J/ApJS/124/195 PN medium-resolution spectra (Hora+, 1999)
Investigating the near-infrared properties of planetary nebulae.
II. Medium-resolution spectra.
Hora J.L., Latter W.B., Deutsch L.K.
<Astrophys. J. Suppl. Ser., 124, 195-240 (1999)>
=1999ApJS..124..195H 1999ApJS..124..195H
ADC_Keywords: Planetary nebulae ; Spectra, infrared
Keywords: infrared: ISM: continuum - infrared: ISM: lines and bands -
ISM: molecules - ISM: structure - molecular processes -
planetary nebulae: general
Abstract:
We present medium-resolution (R∼700) near-infrared (lambda=1-2.5m)
spectra of a sample of planetary nebulae (PNe). A narrow slit was used
which sampled discrete locations within the nebulae; observations were
obtained at one or more positions in the 41 objects included in the
survey. The PN spectra fall into one of four general categories: HI
emission line-dominated PNe, HI and H2 emission line PNe, H2
emission line-dominated PNe, and continuum-dominated PNe. These
categories correlate with morphological type, with the elliptical PNe
falling into the first group, and the bipolar PNe primarily in the
H2 and continuum emission groups. The categories also correlate with
C/O ratio, with the O-rich objects generally falling into the first
group and the C-rich objects in the other groups. Other spectral
features were observed in all categories, such as continuum emission
from the central star, C2, CN, and CO emission, and warm dust
continuum emission toward the long wavelength end of the spectra.
Molecular hydrogen was detected for the first time in four PNe. An
excitation analysis was performed using the H2 line ratios for all
of the PN spectra in the survey where a sufficient number of lines
were observed.
Description:
The observations were performed on several runs during the period 1992
October through 1994 September at the University of Hawaii 2.2m
telescope on Mauna Kea, using the near-IR KSPEC spectrograph
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
objects.dat 101 41 PN positions (from Simbad)
table1.dat 194 41 PN survey summary
fluxes.dat 77 4963 Line fluxes
table8.dat 64 28 H2 excitation analysis results
sp/* . 83 Ascii files of individual spectra
fits/* . 83 FITS files of individual spectra
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See also:
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992)
V/127 : MASH Catalog of Planetary Nebulae (Parker+ 2006)
Byte-by-byte Description of file: objects.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name PN name
15- 16 I2 h RAh Simbad right ascension (J2000)
18- 19 I2 min RAm Simbad right ascension (J2000)
21- 26 F6.3 s RAs Simbad right ascension (J2000)
28 A1 --- DE- Simbad declination sign (J2000)
29- 30 I2 deg DEd Simbad declination (J2000)
32- 33 I2 arcmin DEm Simbad declination (J2000)
35- 40 F6.3 arcsec DEs Simbad declination (J2000)
42- 55 A14 --- Lines1 Line fluxes: first source name in fluxes.dat
57- 70 A14 --- Lines2 Line fluxes: second source name in fluxes.dat
72- 85 A14 --- Lines3 Line fluxes: third source name in fluxes.dat
87-101 A15 --- SName Simbad name of the PN
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/41] Sequential number
4- 14 A11 --- Name Object name
15 A1 --- n_Name [e] e: New detection of H2
16- 17 I2 h RAh Right ascension (J2000)
19- 20 I2 min RAm Right ascension (J2000)
22- 27 F6.3 s RAs Right ascension (J2000)
29 A1 --- DE- Declination sign (J2000)
30- 31 I2 deg DEd Declination (J2000)
33- 34 I2 arcmin DEm Declination (J2000)
36- 40 F5.2 arcsec DEs Declination (J2000)
42- 51 A10 --- PNG PNG designation (1)
53- 62 A10 "YYYY-MM-DD" ObsDate Observation date (UT)
63 A1 --- --- [&]
64- 68 A5 --- ObsDate2 Additional observation date (MM-DD)
70- 74 A5 --- Slit Slit orientation
76- 99 A24 --- Pos Positions information (2)
101-119 A19 --- SpecComp Spectral components (3)
121-123 A3 --- MClass Classical morphology (4)
125-136 A12 --- Sp1 Name of spectrum file in subdirectory sp (5)
138-151 A14 --- Sp2 Name of spectrum file in subdirectory sp (5)
153-166 A14 --- Sp3 Name of spectrum file in subdirectory sp (5)
168-180 A13 --- Sp4 Name of spectrum file in subdirectory sp (5)
182-194 A13 --- Sp5 Name of spectrum file in subdirectory sp (5)
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Note (1): Strasbourg Planetary Nebulae catalog number
(Acker et al., 1992, Cat. V/84)
Note (2): Unless otherwise specified, the slit was centered on the
brightest part of component specified. CS = Central Star
Note (3): Spectral components are:
H1 = hydrogen recombination lines
H2 = molecular hydrogen
Cs = stellar continuum
Cw = warm dust continuum
CO = CO bandhead emission
Note (4): Classical morphology categories as follows:
E = elliptical
eE = early elliptical
mE = middle elliptical
lE = late elliptical
B = Bipolar
mB = middle Bipolar
Ri = ring
Ro = round
eRo = early round
S = stellar (i.e., unresolved)
P = peculiar
I = irregular
Note (5): The spectra are also available as FITS files in the "fits"
subdirectory. The name is the same as in the "sp" subdirectory but
with the .fit extension instead of .dat.
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Byte-by-byte Description of file: fluxes.dat
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Bytes Format Units Label Explanations
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1 A1 --- n_Source [1-3] Source features (1)
3- 16 A14 --- Source Source designation (2)
18- 22 I5 0.1nm lambda Wavelength (3)
24- 31 F8.3 10-17W/m2 Flux ?=9.99 Line flux (4)
32- 36 F5.2 10-17W/m2 e_Flux ?=9.99 rms uncertainty on Flux
38- 77 A40 --- Ident Identification (5)
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Note (1): Flag as follows:
2 = H I PN (tables 2-4)
2 = H2 + HI PN (table 5-6)
3 = H2-dominated PN, HII region (table7)
Note (2):
-- For Hb 12 sources, see See Hora & Latter (1996ApJ...461..288H 1996ApJ...461..288H)
for an explanation of slit positions
-- For M2-9 and AFGL 2688 sources, See Hora & Latter
(1994ApJ...437..281H 1994ApJ...437..281H) for an explanation of slit positions
Note (3): These are the measured wavelengths, with a 1σ error of ∼5Å.
Note (4): Fluxes are in units of 10-14erg/cm2/s, and have not been
corrected for extinction.
Note (5): Uc for unidentified lines observed in several other PNe (see text)
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name Object/Position
20- 23 A4 -- UV [Yes/No ?-] Presence of UV-excited H2 lines
24 I1 --- n_UV [4/6]? Note (1)
26- 29 I4 K Tex(J) ?=- Excitation temperature (2)
31- 33 I3 K E_Tex(J) ? Error on Tex(J) (upper limit)
35- 37 I3 K e_Tex(J) ? Error on Tex(J) (lower limit)
40- 43 F4.2 --- UVratio ?=- H2 2-1S(1)/1-0S(1) line ratio
(λ=22471/21213Å)
45- 47 F3.1 --- O/P ?=- ortho-to-para (O/P) H2 abundance ratio (3)
49- 51 F3.1 --- e_O/P ? rms uncertainty on O/P
53- 55 F3.1 mag AV ?=- Visual attenuation (4)
57- 60 F4.1 mag E_AV ? Error on AV (upper limit)
62- 64 F3.1 mag e_AV ? Error on AV (lower limit)
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Note (1): Note as follows:
4 = v=1 detections only.
5 = v=8 transition(s) detected.
6 = means there are not enough lines detected to make an
excitation analysis.
Note (2): For UV excited spectra Tex(J) is the rotational excitation
temperature. For collisionally excited spectra Tex(J)=Tex(v).
Note (3): Listed only for those objects with enough lines well detected
to make an estimate of the O/P ratio (see Sternberg & Neufeld,
1999ApJ...516..371S 1999ApJ...516..371S)
Note (4): Value of visual attenuation used to deredden the H2 spectra
for the excitation analysis (as determined from the H2 lines only
and using a standard interstellar extinction law; Rieke & Lebofsky,
1985ApJ...288..618R 1985ApJ...288..618R). Entries with errors shown are determined to
greater accuracy than those without, which should be considered highly
uncertain. In no case does the value of AV change the basic results
of the analysis.
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Acknowledgements:
Joseph Hora, jhora(at)cfa.harvard.edu
References:
Latter et al., Paper I 1995ApJS..100..159L 1995ApJS..100..159L
(End) Patricia Vannier [CDS] 18-Oct-2007