A Comprehensive Study of Hα Emitters at z ∼ 0.62 in the DAWN Survey: The Need for Deep and Wide Regions - INSU - Institut national des sciences de l'Univers
Journal Articles The Astrophysical Journal Year : 2020

A Comprehensive Study of Hα Emitters at z ∼ 0.62 in the DAWN Survey: The Need for Deep and Wide Regions

Santosh Harish
  • Function : Author
Alicia Coughlin
  • Function : Author
James E. Rhoads
  • Function : Author
Sangeeta Malhotra
  • Function : Author
Steven L. Finkelstein
  • Function : Author
Matthew Stevans
  • Function : Author
Vithal S. Tilvi
  • Function : Author
Ali Ahmad Khostovan
  • Function : Author
Sylvain Veilleux
  • Function : Author
Junxian Wang
  • Function : Author
Pascale Hibon
  • Function : Author
Bhavin Joshi
  • Function : Author
John Pharo
  • Function : Author
Isak Wold
  • Function : Author
Lucia A. Perez
  • Function : Author
Zhen-Ya Zheng
  • Function : Author
Ronald Probst
  • Function : Author
Rob Swaters
  • Function : Author
Bahram Mobasher
  • Function : Author
Tianxing Jiang
  • Function : Author
Huan Yang
  • Function : Author

Abstract

We present new estimates of the luminosity function (LF) and star formation rate density (SFRD) for an Hα-selected sample at z ∼ 0.62 from the Deep And Wide Narrow-band (DAWN) survey. Our results are based on a new Hα sample in the extended COSMOS region (compared to Coughlin et al.) with the inclusion of flanking fields, resulting in a total area coverage of ∼1.5 deg2. A total of 241 Hα emitters were selected based on robust selection criteria using spectrophotometric redshifts and broadband color-color classification. Given that dust extinction is a dominant uncertainty in the estimation of LF and SFRD, we explore the effect of different dust-correction prescriptions by calculating the LF and SFRD using a constant dust extinction correction, A = 1 mag, a luminosity-dependent correction, and a stellar-mass-dependent correction. The resulting Hα LFs are well fitted using Schechter functions with best-fit parameters: L* = 1042.24 erg s-1, φ* = 10-2.85 Mpc-3, α = -1.62 for constant dust correction, L*=1042.31 erg s-1, φ* = 10-2.8 Mpc-3, α = -1.39 for luminosity-dependent dust correction, and L* = 1042.36 erg s-1, φ* = 10-2.91 Mpc-3, α = -1.48, for stellar-mass-dependent dust correction. The deep and wide nature of the DAWN survey effectively samples Hα emitters over a wide range of luminosities, thereby providing better constraints on both the faint and bright ends of the LF. Also, the SFRD estimates ρSFR = 10-1.39 M yr-1 Mpc-3 (constant dust correction), ρSFR = 10-1.47 M yr-1 Mpc-3 (luminosity-dependent dust correction), and ρSFR = 10-1.46 M yr-1 Mpc-3 (stellar-mass-dependent dust correction) are in good agreement with the evolution of SFRD across redshifts (0 < z < 2) seen from previous Hα surveys.

Dates and versions

insu-03711477 , version 1 (01-07-2022)

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Cite

Santosh Harish, Alicia Coughlin, James E. Rhoads, Sangeeta Malhotra, Steven L. Finkelstein, et al.. A Comprehensive Study of Hα Emitters at z ∼ 0.62 in the DAWN Survey: The Need for Deep and Wide Regions. The Astrophysical Journal, 2020, 892, ⟨10.3847/1538-4357/ab7015⟩. ⟨insu-03711477⟩
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