!∀#∃#%&∋()∗%+(%,#∋−.∋/∀∗#∋0−∃1(,&∋

23(4.∋5(∀(67#8∋.4−∃∋9299∋2:;!<73−%∋0=∗%>∋#&∋(∀?∋∋∋∀#∃%&%∋(!)∋∗+%∋,!−%./012.345!6+10∋!

log N

/O

12+log O/H

7.6 7.8 8.0 8.2 8.4 8.612+log(O/H)

-2.0

-1.8

-1.6

-1.4

-1.2

-1.0

-0.8

log(N

/O)

7.23∃1809!:∀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?!!

7.23∃1809!:∀7!

)+1(∋,!:∀7!

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 (AV > 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 disruptedand harrassed galaxies

The faint western galaxies are mainly blue, and therefore late-type or issued from late-type galaxies in the infallinglayers

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

Atypical faint galaxies in Coma: faint imaging view

Florence Durret, Christophe Adami et al.

!

∀#∃%∀ ∀∀&∋&()∗∋+#,∗−∃%∋(./! %−

!∀# ∃%&

∋ ( ) ∗+

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∀ 2+ ! /

/ ∋

∋ (!.

34 !5265 ∋∋∃%&

74 !∀#! ∋ (/.

!∀ #

!

∀ #∃%&∋

∀ #∃%&∋

(!) ∋ ) #∃%& ∗+,

(!) ∋ ) #∃%& ∗+,

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

MElliptical-µ0 diagram Mbh-! diagram

Central Stellar Deficits

Additional Nuclear Components (Central Massive Object)-(Host Spheroid) mass relation

Fornax, Virgo, Coma et al. (ESO Garching, 27 June - 1 July, 2011)

!∀#∃%&∃&∋()∗+,∋−./0#∃∗∋−1#1.,+∋∃#∋1.2∋ ∋3/4∋5)678∋3,,9−:1%+∋;∃<78∋!,%9−:1%+∋3/%+=8∋>:,∗0#∃%∋?)04∃∗≅8∋∋Α∃.6/#∋Β∃∗Χ∃%∆8∋∋∋

∋∋∋Ε,%:<∃,%+∋Φ)78∋Φ,/%+Γ1∃∋?∃∃78∋Β)Η,%∋−:/%+78∋∋Ι)%1∋ϑ1478∋1%&∋∋Β1∃61%%∋4</%+= ∋∋

!∀#∃%&∋()∃

∗+∃%&∋()∃

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Ultraviolet Properties of galaxies in the Fornax cluster

Virgo cluster Fornax cluster

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 ~ -30 - Field : 126 fields - 100 fields : 88sec ~ 1,000sec - 26 fields : 1,000sec ~ 34,814sec

Optical data HyperLeda databases (B band) HyperLeda databases (B band)

1. Data

3. Environmental Effect

2. UV CMR

BAR AND DISK FORMATION IN DIFFERENT ENVIRONMENTS:BAR AND DISK FORMATION IN DIFFERENT ENVIRONMENTS:VIRGO, COMA & FIELDVIRGO, COMA & FIELD

J. Méndez-AbreuR. Sánchez-Janssen, J. A. L. Aguerri, E. M. Corsini, S. Zarattini

Optical bar fraction of Coma (Red shadedregion) 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). Thegrey line indicates the limiting magnitudebelow which low-mass galaxies start to be systematically thicker (Sánchez-Janssen et al. 2010).

FIELDFIELD Aguerri et al. (2009, A&A, 495, 491); THICKS DISKS REGIONTHICKS DISKS REGION Sánchez-Janssen et al. (2010, MNRAS, 406, 65); COMACOMA Méndez-Abreu et al. (2010, ApJ, 711, 61); VIRGOVIRGO Zarattini et al. (2011, in prep)

PROPERTIES AND EVOLUTION OF VIRGO

LATE-TYPE GALAXIES

ARI, Zentrum für Astronomie, University of Heidelberg

H.T. Meyer , T. Lisker1 1

1!∀#∃%&%∋%(#)(∗+,#∃−.−/012,2%∃(3∗4∃−563##67889(%,#∃−:.2#

-20

-19

-18

-17

-16

-15

-14

-13

-12-0.5 0 0.5 1 1.5 2

Mr [m

ag]

g-i [mag]

Analysis of

structure properties

and

colours

of late-type galaxies

(g-i) [mag]

M [

mag

]r

Radius [arcsec]

µ

18

19

20

21

22

23

24

25

26

27

0 5 10 15 20 25 30

BCD surface brightness profiles

Lorenzo Morelli (Dip. Astronomia, Università di Padova)

HSB

LSB S0

Disky E

Nuclear Disks

WHAT ARE NUCLEAR STELLAR DISCS (NSDs)

Size Light profiles and geometry Kinematics Dynamics Stellar populations Star formation

WHAT WE CAN STUDY OF 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.

WHY TO STUDY NSDs

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, 573 131P.

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.

Data

Optical data : SDSS DR7

Ultraviolet data : GALEX GR5

V0 1700km/s

Early-type galaxies

with blue centre

UV Colour -Magnitude Relations

Mina Pak1, Soo-Chang Rey1 Youngdae Lee1, Suk Kim1, Eon-Chang Sung2 Thorsten Lisker3 Helmut Jerjen4

Peculiar Early-type Galaxies

Early-type galaxies

with disk

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∆∋,∀#−Γ,(∀Α[Γ#51∋68Ι#

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