The Hα‐based Star Formation Rate Density of the Universe at<i>z</i>= 0.84

Villar, V.; Gallego, J.; Pérez‐González, Pablo G.; Pascual, S.; Noeske, K. G.; Koo, David C.; Barro, Guillermo; Zamorano, J.

doi:10.1086/528942

Cited by 95 publications

(157 citation statements)

References 75 publications

(154 reference statements)

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“…(Villar et al 2008;Sobral et al 2012). Given the representative spectroscopic follow-up of our Hα emitters, we can directly test whether the polynomial correction presented in Sobral et al (2012, based Fig.…”

Section: Flux Corrections: [N Ii]/hα Correctionmentioning

confidence: 97%

CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O iii] + Hβ and [O ii] luminosity functions at z = 0.8, 1.4 and 2.2

Sobral

Matthee

Best

et al. 2015

Monthly Notices of the Royal Astronomical Society

124

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We present results from the largest contiguous narrow-band survey in the near-infrared. We have used WIRCam/CFHT and the lowOH2 filter (1.187 ± 0.005 µm) to survey ≈10 deg 2 of contiguous extragalactic sky in the SA22 field. A total of ∼ 6000 candidate emission-line galaxies are found. We use deep ugrizJK data to obtain robust photometric redshifts. We combine our data with the High-redshift Emission Line Survey (HiZELS), explore spectroscopic surveys (VVDS, VIPERS) and obtain our own spectroscopic follow-up with KMOS, FMOS and MOSFIRE to derive large samples of high-redshift emission-line selected galaxies: 3471 Hα emitters at z = 0.8, 1343 [OIII]+Hβ emitters at z = 1.4 and 572 [OII] emitters at z = 2.2. We probe co-moving volumes of > 10 6 Mpc 3 and find significant over-densities, including an 8.5 σ (spectroscopically confirmed) over-density of Hα emitters at z = 0.81. We derive Hα, [OIII]+Hβ and [OII] luminosity functions at z = 0.8, 1.4, 2.2, respectively, and present implications for future surveys such as Euclid. Our uniquely large volumes/areas allow us to sub-divide the samples in thousands of randomised combinations of areas and provide a robust empirical measurement of sample/cosmic variance. We show that surveys for star-forming/emission-line galaxies at a depth similar to ours can only overcome cosmicvariance (errors < 10%) if they are based on volumes > 5 × 10 5 Mpc 3 ; errors on L * and φ * due to sample (cosmic) variance on surveys probing ∼ 10 4 Mpc 3 and ∼ 10 5 Mpc 3 are typically very high: ∼ 300% and ∼ 40 − 60%, respectively.

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Section: Flux Corrections: [N Ii]/hα Correctionmentioning

confidence: 97%

CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O iii] + Hβ and [O ii] luminosity functions at z = 0.8, 1.4 and 2.2

Sobral

Matthee

Best

et al. 2015

Monthly Notices of the Royal Astronomical Society

124

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“…In detail, the selection process of the candidates was performed through a colour-magnitude diagram using the technique described in Pascual et al (2007) and applied by our group in Villar et al (2008). The criterion used was…”

Section: Sample Selectionmentioning

confidence: 99%

“…Several studies employed HST/NICMOS grism spectroscopy at 0.7 < z < 1.9 (Yan et al 1999;Hopkins et al 2000;Shim et al 2009). Narrow-band NIR works include redshift windows that are less affected by atmospheric features, such as z ∼ 0.84 (Villar et al 2008;Sobral et al 2009;Ly et al 2011), z ∼ 1.47 (Sobral et al 2012), and z ∼ 2.23 (Moorwood et al 2000;Geach et al 2008;Hayes et al 2010;Tadaki et al 2011). The HiZELS survey has recently combined narrow-band data at common redshift windows z ∼ 0.4, 0.84, 1.47, 2.23 and has obtained a view of the last 11 Gyr of evolution of star-forming galaxies (SFGs) by employing a homogeneously selected sample of Hα emitters (Sobral et al 2013).…”

Section: Introductionmentioning

confidence: 99%

“…We then extended the study to z ∼ 0.24 and z ∼ 0.4 with an optical narrow-band technique (Pascual et al 2001;Pascual 2005). More recently, we applied this technique in the NIR at z ∼ 0.84 (Villar et al 2008). In the mentioned redshift gap 0.5 < z < 0.8 in Hα-based studies, we only find a few objects in the lower limits of the NIR spectroscopic surveys indicated above.…”

Section: Introductionmentioning

confidence: 99%

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Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Gómez-Guijarro

Gallego

Villar

et al. 2016

A&A

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Context. Studies measuring the star formation rate density, luminosity function, and properties of star-forming galaxies are numerous. However, it exists a gap at 0.5 < z < 0.8 in Hα-based studies. Aims. Our main goal is to study the properties of a sample of faint Hα emitters at z ∼ 0.62. We focus on their contribution to the faint end of the luminosity function and derived star formation rate density, characterising their morphologies and basic photometric and spectroscopic properties. Methods. We use a narrow-band technique in the near-infrared, with a filter centred at 1.06 µm. The data come from ultra-deep VLT/HAWK-I observations in the GOODS-S field with a total of 31.9 h in the narrow-band filter. In addition to our survey, we mainly make use of ancillary data coming from the CANDELS and Rainbow Cosmological Surveys Database, from the 3D-HST for comparison, and also spectra from the literature. We perform a visual classification of the sample and study their morphologies from structural parameters available in CANDELS. In order to obtain the luminosity function, we apply a traditional V/V max method and perform individual extinction corrections for each object to accurately trace the shape of the function. Results. Our 28 Hα-selected sample of faint star-forming galaxies reveals a robust faint-end slope of the luminosity function α = −1.46 +0.16 −0.08 . The derived star formation rate density at z ∼ 0.62 is ρ SFR = 0.036 +0.012 −0.008 M yr −1 Mpc −3 . The sample is mainly composed of disks, but an important contribution of compact galaxies with Sérsic indexes n ∼ 2 display the highest specific star formation rates. Conclusions. The luminosity function at z ∼ 0.62 from our ultra-deep data points towards a steeper α when an individual extinction correction for each object is applied. Compact galaxies are low-mass, low-luminosity, and starburst-dominated objects with a light profile in an intermediate stage from early to late types.

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“…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%

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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The Hα‐based Star Formation Rate Density of the Universe atz= 0.84

Cited by 95 publications

References 75 publications

CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O iii] + Hβ and [O ii] luminosity functions at z = 0.8, 1.4 and 2.2

CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O iii] + Hβ and [O ii] luminosity functions at z = 0.8, 1.4 and 2.2

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

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

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The Hα‐based Star Formation Rate Density of the Universe atz= 0.84

Cited by 95 publications

References 75 publications

CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O iii] + Hβ and [O ii] luminosity functions at z = 0.8, 1.4 and 2.2

CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O iii] + Hβ and [O ii] luminosity functions at z = 0.8, 1.4 and 2.2

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

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

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