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The Lower Main Sequence and Mass Function of the Globular Cluster Messier 4 | | Harvey B. Richer
; James Brewer
; Gregory G. Fahlman
; Brad K. Gibson
; Brad M. Hansen
; Rodrigo Ibata
; Jasonjot S. Kalirai
; Marco Limongi
; R. Michael Rich
; Ivo Saviane
; Michael M. Shara
; Peter B. Stetson
; | | Date: |
6 May 2002 | | Journal: | Astrophys.J. 574 (2002) L151-L154 | | Subject: | astro-ph | | Affiliation: | UBC), James Brewer (UBC), Gregory G. Fahlman (CFHT), Brad K. Gibson (Swinburne Univ.), Brad M. Hansen (UCLA/Princeton), Rodrigo Ibata (Obs. Strasbourg), Jasonjot S. Kalirai (UBC), Marco Limongi (Oss. Roma), R. Michael Rich (UCLA), Ivo Saviane (ESO), Mi | | Abstract: | The deepest optical image ever in a globular star cluster, a Hubble Space Telescope (HST) 123 orbit exposure in a single field of Messier 4, was obtained in 2 filters (F606W, F814W) over a 10 week period in early 2001. A somewhat shallower image obtained in 1995 allowed us to select out cluster and field objects via their proper motion displacement resulting in remarkably clean color-magnitude diagrams that reach to V = 30, I = 28. The cluster main sequence luminosity function contains very few stars fainter than MV = 15.0, MI = 11.8 which, in both filters, is more than 2 magnitudes brighter than our limit. This is about the faintest luminosity seen among field Population II subdwarfs of the same metallicity. However, there remains a sprinkling of potential cluster stars to lower luminosity all the way down to our limiting magnitudes. These latter objects are significantly redder than any known metal-poor field subdwarf. Comparison with the current generation of theoretical stellar models implies that the masses of the lowest luminosity cluster stars observed are near 0.09 Msun. We derive the mass function of the cluster in our field and find that it is very slowly rising towards the lowest masses with no convincing evidence of a turnover even below 0.1 Msun. The formal slope between 0.65 and 0.09 Msun is alpha = 0.75 (Salpeter of 2.35) with a 99% confidence interval 0.55 - 1.05. A consistency check between these slopes and the number of observed cluster white dwarfs yields a range of possible conclusions, one of which is that we have indeed seen the termination of the white dwarf cooling sequence in M4. | | Source: | arXiv, astro-ph/0205086 | | Services: | Forum | Review | PDF | Favorites | |
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