A planetary nebula around Nova V458 vulpeculae undergoing flash ionization

R. Wesson; M. J. Barlow; R. L M Corradi; J. E. Drew; P. J. Groot; C. Knigge; D. Steeghs; B. T. Gaensicke; R. Napiwotzki; P. Rodriguez-Gil; A. A. Zijlstra; M. F. Bode; J. J. Drake; D. J. Frew; E. A. Gonzalez-Solares; R. Greimel; M. J. Irwin; L. Morales-Rueda; G. Nelemans; Q. A. Parker; S. E. Sale; J. L. Sokoloski; A. Somero; H. Uthas; N. A. Walton; B. Warner; C. A. Watson; N. J. Wright

doi:10.1086/594366

A planetary nebula around Nova V458 vulpeculae undergoing flash ionization

R. Wesson^*, M. J. Barlow, R. L M Corradi, J. E. Drew, P. J. Groot, C. Knigge, D. Steeghs, B. T. Gaensicke, R. Napiwotzki, P. Rodriguez-Gil, A. A. Zijlstra, M. F. Bode, J. J. Drake, D. J. Frew, E. A. Gonzalez-Solares, R. Greimel, M. J. Irwin, L. Morales-Rueda, G. Nelemans, Q. A. Parker & 8 others S. E. Sale, J. L. Sokoloski, A. Somero, H. Uthas, N. A. Walton, B. Warner, C. A. Watson, N. J. Wright

^*Corresponding author for this work

Research output: Contribution to journal › Article

50 Citations (Scopus)

Abstract

Nova V458 Vul erupted on 2007 August 8 and reached a visual magnitude of 8.1 a few days later. Ha images obtained 6 weeks before the outburst as part of the IPHAS Galactic plane survey reveal an 18th magnitude progenitor surrounded by an extended nebula. Subsequent images and spectroscopy of the nebula reveal an inner nebular knot increasing rapidly in brightness due to flash ionization by the nova event. We derive a distance of 13 kpc based on light travel time considerations, which is supported by two other distance estimation methods. The nebula has an ionized mass of 0.2 M_&o.;, and a low expansion velocity: this rules it out as ejecta from a previous nova eruption, and is consistent with it being a-14,000 year old planetary nebula, probably the product of a prior common envelope (CE) phase of evolution of the binary system. The large derived distance means that the mass of the erupting WD component of the binary is high. We identify two possible evolutionary scenarios, in at least one of which the system is massive enough to produce a Type Ia supernova upon merging.

Original language	English
Pages (from-to)	L21–L24
Number of pages	4
Journal	Astrophysical Journal
Volume	688
Issue number	1 PART 2
DOIs	https://doi.org/10.1086/594366
Publication status	Published - 2008

Keywords

Cataclysmic variables
Ism: abundances
Novae

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Wesson, R. ; Barlow, M. J. ; Corradi, R. L M ; Drew, J. E. ; Groot, P. J. ; Knigge, C. ; Steeghs, D. ; Gaensicke, B. T. ; Napiwotzki, R. ; Rodriguez-Gil, P. ; Zijlstra, A. A. ; Bode, M. F. ; Drake, J. J. ; Frew, D. J. ; Gonzalez-Solares, E. A. ; Greimel, R. ; Irwin, M. J. ; Morales-Rueda, L. ; Nelemans, G. ; Parker, Q. A. ; Sale, S. E. ; Sokoloski, J. L. ; Somero, A. ; Uthas, H. ; Walton, N. A. ; Warner, B. ; Watson, C. A. ; Wright, N. J. / A planetary nebula around Nova V458 vulpeculae undergoing flash ionization. In: Astrophysical Journal. 2008 ; Vol. 688, No. 1 PART 2. pp. L21–L24.

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title = "A planetary nebula around Nova V458 vulpeculae undergoing flash ionization",

abstract = "Nova V458 Vul erupted on 2007 August 8 and reached a visual magnitude of 8.1 a few days later. Ha images obtained 6 weeks before the outburst as part of the IPHAS Galactic plane survey reveal an 18th magnitude progenitor surrounded by an extended nebula. Subsequent images and spectroscopy of the nebula reveal an inner nebular knot increasing rapidly in brightness due to flash ionization by the nova event. We derive a distance of 13 kpc based on light travel time considerations, which is supported by two other distance estimation methods. The nebula has an ionized mass of 0.2 M&o.;, and a low expansion velocity: this rules it out as ejecta from a previous nova eruption, and is consistent with it being a-14,000 year old planetary nebula, probably the product of a prior common envelope (CE) phase of evolution of the binary system. The large derived distance means that the mass of the erupting WD component of the binary is high. We identify two possible evolutionary scenarios, in at least one of which the system is massive enough to produce a Type Ia supernova upon merging.",

keywords = "Cataclysmic variables, Ism: abundances, Novae",

author = "R. Wesson and Barlow, {M. J.} and Corradi, {R. L M} and Drew, {J. E.} and Groot, {P. J.} and C. Knigge and D. Steeghs and Gaensicke, {B. T.} and R. Napiwotzki and P. Rodriguez-Gil and Zijlstra, {A. A.} and Bode, {M. F.} and Drake, {J. J.} and Frew, {D. J.} and Gonzalez-Solares, {E. A.} and R. Greimel and Irwin, {M. J.} and L. Morales-Rueda and G. Nelemans and Parker, {Q. A.} and Sale, {S. E.} and Sokoloski, {J. L.} and A. Somero and H. Uthas and Walton, {N. A.} and B. Warner and Watson, {C. A.} and Wright, {N. J.}",

year = "2008",

doi = "10.1086/594366",

language = "English",

volume = "688",

pages = "L21–L24",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing",

number = "1 PART 2",

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Wesson, R, Barlow, MJ, Corradi, RLM, Drew, JE, Groot, PJ, Knigge, C, Steeghs, D, Gaensicke, BT, Napiwotzki, R, Rodriguez-Gil, P, Zijlstra, AA, Bode, MF, Drake, JJ, Frew, DJ, Gonzalez-Solares, EA, Greimel, R, Irwin, MJ, Morales-Rueda, L, Nelemans, G, Parker, QA, Sale, SE, Sokoloski, JL, Somero, A, Uthas, H, Walton, NA, Warner, B, Watson, CA & Wright, NJ 2008, 'A planetary nebula around Nova V458 vulpeculae undergoing flash ionization', Astrophysical Journal, vol. 688, no. 1 PART 2, pp. L21–L24. https://doi.org/10.1086/594366

A planetary nebula around Nova V458 vulpeculae undergoing flash ionization. / Wesson, R.; Barlow, M. J.; Corradi, R. L M; Drew, J. E.; Groot, P. J.; Knigge, C.; Steeghs, D.; Gaensicke, B. T.; Napiwotzki, R.; Rodriguez-Gil, P.; Zijlstra, A. A.; Bode, M. F.; Drake, J. J.; Frew, D. J.; Gonzalez-Solares, E. A.; Greimel, R.; Irwin, M. J.; Morales-Rueda, L.; Nelemans, G.; Parker, Q. A.; Sale, S. E.; Sokoloski, J. L.; Somero, A.; Uthas, H.; Walton, N. A.; Warner, B.; Watson, C. A.; Wright, N. J.

In: Astrophysical Journal, Vol. 688, No. 1 PART 2, 2008, p. L21–L24.

Research output: Contribution to journal › Article

TY - JOUR

T1 - A planetary nebula around Nova V458 vulpeculae undergoing flash ionization

AU - Wesson, R.

AU - Barlow, M. J.

AU - Corradi, R. L M

AU - Drew, J. E.

AU - Groot, P. J.

AU - Knigge, C.

AU - Steeghs, D.

AU - Gaensicke, B. T.

AU - Napiwotzki, R.

AU - Rodriguez-Gil, P.

AU - Zijlstra, A. A.

AU - Bode, M. F.

AU - Drake, J. J.

AU - Frew, D. J.

AU - Gonzalez-Solares, E. A.

AU - Greimel, R.

AU - Irwin, M. J.

AU - Morales-Rueda, L.

AU - Nelemans, G.

AU - Parker, Q. A.

AU - Sale, S. E.

AU - Sokoloski, J. L.

AU - Somero, A.

AU - Uthas, H.

AU - Walton, N. A.

AU - Warner, B.

AU - Watson, C. A.

AU - Wright, N. J.

PY - 2008

Y1 - 2008

N2 - Nova V458 Vul erupted on 2007 August 8 and reached a visual magnitude of 8.1 a few days later. Ha images obtained 6 weeks before the outburst as part of the IPHAS Galactic plane survey reveal an 18th magnitude progenitor surrounded by an extended nebula. Subsequent images and spectroscopy of the nebula reveal an inner nebular knot increasing rapidly in brightness due to flash ionization by the nova event. We derive a distance of 13 kpc based on light travel time considerations, which is supported by two other distance estimation methods. The nebula has an ionized mass of 0.2 M&o.;, and a low expansion velocity: this rules it out as ejecta from a previous nova eruption, and is consistent with it being a-14,000 year old planetary nebula, probably the product of a prior common envelope (CE) phase of evolution of the binary system. The large derived distance means that the mass of the erupting WD component of the binary is high. We identify two possible evolutionary scenarios, in at least one of which the system is massive enough to produce a Type Ia supernova upon merging.

AB - Nova V458 Vul erupted on 2007 August 8 and reached a visual magnitude of 8.1 a few days later. Ha images obtained 6 weeks before the outburst as part of the IPHAS Galactic plane survey reveal an 18th magnitude progenitor surrounded by an extended nebula. Subsequent images and spectroscopy of the nebula reveal an inner nebular knot increasing rapidly in brightness due to flash ionization by the nova event. We derive a distance of 13 kpc based on light travel time considerations, which is supported by two other distance estimation methods. The nebula has an ionized mass of 0.2 M&o.;, and a low expansion velocity: this rules it out as ejecta from a previous nova eruption, and is consistent with it being a-14,000 year old planetary nebula, probably the product of a prior common envelope (CE) phase of evolution of the binary system. The large derived distance means that the mass of the erupting WD component of the binary is high. We identify two possible evolutionary scenarios, in at least one of which the system is massive enough to produce a Type Ia supernova upon merging.

KW - Cataclysmic variables

KW - Ism: abundances

KW - Novae

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U2 - 10.1086/594366

DO - 10.1086/594366

M3 - Article

VL - 688

SP - L21–L24

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1 PART 2

ER -