18 research outputs found

    Search for continuous gravitational wave emission from the Milky Way center in O3 LIGO--Virgo data

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    We present a directed search for continuous gravitational wave (CW) signals emitted by spinning neutron stars located in the inner parsecs of the Galactic Center (GC). Compelling evidence for the presence of a numerous population of neutron stars has been reported in the literature, turning this region into a very interesting place to look for CWs. In this search, data from the full O3 LIGO--Virgo run in the detector frequency band [10,2000] Hz[10,2000]\rm~Hz have been used. No significant detection was found and 95%\% confidence level upper limits on the signal strain amplitude were computed, over the full search band, with the deepest limit of about 7.6×10−267.6\times 10^{-26} at ≃142 Hz\simeq 142\rm~Hz. These results are significantly more constraining than those reported in previous searches. We use these limits to put constraints on the fiducial neutron star ellipticity and r-mode amplitude. These limits can be also translated into constraints in the black hole mass -- boson mass plane for a hypothetical population of boson clouds around spinning black holes located in the GC.Comment: 25 pages, 5 figure

    Search for subsolar-mass binaries in the first half of Advanced LIGO's and Advanced Virgo's third observing run

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    We report on a search for compact binary coalescences where at least one binary component has a mass between 0.2 M⊙ and 1.0 M⊙ in Advanced LIGO and Advanced Virgo data collected between 1 April 2019 1500 UTC and 1 October 2019 1500 UTC. We extend our previous analyses in two main ways: we include data from the Virgo detector and we allow for more unequal mass systems, with mass ratio q ≄ 0.1. We do not report any gravitational-wave candidates. The most significant trigger has a false alarm rate of 0.14 yr-1. This implies an upper limit on the merger rate of subsolar binaries in the range [220-24200] Gpc-3 yr-1, depending on the chirp mass of the binary. We use this upper limit to derive astrophysical constraints on two phenomenological models that could produce subsolar-mass compact objects. One is an isotropic distribution of equal-mass primordial black holes. Using this model, we find that the fraction of dark matter in primordial black holes in the mass range 0.2 M &lt; mPBH &lt; 1.0 M⊙ is fPBH ≡ ΩPBH/ΩDM ≀ 6%. This improves existing constraints on primordial black hole abundance by a factor of ∌3. The other is a dissipative dark matter model, in which fermionic dark matter can collapse and form black holes. The upper limit on the fraction of dark matter black holes depends on the minimum mass of the black holes that can be formed: the most constraining result is obtained at Mmin = 1 M⊙, where fDBH ≡ ΩDBH/ΩDM ≀ 0.003%. These are the first constraints placed on dissipative dark models by subsolar-mass analyses.<br/

    Search for subsolar-mass binaries in the first half of Advanced LIGO’s and Advanced Virgo’s third observing run

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    We report on a search for compact binary coalescences where at least one binary component has a mass between 0.2 M_\odot and 1.0 M_\odot in Advanced LIGO and Advanced Virgo data collected between 1 April 2019 1500 UTC and 1 October 2019 1500 UTC. We extend previous analyses in two main ways: we include data from the Virgo detector and we allow for more unequal mass systems, with mass ratio q \geq 0.1. We do not report any gravitational-wave candidates. The most significant trigger has a false alarm rate of 0.14 \mathrm{yr}^-1. This implies an upper limit on the merger rate of subsolar binaries in the range [220–24200] \mathrm{Gpc}^{-3} \, \mathrm{yr}^{-1}, depending on the chirp mass of the binary. We use this upper limit to derive astrophysical constraints on two phenomenological models that could produce subsolar-mass compact objects. One is an isotropic distribution of equal-mass primordial black holes. Using this model, we find that the fraction of dark matter in primordial black holes is f_\mathrm{PBH}\equiv \Omega_\mathrm{PBH}/\Omega_\mathrm{DM}\lesssim 6\%. The other is a dissipative dark matter model, in which fermionic dark matter can collapse and form black holes. The upper limit on the fraction of dark matter black holes depends on the minimum mass of the black holes that can be formed: the most constraining result is obtained at M_\mathrm{min}=1 M_\odot, where f_\mathrm{DBH}\equiv \Omega_\mathrm{PBH}/\Omega_\mathrm{DM}\lesssim 0.003\%. These are the tightest limits on spinning subsolar-mass binaries to date

    Search for gravitational waves from Scorpius X-1 with a hidden Markov model in O3 LIGO data

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    Results are presented for a semi-coherent search for continuous gravitational waves from the low-mass X-ray binary Scorpius X-1, using a hidden Markov model (HMM) to allow for spin wandering. This search improves on previous HMM-based searches of Laser Interferometer Gravitational-wave Observatory (LIGO) data by including the orbital period in the search template grid, and by analyzing data from the latest (third) observing run (O3). In the frequency range searched, from 60 to 500 Hz, we find no evidence of gravitational radiation. This is the most sensitive search for Scorpius X-1 using a HMM to date. For the most sensitive sub-band, starting at 256.06256.06Hz, we report an upper limit on gravitational wave strain (at 95%95 \% confidence) of h095%=6.16×10−26h_{0}^{95\%}=6.16\times10^{-26}, assuming the orbital inclination angle takes its electromagnetically restricted value Îč=44∘\iota=44^{\circ}. The upper limits on gravitational wave strain reported here are on average a factor of ∌3\sim 3 lower than in the O2 HMM search. This is the first Scorpius X-1 HMM search with upper limits that reach below the indirect torque-balance limit for certain sub-bands, assuming Îč=44∘\iota=44^{\circ}.Comment: 23 pages, 5 figure

    All-sky, all-frequency directional search for persistent gravitational waves from Advanced LIGO&apos;s and Advanced Virgo&apos;s first three observing runs

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    We present the first results from an all-sky all-frequency (ASAF) search for an anisotropic stochastic gravitational-wave background using the data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. Upper limit maps on broadband anisotropies of a persistent stochastic background were published for all observing runs of the LIGO-Virgo detectors. However, a broadband analysis is likely to miss narrowband signals as the signal-to-noise ratio of a narrowband signal can be significantly reduced when combined with detector output from other frequencies. Data folding and the computationally efficient analysis pipeline, PyStoch, enable us to perform the radiometer map-making at every frequency bin. We perform the search at 3072 HEALPix equal area pixels uniformly tiling the sky and in every frequency bin of width 1/32 Hz in the range 20-1726 Hz, except for bins that are likely to contain instrumental artefacts and hence are notched. We do not find any statistically significant evidence for the existence of narrowband gravitational-wave signals in the analyzed frequency bins. Therefore, we place 95% confidence upper limits on the gravitational-wave strain for each pixel-frequency pair, the limits are in the range (0.030-9.6) x 10(-24). In addition, we outline a method to identify candidate pixelfrequency pairs that could be followed up by a more sensitive (and potentially computationally expensive) search, e.g., a matched-filtering-based analysis, to look for fainter nearly monochromatic coherent signals. The ASAF analysis is inherently independent of models describing any spectral or spatial distribution of power. We demonstrate that the ASAF results can be appropriately combined over frequencies and sky directions to successfully recover the broadband directional and isotropic results.Y

    All-sky, all-frequency directional search for persistent gravitational waves from Advanced LIGO's and Advanced Virgo's first three observing runs

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    Search for Subsolar-Mass Binaries in the First Half of Advanced LIGO's and Advanced Virgo's Third Observing Run

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    Search for continuous gravitational wave emission from the Milky Way center in O3 LIGO-Virgo data

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    Search for Subsolar-Mass Binaries in the First Half of Advanced LIGO&apos;s and Advanced Virgo&apos;s Third Observing Run

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    We report on a search for compact binary coalescences where at least one binary component has a mass between 0.2 M-circle dot and 1.0 M-circle dot in Advanced LIGO and Advanced Virgo data collected between 1 April 2019 1500 UTC and 1 October 2019 1500 UTC. We extend our previous analyses in two main ways: we include data from the Virgo detector and we allow for more unequal mass systems, with mass ratio q &gt;= 0.1. We do not report any gravitational-wave candidates. The most significant trigger has a false alarm rate of 0.14 yr(-1). This implies an upper limit on the merger rate of subsolar binaries in the range [220 - 24200] Gpc(-3) yr(-1), depending on the chirp mass of the binary. We use this upper limit to derive astrophysical constraints on two phenomenological models that could produce subsolar-mass compact objects. One is an isotropic distribution of equal-mass primordial black holes. Using this model, we find that the fraction of dark matter in primordial black holes in the mass range 0.2 M-circle dot &lt; m(PBH) &lt; 1.0 M-circle dot is f(PBH) equivalent to Omega(PBH)/Omega(DM) less than or similar to 6%. This improves existing constraints on primordial black hole abundance by a factor of similar to 3. The other is a dissipative dark matter model, in which fermionic dark matter can collapse and form black holes. The upper limit on the fraction of dark matter black holes depends on the minimum mass of the black holes that can be formed: the most constraining result is obtained at M-min = 1 M-circle dot, where f(DBH) equivalent to Omega(DBH)/Omega(DM) less than or similar to 0.003%. These are the first constraints placed on dissipative dark models by subsolar-mass analyses.Y

    All-sky, all-frequency directional search for persistent gravitational waves from Advanced LIGO's and Advanced Virgo's first three observing runs

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    International audienceWe present the first results from an all-sky all-frequency (ASAF) search for an anisotropic stochastic gravitational-wave background using the data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. Upper limit maps on broadband anisotropies of a persistent stochastic background were published for all observing runs of the LIGO-Virgo detectors. However, a broadband analysis is likely to miss narrowband signals as the signal-to-noise ratio of a narrowband signal can be significantly reduced when combined with detector output from other frequencies. Data folding and the computationally efficient analysis pipeline, PyStoch, enable us to perform the radiometer map-making at every frequency bin. We perform the search at 3072 HEALPix equal area pixels uniformly tiling the sky and in every frequency bin of width 1 /32 Hz in the range 20-1726 Hz, except for bins that are likely to contain instrumental artefacts and hence are notched. We do not find any statistically significant evidence for the existence of narrowband gravitational-wave signals in the analyzed frequency bins. Therefore, we place 95% confidence upper limits on the gravitational-wave strain for each pixel-frequency pair, the limits are in the range (0.030 -9.6 )×10-24. In addition, we outline a method to identify candidate pixel-frequency pairs that could be followed up by a more sensitive (and potentially computationally expensive) search, e.g., a matched-filtering-based analysis, to look for fainter nearly monochromatic coherent signals. The ASAF analysis is inherently independent of models describing any spectral or spatial distribution of power. We demonstrate that the ASAF results can be appropriately combined over frequencies and sky directions to successfully recover the broadband directional and isotropic results
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