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Start Over Author "Barton MA" Publisher escholarship, university of california
5 results on '"Barton MA"'

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

Author

Abbott, R, Abbott, TD, Acernese, F, Ackley, K, Adams, C, Adhikari, N, Adhikari, RX, Adya, VB, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Albanesi, S, Allocca, A, Altin, PA, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, SB, Anderson, WG, Andrade, T, Andres, N, Andrić, T, Angelova, SV, Ansoldi, S, Antelis, JM, Antier, S, Appert, S, Arai, K, Araya, MC, Areeda, JS, Arène, M, Arnaud, N, Aronson, SM, Arun, KG, Asali, Y, Ashton, G, Assiduo, M, Aston, SM, Astone, P, Aubin, F, Austin, C, Babak, S, Badaracco, F, Bader, MKM, Badger, C, Bae, S, Baer, AM, Bagnasco, S, Bai, Y, Baird, J, Ball, M, Ballardin, G, Ballmer, SW, Balsamo, A, Baltus, G, Banagiri, S, Bankar, D, Barayoga, JC, Barbieri, C, Barish, BC, Barker, D, Barneo, P, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, MA, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, JC, Baylor, AC, Bazzan, M, Bécsy, B, Bedakihale, VM, Bejger, M, Belahcene, I, Benedetto, V, Beniwal, D, Bennett, TF, Bentley, JD, BenYaala, M, Bergamin, F, Berger, BK, Bernuzzi, S, Berry, CPL, Bersanetti, D, Bertolini, A, Betzwieser, J, and Beveridge, D

Subjects
LIGO Scientific Collaboration and Virgo Collaboration, Mathematical Sciences, Physical Sciences, Engineering, General Physics
Abstract

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_{⊙}

Published
2022

2. Diving below the Spin-down Limit: Constraints on Gravitational Waves from the Energetic Young Pulsar PSR J0537-6910

Author

Abbott, R, Abbott, TD, Abraham, S, Acernese, F, Ackley, K, Adams, A, Adams, C, Adhikari, RX, Adya, VB, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Aleman, KM, Allen, G, Allocca, A, Altin, PA, Amato, A, Anand, S, Ananyeva, A, Anderson, SB, Anderson, WG, Ando, M, Angelova, SV, Ansoldi, S, Antelis, JM, Antier, S, Appert, S, Arai, Koya, Arai, Koji, Arai, Y, Araki, S, Araya, A, Araya, MC, Areeda, JS, Arène, M, Aritomi, N, Arnaud, N, Aronson, SM, Arun, KG, Asada, H, Asali, Y, Ashton, G, Aso, Y, Aston, SM, Astone, P, Aubin, F, Aufmuth, P, AultONeal, K, Austin, C, Babak, S, Badaracco, F, Bader, MKM, Bae, S, Bae, Y, Baer, AM, Bagnasco, S, Bai, Y, Baiotti, L, Baird, J, Bajpai, R, Ball, M, Ballardin, G, Ballmer, SW, Bals, M, Balsamo, A, Baltus, G, Banagiri, S, Bankar, D, Bankar, RS, Barayoga, JC, Barbieri, C, Barish, BC, Barker, D, Barneo, P, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, MA, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, JC, Baylor, AC, Bazzan, M, Bécsy, B, Bedakihale, VM, Bejger, M, and Belahcene, I

Subjects
Astronomical Sciences, Physical Sciences, Gravitational waves, astro-ph.HE, gr-qc, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Space sciences
Abstract

We present a search for quasi-monochromatic gravitational-wave signals from the young, energetic X-ray pulsar PSR J0537-6910 using data from the second and third observing runs of LIGO and Virgo. The search is enabled by a contemporaneous timing ephemeris obtained using Neutron star Interior Composition Explorer (NICER) data. The NICER ephemeris has also been extended through 2020 October and includes three new glitches. PSR J0537-6910 has the largest spin-down luminosity of any pulsar and exhibits fRequent and strong glitches. Analyses of its long-term and interglitch braking indices provide intriguing evidence that its spin-down energy budget may include gravitational-wave emission from a time-varying mass quadrupole moment. Its 62 Hz rotation frequency also puts its possible gravitational-wave emission in the most sensitive band of the LIGO/Virgo detectors. Motivated by these considerations, we search for gravitational-wave emission at both once and twice the rotation frequency from PSR J0537-6910. We find no signal, however, and report upper limits. Assuming a rigidly rotating triaxial star, our constraints reach below the gravitational-wave spin-down limit for this star for the first time by more than a factor of 2 and limit gravitational waves from the l = m = 2 mode to account for less than 14% of the spin-down energy budget. The fiducial equatorial ellipticity is constrained to less than about 3 ×10-5, which is the third best constraint for any young pulsar.

Published
2021

3. Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

Author

Abbott, BP, Abbott, R, Abbott, TD, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adya, VB, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Allen, G, Allocca, A, Aloy, MA, Altin, PA, Amato, A, Ananyeva, A, Anderson, SB, Anderson, WG, Ando, M, Angelova, SV, Antier, S, Appert, S, Arai, K, Arai, Koya, Arai, Y, Araki, S, Araya, A, Araya, MC, Areeda, JS, Arène, M, Aritomi, N, Arnaud, N, Arun, KG, Ascenzi, S, Ashton, G, Aso, Y, Aston, SM, Astone, P, Aubin, F, Aufmuth, P, AultONeal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, MKM, Bae, SW, Bae, YB, Baiotti, L, Bajpai, R, Baker, PT, Baldaccini, F, Ballardin, G, Ballmer, SW, Banagiri, S, Barayoga, JC, Barclay, SE, Barish, BC, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, MA, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, JC, Bazzan, M, Bécsy, B, Bejger, M, Belahcene, I, Bell, AS, Beniwal, D, Berger, BK, Bergmann, G, Bernuzzi, S, Bero, JJ, Berry, CPL, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, IA, and Bilgili, SA

Subjects
Gravitational waves, Gravitational-wave detectors, Electromagnetic counterparts, Data analysis, KAGRA Collaboration, LIGO Scientific Collaboration and Virgo Collaboration, Astronomical and Space Sciences, Nuclear & Particles Physics
Abstract

We present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is binary neutron star, neutron star-black hole, and binary black hole systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. During O3, the median localization volume (90% credible region) is expected to be on the order of 105,106,107Mpc3 for binary neutron star, neutron star-black hole, and binary black hole systems, respectively. The localization volume in O4 is expected to be about a factor two smaller than in O3. We predict a detection count of 1-1+12 ( 10-10+52 ) for binary neutron star mergers, of 0-0+19 ( 1-1+91 ) for neutron star-black hole mergers, and 17-11+22 ( 79-44+89 ) for binary black hole mergers in a one-calendar-year observing run of the HLV network during O3 (HLVK network during O4). We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers.

Published
2020

4. FIRST SEARCHES FOR OPTICAL COUNTERPARTS TO GRAVITATIONAL-WAVE CANDIDATE EVENTS

Author

Aasi, J, Abadie, J, Abbott, BP, Abbott, R, Abbott, T, Abernathy, MR, Accadia, T, Acernese, F, Adams, C, Adams, T, Adhikari, RX, Affeldt, C, Agathos, M, Aggarwal, N, Aguiar, OD, Ajith, P, Allen, B, Allocca, A, Ceron, E Amador, Amariutei, D, Anderson, RA, Anderson, SB, Anderson, WG, Arai, K, Araya, MC, Arceneaux, C, Areeda, J, Ast, S, Aston, SM, Astone, P, Aufmuth, P, Aulbert, C, Austin, L, Aylott, BE, Babak, S, Baker, PT, Ballardin, G, Ballmer, SW, Barayoga, JC, Barker, D, Barnum, SH, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barton, MA, Bartos, I, Bassiri, R, Basti, A, Batch, J, Bauchrowitz, J, Bauer, Th S, Bebronne, M, Behnke, B, Bejger, M, Beker, MG, Bell, AS, Bell, C, Belopolski, I, Bergmann, G, Berliner, JM, Bertolini, A, Bessis, D, Betzwieser, J, Beyersdorf, PT, Bhadbhade, T, Bilenko, IA, Billingsley, G, Birch, J, Bitossi, M, Bizouard, MA, Black, E, Blackburn, JK, Blackburn, L, Blair, D, Blom, M, Bock, O, Bodiya, TP, Boer, M, Bogan, C, Bond, C, Bondu, F, Bonelli, L, Bonnand, R, Bork, R, Born, M, Bose, S, Bosi, L, Bowers, J, Bradaschia, C, Brady, PR, Braginsky, VB, Branchesi, M, Brannen, CA, Brau, JE, Breyer, J, Briant, T, Bridges, DO, Brillet, A, and Brinkmann, M

Subjects
Astronomical Sciences, Physical Sciences, binaries: close, catalogs, gravitational waves, stars: neutron, surveys, astro-ph.IM, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences
Abstract

During the Laser Interferometer Gravitational-wave Observatory and Virgo joint science runs in 2009-2010, gravitational wave (GW) data from three interferometer detectors were analyzed within minutes to select GW candidate events and infer their apparent sky positions. Target coordinates were transmitted to several telescopes for follow-up observations aimed at the detection of an associated optical transient. Images were obtained for eight such GW candidates. We present the methods used to analyze the image data as well as the transient search results. No optical transient was identified with a convincing association with any of these candidates, and none of the GW triggers showed strong evidence for being astrophysical in nature. We compare the sensitivities of these observations to several model light curves from possible sources of interest, and discuss prospects for future joint GW-optical observations of this type. © 2014. The American Astronomical Society. All rights reserved.

Published
2014

5. First searches for optical counterparts to gravitational-wave candidate events

Author

Constancio, M, Aasi, J, Abadie, J, Abbott, BP, Abbott, R, Abbott, T, Abernathy, MR, Accadia, T, Acernese, F, Adams, C, Adams, T, Adhikari, RX, Affeldt, C, Agathos, M, Aggarwal, N, Aguiar, OD, Ajith, P, Allen, B, Allocca, A, Amador Ceron, E, Amariutei, D, Anderson, RA, Anderson, SB, Anderson, WG, Arai, K, Araya, MC, Arceneaux, C, Areeda, J, Ast, S, Aston, SM, Astone, P, Aufmuth, P, Aulbert, C, Austin, L, Aylott, BE, Babak, S, Baker, PT, Ballardin, G, Ballmer, SW, Barayoga, JC, Barker, D, Barnum, SH, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barton, MA, Bartos, I, Bassiri, R, Basti, A, Batch, J, Bauchrowitz, J, Bauer, TS, Bebronne, M, Behnke, B, Bejger, M, Beker, MG, Bell, AS, Bell, C, Belopolski, I, Bergmann, G, Berliner, JM, Bertolini, A, Bessis, D, Betzwieser, J, Beyersdorf, PT, Bhadbhade, T, Bilenko, IA, Billingsley, G, Birch, J, Bitossi, M, Bizouard, MA, Black, E, Blackburn, JK, Blackburn, L, Blair, D, Blom, M, Bock, O, Bodiya, TP, Boer, M, Bogan, C, Bond, C, Bondu, F, Bonelli, L, Bonnand, R, Bork, R, Born, M, Bose, S, Bosi, L, Bowers, J, Bradaschia, C, Brady, PR, Braginsky, VB, Branchesi, M, Brannen, CA, Brau, JE, Breyer, J, Briant, T, Bridges, DO, and Brillet, A

Subjects
binaries: close, catalogs, gravitational waves, stars: neutron, surveys, astro-ph.IM, astro-ph.HE, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

During the Laser Interferometer Gravitational-wave Observatory and Virgo joint science runs in 2009-2010, gravitational wave (GW) data from three interferometer detectors were analyzed within minutes to select GW candidate events and infer their apparent sky positions. Target coordinates were transmitted to several telescopes for follow-up observations aimed at the detection of an associated optical transient. Images were obtained for eight such GW candidates. We present the methods used to analyze the image data as well as the transient search results. No optical transient was identified with a convincing association with any of these candidates, and none of the GW triggers showed strong evidence for being astrophysical in nature. We compare the sensitivities of these observations to several model light curves from possible sources of interest, and discuss prospects for future joint GW-optical observations of this type. © 2014. The American Astronomical Society. All rights reserved.

Published
2014

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