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6 results on '"Trebitsch M"'

1. Formation of compact galaxies in the Extreme-Horizon simulation.

Author

Chabanier, S., Bournaud, F., Dubois, Y., Codis, S., Chapon, D., Elbaz, D., Pichon, C., Bressand, O., Devriendt, J., Gavazzi, R., Kraljic, K., Kimm, T., Laigle, C., Lekien, J.-B., Martin, G., Palanque-Delabrouille, N., Peirani, S., Piserchia, P.-F., Slyz, A., and Trebitsch, M.

Subjects
INTERSTELLAR medium, STELLAR mass, ACTIVE galactic nuclei, GALACTIC redshift, GAS flow, STAR formation, GALAXY formation
Abstract

We present the Extreme-Horizon (EH) cosmological simulation, which models galaxy formation with stellar and active galactic nuclei (AGN) feedback and uses a very high resolution in the intergalactic and circumgalactic medium. Its high resolution in low-density regions results in smaller-size massive galaxies at a redshift of z = 2, which is in better agreement with observations compared to other simulations. We achieve this result thanks to the improved modeling of cold gas flows accreting onto galaxies. In addition, the EH simulation forms a population of particularly compact galaxies with stellar masses of 1010−11 M⊙ that are reminiscent of observed ultracompact galaxies at z ≃ 2. These objects form primarily through repeated major mergers of low-mass progenitors and independently of baryonic feedback mechanisms. This formation process can be missed in simulations with insufficient resolution in low-density intergalactic regions. [ABSTRACT FROM AUTHOR]

Published
2020
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2. RASCAS: RAdiation SCattering in Astrophysical Simulations.

Author

Michel-Dansac, L., Blaizot, J., Garel, T., Verhamme, A., Kimm, T., and Trebitsch, M.

Subjects
MONTE Carlo method, ASTROPHYSICAL radiation, RADIATIVE transfer equation, RADIATIVE transfer, PHOTON scattering, OPTICAL depth (Astrophysics), INTERSTELLAR medium
Abstract

Context. Resonant lines are powerful probes of the interstellar and circumgalactic medium of galaxies. Their transfer in gas being a complex process, the interpretation of their observational signatures, either in absorption or in emission, is often not straightforward. Numerical radiative transfer simulations are needed to accurately describe the travel of resonant line photons in real and in frequency space, and to produce realistic mock observations. Aims. This paper introduces RASCAS, a new public 3D radiative transfer code developed to perform the propagation of any resonant line in numerical simulations of astrophysical objects. RASCAS was designed to be easily customisable and to process simulations of arbitrarily large sizes on large supercomputers. Methods. RASCAS performs radiative transfer on an adaptive mesh with an octree structure using the Monte Carlo technique. RASCAS features full MPI parallelisation, domain decomposition, adaptive load-balancing, and a standard peeling algorithm to construct mock observations. The radiative transport of resonant line photons through different mixes of species (e.g. Hi, Si ii, Mgii, Fe ii), including their interaction with dust, is implemented in a modular fashion to allow new transitions to be easily added to the code. Results. RASCAS is very accurate and efficient. It shows perfect scaling up to a minimum of a thousand cores. It has been fully tested against radiative transfer problems with analytic solutions and against various test cases proposed in the literature. Although it was designed to describe accurately the many scatterings of line photons, RASCAS may also be used to propagate photons at any wavelength (e.g. stellar continuum or fluorescent lines), or to cast millions of rays to integrate the optical depths of ionising photons, making it highly versatile. [ABSTRACT FROM AUTHOR]

Published
2020
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3. Modeling small galaxies during the Epoch of Reionisation

Author

Trebitsch, M., Blaizot, J., and Rosdahl, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Small galaxies are thought to be the main contributors to the ionising budget of the Universe before reionisation was complete. There have been a number of numerical studies trying to quantify their ionising efficiency through the escape fraction $f_{esc}$. While there is a clear trend that $f_{esc}$ is higher for smaller haloes, there is a large scatter in the distribution of $f_{esc}$ for a single halo mass. We propose that this is due to the intrinsic burstiness of star formation in low mass galaxies. We performed high resolution radiative hydrodynamics simulations with Ramses-RT to model the evolution of three galaxies and their ionising efficiency. We found that the variability of $f_{esc}$ follows that of the star formation rate. We then discuss the consequences of this variability on the observability of such galaxies by JWST., 4 pages, 3 figures, to appear in the proceedings of SF2A 2015

Published
2015

4. Black hole mergers from dwarf to massive galaxies with the NewHorizon and Horizon-AGN simulations

Author

R. A. Jackson, Christopher J. Conselice, Marta Volonteri, Sukyoung K. Yi, Maxime Trebitsch, Christophe Pichon, R. S. Beckmann, Monica Colpi, Katarina Kraljic, Sébastien Peirani, Yohan Dubois, Garreth Martin, Hugo Pfister, Julien Devriendt, Massimo Dotti, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Dipartimento di Fisica 'Giuseppe Occhialini' = Department of Physics 'Giuseppe Occhialini' [Milano-Bicocca], Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Istituto Nazionale di Fisica Nucleare, Universita Milano-Bicocca (INFN), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)- Istituto Nazionale di Fisica Nucleare (INFN), Centre for Astronomy and Particle Theory, University of Nottingham, Steward Observatory, University of Arizona, Korea Astronomy and Space Science Institute (KASI), Okayama University, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Yonsei University Observatory, Oxford Astrophysics, University of Oxford [Oxford], Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Volonteri, M, Pfister, H, Beckmann, R, Dubois, Y, Colpi, M, Conselice, C, Dotti, M, Martin, G, Jackson, R, Kraljic, K, Pichon, C, Trebitsch, M, Yi, S, Devriendt, J, and Peirani, S

Subjects
ACTIVE GALACTIC NUCLEI, Time delays, Population, FOS: Physical sciences, ORBITAL DECAY, FREQUENCY GRAVITATIONAL-WAVES, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, DARK, STAR-FORMATION, Physical cosmology, methods: numerical, Pulsar, 0103 physical sciences, Dynamical friction, education, POST-NEWTONIAN EVOLUTION, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, ILLUSTRIS PROJECT, education.field_of_study, Quasars: supermassive black hole, 010308 nuclear & particles physics, Gravitational wave, supermassive black holes [quasars], quasars: supermassive black holes, numerical [methods], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, BINARY-SYSTEMS, COSMOLOGICAL SIMULATIONS, gravitational waves, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), GROWTH, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Massive black hole (MBH) coalescences are powerful sources of low-frequency gravitational waves. To study these events in the cosmological context we need to trace the large-scale structure and cosmic evolution of a statistical population of galaxies, from dim dwarfs to bright galaxies. To cover such a large range of galaxy masses, we analyse two complementary simulations: Horizon-AGN with a large volume and low resolution which tracks the high-mass (> 1e7 Msun) MBH population, and NewHorizon with a smaller volume but higher resolution that traces the low-mass (< 1e7 Msun) MBH population. While Horizon-AGN can be used to estimate the rate of inspirals for Pulsar Timing Arrays, NewHorizon can investigate MBH mergers in a statistical sample of dwarf galaxies for LISA, which is sensitive to low-mass MBHs. We use the same method to analyse the two simulations, post-processing MBH dynamics to account for time delays mostly determined by dynamical friction and stellar hardening. In both simulations, MBHs typically merge long after the galaxies do, so that the galaxy morphology at the time of the MBH merger is no longer determined by the galaxy merger from which the MBH merger originated. These time delays cause a loss of high-z MBH coalescences, shifting the peak of the MBH merger rate to z~1-2. This study shows how tracking MBH mergers in low-mass galaxies is crucial to probing the MBH merger rate for LISA and investigate the properties of the host galaxies., MNRAS in press

Published
2020

5. Super-Eddington accretion and feedback from the first massive seed black holes

Author

Alessandro Lupi, R. S. Beckmann, Maxime Trebitsch, John A. Regan, Turlough P. Downes, Marta Volonteri, Yohan Dubois, Interactions Sol Plante Atmosphère (UMR ISPA), Institut National de la Recherche Agronomique (INRA)-Ecole Nationale Supérieure des Sciences Agronomiques de Bordeaux-Aquitaine (Bordeaux Sciences Agro), School of Mathematical Science, Dublin City University [Dublin] (DCU), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Interactions Sol Plante Atmosphère (ISPA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Regan, J, Downes, T, Volonteri, M, Beckmann, R, Lupi, A, Trebitsch, M, Dubois, Y, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and ANR-16-CE31-0011,LYRICS,Le cycle du gaz autour des galaxies : origine et conditions physiques des flots de gaz froid(2016)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Mass loading, methods: numerical, Accretion rate, General Relativity and Quantum Cosmology, cosmology: theory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, Supermassive black hole, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Black hole, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo, large-scale structure of Universe
Abstract

Super-Eddington accretion onto massive black hole seeds may be commonplace in the early Universe, where the conditions exist for rapid accretion. Direct collapse black holes are often invoked as a possible solution to the observation of super massive black holes (SMBHs) in the pre-reionisation Universe. We investigate here how feedback, mainly in the form of bipolar jets, from super-Eddington accreting seed black holes will affect their subsequent growth. We find that, nearly independent of the mass loading of the bipolar jets, the violent outflows generated by the jets evacuate a region of approximately 0.1 pc surrounding the black hole seed. However, the jet outflows are unable to break free of the halo and their impact is limited to the immediate vicinity of the black hole. The outflows suppress any accretion for approximately a dynamical time. The gas then cools, recombines and falls back to the centre where high accretion rates are again observed. The overall effect is to create an effective accretion rate with values of between 0.1 and 0.5 times the Eddington rate. If this episodic accretion rate is maintained for order 500 million years then the black hole will increase in mass by a factor of between 3 and 300 but far short of the factor of $10^4$ required for the seeds to become the SMBHs observed at $z>6$. Therefore, direct collapse black holes born into atomic cooling haloes and which experience strong negative mechanical feedback will require external influences (e.g. rapid major mergers with other haloes) to promote efficient accretion and reach SMBH masses within a few hundred million years., 16 pages. MNRAS accepted

Published
2019

6. Detection of stellar light from quasar host galaxies at redshifts above 6.

Author

Ding X, Onoue M, Silverman JD, Matsuoka Y, Izumi T, Strauss MA, Jahnke K, Phillips CL, Li J, Volonteri M, Haiman Z, Andika IT, Aoki K, Baba S, Bieri R, Bosman SEI, Bottrell C, Eilers AC, Fujimoto S, Habouzit M, Imanishi M, Inayoshi K, Iwasawa K, Kashikawa N, Kawaguchi T, Kohno K, Lee CH, Lupi A, Lyu J, Nagao T, Overzier R, Schindler JT, Schramm M, Shimasaku K, Toba Y, Trakhtenbrot B, Trebitsch M, Treu T, Umehata H, Venemans BP, Vestergaard M, Walter F, Wang F, and Yang J

Abstract

The detection of starlight from the host galaxies of quasars during the reionization epoch (z > 6) has been elusive, even with deep Hubble Space Telescope observations 1,2 . The current highest redshift quasar host detected 3 , at z = 4.5, required the magnifying effect of a foreground lensing galaxy. Low-luminosity quasars 4-6 from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) 7 mitigate the challenge of detecting their underlying, previously undetected host galaxies. Here we report rest-frame optical images and spectroscopy of two HSC-SSP quasars at z > 6 with the JWST. Using near-infrared camera imaging at 3.6 and 1.5 μm and subtracting the light from the unresolved quasars, we find that the host galaxies are massive (stellar masses of 13 × and 3.4 × 10 10  M ☉ , respectively), compact and disc-like. Near-infrared spectroscopy at medium resolution shows stellar absorption lines in the more massive quasar, confirming the detection of the host. Velocity-broadened gas in the vicinity of these quasars enables measurements of their black hole masses (1.4 × 10 9 and 2.0 × 10 8  M ☉ , respectively). Their location in the black hole mass-stellar mass plane is consistent with the distribution at low redshift, suggesting that the relation between black holes and their host galaxies was already in place less than a billion years after the Big Bang., (© 2023. The Author(s), under exclusive licence to Springer Nature Limited.)

Published
2023
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