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KMOS Clusters and VIRIAL GTO Surveys

Published online by Cambridge University Press:  09 February 2015

D. Wilman
Affiliation:
Universitäts-Sternwarte München, Scheinerstr. 1, D-81679Munich, Germany Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
R. Bender
Affiliation:
Universitäts-Sternwarte München, Scheinerstr. 1, D-81679Munich, Germany Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
R. L. Davies
Affiliation:
Physics Department, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
J. T. Mendel
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
J. Chan
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
A. Beifiori
Affiliation:
Universitäts-Sternwarte München, Scheinerstr. 1, D-81679Munich, Germany Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
R. Houghton
Affiliation:
Physics Department, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
R. Saglia
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
N. Förster Schreiber
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
S. Wuyts
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
P. van Dokkum
Affiliation:
Department of Astronomy, Yale University, New Haven, CT06511, USA
M. Cappellari
Affiliation:
Physics Department, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
J. Stott
Affiliation:
Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK
R. Smith
Affiliation:
Department of Physics, University of Durham, South Road, DurhamDH1 3LE, UK
M. Fossati
Affiliation:
Universitäts-Sternwarte München, Scheinerstr. 1, D-81679Munich, Germany Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
S. Kulkarni
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
S. Seitz
Affiliation:
Universitäts-Sternwarte München, Scheinerstr. 1, D-81679Munich, Germany
M. Fabricius
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, D-85741Garching, Germany
R. Sharples
Affiliation:
Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK
G. Brammer
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD21218, USA
E. Nelson
Affiliation:
Department of Astronomy, Yale University, New Haven, CT06511, USA
I. Momcheva
Affiliation:
Department of Astronomy, Yale University, New Haven, CT06511, USA
M. Wegner
Affiliation:
Universitäts-Sternwarte München, Scheinerstr. 1, D-81679Munich, Germany
I. Lewis
Affiliation:
Physics Department, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
Corresponding
E-mail address:
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Abstract

We present the KMOS (K-band Multi-Object Spectrograph) Cluster and VIRIAL (VLT IRIFU Absorption Line) Guaranteed Time Observation (GTO) programs. KMOS provides 24 arms each feeding an integral field unit (14×14 spaxels of 0.2″ pixels) for IZ, YJ, H and K band near infrared (NIR) medium resolution spectroscopy (R ∼ 3500). Targets are selected from a 7.2′ diameter patrol field. Ultra-deep spectroscopy of ∼ 80 early-type cluster galaxies (∼ 20hr on source) and ∼ 200 (∼ 10hr on source) early-type field galaxies at 1 < z < 2 will dramatically improve the situation at z > 1 for which measurements of stellar velocity dispersions and absorption indices are limited to a few, often relatively young passively evolving galaxies (e.g. Bezanson 2013). In ESO Periods P92 and P93, 15 nights worth of data has been collected for KMOS-Clusters and 6 nights for VIRIAL: this will be supplemented with more data in upcoming semesters. All galaxies have multiband HST imaging including existing or upcoming WFC3 IR imaging, providing stellar mass maps and sizes. Combined with our dispersion measurements, this will allow us to examine the fundamental plane and the dynamical mass of a large sample of z > 1 galaxies for the first time, for both cluster and field galaxies.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2015 

References

Jee, M. J., et al., 2011, ApJ, 737, 59CrossRefGoogle Scholar
Mullis, C. R., et al., 2005, ApJ, 623, L85CrossRefGoogle Scholar
Kurk, J., et al., 2009, A&A, 504, 331Google Scholar
Bezanson, R., et al., 2013, ApJ, 779, L21CrossRefGoogle Scholar

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