A survey of molecular clouds in the Galactic center’s outflow

¹ Università di Firenze, Dipartimento di Fisica e Astronomia, via G. Sansone 1, 50019 Sesto Fiorentino, Firenze, Italy
² INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
³ Astronomy Department, University of Massachusetts, Amherst, MA 01003, USA
⁴ Research School of Astronomy and Astrophysics – The Australian National University, Canberra, ACT 2611, Australia
⁵ Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
⁶ Green Bank Observatory, Green Bank, WV 24944, USA
⁷ National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA

^★ Corresponding author: This email address is being protected from spambots. You need JavaScript enabled to view it.

Received: 17 October 2025
Accepted: 17 December 2025

Abstract

The nucleus of the Milky Way is known to drive a large-scale, multiphase galactic outflow, with gas phases ranging from the hot highly ionized component to the cold molecular one. In this work, we present the first systematic search for molecules in the Milky Way wind. We used the Atacama Pathfinder EXperiment (APEX) to observe the ¹²CO(2→1) emission line in 19 fields centered on previously known high-velocity atomic hydrogen (Hi) clouds associated with the outflow. Over 200 CO clumps are detected within 16 different Hi clouds. These clumps have typical radii of 1–3 parsec, high velocity dispersions of 1–6 km s⁻¹, and molecular gas masses ranging from a few to several hundred M_⊙. Molecular clumps in the wind sit at the low-mass end of the mass-size relation of regular molecular clouds, but are far displaced from the mass (or size) – linewidth relation, being generally more turbulent and showing high internal pressures. Nearly 90% of the clumps are gravitationally unbound with virial parameters of α_vir ≫ 10–100, indicating that these structures are either being disrupted or else confined by external pressure from the surrounding hot medium. While the observed properties of CO clumps do not seem to evolve clearly with latitude, we find that molecular gas is not detected in any of the 6 Hi clouds with projected distances over 1 kpc from the Galactic center, suggesting the existence of a maximum timescale of ~3 Myr for the dissociation of molecular gas within the wind. Overall, current observations in the Galactic center support a scenario in which a hot wind entrains cold gas clouds from the disk, driving their progressive transformation from molecular to atomic and ultimately ionized gas through stripping, turbulence, and dissociation.