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Discovery and multiwavelength follow-up of PTF10qts, a broad-line type Ic supernova.

ATEL # 2817; A. Gal-Yam, I. Arcavi, D. Xu, S. Ben-Ami (Weizmann Institute of Science), R. M. Quimby, E. O. Ofek, M. M. Kasliwal, A. Corsi, S. R. Kulkarni (Caltech), M. Sullivan (Oxford), D. Frail (NRAO), E. Walker, P. Mazzali (INAF/SNS Pisa), P. Nugent (LBNL), J. S. Bloom (UC Berkeley), N. M. Law (U. Toronto), R. G. Dekany, G. Rahmer, David Hale, R. Smith, J. Zolkower, V. Velur, R. Walters, J. Henning, K. Bui, D. McKenna (Caltech), and J. Jacobsen (LBNL) on behalf of the Core-Collapse working group of the Palomar Transient Factory (ATEL#1964)
on 25 Aug 2010; 10:09 UT
Distributed as an Instant Email Notice (Supernova)
Password Certification: Avishay Gal-Yam (

Subjects: Radio, Optical, X-ray, Nova, Supernova

The PTF (ATEL #1964; reports the discovery of a new supernova, PTF10qts. The supernova was discovered and classified by Oarical, an autonomous software framework of the PTF collaboration, on Aug 8 UT at RA(J2000) = 16:41:37.60 and DEC(J2000) = +28:58:21.1 at a magnitude of 19.4 in R-band (calibrated with respect to the USNO-B catalog) in an anonymous host galaxy. The supernova was not detected down to mag 21.0 in previous PTF images taken during 2009 and 2010 (3-sigma). A spectrum was obtained using the Double-Beam Spectrograph (DBSP; Oke \& Gunn 1982, PASP, 94, 586) on the Palomar 5-m Hale telescope on August 13 UT, revealing the supernova to be a broad-line type Ic, similar to SN 1998bw, at z=0.0907. A low-resolution optical spectrum was obtained using DOLORES on the TNG on August 17; preliminary analysis confirms the nature of the target as SN Ic-BL with some spectral evolution seen in the bluer features. ToO EVLA follow-up observations at 8.46 GHz obtained as part of the program "Exploring Transients in the Local Universe" (PI Kasliwal) on August 18.03 yield an upper limit of 86 uJy at the SN location (3 sigma). We requested Swift observations, which began on August 18. The XRT data yield an upper limit of 0.004 counts/sec. We measure the following preliminary UVOT (Vega) magnitudes for the transient plus its host: (U UVW1 UVM2 UVW2) = (19.53 20.14 21.15 20.60) +/- (0.16 0.22 0.41 0.20). Additional observations are underway. We thank the Swift team for scheduling the ToO observations.

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R. E. Rutledge , Editor
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