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ATEL # 2397; R. Chornock, R. J. Foley, E. Berger, A. Rest, G. Narayan (Harvard/CfA), M. Huber (JHU), J. Tonry, P. A. Price (IfA/Hawaii), C. Stubbs (Harvard), A. Riess (JHU), W. M. Wood-Vasey (Pitt), S. J. Smartt (Queen's Univ. Belfast), R. P. Kirshner, D. J. Sand, A. M. Soderberg (Harvard/CfA), and the PS1 Builders.
on 23 Jan 2010; 11:30 UT
Password Certification: Ryan Chornock (email@example.com)
Subjects: Optical, Nova, Supernova, Transients
Referred to by ATEL #: 2398
Further to ATels #2214, #2229, and #2249, we report the discovery of supernovae in Pan-STARRS1 Medium Deep Survey imaging data obtained from 2010 Jan. 10 - Jan. 20 by the 1.8-m PS1 survey telescope on Haleakala, Hawaii. Images were processed through the Harvard/JHU transient pipeline and 86 good supernova candidates were identified. Sixteen of these candidates were selected for spectroscopic followup and have been confirmed using GMOS on the 8-m Gemini-North and Gemini-South telescopes (PI: Berger) and MagE on the 6.5-m Magellan Clay telescope (PI: Foley). The first eight are listed below.
|Pan-STARRS Designation||RA(J2000)||Dec(J2000)||Discovery Date (UT)||Peak Magnitude||Type||Redshift||Age||Spectrum Date (UT)||Telescope|
|PS1-1000009||02:20:22.959||-04:40:21.04||Jan. 10||r=19.8||SN Ia||0.15||+10 days||Jan. 21||Magellan|
|PS1-1000007||02:23:30.712||-04:38:10.75||Jan. 10||r=19.6||SN Ia||0.14||+2 weeks||Jan. 21||Magellan|
|PS1-1000008||02:24:15.946||-03:11:11.55||Jan. 10||r=20.8||SN Ia||0.25||+0 days||Jan. 20||Magellan|
|PS1-1000001||03:29:48.738||-29:04:30.11||Jan. 11||i=19.7||SN II||0.071||young||Jan. 16||Gemini-S|
|PS1-1000004||03:33:27.950||-28:22:17.57||Jan. 11||i=21.6||SN Ia||0.231||+3 weeks||Jan. 20||Magellan|
|PS1-1000002||08:37:02.601||+43:44:16.89||Jan. 11||r=22.5||SN IIP||0.260||near max||Jan. 18||Gemini-N|
|PS1-1000003||08:37:18.938||+44:20:01.44||Jan. 11||g=20.8||SN Ia||0.15||+0 days||Jan. 18||Gemini-N|
|PS1-1000005||09:58:59.759||+03:09:27.11||Jan. 12||r=21.1||SN Ia||0.25||+0 days||Jan. 21||Magellan|
Redshifts reported with three significant figures were obtained from host galaxy spectra, while those with two significant digits were determined by cross-correlation with a library of supernova templates using the SNID code (Blondin & Tonry 2007, ApJ, 666, 1024). Ages relative to maximum light were also determined with SNID and generally have an uncertainty of 4 days for SNe Ia.
These discoveries were enabled using the PS1 System operated by the PS1 Science Consortium (PS1SC) and its member institutions. The PS1 Surveys have been made possible through the combination of the Institute for Astronomy at the University of Hawaii, The Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestial Physics, Garching, The Johns Hopkins University, the University of Durham, the University of Edinburgh, the Queen's University of Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Network, and the National Central University of Taiwan.
We thank the staffs at the PS1, Gemini-North, Gemini-South, and Magellan Clay telescopes for their assistance in obtaining these observations.
Pan-STARRs Acknowledgment and Builders List