2015A&A...579A..67S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST04:35:11

2015A&A...579A..67S - Astronomy and Astrophysics, volume 579A, 67-67 (2015/7-1)

Herschel PACS and SPIRE spectroscopy of the photodissociation regions associated with S 106 and IRAS 23133+6050.

STOCK D.J., WOLFIRE M.G., PEETERS E., TIELENS A.G.G.M., VANDENBUSSCHE B., BOERSMA C. and CAMI J.

Abstract (from CDS):

Photodissociation regions (PDRs) contain a large portion of all of the interstellar matter in galaxies. Classical examples include the boundaries between ionized regions and molecular clouds in regions of massive star-formation, marking the point where all of the photons that are energetic enough to ionize hydrogen have been absorbed. To determine the physical properties of the PDRs associated with the star-forming regions IRAS 23133+6050 and S 106 and present them in the context of other Galactic PDRs associated with massive star-forming regions. We employ Herschel PACS and SPIRE spectroscopic observations to construct a full 55-650µm spectrum of each object from which we measure the PDR cooling lines, other fine- structure lines, CO lines, and the total far-infrared flux. These measurements (and combinations thereof) are then compared to standard PDR models. Subsequently, detailed numerical PDR models are compared to these predictions, yielding additional insight into the dominant thermal processes in the PDRs and their structures. We find that the PDRs of each object are very similar and can be characterized by a two-phase PDR model with a very dense, highly UV irradiated phase (n∼106cm–3, G0∼105) interspersed within a lower density, weaker radiation field phase (n∼104cm–3, G0∼104). We employed two different numerical models to investigate the data. We first used RADEX models to fit the peak of the 12CO ladder, which in conjunction with the properties derived, yielded a temperature of around 300 K. Subsequent numerical modeling with a full PDR model revealed that the dense phase has a filling factor of around 0.6 in both objects. The shape of the 12CO ladder was consistent with these components, with heating dominated by grain photoelectric heating. An extra excitation component for the hightest-J lines (J>20) is required for S 106.

Abstract Copyright:

Journal keyword(s): ISM: general - ISM: molecules - photon-dominated region (PDR) - infrared: ISM - stars: formation - stars: massive

Simbad objects: 25

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Number of rows : 25

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 W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 329 0
2 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 962 3
3 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 480 0
4 NAME Ori Complex Cld 05 35.3 -05 23           ~ 334 0
5 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 716 0
6 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1734 1
7 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 570 1
8 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1071 1
9 [BCB89] IRS 2b * 05 41 45.50 -01 54 28.7           O8V 34 1
10 NGC 2245 RNe 06 32 41.3 +10 09 34   11       A0 49 0
11 NGC 2316 Cl* 06 59 41.7 -07 46 07           ~ 45 1
12 NGC 3372 HII 10 44 19.0 -59 53 21           ~ 888 2
13 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1909 1
14 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1484 0
15 OH 34.26 +0.15 SFR 18 53 18.54 +01 14 57.9           ~ 460 0
16 W 49a SFR 19 10 15.7 +09 06 05           ~ 258 2
17 NAME SH 2-106 IR Y*O 20 27 26.502 +37 22 42.03           ~ 157 1
18 SH 2-106 HII 20 27 26.8 +37 22 49           ~ 409 2
19 NGC 7023 RNe 21 01 36.9 +68 09 48           ~ 630 0
20 SH 2-125 HII 21 53 30 +47 21.2           ~ 38 1
21 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 634 2
22 NAME Cep B cor 22 57 07.00 +62 37 22.3           ~ 79 0
23 NGC 7538 OpC 23 13 37 +61 30.0           ~ 827 0
24 SH 2-159 Y*O 23 15 31.27440 +61 07 10.4450           ~ 175 2
25 Ass Cas OB 2 As* 23 20 +60.9           ~ 64 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-04:35:11

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