%Subject: notes.tex (DS1259)

\documentstyle{l-aa}
\input{epsf}
\begin{document}
\begin{center}
Notes on individual objects
\end{center}
\scriptsize
\hrule
\vspace{0.2cm} 
\def\deg{^o}
\begin{description}

\parskip 0pt

\item{ 9*} Member of the young open cluster NGC 225. The optical spectrum 
shows H$\alpha$ emission over a red stellar continuum. 

\item{11*} Member of the young open cluster NGC 225. The  optical
spectrum corresponds to an intermediate-type star without emission lines.

\item{20*} Star with nebular emission lines together with 
a strong H$\alpha$ emission over a faint continuum. The strength of the
sulphur doublet compared to H$\alpha$ indicates, according to diagnostic 
diagrams, that the source is probably an HII region. H$_2$O maser emission 
not detected  by Wouterloot et al. (1993).

\item{21*} H$_2$O maser emission not detected by Wouterloot et al. (1993).

\item{24*} New Seyfert 2 galaxy discovered during this survey. A detailed
analysis can be found in P\'erez et al. (1990). Recently detected in the 
near infrared below our detection limit by Heisler et al. (1996), who 
report the following near infrared magnitudes: $K$ = 12.43; $J-H$ = 0.96; 
$H-K$ = 0.66, corresponding to our region IV in the colour-colour diagram. 

\item{26*} The counterpart is a bright star (m$_V$ $\sim$12) showing 
H$\alpha$ emission over a G-type stellar continuum. The source is located in
the direction of the nearby strongly reddened open cluster Stock 2. 

\item{30*} H$_2$O maser emission detected by Zuckerman and Lo (1987)
and confirmed by Wouterloot et al. (1993). CS (2$\rightarrow$1) emission 
detected by Bronfman et al. (1996). 

\item{32*} Close to the HII region W5. However, the LRS spectrum 
provided by Volk et al. (1991) shows a strong sillicate absorption 
similar to those usually observed in extreme OH/IR stars. 
 
\item{33*} Probably associated to the nearby star forming region S199.

\item{34*} A-type star with H$\alpha$ emission over the stellar continuum. 
Radio continuum emission not detected by Crawford et al. (1996). 
Misidentified as a galaxy in Cohen (1992). 

\item{48*} T-Tauri star associated to the Taurus-Auriga star forming region.
The star shows an F6-type spectral continuum with H$\alpha$ in 
emission while H$\beta$ appears in absorption.  Additional near infrared 
photometry is available in Kenyon et al. (1990), which report the following
values: $K$ = 8.53; $J-H$ = 0.64; $H-K$ = 0.67.

\item{49*} Probably associated to the star forming region BFS34. H$_2$O 
maser emission not detected by Wouterloot et al. (1988). Although the 
surprisingly high IRAS variability index points to the possibility of this 
star being a variable OH/IR star, the IRAS colours correspond 
to a young stellar object. 

\item{51*} Associated to the dark cloud LDN 1473. M-type star with H$\alpha$ 
emission. Weintraub and Kastner 
(1992) suggest that the object is multiple and that one of the components 
might be a Mira variable according to the strong brightness variations observed
in the near infrared, although the IRAS colours correspond to a young 
stellar object. Additional near infrared photometry is available in 
Persi et al. (1988). They report the following values: $K$ = 11.05;
$J-H$ = 0.90; $H-K$ = 1.91, almost 3 magnitudes fainter than the values 
reported in our Paper I. H$_2$O maser emission detected by Wouterloot et al.
(1993), although not 
confirmed by Gyulbudaghian et al. (1987) and Persi et al. (1994).

\item{53*} Probably associated to the Taurus-Auriga star forming region. 
The IRAS position coincides with a bright A-type star with H$\alpha$ emission 
over absorption. Classified as A1e by Kenyon et al. (1990), they 
report the following near infrared data: $K$ = 8.24; $J-H$ = 0.47;
$H-K$ = 0.56. 

\item{56*} This source has tentatively been identified as a galaxy 
since it does not show any bright optical counterpart, it is not associated 
to any known star forming region and it is located at a high galactic 
latitude. A deep CCD image is needed to confirm this classification. 
H$_2$O maser emission was not detected by Wouterloot et al. (1993). 

\item{61*} H$_2$O maser emission was not detected by Wouterloot et al. (1993).

\item{62*} Binary star, according to Kenyon et al. (1990). The two stars 
are separated 3".5 and have the same brightness in the K band. The optical
spectrum of the NW source corresponds to a K1-type star while the SE source 
shows a K0-type stellar spectrum together with a possible emission at 3727 \AA. 
They suggest that this source might be a galaxy. In addition, they report the 
following near infrared magnitudes (mean of two measurements): $K$ = 10.66; 
$J-H$ = 0.96; $H-K$ = 0.28. H$_2$O maser emission not detected by Wouterloot 
et al. (1993). 

\item{63*} H$_2$O maser emission not detected by Gyulbudaghian et al. (1987) 
and Wouterloot et al. (1993). 

\item{74*} C-rich post-AGB star classified as G0Ia (m$_V$ = 14.21) 
by Hrivnak (1995). This is one of the few objects showing the unidentified 21 
$\mu$m emission feature (Kwok et al. 1989). HCN emission detected by 
Omont et al. (1993). Previous near infrared photometry available in Hrivnak 
and Kwok  (1991). They report the following values (the mean of two 
measurements): $K$ = 8.21; $J-H$ = 0.99; $H-K$ = 0.45.  

\item{75*} K-type stellar continuum with H$\alpha$ clearly in emission.

\item{87*} M-type star. H$_2$O maser emission not detected by Likkel (1989).

\item{88*} Classified as a C-rich G8Ia post-AGB star by Hrivnak (1995).  Kwok 
et al. (1995) report the possible detection of the 21 $\mu$m emission feature 
and the following near infrared photometry: $K$ = 8.06; $J-H$ = 0.64;
$H-K$ = 0.28. 

\item{90*} The bright (m$_V$ = 7.8) optical counterpart is the A2-type Vega-like 
star SAO 77144, recently described as a binary system in which both components
show a similar $V$ brightness (Sylvester et al. 1996). H$_2$O maser emission 
was not detected by Wouterloot et al. (1993). 

\item{91*} Associated to the bright (m$_V$ $\sim$10.4) F0-type star HD 290380. 
The spectrum shows a bright H$\alpha$ emission over the stellar absorption. 
Recently identified as a possible Herbig Ae/Be star by Torres et al. (1995).


\item{93*} The optical counterpart is a bright A3-type star (m$_V$ $\sim$9.9)
recently identified as a possible T-Tauri star by Torres et al. (1995). 

\item{95*} The bright (m$_V$=10.5) M-type star measured in the near infrared 
is probably not the right counterpart, since it is located around 45" SE  
from the IRAS position. The right optical counterpart might be a 
fainter F-type star, not detected in the near infrared, but closer to the 
original IRAS position. 

\item{96*} Associated to the bright (m$_V$ = 10.0) B8.5Ve-type star HD 
290409. Our optical spectrum shows H$\alpha$ emission over absorption. Also 
identified as a possible Herbig Ae/Be star by Torres et al. (1995).

\item{100*} The optical counterpart is a bright (m$_V$ =8.1) A3e-type star. 
H$_2$O maser emission was not detected by Zuckerman and Lo (1987). The
non-detection was confirmed by Wouterloot et al. (1993).  

\item{102*} This is one of the most heavily obscured OH/IR stars detected
in our survey. Although not detected by us in October 1992, we could measure
the object in the K band well above our detection limit in December 1993, 
confirming the variability of the source. It shows no optical counterpart. 
Blommaert et al. (1993) report the detection of the object in the H and K 
bands on November 1, 1989.  They provide the following 
near infrared data: $K$ = 10.81, $H-K$ = 4.30, $K-L'$ = 5.29, $L'-M$ = 1.17. 
H$_2$O maser emission not detected by Engels and Lewis (1996). 

\item{104*} H$_2$O maser emission not detected by Wouterloot et al. (1993).

\item{106*} PAH's features around 3.3 $\mu$m detected by Geballe and  
van der Veen (1990). The spectrum of the optical counterpart corresponds 
to a reddened C-rich F-type star. Kwok et al. (1995) reported the possible 
detection of the 21 $\mu$m feature in the infrared spectrum of
this object. A detailed analysis of the 
chemical composition of this star can be found in Reddy et al. (1996). 
Previous near infrared measurements are available in Blommaert et al. (1993), 
who report the following values: $K$ = 9.06; $J-H$ = 0.59; $H-K$ = 0.33. 

\item{107*} Close to our detection limit, we could not measure this object in 
the near infrared. However, Campbell et al. (1989) provide the 
following near infrared photometry: $K$ = 10.34; $J-H$ = 1.65; $H-K$ = 1.91;
$K-L$ = 2.43; $L-M$ = 1.86,  typical of heavily obscured young stellar 
objects, and correspond to our region III in the near infrared colour-colour 
diagram. A faint nebulosity is observed in the Palomar prints at the 
IRAS position. H$_2$O maser emission not detected by Wouterloot et al. (1993).

\item{108*} The optical counterpart is a bright (m$_V$ = 9.9) A5 star 
with H$\alpha$ emission (MacConnell 1982). H$_2$O maser emission not 
detected by Wouterloot and Walsmley (1986). 

\item{109*} Faint H$\alpha$ emission over a bright (m$_V$ = 10.5) F8-type 
stellar continuum. Also identified as a possible T-Tauri star by Torres 
et al. (1995).

\item{111*} H$_2$O maser emission detected by Wouterloot et al. (1993).

\item{117*} The bright (m$_V$ $\sim$11) optical counterpart is a 
GI-type star, according to Hrivnak et al. (1994), who also suggest 
that the object might be a C-rich post-AGB star.

\item{119*} Very red optical counterpart (m$_V$ = 13.2) with H$\alpha$ and 
H$\beta$ in emission. Associated to a cometary nebula clearly visible on the 
Palomar prints. Identified as an FU Ori-like star by Torres et al. (1995) 
who assigned an F5 II spectral type. H$_2$O maser emission not detected by 
Wouterloot et al. (1993). 

\item{131*} Probably associated to the galactic HII region BFS 50. The 
bright optical counterpart is an emission line star surrounded by an
extended nebulosity clearly observed in the Palomar prints showing the 
Balmer lines in emission together with many other emision lines, most of 
them attributed to iron. The spectrum looks very similar to those of
other well-known BQ[~] stars, such as HD 51585. Previous near infrared 
photometry in Allen (1974), who reports the following values: $K$ = 7.84;
$H-K$ = 0.81; $K-L$ = 1.54. Radio continuum emission not detected by 
Fich (1993). H$_2$O maser emission not detected by Wouterloot et al. (1993). 

\item{132*} New Herbig-Haro object discovered during this survey. 
A detailed analysis can be found in Manchado et al. (1990). H$_2$O maser 
emission detected by Zuckerman and Lo (1987) at the IRAS position, 
according to the authors. However, the object is misidentified with the 
nearby star BC Tau in this paper and also in the SIMBAD database. 
More recently, H$_2$O maser emission
was not detected by Wouterloot et al. (1993) and nor by Engels and Lewis 
(1996), which makes the first detection uncertain. 

\item{135*} Associated to the dark cloud LDN 1550. The optical counterpart 
shows a very red and faint continuum with no emission lines. Additional near 
infrared photometry available in Campbell et al. (1989), who reported the 
following magnitudes: $K$ = 7.51; $J-H$ = 2.85; $H-K$ = 2.49; $K-L$ = 1.98; 
$L-M$ = 1.35. The object is surrounded by an extended nebulosity clearly 
observable in the Palomar prints. H$_2$O maser emission was not detected by 
Wouterloot et al. (1993)  and Persi et al. (1994)

\item{136*} H$_2$O maser emission not detected by Wouterloot et al. 
(1993) and Persi et al. (1994). 

\item{137*} Associated to the Gemini OB1 molecular cloud complex.
The optical counterpart is a bright (m$_V$ = 9.1) well known A0e-type 
Herbig Ae/Be star. Previous near infrared photometry can be found in 
Allen (1973), with the following magnitudes: $K$ = 6.77; $H-K$ = 0.88; 
$K-L$ = 1.20. H$_2$O maser emission not detected by Persi et al. (1994).

\item{138*} Bright (m$_V$ = 10.2) A-type star with H$\alpha$ emission 
(Merrill \& Burwell 1950). Also identified as a possible 
Herbig Ae/Be star by Gregorio-Hetem et al. (1992). 

\item{140*} The optical counterpart seems to be a faint K-type star with no 
emission lines. 

\item{155*} Clemens and Barvainis (1988) suggest its association to a small 
nearby molecular cloud. The optical counterpart shows H$\alpha$ emission 
over absorption. The star has also recently been identified as a possible 
Herbig Ae/Be star (m$_V$=13.26) by Gregorio-Hetem et al. (1992). Additional
near infrared photometry is available in Blommaert et al. (1993)
who report the following near infrared magnitudes: $K$ = 9.80; $J-H$ 
= 0.88; $H-K$ = 0.89, who correspond to our Region IV in the near infrared 
colour-colour diagram. 

\item{159*} No optical counterpart is found at the IRAS position where
we did not detect any near infrared counterpart above our detection 
limit. In November 1989 we measured a faint (m$_V$ $\sim$13) star 40" 
east and 10" north of the IRAS position which 
might not be the true optical counterpart. The detection of 
CS(2$\rightarrow$1) by Bronfman et al. (1996) indicates that this object 
is probably a heavily obscured ultra-compact HII 
region and not the star observed in the near infrared. H$_2$O maser 
emission was not detected by Wouterloot et al. (1993). 

\item{160*} New planetary nebula discovered in this survey. The central 
star is a WC5 Wolf-Rayet star, with a complex nebular component extended over 
20" and an expansion velocity of 35 km s$^{-1}$. 


\item{161*} The optical counterpart is a faint (m$_V$ = 14.0) and red 
FOI-type star (Hu et al. 1993a) with no emission lines. Hu et al. 
report the following near infrared magnitudes: $K$ = 8.48; $J-H$ = 0.79; 
$H-K$ = 0.44. H$_2$O  maser emission not detected by Likkel (1989) and 
Wouterloot et al. (1993). 

\item{162*} A bright B-type star with broad absorption lines is found 
$\sim$ 20" east of the IRAS position. However, it is still not 
clear whether this is the right counterpart, since the spectrum does not 
correspond to what one would expect from neither a post-AGB star nor a
Herbig Ae/Be star. A deeper near infrared search is needed at the nominal
IRAS position.

\item{163*} The optical counterpart is the bright (m$_V$ = 11.1) 
well-known BQ star HD 51585. The optical spectrum show the Balmer lines in 
emission together with many other emission lines, most of them attributed to
iron.  A recent detailed analysis of the optical spectrum can be found in 
Jaschek et al. (1996). Previous near infrared photometry is available in 
Allen (1974), who reports the following magnitudes: $K$ = 8.11; $H-K$ = 1.15;
$K-L$ = 1.45. 

\item{165*} The object is located in the direction of an OB
association and it is probably one of its members. It shows the 
Balmer lines in emission together with forbidden emission lines
of [N II] and [S II] and is surrounded by a reflection nebula extended over
30". [O III] was detected only in a spectrum taken in 
February 1990, but not in previous spectra in December 1987 and October 1988,
nor in March 1992. A detailed analysis of this object and its spectral 
variations can be  found in Garc\'\i a-Lario et al. (1993). Additional
molecular observations carried out at Pico Veleta in 1993 revealed the 
presence of a narrow extended CO emission around this star suggesting 
that the object is not a post-AGB star but a massive young star. The 
spectral changes observed might be  similar  to 
those usually observed in Luminous Blue Variables. 
 Additional near infrared photometry is available 
in Campbell et al. (1989), who report the following values: $K$ = 9.0;  
$H-K$ = 0.9. H$_2$O maser emission not detected by Wouterloot et al. 
(1988, 1993).

\item{169*} Associated to the galactic HII region Sh 2-287 C. H$_2$O maser 
emission not detected by Felli et al. (1992).

\item{170*} New very low excitation planetary nebula, probably in a very
early stage of evolution, discovered by Menzies and Wolstencroft (1990).
The central star is a WC11 Wolf-Rayet star. A detailed analysis of this 
object can be found in Zijlstra et al. (1991). The infrared spectrum shows 
PAH's features and is one of the few objects known in which both CO and 
OH emission has been found so far, which makes this object specially 
interesting for further studies. The radial velocity shift between the 
CO emission and the OH maser suggests that only one of the OH peaks 
has been detected and that the expansion velocity in OH is then close to
20 km s$^{-1}$. Additional near infrared photometry is available in 
Zijlstra et al. (1991), who report the following magnitudes: $K$ =  8.20;
$J-H$ = 2.01; $H-K$ = 2.00; $K-L$ = 2.87, and in Fouque et al. (1992), who 
also report very similar values: $K$ = 8.25, $H-K$ = 2.00 
(they did not detect the object in the J band).
 

\item{174*} Well known C-rich post-AGB star showing the unidentified 21 
$\mu$m emission feature (Kwok et al. 1989). The spectrum of the optical 
counterpart corresponds to a bright (m$_V$ $\sim$8.3) F5I-type star 
without emission lines (Hrivnak 1995). Hrivnak et al. (1989) report the 
following near infrared measurements (mean of two measurements): $K$ = 
6.65; $J-H$ = 0.26; $H-K$ = $-$0.02. HCN emission detected by Bujarrabal
et al. (1992) and Omont et al. (1993). H$_2$O maser emission not detected 
by Zuckerman and Lo (1987) and Likkel (1989). 

\item{178*} A detailed analysis of this star can be found in 
Manchado et al. (1990). The bright (m$_V$ $\sim$13.0) optical counterpart
shows the Balmer lines in emission with strong  P-Cygni profiles and 
multiple iron lines in emission corresponding to different ionization states. 
Previous near infrared photometry available in Persson and Campbell (1987),
who report the following values: $K$ = 6.30; $J-H$ = 1.39; $H-K$ = 1.34;
$K-L$ = 1.62; $L-M$ = 1.59. H$_2$O maser emission not detected by 
Henning et al. (1992) and Wouterloot et al. (1993). 

\item{181*} Located very close to the Herbig-Haro-like nebulosity GGD 20, 
where H2O maser emission was detected by Gyulbudaghian et al. (1987). 
There are several near infrared sources in the field but the one measured is 
the reddest and the closest to the IRAS position and corresponds to the 
source IRS3 found by Reipurth and Wamsteker (1983) in a previous study of the 
same field. They reported the following near infrared photometry: $K$ = 9.77;
$J-H$ = 0.98; $H-K$ = 0.90. 


\item{182*} The spectrum of the optical counterpart corresponds to a K-type 
star without emission lines. The visual magnitude is m$_V$=12.58, according 
to Torres et al. (1995).

\item{183*} The right optical counterpart is not the bright (m$_V$ = 9.3) 
nearby A-type star HD 59049, as suggested in Paper II, but a fainter 
(m$_V$ $\sim$13) F-type star with a faint H$\alpha$ emission over the stellar 
absorption, which was the star measured in the near infrared, closer to the
nominal IRAS position. Additional near infrared measurements of this star 
are available in Blommaert et al. (1993), who report the following 
magnitudes: $K$ = 9.02; $J-H$ = 0.93; $H-K$ = 1.30. 

\item{186*} Associated to a galactic HII region. The new LRS spectrum obtained 
by Volk et al. (1991) corresponds to a very red object in which PAH features 
might be present. H$_2$O maser emission not detected by Wouterloot et al.
(1988). 

\item{187*} Associated to the dark cloud LDN 1665. The spectrum of the 
optical counterpart shows the Balmer lines in emission over a faint 
red continuum. H$_2$O maser emission not detected by Wouterloot et al. 
(1993).

\item{188*} The optical counterpart is the bright (m$_V$ $\sim$9.8) G5Iab-type 
star AI CMi, for which a detailed analysis can be found in Luck and Bond
(1989), who classified this star as a low mass supergiant variable
and found a faint H$\alpha$ emission over absorption. H$_2$O
maser emission has recently been detected by Engels and Lewis (1996). HCN 
emission was not detected by Omont et al. (1993).

\item{189*} H$_2$O maser emission not detected by Wouterloot et al. (1993).

\item{191*} This well known bipolar proto-planetary reflection nebula is 
one of the few transition objects in which both CO and OH have been detected. 
The bright (m$_V$ $\sim$9.5) M6-type central star seems to be variable 
with a period of around 700 days. Both the period and the amplitude 
of the variability seem to be increasing with time (Kastner et al. 1992). 
The object shows a very rich chemistry (Morris et al. 1987; 
Bujarrabal et al. 1994) and a high velocity outflow, spanning a range of 
more than 100 km s$^{-1}$. No radio continuum emission was detected by 
Knapp et al. (1995). A detailed study of the near infrared 
behaviour of this object can be found in Kastner et al. (1992). Additional 
near infrared measurements are available in Lepine et al. 
(1995) who report the following values: $K$ = 5.41; $J-H$ = 1.42; $H-K$ 
= 1.20; $K-L'$ = 2.27; $L-M$ = 1.01. 

\item{192*} The optical counterpart is a K-type supergiant star without 
emission lines, also classified as G-K I by Hrivnak et al. (1994), from 
the analysis of the near infrared spectrum.

\item{197*} The optical counterpart is a faint star of undetermined spectral 
type with a weak H$\alpha$ emission overimposed on the stellar continuum. The 
object is not associated to any known star forming region. Previous
near infrared measurements are available in Blommaert et al. (1993), who 
report the following values: $K$ = 12.21; $J-H$ = 0.77; $H-K$ = 0.61. 

\item{200*} Late G-type star with no emission lines. 

\item{201*} The spectrum of the optical counterpart corresponds to a 
G-type star with no emission lines. A visual magnitude of m$_V$ = 15.32 is 
assigned by Hu et al. (1993a), who also report the following near infrared 
magnitudes: $K$ = 11.39; $J-H$ = 0.63; $H-K$ = 0.23. Radio continuum 
emission not detected by van de Steene and Pottasch (1993). H$_2$O maser 
emission not detected by Wouterloot et al. (1993). 


\item{202*} Bright (m$_V$ $\sim$11.5) F5Iae-type star, according to 
Hrivnak (1995), who also reports the presence of C-rich features in the
optical spectrum. It shows a strong Balmer emission  together with many 
other weak emission lines, most of them attributed to iron at different 
ionization states (Manchado et al. 1989b; Slijkhuis et al. 1991).  
Additional near infrared data are available in Hu et al. (1993a),
who report the following photometry (mean of two measurements): $K$ =
5.55; 
$J-H$ = 1.15; $H-K$ = 1.30; $K-L$ = 2.09; $L-M$ = 0.65, and in Lepine et al. 
(1995), who found the object with: $K$ = 5.71; $J-H$ = 1.11; 
$H-K$ = 1.31; $K-L'$ = 2.21; $L'-M$ = 0.68. The multiple peaks detected in 
OH by te Lintel Hekkert et al. (1991) span a wide range of velocities 
($\sim$100 km s$^{-1}$) with center at v$_{LSR}$ = +46.7 km s$^{-1}$. 
H$_2$O maser emission was not detected by Likkel (1989) and Wouterloot et 
al. (1993). 

\item{204*} Bright F-type star (m$_V$ $\sim$10) without emission lines.

\item{205*} The spectrum of the optical counterpart found corresponds to a
bright G-type star with H$\alpha$ emission. The visual magnitude is 
m$_V$ $\sim$10.74, according to Gregorio-Hetem et al. (1992), who identify 
the same IRAS source as a T-Tauri star with an F-G spectral type. However,
the object is not located in the direction of any known star forming 
region. 

\item{206*} Late G-type star with no emission lines. Confirmed as the 
right counterpart by the near infrared photometry. Radio continuum emission not 
detected by van de Steene and Pottasch (1993).

\item{209*} Bright (m$_V$ $\sim$8.9) F6Ib-type star. Our high resolution 
spectrum shows the presence of a weak H$\alpha$ emission over the stellar 
continuum. 

\item{210*} Identified as a possible Vega-like star by Walker and
Wolstencroft (1988). A detailed analysis can be found in Skinner et al. 
(1995). Additional near infrared photometry is available in 
Miroshnichenko et al. (1996). They report the following magnitudes
(mean of two measurements): $K$ =  6.63; $J-H$ = 0.57; $H-K$ = 0.14.  
H$_2$O maser emission not detected by Zuckerman and Lo (1987).

\item{212*} Bright F-type star (m$_V$ $\sim$11) with H$\alpha$ clearly in 
emission over the photospheric absorption. 

\item{213*} Probably associated to a molecular cloud detected in 
CO by Wouterloot and Brand (1989) in which a high density of IRAS sources 
with colours usually observed in young stellar objects are found.

\item{214*} M-type star, confirmed as the right counterpart by our
near infrared observations. 

\item{217*} The optical counterpart is a late K-type star without 
emission lines. 

\item{218*} Previously identified in the near infrared, the optical 
counterpart is a G-type star with no H$\alpha$ emission. Radio continuum
emission not detected by van de Steene and Pottasch (1993). 


\item{222*} No optical counterpart found at the IRAS position. Nothing 
was detected in a long blind exposure taken in the optical range. Although 
the faint near infrared source measured was located not too far from the 
nominal IRAS position, this could be a field star and not the right 
counterpart. It was not detected in the near infrared by Blommaert et 
al. (1993). According to Volk et al. (1993), this object belongs to a 
small group of objects with a very red and featureless LRS spectrum, 
identified as extremely reddened C-rich post-AGB stars, which might only be
detectable in the mid-infrared, and are probably below our detection 
limit in the near infrared. 

\item{223*} New planetary nebula with a ring-like nebular component 
extended over 12". The central star is visible on a CCD image taken 
in the V filter at the ESO 3.60 m telescope as an extremely faint (m$_V$ 
$\sim$ 20) object in the center of the ring. The excitation class is low. 
The [O III] nebular emission lines at 4959 and 5007 \AA~ are clearly visible in 
the spectrum, together with the Balmer lines of hydrogen. Much fainter, 
the [N II] lines at 6548 and 6584 \AA~ are also present. The first near 
infrared measurement obtained in May 1990 might have been contaminated by a 
field star. Radio continuum emission extended over 12".6 detected by 
Whiteoak (1992) and by van de Steene and Pottasch (1993). The narrow CO 
emission detected in the direction of this object is probably not related 
with the IRAS source.

\item{228*} Several faint optical counterparts around the IRAS 
position were observed in the optical range. None of them showed
H$\alpha$ emission or any other remarkable feature. A more recent 
blind spectrum centered at the IRAS position revealed the presence of
an extremely faint and red optical counterpart which might be the 
right counterpart observed in the near infrared. Additional near infrared
photometry of this second source 
is available in Blommaert et al. (1993), who did not detect 
the object in the J band and report the following magnitudes: $K$ = 10.79;
$H-K$ = 1.33; $K-L'$ =4.40, confirming the variability of the source.


\item{230*} Located in what it seems to be a dark cloud. The object shows 
extremely reddened near infrared colours but no strong variations in 
brightness, as suggested by the comparison of our data with those taken 
by Gaylard and Whitelock (1988), Persson and Campbell (1988) and Liseau et
al. (1992), all them reporting values very similar to ours.  
Radio continuum emission was not detected by van de Steene and Pottasch (1993). 

\item{236*} New planetary nebula of intermediate excitation class. The 
extension is about 10" in H$\alpha$. Radio contiuum emission extended over 
only 3".1 was detected by van de Steene and Pottasch (1993). 

\item{239*} A red object was detected in the near infrared close to the 
IRAS position which might be the right counterpart. In the optical range,
we did not find any counterpart or this was very faint. It belongs to the 
small group of IRAS sources with a very red and featureless LRS spectrum, 
identified as possible extremely reddened C-rich post-AGB stars by Volk et 
al. (1993). However, it was not detected in CO by Loup et al. (1990). 
On the other hand, the far infrared IRAS colours and the high variability 
index are typical of a variable OH/IR star. 

\item{241*} According to Hu et al. (1993a), the optical counterpart is 
not a relatively bright G-type star with no emission lines (as derived from 
our optical spectrum) found close to the IRAS position and not detected by us
in the near infrared, but a much fainter (m$_V$ = 18.31) star, for which 
they report the following near infrared data (mean of two measurements), 
slightly below our  detection limit: $K$ = 11.79; $J-H$ = 1.15; $H-K$ = 
1.41; $K-L$ = 2.14, which corresponds to the limit between our regions III 
and IV in the near infrared two-colour diagram. 


\item{248*} F-type star with no emission lines. Although classified as a 
post-AGB star, it is located very close to a giant HII region. So, we cannot 
rule out the possibility of this IRAS source being a young stellar object 
until a more detailed analysis of the spectrum of the star is carried out.

\item{254*} New compact planetary nebula detected in this survey. Radio 
continuum emission was detected by van de Steene and Pottasch (1993) with an 
extension of only 2".0. 

\item{255*} Not detected by us in the near infrared. The optical counterpart 
was initially thought to be a bright (m$_V$ $\sim$12) G-type star with 
no emission lines, very close to the IRAS position. However, Hu et al. (1993a) 
classified the same counterpart as G9 III and suggested that this might not 
be the right one, since the IRAS source was detected very bright in the 
N-band 7" away from the position of this star with very red infrared 
colours ($K$ $\sim$ 13.8, while $M$ $\sim$ 6.6), which do not correspond at 
all to the brightness of the star observed in the optical. This new 
identification is consistent with the red and featureless LRS spectrum 
reported by Volk et al. (1993), usually associated to extremely reddened
C-rich post-AGB stars.

\item{260*} Extremely reddened C-star with H$\alpha$ in emission. 
Also observed in the near infrared by Fouque et al. (1992), who report the
following near infrared measurements: $K$ = 3.39; $J-H$ = 1.41; $H-K$ = 1.08,
confirming the variability of the source. H$_2$O maser emission not detected 
by Deguchi et al. (1989). 

\item{263*} The optical counterpart seems to be a very faint (m$_V$ = 19.37) 
star (Hu et al. 1993a), from which compact radio continuum emission ($\le$ 3".4) 
has recently been detected (van de Steene \& Pottasch 1993). The optical 
spectrum shows the presence of H$\alpha$ in emission together with the 
forbidden emission lines of [N II]. Additional near infrared photometry can
be found in Hu et al. (1993a), who report the following values (mean of two 
measurements): $K$ = 10.55; $J-H$ = 1.25; $H-K$ = 1.11. 

\item{268*} New very low excitation planetary nebula, with only the 
Balmer lines in emission and forbidden lines of [N II] and [S II] found 
in this survey. Radio continuum emission detected with an extension $\le$ 6".1 
by van de Steene and Pottasch (1993). 

\item{270*} Very low excitation highly collimated bipolar planetary nebula 
probably in a very early evolutionary stage. A thick equatorial disk seems 
to be collimating the outflow, which extends over 20" x 10". The lobes are 
predominantly neutral and reflect the very reddened B1-type continuum 
of the central star and a bright H$\alpha$ and [N II] emission. The 
inner nebular region shows, in addition, multiple emission lines of iron 
at different ionization states and a possible very faint [O III] emission. 
Allen and Glass (1975) report the following near infrared magnitudes: $K$ = 
9.0; $H$ = 9.8.

\item{271*} This is one of the objects identified by Volk et al. (1993) 
as a possible extremely reddened C-rich post-AGB star, according to its
red and featureless LRS spectrum. We did not find any optical counterpart
at the IRAS position and nor did Hu et al. (1993a), who detected the object 
in the N-band and report a value of $M$ = 6.2 and the tentative detection of 
the IRAS source in the $K$ band with a magnitude around 15. No radio 
continuum emission was detected by van de Steene and Pottasch (1993). 

\item{272*} This object is a well known bipolar proto-planetary nebula in 
a very early stage of evolution (see e.g. Allen et al. 1980). The emission 
coming from the lobes is reflection from the A2Iabe-type central star, 
probably in the post-AGB phase, still evolving toward higher temperatures in 
its way to become hot enough to ionize the surrounding material. Strong 
PAH's features have been detected in the mid-infrared (Cohen et al. 1989), 
suggesting a C-rich nature. Additional near infrared photometry is 
available in  Lepine et al. (1995), who found: $K$ = 7.10; $J-H$ = 1.08; 
$H-K$ = 0.78; $K-L'$ = 2.19; $L'-M$ = 1.00, from measurements taken 
in January 1992. The detection of both CO and OH makes this object specially 
interesting for further studies. 

\item{275*} Bright (m$_V$ = 8.73) G5I-type post-AGB star with H$\alpha$ 
emission and faint nebular emission lines of [N II] and [S II] over the 
stellar continuum. A detailed analysis of this star can be found in 
Garc\'\i a-Lario et al. (1994). Additional near infrared data
are available in Hrivnak et al. (1989), who report the following values:
$K$ = 3.02; $J-H$ = 1.12; $H-K$ = 0.47; $K-L$ = 0.44. 

\item{277*} Intermediate spectral type star with a very reddened 
continuum and a strong H$\alpha$ emission. Radio continuum emission
not detected by van de Steene and Pottasch (1993).

\item{280*} Faint stellar continuum on which the Balmer lines are clearly 
in emission. Although no nebular emission lines are detected, the far infrared
colours undoubtfully correspond to an evolved object. Thus, we consider this
IRAS source as a new proto-planetary nebula. Radio continuum emission 
not detected by van de Steene and Pottasch (1993). 

\item{289*} The optical counterpart is a bright possibly fading 
(m$_V$ $\sim$ 12) variable star recently identified as a new member of 
the small group of galactic 
Luminous Blue Variables (LBV's) by Hu et al. (1990). The optical spectrum 
shows a B-type stellar continuum on which multiple emission lines of iron 
at different ionization states are observed, together with strong 
Balmer emission and some nebular emission lines. The low excitation nebular 
component is slightly extended and includes forbidden emission lines 
of [N II], [S II] and [O I]. Additional near infrared photometry is 
available in Hu et al. (1990), who found the object variable in the near 
infrared and report the following values: $K$ = 6.46; $J-H$ = 0.77; 
$H-K$ = 0.48, from data taken in December 1984 and a fainter $K$ = 6.98; 
$J-H$ = 0.87; $H-K$ = 0.52, in March 1989.

\item{294*} The bright (m$_V$ = 8.89) K5V-type star is a member of a 
binary system in which the companion seems to be a fainter G-type star
separated just 0".2. Classified as T-Tauri star by Gregorio-Hetem et al. 
(1992) and as a possible Vega-like star by Sylvester et al. (1994). 
The brighter component shows a very weak Halpha emission over absorption and
a remarkably strong lithium line at 6707.8 \AA, which is used by Fekel and 
Bopp (1993) to identify the object as a young cromospherically active star. 

\item{300*} Bright A9V-type star (m$_V$ $\sim$7.9) with a very broad H$\alpha$ 
emission over the stellar absorption. Fouque et al. (1992) report the
following near infrared measurements: $K$ = 5.80; $J-H$ = 0.55; $H-K$ = 0.78. 

\item{302*} Bright B9Vne-type star (m$_V$ $\sim$6.77) with strong H$\alpha$ 
emission over the stellar absorption. Fouque et al. (1992) report the 
following near infrared measurements: $K$ = 5.07; $J-H$ = 0.60; $H-K$ = 0.68. 
A detailed photometric and spectroscopic study of this star can be found
in Hu et al. (1989), who also obtained additional near infrared data, 
reporting the following values: $K$ = 5.09; $J-H$ = 0.58; $H-K$ = 0.66;
$K-L$ = 1.07; $L-M$ = 0.27. 

\item{303*} The faint near infrared counterpart measured was found very 
close to the nominal IRAS position. The probable optical counterpart 
is a very faint M-type star. The same near infrared counterpart 
was observed by Hu et al. (1993a), who did not find any optical counterpart
but report very similar near infrared colours: $K$ = 11.41; $J-H$ = 1.13; 
$H-K$ = 0.46; $K-L$ = 2.3. Radio continuum emission was not detected by van de 
Steene and Pottasch (1993).

\item{307*} The optical counterpart is a bright (m$_V$ $\sim$12) G-type star 
with H$\alpha$ emission, not measured by Hu et al. (1993a), as they thought 
it was not the right counterpart. However, the presence of H$\alpha$ 
emission confirms that our identification is right.
Radio continuum emission not detected by van de Steene and Pottasch (1993).

\item{308*} A very reddened G-type star is located at the nominal
IRAS position. No other bright near infrared source was found in our raster
scan in the $K$ band. Radio continuum emission was not detected by 
van de Steene and Pottasch (1993).

\item{309*} Although the IRAS variability index is very low, our 
near infrared photometric observations, combined with those taken 
by Gaylard et al. (1989) in March 1987 and Lepine et al. (1995) in March 1992
confirm that the object is strongly variable in the  near infrared.
We estimate a period close to 1200 days from the data available so far.
The objects shows no optical counterpart at all and is so red that it 
has never been detected in the J band. The $H-K$ and $K-L'$ colours are 
both larger than 6 magnitudes and the brightness in the $K$ band shows 
variations of at least 3.8 magnitudes (from $K$ = 7.84 in January 1992 to 
$K$ = 11.64 in May 1990). H$_2$O maser emission not detected by Deguchi et 
al. (1989). 

\item{310*} The very low galactic latitude and the proximity of an OB 
association in Crux open the possibility of this star being a young stellar 
object, although the IRAS colours suggest that the object is an evolved star. 

\item{312*} The optical counterpart is relatively bright (m$_V$ = 12.90) 
and has been identified as a T-Tauri star by Gregorio-Hetem et al. (1992). 
Although located in the overlapping region of the IRAS two-colour diagram 
between young stellar objects and evolved stars and at a high galactic 
latitude (b$\sim$ $-$17$\deg$), it might be connected to the nearby
Chameleon star forming region. Radio continuum emission not detected by van 
de Steene and Pottasch (1993). 

\item{315*} This is one of the objects with a red and featureless LRS 
spectrum identified by Volk et al. (1993) a as possible heavily obscured 
C-rich post-AGB star. Although we did not find any near infrared
counterpart at the IRAS position, Hu et al. (1993a) were able to detect and 
measure a bright emission in the $M$ band ($M$ = 6.2) and close to their 
detection limit in the $L$ band ($L$ $\sim$10) at the same position where they 
found a very bright N-band source, supporting the identification of the object
as a very red source with no optical counterpart. 


\item{318*} This is a well known bright (m$_V$ $\sim$9.7) RV Tauri variable 
with a period of 65 days. The spectral type is also found to vary from A7Ip
to K3Ip, sometimes showing the Balmer lines strongly in emission. In 
our high resolution spectrum, taken in February 1990, we detected a faint 
H$\alpha$ emission over a G-type stellar continuum. In previous near infrared
measurements the object was found more than 1 magnitude brighter, but no
photometric period has yet been determined in the near infrared. 
Elias (1978) reports the following values: $K$ = 5.01; $J-H$ 
= 0.73; $H-K$ = 0.58, and Lloyd-Evans (1985) found: $K$ = 5.03; $J-H$ = 
0.70; $H-K$ = 0.64. A detailed analysis of the chemical composition of this
star can be found in Luck and Bond (1989).  H$_2$O maser emission was 
not detected by Deguchi et al. (1989). 

\item{320*} Two possible counterparts were observed in the optical, 
but none of them show remarkable features. One of them, closer 
to the IRAS position, was measured in the near infrared, but it might not 
be the right counterpart of the IRAS source, since the colours observed 
do not correspond to a very reddened object, as one would expected for an  
object showing OH maser emission and a high IRAS variability index. 
We suggest a more likely identification as a variable OH/IR star 
with no optical counterpart.  

\item{321*} The optical counterpart is a bright (m$_V$ = 9.3) F2-type star 
with H$\alpha$ in emission over the stellar continuum. Additional near infrared
photometry is available in Hrivnak et al. (1989), who report the following 
magnitudes (mean of two measurements): $K$ = 8.14; $J-H$ = 0.20; $H-K$ = 0.10;
$K-L$ = 0.11, and in Fouque et al. (1992), who give:
$K$ = 8.14; $J-H$ = 0.17; $H-K$ = 0.13; $K-L$ = 0.17; $L-M$ = 0.77.

\item{333*} Although the IRAS variability index is low, the strong
variations found in our near infrared photometry, combined with 
the data taken in this spectral range by Hu et al. (1993a) confirms 
that this is a very long period variable OH/IR star. Hu et al. (1993a) 
obtained photometric measurements at two different epochs of the same star 
in the $KLM$ bands reporting the following values: $K$ = 11.64; $K-L$ = 6.37; 
$L-M$ = 1.07, in March 1990, and $K$ = 10.60; $K-L$ = 6.11; $L-M$ = 1.58, in 
April 1990, and also found an extremely faint and red optical counterpart
with m$_R$ = 17.90. The combination of all the data available in the near 
infrared suggests a period larger than 1000 days.  

\item{334*} The optical counterpart might be a reddened F-type star 
with no peculiar features located close to the IRAS position. 
No other near infrared source was found in our
raster scan in the $K$ band. Radio continuum emission 
was not detected by van de Steene and Pottasch (1993).

\item{342*} The positions of the optical and near infrared counterparts 
exactly coincide with the IRAS position. The optical spectrum corresponds 
to a late G-type star without emission lines. 

\item{345*} The most probable optical counterpart is a bright and 
considerably reddened late F-type star (m$_V$ $\sim$12.5) with no 
emission lines, located very close to the IRAS position. Radio  continuum 
emission not detected by van de Steene and Pottasch (1993). 

\item{347*} Bright F-type star (m$_V$ $\sim$13) with H$\alpha$ emission. 
Radio continuum emission not detected by van de Steene and Pottasch (1993).

\item{348*} Bright B-type star (m$_V$ $\sim$10.7) with the Balmer lines 
in emission (spectrum available in Manchado et al. 1989b). Fouque et al. 
(1992) report additional near infrared measurements: $K$ = 9.42; $J-H$ 
= 0.17; $H-K$ = 0.17, slightly brighter than ours. 

\item{353*} The optical counterpart seems to be a red G-type star with no 
emission lines close to the IRAS position. Radio continuum emission not 
detected by van de Steene and Pottasch (1993).

\item{361*} Observed twice in the near infrared at two different epochs
separated by 2 years. Although the variations found are small and the 
IRAS variability index is low, the position in the IRAS two-colour diagram
corresponds to the usual location of variable OH/IR stars. Given the rarity 
of truly non-variable OH/IR stars, we prefer to keep the classification of 
this star as non-variable as just tentative. 

\item{362*} New very low excitation planetary nebula discovered in this 
survey. The optical counterpart shows the Balmer lines in emission 
together with the forbidden emission lines of [N II] around H$\alpha$ 
over a faint stellar continuum. Radio emission was not detected by van 
de Steene and Pottasch (1993). We could only detect the object in the 
$K$ band.

\item{363*} This object shows an extremely red LRS spectrum (Volk et al. 1991) 
and also very red near infrared colours. Additional near infrared measurements
are available in van der Veen et al. (1989), who report very similar values:
$K$ = 9.07; $J-H$ = 1.77; $H-K$ = 1.50; $K-L'$ = 2.45; $L'-M$ = 1.32.   
Radio continuum emission not detected by van de Steene and Pottasch (1993). 
Never observed in the optical range.

\item{368*} The near infrared counterpart measured is located 20" 
north and 45" east of the IRAS position. Although far from the nominal 
IRAS position the red near infrared colours suggest that this is the 
right counterpart. Nothing is visible at that position in the optical range. 

\item{374*} This is a poorly known young and dusty planetary nebula for 
which the possible detection of a faint OH maser emission has been 
reported by Zijlstra et al. (1989). Additional near infrared measurements 
are available in Persi et al. (1987), who report the following magnitudes:
$K$ = 7.70; $J-H$ = 1.23; $H-K$ = 0.78, more than one magnitude brighter, but 
with similar colours. Our optical spectrum confirms that the object is 
a genuine planetary nebula. The LRS spectrum is completely dominated by 
dust emission, not showing any nebular emission line (Volk \& Cohen 1990).

\item{375*} Observed at two different epochs in the near infrared separated
two years with the same photometric magnitudes and associated to a low 
IRAS variability index, it has been classified as a candidate for being a 
non-variable OH/IR star. However, a long-term monitoring is needed to check 
this identification.

\item{377*} New planetary nebula discovered in this survey, confirmed as 
such through low resolution optical spectroscopy. Probably 
associated to the radio continuum emission detected 18" east and 
11"  south of the IRAS position, extended over less than 4".5, by van de 
Steene and Pottasch (1993). It is important to note that we may have 
measured the wrong near infrared counterpart since, according to 
Hu et al. (1993a), the bright near infrared source that we (and they) have 
measured is a very red strongly variable M-type star (m$_R$ = 19.4 in 
March 1989) 16" west and 8" north of the nominal IRAS position.
However, contrary to what they claim, this bright near infrared source
seems to be not variable at all, since observations at three different epochs
(their measurements in March 1989 and April 1990 and our measurements in 
March 1992) do not show any significant variation. 

\item{381*} New planetary nebula discovered in this survey. The optical 
spectrum shows the presence of the Balmer lines in emission and the 
characteristic nebular forbidden emission lines usually found in planetary 
nebulae over a faint and red continuum. The line ratios correspond to an 
intermediate excitation class planetary nebula. The nebular component 
extends over 6" and shows a bipolar morphology. Radio continuum emission has 
also been detected by van de Steene and Pottasch (1993). 

\item{382*} Although the OH maser detection is tentative, the high IRAS
variability index, the extremely reddened near infrared colours and the 
characteristic location in the IRAS two-colour diagram clearly indicate 
that the object should be classified as a variable OH/IR star.

\item{385*} The optical counterpart is a bright (m$_V$ = 10.89) 
B-type star with the Balmer lines strongly in emission. Although we have 
not detected the presence of forbidden emission lines, the position 
in the IRAS two-colour diagram corresponds to the region where only evolved 
objects are located. A low resolution optical spectrum is available 
in Manchado et al. (1989b). The detection of broad CO emission corresponding 
to an expansion velocity of $\sim$ 15 km s$^{-1}$ confirms its 
identification as a transition object, rapidly evolving towards the 
planetary nebula phase. 

\item{398*} The LRS type, the far infrared colours and the high IRAS 
variability index undoubtfully suggest that the object is a 
variable OH/IR star. However, the object has only been measured once 
in the near infrared and more observations are needed to confirm this 
variability.

\item{403*} The red optical counterpart shows a nebular appearance and 
the Balmer lines in emission over a very faint stellar continuum. 
Since its location in the IRAS two-colour diagram undoubtfully corresponds to 
an evolved object, we have classified this IRAS source tentatively as a 
new very low excitation planetary nebula, although we did not detect the 
presence of forbidden emission lines in our low resolution optical
spectrum, and it might still be considered as a transition object. 
Radio continuum emission was not detected by van de Steene and Pottasch 
(1993).  Not detected in CS (2 $\rightarrow$ 1) by Bronfman et al. (1996). 

\item{405*} The near infrared counterpart exactly coincides with the IRAS 
position. However, we did not find any optical counterpart in the ESO
prints and nothing was detected after a blind exposure of 30 minutes taken at 
the 1.52 m ESO telescope. Strong radio continuum emission has been 
detected by van de Steene and Pottasch (1993) 22" east and 7" 
south of the IRAS position. This object could be either a compact 
H II region or a heavily obscured planetary nebula. More observations 
are needed to reach a definitive conclusion. 

\item{409*} New hydrogen-deficient planetary nebula discovered in this 
survey. The central star is a WC star, while the nebular component extends 
over 10". The physical conditions, chemical abundances and other 
characteristics are discussed in Manchado et al. (1989c). Radio continuum 
emission not detected by van de Steene and Pottasch (1993). 

\item{424*} There is an extreme M-type star very close to the IRAS 
position, which must be the right optical counterpart. 


\item{426*} The optical counterpart is a very late M-type star
(later than M7), according to Le Bertre (1993). He has monitored this 
IRAS source in the near infrared for several years and conclude that the 
star is probably an M-type supergiant, since the variations found 
are irregular and not as large as expected from a late AGB star. Additional 
near infrared measurements were previously reported by Epchtein et 
al. (1987), Gaylard et al. (1989) and Nyman et al. (1993), who also provide 
very similar photometric measurements. However, we suggest that 
the IRAS source is not a supergiant but a non-variable OH/IR star, 
as derived from the presence of OH maser emission at 1612 MHz and the far 
infrared colours, which  undoubtfully correspond to an evolved object. 
The object shows a continuous progressive fading in the near infrared 
since 1986 and is now 0.4 magnitudes fainter in the K band while the 
colours have not changed at all so far. The detection of SiO maser emission at 
a variable velocity was reported by Le Bertre and Nyman (1990). 
H$_2$O maser emission not detected by Deguchi et al. (1989). 

\item{435*} Additional near infrared HKL photometry is available in 
Gaylard and Whitelock (1988), who report redder colours and the following 
magnitudes: $K$ = 10.08; $H-K$ = 1.64; $K-L$ = 3.64, from observations 
taken in October 1987, not detecting the object in the J band. Additional
observations would be needed to confirm that we observed the same near 
infrared counterpart.

\item{440*} We did not find any optical counterpart for this IRAS 
source in the ESO prints. Henning et al. (1996) report the possible 
presence of the 21 $\mu$m feature for this star in its LRS spectrum.
Radio continuum emission not detected by van de Steene and Pottasch (1993).

\item{441*} The optical counterpart is a bright (m$_V$ = 10.3) G5Ie star
classified by different authors either as a Vega-like star 
(Sylvester et al. 1994)  or as a T-Tauri (Downes \& Keyes 1988).  
Our high resolution spectrum shows the presence of a broad H$\alpha$ emission
overimposed on the stellar continnuum.  The far infrared colours and near 
infrared photometry are also against the classification of the star as a 
post-AGB star. 

\item{447*} Not detected in the near infrared. It might be too red to be 
detected in the $K$ band above our detection limit. The detection of OH maser
emission and the high IRAS variability index suggest its classification as 
a variable OH/IR star. Radio continuum emission not detected by van 
de Steene and Pottasch (1993).

\item{453*} The optical counterpart is a relatively bright (m$_V$ = 11.77)
K-type T-Tauri star with a variable and very weak H$\alpha$ emission, according to 
Gregorio-Hetem et al. (1992). 

\item{456*}  New high excitation planetary nebula discovered in this 
survey extended over 8" in the light of H$\alpha$. Radio continuum 
emission has also been detected by van de Steene and Pottasch (1993)
extended over 6".5.

\item{480*} The spectrum of the optical counterpart is dominated by the 
presence of strong molecular bands usually associated to  late M-type stars. 
The presence of high velocity features in both 
the H$_2$O maser emission and in OH (Zuckerman \& Lo 1987; Likkel \&
Morris 1988; te Lintel Hekkert et al. 1988; Likkel et al. 1992) 
suggest a bipolar structure and a high velocity outflow, larger 
than 50 km s$^{-1}$. The highly variable in intensity H$_2$O emission covers 
a wide velocity range, from $-$89 km s$^{-1}$ up to +172 km s$^{-1}$, while in 
OH it is restricted to the range between $-$11 and  +105 km s$^{-1}$. 
Additional near infrared photometry is available in van der Veen 
et al. (1989), who provide the following magnitudes: $K$ = 9.61;
$J-H$ = 1.42; $H-K$ = 1.14; $K-L'$ = 1.74; $L'-M$ = 0.66, from measurements 
obtained in July 1986. Fouque et al. (1992), however, found the object  
significantly brighter and bluer: $K$ = 8.02;  $J-H$ = 0.99; $H-K$ = 0.69,  
in June 1990, with very similar colours to those we measured 
just one month before, in May 1990. It has 
been suggested, according to the blue colours observed in the 
optical range, that the object might be a binary system in which one of 
the components is a much hotter early-type star (Guertler et al. 1996). 

\item{498*} The optical counterpart seems to be a late G-type star with 
no emission lines classified as G9III by Hu et al. (1993a), who also 
report the presence of a compact reflection nebula surrounding this IRAS 
source and the following near infrared data: $K$ = 10.32; $J-H$ = 0.73; 
$H-K$ = 0.16; $K-L$ = 0.7, and a visual magnitude m$_V$ = 13.32 in March 1989. 

\item{500*} The spectrum of the optical counterpart is an F5-type star 
with H$\alpha$ emission over the stellar absorption continuum. Hu et al. 
(1993a) also classified the same object as a relatively bright (m$_V$ = 13.20) 
F5I star with H$\alpha$ filled in and report the detection of a reflection 
nebula extended over 12" surrounding the central star. They also report 
the following near infrared measurements: $K$ = 9.28; $J-H$ = 0.89; 
$H-K$ = 1.65; $K-L$ = 3.29; $L-M$ = 1.31, in March 1989, consistent with our   
measurements and with additional near infrared data available in 
Fouque et al. (1992), who gives: $K$ = 9.33; $H-K$ = 1.66. 
Radio continuum emission not detected 
by Zijlstra et al. (1989). H$_2$O maser emission not detected by Likkel (1989).

\item{507*} New very low excitation planetary nebula discovered in this
survey. Although it only shows H$\alpha$ emission and the possible presence
of faint [N II] lines at 6548 and 6584 \AA~ over a very faint continuum,
the infrared colours and the extended nebular appearance (around 10", with 
an elliptical morphology) confirm this classification. Additional near 
infrared data can be found in van der Veen et al. (1989), who report the 
following values: $K$ = 8.17; $J-H$ = 1.00; $H-K$ = 0.76; $K-L'$ = 1.41;
$L'-M$ = 1.09, from photometry obtained in July 1986.  Radio continuum 
emission was not detected by van de Steene and Pottasch (1993).

\item{509*} The far infrared colours suggest that the object is a 
post-AGB star surrounded by a very cold dust shell. On the other hand, 
the object seems to be still heavily obscured, according to the near infrared 
colours found. Measurements taken at two different epochs separated by two 
years suggest that the object might be variable. Radio continuum emission 
was not detected by van de Steene and Pottasch (1993).

\item{514*} Not detected in the near infrared, the object is probably too red
to be detected above our detection limit in the $K$ band. Although the 
IRAS variability is low, its position in the IRAS two-colour diagram does not
indicate the presence of a detached dust shell. Thus, its classification as
non-variable OH/IR star is just tentative. 
Radio continuum emission not detected by Zijlstra et al. (1989).

\item{515*} A bright near infrared source has been found close to the 
nominal IRAS position which might be the right counterpart. The 
object has been detected in OH as a double-peaked maser, but the IRAS 
variability index is very low and the far infrared colours are 
characteristic of post-AGB stars with detached cold dust shells. 
Thus, we have classified the object as a non-variable OH/IR star, although
a long-term monitoring in the near infrared is needed to confirm
this identification.

\item{519*} The non-detection of OH maser emission from this IRAS source 
is puzzling, since its position in the IRAS two-colour diagram and the 
high IRAS variability index correspond to a variable OH/IR star. The LRS 
spectrum, however, obtained by Volk et al. (1991) show an unusual red 
continuum with no indication of silicate absorption at 9.7 $\mu$m,
which might be indicative of a C-rich nature.  


\item{522*} The optical counterpart is a bright (m$_V$ = 9.5) B-type
star showing a strong H$\alpha$ emission with a deep P-Cygni profile. 
In addition, very faint nebular emission lines of [N II] and [S II] are 
clearly visible in our high resolution spectrum. The far infrared
colours undoubtfully correspond to an evolved star surrounded by a very
cold dust shell, which supports our classification as an incipient very low 
excitation planetary nebula. 


\item{525*} New very low excitation compact planetary nebula discovered during 
this survey. Although it only shows the Balmer lines in emission, and faint
forbidden emission lines of [N II] at 6548 and 6584 \AA~ and [O I] at 
6300 \AA, the far infrared colours are those expected for an evolved
object. The underlying continuum corresponds to a bright (m$_V$ $\sim$12) 
B-type star. Radio continuum emission was detected 
by Ratag and Pottasch (1991). The IUE spectra taken in 
August 1993 correspond to a colder star (may be A-type), which makes this 
object specially interesting for further studies, since it may be 
rapidly evolving in the H-R diagram towards hotter effective temperatures. 

\item{527*} The near infrared counterpart found was also detected in August 
1986 by van der Veen et al. (1989) as a bright and red source in the near 
infrared, who report the following magnitudes: $K$ = 9.22; $J-H$ = 1.50; 
$H-K$ = 0.46; $K-L'$ = 0.32; $L'-M$ = 0.55. It seems that this is the same 
near infrared counterpart measured by Epchtein and
Nguyen-Q-Rieu (1982) in February 1981, who report very similar values:
$K$ = 9.12; $J-H$ = 1.42; $H-K$ = 0.57, although they suggest that the 
object is a very red field star and not the right counterpart. The 
detection of the characteristic double-peaked OH maser emission, the low 
IRAS variability index and the absence of significant variations in the 
near infrared suggest the identification of the object as a 
non-variable OH/IR star. Radio continuum emission was not detected by 
van de Steene and Pottasch (1993).

\item{528*} The optical counterpart is a bright (m$_V$ = 8.72) B9-type star, 
probably associated to the nearby dark cloud LDN 1693. Previous near 
infrared photometry was obtained in June 1987 by van der Veen et al. (1989), 
who report the following magnitudes: $K$ = 8.32; $J-H$ = $-$0.03; $H-K$ = 0.29;
$K-L'$ = 0.16; $L'-M$ = 0.4. 

\item{531*} The far infrared colours of this IRAS source indicate 
the presence of a very cold detached dust shell, suggesting that the 
object has already left the AGB and is now evolving as a post-AGB star. 
Since the object has been detected in OH by Silva et al. (1993) and the 
IRAS variability index is very low, we have classified the object as a 
non-variable OH/IR star, although a detailed monitoring of the object in the
near infrared is needed to confirm this non-variability. 


\item{535*} New low excitation planetary nebula discovered in this survey.
The optical spectrum obtained by Henize around 1950 and a second one 
taken by Kilkenny in 1971 show only a faint H$\alpha$ emission over a 
B0-B3Ie-type stellar continuum, while our optical spectra taken at the 
1.52 m ESO telescope in 1990 revealed dramatic spectral changes and a 
hotter spectral type, which has produced the ionization of the material
in the surrounding envelope.  The object is now a planetary nebula which, 
according to our data, has become ionized in the lapse of only 20 years.
The object has been monitored since 1990 in the optical and the ultraviolet 
range and additional spectral changes have been observed in the IUE 
spectra, which suggest that the evolution observed is the consequence of an
episode of mass loss. A detailed analysis of the changes observed so far can be
found in Parthasarathy et al. (1993, 1995). In addition, HST observations 
have recently revealed the presence of a compact but slightly extended 
(over $\sim$ 2") nebula around the central star with an elliptical 
morphology and a ring-like equatorial enhancement (Bobrowsky 1994).   

\item{537*} The possible optical counterpart is a faint G-type star with 
no emission lines. Radio continuum emission was not detected by van 
der Steene and Pottasch (1993). 

\item{539*} The optical counterpart has been identified as a bright 
source in the CCD image taken in the Z band at the 1 m JKT telescope in 
July 1990, but it looks extremely faint in the V band. An optical 
spectrum taken at the 1.5m ESO telescope in February 1995 shows an extreme
M-type star at this position. The object was not detected in 
the $K$ band by Hu et al. (1993a) in April 1990, while we found a 
very bright source in the $K$ band in May 1989 very close to the IRAS position. 
A bright and compact radio continuum source was found by Pottasch et al. (1988) 
at a position located slightly more than 1' away from the nominal IRAS 
position, making the identification with the IRAS source uncertain. 

\item{540*} The optical counterpart is a bipolar reflection nebula extended 
over a few arcsecs, with m$_V$ = 14.54, according to Hu et al. (1994).  The 
optical spectrum corresponds to an extremely reddened G2I-type star. 
This is one of the very few objects from which bot CO and OH emission has 
been detected and it can be considered as a transition object in between 
the post-AGB stage and proto-planetary nebulae. A detailed analysis of this
IRAS source can be found in Hu et al. (1993b), where the following near 
infrared measurements are reported: $K$ = 9.52; $J-H$ = 0.80; $H-K$ = 0.72;
$K-L$ = 2.0; $L-M$ = 2.1, derived from observations carried out in March 
1989, almost identical to the values we found in May 1990. However, 
the  near infrared source may show small variations in brightness, since 
these magnitudes are slightly brighter than those reported by van der Veen et
al. (1989): $K$ =9.68; $J-H$ = 0.77; $H-K$ = 0.78, from data taken in 
July 1986. H$_2$O maser emission not detected by Zuckerman and Lo (1987). 

\item{542*} There is a very bright near infrared source very close to the 
IRAS position whose optical spectrum corresponds to an extremely reddened 
G-type star with no emission lines which seems to be the right counterpart. 
However, radio continuum emission extended over 2".5 has been detected by 
Ratag et al. (1990) 36" west and 32" north 
of the nominal IRAS position. Additional observations are needed to 
clarify whether this emission is coming from a different object, which 
might then be the right counterpart. 

\item{546*} The optical counterpart corresponds to an extremely reddened 
and compact planetary nebula discovered in this survey from which 
radio continuum emission has been detected by Ratag et al. (1990) with 
an extension $\le$ 2".1.  This is one of the very few cases 
in which OH has been detected from a planetary nebula, making the object
specially interesting for further studies.

\item{547*} The optical counterpart could be a red K-type star located
very close to the IRAS position but this area of the sky is extremely crowded, 
making the identification uncertain. The position of the near infrared 
counterpart measured exactly coincides with the IRAS position, 
but the source was not visible on the TV screen. The object appears as a 
star with emission lines in Wackerling's catalogue (1970). However, we 
did not find any emission-line object in the vicinity of the IRAS position.
Epchtein and Nguyen-Q-Rieu found also a near infrared counterpart 
close to the IRAS position which might be the same one we have measured, 
although they found the object 0.5 magnitudes fainter and slightly bluer
in February 1981, with  $K$ = 10.07; $J-H$ = 1.3; $H-K$ = 1.20, and 
suggest that it may be a red field star and not the right counterpart. 

\item{550*} The optical counterpart is an F-type star with H$\alpha$ emission
over the stellar absorption. Although the far infrared colours are similar 
to those found in T-Tauri stars, we believe that the object is an evolved 
star, since the object is not located close to any known star forming 
region.  Radio continuum emission has been detected by Ratag and 
Pottasch (1991) from a compact source very close to the IRAS position.

\item{558*} There are two M-type stars with similar near infrared colours 
very close to the IRAS position. High spatial resolution CCD imaging is 
needed to determine whether the emission comes from two different objects 
not physically related or they are just the two lobes of a single bipolar 
structure.

\item{563*} Radio continuum emission extended over 4".5 was detected by 
Ratag et al. (1990) and confirmed by van de Steene and Pottasch (1993)
42" east and 8" south of the IRAS position. Detected in the 
near infrared as a bright and red source, we have tentatively classified 
the object as a new planetary nebula, since the far infrared colours 
and low IRAS variability index are consistent with this identification. 
However, a confirmation via optical spectroscopy is still pending. 

\item{564*} Apparently extended in the near infrared, the object seems to 
be a variable OH/IR star, according to the detection of OH maser emission, 
the characteristic far infrared colours and the high IRAS variability index.
An infrared image would help to determine its morphology and confirm the 
extended nature of this source.

\item{565*} A visual inspection of the poor signal-to-noise IRAS Low 
Resolution Spectrum indicates that the association to the LRS class 94 is 
wrong.  The possible optical counterpart is an extremely red late G-type 
star with no emission lines. Although it has only been observed once in 
the near infrared, the recent detection of OH maser emission, together with 
the presence of a detached cold dust shell surrounding the central star, 
as derived from the far infrared colours, and the very low 
IRAS variability index, indicate that the object is already in the 
post-AGB stage and must be classified as a non-variable OH/IR star. 

\item{572*} New very low excitation planetary nebula discovered in this
survey. It has been detected in the near infrared as a bright and red 
source. 

\item{574*} A very bright near infrared counterpart has been found very 
close to the IRAS position which seems to be the right counterpart. 
Optical spectroscopy, however, is still pending.

\item{575*} Although the spectrum of the optical counterpart corresponds to 
a faint B-type stellar continuum with only the Balmer lines in emission, 
its position in the IRAS two-colour diagram undoubtfully corresponds to 
an evolved object. In addition, radio continuum emission has been detected 
by Ratag and Pottasch (1991), suggesting its classification as a new very low 
excitation planetary nebula. A strong P-Cygni profile in H$\alpha$ is also 
observed in a high resolution spectrum taken in August 1994, similar to 
those found in other transition objects included in this survey.
H$_2$O maser emission not detected (Likkel 1989). 



\item{581*} The optical counterpart is a bright (m$_V$ = 10.74) B-type star 
with only the Balmer lines strongly in emission. Although we did not detect
the presence of forbidden emission lines in our low resolution spectrum, 
the position  in the IRAS two-colour diagram corresponds to the region where 
only evolved objects are located and is consistent with its 
identification as a transition object, rapidly evolving towards the 
planetary nebula phase. Previous near infrared measurements are 
available in van der Veen et al. (1989), who derive very similar
values: $K$ = 9.08; $J-H$ = 0.24; $H-K$ = 0.34; $K-L'$ = 1.0; $L'-M$ = 1.3, 
from measurements taken in June 1987. However, Fouque et al. (1992)
observed the same star almost simultaneously with us, finding a  
considerably faint emission, specially in the J band, with: $K$ = 9.36; 
$J-H$ = 0.94; $H-K$ = 0.22, which we believe it must be the result of a 
contamination in their photometric data.


\item{583*} Located in an extremely crowded area,  several bright 
near infrared counterparts have been found by different authors close to 
the IRAS position. The object we have measured shows moderate 
red colours in the near infrared, but it is 3 magnitudes brighter than the 
one reported by Persi et al. (1990), from measurements taken in December 
1987. They report the following magnitudes: $K$ = 11.68; $J-H$ = 1.89; 
$H-K$ = 0.69; $K-L$ = 2.39; $L-M$ = 2.42, from a source also located 
very close to the nominal IRAS position. A third measurement is given by 
Epchtein and Nguyen-Q-Rieu (1982) in February 1981, who found a much 
brighter object in the $K$ band, with: $K$ = 6.71; $J-H$ = 1.46; $H-K$ = 
1.22; $K-L$ = 0.52. They suggest that it is a red field star and not the 
right counterpart. It is not clear whether any of these measurements 
correspond to the same source. If so, it must be strongly variable and 
could be able to contribute significantly to the IRAS fluxes observed. 
However, it seems that there is a much more reddened near infrared counterpart 
in the vicinities of the IRAS position, which is the one monitored
by Le Bertre (1993) for several years, deriving a very large amplitude
and a long photometric period of 1430 days from measurements taken only in 
the L' and M bands, where it is extremely bright ($<L'>$ = 3.46; 
$<M>$ = 1.36). This object was first detected by  Jones et al. (1982) 
in February 1981 with $K-L'$ = 8.17, 
and has also been measured by Nyman et al. (1993) 
in May 1990, reporting the following values: $K$ = 10.28; $J-H$ =2.15;
$H-K$ = 2.41; $K-L'$ = 7.89; $L'-M$ = 1.83. 
Radio continuum emission not detected by Zijlstra et al. (1989). 
H$_2$O maser emission not detected by G\'omez et al. (1990). SiO emission at 
43 GHz was detected by Nyman et al. (1993). 

\item{584*} The bright near infrared counterpart found close to the 
IRAS position shows only a moderate reddening and might not be the
right counterpart. However, it has been classified as a possible 
non-variable OH/IR star, since it shows OH maser emission and far 
infrared colours which suggest the presence of a very cold envelope, 
indicating that the object is already in the post-AGB stage. 
Optical spectroscopy of two possible very faint optical counterparts has 
been obtained but none of them show emission lines or any other 
remarkable feature. Radio continuum emission was not detected by 
Zijlstra et al. (1989).

\item{588*} The optical counterpart seems to be a red and faint K-type star 
without emission lines. 


\item{591*} The near infrared counterpart is found to be strongly variable.
The same object observed in May 1989 with $K$ = 8.84 was 3 magnitudes
fainter in the $K$ band in May 1992, and it is probably the same object
observed by van der Veen et al. (1989) in June 1987 with $K$ = 10.86; 
$K-L'$ = 4.26; $L'-M$ = 0.8. Strong radio continuum emission was detected 
extended over less than 1".4 by Ratag et al. (1990).

\item{592*} An extremely bright and red near infrared source has been 
found close to the IRAS position and seems to be the right 
counterpart. The IRAS source has tentatively been classified as a 
non-variable OH/IR star because it shows a very low
IRAS variability index. However, it is located in the region of the 
IRAS two-colour diagram where many other variable OH/IR stars are found, 
which makes this identification uncertain. Additional observations 
are clearly needed. Radio continuum emission was not detected by 
Zijlstra et al. (1989). 

\item{593*} The bright near infrared counterpart observed shows no or little 
reddening. The spectrum of the optical counterpart corresponds to 
a red K-type stellar continuum with no emission lines. Additional 
observations are needed to confirm that the object is not a field star.
However, the far infrared colours undoubtfully correspond to a star in the 
post-AGB stage, and these are sometimes found showing no reddening at all.

\item{600*} Although located in the direction of the dark cloud LDN 174, 
the infrared colours correspond to an evolved star in the post-AGB phase.
The spectrum of the possible optical counterpart only shows a faint and red 
continuum of undetermined spectral type and no emission lines.

\item{602*} A very bright near infrared counterpart was detected very
close to the IRAS position and seems to be the right counterpart. 
However, the observed optical counterpart, a red G-type star with no 
emission lines, might not be the right one, since the position 
of the IRAS source in the two-colour diagram and the high variability 
index usually correspond to variable OH/IR stars, although the object has not 
been detected in OH by several authors. Radio continuum emission has 
been detected by Ratag and Pottasch (1991) at a position located 52" 
east and 38" north of the nominal IRAS position.
Additional observations are needed to confirm whether the radio emission is 
related with the IRAS source.

\item{616*} Although optical spectroscopy is still pending, the bright 
near infrared source found close to the IRAS position has been classified as
a post-AGB star since, according to the far infrared colours, it shows 
a very cold dust envelope and the near infrared photometry shows stellar-like
colours.  


\item{620*} One of the very few objects for which both CO and OH emission has
been detected, together with the presence of radio continuum emission 
(Pottasch et al. 1987, 1988). A low resolution spectrum of the 
possible red optical counterpart only shows a red and featureless continuum. 
Not detected in CS (2$\rightarrow$1) by Bronfman et al. 1996. 

\item{621*} New low excitation planetary nebula discovered during this survey
extended about 4" in H$\alpha$. A companion star is seen at a distance of 
only 2", which might be a physical companion in a binary system. The 
emission from this star is probably producing the stellar-like emission 
observed in the near infrared. High resolution optical spectroscopy and 
deep CCD imaging are required to determine whether both stars are 
physically associated. 

\item{624*} A possible optical counterpart is visible as a faint object 
in the CCD image taken in the $Z$ band at the 1 m JKT telescope in July 1990,
while nothing is observed at this position in the $R$ band. This object has 
been detected in both CO and OH, making it specially interesting for further 
studies. It shows a strong silicate absorption in the IRAS LRS spectrum
(Volk \& Cohen 1989). We have detected a bright and red
near infrared counterpart close to the IRAS position but, unfortunately, we
could not measure the object in the $L'$ band because of the weather 
conditions and it is not clear whether the source we observed is the 
same reported in Lepine et al. (1995), who derive very extreme
near infrared colours: $K$ = 10.09; $K-L$ = 7.88; 
$L-M$ = 2.21, from measurements obtained in May 1991. The object was not 
detected by them in the $H$ and $J$ bands. H$_2$O maser emission not 
detected by Zuckerman and Lo (1987). 

\item{625*} The far infrared colours undoubtfully correspond to an evolved 
object in the post-AGB phase. A bright near infrared source has been found close
to the IRAS position but the obtention of an optical spectrum of this 
source is still pending.

\item{631*} The position of this source in the IRAS two-colour diagram
together with the detection of radio continuum emission 
coming from this source extended over 3".1 by Ratag et al. (1990)
suggest its identification as a new planetary nebula. However, confirmation 
through optical spectroscopy is still pending. 

\item{632*} The optical counterpart corresponds to a bright bipolar 
nebula with extremely high velocity outflows extended over 11".5 in H$\alpha$. 
Several point-symmetric blobs of emission are detected along the major axis, 
which have been interpreted as the result of episodic mass loss from a
precessing source. A detailed analysis of this object can be found in 
Riera et al. (1995) and Bobrowsky et al. (1995). The spectrum of the 
central star corresponds to a B-type star with the Balmer lines 
in emission. The core shows the infrared calcium triplet strongly in emission 
as well as many iron emission lines, while the nebular component shows 
emission lines of  N, O and S. Radio continuum emission has recently been 
detected by Knapp et al. (1995)


\item{637*} The spectrum of the optical counterpart (m$_V$ $\sim$15) 
corresponds to an M-type stellar continuum without emission lines. Classified 
as M2I by Hu et al. (1993a), they report the following near infrared magnitudes:
$K$ = 8.69; $J-H$ = 1.16; $H-K$ = 0.35; $K-L$ = 0.8; $L-M$ = 1.4, 
from measurements taken in April 1990, very similar to the values we obtained 
in May 1989.  Although detected in OH, the object might already be in the
post-AGB stage, since it is associated to a low IRAS variability index and it 
seems to be not variable in the near infrared. H$_2$O maser emission not 
detected by Likkel (1989). 

\item{639*} The optical counterpart is a bright (m$_V$ $\sim$7.1) F3Ib-type
star with a very faint H$\alpha$ emission over absorption, as derived from
our high resolution optical spectrum, taken in June 1995. It shows small 
fluctuations of brightness which are probably due to stellar pulsation.
Additional near infrared photometry is reported in Hrivnak et al. (1989)
and in Kastner and Weintraub (1995), both with almost identical 
values to those we report in Paper II. H$_2$O maser emission not detected 
(Zuckerman \& Lo 1987; Likkel 1989). 

\item{640*} The object shows a red featureless LRS spectrum
(Volk et al. 1993), usually associated to heavily obscured C-rich
post-AGB stars. Narrow CO emission extended over 90"$-$100" was detected by 
Likkel et al. (1991) at v$_{LSR}$ = +128 km s$^{-1}$, but this emission 
is probably of interstellar origin. Hu et al. (1993a) found a weaker
but broader CO emission at v$_{LSR}$ = +5 km s$^{-1}$ 40" away from
the IRAS position, which seems to be of circumstellar origin and might 
correspond to the right counterpart. However, while they say that the 
CO emission is found 40" west of the IRAS position, they provide 
the near infrared photometry of an object which is 40"  east of it. 
They found the following near infrared colours: $K$ = 9.78; $J-H$ = 1.11; 
$H-K$ = 0.77; $K-L$ = 2.17; $L-M$ = 1.9, from measurements obtained in 
April 1990, not too different from those reported in this Paper, but 
consistently fainter ($\sim$ 0.5 magnitudes) in all filters. Slightly 
different colours were derived by van der Veen et al. (1989) from measurements
taken in August 1986. They report: $K$ = 9.66; $J-H$ = 1.45; $H-K$ = 
0.43. According to Hu et al. (1993a), this is not the same near 
infrared source, but we cannot rule out this possibility, since 
there is still too much confusion about the accurate coordinates of the 
counterpart. H$_2$O maser emission not detected by Likkel (1989). 

\item{643*} New compact planetary nebula discovered during this survey. 
It shows only the characteristic nebular emission lines associated to 
intermediate excitation planetary nebulae with no traces of the stellar
continuum. Radio emission extended over 1".4  was detected by Pottasch et al. 
(1988).

\item{646*} The optical counterpart is a bright (m$_V$ $\sim$7.9) B0-type 
star probably associated to the HII region S15 and member of the Sgr OB5
association.  Radio continuum emission detected by Ratag et al. (1990). 

\item{647*} Although a confirmation via optical spectroscopy is still
pending, this IRAS source is probably a new planetary nebula. Radio 
continuum emission extended over  6" has been detected by Ratag et al.
(1990) and the optical counterpart has been detected as an 
object with H$\alpha$ emission and no continuum 
in the CCD images taken at the Danish 1.5 m ESO telescope. 

\item{652*} Located very close to a wide and bright visual binary, the 
near infrared source was not visible in the TV screen at the 1 m ESO 
telescope. The detection of OH maser emission, the low IRAS variability
index and the position in the IRAS two-colour diagram, which indicates 
the presence of a detached sust shell, suggest that the object is in the
post-AGB stage. Thus, we have tentatively classified the source as a 
non-variable OH/IR star, although additional observations are needed
to confirm this non-variability.

\item{656*} Althoug the IRAS LRS spectrum of this IRAS
source is classified as 39, which corresponds to O-rich envelopes 
with a silicate absorption band around 9.7 $\mu$m, the object has only  
been detected in CO and not in OH. However, the IRAS variability index 
is very high and the position in the IRAS two-colour diagram is usually
associated to variable OH/IR stars. The source measured in the near infrared
has an optical counterpart which corresponds to a red K-type stellar 
continuum. High resolution optical spectroscopy of this star would be needed
to confirm that this is the right counterpart. HCN emission not detected 
by Omont et al. (1993). 


\item{660*} The near infrared counterpart found is not very red and might
be a field star. According to the IRAS colours, the recent detection of 
a faint double-peaked OH maser emission and the low IRAS variability index 
it has tentatively classified as a non-variable OH/IR star, but 
additional observations are needed. 

\item{661*} New very low excitation planetary nebula extended over 18"
discovered during this survey and, independently, by Hu and Bibo (1990). 
The central star is WC11-type. A detailed analysis of this IRAS 
source can be found in Pollacco and Hill (1994). Additional near infrared
photometry is available in Hu and Bibo (1990), who report the following
values: $K$ = 8.97; $J-H$ = 1.38; $H-K$ = 2.03; $K-L$ = 3.30; $L-M$ = 
0.96, from measurements obtained in March 1989. H$_2$O maser emission 
not detected by Likkel (1989).

\item{662*} The bright and extremely red source detected in the 
near infrared has a very faint and red optical counterpart showing a 
strong Halpha emission over a red continuum. Other emission lines of
hydrogen have also been detected in the near infrared by van der Veen et al. 
(1989), who also report the following near infrared photometry: 
$K$ = 5.15; $J-H$ = 1.88; $H-K$ = 1.85; $K-L'$ = 2.56; $L'-M$ = 0.78, 
from measurements taken in June 1987, remarkably similar to those reported
by us in Paper I, suggesting that the object is not variable in the near 
infrared. The detection of double-peaked OH maser emission confirms the 
evolved nature of the object and suggests its clasification as a 
non-variable OH/IR star, also supported by its association with a very 
low IRAS variability index. 

\item{664*} Probably too red to be detected above our detection limit in the
$K$ band. Recently, a very faint double-peaked OH maser emission has been 
detected, which confirms its classification as a variable OH/IR star. 

\item{668*} A very bright and red source is found in the near infrared 
close to the IRAS position. The detection of the characteristic double-peaked 
OH maser emission, the low IRAS variability index and the position in the IRAS 
two-colour diagram are all consistent with the classification of this 
source as a non-variable OH/IR star. In addition, very similar photometry 
was obtained by Lepine et al. (1995) from measurements taken in August 1991. 
They report the following values: $K$ = 6.83; $J-H$ = 1.72; $H-K$ = 0.99;
$K-L'$ = 0.82; $L'-M$ = 0.20. Radio continuum emission not detected by
Zijlstra et al. (1989). H$_2$O maser emission not detected by G\'omez et 
al. (1990).

\item{669*} An optical counterpart has been found showing a strong 
H$\alpha$ emission over a stellar continuum. 

\item{670*} It is not clear whether the object observed in the near infrared
is bipolar or they are two different stars very close in the sky. 
Additional observations are needed to clarify this point.

\item{674*} Two near infrared counterparts with very similar colours
have been measured very close in the sky. Additional observations would be
needed to determine whether this is a single object with a bipolar
structure or two different ones. The far infrared colours and the low
variability index suggest that the object might be a non-variable 
OH/IR star. 

\item{676*} Although the far infrared colours are those usually observed
in variable OH/IR stars, the IRAS variability index is very low and it has 
not been detected in OH. Thus, we have tentatively classified this source 
as a post-AGB star.

\item{678*} Although detected in OH, it shows a cold dust shell and a low
IRAS variability index. Therefore, it has been classified as a possible
non-variable OH/IR star, although more observations are needed to confirm
this non-variability. Radio continuum emission not detected by Zijlstra et al. 
(1989). H$_2$O maser emission not detected by G\'omez et al. (1990).

\item{681*} A bright and red counterpart has been detected in the 
near infrared, which in our optical CCD images appears as a strongly reddened 
star with no H$\alpha$ emission. Optical spectroscopy is still pending.
Recently detected in OH, it shows a cold detached dust shell and a low 
IRAS variability index, which is consistent with its classification as a 
non-variable OH/IR star.

\item{686*} The bright near infrared counterpart measured shows stellar-like
colours. The optical counterpart seems to be a red and bright (m$_V$ $\sim$11) 
G-type star with no apparent emission lines, which seems to be surrounded by a 
faint reflection nebula in the light of H$\alpha$. Radio continuum emission 
has been detected by Ratag et al. (1990). This, combined with the 
detection of OH maser emission at 1612 MHZ, makes this object specially
interesting for further studies. 

\item{687*} A very red and not strongly variable source, according to 
the data available,  has been found
in the near infrared close to the IRAS position. The possible optical 
counterpart is a red K-type star, identified as a K0-type by Hu et al. 
(1993a). They also provide additional near infrared photometry of this 
object: $K$ = 9.15; $J-H$ = 2.9; $H-K$ = 1.68; $K-L$ = 1.8; $L-M$ = 0.8, 
from measurements taken in April 1990.  Radio continuum emission detected by 
Ratag et al. (1990) extended over 6".7, although additional observations are 
needed to confirm the connection with the IRAS source. 

\item{688*} The possible optical counterpart is a faint late K-type star 
with no emission lines. 

\item{689*} A very bright near infrared source is found close to the 
IRAS position showing stellar-like colours. The optical counterpart is a 
bright (m$_V$ $\sim$13) K-type star with no emission lines. The 
recent detection of OH maser emission together with the low IRAS variability
index and the far infrared colours suggest its classification as a 
non-variable OH/IR star. 

\item{691*} The extremely red colours of the near infrared source found
undoubtfully correspond to the right counterpart, which also shows 
the characteristic far infrared colours of variable OH/IR stars. 

\item{692*} The extremely bright source detected in the near infrared 
must be the right counterpart. Although according to Kwok et al. (1987)
there is no optical counterpart at the IRAS position, several faint stars
are located in the vicinities, any of which could be the 
right one. It is clear that additional observations of this field 
are needed. 

\item{698*} This is a new very low excitation planetary nebula discovered 
in this survey extended over a few arcsecs. The central star seems to be
a late WC star. 

\item{704*} There is a bright near infrared source close to the 
IRAS position showing stellar-like colours, which has been identified 
in the optical as a K-type star with no emission lines. However, it might 
not be the right optical counterpart, since the object seems to be a 
variable OH/IR star, according to the detection of the OH maser emission 
at 1612 MHz and the characteristic far infrared colours. 

\item{706*} Not detected in the near infrared above our detection limit 
in the $K$ band. Detected in OH, the far infrared colours and low IRAS 
variability index suggest its classification as a heavily obscured
non-variable OH/IR star. H$_2$O maser emission not detected by 
G\'omez et al. (1990).


\item{707*} The red optical counterpart has been identified as a very low 
excitation planetary nebula, according to our low and high 
resolution spectroscopy. It shows H$\alpha$ and the forbidden lines of 
[N II] in emission and has been detected as a compact radio source 
at 20 cm by Becker et al. (1990). From the flux ratio [S III]$\lambda$ 9532 
/ Pa9$\lambda$9225 obtained employing narrow band CCD images, 
Kistiakowsky and Helfand (1995) also conclude that the object is a planetary
nebula. 

\item{712*} The stellar-like colours observed in the near infrared are not
consistent with the classification of this source as a variable OH/IR star 
and might not correspond to the right counterpart. Additional observations 
are needed to determine whether this star shows the same (or similar) 
peculiar very high radial velocity of +259 km s$^{-1}$ derived from the 
single-peaked OH maser emission. 

\item{713*} The optical counterpart observed is a bright (m$_V$ $\sim$12) 
G-type star with no emission lines. Classified as a G2I by Hu et al.
(1993a), they report additional near infrared data, with the 
following values: $K$ = 7.60; $J-H$ = 0.60; $H-K$ = 0.33, from 
measurements taken in March 1989, and almost the same colours are 
found by Fouque et al. (1992), from measurements obtained in 1990. 

\item{717*} Radio continuum emission not detected by Zijlstra et al. (1989). 


\item{724*} The optical counterpart is a bright  B-type star 
with a strong H$\alpha$ emission and very faint forbidden 
nebular emission lines of [N II] and [S II], which are only visible in our 
high resolution spectra, as well as iron lines corresponding to different 
ionization states. The IRAS colours undoubtfully correspond to an evolved
object. Classified as A5 in the SAO Catalogue and as a Be-type
star by Downes and Keyes (1988), it might be a transition object 
rapidly evolving towards hotter effective temperatures, in its 
way to become a planetary nebula. Arkhipova et al. (1996) suggest a 
B5I-type spectrum in 1995 for the central star and its continuous fading 
from m$_V$ $\sim$9.4 to m$_V$ $\sim$11.5 in the last 30 years, as well as 
the detection of night to night variations of up to 0.4 magnitudes in the 
$V$ band. Additional near infrared photometry can be found in Lawrence et al. 
(1990), who report the following values: $K$ = 10.21; $K-L'$ = 0.60; $L'-M$ \
= 2.31, from measurements obtained in August 1987. 

\item{726*} The bright near infrared source found close to the IRAS 
position corresponds in the optical to a red late G-type star 
with m$_V$ $\sim$15 and no emission lines.

\item{729*} Detected in OH, the far infrared colours and low IRAS 
variability index suggest its classification as a heavily obscured
non-variable OH/IR star. Radio continuum emission not detected by Zijlstra 
et al. (1989). H$_2$O maser emission not detected by G\'omez et al. (1990). 

\item{735*} The optical counterpart is a bright (m$_V$ $\sim$10.4) F3Ib-type 
star with a faint H$\alpha$ emission over the stellar absorption, as can be
observed in our high resolution spectrum taken in June 1995. A detailed
analysis of this star can be found in Hrivnak et al. (1988) and in 
Klochkova (1995). Additional near infrared photometry is available in 
Hrivnak et al. (1988), van der Veen et al. (1989), Lawrence et al. (1990)
and Kastner and Weintraub (1995), who report very similar brightness and
colours. H$_2$O maser emission not detected (Zuckerman \& Lo 1987; 
G\'omez et al. 1990; Engels \& Lewis 1996).

\item{737*} The possible optical counterpart shows a G-type stellar
continuum with no emission lines.

\item{740*} The optical counterpart corresponds to a relatively 
bright (m$_V$ $\sim$14)  late M-type star. A compact radio continuum 
emission was detected by Ratag and Pottasch (1991) very close to the 
nominal IRAS position. Additional observations are needed to confirm 
its connection with the IRAS source. 

\item{756*} A very long period of 1012 days has been derived by Herman 
and Habing (1985) from observations of the strongly variable OH maser 
emission. Volk and Cohen (1989) report the presence of a strong 
silicate absorption in the LRS spectrum. Radio continuum emission 
not detected by Zijlstra et al. (1989). H$_2$O maser emission 
detected by G\'omez et al. (1990).

\item{759*} New planetary nebula discovered during this survey. The spectrum
shows nebular emission lines corresponding to an 
intermediate excitation planetary nebula extended over 8" in H$\alpha$. 

\item{771*} The spectrum of the optical counterpart corresponds to a
very faint stellar continuum of undetermined spectral type with 
H$\alpha$ clearly in emission. The infrared colours are typical of 
a compact HII region. However, this object is not associated to any known 
star forming region. Additional observations are needed to discard 
the possibility of this source being an extremely reddened very low excitation
planetary nebula. 

\item{774*} The bright near infrared counterpart found at the IRAS 
position is invisible in the optical range. Detected in OH, the far infrared 
colours and low IRAS variability index suggest its classification as a 
heavily obscured non-variable OH/IR star. 

\item{777*} The high expansion velocity derived from the analysis of the 
OH maser emission and its position on the IRAS two-colour diagram 
indicate that this IRAS source is probably associated to a considerably 
massive progenitor star, rapidly evolving toward the planetary nebula 
stage. The very cold dust shell and the low IRAS variability index suggest 
its classification as a non-variable OH/IR star. 
The noisy optical spectrum of a possible faint counterpart does not 
show any emission lines. H$_2$O maser emission not detected by G\'omez et al. 
(1990). CS (2$\rightarrow$1) not detected by Bronfman et al. (1996)

\item{781*} New planetary nebula, according to Kistiakowsky and Helfand 
(1995),  who conclude this from the analysis of the flux ratio 
[S III]$\lambda$ 9532 / Pa9$\lambda$9225. Radio continuum emission
detected by Zoonematkermani et al. (1990). 

\item{783*} The optical counterpart is an extremely red Mira variable  
with a very long period of 1785 days (Nyman et al. 1993). 
H$_2$O maser emission not detected by G\'omez et al. (1990).

\item{794*} Radio continuum emission not detected by Zijlstra et al. 
(1989). The LRS available in Volk et al. (1991), although noisy, 
shows a very red continuum with no peculiar features. 

\item{805*} The near infrared counterpart is an invisible source 
in the optical range. New planetary nebula, according to Kistiakowsky and 
Helfand (1995),  who conclude this from the analysis of the flux ratio 
[S III]$\lambda$ 9532 / Pa9$\lambda$9225. Radio continuum emission detected
by Zoonematkermani et al. (1990), Ratag (1991) and Griffith et al. (1995). 

\item{809*} Not detected in the near infrared. There is a bright 
(m$_V$ $\sim$13) star located 35"  south and 7" east of the IRAS position 
whose spectrum corresponds to a B-type star with no emission lines,
which is probably not the right counterpart. H$_2$O maser emission not 
detected by G\'omez et al. (1990). The low IRAS variability index and 
the small irregular variations observed in the OH maser emission (Herman \&
Habing 1985) suggest its classification as a non-variable OH/IR star.

\item{816*} The optical counterpart is a bright (m$_V$ $\sim$12) B-type
star with no emission lines. Fouque et al. (1992) report the
following near infrared measurements: $K$ = 10.19; $J-H$ = 0.20; 
$H-K$ = 0.32. 

\item{817*} The spectrum of the optical counterpart shows an A-type stellar
continuum with no emission lines. However, additional observations are 
needed to confirm that this is the right counterpart.

\item{818*} The optical counterpart could be a bright (m$_V$ $\sim$12.5) 
star, located very close to the nominal IRAS position. However, no 
optical spectrum of this star has been obtained yet.  

\item{823*} The optical counterpart seems to be a K-type star with no
emission lines. Detected in OH, the very cold dust shell and the low IRAS
variability index suggest its classification as a non-variable OH/IR star.
Radio continuum emission not detected by Herman et al. (1985). 
H$_2$O maser emission not detected by G\'omez et al. (1990). 
CS (2$\rightarrow$1) not detected by Bronfman et al. (1996).

\item{841*} Although close to a star forming region, the infrared colours 
undoubtfully correspond to an evolved star. The possible optical 
counterpart is a star with H$\alpha$ in absorption.

\item{844*} New very low excitation planetary nebula. Spectrum available
in Becker et al. (1990). Kistiakowsky and Helfand (1995), from the 
analysis of the flux ratio [S III]$\lambda$ 9532 
/ Pa9$\lambda$9225 also conclude that the object is a planetary 
nebula. Radio continuum emission detected by Zoonematkermani et al. (1990). 
The near infrared counterpart found is invisible on the Palomar prints.


\item{845*} New extremely red planetary nebula discovered in this survey. 
Radio continuum emission detected by Ratag (1991). The presence of 
H$\alpha$ emission is obvious from the CCD image taken in July 1990 at 
the 1 m JKT telescope. However, no optical spectrum is available yet.

\item{849*} The possible optical counterpart is a faint M-type star with 
no emission lines.

\item{855*} The extremely red and bright near infrared counterpart is 
invisible in the optical range. H$_2$O maser emission 
not detected (Zuckerman \& Lo 1987; Likkel 1989). The LRS spectrum
(Volk and Cohen, 1989) shows a very red continuum and a possible 
silicate absorption feature. 

\item{858*} The optical counterpart is a bright K-type star 
(m$_V$ $\sim$12.6) with no emission lines. 

\item{864*} The possible optical counterpart is a relatively bright
(m$_V$ $\sim$14) star with an intermediate spectral type and no emission lines.


\item{869*} New very low excitation planetary nebula. The optical 
spectrum shows the presence of the Balmer lines in emission together with 
nebular emission lines of [N II] over a faint and red continuum. The 
H$\alpha$ image obtained at the 1 m JKT telescope in July 1990 
indicates that the emission is not extended. Additional near infrared
photometry is available in van der Veen et al. (1989), who report the
following values: $K$ = 10.26; $J-H$ = 1.4; $H-K$ = 1.43; $K-L'$ = 3.06;
$L'-M$ = 1.0, from measurements taken in June 1987 and Fouque et al. (1992), 
who derived: $K$ = 10.29; $J-H$ = 1.21; $H-K$ = 1.39, from measurements taken 
in 1990. The near infrared photometry reported in Paper I corresponds to 
a wrong near infrared counterpart. H$_2$O maser emission not detected by 
Likkel (1989). 

\item{870*} The optical counterpart is a not a bright F-type star 
(m$_V$ $\sim$12) with no emission lines close to the nominal IRAS 
position but a fainter nearby object showing H$\alpha$ emission over
the stellar absorption.  H$_2$O maser emission not detected by Likkel (1989). 

\item{879*} The infrared colours undoubtfully correspond to an evolved 
star, but the object is located very close to a known star forming region. 
The source detected in the near infrared is an optically invisible object 
located 83" north and 9" west of a bright star with  m$_V$ $\sim$13.
Radio continuum emission detected by Zoonematkermani et al. (1990). 
Additional observations are needed to clarify the nature of this IRAS 
source.

\item{880*} The spectrum of the optical counterpart shows a very red and faint
stellar continuum of undetermined spectral type with no emission lines.
H$_2$O maser emission not detected by Likkel (1989). 

\item{887*} New extremely reddened high excitation planetary nebula 
discovered in this survey. The optical spectrum is available in van 
de Steene et al. (1996a).

\item{895*} New very low excitation compact planetary nebula discovered in 
this survey. 

\item{898*} The near infrared counterpart is a faint and red star for which 
the obtention of an optical spectrum is still pending.

\item{900*} Not detected in the near infrared. A visual inspection of the 
Palomar prints indicate that there is no optical counterpart close to the 
IRAS position. 

\item{903*} Possibly associated to the nearby dark cloud LDN 673.

\item{905*}  The possible optical counterpart is an extremely faint and 
reddened star with no emission lines. H$_2$O maser emission not detected by 
G\'omez et al. (1990). CS (2$\rightarrow$1) emission not detected by 
Bronfman et al. (1996). 

\item{907*} The optical counterpart seems to be a faint and red star 
with an intermediate spectral type and no emission lines. 

\item{911*} Close to a star forming region. Radio continuum emission detected
by Zoonematkermani et al. (1990).

\item{915*} Extremely brigt and red in the near infrared, 
the optical counterpart is a bright K1-K4 type star
with no emission lines. Although the far infrared colours and the high IRAS
variability index suggest its classification as a variable OH/IR star, 
the OH maser emission only show small irregular variations in brightness,
according to Herman and Habing (1985). Thus, we have classified this IRAS 
source as a non-variable OH/IR star.  H$_2$O maser emission not 
detected (Likkel 1989; G\'omez et al. 1990; Engels \& Lewis 1996).

\item{920*} The simultaneous detection of CO and OH makes this object 
specially interesting for further studies. It showed no optical 
counterpart at the moment of our observations, although Kleinmann et al. 
(1981) classified the object as M-type. H$_2$O maser emission not detected 
(Likkel 1989; G\'omez et al. 1990; Engels \& Lewis 1996). 

\item{923*} The optical counterpart corresponds to a faint K-type star with 
no emission lines  9" north and 42" east of a bright (m$_V$ $\sim$13) star. 
H$_2$O maser emission not detected (Likkel 1989). 

\item{935*} Although this source is close to a known star forming region,
the infrared colours correspond to an evolved star. The near infrared 
counterpart is invisible in the optical range and it is located in the 
vicinities of a bright late G-type star. 

\item{950*} The object measured in the near infrared is probably not the
right counterpart, but a field star. The right one  
is probably a heavily obscured C-rich post-AGB star invisible in the
optical range. Optical spectroscopy has been obtained for two possible faint 
optical counterparts. They show B-type and K-type stellar
spectra respectively, both with no emission lines. Probably none of 
them is the right counterpart. 
Lawrence et al.(1990) found the star in September 1987 with $K$ = 10.12
and $N$ = 1.29. HCN emission detected by Omont et al. (1993). 
H$_2$O maser emission not detected by Likkel (1989). 

\item{951*} The optical counterpart is a bright (m$_V$ $\sim$10) F3Ib-type star 
with a faint H$\alpha$ emission over the stellar absorption. 
 Kastner and Weintraub (1995) found the star in
June 1992 with $K$ = 7.30. H$_2$O maser emission not detected by Likkel 
(1989). CS (2$\rightarrow$1) emission not detected by Bronfman et al. (1996).

\item{952*} The optical counterpart is a faint star 25" NE 
of a bright nearby B-type star (m$_V$ $\sim$12). 
Lawrence et al. (1990) found the star in September 1987 with $K$ = 9.26.
H$_2$O maser emission not detected by Likkel (1989). 

\item{953*} The possible optical counterpart is an extremely faint star with 
no emission lines. The object is probably a heavily obscured C-rich post-AGB 
star, not detected in the near infrared. 
HCN emission detected by Omont et al. (1993). H$_2$O maser emission not
detected by Likkel (1989). 

\item{954*} The optical counterpart is a bright (m$_V$ $\sim$9.0) 
F3I-type star with H$\alpha$ emission over the stellar absorption. Recently,
van Winckel et al. (1996) derived a hotter A2I spectral type for this star
which might be rapidly evolving in the HR diagram in its way to become 
a planetary nebula. HCN emission not detected by Omont et al. (1993). 
Additional near infrared measurements are available in van der Veen et al.
(1989), Hrivnak et al. (1989), Fouque et al. (1992) and Kastner and
Weintraub (1995), all them reporting very similar brightness and colours.
H$_2$O maser emission not detected (Likkel 1989;  Deguchi et al. 1989).

\item{960*} H$_2$O maser emission not detected (Nyman et al. 1986;
Likkel 1989; G\'omez et al. 1990; Engels \& Lewis 1996). 

\item{961*} There are two possible optical counterparts close to the IRAS 
position. The brighter is an F8-type star with no emission lines. 

\item{963*} The spectrum of the optical counterpart corresponds to a
relatively bright (m$_V$ = 13.3) but extremely reddened G8Ia-type star 
(Hrivnak 1995) with no emission lines.  Kwok et al. (1995) classify this
IRAS source as a C-rich post-AGB star with the 21 $\mu$m feature in emission
and report the following near infrared magnitudes: $K$ = 6.73; $J-H$ = 0.90;
$H-K$ = 0.30. In addition, HCN emission has also been detected by Omont et al. 
(1993). H$_2$O maser emission not detected by Likkel (1989). 

\item{966*} The optical counterpart shows an extremely reddened  
late-type stellar continuum. H$_2$O maser 
emission not detected (G\'omez et al. 1990; Engels \& Lewis 1996). 

\item{967*} The optical counterpart shows a nebular appearance with an 
extension of  40" x 20" and a complex shell structure. The infrared 
colours correspond to a compact HII region although the object has also 
been identified as a supernova remnant by several authors in the recent past.
A detailed kinematic study is necessary to determine 
its nature. The multiple forbidden emission lines present in the spectrum 
show that the excitation is due to shocks. Kulkarni et al. (1992) 
suggest the identification of this nebula as a bow shock powered by a 
radio pulsar/Be-star binary. 


\item{968*} The optical counterpart could be a faint M-type 
star with no emission lines close to the nominal IRAS position. HCN emission 
not detected by Omont et al. (1993). 
H$_2$O maser emission not detected (Zuckerman \& Lo 1987; Likkel 1989). 

\item{971*} The possible optical counterpart is a faint K-type star 
with no emission lines close to the nominal IRAS position. 

\item{972*} H$_2$O maser emission not detected (Zuckerman \& Lo 1987;
Likkel 1989; Engels \&  Lewis 1996).

\item{976*} The object measured in the near infrared is an A-type star 
with no emission lines located close very close to the nominal IRAS 
position. 

\item{977*} Probably associated to a nearby star forming region. Not detected
in CS (2$\rightarrow$1) by Bronfman et al. (1996).

\item{982*} The spectrum of the optical counterpart corresponds
to a G-type star with no emission lines suggested to be C-rich by 
Kwok et al. (1995). 

\item{985*} The optical counterpart seems to be an F-type star with no 
emission lines located very close to the nominal IRAS position. 

\item{986*} H$_2$O maser emission detected by Zuckerman and Lo (1987).  
 
\item{995*} The optical counterpart shows a strong H$\alpha$ emission
over an extremely red continuum together with multiple forbidden emission 
lines extended over 10". The line ratios observed correspond to those 
usually found in compact  HII regions. 

\item{999*} A period of 1652 days is reported by van Langevelde et al.
(1990). H$_2$O maser emission not detected (Likkel 1989; 
G\'omez et al. 1990; Engels \& Lewis 1996). 

\item{1000*} Radio continuum emission detected by Ratag (1991). 
The possible optical counterpart is located close to a bright and
compact nebulosity and only shows a red continuum 
with no emission lines. More observations are needed to confirm this 
identification.

\item{1002*} CS (2$\rightarrow$1) emission not detected by Bronfman et al. 
(1996). 

\item{1003*} The counterpart has been detected in the Z band at the 1m 
JKT telescope in July 1990, but it is extremely faint in R and H$\alpha$, and 
completely invisible in the V band. The detection of radio continuum 
emission by Ratag (1991) confirms that the ionization of the envelope 
is already  in progress. An optical spectrum is needed to confirm the nature
and the evolutionary stage of this IRAS source. H$_2$O maser emission not 
detected by Likkel (1989). 

\item{1007*} The spectrum of the possible optical counterpart only shows a 
red continuum of undetermined spectral type with no emission lines. 

\item{1008*} The optical counterpart is a bright (m$_V$ $\sim$11) B-type
star. Parthasarathy (1993) first suggested that the object is a low mass 
post-AGB star and not a massive supergiant. 
The radio continuum emission detected by Ratag (1991) and the 
presence of very low excitation forbidden emission lines in the optical 
spectrum indicates that the ionization of the circumstellar envelope is
already  in progress. A strong and variable P-Cygni profile has been 
observed in the line of H$\alpha$. A  detailed study of this star 
is available in Garc\'\i a-Lario et al. (1997b)


\item{1012*} The spectrum of the optical counterpart corresponds to a
bright A-type 
star with a faint H$\alpha$ emission over the stellar absorption.  
H$_2$O maser emission not detected by Wouterloot et al. (1993). The source 
was found 3 magnitudes brighter in  October 1992. Additional observations are
needed to confirm whether these variations are real. 

\item{1013*} The optical counterpart seems to be a bipolar reflection nebula  
illuminated by an A-type central star. The spectrum shows the presence of
H$\alpha$ emission over the stellar absorption. Radio continuum emission 
detected by Ratag (1991).  

\item{1015*} The bright (m$_V$ = 11.6) optical counterpart shows a 
clear emission in H$\alpha$ over an F-type stellar continuum. A 
detailed study of this object  can be found in Arkhipova and 
Ikonnikova (1994). 

\item{1017*} Probably associated to the nearby dark cloud LDN 1003. 
The optical counterpart shows a clear emission in H$\alpha$ over the
stellar continuum.

\item{1019*} Probably associated to the nearby dark cloud LDN 988.
The bright (m$_V$ = 11.6) optical counterpart shows a 
strong H$\alpha$ emission with P-Cygni profile, together with 
multiple faint emission lines of iron over a G-type stellar continuum. 
Previously measured in the near infrared by Cohen (1974) who 
report the following magnitudes: $K$ = 7.75; $K-L$ = 1.45. 

\item{1024*} The faint optical counterpart shows a clear emission in 
H$\alpha$ over a stellar continuum of undetermined spectral type.
H$_2$O maser emission not detected by Wouterloot et al. (1993). 
CS (2$\rightarrow$1) emission not detected by Bronfman et al. (1996).

\item{1026*} The spectrum of the possible optical counterpart 
corresponds to a reddened F-type star with no emission lines.

\item{1031*} According to the far infrared colours, it should be 
classified as a planetary nebula. However, assuming a distance of
7 kpc as derived from HI radio observations, a very high luminosity
is obtained, which has been argued by several authors to 
identify this IRAS source as a compact HII region (Zijlstra et al. 
1990).

\item{1032*} The spectrum of the possible optical counterpart 
corresponds to an intermediate-type star with no emission lines. 
More observations are needed to confirm that this is the right 
counterpart. H$_2$O maser emission detected by Likkel (1989). 

\item{1040*} There is a very faint optical counterpart on the red 
Palomar print located in the center of a large nebulosity, associated 
to the nearby star forming region IC 1396. 
H$_2$O maser emission detected 
by Wouterloot et al. (1993) and Gyulbudaghian et al. (1990). 
Detected also in CS (2$\rightarrow$1) by Bronfman et al. (1996).

\item{1041*} Probably associated also to the nearby IC 1396 complex.
H$_2$O maser emission not detected by Wouterloot et al. 
(1993). 

\item{1043*} The optical counterpart seems to be a faint star of
intermediate spectral type with no emission lines. 

\item{1044*} H$_2$O maser emission not detected by Likkel (1989). 

\item{1046*} H$_2$O maser emission detected by Wouterloot et al. (1993). 

\item{1047*} New very low excitation compact planetary nebula 
discovered during this survey. 

\item{1048*} One of the few objects in which both CO and OH emission 
have been detected. The IRAS source has tentatively been classified 
as a non-variable OH/IR star because it shows a very low
IRAS variability index. However, it is located in the region of the 
IRAS two-colour diagram where many other variable OH/IR stars 
are found, which makes this identification uncertain. 
HCN emission not detected by Omont et al. (1993). 
H$_2$O maser emission not detected (Zuckerman \&  Lo 1987; 
Wouterloot et al. 1993).

\item{1049*} Probably associated to the dark cloud LDN 1143. 
H$_2$O maser emission not detected (Gyulbudaghian et al.
1987; Wouterloot et al. 1993). 

\item{1051*} The optical counterpart is a bright (m$_V$ $\sim$11) 
B-type star which shows the presence of very low excitation nebular
emision lines overimposed on the spectrum of the central star. 
The detection of radio continuum emission (Ratag 1991) confirms 
the identification of this IRAS source as a new planetary nebula. 

\item{1052*} The counterpart of this IRAS source is not the bright 
nearby star SAO 34043, but a bright near infrared source located 35" 
south and 15" west of it, with a very faint and red 
optical counterpart. The high expansion velocity (24.5 km s$^{-1}$) 
derived from the OH maser emission and the position in the IRAS 
two-colour diagram indicate that the progenitor star is 
probably massive. On the other hand, the object shows a very low IRAS
variability index and it has been measured in 
the near infrared at three different epochs showing only small 
variations in brightness, which suggest its classification as a 
non-variable OH/IR star. H$_2$O maser emission not detected (Zuckerman 
\& Lo 1987; Wouterloot et al. 1993). 

\item{1054*} The spectrum of the optical counterpart seems to be a 
red G-type star with no emission lines. Additional observations are
needed to confirm that this is the right counterpart.  Previous near 
infrared photometry is available in Campbell et al. (1989). 
They report the following values: $K$ = 10.60; $J-H$ = 2.09; $H-K$ = 
2.55; $K-L$ = 2.87; $L-M$ = 2.64 H$_2$O maser emission detected by  
Wouterloot et al. (1993). 

\item{1058*} The spectrum of the optical counterpart corresponds to a 
bright star with no emission lines, classified as G0Ia by Hrivnak 
(1995). We have detected the presence of a faint H$\alpha$ emission 
over the stellar absorption.  Additional near infrared photometry is 
available in Kwok et al. (1995). They report the following values:
$K$ = 7.25; $J-H$ = 0.43; $H-K$ = 0.21. They also suggest that the 
object is a C-rich post-AGB star, since the IRAS LRS shows the 
characteristic 21 $\mu$m  emission feature (Kwok et al. 1995). 
In addition, HCN has also been detected by Omont et al. (1993).
H$_2$O maser emission not detected by Likkel (1989). 

\item{1059*} The optical counterpart is a bright (m$_V$ = 9.6) 
star whose spectral type is classified as G2I by Kastner and 
Weintraub (1995) and Zacs et al. (1995), although the star is classified
as M0 in the SAO catalogue. Zacs et al. (1995) 
find the object metal-poor and C-rich, 
with a strong enrichment in s-process elements. The C-rich nature is 
confirmed by the detection of HCN emission  (Lindqvist et al. 1988; 
Likkel 1989; Omont et al. 1993) and by the presence of the 21 $\mu$m 
emission feature in its 
IRAS LRS spectrum  (Kwok et al. 1989). Geballe et al. (1992) report 
the possible presence of PAH's features in the infrared spectrum of this star.
Additional near infrared photometry is available in van der Veen et al. 
(1989), who report the following magnitudes: $K$ = 4.72; $J-H$ = 0.34;
$H-K$ = 0.25; $K-L'$ = 0.41; $L'-M$ = 0.45, and only in the $K$ band by 
Kastner and Weintraub (1995), who give $K$ = 4.8. 
H$_2$O maser emission not detected (Zuckerman \& Lo 1987; Wouterloot 
et al. 1993). CS (2$\rightarrow$1) emission detected by Lindqvist et al. 
(1988) and CS (3$\rightarrow$2) emission by Omont et al. (1993).

\item{1062*} Its location on the red Palomar print coincides with a large 
nebulosity associated to the HII region S139. Detected in CS 
(2$\rightarrow$1) by Bronfman et al. (1996).

\item{1068*} New very low excitation heavily reddened bipolar planetary 
nebula discovered during this survey. A detailed analysis can be found 
in Garc\'\i a-Lario et al. (1991).

\item{1072*} H$_2$O maser emission not detected by Wouterloot and Walmsley 
(1986). NH$_3$ emission detected by Wouterloot et al. (1988). The spectrum of
the possible counterpart corresponds to a red A-type star. 

\item{1073*} Although far from any known molecular cloud and showing 
unusual colours for a young object, this IRAS source has
recently been identified as a T-Tauri star by Whitelock et al. (1995). 
This identification is based on the small amplitude and rapid variations 
observed in 
the near infrared and confirms a previous identification of this star as 
a young stellar object by  Downes and Keyes (1988) and by Gregorio-Hetem 
et al. (1992). Whitelock et al. (1995) report the following mean near infrared
magnitudes: $K$ = 7.41; $J-H$ = 1.12; $H-K$ = 0.91. The optical spectrum 
displays, together with a strong and broad H$\alpha$ emission which might be 
originated in a circumstellar disk,  forbidden nebular emission lines of
[N II] and [S II], and the underlying continuum  corresponds to a 
G-type star with m$_V$ $\sim$ 12.5. 

\item{1078*} The optical spectrum of the relatively bright (m$_V$ = 13.15)
counterpart corresponds to a G2I type star, according to Hrivnak (1995). 
Identified as a C-rich post-AGB star by Kwok et al. (1989) because of the 
presence of the characteristic 21$\mu$m emission feature in its IRAS 
LRS spectrum and the detection of HCN emission by Omont et al. (1993). 
Tentatively  detected in CS (3$\rightarrow$2) by Omont et al. (1993). 
Previous near infrared photometry is available in Hrivnak and Kwok (1991). 
They report the following values: $K$ = 7.67; $J-H$ = 0.72; $H-K$ = 0.16. 
H$_2$O maser emission not detected (Likkel 1989). 

\item{1079*} The IRAS position coincides with the central star of a large 
nebulosity clearly visible on the Palomar prints, which corresponds to the 
HII region S163. Not detected in CS (2$\rightarrow$1) 
by Bronfman et al. (1996).

\item{1083*} Probably associated to the dark cloud LDN 1252, the 
spectrum of the optical counterpart shows a clear H$\alpha$ emission 
over a K-type stellar continuum.
\end{description}

\vspace{0.2cm}
\hrule
\end{document}
