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CHARM2: An updated Catalog of High Angular Resolution Measurements
We present an update of the Catalog of High Angular ResolutionMeasurements (CHARM, Richichi & Percheron \cite{CHARM}, A&A,386, 492), which includes results available until July 2004. CHARM2 is acompilation of direct measurements by high angular resolution methods,as well as indirect estimates of stellar diameters. Its main goal is toprovide a reference list of sources which can be used for calibrationand verification observations with long-baseline optical and near-IRinterferometers. Single and binary stars are included, as are complexobjects from circumstellar shells to extragalactic sources. The presentupdate provides an increase of almost a factor of two over the previousedition. Additionally, it includes several corrections and improvements,as well as a cross-check with the valuable public release observationsof the ESO Very Large Telescope Interferometer (VLTI). A total of 8231entries for 3238 unique sources are now present in CHARM2. Thisrepresents an increase of a factor of 3.4 and 2.0, respectively, overthe contents of the previous version of CHARM.The catalog is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/431/773
| CHARM: A Catalog of High Angular Resolution Measurements
The Catalog of High Angular Resolution Measurements (CHARM) includesmost of the measurements obtained by the techniques of lunaroccultations and long-baseline interferometry at visual and infraredwavelengths, which have appeared in the literature or have otherwisebeen made public until mid-2001. A total of 2432 measurements of 1625sources are included, along with extensive auxiliary information. Inparticular, visual and infrared photometry is included for almost allthe sources. This has been partly extracted from currently availablecatalogs, and partly obtained specifically for CHARM. The main aim is toprovide a compilation of sources which could be used as calibrators orfor science verification purposes by the new generation of largeground-based facilities such as the ESO Very Large Interferometer andthe Keck Interferometer. The Catalog is available in electronic form atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/386/492, and from theauthors on CD-Rom.
| New binary stars discovered by lunar occultations. II.
This paper is the second in a series, following the one by Richichi etal. (1994a, hereafter Paper I), reporting discoveries of new binarystars in the course of routine lunar occultation programs at the TIRGOand Calar Alto observatories, or re-observations of known or suspectedbinaries where only incomplete information was available. We report on atotal of 15 sources. In the following eight cases, we detected acompanion for the first time: SAO 93127, SAO 93195, SAO 95677, SAO96110, SAO 97246, SAO 97258, SAO 183637, AG +15 845. For two stars, SAO76131 and SAO 184822, we confirm previous reports of binarity, with ourIR measurements complementing existing visual information. In the caseof the five stars SAO 93484, SAO 96746, SAO 128467, SAO 157923 (αVir), and SAO 162413, a companion had also been previously observed, butwe could not detect it in our observation. Our negative detection inmost of these cases provides a constraint on the characteristics of thecompanion. The projected separations in our positive results range from0.79" to 0.006", and the range of brightness ratios from =~1:1 to 1:150.The faintest companion has K=~11. The performance of the lunaroccultations technique offers a valid complement to other more modernmethods such as speckle interferometry and long baseline interferometry,and in fact many of the stars in our list could not be resolved byprevious attempts using these latter techniques. In addition to standardobservations by fast photometers, in this paper we include and describethe routine use of an IR array detector to record lunar occultations,which offered significant improvement in sensitivity.
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