{"id":173,"date":"2014-01-10T13:51:18","date_gmt":"2014-01-10T04:51:18","guid":{"rendered":"http:\/\/guas-astronomy.jp\/weblog\/?p=173"},"modified":"2016-06-16T11:34:31","modified_gmt":"2016-06-16T02:34:31","slug":"mass-map-measurement-for-deep-lens-survey-field","status":"publish","type":"post","link":"https:\/\/guas-astronomy.jp\/weblog\/?p=173","title":{"rendered":"Mass map measurement for Deep Lens Survey Field"},"content":{"rendered":"<p>[Speaker 1]<br \/>\nJunya Sakurai M2, SOKENDAI, Mitaka\uff08supervisor : Satoshi Mitayaki\uff09<br \/>\n[Title]<br \/>\nMass map measurement for Deep Lens Survey Field<br \/>\n[Abstract]<br \/>\nMeasurement the evolution of dark matter distribution is the important<br \/>\ncosmological probe. For this probe, one of the promising techniques is<br \/>\nweak gravitational lensing. This measurement is sensitive to any<br \/>\nsystematic biases in measured quantities. lensfit (L. Miller et al., 2007)<br \/>\nwe use is able to yield unbiased measurement. Since lensfit has<br \/>\nrecognized as one of the most reliable tools based on mock simulation<br \/>\ndata analysis, we try to apply lensfit to Subaru Suprime-Cam data<br \/>\nanalysis.<\/p>\n<p>We get optical imaging data of Deep Lens Survey Field 2 from SMOKA. We<br \/>\nselect galaxies with 23<mag<26 and 4.0pix<FWHM<30.0pix as lensed galaxies,\nand then galaxy number density is 30.2\/arcmin^2. We reconstruct mass\ndistribution using these galaxies. We find 4 peaks at 4 times noise level\nin Deep Lens Survey Field 2 that are almost consistent with Y. Utsumi et\nal. (2013) using other method. In order to systematic errors, we measure\npixel distribution function (PDF). If there are no systematic errors, PDF of\ncross mode should be Gaussian form. Our result is close to Gaussian form, \nbut cross mode has excess on negative side that exist still systematic errors.\nTherefore, lensift reduces systematic errors, but we need to investigate \nexcess on negative side in PDF.\n\n<\/p>\n","protected":false},"excerpt":{"rendered":"<p>[Speaker 1] Junya Sakurai M2, SOKENDAI, Mitaka\uff08supervisor : Satoshi Mitayaki\uff09 [Title] Mass map measurement for [&hellip;]<\/p>\n","protected":false},"author":2,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[6,5],"tags":[],"class_list":["post-173","post","type-post","status-publish","format-standard","hentry","category-6","category-5"],"_links":{"self":[{"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/posts\/173","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/users\/2"}],"replies":[{"embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fcomments&post=173"}],"version-history":[{"count":0,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/posts\/173\/revisions"}],"wp:attachment":[{"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=173"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=173"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=173"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}