The Gas-Star Formation Cycle in Nearby Star-forming Galaxies. II. Resolved Distributions of CO and Hα Emission for 49 PHANGS Galaxies

被引：31

作者：

Pan, Hsi-An ^{[1
,2
]}

Schinnerer, Eva ^{[1
]}

Hughes, Annie ^{[3
]}

Leroy, Adam ^{[4
]}

Groves, Brent ^{[5
]}

Barnes, Ashley Thomas ^{[6
]}

Belfiore, Francesco ^{[7
]}

Bigiel, Frank ^{[6
]}

Blanc, Guillermo A. ^{[8
,9
]}

Cao, Yixian ^{[10
]}

Chevance, Melanie ^{[11
]}

Congiu, Enrico ^{[9
]}

Dale, Daniel A. ^{[12
]}

Eibensteiner, Cosima ^{[6
]}

Emsellem, Eric ^{[13
,14
]}

Faesi, Christopher M. ^{[15
]}

Glover, Simon C. O. ^{[16
]}

Grasha, Kathryn ^{[17
]}

Herrera, Cinthya N. ^{[18
]}

Ho, I-Ting ^{[1
]}

Klessen, Ralf S. ^{[16
,19
]}

Kruijssen, J. M. Diederik ^{[11
]}

Lang, Philipp ^{[1
]}

Liu, Daizhong ^{[1
]}

McElroy, Rebecca ^{[20
]}

Meidt, Sharon E. ^{[21
]}

Murphy, Eric J. ^{[22
]}

Pety, Jerome ^{[18
,23
]}

Querejeta, Miguel ^{[24
]}

Razza, Alessandro ^{[9
]}

Rosolowsky, Erik ^{[25
]}

Saito, Toshiki ^{[1
]}

Santoro, Francesco ^{[1
]}

Schruba, Andreas ^{[26
]}

Sun, Jiayi ^{[4
]}

Tomicic, Neven ^{[27
]}

Usero, Antonio ^{[24
]}

Utomo, Dyas ^{[22
]}

Williams, Thomas G. ^{[1
]}

机构：

[1] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[2] Tamkang Univ, Dept Phys, 151 Yingzhuan Rd, New Taipei 251301, Taiwan

[3] IRAP, CNRS, Av Colonel Roche BP 44346, F-31028 Toulouse 4, France

[4] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA

[5] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia

[6] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany

[7] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50157 Florence, Italy

[8] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[9] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile

[10] Aix Marseille Univ, LAM Lab Astrophys Marseille, CNRS, F-13388 Marseille, France

[11] Heidelberg Univ, Astron Rech Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany

[12] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA

[13] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[14] Univ Lyon 1, Ctr Rech Astrophys Lyon UMR5574, CNRS, ENS Lyon,Univ Lyon, F-69230 St Genis Laval, France

[15] Univ Massachusetts, 710 N Pleasant St, Amherst, MA 01003 USA

[16] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany

[17] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia

[18] Inst Radioastron Millimetr IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France

[19] Heidelberg Univ, Interdisziplinares Zentrum Wissensch Liches Rechn, Neuenheimer Feld 205, D-69120 Heidelberg, Germany

[20] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia

[21] Univ Ghent, Sterrenkundig Observ, Krijgslaan 281 S9, B-9000 Ghent, Belgium

[22] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA

[23] Sorbonne Univ, Univ PSL, Observ Paris, LERMA,CNRS, F-75014 Paris, France

[24] Observ Astron Nacl IGN, C Alfonso XII,3, E-28014 Madrid, Spain

[25] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada

[26] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany

[27] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

来源：

ASTROPHYSICAL JOURNAL | 2022年 / 927卷 / 01期

基金：

欧洲研究理事会; 欧盟地平线“2020”; 美国国家科学基金会; 加拿大自然科学与工程研究理事会;

关键词：

DIFFUSE IONIZED-GAS; CO-TO-H-2 CONVERSION FACTOR; GIANT MOLECULAR CLOUDS; SDSS-IV MANGA; ATOMIC GAS; MILKY-WAY; UNCERTAINTY PRINCIPLE; FORMATION EFFICIENCY; LUMINOSITY FUNCTION; MAGELLANIC-CLOUD;

D O I：

10.3847/1538-4357/ac474f

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The relative distribution of molecular gas and star formation in galaxies gives insight into the physical processes and timescales of the cycle between gas and stars. In this work, we track the relative spatial configuration of CO and H alpha emission at high resolution in each of our galaxy targets and use these measurements to quantify the distributions of regions in different evolutionary stages of star formation: from molecular gas without star formation traced by H alpha to star-forming gas, and to H ii regions. The large sample, drawn from the Physics at High Angular resolution in Nearby GalaxieS ALMA and narrowband H alpha (PHANGS-ALMA and PHANGS-H alpha) surveys, spans a wide range of stellar masses and morphological types, allowing us to investigate the dependencies of the gas-star formation cycle on global galaxy properties. At a resolution of 150 pc, the incidence of regions in different stages shows a dependence on stellar mass and Hubble type of galaxies over the radial range probed. Massive and/or earlier-type galaxies in our sample exhibit a significant reservoir of molecular gas without star formation traced by H alpha, while lower-mass galaxies harbor substantial H ii regions that may have dispersed their birth clouds or formed from low-mass, more isolated clouds. Galactic structures add a further layer of complexity to the relative distribution of CO and H alpha emission. Trends between galaxy properties and distributions of gas traced by CO and H alpha are visible only when the observed spatial scale is MUCH LESS-THAN500 pc, reflecting the critical resolution requirement to distinguish stages of the star formation process.

引用

页数：49

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