Photometric redshift analysis in the Dark Energy Survey Science Verification data
In this study, we present results from a study of the photometric redshift performance of the Dark Energy Survey (DES), using the early data from a Science Verification period of observations in late 2012 and early 2013 that provided science-quality images for almost 200 sq. deg. at the nominal dept...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2014-10, Vol.445 (2) |
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| creator | Sanchez, C. Carrasco Kind, M. Lin, H. Miquel, R. Abdalla, F. B. Amara, A. Banerji, M. Bonnett, C. Brunner, R. Capozzi, D. Carnero, A. Castander, F. J. da Costa, L. A. N. Cunha, C. Fausti, A. Gerdes, D. Greisel, N. Gschwend, J. Hartley, W. Jouvel, S. Lahav, O. Lima, M. Maia, M. A. G. Marti, P. Ogando, R. L. C. Ostrovski, F. Pellegrini, P. Rau, M. M. Sadeh, I. Seitz, S. Sevilla-Noarbe, I. Sypniewski, A. de Vicente, J. Abbot, T. Allam, S. S. Atlee, D. Bernstein, G. Bernstein, J. P. Buckley-Geer, E. Burke, D. Childress, M. J. Davis, T. DePoy, D. L. Dey, A. Desai, S. Diehl, H. T. Doel, P. Estrada, J. Evrard, A. Fernandez, E. Finley, D. Flaugher, B. Frieman, J. Gaztanaga, E. Glazebrook, K. Honscheid, K. Kim, A. Kuehn, K. Kuropatkin, N. Lidman, C. Makler, M. Marshall, J. L. Nichol, R. C. Roodman, A. Sanchez, E. Santiago, B. X. Sako, M. Scalzo, R. Smith, R. C. Swanson, M. E. C. Tarle, G. Thomas, D. Tucker, D. L. Uddin, S. A. Valdes, F. Walker, A. Yuan, F. Zuntz, J. |
| description | In this study, we present results from a study of the photometric redshift performance of the Dark Energy Survey (DES), using the early data from a Science Verification period of observations in late 2012 and early 2013 that provided science-quality images for almost 200 sq. deg. at the nominal depth of the survey. We assess the photometric redshift (photo-z) performance using about 15 000 galaxies with spectroscopic redshifts available from other surveys. These galaxies are used, in different configurations, as a calibration sample, and photo-z's are obtained and studied using most of the existing photo-z codes. A weighting method in a multidimensional colour–magnitude space is applied to the spectroscopic sample in order to evaluate the photo-z performance with sets that mimic the full DES photometric sample, which is on average significantly deeper than the calibration sample due to the limited depth of spectroscopic surveys. In addition, empirical photo-z methods using, for instance, artificial neural networks or random forests, yield the best performance in the tests, achieving core photo-z resolutions σ68 ~ 0.08. Moreover, the results from most of the codes, including template-fitting methods, comfortably meet the DES requirements on photo-z performance, therefore, providing an excellent precedent for future DES data sets. |
| format | Article |
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J. ; da Costa, L. A. N. ; Cunha, C. ; Fausti, A. ; Gerdes, D. ; Greisel, N. ; Gschwend, J. ; Hartley, W. ; Jouvel, S. ; Lahav, O. ; Lima, M. ; Maia, M. A. G. ; Marti, P. ; Ogando, R. L. C. ; Ostrovski, F. ; Pellegrini, P. ; Rau, M. M. ; Sadeh, I. ; Seitz, S. ; Sevilla-Noarbe, I. ; Sypniewski, A. ; de Vicente, J. ; Abbot, T. ; Allam, S. S. ; Atlee, D. ; Bernstein, G. ; Bernstein, J. P. ; Buckley-Geer, E. ; Burke, D. ; Childress, M. J. ; Davis, T. ; DePoy, D. L. ; Dey, A. ; Desai, S. ; Diehl, H. T. ; Doel, P. ; Estrada, J. ; Evrard, A. ; Fernandez, E. ; Finley, D. ; Flaugher, B. ; Frieman, J. ; Gaztanaga, E. ; Glazebrook, K. ; Honscheid, K. ; Kim, A. ; Kuehn, K. ; Kuropatkin, N. ; Lidman, C. ; Makler, M. ; Marshall, J. L. ; Nichol, R. C. ; Roodman, A. ; Sanchez, E. ; Santiago, B. X. ; Sako, M. ; Scalzo, R. ; Smith, R. C. ; Swanson, M. E. C. ; Tarle, G. ; Thomas, D. ; Tucker, D. L. ; Uddin, S. A. ; Valdes, F. ; Walker, A. ; Yuan, F. ; Zuntz, J.</creator><creatorcontrib>Sanchez, C. ; Carrasco Kind, M. ; Lin, H. ; Miquel, R. ; Abdalla, F. B. ; Amara, A. ; Banerji, M. ; Bonnett, C. ; Brunner, R. ; Capozzi, D. ; Carnero, A. ; Castander, F. J. ; da Costa, L. A. N. ; Cunha, C. ; Fausti, A. ; Gerdes, D. ; Greisel, N. ; Gschwend, J. ; Hartley, W. ; Jouvel, S. ; Lahav, O. ; Lima, M. ; Maia, M. A. G. ; Marti, P. ; Ogando, R. L. C. ; Ostrovski, F. ; Pellegrini, P. ; Rau, M. M. ; Sadeh, I. ; Seitz, S. ; Sevilla-Noarbe, I. ; Sypniewski, A. ; de Vicente, J. ; Abbot, T. ; Allam, S. S. ; Atlee, D. ; Bernstein, G. ; Bernstein, J. P. ; Buckley-Geer, E. ; Burke, D. ; Childress, M. J. ; Davis, T. ; DePoy, D. L. ; Dey, A. ; Desai, S. ; Diehl, H. T. ; Doel, P. ; Estrada, J. ; Evrard, A. ; Fernandez, E. ; Finley, D. ; Flaugher, B. ; Frieman, J. ; Gaztanaga, E. ; Glazebrook, K. ; Honscheid, K. ; Kim, A. ; Kuehn, K. ; Kuropatkin, N. ; Lidman, C. ; Makler, M. ; Marshall, J. L. ; Nichol, R. C. ; Roodman, A. ; Sanchez, E. ; Santiago, B. X. ; Sako, M. ; Scalzo, R. ; Smith, R. C. ; Swanson, M. E. C. ; Tarle, G. ; Thomas, D. ; Tucker, D. L. ; Uddin, S. A. ; Valdes, F. ; Walker, A. ; Yuan, F. ; Zuntz, J. ; SLAC National Accelerator Lab., Menlo Park, CA (United States) ; Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States) ; Argonne National Lab. (ANL), Argonne, IL (United States) ; Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><description>In this study, we present results from a study of the photometric redshift performance of the Dark Energy Survey (DES), using the early data from a Science Verification period of observations in late 2012 and early 2013 that provided science-quality images for almost 200 sq. deg. at the nominal depth of the survey. We assess the photometric redshift (photo-z) performance using about 15 000 galaxies with spectroscopic redshifts available from other surveys. These galaxies are used, in different configurations, as a calibration sample, and photo-z's are obtained and studied using most of the existing photo-z codes. A weighting method in a multidimensional colour–magnitude space is applied to the spectroscopic sample in order to evaluate the photo-z performance with sets that mimic the full DES photometric sample, which is on average significantly deeper than the calibration sample due to the limited depth of spectroscopic surveys. In addition, empirical photo-z methods using, for instance, artificial neural networks or random forests, yield the best performance in the tests, achieving core photo-z resolutions σ68 ~ 0.08. 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(LBNL), Berkeley, CA (United States)</creatorcontrib><title>Photometric redshift analysis in the Dark Energy Survey Science Verification data</title><title>Monthly notices of the Royal Astronomical Society</title><description>In this study, we present results from a study of the photometric redshift performance of the Dark Energy Survey (DES), using the early data from a Science Verification period of observations in late 2012 and early 2013 that provided science-quality images for almost 200 sq. deg. at the nominal depth of the survey. We assess the photometric redshift (photo-z) performance using about 15 000 galaxies with spectroscopic redshifts available from other surveys. These galaxies are used, in different configurations, as a calibration sample, and photo-z's are obtained and studied using most of the existing photo-z codes. A weighting method in a multidimensional colour–magnitude space is applied to the spectroscopic sample in order to evaluate the photo-z performance with sets that mimic the full DES photometric sample, which is on average significantly deeper than the calibration sample due to the limited depth of spectroscopic surveys. In addition, empirical photo-z methods using, for instance, artificial neural networks or random forests, yield the best performance in the tests, achieving core photo-z resolutions σ68 ~ 0.08. Moreover, the results from most of the codes, including template-fitting methods, comfortably meet the DES requirements on photo-z performance, therefore, providing an excellent precedent for future DES data sets.</description><subject>Astronomical data bases: surveys</subject><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>galaxies: distances and redshifts</subject><subject>galaxies: statistics</subject><subject>INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY</subject><subject>large-scale structure of Universe</subject><issn>0035-8711</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><recordid>eNqNyr0KwjAQAOAMCtafdzjcC4mpVmetOCqKawnp1ZzWBJJT6Nvr4AM4fcs3EJmUepmvS6VGYpzSXUpZ6MUqE6ejCxyeyJEsRGySo5bBeNP1iRKQB3YIOxMfUHmMtx7Or_jGL5bQW4QrRmrJGqbgoTFspmLYmi7h7OdEzPfVZXvIQ2KqkyVG62zwHi3XSpdFqTb6r_QB2JU-3g</recordid><startdate>20141009</startdate><enddate>20141009</enddate><creator>Sanchez, C.</creator><creator>Carrasco Kind, M.</creator><creator>Lin, H.</creator><creator>Miquel, R.</creator><creator>Abdalla, F. 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T.</creatorcontrib><creatorcontrib>Doel, P.</creatorcontrib><creatorcontrib>Estrada, J.</creatorcontrib><creatorcontrib>Evrard, A.</creatorcontrib><creatorcontrib>Fernandez, E.</creatorcontrib><creatorcontrib>Finley, D.</creatorcontrib><creatorcontrib>Flaugher, B.</creatorcontrib><creatorcontrib>Frieman, J.</creatorcontrib><creatorcontrib>Gaztanaga, E.</creatorcontrib><creatorcontrib>Glazebrook, K.</creatorcontrib><creatorcontrib>Honscheid, K.</creatorcontrib><creatorcontrib>Kim, A.</creatorcontrib><creatorcontrib>Kuehn, K.</creatorcontrib><creatorcontrib>Kuropatkin, N.</creatorcontrib><creatorcontrib>Lidman, C.</creatorcontrib><creatorcontrib>Makler, M.</creatorcontrib><creatorcontrib>Marshall, J. L.</creatorcontrib><creatorcontrib>Nichol, R. C.</creatorcontrib><creatorcontrib>Roodman, A.</creatorcontrib><creatorcontrib>Sanchez, E.</creatorcontrib><creatorcontrib>Santiago, B. X.</creatorcontrib><creatorcontrib>Sako, M.</creatorcontrib><creatorcontrib>Scalzo, R.</creatorcontrib><creatorcontrib>Smith, R. C.</creatorcontrib><creatorcontrib>Swanson, M. E. C.</creatorcontrib><creatorcontrib>Tarle, G.</creatorcontrib><creatorcontrib>Thomas, D.</creatorcontrib><creatorcontrib>Tucker, D. L.</creatorcontrib><creatorcontrib>Uddin, S. A.</creatorcontrib><creatorcontrib>Valdes, F.</creatorcontrib><creatorcontrib>Walker, A.</creatorcontrib><creatorcontrib>Yuan, F.</creatorcontrib><creatorcontrib>Zuntz, J.</creatorcontrib><creatorcontrib>SLAC National Accelerator Lab., Menlo Park, CA (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Argonne National Lab. (ANL), Argonne, IL (United States)</creatorcontrib><creatorcontrib>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Sanchez, C.</au><au>Carrasco Kind, M.</au><au>Lin, H.</au><au>Miquel, R.</au><au>Abdalla, F. B.</au><au>Amara, A.</au><au>Banerji, M.</au><au>Bonnett, C.</au><au>Brunner, R.</au><au>Capozzi, D.</au><au>Carnero, A.</au><au>Castander, F. J.</au><au>da Costa, L. A. N.</au><au>Cunha, C.</au><au>Fausti, A.</au><au>Gerdes, D.</au><au>Greisel, N.</au><au>Gschwend, J.</au><au>Hartley, W.</au><au>Jouvel, S.</au><au>Lahav, O.</au><au>Lima, M.</au><au>Maia, M. A. G.</au><au>Marti, P.</au><au>Ogando, R. L. C.</au><au>Ostrovski, F.</au><au>Pellegrini, P.</au><au>Rau, M. M.</au><au>Sadeh, I.</au><au>Seitz, S.</au><au>Sevilla-Noarbe, I.</au><au>Sypniewski, A.</au><au>de Vicente, J.</au><au>Abbot, T.</au><au>Allam, S. S.</au><au>Atlee, D.</au><au>Bernstein, G.</au><au>Bernstein, J. P.</au><au>Buckley-Geer, E.</au><au>Burke, D.</au><au>Childress, M. J.</au><au>Davis, T.</au><au>DePoy, D. L.</au><au>Dey, A.</au><au>Desai, S.</au><au>Diehl, H. T.</au><au>Doel, P.</au><au>Estrada, J.</au><au>Evrard, A.</au><au>Fernandez, E.</au><au>Finley, D.</au><au>Flaugher, B.</au><au>Frieman, J.</au><au>Gaztanaga, E.</au><au>Glazebrook, K.</au><au>Honscheid, K.</au><au>Kim, A.</au><au>Kuehn, K.</au><au>Kuropatkin, N.</au><au>Lidman, C.</au><au>Makler, M.</au><au>Marshall, J. L.</au><au>Nichol, R. C.</au><au>Roodman, A.</au><au>Sanchez, E.</au><au>Santiago, B. X.</au><au>Sako, M.</au><au>Scalzo, R.</au><au>Smith, R. C.</au><au>Swanson, M. E. C.</au><au>Tarle, G.</au><au>Thomas, D.</au><au>Tucker, D. L.</au><au>Uddin, S. A.</au><au>Valdes, F.</au><au>Walker, A.</au><au>Yuan, F.</au><au>Zuntz, J.</au><aucorp>SLAC National Accelerator Lab., Menlo Park, CA (United States)</aucorp><aucorp>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</aucorp><aucorp>Argonne National Lab. (ANL), Argonne, IL (United States)</aucorp><aucorp>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Photometric redshift analysis in the Dark Energy Survey Science Verification data</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2014-10-09</date><risdate>2014</risdate><volume>445</volume><issue>2</issue><issn>0035-8711</issn><abstract>In this study, we present results from a study of the photometric redshift performance of the Dark Energy Survey (DES), using the early data from a Science Verification period of observations in late 2012 and early 2013 that provided science-quality images for almost 200 sq. deg. at the nominal depth of the survey. We assess the photometric redshift (photo-z) performance using about 15 000 galaxies with spectroscopic redshifts available from other surveys. These galaxies are used, in different configurations, as a calibration sample, and photo-z's are obtained and studied using most of the existing photo-z codes. A weighting method in a multidimensional colour–magnitude space is applied to the spectroscopic sample in order to evaluate the photo-z performance with sets that mimic the full DES photometric sample, which is on average significantly deeper than the calibration sample due to the limited depth of spectroscopic surveys. In addition, empirical photo-z methods using, for instance, artificial neural networks or random forests, yield the best performance in the tests, achieving core photo-z resolutions σ68 ~ 0.08. Moreover, the results from most of the codes, including template-fitting methods, comfortably meet the DES requirements on photo-z performance, therefore, providing an excellent precedent for future DES data sets.</abstract><cop>United States</cop><pub>Royal Astronomical Society</pub><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0035-8711 |
| ispartof | Monthly notices of the Royal Astronomical Society, 2014-10, Vol.445 (2) |
| issn | 0035-8711 |
| language | eng |
| recordid | cdi_osti_scitechconnect_1374719 |
| source | Oxford Journals Open Access Collection |
| subjects | Astronomical data bases: surveys ASTRONOMY AND ASTROPHYSICS galaxies: distances and redshifts galaxies: statistics INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY large-scale structure of Universe |
| title | Photometric redshift analysis in the Dark Energy Survey Science Verification data |
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