science with decigo naoki seto (kyoto u) 2008.11.12 the 1st international lisa-decigo
DESCRIPTION
LISA LIGO,VIRGO,LCGT 2 nd generation DECIGO correlation Quick Introduction h~10 -23~-24 1HzTRANSCRIPT
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Science with DECIGO
Naoki Seto (Kyoto U)2008.11.12
The 1st International LISA-DECIGO
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Outline• Quick introduction of DECIGO band• ①Stochastic Background from early universe• ②Binary subtraction problem• Other science
– ③Dark energy– ④Intermediate mass black hole (IMBH)
• Summary
DECIGO shares many interesting (and challenging) aspects with LISA and grand-based detectors
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LISA
LIGO,VIRGO,LCGT2nd generation
DECIGO
DECIGOcorrelation
Quick Introduction
h~10-23~-24
1Hz
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LISA
DECIGO
DECIGOcorrelation
WD+WDconfusion
1/ 2
6 3~ ~110
f G Hzg cm
Frequency (f~1Hz)
High density; compact binaries (NS, stellar mass BH, IMBH,…)
e.g. Farmer & Phinney 03
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NS+NS@z=11yr
NS+NSForegroundwith R~105/yr
5/38/3
~10.2 1.2
CGW
Sun
MfT yrHz M
Signal duration (binaries)
Large number (~108) of rotations with frequency evolution
transient
stationary
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Individual NS+NS
Deep Window for GWs from Early universe?
16~10GW
Inflation?
Their foreground(to be removed)
DECIGO
correlation
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Topics in my talk
①GW fromEarly universe
②Binary Subtractionproblem
③Dark Energy with ~105binaries④IMBH evolution
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①Stochastic GW backgroundGW propagation: almost no interaction, not easy to detect,
But a crucial fossil from very Early universe!!
NASA
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GW from Inflation
• An important prediction of inflation– Origin: Quantum fluctuation– Energy scale of inflation
– Nearly flat spectrum above 10-15Hz (equal time)
– 0.1Hz: Largely different scale from CMB scale
1/ 2 2inf inf~ ~ ~ ( )h H V energy scale
4( ) ~GW energy scale const
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Smith et al.2006
1510GW
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Correlation analysisTwo sets of detectors
1 1
22
SS
nhh n
No overlap with LISA
DECIGO
DECIGOcorrelation
(fTobs)1/4
Designed to detect16~10GW
Interesting level with current constraints
But Tinto et al. 01, Hogan & Bender 01
DECIGO
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② Foreground cleaning is essential!
Individual NS+NS
NS,BH binaries NS+NS merger rate: ~(10/yr)x(10Gpc/300Mpc)3~105/yr~10-3/secOther potential foregrounds popIII SNe,…..? (might be a problem)
An inevitable problem for GW astronomy
Can we remove NS+NSs?
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In principle, Yes• (total fitting parameters)/(data amount) ~(R x Tobs x n) / (f x Tobs)
R: merger rateTobs: observational timen: number of fitting parameters for individual binaries~10f: band width ~ freqeuncy
mass, direction,…
~10-3 101 /1=10-2<<1
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• large cycle;~108
– need huge number of templates• ~1040 templates for 1yr integration
– full coherent integration; difficult• even with Moore’s law extrapolated to ~2020• need efficient detection method
– LISA(WD+WD, EMRI), LIGO-pulsar search» mock LISA data challenge, Einstein@home,...
• requirement for detector sensitivity and configuration– must detect them in short integration time– no dead angles– ongoing: careful evaluation for sensitivity and configuration
Cuter&Harms 06 (for BBO)
In reality…
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③Science with NS+NSs• Basic characters
– Huge number: ~105/yr– Excellent clocks– SNR: weak dependence on redshift z
• asymptotically (1+z)1/6– Short GRB? or EMW counterpart
• GW localization: ~1min2 with three sets• redshift estimation
• Dark energy– dL-z relation, only with basic physics– Probes for high redshift universe?
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④BH (stellar, intermediate mass)
• IMBH:highly unknown– rate, formation and evolution?– detectable with high SNR even at high-z
• 1000+1000Msun@z=1: SNR>103
• clue to understand SMBH?
• BH+NS– test for general relativity (Yagi)
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Summary
• Interesting science with DECIGO– GW background form early universe
• 1Hz: (potential) deep window for GWs• direct detection of inflation background(?), ….
– Foreground cleaning is essential!!• LISA (WD+WD,EMRI), Ground-base (unknown pulsars)
– NS+NS: ~105 good clocks available• use them for cosmology and astrophysics
– IMBHs and more