1999ApJS..124..195H


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.22CEST01:06:06

1999ApJS..124..195H - Astrophys. J., Suppl. Ser., 124, 195-240 (1999/September-0)

Investigating the near-infrared properties of planetary nebulae. II. Medium-resolution spectra.

HORA J.L., LATTER W.B. and DEUTSCH L.K.

Abstract (from CDS):

We present medium-resolution (R∼700) near-infrared (λ=1-2.5 µm) 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: H I emission line-dominated PNe, H I 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. From the near-infrared spectrum, we determined an ortho-to-para ratio, the rotational and vibrational excitation temperatures, and the dominant excitation mechanism of the H2 for many objects surveyed. One unexpected result from this analysis is that the H2 is excited by absorption of ultraviolet photons in most of the PNe surveyed, although for several PNe in our survey collisional excitation in moderate velocity shocks plays an important role. The correlation between bipolar morphology and H2 emission has been strengthened with the new detections of H2 in this survey. We discuss the role of winds and photons to the excitation of H2 in PNe, and consider some implications to the utility of H2 as a nebular diagnostic and to our understanding of PNe structure and evolution.

Abstract Copyright:

Journal keyword(s): Infrared: ISM: Continuum - Infrared: ISM: Lines and Bands - ISM: Molecules - ISM: Structure - Molecular Processes - ISM: Planetary Nebulae: General

VizieR on-line data: <Available at CDS (J/ApJS/124/195): objects.dat table1.dat fluxes.dat table8.dat fits/*>

Simbad objects: 41

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Number of rows : 41

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 40 PN 00 13 01.0170260109 +72 31 19.032886305   11.63 11.46     [WC8] 595 2
2 IC 351 PN 03 47 32.9811922252 +35 02 48.633107981   13.11 12.27 14.35   Of(H) 251 0
3 IC 2003 PN 03 56 21.9883931981 +33 52 30.752777910   13.11 11.87 13.44   [WC3?] 244 0
4 NGC 1535 PN 04 14 15.7689951134 -12 44 21.934169738   12.01 12.82     sdO3: 504 0
5 PN M 4-18 PN 04 25 50.8357219366 +60 07 12.778708522   14.22 13.96     [WC11] 170 0
6 RAFGL 618 pA* 04 42 53.6245215366 +36 06 53.397219192   16.32   12.59   C-rich 967 0
7 Jonckheere 320 PN 05 05 34.2774523754 +10 42 22.923399381           O3V(f) 275 2
8 IC 418 PN 05 27 28.2060343141 -12 41 50.282659007   9.78 13.0     O7fp 1006 2
9 NGC 2022 PN 05 42 06.1905641397 +09 05 10.584345578   14.9 14.2     [WC] 350 0
10 IC 2149 PN 05 56 23.9008985692 +46 06 17.206983220   11.21 11.35     O7.5 420 0
11 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 727 0
12 PN VV 28 PN 06 25 57.2723419700 +17 47 27.124872408     12.5     [WC] 283 0
13 NGC 2346 PN 07 09 22.5216571385 -00 48 23.611157830   11.76 11.58     A5V 557 0
14 NGC 2392 PN 07 29 10.7669120392 +20 54 42.478515772     9.68     O6f 703 1
15 PN M 1-16 PN 07 37 18.902 -09 38 47.96   12.7       ~ 176 0
16 NGC 2440 PN 07 41 54.91 -18 12 29.7   18.9       ~ 632 2
17 NGC 3242 PN 10 24 46.1335198512 -18 38 32.294434711   11.83 12.15     ~ 805 1
18 IC 3568 PN 12 33 06.8549263326 +82 33 50.203860251   11.809 10.730 12.651   ~ 391 0
19 IC 4593 PN 16 11 44.5480003321 +12 04 17.033164436   10.91 10.84     O7fp 441 0
20 NGC 6210 PN 16 44 29.5195973291 +23 47 59.491267229   12.3 11.7     Of/[WR] 576 0
21 PN M 2-9 PN 17 05 37.952 -10 08 34.58   12.59 14.7     Be 507 0
22 NGC 6543 PN 17 58 33.4042519454 +66 37 58.748961810   11.09 11.28     [WC] 1133 1
23 NGC 6572 PN 18 12 06.3140077888 +06 51 13.030152295   9.3 10.8     [WC] 740 0
24 M 57 PN 18 53 35.0969571234 +33 01 44.883146221   15.405 15.769 15.901 16.062 DA(O?) 797 2
25 NGC 6790 PN 19 22 56.966 +01 30 46.46   12.52 10.45     wels 314 0
26 PN Vy 2-2 PN 19 24 22.2390166933 +09 53 56.259102426   14.02 12.65 13.38   ~ 251 0
27 IRC +10420 pA* 19 26 48.0981288433 +11 21 16.756524951   13.98 11.66     F8Ia+e 458 0
28 NGC 6803 PN 19 31 16.47 +10 03 21.7     15.2     ~ 244 0
29 HD 184738 PN 19 34 45.2337512278 +30 30 58.951476338   10.41 10.44     [WC9] 925 0
30 Min 1-92 pA* 19 36 18.9292148675 +29 32 49.838032394 12.13 12.35 11.75 11.54   B0.5IV[e] 237 1
31 NGC 6826 PN 19 44 48.1500835472 +50 31 30.250916761   10.21 9.6     O6fp 704 0
32 V* V1610 Cyg pA* 21 02 18.27 +36 41 37.0           F5Iae 840 1
33 NGC 7009 PN 21 04 10.8153350719 -11 21 48.581808296   12.48 12.07     ~ 972 1
34 NGC 7026 PN 21 06 18.5721833093 +47 51 06.780221314   15.33 15.1     [WC3] 407 1
35 NGC 7027 PN 21 07 01.571952 +42 14 10.47120   10.358 8.831 10.157   ~ 2363 1
36 IRAS 21190+5140 HII 21 20 44.8 +51 53 28           ~ 128 2
37 [D75b] Em* 21-021 PN 21 29 58.4712776885 +51 04 00.323547316   15.66 14.20 13.89   O7(f)/[WC11] 229 0
38 PN K 4-45 Y*O 21 35 21.061 +53 47 11.21           ~ 55 2
39 NGC 7662 PN 23 25 53.6 +42 32 06   9.4 12     ~ 913 0
40 PN Hb 12 PN 23 26 14.8207203464 +58 10 54.538636094   13.51 11.49 12.44   Oe 317 0
41 PN M 2-56 pA* 23 56 36.4101419399 +70 48 18.253127954   19.81 17 17.27 17.64 Be 89 0

    Equat.    Gal    SGal    Ecl

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2021.06.22-01:06:06

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