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(CEOU), 2Astronomy Program, FPRD, Department Of 2018 봄 학술대회 & KGU 연합학술대회 Park4 ~ ⊙ at ~ 0.5 and 0.7 respectively. 1 Center fore the Exploration of the Origin of the Photometric redshifts of the selected galaxies were 2 Universe (CEOU), Astronomy Program, FPRD, derived using LePHARE and Coleman Extended Department of Physics & Astronomy, Seoul templates. ~98% S11 selected galaxies are galaxies 3 4 National University, LOCOOP, Inc., Korea with 〈〉(median redshift) ~ 0.4, and ~96% L15 5 Astronomy and Space Science Institute, University selected galaxies are galaxies with 〈〉 ~ 0.6. Star 6 of Science and Technology, Korea Institute for formation rates and stellar mass of these galaxies 7 8 Advanced Study, Nature Astronomy, Arizona were calculated using MAGPHYS which derives State University, School of Earth and Space physical parameters with SED fitting. In the - Exploration, 9Subaru Telescope, National ⋆ diagram, 11 /15 selected galaxies are 10 Astronomical Observatory of Japan, School of located in the main sequence of star-forming Space Research and Institute of Natural Sciences, galaxies at ~ 1. Kyung Hee University [포GC-13] Photometric Properties and Spatial To investigate the impact of the high-redshift Distribution of RSGs of Nearby Galaxy quasars on cosmic reionization, the faint end slope System: Leo Triplet of the quasars luminosity function has to be determined precisely. More quasars with low Sowon Lee1, Howoo Chiang1 and Young-Jong Sohn1 luminosity are needed to constrain the contribution 1Department of Astronomy, Yonsei University to reionization in the early universe. However, finding these quasars has been regarded as tough We present the near infrared JHK photometric process owing to the improper shallow depth of properties and the spatial distribution of red imaging data. In recent days, the release data of supergiants(RSGs) of NGC 3623, NGC 3627 and NGC Subaru Hyper Suprime-Cam (HSC) Strategic 3628 in the Leo Triplet system using the data Program survey which provide the deep images obtained with 3.8m UKIRT(United Kingdom reaching ~ 25 mag facilitates searching the faint Infra-Red Telescope) at Hawaii. We checked quasars candidates. To find faint quasar interaction between the three galaxies by making a candidates in ELAIS-N1 field, along with the HSC spatial density map of RSGs. From (J-K,K)0 data, two near-infrared (NIR) data sets also be Color-Magnitude Diagram which include resolved used : The Infrared Medium-deep Survey (IMS) and stars in three galaxy and control field with PARSEC The UKIRT Infrared Deep Sky Survey (UKIDSS) – isochrone, we figured out the RSG candidates of Deep Extragalactic Survey (DXS). Quasar the Leo triplet are at 0.9<(J-K)0<1.2, mK<17.5 and candidates selected from the multi-band color cut separated them from background and foreground were observed by the SED camera for QUasars in sources. Using gaussian kernel density estimation, EArly uNiverse (SQUEAN) instrument. To trace the we drew spatial density map of RSGs in the Leo redshifted Lyman break efficiently, appropriate triplet with an assumption that all RSGs are an medium bands comparable to targeted redshift identical population. The density map shows range are chosen. The most reliable quasar extended features of NGC 3628 to NGC 3627 along candidates are finally determined through SED the declination direction. The asymmetries between fitting. Using this less luminous quasars NGC 3627 and NGC 3628 might be evidence for that candidates, we can speculate the relation between the distribution of actual star components(RSGs) the quasar growth and the host galaxy unbiasedly follows the neutral hydrogen distribution and also and estimate the contribution to the cosmic for interaction between two galaxies. And the reionization. extended features along the right ascension direction might be a supporting evidence for the [포GC-12] Specific star formation rate of the existence of a TDG(Tidal Dwarf Galaxy). In case of MIR-selected galaxies in AKARI NEP-Wide NGC 3623, we could not see any sign of interaction in density map. Dongseob Lee(이동섭), Hyunjin Shim(심현진) Kyungpook National University(경북대학교, KNU) [포GC-14] Hydrodynamics Simulation of the Off-Axis Cluster Merger Abell 115 We investigate the -⋆ relation of the infrared luminous galaxies selected in either 11 Wonki Lee, Mincheol Kim, M. James Jee and 15 from the 5.6 deg of the AKARI Department of Astronomy, Yonsei University NEP-Wide field. From the constructed multi-wavelength catalog spanning 0.3 to 24 Abell 115 is a renowned cluster merger at , we select 3,408 S11 > 50 galaxies and z=0.197. It exhibits an asymmetric X-ray 1,896 L15 > 20 galaxies which corresponds to 60 / Bull. Kor. Astron. Soc. Vol. 43 No.1, Apr. 2018 포스터발표초록 distribution with cometary tails and a Department of Astronomy. Yonsei University megaparsec-sized radio relic stretching in the northeastern direction from the core of the ZwCL 1447.2+2619 is a merging galaxy cluster at northern cluster. Many observations have z=0.37 with clear substructures in X-ray emission concluded that this cluster merger has a large and galaxy distribution. In addition, the system impact parameter, but there has been no possesses distinct radio relics. In order to numerical analysis on the structure of Abell 115. constrain the merger scenario, it is necessary to In this study, we simulate Abell 115 with Gadget2 measure both the distribution and mass of the N-body/SPH code to reproduce the X-ray and cluster dark matter. We perform weak lensing weak lensing features of Abell 115. We find a new analysis of ZwCL 1447.2+2619 using Subaru plausible merger scenario of Abell 115, wherein the imaging data. We detect clear lensing signal from northern cluster is currently in an outgoing phase. the cluster after carefully addressing instrumental The predicted X-ray emission has a similar systematics. In this poster, we present our morphology to the observed tail of the northern preliminary results on our mass reconstruction cluster. However, in order to reproduce the and discuss the comparison with X-ray and radio observed line-of-sight velocity and projected results. distance while maintaining the two systems gravitationally bound, the system should possess a [포GC-17] Preprocessing of dark halos in large projection angle, which makes the shock look hydrodynamic cluster zoom-in simulations considerably more diffused than the observed radio relic. San Han1, Rory Smith2, Hoseung Choi1, Luca Cortese3, Barbara Catinella3 [포GC-15] Determining the star formation 1Department of Astronomy, Yonsei University, 50 rate of type 2 AGNs with multi-wavelength Yonsei-ro, Seodaemun-gu, Seoul 03722, Republic SED from UV to radio of Korea, 2Korea Astronomy & Space Science Institute, Daejeon 305-348, Republic of Korea, 3 Jeong Ae Lee, and Jong-Hak Woo International Centre for Radio Astronomy Astronomy Program, Department of Physics and Research, University of Western Australia, 35 Astronomy, Seoul National University Stirling Highway, Crawley, WA 6009, Australia Outflows are common among local AGNs. Woo et To understand the assembly of the galaxy al. (2017) suggested that AGN feedback through population in clusters today, it is important to first outflows is delayed by a dynamical time scale understand the impact of previous environments before the suppression of SFR is observationally prior to cluster infall, namely preprocessing. We detected. However, these SFR have large use 15 cluster samples from hydrodynamic uncertainties because they were estimated by zoom-in simulation YZiCS to determine the Artificial Neural Network (ANN) method (Ellison et significance of preprocessing focusing primarily on al. 2016). the tidal mass loss of dark matter halos. We find We measured the SFR of 21 far-IR matched ~48% of the cluster member halos were once sources (z < 0.1) with total IR luminosity from satellites of another host. The preprocessed multi-wavelength SED fitting from UV to radio. 15 fraction is not a clear function of cluster mass. out of 21 sources were observed with JCMT Instead, we find it is related to each individual SCUBA-2 450 and 850um and 4 and 2 sources were cluster's recent mass growth history. We find that matched with archival data of JCMT SCUBA-2 and the total mass loss is a clear function of time spent Herschel SPIRE, respectively. We compared the in a host. However, two factors can considerably true SFR by SED fitting with ANN-based one. In increase the mass loss rate. First, if the satellite addition, we confirmed that sub-mm data are mass is approaching the mass of its host. Second, important to determine the SFR with total IR when the halo suffers tidal mass loss at a higher luminosity from SED fitting. Finally, we discuss the redshift. The preprocessing provides an significance of true SFR and further the AGN-SF opportunity for halos to experience tidal mass loss link. for a more extended period of time than would be possible if they simply fell directly into the cluster, [포GC-16] Subaru Weak-lensing Analysis of and at earlier epochs when hosts were more destructive to their satellites. the Merging Cluster ZwCL 1447.2+2619 at z=0.37 [포GC-18] Effects of galaxy-galaxy encounters on galactic spin and central Juheon Lee, Myungkook J. Jee mass distribution 한국천문학회보 제43권 1호, 2018년 5월 / 61.
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