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IRAS F13342+3932

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Galaxy in the constellation Canes Venatici
IRAS F13342+3932
SDSS image of IRAS F13342+3932
Observation data (J2000.0 epoch)
Constellation Canes Venatici
Right ascension 13h 36m 24.05s[1]
Declination +39°17′31.13′′[1]
Redshift 0.179050[1]
Heliocentric radial velocity 53,678 ± 8 km/s [1]
Distance 2,585.5±181.0Mly (792.71±55.49Mpc)[1]
magnitude(J)14.53[1]
magnitude(H)13.63[1]
Characteristics
Type ULIRG Sy1[1]
Size~485,000ly (148.8kpc) (estimated)[1]
Other designations
2MASX J13362406+3917305, IRAS 13342+3932, NVSS J133623+391733, LQAC 204+039 002, LEDA 84036[1]

IRAS F13342+3932 is an ultraluminous infrared galaxy located in the constellation of Canes Venatici. The redshift of the galaxy is (z) 0.179[1] and it was first discovered by astronomers from a sample of IRAS catalogue sources in April 1986 and such has a faint companion.[2] It is categorized as a broad-line Type 1 Seyfert galaxy.[3] [4]

Description

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IRAS F13342+3932 is classified as a quasar.[5] When observed with Hubble Space Telescope (HST), its host galaxy is found to contain at least two spiral arms.[6] The mass of the central supermassive black hole is estimated to be 9.12+0.5-0.5 Mʘ and the total bolometric luminosity of the entire galaxy is estimated as 12.49 Lʘ.[7] Observations in 2019 has found the host galaxy has H II regions with smaller photoionized regions of both AGN and LINER type. It is also evident there are presence of massive young OB stars located with the star forming regions of the host galaxy which in turn, is photoionizing the surrounding interstellar gas.[8] The radio structure of the galaxy is compact with a resolved radio core based on Very Large Array (VLA) imaging. The core is estimated to have a radio power of 22.73 watts per hertz.[4]

It is found that the galaxy contains molecular gas outflows. When observed, the velocity field of the gas is mainly traced by emission lines, with the field itself being rotation dominated. Carbon oxide mapping observations also showed the optical spectrum of the galaxy has a line profile, described as triple-peaked. Evidence also found the blue and red peaks of the profile are emitted out from both regions located in the northeast and southwest while the central peak on the other hand, is shown originating from central and southeast regions.[6] A hydrogen gas mass of 2 ×ばつ 108 Mʘ has been estimated for the entire galaxy, with the gas reaching hot temperatures of 1400 ± 60 Kelvin. The molecular mass of the galaxy is calculated as 3 ± 2 ×ばつ 106 Mʘ.[9]

References

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  1. 1 2 3 4 5 6 7 8 9 10 11 "NED Search results for IRAS F13342+3932". NASA/IPAC Extragalactic Database. Retrieved 2026年04月12日.
  2. ↑ Lawrence, A.; Walker, D.; Rowan-Robinson, M.; Leech, K. J.; Penston, M. V. (April 1986). "Studies of IRAS sources at high galactic latitudes - II. Results froma redshift survey at b>60 : distribution in depth, luminosity function, and physical nature of IRAS galaxies". Monthly Notices of the Royal Astronomical Society. 219 (3): 687–701. Bibcode:1986MNRAS.219..687L. doi:10.1093/mnras/219.3.687 . ISSN 0035-8711.
  3. ↑ Sani, E.; Lutz, D.; Risaliti, G.; Netzer, H.; Gallo, L. C.; Trakhtenbrot, B.; Sturm, E.; Boller, T. (April 2010). "Enhanced star formation in narrow-line Seyfert 1 active galactic nuclei revealed by Spitzer". Monthly Notices of the Royal Astronomical Society. 403 (3): 1246–1260. arXiv:0908.0280 . Bibcode:2010MNRAS.403.1246S. doi:10.1111/j.1365-2966.2009.16217.x . ISSN 0035-8711.
  4. 1 2 Nagar, N. M.; Wilson, A. S.; Falcke, H.; Veilleux, S.; Maiolino, R. (2003年10月01日). "The AGN content of ultraluminous IR galaxies: High resolution VLA imaging of the IRAS 1 Jy ULIRG sample". Astronomy & Astrophysics. 409 (1): 115–121. arXiv:astro-ph/0309298 . Bibcode:2003A&A...409..115N. doi:10.1051/0004-6361:20031069. ISSN 0004-6361.
  5. ↑ Xia, X. Y.; Gao, Y.; Hao, C.-N.; Tan, Q. H.; Mao, S.; Omont, A.; Flaquer, B. O.; Leon, S.; Cox, P. (2012年02月29日), "Molecular Gas in Infrared Ultraluminous QSO Hosts", The Astrophysical Journal, 750 (2): 92, arXiv:1202.6490 , Bibcode:2012ApJ...750...92X, doi:10.1088/0004-637X/750/2/92
  6. 1 2 Runnoe, Jessie C; Gültekin, Kayhan; Rupke, David; López-Sepulcre, Ana (2021年07月02日). "Properties of cold molecular gas in four type-1 active galaxies hosting outflows". Monthly Notices of the Royal Astronomical Society. 505 (4): 6017–6036. arXiv:2105.13460 . doi:10.1093/mnras/stab1579 . ISSN 0035-8711.
  7. ↑ Rupke, David S. N.; Gültekin, Kayhan; Veilleux, Sylvain (2017年11月15日). "Quasar-mode Feedback in Nearby Type 1 Quasars: Ubiquitous Kiloparsec-scale Outflows and Correlations with Black Hole Properties". The Astrophysical Journal. 850 (1): 40. arXiv:1708.05139 . Bibcode:2017ApJ...850...40R. doi:10.3847/1538-4357/aa94d1 . ISSN 0004-637X.
  8. ↑ Hinkle, Jason T.; Veilleux, Sylvain; Rupke, David S. N. (2019年08月09日). "Ionization Mechanisms in Quasar Outflows". The Astrophysical Journal. 881 (1): 31. arXiv:1906.10249 . Bibcode:2019ApJ...881...31H. doi:10.3847/1538-4357/ab2bfa . ISSN 0004-637X.
  9. ↑ Higdon, S. J. U.; Armus, L.; Higdon, J. L.; Soifer, B. T.; Spoon, H. W. W. (2006年06月14日), "A Spitzer Space Telescope Infrared Spectrograph Survey of Warm Molecular Hydrogen in Ultraluminous Infrared Galaxies", The Astrophysical Journal, 648 (1): 323–339, arXiv:astro-ph/0605359 , Bibcode:2006ApJ...648..323H, doi:10.1086/505701, arXiv:astro-ph/0605359
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