francisco javier castander serentill
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Exploiting the Mid-InfraRed to understand galaxies Extragalactic research from Dome C. Francisco Javier Castander Serentill. Institut d’Estudis Espacials de Catalunya (IEEC) Institut de Ci ències de l’Espai (ICE /CSIC) Barcelona. - PowerPoint PPT PresentationTRANSCRIPT
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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
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• 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?
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Understanding galaxies
Properties distribution functions: mass, luminosity, morphology, kinematics, colour, metallicity
Correlations
Environment
Evolution
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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
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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
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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
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Extragalactic Surveys
A compromise between area and depth taking into account time and facilities constraints and science goals
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Low redshift• SDSS
• 2dFGRS
• 2MASS, DENIS
Where do we stand?Where do we stand?
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Blanton et al 2003
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Blanton et al 2003
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Brinchmann et al 04
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Intermediate redshift• VVDS
• DEEP2
• COMBO-17, ALHAMBRA
• CFHTLS
Where do we stand?Where do we stand?
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High redshift
• HST
• Spitzer
• (Chandra, XXM-Newton, GALEX)
Where do we stand?Where do we stand?
Deep Surveys
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• CFHT-LS
• VST/VISTA/UKIDSS
• DES/PanStarrs
What is coming next?What is coming next?
• WFMOS
• KMOS/EMIR
• LST
• ELT
• JDEM, JWST, Herschel, WISE,….
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VISTA Dark Energy SurveyBaryon Acoustic Oscillations
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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?
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Area-depth-wavelength coverage parameter space
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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
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Davoodi et al 2006
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Davoodi et al 2006
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Mid-IR Band informationMid-IR Band information• L: stellar mass
• N: PAH
• Q: dust
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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
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Other possible advantages of Other possible advantages of Dome CDome C
• Seeing: (Busarella’s talk yesterday)
• Synergies with SZ surveys
• Photo-z
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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