Galex and Pan-Starrs1 Discovery of SN IIP 2010 aq: The First Few Days After Shock Breakout in a Red Supergiant Star

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Galex and Pan-Starrs1 Discovery of SN IIP 2010 aq: The First Few Days After Shock Breakout in a Red Supergiant Star

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Title: Galex and Pan-Starrs1 Discovery of SN IIP 2010 aq: The First Few Days After Shock Breakout in a Red Supergiant Star
Author: Gezari, S.; Rest, A.; Huber, M. E.; Narayan, G.; Forster, K.; Neill, J. D.; Martin, D. C.; Valenti, S.; Smartt, S. J.; Chornock, R; Berger, Edo; Soderberg, Alicia M.; Mattila, S.; Kankare, E.; Burgett, W. S.; Chambers, K. C.; Dombeck, T.; Grav, T.; Heasley, J. N.; Hodapp, K. W.; Jedicke, R.; Kaiser, N.; Kudritzki, R.; Luppino, G.; Lupton, R. H.; Magnier, E. A.; Monet, D. G.; Morgan, J. S.; Onaka, P. M.; Price, P. A.; Rhoads, P. H.; Siegmund, W. A.; Stubbs, Christopher William; Tonry, J. L.; Wainscoat, R. J.; Waterson, M. F.; Wynn-Williams, C. G.

Note: Order does not necessarily reflect citation order of authors.

Citation: Gezari, S., A. Rest, M. E. Huber, G. Narayan, K. Forster, J. D. Neill, D. C. Martin, et al. 2010. Galex and Pan-Starrs1 Discovery of SN IIP 2010 aq: The First Few Days After Shock Breakout in a Red Supergiant Star. The Astrophysical Journal 720, no. 1: L77–L81. doi:10.1088/2041-8205/720/1/l77.
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Abstract: We present the early UV and optical light curve of Type IIP supernova (SN) 2010aq at z = 0.0862, and compare it to analytical models for thermal emission following SN shock breakout in a red supergiant star. SN 2010aq was discovered in joint monitoring between the Galaxy Evolution Explorer (GALEX) Time Domain Survey (TDS) in the NUV and the Pan-STARRS1 Medium Deep Survey (PS1 MDS) in the g, r, i, and z bands. The GALEX and Pan-STARRS1 observations detect the SN less than 1 day after shock breakout, measure a diluted blackbody temperature of 31, 000 ± 6, 000 K 1 day later, and follow the rise in the UV/optical light curve over the next 2 days caused by the expansion and cooling of the SN ejecta. The high signal-to-noise ratio of the simultaneous UV and optical photometry allows us to fit for a progenitor star radius of 700 ± 200R⊙, the size of a red supergiant star. An excess in UV emission two weeks after shock breakout compared to SNe well fitted by model atmosphere-code synthetic spectra with solar metallicity, is best explained by suppressed line blanketing due to a lower metallicity progenitor star in SN 2010aq. Continued monitoring of PS1 MDS fields by the GALEX TDS will increase the sample of early UV detections of Type II SNe by an order of magnitude, and probe the diversity of SN progenitor star properties.
Published Version: doi:10.1088/2041-8205/720/1/l77
Other Sources: https://arxiv.org/pdf/1007.4551.pdf
Terms of Use: This article is made available under the terms and conditions applicable to Open Access Policy Articles, as set forth at http://nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of-use#OAP
Citable link to this page: http://nrs.harvard.edu/urn-3:HUL.InstRepos:30410831
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