A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST

We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with P obs = 2.77 days containing a possible massive white dwarf (WD) or a neutron star (NS) using LAMOST spectroscopic data. By a joint fitting of the radial velocity from LAMOST and the light curve from TESS, we de...

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Published inThe Astrophysical journal Vol. 977; no. 2; pp. 245 - 256
Main Authors Zhao, Xinlin, Wang, Song, Wang, Pengfei, Zheng, Chuanjie, Yuan, Haibo, Liu, Jifeng
Format Journal Article
LanguageEnglish
Published Philadelphia The American Astronomical Society 01.12.2024
IOP Publishing
Subjects
Binary stars
Curve fitting
Light curve
Neutron stars
Neutrons
Radial velocity
Radio signals
Stars
Supernova
White dwarf stars
X ray binaries
X ray stars
X-ray astronomy
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Abstract We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with P obs = 2.77 days containing a possible massive white dwarf (WD) or a neutron star (NS) using LAMOST spectroscopic data. By a joint fitting of the radial velocity from LAMOST and the light curve from TESS, we derived a circular Keplerian orbit with an inclination of i = 81.°31 − 7.85 ° + 6.26 ° , which is consistent with that derived from v sin i . Together with the mass of the visible star, we derived the mass of the invisible object to be 1.34 − 0.40 + 0.35 M ⊙ . Spectral disentangling with the LAMOST medium-resolution spectra shows no absorption feature from an additional component, suggesting the presence of a compact object. No X-ray or radio pulsed signal is detected from ROSAT and FAST archive observations. J0606+2132 could evolve into either a Type Ia supernova or an NS through accretion-induced collapse if it is a WD or into an intermediate-mass X-ray binary if it is an NS.
AbstractList We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with P _obs = 2.77 days containing a possible massive white dwarf (WD) or a neutron star (NS) using LAMOST spectroscopic data. By a joint fitting of the radial velocity from LAMOST and the light curve from TESS, we derived a circular Keplerian orbit with an inclination of i = 81.°31 _{-7.85^\circ }^{+6.26^\circ }$ , which is consistent with that derived from $v\,\sin \,i$ . Together with the mass of the visible star, we derived the mass of the invisible object to be ${1.34}_{-0.40}^{+0.35}{M}_{\odot }$ . Spectral disentangling with the LAMOST medium-resolution spectra shows no absorption feature from an additional component, suggesting the presence of a compact object. No X-ray or radio pulsed signal is detected from ROSAT and FAST archive observations. J0606+2132 could evolve into either a Type Ia supernova or an NS through accretion-induced collapse if it is a WD or into an intermediate-mass X-ray binary if it is an NS.
We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with P obs = 2.77 days containing a possible massive white dwarf (WD) or a neutron star (NS) using LAMOST spectroscopic data. By a joint fitting of the radial velocity from LAMOST and the light curve from TESS, we derived a circular Keplerian orbit with an inclination of i = 81.°31 − 7.85 ° + 6.26 ° , which is consistent with that derived from v sin i . Together with the mass of the visible star, we derived the mass of the invisible object to be 1.34 − 0.40 + 0.35 M ⊙ . Spectral disentangling with the LAMOST medium-resolution spectra shows no absorption feature from an additional component, suggesting the presence of a compact object. No X-ray or radio pulsed signal is detected from ROSAT and FAST archive observations. J0606+2132 could evolve into either a Type Ia supernova or an NS through accretion-induced collapse if it is a WD or into an intermediate-mass X-ray binary if it is an NS.
We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with Pobs = 2.77 days containing a possible massive white dwarf (WD) or a neutron star (NS) using LAMOST spectroscopic data. By a joint fitting of the radial velocity from LAMOST and the light curve from TESS, we derived a circular Keplerian orbit with an inclination of i = 81.°31−7.85°+6.26°, which is consistent with that derived from vsini. Together with the mass of the visible star, we derived the mass of the invisible object to be 1.34−0.40+0.35M⊙. Spectral disentangling with the LAMOST medium-resolution spectra shows no absorption feature from an additional component, suggesting the presence of a compact object. No X-ray or radio pulsed signal is detected from ROSAT and FAST archive observations. J0606+2132 could evolve into either a Type Ia supernova or an NS through accretion-induced collapse if it is a WD or into an intermediate-mass X-ray binary if it is an NS.
Author Zheng, Chuanjie
Zhao, Xinlin
Wang, Song
Yuan, Haibo
Wang, Pengfei
Liu, Jifeng
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Snippet We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with P obs = 2.77 days containing a possible massive white dwarf (WD) or a...
We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with Pobs = 2.77 days containing a possible massive white dwarf (WD) or a...
We report the discovery of a close binary J0606+2132 (Gaia DR3 3423365496448406272) with P _obs = 2.77 days containing a possible massive white dwarf (WD) or a...
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StartPage 245
SubjectTerms Binary stars
Curve fitting
Light curve
Neutron stars
Neutrons
Radial velocity
Radio signals
Stars
Supernova
White dwarf stars
X ray binaries
X ray stars
X-ray astronomy
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Title A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST
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