Metal-poor star uvby-beta photometry. X. (Schuster+, 2004)

Details Metal-poor star uvby-beta photometry. X. (Schuster+, 2004) Metal-poor star uvby-beta photometry. X. (Schuster+, 2004)

Mar 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004ycat..34220527s&link_type=abstract

VizieR On-line Data Catalog: J/A+A/422/527. Originally published in: 2004A&A...422..527S

Physics

Stars: High-Velocity, Stars: Metal-Deficient, Photometry: Uvby: Beta, Abundances: [Fe/H]

Scientific paper

Table 1 lists the Stroemgren (uvby) and H-beta photometry observed at the San Pedro Martir observatory, Mexico, plus the number of independent uvby and H-beta observations and Notes concerning the observing conditions, stellar types, and photometric variability.
Table 2 contains the Stroemgren (uvby) photometry observed at the La Silla, Chile, observatory, plus the number of independent uvby observations and Notes concerning possible photometric variability.
Table 3 gives a list of the 497 very metal poor stars with their positions, both equatorial and Galactic; broadband V and B-V photometry, where available; the reddenings in the stellar directions obtained by interpolation in the maps of Schlegel, Finkbeiner, & Davis (1998ApJ...500..525S); our final adopted reddening according to Eq. 1; the resulting dereddened B-V; also B-V dereddened according to the intrinsic-color calibration of Schuster & Nissen (1989, Cat. ); and finally asterisks in the final two columns which indicate the stars that are CH-star candidates according to Fig. 5, and those that are photometric outliers as seen in Figs. 1 and 4, respectively.
Table 4 contains the cross-identifications for a number of the very metal poor stars; these are stars identified as very-metal-poor in more than one of the overlapping fields from the HK survey.
Table 5 gives the dereddened values V0, (b-y)0, m0, and c0 for our uvby photometry, the reddening excesses for (b-y) and (B-V), and the photometric classification according to our c0,(b-y)0 diagram, Fig. 6.
Table 6 shows the line-strength indices from the HK survey. KP is the index that measures the strength of the CaII K line; HP2 and HG2 measure the strengths of the Balmer lines H-delta and H-gamma, respectively; GP measures the strength of the CH G-band.
Table 7 lists the [Fe/H] values from our different calibration procedures with the adopted mean in column 6 and Notes in column 7.
Table 8 contains observed and derived quantities for the probable metal-rich BS (Am) stars.
Table 9 gives the photometric absolute magnitudes and stellar distances for the 497 very-metal-poor stars; stellar distances are given from both the BV and uvby photometries.
(10 data files).

Affiliated with

Also associated with

No associations

Rating

Metal-poor star uvby-beta photometry. X. (Schuster+, 2004) does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Metal-poor star uvby-beta photometry. X. (Schuster+, 2004), we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Metal-poor star uvby-beta photometry. X. (Schuster+, 2004) will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1030724