{"id":116,"date":"2012-04-24T16:37:59","date_gmt":"2012-04-24T07:37:59","guid":{"rendered":"http:\/\/guas-astronomy.jp\/weblog2\/?p=116"},"modified":"2012-04-24T16:37:59","modified_gmt":"2012-04-24T07:37:59","slug":"high-z_qso_survey_at_z_6_and_7_1","status":"publish","type":"post","link":"https:\/\/guas-astronomy.jp\/weblog\/?p=116","title":{"rendered":"High-z QSO survey at z ~ 6 and 7 with Suprime-Cam \/ The new black hole mass estimator: Pa\u03b1"},"content":{"rendered":"<p>\u3010\u65e5\u6642\u30114\u670825\u65e5(\u6c34)\u300010:30\uff5e12:00<br \/>\n\u3010\u5834\u6240\u3011\u56fd\u7acb\u5929\u6587\u53f0\u30fb\u4e09\u9df9\u3000\u4e2d\u592e\u68df\uff08\u5317\uff091\u968e \u8b1b\u7fa9\u5ba4<br \/>\n\u3010\u767a\u8868\u8005\uff11\u3011Yoshifumi Ishizaki \uff08\u7dcf\u7814\u5927 D2\u30fb\u4e09\u9df9\u3001\u6307\u5c0e\u6559\u54e1 : Nobunari Kashikawa\uff09<br \/>\n\u3010\u30bf\u30a4\u30c8\u30eb\u3011High-z QSO survey at z ~ 6 and 7 with Suprime-Cam<br \/>\n\u30a2\u30d6\u30b9\u30c8\u30e9\u30af\u30c8<br \/>\nWe are on going deep zB\/zR imagings for 7 deg^2 in total of UKIDSS-DXS \ufb01elds in order to detect high-z QSOs around z \u223c 7 down to J<23.5. This observation is a new search for the most distant QSOs around z = 6 and 7 utilizing the unique capabilities of wide-\ufb01eld imaging of Subaru\/Suprime-Cam,\nits high-sensitivity CCDs at \u301c 1\u03bcm, and special filters to effectively isolate high-z QSOs from M\/L\/T dwarfs. I will speak about the unique way of observation mainly.\n\u3010\u767a\u8868\u8005\uff12\u3011Keisuke Imase \uff08\u7dcf\u7814\u5927 D2\u30fb\u4e09\u9df9\u3001\u6307\u5c0e\u6559\u54e1 : Masatoshi Imanishi\uff09\n\u3010\u30bf\u30a4\u30c8\u30eb\u3011The new black hole mass estimator: Pa\u03b1\n\u30a2\u30d6\u30b9\u30c8\u30e9\u30af\u30c8\nActive Galactic Nuclei (AGNs) are luminous objects, found in the centre of galaxies.\nIt is believed that they have supermassive black hole and accretion disk in their central region, surrounded with broad-line region(BLR).\nThis picture is called \"Unified model for AGN\" (e.g., Antonucci 1993)\nToday, the correlation between masses of black holes of AGNs (MBHs) and the properties of their host galaxies has been found (so-called \"co-evolution\").\nTherefore, it is very important to estimate MBHs of more AGNs in more accurate way.\nMBHs are mainly estimated with broad optical and UV emission lines (H\u03b2, MgII), using their line width and flux.\nMore than half of AGNs, however, are affected with the foreground gas and dust.\nFor such AGNs (so-called \"dusty AGNs\"), it is difficult to use UV\/optical lines as estimators of MBHs.\nOn the other hand, Pa\u03b1 line, the strongest line in near-infrared(NIR) and free of blending, are detectable in \"dusty AGNs\" and ultra luminous IR galaxy(ULIRG).\nWe have observed 21 nearby PG QSOs with IRTF\/SpeX in order to establish Pa\u03b1 lines as a new estimator of MBHs for dusty AGNs.\nIn the colloquium, we report the present results and our future work.\n\n<\/p>\n","protected":false},"excerpt":{"rendered":"<p>\u3010\u65e5\u6642\u30114\u670825\u65e5(\u6c34)\u300010:30\uff5e12:00 \u3010\u5834\u6240\u3011\u56fd\u7acb\u5929\u6587\u53f0\u30fb\u4e09\u9df9\u3000\u4e2d\u592e\u68df\uff08\u5317\uff091\u968e \u8b1b\u7fa9\u5ba4 \u3010\u767a\u8868\u8005\uff11\u3011Yoshifumi Ishizaki \uff08\u7dcf\u7814\u5927 D2\u30fb\u4e09\u9df9\u3001\u6307\u5c0e\u6559\u54e1 : Nobunari Kashika [&hellip;]<\/p>\n","protected":false},"author":2,"featured_media":0,"comment_status":"open","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[6,5],"tags":[],"class_list":["post-116","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\/116","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=116"}],"version-history":[{"count":0,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/posts\/116\/revisions"}],"wp:attachment":[{"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=116"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=116"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=116"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}