The Assembly History of Disk Galaxies. II. Probing the Emerging Tully-Fisher Relation during 1 < z < 1.7
Abstract
Through extended integrations using the recently installed deep depletion CCD on the red arm of the Keck I Low Resolution Imaging Spectrograph, we present new measurements of the resolved spectra of 70 morphologically selected star-forming galaxies with i_(AB) < 24.1 in the redshift range 1≾z < 1.7. Using the formalism introduced in Paper I of this series and available Hubble Space Telescope (HST) Advanced Camera for Surveys images, we successfully recover rotation curves using the extended emission line distribution of [O II] 3727 Å to 2.2 times the disk scale radius for a sample of 42 galaxies. Combining these measures with stellar masses derived from HST and ground-based near-infrared photometry enables us to construct the stellar mass Tully-Fisher relation (M_*-TFR) in the time interval between the well-constructed relation defined at z ≃ 1 in Paper I and the growing body of resolved dynamics probed with integral field unit spectrographs at z > 2. Remarkably, we find a well-defined TFR with up to 60% increase in scatter and zero-point shift constraint of ΔM_* = 0.02 ± 0.02 dex since z ~ 1.7, compared to the local relation. Although our sample is incomplete in terms of either a fixed stellar mass or star formation rate limit, we discuss the implications that typical star-forming disk galaxies evolve to arrive on a well-defined TFR within a surprisingly short period of cosmic history.
Additional Information
© 2012 The American Astronomical Society. Received 2012 January 19; accepted 2012 April 30; published 2012 June 14. S.H.M. thanks the Rhodes Trust, the British Federation of Women Graduates, the sub-department of Astrophysics and New College at the University of Oxford, and the California Institute of Technology for supporting her work. We thank P. Capak for generously allowing us to use his SSA22 photometry catalog. We also thank A. Benson for preliminary results from the Galacticus model to compare to our observations, and we thank C. Peng for supplying us with galfit 3.0. We also thank C. Conroy, A. Dutton, L. Hernquist, J. Gunn, and A. Loeb for helpful discussions on this work. We thank the anonymous referee for improving the quality of thiswork. The spectroscopic data were secured with the W. M. Keck Observatory on Mauna Kea. We thank the observatory staff for their dedication and support. The authors recognize and acknowledge the cultural role and reverence that the summit of Mauna Kea has always had with the indigenous Hawaiian community, and we are most fortunate to have the opportunity to conduct observations from this mountain. Facilities: Keck:I (LRIS), HST (ACS)Attached Files
Published - Miller2012p18935Astrophys_J.pdf
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Additional details
- Eprint ID
- 32640
- Resolver ID
- CaltechAUTHORS:20120723-110020521
- Rhodes Trust
- British Federation of Women Graduates
- University of Oxford
- Caltech
- Created
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2012-07-24Created from EPrint's datestamp field
- Updated
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2021-11-09Created from EPrint's last_modified field