Sur les fusions dtoiles neutrons Lavnement de lastrophysique - - PowerPoint PPT Presentation

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Sur les fusions dtoiles neutrons Lavnement de lastrophysique - - PowerPoint PPT Presentation

Jun 21, 2023 48 likes •468 views

Sur les fusions dtoiles neutrons Lavnement de lastrophysique multjmessager Eric Chassande-Mottjn AstroPartjcule et Cosmologie (APC) CNRS Univ Paris Diderot Credits : NASA Goddard Plan de la prsentatjon Un peu de contexte

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Sur les fusions d’étoiles à neutrons

L’avènement de l’astrophysique multjmessager

Credits : NASA Goddard

Eric Chassande-Mottjn

AstroPartjcule et Cosmologie (APC) CNRS Univ Paris Diderot

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Plan de la présentatjon

  • Un peu de contexte
  • Le signal gravitatjonnel GW170817
  • GW170817 et l’astronomie multj-messager
  • Implicatjons en physique, en astrophysique et en cosmologie
  • Perspectjves
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2015 2016 2017 2018 2019 O1 4 months ~50 days

coincident

O2 6 months ~ 100 days

coincident

Virgo

O3 1 yr from Apr 2019

LIGO only LIGO & Virgo

2020

LIGO Handford H1 LIGO Livingston L1 Virgo V1

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LIGO Handford H1 LIGO Livingston L1 Virgo V1

Quasi-omnidirectjonal (no pointjng)

~3000 km (10 light-ms) ~10000 km (30 light-ms)

Sensitjvitjes during O2 (2017) H1: 60 Mpc L1: 80 Mpc V1: 25 Mpc BNS range

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Compact binary merger

inspiral merger ringdown

Characteristj tjc waveform signature Chirp mass

The signal is described by 15 parameters component masses and spins tjme and geometry: space locatjon and orientatjon

In-band duratjon

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Catalog GWTC#1

include Virgo arXiv:1811.12907, htups:/ /www.gw-openscience.org/catalogs/

populatjon of objects hidden to conventjonal astronomy populatjon of objects hidden to conventjonal astronomy populatjon of objects hidden to conventjonal astronomy Confjdent detectjons: 10 binary black hole mergers

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Plan de la présentatjon

  • Un peu de contexte
  • Le signal gravitatj

tjonnel GW170817

  • GW170817 et l’astronomie multj-messager
  • Implicatjons en physique, en astrophysique et en cosmologie
  • Perspectjves
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chirp mass GW170817

Aug 17, 2017

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10 post- merger matuer/tjdal efgects inspiral

A lot of physics in one signal

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11 inspiral

From signal phase, chirp mass estjmate

Phase matching: measurement accuracy scales with 1/Ncycles Ncycles ≈ 3000 detector-frame chirp mass

From signal amplitude, distance/inclinatjon (degenerate) Can be converted to source frame by assuming a ref. cosmology (Planck)

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12 inspiral

From signal phase, chirp mass estjmate

Phase matching: measurement accuracy scales with 1/Ncycles Ncycles ≈ 3000 detector-frame chirp mass

From signal amplitude, distance/inclinatjon (degenerate) Can be converted to source frame by assuming a ref. cosmology (Planck)

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13 tjdal

Tidal deformatjon by the gravity gradient due to companion

Efgect observable in the fjnal tens of GW cycles before merger

fGW > 400 Hz – Keplerian orbital radius ~ 60 km is comparable to NS radius

Selectjon of EoS from J. S. Read et al

  • Phys. Rev. D79, 124032 (2009) and refs therein

large star small star excluded

Cf Jerôme Margeron, Jogly 1

Figure from arXiv:1603.01286

tjdal efgects post- merger

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14 post- merger

What is the remnant? prompt collapse to a black hole QNM at 6 kHz hypermassive NS [preferred] livetjme ~ 1 s f-mode, 2-4 kHz supramassive NS livetjme ~ 10−104 s stable NS magnetar, bar mode or r-mode instability

No evidence for a post-merger signal Not enough sensitjvity at f > 2 kHz to conclude

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Plan de la présentatjon

  • Un peu de contexte
  • Le signal gravitatjonnel GW170817
  • GW170817 et l’astronomie multj

tj-messager

  • Implicatjons en physique, en astrophysique et en cosmologie
  • Perspectjves
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17 LIGO-Virgo LIGO only LIGO-Virgo sky localizatjon fjnal

(28 deg2)

rapid

(31 deg2)

(190 deg2)

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GW170817 follow-up

fjrst month only

213 GCN Circulars Peak 50/day

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Three tjme scales: seconds

T0+1.7 s : gamma-ray burst Short duratjon, ~ 2 sec Eiso ~ 1.2 x 1046 erg (assuming DL = 40 Mpc) Atypical GRB: several orders of mag less energetjc, sofuer spectrum

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Three tjme scales: hours/day

T0+~1 d : UV, optjcal and IR Host galaxy identjfjcatjon NGC4933 “Kilonova”: radioactjve-decay (r-process) powered emission from the merger ejecta

647 fmux measurements from 18 papers and 46 instruments

  • V. Ashley Villar et al,

arXiv:1710.11576

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22 HST/WFC3-IR F110W tc+4.79d Tanvir et al, ApJL 848:L27 2017

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23 A Levan, arXiv:1710.05444 MUSE

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Three tjme scales: weeks/months

X-ray T0+9 d, radio T0+16 d

Peak in X-ray & radio (100 μJy) at T0+~150 d and optjcal (m=26.5) at T0+110 d

Ghirlanda et al. ArXiv:1808.00469

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25 Credits: F Daigne

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26 Credits: F Daigne

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Jet seen ofg-axis Quasi spherical outglow Jet with lateral structure

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Late tjme radio VLBI observatjons

Mooley et al, ArXiv:1806.09693 Ghirlanda et al. ArXiv:1808.00469

  • Mooley et al & Ghirlanda et al

T0+ ~200 days

  • Very-long based interf [10 000 km]

> 32 radiotelescopes [worldwide]

  • Moving collimated jet observed
  • midly relatjvistjc jet Γ ~ 4, θjet ~ 4º
  • viewing angle θobs ~ 20º

T0+230 d T0+75 d

~2.4 mas

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Jet seen ofg-axis Quasi spherical outglow Jet with lateral structure

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Plan de la présentatjon

  • Un peu de contexte
  • Le signal gravitatjonnel GW170817
  • GW170817 et l’astronomie multj-messager
  • Implicatj

tjons en physique, en astrophysique et en cosmologie

  • Perspectjves
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Implicatjons (1): nucleosynthesis

647 fmux measurements from 18 papers and 46 instruments

  • V. Ashley Villar et al, arXiv:1710.11576
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Implicatjons (2): modifjed gravity

  • Coincidence with GRB170817A within 1.7 s
  • Very stringent constraints on the speed of gravity |c/cg – 1| < 5 x 10
  • 16
  • Incompatjble with a large set of alt. gravity scalar-tensor theories

brought forward to explain dark energy

h tu p s : / / a r x i v .

  • r

g / a b s / 1 7 1 . 5 9 1 h tu p s : / / a r x i v .

  • r

g / a b s / 1 7 1 . 5 8 7 7

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Implicatjons (3): extra-dimensions

  • Test extra-dimensional theories of gravity

–

Compare the luminosity distance extracted from the GW signal to the EM-measured distance of NGC4933

arXiv:1801.08160 vs

gravitatjonal leakage

num of space-tjme dimensions

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Implicatjons (4): Cosmology

from GW signal amplitude [no “cosmological ladder”!]

from host galaxy identjf.

Hubble Lemaître law

1929, distances from Cepheids variables

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Plan de la présentatjon

  • Un peu de contexte
  • Le signal gravitatjonnel GW170817
  • GW170817 et l’astronomie multj-messager
  • Implicatjons en physique, en astrophysique et en cosmologie
  • Perspectj

tjves

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GW astronomy today

  • Advanced LIGO and Virgo observing
  • Stable operatjon (~70 %) since April 1st 2019
  • Improved sensitjvies wrt O2:

Virgo x ~2, LIGO HL + 65 %

  • Public alerts within minutes
  • 36 GW alerts – 7 retractjons
  • 21 events classifjed as BBH, 4 as BNS and

2 events as NS-BH

  • Now commissioning break for a month
  • No electromagnetjc counterpart

detected so far

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Alert retracted O3a summary

~ 1 alert/week

Binary neutron star (6) Binary black hole (21) Neutron star-black hole (4)

htups:/ /arxiv.org/abs/1304.0670

“Mass gap” – 3 to 5 Msun (2)

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GW astronomy in 2025

  • Five large-scale detectors in operatjon
  • Best BNS range ~ 300 Mpc – Horizon z ~ 0.15
  • ~3 x current sensitjvity

rough extrapolatjon from 03 → ~4 events/day (!)

  • O(100) BBH and O(10) BNS per year

[rates will be revised afuer O3]

  • How many with an observed electromagnetjc

counterpart?

adV+ A+ A+ Kagra+

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gw-openscience.org

“Only days afuer they announced the fjrst observatjon of gravitatjonal waves, the LIGO and Virgo collaboratjons made public their data.”

  • Whole science-run data and GW event catalogs

✔

80+ papers using open data

  • Documentatjon, usage recommendatjons
  • Online training: video tutorials and Jupyter notebooks
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Concluding remarks

  • Multj-messenger astronomy in its infancy

–

Joint GW and EM signals allows unique tests in a range of fjelds

–

Many breakthroughs with only one event

  • Is this going to happen again (during O3)?

–

In principle, yes but we probably got lucky with GW170817 (close source) Back-of-the-envelope calculatjon : ~3 % in six months

–

Major facilitjes in the next 10 years CTA; SVOM; LSST and JWST; SKA Game changer for electromagnetjc follow-up

  • Part of the Universe observable in GW is expanding very fast

–

Sensitjvitjes ~+20 % / year (x 2 every four years)

–

More detectors around the globe soon (Japan, India)

  • Very promising science program with large discovery potentjal!!
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Cosmography with standard sirens

  • Tension in the current H0 measurements from early/late tjmes
  • Infer H0 from D-z measurement from BNS “standard sirens”
  • Demonstrated with GW170817
  • Need ~200 BNS D-z measurement to reach the percent level
  • May reach this goal with 2G
  • This will depend on our ability to fjnd EM counterparts
  • We see in O3 this is diffjcult – 10-100 sq degrees loc
  • A network 3G instruments will localize 104 BNS / yr

within 1 square degree

  • 3G will observe more distant BNS

Allow to measure other cosmological parameters