The KMOS Redshift One Spectroscopic Survey (KROSS): The Tully-Fisher Relation at z ˜ 1

Alfred L. Tiley, John P. Stott, A. M. Swinbank, Martin Bureau, Chris M. Harrison, Richard Bower, Helen L. Johnson, Andrew J. Bunker, Matt J. Jarvis, Georgios Magdis, Ray Sharples, Ian Smail, David Sobral, Philip Best

Research output: Contribution to journalArticlepeer-review


We present the stellar mass (M★), and K-corrected K-band absolute magnitude (MK) Tully-Fisher relations (TFRs) for sub-samples of the 584 galaxies spatially resolved in Hα emission by the KMOS Redshift One Spectroscopic Survey (KROSS). We model the velocity field of each of the KROSS galaxies and extract a rotation velocity, V80 at a radius equal to the major axis of an ellipse containing 80% of the total integrated Hα flux. The large sample size of KROSS allowed us to select 210 galaxies with well measured rotation speeds. We extract from this sample a further 56 galaxies that are rotationally supported, using the stringent criterion V80/σ > 3, where σ is the flux weighted average velocity dispersion. We find the MK and M★ TFRs for this sub-sample to be MK / {mag}= (-7.3 ± 0.9) × [(log (V_{80}/{km s^{-1}})-2.25]- 23.4 ± 0.2 , and log (M_{*} / M_{⊙})= (4.7 ± 0.4) × [(log (V_{80}/{km s^{-1}}) - 2.25] + 10.0 ± 0.3, respectively. We find an evolution of the M★ TFR zero-point of -0.41 ± 0.08 dex over the last ˜8 billion years. However, we measure no evolution in the MK TFR zero-point over the same period. We conclude that rotationally supported galaxies of a given dynamical mass had less stellar mass at z ˜ 1 than the present day, yet emitted the same amounts of K-band light. The ability of KROSS to differentiate, using integral field spectroscopy with KMOS, between those galaxies that are rotationally supported and those that are not explains why our findings are at odds with previous studies without the same capabilities.
Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Early online date21 Apr 2016
Publication statusE-pub ahead of print - 21 Apr 2016


  • galaxies: evolution
  • galaxies: general
  • galaxies: kinematics and dynamics


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