Properties of the cluster population of NGC 1566 and their implications
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
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.
galaxies: individual: NGC1566, galaxies: star clusters: general
Astronomy, Astrophysics and Cosmology
IdentifiersURN: urn:nbn:se:su:diva-134272DOI: 10.1093/mnras/stw1142ISI: 000379832800074OAI: oai:DiVA.org:su-134272DiVA: diva2:1033435