\begin{center}{\Large\bf 
The stellar population of the star-forming region G61.48+0.09}\end{center} 

\centerline{\bf A. Marin-Franch (1), A. Herrero (1,2), A. Lenorzer (1), F. Najarro (3), S. Ramirez (1), A. Font-Ribera (1), D. Figer (4)
}{\footnotesize (1) Instituto de Astrofisica de Canarias, 38200 La Laguna, Tenerife, Spain
(2) Departamento de Astrofisica, Universidad de La Laguna, Spain
(3) Departamento de Astrofisica Molecular e Infrarroja, IEM, CSIC, Madrid, Spain
(4) Rochester Institute of Technology, Rochester, NY, USA}
}
 
- 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_S} = 0.9 to A_{K_S} = 2.6, (or A_{V}~8 to A_{V}~23). G61.48+0.09 is a star forming region located at 2.5+/-0.4 Kpc. The cluster is younger than 10 Myr and has a minimum stellar mass of 1500+/-500 Solar masses. However, the actual total mass of the cluster remains undetermined, as we cannot see its whole stellar content.

{\bf Reference: http://arxiv.org/abs/0904.3202} \\{\it Status:} Manuscript has been accepted
 \\ {\it Comments:} 

{\it On the web at:} {\tt } 

{\it Preprints from:} {\tt  amarin@iac.es} 
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