Slide 1

Florent Rostagni 1 Slide 2 Context Sample Algorithm for detection and classification Star formation X-ray optical study Perspectives - Conclusion 2 Slide 3 t Big-Bang~380 000 years Present Cosmic Microwave Background Galaxy distribution T/T ~10 -5 / ~ 200 GRAVITATION 3 Slide 4 STRUCTURES: FILAMENTS CLUSTERS > 100 galaxies 10 13 M. M 10 15 M. ~ 1 Mpc 4 Slide 5 structure formation rate cosmological parameters dynamical state of clusters 5 Slide 6 6 Cohn & White 2005 1.510.5 z 1.510.5 z Slide 7 7 Cohn et al. 2001 Slide 8 GALAXIES 1930 optical 5% of the mass GAS 1980 X-ray 15% of the mass DARK MATTER 1980 gravitationnal lens 80% of the mass 8 Slide 9 REGULAR CLUSTERIRREGULAR CLUSTER 9 Slide 10 Projected galaxy disribution King profile 1 Mpc Galaxy orbits gaussian velocity distribution 10 Slide 11 OPTICALX-RAY Galaxy contents Wavelets Adaptive kernel Centroid shift Power ratio elliptcity - projection effects - point distribution + whole cluster + no projection effect + continuous field - cluster core SKY PLANE 11 Slide 12 Redshift information along the line of sight SDSS 25% of the sky spec. complete up to r=17.5 best survey at low z available C4 clusters: detected using 4 colors 12 Slide 13 Search for concentration of galaxies in a 4 color space Galaxy with 6-th nearest distance neighbour = C4 cluster center All galaxies within r 15 are assigned to the cluster 13 Slide 14 Results: 90% complete 95% pur 98% of X-Ray clusters 90% of Abell clusters 14 Slide 15 Centering: Definition of the cluster center (6-th nearest neighbour in color space) Piling up of structures along the line of sight: Due to only use of colors 1. Loss of some C4 clusters 2. Split of C4 clusters in several units 15 Slide 16 What we have: 218 catalogs (fields) of galaxies around 10Mpc of C4 clusters with enough measured spectra What we use: Position Photometric magnitude in r-band Spectroscopic (60%) and photometric redshift 16 Slide 17 Search for galaxy concentrations in phase space 6 coordinates of galaxies ( , ,z) only available 3D ( , ,z) ? 1D (z) + 2D ( , ) Construction of distribution functions based on wavelets + measure of deviations to relaxed ones 17 Slide 18 Fields z Fields z f(z) wavelets 18 Slide 19 Fields z Fields z f(z) wavelets Packets Peaks Ngal>50 EMMIX 19 Slide 20 22 20 Slide 21 21 Fields z Fields z f(z) wavelets Packets Peaks Ngal>50 EMMIX Slide 22 22 156 peaks Slide 23 List of peaks 2 cases distant peaks close peaks 23 POTENTIALLY RELAXED INTERACTION Slide 24 24 Slide 25 Isolated or interacting peak ( , ) Isolated or interacting peak ( , ) Density maps ( 2-10Mpc) Density maps ( 2-10Mpc) Cluster catalog waveletsSExtractor 3Mpc density maps (0.5-3Mpc) 3Mpc density maps (0.5-3Mpc) wavelets Sub-stucture catalog SExtractor Ngal > Ngal max / 10 25 Cluster catalog Slide 26 3 cases 1 clump one main clump several heavy clumps POTENTIALLY RELAXED INTERACTION weight criteria: 1:10 26 Sub-stucture catalog Slide 27 POTENTIALLY RELAXED POTENTIALLY RELAXED INTERACTION PEAKS POTENTIALLY RELAXED INTERACTION CLUMPS RELAXED INTERACTION 27 Slide 28 218 C4 fields 110 packets 156 peaks 98 isolated peaks 216 clusters 29 isolated clusters 28 Isolated clusters rate ~ 13% Slide 29 Classification: relaxed interacting Improvements: introduce ellipticity in classification interacting: elaborate sub-categories with bimodal.... 29 Slide 30 Collaboration with H. Bourdin Data for 18 C4 clusters with XMM Galaxy: collisionless Gas: collisional Different dynamical time Different morphologies Dynamical state + Fusion stage 30 Slide 31 31 OpticalX-Ray Slide 32 Temperature maps dynamical state, cold core 32 Slide 33 What is the influence of cluster dynamical state on star formation rate of their host galaxies? Does cluster merging speed up star formation in galaxies or in contrary does it stop star formation? Is it the case for all galaxies? If not, where are star forming galaxies and/or star formation stopping galaxies? 33 Slide 34 Galaxy type determined by spectra: Unclassified or not used Star forming Composite AGN Low S/N liner Fraction of SF galaxies in clumps 34 Slide 35 Classification of galaxy clusters ~13 % isolated clusters 35 Slide 36 Use of z phot : Impact of its use on classification, control of errors Application of classification to CFHT-LS data: more galaxies deeper Evolution of fusion rate with time 36 Slide 37 37