Evolution of the H β + [O iii] and [O ii] luminosity functions and the [O ii] star formation history of the Universe up to<i>z</i> ∼ 5 from HiZELS

Khostovan, Ali Ahmad; Sobral, David; Mobasher, Bahram; Best, P. N.; Smail, Ian; Stott, John P.; Hemmati, Shoubaneh; Nayyeri, Hooshang

doi:10.1093/mnras/stv1474

Cited by 117 publications

(259 citation statements)

References 84 publications

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“…Therefore, we apply the same survey volume to emission-line galaxies with a given observed luminosity. (Ly et al 2007;Drake et al 2013;Khostovan et al 2015) are also plotted for comparison.…”

Section: Survey Volumementioning

confidence: 99%

“…Many surveys, targeting emission-line galaxies at z < ∼ 2, have been conducted so far (e.g., Bunker et al 1995;Thompson et al 1996;Moorwood et al 2000;van der Werf et al 2000;Fujita et al 2003;Doherty et al 2006;Shioya et al 2008;Villar et al 2008;Dale et al 2010;Ly et al 2007;Ly et al 2011;Bayliss et al 2011;Lee et al 2012;Best et al 2013;Colbert et al 2013;Ciardullo et al 2013;Drake et al 2013;Pirzkal et al 2013;Sobral et al 2013;Sobral et al 2015;An et al 2014;Khostovan et al 2015;Comparat et al 2015;Comparat et al 2016;Stroe & Sobral 2015;Stroe et al 2017). As a result, the cosmic SFR density has been established with a peak at z = 1-3 and then a gradually decline towards the local Universe (e.g., Hopkins & Beacom 2006;Madau & Dickinson 2014).…”

Section: Introductionmentioning

confidence: 99%

“…Indeed, previous studies with NBs (e.g., Ly et al 2007;Drake et al 2013;Sobral et al 2011;Sobral et al 2013;Sobral et al 2015;Khostovan et al 2015;Matthee et al 2017) have succeeded in constructing large samples of emission-line galaxies at z < 2. Ly et al (2007) have selected 200-900 emissionline galaxies with 11 individual redshift slices at z < 1.5 from deep imaging with 4 NB filters in 0.24 deg 2 of the Subaru Deep Field (SDF).…”

Section: Introductionmentioning

confidence: 99%

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A 16 deg2 survey of emission-line galaxies at z < 1.5 in HSC-SSP Public Data Release 1

Hayashi¹,

Tanaka²,

Shimakawa³

et al. 2017

Publications of the Astronomical Society of Japan

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We present initial results from the Subaru Strategic Program (SSP) with Hyper Suprime-Cam (HSC) on a comprehensive survey of emission-line galaxies at z < 1.5 based on narrowband imaging. The first Public Data Release (PDR1) provides us with data from two narrowband filters, specifically NB816 and NB921 over 5.7 deg 2 and 16.2 deg 2 respectively. The 5σ limiting magnitudes are 25.2 (UltraDeep layer, 1.4 deg 2 ) and 24.8 (Deep layer, 4.3 deg 2 ) mag in NB816, and 25.1 (UltraDeep, 2.9 deg 2 ) and 24.6-24.8 (Deep, 13.3 deg 2 ) mag in NB921. The wide-field imaging allows us to construct unprecedentedly large samples of 8,054 Hα emitters c 2017. Astronomical Society of Japan. 2Publications of the Astronomical Society of Japan, (2017), Vol. 00, No. 0 at z ≈ 0. 25 and 0.40, 8,656 [OIII] emitters at z ≈ 0. 63 and 0.84, and 16,877 [OII] emitters at z ≈ 1.19 and 1.47. We map the cosmic web on scales out to about 50 comoving Mpc that includes galaxy clusters, identified by red sequence galaxies, located at the intersection of filamentary structures of star-forming galaxies. The luminosity functions of emission-line galaxies are measured with precision and consistent with published studies. The wide field coverage of the data enables us to measure the luminosity functions up to brighter luminosities than previous studies. The comparison of the luminosity functions between the different HSC-SSP fields suggests that a survey volume of > 5 × 10 5 Mpc 3 is essential to overcome cosmic variance. Since the current data have not reached the full depth expected for the HSC-SSP, the color cut in i−NB816 or z−NB921 induces a bias towards star-forming galaxies with large equivalent widths, primarily seen in the stellar mass functions for the Hα emitters at z ≈ 0.25-0.40. Even so, the emission-line galaxies clearly cover a wide range of luminosity, stellar mass, and environment, thus demonstrating the usefulness of the narrowband data from the HSC-SSP to investigate star-forming galaxies at z < 1.5.

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Section: Survey Volumementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A 16 deg2 survey of emission-line galaxies at z < 1.5 in HSC-SSP Public Data Release 1

Hayashi¹,

Tanaka²,

Shimakawa³

et al. 2017

Publications of the Astronomical Society of Japan

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“…Its LF has been measured from redshift 0 to 4.7 (e.g. Ly et al 2007;Zhu, Moustakas & Blanton 2009;Gilbank et al 2010;Bayliss et al 2011;Sobral et al 2012;Comparat et al 2015b;Khostovan et al 2015), mostly due to interests in using [O II] as an empirical star formation rate (SFR) indicator (see Kennicutt 1998;Kewley, Geller & Jansen 2004;Moustakas, Kennicutt & Tremonti 2006). The [O III] and Hβ LFs have been studied between redshift 0 and 3.3 mostly with narrowband imaging and are usually measured together (including [O III] λ4959) as a single LF due to the low spectral resolution (e.g.…”

mentioning

confidence: 99%

“…The [O III] and Hβ LFs have been studied between redshift 0 and 3.3 mostly with narrowband imaging and are usually measured together (including [O III] λ4959) as a single LF due to the low spectral resolution (e.g. Ly et al 2007;Drake et al 2013;Khostovan et al 2015;Sobral et al 2015). Over the redshift range we are interested in, we did not find a measurement of the Hβ (λ4861) LF alone (without [O III] (Le Fèvre et al 2013;Newman et al 2013, respectively).…”

mentioning

confidence: 99%

The evolution of the [O ii], H β and [O iii] emission line luminosity functions over the last nine billions years

Comparat

Zhu

González-Pérez

et al. 2016

Mon. Not. R. Astron. Soc.

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Citation for published item:gomp r tD tF nd huD qF nd qonz lezE erezD F nd xor ergD F nd xewm nD tF nd resseD vF nd i h rdD tF nd epesD qF nd unei D tFE F nd i hoorD eF nd r d D pF nd w r stonD gF nd e heD gF nd helu D F nd tulloD iF @PHITA 9 he evolution of the y ss D r nd y sss emission line luminosity fun tions over the l st nine illions ye rsF9D wonthly noti es of the oy l estronomi l o ietyFD RTI @IAF ppF IHUTEIHVUF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTEmission line galaxies are one of the main tracers of the large-scale structure to be targeted by the next-generation dark energy surveys. To provide a better understanding of the properties and statistics of these galaxies, we have collected spectroscopic data from the VVDS and DEEP2 deep surveys and estimated the galaxy luminosity functions (LFs) of three distinct emission lines, [O II] (λλ3726, 3729) (0.5 < z < 1.3), Hβ (λ4861) (0.3 < z < 0.8) and [O III] (λ5007) (0.3 < z < 0.8). Our measurements are based on 35 639 emission line galaxies and cover a volume of ∼10 7 Mpc 3 . We present the first measurement of the Hβ LF at these redshifts. We have also compiled LFs from the literature that were based on independent data or covered different redshift ranges, and we fit the entire set over the whole redshift range with analytic Schechter and Saunders models, assuming a natural redshift dependence of the parameters. We find that the characteristic luminosity (L * ) and density (φ * ) of all LFs increase with redshift. Using the Schechter model over the redshift ranges considered, we find that, for [O II] emitters, the characteristic luminosity L * (z = 0.5) = 3.2 × 10 41 erg s −1 increases by a factor of 2.7 ± 0.2 from z = 0.5 to 1.3; for Hβ emitters L * (z = 0.3) = 1.3 × 10 41 erg s −1 increases by a factor of 2.0 ± 0.2 from z = 0.3 to 0.8; and for [O III] emitters L * (z = 0.3) = 7.3 × 10 41 erg s −1 increases by a factor of 3.5 ± 0.4 from z = 0.3 to 0.8.

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Modeling Emission Line Galaxies

Moriwaki

2022

Large-Scale Structure of the Universe

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Evolution of the H β + [O iii] and [O ii] luminosity functions and the [O ii] star formation history of the Universe up toz ∼ 5 from HiZELS

Cited by 117 publications

References 84 publications

A 16 deg2 survey of emission-line galaxies at z < 1.5 in HSC-SSP Public Data Release 1

A 16 deg2 survey of emission-line galaxies at z < 1.5 in HSC-SSP Public Data Release 1

The evolution of the [O ii], H β and [O iii] emission line luminosity functions over the last nine billions years

Modeling Emission Line Galaxies

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Evolution of the H β + [O iii] and [O ii] luminosity functions and the [O ii] star formation history of the Universe up toz ∼ 5 from HiZELS

Cited by 117 publications

References 84 publications

A 16 deg2 survey of emission-line galaxies at z &lt; 1.5 in HSC-SSP Public Data Release 1

A 16 deg2 survey of emission-line galaxies at z &lt; 1.5 in HSC-SSP Public Data Release 1

The evolution of the [O ii], H β and [O iii] emission line luminosity functions over the last nine billions years

Modeling Emission Line Galaxies

Contact Info

Product

Resources

About

A 16 deg2 survey of emission-line galaxies at z < 1.5 in HSC-SSP Public Data Release 1

A 16 deg2 survey of emission-line galaxies at z < 1.5 in HSC-SSP Public Data Release 1