The CMB as a detector of gravitational waves - Camilo A. Garcia Cely - Max-Planck-Institut für Astrophysik Cosmology Seminar June 15, 2021 ...
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The CMB as a detector
of gravitational waves
Camilo A. Garcia Cely
Alexander von Humboldt Fellow
Max-Planck-Institut für Astrophysik
Cosmology Seminar
June 15, 2021
Based on
PHYSICAL REVIEW LETTERS 126, 021104 (2021)
Potential of Radio Telescopes as High-Frequency Gravitational Wave Detectors
1,2,3,* 1,†
Valerie Domcke and Camilo Garcia-Cely
1
Deutsches Elektronen-Synchrotron DESY, Notkestrasse 85, 22607 Hamburg, Germany
2
Theoretical Physics Department, CERN, 1 Esplanade des Particules, CH-1211 Geneva 23, Switzerland
3
Institute of Physics, Laboratory for Particle Physics and Cosmology (LPPC),
École Polytechnique Fédérale de Lausanne (EPFL), CH-1015 Lausanne, Switzerland
(Received 11 June 2020; revised 6 August 2020; accepted 7 December 2020; published 14 January 2021)
In the presence of magnetic fields, gravitational waves are converted into photons and vice versa. We
Outline
• Motivation
• Gravitational Waves and the Gertsenhstein Effect
• CMB obser vations and 21–cm cosmology
• Conclusions
Camilo A. Garcia Cely
Motivation
Gravitational Waves
• Predicted by Poincaré (1905)
• Einstein provided a firm theoretical background for them (1916)
Camilo A. Garcia Cely
Gravitational Waves
• Predicted by Poincaré (1905)
• Einstein provided a firm theoretical background for them (1916)
□ hμν = − 16πGTμν
Camilo A. Garcia Cely
Gravitational Waves
• Predicted by Poincaré (1905)
• Einstein provided a firm theoretical background for them (1916)
□ hμν = − 16πGTμν
Camilo A. Garcia Cely
Gravitational Waves
• Predicted by Poincaré (1905)
• Einstein provided a firm theoretical background for them (1916)
□ hμν = − 16πGTμν
Camilo A. Garcia Cely
Gravitational Wave Spectrum
Credit: NASA Goddard Space Flight Center
Camilo A. Garcia Cely
Gravitational Wave Spectrum
Credit: NASA Goddard Space Flight Center
Camilo A. Garcia CelyGravitational Wave Spectrum
what about high frequencies?
LIGO - VIRGO, 2014
Camilo A. Garcia CelyGravitational Wave Spectrum
what about high frequencies?
LIGO - VIRGO, 2014
Radio and TeV astronomy
Domcke, CGC 2021
Camilo A. Garcia CelyGravitational Wave Spectrum
what about high frequencies?
LIGO - VIRGO, 2014
Cosmological const raints
on radiation energy Neff
Radio and TeV astronomy
Domcke, CGC 2021
Camilo A. Garcia CelyGravitational Waves and the Gertsenhstein Effect
Revisiting Gertsenhstein’s ideas
Camilo A. Garcia CelyRevisiting Gertsenhstein’s ideas
Camilo A. Garcia CelyThe Gertsenhstein Effect
• The conversion of gravitational waves into
electromagnetic waves is a classical process.
Its rate does not involve ℏ
• The process is strictly analogous to axion-
photon conversion.
• Involving gravity the conversion probabilities
are extremely small. It may be compensated by
a ‘detector’ of cosmological size.
• Distortions of the CMB
Camilo A. Garcia CelyThe Gertsenhstein Effect
• The conversion of gravitational waves into
electromagnetic waves is a classical process.
Its rate does not involve ℏ
• The process is strictly analogous to axion-
photon conversion. Raffelt, Stodolski’89
• Involving gravity the conversion probabilities
Ringwald, Jan Schütte-Engel, Tamarit 2011.04731
are extremely small. It may be compensated by
a ‘detector’ of cosmological size.
Domcke, CGC 2021
• Distortions of the CMB Dolgov, Ejlli 2012
Pshirkov, Baskaran 2009
Chen 1995
Camilo A. Garcia CelyThe Gertsenhstein Effect
• The conversion of gravitational waves into
electromagnetic waves is a classical process.
Its rate does not involve ℏ
• The process is strictly analogous to axion-
photon conversion. Raffelt, Stodolski’89
• Involving gravity the conversion probabilities
Ringwald, Jan Schütte-Engel, Tamarit 2011.04731
are extremely small. It may be compensated by
a ‘detector’ of cosmological size.
Domcke, CGC 2021
• Distortions of the CMB Dolgov, Ejlli 2012
Pshirkov, Baskaran 2009
Chen 1995
Camilo A. Garcia CelyThe Gertsenhstein Effect
• The conversion of gravitational waves into
electromagnetic waves is a classical process.
Its rate does not involve ℏ
• The process is strictly analogous to axion-
photon conversion. Raffelt, Stodolski’89
• Involving gravity the conversion probabilities
Ringwald, Jan Schütte-Engel, Tamarit 2011.04731
are extremely small. It may be compensated by
a ‘detector’ of cosmological size.
Domcke, CGC 2021
• Distortions of the CMB
Camilo A. Garcia CelyThe Gertsenhstein Effect
• The conversion of gravitational waves into
electromagnetic waves is a classical process.
Its rate does not involve ℏ
• The process is strictly analogous to axion-
photon conversion. Raffelt, Stodolski’89
• Involving gravity the conversion probabilities
Ringwald, Jan Schütte-Engel, Tamarit 2011.04731
are extremely small. It may be compensated by
a ‘detector’ of cosmological size.
Domcke, CGC 2021
• Distortions of the CMB Dolgov, Ejlli 2012
Pshirkov, Baskaran 2009
Chen 1995
Camilo A. Garcia CelyCosmic magnetic fields and multi-messenger astronomy
Domcke, CGC 2021
10-9
CMB
magnetic field B0 (G)
10-12
10-15
10-18
10-6 10-3 100 103
coherence length 0B (Mpc)
Camilo A. Garcia CelyCosmic magnetic fields and multi-messenger astronomy
Domcke, CGC 2021
10-9
CMB
magnetic field B0 (G)
10-12
10-15
Blazars
10-18
10-6 10-3 100 103
coherence length 0B (Mpc)
Camilo A. Garcia CelySynergy with TeV γ ray observatories
Kronberg , 2016
Cambridge University Press
Camilo A. Garcia CelySynergy with TeV γ ray observatories
Kronberg , 2016
Cambridge University Press
Camilo A. Garcia CelySynergy with TeV γ ray observatories
Kronberg , 2016
Cambridge University Press
Fermi HESS
c as c ade Bound
Primary
(unabsorbed)
spectrum
Camilo A. Garcia CelySynergy with TeV γ ray observatories
Kronberg , 2016
Cambridge University Press
Camilo A. Garcia CelySynergy with TeV γ ray observatories
Kronberg , 2016
Cambridge University Press
CTA consortium 2017
Dermer et al
Camilo A. Garcia CelyCosmic magnetic fields and multi-messenger astronomy
Domcke, CGC 2021
10-9
CMB
magnetic field B0 (G)
10-12
10-15
10-18
10-6 10-3 100 103
coherence length 0B (Mpc)
Camilo A. Garcia CelyCosmic magnetic fields and multi-messenger astronomy
Domcke, CGC 2021
10-9
CMB
magnetic field B0 (G)
10-12
10-15
10-18 Potential solution to the
10-6 10-3 100 103
coherence length 0B (Mpc) Hubble tension
Camilo A. Garcia CelyCosmic magnetic fields and multi-messenger astronomy
Domcke, CGC 2021
Camilo A. Garcia CelyCMB observations and 21-cm cosmology
CMB distortions
dn/dx[cm ]
−3
FIRAS
x = ω/TCMB THE ASTROPHYSICAL JOURNAL, 473 : 576È587, 1996 December 20
( 1996. The American Astronomical Society. All rights reserved. Printed in U.S.A.
THE COSMIC MICROWAVE BACKGROUND SPECTRUM FROM THE FULL COBE1
FIRAS DATA SET
D. J. FIXSEN,2 E. S. CHENG,3 J. M. GALES,2 J. C. MATHER,3 R. A. SHAFER,3 AND E. L. WRIGHT4
Competes with the
Received 1996 January 19 ; accepted 1996 July 11
ABSTRACT
We have reÐned the analysis of the data from the FIRAS (Far-InfraRed Absolute Spectrophotometer)
cosmological const raints on board the COBE (COsmic Background Explorer). The FIRAS measures the di†erence between the
cosmic microwave background and a precise blackbody spectrum. We Ðnd new, tighter upper limits on
general deviations from a blackbody spectrum. The rms deviations are less than 50 parts per million of
the peak of the cosmic microwave background radiation. For the Comptonization and chemical poten-
on radiation energy Neff tial, we Ðnd o y o \ 15 ] 10~6 and o k o \ 9 ] 10~5 (95% conÐdence level [CL]). There are also reÐne-
ments in the absolute temperature, 2.728 ^ 0.004 K (95% CL), the dipole direction, (l, b) \ (264¡.14
^ 0.30, 48¡.26 ^ 0.30) (95% CL), and the amplitude, 3.372 ^ 0.014 mK (95% CL). All of these results
agree with our previous publications.
Subject headings : cosmic microwave background È cosmology : observations
Camilo A. Garcia CelyRayleigh-Jeans Tail
dn/dx[cm ]
−3
FIRAS
E 2
CAD
A R
x = ω/TCMB
• Largely unexplored with upcoming
advances in radio astronomy probing
it in the near future.
Camilo A. Garcia CelyRayleigh-Jeans Tail
dn/dx[cm ]
−3
FIRAS
E 2
CAD
A R
x = ω/TCMB
• Largely unexplored with upcoming
advances in radio astronomy probing
it in the near future.
• Puzzling signal by EDGES.
(Experiment to Detect the Global
Epoch of Reionization Signature) Camilo A. Garcia CelyExpectations for a 21 cm signal
Valdes et al 2013
Camilo A. Garcia CelyExpectations for a 21 cm signal
on a Valdes et al 2013
hat
Temperature, T (K)
5,000
an
3,000
of
1,000
gan
50 60 70 80 90 100
the b c
th-
Temperature, T (K)
0.2 r.m.s. = 0.087 K r.m.s. = 0.025 K
ess
ver 0
Hz
–0.2
ver
50 60 70 80 90 100 50 60 70 80 90 100
ffi-
d e
nts
Temperature, T (K)
nd 0
–0.2
nal
–0.4
ca-
–0.6
50 60 70 80 90 100 50 60 70 80 90 100
um Frequency, Q (MHz) Frequency, Q (MHz)
its.
se, Figure 1 | Summary of detection. a, Measured spectrum for the reference
dataset after filtering for data quality and radio-frequency interference.
out
The spectrum is dominated by Galactic synchrotron emission.
ctic b, c, Residuals after fitting and removing only the foreground
nd model (b) or the foreground and 21-cm models (c). d, Recovered
m, model profile of the 21-cm absorption, with a signal-to-noise
ds) ratio of 37, amplitude of 0.53 K, centre frequency of 78.1 MHz and
K. width of 18.7 MHz. e, Sum of the 21-cm model (d) and its residuals (c).
Camilo A. Garcia CelyExpectations for a 21 cm signal
on a Valdes et al 2013
hat
The absorption feature was
Temperature, T (K)
5,000
an
3,000
gan found to be roughly t wice as
of
1,000
50 60 70 80 90 100
the
strong as previously expected.
b c
th-
Temperature, T (K)
0.2 r.m.s. = 0.087 K r.m.s. = 0.025 K
ess
ver
Hz C o n s e r v a t i v e l y, we m ay
0
–0.2
ver
50 60 70 80 90 100 50 60 70 80 90 100
nts assume that the de v iat ion
ffi-
d e
Temperature, T (K)
nd 0
ca- from the expected value is due
–0.2
nal
–0.4
–0.6
um to foreground contamination,
50 60 70 80
Frequency, Q (MHz)
90 100 50 60 70 80
Frequency, Q (MHz)
90 100
its.
se, Figure 1 | Summary of detection. a, Measured spectrum for the reference
out and place a bound on any
dataset after filtering for data quality and radio-frequency interference.
The spectrum is dominated by Galactic synchrotron emission.
ctic b, c, Residuals after fitting and removing only the foreground
m, stochastic GW background by
nd model (b) or the foreground and 21-cm models (c). d, Recovered
model profile of the 21-cm absorption, with a signal-to-noise
ds) ratio of 37, amplitude of 0.53 K, centre frequency of 78.1 MHz and
K.
using δfγ/fγ ≲ 1 at 78 MHz
width of 18.7 MHz. e, Sum of the 21-cm model (d) and its residuals (c).
Camilo A. Garcia CelyUpper bounds on stochastic gravitational waves
PHYSICAL REVIEW LETTERS 126, 021104 (2021)
Potential of Radio Telescopes as High-Frequency Gravitational Wave Detectors
1,2,3,* 1,†
Valerie Domcke and Camilo Garcia-Cely
1
Deutsches Elektronen-Synchrotron DESY, Notkestrasse 85, 22607 Hamburg, Germany
Camilo A. Garcia CelyOutlook and Future Prospects
this talk
Camilo A. Garcia CelyOutlook and Future Prospects
this talk Modifications of the idea
Camilo A. Garcia CelyOutlook and Future Prospects
this talk Modifications of the idea
Camilo A. Garcia CelyConclusions
• The Gertsenshtein effect during the dark ages provides a powerful way to probe
gravitational waves in the MHz-GHz range from distortions of the Rayleigh-
Jeans CMB tail.
• With upcoming advances in 21cm astronomy targeting precisely this frequency
range with increasing accuracy, it becomes conceivable to push the limits
derived from radio telescopes below the cosmological bound constraining the
total energy in gravitational waves.
• This highlights the interesting prospects associated with multi-messenger
astronomy.
Camilo A. Garcia CelyYou can also read
