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1. Enhancing Gravitational Wave Parameter Estimation with Non-Linear Memory: Breaking the Distance-Inclination Degeneracy

Author

Xu, Yumeng, Rosselló-Sastre, Maria, Tiwari, Shubhanshu, Ebersold, Michael, Hamilton, Eleanor Z, García-Quirós, Cecilio, Estellés, Héctor, and Husa, Sascha

Subjects
General Relativity and Quantum Cosmology
Abstract

In this study, we investigate the role of the non-linear memory effect in gravitational wave (GW) parameter estimation, particularly we explore its capability to break the degeneracy between luminosity distance and inclination angle in binary coalescence events. Motivated by the rapid growth in GW detections and the increasing sensitivity of GW observatories enhancing the precision of cosmological and astrophysical measurements is crucial. We propose leveraging the non-linear memory effect -- a subtle, persistent feature in the GW signal resulting from the cumulative impact of emitted gravitational waves -- as a novel approach to enhance parameter estimation accuracy. Through a comprehensive series of injection studies, encompassing both reduced and full parameter spaces, we evaluate the effectiveness of non-linear memory in various scenarios for aligned-spin systems. Our findings demonstrate the significant potential of non-linear memory in resolving the inclination-distance degeneracy, particularly for events with high signal-to-noise ratios (SNR $>$ 90) for the current generation of detectors or closer than 1 Gpc in the context of future detector sensitivities such as the planned LIGO A$^\sharp$ upgrade. The results also suggest that excluding non-linear memory from parameter estimation could introduce significant systematics in future LIGO A$^\sharp$ detections. This observation will hold even greater weight for next-generation detectors, highlighting the importance of including non-linear memory in GW models for achieving high-accuracy measurements for gravitational wave (GW) astronomy., Comment: 10 pages, 9 figures

Published
2024
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2. Leveraging gravitational-wave memory to distinguish neutron star--black hole binaries from black hole binaries

Author

Tiwari, Shubhanshu, Ebersold, Michael, and Hamilton, Eleanor Z.

Subjects
General Relativity and Quantum Cosmology, Astrophysics - High Energy Astrophysical Phenomena
Abstract

In the observation of gravitational waves (GWs) from a compact binary coalescence system where the mass of one of the companions is $\leq 5~M_{\odot}$ the nature of the object is ambiguous until the measurements of tidal effects give evidence for the presence of a neutron star (NS) or a low mass black hole (BH). The relevance of tidal effects in a neutron star--black hole (NSBH) binary system depends crucially upon the mass and the spin of the companion BH. These effects become important predominantly when the binary system is of comparable mass and/or has large aligned spins. Depending upon the masses and spins the NS can even get tidally disrupted before the innermost stable circular orbit (ISCO) is reached. The gravitational-wave signatures of various tidal effects are encoded in the phasing of the signal and in the case of tidal disruption an abrupt cutoff of the signal amplitude occurs. In this work we show that tidal effects can also be captured by the nonlinear memory of the GW signal. Although small in amplitude, nonlinear memory is present at low frequency in contrast to the oscillatory GW signal. We introduce nonlinear memory in the NSBH and binary black hole (BBH) waveform models and show how the addition of memory aids in distinguishing NSBH systems from BBH systems for a larger part of the parameter space. We discuss the recently detected events of interest by LIGO-Virgo and provide the future prospects for the third generation detectors where nonlinear memory can play a crucial role in inferring the nature of the coalescence as BBH or NSBH from its GW signal alone., Comment: Accepted in PRD

Published
2021
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4. Searches for Gravitational Waves from Known Pulsars at Two Harmonics in the Second and Third LIGO-Virgo Observing Runs

Author

Ebersold, Michael, Haney, M, Hamilton, Eleanor Z, Lopez, D, Tiwari, S, Adhikari, R X, Adkins, V K, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Alfaidi, R A, Allocca, A, Altin, P A, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B, Anderson, W G, Ando, M, Andrade, T, et al, and University of Zurich

Subjects
1912 Space and Planetary Science, 530 Physics, 3103 Astronomy and Astrophysics, 10192 Physics Institute
Published
2022
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5. Narrowband Searches for Continuous and Long-duration Transient Gravitational Waves from Known Pulsars in the LIGO-Virgo Third Observing Run

Author

Ebersold, M, Hamilton, Eleanor Z, Haney, M, Lopez, D, Tiwari, S, Adhikari, N, Adhikari, R X, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P A, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B, Anderson, W G, Ando, M, Andrade, T, Andres, N, et al, and University of Zurich

Subjects
1912 Space and Planetary Science, 530 Physics, Space and Planetary Science, 3103 Astronomy and Astrophysics, Astronomy and Astrophysics, 10192 Physics Institute
Published
2022

6. Search of the early O3 LIGO data for continuous gravitational waves from the Cassiopeia A and Vela Jr. supernova remnants

Author

Ebersold, M, Hamilton, Eleanor Z, Haney, M, Lopez, D, Tiwari, S, Adhikari, N, Adhikari, R X, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D, Aiello, L, Ain, A, Ajith, P, Albanesi, S, Allocca, A, Altin, P A, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B, Anderson, W G, Andrade, T, Andres, N, Andrić, T, Angelova, S V, et al, and University of Zurich

Subjects
530 Physics, 10192 Physics Institute, 3106 Nuclear and High Energy Physics
Published
2022

7. Model-based Cross-correlation Search for Gravitational Waves from the Low-mass X-Ray Binary Scorpius X-1 in LIGO O3 Data

Author

Tiwari, S, Lopez, D, Haney, M; https://orcid.org/0000-0002-8648-0767, Ebersold, M, Hamilton, Eleanor Z; https://orcid.org/0000-0003-0098-9114, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M; https://orcid.org/0000-0002-9072-1121, Aguiar, O D; https://orcid.org/0000-0002-2139-4390, Aiello, L; https://orcid.org/0000-0003-2771-8816, Ain, A, Ajith, P; https://orcid.org/0000-0001-7519-2439, Akutsu, T; https://orcid.org/0000-0003-0733-7530, Albanesi, S, Alfaidi, R A, Alléné, C, Allocca, A; https://orcid.org/0000-0002-5288-1351, Amato, A; https://orcid.org/0000-0001-9557-651X, Altin, P A; https://orcid.org/0000-0001-8193-5825, Anand, S, Ananyeva, A, Anderson, S B; https://orcid.org/0000-0003-2219-9383, Anderson, W G; https://orcid.org/0000-0003-0482-5942, Ando, M, Andrade, T, Andres, N; https://orcid.org/0000-0002-5360-943X, et al, Tiwari, S, Lopez, D, Haney, M; https://orcid.org/0000-0002-8648-0767, Ebersold, M, Hamilton, Eleanor Z; https://orcid.org/0000-0003-0098-9114, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M; https://orcid.org/0000-0002-9072-1121, Aguiar, O D; https://orcid.org/0000-0002-2139-4390, Aiello, L; https://orcid.org/0000-0003-2771-8816, Ain, A, Ajith, P; https://orcid.org/0000-0001-7519-2439, Akutsu, T; https://orcid.org/0000-0003-0733-7530, Albanesi, S, Alfaidi, R A, Alléné, C, Allocca, A; https://orcid.org/0000-0002-5288-1351, Amato, A; https://orcid.org/0000-0001-9557-651X, Altin, P A; https://orcid.org/0000-0001-8193-5825, Anand, S, Ananyeva, A, Anderson, S B; https://orcid.org/0000-0003-2219-9383, Anderson, W G; https://orcid.org/0000-0003-0482-5942, Ando, M, Andrade, T, Andres, N; https://orcid.org/0000-0002-5360-943X, and et al

Abstract

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 h $_{0}$ 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.

Published
2022

8. All-sky search for gravitational wave emission from scalar boson clouds around spinning black holes in LIGO O3 data

Author

Ebersold, M, Hamilton, Eleanor Z; https://orcid.org/0000-0003-0098-9114, Haney, Maria; https://orcid.org/0000-0001-7554-3665, Lopez, D, Tiwari, S, Adhikari, R X, Adkins, V K, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D; https://orcid.org/0000-0002-2139-4390, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Alfaidi, R A, Allocca, A, Altin, P A; https://orcid.org/0000-0001-8193-5825, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B; https://orcid.org/0000-0003-2219-9383, Anderson, W G; https://orcid.org/0000-0003-0482-5942, Ando, M, Andrade, T, et al, Ebersold, M, Hamilton, Eleanor Z; https://orcid.org/0000-0003-0098-9114, Haney, Maria; https://orcid.org/0000-0001-7554-3665, Lopez, D, Tiwari, S, Adhikari, R X, Adkins, V K, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D; https://orcid.org/0000-0002-2139-4390, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Alfaidi, R A, Allocca, A, Altin, P A; https://orcid.org/0000-0001-8193-5825, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B; https://orcid.org/0000-0003-2219-9383, Anderson, W G; https://orcid.org/0000-0003-0482-5942, Ando, M, Andrade, T, and et al

Abstract

This paper describes the first all-sky search for long-duration, quasimonochromatic gravitational-wave signals emitted by ultralight scalar boson clouds around spinning black holes using data from the third observing run of Advanced LIGO. We analyze the frequency range from 20 to 610 Hz, over a small frequency derivative range around zero, and use multiple frequency resolutions to be robust towards possible signal frequency wanderings. Outliers from this search are followed up using two different methods, one more suitable for nearly monochromatic signals, and the other more robust towards frequency fluctuations. We do not find any evidence for such signals and set upper limits on the signal strain amplitude, the most stringent being ≈10−25 at around 130 Hz. We interpret these upper limits as both an “exclusion region” in the boson mass/black hole mass plane and the maximum detectable distance for a given boson mass, based on an assumption of the age of the black hole/boson cloud system.

Published
2022

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

Author

Ebersold, M, Hamilton, Eleanor Z; https://orcid.org/0000-0003-0098-9114, Haney, M, Lopez, D, Tiwari, S, Adhikari, N, Adhikari, R X; https://orcid.org/0000-0002-5731-5076, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D; https://orcid.org/0000-0002-2139-4390, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P A; https://orcid.org/0000-0001-8193-5825, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B; https://orcid.org/0000-0003-2219-9383, Anderson, W G; https://orcid.org/0000-0003-0482-5942, Ando, M, Andrade, T, Andres, N, et al, Ebersold, M, Hamilton, Eleanor Z; https://orcid.org/0000-0003-0098-9114, Haney, M, Lopez, D, Tiwari, S, Adhikari, N, Adhikari, R X; https://orcid.org/0000-0002-5731-5076, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D; https://orcid.org/0000-0002-2139-4390, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P A; https://orcid.org/0000-0001-8193-5825, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B; https://orcid.org/0000-0003-2219-9383, Anderson, W G; https://orcid.org/0000-0003-0482-5942, Ando, M, Andrade, T, Andres, N, and et al

Abstract

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)×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.

Published
2022

10. Transient acceleration events in LISA Pathfinder data: Properties and possible physical origin

Author

Jetzer, P, Tiwari, S, Lopez, D, Haney, M, Ebersold, M, Boitier, A, Hamilton, Eleanor Z; https://orcid.org/0000-0003-0098-9114, Xu, Y, Cesarini, A, Chiavegato, V, Cruise, A M, Dal Bosco, D, Danzmann, K, De Deus Silva, M, Diepholz, I, Dixon, G, Dolesi, R, Ferraioli, L, Ferroni, V, Fitzsimons, E D, Freschi, M, Gesa, L, Giardini, D, Gibert, F, Giusteri, R, Grimani, C, Grzymisch, J, Harrison, I, Hartig, M S, Heinzel, G, et al, Jetzer, P, Tiwari, S, Lopez, D, Haney, M, Ebersold, M, Boitier, A, Hamilton, Eleanor Z; https://orcid.org/0000-0003-0098-9114, Xu, Y, Cesarini, A, Chiavegato, V, Cruise, A M, Dal Bosco, D, Danzmann, K, De Deus Silva, M, Diepholz, I, Dixon, G, Dolesi, R, Ferraioli, L, Ferroni, V, Fitzsimons, E D, Freschi, M, Gesa, L, Giardini, D, Gibert, F, Giusteri, R, Grimani, C, Grzymisch, J, Harrison, I, Hartig, M S, Heinzel, G, and et al

Abstract

We present an in depth analysis of the transient events, or glitches, detected at a rate of about one per day in the differential acceleration data of LISA Pathfinder. We show that these glitches fall in two rather distinct categories: fast transients in the interferometric motion readout on one side, and true force transient events on the other. The former are fast and rare in ordinary conditions. The second may last from seconds to hours and constitute the majority of the glitches. We present an analysis of the physical and statistical properties of both categories, including a cross-analysis with other time series like magnetic fields, temperature, and other dynamical variables. Based on these analyses we discuss the possible sources of the force glitches and identify the most likely, among which the outgassing environment surrounding the test-masses stands out. We discuss the impact of these findings on the LISA design and operation, and some risk mitigation measures, including experimental studies that may be conducted on the ground, aimed at clarifying some of the questions left open by our analysis.

Published
2022

11. Constraints on dark photon dark matter using data from LIGO’s and Virgo’s third observing run

Author

Ebersold, M, Hamilton, Eleanor Z, Haney, M, Lopez, D, Tiwari, Shubhanshu, Adhikari, N, Adhikari, R X, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P A, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B, Anderson, W G, Ando, M, Andrade, T, Andres, N, et al, and University of Zurich

Subjects
530 Physics, 10192 Physics Institute, 3106 Nuclear and High Energy Physics
Published
2022

12. Search for continuous gravitational waves from 20 accreting millisecond x-ray pulsars in O3 LIGO data

Author

Ebersold, M, Hamilton, Eleanor Z, Haney, M, Lopez, D, Tiwari, S, Adhikari, N, Adhikari, R X, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D, Aiello, L, Ain, A, Akutsu, T, Albanesi, S, Allocca, A, Altin, P A, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B, Anderson, W G, Ando, M, Andrade, T, Andres, N, Andrić, T, et al, and University of Zurich

Subjects
530 Physics, 10192 Physics Institute, 3106 Nuclear and High Energy Physics
Published
2022
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13. Search for intermediate-mass black hole binaries in the third observing run of Advanced LIGO and Advanced Virgo

Author

Ebersold, M, Hamilton, Eleanor Z, Haney, M, Lopez, D, Tiwari, S, Adhikari, N, Adhikari, R X, Adya, V B, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O D, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P A, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S B, Anderson, W G, Ando, M, Andrade, T, Andres, N, et al, and University of Zurich

Subjects
1912 Space and Planetary Science, 530 Physics, Space and Planetary Science, 3103 Astronomy and Astrophysics, Astronomy and Astrophysics, 10192 Physics Institute
Published
2022
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15. Leveraging gravitational-wave memory to distinguish neutron star-black hole binaries from black hole binaries

Author

Tiwari, Shubhanshu; https://orcid.org/0000-0003-1611-6625, Ebersold, Michael; https://orcid.org/0000-0003-4631-1771, Hamilton, Eleanor Z, Tiwari, Shubhanshu; https://orcid.org/0000-0003-1611-6625, Ebersold, Michael; https://orcid.org/0000-0003-4631-1771, and Hamilton, Eleanor Z

Abstract

In the observation of gravitational waves (GWs) from a compact binary coalescence where the mass of one of the companions is <5 M⊙ the nature of the object is ambiguous until the measurements of tidal effects give evidence for the presence of a neutron star (NS) or a low mass black hole (BH). The relevance of tidal effects in a neutron star-black hole (NSBH) binary system depends crucially upon the mass and the spin of the companion BH. These effects become important predominantly when the binary system is of comparable mass and/or has large aligned spins. Depending upon the masses and spins the NS can even get tidally disrupted before the innermost stable circular orbit (ISCO) is reached. The gravitational-wave signatures of various tidal effects are encoded in the phasing of the signal and in the case of tidal disruption an abrupt cutoff of the signal amplitude occurs. In this work we show that tidal effects can also be captured by the nonlinear memory of the GW signal. Although small in amplitude, nonlinear memory is present at low frequency in contrast to the oscillatory GW signal. We introduce nonlinear memory in the NSBH and binary black hole (BBH) waveform models and show how the addition of memory aids in distinguishing NSBH systems from BBH systems for a larger part of the parameter space. We discuss the recently detected events of interest by LIGO-Virgo and provide the future prospects for the third generation detectors where nonlinear memory can play a crucial role in inferring the nature of the coalescence as BBH or NSBH from its GW signal alone.

Published
2021

16. Full band all-sky search for periodic gravitational waves in the O1 LIGO data

Author

Abbott, Benjamin P., Abbott, Rich, Abbott, Thomas D., Acernese, Fausto, Ackley, Kendall, Adams, Carl, Adams, Thomas, Addesso, Paolo, Adhikari, Rana X., Adya, Vaishali B., Affeldt, Christoph, Afrough, Mohammad, Agarwal, Bhanu, Agathos, Michalis, Agatsuma, Kazuhiro, Aggarwal, Nancy, Aguiar, Odylio D., Aiello, Lorenzo, Ain, Anirban, Allen, Bruce, Allen, Gabrielle, Allocca, Annalisa, Altin, Paul A., Amato, Alex, Ananyeva, Alena, Anderson, Stuart B., Anderson, Warren G., Angelova, Svetoslava V., Antier, Sarah, Appert, Stephen, Arai, Koji, Araya, Melody C., Areeda, Joseph S., Arnaud, Nicolas, Ascenzi, Stefano, Ashton, Gregory, Ast, M., Aston, Stuart M., Astone, Pia, Atallah, Dany V., Aufmuth, Peter, Aulbert, Carsten, AultONeal, K., Austin, Corey, Avila-Alvarez, A., Babak, Stanislav, Bacon, Philippe, Bader, Maria K.M., Bae, Sangwook, Baker, Paul T., Baldaccini, Francesca, Ballardin, Giulio, Ballmer, Stefan W., Banagiri, Sharan, Barayoga, Juan C., Barclay, Sheena E., Barish, Barry C., Barker, David, Barkett, Kevin, Barone, Fabrizio, Barr, Bryan, Barsotti, Lisa, Barsuglia, Matteo, Barta, Daniel, Bartlett, Jeffrey, Bartos, Imre, Bassiri, Riccardo, Basti, Andrea, Batch, James C., Bawaj, Mateusz, Bayley, Joseph C., Bazzan, Marco, Bécsy, Bence, Beer, Christian, Bejger, Michal, Belahcene, Imene, Bell, Angus S., Berger, Beverly K., Bergmann, Gerald, Bero, John J., Berry, Christopher P.L., Bersanetti, Diego, Bertolini, Alessandro, Betzwieser, Joseph, Bhagwat, Swetha, Bhandare, Rohan, Bilenko, Igor A., Billingsley, Garilynn, Billman, Chris R., Birch, Jeremy, Birney, Ross, Birnholtz, Ofek, Biscans, Sebastien, Biscoveanu, Sylvia, Bisht, Aparna, Bitossi, Massimiliano, Biwer, Christopher, Bizouard, Marieanne A., Blackburn, J.K., Blackman, Jonathan, Blair, Carl D., Blair, David G., Blair, Ryan M., Bloemen, Steven, Bock, Oliver, Bode, Nina, Boer, Michel, Bogaert, Gilles, Bohe, Alejandro, Bondu, Francois, Bonilla, Edgard, Bonnand, Romain, Boom, Boris A., Bork, Rolf, Boschi, Valerio, Bose, Sukanta, Bossie, Ken, Bouffanais, Yann, Bozzi, Antonella, Bradaschia, Carlo, Brady, Patrick R., Branchesi, Marica, Brau, Jim E., Briant, Tristan, Brillet, Alain, Brinkmann, Marc, Brisson, Violette, Brockill, Patrick, Broida, Jacob E., Brooks, Aidan F., Brown, Duncan A., Brown, Daniel D., Brunett, Sharon, Buchanan, Christopher C., Buikema, Aaron, Bulik, Tomasz, Bulten, Henk J., Buonanno, Alessandra, Buskulic, Damir, Buy, Christelle, Byer, Robert L., Cabero, Miriam, Cadonati, Laura, Cagnoli, Giampietro, Cahillane, Craig, Calderón Bustillo, J., Callister, Thomas A., Calloni, Enrico, Camp, Jordan B., Canepa, Maurizio, Canizares, Priscilla, Cannon, Kipp C., Cao, H., Cao, Junwei, Capano, Collin D., Capocasa, Eleonora, Carbognani, Franco, Caride, Santiago, Carney, Matthew F., Casanueva Diaz, J., Casentini, Claudio, Caudill, Sarah, Cavaglià, Marco, Cavalier, Fabien, Cavalieri, Roberto, Cella, Giancarlo, Cepeda, Christian B., Cerdá-Durán, P., Cerretani, Giovanni, Cesarini, Elisabetta, Chamberlin, Sydney J., Chan, Manleong, Chao, Shiuh, Charlton, Philip, Chase, Eve, Chassande-Mottin, E., Chatterjee, Deep, Cheeseboro, Belinda D., Chen, H.Y., Chen, Xu, Chen, Yanbei, Cheng, H.-P., Chia, Hanyu Y., Chincarini, Andrea, Chiummo, Antonino, Chmiel, Theresa, Cho, Heesuk S., Cho, M., Chow, Jong H., Christensen, Nelson, Chu, Qi, Chua, Alvin J.K., Chua, Sheon, Chung, A.K.W., Chung, Shinkee, Ciani, Giacomo, Ciecielag, P., Ciolfi, Riccardo, Cirelli, Carissa E., Cirone, Alessio, Clara, Filiberto, Clark, James A., Clearwater, Patrick, Cleva, Frederic, Cocchieri, Camillo, Coccia, Eugenio, Cohadon, P.-F., Cohen, David, Colla, Alberto, Collette, Christophe G., Cominsky, Lynn R., Constancio, M., Conti, Livia, Cooper, Sam J., Corban, Paul, Corbitt, Thomas R., Cordero-Carrión, I., Corley, Kenneth R., Cornish, Neil, Corsi, Alessandra, Cortese, Stefano, Costa, Cesar A., Coughlin, Eric T., Coughlin, Michael W., Coughlin, Scott B., Coulon, J.-P., Countryman, Stefan T., Couvares, Peter, Covas, 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Maria A., Parida, Abhishek, Parker, William, Pascucci, Daniela, Pasqualetti, Antonio, Passaquieti, Roberto, Passuello, Diego, Patil, M., Patricelli, Barbara, Pearlstone, Brynley L., Pedraza, Mike, Pedurand, Richard, Pekowsky, L., Pele, Arnaud, Penn, Steven, Perez, Carlos J., Perreca, Antonio, Perri, Leah M., Pfeiffer, Harald P., Phelps, Margot, Piccinni, Ornella J., Pichot, Mikhael, Piergiovanni, Francesco, Pierro, Vincenzo, Pillant, Gabriel, Pinard, Laurent, Pinto, Innocenzo M., Pirello, Marc, Pisarski, A., Pitkin, Matthew, Poe, Mark, Poggiani, Rosa, Popolizio, Pasquale, Porter, K., Post, Alexander, Powell, Jade, Prasad, Jayanti, Pratt, James W.W., Pratten, Geraint, Predoi, Valeriu, Prestegard, Tanner, Prijatelj, Mirko, Principe, Maria, Privitera, Stephen, Prodi, Giovanni A., Prokhorov, Leonid G., Puncken, Oliver, Punturo, Michele, Puppo, Paola, Pürrer, Michael, Qi, Hong, Quetschke, Volker, Quintero, Eric A., Quitzow-James, R., Raab, Fred J., Rabeling, David S., Radkins, Hugh, Raffai, 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Abstract

We report on a new all-sky search for periodic gravitational waves in the frequency band 475-2000 Hz and with a frequency time derivative in the range of [-1.0,+0.1]×10-8 Hz/s. Potential signals could be produced by a nearby spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the data from Advanced LIGO's first observational run O1. No gravitational-wave signals were observed, and upper limits were placed on their strengths. For completeness, results from the separately published low-frequency search 20-475 Hz are included as well. Our lowest upper limit on worst-case (linearly polarized) strain amplitude h0 is ∼4×10-25 near 170 Hz, while at the high end of our frequency range, we achieve a worst-case upper limit of 1.3×10-24. For a circularly polarized source (most favorable orientation), the smallest upper limit obtained is ∼1.5×10-25. © 2018 American Physical Society.

Published
2018

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