Reconstructing the radial velocity distribution of the Milky Way’s circumgalactic medium with HESTIA

Rünger, F ORCID: 0009-0001-5250-269X, Sparre, M ORCID: 0000-0002-9735-3851, Richter, P ORCID: 0000-0002-1188-1435, Damle, M ORCID: 0000-0003-1386-5436, Nuza, SE ORCID: 0000-0002-6913-3560, Grand, RJJ ORCID: 0000-0001-9667-1340, Hoffman, Y ORCID: 0000-0002-8158-0566, Libeskind, N ORCID: 0000-0002-6406-0016, Sorce, JG ORCID: 0000-0002-2307-2432, Steinmetz, M ORCID: 0000-0001-6516-7459 and Tempel, E ORCID: 0000-0002-5249-7018 (2025) Reconstructing the radial velocity distribution of the Milky Way’s circumgalactic medium with HESTIA. Astronomy & Astrophysics, 700. ISSN 0004-6361

Preview

Text Reconstructing the radial velocity distribution of the Milky Ways circumgalactic medium with HESTIA.pdf - Published Version Available under License Creative Commons Attribution. Download (8MB) | Preview

Abstract

The accretion and processing of neutral and ionized gas play substantial roles in the evolution of the Milky Way. From the position of the Sun, circumgalactic gas flows in the Milky Way halo are known to span a large range of radial velocities, but the complex kinematics of the circumgalactic medium (CGM) cannot be fully reconstructed from observations because of the blending with foreground interstellar gas in the Milky Way disk. For this paper we used three zoom-in magnetohydrodynamic simulations of the Milky Way and the Local Group from the HESTIA project to systematically investigate the radial velocity distribution of neutral hydrogen (H I) clouds in the CGM in the (simulated) Local Standard of Rest (LSR) velocity frame. Our three simulations, which exhibit substantial differences in their global CGM properties, reveal that 48–65 percent of the extraplanar H I at z > 2 kpc above the plane is confined to a velocity range |vLSR| ≤ 100 km s−1, implying that the gas is (at least partly) corotating with the underlying disk. In the two most realistic Milky Way realizations, the CGM velocity distribution is skewed toward negative velocities (in particular for H I clouds at vertical distances z > 10 kpc), indicating a net accretion of neutral gas. These results are in line with the statistics from UV absorption-line measurements of the Milky Way CGM, and we also find broad agreement with the Illustris TNG50 simulation. Our study supports a scenario in which a substantial fraction of the Milky Way’s CGM resides close to the disk at |vLSR| ≤ 100 km s−1, where it is hiding from observations as its spectral signatures are covered by foreground interstellar gas features. We furthermore find that 97 percent of the clumps live in the Milky Way halo and are not associated with satellite galaxies. The clumps are magnetized with a magnetic pressure often dominating over the thermal pressure.

Item Type:	Article
Uncontrolled Keywords:	5101 Astronomical Sciences; 51 Physical Sciences; 0201 Astronomical and Space Sciences; Astronomy & Astrophysics; 5101 Astronomical sciences; 5107 Particle and high energy physics; 5109 Space sciences
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	EDP Sciences
Date of acceptance:	30 May 2025
Date of first compliant Open Access:	27 August 2025
Date Deposited:	27 Aug 2025 14:26
Last Modified:	27 Aug 2025 14:30
DOI or ID number:	10.1051/0004-6361/202451355
URI:	https://researchonline.ljmu.ac.uk/id/eprint/27001

View Item