The EXPLORE project.: I.: A deep search for transiting extrasolar planets

Simple item page
dc.contributor.authorMallén-Ornelas, G
dc.contributor.authorSeager, S
dc.contributor.authorYee, HKC
dc.contributor.authorMinniti, D
dc.contributor.authorGladders, MD
dc.contributor.authorMallén-Fullerton, GM
dc.contributor.authorBrown, TM
dc.date.accessioned2025-01-21T01:09:49Z
dc.date.available2025-01-21T01:09:49Z
dc.date.issued2003
dc.description.abstractPlanet transit searches promise to be the next breakthrough for extrasolar planet detection and will bring the characterization of short-period planets into a new era. Every transiting planet discovered will have a measured radius, which will provide constraints on planet composition, evolution, and migration history. Together with radial velocity measurements, the absolute mass of every transiting planet will be determined. In this paper we discuss the design considerations of the Extrasolar Planet Occultation Research (EXPLORE) project, a series of transiting planet searches using 4 m class telescopes to continuously monitor a single field of stars in the Galactic plane in each similar to2 week observing campaign. We discuss the general factors that determine the efficiency and the number of planets found by a transit search, including time sampling strategy and field selection. The primary goal is to select the most promising planet candidates for radial velocity follow-up observations. We show that with very high photometric precision light curves that have frequent time sampling and at least two detected transits, it is possible to uniquely solve for the main parameters of the eclipsing system (including planet radius), based on several important assumptions about the central star. Together with a measured spectral type for the star, this unique solution for orbital parameters provides a powerful method for ruling out most contaminants to transiting planet candidates. For the EXPLORE project, radial velocity follow-up observations for companion mass determination of the best candidates are done on 8 m class telescopes within 2 or 3 months of the photometric campaigns. This same-season follow-up is made possible by the use of efficient pipelines to produce high-quality light curves within weeks of the observations. We conclude by presenting early results from our first search, EXPLORE I, in which we reached better than 1% rms photometric precision (measured over a full night) on similar to37,000 stars with 14.5less than or equal toIless than or equal to18.2.
dc.fuente.origenWOS
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/96624
dc.identifier.wosidWOS:000180282700046
dc.issue.numero2
dc.language.isoen
dc.pagina.final1140
dc.pagina.inicio1123
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.subjectplanetary systems
dc.subjectsurveys
dc.subjecttechniques : photometric
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titleThe EXPLORE project.: I.: A deep search for transiting extrasolar planets
dc.typeartículo
dc.volumen582
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
Files
Collections
Artículos de revistas