1. Resolving the black hole - nuclear cluster - spheroid connection
Isophotal resolution of the inner parsecs of spheroidal
stellar systems (Es, dEs, bulges) with black holes (BH)
and/or nuclear clusters (cusp or core?)
Masses of BHs and NCs in low mass galaxies via high
spatial and spectral resolution spectroscopy + dynamical
modelling (do NCs harbour intermediate-mass BHs?)
Extension of the massBH/NC-sigma and massBH/NC-spheroid
luminosity relation towards dE,Ns and small bulges
(a continuum? Is there a switch from SMBHs to NCs?)
Total time: in nights, using the approximate conversion factor 1n = 10h. Indicate also the ELT primary mirror size.
#Cois: number of co-investigators PI
Total time
#CoIs, team
Michael Hilker
Large Programme: 4x5.0n (ELT 42m)
6-8 CoIs, experienced in AO and IFU data reduction (imaging and spectroscopy), isophotal analysis and dynamical modelling

2. The mass relations for central massive objects (CMOs)
VCC1254
NGC 205
Ferrarese et al. (2006)
Wehner & Harris (2006)
What does this offset mean?
Are there (no) black holes in nuclear clusters?
What is the lowest mass BH in a galaxy core?
Which process determines the switch between NC and BH?
Are NCs the seeds of galaxies or rather assembled later?

3. 1st objective: resolve the surface brightness profiles of nuclei and
cores in the inner few parsecs
for faint Es, dEs and bulges up to
20 Mpc (Virgo/Fornax distance)
Half-light radii of nuclei: 4-20 pc
at 4 Mpc at 20 Mpc
4pc mas mas
20pc mas mas
~ 20x more distant
NGC 205 at 830 kpc Virgo/Fornax dE nuclei at ~17 Mpc
5 mas pixel scale in H,K
(5-10x better than HST)
resolves to inner pc
Vnuc<22 mag, representative
sample of 100 NCs+BH can
be observed in ~10 hours
Butler et al. (2005)

4. 2nd objective: mapping the velocity field of the inner parsecs
of NCs, BHs and bulges with high
spatial and spectral resolution as
input for dynamical modelling
Kinematical study of Virgo dEs
Central velocity dispersion of
nuclei: ~10-30 km/s
Spectral resolution of
sufficient for velocity resolution
of few km/s
Geha et
al. (2002)
Kinematical study of NGC 205
10 mas pixel scale for spectroscopy
200x200 pixel IFU x2’’ FOV
resolves inner 190 pc at 20 Mpc
Vnuc= 22 mag ~5 hours integration
time for R= in H-band
sample of 100 NCs+BH can be
observed in ~16 nights
Large Programme over 4 periods
De Rijcke et al. (2006)

5. ELT Justification: 5x better spatial resolution than ACS/HRC and high spectral resolution with reasonable S/N for faint objects within 20 Mpc.
Legacy Value: Studying the integrated light in the cores of galaxies using population synthesis models.
Data Reduction: Multiplexity: combination of high spatial and spectral resolution in the infrared.
2 µm 
LTAO AO
H band 10
2’’
24n
R:50000
104 B
H,K band 5
20’’
15h
Imaging 1 A
Notes
Pixel
FOV T.
Mode MP
Run
FIRST TABLE
MP – Multiplexity (e.g., number of slits)
Mode – either imaging or spectral resolving power
AO – AO mode: None (seeing limited), GLAO (Ground Layer AO), or LTAO (Laser Tomography AO).
T. – observing time in hours (service mode) or nights (visitor mode).
FOV – field of view
Pixel – pixel scale in mas
 – wavelength range
Notes – free text
SECOND TABLE
Run: single or multiple runs to which the table row applies.
ToT: time on target, in hours (the sum for a given run must be consistent with the run time).
Notes: take advantage to specify, e.g., the signal-to-noise ratio reached.
any
Dec.
S/N > 50
V<22
16n
dE,Ns, bulges B
S/N > 100
10h A
Notes
Mag
ToT
R.A.
Target
Run