THE CLUSTER POPULATION OF THE IRREGULAR GALAXY NGC 4449 AS SEEN BY THE HUBBLE ADVANCED CAMERA FOR SURVEYS

Journal Article · Sat Oct 15 04:00:00 EDT 2011 · Astronomical Journal (New York, N.Y. Online)

DOI:https://doi.org/10.1088/0004-6256/142/4/129· OSTI ID:21582818

Annibali, F; Tosi, M ^[1]; Aloisi, A; Van der Marel, R P ^[2]

---

1. INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna (Italy)
2. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)

We present a study of the star cluster population in the starburst irregular galaxy NGC 4449 based on B, V, I, and H{alpha} images taken with the Advanced Camera for Surveys on the Hubble Space Telescope. We derive cluster properties such as size, ellipticity, and total magnitude. Cluster ages and masses are derived fitting the observed spectral energy distributions with different population synthesis models. Our analysis is strongly affected by the age-metallicity degeneracy; however, if we assume a metallicity of {approx}1/4 solar, as derived from spectroscopy of H II regions, we find that the clusters have ages distributed quite continuously over a Hubble time, and they have masses from {approx}10{sup 3} M{sub sun} up to {approx}2 x 10{sup 6} M{sub sun}, assuming a Salpeter initial mass function down to 0.1 M{sub sun}. Young clusters are preferentially located in regions of young star formation (SF), while old clusters are distributed over the whole NGC 4449 field of view, like the old stars (although we note that some old clusters follow linear structures, possibly a reflection of past satellite accretion). The high SF activity in NGC 4449 is confirmed by its specific frequency of young massive clusters, higher than the average value found in nearby spirals and in the Large Magellanic Cloud (but lower than in other starburst dwarfs such as NGC 1705 and NGC 1569), and by the flat slope of the cluster luminosity function (dN(L{sub V} ){proportional_to}L{sup -1.5}{sub V} dL for clusters younger than 1 Gyr). We use the upper envelope of the cluster log(mass) versus log(age) distribution to quantify cluster disruption, and do not find evidence for the high (90%) long-term infant mortality found by some studies. For the red clusters, we find correlations between size, ellipticity, luminosity, and mass: brighter and more massive clusters tend to be more compact, and brighter clusters also tend to be more elliptical.

• OSTI ID: 21582818
• Journal Information: Astronomical Journal (New York, N.Y. Online), Journal Name: Astronomical Journal (New York, N.Y. Online) Journal Issue: 4 Vol. 142; ISSN 1538-3881
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ENERGY SPECTRA
GALAXIES
LUMINOSITY
MAGELLANIC CLOUDS
MASS
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
SATELLITES
SPECTRA
SPECTROSCOPY
STAR CLUSTERS
STARS
TELESCOPES