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

Comparat, Johan; Zhu, Guangtun; González-Pérez, Violeta; Norberg, Peder; Newman, Jeffrey A.; Tresse, L.; Richard, Johan; Yepes, Gustavo; Kneib, Jean-Paul; Raichoor, Anand; Prada, Francisco; Maraston, Claudia; Yèche, Ch; Delubac, Timothée; Jullo, Eric

doi:10.1093/mnras/stw1393

Cited by 38 publications

(59 citation statements)

References 53 publications

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“…4 to the observational compilation done by Comparat et al (2016a) 10 , that includes data from the VVDS-Deep, VVDS-Wide and DEEP2 surveys among others (Ly et al 2007;Gilbank et al 2010;Sobral et al 2012;Drake et al 2013;Ciardullo et al 2013;Khostovan et al 2015). The model LFs are in reasonable agreement with the observations, with differences within a factor of 5 for densities above 10 −5 Mpc −3 h 3 dex −1 .…”

Section: Luminosity Functionssupporting

confidence: 65%

“…The particular filter response used for the different cuts is indicated by a superscript on the magnitude column. Comparat et al (2016a) are shown as filled circles, with colours matching the cuts used to mimic the corresponding survey selection, as indicated in the legend. The observational errors come from jackknife re-sampling (Comparat et al 2016a) and in some cases are smaller than the symbol.…”

Section: Luminosity Functionsmentioning

confidence: 99%

“…Similar trends are found over the redshift range 0.6 z 1.5, whenever a suffi- Table 2 cuts mimicking DEEP2 (blue), VVDS-Wide (red), eBOSS (yellow), and DESI (green). The grey circles show the observed [O ii] emitters LF constructed using complete data in a particular luminosity bins by Comparat et al (2016a). Data from DEEP2 and VVDS are colour coded like the model galaxies selected to mimic both surveys.…”

Section: Exploring the Elg Selectionmentioning

confidence: 99%

“…Dawson et al 2016;Laureijs et al 2011;DESI Collaboration et al 2016a;Pozzetti et al 2016). Current ELG samples are small and their characteristics are not well understood (Comparat et al 2016a;Kaasinen et al 2017). Initial tests on relatively small area surveys indicate that there are enough ELGs to chart space-time and understand the transition between the dark matter and the dark energy dominated eras (Comparat et al 2013;Okada et al 2016;Delubac et al 2017).…”

Section: Introductionmentioning

confidence: 99%

“…Previous work on modelling [O ii] emitters has shown that semi-analytic galaxy formation models can reproduce their observed luminosity function (LF) at z ∼ 1 (Orsi et al 2014;Comparat et al 2015Comparat et al , 2016a, making them ideal for studying the clustering properties of [O ii] emitters and hence bias. These predictions are used in the design and interpretation of current and future surveys, such as eBOSS (Dawson et al 2016) and DESI (DESI Collaboration et al 2016a).…”

Section: Introductionmentioning

confidence: 99%

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The host dark matter haloes of [O II] emitters at 0.5 < z < 1.5

González-Pérez¹,

Comparat²,

Norberg³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Emission line galaxies (ELGs) are used in several ongoing and upcoming surveys (SDSS-IV/eBOSS, DESI) as tracers of the dark matter distribution. Using a new galaxy formation model, we explore the characteristics of [O ii] emitters, which dominate optical ELG selections at z 1. Model [O ii] emitters at 0.5 < z < 1.5 are selected to mimic the DEEP2, VVDS, eBOSS and DESI surveys. The luminosity functions of model [O ii] emitters are in reasonable agreement with observations. The selected [O ii] emitters are hosted by haloes with M halo 10 10.3 h −1 M , with ∼ 90% of them being central star-forming galaxies. The predicted mean halo occupation distributions of [O ii] emitters has a shape typical of that inferred for star-forming galaxies, with the contribution from central galaxies, N [O ii] cen , being far from the canonical step function. The N [O ii] cen can be described as the sum of an asymmetric Gaussian for disks and a step function for spheroids, which plateaus below unity. The model [O ii] emitters have a clustering bias close to unity, which is below the expectations for eBOSS and DESI ELGs. At z ∼ 1, a comparison with observed g-band selected galaxy, which are expected to be dominated by [O ii] emitters, indicates that our model produces too few [O ii] emitters that are satellite galaxies. This suggests the need to revise our modelling of hot gas stripping in satellite galaxies.

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Section: Luminosity Functionssupporting

confidence: 65%

Section: Luminosity Functionsmentioning

confidence: 99%

Section: Exploring the Elg Selectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The host dark matter haloes of [O II] emitters at 0.5 < z < 1.5

González-Pérez¹,

Comparat²,

Norberg³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The OTELO survey

Bongiovanni

Ramón-Pérez

García

et al. 2020

A&A

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Context. The OSIRIS Tunable Filter Emission Line Object (OTELO) survey is a very deep, blind exploration of a selected region of the Extended Groth Strip and is designed for finding emission-line sources (ELSs). The survey design, observations, data reduction, astrometry, and photometry, as well as the correlation with ancillary data used to obtain a final catalogue, including photo-z estimates and a preliminary selection of ELS, were described in a previous contribution. Aims. Here, we aim to determine the main properties and luminosity function (LF) of the [O III] ELS sample of OTELO as a scientific demonstration of its capabilities, advantages, and complementarity with respect to other surveys. Methods. The selection and analysis procedures of ELS candidates obtained using tunable filter pseudo-spectra are described. We performed simulations in the parameter space of the survey to obtain emission-line detection probabilities. Relevant characteristics of [O III] emitters and the LF ([O III]), including the main selection biases and uncertainties, are presented. Results. From 541 preliminary emission-line source candidates selected around z = 0.8, a total of 184 sources were confirmed as [O III] emitters. Consistent with simulations, the minimum detectable line flux and equivalent width in this ELS sample are ∼5 × 10−19 erg s−1 cm2 and ∼6 Å, respectively. We are able to constrain the faint-end slope (α = −1.03 ± 0.08) of the observed LF ([O III]) at a mean redshift of z = 0.83. This LF reaches values that are approximately ten times lower than those from other surveys. The vast majority (84%) of the morphologically classified [O III] ELSs are disc-like sources, and 87% of this sample is comprised of galaxies with stellar masses of M⋆ < 1010 M⊙.

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J-PLUS: Synthetic galaxy catalogues with emission lines for photometric surveys

Angulo

Orsi

Hurier

et al. 2019

A&A

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We present a synthetic galaxy lightcone specially designed for narrow-band optical photometric surveys. To reduce time-discreteness effects, unlike previous works, we directly include the lightcone construction in the L-Galaxies semi-analytic model applied to the subhalo merger trees of the Millennium simulation. Additionally, we add a model for the nebular emission in star-forming regions, which is crucial for correctly predicting the narrow/medium-band photometry of galaxies. Explicitly, we consider, individually for each galaxy, the contribution of 9 different lines: 6583Å), and [S ii] (6717Å, 6731Å). We validate our lightcone by comparing galaxy number counts, angular clustering, and Hα , Hβ , [O ii] and [O iii] 5007 luminosity functions to a compilation of observations. As an application of our mock lightcones, we generate catalogues tailored for J-PLUS, a large optical galaxy survey featuring 5 broad and 7 medium band filters. We study the ability of the survey to correctly identify, with a simple three filter method, a population of emission-line galaxies at various redshifts. We show that the 4000Å break in the spectral energy distribution of galaxies can be misidentified as line emission. However, all significant excess (larger than 0.4 magnitudes) can be correctly and unambiguously attributed to emission line galaxies. Our catalogues are publicly released to facilitate their use in interpreting narrow-band surveys and for quantifying the impact of line emission in broad band photometry.

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

Cited by 38 publications

References 53 publications

The host dark matter haloes of [O II] emitters at 0.5 < z < 1.5

The host dark matter haloes of [O II] emitters at 0.5 < z < 1.5

The OTELO survey

J-PLUS: Synthetic galaxy catalogues with emission lines for photometric surveys

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