2010A&A...518A..59G


Query : 2010A&A...518A..59G

2010A&A...518A..59G - Astronomy and Astrophysics, volume 518, A59-59 (2010/7-2)

Observations and modeling of the dust emission from the H2-bright galaxy-wide shock in Stephan's Quintet.

GUILLARD P., BOULANGER F., CLUVER M.E., APPLETON P.N., PINEAU DES FORETS G. and OGLE P.

Abstract (from CDS):

Spitzer Space Telescope observations have detected powerful mid-infrared (mid-IR) H2 rotational line emission from the X-ray emitting large-scale shock (∼15x35kpc2) associated with a galaxy collision in Stephan's Quintet (SQ). Because H2 forms on dust grains, the presence of H2 is physically linked to the survival of dust, and we expect some dust emission to originate in the molecular gas. To test this interpretation, IR observations and dust modeling are used to identify and characterize the thermal dust emission from the shocked molecular gas. The spatial distribution of the IR emission allows us to isolate the faint PAH and dust continuum emission associated with the molecular gas in the SQ shock. We model the spectral energy distribution (SED) of this emission, and fit it to Spitzer observations. The radiation field is determined with GALEX UV, HST V-band, and ground-based near-IR observations. We consider two limiting cases for the structure of the H2 gas: it is either diffuse and penetrated by UV radiation, or fragmented into clouds that are optically thick to UV. Faint PAH and dust continuum emission are detected in the SQ shock, outside star-forming regions. The 12/24µm flux ratio in the shock is remarkably close to that of the diffuse Galactic interstellar medium, leading to a Galactic PAH/VSG abundance ratio. However, the properties of the shock inferred from the PAH emission spectrum differ from those of the Galaxy, which may be indicative of an enhanced fraction of large and neutrals PAHs. In both models (diffuse or clumpy H2 gas), the IR SED is consistent with the expected emission from dust associated with the warm (>150K) H2 gas, heated by a UV radiation field of intensity comparable to that of the solar neighborhood. This is in agreement with GALEX UV observations that show that the intensity of the radiation field in the shock is GUV=1.4±0.2[Habing units]. The presence of PAHs and dust grains in the high-speed (∼1000km/s) galaxy collision suggests that dust survives. We propose that the dust that survived destruction was in pre-shock gas at densites higher than a few 0.1cm–3, which was not shocked at velocities larger than ∼200km/s. Our model assumes a Galactic dust-to-gas mass ratio and size distribution, and current data do not allow us to identify any significant deviations of the abundances and size distribution of dust grains from those of the Galaxy. Our model calculations show that far-IR Herschel observations will help in constraining the structure of the molecular gas, and the dust size distribution, and thereby to look for signatures of dust processing in the SQ shock.

Abstract Copyright:

Journal keyword(s): atomic processes - ISM: general - dust, extinction - galaxies: clusters: individual: Stephan's Quintet - shock waves - infrared: ISM

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16002 1
2 SNR J052501-693842 SNR 05 25 02.20 -69 38 39.0           ~ 374 1
3 NGC 7023 RNe 21 01 36.9 +68 09 48           ~ 663 0
4 NGC 7317 Sy2 22 35 51.8681746944 +33 56 41.758033380 15.10 14.57 13.60 12.72   ~ 165 1
5 NAME Stephan's Quintet CGG 22 35 57.5 +33 57 36           ~ 396 1
6 NGC 7318B GiP 22 35 58.3903354632 +33 57 57.827617524   14.06   12.47   ~ 130 0
7 NGC 7320 GiG 22 36 03.4059680280 +33 56 53.623460220 13.12 13.23 12.63 12.38   ~ 182 3
8 NGC 7319 Sy2 22 36 03.602 +33 58 33.18   14.57 13.53 12.65   ~ 266 0
9 NGC 7331 LIN 22 37 04.0506038088 +34 24 56.800076508 10.65 10.35 9.48     ~ 1164 2

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2022.05.25-22:49:26

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