Francisco Javier Castander Serentill

Institut d’Estudis Espacials de Catalunya (IEEC)

Institut de Ciències de l’Espai (ICE/CSIC)

Barcelona

Exploiting the Mid-InfraRed Exploiting the Mid-InfraRed to understand galaxiesto understand galaxies

Extragalactic research from Extragalactic research from Dome CDome C

• How many photons: Flux: colours, SED, luminosity

• How photons are distributed spatially: Morphology: size, shape

• How photons are distributed in λ: SED: redshift, stellar population & gas: Z, t, SFR, IMF

• How photons are distributed in λ: kinematics

What can we measure about What can we measure about galaxies?galaxies?

Understanding galaxies

Properties distribution functions: mass, luminosity, morphology, kinematics, colour, metallicity

Correlations

Environment

Evolution

Surveys to unveil properties of galaxies

• Galaxy properties are diverse, complex and depend on many parameters => Need large number to characterize variance & evolution => Need large volumes at different z

• Large Surveys required

Surveys to characterize Large Scale Structure

• Matter difficult to trace. Galaxies (and clusters) best tracers but biased

• Typical distances few Mpc & cosmic variance => Need large volumes

• Large Surveys required

Surveys to characterize Cosmology

• Dark Matter and Dark Energy

• Dependency: expansion rate H(z) & growth rate of perturbations D(z) => Need large volumes

• Probes: Clustering (BAO), Weak Lensing, Cluster abundances, SNIa

• Large Surveys required

Extragalactic Surveys

A compromise between area and depth taking into account time and facilities constraints and science goals

Low redshift• SDSS

• 2dFGRS

• 2MASS, DENIS

Where do we stand?Where do we stand?

Blanton et al 2003

Blanton et al 2003

Brinchmann et al 04

Intermediate redshift• VVDS

• DEEP2

• COMBO-17, ALHAMBRA

• CFHTLS

Where do we stand?Where do we stand?

High redshift

• HST

• Spitzer

• (Chandra, XXM-Newton, GALEX)

Where do we stand?Where do we stand?

Deep Surveys

• CFHT-LS

• VST/VISTA/UKIDSS

• DES/PanStarrs

What is coming next?What is coming next?

• WFMOS

• KMOS/EMIR

• LST

• ELT

• JDEM, JWST, Herschel, WISE,….

VISTA Dark Energy SurveyBaryon Acoustic Oscillations

Can Dome C play a role in this game?

What is needed next or what What is needed next or what is missing currently?is missing currently?

• Spectroscopy: highly multiplexing?

• Imaging?

Area-depth-wavelength coverage parameter space

What would we learn if we What would we learn if we try to fill the gap?try to fill the gap?

• Modeling & simulations

• Spitzer experience

Davoodi et al 2006

Davoodi et al 2006

Mid-IR Band informationMid-IR Band information• L: stellar mass

• N: PAH

• Q: dust

Is it feasible?Is it feasible?• For a 3-m type telescope in the L band it could be possible to reach galaxies to z~0.5

• M band, to z~0.1

• N and Q only local strong emitters

Other possible advantages of Other possible advantages of Dome CDome C

• Seeing: (Busarella’s talk yesterday)

• Synergies with SZ surveys

• Photo-z

Possibilities for extragalactic studies at Dome C

• Hard to compete with other observatories in wide field surveys

• Low thermal background: Limited gain in mid-IR

• Seeing: possible gains

• Time monitoring: strong lensed QSOs

ConclusionsConclusions