The stellar population of the star-forming region G61.48+0.09

Context. We present the results of a near-infrared photometric and spectroscopic study of the star-forming region G61.48+0.09. Aims. The purpose of this study is to characterize the stellar content of the cluster and to determine its distance, extinction, age, and mass. Methods. The stellar population was studied by using color–magnitude diagrams to select twenty promising cluster members, for which follow-up spectroscopy was done. The observed spectra allowed a spectral classification of the stars. Results. Two stars have emission lines, twelve are G-type stars, and six are late-O or early-B stars. Conclusions. The cluster's extinction varies from $A_{K_{\rm S}} = 0.9$ to $A_{K_{\rm S}} = 2.6$, (or $A_{V} \sim 8$ to $A_{V} \sim 23$). G61.48+0.09 is a star-forming region located at $2.5\pm0.4$ kpc. The cluster is younger than 10 Myr and has a minimum stellar mass of $1.5\pm 0.5 \times 10 ^{3}$ $M_\odot$. However, the actual total mass of the cluster remains undetermined, as we cannot see its whole stellar content.