EDP Sciences
Free access
Issue
A&A
Volume 397, Number 3, January III 2003
Page(s) 839 - 849
Section Galactic structure and dynamics
DOI http://dx.doi.org/10.1051/0004-6361:20021564


A&A 397, 839-849 (2003)
DOI: 10.1051/0004-6361:20021564

Physical properties of two low-luminosity $\mathsf{{\vec z} \sim 1.9}$ galaxies behind the lensing cluster AC 114

M. Lemoine-Busserolle1, T. Contini1, R. Pelló1, J.-F. Le Borgne1, J.-P. Kneib1, 2 and C. Lidman3

1  Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées - UMR 5572, 14 avenue E. Belin, 31400 Toulouse, France
2  California Institute of Technology - Pasadena, CA 91125, USA
3  European Southern Observatory - Alonso de Cordova 3107, Vitacura, Chile

(Received 4 September 2002 / Accepted 22 October 2002 )

Abstract
We present VLT/ISAAC near-infrared spectroscopy of two gravitationally-lensed $z \sim 1.9$ galaxies, A2 and S2, located behind the cluster AC 114. Thanks to large magnification factors, we have been successful in detecting rest-frame optical emission lines (from [O II] $\lambda$3727 to ${\rm H{\alpha}}$ +[N II] $\lambda$6584) in star-forming galaxies 1 to 2 mag fainter than in previous studies of Lyman break galaxies (LBGs) at $z \sim 3$. From the ${\rm H{\alpha}}$ luminosity, we estimate star formation rates (SFRs) of 30 and 15  $M_{\odot}$ yr -1for S2 and A2 respectively. These values are 7 to 15 times higher than those inferred from the UV continuum flux at 1500 Å without dust extinction correction. In setting ${\textit SFR}_{\rm H\alpha}\sim {\textit SFR}_{\rm UV}$, one derives extinction coefficients $E(B-V) \sim 0.3$ for S2 and $E(B-V) \sim 0.4$ for A2. The behavior of S2 and A2 in terms of O/H and N/O abundance ratios are very different, and they are also different from typical LBGs at $z \sim 3$. S2 is a low-metallicity object ( $Z \sim 0.03$  $Z_{\odot}$) with a low N/O ratio, similar to those derived in the most metal-poor nearby HIIgalaxies. In contrast, A2 is a high-metallicity galaxy ( $Z \sim 1.3$ $Z_{\odot}$) with a high N/O abundance ratio, similar to those derived in the most metal-rich starburst nucleus galaxies. The line-of-sight velocity dispersions, derived from emission line widths, are 55 and 105 km s -1, yielding a virial mass of 0.5 and $2.4 \times 10^{10}$ $M_{\odot}$, for S2 and A2 respectively. Thanks to the gravitational amplification, the line profiles of S2 are spatially resolved, leading to a velocity gradient of $\pm 240$ km s -1, which yields a dynamical mass of ${\sim} 1.3 \times 10^{10}$ $M_{\odot}$within the inner 1 kpc radius. Combining these new data with the sample of LBGs at $z \sim 3$, including the lensed galaxy MS 1512-cB58, which is the only LBG for which physical properties have been determined with similar accuracy, we conclude that these three galaxies exhibit different physical properties in terms of abundance ratios, SFRs, $M/L_{\rm B}$ and reddening. High-redshift galaxies of different luminosities could thus have quite different star formation histories.


Key words: galaxies: evolution -- galaxies: starburst -- galaxies: abundances -- galaxies: kinematics and dynamics -- infrared: galaxies

Offprint request: T. Contini, contini@ast.obs-mip.fr

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