The 0.1 &lt;<i>z</i>&lt; 1.65 evolution of the bright end of the [O ii] luminosity function

Comparat, Johan; Richard, Johan; Kneib, Jean-Paul; Ilbert, O.; González-Pérez, Violeta; Tresse, L.; Zoubian, J.; Arnouts, S.; Brownstein, Joel R.; Baugh, C. M.; Delubac, Timothée; Ealet, A.; Escoffier, S.; Ge, Jian; Jullo, Eric; Lacey, Cedric G.; Ross, Nicholas P.; Schlegel, David J.; Schneider, Donald P.; Steele, Oliver; Tasca, L.; Yèche, Ch; Lesser, Michael P.; Jiang, Zhaoji; Jing, Y. P.; Zhang, Fan; Fan, Xiaohui; Ma, Jun; Nie, Jundan; Wang, Jiali; Wu, Zhenyu; Zhang, Tianmeng; Xu, Zhiyong; Zhang, Zhimin; Zou, Hu

doi:10.1051/0004-6361/201424767

Cited by 106 publications

(107 citation statements)

References 70 publications

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“…This result agrees with those from the Comparat et al (2015b) study of the [Oii] luminosity function.…”

Section: [Oii] Fluxsupporting

confidence: 92%

“…The u-band filter used in the SCUSS project is similar to the SDSS u-band filter but slightly bluer. For our aims, this deep u-band imaging brings valuable improvement with respect to the SDSS u-band photometry, given that the u-band magnitude tightly correlates with the [Oii] flux (Comparat et al 2015b) and that the typical ELGs at 0.6 ≤ z spec ≤ 1.0 are too faint to have a robust measurement in the SDSS u-band.…”

Section: Photometrymentioning

confidence: 99%

“…We also add all the SDSS DR12 public spectroscopic redshifts (DR12, Alam et al 2015; SDSS and BOSS spectrographs: 3800-9200 Å and 3650-10 400 Å; R ∼ 1500-2500; 0.75-1 h exposure time) covering those survey regions. Comparat et al (2015b) ELGs. Futhermore, we enlarge our Fisher training sample by adding ∼10 4 ELGs observed as pilot programmes for eBOSS and DESI (Paper I).…”

Section: Fisher Training Samplementioning

confidence: 99%

“…(4)): the efficiency in selecting [Oii] emitters is a byproduct of the presence of the deep SCUSS u-band. Indeed, the faint magnitude cut on the SCUSS photometry favours z ∼ 0.8 starforming galaxies against z ∼ 0.8 passive galaxies, which have faint emission in the u-band (see for instance Comparat et al 2015b). In contrast, we observe that, though having a strong correlation with redshift by training, the Fisher_GRIW1 is inefficient at distinguishing [Oii] emitters.…”

Section: (3)mentioning

confidence: 99%

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The SDSS-IV extended Baryon Oscillation Spectroscopic Survey: selecting emission line galaxies using the Fisher discriminant

Raichoor

Comparat

Delubac

et al. 2015

A&A

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We present a new selection technique of producing spectroscopic target catalogues for massive spectroscopic surveys for cosmology. This work was conducted in the context of the extended Baryon Oscillation Spectroscopic Survey (eBOSS), which will use ∼200 000 emission line galaxies (ELGs) at 0.6 ≤ z spec ≤ 1.0 to obtain a precise baryon acoustic oscillation measurement. Our proposed selection technique is based on optical and near-infrared broad-band filter photometry. We used a training sample to define a quantity, the Fisher discriminant (linear combination of colours), which correlates best with the desired properties of the target: redshift and [Oii] flux. The proposed selections are simply done by applying a cut on magnitudes and this Fisher discriminant. We used public data and dedicated SDSS spectroscopy to quantify the redshift distribution and [Oii] flux of our ELG target selections. We demonstrate that two of our selections fulfil the initial eBOSS/ELG redshift requirements: for a target density of 180 deg −2 , ∼70% of the selected objects have 0.6 ≤ z spec ≤ 1.0 and only ∼1% of those galaxies in the range 0.6 ≤ z spec ≤ 1.0 are expected to have a catastrophic z spec estimate. Additionally, the stacked spectra and stacked deep images for those two selections show characteristic features of star-forming galaxies. The proposed approach using the Fisher discriminant could, however, be used to efficiently select other galaxy populations, based on multi-band photometry, providing that spectroscopic information is available. This technique could thus be useful for other future massive spectroscopic surveys such as PFS, DESI, and 4MOST.

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“…This result agrees with those from the Comparat et al (2015b) study of the [Oii] luminosity function.…”

Section: [Oii] Fluxsupporting

confidence: 92%

Section: Photometrymentioning

confidence: 99%

Section: Fisher Training Samplementioning

confidence: 99%

Section: (3)mentioning

confidence: 99%

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The SDSS-IV extended Baryon Oscillation Spectroscopic Survey: selecting emission line galaxies using the Fisher discriminant

Raichoor

Comparat

Delubac

et al. 2015

A&A

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“…PFS/SuMIRe or DESI). We suggest that the [OIII] luminosity function should be better determined over a large redshift range, as recently completed by Comparat et al (2015) for the [OII] luminosity function over the redshift range [0.1-1.65]. This kind of study can be carried out using the WISP (WFC3 Infrared Spectroscopic Parallel) survey (Atek et al 2010, PI: Malkan) in which several hundred USELS were found by Atek et al (2014) over the redshift range 0.3 < z < 2.3.…”

Section: Discussion and Implication For High-z Surveyssupporting

confidence: 52%

Narrowband selected high-redshift galaxy candidates contaminated by lower redshift [OIII] ultra-strong emitter line galaxies

Pénin

Cuby

Clément

et al. 2015

A&A

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Context. Lyman-break galaxies (LBG) and narrowband (NB) surveys have been successful at detecting large samples of high-redshift galaxies. Both methods are subject to contamination from low-redshift interlopers. Aims. Our aim is to investigate the nature of low-redshift interlopers in NB Lyman-α emitters (LAE) searches. Methods. From previous HAWK-I NB imaging at z ∼ 7.7, we identify three objects that would have been selected as high-redshift LAEs had our optical data been one magnitude shallower (but still one to two magnitudes fainter than the near infrared data). We follow up these objects in spectroscopy with X-Shooter at the VLT. Results. Despite low quality data due to bad weather conditions, for each of the three objects we identify one, and only one emission line, in the spectra of the objects that we identify as the [OIII]5007 Å line. From this result, combined with spectral energy density fitting and tests based on line ratios of several populations of galaxies, we infer that the three objects are ultra-strong line emitters at redshifts ∼1.1. Conclusions. From this work and the literature we remark that the [OIII] line appears to be a common source of contamination in high-redshift LBG and LAE samples and we suggest that efforts be made to characterize with high accuracy the [OIII] luminosity function out to redshift ∼3 or higher.

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Evolution of the specific star formation rate function atz< 1.4 Dissecting the mass-SFR plane in COSMOS and GOODS

Ilbert

Arnouts

Floc’h

et al. 2015

A&A

181

222

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The relation between the stellar mass (M⋆) and the star formation rate (SFR) characterizes how the instantaneous star formation is determined by the galaxy past star formation history and by the growth of the dark matter structures. We deconstruct the M⋆ − SFR plane by measuring the specific SFR functions in several stellar mass bins from z = 0.2 out to z = 1.4 (specific SFR = SFR/M⋆, noted sSFR). Our analysis is primary based on a 24µm selected catalogue combining the COSMOS and GOODS surveys. We estimate the SFR by combining mid-and far-infrared data for 20500 galaxies. The sSFR functions are derived in four stellar mass bins within the range 9.5 < log(M⋆/M ⊙ ) < 11.5. First, we demonstrate the importance of taking into account selection effects when studying the M⋆ − SFR relation. Secondly, we find a mass-dependent evolution of the median sSFR with redshift varying as sSFR ∝ (1 + z) b , with b increasing from b = 2.88 ±0.12 to b = 3.78 ±0.60 between M⋆ = 10 9.75 M ⊙ and M⋆ = 10 11.1 M ⊙ , respectively. At low masses, this evolution is consistent with the cosmological accretion rate and predictions from semi-analytical models (SAM). This agreement breaks down for more massive galaxies showing the need for a more comprehensive description of the star formation history in massive galaxies. Third, we obtain that the shape of the sSFR function is invariant with time at z < 1.4 but depends on the mass. We observe a broadening of the sSFR function ranging from 0.28 dex at M⋆ = 10 9.75 M ⊙ to 0.46 dex at M⋆ = 10 11.1 M ⊙ . Such increase in the intrinsic scatter of the M⋆ − SFR relation suggests an increasing diversity of SFHs as the stellar mass increases. Finally, we find a gradual decline of the sSFR with stellar mass as log10(sSFR) ∝ −0.17M⋆. We discuss the numerous physical processes, as gas exhaustion in hot gas halos or secular evolution, which can gradually reduce the sSFR and increase the SFH diversity.

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The 0.1 <z< 1.65 evolution of the bright end of the [O ii] luminosity function

Cited by 106 publications

References 70 publications

The SDSS-IV extended Baryon Oscillation Spectroscopic Survey: selecting emission line galaxies using the Fisher discriminant

The SDSS-IV extended Baryon Oscillation Spectroscopic Survey: selecting emission line galaxies using the Fisher discriminant

Narrowband selected high-redshift galaxy candidates contaminated by lower redshift [OIII] ultra-strong emitter line galaxies

Evolution of the specific star formation rate function atz< 1.4 Dissecting the mass-SFR plane in COSMOS and GOODS

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