Photometric redshifts for the CFHTLS T0004 deep and wide fields

Coupon, J.; Ilbert, O.; Kilbinger, M.; McCracken, H. J.; Mellier, Y.; Arnouts, S.; Bertin, E.; Hudelot, P.; Schultheis, M.; Fèvre, O. Le; Brun, V. Le; Guzzo, L.; Bardelli, S.; Zucca, E.; Bolzonella, M.; Garilli, B.; Zamorani, G.; Zanichelli, A.; Tresse, L.; Aussel, H.

doi:10.1051/0004-6361/200811413

Cited by 190 publications

(326 citation statements)

References 40 publications

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“…Our photometric redshifts were measured using LePhare (Arnouts et al 2002) following the procedures outlined in Ilbert et al (2006) and Coupon et al (2009). Our primary template set is composed of the four Coleman et al (1980) (CWW) observed spectra (Ell, Sbc, Scd, Irr) complemented with two observed starburst spectral energy distributions (SED) from Kinney et al (1996).…”

Section: Photometric Redshift Estimationmentioning

confidence: 99%

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

Coupon

Kilbinger

McCracken

et al. 2012

A&A

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172

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It has become increasingly apparent that studying how dark matter haloes are populated by galaxies can provide new insights into galaxy formation and evolution. In this paper, we present a detailed investigation of the changing relationship between galaxies and the dark matter haloes they inhabit from z ∼ 1.2 to the present day. We do this by comparing precise galaxy clustering measurements over 133 deg 2 of the "Wide" component of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) with predictions of an analytic halo occupation distribution (HOD) model where the number of galaxies in each halo depends only on the halo mass. Starting from a parent catalogue of ∼3 × 10 6 galaxies at i AB < 22.5 we use accurate photometric redshifts calibrated using ∼10 4 spectroscopic redshifts to create a series of type-selected volume-limited samples covering 0.2 < z < 1.2. Our principal result, based on clustering measurements in these samples, is a robust determination of the luminosity-to-halo mass ratio and its dependence on redshift and galaxy type. For the full sample, this reaches a peak at low redshifts of M peak h = 4.5 × 10 11 h −1 M and moves towards higher halo masses at higher redshifts. For redder galaxies the peak is at higher halo masses and does not evolve significantly over the entire redshift range of our survey. We also consider the evolution of bias, average halo mass and the fraction of satellites as a function of redshift and luminosity. Our observed growth of a factor of ∼2 in satellite fraction between z ∼ 1 and z ∼ 0 is testament to the limited role that galaxy merging plays in galaxy evolution for ∼10 12 h −1 M mass haloes at z < 1. Qualitatively, our observations are consistent with a picture in which red galaxies in massive haloes have already accumulated most of their stellar mass by z ∼ 1 and subsequently undergo little evolution until the present day. The observed movement of the peak location for the full galaxy population is consistent with the bulk of star-formation activity migrating from higher mass haloes at high redshifts to lower mass haloes at lower redshifts.

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Section: Photometric Redshift Estimationmentioning

confidence: 99%

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

Coupon

Kilbinger

McCracken

et al. 2012

A&A

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172

245

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“…To estimate the SSR, we use the photometric redshift catalogues from Ilbert et al (2006Ilbert et al ( , 2009 and Coupon et al (2009) to complement the spectroscopic redshift catalogues. These photometric Table 3 and text for further details.…”

Section: Sampling Rate Correctionsmentioning

confidence: 99%

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

Comparat

Zhu

González-Pérez

et al. 2016

Mon. Not. R. Astron. Soc.

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Citation for published item:gomp r tD tF nd huD qF nd qonz lezE erezD F nd xor ergD F nd xewm nD tF nd resseD vF nd i h rdD tF nd epesD qF nd unei D tFE F nd i hoorD eF nd r d D pF nd w r stonD gF nd e heD gF nd helu D F nd tulloD iF @PHITA 9 he evolution of the y ss D r nd y sss emission line luminosity fun tions over the l st nine illions ye rsF9D wonthly noti es of the oy l estronomi l o ietyFD RTI @IAF ppF IHUTEIHVUF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTEmission line galaxies are one of the main tracers of the large-scale structure to be targeted by the next-generation dark energy surveys. To provide a better understanding of the properties and statistics of these galaxies, we have collected spectroscopic data from the VVDS and DEEP2 deep surveys and estimated the galaxy luminosity functions (LFs) of three distinct emission lines, [O II] (λλ3726, 3729) (0.5 < z < 1.3), Hβ (λ4861) (0.3 < z < 0.8) and [O III] (λ5007) (0.3 < z < 0.8). Our measurements are based on 35 639 emission line galaxies and cover a volume of ∼10 7 Mpc 3 . We present the first measurement of the Hβ LF at these redshifts. We have also compiled LFs from the literature that were based on independent data or covered different redshift ranges, and we fit the entire set over the whole redshift range with analytic Schechter and Saunders models, assuming a natural redshift dependence of the parameters. We find that the characteristic luminosity (L * ) and density (φ * ) of all LFs increase with redshift. Using the Schechter model over the redshift ranges considered, we find that, for [O II] emitters, the characteristic luminosity L * (z = 0.5) = 3.2 × 10 41 erg s −1 increases by a factor of 2.7 ± 0.2 from z = 0.5 to 1.3; for Hβ emitters L * (z = 0.3) = 1.3 × 10 41 erg s −1 increases by a factor of 2.0 ± 0.2 from z = 0.3 to 0.8; and for [O III] emitters L * (z = 0.3) = 7.3 × 10 41 erg s −1 increases by a factor of 3.5 ± 0.4 from z = 0.3 to 0.8.

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“…For both surveys, observations are carried out in five filters (u * , g , r , i and z ), providing catalogs of sources that are 80% complete up to i AB = 26.0 (CFHTLS-D) and i AB = 24.0 (CFHTLS-W) (Mellier et al 2008, http://terapix.iap.fr/cplt/oldSite/Descart/ CFHTLS-T0005-Release.pdf). The CFHTLS-W, in particular, encloses a sample of about 20 × 10 6 galaxies inside a volume size of ∼1 Gpc 3 , with a median redshift of z ∼ 0.92 (Coupon et al 2009). According to the standard cosmological model, the CFHTLS-W (W1, W2, W3, and W4 herafter) is then expected to contain 1000 to 5000 clusters of galaxies with accurate photometric redshifts, most of them in the 0.6 < z < 1.5 range.…”

Section: Introductionmentioning

confidence: 99%

Galaxy structure searches by photometric redshifts in the CFHTLS

Adami¹,

Durret

Benoist

et al. 2010

A&A

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Context. Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. Aims. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). Methods. We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1 × 1 deg 2 ), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i = 25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations. Results. We detected 1200 candidate clusters with various masses (minimal masses between 1.0 × 10 13 and 5.5 × 10 13 and mean masses between 1.3 × 10 14 and 12.6 × 10 14 M ) in the CFHTLS Deep and Wide fields, thus notably increasing the number of known high redshift cluster candidates. We found a correlation function for these objects comparable to that obtained for high redshift cluster surveys. We also show that the CFHTLS deep survey is able to trace the large scale structure of the universe up to z ≥ 1. Our detections are fully consistent with those made in various CFHTLS analyses with other methods. We now need accurate mass determinations of these structures to constrain cosmological parameters. Conclusions. We have shown that a search for galaxy clusters based on density maps built from galaxy catalogs in photometric redshift bins is successful and gives results comparable to or better than those obtained with other methods. By applying this technique to the CFHTLS survey we have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards using cluster counts to measure cosmological parameters.

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Photometric redshifts for the CFHTLS T0004 deep and wide fields

Cited by 190 publications

References 40 publications

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes sincez ~ 1.2

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

Galaxy structure searches by photometric redshifts in the CFHTLS

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