Coincidence analysis between periodic source candidates in C6 and C7 Virgo data

Acernese, F.; Amico, P.; Alshourbagy, M.; Antonucci, F.; Aoudia, S.; Astone, P.; Avino, S.; Babusci, D.; Ballardin, G.; Barone, F.; Barsotti, L.; Barsuglia, M.; Bauer, Th.; Beauville, F.; Bigotta, S.; Birindelli, S.; Bizouard, M. A.; Boccara, Claude; Bondu, F.; Bosi, L.; Bradaschia, C.; Braccini, S.; Brand, J. van den; Brillet, A.; Brisson, V.; Buskulic, D.; Calloni, E.; Campagna, E.; Carbognani, F.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cesarini, E.; Chassande–Mottin, E.; Christensen, N.; Corda, Christian; Corsi, A.; Cottone, F.; Clapson, A. C.; Cleva, F.; Coulon, J.‐P.; Cuoco, E.; Dari, A.; Dattilo, V.; Davier, M.; Prete, M. Del; Rosa, R. De; Fiore, L. Di; Virgilio, A. Di; Dujardin, B.; Eleuteri, A.; Evans, M.; Ferrante, I.; Fidecaro, F.; Fiori, I.; Flaminio, R.; Fournier, J.-D.; Frasca, S.; Frasconi, F.; Gammaitoni, L.; Garufi, F.; Genin, É.; Gennai, A.; Giazotto, A.; Giordano, G.; Giordano, L.; Gouaty, R.; Grosjean, Daniel; Guidi, G. M.; Hamdani, S.; Hebri, S.; Heitmann, H.; Hello, P.; Huet, D.; Karkar, S.; Kreckelbergh, S.; Penna, P. La; Laval, M.; Leroy, N.; Letendre, N.; López, B.; Loriette, V.; Losurdo, G.; Mackowski, J.‐M.; Majorana, E.; Man, C. N.; Mantovani, M.; Marchesoni, F.; Marion, F.; Marque, J.; Martelli, F.; Masserot, A.; Mazzoni, M.; Milano, L.; Menzinger, F.; Moins, C.; Moreau, Julien; Morgado, N.; Mours, B.; Nocera, F.; Palomba, C.; Paoletti, F.; Pardi, S.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Piergiovanni, F.; Pinard, L.; Poggiani, R.; Punturo, M.; Puppo, P.; Putten, S. van der; Qipiani, K.; Rapagnani, P.; Reita, V.; Remillieux, A.; Ricci, F.; Ricciardi, I.; Ruggi, P.; Russo, G.; Solimeno, S.; Spallicci, A.; Tarallo, M.; Tonelli, M.; Toncelli, A.; Tournefier, E.; Travasso, F.; Tremola, C.; Vajente, G.; Verkindt, D.; Vetrano, F.; Viceré, A.; Vinet, J.-Y.; Vocca, H.; Yvert, M.

doi:10.1088/0264-9381/24/19/s12

Cited by 13 publications

(11 citation statements)

References 10 publications

(12 reference statements)

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“…Ref. [394]) observatories. In order to generate GWs over an extended time period, a neutron star must have some kind of a long-living axial asymmetry, e.g., a "mountain" on its surface [395].…”

Section: Symmetry Energy Effects On the Ellipticity And Gw Emissions mentioning

confidence: 99%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry Esym(ρ) is the most uncertain part of the EOS of neutron-rich nucleonic matter especially at supra-saturation densities. Much progresses have been made in recent years in predicting the symmetry energy and understanding why it is still very uncertain using various microscopic nuclear many-body theories and phenomenological models. Simultaneously, significant progresses have also been made in probing the symmetry energy in both terrestrial nuclear laboratories and astrophysical observatories. In light of the GW170817 event as well as ongoing or planned nuclear experiments and astrophysical observations probing the EOS of dense neutron-rich matter, we review recent progresses and identify new challenges to the best knowledge we have on several selected topics critical for understanding astrophysical effects of the nuclear symmetry energy.PACS. 2 6.60.Kp Contents B.A Li, P.G. Krastev, D.H. Wen and N.B. Zhang: Astrophysical Effects of Nuclear Symmetry Energy 5.2.2 Predicted correlation strength between the radii of neutron stars and the symmetry energy from low to high densities 32 5.2.3 Predicted effects of the symmetry energy on the tidal deformability of neutron stars 33 5.3 Post-GW170817 analyses of tidal deformability and radii of neutron stars as well as constraints on the nuclear EOS and symmetry energy . . . 34 5.3.

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Section: Symmetry Energy Effects On the Ellipticity And Gw Emissions mentioning

confidence: 99%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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“…The need for coincidences among candidates obtained in different subsets of data (two in the scheme of Fig. 1) has been discussed in references [6,7,8]. This method is very efficient to reduce the number of spurious candidates at a fixed threshold.…”

Section: Scheme Of the Hierarchical Proceduresmentioning

confidence: 99%

“…Candidate parameters are defined by source frequency, celestial coordinates and first spin-down parameter. The need for coincidences among candidates obtained in different subsets of data (two in the scheme of figure 1) has been discussed in [6][7][8]. This method is very efficient to reduce the number of spurious candidates at a fixed threshold.…”

Section: The Scheme Of the Hierarchical Proceduresmentioning

confidence: 99%

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Detection of periodic gravitational wave sources by Hough transform in the f versus \skew6\dot f plane

Antonucci

Astone

D’Antonio³

et al. 2008

Class. Quantum Grav.

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In the hierarchical search for periodic sources of gravitational waves, the candidate selection, in the incoherent step, can be performed with Hough transform procedures. In this paper we analyze the problem of sensitivity loss due to discretization of the parameters space vs computing cost, comparing the properties of the sky Hough procedure with those of a new frequency Hough, which is based on a transformation from the time -observed frequency plane to the source frequency -spin down plane. Results on simulated peakmaps suggest various advantages in favor of the use of the frequency Hough. The ones which show up to really make the difference are 1) the possibility to enhance the frequency resolution without relevantly affecting the computing cost. This reduces the digitization effects; 2) the excess of candidates due to local disturbances in some places of the sky map. They do not affect the new analysis because each map is constructed for only one position in the sky. Pacs. numbers: 04.80Nn,07.05Kf,97.60Jd

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“…Ref. [10]) laser interferometric observatories. According to General Relativity, a perfectly symmetric rotating object self-bound by gravity does not generate GWs.…”

Section: Introductionmentioning

confidence: 99%

Nuclear limits on gravitational waves from elliptically deformed pulsars

Krastev

Worley

2008

Physics Letters B

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Gravitational radiation is a fundamental prediction of General Relativity. Elliptically deformed pulsars are among the possible sources emitting gravitational waves (GWs) with a strain-amplitude dependent upon the star's quadrupole moment, rotational frequency, and distance from the detector. We show that the gravitational wave strain amplitude $h_0$ depends strongly on the equation of state of neutron-rich stellar matter. Applying an equation of state with symmetry energy constrained by recent nuclear laboratory data, we set an upper limit on the strain-amplitude of GWs produced by elliptically deformed pulsars. Depending on details of the EOS, for several millisecond pulsars at distances $0.18kpc$ to $0.35kpc$ from Earth, the {\it maximal} $h_0$ is found to be in the range of $\sim[0.4-1.5]\times 10^{-24}$. This prediction serves as the first {\it direct} nuclear constraint on the gravitational radiation. Its implications are discussed.Comment: 13 pages, 5 figures, and 2 Table. Accepted for publication in Physics Letters

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Coincidence analysis between periodic source candidates in C6 and C7 Virgo data

Cited by 13 publications

References 10 publications

Towards understanding astrophysical effects of nuclear symmetry energy

Towards understanding astrophysical effects of nuclear symmetry energy

Detection of periodic gravitational wave sources by Hough transform in the f versus \skew6\dot f plane

Nuclear limits on gravitational waves from elliptically deformed pulsars

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