simulation of a planetary microlensing survey by euclid1. euclid an esa mission to probe dark energy...
TRANSCRIPT
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Simulation of a Planetary Microlensing Survey by
EuclidMatthew Penny (JBCA now OSU)
AndEamonn Kerins, Nick Rattenbury
(JBCA)Annie Robin
(Observatoire de Besançon)J-P Beaulieu (IAP Paris)The Euclid Consortium
16th International Conference on Gravitational Microlensing 17th Feb 2012
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1. The Euclid Spacecraft
2. The Science
3. The Simulations
4. The Expected Yields
Overview
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1. Euclid● An ESA mission to
probe dark energy via Weak Lensing (WL) and Baryon Acoustic Oscillations (BAO)
● Wide-field 1.2-m telescope @ L2
● 0.5 deg² NIR and Visual imagers
For more info see:The Euclid Red Book
Laureijs+ 2011arXiv:1110.3193
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1. Euclid InstrumentsNISP
Photo-z + Spectro-z● 16 2k x 2k HgCdTe
arrays● 0.3” pixels● 0.3-0.45” PSF● Y, J, H NIR filters +
2 Grisms● 24th mag in each
VIS
Galaxy shapes etc.● 36 4k x 4k CCDs● 0.1” pixels● 0.2” PSF● Single broad RIZ
filter● Limiting mag 24.5
in 3x~540s
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Two surveys in 6 yrs● Wide survey 15,000-
20,000deg²● Deep survey 40deg²
1. Euclid Main Survey
Scans sky maintaining fixed orientation cf Sun
But can't survey galaxies in Galactic plane
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Euclid is perfectly suited to microlensing observations: ● High resolution● Wide field● Sensitive VIS + NIR photometry
+ has “low-efficiency” time which can be used for other projects
1. μL with Euclid
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2. The Science
Do microlensing with Euclid to probe:● Planet formation
● Core accretion or disc instability?● Mechanisms, timescales, etc.?● How many planets form and what happens to
them?
● Habitable systems● How many systems look like home?● Jupiter, Saturn + warm terrestrial planets?
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Planets build up slowly from grains to gas giants in dusty disc
Core Accretion
Gas giants quickly collapse out of a gaseous disc
Disc Instability
Boss, 2011Bate+ 2003
~10AU ~60AU
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2. And there's migration!● Planets migrate within the disc
Mordasini+ 2011
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2. The M-a diagram
Core accretion happens here
Disc instability happens here
Kepler
Transits
Radial Velocity
GAIA+Ground μL
Direct Imaging
Ida+Lin, 2008
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3. The Simulator - MaBμLS
Manchester-Besancon microLensing Simulator
● Draws events from the Besancon Galactic model
● Simulates photometry with realistic image simulations
● Modular, extensible design
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3. The Besancon Model
Galactic population synthesis model:
Incorporates:● Bulge+bar, thin+thick
discs, stellar halo● Evolutionary tracks● Stellar atmos models● 3d dust model
Generates lists of stars and their properties
Robin+ 1986, 2003, 2012 etc. Marshall et al 2006
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3. Image Simulations
Detector and Noise parameters
Numerical PSFs
Images generated from star lists output by Besancon model
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3. Image simulations
Simulate a CCD
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3. Image simulations
Simulate a CCD● Bias
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3. Image simulations
Simulate a CCD● Bias● Background
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3. Image simulations
Simulate a CCD● Bias● Background● Faint stars
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3. Image simulations
Simulate a CCD● Bias● Background● Faint stars● Stars
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3. Image simulations
Simulate a CCD● Bias● Background● Faint stars● Stars● Bright stars
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3. Image simulations
Simulate a CCD● Bias● Background● Faint stars● Stars● Bright stars● A Source
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3. Image simulations
Simulate a CCD● Bias● Background● Faint stars● Stars● Bright stars● A Source● Lensing
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3. Image Simulations
Simulated image Euclid NISP detector
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Image Simulations
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3. Other Features
● Fully customizable observing sequences
● Multiple ground- and space-based observatories
● Multiple filters
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3. Simulated Lightcurves
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3. Simulated Lightcurves
Euclid NISP detector
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3. Simulated Lightcurves
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4. Expected Yields
Euclid additional science survey:● 300 day survey, split into 5 yearly seasons● 60 days continuous observations each season● 3x0.5deg² fields, each observed every 18 mins● Observations in other bands every 12 hours
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4. Expected Yields
● 300 day survey, split into 5 yearly seasons● 60 days continuous observations each season● 3x0.5deg² fields, each observed every 18 mins● Observations in other bands every 12 hours
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4. Different mass functions
Total detections (-1.5<log(M/Me)<3): Default: 390 RV: 307 uL: 438 uL saturated: 267
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4. Different mass functions
RV: α Cumming et al 2008, f Gould et al 2010. μL: Cassan et al 2012
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4. M-a sensitivity
RV: α Cumming et al 2008, f Gould et al 2010. μL: α Sumi et al 2010, f Gould et al 2010.
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4. What planets will Euclid probe?
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4. Different scenarios
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Conclusions
● Euclid can do exellent exoplanet science● Euclid will detect Earth-mass planets – expect
~4 per month of observations● Euclid has sensitivity below Mercury-mass –
may not have sufficient rate, depends on mass function
● Euclid will complete the census of low-mass exoplanets stared by Kepler
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What's next?
● Calculate expected parameter errors + FoM● Optimize survey for planetary mass
measurements, not detections● Use MaBμLS to fully optimize a Euclid
microlensing survey● Apply MaBμLS to WFIRST and ground-based
surveys (OGLE-IV, VVV, KMTNet)