EDP Sciences
Free Access
Volume 423, Number 3, September I 2004
Page(s) 925 - 934
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361:20040489
Published online 12 August 2004

A&A 423, 925-934 (2004)
DOI: 10.1051/0004-6361:20040489

The distance of M 33 and the stellar population in its outskirts

S. Galleti1, 2, M. Bellazzini1 and F. R. Ferraro2

1  INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
    e-mail: silvia.galleti2@unibo.it;michele.bellazzini@bo.astro.it
2  Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy
    e-mail: francesco.ferraro3@unibo.it

(Received 22 March 2004 / Accepted 10 May 2004)

We present deep V, I photometry of two $9.4\arcmin$  $\times$ $9.4\arcmin$ field in the outer regions of the M 33 galaxy. We obtain a robust detection of the luminosity of the Red Giant Branch Tip ( $I^{{\rm TRGB}}=20.72$  $\pm$ 0.08) from which we derived a new estimate of the distance modulus of M 33, (m-M)0=24.64  $\pm$ 0.15, corresponding to a distance D=847  $\pm$ 60 kpc. By comparison of the color and magnitude of the observed Red Giant Branch stars with ridge lines of template globular clusters we obtained the photometric metallicity distribution of the considered fields in three different metallicity scales. The derived metallicity distributions are very similar over a range of distances from the galactic center $10\arcmin\le R\le 33\arcmin$, and are characterized by a well defined peak at $[M/{\rm H}]\simeq-0.7$ ( $[{\rm Fe/H}]\simeq -1.0$, in the Zinn & West scale) and a weak metal-poor tail reaching $[M/{\rm H}]\la -2.0$. Our observations demonstrate that Red Giant Branch and Asymptotic Giant Branch stars have a radial distribution that is much more extended than the young MS stars associated with the star-forming disc.

Key words: galaxies: individual: M 33 -- galaxies: distances and redshifts

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© ESO 2004

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