Globular cluster photometry with the hubble space telescope. I. Description of the method and analysis of the core of 47 Tuc

Puragra Guhathakurta, Brian Yanny, Donald P. Schneider, John N. Bahcall

Research output: Contribution to journalArticle

63 Scopus citations

Abstract

A method is presented for obtaining accurate photometry (σ≤0.1 mag) of stars in the dense cores of Galactic globular clusters using images taken with the Planetary Camera of the Bubble Space Telescope (HST). The principal challenge is due to the fact that the wings of the point spread function (PSF) extend much further than the typical separation between stars. Further complications arise from the complex structure of the PSF, significant variations of the PSF across the field, and the limited dynamic range of the data compared to the range in stellar brightnesses. If the variation of the PSF across the image is not taken into account, one introduces systematic photometric errors of order 0.2 mag. The core of the HST PSF, however, is about five times sharper than the best angular resolution available in ground based images. Detailed and realistic simulations have been carried out to estimate photometric accuracy and completeness. The technique of empirically modeling the variable PSF and determining stellar brightnesses by PSF fitting has been applied to AST PC images of the dense, metal-rich, disk globular cluster 47 Tue obtained with the F555W and F785LP filters (similar to V and I). An accurate color-magnitude diagram is constructed for post-main-sequence stars brighter than V∼18 - a task that has proved impossible from the ground due to the high degree of crowding in the core of 47 Tuc. The region within 1′ of the center of 47 Tue contains a centrally concentrated population of blue stragglers. The projected distribution of giant stars has a core radius rc=23″±2″ (0.52 pc). The diffuse light from fainter stars (just below turnoff) has a core radius (∼26″) that is slightly larger than that of the giants. No central cusp of light or signature of core collapse is seen in 47 Tue. The data place a 95% upper limit of 2.6×103rms/12 km s-1)2script M sign on the mass of any compact object at the center of the cluster. There is no detectable color gradient in 47 Tuc; Δ(V-I) <0.1 between the center and r=1′.

Original languageEnglish (US)
Pages (from-to)1790-1817
Number of pages28
JournalAstronomical Journal
Volume104
Issue number5
DOIs
StatePublished - Nov 1992

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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