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J/A+A/448/171       BV photometry of 3 globular clusters     (Hilker+, 2006)

Probable member stars of the gravitational theory-testing globular clusters AM 1, Pal 3 and Pal 14. Hilker M. <Astron. Astrophys., 448, 171-180 (2006)> =2006A&A...448..171H
ADC_Keywords: Clusters, globular ; Photometry, UBV Keywords: Galaxy: globular clusters: individual: AM 1, Pal 3, Pal 14 - astrometry - Galaxy: kinematics and dynamics Abstract: Some of the Galactic outer halo globular clusters are excellent tools to probe gravitational theories in the regime of weak accelerations. The measurement of the line-of-sight velocity dispersion among stars in these clusters will differentiate between the validity of Newtonian dynamics (low velocity dispersion) and the possibility of modified Newtonian dynamics (MOND) or dark matter dominated globular clusters (high velocity dispersion). In this paper, the properties of probable member stars of the three best-case gravitational theory-testing clusters AM 1, Pal 3 and Pal 14 are presented. The member selection is based on VLT photometry in Johnson BV. The positions of the stars were determined with an accuracy of the order of ≤0.2", allowing their direct use for follow-up spectroscopy. The distance, reddening, age and metallicities of the clusters were estimated from isochrone fitting. Furthermore, improved structural parameters, like central coordinates, ellipticity, half-light radius, King model core and tidal radius, are presented. Description: The observations were performed in February 2005 with the VLT/UT1 at Paranal (ESO), Chile. The instrument in use was the FORS2 camera with a 4x4 k MIT CCD array attached. The data were read out with a 2x2 binning, resulting in a spatial scale of 0.25"/pixel and a field of view of 6.8'x6.8'. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) (file) ---------------------------------------------------------- 03 55 02.7 -49 36 52 Cl AM 1 = ESO 201- 10 (tablea1) 10 05 31.0 +00 04 15 Cl Pal 3 = UGC 5439 (tablea2) 16 10 59.0 +14 57 42 Cl Pal 14 = GCl 38 (tablea3) ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 58 110 List of probable member stars of AM 1, ordered by increasing V magnitude. tablea2.dat 58 153 List of probable member stars of Pal 3, ordered by increasing V magnitude. tablea3.dat 58 143 List of probable member stars of Pal 14, ordered by increasing V magnitude
See also: J/AJ/117/247 : Ages for globular clusters in the halo (Stetson+, 1999) Byte-by-byte Description of file: tablea?.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Sequential number (1) 5- 6 I2 h RAh Right ascension (J2000) 8- 9 I2 min RAm Right ascension (J2000) 11- 15 F5.2 s RAs Right ascension (J2000) 17 A1 --- DE- Declination sign (J2000) 18- 19 I2 deg DEd Declination (J2000) 21- 22 I2 arcmin DEm Declination (J2000) 24- 27 F4.1 arcsec DEs Declination (J2000) 29- 33 F5.2 mag Vmag V magnitude from PSF fit 35- 38 F4.2 mag B-V B-V colour index 40- 43 F4.2 mag e_Vmag rms uncertainty on Vmag 45- 48 F4.2 mag e_Bmag rms uncertainty on Bmag 50- 53 F4.2 arcmin Rad Projected distance to cluster center 55- 58 A4 --- Type Part of the CMD the star probably belongs (2)
Note (1): Stars are identified as Cl* AM 1 H NNN, Cl* Palomar 3 H NNN and Cl* Palomar 4 H NNN in Simbad, respectively. Note (2): region of the colour-magnitude diagram abbreviated as: RGB = red giant branch, HB = horizontal branch, AGB = asymptotic giant branch
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 17-Nov-2006
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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