LISA Science - Neil J. Cornish Montana State University - IN2P3
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LISA Science
Neil J. Cornish
Montana State University
Outline • LISA science then and now • The science landscape in 2034 • What’s new in LISA science • Triple systems • Multi-band observations • New candidates for EM counterparts • The LISA analysis challenge
You win some, you lose some
1e-17
1e-18
Sn1/2 [Hz-1/2]
1e-19
LISA 2017
1e-20
0.0001 0.001 0.01 0.1 1
f [Hz]
Classic LISA Science Case
• Massive (10 - 10
5 7
M ) Black Hole mergers to high z
as tracers of BH-galaxy co-evolution
• Extreme Mass Ratio Inspirals (EMRIs) for tests of
GR and as probes of galactic cusps
• Galactic binaries for stellar evolution and galactic
structure
• Stochastic backgrounds from early Universe
LISA
Laser Interferometer Space Antenna
for the detection and observation of gravitational waves
An international project in the field of
Fundamental Physics in Space
Pre-Phase A Report
Second Edition
July 1998
MPQ 233 July 1998
20 years later….
Key Science Goal: Understanding Black Hole - Galaxy Coevolution
Understanding Black Hole - Galaxy Coevolution
LISA
ET
LIGO/Virgo BHs LISA BHs • Tens of solar masses • Millions of solar masses • Equal mass • Highly un-equal mass • Low spin • High + Low spins • Zero eccentricity • Significant eccentricity • Low redshift • High redshift
Astrophysics in the 2034
Post JWST Post WFIRST Post Athena Post aLIGO+ Post IPTA
• Assembly and growth of first galaxies observed by JWST
• Expansion history & distance scale to better than 1% from WFIRST
• High SNR (100+) gravitational wave signals detected by LIGO/Virgo
• 100’s of EM counterparts to LIGO/Virgo sources detected
• Athena will have detected many IMBHs
• Supermassive Black Holes observed to high redshift (z~8) by Athena
• Gravitational waves from supermassive black hole binaries discovered by IPTAAstrophysics in the 2034
Post EELT Post GAIA Post LSST Post GRAVITY Post SKA
• EELT will observe first stars in Universe and early black holes
• Census of IMBH masses from stellar velocities in clusters from EELT
• GAIA catalog will include several hundred short period eclipsing WD binaries
• SKA will have discovered pulsars at the galactic center giving insight into EMRI rates
• LSST will detect 100’s of SMBH stellar tidal disruption events per year and give insight into
EMRI populations
• GRAVITY and its successors will have found stars with < year orbits around Sgr A* yielding
insight into EMRI ratesGrowing LISA Science Case
• Classic LISA science case +
• Triple systems everywhere
• Prompt and pre-cursor EM counterparts
•
2 4
Intermediate mass black holes (10 -10 M )
• Multi-band observations (LISA + Ground)
• IMRIs (mass ratios 100-1000)
• EMRI resonances
• WD resonances, detonations
• Unmodeled BurstsGuaranteed Sources: Galactic Binaries
20 min
orbital
periodLISA galaxy catalog over time
LISA galaxy catalog over time
LISA galaxy catalog over time
LISA galaxy catalog over time
LISA galaxy catalog over time
LISA galaxy catalog over time
LISA galaxy catalog over time
LISA galaxy catalog over time
10000 1 Year
# White Dwarfs
1000 1 Month
1 Week
100
1e+06 1e+07 1e+08
t (s)EM Counterparts: Galactic Verification Binaries
11 currently known
Gaia: 15-25 more LSST: 50-75 more
[Korol et al, MNRAS, 470 (2017)]
[Littenberg et al, arXiv:1903.05583]
[Kupfer et al, MNRAS, 480 (2018)]New, loud verification binaries
SDSS J0651+2844 [Brown et al. 2011] WD0931+444 [Kilic et al. 2014] SDSS J104336.275+055149.90 [Brown et al. 2017]
12 minute eclipsing WD-WD binary 20 minute detached WD-WD binary 46 minute detached WD-WD binary
m1 = 0.26 M , m2 = 0.50 M
AAACF3icbVDLSgMxFM3UV62vqks3wSK4KMNMfYIUim7cCBXsAzrDkMmkbWgyGZKMUEr/wo2/4saFIm5159+YPha19cCFwzn3cu89YcKo0o7zY2WWlldW17LruY3Nre2d/O5eXYlUYlLDggnZDJEijMakpqlmpJlIgnjISCPs3Yz8xiORior4QfcT4nPUiWmbYqSNFORtHriwDB27dA69K3gXeCISugi9IuRBCZYd+8yZMYJ8wbGdMeAicaekAKaoBvlvLxI45STWmCGlWq6TaH+ApKaYkWHOSxVJEO6hDmkZGiNOlD8Y/zWER0aJYFtIU7GGY3V2YoC4Un0emk6OdFfNeyPxP6+V6valP6BxkmoS48midsqgFnAUEoyoJFizviEIS2puhbiLJMLaRJkzIbjzLy+Sesl2T+zS/Wmhcj2NIwsOwCE4Bi64ABVwC6qgBjB4Ai/gDbxbz9ar9WF9Tloz1nRmH/yB9fULKISa9w==
m1 = 0.32M , m2 0.14M m1 = 0.183 M , m2 > 0.07 M
AAACGXicbVDLSgMxFM34rPU16tJNsAguSplphRZEKbpxI1SwD+gMQyZN29BkMiQZoQz9DTf+ihsXirjUlX9j+ljU1gMXDufcy733hDGjSjvOj7Wyura+sZnZym7v7O7t2weHDSUSiUkdCyZkK0SKMBqRuqaakVYsCeIhI81wcDP2m49EKiqiBz2Mic9RL6JdipE2UmA7PHDhJXQKbqUEvQt4F3iiI3QeennIgyK8MpZTnnMCO2eUCeAycWckB2aoBfaX1xE44STSmCGl2q4Taz9FUlPMyCjrJYrECA9Qj7QNjRAnyk8nn43gqVE6sCukqUjDiTo/kSKu1JCHppMj3VeL3lj8z2snulvxUxrFiSYRni7qJgxqAccxwQ6VBGs2NARhSc2tEPeRRFibMLMmBHfx5WXSKBbcUqF4f56rXs/iyIBjcALOgAvKoApuQQ3UAQZP4AW8gXfr2Xq1PqzPaeuKNZs5An9gff8CCxSbYg==
DL = 660 kpc
AAAB/3icbVDLSgMxFM3UV62vUcGNm2ARXJWZKlUQoagLFy4q2Ad0hiGTpm1okhmSjFDGLvwVNy4UcetvuPNvTNtZaOuBC4dz7uXee8KYUaUd59vKLSwuLa/kVwtr6xubW/b2TkNFicSkjiMWyVaIFGFUkLqmmpFWLAniISPNcHA19psPRCoaiXs9jInPUU/QLsVIGymw966DW3gBKxUHeucw9SSHgxiPArvolJwJ4DxxM1IEGWqB/eV1IpxwIjRmSKm268TaT5HUFDMyKniJIjHCA9QjbUMF4kT56eT+ETw0Sgd2I2lKaDhRf0+kiCs15KHp5Ej31aw3Fv/z2onunvkpFXGiicDTRd2EQR3BcRiwQyXBmg0NQVhScyvEfSQR1iayggnBnX15njTKJfe4VL47KVYvszjyYB8cgCPgglNQBTegBuoAg0fwDF7Bm/VkvVjv1se0NWdlM7vgD6zPH6+ek/s=
DL = 580 kpc
AAAB/3icbVDLSgMxFM3UV62vUcGNm2ARXJWZqlgQoagLFy4q2Ad0hiGTpm1okhmSjFDGLvwVNy4UcetvuPNvTNtZaOuBC4dz7uXee8KYUaUd59vKLSwuLa/kVwtr6xubW/b2TkNFicSkjiMWyVaIFGFUkLqmmpFWLAniISPNcHA19psPRCoaiXs9jInPUU/QLsVIGymw966DW3gBTysO9M5h6kkOBzEeBXbRKTkTwHniZqQIMtQC+8vrRDjhRGjMkFJt14m1nyKpKWZkVPASRWKEB6hH2oYKxIny08n9I3holA7sRtKU0HCi/p5IEVdqyEPTyZHuq1lvLP7ntRPdrfgpFXGiicDTRd2EQR3BcRiwQyXBmg0NQVhScyvEfSQR1iayggnBnX15njTKJfe4VL47KVYvszjyYB8cgCPggjNQBTegBuoAg0fwDF7Bm/VkvVjv1se0NWdlM7vgD6zPH7Evk/w=
fGW = 2.61 mHz
AAACA3icbVDLSsNAFJ3UV62vqDvdDBbBVUiqqCBC0YVdVrAPaEKYTCft0JkkzEyEGgJu/BU3LhRx60+482+cPhbaeuDC4Zx7ufeeIGFUKtv+NgoLi0vLK8XV0tr6xuaWub3TlHEqMGngmMWiHSBJGI1IQ1HFSDsRBPGAkVYwuB75rXsiJI2jOzVMiMdRL6IhxUhpyTf3Qj+7aeXwElasUwe6FzBzBYe89pD7Ztm27DHgPHGmpAymqPvml9uNccpJpDBDUnYcO1FehoSimJG85KaSJAgPUI90NI0QJ9LLxj/k8FArXRjGQlek4Fj9PZEhLuWQB7qTI9WXs95I/M/rpCo89zIaJakiEZ4sClMGVQxHgcAuFQQrNtQEYUH1rRD3kUBY6dhKOgRn9uV50qxYzrFVuT0pV6+mcRTBPjgAR8ABZ6AKaqAOGgCDR/AMXsGb8WS8GO/Gx6S1YExndsEfGJ8/u/KVqw==
fGW = 1.68 mHz fGW = 0.73 mHz
AAACA3icbVBNS8NAEN3Ur1q/ot70slgETyFphQoiFD3YYwXbCk0Im+2mXbqbhN2NUEPBi3/FiwdFvPonvPlv3LY5aOuDgcd7M8zMCxJGpbLtb6OwtLyyulZcL21sbm3vmLt7bRmnApMWjlks7gIkCaMRaSmqGLlLBEE8YKQTDK8mfueeCEnj6FaNEuJx1I9oSDFSWvLNg9DPrjtjeAFtq1aF7jnMXMEhbzyMfbNsW/YUcJE4OSmDHE3f/HJ7MU45iRRmSMquYyfKy5BQFDMyLrmpJAnCQ9QnXU0jxIn0sukPY3islR4MY6ErUnCq/p7IEJdyxAPdyZEayHlvIv7ndVMVnnkZjZJUkQjPFoUpgyqGk0BgjwqCFRtpgrCg+laIB0ggrHRsJR2CM//yImlXLKdqVW5Oy/XLPI4iOARH4AQ4oAbqoAGaoAUweATP4BW8GU/Gi/FufMxaC0Y+sw/+wPj8Ab1+law=Orion’s Belt Triple
Mintaka
Galactic Triples
Quintuple
TripleGalactic Triples
96% of low mass binaries with periods shorter
than 3 days are in triple or quadruple systems
3-body effects (Lidov-Kozai) can accelerate the
hardening of the inner binary producing LISA
sources
With LISA, systems with outer orbital
period out to 100 years are detectable
[Robson, Cornish, Tamanini, Toonen, Phys.Rev. D98 (2018)]A new solution to the Last Parsec Problem
[Bonetti, Sesana, Barausse & Haardt MNRAS, 477 (2018)]Black Hole Triples
Massive BH + Stellar mass binary
[Meiron, Kocsis & Loeb, ApJ, 834 (2017)]
Massive BH triples
[Inayoshi, Tamanini, Caprini & Haiman, PRD, 96 (2017)]
Stellar mass BH triples Typically have large
orbital eccentricities
[Inayoshi, Tamanini, Caprini & Haiman, PRD, 96 (2017)]
[Randall & Xianyu, arXiv:1805.05335] [Hoffman & Loeb, MNRAS, 377 (2007)]
[Bonetti, Haardt, Sesana & Barausse, MNRAS, 461 (2016)]Electromagnetic Counterparts to SMBHBs
Significant pre and post merger EM counterparts to SMBHBs
[Farris et al. 2015]Electromagnetic Counterparts to SMBHBs
Transient Astrophysics Probe (TAP)
[Dal Canton et al, arXiv:arXiv:1902.01538] Few to dozens of pre-merger LISA counterpartsMulti-Band Observations
[Amaro-Seoane & Santamaria 2010] [Sesana 2016]
Can study stellar mass binary formation channels (eccentricity, spin precession)
Powerful tests of general relativity
Ground based detections can be used to find more LISA signals [Review: Cutler et al, arXiv:1903.04069 ]EMRI orbital resonances
• Each EMRI in LISA band passes through
several resonances
• Jump in the frequency and phasing a
challenge for detection algorithms
• Potential to improve parameter estimation
and provide ultra-stringent GR tests
[Brink, Geyer, Hinderer 13] [Ruangsri, Hughes 13]The LISA analysis challenge Millions of overlapping signals Many complex signals with many harmonics Noise non-stationary on timescale of signals Frequent data gaps and disturbances No second detector to veto noise transients
https://lisa-ldc.lal.in2p3.fr
Exotic Sources
Imagined
Topological defects Pre-heating/Re-heating Warped extra dimensions
Phase transitions- bubble nucleation, Braneworlds
cavitation, collisions
Un-Imagined Burst sources?Detecting Un-modeled Signals
Z
X Y
}
3
A S+ = X
2 Sensitive to GWs and glitches
1
E S = (X + 2Y )
2
1
T S = (X + Y + Z)
3 } Insensitive to GWs, Sensitive to GlitchesLISA Sensitivity - T channel as noise monitor
Two decades of
attenuation
Key to detecting a stochastic background
[Prince et al, Phys. Rev. D66 (2002)]
[Tinto, Armstrong & Estabrook, Phys.Rev.D63 (2001)]
[Hogan & Bender, Phys. Rev. D64 (2001)]
[Adams & Cornish, Phys. Rev. D86 (2010)]Detecting Un-modelled signals
Detecting Un-modelled signals
Separating Burst Signals from Noise
Noise delays
L
t=n
c
Signal delays
L k̂ · L
t=n +
c cSeparating Burst Signals from Noise
A E T
108
21 22 22
⇥10 ⇥10 ⇥10
1.00
op
6 2
0.75 Case 1 12
0.50
4 Burst
ac
7
BB,P M 12 AET
0.25 2
1 21
10
0.00 0 0
BB,AC21 AET
106
BB,P M 12 X
0.25 2
0.50 4 1
0.75
1.00
6
2 105 BB,AC21 X
1.6 1.8 2.0 2.2 2.4 2.6 2.8 3.0 1.6 1.8 2.0 2.2 2.4 2.6 2.8 3.0 1.6 1.8 2.0 2.2 2.4 2.6 2.8 3.0
t [hrs] t [hrs] t [hrs]
104
21 21 21
⇥10 ⇥10 ⇥10
1.5 1.5 1.5
B
1.0 Case 2 1.0 1.0
0.5 0.5 0.5 103
0.0 0.0 0.0
Very Strong: > 150
0.5 0.5 0.5 102
Strong: 20 150
1.0 1.0 1.0
1.5 1.5 1.5
101 Positive: 3 20
2.265 2.270 2.275 2.280 2.285 2.290 2.295 2.265 2.270 2.275 2.280 2.285 2.290 2.295 2.265 2.270 2.275 2.280 2.285 2.290 2.295
t [hrs] t [hrs] t [hrs]
6
⇥10 22
6
⇥10 22
6
⇥10 22
100
Case 3
4 4 4
2 2 2
2.5 5.0 7.5 10.0 12.5 15.0 17.5 20.0
0 0 0 ⇢
2 2 2
4 4 4
With all three channels we can
detect very low SNR burst signals
6 6 6
2.265 2.270 2.275 2.280 2.285 2.290 2.265 2.270 2.275 2.280 2.285 2.290 2.265 2.270 2.275 2.280 2.285 2.290
t [hrs] t [hrs] t [hrs]
[Robson & Cornish, PRD 99 (2019)]Growing LISA Science Case
• Classic LISA science case +
• Triple systems everywhere
• Prompt and pre-cursor EM counterparts
•
2 4
Intermediate mass black holes (10 -10 M )
• Multi-band observations (LISA + Ground)
• IMRIs (mass ratios 100-1000)
• EMRI resonances
• WD resonances, detonations
• Unmodeled BurstsYou can also read
