24 research outputs found
Gravitational-Wave Stochastic Background Detection with Resonant-Mass Detectors
- Author
- Publication venue
- 'American Physical Society (APS)'
- Publication date
- 01/01/1996
- Field of study
In this paper we discuss how the standard optimal Wiener filter theory can be
applied, within a linear approximation, to the detection of an isotropic
stochastic gravitational-wave background with two or more detectors. We apply
then the method to the AURIGA-NAUTILUS pair of ultra low temperature bar
detectors, near to operate in coincidence in Italy, obtaining an estimate for
the sensitivity to the background spectral density of $\simeq 10^{-49}\
Hz^{-1},thatconvertstoanenergydensityperunitlogarithmicfrequencyof\simeq 8\times10^{-5}\times\rho_cwith\rho_c\simeq1.9 \times 10^{-26}\
kg/m^3theclosuredensityoftheUniverse.WealsoshowthatbyaddingtheVIRGOinterferometricdetectorunderconstructioninItalytothearray,andbyproperlyre−orientingthedetectors,onecanreachasensitivityof\simeq 6
\times10^{-5}\times\rho_c.WethencalculatethatthepairformedbyVIRGOandonelargemasssphericaldetectorproperlylocatedinoneofthenearbyavailablesitesinItalycanreahasensitivityof\simeq 2\times10^{-5}\times
\rho_cwhileapairofsuchsphericaldetectorsatthesamesitesofAURIGAandNAUTILUScanachievesensitivitiesof\simeq 2 \times10^{-6}\rho_c$.Comment: 32 pages, postscript file, also available at
http://axln01.lnl.infn.it/reports/stoch.htm
Identification and mitigation of narrow spectral artifacts that degrade searches for persistent gravitational waves in the first two observing runs of Advanced LIGO
- Author
- Publication venue
- 'American Physical Society (APS)'
- Publication date
- 01/01/2018
- Field of study
Searches are under way in Advanced LIGO and Virgo data for persistent gravitational waves from continuous sources, e.g. rapidly rotating galactic neutron stars, and stochastic sources, e.g. relic gravitational waves from the Big Bang or superposition of distant astrophysical events such as mergers of black holes or neutron stars. These searches can be degraded by the presence of narrow spectral artifacts (lines) due to instrumental or environmental disturbances. We describe a variety of methods used for finding, identifying and mitigating these artifacts, illustrated with particular examples. Results are provided in the form of lists of line artifacts that can safely be treated as non-astrophysical. Such lists are used to improve the efficiencies and sensitivities of continuous and stochastic gravitational wave searches by allowing vetoes of false outliers and permitting data cleaning.P.B. Covas … H. Cao … W. Kim … E.J. King … J. Munch … D.J. Ottaway … P.J. Veitch … et al. (LSC Instrument Authors
Erratum: All-sky search for gravitational-wave bursts in the first joint LIGO-GEO-Virgo run (Physical Review D - Particles, Fields, Gravitation and Cosmology - 2010: 81(10) 102001-1-102001-20)
- Author
- Publication venue
- 'American Physical Society (APS)'
- Publication date
- 01/01/2012
- Field of study
This paper was published online on 5 May 2010 with an omission in the Collaboration author list. S. Dwyer has been added as of 12 April 2012. The Collaboration author list is incorrect in the printed version of the journalJ. Abadie... D. J. Hosken... J. Munch... D. J. Ottaway... P. J. Veitch...et al. (LIGO Scientific Collaboration, VIRGO Collaboration
All-sky incoherent search for periodic signals with Explorer 2005 data
- Author
- Publication venue
- IOP PUBLISHING LTD
- Publication date
- Field of study
The data collected during 2005 by the resonant bar Explorer are divided into segments and incoherently summed in order to perform an all-sky search for periodic gravitational wave signals. The parameter space of the search spanned about 40 Hz in frequency, over 23 927 positions in the sky. Neither source orbital corrections nor spindown parameters have been included, with the result that the search was sensitive to isolated neutron stars with a frequency drift less than 6 x 10(-11) Hz s(-1). No gravitational wave candidates have been found by means of the present analysis, which led to a best upper limit of 3.1 x 10(-23) for the dimensionless strain amplitude
Localization and broadband follow-up of the gravitational-wave transient GW150914
- Author
- Abbott B.P.
- Abbott R.
- Abbott T.D.
- Abernathy M.R.
- Acernese F.
- Ackley K.
- Adams C.
- Adams T.
- Addesso P.
- Adhikari R.X.
- Adya V.B.
- Affeldt C.
- Agathos M.
- Agatsuma K.
- Aggarwal N.
- Aguiar O.D.
- Aiello L.
- Ain A.
- Ajith P.
- Allen B.
- Allocca A.
- Altin P.A.
- Anderson S.B.
- Anderson W.G.
- Arai K.
- Araya M.C.
- Arceneaux C.C.
- Areeda J.S.
- Arnaud N.
- Arun K.G.
- Ascenzi S.
- Ashton G.
- Ast M.
- Aston S.M.
- Astone P.
- Aufmuth P.
- Aulbert C.
- Babak S.
- Bacon P.
- Bader M.K.M.
- Baker P.T.
- Baldaccini F.
- Ballardin G.
- Ballmer S.W.
- Barayoga J.C.
- Barclay S.E.
- Barish B.C.
- Barker D.
- Barone F.
- Barr B.
- Barsotti L.
- et al.
- Harvey-Smith Lisa (R19479)
- Publication venue
- 'American Astronomical Society'
- Publication date
- 01/01/2016
- Field of study
A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline, and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams
Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant
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- Zweizig J
- Publication venue
- 'IOP Publishing'
- Publication date
- 01/01/2020
- Field of study
GW170817 is the very first observation of gravitational waves originating from the coalescence of two compact objects in the mass range of neutron stars, accompanied by electromagnetic counterparts, and offers an opportunity to directly probe the internal structure of neutron stars. We perform Bayesian model selection on a wide range of theoretical predictions for the neutron star equation of state. For the binary neutron star hypothesis, we find that we cannot rule out the majority of theoretical models considered. In addition, the gravitational-wave data alone does not rule out the possibility that one or both objects were low-mass black holes. We discuss the possible outcomes in the case of a binary neutron star merger, finding that all scenarios from prompt collapse to long-lived or even stable remnants are possible. For long-lived remnants, we place an upper limit of 1.9 kHz on the rotation rate. If a black hole was formed any time after merger and the coalescing stars were slowly rotating, then the maximum baryonic mass of non-rotating neutron stars is at most 3.05 M-circle dot, and three equations of state considered here can be ruled out. We obtain a tighter limit of 2.67 M-circle dot for the case that the merger results in a hypermassive neutron star
Recommended from our members
Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M <sub>⊙</sub> Compact Object and a Neutron Star
- Author
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- Wysocki DM
- Xu VA
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- Yaala M Ben
- Yadav N
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- Yamamoto T
- Yamamoto TS
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- Yang F
- Yang FW
- Yang KZ
- Yang Y
- Yarbrough Z
- Yasui H
- Yeh S-W
- Yelikar AB
- Yin X
- Yokoyama J
- Yokozawa T
- Yoo J
- Yu H
- Yuan S
- Yuzurihara H
- Zadrożny A
- Zanolin M
- Zeeshan M
- Zelenova T
- Zendri J-P
- Zeoli M
- Zerrad M
- Zevin M
- Zhang AC
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- Zhang R
- Zhang T
- Zhang Y
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- Zhu Z-H
- Zimmerman AB
- Zucker ME
- Zweizig J
- Publication venue
- The Astrophysical Journal Letters
- Publication date
- 26/07/2024
- Field of study
Abstract
We report the observation of a coalescing compact binary with component masses 2.5–4.5 M
⊙ and 1.2–2.0 M
⊙ (all measurements quoted at the 90% credible level). The gravitational-wave signal GW230529_181500 was observed during the fourth observing run of the LIGO–Virgo–KAGRA detector network on 2023 May 29 by the LIGO Livingston observatory. The primary component of the source has a mass less than 5 M
⊙ at 99% credibility. We cannot definitively determine from gravitational-wave data alone whether either component of the source is a neutron star or a black hole. However, given existing estimates of the maximum neutron star mass, we find the most probable interpretation of the source to be the coalescence of a neutron star with a black hole that has a mass between the most massive neutron stars and the least massive black holes observed in the Galaxy. We provisionally estimate a merger rate density of
55
−
47
+
127
Gpc
−
3
yr
−
1
for compact binary coalescences with properties similar to the source of GW230529_181500; assuming that the source is a neutron star–black hole merger, GW230529_181500-like sources may make up the majority of neutron star–black hole coalescences. The discovery of this system implies an increase in the expected rate of neutron star–black hole mergers with electromagnetic counterparts and provides further evidence for compact objects existing within the purported lower mass gap.</jats:p
Search for subsolar-mass black hole binaries in the second part of Advanced LIGO’s and Advanced Virgo’s third observing run
- Author
- Abbott R
- Abe H
- Acernese F
- Ackley K
- Adhicary S
- Adhikari N
- Adhikari RX
- Adkins VK
- Adya VB
- Affeldt C
- Agarwal D
- Agathos M
- Aguiar OD
- Aiello L
- Ain A
- Ajith P
- Akutsu T
- Albanesi S
- Alfaidi RA
- Allocca A
- Alléné C
- Altin PA
- Amato A
- Anand S
- Ananyeva A
- Anderson SB
- Anderson WG
- Ando M
- Andrade T
- Andres N
- Andrić T
- Andrés-Carcasona M
- Ansoldi S
- Antelis JM
- Antier S
- Apostolatos T
- Appavuravther EZ
- Appert S
- Apple SK
- Arai K
- Araya A
- Araya MC
- Areeda JS
- Arellano FEP
- Aritomi N
- Arnaud N
- Arogeti M
- Aronson SM
- Arun KG
- Arène M
- Asada H
- Ashton G
- Aso Y
- Assiduo M
- Aston SM
- Astone P
- Aubin F
- AultONeal K
- Babak S
- Badaracco F
- Badger C
- Bae S
- Bae Y
- Bagnasco S
- Bai Y
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- Publication venue
- 'Oxford University Press (OUP)'
- Publication date
- 28/02/2023
- Field of study
Model-based Cross-correlation Search for Gravitational Waves from the Low-mass X-Ray Binary Scorpius X-1 in LIGO O3 Data
- Author
- Abbott R
- Abe H
- Acernese F
- Ackley K
- Adhicary S
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- Adhikari RX
- Adkins VK
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- Affeldt C
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- Altin PA
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- Ananyeva A
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- Ando M
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- Floden E
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- Frasconi F
- Freed JP
- Frei Z
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- Freitas O
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- Frolov VV
- Fronzo CD
- Fronzé GG
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- Zhu Z-H
- Zimmerman AB
- Zucker ME
- Zweizig J
- Publication venue
- 'American Astronomical Society'
- Publication date
- 01/01/2022
- Field of study
We present the results of a model-based search for continuous gravitational waves from the low-mass X-ray binary Scorpius X-1 using LIGO detector data from the third observing run of Advanced LIGO and Advanced Virgo. This is a semicoherent search that uses details of the signal model to coherently combine data separated by less than a specified coherence time, which can be adjusted to balance sensitivity with computing cost. The search covered a range of gravitational-wave frequencies from 25 to 1600 Hz, as well as ranges in orbital speed, frequency, and phase determined from observational constraints. No significant detection candidates were found, and upper limits were set as a function of frequency. The most stringent limits, between 100 and 200 Hz, correspond to an amplitude h0 of about 10−25 when marginalized isotropically over the unknown inclination angle of the neutron star's rotation axis, or less than 4 × 10−26 assuming the optimal orientation. The sensitivity of this search is now probing amplitudes predicted by models of torque balance equilibrium. For the usual conservative model assuming accretion at the surface of the neutron star, our isotropically marginalized upper limits are close to the predicted amplitude from about 70 to 100 Hz; the limits assuming that the neutron star spin is aligned with the most likely orbital angular momentum are below the conservative torque balance predictions from 40 to 200 Hz. Assuming a broader range of accretion models, our direct limits on gravitational-wave amplitude delve into the relevant parameter space over a wide range of frequencies, to 500 Hz or more
Recommended from our members
Search for Gravitational-lensing Signatures in the Full Third Observing Run of the LIGO–Virgo Network
- Author
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- Vijaykumar A
- Villa-Ortega V
- Vinet J-Y
- Virtuoso A
- Vitale S
- Vocca H
- von Reis ERG
- von Wrangel JSA
- Vorvick C
- Vyatchanin SP
- Wade LE
- Wade M
- Wagner KJ
- Walet RC
- Walker M
- Wallace GS
- Wallace L
- Wang J
- Wang JZ
- Wang WH
- Ward RL
- Warner J
- Was M
- Washimi T
- Washington NY
- Watada K
- Watarai D
- Watchi J
- Wayt KE
- Weaver B
- Weaving CR
- Webster SA
- Weinert M
- Weinstein AJ
- Weiss R
- Weller CM
- Weller RA
- Wellmann F
- Wen L
- Wette K
- Weßels P
- Whelan JT
- White DD
- Whiting BF
- Whittle C
- Wilk OS
- Wilken D
- Williams CE
- Williams D
- Williams MJ
- Williamson AR
- Willis JL
- Willke B
- Wipf CC
- Woan G
- Woehler J
- Wofford JK
- Wojtowicz IA
- Wong D
- Wong ICF
- Wright M
- Wu C
- Wu DS
- Wu H
- Wysocki DM
- Xiao L
- Yadav N
- Yamada T
- Yamamoto H
- Yamamoto K
- Yamamoto T
- Yamashita K
- Yamazaki R
- Yang FW
- Yang KZ
- Yang L
- Yang Y
- Yang Y-C
- Yang Yang
- Yap MJ
- Yeeles DW
- Yeh S-W
- Yelikar AB
- Yokoyama J
- Yokozawa T
- Yoo J
- Yoshioka T
- Yu Hang
- Yu Haocun
- Yuzurihara H
- Zadrożny A
- Zanolin M
- Zeidler S
- Zelenova T
- Zendri J-P
- Zevin M
- Zhan M
- Zhang H
- Zhang J
- Zhang L
- Zhang R
- Zhang T
- Zhang Y
- Zhao C
- Zhao G
- Zhao Y
- Zhao Yue
- Zheng Y
- Zhou R
- Zhu XJ
- Zhu Z-H
- Zimmerman AB
- Zucker ME
- Zweizig J
- Publication venue
- The Astrophysical Journal
- Publication date
- 05/08/2024
- Field of study
Abstract
Gravitational lensing by massive objects along the line of sight to the source causes distortions to gravitational wave (GW) signals; such distortions may reveal information about fundamental physics, cosmology, and astrophysics. In this work, we have extended the search for lensing signatures to all binary black hole events from the third observing run of the LIGO-Virgo network. We search for repeated signals from strong lensing by (1) performing targeted searches for subthreshold signals, (2) calculating the degree of overlap among the intrinsic parameters and sky location of pairs of signals, (3) comparing the similarities of the spectrograms among pairs of signals, and (4) performing dual-signal Bayesian analysis that takes into account selection effects and astrophysical knowledge. We also search for distortions to the gravitational waveform caused by (1) frequency-independent phase shifts in strongly lensed images, and (2) frequency-dependent modulation of the amplitude and phase due to point masses. None of these searches yields significant evidence for lensing. Finally, we use the nondetection of GW lensing to constrain the lensing rate based on the latest merger-rate estimates and the fraction of dark matter composed of compact objects.</jats:p