are lying on a line through
the nearby IRAS source 14563--6250, which is most probably the energy
source (Cohen 1990). It was detected in the 1300 $\mu$m survey of
Reipurth et al. (1993a). The distance of 1 kpc is very
uncertain. Bally et al. (1999) present a millimeter study of the
Circinus cloud complex.

\vspace*{0.3cm}

{\bf HH 77} {\em (14 56, $-$62 55)}.
Original paper: Reipurth \& Graham (1988), who show CCD images. This
is a small curved object located in a region of nebulous stars and
several IRAS sources. Cohen (1990) suggests IRAS 14564--6253 as the
energy source. Bally et al. (1999) present a millimeter study of the
Circinus cloud complex.


\vspace*{0.3cm}

{\bf HH 78} {\em (16 05, $-$38 57)}.
Original paper: Reipurth \& Graham (1988), where a CCD image and a
low-dispersion spectrum are presented. It is a faint knot with a
diffuse tail, located in a region with many H$\alpha$ emission stars
in the Lupus 3 association. Graham \& Heyer (1988) point out that
HH~78 lies close to the axis of the HH~228 (= Th28) jet complex.

\vspace*{0.3cm}

{\bf HH 79} {\em (16 23, $-$24 13)}.  Original paper: Reipurth \& Graham
(1988), who present a large-scale photographic plate. It is located in the
dense region of the $\rho$ Ophiuchi cloud core, which is very active in
star formation. It is a small, highly structured object. Two embedded
sources are found nearby, GSS 39 and Source 1. Wilking et al. (1997a) show
it on a wide-field CCD image, and G\'omez, Whitney, Wood (1998) find
another HH knot, HH 79b, nearby.

\vspace*{0.3cm}

{\bf HH 80/81} {\em (18 16, $-$20 53)}.  Original paper: Reipurth \& Graham
(1988), who present a CCD image and low-dispersion spectra. HH 80 has a
bright core and is associated with a cluster of HH knots, whereas HH~81 is
more isolated. Both HH~80 and 81 belong among the brightest HH objects in
the sky, and at an assumed distance of 1700 pc they are the intrinsically
most luminous HH objects known. Heathcote, Reipurth, Raga (1998) present
detailed CCD images, both groundbased and from HST, high-resolution
spectroscopy and a proper motion study. A line drawn through the objects
intersects the 16000 L$_\odot$ embedded IRAS source 18162--2048, which is
the driving source. Rodr\'\i guez et al.  (1980) detected a compact HII
region there, as well as OH and H$_2$O masers, and the source was detected
at 1300 $\mu$m by Reipurth et al.  (1993a). Rodr\'\i guez \& Reipurth
(1989) detected both HH objects in radio continuum and found the source to
be elongated towards the HH objects. Higher resolution observations at 6 cm
and 3.6 cm by Mart\'\i , Rodr\'\i guez, Reipurth (1993) revealed a highly
collimated bipolar radio continuum jet emanating from the source. Large
proper motions and ejection of new knots in the radio jet were reported by
Mart\'\i, Rodr\'\i guez, Reipurth (1995, 1998). On the opposite side of the
source with respect to HH~80/81 they found a resolved object, HH~80-North,
with the same negative spectral index as HH~80 and 81.  Ammonia was found
downstream from HH 80-North by Girart et al. (1994), and this region was
studied further in HCO$^+$ and $^{13}$CO by Girart, Estalella, Ho (1998).
G\'omez, Rodr\'\i guez, Mart\'\i~(1995) conclude 
that the thermal jet and the nearby H$_2$O
maser are driven by different sources.  Next to the source there is a small
nebula, GGD~27 (Gyulbudaghian, Glushkov, Denisyuk 1978), which was shown to
be a reflection nebula by Hartigan \& Lada (1985). Yamashita et al. (1987a)
found a large infrared reflection nebula, coincident with a large molecular
outflow (Yamashita et al. 1989a). A dense CS disk was found around the HH
driving source perpendicular to the outflow direction by Yamashita et
al. (1990). Aperture synthesis observations by Yamashita et al. (1991)
revealed three unresolved peaks. Aspin et al. (1991) performed
near-infrared imaging and spectroscopy of the source region, and Aspin \&
Geballe (1992) did mid-infrared spectroscopy, finding evidence for a
cluster of sources. Aspin (1994) found extended infrared CO emission around
the source. Aspin et al. (1994) detected the source with 4.7 $\mu$m
imaging. Stecklum et al. (1997) present high resolution imaging at several
infrared wavelengths.  McCutcheon et al. (1995) present maps at 450, 800
and 1100 $\mu$m, and Chini et al. (1997b) at 1300 $\mu$m.  Greaves,
Holland, Ward-Thompson (1997) present 800 $\mu$m polarimetry of the source.

\vspace*{0.3cm}

{\bf HH 82} {\em (18 57, $-$37 01)}.  Original papers: Strom et
al. (1986) and Reipurth \& Graham (1988), both of which present CCD
images. Two groups of HH knots are found on a line straight east of
S~CrA. This star is a close visual binary (Joy \& van Biesbrock 1944)
and Strom et al. (1986) suspect that the fainter companion may be the
driving source. S~CrA has been studied spectroscopically in detail
(e.g. Bertout et al. 1982, Appenzeller, Jankovics, \"Ostreicher 1984,
Appenzeller, Jankovics, Jetter 1986 and references therein). Najita,
Carr, Tokunaga (1996) and Prato \& Simon (1997) present a Br$\gamma$
spectrum of S CrA.  Photometric variability is discussed by Bellingham
\& Rossano (1980). The star is detected in X-rays by Carkner, Kozak,
Feigelson (1998).

\vspace*{0.3cm}

{\bf HH 83} {\em (5 31, $-$06 31)}.  Original papers: Reipurth
(1985a,1989b). This is a well collimated jet with a bow shock, a
counterflow and a bright infrared source (IRAS 05311--0631), which is
associated with a reflection nebula, where the jet breaks out of the
cloud. Designations of knots are defined by Reipurth
(1989b). Spectroscopic observations are presented by Reipurth (1989b)
and Ogura \& Walsh (1991). CCD images are discussed by Reipurth
(1989b) and Mundt, Ray, Raga (1991). The source was observed in the
near-infrared by Reipurth (1989b) and Moneti \& Reipurth (1995), at
1300 $\mu$m by Reipurth et al. (1993a) and at other sub-millimeter
wavelengths by Dent, Matthew, Ward-Thompson (1998), and was detected
at 3.6 cm by Rodr\'\i guez \& Reipurth (1998).  A polarization study
of the reflection nebula was done by Rolph, Scarrott, Wolstencroft
(1990). Mm-observations are discussed by Bally, Castets, Duvert
(1994), Nakano et al. (1994), Miesch \& Bally (1994), and Anglada,
Sep\'ulveda, G\'omez (1997). See also notes for HH 84.

\vspace*{0.3cm}

{\bf HH 84} {\em (5 31, $-$06 35)}.
Original papers: Reipurth (1985a,1989b). This is a large chain of
relatively bright HH knots in a small cloud at the edge of the L1641
complex. The CCD image of Reipurth (1989b) shows a multitude of knots
on a fairly well defined line, suggesting it could be a jet, but no
energy source has been found. Low-dispersion spectra are given by
Reipurth (1989b). A search for $^{12}$CO wings was done by Morgan et
al. (1991). Anglada, Sep\'ulveda, G\'omez (1997) detect a nearby
ammonia core. Reipurth, Bally, Devine (1997) suggest that HH 84 forms
a large distant bow shock in the HH 83 flow.

\vspace*{0.3cm}

{\bf HH 85} {\em (5 32, $-$06 22)}.
Original papers: Reipurth (1985a,1989b). The CCD image of Reipurth
(1989b) shows a long chain of knots, which resembles a finely
collimated jet. Bally \& Devine (1994), however, suggest it is part of
a large bow shock in the red lobe of the HH~34 flow, and this has been
confirmed in a kinematic study by Devine et al. (1997).  Low
dispersion spectra are presented by Reipurth (1989b). The positions
listed by Reipurth (1989b) for HH 85 are in error, and are corrected
in Bally \& Devine (1994).

\vspace*{0.3cm}

{\bf HH 86/87/88} {\em (5 33, $-$06 39)}.
Original papers: Reipurth (1985a,1989b). The CCD image of Reipurth
(1989b) shows the three objects to be closely associated and have
complex sub-structure. Bally \& Devine (1994) suggest that 
they form a southern bow shock of
the HH 34 complex, to which HH~33/40 is the equivalent northern
counterpart in this major outflow region. This has been confirmed in a
kinematic study by Devine et al. (1997).  Low-dispersion spectra are
given by Reipurth (1989b). 
Stanke, McCaughrean, Zinnecker (1998) detect the objects at 2.12 $\mu$m (SMZ 26A,B). Anglada, Sep\'ulveda, G\'omez (1997) map a
nearby ammonia core.

\vspace*{0.3cm}

{\bf HH 89} {\em (5 35, $-$06 47)}.
Original paper: Reipurth (1985a). This object consists of two HH knots
and a reflection nebula. Moneti \& Reipurth (1995) found a
near-infrared source next to the reflection nebula.

\vspace*{0.3cm}

{\bf HH 90/91} {\em (5 39, $-$01 15)}.
Original paper: Reipurth (1985a). A detailed optical/infrared/mm study
is presented by Gredel, Reipurth, Heathcote (1992). HH~90 is a large
outlying bow shock, whereas HH~91 consists of several oppositely
facing bow shocks moving away from a central emission region, which
may contain a faint near-infrared source. The central part of HH~91 is
very intense in near-infrared H$_2$ emission. A K-band image is shown
by Moneti \& Reipurth (1995), and H$_2$ images are presented by Davis,
Mundt, Eisl\"offel (1994). Smith (1994) interprets the near-infrared
spectra in terms of a J-shock.

\vspace*{0.3cm}

{\bf HH 92} {\em (5 39, $-$01 19)}.
Original paper: Reipurth (1985a). CCD images show this to be a little
chain of faint HH knots in the L1630 cloud
(Reipurth, unpublished).

\vspace*{0.3cm}

{\bf HH 93} {\em (5 40, $-$01 27)}.
Original paper: Reipurth (1985a). CCD images show this to be a little
group of faint HH knots (Reipurth, unpublished).

\vspace*{0.3cm}

{\bf HH 94/95} {\em (5 41, $-$02 37)}.
Original papers: Reipurth (1985a,1989b). CCD images and low-dispersion
spectra are given by Reipurth (1989b), who suggested that HH~94 is a
bent HH jet. This idea no longer appears tenable. Rather, HH~94 and
HH~95 are probably bow shocks in a large bipolar outflow. Curiel et
al. (1989a) found a radio continuum source located precisely mid-way
between the two HH objects, which is a likely energy source.

\vspace*{0.3cm}

{\bf HH 96/97/98} {\em (18 58, $-$37 04)}.
Original paper: Hartigan \& Graham (1987), who show a large-scale
photographic plate and obtained spectra. HH~96 and 97 are small HH
knots on the line between HH~100 and HH~101 and they are, like these
objects, blueshifted. HH~98 is on the same line, but on the opposite 
side of the source. See also notes for HH~100.

\vspace*{0.3cm}

{\bf HH 99} {\em (18 58, $-$36 59)}.  Original paper: Cohen et
al. (1984b). Two small knots in the HH~100 flow in the red
north-eastern lobe. Proper motions by Schwartz, Jones, Sirk (1984)
suggest an origin near HH~100 IRS. Spectroscopy by Hartigan \& Graham
(1987). Molecular hydrogen emission detected by Wilking et al. (1990),
and infrared spectra obtained by Gredel (1994).  Infrared H$_2$ and
[FeII] images are presented by Wilking et al. (1997b) who suggest that
HH 99 may be driven by IRS 9.  See also notes for HH~100.


\vspace*{0.3cm}

{\bf HH 100} {\em (18 58, $-$37 02)}.  Original papers: Strom, Strom,
Grasdalen (1974), Strom, Grasdalen, Strom (1974). This is an HH object
surrounded by a large highly structured reflection nebula, seen in the
plates and CCD images of Hartigan \& Lada (1985), Strom et al. (1986), and
Hartigan \& Graham (1987). Polarization measurements of the reflection
nebula have been done by Vrba, Strom, Strom (1975) and Scarrott et
al. (1987), and Graham (1993) reports changes in its
morphology. Spectroscopy is discussed by Strom, Grasdalen, Strom (1974). A
large molecular outflow was mapped by Levreault (1988) and Anderson et
al. (1997), and Loren (1979), Anglada et al. (1989) and Harju et al. (1993)
mapped various molecular species in the region. The energy source, HH~100
IRS, was discovered by Strom, Strom, Grasdalen (1974) and Glass \& Penston
(1975); it is highly variable (Axon et al. 1982, Reipurth \& Wamsteker
1983, (see Molinari, Liseau, Lorenzetti 1993 for a summary of infrared
observations), and was detected in the far-infrared by Cohen et
al. (1984b), in the radio continuum at 6 cm by Brown (1987), and at 1300
$\mu$m by Reipurth et al. (1993a). Spectroscopy of the reflection nebula
shows the source to be an active T~Tauri star (Cohen, Dopita, Schwartz
1986b). Near-infrared spectroscopy is given by Greene \& Lada (1996b).
Strong 3 $\mu$m water-ice absorption has been observed towards the source
(Whittet \& Blades 1980, Graham \& Chen 1991, Chen \& Graham 1993, Tanaka
et al. 1994, Graham 1998). Other absorption features are discussed by 
Whittet et al. (1996) and Chiar et al. (1998). A dust model for HH~100 IRS
is presented by Siebenmorgen \& Gredel (1997).

\vspace*{0.3cm}

{\bf HH 101} {\em (18 58, $-$37 07)}.
Discovered by Strom, Grasdalen, Strom (1974). This is a large bow
shock in the blue lobe of the HH 100 flow. Structure and CCD images
are discussed by Morgan et al. (1984), Hartigan \& Lada (1985),
Reipurth (1985c), Strom et al. (1986), Hartigan \& Graham (1987).
Proper motions are directed away from the driving source HH~100 IRS
(Schwartz, Jones, Sirk 1984). Spectroscopy is analyzed by Strom,
Grasdalen, Strom (1974), Dopita (1978a) and Schwartz (1981). 
H$_2$ emission was
detected by Brown et al. (1983), and HH~101 was also detected in the
radio continuum at 6 cm (Brown 1987). The bow shock nature of HH 101
is discussed by Hartigan (1989).

\vspace*{0.3cm}

{\bf HH 102} {\em (4 28, +18 00)}.
Original paper: Strom, Grasdalen, Strom (1974). This is not an HH
object, but a large amorphous reflection nebula illuminated by the
L1551 IRS 5 source. It is further discussed by e.g. Cudworth \& Herbig
(1979), Draper, Warren-Smith, Scarrott (1985b) and Graham \& Heyer
(1990).

\vspace*{0.3cm}

{\bf HH 103} {\em (21 41, +65 49)}.
Original paper: Strom, Grasdalen, Strom (1974). This is the brightest
HH object in the very complex star forming region around NGC 7129,
which is rich in HH objects. It is a large C-shaped object connected
to HH 232 (formerly GGD 32) with faint knots and filamentary emission
(Eiroa, G\'omez de Castro, Miranda 1992). CCD images are shown by
Hartigan \& Lada (1985), Strom et al (1986), Eiroa, G\'omez de Castro,
Miranda (1992), and Goodrich (1993). Spectra are discussed by Strom,
Grasdalen, Strom (1974), Cohen \& Fuller (1985) and Magakyan et
al. (1994). Proper motion is measured by Ray et al. (1990). King \&
Scarrott (1981) did not measure any polarization in the
object. Wilking et al. (1990) detected H$_2$ in HH~103. Cohen \&
Schwartz (1983) did an infrared search for an energy source.  Further
references on the NGC~7129 region are given in the notes to the HH~167
jet.


\vspace*{0.3cm}

{\bf HH 104} {\em (18 58, $-$37 01)}.  Original papers: Schwartz,
Jones, Sirk (1984) and Graham (1993). This HH flow contains four HH
knots located pair-wise and symmetrically on a straight line through
R~CrA. HH~104A,B form the eastern lobe (Schwartz, Jones, Sirk 1984,
Strom et al. 1986, Hartigan \& Graham 1987), and HH~104C,D form the
western lobe (Graham 1993). The latter reference gives astrometry of
all four objects. HH~104A was detected in molecular hydrogen by
Wilking et al. (1990), and Wilking et al. (1997b) present infrared
H$_2$ and [FeII] images.  A molecular outflow was mapped by Levreault
(1988) and Anderson et al. (1997). R~CrA is a Herbig Ae/Be star (e.g.
Herbig 1960), and is surrounded by a large reflection nebula (e.g.
Graham \& Phillips 1987, Graham 1989) and is located in a large cloud
core (e.g. Harju et al. 1993). Far-infrared photometry is reported by
Cruz-Gonzalez, McBreen, Fazio (1984). Further references to
observations of R CrA is given in Herbig \& Bell (1988).

\vspace*{0.3cm}

{\bf HH 105} {\em (21 42, +65 54)}.  Original paper: Hartigan \& Lada
(1985). This is a faint HH object in the NGC~7129 region. CCD images are
presented by Hartigan \& Lada (1985), Strom et al. (1986), Ray (1987),
Eiroa, G\'omez de Castro, Miranda (1992), and Goodrich (1993). Spectroscopy
is discussed by Magakyan \& Movsesyan (1997a).  The object was detected in
H$_2$ by Wilking et al. (1990). Cohen \& Schwartz (1983) did an infrared
search for an energy source.

\vspace*{0.3cm}

{\bf HH 106/107} {\em (18 27, +01 18)}.  Original paper: Reipurth \&
Eiroa (1992), who present CCD images.  HH~106 has a bow shock
morphology. Gredel (1994) did infrared spectroscopy. HH~107 is larger
and brighter and has a complex structure. In a dense cloud region in
between the two objects one finds the faint H$\alpha$ emission star
ESO~H$\alpha$ 279 (= IRAS 18269+0116), which is the presumed energy
source. It was detected at 1300 $\mu$m by Reipurth et al. (1993a), and
has been studied in detail at optical and infrared wavelengths by
Aspin, Reipurth, Lehmann (1994).  Additional CCD images are presented
by Davis et al. (1999) and Ziener \& Eisl\"offel (1999). For
references to star formation in Serpens see notes for HH~455.

\vspace*{0.3cm}

{\bf HH 108/109} {\em (18 33, $-$00 37)}.
Original paper: Reipurth \& Eiroa (1992), who present CCD images. The
HH objects are only an arcminute apart and are lying on a line through
the nearby IRAS source 18331--0035, which was detected at 1300 $\mu$m
by Reipurth et al. (1993a). Chini et al. (1997b) mapped the region at
1300 $\mu$m, and detected the IRAS source plus a nearby sub-mm
continuum source, either of which could be the driving source.

\vspace*{0.3cm}

{\bf HH 110} {\em (5 48, +02 54)}.  Original reference: Reipurth \&
Olberg (1991). This is a major collimated HH flow, with a rich
sub-structure of knots and a flow-pattern with graceful curves. CCD
images, spectroscopy and mm-observations are discussed by Reipurth \&
Olberg (1991).  Davis, Mundt, Eisl\"offel (1994) and Noriega-Crespo et
al. (1996) present infrared H$_2$ images.  Reipurth, Raga, Heathcote
(1995) present deep large-field interference-filter CCD images which
reveal the presence of another fainter HH flow, HH 270, pointing
towards the apex of HH 110. It is argued that HH 110 is the result of
a grazing collision of the HH 270 flow with a cloud core.
Alternatively, Hurka, Schmid-Burgk, Hardee (1999) consider a
deflection by an abient magnetic field.  The source of HH~270/110 was
detected at 3.6 cm by Rodr\'\i guez et al. (1998a).  Less than an
arcminute west of the apex of HH~110 there is an IRAS source
05487+0255 studied by, among others, Garnavich et al. (1997).

\vspace*{0.3cm}

{\bf HH 111} {\em (5 49, +02 47)}.  Original reference: Reipurth
(1989a). This is a major bipolar and highly collimated Herbig-Haro
complex with a very fine jet and multiple bow shocks. Various parts of
the HH flow have been imaged by Reipurth (1989a), Reipurth, Raga,
Heathcote (1992), and Morse et al.  (1993a). HST images are analyzed
by Reipurth et al. (1997b). Spectra are discussed by Reipurth (1989a),
Morse et al.  (1993a,b), Noriega-Crespo, Garnavich, Raga (1993) and
Reipurth et al. (1997b). High proper motions are found for all parts
of the jet complex (Reipurth, Raga, Heathcote 1992), directed away
from the energy source HH~111 VLA (= IRAS 05491+0247), which is also
detected at 1300 $\mu$m (Reipurth et al. 1993a) and at other
sub-millimeter wavelengths (Dent, Matthew, Ward-Thompson 1998), and as
a 3.6 cm and 2 cm VLA source (Rodr\'\i guez \& Reipurth 1994, Anglada
et al. 1998). A small one-sided radio continuum jet emanates from the
VLA source in the direction of the optical HH jet. A near-infrared
reflection nebula is slightly displaced from the VLA source.  A
counter-jet has been found in the optical by Reipurth, Raga, Heathcote
(1992) and in the infrared by Gredel \& Reipurth (1994) and Davis,
Mundt, Eisl\"offel (1994). Reipurth, Bally, Devine (1997) present
wide-field CCD images, which in addition to finding further knots in
the counterflow demonstrate that HH 113 and HH 311 are distant bow
shocks with proper motions directed away from the HH 111 source; the
HH 111 complex thus spans one degree on the sky, corresponding to a
physical dimension of 7.7 pc.  A major molecular outflow is found
along the jet-axis (Reipurth \& Olberg 1991). High spatial resolution
CO observations by Cernicharo \& Reipurth (1996) reveal a well
collimated molecular jet in the blue lobe, and the presence of three
more distant high-velocity bullets on the jet axis. Mm interferometer
data resolve the blue lobe into a tubular cavity (Reipurth \&
Cernicharo 1995, Nagar et al. 1997, Cernicharo, Neri, Reipurth 1999)
Near-infrared images and spectroscopy are discussed by Gredel \&
Reipurth (1993), who also find a second bipolar infrared jet, HH~121,
emanating from the source, suggesting that it is a close
binary. Proper motions of the H$_2$ knots are discussed by Coppin,
Davis, Micono (1998).  Stapelfeldt \& Scoville (1993) find evidence of
a circumstellar disk around the source based on $^{13}$CO
interferometer observations. Yang et al. (1997) detect a disk
perpendicular to the jet axis in interferometer observations in CS,
which suggest both rotation and infall.  Hartigan, Morse, Raymond
(1994) estimate the mass loss rate through the jet, and Bacciotti,
Chiuderi, Oliva (1995) interpret available observations.  Hodapp
(1994) shows the whole region in a large-field K$'$ band image.

\vspace*{0.3cm}

{\bf HH 112} {\em (5 49, +02 59)}.
Original paper: Reipurth \& Olberg (1991), who show a CCD image. It is
a group of very faint HH knots.

\vspace*{0.3cm}

{\bf HH 113} {\em (5 50, +02 42)}.
Original paper: Reipurth \& Olberg (1991). A large complex of HH
knots, which forms a giant bow shock in the red lobe of the HH 111
flow. Reipurth, Bally, Devine (1997) present CCD images and a proper
motion determination. See also notes for HH 111.

\vspace*{0.3cm}

{\bf HH 114/115} {\em (5 16, +07 08)}.  Original paper: Reipurth,
Bally, Devine (1997). This is a very large bipolar HH complex, with a
projected extent of 2.5 pc. It is probably driven by the IRAS source
05155+0707, located mid-way between the lobes of the HH flow and an
associated molecular outflow, although another close-by class 0 source
was detected at 1300 $\mu$m by Chini et al. (1997b), which could also
be the driving source. Both sources were detected with the VLA at 3.6
cm (Rodr\'\i guez \& Reipurth 1996).  The IRAS source was observed at
sub-millimeter wavelengths by Dent, Matthew, Ward-Thompson (1998).
See also notes for HH 328 and HH 329.

\vspace*{0.3cm}

{\bf HH 116} {\em (5 49, +08 24)}.
Original paper: Reipurth, Bally, Heathcote (1999). This is a small HH object
located at the edge of the L1598 cloud close to the class I IRAS
source 05494+0820. Hodapp (1994) presents a K$'$ band image of this
source. Fukui (1989) reports a molecular outflow in this region.

\vspace*{0.3cm}

{\bf HH 117/118} {\em (5 49, +08 09)}.
Original paper: Reipurth, Bally, Heathcote (1999). A bipolar HH complex
centered on IRAS 05496+0812. Schwartz, Gee, Huang (1988) has reported
a molecular outflow from the same source. The IRAS source has been
imaged in the K$'$ band by Hodapp (1994), and was detected at 3.6 cm by
Rodr\'\i guez \& Reipurth (1998).

\vspace*{0.3cm}

{\bf HH 119} {\em (19 34, +07 27)}.  Original papers: Vrba et
al. (1986), Reipurth, Heathcote, Vrba (1992).  This is a chain of
three little HH objects located on a line through the cold central
source of the Bok globule B335, with HH~119A,B in the western red lobe
of the associated molecular outflow and HH~119C in the eastern blue
lobe, and proper motions in opposite directions away from the source
(Reipurth, Heathcote, Vrba 1992).  Deep near-infrared images are
presented by Hodapp (1998).  ISO-LWS spectra were obtained of the HH
objects by Nisini et al. (1999).  The molecular outflow has been
studied by, among others, Frerking \& Langer (1982), Goldsmith et
al. (1984), Langer, Frerking, Wilson (1986), Davidson (1987), Cabrit,
Goldsmith, Snell (1988), Moriarty-Schieven \& Snell (1989), Hirano et
al. (1988,1992) and Chandler \& Sargent (1993).  The source B335 IRS
(= IRAS 19345+0727) was discovered by Keene et al. (1983), and has
been observed at sub-mm wavelengths (e.g. Gee et al. 1985, Davidson
1987, Chandler et al. 1990), at centimeter wavelengths (Anglada et
al. 1992,1998), and with far-infrared spectroscopy (Nisini et
al. 1999). The globule has been extensively studied at mm-wavelengths
by, among others, Menten et al. (1984), Walmsley \& Menten (1987),
Frerking, Langer, Wilson (1987), Menten et al. (1989), Zhou et
al. (1990), Hasegawa, Rogers, Hayashi (1991), Velusamy, Kuiper, Langer
(1995), and Murphy, Little, Kelly (1998).  Line profiles are modeled
as an inside-out collapse by Choi et al. (1995) and Zhou (1995). An
H$_2$O maser has been studied by e.g. Claussen et al. (1996).

\vspace*{0.3cm}

{\bf HH 120} {\em (8 07, $-$35 56)}.  Original papers: Westerlund
(1963), Reipurth (1981). This is a bright low-excitation HH object
emanating from one of the cometary globules, CG30, in the Gum
Nebula. Pettersson (1984) has presented a detailed study with CCD
images and spectroscopy, and he identified the driving source,
CG30-IRS4, later detected in the far-infrared (Cohen et al.  1984b)
and as an IRAS source (08076--3556, see Cohen \& Schwartz 1987).
Cohen (1990) presents an IRAS LRS spectrum of the source. It was
detected at 1300 $\mu$m by Reipurth et al. (1993a) and Persi et al.
(1994), and at other sub-millimeter wavelengths by Dent, Matthew,
Ward-Thompson (1998).  Near-infrared images are shown by Graham \&
Heyer (1989), Persi et al. (1994), Gredel (1994) and Hodapp \& Ladd
(1995).  Molecular hydrogen emission was detected by Schwartz, Cohen,
Williams (1987) and Wilking et al. (1990), and infrared spectra are
discussed by Gredel (1994).  An optical polarization study was made by
Scarrott et al. (1990). Pettersson (1984) and Cohen, Dopita, Schwartz
(1986b) studied the stellar continuum via the reflection nebula around
the infrared source.  Olberg, Reipurth, Booth (1989) mapped the
globule in $^{12}$CO. The globule is part of a larger complex of
globules (Reipurth 1983), which is mapped in $^{12}$CO and $^{13}$CO
by Nielsen et al. (1998), and other star formation has taken place in
the vicinity (Pettersson 1987).

\vspace*{0.3cm}

{\bf HH 121} {\em (5 49, +02 47)}.
Original paper: Gredel \& Reipurth (1993). This is a small bipolar jet
emanating from the HH~111 jet source, at almost right angles to the
HH~111 jet, suggesting that the source is a binary. The jet is located
in a high extinction region and is only detected in infrared emission
lines. Proper motions are discussed by Coppin, Davis, Micono (1998).

\vspace*{0.3cm}

{\bf HH 122} {\em (5 52, +01 43)}.
Original paper: Reipurth \& Madsen (1989). This is a small HH flow
located in a high extinction region of the L1622 cloud in Orion.

\vspace*{0.3cm}

{\bf HH 123} {\em (4 32, $-$14 19)}.
Original paper: Reipurth \& Heathcote (1990). This is a small
amorphous HH object originating in the main component of the PMS
binary L1642-2, located in the high galactic latitude cloud L1642. CCD
images and spectra by Reipurth \& Heathcote (1990). The source is IRAS
04325--1419 (Sandell, Reipurth, Gahm 1987), which was detected at 1300
$\mu$m (Reipurth et al. 1993a), and it drives a small molecular
outflow (Liljestr\"om, Mattila, Friberg 1989). The cloud has low
extinction (Sandell et al. 1981), and its gas and dust has been
studied by e.g. Magnani, Blitz, Mundy (1985), Laureijs, Mattila,
Schnur (1987) and Liljestr\"om \& Mattila (1988).

\vspace*{0.3cm}

{\bf HH 124} {\em (6 38, +10 17)}.
Original paper: Walsh, Ogura, Reipurth (1992). This is a long chain
forming a bipolar HH flow in NGC 2264, driven by the IRAS source
06382+1017, which was detected at 1300 $\mu$m by Reipurth et
al. (1993a). Distant bow shocks were discovered by Ogura (1995).
Pich\'e, Howard, Pipher (1995) and Moneti \& Reipurth (1995) found a
nebulous source near the symmetry center of the outflow, close to the
IRAS source. Rodr\'\i guez \& Reipurth (1998) detected two VLA sources
at 3.6 cm within the IRAS uncertainty ellipse.  See also notes for
HH~125.

\vspace*{0.3cm}

{\bf HH 125} {\em (6 38, +09 50)}.  Original paper: Walsh, Ogura,
Reipurth (1992), who present CCD images and spectroscopy. This is a
group of giant interconnected filaments, presumably bow shocks. No
energy source has been identified, but the HH objects appear to be
closely associated with HH~225 and 226 (see notes for these objects),
with which they form a line. The region of NGC~2264 is rich in young
low mass stars (e.g. Herbig 1954a, Margulis, Lada, Young 1989), with
large amounts of molecular material (e.g. Kr\"{u}gel et al. 1987), and
much evidence for molecular outflows ( e.g. Margulis \& Lada 1986,
Margulis, Lada, Snell 1988). CS in dense cores is studied by
Wolf-Chase, Walker, Lada (1995).

\vspace*{0.3cm}

{\bf HH 126} {\em (5 33, $-$06 24)}.
Original papers: Reipurth (1985a), Ogura \& Walsh (1991). CCD images
and spectroscopy by Ogura \& Walsh (1991). This object is part of
a large outflow from HH~34 (Bally \& Devine 1994, Devine et al. 1997).

\vspace*{0.3cm}

{\bf HH 127} {\em (5 33, $-$07 02)}.
Original papers: Reipurth (1985a), Ogura \& Walsh (1991). Two small
HH knots; a spectrum of the brighter one shows very low excitation
(Ogura \& Walsh 1991). Reipurth, Devine, Bally (1998) show a CCD image and
suggest that the object comes from the L1641-N cluster and is the
counterlobe to the giant flow HH~403/404.

\vspace*{0.3cm}

{\bf HH 128/129} {\em (5 33, $-$05 06)}.
Original papers: Reipurth (1985a), Ogura \& Walsh (1991). CCD images
are shown by Reipurth, Bally, Devine (1997).  Spectra show both
objects to be of low excitation (Ogura \& Walsh 1991). Together with
HH~41 and 42 (Haro 1953), they form a small cluster of HH objects.
Optical and infrared spectrophotometry of HH 128 is presented by
Schwartz et al. (1995), and infrared images are discussed by Schwartz,
Burton, Herrman (1997). See also notes for HH 294.


\vspace*{0.3cm}

{\bf HH 130} {\em (5 34, $-$06 51)}.
Original papers: Reipurth (1985a), Ogura \& Walsh (1991). Spectroscopy
is presented by Ogura \& Walsh (1991) and Corcoran \& Ray (1995), and
a CCD image by Corcoran \& Ray (1995). This arcuate HH object appears
to be a bow shock in a flow driven by V380~Ori. The opposite lobe of
the flow contains HH~35, see further notes for this object.

\vspace*{0.3cm}

{\bf HH 131} {\em (5 32, $-$08 30)}.
Original paper: Ogura (1991). This is a smattering of emission-line
wisps and filaments stretching over almost half a degree south of and
well outside the L1641 cloud. It does not appear to be associated with
any young object.

\vspace*{0.3cm}

{\bf HH 132} {\em (8 33, $-$40 28)}.
Original paper: Ogura (1990), who presents CCD images. These are very
faint HH knots associated with a reflection nebula close to the IRAS
source 08337--4028, which is embedded in the globule DC259.9-0.0. The
object is very close to the bright nebula NGC 2626.

\vspace*{0.3cm}

{\bf HH 133} {\em (9 09, $-$45 18)}.
Original paper: Ogura (1990), who presents CCD images. The object
consists of a little cluster of faint HH knots.

\vspace*{0.3cm}

{\bf HH 134} {\em (5 33, $-$06 32)}.
Original paper: Reipurth \& Heathcote (1992). This is a small group of
HH knots close to HH~34, but it is not clear if they are related to
that flow or not.

\vspace*{0.3cm}

{\bf HH 135/136} {\em (11 10, $-$58 30)}.  Discovered by Ogura \& Walsh
(1992), who present CCD images and long-slit spectroscopy. HH~135 is a
single bright HH knot, and HH~136 forms a long chain of bright HH
knots. The objects are located in the dark cloud DC290.4+1.9 in Carina, at
the considerable distance of 2.7 kpc, making the HH objects intrinsically
very luminous. Ogura \& Walsh (1992) suggest that the two objects are not
part of the same flow, but that rather HH~135 is driven by IRAS~11101--5829,
while HH~136 is driven by an unidentified source in the middle of the chain
of knots.  Tamura et al. (1997) provide infrared polarimetry, which
suggests that only one source, IRAS 11101$-$5829, drives the two HH
objects. The source has a very high luminosity of 10$^4$ L$_\odot$.
Mm observations are presented by Ogura et al. (1998).

\vspace*{0.3cm}

{\bf HH 137/138} {\em (11 12, $-$60 36)}.
Discovered by Ogura (1993), who presents CCD images and long-slit
spectroscopy. These two objects form a long well-collimated chain of
numerous bright HH knots located in the small cloud DC291.4$-$0.2.
Assuming an association with the nearby open cluster NGC~3590, this
would place the HH objects at the considerable distance of 2.2 kpc.

\vspace*{0.3cm}

{\bf HH~139} {\em (14 56, $-$63 04)}.
Original paper: Reipurth (in preparation). This is a small
chain of HH knots emanating from the cometary nebula vBH~65a (van den
Bergh \& Herbst 1975, Herbst 1975). The nebula is illuminated by an embedded
infrared source (Scarrott, Stockdale, Draper 1994), 
and not as suggested by Perrin \& Sivan (1993) by a
nearby star. The energy source was detected at 1300 $\mu$m by Reipurth
et al. (1993a). A molecular outflow was mapped by Bally et al. (1999).

\vspace*{0.3cm}

{\bf HH 140} {\em (14 59, -63 11)}. Original paper: Ray \& Eisl\"offel
(1994), who present a CCD image. This is a bipolar HH flow emanating
from the young Herbig Ae/Be star vBH~65b (Sanduleak \& Stephenson
1973, van den Bergh \& Herbst 1975, Herbst 1975), located in the
Circinus clouds. Spectroscopic observations of vBH~65b are reported by
Allen (1978), Gahm \& Malmort (1980), and Manchado et al. (1990).  The
star was detected in X-rays by Carkner, Kozak, Feigelson (1998).
H$_2$O maser emission was detected by Scalise, Gahm, Sandell
(1981). Bally et al. (1999) detect a molecular outflow here.

\vspace*{0.3cm}

{\bf HH 141} {\em (14 59, $-$63 12)}. Original paper: Ray \&
Eisl\"offel (1994), who present a CCD image. This is a small chain of
HH knots in the Circinus clouds. See notes for HH~140.

\vspace*{0.3cm}

{\bf HH 142} {\em (14 59, $-$63 10)}. Original paper: Ray \&
Eisl\"offel (1994), who present a CCD image. This is a small cluster
of HH knots in the Circinus clouds. See notes for HH~140.

\vspace*{0.3cm}

{\bf HH 143} {\em (14 59, $-$63 11)}. Original paper: Ray \&
Eisl\"offel (1994), who present a CCD image. This is a single HH knot
in the Circinus clouds. See notes for HH~140.

\vspace*{0.3cm}

{\bf HH 144} {\em (5 33, $-$06 47)}.
Original papers: Bohigas et al. (1985), Strom et al. (1985). Both of
these papers comment on two faint knots just west of the HH~1 jet.
Using deep CCD images, Reipurth et al. (1993b) found a number of
additional faint HH knots, altogether forming an 83 arcsec long
collimated jet, with proper motions pointing away from the HH~1/2
source region. Rodr\'\i guez et al. (1990b) found two VLA sources here,
and the infrared K-band images of Reipurth et al. (1993b) show HH~1/2
VLA2 to be the driving source of HH~144. HH~1/2 VLA1/2 thus appears to
be a pre-main sequence binary with each component driving an HH flow. 
Structure and proper motions are further discussed by Eisl\"offel,
Mundt, B\"ohm (1994).
For references to mm-studies see notes on HH~1/2.

\vspace*{0.3cm}

{\bf HH 145} {\em (5 33, $-$06 48)}.
Original paper: Reipurth et al. (1993b), who present CCD images. This
is a cluster of faint HH knots west of HH~144, but it is not clear if
HH~144 and 145 are related. Structure and proper motions are discussed
by Eisl\"offel, Mundt, B\"ohm (1994).


\vspace*{0.3cm}

{\bf HH 146} {\em (5 33, $-$06 50)}.
Original paper: Reipurth et al. (1993b). An isolated faint HH knot
south-west of HH~2.

\vspace*{0.3cm}

{\bf HH 147} {\em (5 33, $-$06 47)}.
Original paper: Davis, Eisl\"offel, Ray (1994), who present CCD images
and near-infrared H$_2$ images. It is an HH object associated with
reflection nebulosity from an embedded infrared source (IRAS
05339$-$0646) about an arcminute east of HH~1. The star is number 50
in the list of Nakajima et al. (1986) and number 31 in the list of
Strom et al.  (1989); the latter reference gives
optical/infrared/far-infrared photometry and a spectral
classification.  The source was detected at 1300 $\mu$m by Chini et
al. (1997b).  Structure and proper motions are discussed by
Eisl\"offel, Mundt, B\"ohm (1994). Detailed CCD images and
spectroscopy are given by Corcoran \& Ray (1995).

\vspace*{0.3cm}

{\bf HH 148} {\em (5 33, $-$06 44)}. 
Original paper: Strom et al.  (1986), who show CCD images. This is a
small chain of three HH knots emanating to the south-west from the
Herbig Ae/Be star V380~Ori. It is orthogonal to the line defined by
HH~35 and HH~130, which may suggest the presence of another source in
the region. Leinert et al. (1994) found a companion to V380 Ori with a
separation of 0.17 arcsec.

\vspace*{0.3cm}

{\bf HH 149} {\em (22 34, +75 01)}.  
Original paper: Bal\'{a}zs et al. (1992), who present CCD images. This
is a small group of HH knots clustered around the IRAS source
22343+7501 in the L1251 cloud. A molecular outflow around this source
was discovered by Schwartz, Gee, Huang (1988) and further studied by
Sato \& Fukui (1989). Mm observations of L1251 are discussed by Sato
et al. (1994). Ammonia maps are presented by T\'oth \& Walmsley (1996)
and Anglada, Sep\'ulveda, G\'omez (1997).  Hodapp (1994) presents a
wide field K$'$ band image.  Detailed near-infrared images by Rosvick \&
Davidge (1995) reveal that the IRAS source is multiple; these authors
also provide sub-mm photometry. Xiang \& Turner (1995) and Claussen et
al. (1996) detected an H$_2$O maser.  Meehan et al. (1998) present high 
resolution radio and mm-wavelength maps. Kun \& Prusti (1993) discuss the
presence of young stars in L1251 and give further references to the
region. See also notes for HH 189.

\vspace*{0.3cm}

{\bf HH 150} {\em (4 28, +18 07)}.  Original paper: Mundt, Ray,
B\"uhrke (1988). This is a fine bipolar jet emanating from HL~Tau. It
can be traced for 13 arcsec in the NE lobe before it becomes confused
with the HH~151 jet, and longer in the SW lobe. HH 266 may be a
distant bow shock.  {\em Structure and CCD images:} Mundt, Ray,
B\"uhrke (1988), Mundt et al. (1990), Mundt, Ray, Raga (1991), L\'opez
et al. (1995).  {\em HST images:} Stapelfeldt et al. (1995), Ray et
al. (1996).  {\em Spectroscopy:} Mundt et al. (1990), Bacciotti \&
Eisl\"offel (1999).  {\em Proper motions:} Mundt et al. (1990),
L\'opez et al. (1996).  {\em Polarization data:} Bastien (1982),
Hodapp (1984), Gledhill \& Scarrott (1989).  {\em Molecular outflow:}
Edwards \& Snell (1982), Calvet, Cant\'{o}, Rodr\'\i guez (1983),
Torrelles et al. (1987), Levreault (1988), Monin, Pudritz, Lazareff
(1996).  {\em Source:} There is a large body of literature on HL~Tau
and its circumstellar environment, the following are only some of many
references: Cohen \& Kuhi (1979), Cohen (1980b,1983), Grasdalen et
al. (1984), Beckwith et al. (1984), Brown, Drake, Mundt (1985),
Beckwith et al. (1986,1989), Edwards et al. (1987), Sargent \&
Beckwith (1987,1991), Monin et al. (1989), Grasdalen et al. (1989),
Adams, Emerson, Fuller (1990), Carr (1990), Ohashi et al. (1991),
Blake, van Dishoeck, Sargent (1992), Rodr\'\i guez et al. (1992),
Schuster et al. (1993), Reipurth et al. (1993a), Molinari, Liseau,
Lorenzetti (1993), Hayashi, Ohashi, Miyama (1993), G\'omez et
al. (1993), Rodr\'\i guez et al. (1994a), Lay et al. (1994), Hamann et
al. (1994), Lin et al. (1994), Stapelfeldt et al. (1995), Beckwith \&
Birk (1995), Weintraub, Kastner, Whitney (1995), Mundy et al. (1996),
Wilner, Ho, Rodr\'\i guez (1996), Liu et al. (1996), Greene \& Lada
(1996b), Close et al. (1997a), Lay, Carlstrom, Hills (1997), Lucas \&
Roche (1998a), Dent, Matthew, Ward-Thompson (1998).

\vspace*{0.3cm}

{\bf HH 151} {\em (4 28, +18 07)}.
Original paper: Mundt \& Fried (1983).  This is a fine bright bipolar
jet apparently
emanating from the VLA~1 source between HL and XZ Tau.
{\em Structure and CCD images:} Mundt \& Fried (1983), Strom et al.
(1986), Mundt, Ray, B\"uhrke (1988), Mundt et al. (1990), Mundt, Ray,
Raga (1991).
{\em Spectroscopy:} Mundt, Brugel, B\"uhrke (1987), Cohen \& Jones
(1987), Mundt et al. (1990).
{\em Proper motions:} Mundt et al. (1990).
{\em Source:} Brown, Drake, Mundt (1985). The reality of the VLA~1
source is controversial, and Rodr\'\i guez et al. (1994a) were not
able to detect it in a deep high resolution VLA study.

\vspace*{0.3cm}

{\bf HH 152} {\em (4 28, +18 07)}.
Original paper: Mundt, Ray, B\"uhrke (1988). This is a short bipolar
jet emanating from XZ Tau and stretching about 10 arcsec on either
side of the star.  {\em Structure and CCD images:} Strom et
al. (1986), Mundt, Ray, B\"uhrke (1988), Mundt et al. (1990),
Krist et al. (1997). {\em
Spectroscopy:} Mundt et al. (1990), Hirth, Mundt, Solf (1997).  {\em
Proper motions:} Mundt et al. (1990).  {\em Polarization data:}
Bastien (1982), Hodapp (1984), Gledhill \& Scarrott (1989).  {\em
Source:} Cohen \& Kuhi (1979), Brown, Drake, Mundt (1985), Carr
(1990), Molinari, Liseau, Lorenzetti (1993). Haas, Leinert, Zinnecker
(1990) and Leinert et al. (1993) resolved XZ Tau as a close binary
star.

\vspace*{0.3cm}

{\bf HH 153} {\em (4 28, +18 07)}.
Original paper: Mundt, Ray, B\"uhrke (1988). A more detailed study
(CCD images, spectroscopy, proper motions) was carried out by Mundt et
al. (1990). As seen in H$\alpha$ this is a short well-collimated jet,
located about 30$''$ SSE of HL~Tau.
In [SII] the morphology changes dramatically, the jet being replaced
by two bright knots, which may be part of the working surface where
the jet flow terminates. No source has been identified yet. This jet
is part of a small group of flows (HH~150-153) in the HL/XZ~Tau
region. 

\vspace*{0.3cm}

{\bf HH 154} {\em (4 28, +18 01)}.  Original paper: Mundt \& Fried
(1983), who show CCD images of a short (about 20 arcsec) jet emanating
from the L1551 IRS 5 source. {\em CCD images} of the region are
presented by Mundt \& Fried (1983), Snell et al. (1985), Strom et
al. (1986), Campbell et al. (1988), Graham \& Heyer (1990), Davis et
al. (1995) and, in most detail, by Mundt, Ray, Raga (1991) and
Fridlund \& Liseau (1994,1998). {\em Proper motion} of the knots in
the jet are demonstrated by Neckel \& Staude (1987b), Campbell et
al. (1988) and Fridlund \& Liseau (1994).  {\em Optical spectra} are
discussed by Cohen \& Fuller (1985), Sarcander, Neckel, Els\"asser
(1985) and Stocke et al. (1988). {\em Molecular hydrogen emission}
from the jet has been observed by Yamashita \& Tamura (1992) and Davis
et al. (1995), and [OI] 63$\mu$m emission was detected by Cohen et
al. (1988).  {\em Optical/infrared polarization } measurements of the
reflection nebula around the source and the jet are discussed by
Nagata, Sato, Kobayashi (1983), Hodapp (1984), Draper, Warren-Smith,
Scarrott (1985b), Lenzen (1987), Scarrott (1988a), Campbell et
al. (1988), Stocke et al. (1988) and Lucas \& Roche (1997). A major
{\em molecular outflow} is driven by L1551 IRS 5, it has been studied
by, among others, Knapp et al. (1976), Snell, Loren, Plambeck (1980),
Calvet, Cant\'o, Rodr\'\i guez (1983), Fridlund et al. (1984), Snell
\& Schloerb (1985), Mirabel et al. (1985, 1987), Moriarty-Schieven et
al.  (1987b), Rainey et al. (1987), Uchida et al. (1987),
Moriarty-Schieven \& Snell (1988), Lizano et al. (1988), Levreault
(1988), Fridlund \& White (1989), Rodr\'\i guez et al. (1989c), van
der Werf et al. (1989), Liljestr\"om (1989), Pound \& Bally (1991),
Moriarty-Schieven \& Wannier (1991), Parker et al. (1991), Rudolph
(1992), Giovanardi et al. (1992), Barsony, Scoville, Chandler (1993),
Fridlund \& Knee (1993), Bachiller, Tafalla, Cernicharo (1994),
Chernin, Masson, Fuller (1994) and Plambeck \& Snell (1995).  {\em
Extended far-infrared emission} from dust in the outflow cavity is
discussed by Clark \& Laureijs (1986), Edwards et al. (1986) and Clark
et al. (1986). The {\em L1551 IRS 5 source} has been intensely studied
and only a selection of references can be given here. It was
discovered by Strom, Strom, Vrba (1976b), and near- and far-infrared
and sub-millimeter photometric observations are given by Fridlund et
al. (1980), Beichman \& Harris (1981), Phillips et al. (1982),
Davidson \& Jaffe (1984), Cohen, Harvey, Schwartz (1985), Cohen \&
Schwartz (1987), Woody et al.  (1989), Walker et al. (1990), Butner et
al. (1991), Molinari, Liseau, Lorenzetti (1993), Liu et al. (1996),
Harvey et al.(1998).  {\em Optical/infrared spectroscopy} of L1551 IRS
5 and its reflection nebula shows that it is an FU Orionis object
(Mundt et al. 1985, Carr, Harvey, Lester 1987, Stocke et al. 1988,
Sato et al. 1992). {\em Near-infrared imaging} of the source and its
close environment is discussed by Strom et al. (1985b), Moneti et
al. (1989), Hodapp et al. (1988), Hodapp \& Ladd (1995) and Lucas \&
Roche (1996, 1997). {\em VLA radio continuum} observations are
discussed by Cohen, Bieging, Schwartz (1982), Bieging, Cohen, Schwartz
(1984), Snell et al. (1985), Bieging \& Cohen (1985), Rodr\'\i guez et
al. (1986), Snell \& Bally (1986), G\'omez et al. (1993), Rodr\'\i
guez et al. (1998).  Evidence for {\em extended structures or a disk}
is discussed by, among others, Kaifu et al. (1984), Batrla \& Menten
(1985), Menten \& Walmsley (1985), Moriarty-Schieven et al. (1987a),
Duncan et al. (1987), Walmsley \& Menten (1987), Sargent et
al. (1988), Menten et al. (1989), Keene \& Masson (1990), Walker,
Adams, Lada (1990), Butner et al. (1991), Ohashi et al. (1991), Lay et
al. (1994), Ladd et al. (1995), Fuller et al. (1995), Ohashi et
al. (1996), Saito et al. (1996), Hogerheijde et al. (1998) and Momose
et al. (1998).  Evidence that IRS~5 is a {\em binary} is discussed by
Bieging \& Cohen (1985), Rodr\'\i guez et al. (1986), Looney, Mundy,
Welch (1997), and Rodr\'\i guez et al. (1998).  {\em A small
high-density clump} has been observed at the head of HH~154 by
Torrelles et al. (1985a).  The presence of {\em magnetic fields} is
discussed by Simonetti \& Cordes (1986).  {\em The L1551 molecular
cloud} itself has been studied at mm-wavelengths by Snell (1981) and
by Miesch \& Bally (1994). See also notes for HH 28/29.


\vspace*{0.3cm}

{\bf HH 155} {\em (4 19, +19 25)}.  Original paper: Schwartz (1975).
This is a Herbig-Haro flow stretching from T Tauri to the west and
including a knot located 32 arcsec west of T Tau (formerly HH~1555)
and the spatiokinematic flow components A and B very close to T~Tauri
(B\"ohm and Solf 1994). All emission of HH~155 is blue-shifted;
presumably the receding lobe is obscured by a circumstellar disk
around T~Tauri. The region of T~Tauri contains another HH flow,
HH~255, which lies in a north-south direction and includes Burnham's
Nebula south of T~Tauri and the two spatiokinematic flow components C
and D of B\"ohm \& Solf (1994) close to T~Tauri; HH~255 appears to be
driven by T~Tau-S. Speckle interferometry of the H$\alpha$ emission
around T Tauri is presented by Devaney et al. (1995), and Robberto et
al. (1995) discuss coronographic interference filter images.  It is
not clear if knot~A found by Schwartz (1990) south-west of T Tauri
belongs to HH~155 or HH~255. CCD images of HH~155 are shown by
B\"uhrke, Brugel, Mundt (1986), Schwartz (1990) and Eisl\"offel \&
Mundt (1998), and spectroscopy of HH~155 is discussed by Schwartz
(1975) and B\"uhrke, Brugel, Mundt (1986). [OI] 63 $\mu$m emission was
detected by Cohen et al. (1988), and weak 3.6 cm emission extends
about 1 arcsec west of T~Tau (Skinner \& Brown 1994). The molecular
hydrogen emission detected towards T~Tauri appears to come from
Burnham's Nebula, see notes for HH~255. In addition to Burnham's
Nebula south of T~Tauri, which is shock-excited, there is a large
reflection nebula, NGC~1555, west of the star that was discovered by
Hind in 1852 (Astronomische Nachtrichten No.839) and described by
Burnham (1890, 1894), Barnard (1895, 1899), Keeler (1900), Lampland
(1936), Herbig (1953), and Lorre (1975). Spectra show the nebula to
reflect light from T Tauri (Schwartz 1975). The reflection nebula
close to the star is studied by Nakajima \& Golimowski (1995), and
with HST images by Stapelfeldt et al. (1998).  T~Tauri has been
extensively studied, and only a few references are given here; see
Herbig \& Bell (1988) for further references. Its spectrum is
described by Joy (1945), and high-resolution line profiles are
discussed by e.g. Hartmann (1982), Mundt (1984), and Persson et
al. (1984). Infrared spectroscopy is reported by Kelly, Rieke,
Campbell (1994) and Greene \& Lada (1996b). It is irregularly variable
in addition to a regular variability with period 2.8 days (e.g. Herbst
et al. 1986, Zaitseva 1989).  T Tauri has a companion, T~Tau-S, 0.6
arcsecond to the south which is a bright infrared and radio continuum
source, as discussed by Dyck, Simon, Zuckerman (1982), Cohen, Bieging,
Schwartz (1982), de Vegt (1982), Hanson, Jones, Lin (1983), Schwartz
et al. (1984), Schwartz, Simon, Campbell (1986), Maihara \& Kataza
(1991), Ghez et al. (1991), Phillips, Lonsdale, Feigelson (1993),
Skinner \& Brown (1994), Ghez et al. (1995), Simon et al. (1996),
Koresko, Herbst, Leinert (1997), and Ray et al. (1997).  A third
component, located 0.3 arcsec north of T~Tau, was suggested to exist
by Nisenson et al.  (1985) and confirmed by Maihara \& Kataza (1991),
but not seen by Gorham et al. (1992) and its reality is
questionable. Ray et al. (1997) found that the radio source known as T
Tau N is identical to the optically visible star T Tau, and the radio
source T Tau S is identical to the infrared companion. In between
these two sources, Ray et al. (1997) found a third radio source,
called T Tau R, which appears to be part of the system.  X-ray
emission was detected towards the T Tauri system by Carkner, Kozak,
Feigelson (1998).  H$_2$O maser emission has been detected near
T~Tauri (Knapp \& Morris 1976, Thum, Bertout, Downes 1981, Claussen et
al. 1996).  High-velocity CO and possibly HI emanates from the T~Tauri
system (Edwards \& Snell 1982, Ruiz, Alonso, Mirabel 1992). Evidence
for circumstellar material or a disk is given by Weintraub, Masson,
Zuckerman (1987), Weintraub et al. (1992), Schuster et al. (1993), van
Langevelde, van Dishoeck, Blake (1994), Momose et al. (1996),
Hogerheijde et al. (1997a,b,1998), Schuster, Harris, Russell (1997)
and Akeson, Koerner, Jensen (1998). Using near-infrared
spectropolarimetry, Kobayashi et al. (1997) found evidence for
scattering in a compact nebulosity around T~Tau-S. Ray et al. (1997)
find evidence for a large-scale magnetic field in the outflow from T
Tau S.

\vspace*{0.3cm}

{\bf HH 156} {\em (4 15, +28 13)}.  Original paper: Strom et
al. (1986). This is a small bipolar jet emanating from the star
labelled Tau~1 by Cohen \& Kuhi (1979) near CZ and DD~Tau (and
sometimes called CoKu-Tau 1).  Cohen \& Kuhi (1979), Strom \& Strom
(1994) and Kenyon et al. (1998) obtained spectra of the star, and
Strom et al. (1986), Goodrich (1993) and Eisl\"offel \& Mundt (1998)
obtained CCD images.  Proper motions of the jet is presented by
Eisl\"offel \& Mundt (1998).  Movsesyan \& Magakyan (1990) and
Eisl\"offel \& Mundt (1998) obtained long slit spectra of the
jet. Infrared photometry of the star is reported by Strom \& Strom
(1994).  Padgett et al. (1999) present HST/NICMOS images of the
surrounding reflection nebula, and show that the source is a binary
with 0.24 arcsec separation.  The source is detected by IRAS at 12
$\mu$m (IRAS 04155+2812). Skinner, Brown, Stewart (1993) report a
possible radio continuum detection.

\vspace*{0.3cm}

{\bf HH 157} {\em (4 18, +26 50)}.  Original paper: Mundt et
al. (1984). This is an HH jet powered by the T~Tauri star Haro 6-5B (=
FS~Tau~B), a companion about 20 arcsec west of Haro 6-5 (=
FS~Tau). CCD images are discussed by Mundt et al. (1984), Strom et
al. (1986) and Eisl\"offel \& Mundt (1998). Proper motions are
determined by Eisl\"offel \& Mundt (1998). Spectra of the jet are
presented by Mundt, Brugel, B\"uhrke (1987) and Eisl\"offel \& Mundt
(1998), and of the reflection nebula by Cohen \& Fuller
(1985). Polarization data are given by Gledhill, Warren-Smith,
Scarrott (1986) and Gledhill \& Scarrott (1989).  Padgett et
al. (1999) present HST/NICMOS images of the compact reflection nebula
around the source.  The source was observed with optical spectroscopy
by Eisl\"offel \& Mundt (1998), in the near-infrared by Vrba, Rydgren,
Zak (1985), in H$_2$ by Carr (1990), in the far-infrared by Cohen \&
Scwartz (1987) and at 1300 $\mu$m by Reipurth et al. (1993a). HST
images of FS~Tau and Haro~6-5B are discussed by Krist et al. (1998).

\vspace*{0.3cm}

{\bf HH 158} {\em (4 24, +25 59)}.  Original paper: Mundt \& Fried
(1983). This is a short jet emanating from the T~Tauri star
DG~Tau. CCD images are discussed by Mundt \& Fried (1983), Strom et
al. (1986), Mundt, Brugel, B\"uhrke (1987), Eisl\"offel \& Mundt
(1998), and HST images are presented by Kepner et al. (1993).  Proper
motions are determined by Eisl\"offel \& Mundt (1998).  Spectroscopic
observations are analyzed by Mundt \& Fried (1983), Cohen \& Fuller
(1985), Mundt, Brugel, B\"uhrke (1987) and Solf \& B\"ohm (1993).  A
detailed 3D spectro-imaging study in the [OI] 6300 line is presented
by Lavalley et al. (1997).  Optical spectra of DG~Tau are given by
e.g. Cohen \& Kuhi (1979), Levreault (1988), and Hessman \& Guenther
(1997) who derive a spectral type of K6V, and an infrared spectrum is
shown by Greene \& Lada (1996b).  DG~Tau is detected in the radio
continuum (Bertout \& Thum 1982, Cohen, Bieging, Schwartz 1982), and
Bieging, Cohen, Schwartz (1984) find it is extended in the same
direction as the jet.  A reflection nebula is imaged by Nakajima \&
Golimowski (1995).  Polarization measurements are given by Bastien
(1982), Moneti et al.  (1984), and Hodapp (1984). Infrared lunar
occultation observations are analyzed by Leinert et al. (1991) and
Bogdanov \& Cherepashchuk (1993).  Near-infrared observations of DG
Tau are discussed by Carr (1990), Chandler et al. (1993), Molinari,
Liseau, Lorenzetti (1993), Hamann et al. (1994), Chandler, Carlstrom,
Scoville (1995), Najita, Carr, Tokunaga (1996), Biscaya et al. (1997)
and Muzerolle, Hartmann, Calvet (1998), and far-infrared observations
by Cohen, Harvey, Schwartz (1985) and Cohen \& Schwartz (1987), and
sub-mm photometry by Moriarty-Schieven et al. (1994).  Levreault
(1988) did not detect clear evidence for a molecular
outflow. Circumstellar gas or dust has been detected by Ohashi et
al. (1991), Chen et al. (1992), Schuster et al. (1993), Mannings \&
Emerson (1994), and Kitamura, Kawabe, Saito (1996a,b).

\vspace*{0.3cm}

{\bf HH 159} {\em (4 23, +25 59)}.  Original paper: Mundt \& Fried
(1983). This is a more than one arcmin long highly collimated jet
emanating from the low-luminosity star DG~Tau B, located approximately
50 arcsec southwest of DG~Tau. CCD images are presented by Mundt \&
Fried (1983), Mundt, Brugel, B\"uhrke (1987), Mundt, Ray, Raga (1991)
and Eisl\"offel \& Mundt (1998).  Proper motions are determined by
Eisl\"offel \& Mundt (1998).  Spectroscopy is discussed by Jones \&
Cohen (1986), Mundt, Brugel, B\"uhrke (1987) and Eisl\"offel \& Mundt
(1998).  Padgett et al. (1999) present HST/NICMOS images of the
compact reflection nebula around the source.  The source was observed
in the near-infrared by Vrba, Rydgren, Zak (1985), in the far-infrared
by Cohen, Harvey, Schwartz (1985) and Cohen \& Schwartz (1987), and in
the radio continuum by Rodr\'\i guez, Anglada, Raga (1995).  Schwartz
et al. (1995) present near-infrared spectroscopy.  A well-collimated
redshifted molecular outflow was found along the jet-axis by Mitchell
et al. (1994), and further studied by Mitchell, Sargent, Mannings
(1997).

\vspace*{0.3cm}

{\bf HH 160} {\em (7 01, $-$11 28)}.  Original paper: Poetzel, Mundt,
Ray (1989), who present CCD images and long-slit spectroscopy. This is
a finely collimated bipolar jet emanating from Z CMa with the very
large extent of 3.6 pc. Parts of the flow have very high radial
velocities, and the jet near the source shows complex
velocity-structure. Z~CMa itself has been very extensively studied,
see Herbig (1960,1991) for references. It is an FU Orionis object
(Hartmann et al. 1989, Hessman et al. 1991, Welty et al. 1992, Sato et
al. 1992, Liljestr\"om \& Olofsson 1997, Reipurth \& Aspin 1997) and
it has an infrared companion (e.g. Koresko et al.  1991, Haas et
al. 1993, Whitney et al. 1993, Barth, Weigelt, Zinnecker 1994,
Thi\'ebaut et al. 1995). Polarimetry of both components are presented
by Fischer, Stecklum, Leinert (1998).  The photometric behaviour of
Z~CMa is discussed by e.g. Covino et al. (1984), Hessman et al. (1991)
and Teodorani et al. (1997). Rapid spectroscopic variability of Z~CMa
is discussed by Chochol et al. (1998).  The mass loss rate based on
[SII] emission is determined by Corcoran \& Ray (1997).  Submillimeter
observations are presented by Weintraub, Sandell, Duncan (1991),
Henning et al. (1998) and Dent, Matthew, Ward-Thompson (1998), and
radio continuum observations by Bieging, Cohen, Schwartz (1984) and
Skinner, Brown, Stewart (1993). Evidence for a disk is presented by
Malbet et al. (1993).  The inner reflection nebula is imaged by
Nakajima \& Golimowski (1995).  Optical photometry is summarized by
Kolotilov (1991). X-ray observations are reported by Zinnecker \&
Preibisch (1994).  A molecular outflow was detected by Evans et
al. (1994). Mm observations of the surrounding cloud core are
discussed by Liljestr\"om \& Olofsson (1997) and Fuente et al. (1998).
Lamzin et al. (1998) argue that the primary component of the binary is
the main source of activity rather than the infrared companion.

\vspace*{0.3cm}

{\bf HH 161} {\em (0 08, +58 33)}.  Original paper: Strom et
al. (1986), who present CCD images. This is a single bright HH knot
next to the luminous Herbig Ae/Be star LkH$\alpha$ 198 (= V633 Cas). A
deeply embedded companion to LkH$\alpha$ 198 has been detected by
infrared imaging (Lagage et al. 1993) and optically (Corcoran, Ray,
Bastien 1995); the latter paper presents CCD images which show that
the object has a tail pointing back towards the companion LkH$\alpha$
198B. This orientation coincides with the axis of a molecular outflow
(Cant\'{o} et al. 1984, Levreault 1988, Nakano et al. 1990).  The
LkH$\alpha$ 198 region has been extensively studied, see the following
papers and references therein: Herbig (1960), Schwartz \& Buhl (1975),
Loren (1977), Harvey, Thronson, Gatley (1979), Chavarria (1985),
Leinert, Haas, Lenzen (1991), Hodapp (1994), Sandell \& Weintraub
(1994), Mannings (1994), Butner \& Natta (1995), Nisini et al. (1995),
Asselin et al. (1996), Corcoran \& Ray (1997), Koresko et al. (1997),
Fuente et al. (1998), Henning et al. (1998).

\vspace*{0.3cm}

{\bf HH 162} {\em (0 08, +58 33)}.
Original paper: Corcoran, Ray, Bastien (1995). This is a group of HH
objects east of the Herbig Ae/Be star V376 Cas. This star is about 35
arcsec north of LkH$\alpha$ 198. See also notes for HH~161.

\vspace*{0.3cm}

{\bf HH 163} {\em (2 57, +60 17)}.
Original paper: Ray et al. (1990), who present CCD images and
long-slit spectroscopy. This is a short jet in the region of the
luminous star AFGL 4029 (IRAS 02575+6017). The CCD images of Ray et
al. (1990) show that AFGL~4029 consists of two components, A and B, of
which B may be the more likely driving source. Snell et al. (1988)
found a molecular outflow from AFGL~4029. Cohen \& Lewis (1978)
discuss a low-dispersion spectrum of the star. An H$_2$O maser was
detected by Churchwell, Walmsley, Cesaroni (1990).

\vspace*{0.3cm}

{\bf HH 164} {\em (0 08, +58 33)}. Original paper: Corcoran, Ray,
Bastien (1995). This is a jet of several HH knots emanating from
LkH$\alpha$~198. The embedded companion to this star also drives an HH
flow, HH~161, see notes for this object. The object HH~461 is found to
the SE along the HH~164 flow axis, and is probably a bow shock in this
flow (Aspin \& Reipurth 1999).

\vspace*{0.3cm}

{\bf HH 165} {\em (19 40, +23 17)}.
Original paper: Mundt et al. (1984), who present CCD images. This is a
fine jet about 45 arcsec long emanating from the cometary nebula
1548C27, first noted by Craine, Boeshaar, Byard (1981). Spectra of the
jet and nebula are discussed by Mundt, Brugel, B\"uhrke (1987),
Magakyan et al. (1989) and Vilchez et al. (1989). Optical polarization
maps are presented by Scarrott, Rolph, Tadhunter (1991), and Dent \&
Aspin (1992) find a molecular outflow and present near-infrared
imaging and polarimetry. These latter authors argue for a kinematical
distance of 2.4 kpc. Phillips \& Mampaso (1996) discuss CO data around
the cometary nebula. Najita et al. (1996) 
and Biscaya et al. (1997) analyze near-infrared CO
overtone spectra. Chini et al. (1997b) found extended 1300 $\mu$m
emission around the source. The jet points to HH 365, which appears to
be a bow shock in the flow, see notes for that object.


\vspace*{0.3cm}

{\bf HH 166} {\em (20 27, +40 01)}.
Original paper: Poetzel, Mundt, Ray (1992), who present CCD images,
infrared images and long-slit spectroscopy. This is a chain of three
HH knots located next to and approximately on a line through the AFGL
2591 infrared source. Additional knots are seen in the near-infrared,
and the source is surrounded by optical/infrared reflection nebulae.
Very high velocities are measured in the HH flow. The AFGL~2591 region
is well studied, and only some references are given here. Bally \&
Lada (1983) and Torrelles et al. (1983b) found a molecular outflow,
which was studied in more detail by Lada et al. (1984), who also give
near- and far-infrared photometry. Higher-resolution CO and HCO$^+$
maps are presented by Hasegawa \& Mitchell (1995).  Near-infrared
images are discussed by Forrest \& Shure (1986), Lenzen (1987),
Yamashita et al (1987b) and Burns et al.  (1989); polarimetric data
are also presented by the three latter papers. Mitchell, Maillard,
Hasegawa (1991) have obtained infrared spectroscopy, and Tamura \&
Yamashita (1992) mapped H$_2$ and Br$\gamma$ emission. G\"urtler et
al. (1991) discuss mm continuum data, Torrelles et al. (1989a) NH$_3$
observations, and Yamashita et al. (1987b) CS observations. Campbell
(1984) identifies several VLA sources, and Wynn-Williams et al. (1977)
and Tofani et al. (1995) discuss the position of an H$_2$O maser.

\vspace*{0.3cm}

{\bf HH 167} {\em (21 41, +65 53)}.  Original paper: Ray et
al. (1990), who present CCD images and long-slit spectroscopy. This is
a well collimated jet 40 arcsec in length consisting of numerous knots
and emanating from the near vicinity of the luminous Herbig Be star
LkH$\alpha$~234. Radial velocity and density decreases outwards from
the source. LkH$\alpha$~234 and the surrounding NGC~7129 region is
well studied, see the following selected papers and references
therein. The star has been studied by Herbig (1960), Strom et
al. (1972), Bechis et al. (1978), and Weintraub, Kastner, Mahesh
(1994) have found a deeply embedded companion.  Weintraub et
al. (1996) argue that the deeply embedded star is the source of the
jet.  Cabrit et al. (1997) present a high-resolution H$_2$ image of
the jet, plus 10 $\mu$m and 17 $\mu$m images of the infrared
companion.  Far-infrared maps are presented by Di~Francesco et
al. (1998).  There is complex CO outflow activity in the region
(Edwards \& Snell 1983, Bertout 1987), and Mitchell \& Matthews (1994)
show that the redshifted CO outflow is collimated with an axis
approximately opposite the HH~167 jet axis. Fuente et al. (1998) and
Henning et al. (1998) present $^{13}$CO, CS and 1.3 mm continuum
maps. Hodapp (1994) presents a wide field K$'$ band image. Nisini et
al. (1995) derive a mass loss rate from near-infrared HI lines.
Sandell \& Olofsson (1981) summarize available data on several H$_2$O
masers.  Eiroa, Palacios, Casali (1998) present HIRAS maps of the
whole NGC~7129 region.  There are numerous HH objects in the NGC~7129
region, see notes on HH~103, 105, 232, 234, 235, 236, 237, 238, 239
and 242. Overviews of this complex region are given by Hartigan \&
Lada (1985, fig.30) and Ray et al. (1990, fig.6).

\vspace*{0.3cm}

{\bf HH 168} {\em (22 54, +61 45)}.  Original paper: Gyulbudaghian,
Glushkov, Denisyuk (1978). This is a large cluster of interconnected
HH knots mixed with reflection nebulosity (formerly GGD~37). Positions
and knot designations are given by Hartigan \& Lada (1985). The Cep~A
region is very complex with much star formation activity; the most
likely energy source is the high-luminosity radio continuum source
HW~2. {\em Structure and CCD Images:} Hartigan \& Lada (1985),
Hartigan et al. (1986), and Lenzen (1988). {\em Spectroscopy:} Lenzen,
Hodapp, Solf (1984), Hartigan et al. (1986).  {\em Molecular hydrogen
emission and ir images:} Bally \& Lane (1982), Simon \& Joyce (1983),
Doyon \& Nadeau (1988), Lane (1989), Hodapp (1994), Wright et
al. (1996), Hartigan et al. (1996), Goetz et al. (1998).  {\em Proper
Motions:} Lenzen (1988).  {\em Optical/infrared polarization:} Lenzen,
Hodapp, Solf (1984), Joyce \& Simon (1986), Eaton \& Scarrott (1989),
Hodapp (1990), Colom\'e \& Harvey (1995), Casement \& McLean (1996).
{\em Molecular outflow:} Ho, Moran, Rodr\'\i guez (1982), Richardson
et al. (1987), Hayashi, Hasegawa, Kaifu (1988), Levreault (1988),
Phillips \& Mampaso (1991), Choi, Evans, Jaffe (1993), Torrelles et
al. (1993b), Narayanan \& Walker (1996).  {\em Other mm-observations:}
G\"usten, Chini, Neckel (1984), Weliachew et al. (1985), Torrelles et
al. (1986), Moriarty-Schieven, Snell, Hughes (1991), Torrelles et
al. (1993a), Codella, Bachiller, Reipurth (1999).  {\em Radio
continuum observations:} Beichman, Becklin, Wynn-Williams (1979),
Hughes \& Wouterloot (1982, 1984), Hughes (1985, 1988, 1989, 1997),
Hughes \& Moriarty-Schieven (1990), Hughes (1991, 1993), Rodr\'\i guez
et al. (1994b), Hoare \& Garrington (1995), Hughes, Cohen, Garrington
(1995), Torrelles et al. (1996), Garay et al. (1996), Torrelles et
al. (1998).  {\em H$_2$O and OH masers:} Wouterloot, Habing, Herman
(1980), Lada et al. (1981), Cohen, Rowland, Blair (1984), Cohen \&
Brebner (1985), Mattila et al. (1985, 1988), Cohen, Brebner, Potter
(1990), Migenes, Cohen, Brebner (1992), Torrelles et al. (1996),
Mehringer, Zhou, Dickel (1997), Torrelles et al. (1998).  {\em
Far-infrared and sub-mm observations:} Ellis et al. (1990), Gordon
(1990), Colom\'e \& Harvey (1995).  {\em Magnetic fields:} Simonetti
\& Cordes (1986).

\vspace*{0.3cm}

{\bf HH 169} {\em (22 54, +61 46)}. 
Original papers: Lenzen (1988), Corcoran, Ray, Mundt (1993), who
present CCD images. This appears to be the counter-flow to the HH~168
(formerly GGD~37) flow in Cepheus~A. The two main condensations,
HH~169-NE and HH~169-NE2, have bow shock morphologies, facing away
from the luminous embedded star HW~2, which is the likely driving
source. The objects are part of a larger ellipse of emission
(Corcoran, Ray, Mundt 1993). Spectra of HH~169-NE are discussed by
Lenzen (1988), who also present proper motions. For references to the
molecular outflow and other aspects of this complex region, see notes
for HH~168.


\vspace*{0.3cm}

{\bf HH 170} {\em (23 15, +60 34)}.  Original paper: Poetzel, Mundt,
Ray (1992), who present CCD images and long-dispersion
spectroscopy. This is a somewhat poorly collimated bipolar jet flowing
from the high luminosity young Herbig Ae/Be star MWC~1080. A molecular
outflow is reported by Cant\'{o} et al. (1984) and Levreault
(1988). Optical spectroscopy of the star is discussed by Herbig
(1960), Garrison \& Anderson (1977), Cohen \& Kuhi (1979),
Finkenzeller \& Mundt (1984) and Poetzel, Mundt, Ray (1992).  Near-ir
spectroscopy is discussed by Nisini et al. (1995).  ISO-SWS spectra
are presented by Benedettini et al. (1998).  Far-infrared maps are
discussed by Di~Francesco et al. (1998).  Polarization data are given
by Garrison \& Anderson (1978) and Vrba, Schmidt, Hintzen
(1979). Radio continuum observations are discussed by Curiel et
al. (1989b), Skinner, Brown, Linsky (1990) and Skinner, Brown, Stewart
(1993). A companion 0.75 arcsec east of MWC 1080 was found by Leinert
et al. (1994). Sub-mm photometry of the combined system is given by
Mannings (1994). Fuente et al. (1998) and Henning et al. (1998)
present $^{13}$CO, CS and 1.3 mm continuum maps. MWC~1080 was detected
in X-rays by Carkner, Kozak, Feigelson (1998).

\vspace*{0.3cm}

{\bf HH 171} {\em (9 46, $-$54 43)}. 
Original paper: Ogura \& Noumaru (1994), who present CCD images and
spectroscopy. This is a faint HH object in the small dark cloud
D278.6$-$0.9 in Vela. It has an unusually high excitation. The
distance to the region is unknown.

\vspace*{0.3cm}

{\bf HH 172} {\em (18 51, +00 28)}. 
Original paper: Cappellaro et al. (1994), who present CCD images and
spectroscopy. This is a large structured object located next to the
dense dark cloud containing the reflection nebula GGD~30, studied by
G\'omez de Castro \& Eiroa (1991) and Foley et al. (1993). Infrared
sources in the region are discussed by G\'omez de Castro \& Eiroa (1991)
and Cappellaro et al. (1994). Mm observations are discussed by
Rodr\'\i guez et al. (1980).

\vspace*{0.3cm}

{\bf HH 173} {\em (5 33, $-$06 34)}.
Original paper: Bally \& Devine (1994). This is a faint HH object
between HH~34 and HH~86/87/88, which was shown by Devine et al. (1997)
in a kinematic study to be part of the HH~34 outflow.

\vspace*{0.3cm}

{\bf HH 174} {\em (22 54, +61 46)}. 
Original paper: Bally et al.  (1999). This is a Herbig-Haro object in
the Ceph A region located to the east of HH 168 and 169, see notes for
these objects.

\vspace{0.3cm}

{\bf HH 175} {\em (05 42, +09 09)}.  Original paper: Reipurth, Bally,
Heathcote (1999), who present CCD images. This is a bow shock located
4 1/2 arcmin ENE of and facing away from the source IRAS 05417+0907,
which is embedded in the B35 cloud. B35 is a cometary shaped cloud
facing $\lambda$ Ori (Lada \& Black 1976), and is best known for
harboring FU Orionis. The IRAS source is located near the peak of a
dense NH$_3$ core (Benson \& Myers 1989), and is driving a {\em
molecular outflow} (Myers et al. 1988). Terebey, Vogel, Myers (1992)
detected the source at 6 cm, as well as two {\em H$_2$O masers}, which
are further observed by Claussen et al. (1996).

\vspace*{0.3cm}

{\bf HH 176} {\em (5 28, +12 08)}.  Original paper: Goodrich (1993),
who presents CCD images and a spectrum, and suggests it is a bow shock
facing away from the Herbig Ae/Be star HK~Ori. This is confirmed by
higher resolution CCD images by Reipurth, Bally, Heathcote
(1999). HK~Ori is further discussed by Herbig (1960), Strom et
al. (1972), Finkenzeller \& Mundt (1984), and Hillenbrand et
al. (1992) summarize optical/ir/mm photometry. The cloud in which
HK~Ori is located has been studied by Zhou, Butner, Evans (1988). A
close companion to HK Ori with a separation of 0.33 arcsec was found
by Leinert et al. (1994).


\vspace*{0.3cm}

{\bf HH 179 } {\em (05 29, +12 33)}. Original paper: Reipurth,
Bally, Devine (1997), who present a wide-field CCD image. This is a
large diffuse cluster of HH knots, which is a distant bow shock in the
red lobe from the outflow centered on IRAS 05295+1247 which drives
also HH~243, 244 and 245. The HH flow coincides with a major molecular
outflow (Bence, Richer, Padman 1996). See also notes for HH~243.


\vspace*{0.3cm}

{\bf HH 180} {\em (18 14, $-$19 52)}. 
Original paper:  Reipurth (in prep.), who
present CCD images. This is a faint HH knot associated with a small
reflection nebula in the L291 cloud in Sagittarius.

\vspace*{0.3cm}

{\bf HH 183} {\em (5 35, $-$07 04)}.  Original paper: Strom et
al. (1986), who present CCD images. This is a single low-excitation HH
object, next to the bright reflection nebula IC430, illuminated by the
luminous partly embedded young star V883 Ori (= IRAS 05358--0704) in
L1641. Haro (1953) commented on IC430 (his Haro 13a). Allen et
al. (1975) provide optical/ir photometry and a spectrum of V883 Ori,
Nakajima et al. (1986) discuss ir variability, Strom et al. (1989)
give IRAS fluxes, and Reipurth et al. (1993a) found it to be bright at
1300 $\mu$m. Further sub-millimeter photometry is presented by Dent,
Matthew, Ward-Thompson (1998).  Strom \& Strom (1993) obtained spectra
of the reflection nebula and conclude that V883 Ori is a likely FU
Orionis object.

\vspace*{0.3cm}

{\bf HH 184} {\em (4 26, +24 26)}.  Original paper: Elias (1978), who
presents a spectrum and find the HH object to be coincident with an
infrared source (Haro~6-10 = GV Tau = Elias 7 = IRAS 04263+2426).
This is a compact HH knot overlying a young partly embedded star and
with faint outlying emission (Strom et al. 1986, G\'omez, Whitney,
Kenyon 1997).  Devine et al. (1999a) present wide field CCD images and
show that HH~184 is part of a giant HH flow (HH~410/411) stretching
over 38 arcmin.  Cohen \& Fuller (1985) also present a spectrum.
Hirth, Mundt, Solf (1997) present detailed long-slit spectra. A
high-resolution K-band image is discussed by Lucas \& Roche (1997).
Elias (1978) and Cohen \& Schwartz (1983) noted a continuous decline
in infrared brightness of the source. Bieging, Cohen, Schwartz (1984)
detected Haro 6-10 at 6 cm, Reipurth et al. (1993a) measured it at
1300 $\mu$m and Dent, Matthew, Ward-Thompson (1998) at other sub-mm
wavelengths, Carr (1990) and Herbst, Koresko, Leinert (1995) detected
H$_2$ towards the object, and Whittet et al. (1988) obtained near- and
mid-infrared spectra. Leinert \& Haas (1989) discovered a close
infrared companion, which was further observed by M\'{e}nard et
al. (1993) and Koresko, Herbst, Leinert (1997).  No molecular outflow
has been found (Edwards \& Snell 1984, Levreault 1988). Emission from
high-density ammonia gas was detected by Anglada et
al. (1989). HCO$^+$ and 2.7 mm continuum observations are presented by
Hogerheijde et al. (1997a,1998).  A 790 $\mu$m dust map and a
$^{12}$CO J=2-1 map is discussed by Chandler, Barsony, Moore (1998).
See also notes for HH~410/411.

\vspace*{0.3cm}

{\bf HH 185} {\em (15 39, $-$33 59)}.
Original paper: Heyer \& Graham (1989), who present CCD images and
spectra. This is a faint low-excitation HH object located next to the
IRAS source 15398--3359, detected as a faint near-infrared source by
Heyer \& Graham (1989). The object is located in the B228 cloud in the
Lupus 1 complex. The source was detected at 1300 $\mu$m by Reipurth et
al. (1993a).

\vspace*{0.3cm}

{\bf HH 186} {\em (15 42, $-$34 08)}.
Original paper: Heyer \& Graham (1989), who present CCD images
and spectra. This is a highly collimated [SII]-strong jet extending 34
arcsec from the T~Tauri star Sz~68 (= CoD -33$^\circ$10685 = IRAS
15420--3408). Sz~68 was observed spectroscopically by Appenzeller,
Jankovics, Krautter (1982), Finkenzeller \& Basri (1987) and Johns-Krull
\& Hatzes (1997). A faint
companion was found by Reipurth \& Zinnecker (1993). The binary was
detected at 1300 $\mu$m by Reipurth et al. (1993a).

\vspace*{0.3cm}

{\bf HH 187} {\em (15 42, $-$34 08)}.
Original paper: Heyer \& Graham (1989), who present CCD images and
spectroscopy. This is a faint high excitation HH object consisting of
two knots located 72 arcsec due east of Sz~68, see notes for HH~186.

\vspace*{0.3cm}

{\bf HH 188} {\em (8 19, $-$49 25)}.  Original paper: Graham (1986),
who presents CCD images and spectroscopy. Reipurth (1981) drew
attention to a little nebula in a globule in the Gum Nebula, and
Graham (1986) showed that the northern part of the nebula is a
low-excitation HH object, HH~188 (formerly Re~4 head); the main
southern part of Re~4 is a reflection nebula. The energy source is the
embedded star IRAS 08914--4925 (Cohen \& Schwartz 1987), detected in
the near-infrared by Graham \& Heyer (1989), and at 1300 $\mu$m by
Reipurth et al. (1993a). Further sub-millimeter photometry is
presented by Dent, Matthew, Ward-Thompson (1998).  CO observations are
reported by de Vries et al. (1984).

\vspace*{0.3cm}

{\bf HH 189} {\em (22 37, +74 55)}.  Original paper: Eiroa et
al. (1994b), who present CCD images. This is a chain of three HH knots
in L1251 pointing towards the embedded IRAS source 22376+7455, which
seems a likely driving source. The source is detected in the centimeter radio
continuum by Anglada et al. (1998).  Sato \& Fukui (1989) found a
molecular outflow from this source, and this outflow and the
surrounding cloud structure is discussed by Sato et
al. (1994). Ammonia maps are presented by T\'oth \& Walmsley (1996)
and Anglada, Sep\'ulveda, G\'omez (1997).  Hodapp (1994) presents a
wide field K$'$ band image.  Alten et al. (1997) show a large-field
CCD image of the region, which includes two further HH knots, HH 189 D
and E, apparently belonging to the same flow, plus three other groups
of HH objects, HH 364, 373 and 374.  For further details on L1251 see
the notes for HH~149.

\vspace*{0.3cm}

{\bf HH 190} {\em (5 27, +33 45)}.
Original paper: Eiroa et al. (1994b), who present CCD images. This is
a single HH object embedded in the large reflection nebula around the
AFGL~5142 source. Snell et al. (1988) found a molecular outflow from
this source. Mm data and an H$_2$O maser are discussed by
Verdes-Montenegro et al. (1989), Pastor et al. (1991), Torrelles et
al. (1992c), Wouterloot, Brand, Fiegle (1993), Estalella et
al. (1993), Xiang \& Turner (1995), Tofani et al. (1995), and Hunter
et al. (1995).

\vspace*{0.3cm}

{\bf HH 191} {\em (6 11, +13 50)}. 
Original paper: Eiroa et al. (1994c), who present CCD images and
longslit spectroscopy. The HH object has blueshifted radial velocities
up to 400 km/sec. It is associated with a luminous young source,
IRS~2, which is double in near-infrared images. The western component
may be associated with the IRAS source 06117+1350 and H$_2$O and OH
masers in the region and probably powers the HH object. For further
references see Eiroa et al. (1994c).

\vspace*{0.3cm}

{\bf HH 192} {\em (4 36, +25 57)}.
Original paper: Eiroa et al. (1994a), who present CCD images and a
spectrum. This is a small HH object, it is enveloped in a reflection
nebulosity that was discussed by Tamura et al. (1991), and observed
spectroscopically by Kenyon et al. (1998). L1527 is a small cloud core
studied by Benson \& Myers (1989) and Ohashi et al.  (1991). High
velocity CO wings are reported by Heyer et al. (1987) and Terebey et
al. (1989) around the cold source IRAS~04368+2557, which has been
studied by Ladd et al. (1991a,b). Strong near-infrared polarization
was measured by Whitney, Kenyon, G\'omez (1997). The source was also
detected at 3.6 cm by Rodr\'\i guez \& Reipurth (1998). Fuller, Ladd,
Hodapp (1996) found a companion at sub-mm wavelengths. High resolution
mm line and continuum maps of the environment of IRAS 04368+2557 are
discussed by Myers et al. (1995), Zhou, Evans, Wang (1996), Tamura et
al. (1996), Ohashi et al. (1997a), Matsumoto, Hanawa, Nakamura (1997),
and Hogerheijde et al. (1997a,1998).

\vspace*{0.3cm}

{\bf HH 193} {\em (3 21, +30 44)}. 
Original paper: Bally et al. (1997), who present CCD images and
spectra. This is a little chain of three HH knots in the L1448 cloud
(see also notes for HH~197).

\vspace*{0.3cm}

{\bf HH 194} {\em (3 21, +30 37)}. 
Original paper: Bally et al. (1997), who present CCD images and
spectra. These are two HH knots in the L1448 cloud (see also notes for
HH~197).

\vspace*{0.3cm}

{\bf HH 195} {\em (3 22, +30 36)}. 
Original paper: Bally et al. (1997), who present CCD images and
spectra. This is a chain of faint HH knots just north-east of the
reflection nebula RNO~13 in the L1448 cloud (Cohen 1980a). See also
notes for HH~197.

\vspace*{0.3cm}

{\bf HH 196} {\em (3 22, +30 38)}. 
Original paper: Bally et al. (1997), who present CCD images and
spectra. This is a cluster of HH knots in the L1448 cloud (see also
notes for HH~197).

\vspace*{0.3cm}

{\bf HH 197} {\em (3 22, +30 34)}.  Original paper: Eiroa et al.
(1994a), who present CCD images; see also Bally et al. (1997). This is
a single HH object located just south of a compact reflection nebula
apparently associated with the brightest IRAS source, 03225+3034, in
the L1448 cloud. This source is associated with bright H$_2$ emission
clumps (Bally, Lada, Lane 1993, Davis et al. 1994), a strong H$_2$O
maser (Anglada et al. 1989, Wouterloot, Brand, Fiegle 1993, Chernin
1995, Claussen et al. 1996), an ammonia core (Anglada et al. 1989),
and the core has been mapped in HCO$^+$ and CS by Davis et al. (1994)
and in $^{13}$CO by Bally \& Devine (1995).  A molecular outflow was
detected by Bachiller et al. (1990), who also mapped the core in
$^{13}$CO and CS. IRS~3 was detected in the radio continuum as a
double radio source with about 8 arcsec separation (Curiel et
al. 1990). Polarized 800 $\mu$m emission was detected towards IRS~3 by
Greaves, Holland, Ward-Thompson (1997).  The L1448 cloud is a dense
core about one degree south-west of NGC~1333 in the Perseus dark
clouds (Bachiller \& Cernicharo 1986a,b). About 80 arcsec south of
IRS~3 is a deeply embedded source detected at centimeter and sub-mm
wavelengths (Curiel et al. 1990, Bachiller, Andr\'e, Cabrit 1991),
which drives a major bipolar molecular hydrogen complex (Bally, Lada,
Lane 1993, Davis et al. 1994, Davis \& Smith 1995, 1996) and a fast
collimated molecular outflow (Bachiller et al. 1990, Bachiller,
Martin-Pintado, Fuente 1991, 1993, Guilloteau et al. 1992, Bachiller
et al. 1995b, Dutrey, Guilloteau, Bachiller 1997). Ceccarelli et
al. (1997) measured OI 63 $\mu$m emission towards both L1448-mm and
L1448-IRS3. Barsony et al. (1998) present far-infrared, submillimeter
and millimeter images of all the known protostars in L1448.


\vspace*{0.3cm}

{\bf HH 198} {\em (21 00, +78 11}. 
Original paper: Brugel \& Fesen (1990). This object (formerly RNO 129
in Cohen 1980) has been studied with CCD imaging and spectroscopy by
Bally et al. (1995). It consists of two bright H$\alpha$-strong knots
surrounded by a complicated compact nebulosity. The eastern knot
contains a star at its southern end.

\vspace{0.3cm}

{\bf HH 199} {\em (20 55, +77 20)}. 
Original paper: Bally et al. (1995), who present CCD images,
spectroscopy, near-infrared images and mm-data. This is an about 2 pc
long bipolar HH flow consisting of many knots emanating from the low
luminosity source IRAS 20582+7724, embedded in a cloud core in the
L1228 cloud. The source was detected at 3.6 cm with the VLA by Rodr\'\i
guez \& Reipurth (1996). It is associated with a large molecular
outflow (Bally et al. 1995, Tafalla \& Myers 1997).
$^{13}$CO observations of L1228 are discussed by Miesch \&
Bally (1994). An ammonia core was mapped by Anglada, Sep\'ulveda,
G\'omez (1997).  See also notes for HH 200.

\vspace*{0.3cm}

{\bf HH 200} {\em (20 56, +77 19)}.
 Original paper: Bally et al. (1995), who present CCD images,
spectroscopy and mm-data.  This is an about 1.8 pc long bipolar HH
flow emanating from a star embedded in a cloud core in the L1228
cloud. The flow contains a bright and prominent bow shock. There is a
weak molecular outflow coincident with the HH flow. The L1228 cloud
has been studied in $^{12}$CO and $^{13}$CO and at 100 $\mu$m by
Haikala \& Laureijs (1989), and in $^{13}$CO by Miesch \& Bally
(1994). An ammonia core was mapped by Anglada, Sep\'ulveda, G\'omez
(1997).  Many H$\alpha$ emission stars have been found around the
cloud by Ogura \& Sato (1990). 

\vspace*{0.3cm}

{\bf HH 201} {\em (5 32, $-$05 23)}.  Original paper: M\"unch \& Taylor
(1974), Gull et al. (1973). The latter reference gives no position nor a
finding chart, but their object appears to be the same found in the former
reference. This is an isolated HH object (formerly M42-HH1) near the
Trapezium and is resolved into a multitude of sub-knots in HST images
(Hester et al.  1991, O'Dell et al. 1997a).  Spectra of the object are
discussed by M\"unch \& Taylor (1974), M\"unch (1977), Axon \& Taylor
(1984) and Hu (1996). Taylor et al.  (1986) and O'Dell et al. (1997b)
present Fabry-Perot observations. The proper motion studies of Jones \&
Walker (1985) and Hu (1996) show motion away from the BN region.  Infrared
images of Allen \& Burton (1993) show the object to be weak in H$_2$ but
strong in [FeII]. 

\vspace*{0.3cm}

{\bf HH 202} {\em (5 32, $-$05 24)}.  Original paper: Cant\'{o} et
al. (1980), who present photographic plates and spectroscopy. This is
a rather large object (formerly M42-HH2) with a bow shock morphology
located close to the Trapezium, seen well in the HST images of Hester
et al. (1991), O'Dell \& Wong (1996) and O'Dell et al. (1997a).
Spectra are discussed in detail by Meaburn (1986), by O'Dell, Wen,
Hester (1991), and by Clayton \& Meaburn (1994). Fabry-Perot
observations by O'Dell et al. (1997b) reveal a long curved jet-like
feature of high velocity gas which extends to the south-east from HH
202. Detailed HST NICMOS images are presented by Schultz et
al. (1999).

\vspace*{0.3cm}

{\bf HH 203} {\em (5 32, $-$05 26)}.  Original paper: Taylor \& M\"unch
(1978). This is a very fine bow shock (formerly cloudlet~A or M42-HH3)
located just outside the Orion Bar, and with an apparent origin in the
direction of the Trapezium or BN region.  Part of the object appears in the
HST images of O'Dell, Wen, Hu (1993) and it is fully depicted in the HST
images of O'Dell \& Wen (1994), O'Dell \& Wong (1996) and O'Dell et
al. (1997a).  Spectra are discussed by Taylor \& M\"unch (1978), Cant\'{o}
et al. (1980), Walsh (1982), and Hu (1996). O'Dell et al. (1997b) present
Fabry-Perot observations. The infrared images of Allen \& Burton (1993)
show the object to be very weak in H$_2$ and strong in [FeII]. Yusef-Zadeh
(1990) detected the object in the radio continuum at 20 cm.

\vspace*{0.3cm}

{\bf HH 204} {\em (5 32, $-$05 27)}.  Original paper: Taylor \& M\"unch
(1978). This is a bright somewhat amorphous HH object (formerly cloudlet~B
or M42-HH4) close to HH~203 just outside the Orion Bar. It is partly seen
in the HST images of O'Dell \& Wen (1994), and in great detail in HST
images through several interference filters by O'Dell \& Wong (1996) and O'Dell
et al. (1997a).  Spectra are discussed by Taylor \& M\"unch (1978),
Cant\'{o} et al. (1980), Walsh (1982) and Hu (1996), and O'Dell et
al. (1997b) present Fabry-Perot observations. Proper motions are determined
by Cudworth \& Stone (1977) and Hu (1996).  In the infrared images of Allen
\& Burton (1993) it is barely seen in H$_2$ but is very strong in
[FeII]. The object is detected in the radio continuum at 20 cm by
Yusef-Zadeh (1990).

\vspace*{0.3cm}

{\bf HH 205/206/207} {\em (5 32, $-$05 22)}.  Original paper: Axon \&
Taylor (1984), who present electronographic plates and spectra. This
is a chain of HH knots (formerly M42-HH5,6,7) which break into
numerous condensations in the HST images of Hester et al. (1991) and
O'Dell et al. (1997a).  A proper motion determination of HH~205 by
Jones \& Walker (1985) suggests an origin near BN or IRc2. The
infrared images of Allen \& Burton (1993) show that the three HH
objects form part of the brightest of the ``fingers'' streaming out
from the BN/IRc2 region, reminiscent of explosively ejected
matter. Possible formation mechanisms are discussed by Stone, Xu,
Mundy (1995) and Gvaramadze (1997).  The HH objects are visible in
H$_2$ as well as [FeII]. Hu (1996) present a proper motion and radial
velocity study of HH 205 and 206. O'Dell et al. (1997b) analyze
Fabry-Perot observations. A vast literature exists on the BN/IRc2
region, a recent study with references to the main literature is given
by Gezari, Backman, Werner (1998).

\vspace*{0.3cm}

{\bf HH 208} {\em (5 32, -05 24)}.  Original paper: Axon \& Taylor
(1984), who present electronographic plates and spectra. This is a
single little-studied HH object (formerly M42-HH8), seen in the HST
images of Hester et al. (1991), and O'Dell et al. (1997a). Fabry-Perot
observations are discussed by O'Dell et al. (1997b). Detailed HST
NICMOS images are presented by Schultz et al. (1999).

\vspace*{0.3cm}

{\bf HH 209} {\em (5 32, $-$05 23)}.  Original paper: Axon \& Taylor
(1984), who present electronographic plates and spectra. This object
(formerly M42-HH9) is resolved into two close knots and a filament in the
HST images of Hester et al.  (1991) and O'Dell et al. (1997a). It is
detected in the H$_2$ and [FeII] images of Allen \& Burton (1993).
Fabry-Perot observations are discussed by O'Dell et al. (1997b).

\vspace*{0.3cm}

{\bf HH 210} {\em (5 32, $-$05 22)}.  Original paper: Axon \& Taylor
(1984), who present electronographic plates and spectra. This object
(formerly M42-HH10) shows a wealth of detail in the HST images of Hester et
al. (1991) and O'Dell et al. (1997a).  A proper motion study of Jones \&
Walker (1985) suggests an origin in the BN region.  Fabry-Perot
observations are discussed by O'Dell et al. (1997b).  The infrared images
of Allen \& Burton (1993) do not detect it in H$_2$, but it is prominent in
[FeII]. Hu (1996) presents a high-resolution spectrum.

\vspace*{0.3cm}

{\bf HH 211} {\em (3 40, +31 51)}.  Original paper: McCaughrean,
Rayner, Zinnecker (1994).  This is a fine highly collimated bipolar
jet located in the IC 348 region. The jet has so far only been
detected in molecular hydrogen through near-infrared imaging. The jet
is 0.15 pc long and the lobes emanate from a dense NH$_3$ core
(Bachiller, Guilloteau, Kahane 1987). The jet coincides with a
molecular outflow, and both are driven by a cold sub-mm source
(McCaughrean, Rayner, Zinnecker 1994). Sub-millimeter photometry of
the source is given by Dent, Matthews, Ward-Thompson (1998).  The
region is close to IC 348, a cluster of young stars (Strom, Strom,
Carrasco 1974), and harbours a number of H$\alpha$ emission stars
(Herbig 1954b). Infrared images of the cluster are discussed by Lada
\& Lada (1995), and X-ray observations by Preibisch, Zinnecker, Herbig
(1997). A detailed optical/infrared study of the stellar population
within the core of IC~348 was performed by Luhman et al. (1998).

\vspace{0.3cm}

{\bf HH 212} {\em (05 41, $-$01 04)}.  Original paper: Zinnecker,
McCaughrean, Rayner (1998), who present infrared imaging and
spectroscopy. This is a spectacular molecular hydrogen jet, which is
only seen in the infrared except for the most distant bow shock which
also shows up in [SII] emission CCD images. The jet is highly
symmetric, and centered on the cold IRAS source 05413--0104, observed
at 1300 $\mu$m by Zinnecker et al. (1992) and at other sub-millimeter
wavelengths by Dent, Matthew, Ward-Thompson (1998).  Claussen et
al. (1998) have detected a bipolar distribution of masers around the
source along the jet axis, and their VLBI measurements combining
radial velocities and proper motions suggest a flow inclination of
only 4 degrees to the plane of the sky, and an origin of the outflow
as close as 40 AU from the source.

\vspace*{0.3cm}

{\bf HH 213} {\em (17 59, $-$24 17)}.
Original paper: Reipurth (1981). This is a little HH flow consisting
of two knots, one with the appearance of a small bow shock as seen in
CCD images (Reipurth, in preparation). They are located in the active
star formation region M8.

\vspace*{0.3cm}

{\bf HH 214} {\em (20 18, +37 00)}.
Original paper: Neckel \& Staude (1987a), who present CCD images,
long-slit spectroscopy and polarimetry. This is a single HH knot
located in the brighter lobe of a bipolar reflection nebula around the
bright IRAS source 20183+3700, located in small dense cloudlet in
Cygnus. It was found independently through spectroscopy by Magakyan
(1988). The HH object was studied spectroscopically by Magakian \&
Movsessian (1995).  Scarrott, Rolph, Tadhunter (1991b) also did
surface polarimetry of the reflection nebula.

\vspace*{0.3cm}

{\bf HH 215} {\em (20 45, +67 46)}.
Original paper: Neckel et al. (1987), who present CCD images and
long-slit spectroscopy. These are two Herbig-Haro objects lying on a
line through the young star PV~Cephei and partly within its principal
reflection lobe. The reflection nebula is highly variable (Cohen,
Kuhi, Harlan 1977, Cohen et al. 1981, Neckel \& Staude 1984), and is
bipolar (Levreault \& Opal 1987). Spectroscopy of the nebula is
reported by Cohen, Kuhi, Harlan (1977), Cohen et al. (1981), Neckel et
al. (1987). Carr (1990) detected Br$\gamma$ and H$_2$ emission towards
the source. Levreault (1984) mapped a molecular outflow. Anglada et
al. (1992) detected PV~Cep in the radio continuum.  Fuente et
al. (1998) present $^{13}$CO, CS and 1.3 mm continuum maps.  HH 215
forms the innermost part of a much larger bipolar HH flow, HH 315,
from PV Cep. See also notes for HH 415.

\vspace*{0.3cm}

{\bf HH 216} {\em (18 16, $-$13 53)}.
Original paper: Meaburn \& White (1982). This is a large elongated HH
object (formerly M16-HH1) situated in prominent elephant-trunks in
the HII region NGC~6611. Extensive optical and ultraviolet
spectroscopy of the line and continuum emission from this object are
reported by Meaburn \& White (1982), Meaburn (1982), Meaburn \& Walsh
(1984), Krautter, Reipurth, Eichendorf (1984), and Meaburn \&
Whitehead (1990); the latter also present various interference filter
CCD images. No energy source has been identified so far (e.g. Walsh \&
White 1982).

\vspace*{0.3cm}

{\bf HH 217} {\em (8 15, $-$35 43)}. Original paper: Neckel \& Staude
(1995), who present CCD images, infrared images and long-slit
spectroscopy. This is a bipolar Herbig-Haro flow, which is part of the
larger nebulosity GM 1-27 = GN~08.15.9, surrounding the luminous embedded
class~I IRAS source 08159--3543. Centimeter radio emission from an 
ionized wind is reported by Felli et al. (1998).

\vspace*{0.3cm}

{\bf HH 218} {\em (21 38, +50 00)}.  
Original paper: Goodrich (1986b), who presents CCD images and
spectroscopy of an HH object associated with V645 Cygni. This is a
high-luminosity star with L~=~$6 \times 10^4 L_\odot$ at a distance of
3.5 kpc, corresponding to a massive newborn star. It is extensively
studied, and principal references are given here. The star is
associated with a small structured reflection nebula; images are shown
by Cohen (1977), Goodrich (1986b), and Lenzen (1987). Optical spectra
of star and nebulae are discussed by Cohen (1977), Humphreys, Merrill,
Black (1980), Goodrich (1986b), Hamann \& Persson (1989) and Corcoran
\& Ray (1997). Infrared spectroscopy is discussed by Harvey \& Lada
(1980), Geballe \& Persson (1987), Kelly, Rieke, Campbell (1994), and
Carr (1990) detected Br$\gamma$ emission. Radio continuum observations
are reported by Curiel et al. (1989b) and Skinner, Brown, Stewart
(1993). Ammonia emission was mapped by Torrelles et al. (1989b). A
molecular outflow has been observed by Rodr\'\i guez, Torrelles, Moran
(1981), Torrelles et al. (1987), Schulz et al. (1989) and
Verdes-Montenegro et al. (1991). H$_2$O and OH masers are reported by
Lada et al. (1981) and Morris \& Kaz\`{e}s (1982).  A disk/envelope
model has been fitted to the energy distribution by Natta et
al. (1993).

\vspace*{0.3cm}

{\bf HH 219} {\em (8 21, $-$41 59)}.
Original paper: Graham (1991), who presents a photograph and
spectroscopy. This is a relatively compact and knotty object with a
low-excitation spectrum. It is close to a small nebula reflecting
light from the embedded luminous IRAS source 08211--4158, which has
also been observed by Persson \& Campbell (1988). Scarrott et al.
(1992) present surface polarimetry of the reflection nebula.

\vspace*{0.3cm}

{\bf HH 220} {\em (4 11, +28 03)}.  Original paper: G\'{o}mez de Castro
(1993), who presents high-resolution CCD images. This is a short bipolar
jet system stretching 4-6 arcsec on either side of the young star CW~Tau (=
HBC 25).  Hirth, Mundt, Solf (1994a) discuss long-slit spectroscopy of the
HH complex.  CW~Tau is a T~Tauri star observed spectroscopically by
Rydgren, Strom, Strom (1976), Cohen \& Kuhi (1979), Sun et al. (1985),
Edwards et al.  (1987), and Walker (1987), and with near-infrared
spectroscopy by Greene \& Lada (1996b).  Sub-mm observations are given by
Beckwith et al. (1990) and Beckwith \& Sargent (1991). 

\vspace*{0.3cm}

{\bf HH 221} {\em (19 26, +09 32)}.  Original paper: Staude \& Neckel
(1992), who present CCD images and long-slit spectroscopy. This is a
short Herbig-Haro flow oriented along the axis of the cometary
reflection nebula Parsamian~21 (Parsamian 1965).  The nebula was
studied by Petrosian (1984), who derived a spectral type of
F2-F5V. Further spectroscopic observations are discussed by Parsamian,
Gasparian, Ohanian (1996).  Near-infrared spectroscopy is presented by
Greene \& Lada (1996b).  Cohen (1974a) presented infrared photometry
and Eiroa \& Hodapp (1990) infrared images. A polarization study was
done by Draper, Warren-Smith, Scarrott (1985a). Hillenbrand et
al. (1992) summarize optical/infrared photometric observations.
Henning et al. (1998) present a 1300 $\mu$m map.  No molecular outflow
has been found (Bally \& Lada 1983).

\vspace*{0.3cm}

{\bf HH 222} {\em (5 33, $-$06 24)}.
Original paper: Cohen \& Schwartz (1983). This is a peculiar
Herbig-Haro object consisting of a number of large arcs or streamers,
one of them 5~arcmin long, emanating from a common point 15~arcsec SE
of the T~Tauri star V571~Orionis in a region of L1641 rich in star
formation. Reipurth \& Sandell (1985) present CCD images, optical
spectroscopy and mm observations and in the absence of other sources
suggested that a wind from V571 Ori could interact with a cloud ridge
producing the shock. This interpretation became obsolete with the
discovery of a significantly polarized non-thermal VLA source at the
core of the streamers, and with a faint near-infrared counterpart
(Yusef-Zadeh et al. 1990). The VLA source was also observed by Morgan,
Snell, Strom (1990).

\vspace*{0.3cm}

{\bf HH 223} {\em (19 15, +19 06)}.  Original paper: Vrba et
al. (1986), who present CCD images and polarization data. Long slit
spectroscopy is presented by Movsesyan (1989).  This is a Herbig-Haro
object, possibly part of a small group, near the young IRAS source
19156+1906, studied by Davidson (1987) and located in the molecular
cloud L723.  Infrared images are presented by Hodapp (1994) and
Palacios \& Eiroa (1999).  The source is at the center of a four-lobe
molecular outflow (Goldsmith et al. 1984, Mirabel et al. 1987,
Moriarty-Schieven \& Snell 1989, Avery, Hayashi, White 1990, Hayashi,
Hasegawa, Kaifu 1991, Girart et al. 1997).  VLA observations of
Anglada et al. (1991) show a double source, suggesting that each
drives a molecular outflow. Anglada, Rodr\'\i guez, Torrelles (1996)
found a thermal radio jet in the region.  Only one source is detected
at 1300 $\mu$m, corresponding to the north-eastern (VLA~2) of the VLA
sources (Cabrit \& Andr\'e 1991, Reipurth et al. 1993a).
Interferometric CO and single dish CS observations support that VLA~2
is powering the outflow activity (Hirano et al. 1998).

\vspace*{0.3cm}

{\bf HH 224} {\em (16 24, $-$24 40)}.  Original paper: Wilking, Schwartz,
Blackwell (1987), who noted this object in an objective prism survey of the
Ophiuchus clouds. CCD images by Wilking et al. (1997a) and G\'omez, Whitney,
Wood (1998) show this to be a group of faint HH knots stretching towards
the north-west. Reipurth et al. (1993a) suggested that they emanate from
the southern component of the young binary SR~24.  The binary was found by
Struve \& Rudkj\o bing (1949), is identical to IRAS 16239--2438, and was
detected at 1300 $\mu$m by Reipurth et al. (1993a). However, Wilking et
al. (1997a) point out that other possible sources exist, and with the recent
discovery of faint extensions to the north-west, the whole complex looks
like a giant bow shock, which may well be driven by a more distant source.

\vspace*{0.3cm}

{\bf HH 225} {\em (6 38, +09 47)}.
Original paper: Adams, Strom, Strom (1979), who present photographic
plates and spectra. This is a group of HH knots located in the star
formation region NGC~2264. A search for an energy source is discussed
by Cohen \& Schwartz (1983), and Cohen, Harvey, Schwartz (1985).
HH~225 and 226 may be related to HH~125 (Walsh, Ogura, Reipurth 1992),
see notes for this object.

\vspace*{0.3cm}

{\bf HH 226} {\em (6 38, +09 42)}.
Original paper: Adams, Strom, Strom (1979), who present photographic
plates and spectra. This is a group of HH knots located in the star
formation region NGC~2264. A search for an energy source is discussed
by Cohen \& Schwartz (1983), and Cohen, Harvey, Schwartz (1985).
HH~226 and 225 may be related to HH~125 (Walsh, Ogura, Reipurth 1992),
see notes for this object.

\vspace*{0.3cm}

{\bf HH 227} {\em (6 57, $-$04 41)}.
Original paper: Neckel \& Staude (1992), who present CCD images and
long-slit spectroscopy. This is a single HH object located in the S287
molecular cloud next to the 440~L$_\odot$  embedded IRAS source
06571--0441. The source drives a molecular outflow (Fukui 1989).

\vspace*{0.3cm}

{\bf HH 228} {\em (16 05, $-$38 55)}.  Original paper: Krautter
(1986), who presents CCD images, long-slit spectroscopy, proper
motions, and infrared photometry of the source.  This is a bipolar jet
complex emanating from the young star Th~28, which is located in the
Lupus~3 cloud (Th\'e 1962), and is studied spectroscopically by
Appenzeller, Jankovics, Krautter (1983), Appenzeller, Jankovics,
\"{O}streicher (1984), Krautter, Reipurth, Eichendorf (1984) and
Graham \& Heyer (1988). Far-infrared fluxes of Th 28 are given by
Cohen \& Schwartz (1987). Graham \& Heyer (1988) discuss further
long-slit spectroscopy of star and HH flow, and note an additional
eastern bow shock, and point out a possible link to the nearby
HH~78. Bacciotti \& Eisl\"offel (1999) discuss long-slit spectroscopy
of the jet.

\vspace*{0.3cm}

{\bf HH 229} {\em (5 04, +30 20)}.
Original paper: Hirth, Mundt, Solf (1994b). This is a bipolar HH flow
from the T Tauri star RW~Aur, with a total extent of at least 145$''$
(Mundt \& Eisl\"offel 1998).  The two sides are asymmetric in velocity and
excitation.  The physical properties of the jet is discussed by
Bacciotti, Hirth, Natta (1996). Further long-slit spectra are analyzed
by Hirth, Mundt, Solf (1997). A high-resolution spectrum of the star
is presented by Hamann (1994).  RW~Aur is a close visual binary (Joy
\& van Biesbrock 1944), and the companion itself is also a very close
binary (separation 0.12$''$) found by Ghez, Neugebauer, Matthews
(1993).  The star is extensively studied, see Herbig \& Bell (1988)
for references.

\vspace*{0.3cm}

{\bf HH 230} {\em (4 35, +26 04)}.  Original paper: Hirth, Mundt, Solf
(1994b). This is a bipolar HH flow stretching 2 - 4 arcsec on either
side of the T~Tauri star DO~Tau. A large velocity difference is seen
between the two lobes.  Long-slit spectra are analyzed by Hirth,
Mundt, Solf (1997).  Tessier, Bouvier, Lacombe (1994) suggest that DO
Tau may be a binary with 0.2 arcsec separation.  Optical spectroscopy
of the star is discussed by Edwards et al. (1987) and infrared
spectroscopy by Muzerolle, Hartmann, Calvet (1998).  Sub-mm photometry
is given by Manning \& Emerson (1994).  Koerner, Chandler, Sargent
(1995) discuss 7 mm continuum VLA observations, and Koerner \& Sargent
(1995) present aperture synthesis imaging of CO (2-1) emission.  See
Herbig \& Bell (1988) for further references.

\vspace*{0.3cm}

{\bf HH 231} {\em (4 39, +25 10)}. 
Original paper: Hirth, Mundt, Solf (1994b). This is an asymmetric
bipolar HH flow from the T~Tauri star DP~Tau.
Long-slit spectra are analyzed by Hirth, Mundt, Solf (1997), and CCD images
are presented by Mundt \& Eisl\"offel (1998).
For further references on the star, see Herbig \& Bell (1988).

\vspace*{0.3cm}

{\bf HH 232} {\em (21 41, +65 50)}. 
Original papers: Gyulbudaghian \& Magakyan (1977a), Gyulbudaghian,
Glushkov, Denisyuk (1978). This is a fairly bright HH object (formerly
GGD~32) in the NGC~7129 region; it is connected with HH~103, and both
objects are part of a large complex of fainter HH emission (Eiroa,
G\'omez de Castro, Miranda 1992, Magakyan et al. 1994).  CCD images
are presented by Hartigan \& Lada (1985), Strom et al. (1986), Eiroa,
G\'omez de Castro, Miranda (1992), and Goodrich (1993). Spectra are
discussed by Magakyan (1983), Cohen \& Fuller (1985) and Magakyan et
al. (1994). Ray et al. (1990) measured the proper motion of the
object. It was detected in H$_2$ by Wilking et al.  (1990). Cohen \&
Schwartz (1983) searched for an infrared energy source.

\vspace{0.3cm}

{\bf HH 233} {\em (04 35, +26 04)}. Original paper: Magazz\`u \&
Mart\'\i n (1994), who present spectra showing strong forbidden line
emission close to HV~Tauri, a weak-lined T Tauri star in the L1527
cloud.  Woitas \& Leinert (1998) suggest that the object seen by
Magazz\`u \& Mart\'\i n (1994) is not an HH object, but rather an
obscured companion star HV~Tauri~C, which itself has strong emission
lines.  CCD images show a tiny H$\alpha$ strong knot about 18 arcsec
NNW of HV~Tau, suggesting that the outflow is rather extended
(Reipurth, Bally, Devine, unpublished).  Simon et al. (1992) found
HV~Tau to be a triple system.


\vspace*{0.3cm}

{\bf HH 234} {\em (21 42, +65 54)}.  Original papers: Gyulbudaghian \&
Magakyan (1977a), Gyulbudaghian, Glushkov, Denisyuk (1978).  This is a
chain of three HH knots located in the NGC~7129 region.  The HH nature of
HH~234 (formerly GGD~34) was recognized spectroscopically by Magakyan
(1984). Based on CCD images, Ray (1987) suggested HH~234 is a jet. A
detailed imaging and spectroscopic study is presented by G\'omez de Castro,
Miranda, Eiroa (1993). Other CCD images are discussed by Hartigan \& Lada
(1985), Strom et al. (1986), and Eiroa, G\'omez de Castro, Miranda
(1992). Early spectra are presented by Magakyan (1984) and Goodrich
(1986). The radial velocity field was measured by Magakyan \& Movsesyan
(1997a).  Proper motion was measured by Ray et al. (1990). No source has
been found so far (Cohen \& Schwartz 1983), but the presence of a
reflection nebula at the western edge of the jet suggests the source is
located there (Ray 1987, G\'omez de Castro, Miranda, Eiroa 1993).

\vspace*{0.3cm}

{\bf HH 235} {\em (21 42, +65 54)}.  Original papers: Gyulbudaghian \&
Magakyan (1977a), Gyulbudaghian, Glushkov, Denisyuk (1978). This is an
amorphous HH object (formerly GGD 35) close to HH 234 and HH 105 in the NGC
7129 region. CCD images are presented by Hartigan \& Lada (1985), Strom et
al. (1986) and Eiroa, G\'omez de Castro, Miranda (1992). Spectra are
discussed by Magakyan (1983), Cohen \& Fuller (1985), Goodrich (1986),
Magakyan et al. (1994), and Magakyan \& Movsesyan (1997a). Proper motion has
been measured by Ray et al. (1990).

\vspace*{0.3cm}

{\bf HH 236/237/238/239} {\em (21 41, +65 52)}. 
Original paper: Miranda, Eiroa, G\'omez de Castro (1993). These are four
faint HH objects located to the west of LkH$\alpha$~234 in the NGC
7129 region; they do not appear to be physically related. Spectra are
shown of HH 238 and 239 (formerly N7129-HH 3 and 4).

\vspace*{0.3cm} 

{\bf HH 240} {\em (5 17, $-$05 54)}.  Original paper: Cohen (1980a),
who listed this object as RNO~40 in his survey of red and nebulous
objects.  It is located in the small highly opaque cloud L1634.  CCD
images show this to be a chain of HH knots with a bright central core
(Bohigas, Persi, Tapia 1993).  Spectra are discussed by Jones et
al. (1984) and Goodrich (1986), and the object was detected in H$_2$
by Schwartz, Cohen, Williams (1987).  Bohigas, Persi, Tapia (1993)
present near-infrared images which show that a star is at the center
of RNO 40, and they suggest this is the driving source. This is not
supported by the large-field K' band image of Hodapp (1994).
Previously, Cohen, Harvey, Schwartz (1985) found a far-infrared source
to the E-S-E of HH~240. This is IRAS05173--0555 (Cohen \& Schwartz
1987), detected at 1300 $\mu$m by Reipurth et al.  (1993a) and at
other sub-millimeter wavelengths by Dent, Matthew, Ward-Thompson
(1998). Jones et al. (1984) measured a large proper motion of HH~240
with a direction that, within the errors, points away from the
far-infrared source, and moreover found a faint HH object, now HH~241,
on the opposite side of the source (see notes on HH~241), which
suggests that HH~240 and 241 form a bipolar HH complex driven by
IRAS05173--0555. This is confirmed by the infrared H$_2$ images of
Hodapp \& Ladd (1995) and Davis et al. (1997a), who find that HH
240/241 in H$_2$ form a highly symmetric bipolar outflow along a well
defined axis centered on the IRAS 05173--0555 source. Limited CO data
by Davis et al. (1997a) show the presence of a CO outflow, where the
eastern part is redshifted and the western blueshifted.


\vspace*{0.3cm}

{\bf HH 241} {\em (5 17, $-$05 55)}. 
Original paper: Jones et al. (1984), who comment on a faint nebula
east of HH~240. Cohen, Harvey, Schwartz (1985) note that this is an HH
object. CCD images by Reipurth (unpublished) show HH~241 to be a group
of faint HH objects appearing like bow shocks facing towards the east,
away from the IRAS source 05173--0555, located between HH~240 and
241. Jones et al. (1984) show that HH 241 has proper motions directed
away from the IRAS source. See also notes for HH 240.

\vspace*{0.3cm}

{\bf HH 242} {\em (21 41, +65 52)}. 
Original paper: Miranda, Eiroa, G\'omez de Castro (1993), who present
CCD images and long-slit spectroscopy. This is a bow-shaped HH object
located close to a star, HL14, in the NGC~7129 region. The authors find
HL14 to be an emission line star and suggest the HH object could be a
bent jet from HL14. However, a chance superposition cannot be
excluded.

\vspace*{0.3cm}

{\bf HH 243} {\em (5 29, +12 51)}.  Original paper: Cohen (1980a), who
listed this as RNO~43 in his survey of red and nebulous objects. This
is a large HH flow terminating in a bright bow shock. It is bipolar,
with the counterlobe ending in HH~244. CCD images are presented by Ray
(1987), Mundt, Brugel, B\"uhrke (1987), Reipurth (1991), Eisl\"offel
\& Mundt (1997), and Reipurth, Bally, Devine (1997). Spectroscopy is
given by Jones et al. (1984) and Magakyan \& Movsesyan (1994).  Jones
et al. (1984) also show proper motion vectors pointing away from a
far-infrared source found by Cohen, Harvey, Schwartz (1985). This is
an IRAS source 05295+1247 (Cohen \& Schwartz 1987), with a large error
in its position. Accurate positions derived from sub-mm data are given
by Zinnecker et al. (1992) and Reipurth et al. (1993a), and from a
radio continuum counterpart detected by Anglada et al. (1992,1998).
Sub-millimeter photometry is presented by Dent, Matthew, Ward-Thompson
(1998).  A large molecular outflow has been mapped by Edwards \& Snell
(1984), Cabrit, Goldsmith, Snell (1988) and Bence, Richer, Padman
(1996).  Emission from high-density ammonia gas has been detected by
Anglada et al. (1989) and Anglada, Sep\'ulveda, G\'omez (1997).  See
also notes for HH~244, 245 and 179.

\vspace*{0.3cm}

{\bf HH 244} {\em (5 29, +12 43)}.
Original paper: Reipurth (1991). This is a large bow shock in the
receding lobe of a major outflow, which between the tips of HH~243 and
HH~244 spans more than 8~arcminutes ($>$1pc). CCD images are presented
by Reipurth (1991), Eisl\"offel \& Mundt (1997) and Reipurth, Bally,
Devine (1997).  See notes for HH~243.

\vspace*{0.3cm}

{\bf HH 245} {\em (5 29, +12 56)}.
Original paper: Jones et al. (1984), who provide proper motion
estimates. Ray (1987) shows CCD images that reveal HH~245 to be a long
well collimated chain of HH knots terminating in a bright bow shock
(formerly RNO~43 North). He suggests a physical relation to HH~243,
while Mundt, Brugel, B\"uhrke (1987) argue for two separate flows.
Bence, Richer, Padman (1996) demonstrate that the molecular outflow at
HH 245 is part of a single huge outflow driven by HH 243~IRS (= IRAS
05295+1247). Further CCD images are presented by Eisl\"offel \& Mundt
(1997) and Reipurth, Bally, Devine (1997).  Magakyan \& Movsesyan
(1993) present spectra, radial velocities and electron densities. The
molecular flows are complex in this region (Edwards \& Snell 1984,
Cabrit, Goldsmith, Snell 1988). Anglada et al. (1992) draw attention
to a radio continuum source near the base of the HH~245 flow.  See
notes for HH 243.

\vspace*{0.3cm}

{\bf HH 246} {\em (8 19, $-$49 29)}.
Original paper: Graham (1986), who presents photographic plates and
spectroscopy. This is a small, about 10 arcsec long jet emanating from
a faint M-type star.

\vspace*{0.3cm}

{\bf HH 247} {\em (5 39, $-$02 18)}.
Original paper: Malin, Ogura, Walsh (1987), who present photographic
plates, low- and high-dispersion spectra and proper motion
measurements. This is a chain of HH knots (formerly N2023-HH1,4,5)
located at the edge of the large reflection nebula NGC 2023 around the
B-star HD~37903. The region is seen well in the photographs of Witt \&
Malin (1989).  Fuente, Mart\'\i n-Pintado, Gaume (1995) report on
high-density filaments in NGC 2023, and give further references to
studies of the region. An H$_2$O maser was reported by Xiang \& Turner
(1995).  The HH knots are lying on a line, and the proper motion
vectors suggest an origin to the north-east, inside NGC 2023. An
H$\alpha$ emission star (HH 247 star C) is located on the flow axis
and is a likely energy source for the entire flow.  The following
nomenclature is proposed: HH247 A,B,C = N2023 HH1A,B,C, HH247 D =
N2023 HH5, HH247 E = N2023 HH4.

\vspace*{0.3cm}

{\bf HH 248/249} {\em (5 39, $-$02 25)}. 
Original paper: Malin, Ogura, Walsh (1987), who present photographic
plates, spectroscopy and proper motion measurements. These are two
groups of HH knots located south-east of the bright T Tauri star V615
Ori at the base of the Horsehead. HH 248 have proper motion vectors
pointing towards V615 Ori, so this star is unlikely to be the energy
source. It seems probable that the source is located between HH 248
and 249.

\vspace*{0.3cm}

{\bf HH 250} {\em (19 18, +10 46)}. Original paper: Devine, Reipurth,
Bally (1997), who present an H$\alpha$ CCD image. This is a relatively
bright, fine bow shock emanating from the IRAS source 19190+1048.

\vspace*{0.3cm}

{\bf HH 251/252/253/254} {\em (22 18, +63 17)}.
Original paper: Eiroa et al. (1993), who present CCD images. This is a
chain of four Herbig-Haro objects, located in the S140N region, and
situated on a straight line, suggesting
that they represent different episodes of activity in a common driving
source. HH~251 is a large and complex HH object with much substructure and
a component of reflection nebulosity next to two infrared sources.
Eiroa et al. (1993) consider one of these stars a likely energy
source. HH~252, 253 and 254 are smaller HH objects with a simple
structure. Near-infrared H$_2$ images and low resolution CO data are
presented by Davis et al. (1998).
The L1204 molecular cloud region is well known for several
infrared/radio sources around an HII region (Evans et al. 1989 and
references therein). Several radio continuum jets and bullets are
found in the region (Schwartz 1989).
The northern part of the cloud, which contains
the HH objects, is less studied, but contains an IRAS source
22178+6317 with a molecular outflow (Fukui et al. 1986).

\vspace*{0.3cm}

{\bf HH 255} {\em (4 19, +19 24)}. 
Original papers: Burnham (1894), B\"ohm \& Solf (1994). The mass flows
around the binary star T~Tauri are highly complex, and appear to be
the result of two separate Herbig-Haro flows. HH~255 comprises a
north-south bipolar flow, close to the plane of the sky, that
apparently arises in T~Tau-S and includes Burnham's Nebula to the
south of T~Tauri and the two spatiokinematic flow components C and D
of B\"ohm \& Solf (1994) close to T~Tau; further spectroscopy of HH
255 is analyzed by B\"ohm \& Solf (1997). HH~155 is, as described in
the notes for that object, a flow from T~Tauri that stretches to the
west in an approaching lobe closer to the line-of-sight, including a
bright HH knot and the spatiokinematic flow components A and B of
B\"ohm \& Solf (1994) close to T~Tau. Burnham's Nebula was discovered
by Burnham (1894) as a small nebula some arcseconds to the south of
T~Tauri. The extent of shock-excited [SII] emission around T~Tau is
shown by B\"uhrke, Brugel, Mundt (1986, their fig.7). Almost all is
south of T~Tauri, but a small region is west and north of T~Tau, and
may be part of HH~155.  Following B\"ohm \& Solf (1994), it is
recommended to define Burnham's Nebula as the large southern emission
region forming part of the north-south oriented HH~255 flow. Optical
spectroscopy of Burnham's Nebula shows that it has a Herbig-Haro
spectrum (Herbig 1950, Osterbrock 1958, Schwartz 1974, 1975, B\"uhrke,
Brugel, Mundt 1986, Solf, B\"ohm, Raga 1988).  An anomalous Fe/S ratio
was determined by Beck-Winchatz \& B\"ohm (1994), see also
Beck-Winchatz, B\"ohm, Noriega-Crespo (1996).  The reddening of
Burnham's nebula is discussed by Cardelli \& Brugel
(1988). Ultraviolet spectroscopy is reported by Brown et
al. (1981). Molecular hydrogen emission has been detected towards
T~Tauri by Beckwith et al. (1978), Schwartz et al. (1987), van
Langevelde et al. (1994), Herbst et al. (1996), Quirrenbach \&
Zinnecker (1997), and Herbst, Robberto, Beckwith (1997).  The nature
of T~Tau-S, the suspected driving source of HH~255, was discussed by
Bertout (1983). For further references to the T~Tau region, see the
notes for HH~155.

\vspace*{0.3cm}

{\bf HH 256} {\em (4 27, +17 52)}. Original paper: Graham \& Heyer
(1990), who present a CCD image. This is a very faint little cluster
of three HH knots (formerly GH~1), which may form the terminus of the
blue-shifted lobe of the L1551 IRS~5 Herbig-Haro flow. Garnavich,
Noriega-Crespo, Green (1992) show the object is of low-excitation.
The wide-field images pf Devine, Reipurth, Bally (1999) show that
HH~256 is located along the rather well defined axis of the red lobe of
HH~30, and it is conceivable that it forms a distant bow shock in this
flow.

\vspace*{0.3cm}

{\bf HH 257} {\em (4 28, +17 54)}. Original paper: Garnavich,
Noriega-Crespo, Green (1992), who present CCD images. This is a faint
object (formerly GNG~17) between HH~28 and HH~256.

\vspace*{0.3cm}

{\bf HH 258} {\em (4 28, +17 57)}. Original paper: Graham \& Heyer
(1990), who present CCD images. This is a group of faint HH knots,
GH~2 to 8, whose individual
designations should be retained, located immediately
west of HH~28. GH~8 is relatively bright and very close to HH~28. The
whole group is part of a large chain of HH knots winding out from
L1551 IRS~5, including HH~259, HH~29, HH~260 and HH~261.


\vspace*{0.3cm}

{\bf HH 259} {\em (4 28, +17 57)}. Original papers: Stocke et al.
(1988), Rodr\'\i guez et al. (1989a). This is a winding chain of HH
knots, SH~229 and GNG 2, 5, 6, 7, 8, 9, 10 and 11 (it may be practical
to keep these designations for individual knots), located between
HH~28 and 29 and seen well in the CCD images of Graham \& Heyer
(1990), Garnavich, and Noriega-Crespo, Green (1992). Proper motions
are measured by Devine, Reipurth, Bally (1999).


\vspace*{0.3cm}

{\bf HH 260} {\em (4 28, +18 00)}. 
Original paper: Garnavich, Noriega-Crespo, Green (1992), who present
CCD images. This is a faint HH knot (formerly GNG 1) between HH~29 and
HH~261. Further CCD images are presented by Davis et al. (1995).


\vspace*{0.3cm}

{\bf HH 261} {\em (4 28, +18 00)}. Original paper: Stocke et al.
(1988), who present CCD images and spectroscopy. These are HH knots
(formerly SH 219/220)
located just east of HH~29, and seen in the images of Rodr\'\i guez et al.
(1989a), Graham \& Heyer (1990) and Garnavich, Noriega-Crespo, Green
(1992).


\vspace*{0.3cm}

{\bf HH 262} {\em (4 29, +18 05)}.  Original papers: Rodr\'\i guez et
al.  (1989a), Graham \& Heyer (1990). These are a complex group of
many faint HH knots, brightest among them knots GH~9 and 10, in
addition to the fainter knots GNG~18,19,20,21,22 found by Garnavich,
Noriega-Crespo, Green (1992); it is suggested to retain these
designations for the individual knots.  These knots may be either a
counterflow from L1551 IRS5, or may be driven by the nearby class I
source L1551 NE; this latter source has its own outflow activity
(Emerson et al. 1984, Draper, Warren-Smith, Scarrott 1985b, Campbell
et al. 1988, Pound \& Bally 1991, Moriarty-Schieven \& Wannier 1991,
Barsony \& Chandler 1993, Moriarty-Schieven, Butner, Wannier 1995,
Rodr\'\i guez, Anglada, Raga 1995, Hodapp \& Ladd 1995).  Spectra of
knots GH~9 and 10 are presented by Graham \& Rubin (1992), who argue
that the group of HH knots are likely to be a counterflow from L1551
IRS~5. L\'opez et al. (1995) found an additional extended emission
region. A detailed kinematic study of HH~262 based on proper motions
and Fabry-Perot data is presented by L\'opez et al. (1998).  Devine,
Reipurth, Bally (1999) note that the well defined flow axis of HH 454
driven by L1551-NE goes through and along the easternmost part of
HH~262, called HH~262E.

\vspace*{0.3cm}

{\bf HH 263} {\em (4 28, +18 01)}. Original paper: Stocke et al.  (1988),
who obtained CCD images and spectra. This is a small group of HH knots
(formerly SH~214, or GNG~3) south of the HH~102 reflection nebula, seen
well in the CCD images of Graham \& Heyer (1990), Garnavich,
Noriega-Crespo, Green (1992) and Davis et al. (1995).  
Garnavich, Noriega-Crespo, Green (1992) 
suggest that the knots, which lie along the extension of the HH~30
counterjet, may be caused by this jet.


\vspace*{0.3cm}

{\bf HH 264} {\em (4 28, +17 59)}. Original papers: Stocke et al.  (1988),
Graham \& Heyer (1990) and Garnavich, Noriega-Crespo, Green (1992), who all
present CCD images, the first authors also present some spectroscopy. This
is a large, very complex region of emission-knots (formerly GNG~4) south of
the HH 102 reflection nebula. It possibly represents the shock interaction
of the L1551 IRS~5 outflow with the walls of the cavity carved by the
outflow in the L1551 molecular cloud. Designations, positions and
[SII]/H$\alpha$ ratios for individual knots are given by Garnavich,
Noriega-Crespo, Green (1992).  Further CCD images are presented by Davis et
al. (1995).

\vspace*{0.3cm}

{\bf HH 265} {\em (4 28, +18 05)}. Original paper: Garnavich,
Noriega-Crespo, Green (1992), who present CCD images. This is an
isolated low-excitation HH knot (formerly GNG~25) located in the
middle of the L1551 cloud. No energy source has been
identified. Wide-field CCD images showing the location of HH~265
relative to other HH flows in L1551 are presented by Devine, Reipurth,
Bally (1999).


\vspace*{0.3cm}

{\bf HH 266} {\em (4 28, +18 10)}.  Original paper: Garnavich,
Noriega-Crespo, Green (1992), who present CCD images. This is a faint
high-excitation HH knot (formerly GNG~24) located at the north-eastern edge
of the L1551 cloud, possibly related to the HH~30 jet. L\'opez et
al. (1995) present wide-field CCD images of the region, and L\'opez et
al. (1996) discuss proper motions and a radial velocity measurement.


\vspace*{0.3cm}

{\bf HH 267} {\em (3 20, +30 49)}.
Original paper: Bally et al. (1997), who present a CCD image. This is
an extended cluster of HH knots in the L1448 cloud. For further
references to the region, see notes for HH 197.


\vspace*{0.3cm}

{\bf HH 268} {\em (3 21, +30 37)}.
Original paper: Bally et al. (1997), who present CCD images and
spectra. This is a small group of rather faint HH knots in the L1448
cloud. For further references to the region, see notes for HH 197.

\vspace{0.3cm}

{\bf HH 269} {\em (5 32, $-$05 25)}. Original paper: Feibelman (1976), who
recognized this as a high-velocity emission feature. Cudworth \& Stone
(1977) measured proper motions towards the west. In an extensive study
based on low- and high-resolution spectroscopy and HST images, Walter et
al. (1995) found that this object appears to fit into the class of HH
objects. It is an elliptical shell with dimensions 41$''$ $\times$ 23$''$,
with a low excitation spectrum, and some parts with high velocities. O'Dell
et al. (1997b) made a Fabry-Perot map of the Orion Nebula, which includes HH
269.

\vspace{0.3cm}

{\bf HH 270} {\em (5 48, +02 55}.  Original paper: Reipurth, Raga,
Heathcote (1996), who present deep H$\alpha$ and [SII] images. This
flow consists of a chain of five faint HH knots emanating from an
embedded near-infrared source, detected at 3.6 cm by Rodr\'\i guez et
al. (1998a).  The flow is directed towards the apex of the HH 110
flow, and the proper motion vector of HH 270A points in the same
direction. It is therefore suggested that the HH 110 flow is the
result of a grazing collision between the HH 270 flow and a molecular
cloud core detected at mm-wavelengths. Alternatively, Hurka,
Schmid-Burgk, Hardee (1999) suggest a deflection by an ambient
magnetic field.


\vspace*{0.3cm}

{\bf HH 271/272/273} {\em (6 10, $-$06 11)}.  Original paper: Carballo
\& Eiroa (1992), who present CCD images.  These are HH objects
(formerly GGD~17/HH1,2,3) found near the reflection nebula GGD~17 in
the Mon R2 region. HH~261 is a small jet emanating from the rich
emission line T~Tauri star Bretz~4. HH~262 is a group of knots located
further downstream and may be part of the same flow. HH~263 is a faint
knot somewhat more isolated.  The positions of the HH objects are very
approximate. Spectroscopy of Bretz~4 is discussed by Cohen \& Kuhi
(1979) and Carballo \& Eiroa (1992), and infrared photometry by
Carballo, Eiroa, Mampaso (1988).  Bretz~4 is probably identical to the
IRAS source 06103$-$0612, and is observed at 1300 $\mu$m by Reipurth
et al. (1993a) and at more sub-millimeter wavelengths by Dent,
Matthew, Ward-Thompson (1998).


\vspace*{0.3cm} 

{\bf HH 274} {\em (12 49, $-$76 50)}. Original paper: Reipurth
(unpublished). CCD images of IRAS 12496-7650, the driving source of
the HH~52/53/54 complex (Cohen \& Schwartz 1987, Hughes et al. 1989,
1991) reveal a faint optical stellar counterpart with a small HH
object on the side of the star facing the HH~52/53/54 objects.

\vspace{0.3cm}

{\bf HH 276} {\em (04 19, +26 50)}. Original paper: Eisl\"offel \& Mundt
(1998), who present CCD images. This is an about 150$''$ long flow
consisting of at least 4 faint HH knots. The axis of this flow is almost
perpendicular to and in projection runs across the HH 157 jet from
FS~Tau~B. The source of HH 276 has not yet been located.



\vspace*{0.3cm}

{\bf HH 277 } {\em (03 23, +30 28)}. Original paper: Bally et
al. (1997), who present a CCD image. This is a relatively isolated HH
object in L1448, which together with HH~196 lies on a line through
L1448 IRS~3; these two objects are nearly equidistant from this
source, suggesting a possible relation between the two HH objects. See
also notes for HH~197.


\vspace*{0.3cm}

{\bf HH 278} {\em (03 23, +30 15)}. Original paper: Bally et
al. (1997), who present a CCD image. This is a large diffuse object
located midway between the L1448 and L1455 clouds. See also notes for
HH~279.


\vspace*{0.3cm}

{\bf HH 279 } {\em (03 24, +30 06)}. Original paper: Bally et
al. (1997), who present a CCD image. This is a chain of HH emission
extending over about 5 arcminutes, with several condensations, of
which especially one, HH~279C, is very bright. The HH object lies in
the L1455 cloud near the blue lobe of a major molecular outflow
apparently driven by L1455~IRS1 (Goldsmith et al. 1984, Levreault
1988, Bachiller \& Cernicharo 1986b, Juan et al. 1993). L1455~IRS1 (=
IRAS 03245+3002) is a class~I source with a luminosity of 9.7
L$_\odot$ (Davidson \& Jaffe 1984), and is associated with an H$_2$O
maser (Cesaroni et al. 1988, Persi, Palagi, Felli 1994).


\vspace*{0.3cm}

{\bf HH 280} {\em (03 20, +30 07)}. Original paper: Bally et
al. (1997), who present a CCD image. This is a very extended and loose
group of HH knots, which lies some 20 arcmin west of the L1455 cloud
core. See also notes for HH~279.


\vspace*{0.3cm}

{\bf HH 281/282/283/284/285} {\em (5 34, +31 58)}. Original paper:
Torrelles et al. (1992a). This is a small cluster of HH objects
(formerly AFGL 5157/HH1-5) in the region of AFGL 5157 (IRAS
05345+3157). The infrared source illuminates the reflection nebula
NGC~1985. The region has a bipolar outflow (Snell et al. 1988), an
ammonia core (Torrelles et al. 1992a), and H$_2$O maser emission
(Verdes-Montenegro et al. 1989, Torrelles et al. 1992c, Xiang \&
Turner 1995). Chen et al. (1999) present a detailed near-infrared
imaging study of the region, and give more references.

\vspace{0.3cm}

{\bf HH 286} {\em (04 29, +18 10)}. Original paper: Devine, Reipurth,
Bally (1999), who show CCD images. This is a large incomplete bow
shock, located to the north-east of L1551 along the red lobes of the
flows from both L1551-NE and IRS~5. It is not known which of these two
sources is responsible for HH~286.


\vspace*{0.3cm}

{\bf HH 287 } {\em (05 33, $-$05 07)}. Original paper: Reipurth,
Bally, Devine (1997), who present interference filter CCD images. This
is a faint HH knot associated with a small reflection nebula some
arcminutes south of IRAS 05329$-$0505, which drives the HH~294
jet. Yu, Bally, Devine (1997) detect a faint H$_2$ knot (YBD~70)
coincident with HH~287.


\vspace{0.3cm}

{\bf HH 288} {\em (00 34, +63 47)}. Original paper: McCaughrean
(1997), who present an infrared H$_2$O image. This is a compact HH
object associated with a dramatic, 5 arcmin long, collimated H$_2$
flow from the IRAS source 00342+6347 in Cassiopeia. The HH object is
the only place where this infrared flow has an optical counterpart.
Sub-millimeter photometry of the source is given by Dent, Matthews,
Ward-Thompson (1998).  The CO kinematic distance is 2 kpc.


\vspace{0.3cm}

{\bf HH 289} {\em (05 36, $-$01 44)}. Original paper: Mader et
al. (1999), who present CCD images and infrared images. This is a
chain of faint HH knots apparently emanating from the IRAS source
05355$-$0146, which is embedded in the small cometary globule Ori-I-2
in the Orion complex. A molecular outflow was noted here by Sugitani
et al. (1989), and a more complete millimeter study of outflow and
globule was presented by Cernicharo et al. (1992).



\vspace{0.3cm}

{\bf HH 290} {\em (5 44, +20 59)}. Original paper: Moreira \& Yun
(1995), who present CCD images and infrared H$_2$ images. This is a
chain of HH objects emanating from a source embedded in the Bok
globule CB 34. The globule contains a single IRAS source 05440+2059
and a small aggregate of embedded young stars (Alves \& Yun 1995). A
molecular flow has been detected by Yun \& Clemens (1994).  Codella \&
Scappini (1998) mapped CB 34 in NH$_3$. Launhardt \& Henning (1997)
present 1300 $\mu$m photometry of the source and suggest a distance of
1500 pc.


\vspace{0.3cm}

{\bf HH 291} {\em (5 44, +20 58)}. Original paper: Moreira \& Yun
(1995), who present CCD images and infrared H$_2$ images. This is a
faint HH object in the Bok globule CB 34. See also notes for HH 290.



\vspace{0.3cm}

{\bf HH 292} {\em (05 34, $-$06 35)}. Original paper: Mader et al. (1999),
who present CCD images. This is a small bipolar HH flow centered on
the young star BE Ori, which is highly variable (13 $<$ m$_{pg}$ $<$
17.5). It has a spectral type of K0 and bright emission lines (Cohen
\& Kuhi 1979). Near-infrared photometry is given by Nakajima et
al. (1986), and ir polarization measurements by Casali
(1995). Measurements of $^{13}$CO and HCO$^+$ gas is given by Chen,
Fukui, Yang (1992).


\vspace*{0.3cm}

{\bf HH 293 } {\em (05 32, $-$05 03)}. Original paper: Reipurth,
Bally, Devine (1997), who present interference filter CCD images. This
is a short bright jet, which emits exclusively in [SII] with no
H$\alpha$ emission. Yu, Bally, Devine (1997) show that the jet is
bright in molecular hydrogen. HH~293 is located a few arcminutes north
of HH~294, and the two jets have almost parallel axes. See also notes
for HH~294.


\vspace*{0.3cm}

{\bf HH 294} {\em (05 32, $-$05 05)}. Original paper: Reipurth, Bally,
Devine (1997), who present interference filter CCD images. This is a
finely collimated chain of knots emanating along the western lobe of
the Haro~5a/6a reflection nebula in Orion (Haro 1953), centered on the
luminous IRAS source 05329$-$0505 (Wolstencroft et al. 1986), which
appears to be in an FU Orionis state (Reipurth \& Aspin 1997).  IRAS
05329--0505 is also known as MMS~7 and is part of a long filament of
1300 $\mu$m sources in OMC~2/3 (Chini et al. 1997a).  The source was
detected at 3.6 cm with the VLA (Reipurth, Rodr\'\i guez, Chini
1999). The source drives a giant HH flow with HH~41, 42, 128, and 129
in its eastern lobe, and HH~295 in the western lobe (Reipurth, Bally,
Devine 1997), but in a detailed molecular hydrogen study of the
region, Yu, Bally, Devine (1997) suggest that other nearby sources
could also play a role in driving some of these more distant HH
objects. The OMC 2/3 region contains two large star forming cores,
which have been extensively studied, and the following are only some
of numerous studies. Infrared studies of the embedded stellar
population include Gatley (1974), Cohen \& Frogel (1977), Thronson et
al. (1978), Thronson \& Thompson (1982), Pendleton et al. (1986),
Rayner et al. (1989), Johnson et al. (1990) and Jones et
al. (1994). Millimeter studies are presented by Bally et al. (1987),
Tatematsu et al. (1993a), Dutrey et al. (1993), Cesaroni \& Wilson
(1994), Castets \& Langer (1995), and Chini et al. (1997a). 1300
$\mu$m and sub-millimeter maps are presented by Mezger, Wink, Zylka
(1990), Chini et al. (1997a), Lis et al. (1998), and Johnstone \&
Bally (1999).


\vspace*{0.3cm}

{\bf HH 295 } {\em (05 32, $-$05 06)}. Original paper: Reipurth,
Bally, Devine (1997), who present H$\alpha$ and [SII] CCD images. This
is a loose cluster of HH knots spreading across 3 arcminutes, and
located 12 arcmin west of IRAS 05329--0505. HH 295 appears to be one
lobe of a giant HH flow driven by the IRAS source, and with HH 41, 42,
128, and 129 in the eastern lobe. Yu, Bally, Devine (1997) suggest
that several different sources are responsible for the HH and H$_2$
flows in the region. See also notes for HH~294.


\vspace{0.3cm}

{\bf HH 296} {\em (05 33, $-$06 19)}. Original paper: Reipurth,
Devine, Bally (1998), who present a [SII] image. This is a faint group
of HH knots in the L1641-N region. It is possibly associated with HH
297. See also notes for HH 303.


\vspace{0.3cm}

{\bf HH 297} {\em (05 33, $-$06 18)}. Original paper: Reipurth,
Devine, Bally (1998), who present a [SII] image. This is a single
faint HH knot in the L1641-N region. It is possibly associated with HH
296. See also notes for HH 303.

\vspace{0.3cm}

{\bf HH 298} {\em (05 33, $-$06 23)}. Original paper: Reipurth,
Devine, Bally (1998), who present a [SII] image. This is an east-west
chain of three HH knots about 70 arcsec long located in the L1641-N
region. See also notes for HH 303.



\vspace{0.3cm}

{\bf HH 299} {\em (05 33, $-$06 21)}. 
Original paper: Reipurth, Devine, Bally (1998), who present a [SII]
image. This is a fairly bright HH object, linked to diffuse wisps of
emission, and located in the L1641-N region.  At 2.12 $\mu$m it
displays a jet-like morphology (SMZ~9; Stanke, McCaughrean, Zinnecker
1998).  See also notes for HH 303.



\vspace*{0.3cm}

{\bf HH 300 } {\em (04 22, +24 16)}. Original paper: Reipurth, Bally,
Devine (1997), who present interference filter CCD images. This is a
giant HH flow with two major bow shocks located 1.2 pc south-west of
and on a line through the IRAS 04329+2436 source embedded in the B18
cloud in Taurus. Both bow shocks are redshifted. Opposite and very
close to the source there is a small blueshifted knot, HH~300D, which
was also found by G\'omez, Whitney, Kenyon (1997), and observed
spectroscopically by Kenyon et al. (1998). The source is a class I
source with a luminosity of only 1.3 L$_\odot$, and an unusually rich
near-infrared spectrum (Greene \& Lada 1996a). This source was
detected in the near- and mid-infrared by Myers et al. (1987), who
give JHKLMNQ photometry, at 1300 $\mu$m by Moriarty-Schieven et
al. (1994), and at 3.6 cm by Rodr\'\i guez \& Reipurth
(1998). Polarimetric observations are presented by Lucas \& Roche
(1998a). Moriarty-Schieven et al. (1992) suggest that there may be a
molecular outflow at the source. Ungerechts \& Thaddeus (1987) include
B18 in their low-resolution CO map of Taurus.

\vspace{0.3cm}

{\bf HH 301/302} {\em (05 34, $-$06 23)}. 
Original paper: Reipurth, Devine, Bally (1998), who present a [SII]
image. These two objects are among the brightest HH objects in the
L1641-N region. They contain several bright knots plus a chain of
fainter more diffuse emission knots along a well defined axis passing
through the L1641-N cluster, from which it appears to originate.  Both
objects are detected at 2.12 $\mu$m (SMZ~12 and 11; Stanke,
McCaughrean, Zinnecker 1998).  See also notes for HH 303.


\vspace{0.3cm}

{\bf HH 303} {\em (05 33, $-$06 21)}.  Original paper: Reipurth,
Devine, Bally (1998), who present interference filter CCD images. This
is a well collimated chain of knots emanating from IRAS 05338$-$0624
in the L1641-N region. The flow was first seen on photographic plates
by Reipurth (1985a). The HH 303 jet is coinciding with the blue lobe
of the L1641-N {\em molecular outflow}, which has been studied by
Fukui et al. (1986, 1988), Wilking, Blackwell, Mundy (1990), and
Morgan \& Bally (1991).  A {\em molecular hydrogen} image is presented
by Davis \& Eisl\"offel (1995), and Stanke, McCaughrean, Zinnecker
(1998).  An {\em infrared cluster} was studied by Strom, Margulis,
Strom (1989), Hodapp \& Deane (1993) and Chen et al. (1993). The {\em
source} was detected by IRAS (Strom et al. 1989), in the far-infrared
by Di~Francesco et al. (1998), and in the mm and cm continuum by
Wilking et al. (1989), Mundy et al. (1993), Chen, Zhao, Ohashi (1995)
and Anglada et al. (1998), and possibly at 10 $\mu$m by Stanke,
McCaughrean, Zinnecker (1998).  Sub-millimeter photometry is given by
Dent, Matthew, Ward-Thompson (1998).  A {\em water maser} was detected
by Xiang \& Turner (1995) and Claussen et al. (1996). {\em Dense
molecular cores} are discussed by Fukui et al. (1988), Chen, Fukui,
Iwata (1993), McMullin, Mundy, Blake (1994), Chen, Ohashi, Umemoto
(1996), Anglada et al. (1997) and Reipurth, Devine, Bally (1998).

\vspace{0.3cm}

{\bf HH 304} {\em (05 34, $-$06 16)}. 
Original paper: Reipurth, Devine, Bally (1998), who present a [SII]
image. This is a group of HH knots with a complex morphology, and an
axis pointing back towards the L1641-N cluster. It is detected at 2.12
$\mu$m (SMZ~5) by Stanke, McCaughrean, Zinnecker (1998).  See also
notes for HH 303.

\vspace{0.3cm}

{\bf HH 305} {\em (05 34, $-$06 19)}. Original paper: Reipurth,
Devine, Bally (1998), who present a [SII] image. These six HH objects
form a 4 arcmin long chain, possibly a bipolar structure with a center
near the variable star PR Ori, which, however, may not be related to
the flow.


\vspace{0.3cm}

{\bf HH 306/307/308/309/310} {\em (05 33, $-$05 51)}. 
Original paper: Reipurth, Devine, Bally (1998), who present various CCD
images. This is a giant chain of what appears to be very large bow shocks
all facing away from the L1641-N cluster (see references to the cluster under
HH~303). HH~310 is 47 arcmin from the center of the L1641-N cluster,
corresponding to a projected length of 6.3 pc. It is possible that the
infrared flow SMZ~23 forms a 1.8 pc long counterflow (Stanke, McCaughrean,
Zinnecker 1998).

\vspace*{0.3cm}

{\bf HH 311 } {\em (05 47, +02 52)}. Original paper: Winkler \&
Reipurth (1992), who present interference filter CCD images and a few
spectra. This is a several arcminute large and rather filamentary
complex of knots half a degree from the nearest molecular cloud in
Orion, and Winkler \& Reipurth (1992) speculated that it could be a
supernova remnant. However, in an imaging and proper motion study,
Reipurth, Bally, Devine (1997) demonstrated that it is actually a
distant bow shock in the blue lobe of the HH~111 jet complex. Rosado,
Raga, Arias (1999) present a kinematic study based on Fabry-Perot
observations.  See also notes for HH~111.

\vspace*{0.3cm}

{\bf HH 312} {\em (16 22, $-$24 14)}. Original paper: Wilking et
al. (1997a), who present a [SII] CCD image. This is a well collimated
jet that extends 1.5 arcminutes southeast from SR4, which is an
emission line star (Struve \& Rudkj\o bing 1949) of spectral type
K5-K7 (Cohen \& Kuhi 1979) and with a bolometric luminosity of 5.5
L$_\odot$ (Wilking, Lada, Young 1989). It is also a weak X-ray source
(Casanova et al. 1994). The jet is located in a dense region of the
$\rho$ Ophiuchi cloud, which is very rich in star formation. G\'omez, Whitney, Wood (1998) also show a [SII] CCD image.

\vspace*{0.3cm}

{\bf HH 313} {\em (16 23, $-$24 16)}. 
Original paper: Wilking et al. (1997a), who present a [SII] CCD
image. This is a slightly extended [SII] emission knot (also shown in
an image by G\'omez, Whitney, Wood 1998), which coincides with the
{\em infrared H$_2$ knot} labeled 2317.6--1622 (C\'omeron et al. 1993)
or H5 (Dent, Matthews, Walter 1995) or knot A by Davis \& Eisl\"offel
(1995). It is located in the northwest lobe of a well collimated {\em
molecular outflow} (Andr\'e et al. 1990, Dent, Matthews, Walter 1995,
Yu \& Chernin 1997) which is driven by the class~0 object VLA 1623
(Andr\'e et al. 1993, Pudritz et al. 1996). Holland et al. (1996) and
Greaves, Holland, Ward-Thompson (1997) present sub-mm polarimetry. The
source is associated with an H$_2$O maser (Claussen et
al. 1996). Ceccarelli et al. (1997) determined the mass loss rate from
the source through OI 63 $\mu$m emission measurements.

\vspace*{0.3cm}

{\bf HH 314 } {\em (16 23, $-$24 34)}. Original paper: Wilking et
al. (1997a), who present a [SII] CCD image. This is an isolated HH knot in
the $\rho$ Ophiuchi clouds. Wilking et al. (1997a) tentatively associate it
with the young star DoAr 25. G\'omez, Whitney, Wood (1998) show a [SII] CCD
image, and find another object, HH 418, seven arcminutes further to the
west.

\vspace*{0.3cm}

{\bf HH 315 } {\em (20 45, +67 49)}. Original papers: G\'omez,
Kenyon, Whitney (1997) and Reipurth, Bally, Devine (1997), who
independently discovered this HH flow and present interference filter
CCD images. This is a giant bipolar HH flow consisting of a number of
groups of HH knots displaying s-shaped point symmetry around the young
star PV~Cep. The total extent is almost 20 arcminutes, corresponding
to 2.6 pc in projection. The northern lobe is blueshifted and the
southern redshifted. Levreault (1984) mapped a large molecular
outflow, which is coincident with the HH flow. PV~Cep is surrounded by
a reflection nebula GM~29 (Gyulbudaghian \& Magakyan 1977b) or
RNO~125 (Cohen 1980a), which is highly variable (Cohen, Kuhi, Harlan
1977, Cohen et al. 1981) and consists of two lobes (Levreault \& Opal
1987). PV~Cep may be an EXor (Herbig 1989). It was detected in the
radio continuum by Anglada et al. (1992). Near-infrared spectroscopy
of PV~Cep is presented by Hamann et al. (1994) and Greene \& Lada (1996b), 
and optical
spectroscopy by Corcoran \& Ray (1997). Close to the star there is a
group of HH knots, HH~215, found by Neckel et al. (1997), which forms
the innermost part of the giant HH~315 flow. A small HH knot, HH~415,
is located north-east of PV~Cep, and it is unclear if it belongs to
the HH~215/315 flow or is from a separate flow in the region.

\vspace{0.3cm}

{\bf HH 316} {\em (05 33, $-$06 06)}. Original paper: Reipurth,
Devine, Bally (1998), who present an H$\alpha$ CCD image. This is a
finely collimated, slightly curved jet, stretching over
2 arcminutes. It is located just west of the giant HH
307 bow shock in the L1641-N region.



\vspace*{0.3cm}

{\bf HH 317 } {\em (03 24, +30 01)}. Original paper: Bally et
al. (1997) who present a CCD image. This is a large group of HH knots
located in the outskirts of the L1455 cloud core. See also notes for
HH~279.

\vspace*{0.3cm}

{\bf HH 318 } {\em (03 24, +30 03)}.  Original papers: Bally et
al. (1997) and Davis et al. (1997b), who present CCD images.  This is
a several arcmin long chain of HH knots (B,C,D) north-east of and on a
line through the source L1455 IRS1 (= RNO 15-FIR = IRAS 03245+3002 =
L1455 FIR). Knot~A, which is south-west of the source, is only seen in
H$_2$ in the near-infrared images of Hodapp (1994) and Davis et
al. (1997a). The HH flow is co-axial with a well-collimated {\em
molecular outflow}, which is one of several overlapping CO flows in
the region, observed at mm-wavelengths by Frerking \& Langer (1982),
Goldsmith et al. (1984), Bachiller \& Cernicharo (1986b), Levreault
(1988), Juan et al. (1993), and Davis et al. (1997b). The {\em source}
L1455 IRS1 is a cold far-infrared source (Davidson \& Jaffe 1984,
Tapia et al. 1997) and is associated with an {\em H$_2$O maser}
(Cesaroni et al. 1988, Persi, Palagi, Felli 1994).  Wiggling of the
molecular outflow is interpreted as possibly due to the source being a
binary (Terquem et al. 1999).

\vspace*{0.3cm}

{\bf HH 319} {\em (4 29, +24 15)}. Original paper: Haro, Iriarte,
Chavira (1953). This is an H$\alpha$ emission object, also known
as Haro 6-19, with a characteristic HH spectrum. On CCD images it
shows complex structure (Mundt, priv. comm.).


\vspace{0.3cm}

{\bf HH 320} {\em (11 58, $-$64 51)}. Original paper: Corporon \&
Reipurth (1997), who present CCD images. These are two HH knots
located in the red lobe of the molecular outflow from the embedded
source IRAS 11590--6452 in the Sa 136 (= BHR 71) globule. Since the
objects appear rather unobscured and look like bow shocks facing {\em
towards} the IRAS source, it is not clear that they are driven by this
source. See also notes for HH 321.

\vspace{0.3cm}

{\bf HH 321} {\em (11 59, $-$64 53)}. Original paper: Corporon \&
Reipurth (1997), who present CCD images. These are two HH knots
located inside a large impressive flow cavity illuminated by the
source IRAS 11590--6452, which is embedded in the Sa 136 (= BHR 71)
globule. The source drives a well collimated CO outflow, which has
strong enhancements of silicon monoxide and methanol (Bourke et
al. 1997, Garay et al. 1998). Infrared images are presented by Bourke
et al. (1993) and Yun et al. (1997).

\vspace{0.3cm}

{\bf HH 322} {\em (05 32, $-$06 22)}. Original papers: Eisl\"offel
\& Mundt (1997) and Devine et al. (1997), who present CCD images. This is a
single HH knot south-west of HH 33/40, which together with diffuse emission
to the east may form part of the large HH 33/40 working surface (Bally \&
Devine 1994).

\vspace{0.3cm} 

{\bf HH 323} {\em (05 32, $-$06 20)}. Original paper: Devine et
al. (1997), who present CCD images. This is a large, slightly diffuse HH
object an arcminute west of HH 33. It is probably part of the large bow
shock involving HH 33/40 and probably HH 322. Eisl\"offel \& Mundt (1997)
also imaged this object and called it HH 33X.


\vspace{0.3cm} 

{\bf HH 324 } {\em (05 33, $-$06 20)}. Original paper: Devine et
al. (1997), who present CCD images. This is a single faint HH knot east of
the giant HH 34 flow. No source is known.



\vspace{0.3cm} 

{\bf HH 325 } {\em (05 33, $-$06 31)}. Original paper: Devine et
al. (1997), who present CCD images. This is a a group of very faint diffuse
HH knots to the east of HH 134. No source is known.



\vspace{0.3cm} 

{\bf HH 326 } {\em (05 33, $-$06 34)}. Original paper: Devine et
al. (1997), who present CCD images. This is a group of very faint HH knots
north-east of HH 86-88. No source is known.


\vspace{0.3cm} 

{\bf HH 327 } {\em (05 33, $-$06 37)}. Original paper: Eisl\"offel \&
Mundt 1997) and Devine et al. (1997), who present CCD images. This is a
jet-like group of HH knots east of HH 86-88. It seems to be an independent
HH flow, although it cannot at present be excluded that it forms part of
the giant HH 86-88 working surface.



\vspace*{0.3cm}

{\bf HH 328 } {\em (05 15, +07 12)}. Original paper: Reipurth,
Bally, Devine (1997), who show a CCD image. This is a single HH knot
near the HH 114 flow. It is possibly related to HH 329.

\vspace*{0.3cm}

{\bf HH 329 } {\em (05 15, +07 05)}. Original paper: Reipurth,
Bally, Devine (1997), who show a CCD image. This is a single HH knot
near the HH 115 flow. It may form a giant HH flow together with
HH~328, parallel to the HH~114/115 flow.

\vspace{0.3cm}

{\bf HH 330} {\em (05 33, $-$05 06)}. Original paper: Yu, Bally,
Devine (1997), who note that this is an optical counterpart to the
H$_2$ knot YBD~80. This is possibly a bow shock in the east-west flow
originating in IRAS 05329$-$0505, but the outflow activity in the
region is highly complicated, see notes for HH~294.



\vspace*{0.3cm}

{\bf HH 331 } {\em (05 32, $-$05 02)}. Original paper: Yu, Bally,
Devine (1997), who note that it is an optical counterpart to the H$_2$
knot YBD~1, which together with YBD~2, 3 and 7 appears to form a
collimated flow in the OMC~2/3 region.

\vspace*{0.3cm}

{\bf HH 332 } {\em (19 18, +10 55)}. Original paper: Davis,
Eisl\"offel, Smith (1996), who present interference filter CCD
images. These objects are close to HH~32 and AS~353A, but has a quite
different angle to AS~353A than does HH~32, so it is unclear if they
come from this source. See also notes for HH~32.

\vspace*{0.3cm}

{\bf HH 333 } {\em (03 26, +31 15)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. This is a very thin and about
5 arcmin long jet, thus exceedingly collimated, located in the
northern part of the NGC 1333 cloud core. The jet is gently curved,
with s-shaped point symmetry around a central faint H$\alpha$ emission
star. The western half is blueshifted and the eastern is redshifted.

\vspace*{0.3cm}

{\bf HH 334 } {\em (03 25, +31 12)}. Original paper:
Bally, Devine, Reipurth (1996), who present CCD images. This is an HH
jet located about an arcminute north of HH~12, extending on both sides
of a bright H$\alpha$ emission star in the NGC~1333 cloud. A possibly
related isolated HH knot lies about 1 arcminute beyond the eastern end
of the jet. A small bow shaped knot lies 2 arcminutes northwest of the
bright H$\alpha$ star.

\vspace*{0.3cm}

{\bf HH 335} {\em (03 26, +31 12)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. This is a [SII] bright HH
flow located near the center of NGC 1333, and is mostly lost in the
glare of the bright stars, but it is easily seen in H$\alpha$--[SII]
difference images. The flow appears to emanate from the emission line
star LkH$\alpha$ 270.

\vspace*{0.3cm}

{\bf HH 336} {\em (03 26, +31 09)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. This is a bipolar HH jet
centered on a faint H$\alpha$ emission star located east of the
NGC~1333 cloud core.

\vspace*{0.3cm}

{\bf HH 337} {\em (03 25, +31 15)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. This turns out not to be an
HH object, but a glint due to a problem in the optical path of the
instrument used.


\vspace*{0.3cm}

{\bf HH 338} {\em (03 25, +31 09)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. This is a large conglomerate
of HH knots outside and to the west of the NGC~1333 cloud
core. HH~338, HH~339 and HH~15 lie on a line through IRAS 03255+3103
(IRAS~1), which Phillips et al. (1988) found to drive a CO outflow
along the same axis; the outflow was not detected by Knee, Cameron,
Liseau (1990). IRAS~1 was first studied by Jennings et al. (1987).

\vspace*{0.3cm}

{\bf HH 339} {\em (03 25, +31 04)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. This HH object lies close to
IRAS 03255+3103 (IRAS~1), and on a line defined by HH~15 and
HH~338. See also notes for HH~338.

\vspace*{0.3cm}

{\bf HH 340} {\em (03 25, +30 55)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. These are two HH knots in the
southern part of the NGC~1333 cloud.

\vspace*{0.3cm}

{\bf HH 341} {\em (03 25, +30 59)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. This is a tight cluster of HH
knots with some resemblance to a bow shock, and located in the
NGC~1333 cloud core. It lies in the extension of the blue molecular
outflow lobe driven by IRAS~2 (Jennings et al. 1987); this source
powers a quadrupolar molecular outflow (Liseau, Sandell, Knee 1988,
Langer, Castets, Lefloch 1996, Bachiller et al. 1998a). Hodapp \& Ladd
(1995) find evidence for H$_2$ flows from IRAS~2. This source is
observed in the infrared (Jennings et al. 1987), and submillimeter
regime (Sandell et al. 1994, Lefloch et al. 1998a) and evidence for
infall is presented by Ward-Thompson et al. (1996). Greaves, Holland,
Ward-Thompson (1997) present 800 $\mu$m polarimetry.

\vspace*{0.3cm}

{\bf HH 342 } {\em (03 25, +31 00)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. These are two close HH knots
lying on a line between NGC~1333 - IRAS~2 (Jennings et al. 1987) and
HH~341, see notes for that object.

\vspace*{0.3cm}

{\bf HH 343} {\em (03 25, +30 55)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. This is a well-collimated
chain of red-shifted HH knots in the southern part of the NGC~1333
cloud region. No probable source has been identified.

\vspace*{0.3cm}

{\bf HH 344 } {\em (03 25, +31 02)}. Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. These are two HH knots near
the center of the NGC~1333 cloud core. HH~344A coincides with the
H$_2$ filament ASR~98 (Aspin, Sandell, Russell 1994), and HH~344B lies
further to the south and is connected to HH 344A by diffuse emission.

\vspace*{0.3cm}

{\bf HH 345/346 } {\em (03 26, +31 03)}. Original paper: Bally,
Devine, Reipurth (1996), who present CCD images. These two objects
together form a fine collimated HH flow in position angle 215 degrees
emanating from the young star SVS~20 (LkH$\alpha$ 271). A compact,
bright bow shock, HH~346A, is located 10$''$-15$''$ southwest of
SVS~20. An H$\alpha$ bright bubble of emission extends further to the
southwest. Faint H$\alpha$ emission can be traced another 3 arcminutes
to the southwest, where it encounters a large H$\alpha$ bright arc,
HH~345. Northeast of SVS~20 there are faint wisps of H$\alpha$
emission which traces a counterflow. Spectra show that the HH~345/346
lobe SW of SVS~20 is blueshifted, and the NE side is red-shifted.

\vspace*{0.3cm}

{\bf HH 347} {\em (03 26, +31 05)}.  Original paper: Bally, Devine,
Reipurth (1996), who present CCD images. This is a pair of faint HH
knots, which coincide with the H$_2$ patch HL~11 (Hodapp \& Ladd
1995). The H$_2$ knots HL~3, 6, 10 and 11 plus ASR~57 (Aspin, Sandell,
Russell 1994) form an {\em infrared bipolar flow} emanating from
NGC~1333 - IRAS~4a, which is one of a pair of class~0
sources. Haschick et al. (1980) detected a pair of highly variable
{\em H$_2$O masers}, and at the location Jennings et al. (1987) found
a far-infrared source IRAS~4, which Sandell et al. (1991) revealed to
be a 30$''$ separation {\em sub-millimeter binary}. Lay, Carlstrom,
Hills (1995) performed {\em mm interferometry}, which resolved each of
IRAS~4a and 4b into close binaries. Liseau, Sandell, Knee (1988) found
a {\em molecular outflow} emanating from IRAS~4, which Blake et
al. (1995) showed to be quadrupolar. Lefloch et al. (1998a) found 1.3
mm continuum emission tracing the outflow cavity. Chernin, Masson,
Fuller (1994) detected high velocity sulfur monoxide emission towards
IRAS~4.  Lefloch et al. (1998b) found widespread SiO emission in the
region.  Ceccarelli et al. (1997) measured [OI] 63 $\mu$m emission
towards IRAS~4A, and Ceccarelli et al. (1999) detected water emission
lines. A detailed study in CS is presented by Langer, Castets, Lefloch
(1996).  {\em Polarization measurements} at sub-mm wavelengths of
IRAS~4a and 4b are presented by Minchin, Sandell, Murray (1995) and
Greaves, Holland, Ward-Thompson (1997), at 3.4mm of IRAS~4a by Akeson
et al. (1996), and at 3 mm by Akeson \& Carlstrom (1997).

\vspace*{0.3cm}

{\bf HH 348/349} {\em (03 26, +31 03)}. Original paper: Bally,
Devine, Reipurth (1996), who present CCD images. These are two faint
HH knots in the NGC~1333 cloud core, and they appear to be connected
by faint diffuse emission. They are possibly related to one of the
components of the IRAS~4 quadruple system (see notes for HH~347).

\vspace*{0.3cm}

{\bf HH 350} {\em (03 25, +30 54)}. Original paper: Bally, Devine,
Reipurth (1996), who present a CCD image. This is a bow shaped
filament just south of HH~343 in the southern part of the NGC~1333
cloud region.

\vspace*{0.3cm}

{\bf HH 351} {\em (03 25, +30 40)}. Original paper: Bally, Devine,
Reipurth (1996), who present a CCD image. This is an extended cluster
of HH filaments south of the NGC~1333 cloud core. It could be a
distant bow shock in a parsec scale flow from one of the IRAS sources
embedded in the cloud core.

\vspace*{0.3cm}

{\bf HH 352 } {\em (03 26, +30 49)}.  Original paper: Bally, Devine,
Reipurth (1996), who present a CCD image. These are a few HH knots
located south of the NGC~1333 cloud core. Bachiller et al. (1998b)
note that these knots are lying along the axis of a molecular jet from
SVS~13b.

\vspace*{0.3cm}

{\bf HH 353} {\em (03 26, +31 19)}. Original paper: Bally, Devine,
Reipurth (1996). This is a large, faint and diffuse HH object located
north of the NGC~1333 cloud core, and outside of the CCD images
published by Bally, Devine, Reipurth (1996).

\vspace*{0.3cm}

{\bf HH 354 } {\em (22 06, +58 57)}. Original paper: Reipurth, Bally,
Devine (1997), who present a CCD image. This is a single HH object,
which is a distant bow shock in a giant flow from the IRAS source
22051+5848 located in the windswept cloud L1165 in Cepheus. Parker,
Padman, Scott (1991) found a {\em molecular outflow}. The source is
associated with a small {\em reflection nebula} GY~22 (Gyulbudaghian
1982), which has been imaged in the optical and infrared by Tapia et
al. (1997), Reipurth, Bally, Devine (1997) and Reipurth \& Aspin
(1997). {\em Infrared photometry} of the source is given by Persi et
al. (1988), and {\em infrared spectroscopy} by Reipurth \& Aspin
(1997) indicates that the source is in a FUor state.

\vspace*{0.3cm}

{\bf HH 355 } {\em (04 19, +19 36)}. Original paper: Reipurth, Bally,
Devine (1997), who present interference filter CCD images. This is a
pair of very large bow shocks located about 15-20 arcminutes north and
south of T~Tauri, thus forming a giant bipolar HH flow with a total
projected extent of about 1.5 pc. Spectra show that the northern lobe
is redshifted and the southern blueshifted. HH~355 thus shares the
same axis as the tiny HH~255 flow, which also has the same polarity of
its blue and red lobes. Both HH~255 and HH~355 are most probably
driven by the infrared companion to T~Tauri. See also notes for HH~155
and HH~255.

\vspace{0.3cm}

{\bf HH 356} {\em (03 30, +31 16)}. Original paper: Alten et
al. (1997). This is a diffuse HH object about one degree NW of the NGC 1333
cloud core.

\vspace{0.3cm}

{\bf HH 357} {\em (05 32, $-$05 08)}. Original paper: Yu, Bally,
Devine (1997). This is an HH object in the OMC~3 cloud, which
coincides with the bright H$_2$ knots YBD~4/5.



\vspace{0.3cm}

{\bf HH 358} {\em (23 22, +73 56)}. Original paper: Alten et
al. (1997). This is a bright HH object and several fainter knots in
the L1262 cloud. Kun (1998) suggest a distance of 180~pc.

\vspace{0.3cm}

{\bf HH 359} {\em (23 24, +74 06)}. Original paper: Alten et al. (1997). 
This is a single isolated HH knot in the L1262 cloud.



\vspace{0.3cm}

{\bf HH 360} {\em (04 01, +26 10)}. Original paper: Alten et
al. (1997).  These are two HH objects in the L1489 cloud, HH 360A is a
fairly bright compact nebula, while HH 360B is a fainter more extended
structure. Hodapp (1994) shows a K$'$ band image of the region. HH
360A is located very close to IRAS 04016+2610 = L1489 IRS, which was
observed at sub-mm wavelengths by Moriarty-Schieven et al. (1994), and
with near-infrared spectroscopy by Greene \& Lada (1996b) and Chiar et
al. (1998).  Hogerheijde et al. (1997a,1998) present high resolution
mm maps.  Optical spectroscopy of the source is discussed by Kenyon et
al. (1998), and near-infrared polarimetry by Whitney, Kenyon, G\'omez
(1997). Padgett et al. (1999) present HST/NICMOS images of the compact
reflection nebula around the star.


\vspace{0.3cm}

{\bf HH 361} {\em (04 01, +26 13)}. Original paper: Alten et al. (1997).
This is a faint HH object with some resemblance to a bow shock. It is
located some arcminutes NW of HH 360A in the L1489 cloud.

\vspace{0.3cm}

{\bf HH 362} {\em (04 01, +26 12)}. Original paper: Alten et al. (1997).
These are two faint diffuse HH objects a few arcminutes west of HH 361 in
the L1489 cloud.

\vspace*{0.3cm}

{\bf HH 363 } {\em (22 26, +68 45)}. Original paper: Alten et
al. (1997), who present a CCD image. The HH object, which is equally
bright in H$\alpha$ and in [SII], consists of two relatively bright
knots, located close to the IRAS source 22266+6845. This source is
embedded in the small compact and very opaque cloud L1221, and drives
a U-shaped molecular outflow (Umemoto et al. 1991). The region is
imaged at K$'$ by Hodapp (1994).

\vspace*{0.3cm}

{\bf HH 364 } {\em (22 37, +74 57)}. Original paper: Alten et
al. (1997). This is a faint HH knot west of the HH~189 flow in the
L1251 cloud. See notes for HH~189.

\vspace*{0.3cm}

{\bf HH 365 } {\em (19 41, +23 22)}. Original paper: Alten et
al. (1997). This is a bow shaped HH object which lies 9 arcminutes
north-east of 1548C27, and along the axis of the HH~165 jet emanating
from this source. The HH~365 object appears to be a bow shock for the
HH~165 jet. At the presumed distance of 2400 pc, the projected
separation of HH~165 and HH~365 is 6.2 pc, but the distance is very
uncertain. For references to 1548C27, see the notes for HH~165.

\vspace*{0.3cm}

{\bf HH 366 } {\em (03 43, +32 36)}. Original paper: Bally, Devine,
Alten (1996), who present H$\alpha$ + [SII] filter CCD images and
high-resolution optical spectra. HH~366 is a giant bipolar HH flow
stretching across 22 arcmin, corresponding to a projected length of
2.2 pc at a distance of 350 pc. The brighter southwestern lobe is
redshifted, and the fainter eastern lobe is blueshifted. The HH flow
is co-axial with a CO flow studied by Goldsmith, Langer, Wilson
(1986), Fuller et al. (1991), Langer, Velusamy, Xie (1996) and
Velusamy \& Langer (1998). The outflow is driven by the class I object
B5~IRS1 (Benson, Myers, Wright 1984, Beichman et al. 1990), detected
at 3.6 cm by Rodr\'\i guez \& Reipurth (1998), and is associated with
a faint reflection nebula (Heyers et al. 1990, Moore \& Emerson
1992). The source is fading with time at near-infrared wavelengths
(Moore \& Emerson 1994). The cloud core, Barnard~5, has a mass of
about 50 M$_\odot$ (Langer et al. 1989) and is mapped in NH$_3$ by
Benson, Myers, Wright (1984), and in $^{13}$CO and at 100 $\mu$m by
Beichman et al. (1988). Chemical evolution in the circumstellar
structure of B5~IRS1 is suggested by Kelly, Macdonald, Millar
(1996). Polarization studies of stars behind B5 are given by Joshi et
al. (1985), Goodman et al. (1990) and I`lin, Khudyakova, Reshetnikov
(1994).  Starlight through the halo of B5 has been studied by Wannier
et al. (1999).

\vspace*{0.3cm}

{\bf HH 367} {\em (03 43, +32 33)}. Original paper: Bally, Devine,
Alten (1996), who present H$\alpha$ + [SII] filter CCD images. These
are two faint HH knots apparently emerging from B5~IRS3. This source
drives its own molecular outflow (Goldsmith et al. 1986). See also
notes for HH~366.

\vspace{0.3cm}

{\bf HH 368} {\em (03 27, +30 20)}. Original paper: Alten et al. (1997). 
A single faint HH knot.

\vspace{0.3cm}

{\bf HH 369} {\em (03 27, +30 18)}. Original paper: Alten et al. (1997). 
A single faint HH knot two arcminutes south of HH 368.

\vspace{0.3cm}

{\bf HH 370} {\em (03 27, +30 17)}. Original paper: Alten et al. (1997). 
A single faint and diffuse HH knot an arcminute ESE of HH 369.


\vspace{0.3cm}

{\bf HH 371} {\em (03 27, +30 20)}. Original paper: Alten et al. (1997).
These are two closely connected HH knots one and a half arcminutes north of
HH 372.

\vspace{0.3cm}

{\bf HH 372} {\em (03 27, +30 19)}. Original paper: Alten et al. (1997).
These are three bright HH knots forming a small compact cluster.

\vspace*{0.3cm}

{\bf HH 373 } {\em (22 35, +74 59)}. Original paper: Alten et
al. (1997). This is a bright, large complex of HH knots north-west of
the HH~189 flow in the L1251 cloud. See also notes for HH~149 and
HH~189.

\vspace*{0.3cm}

{\bf HH 374 } {\em (22 36, +74 52)}. Original paper: Alten et
al. (1997). This is a chain of two or three HH knots south-west of the
HH~189 flow in the L1251 cloud.

\vspace*{0.3cm}

{\bf HH 375 } {\em (20 38, +67 50)}. Original paper: Devine, Reipurth,
Bally (1997), who show an H$\alpha$ + [SII] CCD image of the entire
L1157 cloud. This is a single HH object, which coincides precisely
with the southern one (A) of several infrared H$_2$ objects emanating
from the embedded source IRAS 20386+6751 (Hodapp 1994, Davis \&
Eisl\"offel 1995). These objects coincide with a molecular outflow,
which has strong enhancements of several species, e.g. SiO, ammonia
and methanol (Umemoto et al. 1992, Mikami et al. 1992, Bachiller,
Martin-Pintado, Fuente 1993, Tafalla \& Bachiller 1995, Bachiller et
al. 1995a, Zhang et al. 1995, Avery \& Chiao 1996, Bachiller \&
P\'erez Guti\'errez 1997). Interferometer data in CO are presented by
Gueth, Guilloteau, Bachiller (1996), and in SiO by Gueth, Guilloteau,
Bachiller (1998). Mm interferometer data of the circumstellar gas of
the source are discussed by Gueth et al. (1997) and Meehan et
al. (1998).  The source is associated with an H$_2$O maser (Claussen
et al. 1996).  A distance of 440 pc is estimated by Viotti (1969). The
source was detected at 3.6 cm by Rodr\'\i guez \& Reipurth (1998).

\vspace*{0.3cm}

{\bf HH 376 } {\em (20 35, +67 43)}. Original paper: Reipurth, Bally,
Devine (1997), who present a CCD image. This HH flow consists of a
bright bow shock HH~376A, and a more distant fainter knot, HH~376B,
both on a line passing through the IRAS source 20359+6745 located in
the small cloud L1152 in Cepheus. The source is associated with a
reflection nebula GM~1-12 (Gyulbudaghian \& Magakyan 1976) or RNO~124
(Cohen 1980a).

\vspace*{0.3cm}

{\bf HH 377} {\em (23 01, +61 25)}. Original paper: Devine, Reipurth,
Bally (1997), who present a [SII] CCD image. This is the optical
counterpart to a bright compact H$_2$ knot in the southern,
blueshifted lobe of a molecular outflow (Eisl\"offel et al. 1996, Ladd
\& Hodapp 1997, Noriega-Crespo, Garnavich, Molinari 1998).  Molecular
hydrogen images at 6.9 and 9.6 $\mu$m are discussed by Noriega-Crespo,
Garnavich, Molinari (1998).  The driving source is IRAS 23011+6126, a
bright class 0 source in the Cep E cloud (Lefloch, Eisl\"offel,
Lazareff 1996), associated with an H$_2$O maser (Wouterloot \&
Walmsley 1986). The presence of two outflows suggests that the source
is a close binary (Terquem et al. 1999).

\vspace*{0.3cm}

{\bf HH 378} {\em (04 32, +54 32)}. Original paper: Devine, Reipurth,
Bally (1997), who present an H$\alpha$ CCD image. This is a very well
collimated chain of four HH knots with a total extent of 7 1/2
arcminutes, forming a bipolar HH flow from the class I source IRAS
04327+5432, located on the flow axis.

\vspace*{0.3cm}

{\bf HH 379} {\em (21 42, +47 18)}. Original paper: Devine, Reipurth,
Bally (1997), who present an H$\alpha$ + [SII] CCD image. The HH
object is located outside a sharp-edged dark cloud, which contains a
cometary reflection nebula, and the nearby IRAS source 21432+4719. The
three objects are probably related.

\vspace*{0.3cm}

{\bf HH 380} {\em (20 57, +52 22)}. Original paper: Devine, Reipurth,
Bally (1997), who show an H$\alpha$ + [SII] CCD image. The HH flow
consists of two groups containing several HH knots. They are located
about 10 arcminutes north-east of IRAS 20568+5217, and the HH~381
objects are on the opposite side of the IRAS source, possibly
suggesting that they together form a single large HH flow.

\vspace*{0.3cm}

{\bf HH 381} {\em (20 56, +52 17)}. Original paper: Devine, Reipurth,
Bally (1997), who show an H$\alpha$ + [SII] CCD image. These are two
very faint HH knots located less than an arcminute from the IRAS
source 20568+5217, which illuminates a large reflection nebula that
opens up to the NNW, suggesting a flow axis at a large angle to the
axis defined by the IRAS source and HH~380 and HH~381. Possibly
several outflows are present in the region.

\vspace*{0.3cm}

{\bf HH 382} {\em (20 56, +52 05)}. Original paper: Devine, Reipurth,
Bally (1997), who show an H$\alpha$ + [SII] CCD image. These are three
HH knots located about 12 arcminutes south of IRAS 20568+5217,
approximately along the axis defined by its associated reflection
nebula.

\vspace*{0.3cm}

{\bf HH 383 } {\em (05 32, $-$05 09)}. Original paper: Yu, Bally,
Devine (1997), who note that it is an optical counterpart to the H$_2$
knot YBD~58 in the OMC~2/3 region.

\vspace*{0.3cm}

{\bf HH 384 } {\em (05 32, $-$05 11)}. Original paper: Yu, Bally,
Devine (1997), who note that it is an optical counterpart to the H$_2$
knot YBD~52 in the OMC~2/3 region.

\vspace*{0.3cm}

{\bf HH 385 } {\em (05 32, $-$05 09)}. Original paper: Yu, Bally,
Devine (1997), who note that it is an optical counterpart to the H$_2$
knot YBD~24 in the OMC~2/3 region.

\vspace*{0.3cm}

{\bf HH 386 } {\em (04 48, +30 42)}. Original paper: Hirth, Mundt,
Solf (1997). This is a bipolar microjet stretching a few arcseconds on
either side of UY Aur at a position angle of approximately 40
degrees. UY Aur is a binary with 0.89 arcsec separation (Joy \& van
Biesbrock 1944, Leinert et al. 1993, Ghez, Neugebauer, Matthews 1993,
Ghez et al. 1995, Koresko, Herbst, Leinert 1997, Close et al. 1998).
A low-dispersion spectrum is presented by Cohen \& Kuhi
(1979). Molecular hydrogen emission was detected towards the companion
by Herbst, Koresko, Leinert (1995). The accretion luminosity is
derived from Pa$\beta$ and Br$\gamma$ emission by Muzerolle, Hartmann,
Calvet (1998).  Duvert et al. (1998) present $^{13}$CO mm
interferometry of a circumbinary disk.

\vspace*{0.3cm}

{\bf HH 387 } {\em (19 36, +10 23)}. Original paper: Hirth, Mundt,
Solf (1997). This is a bipolar microjet, with faint knots stretching
up to 10 - 15 arcsec from V536 Aql at a position angle of about 110
degrees. Mundt \& Eisl\"offel (1998) present interference filter
images. The star is a classical T~Tauri star (Cohen \& Kuhi 1979,
Appenzeller, Jankovics, \"Ostreicher 1984), with a large
polarization. It is a close binary with separation 0.52 arcsec
(Ageorges et al. 1994).

\vspace{0.3cm}

{\bf HH 389} {\em (20 59, +50 09)}. Original paper: Mundt \&
Eisl\"offel (1998), who present interference filter CCD images. This
is a 3 arcmin long HH flow emanating to the south from the peculiar T
Tauri star V1331 Cyg (IRAS 20595+5009). The star has been studied in
the optical by, among others, Kuhi (1964), Chavarria-K. (1981),
Kolotilov (1984), Mundt (1984), Shevchenko et al. (1991), Ivanova
(1994) and Hamann et al. (1994).  Infrared CO spectra are shown by
Biscaya et al. (1997).  Weintraub, Sandell, Duncan (1991) present 450
- 1300 $\mu$m photometry.  Henning et al. (1998) present a 1300 $\mu$m
map.  McMuldroch, Sargent, Blake (1993) use aperture synthesis
$^{13}$CO and continuum observations to detect a disk and
circumstellar envelope, as well as a molecular outflow, also studied
by Levreault (1988). Terquem et al. (1999) discuss precession of the
HH jet axis due to a possible binary nature of the source.  Shevchenko
et al. (1991) suggest a distance of 550 pc.

\vspace*{0.3cm}

{\bf HH 390 } {\em (04 16, +27 08)}. Original paper: G\'omez,
Whitney, Kenyon (1997), who present a [SII] CCD image. This is a
double knot on a line through the IRAS source 04166+2706 in
Taurus. The object is close to the redshifted lobe of a {\em molecular
outflow} (Bontemps et al. 1996).

\vspace*{0.3cm}

{\bf HH 391 } {\em (04 16, +27 02)}. Original paper: G\'omez, Whitney, Kenyon
(1997), who present a [SII] CCD image and an H$_2$ image. This is a
chain of several HH knots, which may form a single HH flow from the
IRAS source 04169+2702. The source drives a {\em molecular outflow}
(Bontemps et al. 1996) and is associated with a compact {\em
reflection nebula} (Tamura et al. 1991, Kenyon et al. 1993, Whitney,
Kenyon, G\'omez 1997). The source was measured at 1300 $\mu$m by
Moriarty-Schieven et al (1994), and Ohashi et al. (1997b) find a flattened
envelope in C$^{18}$O.

\vspace*{0.3cm}

{\bf HH 392 } {\em (04 18, +26 55)}. Original paper: G\'omez, Whitney,
Kenyon (1997), who present a [SII] CCD image. These are three HH knots
A, B, and C spread over 5 arcminutes in the vicinity of IRAS
04181+2655, but there are other infrared sources nearby, and it is
unclear if the three knots form one or more HH flows. Knots A and B
are within the redshifted lobe of a {\em molecular outflow} possibly
associated with IRAS 04181+2655 (Moriarty-Schieven et al 1992,
Bontemps et al. 1996). The IRAS source was measured at 1300 $\mu$m by
Moriarty-Schieven et al. (1994), with near-infrared spectroscopy by
Greene \& Lada (1996b), and with near-infrared polarimetry by Whitney,
Kenyon, G\'omez (1997).

\vspace*{0.3cm}

{\bf HH 393 } {\em (04 27, +24 34)}. Original paper: G\'omez,
Whitney, Kenyon (1997), who present a [SII] CCD image. This is a
diffuse knot south of the T~Tauri star ZZ~Tau. There are other young
stars in the region, so it is not clear which is the driving source.

\vspace*{0.3cm}

{\bf HH 394 } {\em (04 30, +22 48)}. Original paper: G\'omez, Whitney,
Kenyon (1997), who present a [SII] CCD image. This is a chain of HH
knots on a line through the IRAS source 04302+2247. The source drives
a {\em molecular outflow} and is associated with a {\em reflection
nebula} (Tamura et al. 1991).  The nebula was observed with
near-infrared images and displays a butterfly morphology, with a dark
lane, which appears to be a disk seen edge-on (Lucas \& Roche
1997,1998b).  More detailed HST/NICMOS images of the nebula are
presented by Padgett et al. (1999).  The source was observed at 1300
$\mu$m by Moriarty-Schieven et al. (1994). Strong near-infrared
polarization was detected by Whitney, Kenyon, G\'omez (1997).

\vspace*{0.3cm}

{\bf HH 395 } {\em (04 37, +25 40)}. Original paper: G\'omez,
Whitney, Kenyon (1997), who present a [SII] CCD image. There are two
HH knots on a line through IRAS 04369+2539 which illuminates the large
{\em reflection nebula} IC~2087.

\vspace{0.3cm}

{\bf HH 396/397 } {\em (05 55, +16 31)}. Original paper: Devine et
al. (1999b), who present CCD images. This is a giant bipolar HH flow
stretching over a total of 10 pc and centered on the 3000 L$_\odot$ B
star IRAS 05553+1631 associated with the compact HII region
G192.16-3.82 located at 2 kpc distance in Gemini (Hughes \& MacLeod
1993, Shepherd et al. 1998). The young star is embedded in a dense
cloud core observed in ammonia by Molinari et al. (1996), and is
associated with a strong H$_2$O maser (Codella, Felli, Natale 1996,
Shepherd \& Kurtz 1999).  The source drives a massive molecular
outflow (Snell, Dickman, Huang 1990, Shepherd \& Churchwell 1996,
Shepherd et al. 1998, Shepherd \& Kurtz 1999).  Near-infrared images
show a an infrared reflection nebula and H$_2$ emission knots (Hodapp
1994, Shepherd et al. 1998, Devine et al. 1999b).


\vspace{0.3cm}

{\bf HH 398 } {\em (22 32, +40 24)}. Original paper: Corcoran \& Ray
(1998), who present long slit spectroscopy. This is a bipolar HH jet
emanating from the Herbig Ae/Be star LkH$\alpha$ 233.  It is
associated with a bipolar nebula (Herbig 1960, Calvet \& Cohen
1978). Broadband imaging polarimetry suggests the presence of a torus
around the star (Aspin, McLean, McCaughrean 1985). Near infrared
speckle interferometry shows that the source is surrounded by a highly
scattering halo 1$''$ in size (Leinert, Haas, Weitzel 1993). Hamann
(1994) found the [FeII] lines to be strongly blueshifted.  Fuente et
al. (1998) present $^{13}$CO, CS and 1.3 mm continuum maps.




\vspace*{0.3cm}

{\bf HH 399} {\em (17 59, $-$23 04)}. Original papers: Cernicharo et
al. (1997,1998), who present a CCD image. This is a 22 arcsec long
well-collimated jet emanating from a cometary globule, which points
towards HD~164492A, the central massive star in the Trifid
Nebula. About 65 arcsec further downstream the flow terminates in a
bow shock.  At the assumed distance of 1680 pc, this corresponds to a
projected size of 0.7 pc.  The source is deeply embedded, is very cold
and has only been detected at 1300 $\mu$m.



\vspace*{0.3cm}

{\bf HH 401/402 } {\em (05 32, $-$06 31)}. Original paper: Ogura
(1995), who presents a large-field photograph of both objects, and a
low-dispersion spectrum of HH~401. The two objects are separated by
5.9 pc and centered on the HH~1/2 driving source. HH~401 is a giant
bow shock shaped feature north-west of HH~1, while HH~402 is a much
fainter diffuse feature south-east of HH~2. See also references under
HH~1/2.

\vspace{0.3cm}

{\bf HH 403    } {\em (05 34, $-$05 54)}. Original paper: Reipurth, Devine,
Bally (1998), who present a CCD image. This is a several arcminute large
fragmented bow shock, which faces away from the L1641-N cluster half a
degree away to the SW. Together with HH~404 it forms a giant HH flow.

\vspace{0.3cm}

{\bf HH 404   } {\em (05 34, $-$05 45)}. Original paper: 
Reipurth, Devine, Bally (1998), who present a CCD image. The object has a
strong resemblance to a large bow shock. It is 5.4 pc in projection from
the L1641-N cluster from where it appears to come, together with the nearby
HH~403. Reipurth, Devine, Bally (1998) suggest that HH~127 forms the
counterlobe to this flow.

\vspace{0.3cm}

{\bf HH 405/406   } {\em (05 34, $-$05 41)}. Original paper: 
Reipurth, Devine, Bally (1998), who present CCD images. HH 405 appears to
be a small jet pointing towards HH 406, which has the morphology of a bow
shock. No source is known.


\vspace{0.3cm}

{\bf HH 407} {\em (5 32, $-$06 01)}. Original paper: Mader et
al. (1999), who present CCD images. This appears to be a large
fractured bow shock, and it is possible that it is part of a giant HH
flow from the L1641-N region. See also notes for HH~303.

\vspace{0.3cm}

{\bf HH 408} {\em (04 38, +25 50)}. Original paper: Stapelfeldt et
al. (1999b), who present CCD images. This is a bipolar HH flow
associated with the T Tauri star Haro 6-33 (IRAS 04385+2550). There
are two short jets as well as several more distant bow shocks on
either side of the star. Optical, near- and mid-infrared photometry of
Haro~6-33 is given by Myers et al. (1987). Kenyon et al. (1998)
suggest a spectral type of M0, and give emission line strengths.  The
star is located in a small cloud core mapped in C$^{18}$O by Onishi et
al. (1998).

\vspace{0.3cm}

{\bf HH 410/411 } {\em (04 25, +24 12)}. Original paper: Devine et
al. (1999a), who present CCD images. HH~410 is a major bright complex of HH
knots, which forms a bow shock in a giant flow from Haro~6-10. It is
located 24 arcmin to the SW of Haro~6-10. HH~411 lies on the same flow
axis, but on the opposite side of Haro~6-10, 14 arcmin NE of this star. The
total projected extent of the complex at the assumed distance of 140 pc is
1.6 pc. HH~411 is a highly unusual object, consisting of thin filaments
emitting mostly in H$\alpha$ and lying perpendicular to the flow axis. Both
HH~410 and 411 have burst completely out of the L1524 cloud and are seen
against a background of stars and galaxies. See also notes for HH~184.

\vspace{0.3cm}

{\bf HH 412 } {\em (04 26, +24 30)}. Original paper: Devine et
al. (1999a), who present CCD images. This is a one arcminute long
fairly diffuse emission feature located about 7 arcmin NE of Haro~6-10
and on the well defined flow axis of HH~410/411. It is presumably part
of this giant flow.

\vspace{0.3cm}

{\bf HH 413/414 } {\em (04 26, +24 31)}. Original paper: Devine et
al. (1999a), who present CCD images. HH~414 is a small bipolar jet
coinciding with the IRAS source 04264+2433. It points towards HH~413,
5~1/2 arcmin to the ESE, which has the morphology of two bow
shocks. HH~413 is located on the HH~410/411 flow axis, but this
appears to be coincidental. HH~414~IRS is a near- and far-infrared
source with significant polarization and with a total luminosity of
only 0.4 L$_\odot$ (Kenyon et al. 1993, 1994, Whitney, Kenyon, G\'omez
1997). Optical spectroscopy towards the source reveals a red veiled
continuum and typical HH emission lines (Kenyon et al. 1998).

\vspace{0.3cm}

{\bf HH 415 } {\em (20 45, +67 49)}. Original paper: Reipurth,
Bally, Devine (1997), who present a CCD image. This is a single faint
HH knot north-east of PV~Cep, and it is unclear if it is related to
the HH~215/315 flow (see notes for these objects) or belongs to a
separate flow.

\vspace{0.3cm}

{\bf HH 416} {\em (16 24, $-$24 42)}. Original papers: Wilking et
al. (1997a) and G\'omez, Whitney, Wood (1998), who present CCD images. This is
a structured HH complex in the $\rho$ Ophiuchi clouds.

\vspace{0.3cm}

{\bf HH 417} {\em (16 25, $-$24 21)}. Original paper: G\'omez, Whitney,
Wood (1998), who present a CCD image. This is a bright, one arcminute wide
complex of a multitude of HH knots in the $\rho$ Ophiuchi cloud region.


\vspace{0.3cm}

{\bf HH 418} {\em (16 23, $-$24 34)}. Original paper: G\'omez, Whitney,
Wood (1998), who present a CCD image. This is a faint elongated HH knot in
the $\rho$ Ophiuchi clouds, near HH 314.


\vspace{0.3cm}

{\bf HH 419} {\em (16 23, $-$24 24)}. Original paper: G\'omez, Whitney,
Wood (1998), who present a CCD image. This is a large and diffuse HH object
in the $\rho$ Ophiuchi clouds.


\vspace{0.3cm}

{\bf HH 420} {\em (16 25, $-$24 30)}. Original paper: G\'omez, Whitney,
Wood (1998), who present a CCD image. This is a diffuse HH object in the
$\rho$ Ophiuchi clouds.

\vspace{0.3cm}

{\bf HH 421} {\em (21 00, +49 39)}. Original paper: Mundt \&
Eisl\"offel (1998), who present CCD images. This is a 22 arcsec long
jet coming from the emission line star LkH$\alpha$ 321 (IRAS
21002+4939). The star has been observed spectroscopically by Cohen \&
Kuhi (1979) and Mundt (1984), and photometrically by Shevchenko et
al. (1991), who suggest a distance of 550 pc.

\vspace{0.3cm}

{\bf HH 422} {\em (3 24, +30 01)}. Original paper: Davis et al. (1997b),
who present a CCD image. This is a faint HH knot 30$''$ south of the
reflection nebula RNO 15 (Cohen 1980), associated with the source L1455
IRS2 (= IRAS 03247+3001). It is, however, not clear that the HH knot is
associated with this source considering the complexity of outflows in the
region (see notes for HH 318).

\vspace{0.3cm}

{\bf HH 423} {\em (3 24, +30 05)}. Original paper: Davis et al. (1997b),
who present a CCD image. This is a faint HH knot some arcminutes NNW of
L1455 IRS 1 = RNO 15-FIR, but it is unclear if they are related.

\vspace{0.3cm}

{\bf HH 424} {\em (21 00, +49 40)}. Original paper: Mundt \& Eisl\"offel
(1998), who present CCD images. This is an emission line knot located a few
arcseconds from a faint source, called LkH$\alpha$ 321B due to its location
170 arcsec west of LkH$\alpha$ 321. See also notes for HH 421.

\vspace{0.3cm}

{\bf HH 425} {\em (20 18, +41 11)}. Original paper: Magakyan \&
Movsesyan (1997b), who present long-slit spectra and images. This is a
nebulous knot, also seen in the images of Aspin, Sandell, Weintraub
(1994), which is spectroscopically identified as an HH object. It is
associated with the young rather luminous emission line star
LkH$\alpha$ 225 (Herbig 1960), also known as V1318 Cyg. The star is
highly variable (see references in Ibragimov et al. 1988 and
Hillenbrand et al. 1995), and it is a binary (Aspin, Sandell,
Weintraub 1994, Palla et al. 1995). The southern component may drive a
molecular outflow (Palla et al 1995). Henning et al. (1998) present a
1300 $\mu$m map.

\vspace{0.3cm}

{\bf HH 426} {\em (3 25, +30 42)}. Original paper: Yan et al. (1998), who
present a [SII] CCD image. These are two close HH knots located about 9
arcminutes south of HH 14 near NGC 1333.


\vspace{0.3cm}

{\bf HH 427} {\em (3 27, +30 11)}. Original paper: Yan et al. (1998), who
present a [SII] CCD image. A faint HH knot in the Perseus clouds.

\vspace{0.3cm}

{\bf HH 428} {\em (3 27, +30 27)}. Original paper: Yan et al. (1998), who
present a [SII] CCD image. A relatively bright HH object in the Perseus
clouds.


\vspace{0.3cm}

{\bf HH 429} {\em (3 28, +30 59)}. Original paper: Yan et al. (1998), who
present a [SII] CCD image. These are two HH knots in the Perseus clouds, HH
429A is the brighter one, while HH 429B, located an arcminute further east,
is fainter and more diffuse.

\vspace{0.3cm}

{\bf HH 430} {\em (3 29, +31 14)}. Original paper: Yan et al. (1998), who
present a [SII] CCD image. This is a cluster of faint HH knots in the
Perseus clouds.

\vspace{0.3cm}

{\bf HH 431} {\em (3 30, +30 59)}. Original paper: Yan et al. (1998), who
present a [SII] CCD image. Two close somewhat diffuse HH knots in the B1
core in the Perseus clouds. They are located very close to the source IRAS
1 (IRAS 03301+3057), which may be the driving source. A molecular outflow
is driven by this source (Bachiller, Menten, del Rio-Alvarez 1990, Yamamoto
et al. 1992, Hirano et al. 1997). The magnetic field strength in Barnard~1
is discussed by Goodman et al. (1989) and Crutcher et al. (1994).

\vspace{0.3cm}

{\bf HH 432} {\em (3 30, +30 59)}. Original paper: Yan et al. (1998), who
present a [SII] CCD image. These are two faint HH objects in 
the B1 core in the Perseus
clouds, about an arcminute apart. HH 432A is larger and more diffuse, and
HH 432B further to the south-east, contains at least two knots.
See notes for HH 433.

\vspace{0.3cm}

{\bf HH 433} {\em (3 30, +30 54)}. Original paper: Yan et al. (1998),
who present a [SII] CCD image. This is a compact cluster of at least 4
HH knots in the B1 core in the Perseus clouds. Together with HH 432,
these objects are well aligned with a line through the nearby source
IRAS 2 (IRAS 03304+3100 = LkH$\alpha$ 327), a 15th magnitude star of
spectral type K2 studied by Cohen \& Kuhi (1979) and Rydgren \& Vrba
(1983). The B1 core has been studied in mm-transitions by Bachiller,
Menten, del Rio-Alvarez (1990).

\vspace{0.3cm}

%{\bf HH 434/435/436} {\em (4 31, +23 01)}. Original paper: Yan et
%al. (1998), who present a [SII] CCD image. This is a highly complex region
%with a multitude of quite bright HH objects scattered over an area about
%two arcminutes in extent. HH 435 has the characteristic morphology of a
%large bow shock facing towards the south-west.

%\vspace{0.3cm}

%{\bf HH 437} {\em (5 44, +00 20)}. Original paper: Yan et al. (1998), who
%present a [SII] CCD image. This is a compact HH object located in a high
%extinction region in L1630 in Orion.

%\vspace{0.3cm}

%{\bf HH 438} {\em (5 44, +00 10)}. Original paper: Yan et al. (1998), who
%present a [SII] CCD image. This is an almost 2 arcmin long chain of HH
%objects in the L1630 cloud in Orion.

%\vspace{0.3cm}

%{\bf HH 439} {\em (06 04, $-$05 53)}. Original paper: Yan et al. (1998), who
%present a [SII] CCD image. These are two faint HH knots an arcminute apart,
%located in the eastern part of Orion.

%\vspace{0.3cm}

%{\bf HH 440} {\em (.........)}. Original paper: Zhao et al. (1999),
%who present a CCD image.

%\vspace{0.3cm}

%{\bf HH 441} {\em (.........)}. Original paper: Zhao et al. (1999),
%who present a CCD image.

%vspace{0.3cm}

%{\bf HH 442} {\em (.........)}. Original paper: Zhao et al. (1999),
%who present a CCD image.


%\vspace{0.3cm}

%{\bf HH 443} {\em (.........)}. Original paper: Zhao et al. (1999),
%who present a CCD image.





\vspace{0.3cm}

{\bf HH 444} {\em (05 37, $-$02 33)}. Original paper: Reipurth et
al. (1998), who present a CCD image and low-dispersion spectroscopy. This
is a compact jet with several bow shocks stretching over 2 1/2 arcminutes
from the visible T~Tauri star V510 Orionis in the $\sigma$ Orionis HII
region (for details on this variable star, see Herbig \& Bell 1988).

\vspace{0.3cm}

{\bf HH 445} {\em (05 37, $-$02 35)}. Original paper: Reipurth et
al. (1998), who present a CCD image. This is a monopolar jet that is
18 arcsec long, and emanating from the visible H$\alpha$ emission star
A-0976-357 (Wiramihardja et al. 1991) in the $\sigma$ Orionis HII
region. A second fainter jet, called HH~445X appears from the same
source, suggesting that it could be a close binary.

\vspace{0.3cm}

{\bf HH 446} {\em (05 37, $-$02 40)}. Original paper: Reipurth et
al. (1998), who present a CCD image. This is a short, highly asymmetric
bipolar jet driven by a faint visible star in the $\sigma$ Orionis HII
region.

\vspace{0.3cm}

{\bf HH 447} {\em (05 38, $-$02 35)}. Original paper: Reipurth et
al. (1998), who present a CCD image. This is a 7 arcsec long jet coming
from the visible star Haro~5-39 in the $\sigma$ Orionis HII region.

\vspace{0.3cm}

{\bf HH 449} {\em (05 36, $-$07 14)}. Original paper: Strom et
al. (1986). This is a faint chain of HH knots emanating from the young
star Haro~4-249 (sometimes incorrectly listed as Haro~2-249), which is
associated with a prominent reflection nebula. The star was first
noted by Haro (1953), and was observed spectroscopically by Cohen \&
Kuhi (1979). It is associated with IRAS 05363--0714, a 6~L$_\odot$
source. Near-infrared
photometry is given by Nakajima et al. (1986).

%\vspace{0.3cm}

%{\bf HH 450} {\em (.........)}. Original paper: Bally \& Reipurth
%(1999), who present a CCD image and a spectrum. This is an HH object
%driven by the IRAS source 22129+7000, embedded in the Bok globule B175
%(Barnard 1919). A distance of 400 pc to the globule has been rather
%well estimated due to the presence of a B9.5V star BD +69$^o$1231,
%which has a chance encounter with the globule. The star is surrounded
%by a reflection nebula, Ced 201 = vdB 152 (Wolf 1908, Witt et
%al. 1987).


\vspace{0.3cm}

%{\bf HH 451} {\em (.........)}. Original paper: Zhao et al. (1999),
%who present a CCD image.


%\vspace{0.3cm}

%{\bf HH 452} {\em (.........)}. Original paper: Zhao et al. (1999),
%who present a CCD image.


%\vspace{0.3cm}

%{\bf HH 453} {\em (.........)}. Original paper: Zhao et al. (1999),
%who present a CCD image.


%\vspace{0.3cm}

{\bf HH 454} {\em (04 28, +18 02)}. Original paper: Devine, Reipurth,
Bally (1998), who present CCD images. These are three HH knots forming
a bipolar HH flow centered on L1551-NE, a low-luminosity deeply
embedded source discovered by Emerson et al. (1984). Optical, infrared
and mm observations of the source region are discussed by Draper,
Warren-Smith, Scarrott (1985b), Campbell et al. (1988), Pound \& Bally
(1991), Moriarty-Schieven \& Wannier (1991), Barsony \& Chandler (1993),
Moriarty-Schieven, Butner, Wannier (1995), Rodr\'\i guez, Anglada, Raga
(1995), Hodapp \& Ladd (1995), Whitney, Kenyon, G\'omez (1997).

\vspace{0.3cm}

{\bf HH 455} {\em (18 27, +01 14)}. Original papers: Davis et
al. (1999) and Ziener \& Eisl\"offel (1999), who present CCD images.
This is a fine extended and collimated HH flow, with a bright bow
shock at its apex. It points back towards a source, PS~2, seen in the
IRAS 12 $\mu$m HIRES data of Hurt \& Barsony (1996). It is close to
the Serpens Reflection Nebula and the surrounding rich star forming
region, and the following list of references to this well studied
region is not exhaustive. The region has been studied at optical,
infrared, sub-millimeter and millimeter wavelengths by Strom, Vrba,
Strom (1976b), Loren, Evans, Knapp (1979), Nordh et al. (1982), Bally
\& Lada (1983), Ungerechts \& G\"usten (1984), Gomez de Castro, Eiroa,
Lenzen (1988), Rodr\'\i guez et al. (1989d), Eiroa \& Casali (1989,
1992), de Lara, Chavarria-K., L\'opez-Molina (1991), Casali, Eiroa,
Duncan (1993), Curiel et al. (1993), McMullin et al. (1994), White,
Casali, Eiroa (1995), Hurt \& Barsony (1996), Hodapp et al. (1996),
Herbst, Beckwith, Robberto (1997), Huard, Weintraub, Kastner (1997),
Testi \& Sargent (1998), Giovanetti et al. (1998), Hogerheijde et
al. (1999), Codella, Bachiller, Reipurth (1999), Davis et al. (1999),
Ziener \& Eisl\"offel (1999).


\vspace{0.3cm}

{\bf HH 456/457} {\em (18 27, +01 09)}. Original paper: Davis et
al. (1999), who present CCD images. This is a little compact group of
HH knots near the Serpens Reflection Nebula, and of uncertain origin.
See also notes for HH~455.


\vspace{0.3cm}

{\bf HH 458/459} {\em (18 27, +01 12)}. Original papers: Davis et
al. (1999) and Ziener \& Eisl\"offel (1999), who present CCD images.
This appears to be two lobes of a bipolar HH flow, which may originate
in the source SMM~3, just south of the Serpens Reflection Nebula. See
also notes for HH~455.



\vspace{0.3cm}

{\bf HH 460} {\em (18 27, +01 16)}. Original papers: Davis et
al. (1999) and Ziener \& Eisl\"offel (1999), who present CCD images.
This is a group of HH knots, which is located at the bright
north-western tip of a molecular outflow lobe. The high density of
active sources in the region makes it difficult to assign a
source. See also notes for HH~455.

\vspace{0.3cm}

{\bf HH 461} {\em (00 08, +58 31)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. This is a rather bright compact HH
object, located about 1.5 arcmin SSE of LkH$\alpha$~198, on the axis
of the HH~164 flow, which emanates from this star. HH~461 is probably
a bow shock of the HH~164 flow, see also notes for HH~161 and 164.


\vspace{0.3cm}

{\bf HH 462} {\em (03 50, +38 01)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. This is a small  HH flow
located along the symmetry axis of the cometary nebula PP~11, a
reflection nebula illuminated by the partly embedded IRAS 03507+3801
source. Levreault (1988) estimated a V-magnitude of 21.4 for the emerging
star, in the near-infrared it is much brighter (Tapia et al. 1997).


\vspace{0.3cm}

{\bf HH 463} {\em (04 07, +38 00)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. Parsamian \& Petrosian (1979) noted a
small nebula, PP~13, which Cohen et al. (1983) in an infrared study
showed to be associated with two young stars. HH~463 is a short stubby
jet emanating from the southern component, PP13S, which Sandell \&
Aspin (1998) studied in detail, and found to be a FUor candidate. A
faint emission knot is located an arcmin further along the jet axis.
Near-infrared spectroscopy and imaging of PP13S is also presented
by Smith (1993), and Tapia et al. (1997) show optical and
near-infrared images.


\vspace{0.3cm}

{\bf HH 464} {\em (04 07, +37 59)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. This is a faint curved chain of HH
knots probably driven by the young T Tauri star PP~13N. See notes for
HH~463.

\vspace{0.3cm}

{\bf HH 465} {\em (04 07, +38 00)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. This is a small cluster of HH knots
north of PP13N. See notes for HH~463.



\vspace{0.3cm}

{\bf HH 466} {\em (04 30, +24 15)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. These are two HH knots to the NNE of
and pointing back towards the well studied T Tauri star GK Tau, and
only a few references are given here. GK~Tau has a spectral type of
K7~V (Herbig 1977) and coincides with the IRAS source 04305+2414. It
forms a wide pair with the nearby GI~Tau with which it appears to be
coeval (Hartigan, Strom, Strom 1994). Accretion luminosities for GK
and GI~Tau are derived from Pa$\beta$ and Br$\gamma$ emission by
Muzerolle, Hartmann, Calvet (1998).  GK~Tau has a faint companion 2.5
arcsec to the east (Reipurth \& Zinnecker 1993). GK and GI~Tau are
associated with a reflection nebula, and appear to have recently
emerged from the B18 cloud in Taurus.

\vspace{0.3cm}

{\bf HH 467} {\em (04 30, +24 14)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. This is a faint HH knot and an
emission streamer about 45 arcsec SW of GK Tau. See also notes for
HH~466.



\vspace{0.3cm}

{\bf HH 468} {\em (04 30, +24 15)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. This is a faint diffuse HH knot NE of
GK~Tau. See notes for HH~466.


\vspace{0.3cm}

{\bf HH 469} {\em (05 36, $-$07 28)}. Original paper: Aspin \&
Reipurth (1999), who present CCD images. This is a small HH knot
associated with the embedded source Haro~4-255~FIR, a far-infrared
source detected by Evans et al. (1986) about an arcmin NW of the T
Tauri star Haro~4-255.  The HH knot is located next to a compact
reflection nebula (dubbed ``NW'') illuminated by Haro~4-255~FIR.
Anglada et al. (1992, 1998) detected Haro~4-255 in the cm radio
continuum. Davis \& Eisl\"offel (1995) find an H$_2$ flow associated
with Haro~4-255~FIR. Their knot G appears to coincide with HH~469. See
also notes for HH~470.


\vspace{0.3cm}

{\bf HH 470} {\em (05 37, $-$07 29)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. This is a finely collimated jet and a
bright bow shock associated with the young star Haro~4-255 (Haro
1953). Cohen \& Kuhi (1979) estimate a spectral type of K7, a large
H$\alpha$ equivalent width of 100, and an approximate V-magnitude of
15.7. Infrared observations are discussed by Cohen (1974b) and
Nakajima et al. (1986). The IRAS source 05369-0728 is a mixture of
emission from Haro~4-255 and the more deeply embedded source
Haro~4-255~FIR an arcmin further NW. Both stars are clearly seen in
the ir images of Hodapp (1994). Levreault (1988), Morgan et al. (1991)
and Tatematsu et al. (1993b) detect a molecular outflow in the region,
and Aspin \& Reipurth (1999) argue that it can be separated into two
bipolar outflows. Tatematsu et al. (1993) present detailed mm
observations of the surrounding cloud core.


\vspace{0.3cm}

{\bf HH 471/472/473/474} {\em (05 45, +00 37)}. Original paper: Aspin
\& Reipurth (1999), who present CCD images. These are a cluster of HH
knots located in the northern part of the L1630 cloud. They appear to
be associated with a little group of young stars. The brightest is the
nebulous star LkH$\alpha$ 316, which was found by Herbig \& Kuhi
(1963). It has a V-magnitude of around 14.1, a continuous spectrum and
strong H$\alpha$ emission according to Cohen \& Kuhi (1979), who also
noted a fainter nearby star, LkH$\alpha$~316/c (=HBC~511), with
V=16.7, a spectral type of M0.5 and very weak H$\alpha$
emission. About 1.5 arcmin further east is the embedded source IRAS
05451+0037. This source was suggested to drive a molecular outflow
(Iwata, Fukui, Ogawa 1988), but HH~472 and its associated faint star
is located at the center of the bipolar CO flow, with the jet along
the flow axis, suggsting that it is a better candidate for driving the
CO flow than IRAS 05451+0037.. The nearby HH~71 may be associated with
the HH objects in this area.


\vspace{0.3cm}


{\bf HH 475} {\em (20 22, +42 05)}. Original paper: Aspin \& Reipurth
(1999), who present CCD images. The little nebula PP~95 is located in
Cygnus (Parsamian \& Petrosian 1979). HH~475 is located several
arcminutes to the NE of PP~95, but is not necessarily associated with
it. If at the same distance as several other nearby star forming
regions, notably AFGL~2591, then HH~475 is 2 kpc away.



\vspace{0.3cm}


{\bf HH 476} {\em (18 26, +00 27)}. Original paper: Ziener \&
Eisl\"offel (1999), who present a CCD image. This is a single HH knot
close to several IRAS sources and nebulous stars. See also notes for
HH~455.


\vspace{0.3cm}


{\bf HH 477} {\em (18 27, +01 18)}. Original paper: Ziener \&
Eisl\"offel (1999), who present a CCD image. This is a single HH knot
located between the active T Tauri star ESO~H$\alpha$~279 (IRAS
18269+0116) and HH~107 in the Serpens molecular clouds. It is possibly
associated with the large HH~106/107 flow, see notes for these
objects.



\vspace{0.3cm}


{\bf HH 478} {\em (18 27, +01 13)}. Original paper: Ziener \&
Eisl\"offel (1999), who present a CCD image. These are two HH knots
located just north of the Serpens Reflection Nebula. See also notes
for HH~455.



%The next line is introduced by Ka Chun Yu and necessary for the web version

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