An extragalactic spectroscopic survey of the SSA22 field
We present Very Large Telescope VIMOS, Keck DEIMOS and Keck LRIS multi-object spectra of 367 sources in the field of the z ≈ 3.09 protocluster SSA22. Sources are spectroscopically classified via template matching, allowing new identifications for 206 extragalactic sources, including 36 z > 2 Lyman-break galaxies (LBGs) and Lyman α emitters (LAEs), eight protocluster members, and 94 X-ray sources from the ∼400 ks Chandra deep survey of SSA22. Additionally, in the area covered by our study, we have increased by ≈4, 13, and 6 times the number of reliable redshifts of sources at 1.0 < z < 2.0, at z > 3.4, and with X-ray emission, respectively. We compare our results with past spectroscopic surveys of SSA22 to investigate the completeness of the LBGs and the X-ray properties of the new spectroscopically classified sources in the SSA22 field.
Additional Information© 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2015 April 2; Received 2015 March 28; In original form 2014 August 29; First published online May 8, 2015. We would like to thank Ezequiel Treister and the anonymous referee for helpful discussions regarding the interpretations of our results. We would also like to thank Scott Chapman for providing radio images of the SSA22 field. CS acknowledges support from CONICYT-Chile (FONDECYT 3120198, Becas Chile 74140006, and the Anillo ACT1101). FEB acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, Gemini-CONICYT 32120003, 'EMBIGGEN" Anillo ACT1101), and Project IC120009 'Millennium Institute of Astrophysics (MAS)' funded by the Iniciativa Científica Milenio del Ministerio de Economía, Fomento y Turismo. The work of DS was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. JEG thanks the Royal Society. Based on observations made with ESO Telescopes at the Paranal Observatory under programme IDs 085.A-0616 and 089.A-0405. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The 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.
Published - MNRAS-2015-Saez-2615-30.pdf
Submitted - 1504.00737v3.pdf
Supplemental Material - Online.zip