Shappee, BJ, Piro, AL, Holoien, TW-S, Prieto, JL, Contreras, C, Itagaki, K, Burns, CR, Kochanek, CS, Stanek, KZ, Alper, E, Basu, U, Beacom, JF, Bersier, D, Brimacombe, J, Conseil, E, Danilet, AB, Dong, S, Falco, E, Grupe, D, Hsiao, EY et al, Kiyota, S, Morrell, N, Nicolas, J, Phillips, MM, Pojmanski, G, Simonian, G, Stritzinger, M, Szczygieł, DM, Thompson, TA, Thorstensen, J, Wagner, M and Woźniak, PR (2016) The Young and Bright Type Ia Supernova ASASSN-14lp: Discovery, Early-Time Observations, First-Light Time, Distance to NGC 4666, and Progenitor Constraints. ASTROPHYSICAL JOURNAL, 826 (2). ISSN 0004-637X

Preview

Text 1507.04257v1.pdf - Accepted Version Download (4MB) | Preview

Abstract

On 2014 Dec. 9.61, the All-Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin") discovered ASASSN-14lp just $\sim2$ days after first light using a global array of 14-cm diameter telescopes. ASASSN-14lp went on to become a bright supernova ($V = 11.94$ mag), second only to SN 2014J for the year. We present prediscovery photometry (with a detection less than a day after first light) and ultraviolet through near-infrared photometric and spectroscopic data covering the rise and fall of ASASSN-14lp for more than 100 days. We find that ASASSN-14lp had a broad light curve ($\Delta m_{15}(B) = 0.796 \pm 0.001_{\textrm{stat}}$), a $B$-band maximum at $2457015.823 \pm 0.030_{\textrm{stat}}$, a rise time of $16.94^{+ 0.11 }_{- 0.11 }$ days, and moderate host--galaxy extinction ($E(B-V)_{\textrm{host}} = 0.329 \pm 0.001_{\textrm{stat}}$). Using ASASSN-14lp we derive a distance modulus for NGC 4666 of $\mu = 30.834 \pm 0.003_{\textrm{stat}} \pm 0.16_{\textrm{syst}}$ corresponding to a distance of $14.68 \pm 0.02_{\textrm{stat}} \pm 1.15_{\textrm{syst}}$ Mpc. However, a tip of the red giant branch distance to the host galaxy should be measured to allow ASASSN-14lp to be added to the calibrating sample of Type Ia supernovae. Finally, using our early-time photometric and spectroscopic data along with our derived light curve properties, we rule out red giant secondaries with limits on the radius of a non-degenerate companion as small as $0.34 \rm{R}_\odot$ for favorable viewing angles and estimates of the explosion time.

Item Type:	Article
Uncontrolled Keywords:	astro-ph.CO; astro-ph.CO; astro-ph.HE
Subjects:	Q Science > QB Astronomy
Divisions:	Astrophysics Research Institute
Publisher:	American Astronomical Society and IOP Publishing
Related URLs:	http://arxiv.org/abs/1507.04257v1
Date Deposited:	05 Aug 2015 13:14
Last Modified:	04 Sep 2021 14:09
URI:	https://researchonline.ljmu.ac.uk/id/eprint/1685

View Item