TY - JOUR
T1 - Evolution of star-forming galaxies from z = 0.7 to 1.2 with eBOSS emission-line galaxies
AU - Guo, Hong
AU - Yang, Xiaohu
AU - Raichoor, Anand
AU - Zheng, Zheng
AU - Comparat, Johan
AU - Gonzalez-Perez, V.
AU - Kneib, Jean Paul
AU - Schneider, Donald P.
AU - Bizyaev, Dmitry
AU - Oravetz, Daniel
AU - Oravetz, Audrey
AU - Pan, Kaike
N1 - Funding Information:
This work is supported by the National Key R&D Program of China (grant Nos. 2015CB857003, 2015CB857002) and the National Science Foundation of China (Nos. 11621303, 11655002, 11773049, 11833005, and 11828302). H.G.
Funding Information:
acknowledges the support of the 100 Talents Program of the Chinese Academy of Sciences. This work is also supported by a grant from the Science and Technology Commission of Shanghai Municipality (grants No. 16DZ2260200).
Funding Information:
We thank the anonymous reviewer for the helpful comments that significantly improved the presentation of this paper. We thank Yen-Ting Lin for carefully reading the manuscript and providing detailed comments. We thank Rita Tojeiro for useful discussions. We gratefully acknowledge the use of the High Performance Computing Resource in the Core Facility for Advanced Research Computing at the Shanghai Astronomical Observatory. We acknowledge the Gauss Centre for Supercomputing e.V. (www.Gauss-centre.eu) and the Partnership for Advanced Supercomputing in Europe (PRACE;www.prace-ri. eu) for funding the MultiDark simulation project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (LRZ,www.lrz.de).
Funding Information:
Funding for SDSS IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org.
Publisher Copyright:
© 2019 The American Astronomical Society. All rights reserved.
PY - 2019/2/1
Y1 - 2019/2/1
N2 - We study the evolution of star-forming galaxies with 10 10 M ⊙ < M ∗ < 10 11.6 M ⊙ over the redshift range of 0.7 < z < 1.2 using the emission-line galaxies (ELGs) in the extended Baryon Oscillation Spectroscopic Survey (eBOSS). By applying the incomplete conditional stellar mass function (SMF) model proposed in Guo et al., we simultaneously constrain the sample completeness, the stellariVhalo mass relation (SHMR), and the quenched galaxy fraction. We obtain the intrinsic SMFs for star-forming galaxies in the redshift bins of 0.7 < z < 0.8, 0.8 < z < 0.9, 0.9 < z < 1.0, and 1.0 < z < 1.2, as well as the SMF for all galaxies in the redshift bin of 0.7 < z < 0.8. We find that the eBOSS ELG sample only selects about 1%-10% of the star-forming galaxy population at the different redshifts, with the lower redshift samples more complete. There is only weak evolution in the SHMR of the ELGs from z = 1.2 to z = 0.7, as well as the intrinsic galaxy SMFs. Our best-fitting models show that the central ELGs at these redshifts live in halos of mass M ∼ 10 12 M ⊙ , while the satellite ELGs occupy slightly more massive halos of M ∼ 10 12.6 M ⊙ . The average satellite fraction of the observed ELGs varies from 13% to 17%, with the galaxy bias increasing from 1.1 to 1.4 from z = 0.7 to 1.2.
AB - We study the evolution of star-forming galaxies with 10 10 M ⊙ < M ∗ < 10 11.6 M ⊙ over the redshift range of 0.7 < z < 1.2 using the emission-line galaxies (ELGs) in the extended Baryon Oscillation Spectroscopic Survey (eBOSS). By applying the incomplete conditional stellar mass function (SMF) model proposed in Guo et al., we simultaneously constrain the sample completeness, the stellariVhalo mass relation (SHMR), and the quenched galaxy fraction. We obtain the intrinsic SMFs for star-forming galaxies in the redshift bins of 0.7 < z < 0.8, 0.8 < z < 0.9, 0.9 < z < 1.0, and 1.0 < z < 1.2, as well as the SMF for all galaxies in the redshift bin of 0.7 < z < 0.8. We find that the eBOSS ELG sample only selects about 1%-10% of the star-forming galaxy population at the different redshifts, with the lower redshift samples more complete. There is only weak evolution in the SHMR of the ELGs from z = 1.2 to z = 0.7, as well as the intrinsic galaxy SMFs. Our best-fitting models show that the central ELGs at these redshifts live in halos of mass M ∼ 10 12 M ⊙ , while the satellite ELGs occupy slightly more massive halos of M ∼ 10 12.6 M ⊙ . The average satellite fraction of the observed ELGs varies from 13% to 17%, with the galaxy bias increasing from 1.1 to 1.4 from z = 0.7 to 1.2.
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U2 - 10.3847/1538-4357/aaf9ad
DO - 10.3847/1538-4357/aaf9ad
M3 - Article
AN - SCOPUS:85062030184
VL - 871
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 147
ER -