2020ApJ...898...56M


Query : 2020ApJ...898...56M

2020ApJ...898...56M - Astrophys. J., 898, 56-56 (2020/July-3)

The spectacular ultraviolet flash from the peculiar Type Ia supernova 2019yvq.

MILLER A.A., MAGEE M.R., POLIN A., MAGUIRE K., ZIMMERMAN E., YAO Y., SOLLERMAN J., SCHULZE S., PERLEY D.A., KROMER M., DHAWAN S., BULLA M., ANDREONI I., BELLM E.C., DE K., DEKANY R., DELACROIX A., FREMLING C., GAL-YAM A., GOLDSTEIN D.A., GOLKHOU V.Z., GOOBAR A., GRAHAM M.J., IRANI I., KASLIWAL M.M., KAYE S., KIM Y.-L., LAHER R.R., MAHABAL A.A., MASCI F.J., NUGENT P.E., OFEK E., PHINNEY E.S., PRENTICE S.J., RIDDLE R., RIGAULT M., RUSHOLME B., SCHWEYER T., SHUPE D.L., SOUMAGNAC M.T., TERRERAN G., WALTERS R., YAN L., ZOLKOWER J. and KULKARNI S.R.

Abstract (from CDS):

Early observations of Type Ia supernovae (SNe Ia) provide essential clues for understanding the progenitor system that gave rise to the terminal thermonuclear explosion. We present exquisite observations of SN 2019yvq, the second observed SN Ia, after iPTF 14atg, to display an early flash of emission in the ultraviolet (UV) and optical. Our analysis finds that SN 2019yvq was unusual, even when ignoring the initial flash, in that it was moderately underluminous for an SN Ia (Mg~-18.5 mag at peak) yet featured very high absorption velocities (v~15,000 km s–1 for Si II λ6355 at peak). We find that many of the observational features of SN 2019yvq, aside from the flash, can be explained if the explosive yield of radioactive 56Ni is relatively low (we measure M56Ni_=0.31±0.05M) and it and other iron-group elements are concentrated in the innermost layers of the ejecta. To explain both the UV/optical flash and peak properties of SN 2019yvq we consider four different models: interaction between the SN ejecta and a nondegenerate companion, extended clumps of 56Ni in the outer ejecta, a double-detonation explosion, and the violent merger of two white dwarfs. Each of these models has shortcomings when compared to the observations; it is clear additional tuning is required to better match SN 2019yvq. In closing, we predict that the nebular spectra of SN 2019yvq will feature either H or He emission, if the ejecta collided with a companion, strong [Ca II] emission, if it was a double detonation, or narrow [O I] emission, if it was due to a violent merger.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Surveys - Supernovae - Type Ia supernovae - White dwarf stars - Observational astronomy

VizieR on-line data: <Available at CDS (J/ApJ/898/56): table1.dat table2.dat table3.dat sp/*>

Simbad objects: 21

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Number of rows : 21
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 NGC 220 OpC 00 40 55.96 -73 24 10.1 14.24 14.61 14.39   14.49 ~ 34 0
2 SN 2006ot SN* 02 15 04.84 -20 45 58.2     17.4     SNIap 40 1
3 SN 2010lp SN* 02 54 03.50 +02 57 43.4           SNIapec 40 1
4 SN 2002es SN* 03 23 47.23 +40 33 53.5     16.4     SNIapec 55 1
5 SN 2018oh SN* 09 06 39.6 +19 20 18           SNIa-norm 71 0
6 SN 2010jn SN* 09 37 29.95 +23 09 38.8   17.29 16.85     SNIa 34 1
7 SN 2014J SN* 09 55 42.12 +69 40 25.9           SNIa-norm 402 1
8 SN 2002bo SN* 10 18 06.51 +21 49 41.7   13.95       SNIa 306 1
9 NAME Great Attractor SCG 10 32 -46.0           ~ 548 0
10 NGC 4441 GiG 12 27 20.402 +64 48 05.64   13.5       ~ 80 0
11 SN 2019yvq SN* 12 27 21.850 +64 47 59.82           SNIa 28 0
12 ASASSN -14bd SN* 12 52 44.8 +26 28 13           SNIa 81 0
13 SN 1986G SN* 13 25 36.46 -43 01 53.6   12.45 11.44     SNIapec 405 1
14 SN 2011fe SN* 14 03 05.711 +54 16 25.22   10.12 10.06     SNIa-norm 660 1
15 SN 2017cbv SN* 14 32 34.420 -44 08 02.74           SNIa 107 0
16 SN 2017erp SN* 15 09 14.9 -11 20 03           SNIa-norm 35 0
17 PTF 09dnp SN* 15 19 24.5 +49 29 56           SNIa-norm 16 0
18 SN 2006bt SN* 15 56 33.81 +20 03 07.2     17.5     SNIap 99 1
19 SN 2018eag SN* 18 57 16.317 +46 29 56.75           SNIa 6 0
20 SN 2004eo SN* 20 32 54.19 +09 55 42.7   15.07 17.8     SNIa 203 1
21 PTF 10ops SN* 21 47 33.57 +05 51 30.3           SNIa 31 0

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