Herschel protocluster survey: a search for dusty star-forming galaxies in protoclusters at z = 2–3
Abstract
We present a Herschel/SPIRE survey of three protoclusters at z = 2 − 3 (2QZCluster, HS1700, SSA22). Based on the SPIRE colours (S_(350)/S_(250) and S_(500)/S_(350)) of 250 μm sources, we selected high redshift dusty star-forming galaxies potentially associated with the protoclusters. In the 2QZCluster field, we found a 4σ overdensity of six SPIRE sources around 4.5′ (∼ 2.2 Mpc) from a density peak of Hα emitters at z = 2.2. In the HS1700 field, we found a 5σ overdensity of eight SPIRE sources around 2.1′ (∼ 1.0 Mpc) from a density peak of LBGs at z = 2.3. We did not find any significant overdensities in SSA22 field, but we found three 500 μm sources are concentrated 3′ (∼1.4 Mpc) east to the LAEs overdensity. If all the SPIRE sources in these three overdensities are associated with protoclusters, the inferred star-formation rate densities are 10^3 − 10^4 times higher than the average value at the same redshifts. This suggests that dusty star-formation activity could be very strongly enhanced in z ∼ 2 − 3 protoclusters. Further observations are needed to confirm the redshifts of the SPIRE sources and to investigate what processes enhance the dusty star-formation activity in z ∼ 2 − 3 protoclusters.
Additional Information
© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 May 19. Received 2016 May 16. In original form 2016 March 18. First published online May 23, 2016. We thank the anonymous referee for helpful comments which significantly improved the clarity of this paper. We thank Scott Chapman, James Colbert, Emanuele Daddi, Koichiro Nakanishi, and Kazuhiro Shimasaku for useful discussions and supports. Rhythm Shimakawa and Mariko Kubo made enormous contribution to analyses. We acknowledge Masaru Kajisawa for our use of his MOIRCS fringe-removal software (Kajisawa et al. 2015) during the data reduction. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK). Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. UKIRT is funded by the STFC (UK). The W.M. Keck Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research was supported in part by a grant from the Hayakawa Satio Fund awarded by the Astronomical Society of Japan. YM acknowledges support from JSPS KAKENHI Grant Number 20647268. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit Award. BH acknowledges support from JSPS KAKENHI Grant Number 15K17616. HU acknowledges support from Grant-in-Aid for JSPS Fellows, 26.11481.Attached Files
Published - MNRAS-2016-Kato-3861-72.pdf
Submitted - 1605.07370v1.pdf
Supplemental Material - Supplement.zip
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Additional details
- Eprint ID
- 70852
- Resolver ID
- CaltechAUTHORS:20161005-073437352
- W. M. Keck Foundation
- Astronomical Society of Japan
- 20647268
- Japan Society for the Promotion of Science (JSPS)
- ST/L00075X/1
- Science and Technology Facilities Council (STFC)
- DUSTYGAL 321334
- European Research Council (ERC)
- Royal Society
- 15K17616
- Japan Society for the Promotion of Science (JSPS)
- 26.11481
- Japan Society for the Promotion of Science (JSPS)
- Created
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2016-10-05Created from EPrint's datestamp field
- Updated
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2021-11-11Created from EPrint's last_modified field