Detection of an ultra-bright submillimeter galaxy in the Subaru/XMM-Newton Deep Field using AzTEC/ASTE
| Autor: | 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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| Rok vydání: | 2010 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1111/j.1365-2966.2011.18918.x |
| Popis: | 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 |
| Databáze: | arXiv |
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