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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.

Dr Harley Katz

Visitor

Sub department

  • Astrophysics
harley.katz@physics.ox.ac.uk
Telephone: 01865 273348
Denys Wilkinson Building, room 532D
  • About
  • Publications

The Obelisk simulation: galaxies contribute more than AGN to HI reionization of protoclusters

(2020)

Authors:

Maxime Trebitsch, Yohan Dubois, Marta Volonteri, Hugo Pfister, Corentin Cadiou, Harley Katz, Joakim Rosdahl, Taysun Kimm, Christophe Pichon, Ricarda S Beckmann, Julien Devriendt, Adrianne Slyz

Abstract:

We present the Obelisk project, a cosmological radiation-hydrodynamics simulation following the assembly and reionization of a protocluster progenitor during the first two billions of years from the big bang, down to z = 3.5. The simulation resolves haloes down to the atomic cooling limit, and tracks the contribution of different sources of ionization: stars, active galactic nuclei, and collisions. The Obelisk project is designed specifically to study the coevolution of high redshift galaxies and quasars in an environment favouring black hole growth. In this paper, we establish the relative contribution of these two sources of radiation to reionization and their respective role in establishing and maintaining the high redshift ionizing background. Our volume is typical of an overdense region of the Universe and displays star formation rate and black hole accretion rate densities similar to high redshift protoclusters. We find that hydrogen reionization happens inside-out and is completed by z ∼ 6 in our overdensity, and is predominantly driven by galaxies, while accreting black holes only play a role at z ∼ 4.
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The absence of [C ii] 158 $\mu$m emission in spectroscopically confirmed galaxies at z > 8

Monthly Notices of the Royal Astronomical Society: Letters Oxford University Press (OUP) 487:1 (2019) l81-l85

Authors:

N Laporte, H Katz, RS Ellis, G Lagache, FE Bauer, F Boone, AK Inoue, T Hashimoto, H Matsuo, K Mawatari, Y Tamura
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Understanding the escape of LyC and Lyα photons from turbulent clouds

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 486:2 (2019) 2215-2237

Authors:

Taysun Kimm, Jérémy Blaizot, Thibault Garel, Léo Michel-Dansac, Harley Katz, Joakim Rosdahl, Anne Verhamme, Martin Haehnelt
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Black hole formation in the first stellar clusters

Chapter in Formation of the First Black Holes, World Scientific Publishing (2019) 125-143
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The baryonic Tully–Fisher relation for different velocity definitions and implications for galaxy angular momentum

Monthly Notices of the Royal Astronomical Society Oxford University Press 484:3 (2019) 3267-3278

Authors:

F Lelli, SS McGaugh, JM Schombert, Harry Desmond, Harley Katz

Abstract:

We study the baryonic Tully–Fisher relation (BTFR) at z ≃ 0 using 153 galaxies from the Spitzer Photometry and Accurate Rotation Curve sample. We consider different definitions of the characteristic velocity from H I and H α rotation curves, as well as H I line-widths from single-dish observations. We reach the following results: (1) The tightest BTFR is given by the mean velocity along the flat part of the rotation curve. The orthogonal intrinsic scatter is extremely small (⁠∼6 per cent⁠) and the best-fitting slope is 3.85 ± 0.09, but systematic uncertainties may drive the slope from 3.5 to 4.0. Other velocity definitions lead to BTFRs with systematically higher scatters and shallower slopes. (2) We provide statistical relations to infer the flat rotation velocity from H I line-widths or less extended rotation curves (like H α and CO data). These can be useful to study the BTFR from large H I surveys or the BTFR at high redshifts. (3) The BTFR is more fundamental than the relation between angular momentum and galaxy mass (the Fall relation). The Fall relation has about seven times more scatter than the BTFR, which is merely driven by the scatter in the mass-size relation of galaxies. The BTFR is already the ‘Fundamental Plane’ of galaxy discs: no value is added with a radial variable as a third parameter.
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