galaxy co-evolution with black holes dark energy and gravitational-wave (gw) detection

1

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, [email protected]

Galaxy Co-Evolution with Black Holes

Dark Energy and Gravitational-Wave (GW) Detection

2011.04.05. HsinchuGalaxy-BH co-evolution, Dark Energy and GW detection W-T

Ni

Outline

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

2011.04.05. Hsinchu Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni 2


Gravitational Wave Detection

Explore fundamental physics and cosmology ；

As a tool to study Astronomy and Astrophysics

The effect of a plus-polarized/cross-polarized gravitational wave on a ring

of particles


plus-polarized cross-polarized

Complete GW Classificationhttp://astrod.wikispaces.com/file/view/GW-classification.pdf

(Modern Physics Letters A 25 [2010] pp. 922-935; arXiv:1003.3899v1 [astro-ph.CO])



0.1mHz-1 Hz ~10Hz-kHz


LIGO staff installing a mode-matching mirror and suspension into a vacuum chamber during the construction of LIGO

2011.04.05. HsinchuGalaxy-BH co-evolution, Dark Energy and GW detection W-T Ni 9

LIGO instrumental sensitivity for science runs S1 (2002) to S5 (present) in units of gravitational-wave strain per Hz1/2 as a function of frequency


Experimental Layout of LFF

In addition to adLIGO and adVirgo, LCGT construction started this yearLed by ICRR (Kajita and Kuroda)


Chinese ParticipantsTsing Hua U.

W-T Ni, H-H MeiCMS, ITRI

S-s Pan, S-R ChenBeijing N. U.

Z ZhuTsinghua U.

J CaoUSTC

Y ZhangShanghai N. U.

W-T Ni, P Xi,X Zhai

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

Second Generation Detectors


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.


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.


ASTROD-GW has the best sensitivity in the 100 nHz – 1 mHz band and fills the gap


ASTROD-GW


IJMPD, in press, 2011

FAST


Figure Sketch of the cabin suspension system.

Figure New demonstrator with complete mechanisms at Miyun station.

Guo Shou-Jin Telescope (LAMOST) and Guo Shou-Jin: Shou-Shi Li, 1280 Nathan Sivin: Granting the Seasons, Springer 2009



Massive Black Hole Systems: Massive BH Mergers &

Extreme Mass Ratio Mergers (EMRIs)

Nature, Jan. 20, 2011



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 10-2-10-3 Hz. To measure the properties of massive black hole binaries also requires good sensitivity down at least to 10-4 Hz. (2020)

Primordial Black Holes

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)


Remnants of massive single stars as a function of initial metallicity (y-axis; qualitatively) and initial mass (x-axis)


BH Coevolution with galaxies

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).


Models of formation of massive black hole binary systems (1)

(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).


Models of formation of massive black hole binary systems (2) 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.


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


A candidate sub-parsec supermassive binary blackhole system (Nature 2009) Todd A.

Boroson & Tod R. Lauer

(dubious from more recent GMRT observation)

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.



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 10-2-10-3 Hz. To measure the properties of massive black hole binaries also requires good sensitivity down at least to 10-4 Hz. (2020)

One Science Goal of LISA


2011.04.05. HsinchuGalaxy-BH co-evolution, Dark Energy and GW detection W-T Ni 33


LISA Instrument & Sciencecraft

LISA Pathfinder

Paul McNamara for the LPF Team LISA Pathfinder Project Scientist GWADW 10th - 15th May 20092011.04.05.

Hsinchu 37Galaxy-BH co-evolution, Dark Energy and GW detection W-T Ni


Drag-free AOC requirements

Thruster requirements

Proof massProof mass-S/C couplingThrust noise Control loop

gain

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.

LISA Pathfinder in Assembly Clean Room


Complete GW Classificationhttp://astrod.wikispaces.com/file/view/GW-classification.pdf

(Modern Physics Letters A 25 [2010] pp. 922-935; arXiv:1003.3899v1 [astro-ph.CO])


NANOGrav and PTA expectations


Demorest et al white paper Summary

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.


probing the black hole co-evolution with galaxies


ASTROD-GW has the best sensitivity in the 100 nHz – 1 mHz band and fills the gap


ASTROD-GW

ASTROD-GW Mission Orbit

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.


(L3)S/C 2

S/C 3 (L5)

S/C 1 (L4)

L1 L2

60

60

地球SunEarth

Weak-Light Phase Locking To 2pW A.-C. Liao, W.-T. Ni and J.-T.

Shy, On the study of weak-light phase-locking 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).


Sensitivities of Ground and Space Interferometers


AI

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

Time-delay interferometry for LISA and ASTROD-GW


Numerical Results (Wang

& Ni)


a - b

[a, b]

Numerical Results

(Wang & Ni)


[ab, ba]

[abba, baab]


The Gravitational Wave Background from Cosmological Compact BinariesAlison 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) single-arm

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 GalacticMS–MS signal at low

frequencies.

Super-ASTRODRegion DECIGO

BBO Region


BIG BANG OBSERVATORY BBO; http://universe.gsfc.nasa.gov/be/roadmap.htm

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.

Space GW Detectors (Summary)

Space interferometers (LISA,28 ASTROD,29,30 ASTROD-GW,12,14 Super-ASTROD,31 DECIGO,32 and Big Bang Observer33,34) for gravitational-wave detection hold the most promise with signal-to-noise ratio.

LISA28 (Laser Interferometer Space Antenna) is aimed at detection of low-frequency (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.


Summary

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


Summary

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 co-evolution of galaxies with BHs.


ASTROD 5 @ Raman Research Institute, July 13-15, 2012


Fifth International ASTROD Symposium

on Laser Astrodynamics,

Space Test of Relativity and

Gravitational-Wave AstronomyJuly 11 - 13, 2012, Bangalore,

India

Thank you!


galaxy co-evolution with black holes dark energy and gravitational-wave (gw) detection

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