The results of Suzaku observations of the outskirts of Abell 3395 including a large-scale structure filament toward Abell 3391 are presented .
We measured temperature and abundance distributions from the southern outskirt of Abell 3395 to the north at the virial radius , where a filament structure has been found in the former X-ray and Sunyaev-Zel ’ dovich effect observations between Abell 3391 and 3395 .
The overall temperature structure is consistent with the universal profile proposed by \citet Okab14 for relaxed clusters except for the filament region .
A hint of the ICM heating is found between the two clusters , which might be due to the interaction of them in the early phase of a cluster merger .
Although we obtained relatively low metal abundance of Z = 0.169 ^ { +0.164 + 0.009 + 0.018 } _ { -0.150 - 0.004 - 0.015 } solar , where the first , second , and third errors are statistical , cosmic X-ray background systematic , and non X-ray background systematic , respectively , at the virial radius in the filament , our results are still consistent with the former results of other clusters ( Z \sim 0.3 solar ) within errors .
Therefore , our results are also consistent with the early enrichment scenario .
We estimated Compton y parameters only from X-ray results in the region between Abell 3391 and 3395 assuming a simple geometry .
They are smaller than the previous SZ results with Planck satellite .
The difference could be attributed to a more elaborate geometry such as a filament inclined to the line-of-sight direction , or underestimation of the X-ray temperature because of the unresolved multi-temperature structures or undetected hot X-ray emission of the shock heated gas .