Extragalactic Magnetism with SOFIA (SALSA Legacy Program). VII. A Tomographic View of Far-infrared and Radio Polarimetric Observations through MHD Simulations of Galaxies

The Astrophysical Journal American Astronomical Society 966:1 (2024) 43


Sergio Martin-Alvarez, Enrique Lopez-Rodriguez, Tara Dacunha, Susan E Clark, Alejandro S Borlaff, Rainer Beck, Francisco Rodríguez Montero, Seoyoung L Jung, Julien Devriendt, Adrianne Slyz, Julia Christine Roman-Duval, Evangelia Ntormousi, Mehrnoosh Tahani, Kandaswamy Subramanian, Daniel A Dale, Pamela M Marcum, Konstantinos Tassis, Ignacio del Moral-Castro, Le Ngoc Tram, Matt J Jarvis

Impact of Ejecta Temperature and Mass on the Strength of Heavy Element Signatures in Kilonovae

The Astrophysical Journal American Astronomical Society 967:1 (2024) 54


Donggeun Tak, Z Lucas Uhm, James H Gillanders

WISDOM Project – XIX. Figures of merit for supermassive black hole mass measurements using molecular gas and/or megamaser kinematics

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2024) stae1106-stae1106


Hengyue Zhang, Martin Bureau, Mark D Smith, Michele Cappellari, Timothy A Davis, Pandora Dominiak, Jacob S Elford, Fu-Heng Liang, Ilaria Ruffa, Thomas G Williams


<jats:title>Abstract</jats:title> <jats:p>The mass (MBH) of a supermassive black hole (SMBH) can be measured using spatially-resolved kinematics of the region where the SMBH dominates gravitationally. The most reliable measurements are those that resolve the smallest physical scales around the SMBHs. We consider here three metrics to compare the physical scales probed by kinematic tracers dominated by rotation: the radius of the innermost detected kinematic tracer Rmin normalised by respectively the SMBH’s Schwarzschild radius (RSchw ≡ 2GMBH/c2, where G is the gravitational constant and c the speed of light), sphere-of-influence (SOI) radius ($R_\mathrm{SOI}\equiv GM_\mathrm{BH}/\sigma _\mathrm{e}^2$, where σe is the stellar velocity dispersion within the galaxy’s effective radius) and equality radius (the radius Req at which the SMBH mass equals the enclosed stellar mass, MBH = M*(Req), where M*(R) is the stellar mass enclosed within the radius R). All metrics lead to analogous simple relations between Rmin and the highest circular velocity probed Vc. Adopting these metrics to compare the SMBH mass measurements using molecular gas kinematics to those using megamaser kinematics, we demonstrate that the best molecular gas measurements resolve material that is physically closer to the SMBHs in terms of RSchw but is slightly farther in terms of RSOI and Req. However, molecular gas observations of nearby galaxies using the most extended configurations of the Atacama Large Millimeter/sub-millimeter Array can resolve the SOI comparably well and thus enable SMBH mass measurements as precise as the best megamaser measurements.</jats:p>

Discovery of the optical and radio counterpart to the fast X-ray transient EP240315a

ArXiv 2404.1066 (2024)


JH Gillanders, L Rhodes, S Srivastav, F Carotenuto, J Bright, ME Huber, HF Stevance, SJ Smartt, KC Chambers, T-W Chen, R Fender, A Andersson, AJ Cooper, PG Jonker, FJ Cowie, T deBoer, N Erasmus, MD Fulton, H Gao, J Herman, C-C Lin, T Lowe, EA Magnier, H-Y Miao, P Minguez, T Moore, C-C Ngeow, M Nicholl, Y-C Pan, G Pignata, A Rest, X Sheng, IA Smith, KW Smith, JL Tonry, RJ Wainscoat, J Weston, S Yang, DR Young

EDGE – Dark matter or astrophysics? Breaking dark matter heating degeneracies with H i rotation in faint dwarf galaxies

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2024) stae718


Martin P Rey, Matthew DA Orkney, Justin I Read, Payel Das, Oscar Agertz, Andrew Pontzen, Anastasia A Ponomareva, Stacy Y Kim, William McClymont