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1 ! # #%& () %+(%,#. / # 0 1(,& 23(4. 5( (67# :;! <73 % 0= %> #& (? # %&% (!) +%,! %./ !6+10! !: 7! )+1(,!: 7! log N/O log O/H !: 72!# /0!24230(.;,,4!! #.&#01!)<=!1 +! 3!!&./0%!=<>?! #1+ &#!3#0!.%301 ; +%!+1!(01&01!! 803Α00%!&, Β.025!)!( 4!80!! 0%1.;#09!/.!Χ+, ΕΦ 403!23 1?!!

2 Atypical faint galaxies in Coma: faint imaging view Florence Durret, Christophe Adami et al. Low surface brightness galaxies (LSBs): deep imaging 735 faint galaxies with absolute magnitudes B=-13 to -9 and central surface brightness as faint as 27 mag arcsec2 grouped around NGC 4889 and NOT around NGC 4874 Some of the LSBs associated with the western X-ray overdensities Large scale diffuse light structures are detected around NGC 4874 LSBs are remnants of normal galaxies transformed into LSBs by galaxy harassment and tidal stripping Spectral energy distributions Coma cluster LSBs are predominantly young (age < 2.3 Gyr) non-starburst objects A significant fraction of these LSBs is dusty (A V > 1.5) They are low stellar mass objects, with stellar masses comparable to globular clusters for the faintest ones The very faint end of the galaxy luminosity function The slopes of the GLFs are very steep (α~-2) and show no dip, and are consistent with debris from brighter disrupted and harrassed galaxies The faint western galaxies are mainly blue, and therefore late-type or issued from late-type galaxies in the infalling layers LSBs around the two main galaxies are predominantly blue, possibly coming from disk-like disrupted disks 5 candidate ultra compact dwarfs spectroscopically confirmed in Coma

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5 Massive black holes, nuclear star clusters, partially depleted cores and the connection with the host spheroid Alister W. Graham (Swinburne University of Technology) Galaxy Nuclei Central Stellar Deficits Additional Nuclear Components (Central Massive Object)-(Host Spheroid) mass relation M Elliptical -µ 0 diagram M bh - diagram Fornax, Virgo, Coma et al. (ESO Garching, 27 June - 1 July, 2011)

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7 Ultraviolet Properties of galaxies in the Fornax cluster 1. Data Virgo cluster Fornax cluster 2. UV CMR UV data GALEX (FUV,NUV) GR6 - RA(deg): 192 ~ 181, DEC(deg): 2 ~ 19 - Field : 97 fields - 80 fields : 50sec ~ 1,000sec - 17 fields : 1,000sec ~ 3,000sec GALEX (FUV,NUV) GR6 - RA(deg): 46 ~ 60, DEC(deg): -40 ~ Field : 126 fields fields : 88sec ~ 1,000sec - 26 fields : 1,000sec ~ 34,814sec Optical data HyperLeda databases (B band) HyperLeda databases (B band) 3. Environmental Effect

8 BAR AND DISK FORMATION IN DIFFERENT ENVIRONMENTS: VIRGO, COMA & FIELD J. Méndez-Abreu R. Sánchez-Janssen, J. A. L. Aguerri, E. M. Corsini, S. Zarattini Optical bar fraction of Coma (Red shaded region) and Virgo (Blue shaded region) galaxies as a function of the galaxy absolute magnitude in r-band. Black circles represent the bar fraction of the field sample by Aguerri et al. (2009). The grey line indicates the limiting magnitude below which low-mass galaxies start to be systematically thicker (Sánchez-Janssen et al. 2010). FIELD Aguerri et al. (2009, A&A, 495, 491); THICKS DISKS REGION Sánchez-Janssen et al. (2010, MNRAS, 406, 65); COMA Méndez-Abreu et al. (2010, ApJ, 711, 61); VIRGO Zarattini et al. (2011, in prep)

9 PROPERTIES AND EVOLUTION OF VIRGO LATE-TYPE GALAXIES 1 1 H.T. Meyer, T. Lisker 1 ARI, Zentrum für Astronomie, University of Heidelberg! # %&% %(#)( +,#. /0 12,2% ( ##67889 %,# :.2# Analysis of M r M [mag] r structure properties and colours µ BCD surface brightness profiles -13 of late-type galaxies [mag] (g-i) [mag] Radius [arcsec]

10 Lorenzo Morelli (Dip. Astronomia, Università di Padova) WHAT ARE NUCLEAR STELLAR DISCS (NSDs) Nuclear Disks Disky E HSB S0 LSB WHY TO STUDY NSDs They are common structure (up to 23% in early type galaxies) and present in all morphological types. They are, together with NSCs, the only bright structures in the very central region of galaxies. WHAT WE CAN STUDY OF NSDs Size Light profiles and geometry Kinematics Dynamics Stellar populations Star formation WHAT WE CAN LEARN FROM NSDs To understand the internal/external processes regulating their formation and evolution. To improve our knowledge on the formation, evolution and end (NSD will not survive to a major merging) of galaxies. To infer important clues in the coevolution between the galaxy and its BH. 1) Nuclear stellar disks in spiral galaxies, Pizzella, A., Corsini, E. M., Morelli, L., Sarzi, M., Scarlata, C., Stiavelli, M., & Bertola, F.,2002 ApJ, P. 2) Nuclear stellar discs in low-luminosity elliptical galaxies: NGC 4458 and NGC 4478, Morelli L., Halliday, C., Corsini, E. M., Pizzella, A., Thomas, D., Saglia, R. P., Davies, R. L., Bender, R., Birkinshaw, M. & Bertola, F., 2004 MNRAS, 354, 753M 3) Multiband photometric decomposition of nuclear stellar disks, Morelli, L., Cesetti, M., Corsini, E. M., Pizzella, A., Dalla Bontà, E., Sarzi, M.,Bertola, F. 2010, A&A, 518, 32M. 4) A census of nuclear stellar disk in early-type galaxies, Ledo, H. R., Sarzi, M., Dotti, M., Khochfar, S., Morelli, L., 2010, MNRAS, 407, 969L.

11 Mina Pak 1, Soo-Chang Rey 1 Youngdae Lee 1, Suk Kim 1, Eon-Chang Sung 2 Thorsten Lisker 3 Helmut Jerjen 4 Data Optical data : SDSS DR7 Ultraviolet data : GALEX GR5 V km/s Peculiar Early-type Galaxies Early-type galaxies with disk Early-type galaxies with blue centre UV Colour -Magnitude Relations

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