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We aim to characterise the properties of a third massive, red supergiantdominated galactic cluster. To accomplish this we utilised a combination ofnear/mid-IR photometry and spectroscopy to identify and classify the propertiesof cluster members, and statistical arguments to determine the mass of thecluster. We found a total of 16 strong candidates for cluster membership, forwhich formal classification of a subset yields spectral types from K3-M4 Ia andluminosities between log(L/L_sun)~4.5-4.8 for an adopted distance of 6+/-1 kpc.For an age in the range of 16-20 Myr, the implied mass is 2-4x10^4 M_sun,making it one of the most massive young clusters in the Galaxy. This discoverysupports the hypothesis that a significant burst of star formation occurred atthe base of Scutum-Crux arm between 10-20 Myr ago, yielding a stellar complexcomprising at least ~10^5M_sun of stars (noting that since the clusteridentification criteria rely on the presence of RSGs, we suspect that the truestellar yield will be significantly higher). We highlight the apparent absenceof X-ray binaries within the star formation complex and finally, given thephysical association of at least two pulsars with this region, discuss theimplications of this finding for stellar evolution and the production andproperties of neutron stars.

A third red supergiant rich cluster in the Scutum-Crux Arm