{"id":186,"date":"2014-01-29T15:00:24","date_gmt":"2014-01-29T06:00:24","guid":{"rendered":"http:\/\/guas-astronomy.jp\/weblog\/?p=186"},"modified":"2016-06-16T11:34:31","modified_gmt":"2016-06-16T02:34:31","slug":"experimental-confirmation-for-clasps-spectrograph-alignment-procedure-etc","status":"publish","type":"post","link":"https:\/\/guas-astronomy.jp\/weblog\/?p=186","title":{"rendered":"Experimental confirmation for CLASP&#8217;s spectrograph alignment procedure etc."},"content":{"rendered":"<p>[Speaker 1]<br \/>\nGiono Gabriel  D1, SOKENDAI, Mitaka\uff08supervisor : Yoshinori Suematsu\uff09<br \/>\n[Title]<br \/>\nExperimental confirmation for CLASP&#8217;s spectrograph alignment procedure<br \/>\n[Abstract]<br \/>\n&#8211;<\/p>\n<p>[Speaker 2]<br \/>\nOnoue Masfusa  M1, SOKENDAI, Mitaka\uff08supervisor : Nobunari Kashikawa\uff09<br \/>\n[Title]<br \/>\nHigh-z Quasar Selection with Hyper Suprime-Cam<br \/>\n[Abstract]<br \/>\nQuasars at high (>6) redshift are one of the best tracers of early Universe,<br \/>\n thanks to its high luminosity and characteristic spectrum.<br \/>\n However, quasars are very rare objects and it is important to establish a method to<br \/>\n select quasars effectively.<br \/>\n Based on the above, I will present the strategy for identifying high-z quasars by using SED fitting (#HSC project 47).<br \/>\n The goal of this study is to effectively isolate high-z quasars from contaminating sources such as brown dwarfs.<br \/>\n We are going to apply SED fitting method for quasar selection along with conservative two-color selection.<br \/>\n I will report the current status of SED fitting code development, and preliminary results of its application.<br \/>\n In addition, I would like to introduce the recently found three z~7 quasars (Venemans+13). <\/p>\n","protected":false},"excerpt":{"rendered":"<p>[Speaker 1] Giono Gabriel D1, SOKENDAI, Mitaka\uff08supervisor : Yoshinori Suematsu\uff09 [Title] Experimental confirmat [&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-186","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\/186","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=186"}],"version-history":[{"count":0,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/posts\/186\/revisions"}],"wp:attachment":[{"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=186"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=186"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=186"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}