Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126

M. Henze, W. Pietsch, F. Haberl, M. Della Valle, A. Riffeser, G. Sala, D. Hatzidimitriou, F. Hofmann, D. H. Hartmann, J. Koppenhoefer, S. Seitz, George G Williams, K. Hornoch, K. Itagaki, F. Kabashima, K. Nishiyama, G. Xing, C. H. Lee, E. Magnier, K. Chambers

Research output: Contribution to journalArticle

12 Citations (Scopus)

Abstract

Context. Classical novae (CNe) represent the main class of supersoft X-ray sources (SSSs) in the central region of our neighbouring galaxy M 31. Only three confirmed novae and three SSSs have been discovered in globular clusters (GCs) of any galaxy so far, of which one nova and two SSSs (including the nova) were found in M 31 GCs. Aims. To study the SSS state of CNe we carried out a high-cadence X-ray monitoring of the M 31 central area with XMM-Newton and Chandra. This project is supplemented by regular optical monitoring programmes at various observatories. Methods. We analysed X-ray and optical monitoring data of a new transient X-ray source in the M 31 GC Bol 126, discovered serendipitously in Swift observations. Our optical data set was based on regular M 31 monitoring programmes from five different small telescopes and was reduced using a homogeneous method. Additionally, we made use of Pan-STARRS 1 data obtained during the PAndromeda survey. We extracted light curves of the source in the optical and X-rays, as well as X-ray spectra. Results. Our observations reveal that the X-ray source in Bol 126 is the third SSS in an M 31 GC and can be confirmed as the second CN in the M 31 GC system. This nova is named M31N 2010-10f. Its properties in the X-ray (high black-body temperature, short SSS phase) and optical (relatively high maximum magnitude, fast decline) regimes agree with a massive white dwarf (MWD ≳ 1.3 M) in the binary system. Incorporating the data on previously found (suspected) novae in M 31 GCs we used our high-cadence X-ray monitoring observations to estimate a tentative nova rate in the M 31 GC system of 0.05 yr-1 GC-1. An optical estimate, based on the recent 10.5-year WeCAPP survey, gives a lower nova rate, which is compatible with the X-ray rate on the 95% confidence level. Conclusions. Although still based on small-number statistics, there is growing evidence that the nova rate in GCs is higher than expected from primordial binary formation and under conditions as in the field. Dynamical binary formation and/or additional accretion from the intracluster medium are possible scenarios for an increased nova rate, but observational confirmation for this enhancement has been absent, so far. Regular X-ray monitoring observations of M 31 provide a promising strategy to find these novae.

Original languageEnglish (US)
Article numberA120
JournalAstronomy and Astrophysics
Volume549
DOIs
StatePublished - 2013

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globular clusters
x rays
novae
monitoring
galaxies
body temperature
XMM-Newton telescope
estimates
newton
light curve
confidence
observatories

Keywords

  • Galaxies: individual: M 31
  • Globular clusters: individual: Bol 126
  • Novae cataclysmic variables
  • Stars: individual: M31N 2010-10f
  • X-rays: binaries

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Henze, M., Pietsch, W., Haberl, F., Della Valle, M., Riffeser, A., Sala, G., ... Chambers, K. (2013). Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126. Astronomy and Astrophysics, 549, [A120]. https://doi.org/10.1051/0004-6361/201220196

Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126. / Henze, M.; Pietsch, W.; Haberl, F.; Della Valle, M.; Riffeser, A.; Sala, G.; Hatzidimitriou, D.; Hofmann, F.; Hartmann, D. H.; Koppenhoefer, J.; Seitz, S.; Williams, George G; Hornoch, K.; Itagaki, K.; Kabashima, F.; Nishiyama, K.; Xing, G.; Lee, C. H.; Magnier, E.; Chambers, K.

In: Astronomy and Astrophysics, Vol. 549, A120, 2013.

Research output: Contribution to journalArticle

Henze, M, Pietsch, W, Haberl, F, Della Valle, M, Riffeser, A, Sala, G, Hatzidimitriou, D, Hofmann, F, Hartmann, DH, Koppenhoefer, J, Seitz, S, Williams, GG, Hornoch, K, Itagaki, K, Kabashima, F, Nishiyama, K, Xing, G, Lee, CH, Magnier, E & Chambers, K 2013, 'Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126', Astronomy and Astrophysics, vol. 549, A120. https://doi.org/10.1051/0004-6361/201220196
Henze, M. ; Pietsch, W. ; Haberl, F. ; Della Valle, M. ; Riffeser, A. ; Sala, G. ; Hatzidimitriou, D. ; Hofmann, F. ; Hartmann, D. H. ; Koppenhoefer, J. ; Seitz, S. ; Williams, George G ; Hornoch, K. ; Itagaki, K. ; Kabashima, F. ; Nishiyama, K. ; Xing, G. ; Lee, C. H. ; Magnier, E. ; Chambers, K. / Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126. In: Astronomy and Astrophysics. 2013 ; Vol. 549.
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title = "Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126",
abstract = "Context. Classical novae (CNe) represent the main class of supersoft X-ray sources (SSSs) in the central region of our neighbouring galaxy M 31. Only three confirmed novae and three SSSs have been discovered in globular clusters (GCs) of any galaxy so far, of which one nova and two SSSs (including the nova) were found in M 31 GCs. Aims. To study the SSS state of CNe we carried out a high-cadence X-ray monitoring of the M 31 central area with XMM-Newton and Chandra. This project is supplemented by regular optical monitoring programmes at various observatories. Methods. We analysed X-ray and optical monitoring data of a new transient X-ray source in the M 31 GC Bol 126, discovered serendipitously in Swift observations. Our optical data set was based on regular M 31 monitoring programmes from five different small telescopes and was reduced using a homogeneous method. Additionally, we made use of Pan-STARRS 1 data obtained during the PAndromeda survey. We extracted light curves of the source in the optical and X-rays, as well as X-ray spectra. Results. Our observations reveal that the X-ray source in Bol 126 is the third SSS in an M 31 GC and can be confirmed as the second CN in the M 31 GC system. This nova is named M31N 2010-10f. Its properties in the X-ray (high black-body temperature, short SSS phase) and optical (relatively high maximum magnitude, fast decline) regimes agree with a massive white dwarf (MWD ≳ 1.3 M⊙) in the binary system. Incorporating the data on previously found (suspected) novae in M 31 GCs we used our high-cadence X-ray monitoring observations to estimate a tentative nova rate in the M 31 GC system of 0.05 yr-1 GC-1. An optical estimate, based on the recent 10.5-year WeCAPP survey, gives a lower nova rate, which is compatible with the X-ray rate on the 95{\%} confidence level. Conclusions. Although still based on small-number statistics, there is growing evidence that the nova rate in GCs is higher than expected from primordial binary formation and under conditions as in the field. Dynamical binary formation and/or additional accretion from the intracluster medium are possible scenarios for an increased nova rate, but observational confirmation for this enhancement has been absent, so far. Regular X-ray monitoring observations of M 31 provide a promising strategy to find these novae.",
keywords = "Galaxies: individual: M 31, Globular clusters: individual: Bol 126, Novae cataclysmic variables, Stars: individual: M31N 2010-10f, X-rays: binaries",
author = "M. Henze and W. Pietsch and F. Haberl and {Della Valle}, M. and A. Riffeser and G. Sala and D. Hatzidimitriou and F. Hofmann and Hartmann, {D. H.} and J. Koppenhoefer and S. Seitz and Williams, {George G} and K. Hornoch and K. Itagaki and F. Kabashima and K. Nishiyama and G. Xing and Lee, {C. H.} and E. Magnier and K. Chambers",
year = "2013",
doi = "10.1051/0004-6361/201220196",
language = "English (US)",
volume = "549",
journal = "Astronomy and Astrophysics",
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TY - JOUR

T1 - Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126

AU - Henze, M.

AU - Pietsch, W.

AU - Haberl, F.

AU - Della Valle, M.

AU - Riffeser, A.

AU - Sala, G.

AU - Hatzidimitriou, D.

AU - Hofmann, F.

AU - Hartmann, D. H.

AU - Koppenhoefer, J.

AU - Seitz, S.

AU - Williams, George G

AU - Hornoch, K.

AU - Itagaki, K.

AU - Kabashima, F.

AU - Nishiyama, K.

AU - Xing, G.

AU - Lee, C. H.

AU - Magnier, E.

AU - Chambers, K.

PY - 2013

Y1 - 2013

N2 - Context. Classical novae (CNe) represent the main class of supersoft X-ray sources (SSSs) in the central region of our neighbouring galaxy M 31. Only three confirmed novae and three SSSs have been discovered in globular clusters (GCs) of any galaxy so far, of which one nova and two SSSs (including the nova) were found in M 31 GCs. Aims. To study the SSS state of CNe we carried out a high-cadence X-ray monitoring of the M 31 central area with XMM-Newton and Chandra. This project is supplemented by regular optical monitoring programmes at various observatories. Methods. We analysed X-ray and optical monitoring data of a new transient X-ray source in the M 31 GC Bol 126, discovered serendipitously in Swift observations. Our optical data set was based on regular M 31 monitoring programmes from five different small telescopes and was reduced using a homogeneous method. Additionally, we made use of Pan-STARRS 1 data obtained during the PAndromeda survey. We extracted light curves of the source in the optical and X-rays, as well as X-ray spectra. Results. Our observations reveal that the X-ray source in Bol 126 is the third SSS in an M 31 GC and can be confirmed as the second CN in the M 31 GC system. This nova is named M31N 2010-10f. Its properties in the X-ray (high black-body temperature, short SSS phase) and optical (relatively high maximum magnitude, fast decline) regimes agree with a massive white dwarf (MWD ≳ 1.3 M⊙) in the binary system. Incorporating the data on previously found (suspected) novae in M 31 GCs we used our high-cadence X-ray monitoring observations to estimate a tentative nova rate in the M 31 GC system of 0.05 yr-1 GC-1. An optical estimate, based on the recent 10.5-year WeCAPP survey, gives a lower nova rate, which is compatible with the X-ray rate on the 95% confidence level. Conclusions. Although still based on small-number statistics, there is growing evidence that the nova rate in GCs is higher than expected from primordial binary formation and under conditions as in the field. Dynamical binary formation and/or additional accretion from the intracluster medium are possible scenarios for an increased nova rate, but observational confirmation for this enhancement has been absent, so far. Regular X-ray monitoring observations of M 31 provide a promising strategy to find these novae.

AB - Context. Classical novae (CNe) represent the main class of supersoft X-ray sources (SSSs) in the central region of our neighbouring galaxy M 31. Only three confirmed novae and three SSSs have been discovered in globular clusters (GCs) of any galaxy so far, of which one nova and two SSSs (including the nova) were found in M 31 GCs. Aims. To study the SSS state of CNe we carried out a high-cadence X-ray monitoring of the M 31 central area with XMM-Newton and Chandra. This project is supplemented by regular optical monitoring programmes at various observatories. Methods. We analysed X-ray and optical monitoring data of a new transient X-ray source in the M 31 GC Bol 126, discovered serendipitously in Swift observations. Our optical data set was based on regular M 31 monitoring programmes from five different small telescopes and was reduced using a homogeneous method. Additionally, we made use of Pan-STARRS 1 data obtained during the PAndromeda survey. We extracted light curves of the source in the optical and X-rays, as well as X-ray spectra. Results. Our observations reveal that the X-ray source in Bol 126 is the third SSS in an M 31 GC and can be confirmed as the second CN in the M 31 GC system. This nova is named M31N 2010-10f. Its properties in the X-ray (high black-body temperature, short SSS phase) and optical (relatively high maximum magnitude, fast decline) regimes agree with a massive white dwarf (MWD ≳ 1.3 M⊙) in the binary system. Incorporating the data on previously found (suspected) novae in M 31 GCs we used our high-cadence X-ray monitoring observations to estimate a tentative nova rate in the M 31 GC system of 0.05 yr-1 GC-1. An optical estimate, based on the recent 10.5-year WeCAPP survey, gives a lower nova rate, which is compatible with the X-ray rate on the 95% confidence level. Conclusions. Although still based on small-number statistics, there is growing evidence that the nova rate in GCs is higher than expected from primordial binary formation and under conditions as in the field. Dynamical binary formation and/or additional accretion from the intracluster medium are possible scenarios for an increased nova rate, but observational confirmation for this enhancement has been absent, so far. Regular X-ray monitoring observations of M 31 provide a promising strategy to find these novae.

KW - Galaxies: individual: M 31

KW - Globular clusters: individual: Bol 126

KW - Novae cataclysmic variables

KW - Stars: individual: M31N 2010-10f

KW - X-rays: binaries

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