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70 results on '"Mallory S. E. Roberts"'

1. 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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2. 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

3. 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

4. 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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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. 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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7. 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

8. 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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9. 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

10. 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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11. 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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12. 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. 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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. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singer, L. P., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stiles, D., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Van Bakel, N., Van Beuzekom, M., Van Den Brand, J. F. J., Van Den Broeck, C., Vander Hyde, D. C., Van Der Schaaf, L., Van Heijningen, J. V., Van Veggel, A. A., Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D. V., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. P., Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Archibald, A. M., Banaszak, S., Berndsen, A., Boyles, J., Cardoso, R. F., Chawla, P., Cherry, A., Dartez, L. P., Day, D., Epstein, C. R., Ford, A. J., Flanigan, J., Garcia, A., Hessels, J. W. T., Hinojosa, J., Jenet, F. A., Karako Argaman, C., Kaspi, V. M., Keane, E. F., Kondratiev, V. I., Kramer, M., Leake, S., Lorimer, D., Lunsford, G., Lynch, R. S., Martinez, J. G., Mata, A., Mclaughlin, M. A., Mcphee, C. A., Penucci, T., Ransom, S., Roberts, M. S. E., Rohr, M. D. W., Stairs, I. H., Stovall, K., Van Leeuwen, J., Walker, A. N., Wells, B. L., Abbott, B. .p., Abbott, T. .d., Abernathy, M. .r., Adhikari, R. .x., Adya, V. .b., Aguiar, O. .d., Altin, P. .a., Anderson, S. .b., Anderson, W. .g., Araya, M. .c., Arceneaux, C. .c., Areeda, J. .s., Arun, K. .g., Aston, S. .m., Bader, M. .k. .m., Baker, P. .t., Ballmer, S. .w., Barayoga, J. .c., Barclay, S. .e., Barish, B. .c., Batch, J. .c., Bell, A. .s., Bell, C. .j., Berger, B. .k., Berry, C. .p. .l., Bilenko, I. .a., Bizouard, M. .a., Blackburn, J. .k., Blair, C. .d., Blair, D. .g., Blair, R. .m., Bodiya, T. .p., Boom, B. .a., Brady, P. .r., Braginsky, V. .b., BRANCHESI, MARICA, Brau, J. .e., Brooks, A. .f., Brown, D. .a., Brown, D. .d., Brown, N. .m., Buchanan, C. .c., Bulten, H. .j., Byer, R. .l., Calloni, E., Camp, J. .b., Cannon, K. .c., Capano, C. .d., Cepeda, C. .b., CERBONI BAIARDI, LORENZO, Chamberlin, S. .j., Chen, H. .y., Cho, H. .s., Chow, J. .h., Clark, J. .a., Collette, C. .g., Corbitt, T. .r., Costa, C. .a., Coughlin, M. .w., Coughlin, S. .b., Countryman, S. .t., Coward, D. .m., Cowart, M. .j., Coyne, D. .c., Creighton, J. .d. .e., Crowder, S. .g., Danilishin, S. .l., D’Antonio, S., Darman, N. .s., Daveloza, H. .p., Davies, G. .s., Daw, E. .j., De Laurentis, M., De Rosa, R., Derosa, R. .t., Díaz, M. .c., Di Girolamo, T., Dooley, K. .l., Downes, T. .p., Drever, R. .w. .p., Driggers, J. .c., Dwyer, S. .e., Edo, T. .b., Edwards, M. .c., Eikenberry, S. .s., Essick, R. .c., Evans, T. .m., Farr, W. .m., Fejer, M. .m., Ferreira, E. .c., Fisher, R. .p., Fricke, T. .t., Frolov, V. .v., Gabbard, H. .a. .g., Gair, J. .r., Gaonkar, S. .g., Garufi, F., Giaime, J. .a., Giardina, K. .d., Gordon, N. .a., Gorodetsky, M. .l., Gossan, S. .e., Graff, P. .b., GRECO, GIUSEPPE, Green, A. .c., GUIDI, GIANLUCA MARIA, Gupta, M. .k., Gushwa, K. .e., Gustafson, E. .k., Hacker, J. .j., Hall, B. .r., Hall, E. .d., Hanke, M. .m., Hannam, M. .d., HARMS, JAN, Harry, G. .m., Harry, I. .w., Hart, M. .j., Hartman, M. .t., Heintze, M. .c., Heng, I. .s., Heptonstall, A. .w., Hodge, K. .a., Hollitt, S. .e., Holz, D. .e., Hosken, D. .j., Houston, E. .a., Howell, E. .j., Hu, Y. .m., Huerta, E. .a., Huttner, S. .h., Ingram, D. .r., Isa, H. .n., Iyer, B. .r., Johnson, W. .w., Jones, D. .i., Jonker, R. .j. .g., Kalaghatgi, C. .v., Kanner, J. .b., Kehl, M. .s., Kelley, D. .b., Key, J. .s., Khalili, F. .y., Khazanov, E. .a., King, E. .j., King, P. .j., Kinzel, D. .l., Kissel, J. .s., Koehlenbeck, S. .m., Korth, W. .z., Kozak, D. .b., Lackey, B. .d., Lasky, P. .d., Lebigot, E. .o., Lee, C. .h., Lee, H. .k., Lee, H. .m., Leong, J. .r., Levine, B. .m., Li, T. .g. .f., Littenberg, T. .b., Lockerbie, N. .a., Lombardi, A. .l., Lord, J. .e., Lough, J. .d., Lundgren, A. .p., Macleod, D. .m., Magee, R. .m., Mansell, G. .l., Markosyan, A. .s., MARTELLI, FILIPPO, Martin, I. .w., Martin, R. .m., Martynov, D. .v., Marx, J. .n., Massinger, T. .j., Mcclelland, D. .e., Mcguire, S. .c., Mcmanus, D. .j., Mcwilliams, S. .t., Meadors, G. .d., Mercer, R. .a., Merilh, E. .l., Meyers, P. .m., 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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13. 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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14. 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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15. 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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16. 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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17. 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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18. 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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19. 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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20. 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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21. 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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22. 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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23. 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

24. 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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25. [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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26. 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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27. 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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28. 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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29. 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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30. 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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31. 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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32. 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

33. 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

34. 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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35. 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

36. 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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37. 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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38. 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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39. Chandra Observations of Black-Widow Pulsars

Author

Fernando Camilo, Scott M. Ransom, Ingrid H. Stairs, Paul S. Ray, Mallory S. E. Roberts, Maura McLaughlin, Jason W. T. Hessels, Matthew Kerr, and Peter A. Gentile

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Solar mass, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Orbit, Pulsar, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Millisecond pulsar, Observatory, Black-body radiation, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR), Fermi Gamma-ray Space Telescope
Abstract

We describe the first X-ray observations of binary millisecond pulsars PSRs J0023+0923, J1810+1744, J2215+5135, and J2256-1024. All four are Fermi gamma-ray sources and three are 'black-widow' pulsars, with companions of mass < 0.1 solar masses. Data were taken using the 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 and X-ray flux minima at the times of eclipses observed at radio wavelengths. This phenomenon is consistent with intrabinary shock emission characteristic of black-widow pulsars. The other two pulsars, PSRs J0023+0923 and J1810+1744, do not demonstrate significant variability, but are fainter than the other two sources. Spectral fits yield power-law indices that range from 1.4 to 2.3 and blackbody temperatures in the hundreds of eV. The spectrum for PSR J2215+5135 shows a significant hard X-ray component (41% of counts are above 2 keV), which is additional evidence for the presence of intrabinary shock emission., 3 pages, 2 figures, 1 table, 2012 IAU General Assembly

Published
2012

40. Discovery of the Optical/Ultraviolet/Gamma-ray Counterpart to the Eclipsing Millisecond Pulsar J1816+4510

Author

V. I. Kondratiev, Maura McLaughlin, L. P. Dartez, V. M. Kaspi, Kevin Stovall, D. Day, Alejandro Garcia, Fredrick A. Jenet, Mallory S. E. Roberts, Scott M. Ransom, Ingrid H. Stairs, A. J. Ford, C. Karako, Ryan S. Lynch, Duncan R. Lorimer, J. van Leeuwen, Xavier Siemens, Jason W. T. Hessels, Anne M. Archibald, Ralf Kotulla, Christopher M. Biwer, Jason Boyles, David L. Kaplan, M. D. Rohr, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Green Bank Telescope, White dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 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, 010306 general physics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract

The energetic, eclipsing millisecond pulsar J1816+4510 was recently discovered in a low-frequency radio survey with the Green Bank Telescope. With an orbital period of 8.7 hr and minimum companion mass of 0.16 Msun it appears to belong to an increasingly important class of pulsars that are ablating their low-mass companions. We report the discovery of the gamma-ray counterpart to this pulsar, and present a likely optical/ultraviolet counterpart as well. Using the radio ephemeris we detect pulsations in the unclassified gamma-ray source 2FGL J1816.5+4511, implying an efficiency of ~25% in converting the pulsar's spin-down luminosity into gamma-rays and adding PSR J1816+4510 to the large number of millisecond pulsars detected by Fermi. The likely optical/UV counterpart was identified through position coincidence (15,000 K it would be among the brightest and hottest of low-mass pulsar companions, and appears qualitatively different from other eclipsing pulsar systems. In particular, current data suggest that it is a factor of two larger than most white dwarfs of its mass, but a factor of four smaller than its Roche lobe. We discuss possible reasons for its high temperature and odd size, and suggest that it recently underwent a violent episode of mass loss. Regardless of origin, its brightness and the relative unimportance of irradiation make it an ideal target for a mass, and hence a neutron star mass, determination., 10 pages, 6 figures. Accepted for publication in the Astrophysical Journal

Published
2012
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41. The Green Bank Telescope 350 MHz Drift-scan Survey I: Survey Observations and the Discovery of 13 Pulsars

Author

R. F. Cardoso, V. I. Kondratiev, Jason W. T. Hessels, V. M. Kaspi, Maura McLaughlin, C. Karako-Argaman, Scott M. Ransom, Aaron Berndsen, Courtney R. Epstein, Joeri van Leeuwen, Ingrid H. Stairs, Jason Boyles, Christie A. McPhee, Duncan R. Lorimer, Kevin Stovall, Mallory S. E. Roberts, Ryan S. Lynch, Timothy T. Pennucci, Anne M. Archibald, Angus Cherry, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, 010308 nuclear & particles physics, Green Bank Telescope, Search procedure, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Star system, Neutron star, Orbit, Pulsar, Space and Planetary Science, Millisecond pulsar, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

Over the summer of 2007, we obtained 1191 hours of `drift-scan' pulsar search observations with the Green Bank Telescope at a radio frequency of 350 MHz. Here we describe the survey setup, search procedure, and the discovery and follow-up timing of thirteen pulsars. Among the new discoveries, one (PSR J1623-0841) was discovered only through its single pulses, two (PSRs J1327-0755 and J1737-0814) are millisecond pulsars, and another (PSR J2222-0137) is a mildly recycled pulsar. PSR J1327-0755 is a 2.7 ms pulsar at a DM of 27.9 pc cm^{-3} in a 8.7 day orbit with a minimum companion mass of 0.22 solar mass. PSR J1737-0814 is a 4.2 ms pulsar at a DM of 55.3 pc cm^{-3} in a 79.3 day orbit with a minimum companion mass of 0.06 solar mass. PSR J2222-0137 is a 32.8 ms pulsar at a very low DM of 3.27 pc cm^{-3} in a 2.4 day orbit with a minimum companion mass of 1.11 solar mass. It is most likely a white dwarf-neutron star system or an unusual low-eccentricity double neutron star system. Ten other pulsars discovered in this survey are reported in the companion paper Lynch et al. 2012., Comment: Companion paper to "The Green Bank Telescope 350 MHz Drift-scan Survey II: Data Analysis and the Timing of 10 New Pulsars, Including a Relativistic Binary", Submitted to ApJ, 29 pages, 7 figures, 8 tables

Published
2012
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42. Three Millisecond Pulsars in FERMI LAT Unassociated Bright Sources

Author

Fernando Camilo, Michael Kramer, David A. Smith, Roger W. Romani, Davide Donato, Michael Keith, C. Gwon, D. Parent, Mallory S. E. Roberts, M. E. DeCesar, Lucas Guillemot, Gregory Desvignes, Michael T. Wolff, Scott M. Ransom, Gilles Theureau, Paul S. Ray, Andrew Lyne, Ismaël Cognard, Simon Johnston, Timothy T. Pennucci, Ben Stappers, A. A. Abdo, J. E. Grove, Paulo C. C. Freire, Matthew Kerr, K. S. Wood, C. C. Cheung, Elizabeth C. Ferrara, Peter F. Michelson, Patrick Weltevrede, Neil Gehrels, D. J. Thompson, Alice K. Harding, P. M. Saz Parkinson, O. Celik, M. Ziegler, 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), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), and Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Binary number, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 97.60.Gb, 95.85.Bh, Spectral line, Pulsar, Millisecond pulsar, pulsars: general, 0103 physical sciences, pulsars: individual (J0614−3329 J1231−1411 J2214+3000), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::Instrumentation and Methods for Astrophysics, Green Bank Telescope, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract

We searched for radio pulsars in 25 of the non-variable, unassociated sources in the Fermi LAT Bright Source List with the Green Bank Telescope at 820 MHz. We report the discovery of three radio and gamma-ray millisecond pulsars (MSPs) from a high Galactic latitude subset of these sources. All of the pulsars are in binary systems, which would have made them virtually impossible to detect in blind gamma-ray pulsation searches. They seem to be relatively normal, nearby (, Accepted for publication in ApJ Letters

Published
2011
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43. A two-solar-mass neutron star measured using Shapiro delay

Author

Timothy T. Pennucci, Paul Demorest, Jason W. T. Hessels, Mallory S. E. Roberts, Scott M. Ransom, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Physics, Neutron star, Multidisciplinary, Pulsar, Quark star, Millisecond pulsar, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, Astronomy, Astrophysics, Shapiro delay, Binary pulsar, X-ray pulsar
Abstract

Neutron stars are composed of the densest form of matter known to exist in our Universe, the composition and properties of which are still theoretically uncertain. Measurements of the masses or radii of these objects can strongly constrain the neutron star matter equation of state and rule out theoretical models of their composition(1,2). The observed range of neutron star masses, however, has hitherto been too narrow to rule out many predictions of 'exotic' non-nucleonic components(3-6). The Shapiro delay is a general-relativistic increase in light travel time through the curved space-time near a massive body(7). For highly inclined (nearly edge-on) binary millisecond radio pulsar systems, this effect allows us to infer the masses of both the neutron star and its binary companion to high precision(8,9). Here we present radio timing observations of the binary millisecond pulsar J1614-2230(10,11) that show a strong Shapiro delay signature. We calculate the pulsar mass to be (1.97 +/- 0.04) M-circle dot, which rules out almost all currently proposed(2-5) hyperon or boson condensate equations of state (M-circle dot, solar mass). Quark matter can support a star this massive only if the quarks are strongly interacting and are therefore not 'free' quarks(12).

Published
2010

44. Radio detection of LAT PSRs J1741-2054 and J2032+4127: no longer just gamma-ray pulsars

Author

Roger W. Romani, Paul Demorest, Alice K. Harding, Scott M. Ransom, Tyrel J. Johnson, Michael Kramer, Fronefield Crawford, P. M. Saz Parkinson, M. Dormody, Matthew Kerr, K. S. Wood, Eric V. Gotthelf, John Reynolds, W. van Straten, David A. Smith, Simon Johnston, D. J. Thompson, Michael Keith, A. A. Abdo, Patrick Weltevrede, Paulo C. C. Freire, Fernando Camilo, Paul S. Ray, Jules P. Halpern, Mallory S. E. Roberts, M. Burgay, M. Ziegler, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), and Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, ISM: individual: TeV J2032+4130, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar wind nebula, X-rays: individual: Swift J174157.6-205411, Luminosity, law.invention, Telescope, Pulsar, Spitzer Space Telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, open clusters and associations: individual: Cyg OB2, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), pulsars: individual: PSR J1741-2054 PSR J2032+4127, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Green Bank Telescope, HEGRA, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, gamma rays: observations, Fermi Gamma-ray Space Telescope
Abstract

Sixteen pulsars have been discovered so far in blind searches of photons collected with the Large Area Telescope on the Fermi Gamma-ray Space Telescope. We here report the discovery of radio pulsations from two of them. PSR J1741-2054, with period P=413ms, was detected in archival Parkes telescope data and subsequently has been detected at the Green Bank Telescope (GBT). Its received flux varies greatly due to interstellar scintillation and it has a very small dispersion measure of DM=4.7pc/cc, implying a distance of ~0.4kpc and possibly the smallest luminosity of any known radio pulsar. At this distance, for isotropic emission, its gamma-ray luminosity above 0.1GeV corresponds to 25% of the spin-down luminosity of dE/dt=9.4e33erg/s. The gamma-ray profile occupies 1/3 of pulse phase and has three closely-spaced peaks with the first peak lagging the radio pulse by delta=0.29P. We have also identified a soft Swift source that is the likely X-ray counterpart. In many respects PSR J1741-2054 resembles the Geminga pulsar. The second source, PSR J2032+4127, was detected at the GBT. It has P=143ms, and its DM=115pc/cc suggests a distance of ~3.6kpc, but we consider it likely that it is located within the Cyg OB2 stellar association at half that distance. The radio emission is nearly 100% linearly polarized, and the main radio peak precedes by delta=0.15P the first of two narrow gamma-ray peaks that are separated by Delta=0.50P. Faint, diffuse X-ray emission in a Chandra image is possibly its pulsar wind nebula. PSR J2032+4127 likely accounts for the EGRET source 3EG J2033+4118, while its pulsar wind is responsible for the formerly unidentified HEGRA source TeV J2032+4130., Comment: accepted for publication in ApJ

Published
2009
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45. A radio pulsar/X-ray binary link

Author

David Champion, Ingrid H. Stairs, Duncan R. Lorimer, Jason W. T. Hessels, Mallory S. E. Roberts, Brad N. Barlow, R. Rosen, V. I. Kondratiev, Frederick Jenet, Anne M. Archibald, Ronald A. Remillard, Scott M. Ransom, B. H. Dunlap, Joeri van Leeuwen, Jason Boyles, Ryan S. Lynch, Victoria M. Kaspi, Maura McLaughlin, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Millisecond, Multidisciplinary, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, FOS: Physical sciences, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Binary pulsar, Neutron star, Astrophysics - Solar and Stellar Astrophysics, Pulsar, Millisecond pulsar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Circular orbit, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), X-ray pulsar
Abstract

Radio pulsars with millisecond spin periods are thought to have been spun up by transfer of matter and angular momentum from a low-mass companion star during an X-ray-emitting phase. The spin periods of the neutron stars in several such low-mass X-ray binary (LMXB) systems have been shown to be in the millisecond regime, but no radio pulsations have been detected. Here we report on detection and follow-up observations of a nearby radio millisecond pulsar (MSP) in a circular binary orbit with an optically identified companion star. Optical observations indicate that an accretion disk was present in this system within the last decade. Our optical data show no evidence that one exists today, suggesting that the radio MSP has turned on after a recent LMXB phase., Comment: published in Science

Published
2009

46. Pulsars Everywhere! A Galactic EGRET Source Retrospective

Author

Mallory S. E. Roberts, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi

Subjects
Physics, biology, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, biology.organism_classification, Pulsar wind nebula, Galaxy, Supernova, Neutron star, Pulsar, Astrophysics::Solar and Stellar Astrophysics, Egret, Gamma-ray burst, Supernova remnant, Astrophysics::Galaxy Astrophysics
Abstract

At the end of the EGRET mission, the only firmly identified sources of GeV emission in our Galaxy were a handful of young pulsars and a solar flare. With the recent launch of AGILE and the imminent launch of GLAST, the sources that EGRET saw will again be studied in γ‐rays. We review the multiwavelength observations of the error boxes of Galactic EGRET sources to see what types of sources this new generation of γ‐ray telescopes will be studying. I note that most, if not all, of the sources seem to be related to pulsars. Several are probably radio pulsars not known during the time of EGRET. Others are radio‐quiet pulsars like Geminga. Still others are probably the product of a pulsar wind interacting with a dense environment. The rest seem to be coincident with things associated with the birth of pulsars i.e. supernova remnants, molecular clouds, and massive star associations.

Published
2008
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47. Pulsar Timing for the Fermi Gamma-ray Space Telescope

Author

Na Wang, Ismaël Cognard, Mallory S. E. Roberts, D. Dumora, Michael Kramer, Patrick Weltevrede, Victoria M. Kaspi, Roger W. Romani, Richard N. Manchester, Andrew Lyne, A. Noutsos, Maura McLaughlin, Eric V. Gotthelf, Stephen E. Thorsett, Paulo C. C. Freire, Ben Stappers, Fernando Camilo, D. J. Thompson, David A. Smith, F. E. Marshall, Scott M. Ransom, Alice K. Harding, George Hobbs, Gilles Theureau, Simon Johnston, Margaret A. Livingstone, L. Guillemot, Cristobal M. Espinoza, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique et chimie de l'environnement (LPCE), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and 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)

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Supernova, Neutron star, Spitzer Space Telescope, Pulsar, Space and Planetary Science, law, 0103 physical sciences, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract

We describe a comprehensive pulsar monitoring campaign for the Large Area Telescope (LAT) on the {\em Fermi Gamma-ray Space Telescope} (formerly GLAST). The detection and study of pulsars in gamma rays give insights into the populations of neutron stars and supernova rates in the Galaxy, into particle acceleration mechanisms in neutron star magnetospheres, and into the "engines" driving pulsar wind nebulae. LAT's unprecedented sensitivity between 20 MeV and 300 GeV together with its 2.4 sr field-of-view makes detection of many gamma-ray pulsars likely, justifying the monitoring of over two hundred pulsars with large spin-down powers. To search for gamma-ray pulsations from most of these pulsars requires a set of phase-connected timing solutions spanning a year or more to properly align the sparse photon arrival times. We describe the choice of pulsars and the instruments involved in the campaign. Attention is paid to verifications of the LAT pulsar software, using for example giant radio pulses from the Crab and from PSR B1937+21 recorded at Nan\c{c}ay, and using X-ray data on PSR J0218+4232 from XMM-Newton. We demonstrate accuracy of the pulsar phase calculations at the microsecond level. Data Table 1 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/ ., Comment: 13 pages, 6 figures. Accepted for publication in Astronomy & Astrophysics

Published
2008
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48. The Unusual Binary Pulsar PSR J1744-3922: Radio Flux Variability, Near-infrared Observation and Evolution

Author

A. J. Faulkner, Rene P. Breton, Scott M. Ransom, Victoria M. Kaspi, Mallory S. E. Roberts, Martin Durant, and Pierre Bergeron

Subjects
Physics, 010504 meteorology & atmospheric sciences, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Astrophysics, Magnetar, 01 natural sciences, Binary pulsar, Orbit, Common envelope, Neutron star, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

PSR J1744-3922 is a binary pulsar exhibiting highly variable pulsed radio emission. We report on a statistical multi-frequency study of the pulsed radio flux variability which suggests that this phenomenon is extrinsic to the pulsar and possibly tied to the companion, although not strongly correlated with orbital phase. The pulsar has an unusual combination of characteristics compared to typical recycled pulsars: a long spin period (172 ms); a relatively high magnetic field strength (1.7x10^10 G); a very circular, compact orbit of 4.6 hours; and a low-mass companion (0.08 Msun). These spin and orbital properties are likely inconsistent with standard evolutionary models. We find similarities between the properties of the PSR J1744-3922 system and those of several other known binary pulsar systems, motivating the identification of a new class of binary pulsars. We suggest that this new class could result from either: a standard accretion scenario of a magnetar or a high-magnetic field pulsar; common envelope evolution with a low-mass star and a neutron star, similar to what is expected for ultra-compact X-ray binaries; or, accretion induced collapse of a white dwarf. We also report the detection of a possible K'=19.30(15) infrared counterpart at the position of the pulsar, which is relatively bright if the companion is a helium white dwarf at the nominal distance, and discuss its implications for the pulsar's companion and evolutionary history., 18 pages, 8 figures, accepted for publication of ApJ

Published
2007

49. Runaway Massive Binaries and Cluster Ejection Scenarios

Author

Scott M. Ransom, M. Virginia McSwain, Mallory S. E. Roberts, Tabetha S. Boyajian, and Erika D. Grundstrom

Subjects
Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Compact star, 01 natural sciences, Stars, Supernova, Neutron star, Pulsar, Space and Planetary Science, 0103 physical sciences, Binary star, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Open cluster
Abstract

The production of runaway massive binaries offers key insights into the evolution of close binary stars and open clusters. The stars HD 14633 and HD 15137 are rare examples of such runaway systems, and in this work we investigate the mechanism by which they were ejected from their parent open cluster, NGC 654. We discuss observational characteristics that can be used to distinguish supernova ejected systems from those ejected by dynamical interactions, and we present the results of a new radio pulsar search of these systems as well as estimates of their predicted X-ray flux assuming that each binary contains a compact object. Since neither pulsars nor X-ray emission are observed in these systems, we cannot conclude that these binaries contain compact companions. We also consider whether they may have been ejected by dynamical interactions in the dense environment where they formed, and our simulations of four-body interactions suggest that a dynamical origin is possible but unlikely. We recommend further X-ray observations that will conclusively identify whether HD 14633 or HD 15137 contain neutron stars., Comment: Accepted to ApJ, 11 pages

Published
2007
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50. What Will Be The Brightest GLAST Sources in the Galaxy?

Author

Mallory S. E. Roberts

Subjects
Physics, Photon emission, biology, Solar flare, Pulsar, Egret, Astronomy, Astronomical telescopes, Astrophysics, biology.organism_classification, Gamma-ray burst, Galaxy, Gamma ray detection
Abstract

At the end of the EGRET mission, only 6 Galactic sources in the 3rd EGRET catalog had firm identifications: 5 young pulsars and a solar flare. Another dozen or so had plausible counterparts. Now, at the dawn of the GLAST era, around 30 sources detected at other wavelengths have been identified as probable or plausible counterparts. These include nearly all of the sources with significant emission above 1 GeV, which will be the sources GLAST will best be able to study. I review the current status of our knowledge of these sources based on radio, infrared, and X‐ray data. These Galactic sources are destined to be the first sources firmly identified by GLAST.

Published
2007
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