596 citations · 6.7k across the 101 of their papers we have counts for
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Spitzer spectroscopy of carbon stars in the Small Magellanic Cloud
Eric Lagadec, Albert A. Zijlstra, G. C. Sloan +12
We present Spitzer Space telescope spectroscopic observations of 14 carbon-rich AGB stars in the Small Magellanic Cloud. SiC dust is seen in most of the carbon-rich stars but it is…
OGLE 2004-BLG-254: a K3 III Galactic Bulge Giant spatially resolved by a single microlens
A. Cassan, J. -P. Beaulieu, P. Fouque +37
We present an analysis of OGLE 2004-BLG-254, a high-magnification and relatively short duration microlensing event in which the source star, a Bulge K3-giant, has been spatially re…
The period-luminosity relation for type II Cepheids in globular clusters
Noriyuki Matsunaga, Hinako Fukushi, Yoshikazu Nakada +11
We report the result of our near-infrared observations (JHKs) for type II Cepheids (including possible RV Tau stars) in galactic globular clusters. We detected variations of 46 var…
Spitzer observations of acetylene bands in carbon-rich AGB stars in the Large Magellanic Cloud
M. Matsuura, P. R. Wood, G. C. Sloan +13
We investigate the molecular bands in carbon-rich AGB stars in the Large Magellanic Cloud (LMC), using the InfraRed Spectrograph (IRS) on board the Spitzer Space Telescope (SST) ov…
Carbon-Rich Mira Variables: Kinematics and Absolute Magnitudes
Michael W. Feast, Patricia A. Whitelock, John W. Menzies
The kinematics of galactic C-Miras are discussed on the basis of the bolometric magnitudes and radial velocities of Papers I and II of this series. Differential galactic rotation i…
Carbon-Rich Mira Variables: Radial Velocities and Distances
John W. Menzies, Michael W. Feast, Patricia A. Whitelock
Optical radial velocities have been measured for 38 C-type Mira variables. These data together with others in the literature are used to study the differences between optical and C…
Discovery of a Cool Planet of 5.5 Earth Masses Through Gravitational Microlensing
J. -P. Beaulieu, D. P. Bennett, P. Fouque +46
In the favoured core-accretion model of formation of planetary systems, solid planetesimals accumulate to build up planetary cores, which then accrete nebular gas if they are suffi…