Статья

YSOVAR: THE FIRST SENSITIVE, WIDE-AREA, MID-INFRARED PHOTOMETRIC MONITORING OF THE ORION NEBULA CLUSTER

M. Morales‐CalderónSpitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA; [email protected]J. R. StaufferSpitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA; [email protected]Lynne A. HillenbrandAstronomy Department, California Institute of Technology, Pasadena, CA 91125, USARobert GutermuthDepartment of Astronomy, University of Massachusetts, Amherst, MA 01003, USAInseok SongDepartment of Physics and Astronomy, University of Georgia, Athens, GA 30602, USAL. M. RebullSpitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA; [email protected]Peter PlavchanNASA Exoplanet Science Institute, California Institute of Technology, Pasadena, CA 91125, USAJohn M. CarpenterAstronomy Department, California Institute of Technology, Pasadena, CA 91125, USAB. A. WhitneySpace Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USAKevin R. CoveyDepartment of Astronomy, Boston University, Boston, MA 02215, USACatarina Alves de OliveiraLaboratoire d’Astrophysique de Grenoble, Observatoire de Grenoble, 38041 Grenoble Cedex 9, FranceElaine WinstonAstrophysics Group, College of Engineering, Mathematics, and Physical Sciences, University of Exeter, UKM. J. McCaughreanAstrophysics Group, College of Engineering, Mathematics, and Physical Sciences, University of Exeter, UKJ. BouvierUJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, F-38041, FranceSylvain GuieuEuropean Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, ChileF. J. VrbaU.S. Naval Observatory, Flagstaff Station, 10391 W. Naval Observatory Road, Flagstaff, AZ 86001-8521, USAJon A. HoltzmanNew Mexico State University, Box 30001/MSC 4500, Las Cruces, NM 88003, USAFranck MarchisDepartment of Astronomy, UC Berkeley, 601 Campbell Hall, Berkeley, CA 94720, USAJoseph L. HoraHarvard-Smithsonian Center of Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAL. H. WassermanLowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USAS. TerebeyDepartment of Physics and Astronomy, California State University at Los Angeles, Los Angeles, CA 90032, USAS. T. MegeathDepartment of Physics and Astronomy, The University of Toledo, 2801 West Bancroft Street, Toledo, OH 43606, USAE. F. GuinanDepartment of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085, USAJan ForbrichHarvard-Smithsonian Center of Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAN. HuélamoCentro de Astrobiología (INTA-CSIC), LAEFF, P.O. Box 78, E-28691 Villanueva de la Canada, SpainP. Riviére-MarichalarCentro de Astrobiología (INTA-CSIC), LAEFF, P.O. Box 78, E-28691 Villanueva de la Canada, SpainD. BarradoCalar Alto Observatory, Centro Astronómico Hispano Alemán, Almería, SpainKarl R. StapelfeldtJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USAJesús HernándezL. E. AllenNational Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USAD. R. ArdilaNASA Herschel Science Center, California Institute of Technology, Pasadena, CA 91125, USAA. BayoEuropean Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, ChileF. FavataEuropean Space Agency, Research & Scientific Support Department, ESTEC, Noordwijk, The NetherlandsD. J. JamesCerro Tololo Inter-American Observatory, Casilla 603, La Serena, ChileM. W. WernerJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USAKenneth WoodSchool of Physics & Astronomy, University of St Andrews, North Haugh, St Andrews, Fife, KY16 9AD, UK

2011en

ABI

Аннотация

We present initial results from time-series imaging at infrared wavelengths of 0.9 deg^2 in the Orion Nebula Cluster (ONC). During Fall 2009 we obtained 81 epochs of Spitzer 3.6 and 4.5 μm data over 40 consecutive days. We extracted light curves with ~3% photometric accuracy for ~2000 ONC members ranging from several solar masses down to well below the hydrogen-burning mass limit. For many of the stars, we also have time-series photometry obtained at optical (I_c) and/or near-infrared (JK_s ) wavelengths. Our data set can be mined to determine stellar rotation periods, identify new pre-main-sequence eclipsing binaries, search for new substellar Orion members, and help better determine the frequency of circumstellar disks as a function of stellar mass in the ONC. Our primary focus is the unique ability of 3.6 and 4.5 μm variability information to improve our understanding of inner disk processes and structure in the Class I and II young stellar objects (YSOs). In this paper, we provide a brief overview of the YSOVAR Orion data obtained in Fall 2009 and highlight our light curves for AA-Tau analogs—YSOs with narrow dips in flux, most probably due to disk density structures passing through our line of sight. Detailed follow-up observations are needed in order to better quantify the nature of the obscuring bodies and what this implies for the structure of the inner disks of YSOs.

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Идентификаторы

DOI: 10.1088/0004-637x/733/1/50

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Цитирований: 3Использованных источников: 0

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