• DOI:10.1111/j.1365-2966.2004.08323.x
• Corpus ID: 54919723

Hα kinematics of a z∼ 1 disc galaxy from near‐infrared integral field spectroscopy

@article{Smith2004HKO,
  title={H$\alpha$ kinematics of a z∼ 1 disc galaxy from near‐infrared integral field spectroscopy},
  author={J. K. Smith and A. J. Bunker and N. P. Vogt and R. G. Abraham and Alfonso Arag{\'o}n-Salamanca and R G Bower and I. R. Parry and Rob Sharp and A. M. Swinbank Institute of Astronomy and Cambridge and University of Exeter and New Mexico State University and University of Toronto and University of Nottingham and Univeristy of Durham Anglo-Australian Observatory},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2004},
  volume={354}
}

• J. Smith, A. Bunker, +12 authors Univeristy of Durham Anglo-Australian Observatory
• Published 25 August 2004
• Physics
• Monthly Notices of the Royal Astronomical Society

In this Letter we present the first 3D spectroscopic study of Hα emission in a z ∼ 1 field galaxy with an integral field unit. Using the Cambridge Infrared Panoramic Survey Spectrograph (CIRPASS) on Gemini-South, we map the spatial and velocity distribution of Hα emission in the z = 0.819 galaxy CFRS 22.1313. We detect two Hα emitting regions with a velocity separation of 220 ± 10 km s −1 . Combining the 2D map of Hα emission with Hubble Space Telescope F814W imaging, we determine a lower limit of 180 ± 20 km s −1 for the rotation velocity of this MB(rest) ∼− 21 galaxy. We note that our value is significantly higher than the rotation velocity of 120 ± 10 km s −1 reported by Barden et al. for their long-slit spectroscopic study of this galaxy. Our lower limit on the rotation velocity is entirely consistent with no evolution of the rest B-band Tully‐Fisher relation. The position of this galaxy relative to the mean rest B-band Tully‐Fisher relation of Pierce & Tully is consistent with brightening of no more than ∼1 mag at z = 0.8. A larger integral field unit sample, without the uncertainties inherent to long-slit samples, is needed to determine the evolution of the Tully‐Fisher relation accurately out to z ∼ 1. Ke yw ords: instrumentation: spectrographs ‐ galaxies: evolution ‐ galaxies: individual: CFRS22.1313 ‐ galaxies: kinematics and dynamics ‐ galaxies: spiral.