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Black Hole

Lensing of space time around a black hole. At Oxford we study black holes observationally and theoretically on all size and time scales - it is some of our core work.

Credit: ALAIN RIAZUELO, IAP/UPMC/CNRS. CLICK HERE TO VIEW MORE IMAGES.

Professor Roger Davies

Emeritus Wetton Professor

Research theme

  • Astronomy and astrophysics
  • Instrumentation

Sub department

  • Astrophysics

Research groups

  • Astronomical instrumentation
  • Cosmology
  • Galaxy formation and evolution
  • Hintze Centre for Astrophysical Surveys
  • Rubin-LSST
  • Extremely Large Telescope
Roger.Davies@physics.ox.ac.uk
  • About
  • Publications

Distribution of slow and fast rotators in the Fornax cluster

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 441:1 (2014) 274-288

Authors:

Nicholas Scott, Roger L Davies, Ryan CW Houghton, Michele Cappellari, Alister W Graham, Kevin A Pimbblet
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THE SINS/zC-SINF SURVEY OF z ∼ 2 GALAXY KINEMATICS: EVIDENCE FOR POWERFUL ACTIVE GALACTIC NUCLEUS-DRIVEN NUCLEAR OUTFLOWS IN MASSIVE STAR-FORMING GALAXIES**Based on observations obtained at the Very Large Telescope of the European Southern Observatory, Paranal, Chile (ESO program IDs 074.A-0911, 075.A-0466, 076.A-0527, 078.A-0600, 082.A-0396, 183.A-0781, 088.A-0202, 091.A-0126). Also based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555; these observations are associated with GO programs Nos. 10924 and 12578.

The Astrophysical Journal American Astronomical Society 787:1 (2014) 38

Authors:

NM Förster Schreiber, R Genzel, SF Newman, JD Kurk, D Lutz, LJ Tacconi, S Wuyts, K Bandara, A Burkert, P Buschkamp, CM Carollo, G Cresci, E Daddi, R Davies, F Eisenhauer, EKS Hicks, P Lang, SJ Lilly, V Mainieri, C Mancini, T Naab, Y Peng, A Renzini, D Rosario, K Shapiro Griffin, AE Shapley, A Sternberg, S Tacchella, D Vergani, E Wisnioski, E Wuyts, G Zamorani
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THE SINS/zC-SINF SURVEY OF z ∼ 2 GALAXY KINEMATICS: EVIDENCE FOR GRAVITATIONAL QUENCHING**Based on observations obtained at the Very Large Telescope of the European Southern Observatory, Paranal, Chile (ESO program IDs 076.A-0527, 079.A-0341, 080.A-0330, 080.A-0339, 080.A-0635, 081.A-0672, 082.A-0396, 183.A-0781, 087.A-0081, 088.A-0202, 088.A-0202, 088.A-0209, 091.A-0126). Also based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555 (GO programs Nos. 10924 and 12587).

The Astrophysical Journal American Astronomical Society 785:1 (2014) 75

Authors:

R Genzel, NM Förster Schreiber, P Lang, S Tacchella, LJ Tacconi, S Wuyts, K Bandara, A Burkert, P Buschkamp, CM Carollo, G Cresci, R Davies, F Eisenhauer, EKS Hicks, J Kurk, SJ Lilly, D Lutz, C Mancini, T Naab, S Newman, Y Peng, A Renzini, K Shapiro Griffin, A Sternberg, D Vergani, E Wisnioski, E Wuyts, G Zamorani
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NGC 1266 as a local candidate for rapid cessation of star formation

Astrophysical Journal 780:2 (2014)

Authors:

K Alatalo, K Nyland, G Graves, S Deustua, KS Griffin, PA Duc, M Cappellari, RM McDermid, TA Davis, AF Crocker, LM Young, P Chang, N Scott, SL Cales, E Bayet, L Blitz, M Bois, F Bournaud, M Bureau, RL Davies, PT De Zeeuw, E Emsellem, S Khochfar, D Krajnović, H Kuntschner, R Morganti, T Naab, T Oosterloo, M Sarzi, P Serra, AM Weijmans

Abstract:

We present new Spectrographic Areal Unit for Research on Optical Nebulae (SAURON) integral-field spectroscopy and Swift Ultraviolet Optical Telescope (UVOT) observations of molecular outflow host galaxy NGC 1266 that indicate NGC 1266 has experienced a rapid cessation of star formation. Both the SAURON maps of stellar population age and the Swift UVOT observations demonstrate the presence of young (<1 Gyr) stellar populations within the central 1 kpc, while existing Combined Array for Research in Millimeter-Wave Astronomy CO(1-0) maps indicate that the sites of current star formation are constrained to only the inner few hundred parsecs of the galaxy. The optical spectrum of NGC 1266 from Moustakas & Kennicutt reveal a characteristic poststarburst (K+A) stellar population, and Davis et al. confirm that ionized gas emission in the system originate from a shock. Galaxies with K+A spectra and shock-like ionized gas line ratios may comprise an important, overlooked segment of the poststarburst population, containing exactly those objects in which the active galactic nucleus (AGN) is actively expelling the star-forming material. While AGN activity is not the likely driver of the poststarburst event that occurred 500 Myr ago, the faint spiral structure seen in the Hubble Space Telescope Wide-field Camera 3 Y-, J- and H-band imaging seems to point to the possibility of gravitational torques being the culprit. If the molecular gas were driven into the center at the same time as the larger scale galaxy disk underwent quenching, the AGN might be able to sustain the presence of molecular gas for ≳ 1 Gyr by cyclically injecting turbulent energy into the dense molecular gas via a radio jet, inhibiting star formation. © 2014. The American Astronomical Society. All rights reserved.
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How typical is the Coma cluster?

Monthly Notices of the Royal Astronomical Society 438:4 (2014) 3049-3057

Authors:

KA Pimbblet, SJ Penny, RL Davies

Abstract:

Coma is frequently used as the archetype z ∼ 0 galaxy cluster to compare higher redshift work against. It is not clear, however, how representative the Coma cluster is for galaxy clusters of its mass or X-ray luminosity, and significantly, recent works have suggested that the galaxy population of Coma may be in some ways anomalous. In this work, we present a comparison of Coma to an X-ray-selected control sample of clusters. We show that although Coma is typical against the control sample in terms of its internal kinematics (sub-structure and velocity dispersion profile), it has a significantly high (∼3σ) X-ray temperature set against clusters of comparable mass. By de-redshifting our control sample cluster galaxies star formation rates using a fit to the galaxy main-sequence evolution at z < 0.1, we determine that the typical star formation rate of Coma galaxies as a function of mass is higher than for galaxies in our control sample at a confidence level of >99 per cent. One way to alleviate this discrepancy and bring Coma in line with the control sample would be to have the distance to Coma to be slightly lower, perhaps through a non-negligible peculiar velocity with respect to the Hubble expansion, but we do not regard this as likely given precision measurements using a variety of approaches. Therefore, in summary, we urge caution in using Coma as a z ∼ 0 baseline cluster in galaxy evolution studies. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
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