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First SN Discoveries from the Dark Energy Survey

ATel #4668; T. Abbott (1), F. Abdalla (2), I. Achitouv (3), E. Ahn (4), G. Aldering (6), S. Allam (4), D. Alonso (5), A. Amara (8), J. Annis (4), M. Antonik (2), A. Aragon-Salamanca (9), R. Armstrong (10), C. Ashall (2), J. Asorey (11), D. Bacon (12), E. Balbinot (13, 14), M. Banerji (15), K. Barbary (16), W. Barkhouse (17), L. Baruah (18), A. Bauer (11), K. Bechtol (19), M. Becker (19), R. Bender (3), C. Benoist (20, 14), A. Benoit-Levy (2), M. Bernardi (10), G. Bernstein (10), J. P. Bernstein (16), R. Bernstein (21), E. Bertin (22), E. Beynon (12), S. Bhattacharya (16), T. Biesiadzinski (23), R. Biswas (16), C. Blake (24), J. S. Bloom (6), S. Bocquet (3), C. Brandt (25, 14), S. Bridle (2), D. Brooks (2), P. J. Brown (32), R. Brunner (26), E. Buckley-Geer (4), D. Burke (27), A. Burkert (3), M. Busha (28), J. Campa (7), H. Campbell (12), R. Cane (10), D. Capozzi (12), J. Carlstrom (19), A. Carnero Rosell (29, 14), M. Carollo (8), M. Carrasco-Kind (26), J. Carretero (11), M. 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Walker (35), R. Wechsler (27), D. Weinberg (35), J. Weller (3), W. Wester (4), M. Wetzstein (3), M. White (6), H. Wilcox (12), D. Wilman (3), B. Yanny (4), J. Young (35), A. Zablocki (19), A. Zenteno (3), Y. Zhang (23), J. Zuntz (2); (1) NOAO/CTIO, (2) University College London, (3) Ludwig Maximilians University, Munich, (4) Fermilab, (5) Universidad Autonoma de Madrid, (6) Lawrence Berkeley National Laboratory, (7) CIEMAT, (8) ETH-Zurich, (9) University of Nottingham, (10) University of Pennsylvania, (11) Institut de Ciencies de l'Espai (IEEC/CSIC), (12) University of Portsmouth, (13) UFRGS, (14) LIneA, (15) University of Cambridge, (16) Argonne National Laboratory, (17) University of North Dakota, (18) University of Sussex, (19) University of Chicago, (20) Observatoire de la Cote d'Azur, (21) UC Santa Cruz, (22) Institut Astrophysique de Paris, (23) University of Michigan, (24) Swinburne University of Technology, (25) CBPF, (26) University of Illinois / NCSA, (27) Kavli Institute for Particle Astrophysics & Cosmology, SLAC National Accelerator Laboratory, Stanford University, (28) University of Zurich, (29) Observatorio Nacional, (30) Australian Astronomical Observatory, (31) University of Queensland, (32) Texas A&M University, (33) IFAE, (34) Boston Consulting Group, (35) Ohio State University, (36) University of Oxford, (37) University of Texas at Dallas, (38) University of the Western Cape, (39) Taiwan Central University, (40) University of Edinburgh, (41) Brookhaven National Laboratory, (42) Australian National University, (43) University of Southampton, (44) Queen Mary London, (45) Harvard-Smithsonian CfA
on 22 Dec 2012; 14:34 UT
Distributed as an Instant Email Notice Supernovae
Credential Certification: Masao Sako (masao@sas.upenn.edu)

Subjects: Optical, Supernovae

First SN Discoveries from the Dark Energy Survey The Dark Energy Survey (DES) report the discovery of the first set of supernovae (SN) from the project. Images were observed as part of the DES Science Verification phase using the newly-installed 570-Megapixel Dark Energy Camera on the CTIO Blanco 4-m telescope by observers J. Annis, E. Buckley-Geer, and H. Lin. SN observations are planned throughout the observing campaign on a regular cadence of 4-6 days in each of the ten 3-deg2 fields in the DES griz filters. The SN candidates are named according to the season and field in which they were discovered. We adopt the convention -- DES{season}{field}{index} -- where {season} is the year pertaining to the beginning of each observing season, {field} denotes one of the ten SN search fields (E1,E2,S1,S2,X1,X2,X3,C1,C2,C3) in Elais-S1 (E), Stripe 82 (S), XMM-LSS (X) and CDF-S (C), and {index} is one or more lower-case letters starting from a-z, then aa-az, and so on. The DES SN Survey strategy is described in Bernstein et al. (2012, ApJ, 753, 152).

Spectroscopic classifications were performed by the OzDES collaboration from spectra (350-900 nm) obtained at the Anglo-Australian Telescope with AAOmega-2dF observed by C. Lidman, R. Sharp, and S. A. Uddin. Classifications were performed using Superfit (Howell et al 2002, BAAS, 34, 1256) or SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Redshifts measured from narrow galaxy lines are quoted to 3 significant figures. Those measured from broad SN features are quoted to 2 significant figures. SN phases are based on both the optical spectra and multi-band light curves at the time of the spectroscopic measurements.

 
Name     | RA(J2000)  |  Dec(J2000) |  Discovery  | Discovery | Spectrum    | redshift | type | phase 
         |            |             |  date (UT)  | r mag     | date (UT)   |          |      | 
DES12C1a | 03:38:54.5 | -27:32:28.2 | 2012 Dec 07 | 22.0      | 2012 Dec 13 | 0.303    | Ia   | near max 
DES12C1b | 03:35:05.8 | -26:45:53.9 | 2012 Dec 07 | 20.9      | 2012 Dec 13 | 0.243    | Ia   | near max 
DES12C2a | 03:41:13.1 | -28:59:37.9 | 2012 Dec 04 | 21.5      | 2012 Dec 14 | 0.21     | Ia   | near max