We describe the first public data release of the Dark Energy Survey, DES DR1, consisting of reduced single-epoch images, co-added images, co-added source catalogs, and associated products and services assembled over the first 3 yr of DES science operations. DES DR1 is based on optical/near-infrared imaging from 345 distinct nights (2013 August to 2016 February) by the Dark Energy Camera mounted on the 4 m Blanco telescope at the Cerro Tololo Inter-American Observatory in Chile. We release data from the DES wide-area survey covering ∼5000 deg2 of the southern Galactic cap in five broad photometric bands, grizY. DES DR1 has a median delivered point-spread function of g=1.12, r = 0.96, i = 0.88, z = 0.84, and Y = 0.″90 FWHM, a photometric precision of <1% in all bands, and an astrometric precision of 151 {mas}. The median co-added catalog depth for a 1.″95 diameter aperture at signal-to-noise ratio (S/N) = 10 is g = 24.33, r = 24.08, i = 23.44, z = 22.69, and Y = 21.44 {mag} . DES DR1 includes nearly 400 million distinct astronomical objects detected in ∼10,000 co-add tiles of size 0.534 deg2 produced from ∼39,000 individual exposures. Benchmark galaxy and stellar samples contain ∼310 million and ∼80 million objects, respectively, following a basic object quality selection. These data are accessible through a range of interfaces, including query web clients, image cutout servers, jupyter notebooks, and an interactive co-add image visualization tool. DES DR1 constitutes the largest photometric data set to date at the achieved depth and photometric precision.

The Dark Energy Survey: Data Release 1 / Abbott, T. M. C.; Abdalla, F. B.; Allam, S.; Amara, A.; Annis, J.; Asorey, J.; Avila, S.; Ballester, O.; Banerji, M.; Barkhouse, W.; Baruah, L.; Baumer, M.; Bechtol, K.; Becker, M. R.; Benoit-Lévy, A.; Bernstein, G. M.; Bertin, E.; Blazek, J.; Bocquet, S.; Brooks, ; D., Brout; Buckley-Geer, E.; Burke, D. L.; Busti, V.; Campisano, R.; Cardiel-Sas, L.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.; Castander, F. J.; Cawthon, R.; Chang, C.; Chen, X.; Conselice, C.; Costa, G.; Crocce, M.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.; Das, R.; Daues, G.; Davis, T. M.; Davis, C.; De Vicente, J.; Depoy, D. L.; Derose, J.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Dodelson, S.; Doel, P.; Drlica-Wagner, A.; Eifler, T. F.; Elliott, A. E.; Evrard, A. E.; Farahi, A.; Fausti Neto, A.; Fernandez, E.; Finley, D. A.; Flaugher, B.; Foley, R. J.; Fosalba, P.; Friedel, D. N.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; Gerdes, D. W.; Giannantonio, T.; Gill, M. S. S.; Glazebrook, K.; Goldstein, D. A.; Gower, M.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gupta, R. R.; Gutierrez, G.; Hamilton, S.; Hartley, W. G.; Hinton, S. R.; Hislop, J. M.; Hollowood, D.; Honscheid, K.; Hoyle, B.; Huterer, D.; Jain, B.; James, D. J.; Jeltema, T.; Johnson, M. W. G.; Johnson, M. D.; Kacprzak, T.; Kent, S.; Khullar, G.; Klein, M.; Kovacs, A.; Koziol, A. M. G.; Krause, E.; Kremin, A.; Kron, R.; Kuehn, K.; Kuhlmann, S.; Kuropatkin, N.; Lahav, O.; Lasker, J.; Li, T. S.; Li, R. T.; Liddle, A. R.; Lima, M.; Lin, H.; López-Reyes, P.; Maccrann, N.; Maia, M. A. G.; Maloney, J. D.; Manera, M.; March, M.; Marriner, J.; Marshall, J. L.; Martini, P.; Mcclintock, T.; Mckay, T.; Mcmahon, R. G.; Melchior, P.; Menanteau, F.; Miller, C. J.; Miquel, R.; Mohr, J. J.; Morganson, E.; Mould, J.; Neilsen, E.; Nichol, R. C.; Nogueira, F.; Nord, B.; Nugent, P.; Nunes, L.; Ogando, R. L. C.; Old, L.; Pace, A. B.; Palmese, A.; Paz-Chinchón, F.; Peiris, H. V.; Percival, W. J.; Petravick, D.; Plazas, A. A.; Poh, J.; Pond, C.; Porredon, A.; Pujol, A.; Refregier, A.; Reil, K.; Ricker, P. M.; Rollins, R. P.; Romer, A. K.; Roodman, A.; Rooney, P.; Ross, A. J.; Rykoff, E. S.; Sako, M.; Sanchez, M. L.; Sanchez, E.; Santiago, B.; Saro, A.; Scarpine, V.; Scolnic, D.; Serrano, S.; Sevilla-Noarbe, I.; Sheldon, E.; Shipp, N.; Silveira, M. L.; Smith, M.; Smith, R. C.; Smith, J. A.; Soares-Santos, M.; Sobreira, F.; Song, J.; Stebbins, A.; Suchyta, E.; Sullivan, M.; Swanson, M. E. C.; Tarle, G.; Thaler, J.; Thomas, D.; Thomas, R. C.; Troxel, M. A.; Tucker, D. L.; Vikram, V.; Vivas, A. K.; Walker, A. R.; Wechsler, R. H.; Weller, J.; Wester, W.; Wolf, R. C.; Wu, H.; Yanny, B.; Zenteno, A.; Zhang, Y.; Zuntz, J.; Des, Collaboration; Juneau, S.; Fitzpatrick, M.; Nikutta, R.; Nidever, D.; Olsen, K.; Scott, A.; NOAO Data, Lab. - In: ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES. - ISSN 0067-0049. - 239:2(2018), pp. 1-25. [10.3847/1538-4365/aae9f0]

The Dark Energy Survey: Data Release 1

Saro, A.;
2018-01-01

Abstract

We describe the first public data release of the Dark Energy Survey, DES DR1, consisting of reduced single-epoch images, co-added images, co-added source catalogs, and associated products and services assembled over the first 3 yr of DES science operations. DES DR1 is based on optical/near-infrared imaging from 345 distinct nights (2013 August to 2016 February) by the Dark Energy Camera mounted on the 4 m Blanco telescope at the Cerro Tololo Inter-American Observatory in Chile. We release data from the DES wide-area survey covering ∼5000 deg2 of the southern Galactic cap in five broad photometric bands, grizY. DES DR1 has a median delivered point-spread function of g=1.12, r = 0.96, i = 0.88, z = 0.84, and Y = 0.″90 FWHM, a photometric precision of <1% in all bands, and an astrometric precision of 151 {mas}. The median co-added catalog depth for a 1.″95 diameter aperture at signal-to-noise ratio (S/N) = 10 is g = 24.33, r = 24.08, i = 23.44, z = 22.69, and Y = 21.44 {mag} . DES DR1 includes nearly 400 million distinct astronomical objects detected in ∼10,000 co-add tiles of size 0.534 deg2 produced from ∼39,000 individual exposures. Benchmark galaxy and stellar samples contain ∼310 million and ∼80 million objects, respectively, following a basic object quality selection. These data are accessible through a range of interfaces, including query web clients, image cutout servers, jupyter notebooks, and an interactive co-add image visualization tool. DES DR1 constitutes the largest photometric data set to date at the achieved depth and photometric precision.
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