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A cautionary tale : marvels brown dwarf candidate reveals itself to be a very long period, highly eccentric spectroscopic stellar binary
dc.contributor.author | Mack, C. E. | pt_BR |
dc.contributor.author | Ge, Jian | pt_BR |
dc.contributor.author | Deshpande, Rohit | pt_BR |
dc.contributor.author | Wisniewski, J.P. | pt_BR |
dc.contributor.author | Stassun, Keivan G. | pt_BR |
dc.contributor.author | Gaudi, B. S. | pt_BR |
dc.contributor.author | Fleming, S.W. | pt_BR |
dc.contributor.author | Mahadevan, Suvrath | pt_BR |
dc.contributor.author | De Lee, Nathan M. | pt_BR |
dc.contributor.author | Eastman, Jason | pt_BR |
dc.contributor.author | Ghezzi, Luan | pt_BR |
dc.contributor.author | González Hernández, Jonay I. | pt_BR |
dc.contributor.author | Femenía Castellá, B. | pt_BR |
dc.contributor.author | Ferreira, Letícia D. | pt_BR |
dc.contributor.author | Mello, Gustavo Frederico Porto de | pt_BR |
dc.contributor.author | Crepp, Justin R. | pt_BR |
dc.contributor.author | Mata Sánchez, Daniel | pt_BR |
dc.contributor.author | Agol, Eric | pt_BR |
dc.contributor.author | Beatty, Thomas G. | pt_BR |
dc.contributor.author | Bizyaev, D. | pt_BR |
dc.contributor.author | Brewington, Howard J. | pt_BR |
dc.contributor.author | Cargile, Phillip A. | pt_BR |
dc.contributor.author | Costa, Luiz N. da | pt_BR |
dc.contributor.author | Esposito, Massimiliano | pt_BR |
dc.contributor.author | Ebelke, Garrett L. | pt_BR |
dc.contributor.author | Hebb, Leslie | pt_BR |
dc.contributor.author | Jiang, Peng | pt_BR |
dc.contributor.author | Kane, Stephen R. | pt_BR |
dc.contributor.author | Lee, Brian L. | pt_BR |
dc.contributor.author | Maia, Marcio Antonio Geimba | pt_BR |
dc.contributor.author | Malanushenko, E. | pt_BR |
dc.contributor.author | Malanushenko, V. | pt_BR |
dc.contributor.author | Oravetz, Daniel J. | pt_BR |
dc.contributor.author | Paegert, Martin | pt_BR |
dc.contributor.author | Pan, K. | pt_BR |
dc.contributor.author | Allende Prieto, Carlos | pt_BR |
dc.contributor.author | Pepper, J. | pt_BR |
dc.contributor.author | Rebolo, Rafael | pt_BR |
dc.contributor.author | Roy, Arpita | pt_BR |
dc.contributor.author | Santiago, Basilio Xavier | pt_BR |
dc.contributor.author | Schneider, D.P. | pt_BR |
dc.contributor.author | Simmons, Audrey E. | pt_BR |
dc.contributor.author | Siverd, Robert J. | pt_BR |
dc.contributor.author | Snedden, S.A. | pt_BR |
dc.contributor.author | Tofflemire, Benjamin M. | pt_BR |
dc.date.accessioned | 2014-12-12T02:15:55Z | pt_BR |
dc.date.issued | 2013 | pt_BR |
dc.identifier.issn | 0004-6256 | pt_BR |
dc.identifier.uri | http://hdl.handle.net/10183/108159 | pt_BR |
dc.description.abstract | We report the discovery of a highly eccentric, double-lined spectroscopic binary star system (TYC 3010-1494-1), comprising two solar-type stars that we had initially identified as a single star with a brown dwarf companion. At the moderate resolving power of the MARVELS spectrograph and the spectrographs used for subsequent radialvelocity (RV) measurements (R 30,000), this particular stellar binary mimics a single-lined binary with an RV signal that would be induced by a brown dwarf companion (M sin i ∼ 50MJup) to a solar-type primary. At least three properties of this system allow it to masquerade as a single star with a very-low-mass companion: its large eccentricity (e ∼ 0.8), its relatively long period (P ∼ 238 days), and the approximately perpendicular orientation of the semi-major axis with respect to the line of sight (ω ∼ 189◦). As a result of these properties, for ∼95% of the orbit the two sets of stellar spectral lines are completely blended, and the RV measurements based on centroiding on the apparently single-lined spectrum is very well fit by an orbit solution indicative of a brown dwarf companion on a more circular orbit (e ∼ 0.3). Only during the ∼5% of the orbit near periastron passage does the true, double-lined nature and large RV amplitude of ∼15 km s−1 reveal itself. The discovery of this binary system is an important lesson for RV surveys searching for substellar companions; at a given resolution and observing cadence, a survey will be susceptible to these kinds of astrophysical false positives for a range of orbital parameters. Finally, for surveys like MARVELS that lack the resolution for a useful line bisector analysis, it is imperative to monitor the peak of the cross-correlation function for suspicious changes in width or shape, so that such false positives can be flagged during the candidate vetting process. | en |
dc.format.mimetype | application/pdf | pt_BR |
dc.language.iso | eng | pt_BR |
dc.relation.ispartof | The Astronomical journal. Vol. 145, no. 5 (May 2013), 139, 15 p. | pt_BR |
dc.rights | Open Access | en |
dc.subject | Binaries: spectroscopic | en |
dc.subject | Estrelas binarias | pt_BR |
dc.subject | Anãs marrons | pt_BR |
dc.subject | Brown dwarfs | en |
dc.subject | Stars: individual (TYC 3010-1494-1) | en |
dc.title | A cautionary tale : marvels brown dwarf candidate reveals itself to be a very long period, highly eccentric spectroscopic stellar binary | pt_BR |
dc.type | Artigo de periódico | pt_BR |
dc.identifier.nrb | 000900798 | pt_BR |
dc.type.origin | Estrangeiro | pt_BR |
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