The Spectral Energy Distribution of the Hyperluminous, Hot Dust-obscured Galaxy W2246-0526
Artikel i vetenskaplig tidskrift, 2018

Hot dust-obscured galaxies (Hot DOGs) are a luminous, dust-obscured population recently discovered in the WISE All-Sky survey. Multiwavelength follow-up observations suggest that they are mainly powered by accreting supermassive black holes (SMBHs), lying in dense environments, and being in the transition phase between extreme starburst and UV-bright quasars. Therefore, they are good candidates for studying the interplay between SMBHs, star formation, and environment. W2246-0526 (hereafter, W2246), a Hot DOG at z ∼ 4.6, has been taken as the most luminous galaxy known in the universe. Revealed by the multiwavelength images, the previous Herschel SPIRE photometry of W2246 is contaminated by a foreground galaxy (W2246f), resulting in an overestimation of its total IR luminosity by a factor of about two. We perfor m the rest-frame UV/optical-to-far-IR spectral energy distribution (SED) analysis with SED3FIT and re-estimate its physical properties. The derived stellar mass M ∗ = 4.3 × 10 11 M ⊙ makes it among the most massive galaxies with spectroscopic redshift z > 4.5. Its structure is extremely compact and requires an effective mechanism to puff-up. Most of ( > 95%) its IR luminosity is from AGN torus emission, revealing the rapid growth of the central SMBH. We also predict that W2246 may have a significant molecular gas reservoir based on the dust mass estimation.

infrared: galaxies

galaxies: active

galaxies: individual (W22460526)

galaxies: high-redshift

submillimeter: galaxies

Författare

Lulu Fan

Shandong University, Weihai

Ying Gao

Shandong University, Weihai

Kirsten Kraiberg Knudsen

Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik, Extragalaktisk astrofysik

X. W. Shu

Anhui Normal University

Astrophysical Journal

0004-637X (ISSN) 1538-4357 (eISSN)

Vol. 854 157

Ämneskategorier

Astronomi, astrofysik och kosmologi

Atom- och molekylfysik och optik

Den kondenserade materiens fysik

DOI

10.3847/1538-4357/aaaaae