Welcome to the new version of CaltechAUTHORS. Login is currently restricted to library staff. If you notice any issues, please email coda@library.caltech.edu
Published September 20, 2013 | Submitted + Published
Journal Article Open

Discovery, Progenitor and Early Evolution of a Stripped Envelope Supernova iPTF13bvn


The intermediate Palomar Transient Factory reports our discovery of a young supernova, iPTF13bvn, in the nearby galaxy, NGC 5806 (22.5 Mpc). Our spectral sequence in the optical and infrared suggests a Type Ib classification. We identify a blue progenitor candidate in deep pre-explosion imaging within a 2σ error circle of 80 mas (8.7 pc). The candidate has an M_B luminosity of −5.52 ± 0.39 mag and a B − I color of 0.25 ± 0.25 mag. If confirmed by future observations, this would be the first direct detection for a progenitor of a Type Ib. Fitting a power law to the early light curve, we find an extrapolated explosion date around 0.6 days before our first detection. We see no evidence of shock cooling. The pre-explosion detection limits constrain the radius of the progenitor to be smaller than a few solar radii. iPTF13bvn is also detected in centimeter and millimeter wavelengths. Fitting a synchrotron self-absorption model to our radio data, we find a mass-loading parameter of 1.3×10^(12) g cm^(−1). Assuming a wind velocity of 10^3 km s^(−1), we derive a progenitor mass-loss rate of 3 × 10^(−5) M☉ yr^(−1). Our observations, taken as a whole, are consistent with a Wolf–Rayet progenitor of the supernova iPTF13bvn.

Additional Information

© 2013 The American Astronomical Society. Received 4 July 2013, accepted for publication 15 August 2013. Published 30 August 2013. We thank A. L. Piro for valuable discussions. We thank the following people for co-operating with our target of opportunity or queue observations: M. Roth (Magellan), A. Hartuynan (TNG), J. Johnson (Keck), and J. Caldwell (HET). We thank A. Howard and H. Isaacson for HIRES data reduction. We thank R. Campbell, Hien Tran, and S. Tendulkar for helping with OSIRIS LGS-AO observation and data reduction. We thank P. Vreeswijk for assisting with HST image registration. We thank J. Vinko, R. Foley, B. Kirshner, D. Perley, A. Corsi, and K. Mooley as proposal co-Is. We thank J. Swift, B. Montet, M. Bryan, R. Jensen-Clem, D. Polishook, and S. Tinyanont for assisting with observations. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. N.D. acknowledges the Hubble Fellowship. Research by A.G.Y. and his group was supported by grants from the ISF, BSF, GIF, Minerva, the EU/FP7 via an ERC grant and the Kimmel award. The research of J.C.W. is supported by NSF Grant AST 11-09801. The National Energy Research Scientific Computing Center, supported by the Office of Science of the U.S. Department of Energy, provided staff, computational resources, and data storage for this project. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has been supported by the Australian Research Council through Super Science Fellowship grant FS100100033. The Centre for All-sky Astrophysics is an Australian Research Council Centre of Excellence, funded by grant CE110001020. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities.

Attached Files

Published - 2041-8205_775_1_L7.pdf

Submitted - 1307.1470v2.pdf


Files (1.9 MB)
Name Size Download all
1.2 MB Preview Download
757.6 kB Preview Download

Additional details

August 19, 2023
October 25, 2023