Infrared space observatory short wavelength spectrometer observations of V1425 aquilae (Nova Aquila 1995)

J. E. Lyke; R. D. Gehrz; C. E. Woodward; M. J. Barlow; D. Péquignot; A. Salama; G. J. Schwarz; S. N. Shore; S. Starrfield; A. Evans; R. Gonzales-Riestra; M. A. Greenhouse; R. M. Hjellming; R. M. Humphreys; T. J. Jones; J. Krautter; C. Morisset; H. B. Ögelman; M. Orio; R. M. Wagner; N. A. Walton; R. E. Williams

doi:10.1086/324100

Infrared space observatory short wavelength spectrometer observations of V1425 aquilae (Nova Aquila 1995)

J. E. Lyke, R. D. Gehrz, C. E. Woodward, M. J. Barlow, D. Péquignot, A. Salama, G. J. Schwarz, S. N. Shore, S. Starrfield, A. Evans, R. Gonzales-Riestra, M. A. Greenhouse, R. M. Hjellming, R. M. Humphreys, T. J. Jones, J. Krautter, C. Morisset, H. B. Ögelman, M. Orio, R. M. WagnerN. A. Walton, R. E. Williams

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Abstract

We present observations of the classical nova V1425 Aquilae (Nova Aquila 1995) with the Infrared Space Observatory's (ISO) Short Wavelength Spectrometer, the Isaac Newton Telescope's Intermediate Dispersion Spectrograph, and the International Ultraviolet Explorer's Short-Wavelength Primary Spectrograph. Analysis of He II (1640 Å) development constrains the white dwarf turnoff to ∼400 days after outburst. Photoionization modeling of the optical and ISO spectra obtained during the late nebular phase constrains the mass of the ejecta between 2.5-4.2 × 10^-5 M_⊙. This modeling also suggests C and O in the ejecta were enhanced by a factor of ∼9, and N was enhanced by a factor of ∼ 100 with respect to solar, while Ne was only slightly enhanced. Based upon these analyses, we determine that the white dwarf in the V1425 Aq1 system has a CO composition and is at a distance of 3.0 ± 0.4 kpc.

Original language	English (US)
Pages (from-to)	3305-3312
Number of pages	8
Journal	Astronomical Journal
Volume	122
Issue number	6
DOIs	https://doi.org/10.1086/324100
State	Published - Dec 2001

Keywords

Circumstellar matter
Novae, cataclysmic variables
Stars: individual (Nova Aquila 1995=V1425 Aquilae)

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10.1086/324100

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Lyke, J. E., Gehrz, R. D., Woodward, C. E., Barlow, M. J., Péquignot, D., Salama, A., Schwarz, G. J., Shore, S. N., Starrfield, S., Evans, A., Gonzales-Riestra, R., Greenhouse, M. A., Hjellming, R. M., Humphreys, R. M., Jones, T. J., Krautter, J., Morisset, C., Ögelman, H. B., Orio, M., ... Williams, R. E. (2001). Infrared space observatory short wavelength spectrometer observations of V1425 aquilae (Nova Aquila 1995). Astronomical Journal, 122(6), 3305-3312. https://doi.org/10.1086/324100

Lyke, JE, Gehrz, RD , Woodward, CE, Barlow, MJ, Péquignot, D, Salama, A, Schwarz, GJ, Shore, SN, Starrfield, S, Evans, A, Gonzales-Riestra, R, Greenhouse, MA, Hjellming, RM, Humphreys, RM, Jones, TJ, Krautter, J, Morisset, C, Ögelman, HB, Orio, M, Wagner, RM, Walton, NA & Williams, RE 2001, 'Infrared space observatory short wavelength spectrometer observations of V1425 aquilae (Nova Aquila 1995)', Astronomical Journal, vol. 122, no. 6, pp. 3305-3312. https://doi.org/10.1086/324100

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title = "Infrared space observatory short wavelength spectrometer observations of V1425 aquilae (Nova Aquila 1995)",

abstract = "We present observations of the classical nova V1425 Aquilae (Nova Aquila 1995) with the Infrared Space Observatory's (ISO) Short Wavelength Spectrometer, the Isaac Newton Telescope's Intermediate Dispersion Spectrograph, and the International Ultraviolet Explorer's Short-Wavelength Primary Spectrograph. Analysis of He II (1640 {\AA}) development constrains the white dwarf turnoff to ∼400 days after outburst. Photoionization modeling of the optical and ISO spectra obtained during the late nebular phase constrains the mass of the ejecta between 2.5-4.2 × 10-5 M⊙. This modeling also suggests C and O in the ejecta were enhanced by a factor of ∼9, and N was enhanced by a factor of ∼ 100 with respect to solar, while Ne was only slightly enhanced. Based upon these analyses, we determine that the white dwarf in the V1425 Aq1 system has a CO composition and is at a distance of 3.0 ± 0.4 kpc.",

keywords = "Circumstellar matter, Novae, cataclysmic variables, Stars: individual (Nova Aquila 1995=V1425 Aquilae)",

author = "Lyke, {J. E.} and Gehrz, {R. D.} and Woodward, {C. E.} and Barlow, {M. J.} and D. P{\'e}quignot and A. Salama and Schwarz, {G. J.} and Shore, {S. N.} and S. Starrfield and A. Evans and R. Gonzales-Riestra and Greenhouse, {M. A.} and Hjellming, {R. M.} and Humphreys, {R. M.} and Jones, {T. J.} and J. Krautter and C. Morisset and {\"O}gelman, {H. B.} and M. Orio and Wagner, {R. M.} and Walton, {N. A.} and Williams, {R. E.}",

year = "2001",

month = dec,

doi = "10.1086/324100",

language = "English (US)",

volume = "122",

pages = "3305--3312",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "6",

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TY - JOUR

T1 - Infrared space observatory short wavelength spectrometer observations of V1425 aquilae (Nova Aquila 1995)

AU - Lyke, J. E.

AU - Gehrz, R. D.

AU - Woodward, C. E.

AU - Barlow, M. J.

AU - Péquignot, D.

AU - Salama, A.

AU - Schwarz, G. J.

AU - Shore, S. N.

AU - Starrfield, S.

AU - Evans, A.

AU - Gonzales-Riestra, R.

AU - Greenhouse, M. A.

AU - Hjellming, R. M.

AU - Humphreys, R. M.

AU - Jones, T. J.

AU - Krautter, J.

AU - Morisset, C.

AU - Ögelman, H. B.

AU - Orio, M.

AU - Wagner, R. M.

AU - Walton, N. A.

AU - Williams, R. E.

PY - 2001/12

Y1 - 2001/12

N2 - We present observations of the classical nova V1425 Aquilae (Nova Aquila 1995) with the Infrared Space Observatory's (ISO) Short Wavelength Spectrometer, the Isaac Newton Telescope's Intermediate Dispersion Spectrograph, and the International Ultraviolet Explorer's Short-Wavelength Primary Spectrograph. Analysis of He II (1640 Å) development constrains the white dwarf turnoff to ∼400 days after outburst. Photoionization modeling of the optical and ISO spectra obtained during the late nebular phase constrains the mass of the ejecta between 2.5-4.2 × 10-5 M⊙. This modeling also suggests C and O in the ejecta were enhanced by a factor of ∼9, and N was enhanced by a factor of ∼ 100 with respect to solar, while Ne was only slightly enhanced. Based upon these analyses, we determine that the white dwarf in the V1425 Aq1 system has a CO composition and is at a distance of 3.0 ± 0.4 kpc.

AB - We present observations of the classical nova V1425 Aquilae (Nova Aquila 1995) with the Infrared Space Observatory's (ISO) Short Wavelength Spectrometer, the Isaac Newton Telescope's Intermediate Dispersion Spectrograph, and the International Ultraviolet Explorer's Short-Wavelength Primary Spectrograph. Analysis of He II (1640 Å) development constrains the white dwarf turnoff to ∼400 days after outburst. Photoionization modeling of the optical and ISO spectra obtained during the late nebular phase constrains the mass of the ejecta between 2.5-4.2 × 10-5 M⊙. This modeling also suggests C and O in the ejecta were enhanced by a factor of ∼9, and N was enhanced by a factor of ∼ 100 with respect to solar, while Ne was only slightly enhanced. Based upon these analyses, we determine that the white dwarf in the V1425 Aq1 system has a CO composition and is at a distance of 3.0 ± 0.4 kpc.

KW - Circumstellar matter

KW - Novae, cataclysmic variables

KW - Stars: individual (Nova Aquila 1995=V1425 Aquilae)

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U2 - 10.1086/324100

DO - 10.1086/324100

M3 - Article

AN - SCOPUS:18044403423

SN - 0004-6256

VL - 122

SP - 3305

EP - 3312

JO - Astronomical Journal

JF - Astronomical Journal

IS - 6

ER -

Infrared space observatory short wavelength spectrometer observations of V1425 aquilae (Nova Aquila 1995)

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