首页|The ALMaQUEST Survey XV:The dependence of the molecular-to-atomic gas ratios on resolved optical diagnostics

The ALMaQUEST Survey XV:The dependence of the molecular-to-atomic gas ratios on resolved optical diagnostics

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The atomic-to-molecular gas conversion is a critical step in the baryon cycle of galaxies,which sets the initial conditions for sub-sequent star formation and influences the multi-phase interstellar medium.We compiled a sample of 94 nearby galaxies with observations of multi-phase gas contents by utilizing public H Ⅰ,CO,and optical IFU data from the MaNGA survey together with new FAST H Ⅰ observations.In agreement with previous results,our sample shows that the global molecular-to-atomic gas ratio(Rmol=log MH2/MHⅠ)is correlated with the global stellar mass surface density μ*with a Kendall's τ coefficient of 0.25 and p＜10-3,less tightly but still correlated with stellar mass and NUV-r color,and not related to the specific star formation rate(sSFR).The cold gas distribution and kinematics inferred from the HⅠ and CO global profile asymmetry and shape do not significantly rely on Rmol.Thanks to the availability of kpc-scale observations of MaNGA,we decompose galaxies into HⅡ,composite,and AGN-dominated regions by using the BPT diagrams.With increasing Rmol,the fraction of HⅡ regions within 1.5 effective radius decreases slightly;the density distribution in the spatially resolved BPT diagram also changes significantly,suggesting changes in metallicity and ionization states.Galaxies with high Rmol tend to have high oxygen abundance,both at one effective radius with a Kendall's τ coefficient of 0.37(p＜10-3)and their central regions.Among all parameters investigated here,the oxygen abundance at one effective radius has the strongest relation with global Rmol.The dependence of gas conversion on gas distribution and galaxy ionization states is weak.In contrast,the observed positive relation between oxygen abundance(μ*)and Rmol indicates that the gas conversion is efficient in regions of high metallicity(density).

Galaxiesbaryon cycleradio linesH Ⅰ 21 cmatomic-to-molecular gas conversion

Niankun Yu、Zheng Zheng、Chao-Wei Tsai、Pei Zuo、Sara L.Ellison、David V.Stark、Di Li、Jingwen Wu、Karen L.Masters、Ting Xiao、Yinghui Zheng、Zongnan Li、Kai Zhang、Hongying Chen、Shu Liu、Sihan Jiao、Fanyi Meng

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National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China

Key Laboratory of Radio Astronomy and Technology,Chinese Academy of Sciences,Beijing 100101,China

Institute for Frontiers in Astronomy and Astrophysics,Beijing Normal University,Beijing 102206,China

School of Astronomy and Space Science,University of Chinese Academy of Sciences,Beijing 100049,China

Department of Physics & Astronomy,University of Victoria,Victoria,V8P 1A1,Canada

Departments of Physics and Astronomy,Haverford College,Haverford,19041,USA

Space Telescope Science Institute,San Martin Dr.,Baltimore 21218,USA

Zhejiang Laboratory,Hangzhou 311121,China

New Cornerstone Science Laboratory,Shenzhen 518054,China

School of Physics,Zhejiang University,Hangzhou 310058,China

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National Natural Science Foundation of ChinaNational Natural Science Foundation of ChinaNational Natural Science Foundation of ChinaNational Natural Science Foundation of ChinaNational Natural Science Foundation of ChinaNational Natural Science Foundation of ChinaChina Postdoctoral Science FoundationChina Postdoctoral Science FoundationInternational Partnership Program of Chinese Academy of SciencesNational Key Research and Program of ChinaNational Key Research and Program of ChinaNational Key Research and Program of ChinaMinistry of Science and Technology of ChinaYoung Researcher Grant of Institutional Center for Shared Technologies and Facilities of National Astronomical ObservatoriesNational Natural Science Foundation of Chinafellowship of China National Postdoctoral Program for Innovation Talentsproject funded by China Postdoctoral Science FoundationNational Aeronautics and Space AdministrationCalifornia Institute of Technology

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2024

10.1007/s11433-023-2387-2

中国科学:物理学 力学 天文学(英文版)
中国科学院

中国科学:物理学 力学 天文学(英文版)

CSTPCD
影响因子：0.91
ISSN：1674-7348
年,卷(期)：2024.67(9)