期刊
ASTROPHYSICAL JOURNAL
卷 771, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.1088/0004-637X/771/2/97
关键词
supernovae: general; supernovae: individual (PS1-10bzj)
资金
- National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]
- FAS Science Division Research Computing Group at Harvard University
- European Research Council under the European Union's Seventh Framework Programme/ERC [291222]
- National Science Foundation [AST-1009749, AST-1211196]
- [GS-2010B-Q-4]
- [GS-2011A-Q-29]
- [GS-2011B-Q-44]
- STFC [ST/I001123/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/I001123/1] Funding Source: researchfish
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0907903] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1238877, 1211196, 1009749] Funding Source: National Science Foundation
We present observations and analysis of PS1-10bzj, a superluminous supernova (SLSN) discovered in the Pan-STARRS Medium Deep Survey at a redshift z = 0.650. Spectroscopically, PS1-10bzj is similar to the hydrogenpoor SLSNe 2005ap and SCP 06F6, though with a steeper rise and lower peak luminosity (M-bol similar or equal to -21.4 mag) than previous events. We construct a bolometric light curve, and show that while PS1-10bzj's energetics were less extreme than previous events, its luminosity still cannot be explained by radioactive nickel decay alone. We explore both a magnetar spin-down and circumstellar interaction scenario and find that either can fit the data. PS1-10bzj is located in the Extended Chandra Deep Field South and the host galaxy is imaged in a number of surveys, including with the Hubble Space Telescope. The host is a compact dwarf galaxy (MB approximate to -18 mag, diameter less than or similar to 800 pc), with a low stellar mass (M-* approximate to 2.4 x 10(7) M-circle dot), young stellar population (tau(*) approximate to 5 Myr), and a star formation rate of similar to 2-3 M-circle dot yr(-1). The specific star formation rate is the highest seen in an SLSN host so far (similar to 100 Gyr(-1)). We detect the [OIII] lambda 4363 line, and find a low metallicity: 12 + (O/H) = 7.8 +/- 0.2 (similar or equal to 0.1 Z(circle dot)). Together, this indicates that at least some of the progenitors of SLSNe come from young, low-metallicity populations.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据