A unified pseudo-Cℓ framework

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2019)

Authors:

David Alonso, Javier Sanchez, Anže Slosar

Black hole evolution: II. Spinning black holes in a supernova-driven turbulent interstellar medium

Monthly Notices of the Royal Astronomical Society Oxford University Press 440:3 (2014) 2333-2346

Authors:

Y Dubois, M Volonteri, J Silk, Julien Devriendt, Adrianne Slyz

Abstract:

Supermassive black holes (BH) accrete gas from their surroundings and coalesce with companions during galaxy mergers, and both processes change the BH mass and spin. By means of high-resolution hydrodynamical simulations of galaxies, either idealised or embedded within the cosmic web, we explore the effects of interstellar gas dynamics and external perturbations on BH spin evolution. All these physical quantities were evolved on-the-fly in a self-consistent manner. We use a 'maximal' model to describe the turbulence induced by stellar feedback to highlight its impact on the angular momentum of the gas accreted by the BH. Periods of intense star formation are followed by phases where stellar feedback drives large-scale outflows and hot bubbles. We find that BH accretion is synchronised with star formation, as only when gas is cold and dense do both processes take place. During such periods, gas motion is dominated by consistent rotation. On the other hand, when stellar feedback becomes substantial, turbulent motion randomises gas angular momentum. However BH accretion is strongly suppressed in that case, as cold and dense gas is lacking. In our cosmological simulation, at very early times (z>6), the galactic disc has not yet settled and no preferred direction exists for the angular momentum of the accreted gas, so the BH spin remains low. As the gas settles into a disc (6>z>3), the BH spin then rapidly reaches its maximal value. At lower redshifts (z<3), even when galaxy mergers flip the direction of the angular momentum of the accreted gas, causing it to counter-rotate, the BH spin magnitude only decreases modestly and temporarily. Should this be a typical evolution scenario for BH, it potentially has dramatic consequences regarding their origin and assembly, as accretion on maximally spinning BH embedded in thin Shakura-Sunyaev disc is significantly reduced.

Black hole evolution: II. Spinning black holes in a supernova-driven turbulent interstellar medium

Monthly Notices of the Royal Astronomical Society Oxford University Press 440:3 (2014) 2333-2346

Authors:

Y Dubois, M Volonteri, J Silk, Julien Devriendt, Adrianne Slyz

Abstract:

Supermassive black holes (BH) accrete gas from their surroundings and coalesce with companions during galaxy mergers, and both processes change the BH mass and spin. By means of high-resolution hydrodynamical simulations of galaxies, either idealised or embedded within the cosmic web, we explore the effects of interstellar gas dynamics and external perturbations on BH spin evolution. All these physical quantities were evolved on-the-fly in a self-consistent manner. We use a 'maximal' model to describe the turbulence induced by stellar feedback to highlight its impact on the angular momentum of the gas accreted by the BH. Periods of intense star formation are followed by phases where stellar feedback drives large-scale outflows and hot bubbles. We find that BH accretion is synchronised with star formation, as only when gas is cold and dense do both processes take place. During such periods, gas motion is dominated by consistent rotation. On the other hand, when stellar feedback becomes substantial, turbulent motion randomises gas angular momentum. However BH accretion is strongly suppressed in that case, as cold and dense gas is lacking. In our cosmological simulation, at very early times (z>6), the galactic disc has not yet settled and no preferred direction exists for the angular momentum of the accreted gas, so the BH spin remains low. As the gas settles into a disc (6>z>3), the BH spin then rapidly reaches its maximal value. At lower redshifts (z<3), even when galaxy mergers flip the direction of the angular momentum of the accreted gas, causing it to counter-rotate, the BH spin magnitude only decreases modestly and temporarily. Should this be a typical evolution scenario for BH, it potentially has dramatic consequences regarding their origin and assembly, as accretion on maximally spinning BH embedded in thin Shakura-Sunyaev disc is significantly reduced.

MIGHTEE-HI: The baryonic Tully-Fisher relation over the last billion years

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2021)

Authors:

Anastasia A Ponomareva, Wanga Mulaudzi, Natasha Maddox, Bradley S Frank, Matt J Jarvis, Enrico M Di Teodoro, Marcin Glowacki, Renée C Kraan-Korteweg, Tom A Oosterloo, Elizabeth AK Adams, Hengxing Pan, Isabella Prandoni, Sambatriniaina HA Rajohnson, Francesco Sinigaglia, Nathan J Adams, Ian Heywood, Rebecca AA Bowler, Peter W Hatfield, Jordan D Collier, Srikrishna Sekhar

Abstract:

Abstract Using a sample of 67 galaxies from the MIGHTEE Survey Early Science data we study the H i-based baryonic Tully-Fisher relation (bTFr), covering a period of ∼one billion years (0 ≤ z ≤ 0.081). We consider the bTFr based on two different rotational velocity measures: the width of the global H i profile and Vout, measured as the outermost rotational velocity from the resolved H i rotation curves. Both relations exhibit very low intrinsic scatter orthogonal to the best-fit relation (σ⊥ = 0.07 ± 0.01), comparable to the SPARC sample at z ≃ 0. The slopes of the relations are similar and consistent with the z ≃ 0 studies ($3.66^{+0.35}_{-0.29}$ for W50 and $3.47^{+0.37}_{-0.30}$ for Vout). We find no evidence that the bTFr has evolved over the last billion years, and all galaxies in our sample are consistent with the same relation independent of redshift and the rotational velocity measure. Our results set up a reference for all future studies of the H i-based bTFr as a function of redshift that will be conducted with the ongoing deep SKA pathfinders surveys.

Erratum: Secularly powered outflows from AGNs: The dominance of non-merger driven supermassive black hole growth (Monthly Notices of the Royal Astronomical Society DOI: 10.1093/jeea/stz2443)

Monthly Notices of the Royal Astronomical Society 506:3 (2021) 3419-3420

Authors:

RJ Smethurst, BD Simmons, CJ Lintott, J Shanahan, AL Coil, WC Keel, E Glikman, EC Moran, KL Masters, M Urry, K Willett

Abstract:

(Table Presented) In Smethurst et al. (2019), the [OIII] gas masses in outflows from 12 disk-dominated AGN were calculated using narrowband imaging from the Shane-3m. An error in the standard star flux calibration resulted in the over estimate of the flux in each image by three orders of magnitude. Due to the intricacies of the reduction of the individual sources, this resulted in an overestimate in the range 1.3 - 3.9 dex (with an average of 2.6 dex) of the calculated [OIII] gas masses. This error propagated through to give a typical overestimate of the outflow rates (and in turn the inflow rates) of 2.6 dex. Despite this, all of the conclusions of Smethurst et al. (2019) still hold and are in fact made stronger. Including, that secular mechanisms are more than sufficient to both grow a SMBH and power an outflow from the AGN, and this results in different accretion and outflow properties compared to the merger dominated sample of Bae et al. (2017). We provide the correct gas masses, outflow rates and inflow rates in Table 1 below. The mean outflow rate for the DISK-DOMOUTFLOW sample is now 0.0020 ± 0.0005 M⊙ yr-1. For an updated study please see Smethurst et al. (2021; submitted). Please note, we have also added authors who were involved in the data acquisition but were omitted from the original author list.