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 Prieto; R. 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

doi:10.3847/1538-4357/aaa12a

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

CLAS-NS: Earth and Space Exploration, School of (SESE)

Research output: Contribution to journal › Article › peer-review

11 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 language	English (US)
Article number	108
Journal	Astrophysical Journal
Volume	852
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/aaa12a
State	Published - Jan 10 2018

Keywords

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

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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Finzell, T., Chomiuk, L., Metzger, B. D., Walter, F. M., Linford, J. D., Mukai, K., Nelson, T., Weston, J. H. S., Zheng, Y., Sokoloski, J. L., Mioduszewski, A., Rupen, M. P., Dong, S., Starrfield, S., Cheung, C. C., Woodward, C. E., Taylor, G. B., Bohlsen, T., Buil, C., ... Gould, A. (2018). A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date. Astrophysical Journal, 852(2), [108]. https://doi.org/10.3847/1538-4357/aaa12a

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date. / Finzell, Thomas; Chomiuk, Laura; Metzger, Brian D.; Walter, Frederick M.; Linford, Justin D.; Mukai, Koji; Nelson, Thomas; Weston, Jennifer H.S.; Zheng, Yong; Sokoloski, Jennifer L.; Mioduszewski, Amy; Rupen, Michael P.; Dong, Subo; Starrfield, Sumner; Cheung, C. C.; Woodward, Charles E.; Taylor, Gregory B.; Bohlsen, Terry; Buil, Christian; Prieto, Jose; Wagner, R. Mark; Bensby, Thomas; Bond, I. A.; Sumi, T.; Bennett, D. P.; Abe, F.; Koshimoto, N.; Suzuki, D.; Tristram, P. J.; Christie, Grant W.; Natusch, Tim; McCormick, Jennie; Yee, Jennifer; Gould, Andy.

In: Astrophysical Journal, Vol. 852, No. 2, 108, 10.01.2018.

Research output: Contribution to journal › Article › peer-review

Finzell, T, Chomiuk, L, Metzger, BD, Walter, FM, Linford, JD, Mukai, K, Nelson, T, Weston, JHS, Zheng, Y, Sokoloski, JL, Mioduszewski, A, Rupen, MP, Dong, S, Starrfield, S, Cheung, CC, Woodward, CE, Taylor, GB, Bohlsen, T, Buil, C, Prieto, J, Wagner, RM, Bensby, T, Bond, IA, Sumi, T, Bennett, DP, Abe, F, Koshimoto, N, Suzuki, D, Tristram, PJ, Christie, GW, Natusch, T, McCormick, J, Yee, J & Gould, A 2018, 'A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date', Astrophysical Journal, vol. 852, no. 2, 108. https://doi.org/10.3847/1538-4357/aaa12a

Finzell, Thomas ; Chomiuk, Laura ; Metzger, Brian D. ; Walter, Frederick M. ; Linford, Justin D. ; Mukai, Koji ; Nelson, Thomas ; Weston, Jennifer H.S. ; Zheng, Yong ; Sokoloski, Jennifer L. ; Mioduszewski, Amy ; Rupen, Michael P. ; Dong, Subo ; Starrfield, Sumner ; Cheung, C. C. ; Woodward, Charles E. ; Taylor, Gregory B. ; Bohlsen, Terry ; Buil, Christian ; Prieto, Jose ; Wagner, R. Mark ; Bensby, Thomas ; Bond, I. A. ; Sumi, T. ; Bennett, D. P. ; Abe, F. ; Koshimoto, N. ; Suzuki, D. ; Tristram, P. J. ; Christie, Grant W. ; Natusch, Tim ; McCormick, Jennie ; Yee, Jennifer ; Gould, Andy. / A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date. In: Astrophysical Journal. 2018 ; Vol. 852, No. 2.

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

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.",

keywords = "gamma rays: stars, novae, cataclysmic variables, radio continuum: stars, stars: individual (V1324 Sco)",

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

note = "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). 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: The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are The University of Arizona on behalf of the Arizona university system; Instituto Nazionale di Astrofisica, Italy; LBT Beteili-gungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University; and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota, and University of Virginia. This research is also based on data collected with the European Southern Observatory telescopes, proposal ID 089.B-0047(I).",

year = "2018",

month = jan,

day = "10",

doi = "10.3847/1538-4357/aaa12a",

language = "English (US)",

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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: 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). 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: The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are The University of Arizona on behalf of the Arizona university system; Instituto Nazionale di Astrofisica, Italy; LBT Beteili-gungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University; and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota, and University of Virginia. This research is also based on data collected with the European Southern Observatory telescopes, proposal ID 089.B-0047(I).

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)

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