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, David; Matthee, Jorryt; Best, P. N.; Smail, Ian; Khostovan, Ali Ahmad; Milvang-Jensen, B.; Kim, Jae-Woo; Stott, John P.; Calhau, João; Nayyeri, Hooshang; Mobasher, Bahram

doi:10.1093/mnras/stv1076

Cited by 83 publications

(144 citation statements)

References 72 publications

(218 reference statements)

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“…Therefore, the comparison of the luminosity functions between the fields shows that the luminosity functions in the individual fields are consistent with each other and the survey volume of > 5 × 10 5 Mpc 3 is essential at least to overcome the cosmic variance. Sobral et al (2015) also reach the similar conclusion that a survey volume of > 5 × 10 5 Mpc 3 is required to derive the luminosity functions with an error of less than 10% irrespective of sample variance.…”

Section: Sample Variancesupporting

confidence: 71%

“…Table 5 also show the Schechter parameters of the best-fit function, but α is fixed to be -1.6 according to Sobral et al (2013) and Sobral et al (2015). The luminosity functions are well fit by the Schechter function.…”

Section: Observed Luminosity Functionmentioning

confidence: 92%

“…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%

“…Samples of emissionline galaxies of similar size at z < ∼ 2 are also presented by the High-redshift(Z) Emission Line Survey (HiZELS). Sobral et al (2013) have conducted deep surveys in ∼ 2.0 deg 2 of the COSMOS and SXDS fields, while Sobral et al (2015) have conducted shallower but wider surveys in ∼ 10 deg 2 of the SA22 fields. They map large-scale structures of Hα emitters over these fields (see also Sobral et al 2011).…”

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: Sample Variancesupporting

confidence: 71%

Section: Observed Luminosity Functionmentioning

confidence: 92%

Section: Introductionmentioning

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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Resolving distant, dusty galaxies using observations and simulations

Cochrane

2019

Proc. IAU

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Spatially resolved studies of galaxies in the high-redshift Universe have traditionally been reliant on data at rest-frame optical and UV wavelengths, which can be biased towards the least dust-obscured galaxies. For several years now, we have been able to resolve and probe the morphology of longer-wavelength emission from distant galaxies with ALMA, and a number of recent ALMA studies were presented at the IAU Symposium No. 352. These included our study of the resolved multi-wavelength emission of galaxies at z ∼ 2. As part of the SHiZELS collaboration, we are mapping the Hα emission line (from SINFONI/VLT), UV continuum (from HST), and the far-infrared (from ALMA) emission from a small sample of Hα-selected galaxies. In this proceedings paper, we showcase the high quality of our data, and the spectacular structures displayed by one of our most dusty sources. We also provide an overview of some highly complementary simulation-based work, using galaxies drawn from the FIRE-2 zoom-in cosmological hydrodynamical simulations. Using sophisticated radiative transfer techniques, we have derived predictions for the spatially-resolved emission of a sample of star-forming galaxies, from rest-frame far-ultraviolet to the far-infrared. For both observed and simulated galaxies, emission maps show striking differences with wavelength, with the same galaxy appearing clumpy and extended in the far-ultraviolet yet compact at far-infrared wavelengths.

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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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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

Cited by 83 publications

References 72 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

Resolving distant, dusty galaxies using observations and simulations

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

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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

Cited by 83 publications

References 72 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

Resolving distant, dusty galaxies using observations and simulations

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

Contact Info

Product

Resources

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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