A&A 389, 419 (2002)
DOI: 10.1051/0004-6361:20020718

VLT-UVES spectroscopy of a bulge giant magnified through microlensing: EROS-BLG-2000-5

D. Minniti¹ - B. Barbuy² - V. Hill³ - E. Bica⁴ - S. Ortolani⁵ - R. M. Rich⁶ - K. H. Cook⁷ - T. Vandehei⁸ -
A. Renzini⁹ - L. Pasquini⁹ - D. Bennett¹⁰

1 - Universidad Catolica de Chile, Department of Astronomy & Astrophysics, Casilla 306, Santiago 22, Chile
2 - Universidade de São Paulo, Departamento de Astronomia, CP 3386, São Paulo 01060-970, Brazil - Observatoire de Paris-Meudon, 92195 Meudon Cedex, France
3 - Universidade Federal do Rio Grande do Sul, Departamento de Astronomia, CP 15051, Porto Alegre 91501-970, Brazil
4 - Università di Padova, Dipartimento di Astronomia, Vicolo dell'Osservatorio 2, 35122 Padova, Italy
5 - UCLA, Department of Physics & Astronomy, 8979 Math-Sciences Building, Los Angeles, CA 90095-1562, USA
6 - Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
7 - University of California, Department of Physics, San Diego, CA 92093, USA
8 - European Southern Observatory, Karl Schwarzschild Strasse 2, 85748 Garching bei München, Germany
9 - University of Notre Dame, Department of Physics, Notre Dame, IN 46556, USA

Abstract
A&A, 384, 884-889 (2002), DOI: 10.1051/0004-6361:20020111

We are grateful to M. Albrow and A. Gould for having pointed out to us that our observation of EROS-BLG-2000-5 was misidentified. In fact we have observed a closely projected bulge star $\approx$1$\arcsec$to the northwest of EROS-BLG-2000-5. We have observed a cooler bulge giant which is GSC2.2-S222123214159 located at J2000.0 $\alpha = 17\, 53\, 11.439$ $\delta = -30$5534.72.

Our high dispersion spectroscopic analysis of this star is entirely self-consistent and remains valid, given that we have derived the reddening and the temperature from the spectrum. The distance would be closer to the central bulge than estimated in the paper.