The young star cluster population of M51 with LEGUS - I. A comprehensive study of cluster formation and evolution

被引：40

作者：

Messa, M. ^{[1
]}

Adamo, A. ^{[1
]}

Ostlin, G. ^{[1
]}

Calzetti, D. ^{[2
]}

Grasha, K. ^{[2
]}

Grebel, E. K. ^{[3
]}

Shabani, F. ^{[3
]}

Chandar, R. ^{[4
]}

Dale, D. A. ^{[5
]}

Dobbs, C. L. ^{[6
]}

Elmegreen, B. G. ^{[7
]}

Fumagalli, M. ^{[8
,9
]}

Gouliermis, D. A. ^{[10
,11
]}

Kim, H. ^{[12
]}

Smith, L. J. ^{[13
]}

Thilker, D. A. ^{[14
]}

Tosi, M. ^{[15
]}

Ubeda, L. ^{[16
]}

Walterbos, R. ^{[17
]}

Whitmore, B. C. ^{[16
]}

Fedorenko, K. ^{[18
]}

Mahadevan, S. ^{[18
]}

Andrews, J. E. ^{[2
,19
]}

Bright, S. N. ^{[16
]}

Cook, D. O. ^{[20
]}

Kahre, L. ^{[17
]}

Nair, P. ^{[21
]}

Pellerin, A. ^{[22
]}

Ryon, J. E. ^{[23
]}

Ahmad, S. D. ^{[22
]}

Beale, L. P. ^{[22
]}

Brown, K. ^{[22
]}

Clarkson, D. A. ^{[22
]}

Guidarelli, G. C. ^{[22
]}

Parziale, R. ^{[5
]}

Turner, J. ^{[5
]}

Weber, M. ^{[22
]}

机构：

[1] Stockholm Univ, Oskar Klein Ctr, Dept Astron, Stockholm, Sweden

[2] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA

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

[4] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA

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

[6] Univ Exeter, Sch Phys & Astron, Exeter, Devon, England

[7] IBM Res Div, TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA

[8] Univ Durham, Inst Computat Cosmol, Durham, England

[9] Univ Durham, Ctr Extragalact Astron, Durham, England

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

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

[12] Gemini Observ, Casilla 603, La Serena, Chile

[13] European Space Agcy, Space Telescope Sci Inst, Baltimore, MD 21218 USA

[14] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[15] INAF, Osservatorio Astron Bologna, Bologna, Italy

[16] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[17] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA

[18] Univ Massachusetts, Coll Informat & Comp Sci, Amherst, MA 01002 USA

[19] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA

[20] CALTECH, Pasadena, CA 91125 USA

[21] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35401 USA

[22] SUNY Coll Geneseo, Dept Phys & Astron, Geneseo, NY 14454 USA

[23] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2018年 / 473卷 / 01期

基金：

欧洲研究理事会; 英国科学技术设施理事会;

关键词：

galaxies:; individual:; M51; NGC; 5194; galaxies: star clusters: general; galaxies: star formation; INITIAL MASS FUNCTION; GALACTIC OPEN CLUSTERS; LARGE-MAGELLANIC-CLOUD; GALAXIES NGC 4038/4039; LUMINOSITY FUNCTION; ANTENNAE GALAXIES; STELLAR CLUSTERS; AGE DISTRIBUTIONS; FORMATION HISTORY; SPIRAL GALAXIES;

D O I：

10.1093/mnras/stx2403

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Recently acquired WFC3 UV (F275W and F336W) imaging mosaics under the Legacy Extragalactic UV Survey (LEGUS), combined with archival ACS data of M51, are used to study the young star cluster (YSC) population of this interacting system. Our newly extracted source catalogue contains 2834 cluster candidates, morphologically classified to be compact and uniform in colour, for which ages, masses and extinction are derived. In this first work we study the main properties of the YSC population of the whole galaxy, considering a mass-limited sample. Both luminosity and mass functions follow a power-law shape with slope -2, but at high luminosities and masses a dearth of sources is observed. The analysis of the mass function suggests that it is best fitted by a Schechter function with slope -2 and a truncation mass at 1.00 +/- 0.12 x 10(5) M-circle dot . Through Monte Carlo simulations, we confirm this result and link the shape of the luminosity function to the presence of a truncation in the mass function. A mass limited age function analysis, between 10 and 200 Myr, suggests that the cluster population is undergoing only moderate disruption. We observe little variation in the shape of the mass function at masses above 1 x 10(4) M-circle dot over this age range. The fraction of star formation happening in the form of bound clusters in M51 is similar to 20 per cent in the age range 10-100 Myr and little variation is observed over the whole range from 1 to 200 Myr.

引用

页码：996 / 1018

页数：23

共 40 条

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