Volume 507, Number 1, November III 2009
|Page(s)||481 - 486|
|Section||Planets and planetary systems|
|Published online||27 August 2009|
I. GJ 436b and XO-1b
P. Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile e-mail: firstname.lastname@example.org
2 European Southern Observatory, Av. Alonso de Cordova 3107, Santiago 19001, Chile
3 Specola Vaticana, V00120 Vatican City State, Italy
4 Departamento of Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
Accepted: 5 May 2009
Currently the only technique sensitive to Earth mass planets around nearby stars (that are too close for microlensing) is the monitoring of the transit time variations. We search for additional planets in the systems of the hot Neptune GJ 436b, and the hot-Jupiter XO-1b, using high cadence observations in the J and KS bands. New high-precision transit timing measurements are reported: GJ 436b TC = 2 454 238.47898 ± 0.00046 HJD; XO-1b TC(A) = 2 454 218.83331 ± 0.00114 HJD, TC(B) = 2 454 222.77539 ± 0.00036 HJD, TC(C) = 2 454 222.77597 ± 0.00039 HJD, TC(D) = 2 454 226.71769 ± 0.00034 HJD, and they were used to derive new ephemeris values. We also determined depths for these transits. No statistically significant timing deviations were detected. We demonstrate that the high cadence, ground based near-infrared observations are successful in constraining the mean transit time to ~30 s, and are a viable alternative to space missions.
Key words: stars: planetary systems / stars: individual: GJ 436 / methods: observational / stars: individual: XO-1b
© ESO, 2009
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.