Barkhouse, W. A.Green, P. J.Viklinin, AlexeyKim, D.‐W.Perley, D.Cameron, R.Silverman, J.Mossman, A.Burenin, R.Jannuzi, B. T.Kim, M.Smith, M. G.Smith, R. C.Tananbaum, HarveyWilkes, Belinda2017-02-132006Barkhouse, W. A., P. J. Green, A. Vikhlinin, D.‐W. Kim, D. Perley, R. Cameron, J. Silverman, et al. 2006. “ChaMP Serendipitous Galaxy Cluster Survey.” The Astrophysical Journal 645 (2) (July 10): 955–976. doi:10.1086/504457.0004-637Xhttp://nrs.harvard.edu/urn-3:HUL.InstRepos:30212142We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13 deg2, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about ~10-14 ergs cm-2 s-1, with a median cluster core radius of 21''. For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4 m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z ~ 0.7. From the overlapping 6.1 deg2 X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog). The median redshift of the 13 X-ray/optical clusters is 0.41, and their median X-ray luminosity (0.5-2 keV) is LX = img1.gif × 1043 ergs s-1. The clusters in our sample that are only detected in our optical data are poorer on average (~4 σ) than the X-ray/optically matched clusters, which may partially explain the difference in the detection fractions.en-USGalaxies: clusters: generalSurveysX-rays: galaxies: clustersJournal Article2017-02-1310.1086/504457