On the Giant Horizontal and Asymptotic Branches of Galactic Globular Clusters - Part Five - CCD Photometry of NGC1261

Details On the Giant Horizontal and Asymptotic Branches of Galactic Globular Clusters - Part Five - CCD Photometry of NGC1261 On the Giant Horizontal and Asymptotic Branches of Galactic Globular Clusters - Part Five - CCD Photometry of NGC1261

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.264..273f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 264, NO.2/SEP15, P. 273, 1993

Astronomy and Astrophysics

Astronomy

24

Stars: Abundances - Stars: Evolution - Hertzsprung-Russell (Hr) Diagram - Globular Clusters: Individual: Ngc 1261

Scientific paper

BV CCD photometry is presented for 3352 stars (18 variables) in the globular cluster NGC 126 t. The main conclusions drawn from the structure of the colour-magnitude diagram (CMD) are as follows.
(i) The location and structure of the main branches agree with those found in previous studies, confirming the existence of a well-defined blue horizontal branch (1113) tail in addition to the large number of red 1113 stars.
(ii) The mean metallicity derived from CMD indicators calibrated with the Zinn & West scale is [Fe/H] = -1.4±0.2, and the very small intrinsic width of the various branches yields very low upper limits (Δ[Fe/H]≤0.06, Δ[CNO]≤-0.2) for any chemical abundance spread.
(iii) The `RGB bump' is detected at V= 16.70±0.05 as a clump of stars in the luminosity function of the red giant branch.
(iv) VHB=16.70±0.04 and VTO=20.t4±0.10 yield ΔVTOHB=3.44±0.12. A detailed comparison with the main CMD loci of NGC 288 (a cluster that has similar metallicity but a totally blue 1113) throws doubt on the hypothesis that a clear difference in age (NGC 288 being older) is the `second parameter' necessary to explain the observed differences.
(v) Some evidence is found for differences in the spatial distribution of the red and blue 1113 stars that is worthy of further analysis.

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