Using new U BV RI H \alpha CCD photometric observations and the archival infrared and X-ray data , we have carried out a multi-wavelength study of a Perseus arm young galactic star cluster NGC 7419 .
An age of 22.5 \pm 3.0 Myr and a distance of 3230 ^ { +330 } _ { -430 } pc are derived for the cluster .
Our photometric data indicates a higher value of color excess ratio E ( U - B ) / E ( B - V ) than the normal one .
There is an evidence for mass segregation in this dynamically relaxed cluster and in the range 1.4 - 8.6 M \mbox { $ { } _ { \normalsize \odot } $ } , the mass function slope is in agreement with the Salpeter value .
Excess emissions in near-infrared and H \alpha support the existence of a young ( \leq 2 Myr ) stellar population of Herbig Ae/Be stars ( \geq 3.0 M _ { \odot } ) indicating a second episode of star formation in the cluster region .
Using XMM-Newton observations , we found several X-ray sources in the cluster region but none of the Herbig Ae/Be stars is detected in X-rays .
We compare the distribution of upper limits for Herbig Ae/Be stars with the X-ray distribution functions of the T-Tauri and the Herbig Ae/Be stars from previous studies , and found that the X-ray emission level of these Herbig Ae/Be stars is not more than L _ { X } \sim 5.2 \times 10 ^ { 30 } erg s ^ { -1 } , which is not significantly higher than for the T-Tauri stars .
Therefore , X-ray emission from Herbig Ae/Be stars could be the result of either unresolved companion stars or a process similar to T-Tauri stars .
We report an extended X-ray emission from the cluster region NGC 7419 , with a total X-ray luminosity estimate of { \sim 1.8 \times 10 ^ { 31 } ~ { } erg~ { } s ^ { -1 } ~ { } arcmin ^ { -2 } } .
If the extended emission is due to unresolved emission from the point sources then we estimate \sim 288 T-Tauri stars in the cluster region each having X-ray luminosity { \sim 1.0 \times 10 ^ { 30 } ~ { } erg~ { } s ^ { -1 } } .
Investigation of dust attenuation and ^ { 12 } CO emission map of a square degree region around the cluster indicates the presence of a foreground dust cloud which is most likely associated with the local arm star forming region ( Sh2-154 ) .
This cloud harbors uniformly distributed pre-main-sequence stars ( 0.1 - 2.0 M \mbox { $ { } _ { \normalsize \odot } $ } ) , with no obvious trend of their distribution with either ( H - K ) excess or A _ { { } _ { V } } .
This suggests that the star formation in this cloud depend mostly upon the primordial fragmentation .