Umehata, H. and Tamura, Y. and Kohno, K. and Ivison, R.J. and Alexander, D.M. and Geach, J.E. and Hatsukade, B. and Hughes, D.H. and Ikarashi, S. and Kato, Y. and Izumi, T. and Kawabe, R. and Kubo, M. and Lee, M. and Lehmer, B. and Makiya, R. and Matsuda, Y. and Nakanishi, K. and Saito, T. and Smail, I. and Yamada, T. and Yamaguchi, Y. and Yun, M. (2015) 'ALMA Deep Field in SSA22 : a concentration of dusty starbursts in a z = 3.09 protocluster core.', Astrophysical journal letters., 815 . L8.
We report the results of 1farcm5 × 3' mapping at 1.1 mm with the Atacama Large Millimeter/submillimeter Array toward the central region of the z = 3.09 SSA22 protocluster. By combining our source catalog with archival spectroscopic redshifts, we find that eight submillimeter galaxies (SMGs) with flux densities, S1.1 mm = 0.7–6.4 mJy (LIR ~ 1012.1–1013.1 L⊙) are at z = 3.08–3.10. Not only are these SMGs members of the protocluster, but they in fact reside within the node at the junction of the 50 Mpc scale filamentary three-dimensional structure traced by Lyα emitters in this field. The eight SMGs account for a star formation rate density (SFRD) ~10 M⊙ yr−1 Mpc−3 in the node, which is two orders of magnitudes higher than the global SFRD at this redshift. We find that four of the eight SMGs host an X-ray-luminous active galactic nucleus. Our results suggest that the vigorous star formation activity and the growth of supermassive black holes (SMBHs) occurred simultaneously in the densest regions at z ~ 3, which may correspond to the most active historical phase of the massive galaxy population found in the core of the clusters in the present universe. Two SMGs are associated with Lyα blobs, implying that the two populations coexist in high-density environments for a few cases.
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|Publisher Web site:||http://dx.doi.org/10.1088/2041-8205/815/1/L8|
|Publisher statement:||© 2015. The American Astronomical Society. All rights reserved.|
|Date accepted:||29 October 2015|
|Date deposited:||19 February 2016|
|Date of first online publication:||04 December 2015|
|Date first made open access:||No date available|
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