The Young Open Clusters King 12, NGC 7788, and NGC 7790: Pre-Main Sequence Stars and Extended Stellar Halos

TL;DR

This study investigates the stellar contents, ages, and structural properties of the young open clusters King 12, NGC 7788, and NGC 7790, revealing their pre-main sequence stars, extended halos, and possible common origins.

Contribution

It provides detailed analysis of the clusters' ages, stellar populations, and halo structures using MegaCam data, highlighting the presence of stellar halos and their formation mechanisms.

Findings

King 12 is younger than 20 Myr; NGC 7788 is 20-40 Myr; NGC 7790 is 60-80 Myr.

King 12 and NGC 7788 have stellar halos extending ~3.4 parsecs.

NGC 7790 shows no evidence of a surrounding halo.

Abstract

The stellar contents of the open clusters King 12, NGC 7788, and NGC 7790 are investigated using MegaCam images. Comparisons with isochrones yield an age < 20 Myr for King 12, 20--40 Myr for NGC 7788, and 60 -- 80 Myr for NGC 7790 based on the properties of stars near the main sequence turn-off (MSTO) in each cluster. The reddening of NGC 7788 is much larger than previously estimated. The luminosity functions (LFs) of King 12 and NGC 7788 show breaks that are attributed to the onset of pre-main sequence (PMS) objects, and comparisons with models of PMS evolution yield ages that are consistent with those measured from stars near the MSTO. In contrast, the r' LF of main sequence stars in NGC 7790 is matched to r' = 20 by a model that is based on the solar neighborhood mass function. The structural properties of all three clusters are investigated by examining the two-point angular correlation function of blue main sequence stars. King 12 and NGC 7788 are each surrounded by a stellar halo that extends out to 5 arcmin (~ 3.4 parsecs) radius. It is suggested that these halos form in response to large-scale mass ejection early in the evolution of the clusters, as predicted by models. In contrast, blue main sequence stars in NGC 7790 are traced out to a radius of ~ 7.5 arcmin, with no evidence of a halo. It is suggested that all three clusters may have originated in the same star-forming complex, but not in the same giant molecular cloud.