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Discovery of 4 possible supernovae during the "Deeper, Wider, Faster" program observations

ATel #10072; I. Andreoni (Swinburne Univ. [SUT], CAASTRO, AAO), J. Cooke (SUT, CAASTRO, OzGrav), T. A. Pritchard (SUT), R. Spiewak (SUT), K. Plant (SUT, CAASTRO), U. Mestric (SUT), S. Ryder (AAO), T. Abbott (NOAO), Rebecca Allen (SUT), G. Anderson (ICRAR-Curtin), A. Asher (SUT), M. C. Baglio (INAF/OAB), K. Bannister (CSIRO, CAASTRO), M. Bell (CSIRO, CAASTRO), S. Bernard (Univ. of Melbourne, CAASTRO), S. Bhandari (SUT, CAASTRO), M. Caleb (ANU, SUT, CAASTRO), S. Campana (INAF/OAB), D. Coward (Univ. of Western Australia), C. Curtin (SUT, CAASTRO), P. D'Avanzo (INAF/OAB), J. F. Devlin (SUT), W. Farah (SUT), C. Fluke (SUT), C. Flynn (SUT, CAASTRO), G. Foran (SUT), D. Fugazza (INAF/OAB), B. Gawin (SUT), S. Hegarty (SUT), R. Hodgson (SUT), S. Hodgson (SUT), J. Horst (San Diego State Univ.), E. Howell (Univ. of Western Australia), I. Hussaini (Univ. of Melbourne), C. Jacobs (SUT), M. Ko (SUT), M. Kotze (SAAO, SALT), A. Lien (NASA/Goddard), B. Meade (Univ. of Melbourne), A. Melandri (INAF/OAB), B. Miszalski (SAAO, SALT), A. Moller (ANU, CAASTRO), M. T. Murphy (SUT), T. Nanayakkara (SUT), M. O'Neill (SUT), S. Oslowski (SUT), B. Peng (Univ. of Sci. & Tech. of China), E. Petroff (ASTRON), A. Rest (STScI), F. Robert (SUT), M. Shara (AMNH), B. Tucker (ANU, CAASTRO), F. Valdes (NOAO) and D. Vohl (SUT)
on 13 Feb 2017; 06:15 UT
Credential Certification: Igor Andreoni (igor.andreoni@gmail.com)

Subjects: Optical, Supernovae, Transient

Referred to by ATel #: 10078

We report the discovery of four possible supernovae using the Dark Energy Camera (DECam) at CTIO during our 2-7 February 2017 (UT) “Deeper, Wider, Faster” (DWF) program observations.

      Name       | RA (J2000) | DEC (J2000) | Discovery date | Discovery mag* |    Latest date    | Latest mag*
-----------------|----------------|-----------------|-------------------|---------------------|--------------------|----------------
dwf17a1067   | 5:48:11.647 | -61:42:19.28 | 2017-02-03.32 |           21.2          | 2017-02-07.29 |     21.5
dwf17a104     | 5:56:54.080 | -60:25:42.24 | 2017-02-02.38 |           21.8          | 2017-02-06.28 |     21.7
dwf17a1147   | 6:42:34.352 | -51:18:06.49 | 2017-02-03.44 |           20.6          | 2017-02-07.41 |     20.8
dwf17a852     | 6:46:16.326 | -51:57:09.11 | 2017-02-02.35 |           20.2          | 2017-02-07.41 |     20.7

*All the magnitude values are measured in DECam g filter, with difference image photometry; we compute the zero point by comparing measured magnitudes of stellar sources against the USNO-B1 catalog. Errors are typically ~0.1 mag.

DWF coordinates simultaneous, fast-cadenced observations and real time analysis involving more than 10 multi-messenger facilities (from radio to high energy telescopes to neutrino and gravitational wave detectors) with the goal of detecting and understanding the fastest bursts in the sky.

DECam optical images are compressed immediately after acquisition using our data compression algorithm, based on the JPEG2000 standard. They are then sent to the Green II supercomputer at the Swinburne University of Technology for real-time (in minutes) data processing and assessment of the candidates. The calibration is performed with a custom version of PhotPipe (Rest et al. 2015), the real-time transient candidate identification is performed using the “Mary” pipeline, and candidates are visually inspected in real time by the DWF team using sophisticated visualisation tools and techniques. The papers describing the DWF concept (Cooke et al.), the data compression algorithm (Vohl et al.), the real time analysis pipeline (Andreoni et al.), and the visualisation techniques (Meade et al.) are currently submitted or in preparation.