Cosmology with ESO telescopes

Bruno Leibundgut

Outline

Past and current cosmology projects with ESO telescopes

Future instrumentation capabilities (interferometry?)VLT 2nd generation instrumentsAPEXSurvey telescopes (VST, VISTA)ALMA

ESO-ESA Working Group on Fundamental Cosmology

The way to a European ELT

Current VLT projects

FIRES, GOODS, VVDS, K-20, GMASS, zCOSMOSdetection of new classes of high-z galaxies:

massive, red galaxies

old ellipticals at z~2

large number of star forming galaxies at z>1.5

SNLS, ESSENCEsystematics of SNe Ia

GRBsprobing the end of reionisation?

Variable fine-structure constantFranx et al. (2003) Chand et al. (2003)

Vanzella et al. 2006

Blondin et al. (2006)

VLT 2nd Generation Instruments

X-Shootersingle source spectroscopy (UV through NIR)

GRBs, SNe (physics)HAWK-I

wide-field near-IR imagerEROs, distant galaxies clusters, z>7 galaxies

KMOSmulti-objects IR spectrograph

mass assembly of galaxies, z>7 galaxiesMUSE

optical multi-object, integral-field massive spectrograph

deep Ly-α surveys, black holes Adaptive Opticssupported

Future possibilities

New Facilities– APEX

• Bonn-Berkeley Sunyaev-Zeldovich Survey

– Survey telescopes• VST and VISTA

– KIDS, ATLAS

– ALMA• use the negative K-corrections

– ELT• see Sandro D’Odorico’s talk

Bertoldi

Public Surveys

KIDSweak lensing mass distribution, galaxy

power spectrum, dark energy; very high-z QSOs

1400 sq. degree in five bands (u’g’r’i’z’)(plus JHK from either UKIDSS and/or VISTA)depth r’~24 (AB)

ATLAS(Southern SDSS complement)baryon accoustic oscillations, dark energy

4500 sq. degree in five bands (u’g’r’i’z’)

depth r’~22 (AB)

ALMA

Dust absorption not a problem

Opens up observations of dust at high redshifts

Negative K-corrections

Observations right into the ‘dark ages’

Bertoldi et al (2003)Walter et al. (2003)

ESO-ESA working group on fundamental cosmology

CompositionJohn Peacock (Edinburgh, chair)

Peter Schneider (Bonn, co-chair)

John Ellis (CERN)

Georg Efstathiou (Cambridge)

Bruno Leibundgut (ESO)

Simon Lilly (Zurich)

Yannick Mellier (Paris)

A critical review of global efforts in this area

Assess what ESA & ESO are doing now

Independent opinion on possible new ESA/ESO projects – or adding synergy

Big questions

1. What is the right physics?2. Did inflation happen? 3. What is the dark matter?4. What is the dark energy? 5. What generated the baryon asymmetry?6. Are there other relics to be found (e.g. cosmic strings)?7. Are there extra dimensions?8. Do fundamental constants vary?

First ideas

Some progress identifiedlarge imaging surveys (like KIDS)

weak lensing and acoustic baryonic oscillations (based on photo-z, i.e. requires IR as well)

massive spectroscopic surveysacoustic baryonic oscillations

synergy with spaceimaging from space, photo-z from the ground(e.g. DUNE and darkCAM)

Difficultieslong lead times for instruments

ESA Cosmic Vision setting out plans for 2015-2025ELT operational not before 2015

Extremely Large Telescope

OPTICON science working group

External Review of the OWL Project (November ’05)

Creation of five working groups at ESO(January/February ’06)Science, telescope design, instruments, adaptive optics,

site

ELT science and engineering working group(March/April ’06)

ELT (cont.)

Consolidation of various reports(end of April)

Pre-selection of design by end of 2006

Preliminary design end of 2007

Science themesfirst objects, end of reionisation, cosmology

with SNe, gravitational lensing, galaxy evolution

Science case FOV Spatial ResolutionPhotometric Photometric Spectral Wavelengthmilli-arcsec uniformity accuracy R microns

Galaxies and Cosmology

Dark energy: type Ia Sne as distance indicators - search and light curves >5'x5' GLAO/MACO <5% 0.8-2.5- spectroscopy a few hundred 0.8-2.5Dynamical measurement of universal expansion few arcsec 80& EE in 0.6" 150000 (>= 50000) 0.4-0.68Constraining fundamental constants few arcsec 80& EE in 0.6" 150000 (>= 50000) 0.4-0.68First light - the highest redshift galaxies 17'x17' 200 mas >3000 0.9-2Probing reionization with GRBs and quasars 300 mas 1000-5000 1.0-2.2Metallicity of the low-density IGM 300 mas 100000 0.55-0.7IGM tomography - bright LBGs and quasars >5'x5' 500mas yes few % 10000 0.4-0.7- faint LBGs 5'x5' 500mas yes few % 1000 0.4-0.7Galaxy formation and evolution: 5'x5' 0.1"-0.4" 1000-5000 0.6-2.5Physics of high-z galaxies 5'x5 ' 0.2"-0.4" 1000-10000 0.4-2.5Gravitational lensing 1'x1' 0.1"-0.4" 500-5000 0.4-2.5

Science case Multiplex Magnitude Object Size Exposure Target density(typical) arcsec typical time, hr arcmin^-2 30m 42m 60m JWST

Galaxies and Cosmology

Dark energy: type Ia Sne as distance indicators < 1 - search and light curves see text point sources see text see text yes yes yes yes- spectroscopy low see text point sources see text see text yes yes yes yesDynamical measurement of universal expansion 15-17 point sources 0.2-0.3h x many low yes* yes* yes* noConstraining fundamental constants 15-17 point sources 0.2-0.3h x many low yes* yes* yes* noFirst light - the highest redshift galaxies 100 AB = 28 0.1-0.2 100 0.1 - 1 yes yes yes o/cProbing reionization with GRBs and quasars 22-25.5 point sources 20-80h yes yes yes noMetallicity of the low-density IGM 16-17.3 point sources 20-90h yes yes yes noIGM tomography - bright LBGs and quasars 10 IFU 21-24 0.5" 10-50 0.2 yes yes yes no- faint LBGs >100 IFU 25-27 0.5" 20-80 10 yes yes yes noGalaxy formation and evolution: 50-100 23-26 0.1-0.5" > 5 0.1-1 yes yes yes noPhysics of high-z galaxies 50-100 23-26 0.1-0.5" 5-50h 0.1-1 yes yes yes cGravitational lensing 50-100 24-27 0.1-0.5" 2-20h 1 - 50 yes yes yes yes

Can be done with

Where is cosmology moving to?

large surveys

large teams

exclusive use of telescope resourcescf. CFHTLS, VST, VISTA

Should large telescopes be dedicated to solve specific questions?