A 16 deg$^2$ survey of emission-line galaxies at z<1.6 from HSC-SSP PDR2 and CHORUS

Abstract

We have conducted a comprehensive survey of emission-line galaxies at z < ∼ 1.6 based on narrowband (NB) imaging data taken with Hyper Suprime-Cam (HSC) on the Subaru telescope. In this paper, we update the catalogs of Hα, [OIII], and [OII] emission-line galaxies using the data from the second Public Data Release (PDR2) of Subaru Strategic Program (SSP) of HSC and Cosmic HydrOgen Reionization Unveiled with Subaru (CHORUS) survey along with the spectroscopic redshifts for 2,019 emission-line galaxies selected with the PDR1 data. The wider effective coverage of NB816 and NB921, 16.3 deg 2 and 16.9 deg 2 respectively, are available in the Deep and UltraDeep layers of HSC-SSP from the PDR2. The CHORUS survey provides us with data with additional three NBs (NB527, NB718, and NB973) in the COSMOS field in the UltraDeep layer (1.37 deg 2 ). The five NB datasets allow us to investigate the starforming galaxies presenting emission-lines at 14 specific redshifts ranging from z ∼ 1.6 down to z ∼ 0.05. We revisit the distribution of large-scale structures and luminosity functions (LFs) for the emission-line galaxies with the large samples of 75,377 emission-line galaxies selected. The redshift revolution of LFs shows that the star formation rate densities (SFRDs) decreases monotonically from z ∼ 1.6, which is consistent with the cosmic SFRD ever known. Our samples of emission-line galaxies covering a sufficiently large survey volume are useful to investigate the evolution of star-forming galaxies since the cosmic noon in a wide range of environments including galaxy clusters, filaments, and voids.

The OTELO survey: Faint end of the luminosity function of [OII] emitters at = 1.43

“…We have derived the SFRD by integrating the LF, employing the Kennicutt (1998) relationship andKroupa (2001) IMF. We have found that the data from Khostovan et al (2015) and from Hayashi et al (2020) are at least ∼ 0.25 dex higher. This difference seems to come for our low value of φ * when compared with other results from literature (Ly et al 2007, Drake et al 2013or Hayashi et al 2013 and may be caused by the uncertainties presented in the normalisation of the LF due to CV effects.…”

“…We note that these points are not extinction-corrected, so they are a lower limit for the SFRD, as indicated by the cyan arrows.The filled black circles are data from Khostovan et al (2015). The filled diamonds are data from Hayashi et al (2020). The result of this work is represented by the open square.…”

“…This work + Hayashi et al (2013) * value Several authors (from Khostovan et al 2015) Khostovan et al ( 2015) Hayashi et al (2020) Acknowledgements. This paper is dedicated to the memory of our affable colleague and friend Héctor Castañeda, who passed away on Nov.…”

“…oxig_v3 z < 3.24; and Sobral et al (2015) up to z = 1.4. In addition, there are a series of works were the LF is obtained by employing the doublet [O iii] λλ4959,5007 alone, for example, in Ly et al (2007) at 0.41 < z < 0.84; Bongiovanni et al (2020) at z ∼ 0.83; Khostovan et al (2020) at 0.91 < z < 1.10; or Hayashi et al (2020) at 0.05 < z < 0.94.…”

“…It is located in the bluemost part of the spectrum in rest frame, when compared with Hα, [O iii]λλ 4959, 5007, and Hβ, allowing us to reach larger values of the redshift from ground observations and avoiding the less transparent parts of the atmosphere in the infrared regime. The LF has been derived for this doublet by a number of authors who have employed spectroscopy or narrow-band techniques (Gallego et al 2002 for the local universe; Khostovan et al 2015 for 1.47 < z < 4.69; Khostovan et al 2020 for 1.57 < z < 1.9; Drake et al 2013 for 0.35 < z < 1.64; Ly et al 2007 for 0.89 < z < 1.47; Comparat et al 2015 for 0.1 < z < 1.65; or Hayashi et al 2020 for 0.41 < z < 1.60). It has also been simulated from z = 0.1 to z = 3.0 by Park et al (2015).…”