Accurate photometric redshifts for the CFHT legacy survey calibrated using the VIMOS VLT deep survey

By O. Ilbert, Stéphane Arnouts, H. McCracken, M. Bolzonella, E. Bertin, O. Fèvre, Y. Mellier, G. Zamorani, R. Pell'o, A. Iovino and 42 more. 2006

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We present photometric redshifts for an uniquely large and deep sample of 522286 objects with i'_{AB}<25 in the Canada-France Legacy Survey ``Deep Survey'' fields, which cover a total effective area of 3.2 deg^2. We use 3241 spectroscopic redshifts with 0

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/61f42e07ca65504ec4937b9e40f834e12ea15285

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Citations in the corpus

EVOLUTION OF GALAXIES AND THEIR ENVIRONMENTS AT z = 0.1–3 IN COSMOS (2013, methodology): “Photoz were derived for 218,000 galaxies with Ks (AB)< 24 mag using a χ2 template fitting procedure (Le Phare : Arnouts et al. 2002; Ilbert et al. 2006).”
A Dark Core in Abell 520 (2007, methodology): “To do so, we use the photometric redshift distribution from Ilbert et al. (2006), which are based on the CFHT Legacy Survey Deep fields.”
A CRITICAL ASSESSMENT OF PHOTOMETRIC REDSHIFT METHODS: A CANDELS INVESTIGATION (2013, methodology): “Of these codes, three are common to this investigation (EAZY, LePhare, and HyperZ).”
Evidence of the accelerated expansion of the Universe from weak lensing tomography with COSMOS (2009, methodology): “Ilbert et al. (2009) computed photometric redshift using theLe Pharecode (S. Arnouts & O. Ilbert; also Ilbert et al. 2006), reaching an excellent accuracy ofσ∆z/(1+z) = 0.012 for i+ < 24 andz< 1.25.”
Weak Gravitational Lensing with COSMOS: Galaxy Selection and Shape Measurements (2007, methodology): “For most forthcoming weak-lensing surveys, this will also be the case, hence the importance of the photometric redshift technique to measure redshifts for amajority of the galaxies, to and beyond today’s spectroscopic limits ( Ilbert et al. 2006).”
Photometric redshifts for the CFHTLS T0004 deep and wide fields (2008, methodology): “Following Ilbert et al (2006) spectroscopic redshifts were used to optimise ourSED templates and to correct the systematic offsets between the observations and SEDs.”
The VIMOS Public Extragalactic Survey (VIPERS) - First Data Release of 57 204 spectroscopic measurements (2013, methodology): “An automatic algorithm cross-correlates the spectroscopic measurement (zspec) with the corresponding photometric redshift (zphot), estimated from the five-band CFHTLS photometry using the Le Phare code (Ilbert et al. 2006; Arnouts & Ilbert 2011).”
The Pantheon+ Analysis: The Full Data Set and Light-curve Release (2021, methodology): “In order to determine host-galaxy properties from the photometry of the galaxies, we used the LePHARE SED-fitting method (Ilbert et al. 2006).”
CLASH: THREE STRONGLY LENSED IMAGES OF A CANDIDATE z ≈ 11 GALAXY (2012, methodology): “Le PHARE We also used Le PHARE (Arnouts et al. 1999; Ilbert et al. 2006, 2009) to independently estimate the photometric redshifts.”
Masses of Galaxy Clusters from Gravitational Lensing (2013, methodology): “…in the literature, e.g. from the COSMOS survey (Ilbert et al. 2009) or the Hubble Ultra Deep Field (Coe et al. 2006) or the CFHTLS Deep fields (Ilbert et al. 2006), while taking into account the weights assigned to the background galaxies of different magnitudes when making the weak shear…”
Photometric redshift analysis in the Dark Energy Survey Science Verification data (2014, methodology): “…template fitting methods (e.g. Hyperz, Bolzonella, Miralles & Pell (2000); BPZ, Benitez (2000); Coe et al. (2006); LePhare, Arnouts et al. (2002); Ilbert et al. (2006); EAZY, Brammer, van Dokkum & Coppi (2008)), in which the measured broadband galaxy spectral energy distribution (SED) obtained…”
A Bayesian approach to strong lensing modelling of galaxy clusters (2007, background): “A spectroscopic determination is best, but a photometric redshift (e.g. Ilbert et al. (2006)) can be sufficient if accurate enough (e.g. σz < 0.05 introduces a 2% error on the DLS/DOS ratio for a lens and a source at redshifts zL = 0.2 and zS = 1 respectively) and with no multiple peak in its…”
THE BLANCO COSMOLOGY SURVEY: DATA ACQUISITION, PROCESSING, CALIBRATION, QUALITY DIAGNOSTICS, AND DATA RELEASE (2012, background): “The first, following Ilbert et al. (2006), is the normalized median absolute deviation σ∆z/(1+z) = 1.48×median ( |∆z| 1 + zspec ) .”
CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing (2013, methodology): “The measurements are also corrected for contamination by physically associated sources, as described in VU11, and scaled with〈β〉 = 0.30 which is determined by integrating over the lens and source redshift distributions that were obtained from the CFHTLS “Deep Survey” fields (Ilbert et al. 2006).”
zCOSMOS – 10k-bright spectroscopic sample - The bimodality in the galaxy stellar mass function: exploring its evolution with redshift (2009, methodology): “Following Zucca et al. (2006), we used the empirical set of (62) SEDs described in Ilbert et al. (2006).”
The WiggleZ Dark Energy Survey: survey design and first data release (2009, methodology): “The internal photometric precision of the RCS2 is close to that of the CFHT Legacy Survey (Ilbert et al. 2006), i.e. 0.04 mag in each band; the magnitudes are on the AB system, calculated from a curve-of-growth analysis.”
COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs (2021, methodology): “The method is the same as Ilbert et al. (2006): after having fixed the redshift to the spec-z value, the photometric offset of each band is derived by minimizing the difference between the predicted and observed fluxes.”
Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA (2013, methodology): “The redshift accuracy σ∆z/(1+zs) is computed using the normalised median absolute deviation (Ilbert et al. 2006).”
Spectral Energy Distributions of Hard X-Ray Selected Active Galactic Nuclei in the XMM-Newton Medium Deep Survey (2007, positive): “Photometric redshift techniques have been applied to optical or optical and near-IR data sets, providing reliable photometric redshifts (Rowan-Robinson et al. 2005; Ilbert et al. 2006; Brodwin et al. 2006).”