[Speaker 1]
\nYuriko Saito
\nD1, SOKENDAI, Hawaii\uff08supervisor : Masatoshi Imanishi\uff09
\n[Title]
\nInvestigating the coevolution between SMBHs and galaxies at z~3
\n-our first result-
\n[Abstract]
\nIn the local universe, there is a tight correlation between the masses
\nof super massive black holes (SMBHs) and stars in the spheroidal
\ncomponents (bulge and elliptical galaxies), suggesting that their formation
\nis physically closely related. Various models assuming different physical
\nmechanisms are proposed to explain the observational result at z=0.
\nSince these models predict different redshift evolution of the
\nSMBH-spheroid mass ratio, it is important to observationally constrain
\nthe mass ratio at high redshift. As the predicted difference becomes
\nlarger at higher redshift, going to higher redshift is better to distinguish
\namong these models, but at the same time observational difficulties
\nincrease at higher redshift. By taking into account these factors,
\nwe have concluded that z=3-3.5 is practically the best redshift range.
\nHowever, previous studies have mostly been limited to z<2.\nWe have embarked on (1) systematic near-infrared spectroscopy of\nz=3-3.5 QSOs, to derive the SMBH masses, based on the the Balmer\nbeta emission line width and nearby continuum luminosity,\nand (2) Subaru LGS-AO near-infrared multi-color imaging observations,\nto estimate spheroidal stellar masses in the host galaxies of these QSOs.\n\nWe obtained spectroscopic data for 34 objects, and succeeded to derive\nBH masses for 24 objects among them. We have also performed Subaru AO\nimaging observations of 8 QSOs with estimated SMBH masses, and so far\ncompleted AO imaging data analysis of J0725.\nIn this talk, I will present our first result of SMBH mass \u2013 bulge\nmass ratio calculated for J0725.\n\n[Speaker 2]\nShogo Ishikawa\nM2, SOKENDAI, Mitaka\uff08supervisor : Nobunari Kashikawa\uff09\n[Title]\nThe clustering properties of star-forming galaxies at z~2 by extremely wide-field survey\n[Abstract]\nOne of the most critical method to trace the evolution history of galaxies is to compare the mass of dark haloes. Dark halo mass monotonically grows by merging with cosmic time\u3001 so this parameter reflects the growing history of galaxy directly. In recent years, a number of LBGs\/LAEs at z>3 are obtained and dark halo masses of z>3 galaxies are revealed.
\nOn the other hand, dark halo masses at z~2 is not so much explored because there are technical difficulties to observe galaxies at z~2. That is why z~2 is known as \u201credshift-desert\u201d; however, z~2 is also thought to be a important era to study galaxy formation and evolution.
\nWe conducted the wide field survey to obtain star-forming galaxies at z~2, applying so called \u201cBzK selection technique\u201d. In this talk, we report the results of clustering analysis of star-forming galaxies at z~2. Especially, we performed the full HOD analysis of z~2 galaxies the first in the world.<\/p>\n","protected":false},"excerpt":{"rendered":"
[Speaker 1] Yuriko Saito D1, SOKENDAI, Hawaii\uff08supervisor : Masatoshi Imanishi\uff09 [Title] Investigating the coevo […]<\/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-137","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\/137","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=137"}],"version-history":[{"count":0,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=\/wp\/v2\/posts\/137\/revisions"}],"wp:attachment":[{"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=137"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=137"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/guas-astronomy.jp\/weblog\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=137"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}