Open AccessHα kinematics of a z ∼ 1 disc galaxy from near‐infrared integral field spectroscopy
Author(s) -
Smith J. K.,
Bunker A. J.,
Vogt N. P.,
Abraham R. G.,
AragónSalamanca A.,
Bower R. G.,
Parry I. R.,
Sharp R. S.,
Swinbank A. M.
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.08323.x
Subject(s) - physics , astrophysics , galaxy , tully–fisher relation , galaxy rotation curve , stellar kinematics , peculiar velocity , rest frame , spectroscopy , astronomy , galaxy formation and evolution , redshift , milky way
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 M B (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 .