Twenty Years of Microlensing Observations From the

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Twenty Years of Microlensing Observations From the Andrzej Udalski Warsaw University Observatory Perspecti ve

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Twenty Years of Microlensing Observations From the. Perspective. Andrzej Udalski Warsaw University Observatory. Bohdan Paczyński (1940—2007). Gravitational Microlensing toward the Galactic Bulge. Planetary Microlensing. Search for Gravitational Microlenses. - PowerPoint PPT Presentation

Transcript of Twenty Years of Microlensing Observations From the

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Twenty Years of Microlensing Observations

From the

Andrzej Udalski

Warsaw University Observatory

Perspective

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Bohdan Paczyński (1940—2007)

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Gravitational Microlensing toward the Galactic Bulge

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Planetary Microlensing

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Search for Gravitational Microlenses

• MACHO Project – Mt. Stromlo, Australia (1992 – 1999)

• EROS Project – ESO, Chile (1992 – 2002)

• MOA Project – Mt. Johns, New Zealand (1997– …)

• OGLE Project – Las Campanas, Chile (1992 – …)

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Twenty One Years of the OGLE Survey

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OGLE: The Optical Gravitational Lensing Experiment (1992 - ….)

Four Phases of the OGLE Project

• OGLE-I (1992-1995). 1 m Swope telescope at LCO. ~2 million stars observed. Microlensing

• OGLE-II (1997-2000). 1.3 m Warsaw telescope. ~40 million stars observed. Variable and non-Variable Stars in GB, MC

• OGLE-III (2001– 2009). 8k x 8k mosaic CCD. ~200 million stars observed (GB, GD, MC). Extrasolar Planets, Microlensing

• OGLE-IV (2010– ….). 32-chip 256 Mpixel mosaic CCD

http://ogle.astrouw.edu.pl

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Las Campanas Observatory, Chile

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Discovery of the First Microlensing Events – September 1993

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OGLE-I #1

Microlenses: Discovery of the first events toward the GB (1993).

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First Binary Microlensing (1994)

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Fine Microlensing Effects

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Early Warning System (EWS – 1994)

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Follow-Up Microlensing Projects

< 2001• PLANET

• GMAN

• MOA

>= 2001• microFuN

• PLANET

• Robonet

• MindSTEP

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Three Main Channels

• Search for Dark Matter• Galactic Structure• Extrasolar Planets – Planetary Microlensing

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Dark Matter – MACHO in the Galactic Halo

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OGLE-2005-SMC-001

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OGLE MC Microlensing

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Current O-IV MC Survey – 600 square degrees

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LMC

SMC

Magellanic Bridge

Classical Cepheids in the Magellanic Clouds

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LMC

SMC

Magellanic Bridge

RR Lyrae Stars in the Magellanic Clouds

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Stellar Populations in the Magellanic Bridge

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OGLE-IV Transient Detection System

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Galactic Structure

• Optical depth for microlensing toward CG• High resolution spectroscopy of highly

microlensed bulge dwarfs• Microlensing in the Galactic disk

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Gravitational Microlensing Optical Depth

• probably the best way to constrain the internal structure of the Milky Way

• The recent models of the Galactic Bulge: Kerins,Robin,Marshall (2010)

• OGLE >~10000 microlenses

3.2±0.8 (OGLE3 2007)

2.4±0.4 (MACHO 2000)

2.6±0.8 (MOA 2003)

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Optical Depth

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Microlensing in the Galactic Disk

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OGLE-IV Galactic Disk (l<0)

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Planetary Microlensing

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OGLE-III Hardware and Software (2001)

• 1.3 m OGLE telescope at Las Campanas Observatory, Chile

• 8192 x 8192 pixel mosaic CCD camera (0.26 arcsec/pixel scale): 0.5 x 0.5 sq. degree

• Data Pipeline: photometry derived with image subtraction method (accuracy up to 3 mmag for the brightest stars over a few months long observing run)

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Transiting OGLE Exoplanets

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Planetary Microlensing

O-III ~600 microlensing events per year in real time since 2002.

Short-lived anomaly in the light curve of a typical single mass microlensing event.

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OGLE-2003-BLG-235/MOA-2003-BLG-53First Planetary Microlensing

Planet/star mass ratio: q~0.004

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OGLE-2005-BLG-71

Planet/star mass ratio: q~0.007

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OGLE-2005-BLG-390

Planet/star mass ratio: q~0.00008. Mass of the planet: ~6 Earth masses. The least massive planet at the discovery

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MOA-II Survey (2006– …)

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Microlensing Planets – results

• ~30 microlensing planets found since the first announcement in 2004 (~20 published so far)

• First cool super-Earths of 3-10 Earth masses: low mass planets are common

• OGLE-2006-BLG-109: analog of the solar system (multiplanetary system: Jupiter+Saturn like)

• First estimations of the frequency of planets at and behind the „snow line”

• 2003– 2007: the discovery rate 0-1 exoplanets per season

• 2007–2010: the discovery rate of 2-4 exoplanets per season

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Main Potential of Microlensing

• Full status and characterization of exoplanets in regions located 0.5—10 AU from Host Stars (the regions at and behind the Snow Line)

• Status of exoplanets around wide range of types of Host Stars

• Discovery of low mass planets from the ground

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Second Generation Planetary Microlensing Survey

• Survey and Follow-up in one• Network of 1—2-m class telescopes over the globe with

large field (>1 square degs) cameras• Monitoring of the most microlensing efficient parts of the

Galactic bulge with the cadence of ~15 minutes• No missing planets, easier estimation of survey statistics• Estimations: A network of three 1.3—2 m telescopes: the

detection of 1—4 Earth mass planets, 10—15 super-Earths, 100 Jupiter mass planets per year

• Five year long survey should provide resonable large sample of planets for estimation of the census of exoplanets down to Earth mass at orbits of 0.5—10 AU

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OGLE-IV: 2010 – ….

• 32 chip 256 Mpixel mosaic CCD camera (+ 2 chips for guiding)

• 2048 x 4102 pixel E2V 44-82 DD CCD detectors (15 m).

• 1.4 square degrees field, 0.26”/pixel

• 20 sec. reading time

• First light September 7, 2009

• Regular observations since March 4/5, 2010

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OGLE-IV Nowa Kamera Mozaikowa

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OGLE-IV 2012 BLG SKY

Cadence: red – up to 30 epochs/night

yellow – up to 10 epochs/night

green – up to 3 epochs/night

blue – ~1 epoch/night

cyan – ~1 epoch /2 nights

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Real Time Microlensing: OGLE-IV

• 58 O-IV fields analyzed in real time including all very high and high cadence

• Statistics for 2012 BLG season: ~1700 on-line detections (~20 in O-I, ~60/season in O-II, ~600/season in O-III)

• Total number of OGLE-IV microlensing fields: 107 – they will be gradually included to EWS

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OGLE-IV planetary microlenses 2010Commissioning Mode

MOA-2010-BLG-117 MOA-2010-BLG-328

MOA-2010-BLG-477 MOA-2010-BLG-523

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2012 Planetary Microlensing

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Free-Floating Planets

• Microlensing event characteristic time: tE=RE/vtr

• RE~sqrt(Mlens) → tE~sqrt(Mlens)• tE< 2 days – lensing object has planetary mass• High cadence observations needed for detection : (OGLE-IV:

18-60 min.)• MOA and OGLE data from 2006-2007: 10 short-lived

microlensing events of likely planetary mass. No trace of host stars: population of unbound (FFP) or very distant exoplanets.

• OGLE-IV data much better suited : preliminary estimation – 2011 season: ~40 events with tE< 2 days (shortest corespond statistically to a few Earth mass objects)

• Origin: gravitational interactions – stellar encounters, ejection of planets during planetary system formation

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OGLE-IV 2013 BLG SKY

Cadence: red – up to 30 epochs/night

yellow – up to 10 epochs/night

green – up to 3 epochs/night

blue – ~1 epoch/night

cyan – ~1 epoch /2 nights

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Prospects for Planetary Microlensing Field: Bright

• New facilities: Bisdee Tier Tasmania, LCOGT Network, KMNet

• Space Missions: WFIRST, EUCLID


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