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J/PASP/110/533     BR photometry of Fornax bright stars    (Stetson+ 1998)

Homogeneous photometry for star clusters and resolved galaxies. I. A survey of bright stars in the Fornax dwarf spheroidal galaxy. Stetson P.B., Hesser J.E., Smecker-Hane T.A. <Publ. Astron. Soc. Pac. 110, 533 (1998)> =1998PASP..110..533S
ADC_Keywords: Galaxies, photometry ; Stars, bright ; Stars, late-type Keywords: Galaxies: Individual: Name: Fornax Dwarf Galaxy - Stars: Evolution Abstract: We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg2 field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 85 161 Coordinates and photometry for bright, red stars in Fornax
See also: J/PASP/115/413 : A star catalog for the open cluster NGC 6791 (Stetson+, 2003) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- SHS98 This paper identification number 5- 7 A3 --- DK Demers & Kunkel (1979PASP...91..761D) name (1) 9- 12 A4 --- WEL Westerlund et al. (1987A&A...178...41W) name (1) 16- 17 I2 h RAh Right ascension (J2000) 19- 20 I2 min RAm Right ascension (J2000) 22- 26 F5.2 s RAs Right ascension (J2000) 28 A1 --- DE- Declination sign 29- 30 I2 deg DEd Declination (J2000) 32- 33 I2 arcmin DEm Declination (J2000) 35- 38 F4.1 arcsec DEs Declination (J2000) 40- 45 F6.3 mag Bmag B magnitude 47- 51 F5.3 mag e_Bmag rms uncertainty on Bmag 53- 58 F6.3 mag Rmag R magnitude 60- 64 F5.3 mag e_Rmag rms uncertainty on Rmag 66- 71 F6.3 mag Vmag V magnitude 73- 77 F5.3 mag B-R B-R colour index 79 I1 --- Note [1-7]? Individual note (2) 81- 85 A5 --- SpType Spectral Type
Note (1): Carbon stars and S stars may be distinguished from M stars by the letter "C," "M," or "S" incorporated into the DK or WEL star name. Note (2): Individual notes are numbered as follows: 1 = Star 30 in the unpublished list of Blanco & McCarthy; see Frogel et al. 1982ApJ...252..133F 2 = Member of a close pair of bright red stars. 3 = The coordinates given by WEL appear to contain a typographical error. The star listed here is the one marked in their finding chart. Its coordinates, precessed back to 1950.0, are 02:37:37.3-34:04; while WEL give 02:37:41.2-34:46:33 4 = WEL 126 5 = WEL 157 6 = WEL 187 7 = WEL 202
Table 2: Mean locations of stellar population proxies in at least eight frame pairs -------------------------------------------------------------------------------- Sample +DeltaX=North +DeltaY=West rms Radius N -------------------------------------------------------------------------------- RR Lyraes +46 +228 657 600 Clump -42 +203 594 7969 Blue -13 +212 521 1457 Red (a) -66 +153 509 41 Red (b) -44 +190 600 85 All -45 +198 582 58310 Table 3: Mean locations of stellar population proxies in at least one frame pair -------------------------------------------------------------------------------- Sample +DeltaX=North +DeltaY=West rms Radius N -------------------------------------------------------------------------------- "RR Lyraes" -37 +195 741 5395 Clump -61 +202 756 11396 Blue -27 +179 592 1670 Red (class [a]) -53 +64 595 47 Red (class [b]) -48 +173 736 114 All -59 +194 735 80468 History: From PASP electronic version References: Stetson, Paper II 2000PASP..112..925S Stetson et al., Paper III 2003PASP..115..413S, Cat. J/PASP/115/413
(End) James Marcout, Patricia Bauer [CDS] 12-Aug-1998
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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