Takagi, T. and Mortier, A. M. J. and Shimasaku, K. and Coppin, K. and Pope, A. and Ivison, R. J. and Hanami, H. and Serjeant, S. and Clements, D. L. and Priddey, R. S. and Dunlop, J. S. and Takata, T. and Aretxaga, I. and Chapman, S. C. and Eales, S. A. and Farrah, D. and Granato, G. L. and Halpern, M. and Hughes, D. H. and van Kampen, E. and Scott, D. and Sekiguchi, K. and Smail, I. and Vaccari, M. (2007) The SCUBA HAlf Degree Extragalactic Survey (SHADES) – V. Submillimetre properties of near-infrared-selected galaxies in the Subaru/XMM–Newton deep field. Monthly Notices of the Royal Astronomical Society, 381 (3). pp. 1154-1168. ISSN 0035-8711 http://resolver.caltech.edu/CaltechAUTHORS:20091204-142137561
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We have studied the submillimetre (submm) properties of the following classes of near-infrared-selected (NIR-selected) massive galaxies at high redshifts: BzK-selected star-forming galaxies (BzKs); distant red galaxies (DRGs); and extremely red objects (EROs). We used the SCUBA HAlf Degree Extragalactic Survey (SHADES), the largest uniform submm survey to date. Partial overlap of SIRIUS/NIR images and SHADES in Subaru/XMM–Newton deep field has allowed us to identify four submm-bright NIR-selected galaxies, which are detected in the mid-IR, 24 μm, and the radio, 1.4GHz. We find that all of our submm-bright NIR-selected galaxies satisfy the BzK selection criteria, i.e. BzK≡ (z−K)_(AB)− (B−z)_(AB)≥−0.2 , except for one galaxy whose B−z and z−K colours are however close to the BzK colour boundary. Two of the submm-bright NIR-selected galaxies satisfy all of the selection criteria we considered, i.e. they belong to the BzK–DRG–ERO overlapping population, or 'extremely red'BzKs. Although these extremely red BzKs are rare (0.25 arcmin^(−2)), up to 20 per cent of this population could be submm galaxies. This fraction is significantly higher than that found for other galaxy populations studied here. Via a stacking analysis, we have detected the 850-μm flux of submm-faint BzKs and EROs in our SCUBA maps. While the contribution of z ~ 2 BzKs to the submm background is about 10–15 per cent and similar to that from EROs typically at z ~ 1, BzKs have a higher fraction (~30 per cent) of submm flux in resolved sources compared with EROs and submm sources as a whole. From the spectral energy distribution (SED) fitting analysis for both submm-bright and submm-faint BzKs, we found no clear signature that submm-bright BzKs are experiencing a specifically luminous evolutionary phase, compared with submm-faint BzKs. An alternative explanation might be that submm-bright BzKs are more massive than submm-faint ones.
|Additional Information:||© 2007 The Authors. Journal compilation © 2007 RAS. Accepted 2007 July 31; received July 18; in original form 2007 June 11. We thank all the members of the SHADES consortium, and acknowledge continuous support from the staff of the JCMT.We also thank all the members of the SIRIUS team and acknowledge the SWIRE project team. We thank E. Daddi for useful discussions on the BzK-selection technique. TT acknowledges the Japan Society for the Promotion of Science (JSPS – PD fellow, No. 18·7747). TT and SS acknowledge support by the Particle Physics and Astronomy Research Council under grant number PPA/G/S/2001/00120/2. IS acknowledges support from the Royal Society. This work is partly supported by aGrant-in-Aid for Scientific Research (No. 14540220) by the Japanese Ministry of Education, Culture, Sports, Science and Technology. KC and AP acknowledge the National Science and Engineering Research Council of Canada (NSERC). IA and DHH acknowledge partial support from Conacyt grants 39548-F and 39953-F. The JCMT is operated by the Joint Astronomy Centre on behalf of the UK Particle Physics and Astronomy Research Council, the Canadian National Research Council and the Netherlands Organization for Scientific Research.|
|Subject Keywords:||dust, extinction; galaxies: evolution; galaxies: starburst; infrared: galaxies; submillimetre|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||08 Dec 2009 17:22|
|Last Modified:||26 Dec 2012 11:36|
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