{"id":373,"date":"2014-12-10T13:45:56","date_gmt":"2014-12-10T04:45:56","guid":{"rendered":"http:\/\/guas-astronomy.jp\/weblog\/?p=373"},"modified":"2016-06-16T11:34:10","modified_gmt":"2016-06-16T02:34:10","slug":"searching-for-protoclusters-probabilistic-selection-of-z6-quasars-initial-results-from-the-first-hsc-ssp-data","status":"publish","type":"post","link":"https:\/\/guas-astronomy.jp\/weblog\/?p=373","title":{"rendered":"Searching for Protoclusters \/ Probabilistic Selection of z>6 Quasars: Initial Results from the First HSC SSP Data"},"content":{"rendered":"<p>[Speaker1]<br \/>\nJun Toshikawa, D3, SOKENDAI, Mitaka(supervisor: Nobunari Kashikawa)<br \/>\n[Title1]<br \/>\nSearching for Protoclusters<\/p>\n<p>[Speaker2]<br \/>\nMasafusa Onoue, M2, SOKENDAI, Mitaka(supervisor: Nobunari Kashikawa)<br \/>\n[Title2]<br \/>\nProbabilistic Selection of z>6 Quasars: Initial Results from the First HSC SSP Data<br \/>\n[Abstract]<br \/>\nI will present my high-z quasar selection method using SED fitting and its application to the first HSC-SSP data.<br \/>\nWhile it is a well-known problem that the classical quasar selection based on two colors suffers from contaminating sources such as brown dwarfs, photometric redshift with multi-color photometry is a complementary way to effectively isolate high-z quasars. Since photo-z for AGN has been less explored comparing with photo-z for galaxies, I have developed template SED fitting method by myself to construct the largest z>6 quasar sample with the HSC survey.<br \/>\nIn this talk, I will show how our selection works on the existing quasar samples such as z>3 quasars in the COSMOS field, and then report the result of the first application to the HSC-SSP data products, which results in five z>6 quasar candidates including one possible highest-redshift (z_photo=7.3) quasar.<\/p>\n","protected":false},"excerpt":{"rendered":"<p>[Speaker1] Jun Toshikawa, D3, SOKENDAI, Mitaka(supervisor: Nobunari Kashikawa) [Title1] Searching for Protoclu [&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-373","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\/373","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=373"}],"version-history":[{"count":0,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/posts\/373\/revisions"}],"wp:attachment":[{"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=373"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=373"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=373"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}