moa-ii microlensing survey
DESCRIPTION
MOA-II Microlensing Survey. Takahiro Sumi (Nagoya University) the MOA collaboration Abe,F; Bennett,P.D;Bond, I. A.;Fukui,A;Furusawa,K; Hearnshaw, J. B.; Itow,Y; - PowerPoint PPT PresentationTRANSCRIPT
MOA-II Microlensing SurveyMOA-II Microlensing Survey
Takahiro Sumi (Nagoya University)
the MOA collaborationAbe,F; Bennett,P.D;Bond, I. A.;Fukui,A;Furusawa,K; Hearnshaw, J. B.;Itow,Y;
Kilmartin, P. M.; Koki, K; Masuda, K.; Matsubara, Y.;Miyake,N; Muraki, Y.; Nagaya,M;Okumura,M; Ohnishi,K;Rattenbury, N. J.; Saitou,T;Sako, T.;
Sullivan, D. J.;Sumi, T.;Tristram,P.; Wood, J. N.; Yock, P. C. M.
Takahiro Sumi (Nagoya University)
the MOA collaborationAbe,F; Bennett,P.D;Bond, I. A.;Fukui,A;Furusawa,K; Hearnshaw, J. B.;Itow,Y;
Kilmartin, P. M.; Koki, K; Masuda, K.; Matsubara, Y.;Miyake,N; Muraki, Y.; Nagaya,M;Okumura,M; Ohnishi,K;Rattenbury, N. J.; Saitou,T;Sako, T.;
Sullivan, D. J.;Sumi, T.;Tristram,P.; Wood, J. N.; Yock, P. C. M.
MOA (since 1995)
( Microlensing Observation in Astrophysics )( New Zealand/Mt. John Observatory, Latitude : 44S, Alt: 1029m )
MOA (since 1995)
( Microlensing Observation in Astrophysics )( New Zealand/Mt. John Observatory, Latitude : 44S, Alt: 1029m )
1995~1998:MOA-0: 0.6m, 9Mpix
1999~2005:MOA-I : 0.6m, 24Mpix
2005~ :MOA-II: 1.8m, 80Mpix
1995~1998:MOA-0: 0.6m, 9Mpix
1999~2005:MOA-I : 0.6m, 24Mpix
2005~ :MOA-II: 1.8m, 80Mpix
MOA (until ~1500)
( The world largest bird which was in NZ )
MOA (until ~1500)
( The world largest bird which was in NZ )
• height:3.5 m• weight:240kg• can not fly• extinct 5 00 years
ago
( Maori ate them)
witnesses until ~1850.
Remind me …
• height:3.5 m• weight:240kg• can not fly• extinct 5 00 years
ago
( Maori ate them)
witnesses until ~1850.
Remind me … Nessie
MOA’s scientific goalsMOA’s scientific goals
1,Galactic Dark Matter (towards the LMC & SMC)
Halo MACHOs or self-lensing?
1,Galactic Dark Matter (towards the LMC & SMC)
Halo MACHOs or self-lensing?
Halo Dark Matter?or
Self-lensing?
Halo Dark Matter?or
Self-lensing?
Tisserand et al.2006
MACHO 5.7 yrs & EROS 5yrs
MOA’s scientific goalsMOA’s scientific goals
1,Galactic Dark Matter (towards the LMC & SMC) Halo MACHOs or self-lensing?
2,The Galactic structure (towards the Bulge) Optical depth
time scale,tE
Red Clump Giants
1,Galactic Dark Matter (towards the LMC & SMC) Halo MACHOs or self-lensing?
2,The Galactic structure (towards the Bulge) Optical depth
time scale,tE
Red Clump Giants
the Galactic Bar structure the Galactic Bar structure (face on, from North)
8kpc
G.C.Obs.
1, Microlensing Optical depth, (Alcock et al. 2000; Afonso et al.2003; Sumi et al. 2003;Popowski et al. 2004; Hamadache et al. 2006;Sumi et al. 2006)
Event Timescale, tE=RE/vt, (Evans & Belokurov,2002, Wood & Mao 2005)
M=1.61010M, axis ratio (1:0.3:0.2), ~20
1, Microlensing Optical depth, (Alcock et al. 2000; Afonso et al.2003; Sumi et al. 2003;Popowski et al. 2004; Hamadache et al. 2006;Sumi et al. 2006)
Event Timescale, tE=RE/vt, (Evans & Belokurov,2002, Wood & Mao 2005)
M=1.61010M, axis ratio (1:0.3:0.2), ~20
2, Brightness of Red Clump Giant (RCG)and RRLyrae stars, (Stanek et al. 1997, Sumi 2004; Collinge, Sumi & Fabrycky, 2006)
2, Brightness of Red Clump Giant (RCG)and RRLyrae stars, (Stanek et al. 1997, Sumi 2004; Collinge, Sumi & Fabrycky, 2006)
3, Proper motions of RCG,(Sumi, Eyer & Wozniak, 2003; Sumi et al. 2004;Rattenbury et al.2007), Proper motion of 5M stars, I<18 mag, ~1mas/yr3, Proper motions of RCG,(Sumi, Eyer & Wozniak, 2003; Sumi et al. 2004;Rattenbury et al.2007), Proper motion of 5M stars, I<18 mag, ~1mas/yr
MOA’s scientific goalsMOA’s scientific goals
1,Galactic Dark Matter (towards the LMC & SMC) Halo MACHOs or self-lensing?
2,The Galactic structure (towards the Bulge) Optical depth
time scale,tE
Red Clump Giants
3,Exoplanets (towards the Bulge) Microlensing & transit
1,Galactic Dark Matter (towards the LMC & SMC) Halo MACHOs or self-lensing?
2,The Galactic structure (towards the Bulge) Optical depth
time scale,tE
Red Clump Giants
3,Exoplanets (towards the Bulge) Microlensing & transit
Theoretical v.s. ObservationTheoretical v.s. Observation
red : Gass Giants青: Ice planets緑: Rocky planets
Ida & Lin, 2004
100m/s
10m/s
1m/s
Simulation Observation
Observational targetsObservational targets
LMCLMC
50kpc50kpc
event rate:event rate:
LMC,SMC : LMC,SMC : ~2~2 events/yr (events/yr (~10~10-7-7 ))
Bulge : Bulge : ~500~500events/yr (events/yr (~10~10-6-6 ))
Planetary event : Planetary event : ~10~10-2-2
event rate:event rate:
LMC,SMC : LMC,SMC : ~2~2 events/yr (events/yr (~10~10-7-7 ))
Bulge : Bulge : ~500~500events/yr (events/yr (~10~10-6-6 ))
Planetary event : Planetary event : ~10~10-2-2
7.5kpc, GC7.5kpc, GC7.5kpc, GC7.5kpc, GC
PLANETPLANET
FUNFUN
• Pointing each candidatePointing each candidate• High cadenceHigh cadence• Strategy based on Strategy based on
published photometrypublished photometry to catch short deviation.to catch short deviation.
MOAMOA(NewZealand)(NewZealand)
OGLEOGLE(Chile)(Chile)
• Wide field Wide field • Low cadenceLow cadence• Continuous surveyContinuous survey
Microlensing observation networkMicrolensing observation network
Survey GroupSurvey Group Follow-up GroupFollow-up GroupMicroMicrolensinglensingAlertAlert
AnomalyAnomaly AlertAlert
Anyone who wants alert is welcome to sign up Anyone who wants alert is welcome to sign up on the websites.on the websites.
Paczyński’s LegacyPaczyński’s Legacy
• The planet discovery via microlensing by collaboration of these groups are Paczyński’s Legacy
• Idea of the method.• Idea of putting data on public and sharing photometry
with other groups. useful to decide strategy to catch rare short planetary deviation.
• The planet discovery via microlensing by collaboration of these groups are Paczyński’s Legacy
• Idea of the method.• Idea of putting data on public and sharing photometry
with other groups. useful to decide strategy to catch rare short planetary deviation.
MOA-I (1999~2005)
( Microlensing Observation in Antrophysics )( New Zealand/Mt. John Observatory, Latitude : 44S, Alt: 1029m )
MOA-I (1999~2005)
( Microlensing Observation in Antrophysics )( New Zealand/Mt. John Observatory, Latitude : 44S, Alt: 1029m )
Mirror : 0.6mCCD : 4k x 6k pix.FOV : 1.3 square deg.Seeing:~2 arcsec
Mirror : 0.6mCCD : 4k x 6k pix.FOV : 1.3 square deg.Seeing:~2 arcsec
MOA-I filterMOA-I filter
Difference Image Analysis (DIA)Difference Image Analysis (DIA)
Observed Observed Observed Observed subtractedsubtractedsubtractedsubtracted
Results from MOA-IResults from MOA-I
Mass : Jupiter Sep. : ~3AUMass : Jupiter Sep. : ~3AU
1, Microlensing Optical depth towads GB (Sumi et al. 2003)
2, LP Variable stars in LMC (Noda et al. 2002,2004)
3, Stellar shape & limb darkning (abe et al.2003;Rattenbury et al.2005)
4, The first planet via microlensing (bond et al.2003) OGLE 2003-BLG-235/MOA 2003-BLG-53 (in collaboration with OGLE) etc…
1, Microlensing Optical depth towads GB (Sumi et al. 2003)
2, LP Variable stars in LMC (Noda et al. 2002,2004)
3, Stellar shape & limb darkning (abe et al.2003;Rattenbury et al.2005)
4, The first planet via microlensing (bond et al.2003) OGLE 2003-BLG-235/MOA 2003-BLG-53 (in collaboration with OGLE) etc…
LMC event from MOA-ILMC event from MOA-I(RA,DEC)=(05:13:48.7,-69:45:24.3)
T= 2,122 days
N= 3,743,244 stars
T= 2,122 days
N= 3,743,244 stars
tE=70.80umin=0.1754t0=1818.2308
RED
BLUE
LMC event from MOA-ILMC event from MOA-ItE=70.80umin=0.1754t0=1818.2308
RED
BLUE
Planetary transits in MOA-I Bulge data
Planetary transits in MOA-I Bulge data
• #of stars
<1.0 %: 0.1M stars
<2.0 %: 1M stars
Planning photometric follow-up by IRSF 1.4m IR telescope at SAAO
• #of stars
<1.0 %: 0.1M stars
<2.0 %: 1M stars
Planning photometric follow-up by IRSF 1.4m IR telescope at SAAO
MOA-II1.8m telescope( New Zealand/Mt. John Observatory at NZ, 44S )
Mirror : 1.8mCCD : 8k x 10k pix. FOV : 2.2 deg.2
Mirror : 1.8mCCD : 8k x 10k pix. FOV : 2.2 deg.2
First lightFirst light :: 3/20053/2005Survey startSurvey start : : 4/20064/2006
MOA-cam3CCD :8k x 10k pix. (10 E2V CCD4482)
Pixel size: 15μm FOV : 2.2 deg.2
CCD :8k x 10k pix. (10 E2V CCD4482)
Pixel size: 15μm FOV : 2.2 deg.2
MOA-II filterMOA-II filter
Observational time&Operation rateObservational time&Operation rate
Operation rate = observation time / night time ≒ clear time
BulgeBulge
Observation towards LMC by MOA-IIObservation towards LMC by MOA-II
~3obs/night~3obs/night
~10obs/night~10obs/night
Start alert in a few weeks
Discriminating fromSuper Nova
Discriminating fromSuper Nova
(from SuperMACHO web)(from SuperMACHO web)
Survey towards the Galactic BulgeSurvey towards the Galactic Bulge
• why ?• why ?
need Wide Field for Many stars need Wide Field for Many stars
Probability:Probability:
Microlensing : Microlensing : ~10~10-6-6 events/yr/starevents/yr/star Planetary event : Planetary event : ~10~10-2-2
Probability:Probability:
Microlensing : Microlensing : ~10~10-6-6 events/yr/starevents/yr/star Planetary event : Planetary event : ~10~10-2-2
G.C.G.C.G.C.G.C.SunSunSunSun
Time scale ~ 30days (MTime scale ~ 30days (M))
~ ~ a few daysa few days (M (MJupJup))
~ ~ hours hours (M (M)) need high cadence need high cadence
Observation towards the Bulge by MOA-II
Observation towards the Bulge by MOA-II
•50 deg.2
60GB/night
•1obs./hr (MJup)
1obs./10min. (M)
•50 deg.2
60GB/night
•1obs./hr (MJup)
1obs./10min. (M)
~~170170events (2006)events (2006)~~500500events (2007)events (2007)
http://www.massey.ac.nz/~iabond/alert/alert.html
Observational strategyObservational strategy
(Han (Han & Kim, 2001))
• High magnification event• we know when
• Low magnification event• rate is higher • we do not know when
• High magnification event• we know when
• Low magnification event• rate is higher • we do not know when
Example light curvesExample light curves• 〜50 obs/
day
4days 4days
4days4days
Finite source effect ( MOA-2006-GLB-130 )
Finite source effect ( MOA-2006-GLB-130 )
Is=Is=21.07 mag
Real-time Anomaly check at Mt.JohnReal-time Anomaly check at Mt.John
anomalyanomaly
The first planet via microlensing OGLE 2003-BLG-235/MOA 2003-BLG-53
The first planet via microlensing OGLE 2003-BLG-235/MOA 2003-BLG-53
OGLE 2003-BLG-235/MOA 2003-BLG-53 was detected by the OGLE EWS System on June 22, 2003 andby the MOA group on July 21, 2003.
Mass : Jupiter Sep. : ~3AU
5.5 Earth mass Planet (Beaulieu et al. 2006, Nature,439,437)
Sep~3AUSep~3AU
The smallest PlanetThe smallest Planet !!
2nd & 3rd planets 2nd & 3rd planets OGLE-2005-BLG-071.
1 MJupiter , Udalski et al. 2005OGLE-2005-BLG-169,13MEarth,Gould et al.2006
“Cool Neptune" planets may be relatively common,
with frequency of >16% at 90% confidence.
High mag events in 2007High mag events in 2007High mag events in 2007High mag events in 2007
ttEE==6.240.15days,, A Amaxmax>>400
OGLE-2007-BLG-224(MOA-2007-BLG-163)
MOA-2007-BLG-312(OGLE-2007-BLG-388)
ttEE==3.500.65 days,, A Amaxmax==102
MOA-2007-BLG-397( OGLE-2007-BLG-538 )
ttEE==21.340.03 days,, A Amaxmax==404
MOA-2007-BLG-400ttEE==14.640.2 days,, A Amaxmax>>800800
Same field as ob349/mb379Same field as ob349/mb379
JD JD
JD JD
MOA-2007-BLG-192MOA-2007-BLG-192
q=q=6x10^-5, sep=, sep=0.9RE, 1.1RE,
MOAMOAOGLEOGLE
preliminarypreliminary
MOA-2007-BLG-197MOA-2007-BLG-197
1 年
q=3q=3x10-3, sep=, sep= 1RE
Orange: PLANET (Danis)Orange: PLANET (Danis)Blue : PLANET (Tasmania)Blue : PLANET (Tasmania)Red :PLANET SAAORed :PLANET SAAOBrown : MOABrown : MOA
preliminarypreliminary
OGLE-2007-BLG-368 (MOA-2007-BLG-308)OGLE-2007-BLG-368 (MOA-2007-BLG-308)
q=~q=~1x10^-4
MOAMOAOGLEOGLEPLANET(Danish)PLANET(Danish)PLANET(Tasmania-I)PLANET(Tasmania-I)PLANET(SAAO-I)PLANET(SAAO-I)PLANET(Brasil)PLANET(Brasil)FUN(CTIO-I)FUN(CTIO-I)
OGLE-2007-BLG-349 (MOA-2007-BLG-379)OGLE-2007-BLG-349 (MOA-2007-BLG-379)
q=q=2.8x10^-4, sep=, sep= 0.8RE
VLTVLTHSTHSTImages are Images are
takentaken
preliminarypreliminary
Summary of Planet candidatesSummary of Planet candidates
preliminary. Credit Bennett
Gould et al. 2006:“Cool Neptune" planets may be relatively common with frequency of >16% at 90% confidence.”
Also consistent with formation theory. (Ida & Lin, 2004)
Number of planets via MicrolensingNumber of planets via Microlensing
0
1
2
3
4
5
2003 2004 2005 2006 2007
publishedsubmittedin preparation
Free floating planet candidatesFree floating planet candidates
tE=1.2days
prel
imin
ary
Free floating planet candidatesFree floating planet candidates
tE=1.2days
prel
imin
ary
Nmodel(tE<5) = 0.7(Scalo)Nobserv(tE<5) = 4
54 events in1/3of all fields In 2006
prel
imin
ary
Kamiya et al in preparation
SummarySummary• We are working hard to finish MOA-I
• MOA, OGLE, PLANET and μFUN found ~5 exoplanets candidates via microlensing in 2007. (in preparation)
• Consistent with Gould et al. 2006: “Cool Neptune planets may be
relatively common”
• Planet event rate increasing to ~4 planets/yr by all microlensing community’s effort.
• MOA-II demonstrated the power of wide FOV high cadence survey. OGLE-IV ( & new Korean telescopes ) Global Wide FOV network for 24hrs
• We are working hard to finish MOA-I
• MOA, OGLE, PLANET and μFUN found ~5 exoplanets candidates via microlensing in 2007. (in preparation)
• Consistent with Gould et al. 2006: “Cool Neptune planets may be
relatively common”
• Planet event rate increasing to ~4 planets/yr by all microlensing community’s effort.
• MOA-II demonstrated the power of wide FOV high cadence survey. OGLE-IV ( & new Korean telescopes ) Global Wide FOV network for 24hrs