***[[1705.00013 : Montero-Dorta+ "OBSERVATIONAL EVIDENCE OF GALAXY ASSEMBLY BIAS">https://arxiv.org/pdf/1705.00013.pdf]] [#obb728be]
-SDSS LRGのスペクトルフィット
-Formation @ z=5 と z=1.5に分かれる
-z=5のほうがclustering が強い。assembly bias
**[[Reviews>./Reviews]] [#v621b2c8]
**[[輝線比診断>./輝線比診断]] [#i9a66fd6]
**[[Dust Extinction>./Dust Extinction]] [#m6c60e5f]
**[[Radio Galaxy>./Radio Galaxy]] [#f028315b]
**Galaxy Evolution [#te091550]
***[[Blind Surveys>./Blind Surveys]] [#l6fc50e9]
***[[z=1-3 Galaxies>./z=1-3 Galaxies]] [#obe8b557]
***[[z>5 Galaxies>./zgt5 Galaxies]] [#z92c7e2c]
***[[Submm Galaxies>./Submm Galaxies]] [#c131b660]
***[[Simulation>./Simulation]] [#uf140f68]
***[[FIR Emission Line>./FIR Emission Line]] [#md6abdd5]
***[[Emitters>./Emitters]] [#z89e25bf]
***[[Quiescent Galaxies>./Quiescent Galaxies]] [#db4586c4]
***[[Morphology/Structure>./Morphology Structure]] [#z11e439c]
***[[Molecular Gas>./Molecular Gas]] [#rfb70a65]
***[[Absorption Line Systems>./Absorption Line Systems]] [#hb8ca55f]
***[[Quasar/AGN Host>./Quasar AGN Host]] [#yc214359]
***[[Cluster Galaxies>./Cluster Galaxies]] [#r75a5a02]
**[[Hi-z Quasars>./Hi-z Quasars]] [#c4728182]
**[[Local Galaxies>./Local Galaxies]] [#ibaef5fd]
**[[Reionization>./Reionization]] [#d4c70533]
**[[Instruments>./Instruments]] [#gc033eac]

***[[1705.01946 : Guo+ "CANDELS Sheds Light on the Environmental Quenching of Low-mass Galaxies">https://arxiv.org/pdf/1705.01946.pdf]] [#e593f22c]
-CANDELSのz=0.5-1 quiescent galaxiesのenvironmental quenching の評価
-最も近いmassive companionまでの距離(d_proj)は、星形成銀河に比べて有意に小さい

***[[1705.01559 : Fudamoto+ "The Dust Attenuation of Star-forming Galaxies at z∼3 and Beyond: New Insights from ALMA Observations">https://arxiv.org/pdf/1705.01559.pdf]] [#zcf19fe1]
-z=3-6 1e11Msol gal : ALMA B6 obs => IRX/beta relation
-z=3ではlocalの関係とほぼ同じ。SMC extinction curveは平均としては棄却される
-z>4では崩れる。IRX-beta, IRX-M* 関係は、IRXが小さいほうに振れる(IR luminosity が小さい)。まあ、これについては当たり前、というかこれまでの観測。

***[[1705.01101 : Khostovan+ "The clustering of Hβ+[OIII] and [OII] emitters since z~5: dependencies with line luminosity and stellar mass">https://arxiv.org/pdf/1705.01101.pdf]] [#n805cab7]
-7000個のHb+[OIII](z=0.8-3.2)) & [OII](z=1.5-4.7) emitter clustering
-HbO3 emitter : Mhalo=1e10.7-12.1Msol, O2 emitter : Mhalo=1e11.5-12.6Msol
-lineが強いほどclusteringも強い。見かけ上z依存しないが、luminosity evo.をいれるとする。


トップ   新規 一覧 検索 最終更新   ヘルプ   最終更新のRSS