2012A&A...537A...1A


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.06CET15:27:35

2012A&A...537A...1A - Astronomy and Astrophysics, volume 537A, 1-1 (2012/1-1)

Distinguishing between HII regions and planetary nebulae with Hi-GAL, WISE, MIPSGAL, and GLIMPSE.

ANDERSON L.D., ZAVAGNO A., BARLOW M.J., GARCIA-LARIO P. and NORIEGA-CRESPO A.

Abstract (from CDS):

HII regions and planetary nebulae (PNe) both emit at radio and infrared (IR) wavelengths, and angularly small HII regions can be mistaken for PNe. This problem of classification is most severe for HII regions in an early evolutionary stage, those that are extremely distant, or those that are both young and distant. Previous work has shown that HII regions and PNe can be separated based on their infrared colors. Using data from the Herschel Hi-GAL survey, as well as WISE and the Spitzer MIPSGAL and GLIMPSE surveys, we wish to establish characteristic IR colors that can be used to distinguish between HII regions and PNe. We perform aperture photometry measurements for a sample of 126 HII regions and 43 PNe at wavelengths from 8.0µm to 500µm. We find that HII regions and PNe have distinct IR colors. The most robust discriminating color criteria are [F12/F8]<0.3, [F160/F12]>1.3, and [F160/F24]>0.8 (or alternately [F160/F22]>0.8), where the brackets indicate the log of the flux ratio. All three of these criteria are individually satisfied by over 98% of our sample of HII regions and by ∼10% of our sample of PNe. Combinations of these colors are more robust in separating the two populations; for example all HII regions and no PNe satisfy [F12/F8]<0.4 and [F160/F22]>0.8. When applied to objects of unknown classification, these criteria prove useful in separating the two populations. The dispersion in color is relatively small for HII regions; this suggests that any evolution in these colors with time for HII regions must be relatively modest. The spectral energy distributions (SEDs) of HII regions can be separated into ``warm'' and ``cold'' components. The ``cold'' component is well-fit by a grey-body of temperature 25K. The SEDs of nearly two-thirds of our sample of HII regions peak at 160µm and one third peak at 70µm. For PNe, 67% of the SEDs peak at 70µm, 23% peak at either 22µm or 24µm, and 9% (two sources) peak at 160µm.

Abstract Copyright:

Journal keyword(s): infrared: ISM - stars: formation - dust, extinction - planetary nebulae: general - HII regions

VizieR on-line data: <Available at CDS (J/A+A/537/A1): hii.dat pn.dat>

Nomenclature: Table 1: [AZB2012] GLLL.lll+BB.bbb N=126.

Simbad objects: 80

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Number of rows : 80

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 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14374 1
2 IC 418 PN 05 27 28.2060343141 -12 41 50.282659007   9.78 13.0     O7fp 993 2
3 PN G296.7-00.2 PN 11 57 47.5 -62 26 21           ~ 4 1
4 PN G298.4+00.6 PN 12 13 09.0 -61 50 28           ~ 6 0
5 WRAY 16-115 PN 12 28 46.8457795246 -63 44 37.072611293     15.70     ~ 54 0
6 PN G301.1-00.4 PN 12 35 21.4 -63 18 01           ~ 5 1
7 PN G301.2+00.4 PN 12 37 09.6 -62 23 10           ~ 4 0
8 WRAY 17-56 PN 12 46 26.9183087659 -63 24 27.878516187     16.9 15.1 15.553 ~ 17 1
9 PN G305.6-00.9 PN 13 15 30.4 -63 38 43           ~ 6 1
10 PN Th 2-A PN 13 22 33.79 -63 21 01.3     15.00     ~ 83 0
11 PN G308.1-00.5 PN 13 37 54.9 -62 58 54           ~ 6 1
12 WRAY 16-133 PN 13 42 36.1511904624 -61 22 28.861409573     15.86     ~ 48 0
13 [GGB2012] G308.9176+00.1231 HII 13 43 02.1 -62 08 52           ~ 59 0
14 GAL 309.55-00.74 HII 13 49 56.4 -62 51 18           ~ 7 0
15 GRS G312.95 -00.45 HII 14 17 23.0 -61 38 14           ~ 7 0
16 PN G313.3+00.3 PN 14 18 27.489 -60 47 10.49           ~ 11 0
17 WRAY 16-156 PN 14 33 17.97 -60 49 36.3   16.3 16.7   15.38 ~ 155 0
18 PHR J1437-5949 PN 14 37 53.2 -59 49 25           ~ 8 1
19 IRAS 14345-5858 PN 14 38 19.99 -59 11 46.1           ~ 13 0
20 GAL 318.05+00.08 HII 14 53 43.6 -59 08 57           ~ 3 0
21 PN G318.9+00.7 PN 14 57 35.7 -58 12 09           ~ 12 1
22 MSX6C G320.3311-00.3069 HII 15 10 36.7 -58 23 48           ~ 5 1
23 PN G321.0-00.7 PN 15 16 31.9 -58 23 14           ~ 6 0
24 BMP J1522-5729 PN 15 22 58.997 -57 29 59.59           ~ 8 1
25 PN G322.4-00.1 a PN 15 23 22.5 -57 10 48           ~ 6 1
26 PN Pe 2-8 PN 15 23 42.8864008345 -57 09 25.223411201     15.50     ~ 71 0
27 PN G322.2-00.7 PN 15 24 24.0 -57 46 21           ~ 9 1
28 [CH87] 324.192+0.109 HII 15 32 52.8 -55 56 59           ~ 8 0
29 PN G328.3+00.7 PN 15 52 56.8 -52 54 12           ~ 9 1
30 PN G329.6-00.4 PN 16 04 14.8 -52 59 06           ~ 4 0
31 PN G329.5-00.8 PN 16 05 37.41 -53 19 54.0           ~ 6 1
32 GAL 330.31-00.39 HII 16 07 38 -52 31.5           ~ 8 0
33 IRAS 16056-5125 HII 16 09 24.5 -51 33 08           ~ 4 0
34 PN G332.5-00.1 PN? 16 16 56.40 -50 47 22.6           ~ 4 1
35 PMR 5 WR* 16 19 40.1911099790 -49 13 59.027412470           [WN6]: 31 2
36 PN G333.7+00.3 PN? 16 20 09.4 -49 36 09           ~ 5 0
37 IRAS 16168-5006 HII 16 20 37.4 -50 13 40           ~ 5 0
38 GAL 334.53+00.83 HII 16 21 45 -48 44.1           ~ 7 0
39 PN G337.3+00.6 PN 16 33 58.0 -46 50 07           ~ 11 1
40 PHR J1639-4516 PN 16 39 22.3 -45 16 35           ~ 9 1
41 IRAS 16387-4612 HII 16 42 24.9 -46 18 00           ~ 3 0
42 IRAS 16396-4429 Y*? 16 43 15.984 -44 35 17.88           ~ 20 1
43 IRAS 16445-4459 HII 16 48 05.2 -45 05 09           ~ 15 0
44 PN H 1-3 PN 16 53 31.33 -42 39 22.8     14.00     ~ 42 0
45 PN G342.2-00.3 PN 16 56 33.97 -43 46 14.7           ~ 15 0
46 PN H 1-5 PN 16 57 23.7496825639 -41 37 58.197783456     15.00     ~ 39 0
47 GAL 344.23-00.59 HII 17 04 12.4 -42 19 26           ~ 6 0
48 IC 4637 PN 17 05 10.47 -40 53 07.7     9.20     ~ 123 0
49 HRDS G346.077-00.056 HII 17 07 54.1 -40 31 36           ~ 4 0
50 GAL 345.22-00.75 HII 17 08 06.4 -41 37 56           ~ 5 0
51 IRAS 17052-4001 HII 17 08 42.840 -40 05 06.36           ~ 12 0
52 HRDS G346.875+00.328 HII 17 08 47.1 -39 39 26           ~ 3 0
53 HRDS G346.099-00.364 HII 17 09 16.3 -40 41 37           ~ 2 0
54 GAL 347.39+00.27 HII 17 10 37.1 -39 17 02           ~ 6 0
55 HRDS G347.536+00.084 HII 17 11 50.2 -39 16 12           ~ 2 0
56 HRDS G348.148+00.255 HII 17 12 58.8 -38 40 30           ~ 3 0
57 NGC 6302 PN 17 13 44.339 -37 06 10.95   7.1 10.10     ~ 749 1
58 PN G347.2-00.8 PN 17 14 49.1902267133 -40 06 07.480513443           ~ 8 1
59 PN G356.9+00.9 PN 17 34 34.333 -31 02 07.68           ~ 9 1
60 PN G358.6+00.7 PN 17 39 22.70 -29 41 46.1           ~ 15 0
61 [LPH96] 000.640+0.623 HII 17 44 43.1 -28 03 52           ~ 4 0
62 PN G001.1+00.8 PN 17 45 11.085 -27 32 38.00           ~ 11 0
63 PN G001.6+00.9 PN 17 45 37.36 -27 01 18.4           ~ 6 0
64 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11077 0
65 PN G001.2+00.7 PN 17 45 46.88 -27 30 42.0           ~ 8 0
66 PN M 1-26 PN 17 45 57.6652777318 -30 12 00.874208077   12.89 12.08 12.00   [WR] 201 0
67 HRDS G000.838+00.189 HII 17 46 52.1 -28 07 20           ~ 3 0
68 PN G358.6-01.1 PN 17 46 52.20 -30 37 42.8           ~ 5 0
69 PN Hb 5 PN 17 47 56.20 -29 59 39.6   10.50 10.78     ~ 249 0
70 Terz N 2337 PN 17 48 45.272 -26 43 28.80           ~ 12 0
71 PN G001.6+00.1 PN 17 48 46.174 -27 25 38.73           ~ 11 0
72 HRDS G001.488-00.199 HII 17 49 53.6 -27 45 54           ~ 2 0
73 PN G000.0-01.0 PN 17 50 10.00 -29 19 02.4           ~ 11 0
74 PN G000.0-01.2 PN 17 50 23.174 -28 33 07.28           ~ 13 0
75 PN G000.7-00.8 PN 17 50 46.857 -28 44 39.04           ~ 9 0
76 PN G000.6-01.0 PN 17 51 11.504 -28 56 26.16           ~ 13 0
77 JaSt 81 PN 17 52 04.283 -27 36 38.06           ~ 9 0
78 PN G001.5-00.7 PN 17 52 08.717 -28 02 16.56           ~ 13 0
79 HRDS G002.961-00.053 HII 17 52 42.8 -26 25 29           ~ 2 0
80 HRDS G002.009-00.680 HII 17 52 57.8 -27 33 49           ~ 2 1

    Equat.    Gal    SGal    Ecl

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2019.12.06-15:27:35

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