TY - JOUR
T1 - A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date
AU - Finzell, Thomas
AU - Chomiuk, Laura
AU - Metzger, Brian D.
AU - Walter, Frederick M.
AU - Linford, Justin D.
AU - Mukai, Koji
AU - Nelson, Thomas
AU - Weston, Jennifer H.S.
AU - Zheng, Yong
AU - Sokoloski, Jennifer L.
AU - Mioduszewski, Amy
AU - Rupen, Michael P.
AU - Dong, Subo
AU - Starrfield, Sumner
AU - Cheung, C. C.
AU - Woodward, Charles E.
AU - Taylor, Gregory B.
AU - Bohlsen, Terry
AU - Buil, Christian
AU - Prieto, Jose
AU - Wagner, R. Mark
AU - Bensby, Thomas
AU - Bond, I. A.
AU - Sumi, T.
AU - Bennett, D. P.
AU - Abe, F.
AU - Koshimoto, N.
AU - Suzuki, D.
AU - Tristram, P. J.
AU - Christie, Grant W.
AU - Natusch, Tim
AU - McCormick, Jennie
AU - Yee, Jennifer
AU - Gould, Andy
N1 - Funding Information:
This research has made use of the AstroBetter blog and wiki. It was funded in part by the Fermi Guest Investigator grants NNX14AQ36G (L.C.), NNG16PX24I (C.C.C.), and NNX15AU77G and NNX16AR73G (B. Metzger). It was also supported by the National Science Foundation (AST-1615084), and the Research Corporation for Science Advancement Scialog Fellows Program (RCSA 23810); S.S. gratefully acknowledges NSF and NASA grants to ASU.
Funding Information:
We acknowledge and give thanks to the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. This research has made use of the AstroBetter blog and wiki. It was funded in part by the Fermi Guest Investigator grants NNX14AQ36G (L.C.), NNG16PX24I (C.C.C.), and NNX15AU77G and NNX16AR73G (B. Metzger). It was also supported by the National Science Foundation (AST-1615084), and the Research Corporation for Science Advancement Scialog Fellows Program (RCSA 23810); S.S. gratefully acknowledges NSF and NASA grants to ASU.
Funding Information:
IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. See Tody (1993).
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/1/10
Y1 - 2018/1/10
N2 - It has recently been discovered that some, if not all, classical novae emit GeV gamma-rays during outburst, but the mechanisms involved in the production ofgamma-rays are still not well understood. We present here a comprehensive multiwavelength data set - from radio to X-rays - for the most gamma-ray-luminous classical nova to date, V1324 Sco. Using this data set, we show that V1324 Sco is a canonical dusty Fe ii-type nova, with a maximum ejecta velocity of 2600 km s-1 and an ejecta mass of a few × 10-5 M⊙. There is also evidence for complex shock interactions, including a double-peaked radio light curve which shows high brightness temperatures at early times. To explore why V1324 Sco was so gamma-ray luminous, we present a model of the nova ejecta featuring strong internal shocks and find that higher gamma-ray luminosities result from higher ejecta velocities and/or mass-loss rates. Comparison of V1324 Sco with other gamma-ray-detected novae does not show clear signatures of either, and we conclude that a larger sample of similarly well-observed novae is needed to understand the origin and variation of gamma-rays in novae.
AB - It has recently been discovered that some, if not all, classical novae emit GeV gamma-rays during outburst, but the mechanisms involved in the production ofgamma-rays are still not well understood. We present here a comprehensive multiwavelength data set - from radio to X-rays - for the most gamma-ray-luminous classical nova to date, V1324 Sco. Using this data set, we show that V1324 Sco is a canonical dusty Fe ii-type nova, with a maximum ejecta velocity of 2600 km s-1 and an ejecta mass of a few × 10-5 M⊙. There is also evidence for complex shock interactions, including a double-peaked radio light curve which shows high brightness temperatures at early times. To explore why V1324 Sco was so gamma-ray luminous, we present a model of the nova ejecta featuring strong internal shocks and find that higher gamma-ray luminosities result from higher ejecta velocities and/or mass-loss rates. Comparison of V1324 Sco with other gamma-ray-detected novae does not show clear signatures of either, and we conclude that a larger sample of similarly well-observed novae is needed to understand the origin and variation of gamma-rays in novae.
KW - gamma rays: stars
KW - novae, cataclysmic variables
KW - radio continuum: stars
KW - stars: individual (V1324 Sco)
UR - http://www.scopus.com/inward/record.url?scp=85040659904&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85040659904&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/aaa12a
DO - 10.3847/1538-4357/aaa12a
M3 - Article
AN - SCOPUS:85040659904
VL - 852
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 108
ER -