HUSCAP logo Hokkaido Univ. logo

Hokkaido University Collection of Scholarly and Academic Papers >
Graduate School of Science / Faculty of Science >
Peer-reviewed Journal Articles, etc >

Stellar population and dust extinction in an ultraluminous infrared galaxy at z=1.135

Files in This Item:
MNRAS402-1_335-344.pdf1.22 MBPDFView/Open
Please use this identifier to cite or link to this item:

Title: Stellar population and dust extinction in an ultraluminous infrared galaxy at z=1.135
Authors: Kawara, K. Browse this author
Oyabu, S. Browse this author
Matsuoka, Y. Browse this author
Yoshii, Y. Browse this author
Minezaki, T. Browse this author
Sameshima, H. Browse this author
Asami, N. Browse this author
Ienaka, N. Browse this author
Kozasa, T. Browse this author
Keywords: dust
galaxies: evolution
galaxies: high-redshift
galaxies: individual: SST J1604+4304
galaxies: starburst
galaxies: stellar content
cosmology: observations
infrared: galaxies
Issue Date: Feb-2010
Publisher: Blackwell Publishing
Journal Title: Monthly Notices of the Royal Astronomical Society
Volume: 402
Issue: 1
Start Page: 335
End Page: 344
Publisher DOI: 10.1111/j.1365-2966.2009.15873.x
Abstract: We present the detailed optical to far-infrared (far-IR) observations of SST J1604+4304, an ultraluminous IR galaxy at z = 1.135. Analysing the stellar absorption lines, namely, the Ca II H & K and Balmer H lines in the optical spectrum, we derive the upper limits of an age for the stellar population. Given this constraint, the minimum χ2 method is used to fit the stellar population models to the observed spectral energy distribution from 0.44 to 5.8 μm. We find the following properties. The stellar population has an age 40-200 Myr with a metallicity 2.5 Z⊙. The starlight is reddened by E(B - V) = 0.8. The reddening is caused by the foreground dust screen, indicating that dust is depleted in the starburst site and the starburst site is surrounded by a dust shell. The IR (8-1000 μm) luminosity is L_[ir] = 1.78 ± 0.63 x 10^[12] L⊙. This is two times greater than that expected from the observed starlight, suggesting either that 1/2 of the starburst site is completely obscured at UV-optical wavelengths, or that 1/2 of L_[ir] comes from active galactic nucleus (AGN) emission. The inferred dust mass is 2.0 ± 1.0 x 10^[8] M⊙. This is sufficient to form a shell surrounding the galaxy with an optical depth E(B - V) = 0.8. From our best stellar population model - an instantaneous starburst with an age 40 Myr - we infer the rate of 19 supernovae per year. Simply analytical models imply that 2.5 Z⊙ in stars was reached when the gas mass reduced to 30 per cent of the galaxy mass. The gas metallcity is 4.8 Z⊙ at this point. The gas-to-dust mass ratio is then 120 ± 73. The inferred dust production rate is 0.24 ± 0.12 M⊙ per SN. If 1/2 of L_[ir] comes from AGN emission, the rate is 0.48 ± 0.24 M⊙ per SN. We discuss the evolutionary link of SST J1604+4304 to other galaxy populations in terms of the stellar masses and the galactic winds, including optically selected low-luminosity Lyman α-emitters and submillimeter selected high-luminosity galaxies.
Type: article
Appears in Collections:理学院・理学研究院 (Graduate School of Science / Faculty of Science) > 雑誌発表論文等 (Peer-reviewed Journal Articles, etc)

Submitter: 小笹 隆司

Export metadata:

OAI-PMH ( junii2 , jpcoar_1.0 )

MathJax is now OFF:


 - Hokkaido University