Galaxy Co-Evolution with Black Holes
Dark Energy and Gravitational-Wave
(GW) Detection
倪维斗 W.-T. Ni
Center for Gravitation and Cosmology
Department of Physics,
National Tsing Hua University, Hsinchu
and
Shanghai United Center for Astrophysics,
Shanghai Normal University, Shanghai
weitou@gmail.com
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Outline
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Introduction – GW Detection
Black hole co-evolution with galaxies
Pulsar timing arrays (PTA’s) as very low
frequency GW detectors
Space GW detectors
LISA, ASTROD-GW, DECIGO, Big Bang Observer
Dark Energy, Inflation, Discussion and outlook
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Gravitational Wave Detection
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Explore fundamental physics
and cosmology；
As a tool to study Astronomy
and Astrophysics
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The effect of a plus-polarized/cross-polarized
gravitational wave on a ring of particles
plus-polarized
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cross-polarized
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Complete GW Classification
http://astrod.wikispaces.com/file/view/GW-classification.pdf
(Modern Physics Letters A 25 [2010] pp. 922-935;
arXiv:1003.3899v1 [astro-ph.CO])
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0.1mHz-1 Hz
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~10Hz-kHz
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LIGO staff installing a mode-matching
mirror and suspension into a vacuum
chamber during the construction of LIGO
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LIGO instrumental sensitivity for science runs S1
(2002) to S5 (present) in units of gravitationalwave strain per Hz1/2 as a function of frequency
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Experimental Layout of LFF
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In addition to adLIGO and adVirgo,
LCGT construction started this year
Led by ICRR (Kajita and Kuroda)
Chinese Participants
Tsing Hua U.
W-T Ni, H-H Mei
CMS, ITRI
S-s Pan, S-R Chen
Beijing N. U.
Z Zhu
Tsinghua U.
J Cao
USTC
Y Zhang
Shanghai N. U.
W-T Ni, P Xi,
X Zhai
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Second Generation Detectors
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AdLIGO 10 times enhancement in strain
sensitivity  10 times reach in distance 
1000 times in volume (2015+)
GW detection from ns-ns merging:
1 per 10-20 yrs  50-100 per year
AdVIRGO (2015+)
LCGT (Started construction, June, 2010)
AIGO, INDIGO  meeting in Perth, Feb. 2010
meeting in Delhi, Feb. 2011
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Complete GW Classification (I)
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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)
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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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ASTROD-GW has the best sensitivity in the 100
nHz – 1 mHz band and fills the gap
ASTROD-GW
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FAST
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IJMPD, in press, 2011
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Figure Sketch of the cabin suspension system.
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Figure New demonstrator with complete mechanisms at Miyun
station.
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Guo Shou-Jin Telescope (LAMOST) and
Guo Shou-Jin: Shou-Shi Li, 1280
Nathan Sivin: Granting the Seasons, Springer 2009
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Massive Black Hole Systems:
Massive BH Mergers &
Extreme Mass Ratio Mergers (EMRIs)
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Nature, Jan. 20, 2011
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LISA
LISA consists of a fleet of 3 spacecraft 20º behind earth in solar
orbit keeping a triangular configuration of nearly equal sides (5 × 106 km).
Mapping the space-time outside super-massive black holes by measuring the
capture of compact objects set the LISA requirement sensitivity between 102-10-3 Hz. To measure the properties of massive black hole binaries also
requires good sensitivity down at least to 10-4 Hz. (2020)
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Primordial Black Holes
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Planck Mass BHs (formed at the Planck epoch) to solar mass
(M⊙) BHs (formed at the QCD phase transition) up to 105 M⊙
BHs
Physical or Astrophysical Constraints
(i) BH mass < 5 x 1014 g: already evaporated
due to Hawking radiation;
(ii) BH mass about 1015 g: contribution to
matter density less than 10-8 (constraints
from diffuse gamma ray background;
(iii) BH mass below about 103 (constraints from
microlensing and CMB distorsions)
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Remnants of massive single stars as a
function of initial metallicity (y-axis;
qualitatively) and initial mass (x-axis)
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BH Coevolution with galaxies
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S. Sesana, A. Vecchio and C. N. Colacino, Mon.
Not. R. Astron. Soc. 390, 192-209 (2008).
S. Sesana, A. Vecchio and M. Volonteri, Mon.
Not. R. Astron. Soc. 394, 2255-2265 (2009).
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Models of formation of massive black
hole binary systems (1)
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(i) the VHM model (Volonteri, Haardt & Madau 2003),
(ii) the KBD model (Koushiappas, Bullock & Dekel 2004),
(iii) the BVRhf model (Begelman, Volonteri & Rees 2006) and
(iv) the VHMhopk model.
In these scenarios, seed black holes are massive (M ∼ 104 M⊙) as in
the case of KBD and BVRhf, or light (M ∼ 102 M⊙), as prescribed by
VHM; seed black holes are abundant (VHM, KBD) or just a few (BVRhf).
The VHMhopk model assumes essentially the same assembly history of
the VHM model, but with a somewhat different accretion prescription
(Volonteri, Salvaterra & Haardt 2006).
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Models of formation of massive black
hole binary systems (2)
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the merger hierarchy of 220 dark matter halos in the mass
range 1011 − 1015 M⊙ up to z = 20 (Volonteri, Haardt
& Madau 2003), then populating the halos with seed black
holes and following their evolution to the present time.
For each of the 220 halos all the coalescence events happening
during the cosmic history are collected. The outputs are then
weighted using the EPS (Extended Press-Schechter) halo mass
function and integrated over the observable volume shell at
every redshift to obtain numerically the coalescence rate of
MBHBs as a function of black hole masses and redshift.
the outcome of this procedure is the numerical distribution
d3N/dzdMdt.
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Characteristic GW amplitude hc from massive black hole
binaries, the thick line shows hc produced in a specific
Monte-Carlo realization. (thin line) the prediction
yielded by the semi-analytical approach. The
observation time is T = 5 yr
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A candidate sub-parsec supermassive binary
blackhole system (Nature 2009) Todd A. Boroson & Tod R. Lauer
(dubious from more recent GMRT observation)
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quasar SDSS
J153636.221 044127.0
separated in velocity by
3,500 km/s.
A binary system of two
black holes, having
masses of 10^7.3 and
10^8.9 solar masses
Separated by 0.1 parsec
with an orbital period of
100 years.
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LISA
LISA consists of a fleet of 3 spacecraft 20º behind earth in solar
orbit keeping a triangular configuration of nearly equal sides (5 × 106 km).
Mapping the space-time outside super-massive black holes by measuring the
capture of compact objects set the LISA requirement sensitivity between 102-10-3 Hz. To measure the properties of massive black hole binaries also
requires good sensitivity down at least to 10-4 Hz. (2020)
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One Science Goal of LISA
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LISA Instrument & Sciencecraft
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LISA Pathfinder
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Paul McNamara for the LPF Team
LISA Pathfinder Project Scientist
GWADW
10th - 15th May 2009
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Drag-free AOC requirements
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Atmospheric (terrestrial) air column exclude a resolution of better than 1 mm
This reduces demands on drag-free
AOC by orders of magnitude
Nevertheless, drag-free AOC is needed for
geodesic orbit integration.
Thruster requirements
Thrust noise
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Proof mass
Proof massS/C coupling
Control loop
gain
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LISA
Pathfinder
in Assembly
Clean Room
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Complete GW Classification
http://astrod.wikispaces.com/file/view/GW-classification.pdf
(Modern Physics Letters A 25 [2010] pp. 922-935;
arXiv:1003.3899v1 [astro-ph.CO])
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NANOGrav and PTA expectations
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Demorest et al white paper
Summary
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Given sufficient resources, we expect to detect GWs
through the IPTA within the next five years.
We also expect to gain new astrophysical insight on
the detected sources and, for the first time,
characterize the universe in this completely new
regime.
The international effort is well on its way to
achieving its goals. With sustained effort, and
sufficient resources, this work is poised to offer a
new window into the Universe by 2020.
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probing the black hole co-evolution
with galaxies
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ASTROD-GW has the best sensitivity in the 100
nHz – 1 mHz band and fills the gap
ASTROD-GW
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ASTROD-GW Mission Orbit
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Considering the requirement for
optimizing GW detection while
keeping the armlength, mission
orbit design uses nearly equal
arms.
3 S/C are near Sun-Earth
Lagrange points L3、L4、L5，
forming a nearly equilateral
triangle with armlength 260
million km（1.732 AU）.
3 S/C ranging interferometrically
to each other.
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S/C 1 (L4)
(L3)
S/C 2
Sun
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球地
L1 L2
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S/C 3 (L5)
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Weak-Light Phase Locking
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To 2pW A.-C. Liao, W.-T. Ni and J.-T.
Shy, On the study of weak-light phaselocking for laser astrodynamical
missions, Publications of the Yunnan
Observatory 2002, 88-100 (2002).
To 40 fW G. J. Dick, M., D. Strekalov, K.
Birnbaum, and N. Yu, IPN Progress
Report 42-175 (2008).
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Sensitivities of Ground and Space
Interferometers
AI
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Time-delay interferometry for
LISA and ASTROD-GW
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Using Planetary Ephemeris to numerically calculate the various
solutions of Dhurandhar, Vinet and Rajesh Nayak for time-delay
interferometry of ASTROD-GW to estimate the residual laser
noise and compare. (G. Wang and W.-T. Ni, this afternoon)
Second generation solution (Dhrandhar, Vinet and Nayak):
(i) n=1, [ab, ba] = abba – baab
(ii) n=2, [a2b2, b2a2]; [abab, baba]; [ab2a, ba2b]
(iii) n=3, [a3b3, b3a3], [a2bab2, b2aba2], [a2b2ab, b2a2ba],
[a2b3a, b2a3b], [aba2b2, bab2a2], [ababab, bababa],
[abab2a, baba2b], [ab2a2b, ba2b2a], [ab2aba, ba2bab],
[ab3a2, ba3b2], lexicographic (binary) order
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Numerical Results
(Wang & Ni)
a-b
[a, b]
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Numerical
Results
(Wang & Ni)
[ab, ba]
[abba, baab]
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The Gravitational Wave Background from
Cosmological Compact Binaries
Alison J. Farmer and E. S. Phinney (Mon. Not. RAS [2003])
Optimistic (upper dotted), fiducial
(Model A, lower solid line) and
pessimistic (lower dotted)
extragalactic backgrounds plotted
against the LISA (dashed) singlearm Michelson combination
sensitivity curve. The‘unresolved’
Galactic close WD–WD spectrum
from Nelemans et al. (2001c) is
plotted (with signals from binaries
resolved by LISA removed), as
well as an extrapolated total, in
which resolved binaries are
restored, as well as an
approximation to the Galactic
MS–MS signal at low frequencies.
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Super-ASTROD
Region
Galaxy-BH co-evolution, Dark Energy and GW detection
DECIGO
BBO Region
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BIG BANG OBSERVATORY
BBO; http://universe.gsfc.nasa.gov/be/roadmap.htm
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The Big Bang Observatory is a follow-on mission to LISA, a vision mission of
NASA’s “Beyond Einstein” theme.
BBO will probe the frequency region of 0.01–10 Hz, a region between the
measurement bands of the presently funded ground- and space-based
detectors. Its primary goal is the study of primordial gravitational waves from
the era of the big bang, at a frequency range not limited by the confusion
noise from compact binaries discussed above.
In order to separate the inflation waves from the merging binaries, BBO will
identify and subtract the signal in its detection band from every merging
neutron star and black hole binary in the universe. It will also extend LISA’s
scientific program of measuring wavesfrom the merging of intermediate-mass
black holes at any redshift, and will refine the mapping of space-time around
supermassive black holes with inspiraling compact objects.
The strain sensitivity of BBO at 0.1 Hz is planned to be ∼10−24, with a
corresponding acceleration noise requirement of < 10−16 m/(s2 Hz1/2).
These levels will require a considerable investment in new technology,
including kilowatt-power level stabilized lasers, picoradian pointing capability,
multi-meter-sized mirrors with subangstrom polishing uniformity, and
significant advances in thruster, discharging, and surface potential technology.
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Space GW Detectors (Summary)
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Space interferometers (LISA,28 ASTROD,29,30 ASTROD-GW,12,14 SuperASTROD,31 DECIGO,32 and Big Bang Observer33,34) for gravitationalwave detection hold the most promise with signal-to-noise ratio.
LISA28 (Laser Interferometer Space Antenna) is aimed at detection of lowfrequency (10-4 to 1 Hz) gravitational waves with a strain sensitivity of 4 ×
10-21/(Hz) 1/2 at 1 mHz.
There are abundant sources for LISA, ASTROD and ASTROD-GW:
galactic binaries (neutron stars, white dwarfs, etc.). Extra-galactic targets
include supermassive black hole binaries, supermassive black hole
formation, and cosmic background gravitational waves.
A date of LISA launch is hoped for 2020. More discussions will be
presented in the next section.
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Summary
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Complete Classification of GWs
Detection, LCGT, adLIGO, adVirgo: 2017
PTAs: about 2020
Space detectors for Gravitational Waves
PTAs
BHs coevolution with galaxies
Dark energy, Inflation
Bright future with a lot of works
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Summary
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PTAs are most sensitive in the frequency range 300 pHz -100nHz,
LISA space GW detector is most sensitive in the frequency range 1
mHz -1 Hz, while ASTROD-GW is most sensitive in the frequency
range 100 nHz -1 mHz. PTAs have already been collecting data for
detection of stochastic GW background from supermassive BH
(SMBH) binary mergers, and are aiming at detection around 2020.
LISA and ASTROD-GW will be able to directly observe how massive
black holes form, grow, and interact over the entire history of
galaxy formation.
ASTROD-GW will also be able to observe the GW background of
SMBH merger in the frequency range 100 nHz - 10 μHz. These
observations are significant and important to the study of coevolution of galaxies with BHs.
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ASTROD 5 @ Raman Research
Institute, July 13-15, 2012
Fifth International
ASTROD Symposium
on
Laser Astrodynamics,
Space Test of Relativity
and
Gravitational-Wave Astronomy
July 11 - 13, 2012, Bangalore, India
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Thank you!
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