Gravitational Wave detectors of near future...Space: LISA • LISA is a space-borne Gravitational...

Gravitational Wave detectors

of near future

M. Drago

Gran Sasso Science Institute

Gravitational Waves

➢ Linear approximation⚫ gab = hab + hab |hab|

GWs Generation

➢ The lowest moment of mass-energy tensorwhich generates GWs sources is thequadrupolar⚫ Binary systems

⚫ Singular systems with non axis-symmetry process

➢ Astrophysical sources⚫ Un-modeled bursts (binary mergers, supernovae, GRBs, SGR)

⚫ Modeled bursts, Inspiral (Compact Binary Coalescence)

⚫ Periodic (Pulsar)

⚫ Stochastic (Big Bang)

⚫ Expected amplitude:

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Compact Binary Coalescence

– Inspiral: two objects rotate around each other and approach

– Merger: the objects merge in a single one

– Ring-down: relaxation of the remaining object


• Signals produced from the Coalescence of a Binary system of Compact objects

• Characterized by three phases:Phys. Rev. Lett. 116, 061102 (2016)

Interferometric detectors


3G R&D: Research and Development for the Next Generation of Ground-based Gravitational-wave Detectors

h+ hx

https://gwic.ligo.org/3Gsubcomm/documents/GWIC_3G_R_D_Subcommittee_report_July_2019.pdf

2G observatories

M. Drago 6Neutrini, fotoni e onde gravitationali

2G schedule


arXiv:1304.0670v9

The planned sensitivity evolution and observing runs of the aLIGO, AdV and KAGRA detectors over the coming years. The colored bars show the observing runs, with achieved sensitivitiesin O1, O2 and O3. Uncertainty in start or finish dates is represented by shading.

You are here

https://arxiv.org/abs/1304.0670v9

2G sensitivites

M. Drago 8

aLIGO (top left), AdV (center) and KAGRA (top right) target strain sensitivities as a function of frequency. The quoted range is for a 1.4M+1.4M BNS merger. The BNS range (in megaparsec) achieved in past observing runs and anticipated for future runs is shown. The O1 aLIGO curve is taken from the Hanford detector, the O2 aLIGO curve comes from Livingston. In each case these had the better performance for that observing run. The O3 curves for aLIGO and AdV reflect recent performance. The KAGRA BNS curve may be realized by detuning the signal recycling cavity to significantly improve the BNS range to 155 Mpc once design sensitivity is reached

Neutrini, fotoni e onde gravitationali

arXiv:1304.0670v9

https://arxiv.org/abs/1304.0670v9

O1 + O2


GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers

Observed by LIGO and Virgo during the First and Second Observing RunsPhys. Rev. X 9, 031040 (2019), arXiv:1811.12907

https://journals.aps.org/prx/abstract/10.1103/PhysRevX.9.031040https://arxiv.org/abs/1811.12907

GW150914

• First Gravitational Wave Detection!

• Opening of GW astronomy

• Binary Black Hole Coalescence

• Phys. Rev. Lett. 116, 061102 (2016)


http://journals.aps.org/prl/abstract/10.1103/PhysRevLett.116.061102

GW170817

• First Multi-messenger GW+EM detection

• Binary Neutron Star Coalescence

• Phys. Rev. Lett. 119, 161101 (2017)

• Astrophys. J. Lett. 848, L12 (2017)


http://journals.aps.org/prl/abstract/10.1103/PhysRevLett.119.161101http://iopscience.iop.org/article/10.3847/2041-8213/aa91c9/meta

S190425z skymap

O3

• O3a: April-September 19– 33 public alerts, 8 retractions

• O3b: November 2019 – … 2020– More events coming!

• KAGRA will join soon


S190512atsource classification

https://gracedb.ligo.org/superevents/S190425z/view/https://gracedb.ligo.org/superevents/public/O3/https://gracedb.ligo.org/superevents/S190512at/view/

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BEYOND ADVANCED

DETECTORS


The Next-Generation Global Gravitational-Wave Observatory: New Astrophysics

with the Farthest, Oldest, and Most Violent Events in the Universe

https://gwic.ligo.org/3Gsubcomm/documents/science-case.pdf

3G detectors


3G detectors: ET




3G detectors: CE




3G detectors: Voyager




Space: LISA

• LISA is a space-borne Gravitational Wave Observatory with an arm-length of 2.5 million km.

• LISA will enable us to discover new parts of the universe: such as black holes, the Big Bang, unknown, objects


Time, sky and polarisation averaged LISA sensitivity as defined in the L3 mission proposal in January 2017. Credit: LISA Consortium

LISA will complement traditional astronomical observations based on the electromagnetic spectrum (for example, observations from visible light, infra-red or x-rays).

It will open the gravitational wave window in space and measure gravitational radiation from about 0.1 mHz to 100 mHz

Artist's impression of LISA satellite.Credit: AEI/MM/exozet/NASA/Henze

Detector Sensitivity


Target sensitivity curves for 3G gravitational-wave detectors Einstein telescope (ET) [7], shown in green, and Cosmic Explorer (CE) [8], shown in pink, compared with the design sensitivity of Advanced LIGO, shown in blue. The shades of the curves represent sensitivity to sources with differently distributed locations.



PHYSICS WITH 3G


Observing Stellar-mass Black

Holes Throughout the Universe


Waveform from final stages of inspiral, merger and ringdown of a 100M+100M BBH

• Expanding the black hole mass spectrum• High-precision measurements of binary

properties• Multiband gravitational-wave observation

Extreme matter, extreme

environment


Predicted composition of matter NS interior

NS challenge

• Nature of matter at highestdensities

• Nucleosynthesis in Neutron Star Binary Mergers


• Formation, Demographics and Merger Sites of Compact Binary Mergers

• Jet Physics in Neutron Star Binary Mergers

The figure shows approximateboundaries between different phases of matter and the most relevant degrees of freedom.

Cosmology and the Early History

of the Universe


Stochastic GW background for several model spectra in comparison with past measurements (AdvLIGO UL, big bang nucleosynthesis and CMB observations, low-l CMB observations, and pulsar timing), and future expected sensitivities, (the final sensitivity of Advanced LIGO, CE, and LISA, all assuming 1 year of exposure). Gray band: expected amplitude of compact binary merger background .

Extreme Gravity and

Fundamental Physics


Nature of Gravity

• New fields, particles and polarizations

• Graviton mass• Lorentz violations• Parity violations• Time variability of

gravitational constant• Ultra-light Bosonic Clouds• Large, non-local, quantum

effects


Probing gravity at all scales: Illustration of thereach in curvature scales vs potential scales targeted by different, representative, past/current/future missions. In this figure, M and L are the characteristic mass and length involved in the observable associated to each mission

Nature of black holes

• Perturbed black hole returns to quiescent state by quasi-normal modes oscillations.

• Quasi-normal modes depend on mass and spin.

• 3G detectors can facilitate multiple null-hypothesis tests of the Kerr metric


Test of black hole nature: Projections of the 95% confidence intervals for 2 QNM (complex) frequencies, notably ( f22; t22; f33), as function of the mass (M) and dimensionless spin ( j J=M2) of the final compact object for a single GW150914-like event with advanced detectors at design sensitivity (HLV, dashed curves) and 3G detectors (continuous curves). The yellow star corresponds to the true value of mass and spin used in the simulation.

Nature of dark matter

• Black holes as dark matter candidates (?)– dark matter can be composed (in

part) of BH of masses 0:1–100M ??– BH produced from collapse of large

primordial density fluctuations in the very early Universe or during inflation. (Mass distribution depending on inflation model)


• 3G detectors will be uniquely positioned to determine mass and spatial distribution– GW from binary systems of

objects much lighter than stellar-mass black holes / very high redshift sources -> primordial BH

Upper limits from different observations of microlensing of stars, microlensing of supernovae (SNe), caustic disruption, Planck, stability of Eridanus II. Gravitational-wave constraints correspond to LIGO searches for sub-solar compact objects and highmassestimates. The shaded regions correspond to the mass function imprinted by the quantum chromodynamics (QCD) phase transition, for different primordial black hole abundances and a primordial scale invariant spectrum. 3G detectors can improve the current bounds by many orders of magnitude.

Sources at the Frontier of

Observations


Characteristic strain vs. frequency of three typical 3D core-collapse supernova simulations: C15, W15-4, and TM1 and Expected design sensitivity curves for Einstein Telescope (ET-D), Cosmic Explorer (CE), and Advanced LIGO (aLIGO).

Summary

• 3G gravitational wave observatories will be ten times more sensitive than current instruments

• With 3G detectors we can/will:– chart the evolution of black holes, from stellar-mass to

supermassive, from the early Universe to today– explore the physics of ultra dense matter, the nature of mergers

involving double black holes and black holes and neutron stars.– investigate the fundamental physics of the primeval Universe

and probe its dark sectors.– explore the nature of gravity in regions of spacetime with the

greatest curvature, largest gravity gradients and deepest gravitational potentials.

– enable us to use gravitational waves to understand the inner dynamics of the most extreme matter and violent explosions in the Universe.


Gravitational Wave detectors of near future...Space: LISA • LISA is a space-borne Gravitational...

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