Molecular gas and star formation in central rings across nearby galaxies

doi:10.1051/0004-6361/202557430

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Title:	Molecular gas and star formation in central rings across nearby galaxies
Authors:	Gleis, Damian R.;Stuber, Sophia K.;Schinnerer, Eva;Neumann, Justus;Meidt, Sharon E.;Querejeta, Miguel;Emsellem, Eric;Leroy, Adam K.;Barnes, Ashley T.;Bigiel, Frank;Burton, Charlie;Chevance, Mélanie;Dale, Daniel A.;Grasha, Kathryn;Klessen, Ralf S.;Levy, Rebecca C.;Neumann, Lukas;Pan, Hsi-An;Marina, Ruiz-García;Sormani, Mattia C.;Sun, Jiayi;Teng, Yu-Hsuan;Williams, Thomas G.
Keywords:	ISM: molecules;Galaxy: center;galaxies: ISM;galaxies: star formation;galaxies: structure
Date:	2026-03-02
Issue Date:	2026-04-28 12:05:31 (UTC+8)
Abstract:	Context. Nearby galaxies exhibit a variety of structures, including so-called central or (circum-)nuclear rings that are similar to the Milky Way (MW) Central Molecular Zone (CMZ). These rings are common in barred galaxies and can be gas-rich and highly star-forming. Aims. We aim to study the molecular gas content and star formation rate of central rings within nearby galaxies and link them to global galaxy properties, especially the bar morphology. Methods. We utilized 1″(≲100 pc) resolution CO(2–1) observations from the PHANGS-ALMA survey, visually identifying 20 central rings and determine their properties. For 14 of these rings, MUSE observations tracing star formation rate (SFR) surface density were available. We derived the rings’ geometry, integrated molecular gas masses, SFRs, depletion times, and compared them to host galaxy and bar properties from the literature. Results. Molecular gas is an effective tracer for central rings. Previous studies have used ionized gas and dust tracers to identify central rings in galaxies of similar morphological types as the PHANGS galaxies (numerical Hubble type T ∼ −3 to T ∼ 9). In comparison, molecular gas yields similar fractions of galaxies hosting central rings and similar radii distributions. The gaseous central rings have typical radii of ∼ 400+250−150pc, molecular gas masses of log(M/M⊙) ∼ 8.1+0.17−0.23, and SFRs of ∼ 0.21+0.15−0.16 M⊙/yr. As a result, they contribute 5.6+4.5−2.1% and 13+10−5% to their host galaxies’ molecular gas mass and SFR, respectively. While the MW CMZ sits at the lower end of the radius, molecular gas mass, and SFR distribution, it matches well in terms of ring molecular gas mass and SFR fraction, and depletion time. Longer bars contain more massive molecular central rings, but there is no correlation between the classical bar strength parameters (Qb, εbar, A2max) and the ring’s molecular gas content. Conclusions. Although absolute central ring properties (ring radius, molecular gas mass, SFR) likely depend on host galaxy properties, the similarities between the MW CMZ and PHANGS central rings in relative parameters (molecular gas and SFR fraction, depletion time) suggest that the processes of gas inflow and star formation are similar for central rings across nearby galaxies.
Relation:	Astronomy & Astrophysics 707(A121) , p. 17
DOI:	10.1051/0004-6361/202557430
Appears in Collections:	[物理學系暨研究所] 期刊論文

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