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Effective temperature scale and bolometric corrections from 2MASS photometry
We present a method to determine effective temperatures, angularsemi-diameters and bolometric corrections for population I and II FGKtype stars based on V and 2MASS IR photometry. Accurate calibration isaccomplished by using a sample of solar analogues, whose averagetemperature is assumed to be equal to the solar effective temperature of5777 K. By taking into account all possible sources of error we estimateassociated uncertainties to better than 1% in effective temperature andin the range 1.0-2.5% in angular semi-diameter for unreddened stars.Comparison of our new temperatures with other determinations extractedfrom the literature indicates, in general, remarkably good agreement.These results suggest that the effective temperaure scale of FGK starsis currently established with an accuracy better than 0.5%-1%. Theapplication of the method to a sample of 10 999 dwarfs in the Hipparcoscatalogue allows us to define temperature and bolometric correction (Kband) calibrations as a function of (V-K), [m/H] and log g. Bolometriccorrections in the V and K bands as a function of T_eff, [m/H] and log gare also given. We provide effective temperatures, angularsemi-diameters, radii and bolometric corrections in the V and K bandsfor the 10 999 FGK stars in our sample with the correspondinguncertainties.
| K-band light curves for RR Lyrae stars in the globular clusters M5 and M92
K-band photometry for the RR Lyrae stars V1 and V3 in the extremelymetal-poor globular cluster M92 (NGC 6341) and V8 and V28 in theintermediate-metallicity cluster M5 (NGC 5904) have been acquired duringthe 1987-1990 observing seasons, for use in a Baade-Wesselink analysis.A single-channel photometer as well as IR imagers have been used for thedata acquisition, and the results from the different systems show goodagreement. The reduction procedure for these data and the resultinglight curves, good to better than 0.02 mag, based on 340, 541, 284, and212 measurements for M92-V1, M92-V3, M5-V8, and M5-V28, respectively,are presented. Preliminary distance estimates for the clusters lead tovalues of (m-M)0 = 14.36 for M92 and (m-M)0 = 14.24 for M5.
| The interstellar reddening in front of globular clusters.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975PASP...87...65C&db_key=AST
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