\u3010\u65e5\u6642\u301110\u670812\u65e5(\u6c34)\u300010:30\uff5e12:00
\n\u3010\u5834\u6240\u3011\u56fd\u7acb\u5929\u6587\u53f0\u30fb\u4e09\u9df9\u3000\u4e2d\u592e\u68df\uff08\u5317\uff091\u968e \u8b1b\u7fa9\u5ba4
\n\u3010\u767a\u8868\u8005\uff08\u656c\u79f0\u7565\uff09\u3011\u4eca\u702c \u4f73\u4ecb\uff08\u7dcf\u7814\u5927 D1\u30fb\u30cf\u30ef\u30a4\u3001\u6307\u5c0e\u6559\u54e1 : \u5150\u7389 \u5fe0\u606d & \u4eca\u897f \u660c\u4fca\uff09
\n\u3010\u30bf\u30a4\u30c8\u30eb\u3011\u8fd1\u8d64\u5916\u7ddaPa\u03b1\u306b\u3088\u308bMBH\u306e\u63a8\u5b9a(Estimating Black Hole Masses Using Pa\u03b1 emission line)
\nAbstruct\uff1a
\nActive Galactic Nuclei (AGNs) are luminous objects, found in the nuclei of galaxies.
\nIt is believed that they have suppermassive 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) Today, masses of black holes of AGNs (MBHs) are mainly estimated with broad optical and UV emission lines (H\u03b1, 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 and Pa\u03b2 lines, two of the strongest lines 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, the strongest line in NIR, as a new estimator of MBHs for dusty AGNs.
\nIn the colloquium, we report the present results and our future work.<\/p>\n","protected":false},"excerpt":{"rendered":"
\u3010\u65e5\u6642\u301110\u670812\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\uff08\u656c\u79f0\u7565\uff09\u3011\u4eca\u702c \u4f73\u4ecb\uff08\u7dcf\u7814\u5927 D1\u30fb\u30cf\u30ef\u30a4\u3001\u6307\u5c0e\u6559\u54e1 : \u5150\u7389 \u5fe0\u606d & \u4eca\u897f \u660c\u4fca\uff09 \u3010\u30bf\u30a4\u30c8 […]<\/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-99","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\/99","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=99"}],"version-history":[{"count":0,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/posts\/99\/revisions"}],"wp:attachment":[{"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=99"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=99"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=99"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}