The SINS survey: SINFONI Integral Field Spectroscopy of z ~ 2 Star-forming Galaxies

Details The SINS survey: SINFONI Integral Field Spectroscopy of z ~ 2 Star-forming Galaxies The SINS survey: SINFONI Integral Field Spectroscopy of z ~ 2 Star-forming Galaxies

2009-03-10

arxiv.org/abs/0903.1872v2

Astrophys.J.706:1364-1428,2009

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

81 pages, 34 figures. Revised version accepted for publication in the Astrophysical Journal

Scientific paper

10.1088/0004-637X/706/2/1364

We present the SINS survey with SINFONI of high redshift galaxies. With 80 objects observed and 63 detected, SINS is the largest survey of spatially resolved gas kinematics, morphologies, and physical properties of star-forming galaxies at z~1-3. We describe the selection of the targets, the observations, and the data reduction. We then focus on the "SINS Halpha sample" of 62 rest-UV/optically-selected sources at 1.3~10 star-forming galaxies at z~1.5-2.5, with some bias towards bluer systems compared to pure K-selected samples due to the requirement of secure optical redshift. The sample spans two orders of magnitude in stellar mass and in absolute and specific star formation rates, with median values of approximately log(M*/Msun) = 10.5, 70 Msun/yr, and 3/Gyr. The ionized gas distribution and kinematics are spatially resolved on scales ranging from 1.5 kpc for adaptive optics assisted observations to typically 4-5 kpc for seeing-limited data. The Halpha morphologies tend to be irregular and/or clumpy. About one-third are rotation-dominated yet turbulent disks, another third comprises compact and velocity dispersion-dominated objects, and the remaining galaxies are clear interacting/merging systems; the fraction of rotation-dominated systems increases among the more massive part of the sample. The Halpha luminosities and equivalent widths suggest on average roughly twice higher dust attenuation towards the HII regions relative to the bulk of the stars, and comparable current and past-averaged star formation rates. [Abridged]

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