A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

Stroe, Andra; Sobral, David

doi:10.1093/mnras/stv1555

Cited by 35 publications

(59 citation statements)

References 60 publications

(123 reference statements)

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“…We indicate previous UCM works as blue filled circles. The black circles correspond to the studies of Sobral et al (2012) at z ∼ 1.47; Sobral et al (2013) at z ∼ 0.4, 0.84, 1.47, 2.23; Drake et al (2013) at z ∼ 0.25, 0.4, 0.5; Sobral et al (2015) at z ∼ 0.8; and Stroe & Sobral (2015) at z ∼ 0.2. The compilation in Table B.1 of Gunawardhana et al (2013) is included as grey filled circles.…”

Section: Discussionmentioning

confidence: 96%

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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Section: Discussionmentioning

confidence: 96%

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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“…For a given luminosity, the minimum and maximum redshifts where the emission line can be observed at more than The red curve is a best-fit Schechter function to the red data points, where the solid (dotted) curve is fitted without (with) α fixed. The black curves are the luminosity functions from the literature, where the luminosity range covering the data in each study is shown by thick curve and the other range is shown by thin curve (Ly et al 2007;Drake et al 2013;Stroe & Sobral 2015;Sobral et al 2013). 5σ are calculated based on the filter transmission curve and a limiting flux. Then, the redshift range is converted to a comoving volume.…”

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%

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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“…Cowie et al 2010;Barger et al 2012;Konno et al 2016;Sobral et al 2017). We also plot the Hα LF interpolated from results of Stroe & Sobral (2015) and Sobral et al (2013) to the redshift we trace for CII] in our survey.…”

Section: Methodsmentioning

confidence: 99%

“…However, this effect has not yet been seen at lower redshifts with large surveys designed to capture the bright end well (e.g. Hα LF at z ∼ 0.2 and 0.8, Stroe & Sobral 2015;Sobral et al 2013). This might indicate that at these moderate redshifts, CII] can be significantly triggered in the shocks around more evolved, 'maintenance-mode' galaxies which are accreting at smaller rates (e.g.…”

Section: Cii] Emitters At Z ∼ 068mentioning

confidence: 99%

A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios

Stroe

Sobral

Matthee

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Recently, the CIII] and CIV emission lines have been observed in galaxies in the early Universe (z > 5), providing new ways to measure their redshift and study their stellar populations and AGN. We explore the first blind CII], CIII] and CIV survey (z ∼ 0.68, 1.05, 1.53, respectively) presented in Stroe et al. (2017). We derive luminosity functions (LF) and study properties of CII], CIII] and CIV line emitters through comparisons to the LFs of Hα and Lyα emitters, UV selected star forming (SF) galaxies and quasars at similar redshifts. The CII] LF at z ∼ 0.68 is equally well described by a Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity. The CIII] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter Hα and Lyα LF at their redshift, indicating a SF origin. In stark contrast, the CIV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that the brightest UV sources (M UV < −22) will universally have CIII] and CIV emission. However, on average, CIII] and CIV are not as abundant as Hα or Lyα emitters at the same redshift, with cosmic average ratios of ∼ 0.02 − 0.06 to Hα and ∼ 0.01 − 0.1 to intrinsic Lyα. We predict that the CIII] and CIV lines can only be truly competitive in confirming high redshift candidates when the hosts are intrinsically bright and the effective Lyα escape fraction is below 1 per cent. While CIII] and CIV were proposed as good tracers of young, relatively low-metallicity galaxies typical of the early Universe, we find that, at least at z ∼ 1.5, CIV is exclusively hosted by AGN/quasars, especially at large line equivalent widths.

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A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

Cited by 35 publications

References 60 publications

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

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

A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios

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A large narrow-band Hα survey at z∼ 0.2: the bright end of the luminosity function, cosmic variance and clustering across cosmic time

Cited by 35 publications

References 60 publications

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

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

A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios

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