10_1093_mnrasl_slt131.pdf (374.2 kB)
Herschel observations and a model for IRAS 08572+3915: a candidate for the most luminous infrared galaxy in the local (z < 0.2) Universe
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posted on 2023-06-08, 21:01 authored by A Efstathiou, C Pearson, D Farrah, D Rigopoulou, J Graciá-Carpio, A Verma, H W W Spoon, J Afonso, J Bernard-Salas, D L Clements, A Cooray, D Cormier, M Etxaluze, J Fischer, E González-Alfonso, Pete Hurley, V Lebouteiller, Seb OliverSeb Oliver, M Rowan-Robinson, E SturmWe present Herschel photometry and spectroscopy, carried out as part of the Herschel ultraluminous infrared galaxy (ULIRG) survey, and a model for the infrared to submillimetre emission of the ULIRG IRAS 08572+3915. This source shows one of the deepest known silicate absorption features and no polycyclic aromatic hydrocarbon emission. The model suggests that this object is powered by an active galactic nucleus (AGN) with a fairly smooth torus viewed almost edge-on and a very young starburst. According to our model, the AGN contributes about 90percent of the total luminosity of 1.1 × 10 13 L ? , which is about a factor of 5 higher than previous estimates. The large correction of the luminosity is due to the anisotropy of the emission of the best-fitting torus. Similar corrections may be necessary for other local and high-z analogues. This correction implies that IRAS 08572+3915 at a redshift of 0.05835 may be the nearest hyperluminous infrared galaxy and probably the most luminous infrared galaxy in the local (z < 0.2) Universe. IRAS 08572+3915 shows a low ratio of [C II ] to IR luminosity (log L [C II ] /L IR < -3.8) and a [O I ]63µm to [C II ]158µm line ratio of about 1 that supports the model presented in this Letter.
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Monthly Notices of the Royal Astronomical Society: LettersISSN
1745-3933Publisher
Royal Astronomical SocietyExternal DOI
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1Volume
437Page range
L16-L20Department affiliated with
- Physics and Astronomy Publications
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- Yes
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2015-06-08First Open Access (FOA) Date
2015-06-08First Compliant Deposit (FCD) Date
2015-06-08Usage metrics
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