학술논문
Detection of an ultra-bright submillimeter galaxy in the Subaru/XMM-Newton Deep Field using AzTEC/ASTE
Document Type
Working Paper
Author
Ikarashi, S.; Kohno, K.; Aguirre, J. E.; Aretxaga, I.; Arumugam, V.; Austermann, J. E.; Bock, J. J.; Bradford, C. M.; Cirasuolo, M.; Earle, L.; Ezawa, H.; Furusawa, H.; Furusawa, J.; Glenn, J.; Hatsukade, B.; Hughes, D. H.; Iono, D.; Ivison, R. J.; Johnson, S.; Kamenetzky, J.; Kawabe, R.; Lupu, R.; Maloney, P.; Matsuhara, H.; Mauskopf, P. D.; Motohara, K.; Murphy, E. J.; Nakajima, K.; Nakanishi, K.; Naylor, B. J.; Nguyen, H. T.; Perera, T. A.; Scott, K. S.; Shimasaku, K.; Takagi, T.; Takata, T.; Tamura, Y.; Tanaka, K.; Tsukagoshi, T.; Wilner, D. J.; Wilson, G. W.; Yun, M. S.; Zmuidzinas, J.
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Subject
Language
Abstract
We report the detection of an extremely bright ($\sim$37 mJy at 1100 $\mu$m and $\sim$91 mJy at 880 $\mu$m) submillimeter galaxy (SMG), AzTEC-ASTE-SXDF1100.001 (hereafter referred to as SXDF1100.001 or Orochi), discovered in 1100 $\mu$m observations of the Subaru/XMM-Newton Deep Field using AzTEC on ASTE. Subsequent CARMA 1300 $\mu$m and SMA 880 $\mu$m observations successfully pinpoint the location of Orochi and suggest that it has two components, one extended (FWHM of $\sim$ 4$^{\prime\prime}$) and one compact (unresolved). Z-Spec on CSO has also been used to obtain a wide band spectrum from 190 to 308 GHz, although no significant emission/absorption lines are found. The derived upper limit to the line-to-continuum flux ratio is 0.1--0.3 (2 $\sigma$) across the Z-Spec band. Based on the analysis of the derived spectral energy distribution from optical to radio wavelengths of possible counterparts near the SMA/CARMA peak position, we suggest that Orochi is a lensed, optically dark SMG lying at $z \sim 3.4$ behind a foreground, optically visible (but red) galaxy at $z \sim 1.4$. The deduced apparent (i.e., no correction for magnification) infrared luminosity ($L_{\rm IR}$) and star formation rate (SFR) are $6 \times 10^{13}$ $L_{\odot}$ and 11000 $M_{\odot}$ yr$^{-1}$, respectively, assuming that the $L_{\rm IR}$ is dominated by star formation. These values suggest that Orochi will consume its gas reservoir within a short time scale ($3 \times 10^{7}$ yr), which is indeed comparable to those in extreme starbursts like the centres of local ULIRGs.
Comment: 18 pages, 13 figures
Comment: 18 pages, 13 figures