Wei-Tou Ni Department of Physics National Tsing Hua University [1] W.-T. Ni, http://astrod.wikispaces.com/file/view/GW-classification.pdf (MPLA 25 [2010] pp. 922-935; arXiv:1003.3899v1 [astro- ph.CO]). [2] S. di Serego Alighieri, W.-T. Ni and W.-P. Pan, Astrophys. J. 792, 35 (2014). [3] Mei, Ni, Pan, Xu, di Serego Alighieri, Ap J accepted; arXiv:1412. 8569 Gravitational Waves: Spectrum Classification 2015.04.07 Beijing GWs: Spectrum Classification W.-T. Ni 1
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Wei-Tou Ni Department of Physics National Tsing Hua University [1] W.-T. Ni, (MPLA 25 [2010]
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Wei-Tou NiDepartment of Physics
National Tsing Hua University[1] W.-T. Ni, http://astrod.wikispaces.com/file/view/GW-classification.pdf
(MPLA 25 [2010] pp. 922-935; arXiv:1003.3899v1 [astro-ph.CO]).
[2] S. di Serego Alighieri, W.-T. Ni and W.-P. Pan, Astrophys. J. 792, 35 (2014).
[3] Mei, Ni, Pan, Xu, di Serego Alighieri, Ap J accepted; arXiv:1412.8569
Gravitational Waves:Spectrum Classification
2015.04.07 Beijing GWs: Spectrum Classification W.-T. Ni 1
(MPLA 25 [2010] pp. 922-935; arXiv:1003.3899v1 [astro-ph.CO])
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Space Detection: LF (100 nHz- 100 mHz)
& MF (100 mHz- 10 Hz)
Complete GW Classification (I)
Ultra high frequency band (above 1 THz): Detection methods include Terahertz resonators, optical resonators, and ingenious methods to be invented.
Very high frequency band (100 kHz – 1 THz): Microwave resonator/wave guide detectors, optical interferometers and Gaussian beam detectors are sensitive to this band.
High frequency band (10 Hz – 100 kHz): Low-temperature resonators and laser-interferometric ground detectors are most sensitive to this band.
Middle frequency band (0.1 Hz – 10 Hz): Space interferometric detectors of short armlength (1000-100000 km).
Low frequency band (100 nHz – 0.1 Hz): Laser-interferometer space detectors are most sensitive to this band.
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Complete GW Classification (II)
Very low frequency band (300 pHz – 100 nHz): Pulsar timing observations are most sensitive to this band.
Ultra low frequency band (10 fHz – 300 pHz): Astrometry of quasar proper motions are most sensitive to this band.
Extremely low (Hubble) frequency band ( 1 aHz – 10 fHz): Cosmic microwave background experiments are most sensitive to this band.
Beyond Hubble frequency band (below 1 aHz): Inflationary cosmological models give strengths of GWs in this band. They may be verified indirectly through the verifications of inflationary cosmological models.
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Improved Upper Limits on the Stochastic Gravitational-Wave Background from
2009-2010 LIGO and Virgo DataarXiv1406.4556
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Primordial Gravitational Waves[strain sensitivity (ω^2) energy sensitivity]
-18.0 -14.0 -10.0 -6.0 -2.0 2.0 6.0 10.0-24.0
-22.0
-20.0
-18.0
-16.0
-14.0
-12.0
-10.0
-8.0
-6.0
-4.0
-2.0
0.0
(a)
Nv = 3.2
ms pulsars
(b) String
LIGO or VIRGO
bar-intf
LISA
strings
cosmology
WMAP
ASTROD(correlation detection)
Super-ASTROD
inflation
Nv = 4
(c) cosmic
LIGO II/LCGT/VIRGO II (2 adv intf)
Log f [[[ [f(Hz)]
Log [h02Ω
gw]
2 intf
(single intf)
‘Average’
ExtragalacticExtrapolated
*
*
DECIGO/BBO-grand(correlation detection)ASTROD
Super-ASTROD (correlation detection)
GWs: Spectrum Classification W.-T. Ni
CMB observations7 orders or more improvement in
amplitude, 15 orders improvement in power since 1965
1948 Gamow – hot big bang theory; Alpher & Hermann – about 5 K CMB
Dicke -- oscillating (recycling) universe: entropy CMB 1965 Penzias-Wilson excess antenna temperature at 4.08
GHz 3.5±1 K 2.5 4.5 (CMB temperature measurement ) Precision to 10-(3-4) dipolar (earth) velocity
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BICEP-2
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The BICEP-2 team has a lot to be proud of. They made a wonderful instrument, and collected great data. N. Czakon
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Three processes can produce CMB
B-mode polarization observed
(i) gravitational lensing from E-mode polarization (Zaldarriaga & Seljak 1997), (ii) local quadrupole anisotropies in the CMB within the last scattering region by large scale GWs (Polnarev
1985) (iii) cosmic polarization rotation (CPR) due to pseudoscalar-photon interaction (Ni 1973; for a review, see Ni 2010). (The CPR has also been called Cosmological Birefringence)
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consistent with no CPR detection
The constraint on CPR fluctuation is about 1. 5◦.
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NEW CONSTRAINTS ON COSMIC POLAR-IZATION ROTATION FROM DETECTIONS OF
B-MODE POLARIZATION IN CMBAlighieri, Ni and Pan
Fitting with dust, GWs and Lensing plus CPR
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Discussion & Outlook
GW detection Planck has releases its polarization data on the dust. Due to
Planck’s frequency coverage, we understand now that the dust foreground agrees with the BICEP2 B-mode observation. The GW interpretation needs to subtract this.
100 GHz Keck Array data will be available soon Three frequency BICEP3/Keck Array data (coming 2015?),
should be able to characterize foregrounds.BICEP/Keck has 2 more years
If r is small, it may take 5 years or more for next generation CMB experiments to come out to detect primordial GWs.
PTAs: any time around 2020; more data from binary orbit decays
Space: 20 years later, 2034 launch + 1 yr orbit transfer + Earth-based interferometer: 2015 +2015.04.07 Beijing GWs: Spectrum Classification W.-T. Ni 19
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