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J/AJ/132/2665     QUEST2 BRI photometry of Taurus-Auriga PMS   (Slesnick+, 2006)

A distributed population of low-mass pre-main-sequence stars near the Taurus molecular clouds. Slesnick C.L., Carpenter J.M., Hillenbrand L.A., Mamajek E.E. <Astron. J., 132, 2665-2674 (2006)> =2006AJ....132.2665S
ADC_Keywords: Clusters, open ; Stars, pre-main sequence ; Photometry, infrared ; Spectra, infrared Keywords: open clusters and associations: individual (Taurus) - stars: low-mass, brown dwarfs - stars: pre-main sequence Abstract: We present a drift-scan survey covering a ∼5°x5° region toward the southern portion of the Taurus-Auriga molecular cloud. Data taken in the B,R,I filters with the Quest-2 camera on the Palomar 48 inch (1.2m) Samuel Oschin Telescope were combined with Two Micron All Sky Survey near-infrared photometry to select candidate young stars. Follow-up optical spectroscopy of 190 candidates led to the identification of 42 new low-mass pre-main-sequence stars with spectral types M4-M8, of which approximately half exhibit surface gravity signatures similar to known Taurus stars, while the other half exhibit surface gravity signatures similar to members of the somewhat older Upper Scorpius, TW Hya, and Pic associations. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 86 42 Measured quantities for new PMS stars tablea1.dat 72 148 Measured quantities for candidates spectroscopically confirmed as field dwarfs
See also: J/A+A/312/439 : New T Tauri stars in Taurus-Auriga (Wichmann+, 1996) J/A+AS/101/485 : Multisite UBVRI photometry in Tau-Aur cloud (Bouvier+ 1993) J/A+AS/124/449 : Young stars south of Taurus-Auriga (Magazzu+ 1997) J/A+AS/132/173 : New weak-line T Tauri stars in Taurus-Auriga (Li+ 1998) J/A+AS/145/187 : uvby-β photometry of WTTS (Chavarria-K+, 2000) J/ApJ/581/1194 : Taurus-Auriga PMS stars ages and Teff (Palla+, 2002) J/ApJS/101/117 : UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [SCH] 5- 20 A16 --- [SCH2006b] Stellar identification, JHHMMSSs+DDMMSSs 22 A1 --- f_[SCH2006b] [b] Flag on [SCH2006b] (1) 24- 27 F4.1 mag Bmag ? Quest-2 B band magnitude 29- 32 F4.1 mag Rmag Quest-2 R band magnitude 34- 37 F4.1 mag Imag Quest-2 I band magnitude 39- 43 F5.2 mag Jmag 2MASS J band magnitude 45- 49 F5.2 mag Hmag 2MASS H band magnitude 51- 55 F5.2 mag Ksmag 2MASS KS band magnitude 57- 60 F4.2 --- TiO(7140) The TiO-7140 spectral index 62- 65 F4.2 --- TiO(8165) The TiO-8165 spectral index 67- 70 F4.2 --- Na(8195) The Na-8195 spectral index 72- 76 A5 --- SpType MK spectral type 78- 80 I3 0.1nm EWHa ? The Hα equivalent width in Angstroms 82- 86 A5 --- Age Stellar age, as young (1-2Myr) or int (5-10Myr)
Note (1): Three of our PMS objects were previously identified in the literature: SCH J0429595+2433080 = Gueiu et al., 2006, Cat. J/A+A/446/485 SCH J0431191+2335048 = Luhman, 2006, Cat. J/ApJ/645/676 SCH J0416272+2053093 = Wichmann et al., 1996, Cat. J/A+A/312/439
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [SCH] 5- 22 A18 --- [SCH2006b] Stellar identification, JHHMMSSss+DDMMSSss 24 A1 --- f_[SCH2006b] [b] Flag on [SCH2006b] (1) 26- 29 F4.1 mag Bmag ? Quest-2 B band magnitude 31- 34 F4.1 mag Rmag ? Quest-2 R band magnitude 36- 39 F4.1 mag Imag Quest-2 I band magnitude 41- 45 F5.2 mag Jmag 2MASS J band magnitude 47- 51 F5.2 mag Hmag 2MASS H band magnitude 53- 57 F5.2 mag Ksmag 2MASS KS band magnitude 59- 62 F4.2 --- TiO(7140) The TiO-7140 index 64- 67 F4.2 --- TiO(8165) The TiO-8165 spectral index 69- 72 F4.2 --- Na(8195) The Na-8195 spectral index
Note (1): Two faint candidates observed during the first spectroscopic observing run before the final photometric calibrations were finished do not have R-band photometry.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 30-Jul-2008
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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