English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The presence of a population of a large number ($\sim$400) of almost coeval(100--300 Myr) super star clusters (SSCs) in the disk of M82 offers anopportunity to construct the Cluster Initial Mass Function (CIMF) from theobserved present-day Cluster Mass Function (CMF). We carry out the dynamicaland photometric evolution of the CMF assuming the clusters move in circularorbits under the gravitational potential of the host galaxy using thesemi-analytical simulation code EMACSS. We explore power-law and log-normalfunctions for the CIMFs, and populate the clusters in the disk assuminguniform, power-law, and exponential radial distribution functions. We find thatthe observed CMF is best produced by a CIMF that is power-law in form with anindex of 1.8, for a power-law radial distribution function. More importantly,we establish that the observed turn-over in the present-day CMF is the resultof observational incompleteness rather than due to dynamically induced effects,or an intrinsically log-normal CIMF, as was proposed for the fossil starburstregion B of this galaxy. Our simulations naturally reproduce the mass-radiusrelation observed for a sub-sample of M82 SSCs.

The cluster initial mass function of the M82 disk Super Star Clusters