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Properties of the cluster population of NGC 1566 and their implications
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
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Number of Authors: 5
2016 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 460, no 2, 2087-2102 p.Article in journal (Refereed) Published
Abstract [en]

We present results of a photometric study into the cluster population of NGC 1566, a nearby grand design spiral galaxy, sampled out to a Galactocentric radius of a parts per thousand 5.5 kpc. The shape of the mass-limited age distribution shows negligible variation with radial distance from the centre of the galaxy, and demonstrates three separate sections, with a steep beginning, flat middle and steep end. The luminosity function can be approximated by a power law at lower luminosities with evidence of a truncation at higher luminosity. The power-law section of the luminosity function of the galaxy is best fitted by an index a parts per thousand a' 2, in agreement with other studies, and is found to agree with a model luminosity function, which uses an underlying Schechter mass function. The recovered power law slope of the mass distribution shows a slight steepening as a function of galactocentric distance, but this is within error estimates. It also displays a possible truncation at the high mass end. Additionally, the cluster formation efficiency (I) and the specific U-band luminosity of clusters (T-L(U)) are calculated for NGC 1566 and are consistent with values for similar galaxies. A difference in NGC 1566, however, is that the fairly high star formation rate is in contrast with a low I (SFR) pound and I, indicating that I can only be said to depend strongly on I (SFR) pound, not the star formation rate.

Place, publisher, year, edition, pages
2016. Vol. 460, no 2, 2087-2102 p.
Keyword [en]
galaxies: individual: NGC1566, galaxies: star clusters: general
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-134272DOI: 10.1093/mnras/stw1142ISI: 000379832800074OAI: oai:DiVA.org:su-134272DiVA: diva2:1033435
Available from: 2016-10-06 Created: 2016-10-03 Last updated: 2017-11-30Bibliographically approved

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Adamo, Angela
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