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1. High-resolution Radio Study of the Dragonfly Pulsar Wind Nebula Powered by PSR J2021+3651

Author: Ruolan Jin, C.-Y. Ng, Mallory S. E. Roberts, and Kwan-Lok Li
Subjects: Pulsar wind nebulae, Pulsars, Radio interferometry, Polarimetry, Astrophysics, QB460-466
Abstract: The Dragonfly Nebula (G75.2+0.1) powered by the young pulsar J2021+3651 is a rare pulsar wind nebula (PWN) that shows double tori and polar jets enclosed by a bow-shock structure in X-rays. We present new radio observations of this source taken with the Very Large Array at 6 GHz. The radio PWN has an overall size about two times as large as the X-ray counterpart, consisting of a bright main-body region in the southwest, a narrow and fainter bridge region in the northeast, and a dark gap in between. The nebula shows a radio spectrum much softer than that of a typical PWN. This could be resulting from compression by the ram pressure as the system travels mildly supersonically in the interstellar medium. Our polarization maps reveal a highly ordered and complex B -field structure. This can be explained by a toroidal field distorted by the pulsar motion.
Published: 2023
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2. Discovery of a Gamma-Ray Black Widow Pulsar by GPU-accelerated Einstein@Home

Author: Tom Marsh, Roger W. Romani, Fernando Camilo, B. Machenschalk, C. Aulbert, Mallory S. E. Roberts, M. A. Papa, D. Kandel, S. Kwang, Paul S. Ray, Jayanta Roy, H. J. Pletsch, Michael Kramer, Di Li, Elizabeth C. Ferrara, Paulo C. C. Freire, Cees Bassa, Matthew Kerr, Pei Wang, Scott M. Ransom, Banafsheh Beheshtipour, M. B. Mickaliger, L. Nieder, C. J. Clark, S. Sanpa-arsa, Benjamin William Allen, Lucas Guillemot, Rene P. Breton, C. Choquet, Ramesh Karuppusamy, Ewan Barr, Ismaël Cognard, H. Fehrmann, A. Ashok, Bhaswati Bhattacharyya, O. Behnke, V. S. Dhillon, J. Wu, Jason W. T. Hessels, Zhichen Pan, B. Steltner, Ziggy Pleunis, High Energy Astrophys. & Astropart. Phys (API, FNWI), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)
Subjects: Einstein@Home, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, Orbital period, 01 natural sciences, Binary pulsar, Neutron star, Pulsar, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Millisecond pulsar, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Fermi Gamma-ray Space Telescope
Abstract: We report the discovery of 1.97 ms period gamma-ray pulsations from the 75 minute orbital-period binary pulsar now named PSR J1653-0158. The associated Fermi Large Area Telescope gamma-ray source 4FGL J1653.6-0158 has long been expected to harbor a binary millisecond pulsar. Despite the pulsar-like gamma-ray spectrum and candidate optical/X-ray associations -- whose periodic brightness modulations suggested an orbit -- no radio pulsations had been found in many searches. The pulsar was discovered by directly searching the gamma-ray data using the GPU-accelerated Einstein@Home distributed volunteer computing system. The multi-dimensional parameter space was bounded by positional and orbital constraints obtained from the optical counterpart. More sensitive analyses of archival and new radio data using knowledge of the pulsar timing solution yield very stringent upper limits on radio emission. Any radio emission is thus either exceptionally weak, or eclipsed for a large fraction of the time. The pulsar has one of the three lowest inferred surface magnetic-field strengths of any known pulsar with $B_{\rm surf} \approx 4 \times 10^{7}\,$G. The resulting mass function, combined with models of the companion star's optical light curve and spectra, suggests a pulsar mass $\gtrsim 2\,M_{\odot}$. The companion is light-weight with mass $\sim 0.01\,M_{\odot}$, and the orbital period is the shortest known for any rotation-powered binary pulsar. This discovery demonstrates the Fermi Large Area Telescope's potential to discover extreme pulsars that would otherwise remain undetected., Comment: 12 pages, 3 figures, published in ApJL
Published: 2020
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3. The GBT 350-MHz Drift Scan Pulsar Survey: III. Detection of a magnetic field in the eclipsing material of PSR J2256-1024

Author: Kathryn Crowter, Christie A. McPhee, Duncan R. Lorimer, J. Boyles, Mallory S. E. Roberts, Scott M. Ransom, Jason W. T. Hessels, Kevin Stovall, Ryan S. Lynch, Maura McLaughlin, Anne M. Archibald, Ingrid H. Stairs, Joeri van Leeuwen, C. Karako-Argaman, High Energy Astrophys. & Astropart. Phys (API, FNWI), and Faculty of Science
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Linear polarization, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Polarization (waves), 01 natural sciences, Magnetic field, Wavelength, symbols.namesake, Pulsar, Space and Planetary Science, Millisecond pulsar, 0103 physical sciences, Faraday effect, symbols, Potential source, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: We present the first measurement of a non-zero magnetic field in the eclipsing material of a black widow pulsar. Black widows are millisecond pulsars which are ablating their companions; therefore they are often proposed as one potential source of isolated millisecond pulsars. PSR J2256-1024 is an eclipsing black widow discovered at radio wavelengths and later also observed in the X-ray and gamma parts of the spectrum. Here we present the radio timing solution for PSR J2256-1024, polarization profiles at 350, 820, and 1500~MHz and an investigation of changes in the polarization profile due to eclipsing material in the system. In the latter we find evidence of Faraday rotation in the linear polarization shortly after eclipse, measuring a rotation measure of 0.44(6) rad per meter squared and a corresponding line-of-sight magnetic field of 3.5(17) mG., 14 pages, 8 figures
Published: 2020

4. The Green Bank North Celestial Cap Pulsar Survey: V. Pulsar Census and Survey Sensitivity

Author: Scott M. Ransom, Mayuresh Surnis, M. LaRose, M. Mingyar, Harsha Blumer, Xavier Siemens, H. Al Noori, Megan E. DeCesar, Ann Marie Schmiedekamp, Carl Schmiedekamp, David L. Kaplan, P. Chawla, V. I. Kondratiev, Alexander McEwen, Renée Spiewak, G. Y. Agazie, Joseph K. Swiggum, William Fiore, Kevin Stovall, V. M. Kaspi, Mallory S. E. Roberts, Maura McLaughlin, Ryan S. Lynch, Ingrid H. Stairs, J. van Leeuwen, Lina Levin, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Population, Flux, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar, 0103 physical sciences, Sensitivity (control systems), education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Census, Space and Planetary Science, Sky, Survey data collection, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Green Bank North Celestial Cap (GBNCC) pulsar survey will cover the entire northern sky (δ > −40°) at 350 MHz, and is one of the most uniform and sensitive all-sky pulsar surveys to date. We have created a pipeline to reanalyze GBNCC survey data to take a 350 MHz census of all pulsars detected by the survey, regardless of their discovery survey. Of the 1413 pulsars in the survey region, we were able to recover 670. For these we present measured signal-to-noise ratios (S/N), flux densities, pulse widths, profiles, and where appropriate, refined measurements of dispersion measures (DMs) (656 out of 670) and new or improved spectral indices (339 out of 670 total, 47 new, 292 improved). We also measure the period-pulse width relation at 350 MHz to scale as W ∝ P-0.27. Detection scans for several hundred sources were reanalyzed in order to inspect pulsars' single pulse behavior and 223 were found to exhibit evidence of nulling. With a detailed analysis of measured and expected S/N values and the evolving radio frequency interference environment at 350 MHz, we assess the GBNCC survey's sensitivity as a function of spin period, DM, and sky position. We find the sky-averaged limiting flux density of the survey to be 0.74 mJy. Combining this analysis with PsrPopPy pulsar population simulations, we predict 60/5 nonrecycled/MSP discoveries in the survey's remaining 21,000 pointings, and we begin to place constraints on population model parameters.
Published: 2020

5. First Discovery of a Fast Radio Burst at 350 MHz by the GBNCC Survey

Author: William Fiore, Ann Marie Schmiedekamp, Jason W. T. Hessels, Scott M. Ransom, Evan F. Lewis, G. Y. Agazie, Mayuresh Surnis, A. E. McEwen, V. M. Kaspi, Joseph K. Swiggum, P. Chawla, C. Schmiedekamp, Renée Spiewak, Ingrid H. Stairs, David L. Kaplan, Harsha Blumer, Lina Levin, M. LaRose, V. I. Kondratiev, Maura McLaughlin, M. Mingyar, J. van Leeuwen, Mallory S. E. Roberts, E. Parent, Megan E. DeCesar, Emmanuel Fonseca, H. Al Noori, Xavier Siemens, Ryan S. Lynch, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Electron density, Line-of-sight, 010504 meteorology & atmospheric sciences, Fast radio burst, Astrophysics::High Energy Astrophysical Phenomena, Green Bank Telescope, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Comoving distance, 01 natural sciences, Redshift, Galaxy, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We report the first discovery of a fast radio burst (FRB), FRB 20200125A, by the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey conducted with the Green Bank Telescope at 350 MHz. FRB 20200125A was detected at a Galactic latitude of 58.43 degrees with a dispersion measure of 179 pc cm$^{-3}$, while electron density models predict a maximum Galactic contribution of 25 pc cm$^{-3}$ along this line of sight. Moreover, no apparent Galactic foreground sources of ionized gas that could account for the excess DM are visible in multi-wavelength surveys of this region. This argues that the source is extragalactic. The maximum redshift for the host galaxy is $z_{max}=0.17$, corresponding to a maximum comoving distance of approximately 750 Mpc. The measured peak flux density for FRB 20200125A is 0.37 Jy, and we measure a pulse width of 3.7 ms, consistent with the distribution of FRB widths observed at higher frequencies. Based on this detection and assuming an Euclidean flux density distribution of FRBs, we calculate an all-sky rate at 350 MHz of $3.4^{+15.4}_{-3.3} \times 10^3$ FRBs sky$^{-1}$ day$^{-1}$ above a peak flux density of 0.42 Jy for an unscattered pulse having an intrinsic width of 5 ms, consistent with rates reported at higher frequencies. Given the recent improvements in our single-pulse search pipeline, we also revisit the GBNCC survey sensitivity to various burst properties. Finally, we find no evidence of interstellar scattering in FRB 20200125A, adding to the growing evidence that some FRBs have circumburst environments where free-free absorption and scattering are not significant., Comment: 15 pages, 6 figures, Submitted to ApJ
Published: 2020
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6. X-Ray and Optical Properties of Black Widows and Redbacks

Author: Maura McLaughlin, Paul S. Ray, Jason W. T. Hessels, Peter A. Gentile, Rodrigo Torres, Matthew Kerr, Mallory S. E. Roberts, Rene P. Breton, Scott M. Ransom, Hind Al Noori, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, X-ray, Astrophysics::Instrumentation and Methods for Astrophysics, Binary number, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Photometry (optics), Pulsar, Space and Planetary Science, Millisecond pulsar, 0103 physical sciences, Optical emission spectroscopy, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: Black widows and redbacks are binary systems consisting of a millisecond pulsar in a close binary with a companion having matter driven off of its surface by the pulsar wind. X-rays due to an intra-binary shock have been observed from many of these systems, as well as orbital variations in the optical emission from the companion due to heating and tidal distortion. We have been systematically studying these systems in radio, optical and X-rays. Here we will present an overview of X-ray and optical studies of these systems, including new XMM-Newton and NuStar data obtained from several of them, along with new optical photometry., Comment: 4 pages, 1 figure, Proceedings of IAU Symposium 337 "Pulsar Astrophysics - The Next 50 Years" held in Jodrell Bank Observatory, UK Sept. 4-8 2017
Published: 2018
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7. RAAD: a CubeSat-based soft gamma-ray detector for the study of terrestrial gamma-ray flashes and other short timescale phenomena

Author: Laura Manenti, Mallory S. E. Roberts, Valerio Conicella, Prashanth Reddy Marpu, F. Arneodo, Philip K. Panicker, Noora Almarri, Aisha Al Mannaei, Fatema AlKhouri, Ahlam Al Qasim, Heyam Al Blooshi, Rodrigo Torres, Adriano Di Giovanni, Thu Vu, Lolowa Alkindi, Sohmyung Ha, and Giacomo Bruno
Subjects: Physics, Photomultiplier, Physics::Instrumentation and Detectors, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Gamma ray, Photodetector, Radiation, Optics, Silicon photomultiplier, CubeSat, Spectral resolution, business
Abstract: We present RAAD (Rapid Acquisition Atmospheric Detector), a detector designed to study Terrestrial Gamma ray Flashes (TGFs) and other fast hard X-ray and soft gamma-ray phenomena. TGFs are bursts of radiation from thunderstorms which occur on sub-microsecond timescales. Most detectors used to study TGFs have been limited by deadtime and timing precision, and sometimes poor calibration at lower energies. We will present calibration and space qualification tests of a detector aimed at the 20 keV - 2500 keV range with ~ 100 ns time response and good spectral resolution. This uses 2 X 2 arrays of two different scintillation crystals, Cerium Bromide and Lanthanum BromoChloride, both of which have very fast decay times. We couple them to both standard photomultiplier tubes (PMTs) and silicon photomultipliers (SiPMs) along with custom electronics designed to provide very fast sampling with very low power consumption per channel. Each crystal array fits into < 1U of a cubesat, and provides ~20 cm2 of effective area to photons < 200 keV and ~10 cm2 at 600 keV. The RAAD concept is the winner of the Mini-satellite competition held by the UAE Space Agency in 2018, largely developed with undergraduates at NYUAD, and is expected to be fully developed and launched by 2020. Two detectors, one with PMTs and one with SiPMs will be deployed on a 3U CubeSat, providing head to head performance tests for both crystal types and light sensor types. This will serve as a proof of concept showing how such detectors could be deployed in a network of CubeSats to study TGFs and other phenomena.
Published: 2019
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8. Long Term Variability of a Black Widow's Eclipses -- A Decade of PSR J2051$-$0827

Author: Benjamin Stappers, Gemma H. Janssen, Mallory S. E. Roberts, Rene P. Breton, E. J. Polzin, Charlotte Sobey, Stefan Oslowski, and Bhaswati Bhattacharyya
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Line-of-sight, 010308 nuclear & particles physics, Scattering, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Material density, Astrophysics, Polarization (waves), Orbital period, 01 natural sciences, Magnetic field, Pulsar, Space and Planetary Science, 0103 physical sciences, Radio frequency, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: Contains fulltext : 214467.pdf (Publisher’s version ) (Open Access) In this paper we report on $\sim 10$ yr of observations of PSR J2051$-$0827, at radio frequencies in the range 110–4032 MHz. We investigate the eclipse phenomena of this black widow pulsar using model fits of increased dispersion and scattering of the pulsed radio emission as it traverses the eclipse medium. These model fits reveal variability in dispersion features on time-scales as short as the orbital period, and previously unknown trends on time-scales of months–years. No clear patterns are found between the low-frequency eclipse widths, orbital period variations, and trends in the intrabinary material density. Using polarization calibrated observations we present the first available limits on the strength of magnetic fields within the eclipse region of this system; the average line of sight field is constrained to be $10^{-4}$ G $\lesssim B_{||} \lesssim 10^2$ G, while for the case of a field directed near-perpendicular to the line of sight we find $B_{\perp } \lesssim 0.3$ G. Depolarization of the linearly polarized pulses during the eclipse is detected and attributed to rapid rotation measure fluctuations of $\sigma _{\text{RM}} \gtrsim 100$ rad m$^{-2}$ along, or across, the line of sights averaged over during a subintegration. The results are considered in the context of eclipse mechanisms, and we find scattering and/or cyclotron absorption provide the most promising explanation, while dispersion smearing is conclusively ruled out. Finally, we estimate the mass-loss rate from the companion to be $\dot{M}_{\text{C}} \sim 10^{-12}\, \mathrm{M}_\odot$ yr$^{-1}$, suggesting that the companion will not be fully evaporated on any reasonable time-scale
Published: 2019
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9. The Green Bank North Celestial Cap Pulsar Survey

Author: Megan E. DeCesar, M. D. Rohr, Emmanuel Fonseca, R. Roekle, J. G. Martinez, A. N. Walker, Maura McLaughlin, L. Daniels, Bingyi Cui, Renée Spiewak, Scott M. Ransom, J. van Leeuwen, S. Leake, Ryan S. Lynch, Anne M. Archibald, A. Mata, J. Flanigan, V. M. Kaspi, B. L. Wells, Joseph K. Swiggum, H. Al Noori, Kevin Stovall, David L. Kaplan, Ingrid H. Stairs, D. Day, C. Karako-Argaman, A. Cruz, Christopher M. Biwer, N. Meyers, L. P. Dartez, X. Siemens, Jason Boyles, Mallory S. E. Roberts, Jason W. T. Hessels, R. J. Aloisi, J. Hinojosa, A. Schuett, S. Banaszak, V. I. Kondratiev, A. J. Ford, Lina Levin, P. Chawla, G. Lunsford, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Compact star, 01 natural sciences, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Extreme value theory, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Spin-½
Abstract: We present timing solutions for four pulsars discovered in the Green Bank Northern Celestial Cap (GBNCC) survey. All four pulsars are isolated with spin periods between 0.26$\,$s and 1.84$\,$s. PSR J0038$-$2501 has a 0.26$\,$s period and a period derivative of ${7.6} \times {10}^{-19}\,{\rm s\,s}^{-1}$, which is unusually low for isolated pulsars with similar periods. This low period derivative may be simply an extreme value for an isolated pulsar or it could indicate an unusual evolution path for PSR J0038$-$2501, such as a disrupted recycled pulsar (DRP) from a binary system or an orphaned central compact object (CCO). Correcting the observed spin-down rate for the Shklovskii effect suggests that this pulsar may have an unusually low space velocity, which is consistent with expectations for DRPs. There is no X-ray emission detected from PSR J0038$-$2501 in an archival swift observation, which suggests that it is not a young orphaned CCO. The high dispersion measure of PSR J1949+3426 suggests a distance of 12.3$\,$kpc. This distance indicates that PSR J1949+3426 is among the most distant 7% of Galactic field pulsars, and is one of the most luminous pulsars., Comment: 7 pages, 5 figures
Published: 2019

10. Characterisation of a CeBr$_3$(LB) detector for space application

Author: C. Pittori, Laura Manenti, Mallory S. E. Roberts, F. Arneodo, Thu Vu, A. Al Qasim, Prashanth Reddy Marpu, A. AlMannaei, M. L. Benabderrahmane, Lolowa Alkindi, O. Fawwaz, A. Di Giovanni, Giacomo Bruno, Fatema AlKhouri, Valerio Conicella, and Philip K. Panicker
Subjects: Photomultiplier, Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Scintillator, 01 natural sciences, Electromagnetic radiation, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, 0302 clinical medicine, Optics, Physics - Space Physics, 0103 physical sciences, CubeSat, Instrumentation, Mathematical Physics, Physics, Range (particle radiation), 010308 nuclear & particles physics, Payload, business.industry, Detector, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), Space Physics (physics.space-ph), business
Abstract: We describe the performance of a $\mathrm{23\times 23\times30 ~mm^3}$ low background cerium bromide, CeBr$_3$(LB), scintillator crystal coupled to a Hamamatsu R11265U-200 photomultiplier. This detector will be the building block for a gamma-ray detector array designed to be the payload for a CubeSat to be launched in 2020. The aim of the mission is to study flashes of gamma rays of terrestrial origin. The design of the detector has been tuned for the detection of gamma rays in the 20 keV$-$3 MeV energy range.
Published: 2019
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11. Radio Discovery of and Gamma-Ray Pulsations from PSR J2339-0533

Author: Elizabeth C. Ferrara, Roger W. Romani, Pablo M. Saz Parkinson, Matthew Kerr, Fernando Camilo, Ismaël Cognard, Mallory S. E. Roberts, Bhaswati Bhattacharyya, Jayanta Roy, Andrea Belfiore, Scott M. Ransom, Paul S. Ray, Emil Polisensky, and Lucas Guillemot
Subjects: Physics, Gamma ray, General Medicine, Astrophysics
Published: 2020
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12. The Green Bank North Celestial Cap Pulsar Survey

Author: Ryan S. Lynch, G. Lunsford, Victoria M. Kaspi, J. Flanigan, Mallory S. E. Roberts, Maura McLaughlin, Fredrick A. Jenet, Kevin Stovall, Hind Al Noori, Renée Spiewak, L. P. Dartez, Jason Boyles, D. Day, Megan E. DeCesar, A. J. Ford, Bingyi Cui, S. Leake, Anne M. Archibald, Arielle N. Walker, Emmanuel Fonseca, S. Bradley Cenko, M. D. Rohr, Scott M. Ransom, V. I. Kondratiev, Ingrid H. Stairs, J. Hinojosa, B. L. Wells, Jason W. T. Hessels, S. Banaszak, A. Mata, Xavier Siemens, Lina Levin, Pradip Gatkine, Joeri van Leeuwen, P. Chawla, J. G. Martinez, Joseph K. Swiggum, David L. Kaplan, C. Karako-Argaman, Christopher M. Biwer, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Proper motion, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Green Bank Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Shapiro delay, general [pulsars], Binary pulsar, Neutron star, Pulsar, proper motions, surveys, Space and Planetary Science, Millisecond pulsar, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: We provide timing solutions for 45 radio pulsars discovered by the Robert C. Byrd Green Bank Telescope. These pulsars were found in the Green Bank North Celestial Cap pulsar survey, an all-GBT-sky survey being carried out at a frequency of 350 MHz. We include pulsar timing data from the Green Bank Telescope and Low Frequency Array. Our sample includes five fully recycled millisecond pulsars (MSPs, three of which are in a binary system), a new relativistic double neutron star system, an intermediate mass binary pulsar, a mode-changing pulsar, a 138-ms pulsar with a very low magnetic field, and several nulling pulsars. We have measured two post-Keplerian parameters and thus the masses of both objects in the double neutron star system. We also report a tentative companion mass measurement via Shapiro delay in a binary MSP. Two of the MSPs can be timed with high precision and have been included in pulsar timing arrays being used to search for low-frequency gravitational waves, while a third MSP is a member of the black widow class of binaries. Proper motion is measurable in five pulsars and we provide an estimate of their space velocity. We report on an optical counterpart to a new black widow system and provide constraints on the optical counterparts to other binary MSPs. We also present a preliminary analysis of nulling pulsars in our sample. These results demonstrate the scientific return of long timing campaigns on pulsars of all types., Accepted for publication in The Astrophysical Journal; 30 pages, 9 figures, 8 tables
Published: 2018
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13. X-Ray and Optical Studies of the Redback System PSR J2129–0429

Author: Hind Al Noori, Mallory S. E. Roberts, Paul S. Ray, Jason W. T. Hessels, Peter A. Gentile, Maura McLaughlin, Rodrigo Torres, Matthew Kerr, and Rene P. Breton
Subjects: Physics, 010504 meteorology & atmospheric sciences, Space and Planetary Science, 0103 physical sciences, X-ray, Astronomy and Astrophysics, Magnetic reconnection, Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences
Published: 2018
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14. A search for extragalactic pulsars in the Local Group galaxies IC 10 and Barnard's Galaxy

Author: Mallory S. E. Roberts, H. Al Noori, Scott M. Ransom, D. J. Champion, Paul S. Ray, and Maura McLaughlin
Subjects: Physics, History, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Local Group, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Computer Science Applications, Education, Pulsar, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: As of today, more than 2500 pulsars have been found, nearly all in the Milky Way, with the exception of ~28 pulsars in the Small and Large Magellanic Clouds. However, there have been few published attempts to search for pulsars deeper in our Galactic neighborhood. Two of the more promising Local Group galaxies are IC 10 and NGC 6822 (also known as Barnard's Galaxy) due to their relatively high star formation rate and their proximity to our galaxy. IC 10 in particular, holds promise as it is the closest starburst galaxy to us and harbors an unusually high number of Wolf-Rayet stars, implying the presence of many neutron stars. We observed IC 10 and NGC 6822 at 820 MHz with the Green Bank Telescope for ~15 and 5 hours respectively, and put a strong upper limit of 0.1 mJy on pulsars in either of the two galaxies. We also performed single pulse searches of both galaxies with no firm detections.
Published: 2017

15. A Search for Fast Radio Bursts with the GBNCC Pulsar Survey

Author: Mallory S. E. Roberts, J. van Leeuwen, V. M. Kaspi, Anne M. Archibald, Scott M. Ransom, V. I. Kondratiev, Kevin Stovall, Ryan S. Lynch, Duncan R. Lorimer, Kaustubh Rajwade, A. Josephy, Megan E. DeCesar, David L. Kaplan, P. Chawla, C. Karako-Argaman, Lina Levin, Maura McLaughlin, Ingrid H. Stairs, Jason W. T. Hessels, Joseph K. Swiggum, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, Flux distribution, education.field_of_study, 010308 nuclear & particles physics, Scattering, Canadian Hydrogen Intensity Mapping Experiment, statistical [methods], Monte Carlo method, Bandwidth (signal processing), Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, general [pulsars], 01 natural sciences, surveys, Pulsar, Space and Planetary Science, 0103 physical sciences, data analysis [methods], education, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: We report on a search for Fast Radio Bursts (FRBs) with the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey at 350 MHz. Pointings amounting to a total on-sky time of 61 days were searched to a DM of 3000 pc cm$^{-3}$ while the rest (23 days; 29% of the total time) were searched to a DM of 500 pc cm$^{-3}$. No FRBs were detected in the pointings observed through May 2016. We estimate a 95% confidence upper limit on the FRB rate of $3.6\times 10^3$ FRBs sky$^{-1}$ day$^{-1}$ above a peak flux density of 0.63 Jy at 350 MHz for an intrinsic pulse width of 5 ms. We place constraints on the spectral index $\alpha$ by running simulations for different astrophysical scenarios and cumulative flux density distributions. The non-detection with GBNCC is consistent with the 1.4-GHz rate reported for the Parkes surveys for $\alpha > +0.35 $ in the absence of scattering and free-free absorption and $\alpha > -0.3$ in the presence of scattering, for a Euclidean flux distribution. The constraints imply that FRBs exhibit either a flat spectrum or a spectral turnover at frequencies above 400 MHz. These constraints also allow estimation of the number of bursts that can be detected with current and upcoming surveys. We predict that CHIME may detect anywhere from several to $\sim$50 FRBs a day (depending on model assumptions), making it well suited for interesting constraints on spectral index, the log $N$-log $S$ slope and pulse profile evolution across its bandwidth (400-800 MHz)., Comment: 18 pages, 10 figures, Accepted for publication in ApJ
Published: 2017
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16. Intrabinary shock emission from 'black widows' and 'redbacks'

Author: P. A. Gentile, E. Aliu, Mallory S. E. Roberts, Maura McLaughlin, Paul S. Ray, Jason W. T. Hessels, and Scott M. Ransom
Subjects: Physics, Shock wave, Shock (fluid dynamics), Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Accretion (astrophysics), Pulsar, Space and Planetary Science, Millisecond pulsar, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Low Mass, Astrophysics::Galaxy Astrophysics
Abstract: Eclipsing millisecond pulsars in close (Pb < 1 day) binary systems provide a different view of pulsar winds and shocks than do isolated pulsars. Since 2009, the numbers of these systems known in the Galactic field has increased enormously. We have been systematically studying many of these newly discovered systems at multiple wavelengths. Typically, the companion is nearly Roche-lobe filling and heated by the pulsar which drives mass loss from the companion. The pulsar wind shocks with this material just above the surface of the companion. We discuss various observational properties of this shock, including radio eclipses, orbitally modulated X-ray emission, and the potential for γ-ray emission. Redbacks, whose companions are likely non-degenerate and significantly more massive, generally have more luminous shocks than black widows which have very low mass companions. This is expected since the more massive redback companions intercept a greater fraction of the pulsar wind. We also compare these systems to accreting millisecond pulsars, which may be progenitors of black widows and in some cases can pass back and forth between redback and accretion phases.
Published: 2014
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17. Search for transient gravitational waves in coincidence with short-duration radio transients during 2007-2013

Author: Alejandro Garcia, Michael E Zucker, Courtney R. Epstein, Roman Schnabel, S. Mastrogiovanni, J. E. Brau, A. A. van Veggel, Efim A. Khazanov, G. Ballardin, B. D. Lackey, L. Pinard, J. L. Willis, D. J. McManus, Howard Pan, Denis Martynov, R. Robie, Marco Bazzan, Kipp Cannon, M. Steinke, A. Kutynia, F. Clara, D. Meacher, M. Fays, B. M. Levine, J. Flanigan, A. Cumming, Aaron Buikema, C. C. Wipf, E. J. King, M. J. Cowart, V. Dolique, Federico Ferrini, R. S. Ottens, G. Vajente, P. Kumar, Q. Chu, W. Z. Korth, K. Siellez, C. Baune, Laura Cadonati, E. Genin, F. Baldaccini, Evan Ochsner, D. Ugolini, N. Letendre, B. R. Hall, A. J. Weinstein, A. Di Lieto, V. Boschi, G. Mazzolo, M. Landry, S. Ascenzi, M. Lormand, J. Bergman, H. J. Bulten, J. P. Zendri, Michael Kramer, B. Mours, G. McIntyre, P. Thomas, Z. Patrick, V. Malvezzi, David Jones, Erik Katsavounidis, Vladimir B. Braginsky, H. Vahlbruch, T. Chalermsongsak, Alessandro Bertolini, K. Riles, H. Middleton, M. Weinert, F. Fidecaro, G. M. Guidi, M. Barsuglia, A. Grant, N. Mazumder, M. Prijatelj, T. Dal Canton, J. Warner, H. N. Isa, M. J. Hart, C. J. Bell, N. A. Robertson, L. Kleybolte, J. C. Driggers, P. Puppo, A. W. Muir, C. L. Mueller, C. C. Arceneaux, R. Cavalieri, H. Rew, R. Passaquieti, A. Perreca, Marco Cavaglia, S. J. Chamberlin, M. Vasúth, G. Dojcinoski, Francesco Pannarale, H. Qi, R. F. Cardoso, J. K. Blackburn, A. Sawadsky, Timothy MacDonald, Leo Singer, T. Isogai, M. Branchesi, A. K. Srivastava, Robinjeet Singh, E. Chassande-Mottin, J. C. Batch, Jonathan Cripe, Sheila Rowan, G. A. Prodi, R. DeSalvo, K. Mason, Márton Tápai, David Jonathan Hofman, E. C. Ferreira, E. A. Huerta, B. Behnke, R. Birney, Susan M. Scott, I. Khan, Y. Wang, G. M. Harry, D. Rosińska, K. Venkateswara, Aaron Berndsen, Patrice Hello, Laleh Sadeghian, V. P. Mitrofanov, S. T. Countryman, A. W. Heptonstall, Vivien Raymond, Peter R. Saulson, L. Cerboni Baiardi, T. D. Abbott, O. Puncken, A. Ford, V. Necula, Surabhi Sachdev, Christopher J. Moore, Daniele Trifirò, Chad Hanna, K. A. Hodge, Bala R. Iyer, J. M. Gonzalez Castro, Yuri Levin, S. McCormick, O. V. Palashov, Sean T. McWilliams, M. Merzougui, Carl-Johan Haster, C. Aulbert, F. Piergiovanni, Chang-Hwan Lee, G. Cerretani, L. Trozzo, S. Mirshekari, M. C. Araya, Sanjeev Dhurandhar, Jason W. T. Hessels, Albert Lazzarini, Y. Minenkov, E. G. Thomas, A. Basti, P. G. Murray, Todd Adams, R. Goetz, F. Frasconi, Tarun Souradeep, Liam Cunningham, R. M. Martin, Robert Stone, A. Di Virgilio, A. R. Williamson, W. Del Pozzo, P. F. Cohadon, H. Heitmann, Roy Williams, G. Pillant, V. V. Frolov, L. Rolland, W. D. Vousden, Albrecht Rüdiger, J. Oberling, A. Singhal, L. Matone, Fabrizio Barone, Haocun Yu, Fiodor Sorrentino, B. K. Berger, M. Davier, M. J. Yap, Samaya Nissanke, Jens Birch, Z. Frei, T. Penucci, M. Ast, O. E. S. Sauter, F. Mezzani, Fabien Kéfélian, J. H. Hough, M. Mohan, K. G. Arun, T. Huynh-Dinh, J. Luo, K. Haris, Chunglee Kim, Xing-Jiang Zhu, V. Sequino, M. S. Shahriar, S. Huang, P. Bacon, Daniel E. Holz, S. Márka, D. Barta, J. S. Kissel, V. I. Kondratiev, B. J. J. Slagmolen, Joshua Yablon, D. Passuello, N. Man, Fan Zhang, Collin D. Capano, D. J. Vine, J. R. Palamos, T. Z. Summerscales, Stanislav Babak, D. Day, Namjun Kim, J.-D. Fournier, M. H. Wimmer, K. Kokeyama, J. J. Hacker, Philip F. Hopkins, William Yam, L. Wallace, S. Chung, S. Farinon, M. Constancio, Duncan A. Brown, T. Sadecki, A. Królak, R. Frey, Kenneth A. Strain, Jimin George, M. Sieniawska, A. Moggi, Kevin M. Ryan, H. J. Jang, Gregory Ashton, Fabio Marchesoni, Maria Ilaria Del Principe, B. Patricelli, F. Garufi, C. M. Reed, M. Korobko, G. D. Meadors, Margaret Millhouse, S. Grunewald, M. Agathos, S. G. Gaonkar, D. Bersanetti, S. R. Morriss, Riccardo Bassiri, Magnus Manske, E. Maros, Douglas R. Cook, A. Viceré, Yi Chen, M. E. Normandin, G. Bogaert, Haixing Miao, K. Haughian, J. Eichholz, B. C. Stephens, Marc Favata, V. M. Kaspi, Roger Jones, V. J. Roma, Michele Zanolin, Michael Pürrer, Serena Vinciguerra, F. Nocera, D. J. White, I. Fiori, D. J. Hosken, C. Zhao, E. Coccia, C. Graef, B. A. Weaver, J. G. Rollins, Kyungmin Kim, D. D. Brown, B. O'Reilly, T. J. Massinger, T. Vo, O. J. Piccinni, S. B. Coughlin, S. L. Danilishin, M. Shaltev, O. Bock, L. Di Fiore, James G. Bartlett, K. L. Dooley, G. Mendell, T. Di Girolamo, L.-W. Wei, N. van Bakel, Lisa Barsotti, R. J. G. Jonker, I. Kowalska, S. Kaufer, Eric Oelker, M. Boer, J. B. Kanner, Rainer Weiss, S. Penn, D. Schuette, A. Giazotto, R. Pedurand, Benno Willke, Joonghan Kim, A. Grado, Fredrick A. Jenet, P. Shawhan, Alberto Vecchio, L. Prokhorov, I. Ferrante, C. Cahillane, Will M. Farr, Subhabrata Mitra, R. W. P. Drever, E. A. Quintero, J. Hennig, G. L. Mansell, Jessica Steinlechner, A. Neunzert, Duncan R. Lorimer, Nam-Gyu Kim, S. A. Usman, G. D. Hammond, D. H. Shoemaker, M. Kasprzack, P. Couvares, P. Charlton, Kejia Lee, P. Brockill, G. Vedovato, D. B. Kozak, Tyson Littenberg, T. B. Edo, Gavin Davies, A. Lenon, B. L. Pearlstone, M. Ducrot, Archisman Ghosh, X. F. Wang, Rebecca Fisher, Maura McLaughlin, H. Fehrmann, W. W. Johnson, G. P. Newton, M. Fyffe, Michael L. Gorodetsky, T. Westphal, Ryan Lynch, M. Heurs, S. S. Premachandra, A. Masserot, V. Dattilo, Tejinder Kaur, Edwin J. Son, K. Kawabe, D. Huet, S. H. Huttner, F. Cleva, Marie-Anne Bizouard, S. Walsh, A. Sheperd, Maximiliano Isi, Zifan Zhou, M. Montani, Alessandra Buonanno, R. Metzdorff, Nancy Aggarwal, Zahoor Ali Khan, V. Fafone, Andrew Melatos, Kendall Ackley, R. K. Nayak, D. Mendoza-Gandara, J-Y. Vinet, B. Shapiro, Reed Essick, R. Everett, Jan Harms, D. Talukder, C. V. Torres, S. M. Aston, C. Vorvick, I. W. Harry, Satyanarayan Ray Pitambar Mohapatra, Viswanath Bavigadda, A. Sevigny, P. B. Graff, I. A. Bilenko, J. L. Wright, Alessandra Corsi, David J. Ottaway, A. Paoli, A. R. Wade, R. S. Lynch, G. Kuehn, C. M. Mow-Lowry, Sergey P. Vyatchanin, A. Idrisy, M. Yvert, Lionel Martellini, Kazuhiro Agatsuma, F. Magaña-Sandoval, R. M. Magee, Peter Fritschel, Gabriela Gonzalez, Benjamin William Allen, P. J. Sutton, P. Bojtos, David Blair, Karsten Danzmann, J. Betzwieser, M. Gosselin, Alex B. Nielsen, J. H. Romie, G. Serna, Stefan Hild, Y. Ma, P. Chawla, S. Kandhasamy, B. Sorazu, T. Etzel, Hua Wang, S. E. Hollitt, Vicky Kalogera, G. Lunsford, D. B. Kelley, C. Palomba, J.-M. Isac, Heinz-Bernd Eggenstein, Zhihui Du, V. Predoi, I. W. Martin, L. Rei, M. Masso-Reid, Mark Hannam, I. Dave, Adam A. Libson, M. Fletcher, B. Hughey, Evan Goetz, Michael W. Coughlin, A. L. Stuver, J. E. Lord, M. Mageswaran, C. C. Yancey, A. Ain, B. F. Whiting, J. Casanueva Diaz, Lei Zhang, P. Schale, E. Cuoco, A. Gupta, M. Tonelli, Larry R. Price, John Miller, Leopoldo Milano, Slawomir Gras, C. Bond, Nergis Mavalvala, Sascha Husa, A. Gennai, H. P. Daveloza, C. Van Den Broeck, Arielle N. Walker, Jordan Camp, P. Wessels, T. T. Nguyen, C. S. Unnikrishnan, Lloyd Paul Aiello, R. Douglas, F. J. Raab, David E. McClelland, Scott M. Ransom, B. C. Pant, N. Indik, Andrea Chincarini, T. Prestegard, S. S. Eikenberry, M. S. Kehl, A. Post, Yanxi Zhang, M. Bejger, Hartmut Grote, F. Marion, E. J. Daw, J. Schmidt, Kevin Stovall, C. Krueger, Rosa Poggiani, V. Germain, V. Frey, Jong H. Chow, Paolo Addesso, K. D. Giardina, G. Losurdo, L. Conti, Ingrid H. Stairs, M. Vardaro, A. Pasqualetti, A. Mytidis, A. Pele, P. Raffai, R. Chakraborty, D. M. Macleod, S. E. Gossan, G. Greco, L. E. Wade, J. S. Lange, B. L. Swinkels, Neil J. Cornish, Evan Keane, G. Bergmann, J. Hanks, N. A. Strauss, Timothy A Welborn, V. Tiwari, K. Gill, Walter Winkler, Jiayi Qin, A. Singer, M. C. Díaz, Samuel Deléglise, L. P. Dartez, C. Pankow, P. M. Meyers, Hyun Lee, M. D. Rohr, J. Calderón Bustillo, Jerome Degallaix, Y. Setyawati, C. Casentini, Sebastian Khan, F. Carbognani, E. O. Lebigot, T. Denker, Christopher P. L. Berry, A. D. Silva, H. J. Pletsch, Enrico Calloni, G. Traylor, Thomas Corbitt, L. Salconi, C. A. Costa, L. R. Cominsky, R. Gustafson, M. P. Thirugnanasambandam, N. Straniero, G. Wu, F. Robinet, S. Meshkov, Seog Oh, W. G. Anderson, G. Cella, Giacomo Ciani, B. P. Abbott, E. K. Gustafson, Meng Wang, D.B. DeBra, A. Bisht, M. Leonardi, S. E. Zuraw, Sourav Ghosh, Imre Bartos, V. Quetschke, Bangalore Suryanarayana Sathyaprakash, Martin M. Fejer, J. R. Smith, R. Bork, L. van der Schaaf, S. A. Pai, Cody Messick, Yann Bouffanais, A. Bohe, A. C. Green, Fausto Acernese, Fumiko Kawazoe, D. Moraru, A. S. Markosyan, Madeline Wade, P. Leaci, A. Colla, Harald Lück, D. Verkindt, J. N. Marx, Vuk Mandic, Gianpietro Cagnoli, László Á. Gergely, Tania Regimbau, M. M. Hanke, Barry C. Barish, Christian D. Ott, K. Nedkova, S. Tiwari, S. B. Anderson, M. Cho, Paul J. Groot, M. Zevin, A. Staley, L. Zangrando, Sung-Po Chao, John A. Clark, S. Jawahar, T. Theeg, Ben Farr, V. Re, E. A. Houston, X. Guo, Matthew Evans, S. Vass, A. Glaefke, C. Tomlinson, J. D. Lough, R. Coyne, Mi Zhang, C. Gray, G. H. Ogin, Soma Mukherjee, S. C. McGuire, J. F. Read, M. K. Gupta, J. G. Martinez, John Veitch, S. Di Pace, J. C. Barayoga, D. Nolting, M. Neri, J. A. Giaime, S. Raja, S. E. Strigin, Y. M. Kim, R. De Rosa, Ruslan Vaulin, David B. Tanner, F. Jiménez-Forteza, H. Radkins, N. S. Darman, N. Arnaud, Maggie Tse, Christophe Collette, Ho-Gyu Lee, K. A. Thorne, C. Messenger, Fabrice Matichard, R. Inta, Aviral Singh, P. J. King, W. Kells, S. Klimenko, M. MacInnis, M. Mantovani, H. R. Paris, L. Kuo, H. Yamamoto, E. Capocasa, Thibaut Jacqmin, C. I. Torrie, A. Mata, P. Rapagnani, D. R. Ingram, A. Bozzi, B. A. Boom, S. D'Antonio, A. Allocca, M. Brinkmann, F. Vetrano, J. Zweizig, D. C. Coyne, E. L. Merilh, K. Izumi, M. C. Tringali, I. Nardecchia, Anne M. Archibald, Sebastian Steinlechner, Andreas Freise, Vincenzo Pierro, Paul D. Lasky, S. G. Crowder, J. van Leeuwen, I. Maksimovic, A. Rocchi, D. V. Voss, R. L. Ward, G. Hemming, Matthew Pitkin, D. Stiles, N. Gehrels, N. A. Gordon, Xavier Siemens, P. J. Veitch, Andrew Lundgren, M. Factourovich, S. Koley, S. Leake, A. Schönbeck, T. P. Downes, R. L. Savage, A. S. Bell, D. Pascucci, Mallory S. E. Roberts, J. R. Sanders, J. Prasad, W. Katzman, F. Y. Khalili, M. Saleem, Carlos Cepeda, Robert J. McCarthy, H. Fair, M. Pichot, Andrea Taracchini, J. V. van Heijningen, David Coward, Sheon Chua, R. Bonnand, N. Leroy, M. Granata, Marek Szczepanczyk, Minchuan Zhou, G. Wang, C. Bradaschia, P. Oppermann, Linqing Wen, Ik Siong Heng, K. N. Mukund, Steven Bloemen, Jonathan R. Gair, M. Pedraza, H. A. G. Gabbard, M. Chan, Ettore Majorana, Christie A. McPhee, W. Engels, S. M. Koehlenbeck, Eric Thrane, Maria Alessandra Papa, F. Cavalier, A. Zadro.zny, C. Michel, G. Valdes, S. E. Dwyer, David Keitel, G. Islas, G. Debreczeni, Chia-Liang Cheng, Antoine Heidmann, Gleb Romanov, Nicholas Smith, Qi Fang, Rui Miguel Faisca Rodrigues Pereira, D. Töyrä, N. A. Lockerbie, H. Overmier, T. Hardwick, D. Steinmeyer, P. Ehrens, F. Travasso, Blake Moore, Sarah Caudill, R. Quitzow-James, R. Day, F. Ohme, V. B. Adya, William Parker, Z. Shao, M. Razzano, A. Nitz, S. Banaszak, D. Simakov, E. Schreiber, G. Kang, A. Pal-Singh, M. Was, A. L. Miller, B. Sandeen, M. C. Edwards, C. Bogan, J. Hinojosa, Thomas Dent, Vladimir Dergachev, S. Karki, D. Sellers, James Whelan, M. Bitossi, K. Wette, F. Martelli, Karan Jani, Suvadeep Bose, Gijs Nelemans, Graham Woan, P. Astone, Larne Pekowsky, Robert L. Byer, V. Kondrashov, I. Di Palma, Stuart Reid, A. Samajdar, P. Ajith, M. Punturo, H. Vocca, J. Meidam, John J. Oh, Timothy Evans, Eugeniy E. Mikhailov, R. Gouaty, Z. Márka, E. D. Hall, Jolien D. E. Creighton, S. Caride, Arunava Mukherjee, R. Mittleman, Nelson Christensen, Riccardo Sturani, M. T. Hartman, V. Kringel, Rory Smith, C. Adams, R. M. Blair, D. Sigg, S. W. Ballmer, K. Holt, D. M. Shoemaker, G. Gemme, V. Sandberg, Bernard F. Schutz, D. S. Rabeling, Li Ju, H. Wittel, Daniel A. Shaddock, M. Phelps, T. T. Fricke, C. V. Kalaghatgi, J. Hanson, D. Hoak, Michelle E. Walker, G. Moreno, D. Sentenac, M. 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Cesarini, Kieran Craig, K. V. Tokmakov, Antonios Kontos, Debnandini Mukherjee, J. O'Dell, Junwei Cao, M. Lorenzini, S. Doravari, Samuele Cortese, Innocenzo M. Pinto, A. F. Brooks, S. Privitera, L. Sammut, S. E. Whitcomb, V. Loriette, Francesco Salemi, Rana X. Adhikari, Christelle Lesvigne-Buy, Jessica McIver, P. A. Altin, B. L. Wells, Alexander Khalaidovski, B. Machenschalk, F. Donovan, A. Chiummo, Luca Gammaitoni, D. Barker, B. Sassolas, R. Kennedy, D. C. Vander-Hyde, C. Karako-Argaman, M. K. M. Bader, A. Brillet, D. Tuyenbayev, Christopher M. Biwer, S. Frasca, Tristan Briant, G. Gaur, Stephen Fairhurst, Carl Blair, Archana Pai, F. Paoletti, P. Ruggi, A. Mullavey, L. Sun, Xiaohui Fan, Richard O'Shaughnessy, B. Barr, Malik Rakhmanov, J. Worden, P. T. Baker, N. M. Brown, Roland Schilling, Swetha Bhagwat, S. P. Tarabrin, L. Naticchioni, Salvatore Vitale, Richard J. Abbott, A. L. Urban, R. Flaminio, J.-P. Coulon, Odylio D. Aguiar, H. S. Chen, László Gondán, Angus Cherry, C. Lazzaro, Patricia Schmidt, V. Brisson, A. M. Sintes, P. Aufmuth, Chandra Kant Mishra, R. Bhandare, Piotr Jaranowski, California Institute of Technology, Louisiana State University, Fisciano, Complesso Universitario di Monte S. Angelo, University of Florida, LIGO Livingston Observatory, CNRS/IN2P3, University of Sannio at Benevento, Max-Planck-Institut für Gravitationsphysik, Science Park, Massachusetts Institute of Technology, Instituto Nacional de Pesquisas Espaciais, Gran Sasso Science Institute, Sezione di Roma Tor Vergata, Inter-University Centre for Astronomy and Astrophysics, Tata Institute of Fundamental Research, University of Wisconsin-Milwaukee, Leibniz Universität Hannover, Università di Pisa, Sezione di Pisa, Australian National University, University of Mississippi, California State University Fullerton, Université Paris-Saclay, Chennai Mathematical Institute, Università di Roma Tor Vergata, University of Southampton, Universität Hamburg, Sezione di Roma, Sorbonne Paris Cité, Montana State University, Università di Perugia, Sezione di Perugia, European Gravitational Observatory (EGO), Syracuse University, University of Glasgow, LIGO Hanford Observatory, RMKI, Columbia University, Stanford University, Dipartimento di Fisica e Astronomia, Sezione di Padova, CAMK-PAN, University of Birmingham, Università degli Studi di Genova, Sezione di Genova, RRCAT, Lomonosov Moscow State University, University of the West of Scotland, University of Western Australia, Radboud University Nijmegen, Observatoire Côte d'Azur, Lendulet Astrophysics Research Group, Université de Rennes 1, Washington State University, Università degli Studi di Urbino Carlo Bo, Sezione di Firenze, University of Oregon, Collège de France, Astronomical Observatory Warsaw University, VU University Amsterdam, University of Maryland, Georgia Institute of Technology, Université Claude Bernard Lyon 1, IEEC, NASA/Goddard Space Flight Center, University of Toronto, Tsinghua University, University of Michigan, National Tsing Hua University, Charles Sturt University, University of Chicago, Caltech CaRT, Korea Institute of Science and Technology Information, Carleton College, Università di Roma la Sapienza, University of Brussels, Sonoma State University, Texas Tech University, Cardiff University, University of Minnesota, University of Melbourne, University of Texas Rio Grande Valley, University of Sheffield, Dipartimento di Fisica, Trento Institute for Fundamental Physics and Applications, Montclair State University, Pennsylvania State University, National Astronomical Observatory of Japan, University of Edinburgh, Indian Institute of Technology, Institute for Plasma Research, University of Szeged, Embry-Riddle Aeronautical University, Osservatorio Astronomico di Capodimonte, American University, University of Massachusetts-Amherst, University of Adelaide, West Virginia University, University of Biał Ystok, University of Strathclyde, CET Campus, Northwestern University, Institute of Applied Physics, Pusan National University, Hanyang University, NCBJ, IM-PAN, Rochester Institute of Technology, Monash University, Seoul National University, University of Alabama in Huntsville, CNRS, Southern University and A and M College, College of William and Mary, Universidade Estadual Paulista (UNESP), University of Cambridge, IISER-Kolkata, HSIC, Whitman College, National Institute for Mathematical Sciences, Université de Lyon, Hobart and William Smith Colleges, University of Zielona Góra, Andrews University, Università di Siena, Trinity University, University of Washington, Kenyon College, Abilene Christian University, Netherlands Institute for Radio Astronomy, University of British Columbia, Western Kentucky University, McGill University, Ohio State University, University of Amsterdam, Jodrell Bank Observatory, Lebedev Physical Institute, Max Planck Institute for Radio Astronomy, University of Manchester, National Radio Astronomy Observatory, University of Virginia, Inc., University of New Mexico, Colorado State University, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Science and Engineering Research Board, Canadian Network for Research and Innovation in Machining Technology, Natural Sciences and Engineering Research Council of Canada, Alfred P. Sloan Foundation, Carnegie Trust for the Universities of Scotland, Science and Technology Facilities Council, Ontario Ministry of Economic Development and Innovation, Ministerio de Economía y Competitividad, Scottish Funding Council, Seventh Framework Programme, Industry Canada, Council of Scientific and Industrial Research, Australian Research Council, Royal Society, Narodowe Centrum Nauki, National Aeronautics and Space Administration, 617199, European Research Council, Centre National de la Recherche Scientifique, Max-Planck-Gesellschaft, Department of Science and Technology, Ministry of Science and Technology, Research Corporation for Science Advancement, National Science Foundation, Leverhulme Trust, David and Lucile Packard Foundation, Országos Tudományos Kutatási Alapprogramok, State of Niedersachsen, International Science Linkages, Conselleria d’Economia i Competitivitat and Conselleria d’Educaci, Universitats of the Govern de les Illes Balears, Lyon Institute of Origins, Brazilian Ministry of Science, Technology, and Innovation, Ministry of Human Resource Development, Scottish Universities Physics Alliance, Stichting voor Fundamenteel Onderzoek der Materie, Istituto Nazionale di Fisica Nucleare, National Research Foundation of Korea, Nederlandse Organisatie voor Wetenschappelijk Onderzoek, LIGO, VIRGO, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), The LIGO Scientific Collaboration, The Virgo Collaboration, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), (Astro)-Particles Physics, 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., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Calderón Bustillo, J., Callister, T., Calloni, Enrico, Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Casanueva Diaz, J., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerboni Baiardi, L., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. F., Colla, A., Collette, C. G., Cominsky, L., Constancio, M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. P., Countryman, S. T., Couvares, P., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., Debra, D., Debreczeni, G., Degallaix, J., DE LAURENTIS, Martina, Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dergachev, V., DE ROSA, Rosario, Derosa, R. T., Desalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., DI GIROLAMO, Tristano, Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, Fabio, Gaur, G., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Gonzalez Castro, J. M., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Haris, K., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chunglee, Kim, J., Kim, K., Kim, Nam Gyu, Kim, Namjun, Kim, Y. M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., Macdonald, T., Machenschalk, B., Macinnis, M., Macleod, D. M., Magaña Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso Reid, M., Mastrogiovanni, S., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcguire, S. C., Mcintyre, G., Mciver, J., Mcmanus, D. J., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza Gandara, D., Mercer, R. A., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, Leopoldo, Miller, A. L., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, K. N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, Richard J., O'Reilly, B., O'Shaughnessy, R., Ott, C. D., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Pereira, R., Perreca, A., Phelps, M., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S. S., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Quitzow James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, J. D., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O. E. S., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. 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Mikhailov, E. .e., Milano, L., Miller, A. .l., Mitrofanov, V. .p., Mohapatra, S. .r. .p., MONTANI, MATTEO, Moore, B. .c., Moore, C. .j., Morriss, S. .r., Mow Lowry, C. .m., Mueller, C. .l., Muir, A. .w., Mukund, K. .n., Murphy, D. .j., Murray, P. .g., Nayak, R. .k., Nguyen, T. .t., Nielsen, A. .b., Normandin, M. .e. .n., Nuttall, L. .k., O’Dell, J., Ogin, G. .h., Oh, J. .j., Oh, S. .h., O’Reilly, B., O’Shaughnessy, R., Ott, C. .d., Ottaway, D. .j., Ottens, R. .s., Owen, B. .j., Pai, S. .a., Palamos, J. .r., Pant, B. .c., Papa, M. .a., Paris, H. .r., Pearlstone, B. .l., Piccinni, O. .j., PIERGIOVANNI, FRANCESCO, Pinto, I. .m., Pletsch, H. .j., Premachandra, S. .s., Price, L. .r., Prodi, G. .a., Quintero, E. .a., Raab, F. .j., Rabeling, D. .s., Reed, C. .m., Reitze, D. .h., Robertson, N. .a., Rollins, J. .g., Roma, V. .j., Romano, J. .d., Romie, J. .h., Sanchez, E. .j., Sanders, J. .r., Sathyaprakash, B. .s., Saulson, P. .r., Sauter, O. .e. .s., Savage, R. .l., Schofield, R. .m. .s., Schutz, B. .f., Scott, S. .m., Shaddock, D. .a., Shahriar, M. .s., Shoemaker, D. .h., Shoemaker, D. .m., Silva, A. .d., Singer, L. .p., Sintes, A. .m., Slagmolen, B. .j. .j., Smith, J. .r., Smith, N. .d., Smith, R. .j. .e., Son, E. .j., Srivastava, A. .k., Stephens, B. .c., Strain, K. .a., STRATTA, MARIA GIULIANA, Strauss, N. .a., Stuver, A. .l., Summerscales, T. .z., Sutton, P. .j., Swinkels, B. .l., Szczepańczyk, M. .j., Tanner, D. .b., Tarabrin, S. .p., Thirugnanasambandam, M. .p., Thomas, E. .g., Thorne, K. .a., Tokmakov, K. .v., Torres, C. .v., Torrie, C. .i., Tringali, M. .c., Unnikrishnan, C. .s., Urban, A. .l., Usman, S. .a., van Bakel, N., van Beuzekom, M., van den Brand, J. .f. .j., Vander Hyde, D. .c., van der Schaaf, L., van Heijningen, J. .v., van Veggel, A. .a., Veitch, P. .j., VETRANO, FLAVIO, VICERE', ANDREA, Vine, D. .j., Voss, D. .v., Vousden, W. .d., Vyatchanin, S. .p., Wade, A. .r., Wade, L. .e., Ward, R. .l., Weinstein, A. .j., Whelan, J. .t., Whitcomb, S. .e., White, D. .j., Whiting, B. .f., Williams, R. .d., Williamson, A. .r., Willis, J. .l., Wimmer, M. .h., Wipf, C. .c., Wright, J. .l., Yancey, C. .c., Yap, M. .j., Zhu, X. .j., Zucker, M. .e., Zuraw, S. .e., Archibald, A. .m., Cardoso, R. .f., Dartez, L. .p., Epstein, C. .r., Ford, A. .j., Hessels, J. .w. .t., Jenet, F. .a., Kaspi, V. .m., Keane, E. .f., Kondratiev, V. .i., Lynch, R. .s., Martinez, J. .g., Mclaughlin, M. .a., Mcphee, C. .a., Roberts, M. .s. .e., Rohr, M. .d. .w., Stairs, I. .h., van Leeuwen, J., Walker, A. .n., Wells, B. .l., CALTECH, Louisiana State Univ, Univ Salerno, Ist Nazl Fis Nucl, Univ Florida, LIGO Livingston Observ, Univ Savoie Mont Blanc, Univ Sannio Benevento, Max Planck Inst Gravitat Phys, NIKHEF H, MIT, Inst Nacl Pesquisas Espaciais, Inter Univ Ctr Astron & Astrophys, Tata Inst Fundamental Res, Univ Wisconsin, Leibniz Univ Hannover, Univ Pisa, Australian Natl Univ, Univ Mississippi, Calif State Univ Fullerton, Univ Paris Saclay, Chennai Math Inst, Univ Roma Tor Vergata, Univ Southampton, Univ Hamburg, Universidade de São Paulo (USP), Montana State Univ, Univ Perugia, EGO, Syracuse Univ, Univ Glasgow, LIGO Hanford Observ, Columbia Univ, Stanford Univ, Univ Padua, CAMK PAN, Univ Birmingham, Univ Genoa, Lomonosov Moscow State Univ, Univ West Scotland, Univ Western Australia, Radboud Univ Nijmegen, Univ Cote Azur, MTA Eotvos Univ, Univ Rennes 1, Washington State Univ, Univ Urbino Carlo Bo, Univ Oregon, Univ Paris 06, Warsaw Univ, Vrije Univ Amsterdam, Univ Maryland, Georgia Inst Technol, CNRS IN2P3, Univ Lyon 1, Univ Illes Balears, Univ Naples Federico II, NASA, Univ Toronto, Tsinghua Univ, Univ Michigan, Natl Tsing Hua Univ, Charles Sturt Univ, Univ Chicago, Korea Inst Sci & Technol Informat, Carleton Coll, Univ Roma La Sapienza, Univ Brussels, Sonoma State Univ, Texas Tech Univ, Cardiff Univ, Univ Minnesota, Univ Melbourne, Univ Texas Rio Grande Valley, Univ Sheffield, Univ Trento, Montclair State Univ, Penn State Univ, Natl Astron Observ Japan, Univ Edinburgh, Indian Inst Technol, Inst Plasma Res, Univ Szeged, Embry Riddle Aeronaut Univ, Amer Univ, Univ Massachusetts, Univ Adelaide, W Virginia Univ, Univ Bialystok, Univ Strathclyde, IISER TVM, Northwestern Univ, Inst Appl Phys, Pusan Natl Univ, Hanyang Univ, IM PAN, Rochester Inst Technol, Monash Univ, Seoul Natl Univ, Univ Alabama, Univ Camerino, Southern Univ, A&M Coll, Coll William & Mary, Universidade Estadual Paulista (Unesp), Univ Cambridge, IISER Kolkata, Rutherford Appleton Lab, Whitman Coll, Natl Inst Math Sci, Univ Lyon, Hobart & William Smith Coll, Univ Zielona Gora, Andrews Univ, Univ Siena, Trinity Univ, Univ Washington, Kenyon Coll, Abilene Christian Univ, ASTRON, Univ British Columbia, Western Kentucky Univ, McGill Univ, Ohio State Univ, Univ Amsterdam, SKA Org, Lebedev Phys Inst, Max Planck Inst Radioastron, Univ Manchester, Natl Radio Astron Observ, Univ Virginia, Eureka Sci Inc, Univ New Mexico, Colorado State Univ, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Radio Transients, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Nuclear and High Energy Physics, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, detection, FOS: Physical sciences, Gravitational Wave, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Coincidence, GAMMA-RAY BURST, ENERGY, Pulsar, Settore FIS/05 - Astronomia e Astrofisica, Gravitational Waves, Radio Transients, 0103 physical sciences, Binary star, coincidence, 010303 astronomy & astrophysics, QC, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational Waves, PLASMA, 010308 nuclear & particles physics, Gravitational wave, ORIGIN, Settore FIS/01 - Fisica Sperimentale, Green Bank Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], PULSARS, LIGO, PULSES, Neutron star, Physics and Astronomy, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, GW, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Copyright © 2016 American Physical Society and reproduced in accordance with the publisher copyright policy, We present an archival search for transient gravitational-wave bursts in coincidence with 27 single-pulse triggers from Green Bank Telescope pulsar surveys, using the LIGO, Virgo, and GEO interferometer network. We also discuss a check for gravitational-wave signals in coincidence with Parkes fast radio bursts using similar methods. Data analyzed in these searches were collected between 2007 and 2013. Possible sources of emission of both short-duration radio signals and transient gravitational-wave emission include starquakes on neutron stars, binary coalescence of neutron stars, and cosmic string cusps. While no evidence for gravitational-wave emission in coincidence with these radio transients was found, the current analysis serves as a prototype for similar future searches using more sensitive second-generation interferometers.
Published: 2016
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18. A search for very high energy gamma rays from the missing link binary pulsar J1023+0038 with VERITAS

Author: Wystan Benbow, John L. Quinn, A. Petrashyk, M. J. Lang, P. Kar, O. M. Weiner, Jonathan Biteau, J. P. Finley, B. Zitzer, N. Håkansson, Henrike Fleischhack, David Kieda, A. W. Smith, A. Flinders, Q. Feng, Abraham D. Falcone, Gordon T. Richards, E. Roache, Karlen Shahinyan, E. Pueschel, Geza Gyuk, S. Vincent, Nahee Park, A. Varlotta, N. Kelley-Hoskins, T. B. Humensky, Maria Krause, P. Moriarty, K. L. Byrum, Wei Cui, J. Grube, P. Kaaret, J. V. Cardenzana, J. D. Eisch, S. McArthur, A. McCann, Xuhui Chen, V. Bugaev, L. Ciupik, S. Archambault, Reshmi Mukherjee, Daniel Nieto, A. O'Faolain de Bhroithe, Sinéad M. Griffin, A. Popkow, E. Aliu, Maria Chernyakova, Lucy Fortson, J. Tyler, Matteo Cerruti, Moritz Hütten, J. H. Buckley, R. A. Ong, A. N. Otte, Amy Furniss, Marcos Santander, M. Kertzman, Martin Pohl, S. P. Wakely, P. Fortin, V. Pelassa, C. B. Rulten, Ralph Bird, G. H. Sembroski, A. Loo, K. Meagher, Hugh Dickinson, Mallory S. E. Roberts, M. Buchovecky, M. P. Connolly, D. Pandel, P. T. Reynolds, A. J.R. Weinstein, C. A. Johnson, J. V. Tucci, Gernot Maier, A. Wilhelm, D. Staszak, K. Ragan, I. Telezhinsky, Jamie Holder, David A. Williams, Thanh Huy Nguyen, A. Archer, and G. H. Gillanders
Subjects: nustar observations, Astrophysics::High Energy Astrophysical Phenomena, Flux, Binary number, FOS: Physical sciences, Astrophysics, telescope, 01 natural sciences, Binary pulsar, Pulsar, pulsars: general, psr j1023+0038, emission, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Millisecond, state change, 010308 nuclear & particles physics, pulsars: individual (psr j1023+0038), periastron, Gamma ray, transition, Institut für Physik und Astronomie, Astronomy and Astrophysics, gamma rays: general, 1st j102347.6+003841, Magnetic field, Neutron star, binaries: general, 13. Climate action, Space and Planetary Science, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, millisecond pulsar, discovery
Abstract: The binary millisecond radio pulsar PSR J1023+0038 exhibits many characteristics similar to the gamma-ray binary system PSR B1259--63/LS 2883, making it an ideal candidate for the study of high-energy non-thermal emission. It has been the subject of multi-wavelength campaigns following the disappearance of the pulsed radio emission in 2013 June, which revealed the appearance of an accretion disk around the neutron star. We present the results of very high-energy gamma-ray observations carried out by VERITAS before and after this change of state. Searches for steady and pulsed emission of both data sets yield no significant gamma-ray signal above 100 GeV, and upper limits are given for both a steady and pulsed gamma-ray flux. These upper limits are used to constrain the magnetic field strength in the shock region of the PSR J1023+0038 system. Assuming that very high-energy gamma rays are produced via an inverse-Compton mechanism in the shock region, we constrain the shock magnetic field to be greater than $\sim$2 G before the disappearance of the radio pulsar and greater than $\sim$10 G afterwards., 7 pages, 3 figures, accepted for publication in ApJ
Published: 2016
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19. Surrounded by spiders! New black widows and redbacks in the Galactic field

Author: Mallory S. E. Roberts
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Orbital period, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Space and Planetary Science, Millisecond pulsar, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Low Mass, Fermi Gamma-ray Space Telescope
Abstract: Over the last few years, the number of known eclipsing radio millisecond pulsar systems in the Galactic field has dramatically increased, with many being associated with Fermi gamma-ray sources. All are in tight binaries (orbital period < 24 hr) with many being classical "black widows" which have very low mass companions (companion mass Mc << 0.1 Msol) but some are "redbacks" with low mass (Mc ~ 0.2 - 0.4Msol) companions which are probably non-degenerate. These latter are systems where the mass transfer process may have only temporarily halted, and so are transitional systems between low mass X-ray binaries and ordinary binary millisecond pulsars. Here we review the new discoveries and their multi-wavelength properties, and briefly discuss models of shock emission, mass determinations, and evolutionary scenarios., Proceedings of IAUS 291 "Neutron Stars and Pulsars: Challenges and Opportunities after 80 years", J. van Leeuwen (ed.); 6 pages, 2 figures
Published: 2012
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20. MULTIWAVELENGTH OBSERVATIONS OF THE RUNAWAY BINARY HD 15137

Author: Tabetha S. Boyajian, Douglas R. Gies, Amber N. Marsh, Mallory S. E. Roberts, Rachael M. Roettenbacher, Erika D. Grundstrom, Michaël De Becker, Christina Aragona, and M. Virginia McSwain
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Black hole, Neutron star, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Binary system, Astrophysics - High Energy Astrophysical Phenomena, Low Mass, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, O-type star, Open cluster
Abstract: HD 15137 is an intriguing runaway O-type binary system that offers a rare opportunity to explore the mechanism by which it was ejected from the open cluster of its birth. Here we present recent blue optical spectra of HD 15137 and derive a new orbital solution for the spectroscopic binary and physical parameters of the O star primary. We also present the first XMM-Newton observations of the system. Fits of the EPIC spectra indicate soft, thermal X-ray emission consistent with an isolated O star. Upper limits on the undetected hard X-ray emission place limits on the emission from a proposed compact companion in the system, and we rule out a quiescent neutron star in the propellor regime or a weakly accreting neutron star. An unevolved secondary companion is also not detected in our optical spectra of the binary, and it is difficult to conclude that a gravitational interaction could have ejected this runaway binary with a low mass optical star. HD 15137 may contain an elusive neutron star in the ejector regime or a quiescent black hole with conditions unfavorable for accretion at the time of our observations., Accepted to AJ
Published: 2010
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21. Discovery of High-Energy Gamma-Ray Pulsations from PSR J2021+3651 with AGILE

Author: Marco Tavani, Mallory S. E. Roberts, A. Giuliani, Maura McLaughlin, A. Pellizzoni, Scott M. Ransom, Fernando Camilo, Jules P. Halpern, Eric V. Gotthelf, and R. Mukherjee
Subjects: Physics, Photon, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Gamma ray, Green Bank Telescope, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Ephemeris, Pulse (physics), Pulsar, Space and Planetary Science, Observatory
Abstract: Discovered after the end of the Compton Gamma-Ray Observatory mission, the radio pulsar PSR J2021+3651 was long considered a likely counterpart of the high-energy gamma-ray source 2CG 075+00 = 3EG J2021+3716 = GeV J2020+3658, but it could not be confirmed due to the lack of a contemporaneous radio pulsar ephemeris to fold the sparse, archival gamma-ray photons. Here, we report the discovery of gamma-ray pulsations from PSR J2021+3651 in the 100-1500 MeV range using data from the AGILE satellite gathered over 8 months, folded on a densely sampled, contemporaneous radio ephemeris obtained for this purpose at the Green Bank Telescope. The gamma-ray pulse consists of two sharp peaks separated by 0.47+/-0.01 cycles. The single radio pulse leads the first gamma-ray peak by 0.165+/-0.010 cycles. These properties are similar to those of other gamma-ray pulsars, and the phase relationship of the peaks can be interpreted in the context of the outer-gap accelerator model for gamma-ray emission. Pulse-phase resolved images show that there is only one dominant source, AGL J2020.5+3653 = PSR J2021+3651 in the region previously containing confused sources 3EG J2021+3716 and 3EG J2016+3657., Comment: 4 pages, 4 figures. to appear in The Astrophysical Journal Letters
Published: 2008
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22. Discovery of a New X‐Ray Filled Radio Supernova Remnant around the Pulsar Wind Nebula in 3EG J1809−2328

Author: Mallory S. E. Roberts and Crystal L. Brogan
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Pulsar wind nebula, Supernova, Pulsar, Space and Planetary Science, Coincident, ROSAT, Astrophysics::Solar and Stellar Astrophysics, Supernova remnant, Astrophysics::Galaxy Astrophysics
Abstract: We report the discovery of a partial ~2deg. diameter non-thermal radio shell coincident with Taz, the pulsar wind nebula (PWN) in the error box of the apparently variable gamma-ray source 3EG J1809-2328. We propose that this radio shell is a newly identified supernova remnant (SNR G7.5-1.7) associated with the PWN. The SNR surrounds an amorphous region of thermal X-rays detected in archival ROSAT and ASCA observations putting this system in the mixed-morphology class of supernova remnants. G7.5-1.7 is the fifth such supernova remnant coincident with a bright GeV source, and the fourth containing a pulsar wind nebulae., Comment: 7 pages, 3 figures, to appear in The Astrophysical Journal
Published: 2008
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23. Properties and Evolution of the Redback Millisecond Pulsar Binary PSR J2129-0429

Author: Thomas A. Prince, Branimir Sesar, Ashish Mahabal, Fernando Camilo, Eran O. Ofek, E. Sterl Phinney, Mallory S. E. Roberts, Rene P. Breton, Sumin Tang, Jason W. T. Hessels, David L. Kaplan, Jason Surace, David M. Russell, Andrew J. Drake, Eric C. Bellm, Sumit Dahal, Russ R. Laher, Fraser Lewis, David Levitan, Scott M. Ransom, S. G. Djorgovski, and Varun Bhalerao
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar, Millisecond pulsar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Green Bank Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Orbital period, Light curve, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Asteroid, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: PSR J2129-0429 is a "redback" eclipsing millisecond pulsar binary with an unusually long 15.2 hour orbit. It was discovered by the Green Bank Telescope in a targeted search of unidentified Fermi gamma-ray sources. The pulsar companion is optically bright (mean $m_R = 16.6$ mag), allowing us to construct the longest baseline photometric dataset available for such a system. We present ten years of archival and new photometry of the companion from LINEAR, CRTS, PTF, the Palomar 60-inch, and LCOGT. Radial velocity spectroscopy using the Double-Beam Spectrograph on the Palomar 200-inch indicates that the pulsar is massive: $1.74\pm0.18 M_\odot$. The G-type pulsar companion has mass $0.44\pm0.04 M_\odot$, one of the heaviest known redback companions. It is currently 95\% Roche-lobe filling and only mildly irradiated by the pulsar. We identify a clear 13.1 mmag yr$^{-1}$ secular decline in the mean magnitude of the companion as well as smaller-scale variations in the optical lightcurve shape. This behavior may indicate that the companion is cooling. Binary evolution calculations indicate that PSR J2129-0429 has an orbital period almost exactly at the bifurcation period between systems that converge into tighter orbits as black widows and redbacks and those that diverge into wider pulsar--white dwarf binaries. Its eventual fate may depend on whether it undergoes future episodes of mass transfer and increased irradiation., Comment: 13 pages, 8 figures. Submitted to ApJ
Published: 2015
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24. Pulsar Wind Nebulae in the SKA era

Author: Andrea Possenti, Ben Stappers, Jason W. T. Hessels, Joseph D. Gelfand, Chi-Yung Ng, Mallory S. E. Roberts, and Rene P. Breton
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Ancient history, 7. Clean energy, 01 natural sciences, Abu dhabi, Pulsar, 13. Climate action, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Neutron stars lose the bulk of their rotational energy in the form of a pulsar wind: an ultra-relativistic outflow of predominantly electrons and positrons. This pulsar wind significantly impacts the environment and possible binary companion of the neutron star, and studying the resultant pulsar wind nebulae is critical for understanding the formation of neutron stars and millisecond pulsars, the physics of the neutron star magnetosphere, the acceleration of leptons up to PeV energies, and how these particles impact the interstellar medium. With the SKA1 and the SKA2, it could be possible to study literally hundreds of PWNe in detail, critical for understanding the many open questions in the topics listed above., Comments: 10 pages, 3 figures, to be published in: "Advancing Astrophysics with the Square Kilometre Array", Proceedings of Science, PoS(AASKA14)
Published: 2015

25. Discovery and Follow-up of Rotating Radio Transients with the Green Bank and LOFAR Telescopes

Author: Anne M. Archibald, Jason W. T. Hessels, Lina Levin, Fredrick A. Jenet, Jason Boyles, Maura McLaughlin, J. van Leeuwen, Scott M. Ransom, X. Siemens, Mallory S. E. Roberts, Ryan S. Lynch, Ingrid H. Stairs, Joseph K. Swiggum, David L. Kaplan, C. Karako-Argaman, E. C. Madsen, V. M. Kaspi, V. I. Kondratiev, Kevin Stovall, Duncan R. Lorimer, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Green Bank Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, LOFAR, Astrophysics::Cosmology and Extragalactic Astrophysics, Low frequency, 01 natural sciences, Activity spectrum, Pulsar, Space and Planetary Science, 0103 physical sciences, Dispersion (optics), Radio frequency, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Fourier domain
Abstract: We have discovered 21 Rotating Radio Transients (RRATs) in data from the Green Bank Telescope (GBT) 350-MHz Drift-scan and the Green Bank North Celestial Cap pulsar surveys using a new candidate sifting algorithm. RRATs are pulsars with sporadic emission that are detected through their bright single pulses rather than Fourier domain searches. We have developed {\tt RRATtrap}, a single-pulse sifting algorithm that can be integrated into pulsar survey data analysis pipelines in order to find RRATs and Fast Radio Bursts. We have conducted follow-up observations of our newly discovered sources at several radio frequencies using the GBT and Low Frequency Array (LOFAR), yielding improved positions and measurements of their periods, dispersion measures, and burst rates, as well as phase-coherent timing solutions for four of them. The new RRATs have dispersion measures (DMs) ranging from 15 to 97 pc cm$^{-3}$, periods of 240 ms to 3.4 s, and estimated burst rates of 20 to 400 pulses hr$^{-1}$ at 350 MHz. We use this new sample of RRATs to perform statistical comparisons between RRATs and canonical pulsars in order to shed light on the relationship between the two populations. We find that the DM and spatial distributions of the RRATs agree with those of the pulsars found in the same survey. We find evidence that slower pulsars (i.e. $P>200$ ms) are preferentially more likely to emit bright single pulses than are faster pulsars ($P, 18 pages, 13 figures, 5 tables, published in ApJ
Published: 2015
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26. A Survey of 56 Midlatitude EGRET Error Boxes for Radio Pulsars

Author: Mallory S. E. Roberts, Scott M. Ransom, Margaret A. Livingstone, J. W. T. Hessels, Fronefield Crawford, V. M. Kaspi, and C. R. Tam
Subjects: Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Latitude, Luminosity, Pulsar, Millisecond pulsar, 0103 physical sciences, medicine, Egret, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Confusion, Physics, biology, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, biology.organism_classification, Space and Planetary Science, Middle latitudes, medicine.symptom
Abstract: We have conducted a radio pulsar survey of 56 unidentified gamma-ray sources from the 3rd EGRET catalog which are at intermediate Galactic latitudes (5 deg. < |b| < 73 deg.). For each source, four interleaved 35-minute pointings were made with the 13-beam, 1400-MHz multibeam receiver on the Parkes 64-m radio telescope. This covered the 95% error box of each source at a limiting sensitivity of about 0.2 mJy to pulsed radio emission for periods P > 10 ms and dispersion measures < 50 pc cm-3. Roughly half of the unidentified gamma-ray sources at |b| > 5 deg. with no proposed active galactic nucleus counterpart were covered in this survey. We detected nine isolated pulsars and four recycled binary pulsars, with three from each class being new. Timing observations suggest that only one of the pulsars has a spin-down luminosity which is even marginally consistent with the inferred luminosity of its coincident EGRET source. Our results suggest that population models, which include the Gould belt as a component, overestimate the number of isolated pulsars among the mid-latitude Galactic gamma-ray sources and that it is unlikely that Gould belt pulsars make up the majority of these sources. However, the possibility of steep pulsar radio spectra and the confusion of terrestrial radio interference with long-period pulsars (P > 200 ms) having very low dispersion measures (< 10 pc cm-3, expected for sources at a distance of less than about 1 kpc) prevent us from strongly ruling out this hypothesis. Our results also do not support the hypothesis that millisecond pulsars make up the majority of these sources. Non-pulsar source classes should therefore be further investigated as possible counterparts to the unidentified EGRET sources at intermediate Galactic latitudes., 24 pages, including 4 figures and 3 tables. Accepted for publication in ApJ
Published: 2006
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27. X‐Ray Bursts from the Transient Magnetar Candidate XTE J1810−197

Author: Craig B. Markwardt, Jean H. Swank, Chryssa Kouveliotou, Fotis P. Gavriil, Mallory S. E. Roberts, Alaa I. Ibrahim, Victoria M. Kaspi, Mark H. Finger, and P. M. Woods
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Proportional counter, Flux, Astronomy and Astrophysics, Astrophysics, Radius, Magnetar, Spectral line, Space and Planetary Science, Black-body radiation, Emission spectrum, Equivalent width
Abstract: We have discovered four X-ray bursts, recorded with the Rossi X-ray Timing Explorer Proportional Counter Array between 2003 September and 2004 April, that we show to originate from the transient magnetar candidate XTE J1810-197. The burst morphologies consist of a short spike or multiple spikes lasting ~1 s each followed by extended tails of emission where the pulsed flux from XTE J1810-197 is significantly higher. The burst spikes are likely correlated with the pulse maxima, having a chance probability of a random phase distribution of 0.4%. The burst spectra are best fit to a blackbody with temperatures 4-8 keV, considerably harder than the persistent X-ray emission. During the X-ray tails following these bursts, the temperature rapidly cools as the flux declines, maintaining a constant emitting radius after the initial burst peak. During the brightest X-ray tail, we detect a narrow emission line at 12.6 keV with an equivalent width of 1.4 keV and a probability of chance occurrence less than 4 x 10^-6. The temporal and spectral characteristics of these bursts closely resemble the bursts seen from 1E 1048.1-5937 and a subset of the bursts detected from 1E 2259+586, thus establishing XTE J1810-197 as a magnetar candidate. The bursts detected from these three objects are sufficiently similar to one another, yet significantly different from those seen from soft gamma repeaters, that they likely represent a new class of bursts from magnetar candidates exclusive (thus far) to the anomalous X-ray pulsar-like sources., Accepted for publication in ApJ. 26 pages and 11 figures
Published: 2005
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28. Pulsar Wind Nebulae in Egret Error Boxes

Author: Jason W. T. Hessels, Crystal L. Brogan, Cherry Ng, Mallory S. E. Roberts, Roger W. Romani, and Bryan Gaensler
Subjects: Physics, biology, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, biology.organism_classification, Spectral line, Pulsar, Space and Planetary Science, Coincident, Egret, Radio imaging, Astrophysics::Galaxy Astrophysics
Abstract: A remarkable number of pulsar wind nebulae (PWN) are coincident with EGRET gamma-ray sources. X-ray and radio imaging studies of unidentified EGRET sources have resulted in the discovery of at least 6 new pulsar wind nebulae (PWN). Stationary PWN (SPWN) appear to be associated with steady EGRET sources with hard spectra, typical for gamma-ray pulsars. Their toroidal morphologies can help determine the geometry of the pulsar which is useful for constraining models of pulsed gamma-ray emission. Rapidly moving PWN (RPWN) with more cometary morphologies seem to be associated with variable EGRET sources in regions where the ambient medium is dense compared to what is typical for the ISM., 8 pages, 5 figures, to appear in the proceedings of "The Multiwavelength Approach to Unidentified Sources", ed. G. Romero & K.S. Cheng
Published: 2005
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29. Pulsars and their nebulae as EGRET sources

Author: Mallory S. E. Roberts
Subjects: Atmospheric Science, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Aerospace Engineering, Magnetosphere, Astrophysics, Pulsar, Millisecond pulsar, Astrophysics::Solar and Stellar Astrophysics, Egret, education, Astrophysics::Galaxy Astrophysics, Physics, Nebula, education.field_of_study, biology, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Galactic plane, biology.organism_classification, Geophysics, Space and Planetary Science, Physics::Space Physics, General Earth and Planetary Sciences, X-ray pulsar
Abstract: At the end of the EGRET mission, only 6-8 Galactic sources had been identified as young pulsars. Since then, several energetic pulsars have been discovered in EGRET error boxes along the Galactic plane, as well as several pulsar wind nebulae from which pulsations have not yet been discovered. Some of these nebulae are associated with moderately variable EGRET sources, suggesting that the gamma-ray emission might be coming from the nebula rather than from the pulsar magnetosphere. There is also a population of unidentified EGRET sources at mid-Galactic latitudes which have been proposed to be either nearby middle-aged pulsars or millisecond pulsars. I review the current status of observational studies of pulsars associated with EGRET sources and what they suggest the upcoming AGILE and GLAST gamma-ray missions might observe., Comment: 11 pages, proceedings of talk given at "Young Neutron Stars and Supernova Remnants" session of 35th COSPAR meeting held in Paris, France. To appear in Advances in Space Research
Published: 2005
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30. PSR J2021+3651: a new γ-ray pulsar candidate

Author: Fronefield Crawford, Scott M. Ransom, Paulo C. C. Freire, J. W. T. Hessels, Mallory S. E. Roberts, V. M. Kaspi, and D. R. Lorimer
Subjects: Physics, Rotation period, Atmospheric Science, 010308 nuclear & particles physics, Astrophysics (astro-ph), Pulsar planet, FOS: Physical sciences, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Pulsar wind nebula, Galaxy, Luminosity, Geophysics, Pulsar, Space and Planetary Science, Millisecond pulsar, 0103 physical sciences, General Earth and Planetary Sciences, Arecibo Observatory, 010303 astronomy & astrophysics
Abstract: The COS B high energy gamma-ray source 2CG 075+00, also known as GeV J2020+3658 or 3EG J2021+3716, has avoided identification with a low energy counterpart for over twenty years. We present a likely identification with the discovery and subsequent timing of a young and energetic pulsar, PSR J2021+3651, with the Wideband Arecibo Pulsar Processor at the Arecibo Observatory. PSR J2021+3651 has a rotation period P = 104ms and Pdot = 9.6 x 10^{-14}, implying a characteristic age T_c = 17kyr and a spin-down luminosity Edot = 3.4 x 10^{36} erg s^{-1}. The pulsar is also coincident with the ASCA source AX J2021.1+3651. The implied luminosity of the associated X-ray source suggests the X-ray emission is dominated by a pulsar wind nebula unresolved by ASCA. The pulsar's unexpectedly high dispersion measure DM = 371 pc cm^{-3} and the d > 10kpc DM distance pose a new question: is PSR J2021+3651 an extremely efficient gamma-ray pulsar at the edge of the Galaxy? This is a question for AGILE and GLAST to answer., 6 pages, 2 figures, to appear in "High Energy Studies of Supernova Remnants and Neutron Stars" (COSPAR 2002, Houston), Advances in Space Research, in press
Published: 2004
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31. The Pulsar Wind Nebula in G11.2−0.3

Author: C. R. Tam, Eric V. Gotthelf, Gautam Vasisht, M. Lyutikov, Nobuyuki Kawai, Michael J. Pivovaroff, Victoria M. Kaspi, and Mallory S. E. Roberts
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Pulsar wind nebula, law.invention, Radio telescope, Pulsar, law, Observatory, Stars: Neutron, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Stars: Pulsars: General, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Nebula, Astrophysics (astro-ph), Stars: Pulsars: Individual: Alphanumeric: AX J1811.5-1926, Astronomy and Astrophysics, Synchrotron, Supernova, X-Rays: General, 13. Climate action, Space and Planetary Science, Stars: Supernovae: Individual: Alphanumeric: G11.2-0.3
Abstract: We present an X-ray and radio study of the wind nebula surrounding the central pulsar PSR J1811-1925 in the supernova remnant G11.2-0.3. Using high resolution data obtained with the Chandra X-ray observatory and with the VLA radio telescope we show the X-ray and radio emission is asymmetric around the pulsar, despite the latter's central position in the very circular shell. The new X-ray data allow us to separate the synchrotron emission of the pulsar wind nebula from the surrounding thermal emission and that from the pulsar itself. Based on X-ray data from two epochs, we observe temporal variation of the location of X-ray hot spots near the pulsar, indicating relativistic motion. We compare thermal emission observed within the shell, which may be associated with the forward shock of the pulsar wind nebula, to thermal emission from a nearby portion of the remnant shell, the temperature of which implies an expansion velocity consistent with the identification of the remnant with the historical event of 386 A.D. The measured X-ray and radio spectral indices of the nebula synchrotron emission are found to be consistent with a single synchrotron cooling break. The magnetic field implied by the break frequency is anomalously large given the apparent size and age of the nebula if a spherical morphology is assumed, but is consistent with a bipolar morphology., 14 pages, 7 figures, submitted to the Astrophysical Journal
Published: 2003
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32. A Major Soft Gamma Repeater-like Outburst and Rotation Glitch in the No-longer-so-anomalous X-Ray Pulsar 1E 2259+586

Author: Fotis P. Gavriil, V. M. Kaspi, Deepto Chakrabarty, Joseph B. Jensen, Mallory S. E. Roberts, and P. M. Woods
Subjects: Physics, Infrared, Flux, Astronomy and Astrophysics, Astrophysics, Magnetar, 01 natural sciences, law.invention, Anomalous X-ray pulsar, Telescope, Amplitude, Pulsar, 13. Climate action, Space and Planetary Science, law, 0103 physical sciences, Glitch (astronomy), 010306 general physics, 010303 astronomy & astrophysics
Abstract: We report a major outburst from the Anomalous X-ray Pulsar 1E 2259+586, in which over 80 X-ray bursts were detected in four hours using the Rossi X-ray Timing Explorer. The bursts range in duration from 2 ms to 3 s and have fluences in the 2-10 keV band that range from 3 x 10^{-11} to 5 x 10^{-9} erg cm^{-2}. We simultaneously observed increases of the pulsed and persistent X-ray emission by over an order of magnitude relative to quiescent levels. Both decayed significantly during the course of our 14 ks observation. Correlated spectral hardening was also observed, with the spectrum softening during the observation. In addition, we observed a pulse profile change, in which the amplitudes of the two peaks in the pulse profile were swapped. The profile relaxed back to its pre-outburst morphology after ~6 days. The pulsar also underwent a sudden spin-up (df/f = 4 x 10^{-6}), followed by a large (factor of \~2) increase in spin-down rate which persisted for >18 days. We also observed, using the Gemini-North telescope, an infrared enhancement, in which the K_s (2.15 um) flux increased, relative to that measured in a observation made in 2000, by a factor of ~3, three days post-outburst. The IR counterpart then faded by a factor of ~2 one week later. In addition, we report an upper limit of 50 uJy on radio emission at 1.4 GHz two days post-outburst. The X-ray properties of this outburst are like those seen only in Soft Gamma Repeaters. This conclusively unifies Anomalous X-ray Pulsars and Soft Gamma Repeaters, as predicted uniquely by the magnetar model.
Published: 2003
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33. Spectral Components of the Radio Composite Supernova Remnant G11.2−0.3

Author: C. R. Tam, Victoria M. Kaspi, and Mallory S. E. Roberts
Subjects: Physics, Spectral index, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Alpha (navigation), 01 natural sciences, Pulsar wind nebula, Space and Planetary Science, 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We present a high-resolution radio study of the supernova remnant (SNR) G11.2-0.3 using archival VLA data. Spectral tomography is performed to determine the properties of this composite-type SNR's individual components, which have only recently been distinguished through X-ray observations. Our results indicate that the spectral index of the pulsar wind nebula (PWN), or plerion, is alpha_P ~ 0.25. We observe a spectral index of alpha_S ~ 0.56 throughout most of the SNR shell region, but also detect a gradient in alpha in the south-eastern component. We compare the spectral index and flux density with recent single-dish radio data of the source. Also, the radio efficiency and morphological properties of this PWN are found to be consistent with results for other known PWN systems., Comment: 9 pages, 5 figures, Accepted to the Astrophysical Journal
Published: 2002
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34. [ITAL]Chandra[/ITAL] Imaging of the Gamma-Ray Source G[CLC]e[/CLC]V J1809−2327

Author: Nobuyuki Kawai, Mallory S. E. Roberts, Roger W. Romani, and Timothy M. Braje
Subjects: Physics, Nebula, Pulsar, Wind model, Space and Planetary Science, Point source, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics, Common emitter
Abstract: We report on Chandra imaging observations of the Galactic Unidentified $\gamma$-ray source GEV J1809-2327, comparing the X-ray images with new VLA 1.46 GHz and 4.86 GHz maps. The X-ray images reveal a point source connected to a non-thermal X-ray/radio nebula, supporting a pulsar/wind model for the $\gamma$-ray emitter. We also detect numerous X-ray sources from the young stellar association in the adjacent HII region S32.
Published: 2002
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35. The High-frequency Radio Emission of the Galactic Center Magnetar SGR J1745–29 during a Transitional Period

Author: Chryssa Kouveliotou, Jonathan Granot, Guobao Zhang, Alexander J. van der Horst, Joseph D. Gelfand, Ersin Gogus, Hend Al Ali, Scott M. Ransom, and Mallory S. E. Roberts
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Period (periodic table), 010308 nuclear & particles physics, Galactic Center, Green Bank Telescope, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, High frequency, Magnetar, 01 natural sciences, Jansky, Pulse period, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: The origin of the high-frequency radio emission detected from several magnetars is poorly understood. In this paper, we report the ~40 GHz properties of SGR J1745-29 as measured using Jansky Very Large Array (JVLA) and Robert C. Byrd Green Bank Telescope (GBT) observations between 2013 October 26 and 2014 May 31. Our analysis of a Q-band (45 GHz) GBT observation on 2014 April 10 resulted in the earliest detection of pulsed radio emission at high frequencies (>20 GHz); we found that the average pulse has a singly peaked profile with width ~75 ms (~2% of the 3.764 s pulse period) and an average pulsed flux density of ~100 mJy. We also detected very bright, short (, 9 pages, 4 figure, 2 tables, published in The Astrophysical Journal
Published: 2017
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36. Spatially Resolving the very high Energy Emission from MGRO J2019+37 with VERITAS

Author: I. Telezhinsky, Jamie Holder, S. Vincent, A. Popkow, L. C. Reyes, A. Bouvier, Abraham D. Falcone, Eric V. Gotthelf, Karlen Shahinyan, Sinéad M. Griffin, P. Fortin, P. Kaaret, Jean-Francois Rajotte, Ralph Bird, T. Aune, B. Behera, Daniel Nieto, J. P. Finley, Martin Pohl, C. A. Johnson, M. Kertzman, D. Staszak, D. S. Hanna, T. B. Humensky, J. Dumm, Wystan Benbow, K. Ragan, A. O'Faolain de Bhroithe, L. Ciupik, F. Krennrich, John L. Quinn, V. Bugaev, E. Aliu, R. A. Ong, Matthias Beilicke, B. Zitzer, Oleg Kargaltsev, J. V. Tucci, S. T. Griffiths, Mallory S. E. Roberts, Gernot Maier, K. Berger, J. Grube, Manel Errando, A. McCann, Q. Feng, N. Galante, Y. Khassen, H. Prokoph, Amanda Weinstein, S. McArthur, Xuhui Chen, A. N. Otte, S. P. Wakely, M. P. Connolly, Dirk Pandel, A. W. Smith, S. Federici, A. S Madhavan, David Kieda, Henrike Fleischhack, Gordon T. Richards, E. Roache, G. H. Gillanders, Reshmi Mukherjee, G. Hughes, M. J. Lang, A. Wilhelm, Matteo Cerruti, Amy Furniss, David A. Williams, Wei Cui, P. T. Reynolds, Geza Gyuk, Vikram V. Dwarkadas, J. Tyler, Lucy Fortson, P. Moriarty, N. H. Park, J. Millis, J. H. Buckley, G. H. Sembroski, and R. Welsing
Subjects: stars, Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, supernovae : individual (ctb 87), galactic plane, 01 natural sciences, Spectral line, Pulsar, pulsars : individual (psr j2021+3651), Observatory, 0103 physical sciences, pulsar wind nebula, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, cygnus region, hess, 010308 nuclear & particles physics, Star formation, Institut für Physik und Astronomie, Astronomy, Astronomy and Astrophysics, gamma-ray emission, gamma rays : stars, psr j2021+3651, milagro, Supernova, 13. Climate action, Space and Planetary Science, Milagro, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, discovery, associations
Abstract: We present very high energy (VHE) imaging of MGRO J2019+37 obtained with the VERITAS observatory. The bright extended ($\sim2^{\circ}$) unidentified Milagro source is located towards the rich star formation region Cygnus-X. MGRO J2019+37 is resolved into two VERITAS sources. The faint point-like source VER J2016+371 overlaps CTB 87, a filled-center remnant (SNR) with no evidence of a supernova remnant shell at the present time. Its spectrum is well fit in the $0.65 - 10$ TeV energy range by a power-law model with photon index $2.3\pm0.4$. VER J2019+368 is a bright extended ($\sim1^{\circ}$) source, that likely accounts for the bulk of the Milagro emission and is notably coincident with PSR J2021+3651 and the star formation region Sh 2-104. Its spectrum in the range $1-30$ TeV is well fit with a power-law model of photon index $1.75\pm0.3$, among the hardest values measured in the VHE band, comparable to that observed near Vela-X. We explore the unusual spectrum and morphology in the radio and X-ray bands to constrain possible emission mechanisms for this source., 9 pages, 8 figures, accepted for publication in the Astrophysical Journal
Published: 2014
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37. The Green Bank Northern Celestial Cap Pulsar Survey. I: Survey Description, Data Analysis, and Initial Results

Author: J. Hinojosa, Alejandro Garcia, J. van Leeuwen, S. Leake, Fredrick A. Jenet, Ingrid H. Stairs, Jason W. T. Hessels, J. G. Martinez, V. M. Kaspi, Kevin Stovall, A. N. Walker, Duncan R. Lorimer, V. I. Kondratiev, A. J. Ford, Anne M. Archibald, M. D. Rohr, Maura McLaughlin, Scott M. Ransom, S. Banaszak, D. Day, J. Flanigan, David L. Kaplan, C. Karako-Argaman, Christopher M. Biwer, G. Lunsford, B. L. Wells, Jason Boyles, Mallory S. E. Roberts, Ryan S. Lynch, A. Mata, Xavier Siemens, L. P. Dartez, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar timing array, Pulsar, Millisecond pulsar, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, 010308 nuclear & particles physics, Green Bank Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy, 13. Climate action, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena
Abstract: We describe an ongoing search for pulsars and dispersed pulses of radio emission, such as those from rotating radio transients (RRATs) and fast radio bursts (FRBs), at 350 MHz using the Green Bank Telescope. With the Green Bank Ultimate Pulsar Processing Instrument, we record 100 MHz of bandwidth divided into 4,096 channels every 81.92 $\mu s$. This survey will cover the entire sky visible to the Green Bank Telescope ($\delta > -40^\circ$, or 82% of the sky) and outside of the Galactic Plane will be sensitive enough to detect slow pulsars and low dispersion measure ($, Comment: 18 pages, 10 figures, 5 tables, accepted by ApJ
Published: 2014

38. A millisecond pulsar in a stellar triple system

Author: Mallory S. E. Roberts, J. van Leeuwen, Duncan R. Lorimer, Jason Boyles, David L. Kaplan, C. Karako-Argaman, Anne M. Archibald, Aaron Berndsen, Ryan S. Lynch, Victoria M. Kaspi, Scott M. Ransom, A. Schechtman-Rook, Maura McLaughlin, V. I. Kondratiev, Adam Deller, R. Rosen, Shami Chatterjee, Kevin Stovall, M. H. van Kerkwijk, Ingrid H. Stairs, Jason W. T. Hessels, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: General relativity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Binary pulsar, General Relativity and Quantum Cosmology, Pulsar, Millisecond pulsar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, Solar mass, Multidisciplinary, 010308 nuclear & particles physics, Astronomy, White dwarf, Orbit, Neutron star, Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract: Gravitationally bound three-body systems have been studied for hundreds of years and are common in our Galaxy. They show complex orbital interactions, which can constrain the compositions, masses, and interior structures of the bodies and test theories of gravity, if sufficiently precise measurements are available. A triple system containing a radio pulsar could provide such measurements, but the only previously known such system, B1620-26 (with a millisecond pulsar, a white dwarf, and a planetary-mass object in an orbit of several decades), shows only weak interactions. Here we report precision timing and multi-wavelength observations of PSR J0337+1715, a millisecond pulsar in a hierarchical triple system with two other stars. Strong gravitational interactions are apparent and provide the masses of the pulsar (1.4378(13) Msun, where Msun is the solar mass and the parentheses contain the uncertainty in the final decimal places) and the two white dwarf companions (0.19751(15) Msun and 0.4101(3) Msun), as well as the inclinations of the orbits (both approximately 39.2 degrees). The unexpectedly coplanar and nearly circular orbits indicate a complex and exotic evolutionary past that differs from those of known stellar systems. The gravitational field of the outer white dwarf strongly accelerates the inner binary containing the neutron star, and the system will thus provide an ideal laboratory in which to test the strong equivalence principle of general relativity., 17 pages, 3 figures, 1 table. Published online by Nature on 5 Jan 2014. Extremely minor differences with published version may exist
Published: 2014

39. Two Young Radio Pulsars Coincident with EGRET Sources

Author: A. Possenti, Bryan Gaensler, Mallory S. E. Roberts, N. P. F. McKay, Andrew Lyne, Michael Kramer, Ingrid H. Stairs, Fernando Camilo, V. M. Kaspi, N. D'Amico, R. N. Manchester, Fronefield Crawford, and J. F. Bell
Subjects: Physics, biology, Gamma ray, Astronomy, Astronomy and Astrophysics, Observable, Astrophysics, biology.organism_classification, Dipole, Pulsar, Space and Planetary Science, Observatory, Millisecond pulsar, Coincident, Egret
Abstract: We report the discovery and follow-up timing observations of two young energetic radio pulsars. PSR J1420-6048 has a period P = 68 ms and period derivative = 83 × 10-15, implying a characteristic age τc = 13 kyr and a surface dipole magnetic field strength B = 2.4 × 1012 G. PSR J1837-0604 has P = 96 ms and = 45 × 10-15, implying τc = 34 kyr and B = 2.1 × 1012 G. The two objects have large spin-down luminosities, and, on the basis of an empirical comparison of their properties with those of other young radio pulsars, they are expected to be observable as pulsed γ-ray sources. In fact, they lie within the error circles of γ-ray sources detected by the EGRET instrument on the Gamma Ray Observatory. We show that the pulsars are plausibly associated with the EGRET sources.
Published: 2001
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40. The ASCA Catalog of Potential X‐Ray Counterparts of GeV Sources

Author: Roger W. Romani, Nobuyuki Kawai, and Mallory S. E. Roberts
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Synchrotron, law.invention, Pulsar, Cover (topology), Space and Planetary Science, law, Astrophysics::Galaxy Astrophysics
Abstract: We present a catalog of 2-10 keV ASCA Gas Imaging Spectrometer images of fields containing bright sources of GeV emission. The images cover $\sim 85%$ of the 95% confidence position contour for 28 of the 30 sources with $> 1$ GeV fluxes above $4\times 10^{-8}$ ph ${\rm cm}^{-2} {\rm s}^{-1}$. We find an excess of hard X-ray sources with $F_{2-10 keV} \ga 10^{-12}$ ergs ${\rm cm}^{-2} {\rm s}^{-1}$ positionally coincident with unidentified sources of GeV emission. We comment on radio-loud and radio-quiet pulsar candidates, as well as several SNR and massive binaries as possible sources of the GeV emission. We also find evidence for a class of variable $\gamma-$ray sources associated with extended regions of hard X-ray emission, and propose that for these sources, a significant percentage of the $\gamma-$ray emission is generated in synchrotron nebulae surrounding fast, young pulsars., Comment: 23 pages, 5 figures, to appear in the Astrophysical Journal Supplements. Colour images and auxilliary files available at http://astro.stanford.edu/~mallory/survey.html
Published: 2001
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41. The 'Rabbit': A Potential Radio Counterpart of GeV J1417−6100

Author: Simon Johnston, Roger W. Romani, Anne J. Green, and Mallory S. E. Roberts
Subjects: Physics, Nebula, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Shell (structure), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Ellipse, law.invention, Telescope, Pulsar, Space and Planetary Science, law, Coincident, Astrophysics::Solar and Stellar Astrophysics, Rabbit (cipher)
Abstract: We have mapped the radio emission in the error ellipse of GeV J1417-6100 (2EGS J1418-6049) at 13cm and 20cm using the Australia Telescope Compact Array. We find a large shell with extended wings, at the edge of which is a non-thermal, polarized structure with a center filled morphology (the `Rabbit'), coincident with an extended, hard X-ray source. We discuss the various sources seen within the ellipse as potential counterparts of the gamma-ray source. We conclude that the most likely scenario is that the Rabbit is a wind nebula surrounding a radio-quiet gamma-ray pulsar., 14 pages, 6 figures, to be published in the Astrophysical Journal
Published: 1999
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42. ASCAObservations of the Unidentified EGRET Source 2EGS J1418−6049

Author: Roger W. Romani and Mallory S. E. Roberts
Subjects: Physics, Nebula, Active galactic nucleus, biology, Pulsar, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Egret, Astronomy, Astronomy and Astrophysics, Astrophysics, biology.organism_classification, Astrophysics::Galaxy Astrophysics
Abstract: In a 40 ks ASCA exposure of the GeV EGRET error box of the unidentified source 2EGS J1418-6049, we observe diffuse emission surrounding several unusual hard spectrum X-ray sources. Two of these sources have plausible identifications as absorbed active galactic nuclei (AGNs). Our best candidate for the EGRET source counterpart is an extended nonthermal object, which we argue to be a wind nebula surrounding a pulsar with characteristic age τ ~ 104.5 yr. We also discuss optical and radio data supporting the proposal that the GeV source is a young energetic pulsar. This analysis demonstrates how hard X-ray observations can significantly constrain the nature of GeV γ-ray sources.
Published: 1998
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43. The Ejection of Runaway Massive Binaries

Author: Mallory S. E. Roberts, Tabetha S. Boyajian, Erika D. Grundstrom, M. Virginia McSwain, and Scott M. Ransom
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Binary number, Astronomy and Astrophysics, Astrophysics, Gravitation, Stars, Supernova, Space and Planetary Science, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Open cluster
Abstract: The runaway O-type stars HD 14633 and HD 15137 are both SB1 systems that were probably ejected from the open cluster NGC 654. Were these stars dynamically ejected by close gravitational encounters in the dense cluster, or did the binaries each receive a kick from a supernova in one member? We present new results from our investigation of the optical, X-ray, and radio properties of these binary systems to discuss the probable ejection scenarios. We argue that these binaries may have been ejected via dynamical interactions in the dense cluster environment.
Published: 2006
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44. Enhanced sensitivity of the LIGO gravitational wave detector by using squeezed states of light

Author: Ludovico Carbone, P. Couvares, Benno Willke, K. Wiesner, A. F. Brooks, R. Kurdyumov, S. Kandhasamy, Edwin J. Son, Jordan Camp, Alessandra Buonanno, D. Feldbaum, T. Meier, O. Bock, Stefan Hild, I. Yakushin, G. Mendell, G. Mazzolo, Ryan DeRosa, R. Engel, P. Wessels, T. Denker, L. Sammut, P. Leaci, D. Barker, D. Nolting, C. Aulbert, S. E. Whitcomb, A. Cumming, J. Bowers, Z. Frei, H. Zhu, A. M. Gretarsson, F. Mokler, David H. Shoemaker, Holger J. Pletsch, John Worden, J. K. Blackburn, C. Osthelder, Francesco Salemi, Sheila Rowan, C. I. Torrie, Jan Harms, A. S. Sengupta, Jöran Bauchrowitz, N. Beveridge, S. E. Dwyer, F. Magana-Sandoval, Satyanarayan Ray Pitambar Mohapatra, Honam Yum, Walter Winkler, A. S. Markosyan, M. T. Hartman, S. Roddy, Daniel Friedrich, Evan Goetz, Harald Lück, D. O. Bridges, Rebecca Fisher, Jeffery Kline, Xuan Wang, J. D. Lough, C. J. Bell, S. Meshkov, Seog Oh, E. Nishida, T. T. Fricke, Matthew Evans, J. Garcia, C. C. Arceneaux, Ilya Mandel, E. Deleeuw, Prayush Kumar, Jessica McIver, M. Factourovich, Rana X. Adhikari, B. Machenschalk, Alexander Khalaidovski, Haixing Miao, S. L. Danilishin, J. Betzwieser, R. Inta, Lee Samuel Finn, Stephen S. Eikenberry, B. K. Kim, R. L. Ward, C. Peralta, M. Shaltev, Peter Aufmuth, K. L. Dooley, F. Donovan, Lisa Barsotti, A. Stochino, G. P. Newton, M. Fyffe, Yueh-Feng Liu, Chris Pankow, A. Singer, Atsushi J. Nishizawa, N. Zotov, K. Mason, J. N. Marx, László Á. Gergely, Gabriela Gonzalez, H. J. Jang, K. Haughian, B. Bland, C. Affeldt, K. Venkateswara, Sanjeev Dhurandhar, A. Nitz, S. Klimenko, Y. Wan, Evan Ochsner, A. Effler, Henning Kaufer, A. Perreca, A. J. Weinstein, Guenakh Mitselmakher, J. R. Leong, M. A. Barton, Carl L. Rodriguez, Laura Cadonati, Bastian Schulz, Richard A. Matzner, H. Yamamoto, H. R. Paris, R. Taylor, Steve Drasco, T. Huynh-Dinh, J. B. Kanner, A. M. Sergeev, H. Overmier, Kazuhiro Hayama, D. Talukder, C. V. Torres, I. W. Harry, F. Brückner, E. Amador Ceron, Xin Chen, R. M. Martin, Bala R. Iyer, P. T. Baker, Meng Wang, D. Sellers, Kip S. Thorne, T. Chalermsongsak, Alessandro Bertolini, S. Privitera, T. Etzel, T. Reed, M. Damjanic, T. P. Bodiya, P. T. Beyersdorf, M. V. van der Sluys, M. S. Shahriar, Sunil Susmithan, Robert Stone, Q. Chu, Xavier Siemens, Salvatore Vitale, Jolien D. E. Creighton, S. Caride, Lindy Blackburn, M. Landry, S. Doravari, H. P. Daveloza, Scott Koranda, Albrecht Rüdiger, Hyun Lee, Christian D. Ott, K. Holt, Mallory S. E. Roberts, Fabio Postiglione, J. S. Kissel, L. Matone, V. Sandberg, V. Lhuillier, C. S. Unnikrishnan, Innocenzo M. Pinto, Matthew West, Marc Favata, P. Kwee, K. A. Thorne, W. Z. Korth, Susan M. Scott, Hyung Mok Lee, Teviet Creighton, Stephen Fairhurst, Kieran Craig, Christopher John Messenger, Chad Hanna, Zhen Liu, Yi Chen, Xing-Jiang Zhu, V. P. Mitrofanov, V. Raymond, A. S. Stroeer, J. C. Batch, Badri Krishnan, B. J. J. Slagmolen, D. Hoak, Chiara M. F. Mingarelli, Jonathan R. Gair, A. Grant, Roger Jones, A. R. Wade, G. Kuehn, C. M. Mow-Lowry, Patrick Brady, N. A. Gordon, D. D. Brown, C. R. Ramet, P. J. Veitch, Bernard F. Whiting, J. R. Sanders, Rainer Weiss, R. W. P. Drever, Manuel Meyer, T. D. Abbott, Trevor Sidery, Sergey P. Vyatchanin, David Jones, D. Amariutei, J. O'Dell, T. Dayanga, W. W. Johnson, N. A. Lockerbie, L. Wallace, Riccardo Bassiri, Joshua Yablon, C. Wilkinson, K. A. Hodge, V. Kringel, J. Breyer, L. Zhang, C. Gray, D. Fazi, Imre Bartos, D. J. White, E. Maros, C. Zhao, Alicia M. Sintes, C. Poux, Marco Cavaglia, Patrick J. Sutton, M-K. Fujimoto, P. Thomas, Archana Pai, M. Jacobson, B. Moe, Odylio D. Aguiar, H. Radkins, R. Frey, S. H. Huttner, V. Quetschke, Bangalore Suryanarayana Sathyaprakash, E. Black, D. Atkinson, Thanh Vinh Nguyen, David Blair, Y. J. Jang, Seiji Kawamura, E. A. Huerta, D. H. Reitze, B. Behnke, B. M. Levine, P. J. King, W. Parkinson, B. Shapiro, K. Kawabe, S. M. Aston, D. Ugolini, Ping Koy Lam, T. Bhadbhade, Elizabeth Harstad, Thomas Dent, S. Márka, A. G. Wiseman, D. Simakov, D. L. Jones, Chi-Woong Kim, V. Litvine, A. W. Heptonstall, C. T. Y. Chung, Peter R. Saulson, Michael E Zucker, Namjun Kim, F. Seifert, Andrew Melatos, Peter Fritschel, Vladimir Dergachev, J. R. Smith, R. Bork, Jacob Slutsky, Erik Katsavounidis, J. H. Romie, M. Brinkmann, J. M. Berliner, G. Santostasi, L. Cunningham, T. Nash, Richard O'Shaughnessy, B. Barr, Malik Rakhmanov, M. J. Lubinski, K. Evans, L. Williams, A. Le Roux, Michael W. Coughlin, David Coward, R. Gustafson, E. Forsi, Sheon Chua, C. J. Guido, Christian Röver, A. Dietz, James Whelan, P. Ajith, M. Lormand, R. Abbott, G. H. Ogin, J. Aasi, Kenneth A. Strain, A. Kremin, Y. Bao, A. Castiglia, L. G. Prokhorov, S. Foley, M. Prijatelj, M. Huynh, D. C. Coyne, K. Grover, K. Izumi, Saranya Ghosh, G. Kang, M. C. Araya, J. Wang, Kyungmin Kim, M. Cordier, B. O'Reilly, Vaibhav Tiwari, Kipp Cannon, M. Born, K. Mailand, R. S. Ottens, G. May, Jan Hendrik Pöld, M. E. Normandin, C. Lawrie, B. E. Aylott, K. Loew, E. Jesse, Tobias Eberle, S. Giampanis, Rajesh Kumar, Vladimir B. Braginsky, R. Riesen, H. Vahlbruch, K. Riles, N. Fotopoulos, M. Weinert, Roland Schilling, S. Raja, S. E. Strigin, P. G. Murray, John D. Scott, D. L. Kinzel, R. A. Mercer, L. Rodriguez, M. Mageswaran, S. Verma, A. Mytidis, Andreas Freise, Vincenzo Pierro, E. Macdonald, Paul D. Lasky, M. Pickenpack, Alexander Wanner, R. DeSalvo, J. Logue, Eric Oelker, A. L. Stuver, Jordi Burguet-Castell, R. Kasturi, G. Traylor, Yi Pan, Thomas Corbitt, C. A. Costa, M. Holtrop, R. Mittleman, Nelson Christensen, Joshua L. Willis, Matthew Pitkin, S. Sankar, H. Fehrmann, Michael L. Gorodetsky, M. J. Cowart, T. Westphal, Katrin Dahl, Benjamin William Allen, C. M. Reed, C. Griffo, J. Zweizig, S. P. Tarabrin, R. Wooley, V. Huang, J. C. Barayoga, Sebastian Steinlechner, J. H. Hough, S. T. Countryman, Roman Schnabel, Carlos Kozameh, Douglas R. Cook, R. J. S. Greenhalgh, Gavin Davies, P. Shawhan, John Miller, T. Prestegard, Anton B. Ivanov, G. Szeifert, Karsten Danzmann, Marco Aurelio Diaz, D. Martinov, Samuel J. Waldman, Vicky Kalogera, Larry R. Price, P. Charlton, C. Bogan, Tarun Souradeep, S. C. McGuire, Michele Zanolin, C. L. Mueller, Slawomir Gras, W. D. Vousden, Vuk Mandic, V. Necula, I. Santiago-Prieto, K. McAuley, V. V. Frolov, T. Vo, M. Constancio Junior, J. E. Brau, A. A. van Veggel, Sebastien Biscans, Efim A. Khazanov, Moritz Mehmet, D. R. Ingram, Phil Willems, M. Phelps, M. Wade, J. J. Lee, I. A. Bilenko, O. Puncken, Hartmut Grote, C. Padilla, Jong H. Chow, J. A. Giaime, Y. M. Kim, Charlotte Bond, G. D. Hammond, G. Gelencser, Carlos Cepeda, Stefan Ast, Robert J. McCarthy, Linqing Wen, F. Clara, Thomas N. Williams, J. Macarthur, M. Tse, David J. Ottaway, A. C. Lin, D. B. Kelley, G. R. Skelton, Eric Thrane, Andrew Lundgren, Stanislav Babak, Neil J. Cornish, Zhihui Du, Shaun Hooper, M. H. Wimmer, Duncan A. Brown, G. McIntyre, D. M. Macleod, Leo Singer, Eric W. James, J. Ou, I. Di Palma, D. Lodhia, J. C. Dumas, Shiuh Chao, Timothy A Welborn, Sarah Caudill, R. Quitzow-James, F. Ohme, B. Daudert, J. Heefner, Albert Lazzarini, Matthew Abernathy, Qi Fang, Kasem Mossavi, Takao Mori, Gregory M. Harry, John A. Clark, Ben Farr, P. Raffai, J. Hanks, K. Kokeyama, N. D. Smith-Lefebvre, N. Gehrels, P. Oppermann, Michele Vallisneri, Fumiko Kawazoe, B. J. Kuper, Ik Siong Heng, S. Steplewski, Grant David Meadors, Emma L. Robinson, Roy Williams, J. Birch, C. Tomlinson, Stefan Goßler, C. Graef, J. G. Rollins, Soma Mukherjee, Drew Keppel, W. Katzman, R. J.E. Smith, G. Manca, Subhabrata Mitra, Nergis Mavalvala, Kris Ryan, E. A. Quintero, P. Ehrens, H-S. Cho, V. Predoi, I. W. Martin, V. Kondrashov, Z. Shao, L. E. Wade, Virginio Sannibale, David E. McClelland, G. Bergmann, Joseph Gleason, H. Wittel, K. Wette, Matthew Heintze, John J. Oh, R. K. Nayak, C. Adams, J. C. Driggers, L. Austin, C. Kucharczyk, Michael Thomas, D. Sigg, F. J. Raab, S. W. Ballmer, C-H. Lee, Huan Yang, P. Campsie, G. Moreno, Koji Arai, Lutz Winkelmann, Fan Zhang, D. Nanda Kumar, Douglas E. Stevens, Jessica Steinlechner, M. Heurs, Reed Essick, B. Sorazu, T. Z. Summerscales, John Veitch, M. MacInnis, Alberto Vecchio, Will M. Farr, K. Buckland, B. Hughey, S. E. Gossan, D. Moraru, D. Yeaton-Massey, David Keitel, Suvadeep Bose, Z. Márka, E. Steinert, M. R. Smith, M. Edwards, T. Hong, S. R. Morriss, Alessandra Corsi, E. J. Daw, Paolo Addesso, K. D. Giardina, C. Gill, M. Rodruck, S. B. Anderson, Ruslan Vaulin, David B. Tanner, M. Pedraza, Maria Alessandra Papa, Collin Capano, N. A. Robertson, D. Hammer, K. Haris, Peter Kalmus, B. Lantz, Philip Graff, Michael Britzger, Ben C. Buchler, R. M. S. Schofield, Benjamin J. Owen, Martin Hendry, Christopher Wipf, K. V. Tokmakov, Martin Hewitson, Junwei Cao, Sanichiro Yoshida, Graham Woan, Robert L. Byer, Stuart Reid, Bernard F. Schutz, Li Ju, Daniel A. Shaddock, J. Hanson, M. Stefszky, Guido Mueller, David Murphy, J. Abadie, A. L. Lombardi, R. L. Savage, A. S. Bell, T. Isogai, P. Fulda, F. Y. Khalili, Eric Howell, L. K. Nuttall, S. Gil-Casanova, G. Billingsley, M. Was, S. Grunewald, T. Adams, D. B. Kozak, C. Vorvick, Theodore A. Evans, Maik Frede, P. Schwinberg, C. C. Yancey, W. G. Anderson, Giacomo Ciani, A. Mullavey, B. P. Abbott, E. K. Gustafson, D. E. Clark, S. Vass, R. Vincent-Finley, Fabrice Matichard, W. Kells, Lucía Santamaría, Jesper Munch, M. A. Frei, S. Penn, D. Schuette, Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, The LIGO Scientific Collaboration, LVC Collaboration, The, Pierro, V., and Pinto, I. M.
Subjects: Gravitational-wave observatory, Astronomy, Ciencias Físicas, FOS: Physical sciences, Astrophysics, Gravitational-wave astronomy, NOISE, General Relativity and Quantum Cosmology, Optics, Sensitivity, Atomic and Molecular Physics, Electronic, Quantum metrology, Optical and Magnetic Materials, Electronic, Optical and Magnetic Materials, Atomic and Molecular Physics, and Optics, QC, LIGO Scientific Collaboration, QB, Physics, Gravitational Waves, Quantum Physics, Einstein Telescope, Gravitational wave, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, METROLOGY, LIGO, Astronomía, Detection, Ligo, and Optics, business, Quantum Physics (quant-ph), QUANTUM, INTERFEROMETER, CIENCIAS NATURALES Y EXACTAS, Squeezed coherent state, Optics (physics.optics), Physics - Optics
Abstract: Nearly a century after Einstein first predicted the existence of gravitational waves, a global network of Earth-based gravitational wave observatories1,2,3,4 is seeking to directly detect this faint radiation using precision laser interferometry. Photon shot noise, due to the quantum nature of light, imposes a fundamental limit on the attometre-level sensitivity of the kilometre-scale Michelson interferometers deployed for this task. Here, we inject squeezed states to improve the performance of one of the detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) beyond the quantum noise limit, most notably in the frequency region down to 150 Hz, critically important for several astrophysical sources, with no deterioration of performance observed at any frequency. With the injection of squeezed states, this LIGO detector demonstrated the best broadband sensitivity to gravitational waves ever achieved, with important implications for observing the gravitational-wave Universe with unprecedented sensitivity Fil: Aasi, J.. California Institute of Technology; Estados Unidos Fil: Abadie, J.. California Institute of Technology; Estados Unidos Fil: Abbott, P.. California Institute of Technology; Estados Unidos Fil: Abbott, R.. California Institute of Technology; Estados Unidos Fil: Abbott, T. D.. State University of Louisiana; Estados Unidos Fil: Kozameh, Carlos Nicolas. Universidad Nacional de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina Fil: Winkelmann, L.. Max Planck Institut f¨ur Gravitationsphysik; Alemania. Leibniz Universit¨at Hannover; Alemania Fil: Winkler, W.. Max Planck Institut f¨ur Gravitationsphysik; Alemania. Leibniz Universit¨at Hannover; Alemania Fil: Wip, C. C.. Massachusetts Institute of Technology; Estados Unidos Fil: Wittel, H.. Max Planck Institut f¨ur Gravitationsphysik; Alemania. Leibniz Universit¨at Hannover; Alemania Fil: Woan, G.. University of Glasgow; Reino Unido Fil: Wooley, R.. Livingston Observatory; Estados Unidos Fil: Worden, J.. Hanford Observatory; Estados Unidos Fil: Yablon, J.. Northwestern University; Estados Unidos Fil: Yakushin, I.. Livingston Observatory; Estados Unidos Fil: Yamamoto, H.. California Institute of Technology; Estados Unidos Fil: Yancey, C. C.. University of Maryland; Estados Unidos Fil: Yang, H.. Caltech-CaRT; Estados Unidos Fil: Yeaton Massey, D.. California Institute of Technology; Estados Unidos Fil: Yoshida, S.. Southeastern Louisiana University; Estados Unidos Fil: Yum, H.. Northwestern University; Estados Unidos Fil: Zanolin, M.. Embry-Riddle Aeronautical University; Estados Unidos Fil: Zhang, F.. Massachusetts Institute of Technology; Estados Unidos Fil: Zhang, L.. California Institute of Technology; Estados Unidos Fil: Zhao, C.. University of Western Australia; Australia Fil: Zhu, H.. State University of Pennsylvania; Estados Unidos Fil: Zhu, X. J.. University of Western Australia; Australia Fil: Zotov, N.. Louisiana Tech University; Estados Unidos Fil: Zucker, M. E.. Massachusetts Institute of Technology; Estados Unidos Fil: Zweizig, J.. California Institute of Technology; Estados Unidos
Published: 2013

45. Einstein@Home all-sky search for periodic gravitational waves in LIGO S5 data

Author: R. L. Ward, N. Letendre, A. Langley, S. Penn, P. J. Sutton, F. Paoletti, J. H. Romie, G. Kuehn, L. Cunningham, F. J. Raab, R. Cavalieri, P. Ruggi, Laura Cadonati, Benjamin Aylott, G. Kang, M. Jacobson, R. Gustafson, Michael L. Gorodetsky, T. Westphal, J. Franc, S. Giampanis, M. Di Paolo Emilio, E. Tournefier, A. Basti, S. E. Strigin, J.-P. Coulon, Jens Birch, Z. Frei, N. D. Smith-Lefebvre, V. Dattilo, Stefan Hild, H. Müller-Ebhardt, A. Brillet, K. Kaufman, Susan M. Scott, Teviet Creighton, M. Born, K. Mailand, Hyun-Chul Kim, R. Mittleman, Nelson Christensen, C. T. Y. Chung, Michael E Zucker, J. Zweizig, David H. Shoemaker, Holger J. Pletsch, D. Verkindt, M. V. Plissi, C. Griffo, Richard O'Shaughnessy, B. Barr, Malik Rakhmanov, J. Worden, L. Williams, D. Ugolini, J.-D. Fournier, Sebastian Steinlechner, Chad Hanna, C. Wilkinson, M. Lormand, Kipp Cannon, R. S. Ottens, M. T. Hartman, V. Kringel, I. Di Palma, B. Behnke, V. Necula, R. Paoletti, I. Santiago-Prieto, Hartmut Grote, R. Passaquieti, M. Branchesi, G. Losurdo, J. C. Batch, K. A. Hodge, Jong H. Chow, A. Pasqualetti, J. Macarthur, M. Tse, D. M. Macleod, Riccardo Sturani, K. Venkateswara, E. Forsi, S. Braccini, V. Litvine, T. Bhadbade, G. Cagnoli, S. Chung, M. E. Normandin, Zoltán Keresztes, E. Jesse, R. Riesen, V. V. Frolov, Neil J. Cornish, P. E. Lindquist, G. A. Prodi, Alexander Wanner, Rahul Biswas, I. Fiori, Mirko Prato, F. Robinet, C. J. Bell, Robert Stone, A. Di Virgilio, D. Amariutei, F. Nocera, D. J. White, C. Zhao, Alicia M. Sintes, C. Poux, D. Fazi, F. Piergiovanni, S. H. Huttner, D. Atkinson, L. Palladino, N. Zotov, K. Mason, Sanjeev Dhurandhar, Andrew Melatos, Elena Cesarini, M. Pihlaja, Tomasz Bulik, P. G. Murray, M. Lorenzini, A. Masserot, J. H. Hough, B. Bouhou, Douglas R. Cook, Michele Zanolin, V. Kalogera, B. L. Swinkels, C. Graef, Timothy A Welborn, E. Amador Ceron, Xin Chen, R. M. Martin, M. Prijatelj, Xavier Siemens, Roy Williams, D. H. Reitze, L. Taffarello, G. Gelencser, M. Davier, A. Conte, A. Viceré, Yi Chen, Ilya Belopolski, A. Di Lieto, M. Vasúth, S. Márka, A. Mytidis, N. Beveridge, M. Blom, T. Regimbau, C. I. Torrie, S. P. Tarabrin, J. C. Barayoga, Richard J. Abbott, D. R. Ingram, Phil Willems, Stanislav Babak, Kenneth A. Strain, Jordan Camp, D. Feldbaum, T. Meier, P. Puppo, S. Sankar, Marco Aurelio Diaz, C. Bogan, François Bondu, V. Malvezzi, Fabio Marchesoni, P. Hello, Charlotte Bond, G. D. Hammond, B. J. J. Slagmolen, Hee-Suk Cho, Chiara M. F. Mingarelli, A. M. Cruise, R. L. Savage, A. S. Bell, S. Vitale, Grant David Meadors, T. Isogai, Tenglin Li, Stefan Goßler, I. Kowalska, Atsushi J. Nishizawa, H. J. Bulten, Seiji Kawamura, Reinhard Prix, Elizabeth Harstad, A. F. Brooks, Y. Wan, Duncan A. Brown, N. A. Robertson, C. N. Colacino, W. Chen, D. Hammer, Kyungmin Kim, Y. J. Jang, F. Travasso, Michał Bejger, B. O'Reilly, F. Y. Khalili, G. Mazzolo, V. Lhuillier, Walter Winkler, A. S. Markosyan, T. T. Fricke, Harald Lück, Paul Fulda, M. Britzger, Ilya Mandel, E. Macdonald, I. Maksimovic, J. Marque, B. K. Kim, Richard A. Matzner, Eric Thrane, G. McIntyre, Leo Singer, Riccardo Bassiri, E. Maros, A. E. Villar, Roberto Conte, Nergis Mavalvala, J. Aasi, Masa-Katsu Fujimoto, M. Shaltev, D. S. Rabeling, Vuk Mandic, Eric Oelker, Yi Pan, Peter Aufmuth, A. Singer, M. A. Barton, Carl L. Rodriguez, Sascha Husa, Eric W. James, F. Garufi, L. Rolland, Fabrizio Barone, M. Mohan, D. Rosińska, Jerome Degallaix, Rana X. Adhikari, Jordi Burguet-Castell, J. P. Zendri, A. Allocca, H. Yamamoto, C. Michel, C. Aulbert, Sarah Caudill, D. Simakov, Scott Koranda, R. Quitzow-James, R. Day, L. Matone, Gregory M. Harry, R. G. Oldenberg, Sunil Susmithan, N. Man, J. Heefner, Rocco Romano, A. Effler, T. Accadia, K. Haughian, B. Daudert, John A. Clark, Ben Farr, J. N. Marx, László Á. Gergely, V. Re, Ho-Gyu Lee, Kevin M. Ryan, Piotr Jaranowski, Matthew Evans, A. Gennai, Badri Krishnan, M. Holtrop, Katrin Dahl, H. Kaufer, Meng Wang, A. R. Wade, D.B. DeBra, C. M. Mow-Lowry, Sergey P. Vyatchanin, E. Goetz, T. Dent, Mallory S. E. Roberts, Kazuhiro Hayama, J. Logue, John D. Scott, D. L. Kinzel, A. Giazotto, V. Predoi, I. W. Martin, Peter Kalmus, Virginio Sannibale, J. R. Leong, B. Machenschalk, R. A. Mercer, David E. McClelland, F. Donovan, R. Inta, J. H. Clayton, B. F. Whiting, S. Dorsher, C. Bradaschia, P. Shawhan, I. Ferrante, D. Passuello, F. Cleva, Ik Siong Heng, A. Rüdiger, S. Steplewski, Hyun Lee, M. Galimberti, A. Perreca, G. Gemme, M. Drago, Guenakh Mitselmakher, V. Raymond, Fan Zhang, C. Van Den Broeck, Jonathan R. Gair, M. Pichot, S. Klimenko, M. Was, Th. S. Bauer, Christian D. Ott, C. Palomba, S. Privitera, I. Yakushin, L. Sammut, Fabio Postiglione, P. Charlton, P. Kwee, Ruxandra Bondarescu, S. E. Whitcomb, S. C. McGuire, K. A. Thorne, G. Mendell, J. A. Giaime, N. A. Lockerbie, Y. M. Kim, Emma L. Robinson, O. Puncken, John Nelson, D. Talukder, C. V. Torres, I. Leonor, C. Messenger, A. M. Sergeev, F. Seifert, D. Friedrich, C. Lawrie, H. Vocca, P. Astone, R. J. S. Greenhalgh, S. Ast, I. W. Harry, R. Gouaty, C. M. Reed, F. Marion, N. Leroy, V. Kondrashov, M. Kasprzack, Peter Fritschel, Ping Koy Lam, G. Debreczeni, I. A. Bilenko, David J. Ottaway, Vladimir Dergachev, James Whelan, P. Ajith, A. P. M. ter Braack, M. Bastarrika, M. J. Cowart, Y. Minenkov, Y. Bao, P. J. Veitch, John Miller, S. Foley, Shaun Hooper, D. F. Menéndez, T. Prestegard, Saranya Ghosh, R. De Rosa, V. Loriette, R. Schilling, M. Bebronne, Jonah Kanner, A. Morgia, Alessandra Corsi, M. Cordier, D. B. Kelley, Zhihui Du, H. Wittel, M. S. Meyer, W. Z. Korth, Xiaomin Wang, P. Wessels, A. L. Stuver, Ludovico Carbone, P. Couvares, Benno Willke, R. Kurdyumov, R. Kasturi, Matthew P. Edgar, Namjun Kim, Enrico Calloni, E. J. Daw, G. Traylor, J. C. Driggers, Thomas Corbitt, L. Naticchioni, Kazuhiro Agatsuma, F. Frasconi, A. S. Stroeer, Carlos Cepeda, Jessica McIver, Robert J. McCarthy, J. C. Dumas, Rosa Poggiani, V. Herrera, Albert Lazzarini, Anton B. Ivanov, Samuel J. Waldman, M. Tonelli, Larry R. Price, Takao Mori, C. Osthelder, D. O. Bridges, Rebecca Fisher, Jesper Munch, J. Li, David Jones, Marco Cavaglia, P. Raffai, M. A. Bizouard, J. Hanks, S. Van Der Putten, Ranjan Gupta, M. Heurs, Huan Yang, Koji Arai, C. R. Ramet, R. Flaminio, K. Kokeyama, Rainer Weiss, S. D'Antonio, M. A. Frei, E. Saracco, C. Tomlinson, C. A. Costa, Soma Mukherjee, Fausto Acernese, F. Ricci, J. Breyer, Alessandra Buonanno, Paolo Addesso, K. D. Giardina, C. Gill, S. Doravari, Igor Neri, Linqing Wen, A. W. Heptonstall, Peter R. Saulson, Prayush Kumar, G. P. Newton, M. Fyffe, R. W. P. Drever, Drew Keppel, C. Gray, P. Baker, B. Moe, M. Damjanic, E. Coccia, M. Rodruck, J. G. Rollins, C. L. Mueller, Yueh-Feng Liu, S. Grunewald, M. Mantovani, B. Sorazu, A. Thüring, A. C. Melissinos, Andrea Chincarini, T. Z. Summerscales, W. Katzman, R. J.E. Smith, Gabriela Gonzalez, Ettore Majorana, D. Keitel, L. G. Prokhorov, J. M. Hallam, Innocenzo M. Pinto, Kentaro Somiya, M. Brinkmann, Matthew West, W. W. Johnson, Amanda J. Page, D. Lodhia, P. Ehrens, C-H. Lee, S. B. Anderson, Joseph Gleason, V. Fafone, G. R. Skelton, Andrew Lundgren, G. Santostasi, Ruslan Vaulin, David B. Tanner, M. Bitossi, Maik Frede, B. Mours, M. C. Araya, S. Kandhasamy, A. Chiummo, M. Factourovich, M. E. Gáspár, A. K. Zadrożny, K. Wette, Ryan DeRosa, G. Vedovato, D. B. Kozak, John J. Oh, Timothy Evans, C. Vorvick, V. Brisson, M. Sung, C. Adams, A. Khalaidovski, R. Engel, V. Boschi, Joseph D. Romano, B. Bland, T. Etzel, H. P. Daveloza, Moritz Mehmet, B. Lantz, Thanh Vinh Nguyen, David Blair, F. Salemi, D. Sigg, S. W. Ballmer, Philip Graff, R. M. Cutler, M. Pedraza, J. Steinlechner, P. Campsie, P. Leaci, A. Colla, Luca Gammaitoni, Kasem Mossavi, P. Thomas, D. Nolting, L. Bonelli, P. Schwinberg, Stefaan Franco, Maria Alessandra Papa, C. C. Yancey, G. Moreno, F. Cavalier, A. Nitz, W. G. Anderson, G. Cella, Karoline Wiesner, R. M. S. Schofield, T. Eberle, Erik Katsavounidis, Giacomo Ciani, A. Mullavey, B. P. Abbott, Matthew Benacquista, E. K. Gustafson, D. E. Clark, D. Barker, Benjamin J. Owen, F. Martelli, J. F. J. van den Brand, Collin Capano, S. Vass, S. Frasca, C. Robinson, Benjamin William Allen, M. Tacca, C. Affeldt, Martin Hendry, Christopher Wipf, Douglas H Beck, G. Szeifert, K. V. Tokmakov, Gianluca Persichetti, Fabrice Matichard, W. Kells, Lucía Santamaría, R. Taylor, J. Slutsky, Imre Bartos, M. J. Lubinski, Jolien D. E. Creighton, Karsten Danzmann, M. Colombini, Martin Hewitson, Junwei Cao, N. Morgado, K. Evans, Stephen Fairhurst, S. Caride, Lindy Blackburn, V. Quetschke, Bangalore Suryanarayana Sathyaprakash, E. Black, Sanichiro Yoshida, T. P. Bodiya, J. R. Smith, R. Bork, M. Punturo, Leopoldo Milano, S. Roddy, C. Buy, Graham Woan, K. Holt, Tristan Briant, T. Nash, Robert L. Byer, Stuart Reid, Rajesh Kumar, G. Endroczi, Chunglee Kim, V. Sandberg, S. Mosca, M. Vavoulidis, Vladimir B. Braginsky, Jeffery Kline, G. H. Ogin, L. Pinard, J. D. Lough, B. Schulz, H. Vahlbruch, H. Fehrmann, J. Garcia, J. O'Dell, T. Dayanga, K. Riles, J. Y. Vinet, F. Carbognani, Federico Ferrini, Haixing Miao, S. L. Danilishin, G. Vajente, Bernard F. Schutz, O. Bock, N. Fotopoulos, István Rácz, Li Ju, D. Moraru, Daniel A. Shaddock, Lee Samuel Finn, K. L. Dooley, Kip S. Thorne, T. Chalermsongsak, Alessandro Bertolini, J. Hanson, M. Stefszky, M. Weinert, D. Yeaton-Massey, T. Reed, Lisa Barsotti, F. Fidecaro, G. M. Guidi, J.-F. Hayau, M. Yvert, T. D. Abbott, Guido Mueller, A. Stochino, V. P. Mitrofanov, W. Del Pozzo, P. F. Cohadon, Trevor Sidery, H. Heitmann, B. Rankins, Joshua Yablon, Alessandra Toncelli, David Murphy, R. J. G. Jonker, L. Wallace, H. Radkins, F. Vetrano, A. Królak, M. H. Wimmer, R. Frey, J. Abadie, Evan Ochsner, S. E. Dwyer, P. J. King, B. Shapiro, J. M. Berliner, A. J. Weinstein, J. Pöld, A. G. Wiseman, David Coward, Sheon Chua, P. T. Beyersdorf, C. J. Guido, Christian Röver, R. Bonnand, L. Sperandio, Suvadeep Bose, Z. Márka, D. C. Coyne, K. Grover, Jan Harms, M. Landry, K. Izumi, Satyanarayan Ray Pitambar Mohapatra, L. Di Fiore, E. Steinert, M. R. Smith, Eric Howell, M. Edwards, M. Pickenpack, M. Barsuglia, A. Rocchi, L. K. Nuttall, D. Buskulic, F. Kawazoe, O. Torre, E. Cuoco, S. Gil-Casanova, M. R. Abernathy, Nico Lastzka, G. Billingsley, S. Meshkov, Seog Oh, A. Grant, T. Hong, L. Bosi, A. Cumming, E. Genin, Maria Ilaria Del Principe, L. Zhang, M. Agathos, S. R. Morriss, Alberto Vecchio, A. M. Gretarsson, J. Bauchrowitz, Roman Schnabel, A. Dietz, J. K. Blackburn, E. Chassande-Mottin, J. E. Brau, B. Canuel, A. A. van Veggel, Sheila Rowan, Lutz Winkelmann, Efim A. Khazanov, G. Ballardin, Todd Adams, Fiona C. Speirits, B. Hughey, M. Phelps, John Veitch, C. Titsler, F. Clara, M. MacInnis, P. Rapagnani, Andreas Freise, Vincenzo Pierro, Matthew Pitkin, R. Wooley, M. Wade, M. Granata, M. Parisi, M. G. Beker, T. Huynh-Dinh, Dustin Anderson, J. S. Kissel, Marc Favata, K. Yamamoto, L. E. Wade, Roger Jones, K. Kawabe, S. M. Aston, Michael W. Coughlin, M. Mageswaran, J. Betzwieser, Antoine Heidmann, H. Overmier, D. Sellers, D. Hoak, D. Sentenac, Patrick Brady, Zhi Liu, Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Gravitation ( APC-Gravitation ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, (Astro)-Particles Physics, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Aasi, J., Abadie, J., Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M., Accadia, T., Acernese, F., Adams, C., Adams, T., Addesso, P., Adhikari, R., Affeldt, C., Agathos, M., Agatsuma, K., Ajith, P., Allen, B., Allocca, A., Amador Ceron, E., Amariutei, D., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Ast, S., Aston, S. M., Astone, P., Atkinson, D., Aufmuth, P., Aulbert, C., Aylott, B. E., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Bao, Y., Barayoga, J. C. B., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Basti, A., Batch, J., Bauchrowitz, J., Bauer, T. h. S., Bebronne, M., Beck, D., Behnke, B., Bejger, M., Beker, M. G., Bell, A. S., Bell, C., Belopolski, I., Benacquista, M., Berliner, J. M., Bertolini, A., Betzwieser, J., Beveridge, N., Beyersdorf, P. T., Bhadbade, T., Bilenko, I. A., Billingsley, G., Birch, J., Biswas, R., Bitossi, M., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Blom, M., Bock, O., Bodiya, T. P., Bogan, C., Bond, C., Bondarescu, R., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Boschi, V., Bose, S., Bosi, L., Bouhou, B., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Breyer, J., Briant, T., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Britzger, M., Brooks, A. F., Brown, D. A., Bulik, T., Bulten, H. J., Buonanno, A., Burguet Castell, J., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Calloni, Enrico, Camp, J. B., Campsie, P., Cannon, K., Canuel, B., Cao, J., Capano, C. D., Carbognani, F., Carbone, L., Caride, S., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chalermsongsak, T., Charlton, P., Chassande Mottin, E., Chen, W., Chen, X., Chen, Y., Chincarini, A., Chiummo, A., Cho, H. S., Chow, J., Christensen, N., Chua, S. S. Y., Chung, C. T. Y., Chung, S., Ciani, G., Clara, F., Clark, D. E., Clark, J. A., Clayton, J. H., Cleva, F., Coccia, E., Cohadon, P. F., Colacino, C. N., Colla, A., Colombini, M., Conte, A., Conte, R., Cook, D., Corbitt, T. R., Cordier, M., Cornish, N., Corsi, A., Costa, C. A., Coughlin, M., Coulon, J. P., Couvares, P., Coward, D. M., Cowart, M., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Cumming, A., Cunningham, L., Cuoco, E., Cutler, R. M., Dahl, K., Damjanic, M., Danilishin, S. L., D’Antonio, S., Danzmann, K., Dattilo, V., Daudert, B., Daveloza, H., Davier, M., Daw, E. J., Day, R., Dayanga, T., DE ROSA, Rosario, Debra, D., Debreczeni, G., Degallaix, J., Del Pozzo, W., Dent, T., Dergachev, V., Derosa, R., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Di Palma, I., Di Paolo Emilio, M., Di Virgilio, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Doravari, S., Dorsher, S., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Dumas, J. C., Dwyer, S., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Endrőczi, G., Engel, R., Etzel, T., Evans, K., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fairhurst, S., Farr, B. F., Favata, M., Fazi, D., Fehrmann, H., Feldbaum, D., Ferrante, I., Ferrini, F., Fidecaro, F., Finn, L. S., Fiori, I., Fisher, R. P., Flaminio, R., Foley, S., Forsi, E., Fotopoulos, N., Fournier, J. D., Franc, J., Franco, S., Frasca, S., Frasconi, F., Frede, M., Frei, M. A., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fujimoto, M. K., Fulda, P. J., Fyffe, M., Gair, J., Galimberti, M., Gammaitoni, L., Garcia, J., Garufi, Fabio, Gáspár, M. E., Gelencser, G., Gemme, G., Genin, E., Gennai, A., Gergely, L. Á., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Gil Casanova, S., Gill, C., Gleason, J., Goetz, E., González, G., Gorodetsky, M. L., Goßler, S., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Griffo, C., Grote, H., Grover, K., Grunewald, S., Guidi, G. M., Guido, C., Gupta, R., Gustafson, E. K., Gustafson, R., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hartman, M. T., Haughian, K., Hayama, K., Hayau, J. F., Heefner, J., Heidmann, A., Heitmann, H., Hello, P., Hendry, M. A., Heng, I. S., Heptonstall, A. W., Herrera, V., Heurs, M., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Holt, K., Holtrop, M., Hong, T., Hooper, S., Hough, J., Howell, E. J., Hughey, B., Husa, S., Huttner, S. H., Huynh Dinh, T., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Izumi, K., Jacobson, M., James, E., Jang, Y. J., Jaranowski, P., Jesse, E., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Kasprzack, M., Kasturi, R., Katsavounidis, E., Katzman, W., Kaufer, H., Kaufman, K., Kawabe, K., Kawamura, S., Kawazoe, F., Keitel, D., Kelley, D., Kells, W., Keppel, D. G., Keresztes, Z., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, B. K., Kim, C., Kim, H., Kim, K., Kim, N., Kim, Y. M., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kline, J., Kokeyama, K., Kondrashov, V., Koranda, S., Korth, W. Z., Kowalska, I., Kozak, D., Kringel, V., Krishnan, B., Królak, A., Kuehn, G., Kumar, P., Kumar, R., Kurdyumov, R., Kwee, P., Lam, P. K., Landry, M., Langley, A., Lantz, B., Lastzka, N., Lawrie, C., Lazzarini, A., Leaci, P., Lee, C. H., Lee, H. K., Lee, H. M., Leong, J. R., Leonor, I., Leroy, N., Letendre, N., Lhuillier, V., Li, J., T. G. F., Li, Lindquist, P. E., Litvine, V., Liu, Y., Liu, Z., Lockerbie, N. A., Lodhia, D., Logue, J., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J., Lubinski, M., Lück, H., Lundgren, A. P., Macarthur, J., Macdonald, E., Machenschalk, B., Macinnis, M., Macleod, D. M., Mageswaran, M., Mailand, K., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mcguire, S. C., Mcintyre, G., Mciver, J., Meadors, G. D., Mehmet, M., Meier, T., Melatos, A., Melissinos, A. C., Mendell, G., Menéndez, D. F., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Milano, L., Miller, J., Minenkov, Y., Mingarelli, C. M. F., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moe, B., Mohan, M., Mohapatra, S. R. P., Moraru, D., Moreno, G., Morgado, N., Morgia, A., Mori, T., Morriss, S. R., Mosca, S., Mossavi, K., Mours, B., Mow Lowry, C. M., Mueller, C. L., Mueller, G., Mukherjee, S., Mullavey, A., Müller Ebhardt, H., Munch, J., Murphy, D., Murray, P. G., Mytidis, A., Nash, T., Naticchioni, L., Necula, V., Nelson, J., Neri, I., Newton, G., Nguyen, T., Nishizawa, A., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E., Nuttall, L., Ochsner, E., O’Dell, J., Oelker, E., Ogin, G. H., J. J., Oh, S. H., Oh, Oldenberg, R. G., O’Reilly, B., O’Shaughnessy, R., Osthelder, C., Ott, C. D., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Palladino, L., Palomba, C., Pan, Y., Paoletti, F., Paoletti, R., Papa, M. A., Parisi, M., Pasqualetti, A., Passaquieti, R., Passuello, D., Pedraza, M., Penn, S., Perreca, A., Persichetti, G., Phelps, M., Pichot, M., Pickenpack, M., Piergiovanni, F., Pierro, V., Pihlaja, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Pöld, J., Postiglione, F., Poux, C., Prato, M., Predoi, V., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Quitzow James, R., Raab, F. J., Rabeling, D. S., Rácz, I., Radkins, H., Raffai, P., Rakhmanov, M., Ramet, C., Rankins, B., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Roberts, M., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rodriguez, C., Rodruck, M., Rolland, L., Rollins, J. G., Romano, J. D., Romano, R., Romie, J. H., Rosińska, D., Röver, C., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Salemi, F., Sammut, L., Sandberg, V., Sankar, S., Sannibale, V., Santamaría, L., Santiago Prieto, I., Santostasi, G., Saracco, E., Sathyaprakash, B. S., Saulson, P. R., Savage, R. L., Schilling, R., Schnabel, R., Schofield, R. M. S., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Seifert, F., Sellers, D., Sentenac, D., Sergeev, A., Shaddock, D. A., Shaltev, M., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sidery, T. L., Siemens, X., Sigg, D., Simakov, D., Singer, A., Singer, L., Sintes, A. M., Skelton, G. R., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, R. J. E., Smith Lefebvre, N. D., Somiya, K., Sorazu, B., Speirits, F. C., Sperandio, L., Stefszky, M., Steinert, E., Steinlechner, J., Steinlechner, S., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S. E., Stroeer, A. S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Swinkels, B., Szeifert, G., Tacca, M., Taffarello, L., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, R., ter Braack, A. P. M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Thüring, A., Titsler, C., Tokmakov, K. V., Tomlinson, C., Toncelli, A., Tonelli, M., Torre, O., Torres, C. V., Torrie, C. I., Tournefier, E., Travasso, F., Traylor, G., Tse, M., Ugolini, D., Vahlbruch, H., Vajente, G., van den Brand, J. F. J., Van Den Broeck, C., van der Putten, S., van Veggel, A. A., Vass, S., Vasuth, M., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Villar, A. E., Vinet, J. Y., Vitale, S., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A., Wade, L., Wade, M., Waldman, S. J., Wallace, L., Wan, Y., Wang, M., Wang, X., Wanner, A., Ward, R. L., Was, M., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D. J., Whiting, B. F., Wiesner, K., Wilkinson, C., Willems, P. A., Williams, L., Williams, R., Willke, B., Wimmer, M., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Wittel, H., Woan, G., Wooley, R., Worden, J., Yablon, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yancey, C. C., Yang, H., Yeaton Massey, D., Yoshida, S., Yvert, M., Zadrożny, A., Zanolin, M., Zendri, J. P., Zhang, F., Zhang, L., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Anderson, D. P., Pinto, Innocenzo, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO (Observatory : Massachusetts Institute of Technology), Barsotti, Lisa, Bodiya, Timothy Paul, Corbitt, Thomas R., Donovan, Frederick J., Evans, Matthew J., Fritschel, Peter K., Katsavounidis, Erotokritos, Kissel, Jeffrey S., Kwee, Patrick, MacInnis, Myron E., Matichard, Fabrice, Mavalvala, Nergis, Mittleman, Richard K., Oelker, Eric Glenn, Shoemaker, David H., Vaulin, Ruslan, Wipf, Christopher, Zucker, Michael E., Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), The LIGO Scientific Collaboration, and The Virgo Collaboration
Subjects: Physics and Astronomy (miscellaneous), gravitational waves, pulsar, interferometers, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, general relativity, Range (statistics), PACS number: 04.80.Nn, PACS numbers: 95.55.Ym, PACS number: 97.60.Gb, PACS number: 07.05.Kf, NEUTRON-STAR, HOUGH TRANSFORM, PULSAR, RADIATION, EMISSION, 010303 astronomy & astrophysics, QC, QB, media_common, LIGO Scientific Collaboration, Physics, Settore FIS/01 - Fisica Sperimentale, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Nuclear and High Energy Physics, 3. Good health, Neutron-star, Amplitude, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Instrumentation and Methods for Astrophysics, Gravitation, Einstein@Home, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], media_common.quotation_subject, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Settore FIS/05 - Astronomia e Astrofisica, Pulsar, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010308 nuclear & particles physics, Gravitational wave, LIGO, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Sky, [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: This paper presents results of an all-sky searches for periodic gravitational waves in the frequency range [50, 1190] Hz and with frequency derivative ranges of [-2 x 10^-9, 1.1 x 10^-10] Hz/s for the fifth LIGO science run (S5). The novelty of the search lies in the use of a non-coherent technique based on the Hough-transform to combine the information from coherent searches on timescales of about one day. Because these searches are very computationally intensive, they have been deployed on the Einstein@Home distributed computing project infrastructure. The search presented here is about a factor 3 more sensitive than the previous Einstein@Home search in early S5 LIGO data. The post-processing has left us with eight surviving candidates. We show that deeper follow-up studies rule each of them out. Hence, since no statistically significant gravitational wave signals have been detected, we report upper limits on the intrinsic gravitational wave amplitude h0. For example, in the 0.5 Hz-wide band at 152.5 Hz, we can exclude the presence of signals with h0 greater than 7.6 x 10^-25 with a 90% confidence level., 29 pages, 14 figures, 6 tables. Science summary page at http://www.ligo.org/science/Publication-FullS5EatH/index.php ; Public access area to figures and tables at https://dcc.ligo.org/cgi-bin/DocDB/ShowDocument?docid=p1200026
Published: 2013
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46. Parameter estimation for compact binary coalescence signals with the first generation gravitational-wave detector network

Author: R. De Rosa, Laura Cadonati, Rana X. Adhikari, Carlos Cepeda, Robert J. McCarthy, Linqing Wen, B. Machenschalk, F. Donovan, V. Lhuillier, Susan M. Scott, Teviet Creighton, G. McIntyre, D. Lodhia, Maik Frede, Chad Hanna, M. Branchesi, J. C. Batch, K. A. Hodge, A. K. Zadrożny, V. Boschi, V. Malvezzi, M. Bebronne, Carl-Johan Haster, N. Morgado, L. Rolland, Fabrizio Barone, M. Mohan, N. Man, K. Haughian, Ludovico Carbone, P. Couvares, Benno Willke, E. Goetz, T. Dent, Kazuhiro Hayama, D. Talukder, C. V. Torres, I. W. Harry, R. Gouaty, M. Factourovich, J. Betzwieser, Antoine Heidmann, Leo Singer, L. Naticchioni, M. A. Barton, Carl L. Rodriguez, Sascha Husa, Meng Wang, C. Wilkinson, D. Amariutei, Janyce Franc, David H. Shoemaker, Holger J. Pletsch, D. Verkindt, R. L. Ward, P. J. Sutton, J. H. Romie, R. Kurdyumov, A. F. Brooks, Lutz Winkelmann, Kasem Mossavi, M. T. Hartman, V. Kringel, M. Pihlaja, Tomasz Bulik, François Bondu, Fausto Acernese, V. Kondrashov, H. Overmier, S. Kandhasamy, N. A. Robertson, C. N. Colacino, Jordan Camp, R. G. Oldenberg, D.B. DeBra, S. Braccini, V. Litvine, T. Bhadbade, J. Breyer, C. Gray, G. Kuehn, L. Cunningham, Alessandra Buonanno, M. Mantovani, Kentaro Somiya, M. Brinkmann, F. J. Raab, F. Garufi, G. Santostasi, F. Nocera, D. J. White, C. Zhao, Fiona C. Speirits, John Veitch, D. Sellers, C. Affeldt, D. Hammer, Y. Minenkov, D. Feldbaum, T. Meier, A. Morgia, Fabio Postiglione, S. Chung, C. Poux, R. Gustafson, M. E. Normandin, Eric Howell, I. Yakushin, L. Sammut, Zoltán Keresztes, F. Cleva, C. Titsler, Sunil Susmithan, R. Taylor, W. Chen, W. Z. Korth, P. Wessels, L. Pinard, J. Garcia, Jong H. Chow, A. Pasqualetti, S. E. Whitcomb, P. Kwee, K. A. Thorne, S. Giampanis, A. Gennai, H. Wittel, Federico Ferrini, S. Penn, D. Barker, T. P. Bodiya, G. Vajente, Kazuhiro Agatsuma, M. A. Bizouard, V. Loriette, L. K. Nuttall, M. MacInnis, S. Gil-Casanova, M. R. Abernathy, F. Frasconi, A. S. Stroeer, Peter Kalmus, P. Rapagnani, F. Seifert, Peter Fritschel, T. Accadia, David Jones, S. E. Strigin, C. Buy, B. Behnke, Riccardo Sturani, G. M. Harry, Nico Lastzka, K. Venkateswara, V. Predoi, I. W. Martin, J. C. Driggers, Virginio Sannibale, David E. McClelland, J. Macarthur, Y. Bao, G. Billingsley, S. Roddy, Tristan Briant, Marco Cavaglia, Badri Krishnan, V. Dattilo, M. Tse, D. M. Macleod, L. Bosi, S. Foley, H. Kaufer, D. Hoak, D. Sentenac, S. Mosca, Patrick Brady, R. Schilling, Matthew Evans, P. J. Veitch, G. Kang, M. Vavoulidis, C. R. Ramet, R. Flaminio, B. L. Swinkels, Huan Yang, Kip S. Thorne, T. Chalermsongsak, Alessandro Bertolini, J. Zweizig, Saranya Ghosh, Ryan DeRosa, Koji Arai, Sanichiro Yoshida, Jeffery Kline, Xuan Wang, J. D. Lough, A. R. Wade, C. M. Mow-Lowry, Jessica McIver, Stefan Hild, S. D'Antonio, Graham Woan, M. Rodruck, Jonah Kanner, Sergey P. Vyatchanin, B. Schulz, M. Pichot, R. Kasturi, A. M. Sintes, J. O'Dell, T. Dayanga, R. Inta, S. Klimenko, A. W. Heptonstall, Peter R. Saulson, Zhi Liu, M. Born, K. Mailand, Peter Aufmuth, Sebastian Steinlechner, M. Damjanic, T. Reed, C. Graef, Tania Regimbau, A. Khalaidovski, R. Engel, Robert L. Byer, Stuart Reid, F. Salemi, A. Brillet, A. Conte, K. Kaufman, A. Singer, Lee Samuel Finn, J. C. Dumas, D. Ugolini, B. F. Whiting, T. Huynh-Dinh, Timothy A Welborn, Enrico Calloni, G. Traylor, R. L. Savage, A. S. Bell, Thomas Corbitt, V. Herrera, C. A. Costa, J.-F. Hayau, M. Yvert, T. D. Abbott, Y. J. Jang, Seiji Kawamura, Elizabeth Harstad, Hyun-Chul Kim, R. Mittleman, M. Lormand, Robert Stone, Nelson Christensen, D. Keitel, L. G. Prokhorov, J. S. Kissel, C. J. Bell, A. Stochino, S. B. Anderson, B. Moe, Ruslan Vaulin, P. Leaci, A. Colla, J. Aasi, V. P. Mitrofanov, S. Dorsher, T. Etzel, H. P. Daveloza, A. Di Lieto, C. Van Den Broeck, Chris Pankow, B. Mours, J. N. Marx, László Á. Gergely, Albert Lazzarini, R. Passaquieti, L. Wallace, A. Królak, R. Frey, Marc Favata, K. Yamamoto, L. E. Wade, L. Palladino, Bernard F. Schutz, Masa-Katsu Fujimoto, J. Heefner, Li Ju, M. Shaltev, N. Letendre, A. Langley, E. Jesse, Mirko Prato, W. Del Pozzo, P. F. Cohadon, David B. Tanner, Roger Jones, N. Zotov, K. Mason, T. Isogai, D. Nolting, M. Sung, A. Nitz, F. Y. Khalili, G. Mazzolo, M. Vasúth, L. Bonelli, G. A. Prodi, Alexander Wanner, C. T. Y. Chung, Rahul Biswas, Michael E Zucker, Daniel A. Shaddock, J. Hanson, Trevor Sidery, H. Heitmann, A. Di Virgilio, Karoline Wiesner, P. J. King, T. Eberle, A. Chiummo, B. Shapiro, A. Allocca, M. Stefszky, John A. Clark, Sanjeev Dhurandhar, R. Cavalieri, Jordi Burguet-Castell, V. Re, B. Bland, N. Beveridge, C. I. Torrie, B. Rankins, Joshua Yablon, M. Blom, Elena Cesarini, M. Pedraza, Stefaan Franco, J. P. Zendri, Y. Wan, Ben Farr, F. Martelli, E. Amador Ceron, F. Piergiovanni, Chang-Hwan Lee, Ho-Gyu Lee, Luca Gammaitoni, Guido Mueller, A. G. Wiseman, Kipp Cannon, Walter Winkler, Kevin M. Ryan, D. R. Ingram, Phil Willems, K. Kawabe, Xin Chen, R. M. Martin, J. Slutsky, Imre Bartos, J. H. Clayton, M. Di Paolo Emilio, A. S. Markosyan, Namjun Kim, Grant David Meadors, Takao Mori, V. Quetschke, Bangalore Suryanarayana Sathyaprakash, S. M. Aston, Harald Lück, J. Logue, Michael W. Coughlin, Paul Fulda, Maria Alessandra Papa, F. Cavalier, M. Prijatelj, E. Tournefier, A. Basti, David Murphy, M. Holtrop, D. C. Coyne, K. Grover, K. Izumi, Katrin Dahl, F. Travasso, M. Davier, R. S. Ottens, Michał Bejger, A. Effler, C. Palomba, Collin Capano, A. Giazotto, P. Shawhan, M. H. Wimmer, I. Ferrante, J. Abadie, M. Mageswaran, Xavier Siemens, J.-P. Coulon, B. J. J. Slagmolen, Hee-Suk Cho, M. Britzger, S. C. McGuire, E. Black, Satya Mohapatra, J. R. Smith, R. Bork, S. Privitera, T. Nash, Z. Frei, Ilya Mandel, E. Macdonald, I. Leonor, M. Was, B. Lantz, Andreas Freise, Vincenzo Pierro, Philip Graff, G. H. Ogin, A. Perreca, M. C. Araya, G. Gemme, M. Drago, Guenakh Mitselmakher, John Miller, T. Prestegard, V. Brisson, S. Ast, C. M. Reed, K. Kokeyama, Eric Thrane, Eric W. James, C. Michel, Sarah Caudill, P. Puppo, Chiara M. F. Mingarelli, P. Charlton, H. Vocca, J.-D. Fournier, Alessandra Corsi, Matthew Pitkin, D. Rosińska, I. Maksimovic, O. Puncken, D. Friedrich, J. Marque, B. K. Kim, G. Hemming, R. Wooley, R. J. S. Greenhalgh, D. Passuello, A. Viceré, Hyun Lee, Anton B. Ivanov, A. L. Stuver, A. M. Sergeev, Yi Chen, M. S. Meyer, S. Sankar, C. Griffo, M. Wade, R. Quitzow-James, B. Daudert, P. G. Murray, N. D. Smith-Lefebvre, P. Baker, J. Birch, S. Frasca, R. M. S. Schofield, Matthew Benacquista, E. J. Daw, I. Fiori, Riccardo Bassiri, J. H. Hough, Jolien D. E. Creighton, S. Caride, Rainer Weiss, Benjamin J. Owen, M. Granata, E. Coccia, E. Maros, S. Doravari, Igor Neri, F. Ricci, R. W. P. Drever, Paolo Addesso, K. D. Giardina, Christian D. Ott, C. Gill, Samuel J. Waldman, Marco Aurelio Diaz, C. Bradaschia, M. Tonelli, V. Necula, W. W. Johnson, A. P. M. ter Braack, I. Santiago-Prieto, Innocenzo M. Pinto, Larry R. Price, J. G. Rollins, C. Bogan, I. A. Bilenko, Ik Siong Heng, A. Rüdiger, David J. Ottaway, J. F. J. van den Brand, M. Tacca, V. V. Frolov, Martin Hendry, Christopher Wipf, K. V. Tokmakov, Richard A. Matzner, Lindy Blackburn, B. Bouhou, C. Robinson, Douglas R. Cook, K. Holt, Chunglee Kim, Piotr Jaranowski, Florent Robinet, Matthew West, C. Messenger, Riccardo Paoletti, Thanh Vinh Nguyen, David Blair, M. Parisi, M. G. Beker, S. Steplewski, Emma L. Robinson, Fan Zhang, Michele Zanolin, Martin Hewitson, Junwei Cao, Benjamin William Allen, G. Szeifert, Karsten Danzmann, M. Colombini, V. Kalogera, Stephen Fairhurst, Joseph Gleason, M. Galimberti, V. Sandberg, D. H. Reitze, F. Marion, G. Gelencser, S. Grunewald, N. Leroy, M. Kasprzack, V. Fafone, Charlotte Bond, M. Punturo, Leopoldo Milano, C. Lawrie, G. D. Hammond, Stanislav Babak, John Nelson, Amanda J. Page, Ping Koy Lam, G. Debreczeni, F. Paoletti, Duncan A. Brown, M. Heurs, M. Bastarrika, M. E. Gáspár, G. Vedovato, D. B. Kozak, P. Ruggi, C. Vorvick, M. Jacobson, M. J. Cowart, B. Sorazu, S. Márka, H. Yamamoto, Mallory S. E. Roberts, A. Thüring, Kenneth A. Strain, M. C. Heintze, P. Schwinberg, C. C. Yancey, Ruxandra Bondarescu, G. Mendell, Fabio Marchesoni, P. Hello, Moritz Mehmet, Richard O'Shaughnessy, B. Barr, J. Steinlechner, A. C. Melissinos, Andrea Chincarini, P. Astone, B. Sassolas, G. R. Skelton, W. G. Anderson, C. Osthelder, Andrew Lundgren, G. Cella, C. L. Mueller, V. Raymond, T. Z. Summerscales, Giacomo Ciani, A. Mullavey, B. P. Abbott, E. K. Gustafson, W. Katzman, R. J.E. Smith, D. E. Clark, Jonathan R. Gair, L. A. Forte, D. O. Bridges, Rebecca Fisher, J. Li, B. E. Aylott, F. Carbognani, Malik Rakhmanov, J. Worden, L. Williams, A. Le Roux, Prayush Kumar, S. Vass, N. A. Lockerbie, Roy Williams, Kyungmin Kim, A. M. Cruise, Fabrice Matichard, G. P. Newton, Ettore Majorana, S. Vitale, M. Fyffe, Yueh-Feng Liu, B. O'Reilly, P. Ehrens, Gabriela Gonzalez, J. M. Hallam, W. Kells, Lucía Santamaría, Vladimir Dergachev, James Whelan, M. Bitossi, E. Forsi, P. Ajith, R. Riesen, M. Cordier, K. Wette, Vuk Mandic, John J. Oh, Th. S. Bauer, D. B. Kelley, Timothy Evans, Zhihui Du, C. Adams, D. Sigg, Eric Oelker, S. W. Ballmer, Yi Pan, J. A. Giaime, Y. M. Kim, Tenglin Li, R. M. Cutler, Rosa Poggiani, P. Campsie, G. Moreno, S. P. Tarabrin, Shaun Hooper, D. F. Menéndez, P. Raffai, Stefan Goßler, I. Kowalska, J. Hanks, S. Van Der Putten, Ranjan Gupta, H. Radkins, E. Saracco, J. C. Barayoga, C. Tomlinson, Richard J. Abbott, Soma Mukherjee, Michael L. Gorodetsky, Drew Keppel, J. M. Berliner, T. Westphal, A. E. Villar, H. Müller-Ebhardt, M. V. Plissi, Nergis Mavalvala, David Coward, Jerome Degallaix, Sheon Chua, C. J. Guido, Christian Röver, R. Bonnand, L. Sperandio, D. S. Rabeling, Rocco Romano, I. Di Palma, Hartmut Grote, Farhan Feroz, G. Losurdo, John D. Scott, D. L. Kinzel, R. A. Mercer, Neil J. Cornish, Matthew P. Edgar, Jesper Munch, P. E. Lindquist, M. A. Frei, D. Fazi, S. H. Huttner, D. Atkinson, Andrew Melatos, M. Lorenzini, A. Masserot, L. Taffarello, Ilya Belopolski, A. Mytidis, Atsushi J. Nishizawa, H. J. Bulten, T. T. Fricke, Roberto Conte, C. Aulbert, D. Simakov, Scott Koranda, L. Matone, J. R. Leong, Evan Ochsner, A. J. Weinstein, P. T. Beyersdorf, M. Landry, L. Di Fiore, M. Barsuglia, A. Grant, L. Zhang, Roman Schnabel, J. E. Brau, B. Canuel, A. A. van Veggel, Efim A. Khazanov, G. Ballardin, M. Phelps, F. Clara, P. Thomas, Erik Katsavounidis, Douglas H Beck, M. J. Lubinski, K. Evans, Rajesh Kumar, Vladimir B. Braginsky, H. Vahlbruch, K. Riles, J. Y. Vinet, N. Fotopoulos, M. Weinert, F. Fidecaro, G. M. Guidi, A. Cumming, E. Genin, A. M. Gretarsson, J. Bauchrowitz, J. K. Blackburn, E. Chassande-Mottin, Sheila Rowan, Todd Adams, Gianluca Persichetti, G. Endroczi, Haixing Miao, S. L. Danilishin, O. Bock, István Rácz, K. L. Dooley, Lisa Barsotti, Alessandra Toncelli, R. J. G. Jonker, Jan Harms, D. Buskulic, F. Kawazoe, O. Torre, E. Cuoco, S. Meshkov, Seog Oh, H. Fehrmann, D. Moraru, Gianpietro Cagnoli, D. Yeaton-Massey, F. Vetrano, S. E. Dwyer, J. Pöld, Suvadeep Bose, Z. Márka, Alberto Vecchio, Will M. Farr, A. Dietz, B. Hughey, E. Steinert, M. R. Smith, M. Edwards, M. Pickenpack, A. Rocchi, T. Hong, Maria Ilaria Del Principe, M. Agathos, S. R. Morriss, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), The LIGO Scientific Collaboration, The Virgo Collaboration, Aasi, J., Abadie, J., Abbott, B. 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C., Dwyer, S., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Endr?czi, G., Engel, R., Etzel, T., Evans, K., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fairhurst, S., Farr, B. F., Farr, W. M., Favata, M., Fazi, D., Fehrmann, H., Feldbaum, D., Feroz, F., Ferrante, I., Ferrini, F., Fidecaro, F., Finn, L. S., Fiori, I., Fisher, R. P., Flaminio, R., Foley, S., Forsi, E., Forte, L. A., Fotopoulos, N., Fournier, J. D., Franc, J., Franco, S., Frasca, S., Frasconi, F., Frede, M., Frei, M. A., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fujimoto, M. K., Fulda, P. J., Fyffe, M., Gair, J., Galimberti, M., Gammaitoni, L., Garcia, J., Garufi, Fabio, G?sp?r, M. E., Gelencser, G., Gemme, G., Genin, E., Gennai, A., Gergely, L. ?., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Gil Casanova, S., Gill, C., Gleason, J., Goetz, E., Gonz?lez, G., Gorodetsky, M. L., Go?ler, S., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Griffo, C., Grote, H., Grover, K., Grunewald, S., Guidi, G. M., Guido, C., Gupta, R., Gustafson, E. K., Gustafson, R., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hartman, M. T., Haster, C. J., Haughian, K., Hayama, K., Hayau, J. F., Heefner, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M. A., Heng, I. S., Heptonstall, A. W., Herrera, V., Heurs, M., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Holt, K., Holtrop, M., Hong, T., Hooper, S., Hough, J., Howell, E. J., Hughey, B., Husa, S., Huttner, S. H., Huynh Dinh, T., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Izumi, K., Jacobson, M., James, E., Jang, Y. J., Jaranowski, P., Jesse, E., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Kasprzack, M., Kasturi, R., Katsavounidis, E., Katzman, W., Kaufer, H., Kaufman, K., Kawabe, K., Kawamura, S., Kawazoe, F., Keitel, D., Kelley, D., Kells, W., Keppel, D. G., Keresztes, Z., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, B. K., Kim, C., Kim, H., Kim, K., Kim, N., Kim, Y. M., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kline, J., Kokeyama, K., Kondrashov, V., Koranda, S., Korth, W. Z., Kowalska, I., Kozak, D., Kringel, V., Krishnan, B., Kr?lak, A., Kuehn, G., Kumar, P., Kumar, R., Kurdyumov, R., Kwee, P., Lam, P. K., Landry, M., Langley, A., Lantz, B., Lastzka, N., Lawrie, C., Lazzarini, A., Le Roux, A., Leaci, P., Lee, C. H., Lee, H. K., Lee, H. M., Leong, J. R., Leonor, I., Leroy, N., Letendre, N., Lhuillier, V., Li, J., T. G. F., Li, Lindquist, P. E., Litvine, V., Liu, Y., Liu, Z., Lockerbie, N. A., Lodhia, D., Logue, J., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J., Lubinski, M., L?ck, H., Lundgren, A. P., Macarthur, J., Macdonald, E., Machenschalk, B., Macinnis, M., Macleod, D. M., Mageswaran, M., Mailand, K., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., M?rka, S., M?rka, Z., Markosyan, A., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mcguire, S. C., Mcintyre, G., Mciver, J., Meadors, G. D., Mehmet, M., Meier, T., Melatos, A., Melissinos, A. C., Mendell, G., Men?ndez, D. F., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Milano, L., Miller, J., Minenkov, Y., Mingarelli, C. M. F., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moe, B., Mohan, M., Mohapatra, S. R. P., Moraru, D., Moreno, G., Morgado, N., Morgia, A., Mori, T., Morriss, S. R., Mosca, S., Mossavi, K., Mours, B., Mow?lowry, C. M., Mueller, C. L., Mueller, G., Mukherjee, S., Mullavey, A., M?ller Ebhardt, H., Munch, J., Murphy, D., Murray, P. G., Mytidis, A., Nash, T., Naticchioni, L., Necula, V., Nelson, J., Neri, I., Newton, G., Nguyen, T., Nishizawa, A., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E., Nuttall, L., Ochsner, E., O?dell, J., Oelker, E., Ogin, G. H., J. J., Oh, S. H., Oh, Oldenberg, R. G., O?reilly, B., O?shaughnessy, R., Osthelder, C., Ott, C. D., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Palladino, L., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Paoletti, R., Papa, M. A., Parisi, M., Pasqualetti, A., Passaquieti, R., Passuello, D., Pedraza, M., Penn, S., Perreca, A., Persichetti, G., Phelps, M., Pichot, M., Pickenpack, M., Piergiovanni, F., Pierro, V., Pihlaja, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., P?ld, J., Postiglione, F., Poux, C., Prato, M., Predoi, V., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Quitzow James, R., Raab, F. J., Rabeling, D. S., R?cz, I., Radkins, H., Raffai, P., Rakhmanov, M., Ramet, C., Rankins, B., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Roberts, M., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rodriguez, C., Rodruck, M., Rolland, L., Rollins, J. G., Romano, R., Romie, J. H., Rosi?ska, D., R?ver, C., Rowan, S., R?diger, A., Ruggi, P., Ryan, K., Salemi, F., Sammut, L., Sandberg, V., Sankar, S., Sannibale, V., Santamar?a, L., Santiago Prieto, I., Santostasi, G., Saracco, E., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Savage, R. L., Schilling, R., Schnabel, R., Schofield, R. M. S., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Seifert, F., Sellers, D., Sentenac, D., Sergeev, A., Shaddock, D. A., Shaltev, M., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sidery, T. L., Siemens, X., Sigg, D., Simakov, D., Singer, A., Singer, L., Sintes, A. M., Skelton, G. R., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, R. J. E., Smith Lefebvre, N. D., Somiya, K., Sorazu, B., Speirits, F. C., Sperandio, L., Stefszky, M., Steinert, E., Steinlechner, J., Steinlechner, S., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S. E., Stroeer, A. S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Swinkels, B., Szeifert, G., Tacca, M., Taffarello, L., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, R., ter Braack, A. P. M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Th?ring, A., Titsler, C., Tokmakov, K. V., Tomlinson, C., Toncelli, A., Tonelli, M., Torre, O., Torres, C. V., Torrie, C. I., Tournefier, E., Travasso, F., Traylor, G., Tse, M., Ugolini, D., Vahlbruch, H., Vajente, G., van den Brand, J. F. J., Van Den Broeck, C., van der Putten, S., van Veggel, A. A., Vass, S., Vasuth, M., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Vicer?, A., Villar, A. E., Vinet, J. Y., Vitale, S., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A., Wade, L., Wade, M., Waldman, S. J., Wallace, L., Wan, Y., Wang, M., Wang, X., Wanner, A., Ward, R. L., Was, M., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D. J., Whiting, B. F., Wiesner, K., Wilkinson, C., Willems, P. A., Williams, L., Williams, R., Willke, B., Wimmer, M., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Wittel, H., Woan, G., Wooley, R., Worden, J., Yablon, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yancey, C. C., Yang, H., Yeaton Massey, D., Yoshida, S., Yvert, M., Zadro?ny, A., Zanolin, M., Zendri, J. P., Zhang, F., Zhang, L., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Pinto, Innocenzo, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), ESPCI ParisTech, Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Gravitation ( APC-Gravitation ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and (Astro)-Particles Physics
Subjects: Gravitational-wave observatory, Physics and Astronomy (miscellaneous), ELECTROMAGNETIC COUNTERPARTS, MASS-DISTRIBUTION, BLACK-HOLES, TRANSIENTS, INSPIRALS, COSMOLOGY, PHYSICS, SEARCH, Astrophysics, Parameter space, 01 natural sciences, neutron stars, General Relativity and Quantum Cosmology, Detection of gravitational wave, 010303 astronomy & astrophysics, QC, LIGO Scientific Collaboration, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Estimation theory, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Detector, Settore FIS/01 - Fisica Sperimentale, Nuclear and High Energy Physics, Justice and Strong Institutions, gravitational waves, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, Algorithm, Gravitation, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], SDG 16 - Peace, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, 010308 nuclear & particles physics, Gravitational wave, Model selection, SDG 16 - Peace, Justice and Strong Institutions, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], black holes, LIGO, cosmology: observations, [ SDU.ASTR.HE ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]
Abstract: Compact binary systems with neutron stars or black holes are one of the most promising sources for ground-based gravitational wave detectors. Gravitational radiation encodes rich information about source physics; thus parameter estimation and model selection are crucial analysis steps for any detection candidate events. Detailed models of the anticipated waveforms enable inference on several parameters, such as component masses, spins, sky location and distance that are essential for new astrophysical studies of these sources. However, accurate measurements of these parameters and discrimination of models describing the underlying physics are complicated by artifacts in the data, uncertainties in the waveform models and in the calibration of the detectors. Here we report such measurements on a selection of simulated signals added either in hardware or software to the data collected by the two LIGO instruments and the Virgo detector during their most recent joint science run, including a "blind injection" where the signal was not initially revealed to the collaboration. We exemplify the ability to extract information about the source physics on signals that cover the neutron star and black hole parameter space over the individual mass range 1 Msun - 25 Msun and the full range of spin parameters. The cases reported in this study provide a snap-shot of the status of parameter estimation in preparation for the operation of advanced detectors., Comment: 23 pages, 18 figures. LIGO Document P1200021. See the announcement for this paper on ligo.org at: http://www.ligo.org/science/Publication-S6PE/index.php. For a repository of data used in the publication, go to: https://dcc.ligo.org/LIGO-P1200021/public; Modifications thanks to referee reports
Published: 2013
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47. Discovery of the Optical Counterparts to Four Energetic Fermi Millisecond Pulsars

Author: Rene P. Breton, Scott M. Ransom, Maura McLaughlin, Mallory S. E. Roberts, Paul S. Ray, Fernando Camilo, M. H. van Kerkwijk, Jason W. T. Hessels, Ingrid H. Stairs, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Millisecond, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Luminosity, Neutron star, Pulsar, Space and Planetary Science, Millisecond pulsar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Roche lobe, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract: In the last few years, over 43 millisecond radio pulsars have been discovered by targeted searches of unidentified gamma-ray sources found by the Fermi Gamma-Ray Space Telescope. A large fraction of these millisecond pulsars are in compact binaries with low-mass companions. These systems often show eclipses of the pulsar signal and are commonly known as black widows and redbacks because the pulsar is gradually destroying its companion. In this paper, we report on the optical discovery of four strongly irradiated millisecond pulsar companions. All four sources show modulations of their color and luminosity at the known orbital periods from radio timing. Light curve modelling of our exploratory data shows that the equilibrium temperature reached on the companion's dayside with respect to their nightside is consistent with about 10-30% of the available spin-down energy from the pulsar being reprocessed to increase the companion's dayside temperature. This value compares well with the range observed in other irradiated pulsar binaries and offers insights about the energetics of the pulsar wind and the production of gamma-ray emission. In addition, this provides a simple way of estimating the brightness of irradiated pulsar companions given the pulsar spin-down luminosity. Our analysis also suggests that two of the four new irradiated pulsar companions are only partially filling their Roche lobe. Some of these sources are relatively bright and represent good targets for spectroscopic follow-up. These measurements could enable, among other things, mass determination of the neutron stars in these systems., 11 pages, 5 tables, 1 figure, 4 online tables. ApJ submitted and refereed
Published: 2013

48. X-Ray Observations of Black Widow Pulsars

Author: Jason W. T. Hessels, Paul S. Ray, Matthew Kerr, Mallory S. E. Roberts, Ingrid H. Stairs, Fernando Camilo, Scott M. Ransom, Maura McLaughlin, P. A. Gentile, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Orbital period, 01 natural sciences, Spectral line, Orbit, Pulsar, 13. Climate action, Space and Planetary Science, Millisecond pulsar, Observatory, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: We describe the first X-ray observations of five short orbital period ($P_B < 1$ day), $\gamma$-ray emitting, binary millisecond pulsars. Four of these, PSRs J0023+0923, J1124$-$3653, J1810+1744, and J2256$-$1024 are `black-widow' pulsars, with degenerate companions of mass $\ll0.1 M_{\odot}$, three of which exhibit radio eclipses. The fifth source, PSR J2215+5135, is an eclipsing `redback' with a near Roche-lobe filling $\sim$0.2 solar mass non-degenerate companion. Data were taken using the \textit{Chandra X-Ray Observatory} and covered a full binary orbit for each pulsar. Two pulsars, PSRs J2215+5135 and J2256$-$1024, show significant orbital variability while PSR J1124$-$3653 shows marginal orbital variability. The lightcurves for these three pulsars have X-ray flux minima coinciding with the phases of the radio eclipses. This phenomenon is consistent with an intrabinary shock emission interpretation for the X-rays. The other two pulsars, PSRs J0023+0923 and J1810+1744, are fainter and do not demonstrate variability at a level we can detect in these data. All five spectra are fit with three separate models: a power-law model, a blackbody model, and a combined model with both power-law and blackbody components. The preferred spectral fits yield power-law indices that range from 1.3 to 3.2 and blackbody temperatures in the hundreds of eV. The spectrum for PSR J2215+5135 shows a significant hard X-ray component, with a large number of counts above 2 keV, which is additional evidence for the presence of intrabinary shock emission and is similar to what has been detected in the low-mass X-ray binary to millisecond pulsar transition object PSR J1023+0038., Comment: 8 pages, 6 figures, 2 tables, submitted to ApJ
Published: 2013
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49. G11.2−0.3: THE YOUNG REMNANT OF A STRIPPED-ENVELOPE SUPERNOVA

Author: Mallory S. E. Roberts, Kazimierz J. Borkowski, and Stephen P. Reynolds
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Nebula, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Shell (structure), FOS: Physical sciences, Astronomy and Astrophysics, Torus, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Supernova, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We present results of a 400-ks Chandra observation of the young shell supernova remnant (SNR) G11.2-0.3, containing a pulsar and pulsar-wind nebula (PWN). We measure a mean expansion rate for the shell since 2000 of 0.0277+/-0.0018% per yr, implying an age between 1400 and 2400 yr, and making G11.2-0.3 one of the youngest core-collapse SNRs in the Galaxy. However, we find very high absorption ($A_V \sim 16^m \pm 2^m$), confirming near-IR determinations and ruling out a claimed association with the possible historical SN of 386 CE. The PWN shows strong jets and a faint torus within a larger, more diffuse region of radio emission and nonthermal X-rays. Central soft thermal X-ray emission is anticorrelated with the PWN; that, and more detailed morphological evidence, indicates that the reverse shock has already reheated all ejecta and compressed the PWN. The pulsar characteristic energy-loss timescale is well in excess of the remnant age, and we suggest that the bright jets have been produced since the recompression. The relatively pronounced shell and diffuse hard X-ray emission in the interior, enhanced at the inner edge of the shell, indicate that the immediate circumstellar medium into which G11.2-0.3 is expanding was quite anisotropic. We propose a possible origin for G11.2-0.3 in a stripped-envelope progenitor that had lost almost all its envelope mass, in an anisotropic wind or due to binary interaction, leaving a compact core whose fast winds swept previously lost mass into a dense irregular shell, and which exploded as a Type cIIb or Ibc supernova., Comment: 20 pages, 14 figures, accepted for publication in ApJ
Published: 2016
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50. Discovery of TeV Gamma-ray Emission from CTA 1 by VERITAS

Author: A. N. Otte, G. H. Sembroski, M. P. Connolly, E. Aliu, T. J. N. Nelson, R. Welsing, K. Lee, L. Ciupik, M. Theiling, P. Moriarty, Eric V. Gotthelf, Geza Gyuk, N. Karlsson, J. P. Finley, Wei Cui, Q. Feng, Gernot Maier, T. C. Weekes, I. Telezhinsky, Jamie Holder, S. Thibadeau, D. Gall, Oleg Kargaltsev, A. O'Faolain de Bhroithe, H. Krawczynski, A. Furniss, N. Galante, S. P. Wakely, R. Mukherjee, R. A. Ong, E. Roache, R. Dickherber, H. Prokoph, S. Vincent, A. S. Madhavan, Wystan Benbow, Abraham D. Falcone, S. Griffin, G. Finnegan, A. W. Smith, Mallory S. E. Roberts, S. McArthur, C. Duke, B. Zitzer, P. T. Reynolds, P. Kaaret, K. Ragan, J. Tyler, F. Krennrich, Y. Khassen, M. Schroedter, A. Bouvier, Vikram V. Dwarkadas, M. Vivier, J. Grube, M. Beilicke, Manel Errando, D. Staszak, S. Federici, J. H. Buckley, P. Majumdar, J. S. Perkins, David Kieda, D. B. Saxon, E. Collins-Hughes, Luis C. Reyes, N. H. Park, David A. Williams, Patrick Slane, M. Orr, T. B. Humensky, T. Aune, S. Godambe, G. Hughes, T. Arlen, Lucy Fortson, A. Cesarini, John L. Quinn, Martin Pohl, J. Dumm, Vladimir Vassiliev, A. Varlotta, M. J. Lang, A. Weinstein, K. Tsurusaki, G. H. Gillanders, D. S. Hanna, G. Tešić, V. Bugaev, S. Archambault, and A. McCann
Subjects: catalog, gamma-rays: stars, Photon, Astrophysics::High Energy Astrophysical Phenomena, supernova remnant cta-1, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar wind nebula, atmospheric cherenkov telescopes, Pulsar, Observatory, hess j1825-137, evolution, 0103 physical sciences, pulsations, crab-nebula, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, pulsars: individual (psr j0007+7303), 010308 nuclear & particles physics, Gamma ray, Astronomy and Astrophysics, x-rays: individual (rx j0007.0+7303), astronomy, supernovae: individual (g119.5+10.2), x-ray, Space and Planetary Science, ddc:520, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, pulsar-wind nebulae, Fermi Gamma-ray Space Telescope
Abstract: We report the discovery of TeV gamma-ray emission coincident with the shell-type radio supernova remnant (SNR) CTA 1 using the VERITAS gamma-ray observatory. The source, VER J0006+729, was detected as a 6.5 standard deviation excess over background and shows an extended morphology, approximated by a two-dimensional Gaussian of semi-major (semi-minor) axis 0.30 degree (0.24 degree) and a centroid 5' from the Fermi gamma-ray pulsar PSR J0007+7303 and its X-ray pulsar wind nebula (PWN). The photon spectrum is well described by a power-law dN/dE = N_0 (E/3 TeV)^(-\Gamma), with a differential spectral index of \Gamma = 2.2 +- 0.2_stat +- 0.3_sys, and normalization N_0 = (9.1 +- 1.3_stat +- 1.7_sys) x 10^(-14) cm^(-2) s^(-1) TeV^(-1). The integral flux, F_\gamma = 4.0 x 10^(-12) erg cm^(-2) s^(-1) above 1 TeV, corresponds to 0.2% of the pulsar spin-down power at 1.4 kpc. The energetics, co-location with the SNR, and the relatively small extent of the TeV emission strongly argue for the PWN origin of the TeV photons. We consider the origin of the TeV emission in CTA 1., Comment: 10 pages, 9 figures, accepted for publication in ApJ
Published: 2012
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