SN 2008in-BRIDGING THE GAP BETWEEN NORMAL AND FAINT SUPERNOVAE OF TYPE IIP
- Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital 263 129 (India)
- Istituto Nazionale di Astrofisica, Observatorio Astronomico di Padova (Italy)
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN (United Kingdom)
- Randall Laboratory of Physics, University of Michigan, 450 Church Street, Ann Arbor, MI 48109-1040 (United States)
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 (United States)
- NASA/Goddard Space Flight Center, Astrophysics Science Division, Code 662, Greenbelt, MD 20771 (United States)
- Special Astrophysical Observatory, Nizhnij Arkhyz, Karachaevo-Cherkesia 369167 (Russian Federation)
- Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen (Denmark)
- Department of Astronomy, University of Texas, Austin, TX 787120259 (United States)
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125 (United States)
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)
- Institut de Ciencies de L'Espai (IEEC-CSIC), Campus UAB, 08193 Bellaterra (Spain)
- Space Science and Engineering Division, 6220 Culebra Rd, San Antonio, TX 78238-5166 (United States)
We present optical photometric and low-resolution spectroscopic observations of the Type II plateau supernova (SN) 2008in, which occurred in the outskirts of the nearly face-on spiral galaxy M61. Photometric data in the X-ray, ultraviolet, and near-infrared bands have been used to characterize this event. The SN field was imaged with the ROTSE-IIIb optical telescope about seven days before the explosion. This allowed us to constrain the epoch of the shock breakout to JD = 2454825.6. The duration of the plateau phase, as derived from the photometric monitoring, was {approx}98 days. The spectra of SN 2008in show a striking resemblance to those of the archetypal low-luminosity IIP SNe 1997D and 1999br. A comparison of ejecta kinematics of SN 2008in with the hydrodynamical simulations of Type IIP SNe by Dessart et al. indicates that it is a less energetic event ({approx}5 x 10{sup 50} erg). However, the light curve indicates that the production of radioactive {sup 56}Ni is significantly higher than that in the low-luminosity SNe. Adopting an interstellar absorption along the SN direction of A{sub V} {approx} 0.3 mag and a distance of 13.2 Mpc, we estimated a synthesized {sup 56}Ni mass of {approx}0.015 M{sub sun}. Employing semi-analytical formulae derived by Litvinova and Nadezhin, we derived a pre-SN radius of {approx}126 R{sub sun}, an explosion energy of {approx}5.4 x 10{sup 50} erg, and a total ejected mass of {approx}16.7 M{sub sun}. The latter indicates that the zero-age main-sequence mass of the progenitor did not exceed 20 M{sub sun}. Considering the above properties of SN 2008in and its occurrence in a region of sub-solar metallicity ([O/H] {approx} 8.44 dex), it is unlikely that fall-back of the ejecta onto a newly formed black hole occurred in SN 2008in. We therefore favor a low-energy explosion scenario of a relatively compact, moderate-mass progenitor star that generates a neutron star.
- OSTI ID:
- 21578286
- Journal Information:
- Astrophysical Journal, Vol. 736, Issue 2; Other Information: DOI: 10.1088/0004-637X/736/2/76; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
Similar Records
SN 2009js AT THE CROSSROADS BETWEEN NORMAL AND SUBLUMINOUS TYPE IIP SUPERNOVAE: OPTICAL AND MID-INFRARED EVOLUTION
SUPERNOVA 2003ie WAS LIKELY A FAINT TYPE IIP EVENT