Comparing the pre-SNe feedback and environmental pressures for 6000 HII regions across 19 nearby spiral galaxies

被引：29

作者：

Barnes, A. T. ^{[1
]}

Glover, S. C. O. ^{[2
]}

Kreckel, K. ^{[3
]}

Ostriker, E. C. ^{[4
]}

Bigiel, F. ^{[1
]}

Belfiore, F. ^{[5
]}

Beslic, I ^{[1
]}

Blanc, G. A. ^{[6
,7
]}

Chevance, M. ^{[3
]}

Dale, D. A. ^{[8
]}

Egorov, O. ^{[3
,9
]}

Eibensteiner, C. ^{[1
]}

Emsellem, E. ^{[10
]}

Grasha, K. ^{[11
]}

Groves, B. A. ^{[12
]}

Klessen, R. S. ^{[2
,13
]}

Kruijssen, J. M. D. ^{[3
]}

Leroy, A. K. ^{[14
]}

Longmore, S. N. ^{[15
]}

Lopez, L. ^{[14
]}

McElroy, R. ^{[16
]}

Meidt, S. E. ^{[17
]}

Murphy, E. J. ^{[18
]}

Rosolowsky, E. ^{[19
]}

Saito, T. ^{[16
]}

Santoro, F. ^{[16
]}

Schinnerer, E. ^{[16
]}

Schruba, A. ^{[20
]}

Sun, J. ^{[14
]}

Watkins, E. J. ^{[3
]}

Williams, T. G. ^{[16
]}

机构：

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

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

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

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

[5] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy

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

[7] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile

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

[9] Lomonosov Moscow State Univ, Sternberg Astron Inst, Univ Sky Pr 13, Moscow 119234, Russia

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

[11] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia

[12] Univ Western Australia, Int Ctr Radio Astron Res, 7 Fairway, Crawley, WA 6009, Australia

[13] Heidelberg Univ, Interdisziplinares Zentrum Wissensch Rechnen, D-69120 Heidelberg, Germany

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

[15] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

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

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

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

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2021年 / 508卷 / 04期

基金：

美国国家科学基金会; 欧洲研究理事会;

关键词：

ISM: general; ISM: structure; Hii regions; galaxies: ISM; galaxies: star formation; H II REGIONS; STAR-FORMATION EFFICIENCY; GIANT MOLECULAR CLOUDS; SPECTRAL ENERGY-DISTRIBUTION; UV-RADIATION FEEDBACK; STELLAR FEEDBACK; FORMATION RATES; MASSIVE STARS; STARBURST GALAXIES; IONIZING FEEDBACK;

D O I：

10.1093/mnras/stab2958

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The feedback from young stars (i.e. pre-supernova) is thought to play a crucial role in molecular cloud destruction. In this paper, we assess the feedback mechanisms acting within a sample of 5810 Hii regions identified from the PHANGS-MUSE survey of 19 nearby (<20Mpc) star-forming, main-sequence spiral galaxies [log(M-star/M-circle dot) = 9.4-11]. These optical spectroscopic maps are essential to constrain the physical properties of the Hii regions, which we use to investigate their internal pressure terms. We estimate the photoionized gas (P-therm), direct radiation (P-rad), and mechanical wind pressure (P-wind), which we compare to the confining pressure of their host environment (P-de). The Hii regions remain unresolved within our similar to 50-100pc resolution observations, so we place upper (P-max) and lower (P-min) limits on each of the pressures by using a minimum (i.e. clumpy structure) and maximum (i.e. smooth structure) size, respectively. We find that the P-max measurements are broadly similar, and for P-min the P-therm is mildly dominant. We find that the majority of Hii regions are overpressured, P-tot/P-de = (P-therm + P-wind + P-rad)/P-de > 1, and expanding, yet there is a small sample of compact Hii regions with P-tot,P-max/P-de < 1 (similar to 1 per cent of the sample). These mostly reside in galaxy centres (R-gal < 1kpc), or, specifically, environments of high gas surface density; log(Sigma(gas)/M(circle dot)pc(-2)) similar to 2.5 (measured on kpc-scales). Lastly, we compare to a sample of literature measurements for P-therm and P(rad)to investigate how dominant pressure term transitions over around 5dex in spatial dynamic range and 10dex in pressure.

引用

页码：5362 / 5389

页数：28

共 1 条

[1] Linking stellar populations to H II regions across nearby galaxies I. Constraining pre-supernova feedback from young clusters in NGC 1672
Barnes, A. T.
Chandar, R.
Kreckel, K.
Glover, S. C. O.
Scheuermann, F.
Belfiore, F.
Bigiel, F.
Blanc, G. A.
Boquien, M.
den Brok, J.
Congiu, E.
Chevance, M.
Dale, D. A.
Deger, S.
Kruijssen, J. M. D.
Egorov, O., V
Eibensteiner, C.
Emsellem, E.
Grasha, K.
Groves, B.
Klessen, R. S.
Hannon, S.
Hassani, H.
Lee, J. C.
Leroy, A. K.
Lopez, L. A.
McLeod, A. F.
Pan, H.
Sanchez-Blazquez, P.
Schinnerer, E.
Sormani, M. C.
Thilker, D. A.
Ubeda, L.
Watkins, E. J.
Williams, T. G.
ASTRONOMY & ASTROPHYSICS, 2022, 662

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