Aims. We present and release photometric redshifts for a uniquely large and deep sample of 522286 objects with i'(AB) <= 25 in the Canada-France Hawaii Telescope Legacy Survey (CFHTLS) "Deep Survey" fields D1, D2, D3, and D4, which cover a total effective area of 3.2 deg(2). Methods: We use 3241 spectroscopic redshifts with 0 <= z <= 5 from the VIMOS VLT Deep Survey (VVDS) as a calibration and training set to derive these photometric redshifts. Using the "Le Phare" photometric redshift code, we developed a robust calibration method based on an iterative zero-point refinement combined with a template optimisation procedure and the application of a Bayesian approach. This method removes systematic trends in the photometric redshifts and significantly reduces the fraction of catastrophic errors ( by a factor of 2), a significant improvement over traditional methods. We use our unique spectroscopic sample to present a detailed assessment of the robustness of the photometric redshift sample. Results. For a sample selected at i'(AB) = 24, we reach a redshift accuracy of sigma(Delta z/(1+ z)) = 0.029 with eta = 3.8% of catastrophic errors (eta is defined strictly as those objects with |Delta z|/(1 + z) > 0.15). The reliability of our photometric redshifts decreases for faint objects: we find sigma(Delta z/(1+ z)) = 0.025, 0.034 and. = 1.9%, 5.5% for samples selected at i'(AB) = 17.5 - 22.5 and 22.5 - 24 respectively. We find that the photometric redshifts of starburst galaxies are less reliable: although these galaxies represent only 22% of the spectroscopic sample, they are responsible for 50% of the catastrophic errors. An analysis as a function of redshift demonstrates that our photometric redshifts work best in the redshift range 0.2 <= z <= 1.5. We find an excellent agreement between the photometric and the VVDS spectroscopic redshift distributions at i'(AB) <= 24. Finally, we compare the redshift distributions of i' selected galaxies on the four CFHTLS deep fields, showing that cosmic variance is still present on fields of 0.7-0.9 deg(2). These photometric redshifts are made publicly available at http://terapix.iap.fr(complete ascii catalogues) and http://cencos. oamp.fr/cencos/CFHTLS/(searchable database interface).
Accurate photometric redshifts for the CFHT legacy survey calibrated using the VIMOS VLT deep survey / O. Ilbert, S. Arnouts, H.J. Mccracken, M. Bolzonella, E. Bertin, O. Le Fèvre, Y. Mellier, G. Zamorani, R. Pellò, A. Iovino, L. Tresse, V. Le Brun, D. Bottini, B. Garilli, D. Maccagni, J.P. Picat, R. Scaramella, M. Scodeggio, G. Vettolani, A. Zanichelli, C. Adami, S. Bardelli, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, O. Cucciati, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, A. Pollo, L. Pozzetti, M. Radovich, E. Zucca, M. Bondi, A. Bongiorno, G. Busarello, S. De La Torre, L. Gregorini, F. Lamareille, G. Mathez, P. Merluzzi, V. Ripepi, D. Rizzo, D. Vergani. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 457:3(2006), pp. 841-856. [10.1051/0004-6361:20065138]
Accurate photometric redshifts for the CFHT legacy survey calibrated using the VIMOS VLT deep survey
L. Guzzo;D. Rizzo;
2006
Abstract
Aims. We present and release photometric redshifts for a uniquely large and deep sample of 522286 objects with i'(AB) <= 25 in the Canada-France Hawaii Telescope Legacy Survey (CFHTLS) "Deep Survey" fields D1, D2, D3, and D4, which cover a total effective area of 3.2 deg(2). Methods: We use 3241 spectroscopic redshifts with 0 <= z <= 5 from the VIMOS VLT Deep Survey (VVDS) as a calibration and training set to derive these photometric redshifts. Using the "Le Phare" photometric redshift code, we developed a robust calibration method based on an iterative zero-point refinement combined with a template optimisation procedure and the application of a Bayesian approach. This method removes systematic trends in the photometric redshifts and significantly reduces the fraction of catastrophic errors ( by a factor of 2), a significant improvement over traditional methods. We use our unique spectroscopic sample to present a detailed assessment of the robustness of the photometric redshift sample. Results. For a sample selected at i'(AB) = 24, we reach a redshift accuracy of sigma(Delta z/(1+ z)) = 0.029 with eta = 3.8% of catastrophic errors (eta is defined strictly as those objects with |Delta z|/(1 + z) > 0.15). The reliability of our photometric redshifts decreases for faint objects: we find sigma(Delta z/(1+ z)) = 0.025, 0.034 and. = 1.9%, 5.5% for samples selected at i'(AB) = 17.5 - 22.5 and 22.5 - 24 respectively. We find that the photometric redshifts of starburst galaxies are less reliable: although these galaxies represent only 22% of the spectroscopic sample, they are responsible for 50% of the catastrophic errors. An analysis as a function of redshift demonstrates that our photometric redshifts work best in the redshift range 0.2 <= z <= 1.5. We find an excellent agreement between the photometric and the VVDS spectroscopic redshift distributions at i'(AB) <= 24. Finally, we compare the redshift distributions of i' selected galaxies on the four CFHTLS deep fields, showing that cosmic variance is still present on fields of 0.7-0.9 deg(2). These photometric redshifts are made publicly available at http://terapix.iap.fr(complete ascii catalogues) and http://cencos. oamp.fr/cencos/CFHTLS/(searchable database interface).
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