Current work on AO

NACO archive data on deep fields:• SR across the field• limit mag.• morphology

NICMOS VLT-NACONICMOS VLT-NACO

ghosts

Current work on AO

NACO spectra of high-z quasars

(prop. Maiolino)

arcsec

Galaxies at “high” redshift

Tests of ΛCDM:

• Few large (M>1011Mhalos at z=3

• Few centrifugally supported large disks at z>2

• Large increase in galaxy size from z=3

1. E Fundamental plane

2. E stellar gradients

3. Disk dynamical mass

Galaxy dimensions

Ferguson 1999

S: z<1.2

E: z<1.8

NICMOS

WFPC2

z=1.0

z=1.5

Fundamental plane E

merging of many fragments

Re μe0.8 σ

01.4 scatter ~ 5%

• dynamics, morphology and stellar population

• M/L, age

• cluster – field differencevan Dokkum 2001

Fundamental plane E

Selection of Elliptical at z~2:

spectra

morphology

Stanford et al 2003

Waddinton et al 2002

van dokkum et al 2003

Trujillo et al 2003

EROS

VIMOS -> NO!

Fundamental plane E

z~2:

Re ~ 0.2” R

iso~ 0.6”

K~20 -> below spectroscopic limit ?

Proiezione sul piano Re μe (Kormendy rel.)

Color distribution in Ellipticals• E in the local universe show a moderate change in

stellar population with radius (redder in the nuclei)• 25% of the E in the HDFN show blue cores

1. metallicity gradients? (expected)2. Age gradients? (only from merging)3. both?4. evolution into local E?

spatially resolved spectra and colors(age-sensitive vs. metal-sensitive tests)

Manateau et al 2001

Hinkley et al 2003

Project 1: Project 1:

K-band imaging and spectroscopy (R K-band imaging and spectroscopy (R ~~ 2000) of E with 2000) of E with K K ~20~20

Disk evolution• Gas cooling and contracting in a dark matter halo

• Late formation for large disks :

1.1e-4 Mpc-3 disks with Re>3.6kpc at z ~3

• Dynamical mass output of the cosmological simulations

van Dokkum et al 2001

Erb et al 2003

Moorwood et al 2003

large disk, z=1.34

Evoluzione dei dischiz~2

- Re ~ 0.4 – 0.7”

- K ~ 20-21

Erb et al 2003 Keck, 1 hour, H

Project 2:Project 2:

spectroscopy of disks of K spectroscopy of disks of K ~20~20

THE problem

Not easy to find a nearby star...

Mannucci et al., 2001

Simulazioni MAD:CDFS