Drift-scan mode (3600-6800 Angstrom) spectra with 500 < R < 1000 resolution are presented for 333 galaxies members of nearby clusters, covering the whole Hubble sequence. The majority (225) were obtained for galaxies in the Virgo cluster where a completeness of 36%, if all Hubble types are considered, and of 51%, restricting to late-types, was reached at m(p) less than or equal to 16. Our data can be therefore considered representative of the integrated spectral properties of giant and dwarf galaxies in this cluster. Intensities and equivalent widths (EWs) are derived for the principal lines, both in emission and in absorption. Deblending of the underlying absorption from emission was achieved in most cases

Gavazzi, G., Zaccardo, A., Sanvito, G., Boselli, A., Bonfanti, C. (2004). Spectrophotornetry of galaxies in the Virgo cluster - II. The data. ASTRONOMY & ASTROPHYSICS, 417(2), 499-514 [10.1051/0004-6361:20034105].

Spectrophotornetry of galaxies in the Virgo cluster - II. The data

GAVAZZI, GIUSEPPE;
2004

Abstract

Drift-scan mode (3600-6800 Angstrom) spectra with 500 < R < 1000 resolution are presented for 333 galaxies members of nearby clusters, covering the whole Hubble sequence. The majority (225) were obtained for galaxies in the Virgo cluster where a completeness of 36%, if all Hubble types are considered, and of 51%, restricting to late-types, was reached at m(p) less than or equal to 16. Our data can be therefore considered representative of the integrated spectral properties of giant and dwarf galaxies in this cluster. Intensities and equivalent widths (EWs) are derived for the principal lines, both in emission and in absorption. Deblending of the underlying absorption from emission was achieved in most cases
Articolo in rivista - Articolo scientifico
galaxies : clusters : individual : Virgo; techniques : spectroscopic; catalogs
English
2004
417
2
499
514
none
Gavazzi, G., Zaccardo, A., Sanvito, G., Boselli, A., Bonfanti, C. (2004). Spectrophotornetry of galaxies in the Virgo cluster - II. The data. ASTRONOMY & ASTROPHYSICS, 417(2), 499-514 [10.1051/0004-6361:20034105].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/22466
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