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Mon-735: a new low-mass pre-main-sequence eclipsing binary in NGC 2264

Gillen, Edward and Hillenbrand, Lynne A. and Stauffer, John and Aigrain, Suzanne and Rebull, Luisa and Cody, Ann Marie (2020) Mon-735: a new low-mass pre-main-sequence eclipsing binary in NGC 2264. Monthly Notices of the Royal Astronomical Society, 495 (2). pp. 1531-1548. ISSN 0035-8711. doi:10.1093/mnras/staa1016.

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We present Mon-735, a detached double-lined eclipsing binary (EB) member of the ∼3 Myr old NGC 2264 star-forming region, detected by Spitzer. We simultaneously model the Spitzer light curves, follow-up Keck/HIRES radial velocities, and the system’s spectral energy distribution to determine self-consistent masses, radii, and effective temperatures for both stars. We find that Mon-735 comprises two pre-main-sequence M dwarfs with component masses of M = 0.2918 ± 0.0099 and 0.2661 ± 0.0095 M_⊙, radii of R = 0.762 ± 0.022 and 0.748 ± 0.023 R_⊙, and effective temperatures of T_(eff) = 3260 ± 73 and 3213 ± 73 K. The two stars travel on circular orbits around their common centre of mass in P = 1.9751388 ± 0.0000050 d. We compare our results for Mon-735, along with another EB in NGC 2264 (CoRoT 223992193), to the predictions of five stellar evolution models. These suggest that the lower mass EB system Mon-735 is older than CoRoT 223992193 in the mass–radius diagram (MRD) and, to a lesser extent, in the Hertzsprung–Russell diagram (HRD). The MRD ages of Mon-735 and CoRoT 223992193 are ∼7–9 and 4–6 Myr, respectively, with the two components in each EB system possessing consistent ages.

Item Type:Article
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URLURL TypeDescription Paper
Gillen, Edward0000-0003-2851-3070
Stauffer, John0000-0003-3595-7382
Aigrain, Suzanne0000-0003-1453-0574
Rebull, Luisa0000-0001-6381-515X
Cody, Ann Marie0000-0002-3656-6706
Additional Information:© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model ( Accepted 2020 April 3. Received 2020 March 31; in original form 2019 August 14. The authors thank Hannu Parviainen, Trevor David, Grant Kennedy, and Didier Queloz for helpful discussions, and the anonymous referee for insightful reading of the manuscript and helpful suggestions for improvement. EG gratefully acknowledges support from the David and Claudia Harding Foundation in the form of a Winton Exoplanet Fellowship. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France (DOI: 10.26093/cds/vizier). The original description of the VizieR service was published in A&AS, 143, 23 (Ochsenbein, Bauer & Marcout 2000). This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France (Wenger et al. 2000). This research has made use of the SVO Filter Profile Service (FPS; supported from the Spanish MINECO through grant AYA2017-84089, and described in Rodrigo, Solano & Bayo (2012). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work has made use of data from the European Space Agency (ESA) mission Gaia (, processed by the Gaia Data Processing and Analysis Consortium (DPAC, Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.
Group:Infrared Processing and Analysis Center (IPAC), Astronomy Department
Funding AgencyGrant Number
David and Claudia Harding FoundationUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Ministerio de Economía y Competitividad (MINECO)AYA2017-84089
Gaia Multilateral AgreementUNSPECIFIED
University of MarylandUNSPECIFIED
Eotvos Lorand University (ELTE)UNSPECIFIED
Los Alamos National LaboratoryUNSPECIFIED
Gordon and Betty Moore FoundationUNSPECIFIED
Subject Keywords:binaries: eclipsing, binaries: spectroscopic, stars: fundamental parameters, stars: low-mass, stars: pre-main-sequence, open clusters and associations: individual: NGC 2264
Issue or Number:2
Record Number:CaltechAUTHORS:20200622-104137831
Persistent URL:
Official Citation:Edward Gillen, Lynne A Hillenbrand, John Stauffer, Suzanne Aigrain, Luisa Rebull, Ann Marie Cody, Mon-735: a new low-mass pre-main-sequence eclipsing binary in NGC 2264, Monthly Notices of the Royal Astronomical Society, Volume 495, Issue 2, June 2020, Pages 1531–1548,
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:103955
Deposited By: George Porter
Deposited On:23 Jun 2020 19:21
Last Modified:16 Nov 2021 18:26

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