THE SINS SURVEY: MODELING THE DYNAMICS OF z {approx} 2 GALAXIES AND THE HIGH-z TULLY-FISHER RELATION
- Max-Planck-Institut fuer extraterrestrische Physik, Postfach 1312, D-85741 Garching (Germany)
- Department of Astronomy, Campbell Hall, University of California, Berkeley, CA 94720 (United States)
- Excellence Cluster Universe, Technische Universitaet Muenchen, Boltzmanstr. 2, D-85748 Garching (Germany)
- Universitaets-Sternwarte Ludwig-Maximilians Universitaet (USM), Scheinerstr. 1, Muenchen D-81679 (Germany)
- School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978 (Israel)
- Dipartimento di Astronomia, Universita degli Studi di Bologna, via Ranzani 1, I-40127 Bologna (Italy)
- CEA, Laboratoire AIM-CNRS-Universite Paris Diderot, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette (France)
We present the modeling of SINFONI integral field dynamics of 18 star-forming galaxies at z {approx} 2 from H{alpha} line emission. The galaxies are selected from the larger sample of the SINS survey, based on the prominence of ordered rotational motions with respect to more complex merger-induced dynamics. The quality of the data allows us to carefully select systems with kinematics dominated by rotation, and to model the gas dynamics across the whole galaxy using suitable exponential disk models. We obtain a good correlation between the dynamical mass and the stellar mass, finding that large gas fractions (M {sub gas} {approx} M {sub *}) are required to explain the difference between the two quantities. We use the derived stellar mass and maximum rotational velocity V {sub max} from the modeling to construct for the first time the stellar mass Tully-Fisher relation at z {approx} 2.2. The relation obtained shows a slope similar to what is observed at lower redshift, but we detect an evolution of the zero point. We find that at z {approx} 2.2 there is an offset in log(M {sub *}) for a given rotational velocity of 0.41 {+-} 0.11 with respect to the local universe. This result is consistent with the predictions of the latest N-body/hydrodynamical simulations of disk formation and evolution, which invoke gas accretion onto the forming disk in filaments and cooling flows. This scenario is in agreement with other dynamical evidence from SINS, where gas accretion from the halo is required to reproduce the observed properties of a large fraction of the z {approx} 2 galaxies.
- OSTI ID:
- 21300592
- Journal Information:
- Astrophysical Journal, Vol. 697, Issue 1; Other Information: DOI: 10.1088/0004-637X/697/1/115; Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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