UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995)

Details UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995) UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995)

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ycat..21010117k&link_type=abstract

VizieR On-line Data Catalog: J/ApJS/101/117. Originally published in: 1995ApJS..101..117K

Computer Science

1

Stars: Pre-Main Sequence, Photometry

Scientific paper

Tables A1-A2 list average V and K magnitudes and broadband optical and near-infrared colors for T Tauri stars in the Taurus-Auriga cloud. The quoted errors are 1 sigma dispersions from the average values for objects with 2 or more measurements at V, K, or the appropriate color. For convenience, the authors quote dispersions of 0.00 for objects with only a single measurement. The last columns of Tables A1-A2 list the number of V, K, and N measurements used to compute the average values. The number of data points used to determine average colors is usually close to the number of V or K measurements. Table A3 lists IRAS colors for the Taurus-Auriga sample. For each IRAS source, the authors compiled fluxes from version 2 of the Point Source Catalog, IRAS ADDSCANs, and the IRAS Serendipitous Survey Catalog and averaged fluxes for sources appearing in 2 or 3 catalogs (see section 2 of the printed paper). The authors adopted flux zero points of Fnu(12um)=28.3Jy, Fnu(25um)=6.73Jy, Fnu(60um)=1.19Jy, and Fnu(100um)=0.43Jy to compute IRAS magnitudes and then derived colors using average K magnitudes from Table A2. In some cases, two or more pre-main-sequence stars fall in a typical IRAS beam. The authors summed the K flux of the individual objects to compute a combined K magnitude and color for these IRAS sources. These IRAS colors assume no color correction for the IRAS flux. Table A4 lists various quantities derived from published spectra and the photometry in Tables A1-A3. Infrared colors and the ratio of far-IR to bolometric luminosity set the spectral energy distribution class, SED. The optical spectral type usually was taken from the literature (Herbig & Bell (1988LicOB1111....1H)) or the authors own work. The effective temperature, Teff, is based on compilations by Schmidt-Kaler (1982) and Straizys (1992). The authors estimated optical extinctions, A_V, from comparisons between the observed optical or infrared colors and colors for normal main sequence stars in Table A5. The authors adopted Bessell & Brett's (1988PASP..100.1134B) extinction curve to derive A_V from the optical color excess and to derive the extinction at 1.25um, A_J. The stellar luminosity, L_J, follows from the observed J magnitude, the extinction, and an appropriate bolometric correction from Table A5 for a distance of d=140pc. The 7-135um luminosity, L_FIR, and the bolometric luminosity, L_b, are both integrations over the reddening-corrected flux distribution. The 7-135um luminosity is quoted as an upper limit for sources not detected by IRAS. Lower limits on L_b are quoted for sources with incomplete photometry. Table A5 lists adopted broadband colors for main sequence stars. For the optical colors, this list is based on data compiled by Johnson (1966, ARA&A, 4, 193; U-B, B-V, V-RJ, and V-JC), Schmidt-Kaler ((1982) ; U-B and B-V), and Bessell ((1990A&AS...83..357B) and 1990, PASP, 102, 1181; U-B, B-V, V-R_C, and V-I_C). Bessell & Brett (1988PASP..100.1134B) contains the most comprehensive list of main sequence IR colors. The authors supplemented their Table II with colors from Johnson (1966, ARA&A, 4, 193) for early-type main sequence stars. Johnson (1966, ARA&A, 4, 193) contains the best list of K-N colors for main sequence stars. To complement these data, the authors compiled V-[12] colors using stars selected from the Third Catalog of Nearby Stars (Gliese & Jahreiss 1979A&AS...38..423G). The authors extracted 12um fluxes from version 2 of the IRAS Point Source Catalog, color-corrected the fluxes assuming a color temperature equal to the stellar effective temperature, and computed a V-[12] color assuming a 12um zero point of 28.3Jy. The tabulated color is the median color. The tabulated visual bolometric corrections, BCV=Mbol-M_V, were used to derive absolute J luminosities, LJ. The authors adopted BCV from Schmidt-Kaler (1982; also Straizys 1992) for stars with spectral types earlier than K6; the authors integrated the energy distribution over wavelength to derive BC_V for for later spectral types. (5 data files).

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