THE DISPLACED DUSTY INTERSTELLAR MEDIUM OF NGC 3077: TIDAL STRIPPING IN THE M 81 TRIPLET
| Autor: | Maud Galametz, Daniel A. Dale, Nurur Rahman, Stefano Zibetti, H. W. Rix, Marc Sauvage, G. Aniano, Ramin A. Skibba, P. Beirão, Christine D. Wilson, Bernhard R. Brandl, George Helou, D. Calzetti, J. D. T. Smith, Sharon E. Meidt, Oliver Krause, Alison F. Crocker, Adam K. Leroy, Jin Koda, Cai-Na Hao, Leslie K. Hunt, Charles W. Engelbracht, Mark G. Wolfire, Robert C. Kennicutt, Eric J. Murphy, Bruce T. Draine, Eva Schinnerer, J. Hinz, Fabian Walter, Brent Groves, Lee Armus, Karin Sandstrom, H. Roussel, Alberto D. Bolatto, Kevin V. Croxall |
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| Rok vydání: | 2010 |
| Předmět: |
H-ALPHA
NGC-3077 GARLAND INFRARED-EMISSION Astrophysics::High Energy Astrophysical Phenomena DWARF IRREGULAR GALAXIES Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics ATOMIC-HYDROGEN STAR-FORMATION ARMS Astrophysics::Solar and Stellar Astrophysics M81 GROUP Astrophysics::Galaxy Astrophysics Physics Spiral galaxy ISM [galaxies] general [ISM] interactions [galaxies] Star formation Radiation field Garland) ISM [infrared] Astronomy and Astrophysics MOLECULAR GAS Galaxy Interstellar medium On board Physics and Astronomy Space and Planetary Science Intergalactic medium individual (NGC 3077 [galaxies] H-alpha Astrophysics::Earth and Planetary Astrophysics |
| Zdroj: | ASTROPHYSICAL JOURNAL LETTERS |
| ISSN: | 2041-8213 2041-8205 |
| DOI: | 10.1088/2041-8205/726/1/l11 |
| Popis: | We present the detection of extended (similar to 30 kpc(2)) dust emission in the tidal Hi arm near NGC 3077 (member of the M 81 triplet) using SPIRE on board Herschel. Dust emission in the tidal arm is typically detected where the Hi column densities are >10(21) cm(-2). The SPIRE band ratios show that the dust in the tidal arm is significantly colder (similar to 13 K) than in NGC 3077 itself (similar to 31 K), consistent with the lower radiation field in the tidal arm. The total dust mass in the tidal arm is similar to 1.8 x 10(6) M-circle dot (assuming beta = 2), i.e., substantially larger than the dust mass associated with NGC 3077 (similar to 2 x 10(5) M-circle dot). Where dust is detected, the dust-to-gas ratio is (6 +/- 3) x 10(-3), consistent within the uncertainties with what is found in NGC 3077 and nearby spiral galaxies with Galactic metallicities. The faint H II regions in the tidal arm cannot be responsible for the detected enriched material and are not the main source of the dust heating in the tidal arm. We conclude that the interstellar medium (atomic Hi, molecules, and dust) in this tidal feature was pre-enriched and stripped off NGC 3077 during its recent interaction (similar to 3 x 10(8) yr ago) with M 82 and M 81. This implies that interaction can efficiently remove heavy elements and enriched material (dust and molecular gas) from galaxies. As interactions were more frequent at large look-back times, it is conceivable that they could substantially contribute (along with galactic outflows) to the enrichment of the intergalactic medium. |
| Databáze: | OpenAIRE |
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