We study the young S-stars within a distance of 0.04 pc from the supermassive black hole in the center of our Galaxy .
Given how inhospitable the region is for star formation , their presence is more puzzling the younger we estimate their ages .
In this study , we analyse the result of 12 years of high resolution spectroscopy within the central arcsecond of the Galactic Center ( GC ) .
By co-adding between 55 and 105 hours of spectra we have obtained high signal to noise H- and K-band spectra of eight stars orbiting the central supermassive black hole .
Using deep H-band spectra , we show that these stars must be high surface gravity ( dwarf ) stars .
We compare these deep spectra to detailed model atmospheres and stellar evolution models to infer the stellar parameters .
Our analysis reveals an effective temperature of 21000–28500 K , a rotational velocity of 60-170 km/s , and a surface gravity of 4.1–4.2 .
These parameters imply a spectral type of B0-B3V for these stars .
The inferred masses lie within 8–14 M _ { \odot } .
We derive an age of 6.6 ^ { +3.4 } _ { -4.7 } Myr for the star S2 , which is compatible with the age of the clockwise rotating young stellar disk in the GC .
We estimate the age of all other studied S-stars to be less than 15 Myr , which are compatible with the age of S2 within the uncertainties .
The relatively low ages for these S-stars favor a scenario in which the stars formed in a local disk rather than the field-binary-disruption scenario throughout a longer period of time .