The luminosity, mass, and age distributions of compact star clusters in M83 based on Hubble Space Telescope/Wide Field Camera 3 observations

Rupali Chandar, Bradley C. Whitmore, Hwihyun Kim, Catherine Kaleida, Max Mutchler, Daniela Calzetti, Abhijit Saha, Robert O'Connell, Bruce Balick, Howard Bond, Marcella Carollo, Michael Disney, Michael A. Dopita, Jay A. Frogel, Donald Hall, Jon A. Holtzman, Randy A. Kimble, Patrick McCarthy, Francesco Paresc, Joe Silk & 4 others John Trauger, Alistair R. Walker, Rogier Windhorst, Erick Young

Research output: Contribution to journalArticle

82 Citations (Scopus)

Abstract

The newly installed Wide Field Camera 3 (WFC3) on the Hubble Space Telescope has been used to obtain multiband images of the nearby spiral galaxy M83. These new observations are the deepest and highest resolution images ever taken of a grand-design spiral, particularly in the near-ultraviolet, and allow us to better differentiate compact star clusters from individual stars and to measure the luminosities of even faint clusters in the U band. We find that the luminosity function (LF) for clusters outside of the very crowded starburst nucleus can be approximated by a power law, dN/dL ∝ Lα, with α =-2.04 ± 0.08, down to MV ≈-5.5. We test the sensitivity of the LF to different selection techniques, filters, binning, and aperture correction determinations, and find that none of these contribute significantly to uncertainties in α. We estimate ages and masses for the clusters by comparing their measured UBVI, Hα colors with predictions from single stellar population models. The age distribution of the clusters can be approximated by a power law, dN/dτ ∝ τγ, with γ =-0.9 ± 0.2, for M ≳ few × 103 M and τ ≲ 4 × 108 yr. This indicates that clusters are disrupted quickly, with ≈80%-90% disrupted each decade in age over this time. The mass function of clusters over the same M-τ range is a power law, dN/dM ∝ Mβ, with β =-1.94 ± 0.16, and does not have bends or show curvature at either high or low masses. Therefore, we do not find evidence for a physical upper mass limit, MC, or for the earlier disruption of lower mass clusters when compared with higher mass clusters, i.e., mass-dependent disruption. We briefly discuss these implications for the formation and disruption of the clusters.

Original languageEnglish (US)
Pages (from-to)966-978
Number of pages13
JournalAstrophysical Journal
Volume719
Issue number1
DOIs
StatePublished - Oct 8 2010

Fingerprint

star clusters
mass distribution
Hubble Space Telescope
age structure
cameras
luminosity
power law
image resolution
curvature
spiral galaxies
filter
apertures
prediction
color
filters
stars
nuclei
sensitivity
high resolution
estimates

Keywords

  • Galaxies: Individual (M83), galaxies: Star clusters: General
  • Stars: Formation

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

The luminosity, mass, and age distributions of compact star clusters in M83 based on Hubble Space Telescope/Wide Field Camera 3 observations. / Chandar, Rupali; Whitmore, Bradley C.; Kim, Hwihyun; Kaleida, Catherine; Mutchler, Max; Calzetti, Daniela; Saha, Abhijit; O'Connell, Robert; Balick, Bruce; Bond, Howard; Carollo, Marcella; Disney, Michael; Dopita, Michael A.; Frogel, Jay A.; Hall, Donald; Holtzman, Jon A.; Kimble, Randy A.; McCarthy, Patrick; Paresc, Francesco; Silk, Joe; Trauger, John; Walker, Alistair R.; Windhorst, Rogier; Young, Erick.

In: Astrophysical Journal, Vol. 719, No. 1, 08.10.2010, p. 966-978.

Research output: Contribution to journalArticle

Chandar, R, Whitmore, BC, Kim, H, Kaleida, C, Mutchler, M, Calzetti, D, Saha, A, O'Connell, R, Balick, B, Bond, H, Carollo, M, Disney, M, Dopita, MA, Frogel, JA, Hall, D, Holtzman, JA, Kimble, RA, McCarthy, P, Paresc, F, Silk, J, Trauger, J, Walker, AR, Windhorst, R & Young, E 2010, 'The luminosity, mass, and age distributions of compact star clusters in M83 based on Hubble Space Telescope/Wide Field Camera 3 observations', Astrophysical Journal, vol. 719, no. 1, pp. 966-978. https://doi.org/10.1088/0004-637X/719/1/966
Chandar, Rupali ; Whitmore, Bradley C. ; Kim, Hwihyun ; Kaleida, Catherine ; Mutchler, Max ; Calzetti, Daniela ; Saha, Abhijit ; O'Connell, Robert ; Balick, Bruce ; Bond, Howard ; Carollo, Marcella ; Disney, Michael ; Dopita, Michael A. ; Frogel, Jay A. ; Hall, Donald ; Holtzman, Jon A. ; Kimble, Randy A. ; McCarthy, Patrick ; Paresc, Francesco ; Silk, Joe ; Trauger, John ; Walker, Alistair R. ; Windhorst, Rogier ; Young, Erick. / The luminosity, mass, and age distributions of compact star clusters in M83 based on Hubble Space Telescope/Wide Field Camera 3 observations. In: Astrophysical Journal. 2010 ; Vol. 719, No. 1. pp. 966-978.
@article{ad8ad160ded349e395478b03ab5a2e78,
title = "The luminosity, mass, and age distributions of compact star clusters in M83 based on Hubble Space Telescope/Wide Field Camera 3 observations",
abstract = "The newly installed Wide Field Camera 3 (WFC3) on the Hubble Space Telescope has been used to obtain multiband images of the nearby spiral galaxy M83. These new observations are the deepest and highest resolution images ever taken of a grand-design spiral, particularly in the near-ultraviolet, and allow us to better differentiate compact star clusters from individual stars and to measure the luminosities of even faint clusters in the U band. We find that the luminosity function (LF) for clusters outside of the very crowded starburst nucleus can be approximated by a power law, dN/dL ∝ Lα, with α =-2.04 ± 0.08, down to MV ≈-5.5. We test the sensitivity of the LF to different selection techniques, filters, binning, and aperture correction determinations, and find that none of these contribute significantly to uncertainties in α. We estimate ages and masses for the clusters by comparing their measured UBVI, Hα colors with predictions from single stellar population models. The age distribution of the clusters can be approximated by a power law, dN/dτ ∝ τγ, with γ =-0.9 ± 0.2, for M ≳ few × 103 M⊙ and τ ≲ 4 × 108 yr. This indicates that clusters are disrupted quickly, with ≈80{\%}-90{\%} disrupted each decade in age over this time. The mass function of clusters over the same M-τ range is a power law, dN/dM ∝ Mβ, with β =-1.94 ± 0.16, and does not have bends or show curvature at either high or low masses. Therefore, we do not find evidence for a physical upper mass limit, MC, or for the earlier disruption of lower mass clusters when compared with higher mass clusters, i.e., mass-dependent disruption. We briefly discuss these implications for the formation and disruption of the clusters.",
keywords = "Galaxies: Individual (M83), galaxies: Star clusters: General, Stars: Formation",
author = "Rupali Chandar and Whitmore, {Bradley C.} and Hwihyun Kim and Catherine Kaleida and Max Mutchler and Daniela Calzetti and Abhijit Saha and Robert O'Connell and Bruce Balick and Howard Bond and Marcella Carollo and Michael Disney and Dopita, {Michael A.} and Frogel, {Jay A.} and Donald Hall and Holtzman, {Jon A.} and Kimble, {Randy A.} and Patrick McCarthy and Francesco Paresc and Joe Silk and John Trauger and Walker, {Alistair R.} and Rogier Windhorst and Erick Young",
year = "2010",
month = "10",
day = "8",
doi = "10.1088/0004-637X/719/1/966",
language = "English (US)",
volume = "719",
pages = "966--978",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1",

}

TY - JOUR

T1 - The luminosity, mass, and age distributions of compact star clusters in M83 based on Hubble Space Telescope/Wide Field Camera 3 observations

AU - Chandar, Rupali

AU - Whitmore, Bradley C.

AU - Kim, Hwihyun

AU - Kaleida, Catherine

AU - Mutchler, Max

AU - Calzetti, Daniela

AU - Saha, Abhijit

AU - O'Connell, Robert

AU - Balick, Bruce

AU - Bond, Howard

AU - Carollo, Marcella

AU - Disney, Michael

AU - Dopita, Michael A.

AU - Frogel, Jay A.

AU - Hall, Donald

AU - Holtzman, Jon A.

AU - Kimble, Randy A.

AU - McCarthy, Patrick

AU - Paresc, Francesco

AU - Silk, Joe

AU - Trauger, John

AU - Walker, Alistair R.

AU - Windhorst, Rogier

AU - Young, Erick

PY - 2010/10/8

Y1 - 2010/10/8

N2 - The newly installed Wide Field Camera 3 (WFC3) on the Hubble Space Telescope has been used to obtain multiband images of the nearby spiral galaxy M83. These new observations are the deepest and highest resolution images ever taken of a grand-design spiral, particularly in the near-ultraviolet, and allow us to better differentiate compact star clusters from individual stars and to measure the luminosities of even faint clusters in the U band. We find that the luminosity function (LF) for clusters outside of the very crowded starburst nucleus can be approximated by a power law, dN/dL ∝ Lα, with α =-2.04 ± 0.08, down to MV ≈-5.5. We test the sensitivity of the LF to different selection techniques, filters, binning, and aperture correction determinations, and find that none of these contribute significantly to uncertainties in α. We estimate ages and masses for the clusters by comparing their measured UBVI, Hα colors with predictions from single stellar population models. The age distribution of the clusters can be approximated by a power law, dN/dτ ∝ τγ, with γ =-0.9 ± 0.2, for M ≳ few × 103 M⊙ and τ ≲ 4 × 108 yr. This indicates that clusters are disrupted quickly, with ≈80%-90% disrupted each decade in age over this time. The mass function of clusters over the same M-τ range is a power law, dN/dM ∝ Mβ, with β =-1.94 ± 0.16, and does not have bends or show curvature at either high or low masses. Therefore, we do not find evidence for a physical upper mass limit, MC, or for the earlier disruption of lower mass clusters when compared with higher mass clusters, i.e., mass-dependent disruption. We briefly discuss these implications for the formation and disruption of the clusters.

AB - The newly installed Wide Field Camera 3 (WFC3) on the Hubble Space Telescope has been used to obtain multiband images of the nearby spiral galaxy M83. These new observations are the deepest and highest resolution images ever taken of a grand-design spiral, particularly in the near-ultraviolet, and allow us to better differentiate compact star clusters from individual stars and to measure the luminosities of even faint clusters in the U band. We find that the luminosity function (LF) for clusters outside of the very crowded starburst nucleus can be approximated by a power law, dN/dL ∝ Lα, with α =-2.04 ± 0.08, down to MV ≈-5.5. We test the sensitivity of the LF to different selection techniques, filters, binning, and aperture correction determinations, and find that none of these contribute significantly to uncertainties in α. We estimate ages and masses for the clusters by comparing their measured UBVI, Hα colors with predictions from single stellar population models. The age distribution of the clusters can be approximated by a power law, dN/dτ ∝ τγ, with γ =-0.9 ± 0.2, for M ≳ few × 103 M⊙ and τ ≲ 4 × 108 yr. This indicates that clusters are disrupted quickly, with ≈80%-90% disrupted each decade in age over this time. The mass function of clusters over the same M-τ range is a power law, dN/dM ∝ Mβ, with β =-1.94 ± 0.16, and does not have bends or show curvature at either high or low masses. Therefore, we do not find evidence for a physical upper mass limit, MC, or for the earlier disruption of lower mass clusters when compared with higher mass clusters, i.e., mass-dependent disruption. We briefly discuss these implications for the formation and disruption of the clusters.

KW - Galaxies: Individual (M83), galaxies: Star clusters: General

KW - Stars: Formation

UR - http://www.scopus.com/inward/record.url?scp=78049248992&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=78049248992&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/719/1/966

DO - 10.1088/0004-637X/719/1/966

M3 - Article

VL - 719

SP - 966

EP - 978

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

ER -