2002A&A...390.1089P


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.31CET13:01:52

2002A&A...390.1089P - Astronomy and Astrophysics, volume 390, 1089-1113 (2002/8-2)

The rich 6 to 9 µm spectrum of interstellar PAHs.

PEETERS E., HONY S., VAN KERCKHOVEN C., TIELENS A.G.G.M., ALLAMANDOLA L.J., HUDGINS D.M. and BAUSCHLICHER C.W.

Abstract (from CDS):

IR spectroscopy provides a valuable tool for the characterisation and identification of interstellar molecular species. Here, we present 6-9µm spectra of a sample of reflection nebulae, HII regions, YSOs, evolved stars and galaxies that show strong unidentified infrared bands, obtained with the SWS spectrograph on board ISO. The IR emission features in this wavelength region show pronounced variations. 1) The 6.2µm feature shifts from 6.22 to 6.3µm and clearly shows profile variations. 2) The 7.7µm complex is comprised of at least two subpeaks peaking at 7.6 and one longwards of 7.7µm. In some cases the main peak can apparently shift up to 8µm. Two sources do not exhibit a 7.7µm complex but instead show a broad emission feature at 8.22µm. 3) The 8.6µm feature has a symmetric profile in all sources and some sources exhibit this band at slightly longer wavelengths. For the 6.2, 7.7 and 8.6µm features, the sources have been classified independently based on their profile and peak position. The classes derived for these features are directly linked with each other. Sources with a 6.2µm feature peaking at ∼6.22µm exhibit a 7.7µm complex dominated by the 7.6µm component. In contrast, sources with a 6.2µm profile peaking longwards of 6.24µm show a 7.7µm complex with a dominant peak longwards of 7.7µm and a 8.6µm feature shifted toward the red. Furthermore, the observed 6-9µm spectrum depends on the type of object. All ISM-like sources and a few PNe and Post-AGB stars belong to the first group while isolated Herbig AeBe stars, a few Post-AGB stars and most PNe belong to the second group. We summarise existing laboratory data and theoretical quantum chemical calculations of the modes emitting in this wavelength region of PAH molecules. We discuss the variations in peak position and profile in view of the exact nature of the carrier. We attribute the observed 6.2µm profile and peak position to the combined effect of a PAH family and anharmonicity with pure PAHs representing the 6.3µm component and substituted/complexed PAHs representing the 6.2µm component. The 7.6µm component is well reproduced by both pure and substituted/complexed PAHs but the 7.8µm component remains an enigma. In addition, the exact identification of the 8.22µm feature remains unknown. The observed variations in the characteristics of the IR emission bands are linked to the local physical conditions. Possible formation and evolution processes that may influence the interstellar PAH class are highlighted.

Abstract Copyright:

Journal keyword(s): circumstellar matter - stars: pre-main sequence - HII regions - ISM: molecules - planetary nebulae: general - infrared: ISM: lines and bands

CDS comments: Table 1: IRAS 02219+6125 is a misprint for IRAS 02219+6152.

Simbad objects: 63

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Number of rows : 63

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 2957 2
2 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 330 0
3 IC 1795 HII 02 25 43.5 +62 06 13           ~ 229 0
4 NAME W 3A 02219+6125 HII 02 25 44.6 +62 06 11           ~ 8 0
5 NAME AFGL 4029 IRS 1 Y*O 03 01 29.2 +60 29 12           ~ 109 1
6 LZK 12 Y*O 03 29 10.4138336046 +31 21 59.070333199   16.06 14.25     B5:V+F2: 128 0
7 NAME Orion Peak 1 PoC 05 35 13.57 -05 22 03.8           ~ 31 0
8 NAME Orion Peak 2 PoC 05 35 15.74 -05 22 39.9           ~ 20 0
9 [GSL2002] 16 HII 05 35 18.2 -05 24 40           ~ 5 0
10 NAME OrionBar D8 HII 05 35 18.22 -05 24 39.9           ~ 4 0
11 NAME OrionBar BRGA HII 05 35 19.31 -05 24 59.9           ~ 3 0
12 [GSL2002] 18 HII 05 35 19.8 -05 25 10           ~ 6 0
13 NAME OrionBar D5 HII 05 35 19.81 -05 25 10.0           ~ 8 0
14 NAME OrionBar H2S1 HII 05 35 20.31 -05 25 20.0           ~ 9 0
15 NAME OrionBar D2 HII 05 35 21.40 -05 25 40.1           O6 6 0
16 [VPT2002] Orion Bar 1 HII 05 35 21.4 -05 25 40           ~ 3 0
17 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 574 1
18 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 723 0
19 PN Vo 1 PN 06 59 26.4078328215 -79 38 47.129323563   16.7 15.8     [WC10] 94 0
20 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5371 6
21 HD 89353 pA* 10 18 07.5892879413 -28 59 31.194541133   5.76 5.53     B9.5Ib/II 288 0
22 [BNM96] 289.880-0.799 HII 11 00 59.4870059429 -60 50 22.774209522           ~ 35 0
23 HD 97048 Ae* 11 08 03.3105687971 -77 39 17.491180130 9.03 8.76 9.00   8.64 A0Vep 463 0
24 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 658 1
25 ESO 95-1 HII 12 09 01.260 -63 15 59.63     16.00     ~ 92 2
26 IRAS 12073-6233 mul 12 10 00.4 -62 49 57           ~ 47 0
27 [GS70] 298.2-00.3 HII 12 10 01.886 -62 50 00.46           ~ 65 1
28 IRAS 13416-6243 pA* 13 45 07.2570740611 -62 58 16.832906949           G1I 41 0
29 NAME Circinus Galaxy Sy2 14 13 09.906 -65 20 20.47   10.89 9.84 10.6 10.0 ~ 1019 2
30 WRAY 15-1269 PN 14 59 53.4814028450 -54 18 07.524725528 12.12 12.17 11.64 11.63   [WC11] 229 0
31 IRAS 15384-5348 HII 15 42 17.787 -53 58 30.88           ~ 37 1
32 GAL 327.3-00.5 HII 15 53 05.9 -54 35 21           ~ 17 0
33 IRAS 15502-5302 HII 15 54 07.2 -53 11 20           ~ 44 0
34 IRAS 16279-4757 pA* 16 31 38.7378047645 -48 04 05.640499647           M3II 39 0
35 CD-42 11721 Be* 16 59 06.7622892572 -42 42 08.404916931 12.16 12.28 11.00     B0IVe 155 1
36 NAME Water Lily Nebula pA* 17 03 10.0710345261 -47 00 27.733590141           B7 84 0
37 CPD-56 8032 PN 17 09 00.86008 -56 54 48.0957 11.24 11.48 11.04     [WC10] 250 0
38 IRAS 17279-3350 HII 17 31 18.0 -33 52 50           ~ 23 0
39 IRAS 17347-3139 PN 17 38 00.61 -31 40 55.2           ~ 55 1
40 V* XX Oph ** 17 43 56.4967929636 -06 16 08.787105588 10.51 9.81 8.59     M5IIe+Aep 140 0
41 PN Hb 5 PN 17 47 56.20 -29 59 39.6   10.50 10.78     ~ 253 0
42 GAL 009.62+00.19 HII 18 06 13.9 -20 31 44           ~ 188 0
43 GAL 013.88+00.28 HII 18 14 35.2 -16 45 21           ~ 54 0
44 NAME GGD 27 IRS RNe 18 19 12.0871543084 -20 47 50.895583646           ~ 26 1
45 EM* MWC 922 Be* 18 21 16.059408 -13 01 25.68432     13.80 13.65   B[e] 85 0
46 [WAM82] 023.955+0.152 HII 18 34 24.9 -07 54 50           ~ 70 1
47 GAL 029.96-00.02 Y*O 18 46 03.7 -02 39 21           ~ 334 1
48 [WWB83] G033.91+0.11 HII 18 52 50.4 +00 55 29           ~ 89 1
49 IRAS 18576+0341 s*b 19 00 10.89456 +03 45 47.1096           B8I 83 1
50 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 222 0
51 HD 184738 PN 19 34 45.2337512278 +30 30 58.951476338   10.41 10.44     [WC9] 922 0
52 SH 2-87 HII 19 46 20.7 +24 35 15           ~ 152 2
53 BD+40 4124 Ae* 20 20 28.2415737117 +41 21 51.527810947 11.11 11.36 10.62 10.510   B2Ve 276 1
54 NAME SH 2-106 IR Y*O 20 27 26.502 +37 22 42.03           ~ 157 1
55 NGC 7023 RNe 21 01 36.9 +68 09 48           ~ 640 0
56 V* V1610 Cyg pA* 21 02 18.27 +36 41 37.0           F5Iae 835 1
57 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2338 1
58 IRAS 21190+5140 HII 21 20 44.8 +51 53 28           ~ 128 2
59 [D75b] Em* 21-021 PN 21 29 58.4712776885 +51 04 00.323547316   15.66 14.20 13.89   O7(f)/[WC11] 227 0
60 HD 235858 pA* 22 29 10.3755939027 +54 51 06.341145584   11.40 9.52 8.47 7.34 G5Ia 238 0
61 SH 2-138 HII 22 32 45.7 +58 28 20           ~ 107 2
62 IC 1470 HII 23 05 09.9 +60 14 31   11.5       ~ 168 1
63 SH 2-159 Y*O 23 15 31.27440 +61 07 10.4450           ~ 176 2

    Equat.    Gal    SGal    Ecl

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2020.10.31-13:01:52

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