Transiting extrasolar planetary candidates in the Galactic bulge

Kailash C. Sahu (), Stefano Casertano, Howard E. Bond, Jeff Valenti, T. Ed Smith, Dante Minniti, Manuela Zoccali, Mario Livio, Nino Panagia, Nikolai Piskunov, Thomas M. Brown, Timothy Brown, Alvio Renzini, R. Michael Rich, Will Clarkson and Stephen Lubow
Additional contact information
Kailash C. Sahu: Space Telescope Science Institute
Stefano Casertano: Space Telescope Science Institute
Howard E. Bond: Space Telescope Science Institute
Jeff Valenti: Space Telescope Science Institute
T. Ed Smith: Space Telescope Science Institute
Dante Minniti: Universidad Catolica de Chile
Manuela Zoccali: Universidad Catolica de Chile
Mario Livio: Space Telescope Science Institute
Nino Panagia: Space Telescope Science Institute
Nikolai Piskunov: Uppsala University
Thomas M. Brown: Space Telescope Science Institute
Timothy Brown: High Altitude Observatory
Alvio Renzini: INAF–Osservatorio Astronomico di Padova
R. Michael Rich: University of California at Los Angeles
Will Clarkson: Space Telescope Science Institute
Stephen Lubow: Space Telescope Science Institute

Nature, 2006, vol. 443, issue 7111, 534-540

Abstract: Abstract More than 200 extrasolar planets have been discovered around relatively nearby stars, primarily through the Doppler line shifts owing to reflex motions of their host stars, and more recently through transits of some planets across the faces of the host stars. The detection of planets with the shortest known periods, 1.2–2.5 days, has mainly resulted from transit surveys which have generally targeted stars more massive than 0.75 M⊙, where M⊙ is the mass of the Sun. Here we report the results from a planetary transit search performed in a rich stellar field towards the Galactic bulge. We discovered 16 candidates with orbital periods between 0.4 and 4.2 days, five of which orbit stars of masses in the range 0.44–0.75 M⊙. In two cases, radial-velocity measurements support the planetary nature of the companions. Five candidates have orbital periods below 1.0 day, constituting a new class of ultra-short-period planets, which occur only around stars of less than 0.88 M⊙. This indicates that those orbiting very close to more-luminous stars might be evaporatively destroyed or that jovian planets around stars of lower mass might migrate to smaller radii.

Date: 2006
References: Add references at CitEc
Citations:

Downloads: (external link)
https://www.nature.com/articles/nature05158 Abstract (text/html)
Access to the full text of the articles in this series is restricted.

Related works:
This item may be available elsewhere in EconPapers: Search for items with the same title.

Export reference: BibTeX RIS (EndNote, ProCite, RefMan) HTML/Text

Persistent link: https://EconPapers.repec.org/RePEc:nat:nature:v:443:y:2006:i:7111:d:10.1038_nature05158

Ordering information: This journal article can be ordered from
https://www.nature.com/

DOI: 10.1038/nature05158

Access Statistics for this article

Nature is currently edited by Magdalena Skipper

More articles in Nature from Nature
Bibliographic data for series maintained by Sonal Shukla () and Springer Nature Abstracting and Indexing ().