A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

Thomas Finzell, Laura Chomiuk, Brian D. Metzger, Frederick M. Walter, Justin D. Linford, Koji Mukai, Thomas Nelson, Jennifer H.S. Weston, Yong Zheng, Jennifer L. Sokoloski, Amy Mioduszewski, Michael P. Rupen, Subo Dong, Sumner Starrfield, C. C. Cheung, Charles E. Woodward, Gregory B. Taylor, Terry Bohlsen, Christian Buil, Jose PrietoR. Mark Wagner, Thomas Bensby, I. A. Bond, T. Sumi, D. P. Bennett, F. Abe, N. Koshimoto, D. Suzuki, P. J. Tristram, Grant W. Christie, Tim Natusch, Jennie McCormick, Jennifer Yee, Andy Gould

Research output: Contribution to journalArticlepeer-review

16 Scopus citations

Abstract

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.

Original languageEnglish (US)
Article number108
JournalAstrophysical Journal
Volume852
Issue number2
DOIs
StatePublished - Jan 10 2018

Bibliographical note

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.

Keywords

  • gamma rays: stars
  • novae, cataclysmic variables
  • radio continuum: stars
  • stars: individual (V1324 Sco)

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