CXOGBS J174444.7-260330: a new long orbital period cataclysmic variable in a low state

E. M. Ratti; T. F.J. van Grunsven; P. G. Jonker; C. T. Britt; R. I. Hynes; D. Steeghs; S. Greiss; M. A.P. Torres; Thomas Maccarone; Six Other Authors

CXOGBS J174444.7-260330: a new long orbital period cataclysmic variable in a low state

E. M. Ratti, T. F.J. van Grunsven, P. G. Jonker, C. T. Britt, R. I. Hynes, D. Steeghs, S. Greiss, M. A.P. Torres, Thomas Maccarone, Six Other Authors

Physics

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Abstract

We present phase-resolved spectroscopy and photometry of a source discovered with the Chandra Galactic Bulge Survey (GBS), CXOGBS J174444.7-260330 (aka CX93 and CX153 in the previously published GBS list). We find two possible values for the orbital period P, differing from each other by ˜13 s. The most likely solution is P = 5.690 14(6) h. The optical lightcurves show ellipsoidal modulations, whose modelling provides an inclination of 32±1° for the most likely P. The spectra are dominated by a K5 V companion star (the disc veiling is ≲5 per cent). Broad and structured emission from the Balmer lines is also detected, as well as fainter emission from He i. From the absorption lines we measure K2 = 117 ± 8 km s- 1 and v sin i = 69 ± 7 km s- 1. By solving the system mass function we find M1 = 0.8 ± 0.2 M⊙ for the favoured P and i, consistent with a white dwarf accretor, and M2 = 0.6 ± 0.2 M⊙. We estimate a distance in the range 400-700 pc. Although in a low accretion state, both spectros

Original language	English
Pages (from-to)	3543
Journal	Monthly Notices of the Royal Astronomical Society
State	Published - Feb 2013

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@article{bf68c8dfba6744af8b3e97791eb15f21,

title = "CXOGBS J174444.7-260330: a new long orbital period cataclysmic variable in a low state",

abstract = "We present phase-resolved spectroscopy and photometry of a source discovered with the Chandra Galactic Bulge Survey (GBS), CXOGBS J174444.7-260330 (aka CX93 and CX153 in the previously published GBS list). We find two possible values for the orbital period P, differing from each other by ˜13 s. The most likely solution is P = 5.690 14(6) h. The optical lightcurves show ellipsoidal modulations, whose modelling provides an inclination of 32±1° for the most likely P. The spectra are dominated by a K5 V companion star (the disc veiling is ≲5 per cent). Broad and structured emission from the Balmer lines is also detected, as well as fainter emission from He i. From the absorption lines we measure K2 = 117 ± 8 km s- 1 and v sin i = 69 ± 7 km s- 1. By solving the system mass function we find M1 = 0.8 ± 0.2 M⊙ for the favoured P and i, consistent with a white dwarf accretor, and M2 = 0.6 ± 0.2 M⊙. We estimate a distance in the range 400-700 pc. Although in a low accretion state, both spectros",

author = "Ratti, {E. M.} and Grunsven, {T. F.J. van} and Jonker, {P. G.} and Britt, {C. T.} and Hynes, {R. I.} and D. Steeghs and S. Greiss and Torres, {M. A.P.} and Thomas Maccarone and Authors, {Six Other}",

year = "2013",

month = feb,

language = "English",

pages = "3543",

journal = "Monthly Notices of the Royal Astronomical Society",

}

TY - JOUR

T1 - CXOGBS J174444.7-260330: a new long orbital period cataclysmic variable in a low state

AU - Ratti, E. M.

AU - Grunsven, T. F.J. van

AU - Jonker, P. G.

AU - Britt, C. T.

AU - Hynes, R. I.

AU - Steeghs, D.

AU - Greiss, S.

AU - Torres, M. A.P.

AU - Maccarone, Thomas

AU - Authors, Six Other

PY - 2013/2

Y1 - 2013/2

N2 - We present phase-resolved spectroscopy and photometry of a source discovered with the Chandra Galactic Bulge Survey (GBS), CXOGBS J174444.7-260330 (aka CX93 and CX153 in the previously published GBS list). We find two possible values for the orbital period P, differing from each other by ˜13 s. The most likely solution is P = 5.690 14(6) h. The optical lightcurves show ellipsoidal modulations, whose modelling provides an inclination of 32±1° for the most likely P. The spectra are dominated by a K5 V companion star (the disc veiling is ≲5 per cent). Broad and structured emission from the Balmer lines is also detected, as well as fainter emission from He i. From the absorption lines we measure K2 = 117 ± 8 km s- 1 and v sin i = 69 ± 7 km s- 1. By solving the system mass function we find M1 = 0.8 ± 0.2 M⊙ for the favoured P and i, consistent with a white dwarf accretor, and M2 = 0.6 ± 0.2 M⊙. We estimate a distance in the range 400-700 pc. Although in a low accretion state, both spectros

AB - We present phase-resolved spectroscopy and photometry of a source discovered with the Chandra Galactic Bulge Survey (GBS), CXOGBS J174444.7-260330 (aka CX93 and CX153 in the previously published GBS list). We find two possible values for the orbital period P, differing from each other by ˜13 s. The most likely solution is P = 5.690 14(6) h. The optical lightcurves show ellipsoidal modulations, whose modelling provides an inclination of 32±1° for the most likely P. The spectra are dominated by a K5 V companion star (the disc veiling is ≲5 per cent). Broad and structured emission from the Balmer lines is also detected, as well as fainter emission from He i. From the absorption lines we measure K2 = 117 ± 8 km s- 1 and v sin i = 69 ± 7 km s- 1. By solving the system mass function we find M1 = 0.8 ± 0.2 M⊙ for the favoured P and i, consistent with a white dwarf accretor, and M2 = 0.6 ± 0.2 M⊙. We estimate a distance in the range 400-700 pc. Although in a low accretion state, both spectros

M3 - Article

SP - 3543

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

ER -

CXOGBS J174444.7-260330: a new long orbital period cataclysmic variable in a low state

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