Accretion disk wind in the AGN broad-line region: Spectroscopically resolved line profile variations in Mrk100

An Infrared View ofClusters of Galaxies: CLEVLMyung Gyoon Lee ()Gwang-Ho Lee ()Seoul National UniversitySeoul, KoreaWith AKARI/CLEVL team(H.M. Lee, M. Im, H.S. Hwang, S.J. Kim, N. Hwang, J.C. Lee, S. Lim, H. Shim, J. Ko, H. Seo, H. Matsuhara, T. Kodama, T. Takagi, T. Nakagawa, T. Wada, Y. Koyama, T. Goto, et al.) Hello, My name is Gwang-Ho Lee, phd student from Seoul National University. Unfortunately, prof. Myung Gyoon Lee can not come here, so I present this talk instead of him. The title is An Infrared View of Cluster of Galaxies: CLEVL.

1OutlineOverview of clusters of galaxiesAn AKARI Mission program: The CLusters of galaxies EVoLution (CLEVL)Future WISE studyThis is outline of this talk. I introduce what CLEVL is.and present what we have done. And let you know our future plan with WISE data. 2A New Era for ClustersOptical: clustering of galaxies (~1950s, Zwicky and Abell)X-ray: Discovery of Hot ICM Infrared: Unobscured view of the SFA (NIR/MIR/FIR)Ground-based: 2MASS GMT, TMT, eELT etc.Space: ISO, AKARI, SST, Herschel, WISE JWST, SPICA, etc.

WISEA3395 (z=0.051)AKARIA2219 (z=0.226)Galaxy clusters are the most massive systems in universe, serving as high-density environment.So, they provide an excellent laboratory for studying galaxy evolution. Since the 1950, there are many studies on galaxy clusters using optical & X-ray, radio data. 21C is a new era for studying clusters, because we can have an infrared view of galaxy clustersthanks to several ground-based or space telescopes including AKARI! 3CLEVLCLusters of galaxies EVoLution studiesAKARI Mission Program (PI: Hyung Mol Lee)Instruments: AKARI / IRC (N3, N4, S7, S11, L15, L24) Three GroupsLow-z (z 10 GyrIntermediate MIR-excessages 1~10 Gyrsmall amount of SFStrong MIR-excess

Star-formingThis figure is from Shim et al. 2011 on Merging cluster Abell 2255. She divide galaxies into three group by (N3-S11) color. (N3-S11) red galaxies have a strong MIR-excess, and they are mainly star-forming galaxies. (N3-S11) blue galaxies have a weak MIR-excess, they are mainly passively evolving galaxies with stellar population older than 10 Gyr. Galaxies between two types are intermediate MIR-excess galaxies having small amount of SFwith stellar ages between 1 to 10 Gyr. We performed our analysis based on this classification. 11Color-Magnitude Diagram

+ Crosses(N3-S11) < -2.0 Circles-2.0(N3-S11) < -1.2Weak MIR-excess Diamonds-1.2(N3-S11) < 0.2Intermediate MIR-excess Stars(N3-S11) 0.2Strong MIR-excessThis is color-magnitude diagrams of nine clusters. Circles, diamonds, and stars represent respectively, weak, intermediate, and strong MIR-excess galaxies.

12(N3-S11) Color Distribution

Some clusters (A2219, A2255, A3128) have fraction of high-SFR galaxies larger than 15%.

core-crossingmergingbinary Age (Gyr)1>10Lets see (N3 S11) color distribution of nine Abell clusters.We can focus on several things.

First, the MIR-red, star-forming galaxy fraction varies from cluster to cluster.These three clusters show high star-forming galaxy fraction larger than 15%.

Second point, the color distribution of the MIR-blue galaxies also varies from cluster to cluster.This color dispersion indicates large spread in stellar age. From this result, we get a information on diverse star formation history and starbursting epoch in each cluster.13Radial variationMIR-red galaxies are preferentially located in the outskirt.

This figure displays (N3S11) color versus the clustercentric radius of our clusters.We can see that the MIR-red galaxiesare mainly located in the outer region of each cluster. Whereas central region of cluster is dominated by weak MIR-excess galaxies. 14Spatial distribution of galaxiesAbell 2218 (z = 0.176)Abell 2219 (z = 0.226)Abell 3128 (z = 0.060)and others

From now on, I show you spatial distribution of member galaxies of some clusters. 15Spatial distribution of galaxiesThe central region of A2218 is dominated by weak (or intermediate) MIR-excess galaxies.

Ko et al. 2009

WMIR IMIR SMIR MIR-excessA2218 is a the most relaxed system among our nine clusters. Red line is 1 virial radius of this cluster, and blue line represent 0.5 viral radius.(The central region is dominated by weak or intermediate MIR-excess galaxies.)Ko et al. 2009 focused on early-type galaxies in this cluster. They found MIR-excess early-type galaxies are mainly located in outskirt region. We updated the member galaxies using recent spectroscopic data, found MIR-excess galaxiesmore than before in the central region of the cluster. 16Spatial distribution of galaxiesX-ray: A2219 is elongated in the SE-NW direction.At R0.2 is >20%.A3128 encountered a tidal interaction with A3125 (~ 6Mpc).

Werner et al. 20071 MpcA3125 direction WMIR IMIR SMIRAbell 3128 is very interesting object. X-ray contours show two cores separated by 12 arcmin, corresponding about 1 Mpc.In addition, this cluster is interacting with A3125 away from 6 Mpc toward this direction.

This cluster has a highest fraction of star-forming galaxies. It seems that interaction between two clusters triggers Star formation activity. 18Spatial distribution of galaxies

Compactmerger(starting)ComplexmultiplestructuresBinaryclusterwith A3391Core regionin SSThese plots are for remaining clusters. To save time, I skip this page. 19SSFR for clustersS11 absolute magnitude SFR SSFR = SFR (for SFR > 2.0 M yr-1 within 0.5 R 200,cl) / Mcluster

Bai et al. 2007 This StudyAbell 2255Abell 2218Abell 2219In order to compare the star formation activity of our clusters with the other clusters, we measure Specific star formation rate of clusters using S11 absolute magnitude. Triangles are previous results in literatures, while our result of three cluster, A2218, A2219, and A2255, is marked as red stars. Dotted lined is evolutionary trend of SSFR for galaxy clusters, our three points follow this lines very well.

20Future WISE study Wide-field Infrared Survey ExplorerAll-sky (preliminary DR covers 57% of whole sky)Wavelength: 3.4 (W1), 4.6 (W2), 12 (W3) and 22m (W4)

March 2012Last part of our talk. I introduce our plan for future work with WISE data. WISE is completed all sky survey 2 years ago in four infrared bands, 3.4, 4.6, 12, 22 microns.Last years the 1st data is released covering 57% of whole sky. Next month, we can use 2nd DATA release covering all sky. 21Abell 2199 SuperclusterThe most mass systems in nearby universe: z = 0.03

A2199 is kinematically connected to A2197E/W and infalling galaxy groups.

An excellent laboratory for studying galaxy evolution, thanks to a high-density environment and complex structures.

Lee et al. in prep.

This is wide-field number density map of Abell 2199 supercluster made using WISE data. This supercluster is the most massive system in nearby universe. A2199 is located in the center of the supercluster, and it is kinematically connected to other clustersand several galaxy groups. Our CLEVL data covers only core region of this supercluster. For this reason, there are many limits to study environmental effect on galaxy properties. Therefore, if we use WISE data, we are able to study IR galaxy properties in diverse environment, including cluster, group, even field.

22Summary & ConclusionAKARI (N3-S11) color is a very efficient tool to find MIR excess galaxies in clusters.

The fraction of star forming galaxies varies among clusters.

Star forming galaxies in clusters are located preferentially in the outskirts.

AKARI opened a new era for galaxy clusters, and WISE also will do!

this is summary. Thanks for hearing my talk. 23