0−∃1(,&∋ 23(4.∋5(∀(67#8∋.4−∃∋9299∋2:; · low surface brightness galaxies...
TRANSCRIPT
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23(4.∋5(∀(67#8∋.4−∃∋9299∋2:;!<73−%∋0=∗%>∋#&∋(∀?∋∋∋∀#∃%&%∋(!)∋∗+%∋,!−%./012.345!6+10∋!
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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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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)
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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
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-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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