Prospects for a multi-TeV gamma-ray sky survey with the LHAASO water Cherenkov detector array *
Authors: Aharonian F. , Alekseenko V. , An Q. , Axikegu  , Bai L.X. , Bao Y.W. , Bastieri D. , Bi X.J. , Cai H. , Cao Zhe , Cao Zhen , Chang J. , Chang J.F. , Chang X.C. , Chao S.P. , Chen B.M. , Chen J. , Chen L. , Chen L. , Chen M.L. , Chen M.J. , Chen Q.H. , Chen S.H. , Chen S.Z. , Chen T.L. , Chen X.L. , Chen Y. , Cheng N. , Cheng Y.D. , Cui S.W. , Cui X.H. , Cui Y.D. , Dai B.Z. , Dai H.L. , Dai Z.G. , Danzengluobu  , D'Ettorre Piazzoli B. , Fang J. , Fan J.H. , Fan Y.Z. , Feng C.F , Feng L. , Feng S.H. , Feng Y.L. , Gao B. , Gao Q. , Gao W. , Ge M.M. , Geng L.S. , Gong G.H. , Gou Q.B. , Gu M.H. , Guo Y.Q. , Guo Y.Y. , Han Y.A. , He H.H. , He J.C. , Heller M. , He S.L. , He Y. , Hou C. , Huang D.H. , Huang Q.L. , Huang W.H. , Huang X.T. , Hu H.B. , Hu S. , Jia H.Y. , Jiang K. , Ji F. , Jin C. , Ji X.L. , Levochkin K. , Liang E.W. , Liang Y.F , Li Cheng , Li Cong , Li F. , Li H. , Li H.B. , Li H.C. , Li H.M. , Li J. , Li K. , Li W.L. , Li X. , Li X.R. , Li Y. , Li Z. , Li Z. , Liu B. , Liu C. , Liu D. , Liu H.D. , Liu H. , Liu J. , Liu J.Y. , Liu M.Y. , Liu R.Y. , Liu S.M. , Liu W. , Liu Y.N. , Liu Z.X. , Long W.J. , Lu R. , Lv H.K. , Ma B.Q. , Ma L.L. , Mao J.R. , Masood A. , Ma X.H. , Mitthumsiri W. , Montaruli T. , Nan Y.C. , Pattarakijwanich P. , Pei Z.Y. , Qiao B.Q. , Qi M.Y. , Ruffolo D. , Rulev V. , Sáiz A. , Shao L. , Shchegolev O. , Sheng X.D. , Shi J.R. , Stenkin Y. , Stepanov V. , Sun Z.B. , Tam P.H.T. , Tang Z.B. , Tian W.W. , Volpe D.D. , Wang C. , Wang H. , Wang H.G. , Wang J.C. , Wang L.Y. , Wang W. , Wang W. , Wang X.G. , Wang X.Y. , Wang X.J. , Wang Y.D. , Wang Y.J. , Wang Y.N. , Wang Y.P. , Wang Z. , Wang Z.H. , Wang Z.X. , Wei D.M. , Wei J.J. , Wen T. , Wu C.Y. , Wu H.R. , Wu S. , Wu W.X. , Wu X.F. , Xiang G.M. , Xiao G. , Xin G.G. , Xing Y. , Xu R.X. , Xue L. , Yan D.H. , Yang C.W. , Yang F.F. , Yang L.L. , Yang M.J. , Yang R.Z. , Yang S.B. , Yao Y.H. , Yao Z.G. , Ye Y.M. , Yin L.Q. , Yin N. , You X.H. , You Z.Y. , Yuan Q. , Yu Y.H. , Jiang Z.J. , Zeng H.D. , Zeng T.X. , Zeng W. , Zeng Z.K. , Zha M. , Zhang B.B. , Zhang H.M. , Zhang H.Y. , Zhang J.L. , Zhang J.W. , Zhang L. , Zhang P.F. , Zhang P.P. , Zhang S.R. , Zhang S.S. , Zhang X. , Zhang X.P. , Zhang Yi , Zhang Yong , Zhang Y.F.g , Zhao B. , Zhao J. , Zhao L. , Zhao L.Z. , Zheng F. , Zheng Y. , Zhou J.N. , Zhou P. , Zhou R. , Zhou X.X. , Zhu C.G. , Zhu F.R. , Zhu H. , Zhu K.J. , Zuo X. 
Published: June 2020

The Water Cherenkov Detector Array (WCDA) is a major component of the Large High Altitude Air Shower Array Observatory (LHAASO), a new generation cosmic-ray experiment with unprecedented sensitivity, currently under construction. WCDA is aimed at the study of TeV

-rays. In order to evaluate the prospects of searching for TeV

-ray sources with WCDA, we present a projection of the one-year sensitivity of WCDA to TeV

-ray sources from TeVCat using an all-sky approach. Out of 128 TeVCat sources observable by WCDA up to a zenith angle of

, we estimate that 42 would be detectable in one year of observations at a median energy of 1 TeV. Most of them are Galactic sources, and the extragalactic sources are Active Galactic Nuclei (AGN).