Stellar Dynamics and Star Formation Histories of z ∼ 1 Radio-loud Galaxies

Barišić, Ivana; Wel, Arjen van der; Bezanson, Rachel; Pacifici, Camilla; Noeske, K. G.; Muñoz-Mateos, J. C.; Franx, Marijn; Smolčić, Vernesa; Bell, Eric F.; Brammer, Gabriel; Calhau, João; Chauké, Priscilla; Dokkum, Pieter van; Houdt, Josha van; Gallazzi, Anna; Labbé, Ivo; Maseda, Michael V.; Muzzin, Adam; Sobral, David; Straatman, Caroline; Wu, Po-Feng

doi:10.3847/1538-4357/aa8768

Cited by 37 publications

(38 citation statements)

References 60 publications

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“…with a cap to the velocity increase at 7000 km s −1 . Additionally, a criterion requiring M BH > M BH,lim is added and motivated by observations that show that jets only arise in galaxies with velocity dispersions corresponding to black holes with M BH 10 8 M (McLure & Jarvis 2004; Barišić et al 2017). We conservatively choose M BH,lim = 10 7.5 M .…”

Section: Kinetic Feedbackmentioning

confidence: 99%

Black hole – Galaxy correlations in simba

Thomas

Davé

Anglés-Alcázar

et al. 2019

Monthly Notices of the Royal Astronomical Society

100

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We examine the co-evolution of galaxies and supermassive black holes in the Simba cosmological hydrodynamic simulation. Simba grows black holes via gravitational torque-limited accretion from cold gas and Bondi accretion from hot gas, while feedback from black holes is modeled in radiative and jet modes depending on the Eddington ratio ( f Edd ). Simba shows generally good agreement with local studies of black hole properties, such as the black hole mass-stellar velocity dispersion (M BH − σ) relation, the black hole accretion rate vs. star formation rate (BHAR-SFR), and the black hole mass function. M BH − σ evolves such that galaxies at a given M BH have higher σ at higher redshift, consistent with no evolution in M BH − M . For M BH < ∼ 10 8 M , f Edd is anti-correlated with M BH since the BHAR is approximately independent of M BH , while at higher masses f Edd − M BH flattens and has a larger scatter. BHAR vs. SFR is invariant with redshift, but f Edd drops steadily with time at a given M BH , such that all but the most massive black holes are accreting in a radiatively efficient mode at z > ∼ 2. The black hole mass function amplitude decreases with redshift and is locally dominated by quiescent galaxies for M BH > 10 8 M , but for z > ∼ 1 star forming galaxies dominate at all M BH . The z = 0 f Edd distribution is roughly lognormal with a peak at f Edd < ∼ 0.01 as observed, shifting to higher f Edd at higher redshifts. Finally, we study the dependence of black hole properties with H i content and find that the correlation between gas content and star formation rate is modulated by black hole properties, such that higher SFR galaxies at a given gas content have smaller black holes with higher f Edd .

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Section: Kinetic Feedbackmentioning

confidence: 99%

Black hole – Galaxy correlations in simba

Thomas

Davé

Anglés-Alcázar

et al. 2019

Monthly Notices of the Royal Astronomical Society

100

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“…PSB galaxies are much smaller than star-forming galaxies with the same EW(Hδ). Barišić et al 2017). The star-formation rates thus gradually drop as the cold gas reservoir depletes.…”

Section: Slow Process Large Young Quiescent Galaxiesmentioning

confidence: 99%

Fast and Slow Paths to Quiescence: Ages and Sizes of 400 Quiescent Galaxies from the LEGA-C Survey

Wel

Bezanson

et al. 2018

ApJ

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102

104

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We analyze stellar age indicators (D n 4000 and EW(Hδ)) and sizes of 467 quiescent galaxies with M * ≥ 10 10 M at z ∼ 0.7 drawn from DR2 of the LEGA-C survey. Interpreting index variations in terms of equivalent single stellar population age, we find that the median stellar population is younger for larger galaxies at fixed stellar mass. The effect is significant, yet small; the ages of the larger and the smaller subsets differ by only < 500 Myr, much less than the age variation among individual galaxies (∼ 1.5 Gyr). At the same time, post-starburst galaxies -those experienced recent and rapid quenching events -are much smaller than expected based on the global correlation between age and size of normal quiescent galaxies. These co-existing trends unify seemingly contradictory results in the literature; the complex correlations between size and age indicators revealed by our large sample of galaxies with high-quality spectra suggest that there are multiple evolutionary pathways to quiescence. Regardless of the specific physical mechanisms responsible for the cessation of star formation in massive galaxies, the large scatter in D n 4000 and EW(Hδ) immediately implies that galaxies follow a large variety in evolutionary pathways. On the one hand, we see evidence for a process that slowly shuts off star-formation and transforms star-forming galaxies to quiescent galaxies without necessarily changing their structures. On the other hand, there is likely a mechanism that rapidly quenches galaxies, an event that coincides with dramatic structural changes, producing post-starburst galaxies that can be smaller than their progenitors.

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“…by the direct correlation between BH mass and SF activity (e.g., Terrazas et al 2016) and the large fraction of radio AGN among galaxies with large velocity dispersions both at low and high redshift (e.g., Best et al 2005;Barišić et al 2017).…”

Section: General Trendsmentioning

confidence: 99%

Star Formation Histories of z ∼ 1 Galaxies in LEGA-C

Chauké

Wel

Pacifici

et al. 2018

ApJ

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Using high resolution spectra from the VLT LEGA-C program, we reconstruct the star formation histories (SFHs) of 607 galaxies at redshifts z = 0.6 − 1.0 and stellar masses 10 10 M using a custom full spectrum fitting algorithm that incorporates the emcee and FSPS packages. We show that the mass-weighted age of a galaxy correlates strongly with stellar velocity dispersion (σ * ) and ongoing star-formation (SF) activity, with the stellar content in higher-σ * galaxies having formed earlier and faster. The SFHs of quiescent galaxies are generally consistent with passive evolution since their main SF epoch, but a minority show clear evidence of a rejuvenation event in their recent past. The mean age of stars in galaxies that are star-forming is generally significantly younger, with SF peaking after z < 1.5 for almost all star-forming galaxies in the sample: many of these still have either constant or rising SFRs on timescales > 100 Myrs. This indicates that z > 2 progenitors of z ∼ 1 star-forming galaxies are generally far less massive. Finally, despite considerable variance in the individual SFHs, we show that the current SF activity of massive galaxies (> L * ) at z ∼ 1 correlates with SF levels at least 3 Gyrs prior: SFHs retain 'memory' on a large fraction of the Hubble time. Our results illustrate a novel approach to resolve the formation phase of galaxies, and in identifying their individual evolutionary paths, connects progenitors and descendants across cosmic time. This is uniquely enabled by the high-quality continuum spectroscopy provided by the LEGA-C survey.

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Stellar Dynamics and Star Formation Histories of z ∼ 1 Radio-loud Galaxies

Cited by 37 publications

References 60 publications

Black hole – Galaxy correlations in simba

Black hole – Galaxy correlations in simba

Fast and Slow Paths to Quiescence: Ages and Sizes of 400 Quiescent Galaxies from the LEGA-C Survey

Star Formation Histories of z ∼ 1 Galaxies in LEGA-C

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