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SINFONI Integral Field Spectroscopy of z ~ 2 UV-selected Galaxies: Rotation Curves and Dynamical Evolution

Förster Schreiber, N. M. and Genzel, R. and Lehnert, M. D. and Bouché, N. and Verma, A. and Erb, D. K. and Shapley, A. E. and Steidel, C. C. and Davies, R. and Lutz, D. and Nesvadba, N. and Tacconi, L. J. and Eisenhauer, F. and Abuter, R. and Gilbert, A. and Gillessen, S. and Sternberg, A. (2006) SINFONI Integral Field Spectroscopy of z ~ 2 UV-selected Galaxies: Rotation Curves and Dynamical Evolution. Astrophysical Journal, 645 (2). pp. 1062-1075. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20110721-114249847

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Abstract

We present ~0".5 resolution near-infrared integral field spectroscopy of the Hα line emission of 14 z ~ 2 UV-selected BM/BX galaxies, obtained with SINFONI at the ESO Very Large Telescope. The average Hα half-light radius is r_(1/2)≈ 4 h^(-1)_(70) kpc, and line emission is detected over ≳20 h^(-1)_(70)kpc in several sources. In nine galaxies, we detect spatially resolved velocity gradients, from 40 to 410 km s^(-1) over ~10 h^(-1)_(70) kpc. The kinematics of the larger systems are generally consistent with orbital motions. Four galaxies are well described by rotating clumpy disks, and we extracted rotation curves out to radii ≳10 h^(-1)_(70) kpc. One or two galaxies exhibit signatures more consistent with mergers. Analyzing all 14 galaxies in the framework of rotating disks, we infer mean inclination- and beam-corrected maximum circular velocities of v_c ~ 180 ± 90 km s^(-1) and dynamical masses from ~0.5 to 25 × 10^(10) h^(-1)_(70) M_☉ within r_(1/2). The specific angular momenta of our BM/BX galaxies are similar to those of local late-type galaxies. Moreover, the specific angular momenta of their baryons are comparable to those of their dark matter halos. Extrapolating from the average vc at 10 himg1.gif kpc, the virial mass of the typical halo of a galaxy in our sample is 10^(11.7±0.5) h^(-1)_(70) M_☉. Kinematic modeling of the three best cases implies a ratio of v_c to local velocity dispersion v_(c)/σ ~ 2-4 and, accordingly, a large geometric thickness. We argue that this suggests a mass accretion (alternatively, gas exhaustion) timescale of ~500 Myr. We also argue that if our BM/BX galaxies were initially gas-rich, their clumpy disks would subsequently lose their angular momentum and form compact bulges on a timescale of ~1 Gyr.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/504403DOIArticle
http://iopscience.iop.org/0004-637X/645/2/1062PublisherArticle
ORCID:
AuthorORCID
Genzel, R.0000-0002-2767-9653
Lehnert, M. D.0000-0003-1939-5885
Erb, D. K.0000-0001-9714-2758
Shapley, A. E.0000-0003-3509-4855
Steidel, C. C.0000-0002-4834-7260
Lutz, D.0000-0003-0291-9582
Tacconi, L. J.0000-0002-1485-9401
Additional Information:© 2006 American Astronomical Society. Received 2006 January 21; accepted 2006 March 19. Based on observations obtained at the Very Large Telescope (VLT) of the European Southern Observatory, Paranal, Chile (ESO program IDs 073.B-9018, 074.A-9011, 075.A-0466, and 076.A-0527). We wish to thank the ESO staff for helpful and enthusiastic support during the observations. We thank the referee for useful comments that helped improve the paper.We are also grateful to Norman Murray, Eliot Quataert, Todd Thompson, Ortwin Gerhard, and Sune Toft for interesting discussions and insightful comments on various aspects of this work.
Subject Keywords:galaxies: evolution; galaxies: high-redshift; galaxies: kinematics and dynamics; infrared: galaxies
Issue or Number:2
Record Number:CaltechAUTHORS:20110721-114249847
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20110721-114249847
Official Citation:SINFONI Integral Field Spectroscopy of z ~ 2 UV-selected Galaxies: Rotation Curves and Dynamical Evolution N. M. Förster Schreiber et al. 2006 ApJ 645 1062
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:24497
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:21 Jul 2011 20:08
Last Modified:04 Dec 2019 23:39

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