We present results of 120 ks observation of a compact group of galaxies HCG 62 ( z = 0.0145 ) with Suzaku XIS and HXD-PIN .
The XIS spectra for four annular regions were fitted with two temperature vapec model with variable abundance , combined with the foreground Galactic component .
The Galactic component was constrained to have a common surface brightness among the four annuli , and two temperature apec model was preferred to single temperature model .
We confirmed the multi-temperature nature of the intra-group medium reported with Chandra and XMM-Newton , with a doughnut-like high temperature ring at radii 3.3–6.5 ^ { \prime } in a hardness image .
We found Mg , Si , S , and Fe abundances to be fairly robust .
We examined the possible “ high-abundance arc ” at \sim 2 ^ { \prime } southwest from the center , however Suzaku data did not confirm it .
We suspect that it is a misidentification of an excess hot component in this region as the Fe line .
Careful background study showed no positive detection of the extended hard X-rays previously reported with ASCA , in 5–12 keV with XIS and 12–40 keV with HXD-PIN , although our upper limit did not exclude the ASCA result .
There is an indication that the X-ray intensity in r < 3.3 ^ { \prime } region is 70 \pm 19 % higher than the nominal CXB level ( 5–12 keV ) , and Chandra and Suzaku data suggest that most of this excess could be due to concentration of hard X-ray sources with an average photon index of \Gamma = 1.38 \pm 0.06 .
Cumulative mass of O , Fe and Mg in the group gas and the metal mass-to-light ratio were derived and compared with those in other groups .
Possible role of AGN or galaxy mergers in this group is also discussed .