PHANGS-MeerKAT and MHONGOOSE HI observations of nearby spiral galaxies: Physical drivers of the molecular gas fraction, Rmol

被引：3

作者：

Eibensteiner, Cosima ^{[1
,2
]}

Sun, Jiayi ^{[3
]}

Bigiel, Frank ^{[1
]}

Leroy, Adam K. ^{[4
,5
]}

Schinnerer, Eva ^{[6
]}

Rosolowsky, Erik ^{[7
]}

Kurapati, Sushma ^{[8
]}

Pisano, D. J. ^{[8
]}

de Blok, W. J. G. ^{[8
,9
,10
]}

Barnes, Ashley T. ^{[11
]}

Thorp, Mallory ^{[1
]}

Colombo, Dario ^{[1
]}

Koch, Eric W. ^{[12
]}

Chiang, I-Da ^{[13
]}

Ostriker, Eve C. ^{[3
]}

Murphy, Eric J. ^{[2
]}

Zabel, Nikki ^{[8
]}

Laudage, Sebstian ^{[1
]}

Maccagni, Filippo M. ^{[10
]}

Healy, Julia ^{[10
]}

Sekhar, Srikrishna ^{[14
]}

Utomo, Dyas ^{[2
]}

den Brok, Jakob ^{[10
]}

Cao, Yixian ^{[15
]}

Chevance, Melanie ^{[16
]}

Dale, Daniel A. ^{[17
]}

Faesi, Christopher M. ^{[18
]}

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

He, Hao ^{[1
,19
]}

Jeffreson, Sarah ^{[12
]}

Jimenez-Donaire, Maria J. ^{[20
]}

Klessen, Ralf ^{[21
]}

Neumann, Justus ^{[6
]}

Pan, Hsi-An ^{[22
]}

Pathak, Debosmita ^{[4
]}

Querejeta, Miguel ^{[20
]}

Teng, Yu-Hsuan ^{[23
]}

Usero, Antonio ^{[20
]}

Williams, Thomas G. ^{[24
]}

机构：

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

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

[3] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA

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

[5] Ctr Cosmol & Astroparticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA

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

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

[8] Univ Cape Town, Dept Astron, Private Bag X3, ZA-7701 Rondebosch, South Africa

[9] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands

[10] Netherlands Inst Radio Astron ASTRON, Oude Hoogeveensedijk 4, NL-7991 PD Dwingeloo, Netherlands

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

[12] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA

[13] Acad Sinica, Inst Astron & Astrophys, Astron Math Bldg 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan

[14] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA

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

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

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

[18] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA

[19] McMaster Univ, Dept Phys & Astron, 1280 Main St W, Hamilton, ON L8S 4L8, Canada

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

[21] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany

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

[23] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, 9500 Gilman Dr, La Jolla, CA 92093 USA

[24] Univ Oxford, Subdept Astrophys, Dept Phys, Keble Rd, Oxford OX1 3RH, England

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 691卷

基金：

欧洲研究理事会; 新加坡国家研究基金会; 美国国家航空航天局; 加拿大自然科学与工程研究理事会; 美国国家科学基金会;

关键词：

galaxies: fundamental parameters; galaxies: ISM; galaxies: spiral; STAR-FORMATION EFFICIENCY; MULTIPHASE GALACTIC DISKS; RAM-PRESSURE; METALLICITY DEPENDENCE; INTERSTELLAR-MEDIUM; LINEAR-REGRESSION; CONVERSION FACTOR; STELLAR STRUCTURE; FORMATION RATES; SPITZER SURVEY;

D O I：

10.1051/0004-6361/202449944

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The molecular-to-atomic gas ratio is crucial to our understanding of the evolution of the interstellar medium (ISM) in galaxies. We investigated the balance between the atomic (Sigma(HI)) and molecular gas (Sigma(H2)) surface densities in eight nearby star-forming galaxies using new high-quality observations from MeerKAT and ALMA (for H I and CO, respectively). We defined the molecular gas ratio as R-mol = Sigma(H2)/Sigma(HI) and measured how R-mol depends on local conditions in the galaxy disks using multiwavelength observations. We find that, depending on the galaxy, H I is detected at > 3 sigma out to 20 - 120 kpc in galactocentric radius (r(gal)). The typical radius at which Sigma(HI) reaches 1 M-circle dot pc(-2) is r(H I) approximate to 22 kpc, which corresponds to 1 - 3 times the optical radius (r(25)). We note that, R-mol correlates best with the dynamical equilibrium pressure, P-DE, among potential drivers studied, with a median correlation coefficient of <rho > = 0.89. Correlations between R-mol and the star formation rate surface density, total gas surface density, stellar surface density, metallicity, and Sigma(SFR)/P-DE (a proxy for the combined effect of the UV radiation field and number density) are present but somewhat weaker. Our results also show a direct correlation between P-DE and Sigma(SFR), supporting self-regulation models. Quantitatively, we measured similar scalings as previous works, and attribute the modest differences that we do find to the effect of varying resolution and sensitivity. At r(gal) greater than or similar to 0.4r(25), atomic gas dominates over molecular gas among our studied galaxies, and at the balance of these two gas phases (R-mol = 1), we find that the baryon mass is dominated by stars, with Sigma(*) > 5 Sigma(gas). Our study constitutes an important step in the statistical investigation of how local galaxy properties (stellar mass, star formation rate, or morphology) impact the conversion from atomic to molecular gas in nearby galaxies.

引用

页数：24

共 1 条

[1] CO Multi-line Imaging of Nearby Galaxies (COMING). I. Physical properties of molecular gas in the barred spiral galaxy NGC 2903
Muraoka, Kazuyuki
Sorai, Kazuo
Kuno, Nario
Nakai, Naomasa
Nakanishi, Hiroyuki
Takeda, Miho
Yanagitani, Kazuki
Kaneko, Hiroyuki
Miyamoto, Yusuke
Kishida, Nozomi
Hatakeyama, Takuya
Umei, Michiko
Tanaka, Takahiro
Tomiyasu, Yuto
Saita, Chey
Ueno, Saeko
Matsumoto, Naoko
Salak, Dragan
Morokuma-Matsui, Kana
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 2016, 68 (05)

← 1 →