CLUSTER GLIMPSES WITH RAVEN: AO-CORRECTED NEAR AND MID-INFRARED IMAGES OF GLIMPSE C01 AND GLIMPSE C02∗ ∗ Based on data obtained at the Subaru Telescope, which is operated by the National Optical Observatory of Japan. † † This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration

CLUSTER GLIMPSES WITH RAVEN: AO-CORRECTED NEAR AND MID-INFRARED IMAGES OF GLIMPSE C01 AND GLIMPSE C02∗ ∗ Based on data obtained at the Subaru Telescope, which is operated by the National Optical Observatory of Japan. † † This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration

ABSTRACT We discuss images of the star clusters GLIMPSE C01 (GC01) and GLIMPSE C02 (GC02) that were recorded with the Subaru IRCS. Distortions in the wavefront were corrected with the RAVEN adaptive optics (AO) science demonstrator, allowing individual stars in the central regions of both clusters-w...

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Bibliographic Details
Published in:The Astronomical journal 2016-11, Vol.152 (6)
Main Authors: Davidge, T. J., Andersen, D. R., Lardière, O., Bradley, C., Blain, C., Oya, S., Terada, H., Hayano, Y., Lamb, M., Akiyama, M., Ono, Y. H., Suzuki, G.
Format: Article
Language:eng
Subjects:
Galaxy: stellar content
globular clusters: individual (GLIMPSE C01, GLIMPSE C02)
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Summary:ABSTRACT We discuss images of the star clusters GLIMPSE C01 (GC01) and GLIMPSE C02 (GC02) that were recorded with the Subaru IRCS. Distortions in the wavefront were corrected with the RAVEN adaptive optics (AO) science demonstrator, allowing individual stars in the central regions of both clusters-where the fractional contamination from non-cluster objects is lowest-to be imaged. In addition to J, H, and K′ images, both clusters were observed through a narrow-band filter centered near 3.05 m; GC01 was also observed through two other narrow-band filters that sample longer wavelengths. Stars in the narrow-band images have an FWHM that is close to the telescope diffraction limit, demonstrating that open-loop AO systems like RAVEN can deliver exceptional image quality. The near-infrared color-magnitude diagram of GC01 is smeared by non-uniform extinction with a 1 dispersion ΔAK = 0.13 mag. Spatial variations in AK are not related in a systematic way to location in the field. The Red Clump is identified in the K luminosity function (LF) of GC01, and a distance modulus of 13.6 is found. The K LF of GC01 is consistent with a system that is dominated by stars with an age >1 Gyr. As for GC02, the K LF is flat for K > 16, and the absence of a sub-giant branch argues against an old age if the cluster is at a distance of ∼7 kpc. Archival SPITZER [3.6] and [4.5] images of the clusters are also examined, and the red giant branch-tip is identified. It is demonstrated in the Appendix that the [3.6] surface brightness profiles of both clusters can be traced out to radii of at least 100 arcsec.
ISSN:0004-6256
1538-3881