Portrait of Mathieu Marquis

Mathieu Marquis

mathieu.marquis@mila.quebec
Master's Research - Université de Montréal
Supervisor
Julie Hlavacek-Larrondo
Research Topics
Astronomy
Astrophysics
Galaxy Evolution
GitHub

Publications

JWST Reveals How Black Holes are Fed: Kiloparsec-scale Multiphase Filaments Feed Subkiloparsec Circumnuclear Disks
Julie Hlavacek-Larrondo
Hyunseop Choi
Minghao Guo
Mathieu Marquis
Olivia Pereira
G. Mark Voit
Loïc Albert
J. K. Barrera-Ballesteros
Rebecca Canning
Francesco D’Eugenio
Megan E. Donahue
A. C. Fabian
G. J. Ferland
John S. Gallagher
Marie-Lou Gendron-Marsolais
P. Guillard
Nina Hatch
Ralf Kotulla
Yuan Li
R. Maiolino … (see 18 more)
Allison W. S. Man
M. McDonald
B R McNamara
Valeria Olivares
Marine Prunier
Michael Reefe
Christopher S. Reynolds
Carter Lee Rhea
A. Richard-Laferrière
H. R. Russell
P. Salomé
Ming Sun
Prathamesh Tamhane
Greg B Taylor
Auriane Thilloy
Grant R Tremblay
Benjamin Vigneron
S A Walker
Abstract The Centaurus cluster is one of the most important archetypes of radio-mode active galactic nucleus (AGN) feedback, with its centra… (see more)l galaxy, NGC 4696, launching powerful jets that inflate X-ray cavities and regulate cooling and star formation. NGC 4696 lies within a spectacular multiphase nebula of filaments extending over tens of kiloparsecs and spanning 6 decades in temperature, from hot (10 8 K) X-ray-emitting plasma to cold molecular gas. Owing to its proximity, Hubble Space Telescope H α imaging reveals a striking S-shaped ionized-gas swirl within the black hole’s sphere of influence—the first such structure identified in a cluster core. Here we present the first JWST observations of NGC 4696 with NIRSpec, probing the inner 618 × 618 pc at 10 pc resolution. These data reveal that the ionized swirl is a rotating, multiphase circumnuclear disk (CND) physically and kinematically connected to the larger-scale filamentary network. This provides the long-sought missing link between kiloparsec-scale cooling flows and black hole accretion on 100 pc scales. Strikingly, the observed morphology and kinematics are reproduced by tailored magnetohydrodynamic simulations, in which fila
2026-07-13
Astrophysical Journal Letters (published)
doi.org