Constraints on dark photon dark matter using data from LIGO’s and Virgo’s third observing run
Name
PhysRevD.105.063030.pdf
Description
Published version
Size
1.08 MB
Format
Adobe PDF
Checksum (MD5)
c055f254fd459b2c9edd0afb6543bd35
Author(s)
Sudhir, Vivishek
Date Issued
March 31, 2022
Journal
Physical Review D
Publisher
American Physical Society
Citation
Sudhir, Vivishek. 2022. "Constraints on dark photon dark matter using data from LIGO’s and Virgo’s third observing run." Physical Review D, 105 (6).
Version
Final published version
Abstract
We present a search for dark photon dark matter that could couple to gravitational-wave interferometers using data from Advanced LIGO and Virgo’s third observing run. To perform this analysis, we use two methods, one based on cross-correlation of the strain channels in the two nearly aligned LIGO detectors, and one that looks for excess power in the strain channels of the LIGO and Virgo detectors. The excess power method optimizes the Fourier transform coherence time as a function of frequency, to account for the expected signal width due to Doppler modulations. We do not find any evidence of dark photon dark matter with a mass between
m
A
∼
10
−
14
–
10
−
11
eV
/
c
2
, which corresponds to frequencies between 10–2000 Hz, and therefore provide upper limits on the square of the minimum coupling of dark photons to baryons, i.e.,
U
(
1
)
B
dark matter. For the cross-correlation method, the best median constraint on the squared coupling is
∼
1.31
×
10
−
47
at
m
A
∼
4.2
×
10
−
13
eV
/
c
2
; for the other analysis, the best constraint is
∼
2.4
×
10
−
47
at
m
A
∼
5.7
×
10
−
13
eV
/
c
2
. These limits improve upon those obtained in direct dark matter detection experiments by a factor of
∼
100
for
m
A
∼
[
2
–
4
]
×
10
−
13
eV
/
c
2
, and are, in absolute terms, the most stringent constraint so far in a large mass range
m
A
∼
2
×
10
−
13
–
8
×
10
−
12
eV
/
c
2
.
MIT Department
LIGO (Observatory : Massachusetts Institute of Technology)
Terms of Use
Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1103/physrevd.105.063030
