VLT FORS-1 observations of NGC 6397: Evidence for mass segregation

Free access article

Issue		A&A Volume 425, Number 2, October II 2004


Page(s)		509 - 518
Section		Galactic structure, stellar clusters and populations
DOI		http://dx.doi.org/10.1051/0004-6361:200400011

A&A 425, 509-518 (2004)
DOI: 10.1051/0004-6361:200400011

VLT FORS-1 observations of NGC 6397: Evidence for mass segregation

G. Andreuzzi^{1, 2}, V. Testa¹, G. Marconi^{1, 3}, G. Alcaino⁴, F. Alvarado⁴ and R. Buonanno^{1, 5}

¹ INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone, Italy
e-mail: gloria@mporzio.astro.it
² INAF - Centro Galilei Galilei, Santa Cruz de La Palma, Spain
³ ESO-Chile, Alonso de Cordova 4107, Vitacura, Casilla 19001, Santiago, Chile
⁴ Isaac Newton Institute of Chile, Ministerio de Educacion de Chile, Casilla 8-9, Correo 9, Santiago, Chile
⁵ Dipartimento di Fisica, Università di Roma "Tor Vergata", 00100 Roma, Italy

(Received 26 August 2003 / Accepted 3 June 2004 )

Abstract
We present ( V, V-I) VLT-FORS1 observations of the Galactic Globular Cluster NGC 6397. We derive accurate color-magnitude diagrams and luminosity functions (LFs) of the cluster Main Sequence (MS) for two fields extending from a region near the centre of the cluster out to $\simeq$ 10 $\arcmin$ . The photometry of these fields produces a narrow MS extending down to V $\simeq$ 27, much deeper than any previous ground based study on this system and comparable to previous HST photometry. The V, V-I CMD also shows a deep white dwarf cooling sequence locus, contaminated by many field stars and spurious objects. We concentrate the present work on the analysis of the MSLFs derived for two annuli at different radial distance from the center of the cluster. Evidence of a clear-cut correlation between the slope of the observed LFs before reaching the turn-over, and the radial position of the observed fields inside the cluster area is found. We find that the LFs become flatter with decreasing radius ( x $\simeq$ 0.15 for $1\arcmin$ < R₁ < $5.5\arcmin$ ; x $\simeq$ 0.24 for $5.5\arcmin$ < R₂ < $9.8\arcmin$ ; core radius, $r_{\rm c}=$ 0.05 $\arcmin$ ), a trend that is consistent with the interpretation of NGC 6397 as a dynamically relaxed system. This trend is also evident in the mass function.

Key words: Galaxy: globular clusters: individual: NGC 6397 -- stars: low-mass -- stars: luminosity function, mass function

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