The Monitor project: JW 380 – a 0.26-, 0.15-M⊙, pre-main-sequence eclipsing binary in the Orion nebula cluster

We report the discovery of a low-mass (0.26 ± 0.02, 0.15 ± 0.01 M⊙) pre-main-sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW 380 was detected as part of a high-cadence time-resolved photometric survey (the Monitor project) using the 2.5-m Isaac Newton Telescope and Wide Field Ca...

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Published in	Monthly notices of the Royal Astronomical Society Vol. 380; no. 2; pp. 541 - 550
Main Authors	Irwin, Jonathan, Aigrain, Suzanne, Hodgkin, Simon, Stassun, Keivan G., Hebb, Leslie, Irwin, Mike, Moraux, Estelle, Bouvier, Jerome, Alapini, Aude, Alexander, Richard, Bramich, D. M., Holtzman, Jon, Martín, Eduardo L., McCaughrean, Mark J., Pont, Frédéric, Verrier, P. E., Zapatero Osorio, María Rosa
Format	Journal Article
Language	English
Published	Oxford, UK Blackwell Publishing Ltd 11.09.2007 Oxford University Press
Subjects	Astronomy Astrophysics binaries: eclipsing Double stars Nebulae open clusters and associations: individual: Orion nebula cluster Stars & galaxies stars: individual: JW 380 stars: pre-main-sequence surveys surveys binaries: eclipsing stars: pre-main-sequence stars: individual: JW 380 open clusters and associations: individual: Orion nebula cluster
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Abstract	We report the discovery of a low-mass (0.26 ± 0.02, 0.15 ± 0.01 M⊙) pre-main-sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW 380 was detected as part of a high-cadence time-resolved photometric survey (the Monitor project) using the 2.5-m Isaac Newton Telescope and Wide Field Camera for a survey of a single field in the Orion nebula cluster (ONC) region in V and i bands. The star is assigned a 99 per cent membership probability from proper motion measurements, and radial velocity observations indicate a systemic velocity within 1σ of that of the ONC. Modelling of the combined light and radial velocity curves of the system gave stellar radii of for the primary and the secondary, with a significant third light contribution which is also visible as a third peak in the cross-correlation functions used to derive radial velocities. The masses and radii appear to be consistent with stellar models for 2–3 Myr age from several authors, within the present observational errors. These observations probe an important region of mass–radius parameter space, where there are currently only a handful of known PMS EB systems with precise measurements available in the literature.
AbstractList	We report the discovery of a low-mass (0.26 ± 0.02, 0.15 ± 0.01 M⊙) pre-main-sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW 380 was detected as part of a high-cadence time-resolved photometric survey (the Monitor project) using the 2.5-m Isaac Newton Telescope and Wide Field Camera for a survey of a single field in the Orion nebula cluster (ONC) region in V and i bands. The star is assigned a 99 per cent membership probability from proper motion measurements, and radial velocity observations indicate a systemic velocity within 1σ of that of the ONC. Modelling of the combined light and radial velocity curves of the system gave stellar radii of for the primary and the secondary, with a significant third light contribution which is also visible as a third peak in the cross-correlation functions used to derive radial velocities. The masses and radii appear to be consistent with stellar models for 2–3 Myr age from several authors, within the present observational errors. These observations probe an important region of mass–radius parameter space, where there are currently only a handful of known PMS EB systems with precise measurements available in the literature. ABSTRACT We report the discovery of a low‐mass (0.26 ± 0.02, 0.15 ± 0.01 M⊙) pre‐main‐sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW 380 was detected as part of a high‐cadence time‐resolved photometric survey (the Monitor project) using the 2.5‐m Isaac Newton Telescope and Wide Field Camera for a survey of a single field in the Orion nebula cluster (ONC) region in V and i bands. The star is assigned a 99 per cent membership probability from proper motion measurements, and radial velocity observations indicate a systemic velocity within 1σ of that of the ONC. Modelling of the combined light and radial velocity curves of the system gave stellar radii of 1.19+0.04−0.18 and 0.90+0.17−0.03 R⊙ for the primary and the secondary, with a significant third light contribution which is also visible as a third peak in the cross‐correlation functions used to derive radial velocities. The masses and radii appear to be consistent with stellar models for 2–3 Myr age from several authors, within the present observational errors. These observations probe an important region of mass–radius parameter space, where there are currently only a handful of known PMS EB systems with precise measurements available in the literature. We report the discovery of a low-mass (0.26 +/- 0.02, 0.15 +/- 0.01 Magnitude) pre-main-sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW 380 was detected as part of a high-cadence time-resolved photometric survey (the Monitor project) using the 2.5-m Isaac Newton Telescope and Wide Field Camera for a survey of a single field in the Orion nebula cluster (ONC) region in V and i bands. The star is assigned a 99 per cent membership probability from proper motion measurements, and radial velocity observations indicate a systemic velocity within 1Sigma of that of the ONC. Modelling of the combined light and radial velocity curves of the system gave stellar radii of 1.19+0.04-0.18 and 0.90+0.17-0.03 R[middot in circle] for the primary and the secondary, with a significant third light contribution which is also visible as a third peak in the cross-correlation functions used to derive radial velocities. The masses and radii appear to be consistent with stellar models for 2-3 Myr age from several authors, within the present observational errors. These observations probe an important region of mass-radius parameter space, where there are currently only a handful of known PMS EB systems with precise measurements available in the literature. [PUBLICATION ABSTRACT] We report the discovery of a low-mass (0.26 ± 0.02, 0.15 ± 0.01 M⊙) pre-main-sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW 380 was detected as part of a high-cadence time-resolved photometric survey (the Monitor project) using the 2.5-m Isaac Newton Telescope and Wide Field Camera for a survey of a single field in the Orion nebula cluster (ONC) region in V and i bands. The star is assigned a 99 per cent membership probability from proper motion measurements, and radial velocity observations indicate a systemic velocity within 1σ of that of the ONC. Modelling of the combined light and radial velocity curves of the system gave stellar radii of for the primary and the secondary, with a significant third light contribution which is also visible as a third peak in the cross-correlation functions used to derive radial velocities. The masses and radii appear to be consistent with stellar models for 2-3 Myr age from several authors, within the present observational errors. These observations probe an important region of mass-radius parameter space, where there are currently only a handful of known PMS EB systems with precise measurements available in the literature.
Author	Stassun, Keivan G. Alexander, Richard Pont, Frédéric Zapatero Osorio, María Rosa Verrier, P. E. Bouvier, Jerome Alapini, Aude Holtzman, Jon Hebb, Leslie Hodgkin, Simon Moraux, Estelle McCaughrean, Mark J. Aigrain, Suzanne Irwin, Jonathan Bramich, D. M. Martín, Eduardo L. Irwin, Mike
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Keywords	surveys binaries: eclipsing stars: pre-main-sequence stars: individual: JW 380 open clusters and associations: individual: Orion nebula cluster
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Snippet	We report the discovery of a low-mass (0.26 ± 0.02, 0.15 ± 0.01 M⊙) pre-main-sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW 380 was... ABSTRACT We report the discovery of a low‐mass (0.26 ± 0.02, 0.15 ± 0.01 M⊙) pre‐main‐sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW 380... We report the discovery of a low-mass (0.26 +/- 0.02, 0.15 +/- 0.01 Magnitude) pre-main-sequence (PMS) eclipsing binary (EB) with a 5.3 d orbital period. JW...
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SubjectTerms	Astronomy Astrophysics binaries: eclipsing Double stars Nebulae open clusters and associations: individual: Orion nebula cluster Stars & galaxies stars: individual: JW 380 stars: pre-main-sequence surveys
Title	The Monitor project: JW 380 – a 0.26-, 0.15-M⊙, pre-main-sequence eclipsing binary in the Orion nebula cluster
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