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1. Challenging the Forward Shock Model with the 80 Ms Follow up of the X-ray Afterglow of Gamma-Ray Burst 130427A

Author

Massimiliano De Pasquale, Mathew Page, David Alexander Kann, Samantha R. Oates, Steve Schulze, Bing Zhang, Zach Cano, Bruce Gendre, Daniele Malesani, Andrea Rossi, Neil Gehrels, Eleonora Troja, Luigi Piro, Michel Boër, and Giulia Stratta

Subjects
Gamma-ray bursts, X-ray afterglows, GRB modeling, Astronomy, QB1-991
Abstract

GRB 130427A was the most luminous gamma-ray burst detected in the last 30 years. With an isotropic energy output of 8.5 × 10 53 erg and redshift of 0.34, it combined very high energetics with a relative proximity to Earth in an unprecedented way. Sensitive X-ray observatories such as XMM-Newton and Chandra have detected the afterglow of this event for a record-breaking baseline longer than 80 million seconds. The light curve displays a simple power-law over more than three decades in time. In this presentation, we explore the consequences of this result for a few models put forward so far to interpret GRB 130427A, and more in general the implication of this outcome in the context of the standard forward shock model.

Published
2017
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2. The close environments of accreting massive black holes are shaped by radiative feedback

Author

Andrew C. Fabian, Ezequiel Treister, Michael Koss, Isabella Lamperti, Franz E. Bauer, Anna K. Weigel, Neil Gehrels, Claudio Ricci, Richard F. Mushotzky, Kyuseok Oh, Yanxia Xie, Stéphane Paltani, Benny Trakhtenbrot, Yoshihiro Ueda, Luis C. Ho, Kevin Schawinski, Fabian, Andrew [0000-0002-9378-4072], and Apollo - University of Cambridge Repository

Subjects
galaxies and clusters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, Quasi-star, General Relativity and Quantum Cosmology, Binary black hole, 0103 physical sciences, 010303 astronomy & astrophysics, high-energy astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Supermassive black hole, Multidisciplinary, 010308 nuclear & particles physics, Astronomy, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), 13. Climate action, Intermediate-mass black hole, Astrophysics of Galaxies (astro-ph.GA), Stellar black hole, Astrophysics::Earth and Planetary Astrophysics, Spin-flip, Astrophysics - High Energy Astrophysical Phenomena, Schwarzschild radius, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The large majority of the accreting supermassive black holes in the Universe are obscured by large columns of gas and dust. The location and evolution of this obscuring material have been the subject of intense research in the past decades, and are still highly debated. A decrease in the covering factor of the circumnuclear material with increasing accretion rates has been found by studies carried out across the electromagnetic spectrum. The origin of this trend has been suggested to be driven either by the increase in the inner radius of the obscuring material with incident luminosity due to the sublimation of dust; by the gravitational potential of the black hole; by radiative feedback; or by the interplay between outflows and inflows. However, the lack of a large, unbiased and complete sample of accreting black holes, with reliable information on gas column density, luminosity and mass, has left the main physical mechanism regulating obscuration unclear. Using a systematic multi-wavelength survey of hard X-ray-selected black holes, here we show that radiation pressure on dusty gas is indeed the main physical mechanism regulating the distribution of the circumnuclear material. Our results imply that the bulk of the obscuring dust and gas in these objects is located within the sphere of influence of the black hole (i.e., a few to tens of parsecs), and that it can be swept away even at low radiative output rates. The main physical driver of the differences between obscured and unobscured accreting black holes is therefore their mass-normalized accretion rate., Comment: To appear in the 28 September 2017 issue of Nature. This is the authors' version of the work

Published
2017
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3. How to Swallow a Sun

Author

Neil Gehrels and S. Bradley Cenko

Subjects
Physics, Black hole, General Relativity and Quantum Cosmology, Supermassive black hole, Multidisciplinary, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Astrophysics::Galaxy Astrophysics, Galaxy
Abstract

The article focuses on studies on the growth and behavior of supermassive black holes in the hope to determine how galaxies are born and evolve. Topics covered include how a black hole can shred an entire star passing by, the ability of wide-field telescopes in allowing astronomers to study these cataclysmic events in detail, and how the growth of supermassive black holes shapes their surrounding galaxies.

Published
2017
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4. Multiband Observations of the Quasar PKS 2326–502 during Active and Quiescent Gamma-Ray States in 2010–2012

Author

Michael Dutka, Roberto Nesci, Justin D. Finke, Joern Wilms, Bryce Carpenter, Jamie Stevens, Neil Gehrels, Eleonora Torresi, Matthias Kadler, Roopesh Ojha, Felicia Krauss, Paola Grandi, Philip G. Edwards, Cornelia Mueller, Filippo D'Ammando, ITA, USA, DEU, High Energy Astrophys. & Astropart. Phys (API, FNWI), Dutka Michael S, Carpenter Bryce D, Ojha Roopesh, Finke Justin D, DAmmando F, Kadler Matthia, Edwards Philip G, Stevens Jamie, Torresi Eleonora, Grandi Paola, Nesci Roberto, Krauß Felicia, Müller Cornelia, Wilms Joern, and Gehrels Neil

Subjects
Astronomy, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Electron, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: individual (PKS 2326–502), 01 natural sciences, Radio spectrum, law.invention, law, 0103 physical sciences, gamma rays: galaxie, Astrophysics::Solar and Stellar Astrophysics, Blazar, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Gamma ray, Spectral density, Astronomy and Astrophysics, Quasar, quasars: individual (PKS 2326–502), Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), ultraviolet: galaxie, Spectral energy distribution, radio continuum: galaxie, Astrophysics - High Energy Astrophysical Phenomena, Flare
Abstract

Quasi-simultaneous observations of the Flat Spectrum Radio Quasar PKS 2326-502 were carried out in the gamma-ray, X-ray, UV, optical, near-infrared, and radio bands. Thanks to these observations we are able to characterize the spectral energy distribution of the source during two flaring and one quiescent gamma-ray states. These data were used to constrain one-zone leptonic models of the spectral energy distributions of each flare and investigate the physical conditions giving rise to them. While modeling one flare only required changes to the electron spectrum, the other flare needed changes in both the electron spectrum and the size of the emitting region with respect to the quiescent state. These results are consistent with an emerging pattern of two broad classes of flaring states seen in blazars., Comment: 18 pages, 3 figures. Accepted in the Astrophysical Journal

Published
2017
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5. Galaxy Strategy for LIGO-Virgo Gravitational Wave Counterpart Searches

Author

Mansi M. Kasliwal, John K. Cannizzo, Neil Gehrels, Samaya Nissanke, Jonah Kanner, and Leo Singer

Subjects
Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, Range (statistics), Fading, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Galaxy, LIGO, Afterglow, Space and Planetary Science, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - High Energy Astrophysical Phenomena
Abstract

In this work we continue a line of inquiry begun in Kanner et al. which detailed a strategy for utilizing telescopes with narrow fields of view, such as the Swift X-ray Telescope (XRT), to localize gravity wave (GW) triggers from LIGO/Virgo. If one considers the brightest galaxies that produce ~50% of the light, then the number of galaxies inside typical GW error boxes will be several tens. We have found that this result applies both in the early years of Advanced LIGO when the range is small and the error boxes large, and in the later years when the error boxes will be small and the range large. This strategy has the beneficial property of reducing the number of telescope pointings by a factor 10 to 100 compared with tiling the entire error box. Additional galaxy count reduction will come from a GW rapid distance estimate which will restrict the radial slice in search volume. Combining the bright galaxy strategy with a convolution based on anticipated GW localizations, we find that the searches can be restricted to about 18+/-5 galaxies for 2015, about 23+/-4 for 2017, and about 11+/-2 for 2020. This assumes a distance localization at or near the putative NS-NS merger range for each target year, and these totals are integrated out to the range. Integrating out to the horizon would roughly double the totals. For nearer localizations the totals would decrease. The galaxy strategy we present in this work will enable numerous sensitive optical and X-ray telescopes with small fields of view to participate meaningfully in searches wherein the prospects for rapidly fading afterglow place a premium on a fast response time., 8 pages, 4 figures, The Astrophysical Journal, submitted

Published
2016
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6. Hard X-ray properties of radio-selected blazars

Author

Matthias Kadler, M. Langejahn, Eugenia Litzinger, Craig B. Markwardt, Neil Gehrels, Jack Tueller, Jörn Wilms, Michael Kreter, Wayne H. Baumgartner, and 33379009 - Kreter, Michael

Subjects
statistical [Methods], Active galactic nucleus, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Radio spectrum, Spectral line, Luminosity, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, COSMIC cancer database, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, galaxies [X-rays], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena
Abstract

Context. Hard X-ray properties of beamed active galactic nuclei have been published in the 105-month Swift/BAT catalog, but there have not been any studies carried out so far on a well-defined, radio-selected sample of low-peaked blazars in the hard X-ray band. Aims. Using the statistically complete MOJAVE-1 sample, we aim to determine the hard X-ray properties of radio-selected blazars, including the enigmatic group of gamma-ray-faint blazars. Additionally, we aim to determine the contribution of radio-selected low-peaked blazars to the diffuse cosmic X-ray background (CXB). Methods. We determined photon indices, fluxes, and luminosities in the range of 20 keV–100 keV of the X-ray spectra of blazars and other extragalactic jets from the MOJAVE-1 sample, derived from the 105-month Swift/BAT survey. We calculated log N–log S distributions and determined the luminosity functions. Results. The majority of the MOJAVE-1 blazars are found to be hard X-ray emitters albeit many at low count rates. The log N–log S distribution for the hard X-ray emission of radio-selected blazars is clearly non-Euclidean, in contrast to the radio flux density distribution. Approximately 0.2% of the CXB in the 20 keV–100 keV band can be resolved into MOJAVE-1 blazars. Conclusions. The peculiar log N–log S distribution disparity might be attributed to different evolutionary paths in the X-ray and radio bands, as tested by luminosity-function modeling. X-ray variability can be ruled out as the dominant contributor. Low-peaked blazars constitute an intrinsically different source population in terms of CXB contribution compared to similar studies of X-ray-selected blazars. The hard X-ray flux and spectral index can serve as a good proxy for the gamma-ray detection probability of individual sources. Future observations combining deep X-ray survey, for example, with eROSITA, and targeted gamma-ray observations with CTA can benefit strongly from the tight connection between these high-energy bands for the different blazar sub-classes.

Published
2020
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7. GRB 130831a: Rise and demise of a magnetar at z = 0.5

Author

S. R. Oates, David Alexander Kann, Alexander Kutyrev, José A. de Diego, J. B. Haislip, N. Frank, Silvia Zane, O. M. Littlejohns, Steve Schulze, Vasilij Rumyantsev, Joshua S. Bloom, Eleonora Troja, Judith Racusin, V. Hoette, Alexei Pozanenko, A. A. Breeveld, Massimiliano De Pasquale, Harvey Moseley, A. S. Trotter, Ori D. Fox, Mat Page, Daniel E. Reichart, Zach Cano, J. Jesús González, B. Sbarufatti, Nathaniel R. Butler, Jason X. Prochaska, Alan M. Watson, A. Volnova, A. J. Castro-Tirado, Carlos Román-Zúñiga, Neil Gehrels, R. Russell, Javier Gorosabel, Bing Zhang, Michael G. Richer, O. A. Burkhonov, E. Klunko, Antonino Cucchiara, and A. Y. Lien

Subjects
Physics, Grossman, Field (physics), General relativity, Astronomy, Demise, Gamma-ray burst, Magnetar
Abstract

Open Access.--14th Marcel Grossman Meeting On Recent Developments in Theoretical and Experimental General Relativity, Astrophysics and Relativistic Field Theories; University of Rome "La Sapienza"Rome; Italy; 12 July 2015 through 18 July 2015; Code 142474.-- http://www.icra.it/mg/mg14/, Gamma-ray bursts (GRBs) are the brightest explosions in the universe, yet the properties of their energy sources are far from understood. Very important clues, however, can be deduced by studying the afterglows of these events. We present observations of GRB 130831A and its afterglow obtained with Swift, Chandra, and multiple ground-based observatories. This burst shows an uncommon drop in the X-ray light curve at about 100 ks after the trigger, with a decay slope of α 7. The standard Forward Shock (FS) model offers no explanation for such a behaviour. Instead, a model in which a newly born magnetar outflow powers the early X-ray emission is found to be viable. After the drop, the X-ray afterglow resumes its decay with a slope typical of FS emission. The optical emission, on the other hand, displays no clear break across the X-ray drop and its decay is consistent with that of the late X-rays. Using both the X-ray and optical data, we show that the FS model can explain the emission after 100 ks. We model our data to infer the kinetic energy of the ejecta and thus estimate the efficiency of a magnetar “central engine” of a GRB. Furthermore, we break down the energy budget of this GRB into prompt emission, late internal dissipation, kinetic energy of the relativistic ejecta, and compare it with the energy of the accompanying supernova, SN 2013fu. Copyright © 2018 by the Editors.All rights reserved.

Published
2018

8. The Swift X-ray monitoring campaign of the center of the Milky Way

Author

J. A. Kennea, Rudy Wijnands, Mark Reynolds, Neil Gehrels, Jonah Miller, Nathalie Degenaar, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Swift, Accretion, Milky Way, FOS: Physical sciences, Astrophysics, Magnetar, law.invention, Telescope, X-rays: binaries, Pulsar, law, computer.programming_language, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Supermassive black hole, Galaxy: center, Astronomy, Astronomy and Astrophysics, Black hole physics, Light curve, Stars: neutron, Accretion (astrophysics), Space and Planetary Science, Accretion disks, Astrophysics - High Energy Astrophysical Phenomena, computer
Abstract

In 2006 February, shortly after its launch, Swift began monitoring the center of the Milky Way with the onboard X-Ray Telescope using short 1-ks exposures performed every 1-4 days. Between 2006 and 2014, over 1200 observations have been obtained, amounting to ~1.2 Ms of exposure time. This has yielded a wealth of information about the long-term X-ray behavior of the supermassive black hole Sgr A*, and numerous transient X-ray binaries that are located within the 25'x25' region covered by the campaign. In this review we highlight the discoveries made during these first nine years, which includes 1) the detection of seven bright X-ray flares from Sgr A*, 2) the discovery of the magnetar SGR J1745-29, 3) the first systematic analysis of the outburst light curves and energetics of the peculiar class of very-faint X-ray binaries, 4) the discovery of three new transient X-ray sources, 5) exposing low-level accretion in otherwise bright X-ray binaries, and 6) the identification of a candidate X-ray binary/millisecond radio pulsar transitional object. We also reflect on future science to be done by continuing this Swift's legacy campaign of the Galactic center, which includes high-cadence monitoring of how the interaction between the gaseous object `G2' and Sgr A* plays out in the future., Comment: 13 pages, 6 figures, 4 tables. Invited review to appear in Elsevier's Journal of High Energy Astrophysics dedicated issue "Swift: 10 years of discovery"

Published
2015
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9. X-Ray and Radio Observations of the Magnetar SGR J1935+2154 during Its 2014, 2015, and 2016 Outbursts

Author

Ramandeep Gill, Alice K. Harding, Ersin Gogus, Lin Lin, Amruta Jaodand, Jonathan Granot, George Younes, Matthew G. Baring, Jason W. T. Hessels, Neil Gehrels, Daniela Huppenkothen, Alexander J. van der Horst, Chryssa Kouveliotou, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, Theoretical models, X-ray, FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Magnetar, 01 natural sciences, Imaging analysis, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Density limit, Maximum flux, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, 010303 astronomy & astrophysics
Abstract

We analyzed broad-band X-ray and radio data of the magnetar SGR J1935+2154 taken in the aftermath of its 2014, 2015, and 2016 outbursts. The source soft X-ray spectrum, Comment: 17 pages, 7 figures, 5 tables, submitted to ApJ, comments welcome

Published
2017

10. BAT AGN Spectroscopic Survey (BASS) – VI. The ΓX–L/LEdd relation

Author

Fiona A. Harrison, Kevin Schawinski, Mislav Baloković, Yoshihiro Ueda, Isabella Lamperti, Benny Trakhtenbrot, Daniel Stern, Claudio Ricci, Kyuseok Oh, Sylvain Veilleux, Richard F. Mushotzky, Neil Gehrels, Ezequiel Treister, and Michael Koss

Subjects
Physics, Supermassive black hole, Active galactic nucleus, Photon, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Space and Planetary Science, law, Stellar dynamics, 0103 physical sciences, Spectral energy distribution, Reverberation mapping, Maser, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We study the relation between accretion rate (in terms of L/L_(Edd)) and shape of the hard X-ray spectral energy distribution (namely the photon index Γ_x) for a large sample of 228 hard X-ray-selected, low-redshift active galactic nuclei (AGNs), drawn from the Swift/BAT AGN Spectroscopic Survey (BASS). This includes 30 AGNs for which black hole mass (and therefore L/L_(Edd)) is measured directly through masers, spatially resolved gas or stellar dynamics, or reverberation mapping. The high-quality and broad energy coverage of the data provided through BASS allow us to examine several alternative determinations of both Γ_x and L/L_(Edd). For the BASS sample as a whole, we find a statistically significant, albeit very weak correlation between Γ_x and L/L_(Edd). The best-fitting relations we find, Γ_x ≃ 0.15 log L/L_(Edd) + const., are considerably shallower than those reported in previous studies. Moreover, we find no corresponding correlations among the subsets of AGN with different MBH determination methodology. In particular, we find no robust evidence for a correlation when considering only those AGN with direct or single-epoch MBH estimates. This latter finding is in contrast to several previous studies which focused on z > 0.5 broad-line AGN. We discuss this tension and conclude that it can be partially accounted for if one adopts a simplified, power-law X-ray spectral model, combined with L/L_(Edd) estimates that are based on the continuum emission and on single-epoch broad-line spectroscopy in the optical regime. We finally highlight the limitations on using Γ_x as a probe of supermassive black hole evolution in deep extragalactic X-ray surveys.

Published
2017

11. GRBs in the Era of Rapid Response Telescopes

Author

John K. Cannizzo and Neil Gehrels

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, LOFAR, Kilonova, LIGO, Robotic telescope, Observatory, Astrophysics::Earth and Planetary Astrophysics, MAGIC (telescope), Gamma-ray burst, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

NASA's Swift and Fermi satellites continue to chase gamma-ray bursts (GRBs) and make ground-breaking discoveries. The resulting science has been greatly enhanced by follow-up studies and coincident event searches from a variety of observatories, including RAPTOR, Watcher, REM, Pi of the Sky, MASTER, iPTF, GROND, GTC, RATIR, DCT, Asiago, Nanshan, Liverpool Robotic Telescope, KAIT, NOT, Gemini, Magellan, Keck, VLT, VLA, ACTA, ALMA, AMI, WSRT, GMRT, CARMA, LOFAR, HAWC, VERITAS, MAGIC, HESS, IceCube, ANTARES, LIGO, HST, Chandra, Spitzer, Fermi, AGILE, INTEGRAL, NuSTAR, IPN, MAXI, CALET, and AstroSAT. These observatories have added to our knowledge of the early-time behavior of GRBs, such as the short-lived reverse-shock which has been seen now in a small handful of the brightest bursts. The emphasis on longer term optical observations, days to weeks after the burst, has increased with the prospects in a few years for multiple active gravitational wave observatories providing good localizations for compact object mergers, and the potential for seeing the isotropic kilonova emission if one of the objects is a neutron star.

Published
2017
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12. Swift monitoring of NGC 4151 : evidence for a second X-ray/UV reprocessing

Author

W. N. Brandt, K. L. Page, Misty C. Bentz, Encarni Romero-Colmenero, Dimitrios Emmanoulopoulos, Michael D. Joner, Steven M. Crawford, Hans A. Krimm, Gerard A. Kriss, H. A. Vogler, Tommaso Treu, S. Connolly, Marianne Vestergaard, Kirk T. Korista, J. A. Kennea, Aaron J. Barth, Phil Evans, WeiKang Zheng, Keith Horne, M. H. Siegel, M. R. Goad, Ian M. McHardy, A. A. Breeveld, Hagai Netzer, Alexei V. Filippenko, Chris Done, Simon Vaughan, E. Dalla Bontà, M. C. Bottorff, Dirk Grupe, Edward M. Cackett, Neil Gehrels, Hartmut Winkler, B. M. Peterson, Smita Mathur, Jonathan Gelbord, Michael Fausnaugh, Rick Edelson, Emma Gardner, D. A. Starkey, R. Figuera Jaimes, Gary J. Ferland, D. C. Leonard, J. A. Nousek, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Seyfert [Galaxies], galaxies: active, galaxies: individual (NGC 4151), galaxies: nuclei, galaxies: Seyfert, active [Galaxies], FOS: Physical sciences, Astrophysics, medicine.disease_cause, 01 natural sciences, individual (NGC 4151) [Galaxies], Accretion disc, 0103 physical sciences, medicine, QB Astronomy, 010303 astronomy & astrophysics, QC, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, X-ray, Astronomy and Astrophysics, 3rd-DAS, Light curve, Corona, QC Physics, Space and Planetary Science, nuclei [Galaxies], Astrophysics - High Energy Astrophysical Phenomena, Ultraviolet
Abstract

Swift monitoring of NGC 4151 with ~6 hr sampling over a total of 69 days in early 2016 is used to construct light curves covering five bands in the X-rays (0.3-50 keV) and six in the ultraviolet (UV)/optical (1900-5500 A). The three hardest X-ray bands (>2.5 keV) are all strongly correlated with no measurable interband lag while the two softer bands show lower variability and weaker correlations. The UV/optical bands are significantly correlated with the X-rays, lagging ~3-4 days behind the hard X-rays. The variability within the UV/optical bands is also strongly correlated, with the UV appearing to lead the optical by ~0.5-1 day. This combination of >~3 day lags between the X-rays and UV and, Comment: 14 pages, 6 figures, 7 tables. To appear in ApJ April 2017 issue. This version incorporates minor revisions to conform to published version and corrects the links to the author names above

Published
2017

13. Photospheric Emission in the Joint GBM and Konus Prompt Spectra of GRB 120323A

Author

Dieter H. Hartmann, Neil Gehrels, Chryssa Kouveliotou, Sylvain Guiriec, and J. McEnery

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Spectral shape analysis, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Spectral line, On board, Spitzer Space Telescope, Space and Planetary Science, 0103 physical sciences, Spectral analysis, Emission spectrum, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Fermi Gamma-ray Space Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

GRB 120323A is a very intense short Gamma Ray Burst (GRB) detected simultaneously during its prompt gamma-ray emission phase with the Gamma-ray Burst Monitor (GBM) on board the Fermi Gamma-ray Space Telescope and the Konus experiment on board the Wind satellite. GBM and Konus operate in the keV--MeV regime, however, the GBM range is broader both toward the low and the high parts of the gamma-ray spectrum. Analysis of such bright events provide a unique opportunity to check the consistency of the data analysis as well as cross-calibrate the two instruments. We performed time-integrated and coarse time-resolved spectral analysis of GRB 120323A prompt emission. We conclude that the analyses of GBM and Konus data are only consistent when using a double-hump spectral shape for both data sets; in contrast, the single-hump of the empirical Band function, traditionally used to fit GRB prompt emission spectra, leads to significant discrepancies between GBM and Konus analysis results. Our two-hump model is a combination of a thermal-like and a non-thermal component. We interpret the first component as a natural manifestation of the jet photospheric emission., 7 pages of article (3 figures and 1 table) + 3 pages of Appendix (3 figures). Submitted to ApJ on 2017 March 22

Published
2017

14. Photometric Observations of Supernova 2013cq Associated with GRB 130427A

Author

Nathaniel R. Butler, Alexander Kutyrev, Alan M. Watson, William H. Lee, Antonino Cucchiara, Nissim Fraija, J. Jesús González, O. M. Littlejohns, Vicki Toy, L. Georgiev, Josh Bloom, Rosa L. Becerra, Ori D. Fox, Neil Gehrels, J. A. de Diego, Carlos Román-Zúñiga, Jason X. Prochaska, Enrico Ramirez-Ruiz, Michael G. Richer, Eleonora Troja, and John Capone

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Absolute magnitude, Physics, FOS: Physical sciences, GRB 130427A, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Afterglow, law.invention, Photometry (optics), Telescope, Supernova, Space and Planetary Science, law, 0103 physical sciences, 010306 general physics, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

We observed the afterglow of GRB 130427A with the RATIR instrument on the 1.5-m Harold L. Johnson telescope of the Observatorio Astron\'omico Nacional on Sierra San Pedro M\'artir. Our homogenous $griZYJH$ photometry extends from the night of burst to three years later. We fit a model for the afterglow. There is a significant positive residual which matches the behavior of SN 1998bw in the $griZ$ filters; we suggest that this is a photometric signature of the supernova SN 2013cq associated with the GRB. The peak absolute magnitude of the supernova is $M_r=-18.43\pm0.11$., Comment: 23 pages, 10 figures. Accepted in ApJ

Published
2017

15. Challenging the Forward Shock Model with the 80 Ms Follow up of the X-ray Afterglow of Gamma-Ray Burst 130427A

Author

Neil Gehrels, D. Malesani, Bruce Gendre, Luigi Piro, Zach Cano, Bing Zhang, Massimiliano De Pasquale, Michel Boer, Samantha Oates, David Alexander Kann, Steve Schulze, G. Stratta, Eleonora Troja, Matthew Page, Andrea Rossi, ITA, USA, GBR, FRA, DEU, ESP, ISL, Raunvísindastofnun (HÍ), Science Institute (UI), Verkfræði- og náttúruvísindasvið (HÍ), School of Engineering and Natural Sciences (UI), Háskóli Íslands, and University of Iceland

Subjects
lcsh:Astronomy, Gammageislar, Astrophysics::High Energy Astrophysical Phenomena, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, lcsh:QB1-991, 0103 physical sciences, Gamma-ray bursts, X-ray afterglows, GRB modeling, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, X-ray, GRB 130427A, Astronomy, Röntgentækni, Astronomy and Astrophysics, Light curve, Redshift, Afterglow, Gamma-ray burst, Event (particle physics)
Abstract

GRB 130427A was the most luminous gamma-ray burst detected in the last 30 years. With an isotropic energy output of 8.5 x 10(53) erg and redshift of 0.34, it combined very high energetics with a relative proximity to Earth in an unprecedented way. Sensitive X-ray observatories such as XMM-Newton and Chandra have detected the afterglow of this event for a record-breaking baseline longer than 80 million seconds. The light curve displays a simple power-law over more than three decades in time. In this presentation, we explore the consequences of this result for a few models put forward so far to interpret GRB 130427A, and more in general the implication of this outcome in the context of the standard forward shock model., M.D.P. and M.J.P. thank the UK Space Agency for support. A.R. thanks support from PRIN-INAF 2012/13 and from Premiale LBT 2013. B.G. recognizes financial support of the NASA through the NASA Award NNX13AD28A and the NASA Award NNX15AP95A. Part of this work is under the auspice of the FIGARONet collaborative network, supported by the Agence Nationale de la Recherche, program ANR-14-CE33. D.A.K. acknowledges support by TLS Tautenburg, as a research stipend. D.M. thanks the support of Ida as well as financial support from Instrument Center for Danish Astrophysics (IDA). G.S. acknowledges the financial support, through grant FIRB 2012 RBFR12PM1F, provided by the Italian Ministry of Education, University and Research (MIUR). S.R.O. acknowledges the support provided by the Spanish Ministry, Project Number AYA2012-39727-C03-01, and acknowledges the support of the Leverhulme Trust. Z.C. gratefully acknowledges financial support provided by the Icelandic Research Fund (IRF). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, and by the Chandra Data Archive.

Published
2017
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16. NuSTAR Resolves the First Dual AGN above 10 keV in SWIFT J2028.5+2543

Author

Michael Koss, Poshak Gandhi, Craig B. Markwardt, Roberto J. Assef, Steven E. Boggs, Isabella Lamperti, Fiona A. Harrison, Ana Glidden, Daniel Stern, William W. Zhang, Dominic J. Walton, Charles J. Hailey, Mislav Baloković, Duncan Farrah, Neil Gehrels, Felix Fürst, Franz E. Bauer, Ezequiel Treister, William W. Craig, Claudio Ricci, David R. Ballantyne, and Alberto Masini

Subjects
Swift, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, law.invention, Telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), computer.programming_language, Physics, Luminous infrared galaxy, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Galaxy, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, computer
Abstract

We have discovered heavy obscuration in the dual active galactic nucleus (AGN) in the Swift/Burst Alert Telescope (BAT) source SWIFT J2028.5+2543 using Nuclear Spectroscopic Telescope Array (NuSTAR). While an early XMM-Newton study suggested the emission was mainly from NGC 6921, the superior spatial resolution of NuSTAR above 10 keV resolves the Swift/BAT emission into two sources associated with the nearby galaxies MCG +04-48-002 and NGC 6921 (z = 0.014) with a projected separation of 25.3 kpc (91"). NuSTAR's sensitivity above 10 keV finds both are heavily obscured to Compton-thick levels (N H=(1-2)x10^24 cm-2) and contribute equally to the BAT detection ({L}10-50 {keV}{int}= 6x10^42 erg s-1). The observed luminosity of both sources is severely diminished in the 2-10 keV band, illustrating the importance of >10 keV surveys like those with NuSTAR and Swift/BAT. Compared to archival X-ray data, MCG +04-48-002 shows significant variability (>3) between observations. Despite being bright X-ray AGNs, they are difficult to detect using optical emission-line diagnostics because MCG +04-48-002 is identified as a starburst/composite because of the high rates of star formation from a luminous infrared galaxy while NGC 6921 is only classified as a LINER using line detection limits. SWIFT J2028.5+2543 is the first dual AGN resolved above 10 keV and is the second most heavily obscured dual AGN discovered to date in the X-rays other than NGC 6240., Published in ApJ, 7 pages, 4 figures

Published
2017
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17. BAT AGN Spectroscopic Survey - V. X-ray properties of the Swift/BAT 70-month AGN catalog

Author

Poshak Gandhi, I. Del Vecchio, Michael Koss, Benny Trakhtenbrot, Simon Berney, Franz E. Bauer, Kyuseok Oh, Volker Beckmann, Daniel Asmus, Simona Soldi, Craig B. Markwardt, Stéphane Paltani, Neil Gehrels, Kevin Schawinski, Luis C. Ho, Mislav Baloković, Yoshihiro Ueda, Isabella Lamperti, Ezequiel Treister, Kohei Ichikawa, Claudio Ricci, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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)-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), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ), 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 ), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Swift, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Photon, galaxies: active, galaxies: Seyfert, quasars: general, X-rays: diffuse background, X-rays: general, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, active, X-rays: general [galaxies], 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, computer.programming_language, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Supermassive black hole, 010308 nuclear & particles physics, X-ray, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], computer, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Hard X-ray ($\geq 10$ keV) observations of Active Galactic Nuclei (AGN) can shed light on some of the most obscured episodes of accretion onto supermassive black holes. The 70-month Swift/BAT all-sky survey, which probes the 14-195 keV energy range, has currently detected 838 AGN. We report here on the broad-band X-ray (0.3-150 keV) characteristics of these AGN, obtained by combining XMM-Newton, Swift/XRT, ASCA, Chandra, and Suzaku observations in the soft X-ray band ($\leq 10$ keV) with 70-month averaged Swift/BAT data. The non-blazar AGN of our sample are almost equally divided into unobscured ($N_{\rm H}< 10^{22}\rm cm^{-2}$) and obscured ($N_{\rm H}\geq 10^{22}\rm cm^{-2}$) AGN, and their Swift/BAT continuum is systematically steeper than the 0.3-10 keV emission, which suggests that the presence of a high-energy cutoff is almost ubiquitous. We discuss the main X-ray spectral parameters obtained, such as the photon index, the reflection parameter, the energy of the cutoff, neutral and ionized absorbers, and the soft excess for both obscured and unobscured AGN., ApJS in press. The full tables will be available on ApJS and the on the BASS website [www.bass-survey.com] once the paper is published

Published
2017
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18. A very bright, very hot, and very long flaring event from the M Dwarf Binary system DG CVn

Author

Rudolf Novak, Hans A. Krimm, Enrique de Miguel, Neil Gehrels, J. A. Kennea, Stephen A. Drake, Rachel A. Osten, S. R. Oates, M. J. Page, Adam F. Kowalski, Tomáš Apeltauer, Kosmas Gazeas, and K. L. Page

Subjects
Swift Gamma-Ray Burst Mission, 010504 meteorology & atmospheric sciences, Stars: flare, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, coronae [Stars], 01 natural sciences, law.invention, Photometry (optics), Telescope, law, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, Stars: coronae, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar flare, Stars: individual (DG CVn), Bremsstrahlung, Astronomy and Astrophysics, flare [Stars], Particle acceleration, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, individual (DG CVn) [Stars], Astrophysics - High Energy Astrophysical Phenomena, Flare
Abstract

On April 23, 2014, the Swift satellite responded to a hard X-ray transient detected by its Burst Alert Telescope, which turned out to be a stellar flare from a nearby, young M dwarf binary DG~CVn. We utilize observations at X-ray, UV, optical, and radio wavelengths to infer the properties of two large flares. The X-ray spectrum of the primary outburst can be described over the 0.3-100 keV bandpass by either a single very high temperature plasma or a nonthermal thick-target bremsstrahlung model, and we rule out the nonthermal model based on energetic grounds. The temperatures were the highest seen spectroscopically in a stellar flare, at T$_{X}$ of 290 MK. The first event was followed by a comparably energetic event almost a day later. We constrain the photospheric area involved in each of the two flares to be $>$10$^{20}$ cm$^{2}$, and find evidence from flux ratios in the second event of contributions to the white light flare emission in addition to the usual hot, T$\sim$10$^{4}$K blackbody emission seen in the impulsive phase of flares. The radiated energy in X-rays and white light reveal these events to be the two most energetic X-ray flares observed from an M dwarf, with X-ray radiated energies in the 0.3-10 keV bandpass of 4$\times$10$^{35}$ and 9$\times$10$^{35}$ erg, and optical flare energies at E$_{V}$ of 2.8$\times$10$^{34}$ and 5.2$\times$10$^{34}$ erg, respectively. The results presented here should be integrated into updated modelling of the astrophysical impact of large stellar flares on close-in exoplanetary atmospheres., 48 pages, 9 figures, accepted for publication in the Astrophysical Journal

Published
2016

19. Results of the deepest all-sky survey for continuous gravitational waves on LIGO S6 data running on the Einstein@Home volunteer distributed computing project

Author

L. Kleybolte, A. Perreca, Susan M. Scott, Y. Wang, Daniele Trifirò, Chad Hanna, J. Oberling, Jordan Camp, D. B. Kelley, Heinz-Bernd Eggenstein, M. C. Heintze, T. Hardwick, D. Steinmeyer, Fiodor Sorrentino, F. Carbognani, D. Moraru, Gianpietro Cagnoli, F. Nocera, C. Zhao, Rosa Poggiani, F. Travasso, E. O. Lebigot, Thibaut Jacqmin, M. Merzougui, C. I. Torrie, N. Straniero, Z. Patrick, D. R. Ingram, V. Malvezzi, M. Saleem, H. Fair, Andrea Taracchini, J. V. van Heijningen, Eric Thrane, C. Michel, Sarah Caudill, R. Quitzow-James, R. Day, F. Ohme, V. B. Adya, Christopher P. L. Berry, A. D. Silva, P. J. Sutton, V. Frey, T. B. Edo, Alex B. Nielsen, J. H. Romie, Maximiliano Isi, Lionel Martellini, Peter Fritschel, M. Masso-Reid, S. Qiu, Kazuhiro Agatsuma, Enrico Calloni, G. Traylor, Thomas Corbitt, L. Salconi, C. A. Costa, M. K. Gupta, A. Allocca, F. Vetrano, C. C. Arceneaux, J. M. Gonzalez Castro, B. D. Cheeseboro, Archisman Ghosh, G. Cerretani, A. F. Brooks, G. Gemme, M. Drago, Guenakh Mitselmakher, B. A. Boom, A. M. Sergeev, John A. Clark, Ben Farr, Christophe Collette, Ho-Gyu Lee, Debnandini Mukherjee, G. McIntyre, Leo Singer, G. M. Harry, K. Venkateswara, Yuri Levin, A. Conte, T. A. Callister, N. Kijbunchoo, Reinhard Prix, M. Haney, R. Douglas, F. J. Raab, N. Mukund, L. R. Cominsky, B. L. Pearlstone, V. Fafone, Namjun Kim, Michael E Zucker, S. E. Dwyer, David Keitel, H. S. Cho, Roman Schnabel, T. Isogai, S. Doravari, Carl-Johan Haster, L. Rolland, J. E. Brau, A. A. van Veggel, S. Farinon, A. Pele, Efim A. Khazanov, G. Ballardin, P. Raffai, J. Hanks, D. J. McManus, Kendall Ackley, R. K. Nayak, F. Magaña-Sandoval, A. Staley, S. Jawahar, Matthew Evans, Suvadeep Bose, M. Fays, R. Gouaty, N. Indik, Fabrizio Barone, M. Mohan, N. Man, F. Frasconi, Graham Woan, Robert L. Byer, R. Inta, S. Klimenko, C. Palomba, S. Privitera, M. S. Shahriar, L. Sammut, Lionel London, Peter Aufmuth, Jiayi Qin, A. Singer, Jong H. Chow, B. D. Lackey, A. Di Lieto, S. J. Chamberlin, M. Vasúth, H. J. Jang, K. Haughian, Jade Powell, V. Loriette, T. Huynh-Dinh, Z. Márka, C. M. Reed, R. Robie, Chunglee Kim, Francesco Salemi, T. Sadecki, S. Mirshekari, P. Geng, W. Z. Korth, Jonathan Cripe, V. Mangano, Innocenzo M. Pinto, M. Rakhmanov, Robert Stone, A. Di Virgilio, A. R. Williamson, Lei Zhang, F. Clara, A. Pasqualetti, D. Barta, V. Germain, Marek Szczepanczyk, C. Bradaschia, K. Siellez, J. S. Kissel, J. N. Marx, D. J. Vine, Xing-Jiang Zhu, P. Oppermann, Alberto Vecchio, N. Mazumder, S. Kaufer, S. Grunewald, S. J. Kapadia, Rainer Weiss, Sylvia J. Zhu, Steven Reyes, F. Ricci, László Á. Gergely, Kevin M. Ryan, R. W. P. Drever, M. Boer, J. B. Kanner, M. Korobko, D. Talukder, Sascha Husa, R. Flaminio, J.-P. Coulon, J. S. Areeda, B. J. J. Slagmolen, Meng Wang, D.B. DeBra, D. M. Macleod, Ik Siong Heng, W. W. Johnson, Stuart Reid, G. Valdes, A. Samajdar, S. D'Antonio, Robinjeet Singh, I. W. Harry, M. Yvert, T. D. Abbott, David H. Reitze, Yi-Ming Hu, L. Prokhorov, Y. Setyawati, C. Tomlinson, J. D. Lough, Soma Mukherjee, H. R. Paris, H. J. Bulten, G. D. Meadors, Will M. Farr, G. Greco, S. S. Eikenberry, Tobias Westphal, X. F. Wang, John Miller, T. Prestegard, J. Ming, Riccardo Bassiri, M. Montani, B. L. Swinkels, P. Thomas, P. Weßels, Nancy Aggarwal, Zahoor Ali Khan, David Blair, K. Nedkova, Marc Favata, A. Gennai, Rahul Kumar, Magnus Manske, H. Fehrmann, V. Dolique, A. Chiummo, Erik Katsavounidis, X. Guo, David Jones, R. De Rosa, E. Maros, Bernard F. Schutz, Roger Jones, C. Baune, Li Ju, D. Ugolini, V. J. Roma, M. C. Tringali, A. C. Green, William Yam, L. Wallace, L. Kuo, H. Yamamoto, A. Królak, I. Nardecchia, E. Capocasa, A. Schönbeck, B. Klein, Bala R. Iyer, Odylio D. Aguiar, M. Lormand, P. B. Graff, Fausto Acernese, P. Brockill, Carlos Cepeda, Robert J. McCarthy, A. Glaefke, A. L. Miller, H. S. Chen, T. Dal Canton, J. Warner, K. A. Thorne, A. Sheperd, Luca Gammaitoni, H. Rew, Linqing Wen, Piotr Jaranowski, Florent Robinet, Daniel A. Shaddock, Marco Cavaglia, R. Passaquieti, V. Re, D. D. Brown, Mi Zhang, C. Gray, G. H. Ogin, T. J. Shaffer, Vuk Mandic, László Gondán, J. Prasad, C. Rajan, Vladimir B. Braginsky, Benjamin William Allen, M. Mantovani, R. Frey, Duncan Meacher, Abhirup Ghosh, Karsten Danzmann, Z. Tornasi, Tania Regimbau, S. McCormick, V. Tiwari, S. Brunett, N. A. Gordon, M. Rizzo, Kipp Cannon, V. Predoi, I. W. Martin, M. Steinke, P. Astone, Larne Pekowsky, M. M. Hanke, E. A. Houston, David E. McClelland, G. Vedovato, D. B. Kozak, H. Vahlbruch, K. Riles, G. A. Prodi, R. DeSalvo, H. Middleton, Neil Gehrels, S. Mastrogiovanni, P. J. Veitch, N. van Bakel, Steven Bloemen, Hua Wang, I. Dave, C. V. Kalaghatgi, J. Hanson, M. Punturo, Leopoldo Milano, Slawomir Gras, Yann Bouffanais, O. V. Palashov, Sean T. McWilliams, A. K. Zadrożny, F. Piergiovanni, S. Koley, Chang-Hwan Lee, G. Kang, M. K. M. Bader, G. Wang, W. D. Vousden, A. Brillet, L. Matone, A. Pal-Singh, C. Vorvick, Jonathan R. Gair, V. Kondrashov, B. Shapiro, J. L. Willis, Howard Pan, Arunava Mukherjee, M. Fletcher, B. Hughey, M. Neri, M. van Beuzekom, J. A. Giaime, Matthew Abernathy, M. Weinert, F. Fidecaro, G. M. Guidi, D. Pascucci, L. M. Perri, H. A. G. Gabbard, Kasem Mossavi, S. B. Anderson, Y. M. Kim, Christopher M. Biwer, N. A. Lockerbie, Blake Moore, S. Frasca, Aaron Buikema, M. Factourovich, C. C. Wipf, E. J. King, P. Kumar, B. R. Hall, M. Davier, H. N. Isa, Y. Minenkov, A. Bisht, M. J. Cowart, M. Poe, L. Conti, Evan Ochsner, C. Affeldt, A. J. Weinstein, M. C. Araya, A. Masserot, K. Kawabe, C. Aulbert, R. Cavalieri, Denis Martynov, A. W. Heptonstall, Vivien Raymond, Marco Bazzan, Peter R. Saulson, S. Penn, C. Lazzaro, R. Mittleman, Haocun Yu, Patricia Schmidt, V. Brisson, Guido Mueller, Thomas Dent, L. Trozzo, R. Taylor, A. K. Srivastava, V. Boschi, H. Wittel, Vladimir Dergachev, Stephen Fairhurst, Carl Blair, James Whelan, Nelson Christensen, L. Cerboni Baiardi, S. Mitra, C. C. Yancey, A. Kutynia, L. Pinard, Y.-H. Zhang, M. Landry, A. Bohe, Ruslan Vaulin, Archana Pai, S. M. Aston, R. T. DeRosa, C. Buy, M. Oliver, L. Di Fiore, P. J. King, Michael W. Coughlin, I. Khan, M. Phelps, J. Betzwieser, F. Paoletti, E. G. Thomas, A. Basti, R. Abbott, P. Ruggi, G. L. Mansell, S. E. Gossan, Samaya Nissanke, W. G. Anderson, M. Barsuglia, E. Cesarini, Kieran Craig, Samuele Cortese, Federico Ferrini, G. Vajente, David B. Tanner, A. Mullavey, T. J. N. Nelson, Giacomo Ciani, D. C. Coyne, J. J. Hacker, V. Dattilo, Tejinder Kaur, Xiaohui Fan, Antoine Heidmann, A. Grant, P. G. Murray, S. G. Crowder, J. O'Dell, K. Izumi, M. Turconi, Richard O'Shaughnessy, B. Barr, Terry G. McRae, B. P. Abbott, E. K. Gustafson, Edwin J. Son, J. Worden, F. Jiménez-Forteza, B. K. Berger, Fabien Kéfélian, A. Rüdiger, J. Eichholz, A. Ain, N. M. Brown, J. H. Hough, Andreas Freise, Vincenzo Pierro, J. R. Palamos, J. Birch, B. Mours, Michael Thomas, D. Töyrä, Rana X. Adhikari, H. Overmier, Avneet Singh, Paul D. Lasky, David Murphy, Stefan Hild, Y. Ma, C. C. Buchanan, S. Ascenzi, S. Vass, Francesco Pannarale, Alessandro Bertolini, Douglas R. Cook, Michele Zanolin, D. Schuette, E. Coccia, C. Graef, B. A. Weaver, T. J. Massinger, T. Vo, J. G. Rollins, B. Machenschalk, R. Coyne, Joey Shapiro Key, A. Rocchi, P. Popolizio, Koji Arai, J. R. Sanders, Matthew Pitkin, L.-W. Wei, Roland Schilling, Fabrice Matichard, R. Birney, F. Donovan, Adam A. Libson, J. E. Broida, Sebastien Biscans, J. C. Driggers, Charlotte Bond, S. A. Usman, G. D. Hammond, E. J. Sanchez, W. Kells, Swetha Bhagwat, L. Jian, A. Effler, R. Kennedy, S. P. Tarabrin, D. Sellers, D. Huet, D. Passuello, S. H. Huttner, J. Schmidt, J. C. Barayoga, Laleh Sadeghian, M. Granata, Roy Williams, Mairi Sakellariadou, G. Pillant, S. B. Coughlin, M. Vardaro, J. Meidam, R. L. Savage, A. S. Bell, A. L. Lombardi, P. T. Baker, V. P. Mitrofanov, Minchuan Zhou, F. Cleva, Andrew Melatos, M. Lorenzini, P. A. Altin, B. C. Stephens, C. V. Torres, Hyun Lee, L. Naticchioni, Salvatore Vitale, M. Laxen, J. Calderón Bustillo, J. P. Zendri, Riccardo Sturani, Q. Chu, Tenglin Li, E. A. Quintero, K. S. Karvinen, Maria Ilaria Del Principe, A. L. Urban, W. Del Pozzo, P. F. Cohadon, I. Kowalska, H. Heitmann, J. McIver, F. Y. Khalili, M. Agathos, Shubhanshu Tiwari, D. Barker, Joshua Yablon, Marie-Anne Bizouard, Shiuh Chao, Gleb Romanov, H. Qi, A. Giazotto, P. Puppo, A. W. Muir, P. Shawhan, L. Magaña Zertuche, D. Hoak, D. Sentenac, Patrick Brady, M. Branchesi, I. Ferrante, Nergis Mavalvala, D. C. Vander-Hyde, P. Charlton, Jerome Degallaix, J. C. Batch, T. Theeg, Kejia Lee, O. J. Piccinni, T. P. Downes, P. Fulda, C. Casentini, Nicholas Smith, Qi Fang, Sebastian Khan, B. C. Barish, M. Was, Gavin Davies, Zifan Zhou, I. A. Bilenko, David J. Ottaway, A. Paoli, C. Krueger, R. M. Magee, M. Ast, O. E. S. Sauter, Vicky Kalogera, M. Tonelli, Larry R. Price, J. Woehler, M. Prijatelj, H. Vocca, E. A. Huerta, Eugeniy E. Mikhailov, M. S. Kehl, M. Pedraza, Tristan Briant, M. Leonardi, R. Goetz, A. Mytidis, C. Bogan, Tarun Souradeep, S. E. Zuraw, S. Chung, B. Sandeen, M. C. Edwards, S. J. Kimbrell, G. Bogaert, S. E. Barclay, Chi Woong Kim, K. Gill, B. Sassolas, L. Sun, C. Messenger, M. Chan, Andrew Lundgren, Walter Winkler, A. S. Markosyan, W. S. Kim, Harald Lück, F. Garufi, L. E. Wade, D. Verkindt, D. Bersanetti, M. Cho, G. Gaur, S. C. McGuire, J. F. Read, S. Di Pace, Samuel Deléglise, Eric Howell, A. M. Sintes, S. Leavey, Tyson Littenberg, T. D. Creighton, C. Pankow, P. M. Meyers, Chandra Kant Mishra, R. Bhandare, Badri Krishnan, D. Fiorucci, A. R. Wade, G. Kuehn, C. M. Mow-Lowry, Sergey P. Vyatchanin, I. Maksimovic, L. K. Nuttall, Ettore Majorana, M. Gosselin, D. V. Voss, R. L. Ward, G. Hemming, E. E. Cowan, N. Leroy, B. F. Whiting, J. Casanueva Diaz, P. Schale, M. Pichot, C. Van Den Broeck, Paul J. Groot, M. Zevin, Maria Alessandra Papa, L. Zangrando, F. Cavalier, W. Engels, S. M. Koehlenbeck, John Veitch, G. Billingsley, N. S. Darman, N. Arnaud, Maggie Tse, B. B. Miller, M. MacInnis, P. Rapagnani, P. Ehrens, F. Mezzani, M. Kasprzack, J. B. Lewis, S. R. Morriss, B. Lantz, William Parker, G. Debreczeni, Chia-Liang Cheng, S. Márka, R. M. S. Schofield, E. Schreiber, Benjamin J. Owen, J. F. J. van den Brand, S. Sunil, M. Tacca, Martin Hendry, M. Bitossi, G. Bergmann, K. Wette, M. C. Díaz, K. V. Tokmakov, Antonios Kontos, Junwei Cao, John J. Oh, Timothy Evans, Kenneth A. Strain, Jimin George, Rory Smith, C. Adams, R. M. Blair, D. Sigg, S. W. Ballmer, D. M. Shoemaker, M. Sieniawska, Gregory Ashton, Michelle E. Walker, G. Moreno, Fabio Marchesoni, P. Hello, J. L. Wright, Alessandra Corsi, M. H. Wimmer, H. Radkins, A. Bozzi, A. L. Stuver, D. Rosińska, J. E. Lord, Kyungmin Kim, M. Brinkmann, David Coward, Sheon Chua, R. Bonnand, K. G. Arun, E. J. Daw, I. Di Palma, Z. Frei, V. Sequino, S. Caride, B. O'Reilly, Collin D. Capano, R. Gustafson, M. P. Thirugnanasambandam, G. 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M., Kimbrell, S. .j., King, E. .j., King, P. .j., Kissel, J. .s., Klein, B., Kleybolte, L., Klimenko, S., Koehlenbeck, S. .m., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. .z., Kowalska, I., Kozak, D. .b., Kringel, V., Krishnan, B., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kumar, R., Kuo, L., Kutynia, A., Lackey, B. .d., Landry, M., Lange, J., Lantz, B., Lasky, P. .d., Laxen, M., 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., Lewis, J. .b., Li, T. .g. .f., Libson, A., Littenberg, T. .b., Lockerbie, N. .a., Lombardi, A. .l., London, L. .t., Lord, J. .e., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. .d., Lück, H., Lundgren, A. .p., Lynch, R., Ma, Y., Machenschalk, B., Macinnis, M., Macleod, D. .m., Magaña Sandoval, F., Magaña Zertuche, L., Magee, R. .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, FILIPPO, Martellini, L., Martin, I. .w., 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., Mccarthy, R., Mcclelland, D. .e., Mccormick, S., Mcguire, S. .c., Mcintyre, G., Mciver, J., Mcmanus, D. .j., Mcrae, T., Mcwilliams, S. .t., Meacher, D., Meadors, G. .d., Meidam, J., Melatos, A., Mendell, G., 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, L., Miller, A. .l., Miller, A., Miller, B. .b., 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., 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Subjects
Einstein@Home, Nuclear and High Energy Physics, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], gr-qc, media_common.quotation_subject, Distributed computing, Astronomy, FOS: Physical sciences, S6, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], 0103 physical sciences, Range (statistics), Sensitivity (control systems), LIGO, 010306 general physics, Hardware_REGISTER-TRANSFER-LEVELIMPLEMENTATION, Instrumentation and Methods for Astrophysics (astro-ph.IM), STFC, QC, media_common, QB, Physics, Gravitational Waves, 010308 nuclear & particles physics, Gravitational wave, Physique, RCUK, Einstein@Home, LIGO, S6, Gravitational Waves, Neutron star, Amplitude, Physics and Astronomy, Sky, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Instrumentation and Methods for Astrophysics, astro-ph.IM
Abstract

We report results of a deep all-sky search for periodic gravitational waves from isolated neutron stars in data from the S6 LIGO science run. The search was possible thanks to the computing power provided by the volunteers of the Einstein@Home distributed computing project. We find no significant signal candidate and set the most stringent upper limits to date on the amplitude of gravitational wave signals from the target population. At the frequency of best strain sensitivity, between 170.5 and 171 Hz we set a 90% confidence upper limit of 5.5×10^{-25}, while at the high end of our frequency range, around 505 Hz, we achieve upper limits ≃10^{-24}. At 230 Hz we can exclude sources with ellipticities greater than 10^{-6} within 100 pc of Earth with fiducial value of the principal moment of inertia of 10^{38} kg m^{2}. If we assume a higher (lower) gravitational wave spin-down we constrain farther (closer) objects to higher (lower) ellipticities., National Science Foundation (U.S.), United States. National Aeronautics and Space Administration, Carnegie Trust, Leverhulme Trust, David & Lucile Packard Foundation, Research Corporation, Alfred P. Sloan Foundation

Published
2016
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20. BAT AGN Spectroscopic Survey-III. An observed link between AGN Eddington ratio and narrow emission line ratios

Author

Kevin Schawinski, Isabella Lamperti, Benny Trakhtenbrot, Sylvain Veilleux, N. Masetti, Neil Gehrels, D. Michael Crenshaw, Claudio Ricci, Kurt T. Soto, Daniel Stern, Fiona A. Harrison, Yoshihiro Ueda, Richard F. Mushotzky, Ezequiel Treister, Michael Koss, Simon Berney, Kyuseok Oh, ITA, and USA

Subjects
Active galactic nucleus, Stellar mass, active [Galaxies], Metallicity, Doubly ionized oxygen, FOS: Physical sciences, Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, active, Galaxies: nuclei, Quasars: general [Black hole physics, Galaxies], 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Quasar, general [Quasars], Galaxies: active, Black hole physics, Astrophysics - Astrophysics of Galaxies, Galaxy, Quasars: general, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), nuclei [Galaxies], Light emission
Abstract

We investigate the observed relationship between black hole mass (MBH), bolometric luminosity (Lbol) and Eddington ratio (λEdd) with optical emission-line ratios ([N II] λ6583/Hα, [S II] λλ6716, 6731/Hα, [O I] λ6300/Hα, [O III] λ5007/Hβ, [Ne III] λ3869/Hβ and He II λ4686/Hβ) of hard X-ray-selected active galactic nuclei (AGN) from the BAT AGN Spectroscopic Survey. We show that the [N II] λ6583/Hα ratio exhibits a significant correlation with λEdd (RPear = −0.44, p-value = 3 × 10−13, σ = 0.28 dex), and the correlation is not solely driven by MBH or Lbol. The observed correlation between [N II] λ6583/Hα ratio and MBH is stronger than the correlation with Lbol, but both are weaker than the λEdd correlation. This implies that the large-scale narrow lines of AGN host galaxies carry information about the accretion state of the AGN central engine. We propose that [N II] λ6583/Hα is a useful indicator of Eddington ratio with 0.6 dex of rms scatter, and that it can be used to measure λEdd and thus MBH from the measured Lbol, even for high-redshift obscured AGN. We briefly discuss possible physical mechanisms behind this correlation, such as the mass–metallicity relation, X-ray heating, and radiatively driven outflows., Monthly Notices of the Royal Astronomical Society, 464 (2), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711

Published
2016

21. GRB 080503: IMPLICATIONS OF A NAKED SHORT GAMMA-RAY BURST DOMINATED BY EXTENDED EMISSION

Author

Jason X. Prochaska, Neil Gehrels, Enrico Ramirez-Ruiz, Karl Glazebrook, Andrew J. Levan, Jonathan Granot, Alexei V. Filippenko, Nial R. Tanvir, Weidong Li, Sebastian Lopez, Andrew Bunker, Brian D. Metzger, Anthony L. Piro, Nathaniel R. Butler, Kevin Hurley, Josh Bloom, Daniel Kocevski, Adam A. Miller, Jay P. Norris, Takanori Sakamoto, Daniel A. Perley, Dovi Poznanski, Eliot Quataert, Hsiao-Wen Chen, and Patrick B. Hall

Subjects
Physics, Brightness, Spectral index, 010308 nuclear & particles physics, Conjunction (astronomy), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Luminosity, Afterglow, Space and Planetary Science, 0103 physical sciences, Gamma-ray burst, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, Active star, QB
Abstract

We report on observations of GRB 080503, a short gamma-ray burst with very bright extended emission (about 30 times the gamma-ray fluence of the initial spike) in conjunction with a thorough comparison to other short Swift events. In spite of the prompt-emission brightness, however, the optical counterpart is extraordinarily faint, never exceeding 25 mag in deep observations starting at ~1 hr after the BAT trigger. The optical brightness peaks at ~1 day and then falls sharply in a manner similar to the predictions of Li & Paczynski (1998) for supernova-like emission following compact-binary mergers. However, a shallow spectral index and similar evolution in X-rays inferred from Chandra observations are more consistent with an afterglow interpretation. The extreme faintness of this probable afterglow relative to the bright gamma-ray emission argues for a very low-density medium surrounding the burst (a "naked" GRB), consistent with the lack of a coincident host galaxy down to 28.5 mag in deep HST imaging. Our observations reinforce the notion that short GRBs generally occur outside regions of active star formation, but demonstrate that in some cases the luminosity of the extended prompt emission can greatly exceed that of the short spike, which may constrain theoretical interpretation of this class of events. Because most previous BAT short bursts without observed extended emission are too faint for this signature to have been detectable even if it were present at typical level, conclusions based solely on the observed presence or absence of extended emission in the existing Swift sample are premature. (abridged), 16 pages, 11 figures; accepted for publication in ApJ

Published
2016
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22. Early radio and X-ray observations of the youngest nearby Type Ia supernova PTF11kly (SN2011fe)

Author

Chryssa Kouveliotou, Michael M. Shara, Peter Nugent, Robert M. Quimby, S. Bradley Cenko, Kate Maguire, Atish Kamble, A. G. de Bruyn, D. Andrew Howell, John M. Carpenter, Mansi M. Kasliwal, Philipp Podsiadlowski, Dovi Poznanski, Assaf Horesh, Eran O. Ofek, S. R. Kulkarni, Neil Gehrels, Alexander J. van der Horst, Derek B. Fox, Ralph A. M. J. Wijers, Mark Sullivan, Nicholas M. Law, Avishay Gal-Yam, High Energy Astrophys. & Astropart. Phys (API, FNWI), and Astronomy

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Red giant, SYMBIOTIC-STAR PROGENITOR, radio continuum: general, FOS: Physical sciences, Context (language use), Astrophysics, X-rays: general, 01 natural sciences, BINARIES, supernovae: general, RS-OPHIUCHI, CHANNEL, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), SWIFT, EXPLOSION, 010308 nuclear & particles physics, Astronomy and Astrophysics, NOVAE, EVOLUTION, Stars, Supernova, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, WHITE-DWARF MODELS, Millimeter, Astrophysics - High Energy Astrophysical Phenomena, EMISSION, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

On August 24 (UT) the Palomar Transient Factory (PTF) discovered PTF11kly (SN 2011fe), the youngest and most nearby type Ia supernova (SN Ia) in decades. We followed this event up in the radio (centimeter and millimeter bands) and X-ray bands, starting about a day after the estimated explosion time. We present our analysis of the radio and X-ray observations, yielding the tightest constraints yet placed on the pre-explosion mass-loss rate from the progenitor system of this supernova. We find a robust limit of dM/dt, 24 pages, 2 figures, ApJ accepted, X-ray data table and missing references added

Published
2016
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23. PTF 10fqs: A LUMINOUS RED NOVA IN THE SPIRAL GALAXY MESSIER 99

Author

Dale A. Frail, Io K. W. Kleiser, Avishay Gal-Yam, Shriharsh P. Tendulkar, S. Bradley Cenko, Gustavo Rahmer, Eran O. Ofek, Khanh Bui, J. A. Kennea, Neil Gehrels, John Henning, Janet Jacobsen, Robert M. Quimby, Roger Smith, Dovi Poznanski, D. McKenna, Mansi M. Kasliwal, James D. Neill, Dan L. Starr, Cullen H. Blake, Richard Walters, David Hale, O. Yaron, Karl Forster, Weidong Li, Joshua S. Bloom, Richard Dekany, Peter Nugent, Yoav Green, Lars Bildsten, Alexei V. Filippenko, Jeff Zolkower, J. L. Howell, Nicholas M. Law, D. B. Fox, Adam Miller, Iair Arcavi, George Helou, Christopher Martin, Shri Kulkarni, Mark Sullivan, and Viswa Velur

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Spiral galaxy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Galaxy, Luminosity, Supernova, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Bulge, 0103 physical sciences, Luminous red nova, Variable star, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Palomar Transient Factory (PTF) is systematically charting the optical transient and variable sky. A primary science driver of PTF is building a complete inventory of transients in the local Universe (distance less than 200 Mpc). Here, we report the discovery of PTF10fqs, a transient in the luminosity "gap" between novae and supernovae. Located on a spiral arm of Messier 99, PTF 10fqs has a peak luminosity of Mr = -12.3, red color (g-r = 1.0) and is slowly evolving (decayed by 1 mag in 68 days). It has a spectrum dominated by intermediate-width H (930 km/s) and narrow calcium emission lines. The explosion signature (the light curve and spectra) is overall similar to thatof M85OT2006-1, SN2008S, and NGC300OT. The origin of these events is shrouded in mystery and controversy (and in some cases, in dust). PTF10fqs shows some evidence of a broad feature (around 8600A) that may suggest very large velocities (10,000 km/s) in this explosion. Ongoing surveys can be expected to find a few such events per year. Sensitive spectroscopy, infrared monitoring and statistics (e.g. disk versus bulge) will eventually make it possible for astronomers to unravel the nature of these mysterious explosions., 12 pages, 12 figures, Replaced with published version

Published
2016
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24. Real-Time Detection and Rapid Multiwavelength Follow-up Observations of a Highly Subluminous Type II-P Supernova from the Palomar Transient Factory Survey

Author

Emma S. Walker, D. Bersier, Peter Nugent, Mark Sullivan, D. Andrew Howell, C. Akerlof, Mansi M. Kasliwal, S. Bradley Cenko, Kate Maguire, Yoav Green, Phil A. James, Joshua S. Bloom, Assaf Sternberg, Wei Li, D. B. Fox, Dovi Poznanski, Avishay Gal-Yam, Nicholas M. Law, Sagi Ben-Ami, Dale A. Frail, Alexei V. Filippenko, J. M. Silverman, Fang Yuan, Paolo A. Mazzali, Shrinivas R. Kulkarni, Richard Walters, Robert M. Quimby, O. Yaron, Eran O. Ofek, Neil Gehrels, Iair Arcavi, and Dong Xu

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Field of view, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Luminosity, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Schmidt camera, Supernova, 13. Climate action, Space and Planetary Science, Sky, Factory (object-oriented programming), Transient (oscillation), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Palomar Transient Factory (PTF) is an optical wide-field variability survey carried out using a camera with a 7.8 square degree field of view mounted on the 48-in Oschin Schmidt telescope at Palomar Observatory. One of the key goals of this survey is to conduct high-cadence monitoring of the sky in order to detect optical transient sources shortly after they occur. Here, we describe the real-time capabilities of the PTF and our related rapid multiwavelength follow-up programs, extending from the radio to the gamma-ray bands. We present as a case study observations of the optical transient PTF10vdl (SN 2010id), revealed to be a very young core-collapse (Type II-P) supernova having a remarkably low luminosity. Our results demonstrate that the PTF now provides for optical transients the real-time discovery and rapid-response follow-up capabilities previously reserved only for high-energy transients like gamma-ray bursts., Comment: ApJ, in press; all spectroscopic data available from the Weizmann Institute of Science Experimental Astrophysics Spectroscopy System (WISEASS; http://www.weizmann.ac.il/astrophysics/wiseass/)

Published
2016
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25. DDOTI: the deca-degree optical transient imager

Author

Michel Boer, Eleonora Troja, Alexander Kutyrev, José A. de Diego, Carlos Román-Zúñiga, Nathaniel R. Butler, Pierre Thierry, Jaime Ruíz-Diáz-Soto, Alan M. Watson, F. Quirós, Alain Klotz, William H. Lee, Neil Gehrels, Stéphane Basa, M. Reyes-Ruiz, Pierre-Eric Blanc, Yilen Gómez Maqueo Chew, Silvio J. Tinoco, Liliana Figueroa, Fernando Ángeles, and Alejandro Farah

Subjects
Physics, Equatorial mount, FOS: Physical sciences, Astronomy, Field of view, Gamma-ray astronomy, 01 natural sciences, law.invention, Telescope, law, Limiting magnitude, 0103 physical sciences, Hot Jupiter, Satellite, Astrophysics - Instrumentation and Methods for Astrophysics, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract

DDOTI will be a wide-field robotic imager consisting of six 28-cm telescopes with prime focus CCDs mounted on a common equatorial mount. Each telescope will have a field of view of 12 square degrees, will have 2 arcsec pixels, and will reach a 10-sigma limiting magnitude in 60 seconds of r = 18.7 in dark time and r = 18.0 in bright time. The set of six will provide an instantaneous field of view of about 72 square degrees. DDOTI uses commercial components almost entirely. The first DDOTI will be installed at the Observatorio Astron\'omico Nacional in Sierra San Pedro Mart\'ir, Baja California, M\'exico in early 2017. The main science goals of DDOTI are the localization of the optical transients associated with GRBs detected by the GBM instrument on the Fermi satellite and with gravitational-wave transients. DDOTI will also be used for studies of AGN and YSO variability and to determine the occurrence of hot Jupiters. The principal advantage of DDOTI compared to other similar projects is cost: a single DDOTI installation costs only about US$500,000. This makes it possible to contemplate a global network of DDOTI installations. Such geographic diversity would give earlier access and a higher localization rate. We are actively exploring this option., Comment: To appear in the proceedings of SPIE conference 9910 "Observatory Operations: Strategies, Processes, and Systems VI". 12 pages

Published
2016
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26. Search of the Orion spur for continuous gravitational waves using a loosely coherent algorithm on data from LIGO interferometers

Author

M. Turconi, D. Huet, R. Chakraborty, F. Cleva, Andrew Melatos, D. S. Rabeling, A. Di Lieto, M. Di Giovanni, R. M. Martin, S. E. Hollitt, Mark Hannam, H. P. Daveloza, Rocco Romano, Huiyuan Wang, D. L. Kinzel, R. L. McCarthy, A. J. Weinstein, J. B. Camp, L. Sun, Vuk Mandic, A. S. Bell, V. Boschi, R. J. G. Jonker, Craig A. Bond, Alex B. Nielsen, A. Moggi, C. Krueger, G. Kuehn, L. Cunningham, Carrie Reinhardt Adams, M. Neri, B. R. Hall, A. Pasqualetti, T. J. Massinger, J. Ming, R. Bhandare, R. M. S. Schofield, Lu Zhang, Rana X. Adhikari, A. Sergeev, J. E. Brau, D. Buskulic, K. Williams, Archana Pai, W. D. Vousden, A. Heptonstall, F. J. Raab, P. Shawhan, Michael Pürrer, F. Donovan, P. Couvares, Benno Willke, J. Clark, T. Vo, Eric K. Gustafson, Y. M. Kim, V. Sequino, A. Di Virgilio, C. C. Buchanan, Riccardo Sturani, Yuri Levin, Achamveedu Gopakumar, Sourav Ghosh, X. Siemens, J. Warner, L. Pinard, M. Jacobson, P. Ehrens, N. Straniero, B. Mours, D. B. Kozak, D. Passuello, Y. Minenkov, M. Barsuglia, Oleg Palashov, G. Mendell, Lynn Kuo, P. T. Baker, M. De Laurentis, A. Lazzarini, O. J. Piccinni, G. Islas, M. Manske, R. Flaminio, Andrzej Królak, J.-P. Coulon, J. Hennig, Michael I. Andersen, S. S. Eikenberry, S. A. Pai, Andrea Taracchini, B. Moe, Odylio D. Aguiar, László Gondán, B. Behnke, L. Naticchioni, Salvatore Vitale, A. L. Urban, S. M. Aston, Richard O'Shaughnessy, B. Barr, Malik Rakhmanov, R. Taylor, A. Corsi, J. Worden, Patricia Schmidt, V. Brisson, D. Meacher, L. Williams, A. Rüdiger, S. E. Strigin, S. Walsh, W. Z. Korth, Alessandra Buonanno, H. Yamamoto, G. Kang, C. C. Yancey, M. A. Papa, J. Zweizig, Joseph Gleason, V. Fafone, K. Siellez, M. Pedraza, T. P. Bodiya, E. Cesarini, R. S. Ottens, G. Pillant, C. Michel, G. Newton, H. Lück, Christopher P. L. Berry, A. D. Silva, H. Dereli, N. Mangini, M. Bejger, F. Marion, Kendall Ackley, R. K. Nayak, B. Lantz, Sarah Caudill, Sergey Klimenko, M. Was, R. Robie, M. M. Hanke, R. Quitzow-James, R. Day, Z. Patrick, Sebastian Steinlechner, Swetha Bhagwat, Gianluca Gemme, Bernard F. Whiting, C. Messenger, Tobias Westphal, V. Quetschke, G. M. Guidi, W. Kells, J. Bergman, YingLiang Ma, S. P. Tarabrin, V. B. Adya, Rosemary Frey, A. Colla, A. Grant, Jonathan F. Stebbins, V. V. Frolov, A. Idrisy, N. Kim, M. Razzano, M. Born, S. McCormick, Laura Cadonati, J. Hanks, Richard J. Abbott, Andreas Freise, M. H. Wimmer, A. L. Stuver, E. J. Daw, M. Punturo, S. Gras, H. Vocca, Eugeniy E. Mikhailov, V. Necula, N. Letendre, V. Branco, V. Malvezzi, Ben Farr, W. Katzman, L. van der Schaaf, Cody Messick, Alberto Gatto, Marco Cavaglia, Chris Pankow, A. Chiummo, Y. Pan, I. Yakushin, Xing-Jiang Zhu, B. J. J. Slagmolen, Hee-Suk Cho, J. O'Dell, M. Damjanic, K. Riles, L. Matone, Ryan DeRosa, C. Cepeda, Paul D. Lasky, Christophe Collette, N. Van Bakel, P. Brockill, N. Leroy, Josh Logue, K. E. Gushwa, J. H. Romie, Jesper Munch, M. Drago, J. Meidam, Timothy MacDonald, G. Wang, C. Aulbert, A. Perreca, T. Sadecki, Huang-Wei Pan, Gijs Nelemans, F. Nocera, E. D. Hall, Paolo Addesso, Jolien D. E. Creighton, S. H. Oh, Susan M. Scott, Teviet Creighton, K. Mason, S. Caride, J. A. Giaime, M. Merzougui, F. Garufi, M. Boer, C. Palomba, M. Cho, Matthew Pitkin, Chia-Liang Cheng, J. Gonzalez, Luca Gammaitoni, S. P. Vyatchanin, J. B. Kanner, V. Germain, Moritz Mehmet, Vivien Raymond, M. Mageswaran, Chad Hanna, Jiayi Qin, S. G. Crowder, Gregory E. Vansuch, Marek Szczepanczyk, Riccardo Bassiri, N. A. Strauss, R. Passaquieti, W. W. Johnson, Madeline Wade, Peter R. Saulson, Erik Katsavounidis, L. Cerboni Baiardi, J. Prasad, M. Meinders, A. K. Srivastava, Ik Siong Heng, T. Souradeep, Matthew Evans, E. Cuoco, S. Steplewski, M. Zanolin, Maria Okounkova, T. Isogai, E. J. King, T. B. Edo, Xin Chen, G. McIntyre, S. Karki, D. Sentenac, Ellen S. Howell, J. G. Rollins, Richard J. Oram, E. J. Sanchez, M. V. Van Der Sluys, Zsolt Frei, F. Clara, R. Gustafson, V. Kringel, D. Rosińska, D. Amariutei, A. Brillet, T. Huynh-Dinh, Archisman Ghosh, Christopher M. Biwer, S. Frasca, M. C. Tringali, A. Singer, I. Nardecchia, Leo Singer, Sammanani S. Premachandra, P. Leaci, J. N. Marx, D. Nolting, László Á. Gergely, E. O. Lebigot, M. Granata, K. D. Giardina, J. R. Leong, D. Bersanetti, M. P. Thirugnanasambandam, M. C. Díaz, M. Tacca, E. Ochsner, S. Grunewald, Carl-Johan Haster, L. G. Prokhorov, Mingliang Zhou, S. Mirshekari, S. E. Gossan, V. Sandberg, F. Paoletti, Patrice Hello, Alicia M. Sintes, Benjamin William Allen, L. Rolland, Stephen Fairhurst, Carl Blair, Shiuh Chao, N. Indik, Innocenzo M. Pinto, J. Eichholz, Keiko Kokeyama, Fabrizio Barone, M. Mohan, K. Holt, Máté Nagy, Piotr Jaranowski, F. Y. Khalili, D. Sellers, Tania Regimbau, H. K. Lee, K. Nedkova, Vladimir B. Braginsky, H. Vahlbruch, D. Brown, T. Adams, Geraint Davies, Linqing Wen, Karsten Danzmann, A. Mytidis, I. Di Palma, Neil Gehrels, Maik Frede, M. Colombini, C. Affeldt, I. Santiago-Prieto, Surabhi Sachdev, B. R. Iyer, D. Moraru, M. Factourovich, C. Gray, A. Libson, Leopoldo Milano, J. Calderón Bustillo, J. J. Hacker, M. S. Shahriar, P. Ruggi, A. Viceré, D. Simakov, Yi Chen, I. Dave, W. Ortega, H. Middleton, Pierre-François Cohadon, B. C. Barish, F. Fidecaro, K. A. Thorne, N. Mazumder, V. Dattilo, Tejinder Kaur, J. Betzwieser, D. Ugolini, Z. Márka, Stefan Hild, Robinjeet Singh, T. D. Abbott, C. Celerier, V. Re, Ruslan Vaulin, David B. Tanner, F. Travasso, F. Jiménez-Forteza, James G. Bartlett, N. Man, S. Dhurandhar, David Coward, Badri Krishnan, P. Astone, Larne Pekowsky, R. DeSalvo, C. Vorvick, S. Reid, T. Z. Summerscales, F. Magana-Sandoval, Sheon Chua, C. J. Guido, R. Bonnand, P. G. Murray, Denis Martynov, H. J. Jang, P. Charlton, C. M. Reed, E. Coccia, A. Kutynia, Lionel Martellini, L.-W. Wei, Peter Fritschel, S. Privitera, D. J. White, E. Schreiber, C. M. Mow-Lowry, K. Haughian, J. Poeld, S. B. Coughlin, Gregory Harry, J. L. Willis, E. J. Son, H. J. Bulten, Kasem Mossavi, B. M. Levine, Margaret Millhouse, Roman Schnabel, F. Cavalier, A. R. Wade, M. Phelps, G. Romanov, A. Sevigny, S. Chung, Matthew Heintze, Stanislav Babak, William Yam, X. Guo, L. Rei, P. J. King, Federico Ferrini, T. B. Littenberg, G. Vajente, M. Lubinski, G. Traylor, L. Di Fiore, M. Heurs, Richard L. Savage, Y. Ji, T. Hardwick, E. A. Houston, Bruce Gendre, T. Etzel, J. J. Oh, J. R. Sanders, G. Moreno, F. Piergiovanni, J. Yablon, G. Mazzolo, T. Dent, M. van Beuzekom, N. A. Robertson, C. Lazzaro, M. Saleem, Chi-Woong Kim, G. Dojcinoski, Jonathan Cripe, J. Casanueva Diaz, T. t. Fricke, Rainer Weiss, F. Ricci, Nándor Kelecsényi, H.-B. Eggenstein, B. C. Stephens, Nicholas Smith, T. Prestegard, Qi Fang, G. Debreczeni, S. Kandhasamy, Kip S. Thorne, V. Lockett, A. Giazotto, M. Tápai, I. Ferrante, C. Mishra, Irene Fiori, K. Venkateswara, G. A. Prodi, C. C. Arceneaux, Remington P. S. Stone, E. A. Quintero, S. G. Gaonkar, T. Chalermsongsak, Alessandro Bertolini, K. Grover, J. C. Driggers, Aaron Buikema, R. Douglas, V. Loriette, Francesco Salemi, Thomas Corbitt, Satya Mohapatra, Joey Shapiro Key, Haixing Miao, J. Lee, O. Bock, A. Zadrożny, Michael Thomas, Subhasish Mitra, Efim A. Khazanov, G. Ballardin, Jessica McIver, C. V. Torres, Q. Chu, A. Ain, István Rácz, K. L. Dooley, Sabrina D'Antonio, J. R. Palamos, E. Dominguez, Enrico Calloni, David Jonathan Hofman, D. Hammer, M. Vallisneri, H. M. Lee, F. Carbognani, Michael E Zucker, P. Bojtos, David Blair, R. P. Fisher, Fan Zhang, Collin D. Capano, A. R. Williamson, R. Birney, Jessica Steinlechner, M. K. Gupta, M. Wang, G. Mitselmakher, V. Dolique, B. D. Lackey, P. Hopkins, S. C. McGuire, S. H. Huttner, Koji Arai, B. L. Swinkels, J. Luo, Kevin M. Ryan, F. Vetrano, Matthew R. Abernathy, Zeyaur R. Khan, C. Baune, A. Mullavey, Lisa Barsotti, B. P. Abbott, V. P. Mitrofanov, D. Barker, A. Schönbeck, J-Y. Vinet, M. C. Araya, John K. Scott, B. Sassolas, W. Del Pozzo, Trevor Sidery, H. Heitmann, M. Leonardi, C. Graef, Kipp Cannon, M. Steinke, J. Karlen, S. Vass, J. S. Kissel, Ashok Kumar, M. Korobko, S. T. Countryman, E. Thrane, D. M. Macleod, P. J. Sutton, M. Branchesi, R. Schilling, M. Ducrot, Vincenzo Pierro, Tristan Briant, V. Predoi, I. W. Martin, Daniel R. Brown, T. Dal Canton, R. Everett, G. Billingsley, F. Mezzani, Prayush Kumar, C. L. Mueller, S. Franco, David E. McClelland, M. Huynh, Alexander H. Nitz, Jeffery Kline, Xuan Wang, J. C. Batch, K. A. Hodge, Fabrice Matichard, D. Feldbaum, M. E. N. Normandin, M. Fays, B. Sorazu, S. Márka, B. C. Pant, A. Rocchi, R. Goetz, Roger Jones, A. L. Lombardi, S. Farinon, E. Oelker, A. Pal-Singh, D. D. Brown, M. Fyffe, I. Bartos, M. Constancio, Roy Williams, R. Essick, P. Puppo, Kenneth A. Strain, E. Macdonald, Chunnong Zhao, P. Aufmuth, R. Inta, David H. Shoemaker, F. Frasconi, R. Coyne, J. Hoelscher-Obermaier, A. Masserot, I. A. Bilenko, V. Dergachev, Gregory Ashton, Fabio Marchesoni, Sean T. McWilliams, S. Penn, David J. Ottaway, Chang-Hwan Lee, E. A. Huerta, Kyungmin Kim, D. DeBra, Peter Shaffery, John Miller, I. W. Harry, D. x. Madden-Fong, M. Prijatelj, M. Weinert, M. J. Cowart, R. Cavalieri, D. C. Coyne, David O. Cook, M. Davier, C. Buy, T. T. Nguyen, O. Puncken, L. E. Wade, M. T. Hartman, Samuel Deléglise, L. Wallace, M. Kasprzack, D. Hoak, S. Goßler, Shuiyao Huang, Andrea Chincarini, W. G. Anderson, P. M. Meyers, Michael L. Gorodetsky, Suresh Tiwari, Ryan Lynch, Paul J. Groot, I. Kowalska, G. Bogaert, L. Zangrando, A. C. Lin, G. Serna, Simon Stevenson, M. Vardaro, H. Overmier, S. B. Anderson, P. Oppermann, R. Mittleman, Nelson Christensen, K. Craig, J. V. Van Heijningen, Jan Harms, Hartmut Grote, T. P. Downes, D. Verkindt, H. Radkins, Paul Fulda, T. Denker, G. Losurdo, J. Cao, E. Genin, M. W. Coughlin, K. Haris, S. L. Danilishin, Ilya Mandel, J. K. Blackburn, Neil J. Cornish, Tomasz Bulik, W. Winkler, I. Maksimovic, R. L. Ward, B. Weaver, G. Hemming, M. Pichot, E. Maros, François Bondu, Marie-Anne Bizouard, B. Shapiro, Ettore Majorana, Viswanath Bavigadda, R. De Rosa, John R. Smith, A. Brooks, Fausto Acernese, S. Kaufer, E. Capocasa, J. B. Lewis, Nergis Mavalvala, Jerome Degallaix, M. Yvert, E. C. Ferreira, Z. Shao, Mi Zhang, M. Mantovani, D. Schuette, M. Bitossi, Evan Goetz, D. Steinmeyer, C. Casentini, K. Wette, M. Brinkmann, G. Cerretani, C. Bradaschia, Sebastien Biscans, D. I. Jones, J. Kerrigan, A. Gupta, F. Robinet, Rory Smith, S. Doravari, Vaibhav Tiwari, D. Sigg, A. Post, A. Cumming, B. Hughey, M. Lorenzini, Michelle E. Walker, Jong H. Chow, J. Macarthur, M. Tse, S. M. Koehlenbeck, F. Baldaccini, J. Birch, D. Lodhia, G. Bergmann, Timothy A Welborn, G. H. Ogin, M. J. Hart, C. S. Unnikrishnan, Grant David Meadors, M. Lormand, S. Raja, E. Chassande-Mottin, P. Thomas, Sheila Rowan, S. E. Dwyer, L. Sammut, Giancarlo Cella, Steven Bloemen, C. A. Costa, Jonathan R. Gair, H. A. G. Gabbard, N. A. Lockerbie, Blake Moore, Jedidah C. Isler, A. Basti, A. Conte, B. O'Reilly, N. Kijbunchoo, Reinhard Prix, M. Haney, James Whelan, C. Van den Broeck, J.-D. Fournier, J. Aasi, Jade Powell, V. Mangano, P. Schale, M. Shaltev, P. Ajith, David H. Reitze, Yi-Ming Hu, D. B. Kelley, Sweta Shah, V. J. Roma, Nam Gyu Kim, T. Evans, T. Theeg, Zhihui Du, G. Ciani, A. A. van Veggel, Nicolas Brown, Graham Woan, Robert L. Byer, C. Belczynski, M. A. Barton, D. Talukder, H. Fehrmann, G. Greco, Sascha Husa, V. Kondrashov, Yanxi Zhang, G. Valdes, Arunava Mukherjee, Kazuhiro Agatsuma, R. M. Magee, Holger Wittel, Mauro Tonelli, Gianpietro Cagnoli, J. Hanson, J. P. Zendri, Rosa Poggiani, Frank Ohme, Vicky Kalogera, Larry R. Price, G. González, M. S. Kehl, N. A. Gordon, P. J. Veitch, Bernard F. Schutz, M. M. Fejer, Li Ju, S. E. Zuraw, Daniel A. Shaddock, A. Pele, A. Allocca, P. Raffai, D. R. Ingram, G. L. Mansell, A. S. Markosyan, Andrew Lundgren, Antoine Heidmann, B. Machenschalk, David Keitel, Calum Torrie, M. Pickenpack, R. Bork, Guido Mueller, M. Gosselin, Fumiko Kawazoe, Patrick Brady, J. S. Areeda, C. Tomlinson, J. D. Lough, Soma Mukherjee, Suvadeep Bose, R. Gouaty, David Murphy, H. R. Paris, A. s. Rodger, A. Effler, S. Meshkov, S. W. Ballmer, Mátyás Vasúth, M. Edwards, M. Favata, Francesco Pannarale, R. A. Mercer, B. K. Berger, Fabien Kéfélian, J. H. Hough, G. Vedovato, D. Trifirò, S. J. Chamberlin, A. Staley, Maria Ilaria Del Principe, K. Kawabe, M. Agathos, S. R. Morriss, Alberto Vecchio, F. Martelli, Will M. Farr, S. Jawahar, M. Montani, P. Weßels, Nancy Aggarwal, L. Conti, S. Koley, R. W. P. Drever, C. Padilla, P. B. Graff, Benjamin J. Owen, J. F. J. van den Brand, A. Sawadsky, S. A. Usman, G. D. Hammond, Martin Hendry, A. Gennai, Keisuke Izumi, Christopher Wipf, K. V. Tokmakov, L. Sadeghian, S. E. Barclay, Tjonnie G. F. Li, Michael Landry, S. Leavey, John Veitch, L. K. Nuttall, J. C. Barayoga, N. S. Darman, N. Arnaud, David Hosken, M. MacInnis, P. 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Calderón, Calloni, E., Camp, J. .b., Cannon, K. .c., Cao, J., Capano, C. .d., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Celerier, C., Cella, G., Cepeda, C., CERBONI BAIARDI, LORENZO, Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. .j., Chao, S., Charlton, P., Chassande Mottin, E., Chen, X., 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., Colombini, M., Constancio, M., Conte, A., Conti, L., Cook, D., Corbitt, T. .r., Cornish, N., Corsi, A., 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., Creighton, T., Cripe, J., Crowder, S. .g., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Damjanic, M. .d., 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, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., De Rosa, R., Derosa, R. .t., Desalvo, R., Dhurandhar, S., Díaz, M. .c., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Dominguez, E., 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., Edwards, M., Effler, A., Eggenstein, H. 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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., Hoelscher Obermaier, J., Hofman, D., Hollitt, S. .e., Holt, K., 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, M., Huynh Dinh, T., Idrisy, A., Indik, N., Ingram, D. .r., Inta, R., Islas, G., Isler, J. .c., Isogai, T., Iyer, B. .r., Izumi, K., Jacobson, M. .b., Jang, H., Jaranowski, P., Jawahar, S., Ji, Y., Jiménez Forteza, F., Johnson, W. .w., Jones, D. .i., Jones, R., Jonker, R. .j. .g., Ju, L., Haris, K., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. .b., Karki, S., Karlen, J. .l., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. .s., Keitel, D., Kelecsenyi, N., Kelley, D. .b., Kells, W., Kerrigan, J., Key, J. .s., Khalili, F. .y., Khan, Z., Khazanov, E. .a., Kijbunchoo, N., Kim, C., Kim, K., Kim, N. .g., Kim, N., Kim, Y. M., King, E. .j., King, P. .j., Kinzel, D. .l., Kissel, J. .s., Klimenko, S., Kline, J. .t., Koehlenbeck, S. .m., Kokeyama, K., Koley, S., Kondrashov, V., Korobko, M., Korth, W. .z., Kowalska, I., Kozak, D. .b., Kringel, V., Krishnan, B., Królak, A., Krueger, C., Kuehn, G., Kumar, A., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. .d., Landry, M., 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, J., Lee, J. .p., Leonardi, M., Leong, J. .r., Leroy, N., Letendre, N., Levin, Y., Levine, B. .m., Lewis, J. .b., Li, T. .g. .f., Libson, A., Lin, A. .c., Littenberg, T. .b., Lockerbie, N. .a., Lockett, V., Lodhia, D., Logue, J., Lombardi, A. .l., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. .d., Lubinski, M. .j., Lück, H., Lundgren, A. .p., Luo, J., Lynch, R., Ma, Y., Macarthur, J., Macdonald, E. .p., Macdonald, T., Machenschalk, B., Macinnis, M., Macleod, D. .m., Madden Fong, D. .x., Magaña Sandoval, F., Magee, R. .m., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mangini, N. .m., Mansell, G. .l., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. .s., Maros, E., MARTELLI, FILIPPO, Martellini, L., Martin, I. .w., Martin, R. .m., Martynov, D. .v., Marx, J. .n., Mason, K., Masserot, A., Massinger, T. .j., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. .e., Mccormick, S., Mcguire, S. .c., Mcintyre, G., Mciver, J., Mcwilliams, S. .t., Meacher, D., Meadors, G. .d., Mehmet, M., Meidam, J., Meinders, M., Melatos, A., Mendell, G., Mercer, R. .a., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. .m., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. .e., Milano, L., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. .p., Mitselmakher, G., 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D., Amariutei, D. V., Anderson, S. B., Anderson, W. G., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Aston, S. M., Baker, P. T., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barton, M. A., Batch, J. C., Bell, A. S., Berger, B. K., Berry, C. P. L., Bilenko, I. A., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Bodiya, T. P., Brady, P. R., Braginsky, V. B., Branchesi, M., 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, Enrico, Camp, J. B., Cannon, K. C., Capano, C. D., Baiardi, L. Cerboni, Chamberlin, S. J., 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., Damjanic, M. D., Danilishin, S. L., D'Antonio, S., Darman, N. S., Daveloza, H. P., Davies, G. S., Daw, E. J., DE LAURENTIS, Martina, DE ROSA, Rosario, Derosa, R. T., Díaz, M. C., Dooley, K. L., Downes, T. P., Drever, R. W. P., Driggers, J. C., Dwyer, S. E., Edo, T. B., Edwards, M. C., Eichholz, J. M., 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, Fabio, Gergely, L. Á., Giaime, J. A., Giardina, K. D., Gleason, J. R., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Graff, P. B., Greco, G., Guidi, G. M., Guido, C. J., 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, J., 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., Hosken, D. J., Houston, E. A., Howell, E. J., Hu, Y. M., Huerta, E. A., Huttner, S. H., Ingram, D. R., Isler, J. C., Iyer, B. R., Jacobson, M. B., Johnson, W. W., Jones, D. I., Jonker, R. J. G., Kanner, J. B., Karlen, J. 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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., Ortega, W. E., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Owen, B. J., Padilla, C. T., Pai, S. A., Palamos, J. R., Pant, B. C., Papa, M. A., Paris, H. R., Piergiovanni, F., Pinto, I. M., Poeld, J. H., 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., Rodger, A. S., Rollins, J. G., Roma, V. J., Romie, J. H., Sanders, J. R., Saulson, P. R., Schofield, R. M. S., Schutz, B. F., Scott, S. M., Shaddock, D. A., Shahriar, M. S., Shoemaker, D. H., Sidery, T. L., 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., Stevenson, S. P., Strain, K. A., Strauss, N. A., Stuver, A. L., Summerscales, T. Z., Sutton, P. J., Swinkels, B. L., Szczepanczyk, M. J., Tanner, D. B., Tarabrin, S. P., Thirugnanasambandam, M. P., Thorne, K. A., Thorne, K. S., 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., Van Den Broeck, C., Van Der Schaaf, L., Van Der Sluys, M. V., Van Heijningen, J., Van Veggel, A. A., Veitch, P. J., Vetrano, F., Viceré, A., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Ward, R. L., Weinstein, A. J., Whelan, J. T., White, D. J., Whiting, B. F., Williams, K. J., Williams, R. D., Williamson, A. R., Willis, J. L., Wimmer, M. H., Wipf, C. C., Yancey, C. C., Zhu, X. J., Zucker, M. E., and Zuraw, S. E.

Subjects
Nuclear and High Energy Physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, gr-qc, Gravitational Wave, FOS: Physical sciences, Periodic Signals, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Pulsar, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, ddc:530, 010306 general physics, QC, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational Waves, astro-ph.HE, Physics, 010308 nuclear & particles physics, Gravitational wave, Settore FIS/01 - Fisica Sperimentale, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Polarization (waves), 530 Physik, Galaxy, LIGO, Milky Way, Neutron star, Stars, Amplitude, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, pulsars, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, Astrophysics - High Energy Astrophysical Phenomena, Periodic Signal, CW detection, Gravitational Waves, Periodic Signals, Milky Way
Abstract

We report results of a wideband search for periodic gravitational waves from isolated neutron stars within the Orion spur towards both the inner and outer regions of our Galaxy. As gravitational waves interact very weakly with matter, the search is unimpeded by dust and concentrations of stars. One search disk (A) is $6.87^\circ$ in diameter and centered on $20^\textrm{h}10^\textrm{m}54.71^\textrm{s}+33^\circ33'25.29"$, and the other (B) is $7.45^\circ$ in diameter and centered on $8^\textrm{h}35^\textrm{m}20.61^\textrm{s}-46^\circ49'25.151"$. We explored the frequency range of 50-1500 Hz and frequency derivative from $0$ to $-5\times 10^{-9}$ Hz/s. A multi-stage, loosely coherent search program allowed probing more deeply than before in these two regions, while increasing coherence length with every stage. Rigorous followup parameters have winnowed initial coincidence set to only 70 candidates, to be examined manually. None of those 70 candidates proved to be consistent with an isolated gravitational wave emitter, and 95% confidence level upper limits were placed on continuous-wave strain amplitudes. Near $169$ Hz we achieve our lowest 95% CL upper limit on worst-case linearly polarized strain amplitude $h_0$ of $6.3\times 10^{-25}$, while at the high end of our frequency range we achieve a worst-case upper limit of $3.4\times 10^{-24}$ for all polarizations and sky locations., Fixed minor typo - duplicate name in the author list

Published
2016
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28. Perspectives on Gamma-Ray Burst Physics and Cosmology with Next Generation Facilities

Author

Chen Zhang, Jianchao Sun, Jian-Yan Wei, Lorenzo Amati, Diego Götz, Yulei Qiu, Neil Gehrels, Bertrand Cordier, Nicolas Produit, Giancarlo Ghirlanda, Weimin Yuan, Nial R. Tanvir, John K. Cannizzo, and CHN

Subjects
Swift, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, 010309 optics, 0103 physical sciences, Ground segment, 010303 astronomy & astrophysics, Reionization, Instrumentation and Methods for Astrophysics (astro-ph.IM), computer.programming_language, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Galaxy, Redshift, Space and Planetary Science, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, computer
Abstract

High-redshift Gamma-Ray Bursts (GRBs) beyond redshift $\sim6$ are potentially powerful tools to probe the distant early Universe. Their detections in large numbers and at truly high redshifts call for the next generation of high-energy wide-field instruments with unprecedented sensitivity at least one order of magnitude higher than the ones currently in orbit. On the other hand, follow-up observations of the afterglows of high-redshift GRBs and identification of their host galaxies, which would be difficult for the currently operating telescopes, require new, extremely large facilities of at multi-wavelengths. This chapter describes future experiments that are expected to advance this exciting field, both being currently built and being proposed. The legacy of Swift will be continued by SVOM, which is equipped with a set of space-based multi-wavelength instruments as well as and a ground segment including a wide angle camera and two follow-up telescopes. The established Lobster-eye X-ray focusing optics provides a promising technology for the detection of faint GRBs at very large distances, based on which the {THESEUS}, {Einstein Probe} and other mission concepts have been proposed. Follow-up observations and exploration of the reionization era will be enabled by large facilities such as {SKA} in the radio, the 30m class telescopes in the optical/near-IR, and the space-borne {WFIRST} and {JWST} in the optical/near-IR/mid-IR. In addition, the X-ray and $\gamma$-ray polarization experiment POLAR is also introduced., Comment: accepted for publication in Space Science Review; reprinted as a chapter in a book of the Space Sciences Series of ISSI for the proceedings of the ISSI-Beijing workshop " Gamma-Ray Bursts: a Tool to Explore the Young Universe"

Published
2016
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29. Supplement: 'Going the Distance: Mapping Host Galaxies of LIGO and Virgo Sources in Three Dimensions Using Local Cosmography and Targeted Follow-up' (2016, ApJL, 829, L15)

Author

S. Bradley Cenko, Will M. Farr, Hsin-Yu Chen, Salvatore Vitale, A. L. Urban, P. B. Graff, Christopher P. L. Berry, Samaya Nissanke, Ilya Mandel, Ben Farr, Mansi M. Kasliwal, Neil Gehrels, John K. Cannizzo, Vivien Raymond, Larry R. Price, Leo Singer, Satya Mohapatra, John Veitch, Daniel E. Holz, and Michael W. Coughlin

Subjects
Physics, Gravitational wave, HEALPix, media_common.quotation_subject, Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, LIGO, Redshift, Galaxy, Luminosity, Space and Planetary Science, Sky, 0103 physical sciences, 010306 general physics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, Luminosity distance, Astrophysics::Galaxy Astrophysics, media_common
Abstract

This is an online supplement to https://arxiv.org/abs/1603.07333 . In the main Letter, we demonstrated a rapid algorithm for obtaining joint three-dimensional estimates of sky location and luminosity distance from observations of binary neutron star mergers with Advanced LIGO and Virgo. We argued that combining the reconstructed volumes with positions and redshifts of possible host galaxies can provide large-aperture but small field of view instruments with a manageable list of targets to search for optical or infrared emission. In this Supplement, we document the new HEALPix-based file format for 3D localizations of gravitational wave transients. We include Python sample code to show the reader how to perform simple manipulations of the 3D sky maps and extract ranked lists of likely host galaxies. Finally, we include mathematical details of the rapid volume reconstruction algorithm.

Published
2016

30. ASASSN-15lh: A Superluminous Ultraviolet Rebrightening Observed by Swift and Hubble

Author

Melanie Kae Olaes, J. Craig Wheeler, Jeremy Mould, Peter Hoeflich, Lifan Wang, Dietrich Baade, Jeff Cooke, Yang Yang, Justyn R. Maund, Neil Gehrels, Robert M. Quimby, and Peter J. Brown

Subjects
Brightness, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Large Synoptic Survey Telescope, Astrophysics::Cosmology and Extragalactic Astrophysics, medicine.disease_cause, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, medicine, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Redshift, Supernova, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Ultraviolet
Abstract

We present and discuss ultraviolet and optical photometry from the Ultraviolet/Optical Telescope and X-ray limits from the X-Ray Telescope on Swift and imaging polarimetry and ultraviolet/optical spectroscopy with the Hubble Space Telescope of ASASSN-15lh. It has been classified as a hydrogen-poor superluminous supernova (SLSN I) more luminous than any other supernova observed. ASASSN-15lh is not detected in the X-rays in individual or coadded observations. From the polarimetry we determine that the explosion was only mildly asymmetric. We find the flux of ASASSN-15lh to increase strongly into the ultraviolet, with a ultraviolet luminosity a hundred times greater than the hydrogen-rich, ultraviolet-bright SLSN II SN 2008es. We find objects as bright as ASASSN-15lh are easily detectable beyond redshifts of ~4 with the single-visit depths planned for the Large Synoptic Survey Telescope. Deep near-infrared surveys could detect such objects past a redshift of ~20 enabling a probe of the earliest star formation. A late rebrightening -- most prominent at shorter wavelengths -- is seen about two months after the peak brightness, which is itself as bright as a superluminous supernova. The ultraviolet spectra during the rebrightening are dominated by the continuum without the broad absorption or emission lines seen in SLSNe or tidal disruption events and the early optical spectra of ASASSN-15lh. Our spectra show no strong hydrogen emission, showing only LyA absorption near the redshift previously found by optical absorption lines of the presumed host. The properties of ASASSN-15lh are extreme when compared to either SLSNe or tidal disruption events., Comment: submitted to AAS Journals 7 May 2016, accepted for publication in ApJ 16 June 2016, this version includes changes following the referee report and proof checking

Published
2016
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31. The Third Swift Burst Alert Telescope Gamma-Ray Burst Catalog

Author

Kevin Chen, A. Y. Lien, Scott Barthelmy, Jay Cummings, W. H. Baumgartner, T. N. Ukwatta, Nicholas R. Collins, Neil Gehrels, Hans A. Krimm, Michael Stamatikos, John K. Cannizzo, Eleonora Troja, Craig B. Markwardt, T. Sakamoto, and David Palmer

Subjects
Physics, Swift, High Energy Astrophysical Phenomena (astro-ph.HE), Data products, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, law.invention, Telescope, Event data, Space and Planetary Science, law, 0103 physical sciences, False detection, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, computer, computer.programming_language
Abstract

To date, the Burst Alert Telescope (BAT) onboard Swift has detected ~ 1000 gamma-ray bursts (GRBs), of which ~ 360 GRBs have redshift measurements, ranging from z = 0.03 to z = 9.38. We present the analyses of the BAT-detected GRBs for the past ~ 11 years up through GRB151027B. We report summaries of both the temporal and spectral analyses of the GRB characteristics using event data (i.e., data for each photon within approximately 250 s before and 950 s after the BAT trigger time), and discuss the instrumental sensitivity and selection effects of GRB detections. We also explore the GRB properties with redshift when possible. The result summaries and data products are available at http://swift.gsfc.nasa.gov/results/batgrbcat/index.html . In addition, we perform searches for GRB emissions before or after the event data using the BAT survey data. We estimate the false detection rate to be only one false detection in this sample. There are 15 ultra-long GRBs (~ 2% of the BAT GRBs) in this search with confirmed emission beyond ~ 1000 s of event data, and only two GRBs (GRB100316D and GRB101024A) with detections in the survey data prior to the starting of event data. (Some figures shown here are in lower resolution due to the size limit on arXiv. The full resolution version can be found at http://swift.gsfc.nasa.gov/results/batgrbcat/3rdBATcatalog.pdf ), Comment: 110 pages, 35 figures, accepted for publication on ApJS

Published
2016
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32. SDSS J102623.61+254259.5: the second most distant blazar atz = 5.3

Author

Tullia Sbarrato, Luigi Foschini, Neil Gehrels, Gianpiero Tagliaferri, Giancarlo Ghirlanda, Gabriele Ghisellini, Marco Nardini, Fabrizio Tavecchio, Arne Rau, and Jochen Greiner

Subjects
Physics, Solar mass, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Viewing angle, Redshift, Luminosity, Space and Planetary Science, Spectral energy distribution, Blazar, Astrophysics::Galaxy Astrophysics
Abstract

The radio-loud quasar SDSS J102623.61+254259.5, at a redshift z=5.3, is one of the most distant radio-loud objects. Since its radio flux exceeds 100 mJy at a few GHz, it is also one of the most powerful radio-loud sources. We propose that this source is a blazar, i.e. we are seeing its jet at a small viewing angle. This claim is based on the spectral energy distribution of this source, and especially on its strong and hard X-ray spectrum, as seen by Swift, very typical of powerful blazars. Observations by the Gamma-Ray Burst Optical/Near-Infrared Detector (GROND) and by theWide-field Infrared Survey Explorer (WISE) allow to establish the thermal nature of the emission in the near IR-optical band. Assuming that this is produced by a standard accretion disk, we derive that it emits a luminosity of L_d \simeq 9 \times 10^46 erg s^{-1} and that the black hole has a mass between 2 and 5 billion solar masses. This poses interesting constraints on the mass function of heavy (> 10^9 M_sun) black holes at high redshifts.

Published
2012
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33. Particle Acceleration in Relativistic Outflows

Author

Guy Pelletier, Neil Gehrels, Martin Pohl, Martin Lemoine, Andrei M. Bykov, and Henric Krawczynski

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Particle acceleration, Pulsar, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Current (fluid), Astrophysics - High Energy Astrophysical Phenomena, ddc:600, Astrophysics::Galaxy Astrophysics
Abstract

In this review we confront the current theoretical understanding of particle acceleration at relativistic outflows with recent observational results on various source classes thought to involve such outflows, e.g. gamma-ray bursts, active galactic nuclei, and pulsar wind nebulae. We highlight the possible contributions of these sources to ultra-high-energy cosmic rays., Accepted for publication in Space Science Reviews, will also appear as chapter of an ISSI publication

Published
2012
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34. Time-Domain Astronomy with <scp>Swift</scp>, <scp>Fermi</scp> and <scp>Lobster</scp>

Author

John K. Cannizzo, Neil Gehrels, and Scott Barthelmy

Subjects
Physics, Swift, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, law.invention, Tidal disruption event, Supernova, Crab Nebula, Space and Planetary Science, law, Symbiotic star, Astrophysics::Solar and Stellar Astrophysics, computer, Time domain astronomy, Flare, Fermi Gamma-ray Space Telescope, computer.programming_language
Abstract

The dynamic transient gamma-ray sky is revealing many interesting results, largely due to findings by Fermi and Swift. The list includes new twists on gamma-ray bursts (GRBs), a GeV flare from a symbiotic star, GeV flares from the Crab Nebula, high-energy emission from novae and supernovae, and, within the last year, a new type of object discovered by Swift—a jetted tidal disruption event. In this review we present highlights of these exciting discoveries. A new mission concept called Lobster is also described; it would monitor the X-ray sky at order-of-magnitude higher sensitivity than current missions can.

Published
2011
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35. X-ray flare candidates in short gamma-ray bursts

Author

Raffaella Margutti, Jonathan Granot, Neil Gehrels, Maria Grazia Bernardini, Edo Berger, M. Stamatikos, Alicia M. Soderberg, Guido Chincarini, C. Guidorzi, and E. Zaninoni

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Flux, Astronomy and Astrophysics, Astrophysics, Galaxy, law.invention, Afterglow, Luminosity, Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Gamma-ray burst, Isotropic energy, Flare
Abstract

We present the first systematic study of X-ray flare candidates in short gamma-ray bursts (SGRBs) exploiting the large 6-year Swift database with the aim to constrain the physical nature of such fluctuations. We find that flare candidates appear in different types of SGRB host galaxy environments and show no clear correlation with the X-ray afterglow lifetime; flare candidates are detected both in SGRBs with a bright extended emission in the soft gamma-rays and in SGRBs which do not show such component. We furthermore show that SGRB X-ray flare candidates only partially share the set of observational properties of long GRB (LGRB) flares. In particular,the main parameter driving the duration evolution of X-ray variability episodes in both classes is found to be the elapsed time from the explosion, with very limited dependence on the different progenitors, environments, central engine life-times, prompt variability time-scales and energy budgets. On the contrary, SGRB flare candidates significantly differ from LGRB flares in terms of peak luminosity, isotropic energy, flare-to-prompt luminosity ratio and relative variability flux. However, these differences disappear when the central engine time-scales and energy budget are accounted for, suggesting that (i) flare candidates and prompt pulses in SGRBs likely have a common origin; (ii) similar dissipation and/or emission mechanisms are responsible for the prompt and flare emission in long and short GRBs, with SGRBs being less energetic albeit faster evolving versions of the long class. Finally, we show that in strict analogy to the SGRB prompt emission, flares candidates fall off the lag-luminosity relation defined by LGRBs, thus strengthening the SGRB flare-prompt pulse connection.

Published
2011
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36. High-redshift Fermi blazars

Author

Giancarlo Ghirlanda, Gianpiero Tagliaferri, Neil Gehrels, Francesco Haardt, Marta Volonteri, Fabrizio Tavecchio, Gabriele Ghisellini, R. Della Ceca, and Luigi Foschini

Subjects
Physics, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Luminosity, Black hole, Space and Planetary Science, Spectral energy distribution, Blazar, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

With the release of the first year Fermi catalogue, the number of blazars detected above 100 MeV lying at high redshift has been largely increased. There are 28 blazars at z>2 in the "clean" sample. All of them are Flat Spectrum Radio Quasars (FSRQs). We study and model their overall spectral energy distribution in order to find the physical parameters of the jet emitting region, and for all of them we estimate their black hole masses and accretion rates. We then compare the jet with the accretion disk properties, setting these sources in the broader context of all the other bright gamma-ray or hard X-ray blazars. We confirm that the jet power correlates with the accretion luminosity. We find that the high energy emission peak shifts to smaller frequencies as the observed luminosity increases, according to the blazar sequence, making the hard X-ray band the most suitable for searching the most luminous and distant blazars.

Published
2010
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37. PRECURSORS OF SHORT GAMMA-RAY BURSTS

Author

Neil Gehrels, Eleonora Troja, and Stephan Rosswog

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Compact star, Physics::Geophysics, Space and Planetary Science, Quantum gravity, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Systematic search
Abstract

We carried out a systematic search of precursors on the sample of short GRBs observed by Swift. We found that ~8-10% of short GRBs display such early episode of emission. One burst (GRB 090510) shows two precursor events, the former ~13 s and the latter ~0.5 s before the GRB. We did not find any substantial difference between the precursor and the main GRB emission, and between short GRBs with and without precursors. We discuss possible mechanisms to reproduce the observed precursor emission within the scenario of compact object mergers. The implications of our results on quantum gravity constraints are also discussed., Comment: 8 pages, 2 figures, accepted for publication in The Astrophysical Journal

Published
2010
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38. RAPIDLY DECAYING SUPERNOVA 2010X: A CANDIDATE '.Ia' EXPLOSION

Author

Mansi M. Kasliwal, D. Andrew Howell, Dovi Poznanski, D. McKenna, Mark Sullivan, Viswa Velur, Robert M. Quimby, Nicholas M. Law, Joseph Brimacombe Mb ChB Frca, David Hale, Assaf Sternberg, Stefan Immler, Richard Walters, Robert A. Fesen, Joshua S. Bloom, Peter Nugent, Eran O. Ofek, Lars Bildsten, Richard Dekany, S. Bradley Cenko, Neil Gehrels, Gustavo Rahmer, Roger Smith, Avishay Gal-Yam, Iair Arcavi, Shrinivas R. Kulkarni, Paul F. Burke, Ken J. Shen, O. Yaron, Dan Milisavljevic, Eric Hsiao, K. Bui, Janet Jacobsen, Douglas J. Rich, Jeff Zolkower, and John Henning

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Thermonuclear fusion, Accretion (meteorology), Detonation, FOS: Physical sciences, chemistry.chemical_element, White dwarf, Astronomy and Astrophysics, Astrophysics, Light curve, Supernova, Astrophysics - Solar and Stellar Astrophysics, chemistry, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Ejecta, Solar and Stellar Astrophysics (astro-ph.SR), Helium
Abstract

We present the discovery, photometric and spectroscopic follow-up observations of SN 2010X (PTF 10bhp). This supernova decays exponentially with tau_d=5 days, and rivals the current recordholder in speed, SN 2002bj. SN 2010X peaks at M_r=-17mag and has mean velocities of 10,000 km/s. Our light curve modeling suggests a radioactivity powered event and an ejecta mass of 0.16 Msun. If powered by Nickel, we show that the Nickel mass must be very small (0.02 Msun) and that the supernova quickly becomes optically thin to gamma-rays. Our spectral modeling suggests that SN 2010X and SN 2002bj have similar chemical compositions and that one of Aluminum or Helium is present. If Aluminum is present, we speculate that this may be an accretion induced collapse of an O-Ne-Mg white dwarf. If Helium is present, all observables of SN 2010X are consistent with being a thermonuclear Helium shell detonation on a white dwarf, a ".Ia" explosion. With the 1-day dynamic-cadence experiment on the Palomar Transient Factory, we expect to annually discover a few such events., Comment: 6 pages, 5 figures; Minor Changes; Note correction in Fig 4 caption; published by ApJL

Published
2010
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39. The 2008 October Swift detection of X-ray bursts/outburst from the transient SGR-like AXP 1E 1547.0−5408

Author

G. L. Israel, Neil Gehrels, V. Mangano, P. Romano, Sergio Campana, Lorenzo Stella, Diego Götz, Simone Dall'Osso, Sandro Mereghetti, A. De Luca, Silvia Zane, F. Senziani, Lorella Angelini, David Palmer, Paolo Esposito, Roberto Turolla, Andrea Tiengo, Hans A. Krimm, Rosalba Perna, and Nanda Rea

Subjects
Physics, Swift, X-ray, Flux, Astronomy and Astrophysics, Astrophysics, Spectral line, law.invention, Telescope, Pulsar, Space and Planetary Science, law, Black-body radiation, Transient (oscillation), computer, computer.programming_language
Abstract

We report on the detailed study of the 2008 October outburst from the anomalous X-ray pulsar (AXP) 1E 1547.0-5408 discovered through the Swift/Burst Alert Telescope (BAT) detection of SGR-like short X-ray bursts on 2008 October 3. The Swift/X-ray Telescope (XRT) started observing the source after less than 100 s since the BAT trigger, when the flux (about 6E-11 erg/cm^2/s in the 2-10 keV range) was >50 times higher than its quiescent level. Swift monitored the outbursting activity of 1E 1547.0-5408 on a daily basis for approximately three weeks. This strategy allowed us to find a phase-coherent solution for the source pulsations after the burst, which, besides period and period derivative, requires a positive Period second derivative term (spin-down increase). The time evolution of the pulse shape is complex and variable, with the pulsed fraction increasing from 20% to 50% within the Swift observational window. The XRT spectra can be fitted well by means of a single component, either a power-law (PL) or a blackbody (BB). During the very initial phases of the outburst the spectrum is hard, with a PL photon index about 2 (or kT about 1.4 keV) which steepens to about 4 (or kT about 0.8 keV) within one day from the BAT trigger, though the two components are likely present simultaneously during the first day spectra. An INTEGRAL observation carried out five days after the trigger provided an upper limit of about 2E-11 erg/cm^2/s to the emission of 1E 1547.0-5408 in the 18-60 keV band.

Published
2010
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40. GAMMA-RAY BURSTS — OBSERVATIONS

Author

Neil Gehrels and J. K. Cannizzo

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gamma-ray astronomy, Astrophysics, Galaxy, Afterglow, Crab Nebula, Space and Planetary Science, Observatory, Light emission, Gamma-ray burst, Mathematical Physics, Fermi Gamma-ray Space Telescope
Abstract

We are in an exciting period of discovery for gamma-ray bursts. The Swift observatory is detecting 100 bursts per year, providing arcsecond localizations and sensitive observations of the prompt and afterglow emission. The Fermi observatory is observing 250 bursts per year with its medium-energy GRB instrument and about 10 bursts per year with its high-energy LAT instrument. In addition, rapid-response telescopes on the ground are providing new capabilities to study optical emission during the prompt phase and spectral signatures of the host galaxies. The combined data set is enabling great advances in our understanding of GRBs including afterglow physics, short burst origin, and high-energy emission.

Published
2010
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41. Fermi Large Area Telescope Observations of PSR J1836+5925

Author

C. Meurer, R. E. Hughes, E. Hays, S. Murgia, M. T. Wolff, F. Piron, G. M. Madejski, D. J. Thompson, Alice K. Harding, Jean Ballet, Hartmut Sadrozinski, Brian L Winer, K. Watters, Gudlaugur Johannesson, Omer Celik, M. Pierbattista, A. Tramacere, T. L. Usher, T. H. Burnett, Jürgen Knödlseder, A. A. Moiseev, Stefano Ciprini, Takaaki Tanaka, E. J. Siskind, Felix Ryde, Johann Cohen-Tanugi, Y. Edmonds, Nanda Rea, A. Y. Rodriguez, Matthew G. Baring, M. Ziegler, Guido Barbiellini, S. Germani, Stephen Fegan, Scott M. Ransom, R. Claus, W. N. Johnson, Paul S. Ray, M. S. Strickman, M. Frailis, L. S. Rochester, Elliott D. Bloom, P. D. Smith, T. Ylinen, D. Hadasch, Stefan Funk, D. Parent, C. C. Cheung, J. H. Panetta, M. Brigida, James Chiang, M.-H. Grondin, A. Reimer, Hiromitsu Takahashi, A. Chekhtman, F. Loparco, N. Vilchez, Dario Gasparrini, D. Horan, Roger Blandford, Markus Ackermann, R. Dubois, Ronaldo Bellazzini, A. Makeev, M. N. Mazziotta, W. B. Focke, W. B. Atwood, Gianluca Giavitto, W. Mitthumsiri, Julie McEnery, Neil Gehrels, Roger W. Romani, T. Reposeur, G. A. Caliandro, J. P. Norris, A. W. Borgland, A. A. Abdo, E. Orlando, L. Guillemot, Nicola Giglietto, P. Spinelli, M. E. Monzani, M. Razzano, M. Roth, A. De Luca, A. Morselli, Fernando Camilo, V. Vitale, Francesco Giordano, M. N. Lovellette, Tyrel J. Johnson, P. A. Caraveo, Nicola Omodei, Denis Bastieri, J. M. Casandjian, T. Kamae, Stephen E. Thorsett, Alessandro Brez, Persis S. Drell, R. A. Cameron, E. Do Couto E Silva, A. Van Etten, Igor V. Moskalenko, P. Fortin, P. Lubrano, P. L. Nolan, J. Lande, Sylvain Guiriec, J. Bregeon, Carmelo Sgrò, Riccardo Rando, Olaf Reimer, V. Vasileiou, K. S. Wood, Marianne Lemoine-Goumard, Seth Digel, F. Gargano, S. Carrigan, Luca Latronico, Luca Baldini, Martino Marelli, I. A. Grenier, E. Nuss, P. M. Saz Parkinson, J. G. Thayer, David Paneque, T. Ohsugi, Miranda Jackson, M. Kuss, C. Favuzzi, Jonathan F. Ormes, C. Monte, T. A. Porter, O. Tibolla, Gloria Spandre, Y. Kanai, V. Pelassa, D. Dumora, Jun Kataoka, Marco Ajello, J. B. Thayer, Keith Bechtol, L. Tibaldo, A. P. Waite, Eric Charles, Christo Venter, P. Wang, S. Buson, D. J. Suson, A. De Angelis, A. S. Johnson, Diego F. Torres, C. Gwon, Jeffrey D. Scargle, G. Tosti, Christian Farnier, M. Dormody, Emanuele Bonamente, N. Kawai, M. Pepe, Melissa Pesce-Rollins, P. Fusco, B. Berenji, Hideaki Katagiri, Andrea Belfiore, Matthew Kerr, Claudia Cecchi, Jan Conrad, Pascal Bruel, Peter F. Michelson, S. Rainò, Tsunefumi Mizuno, R. P. Johnson, J. E. Grove, Yasushi Fukazawa, Francesco Longo, A. Sander, David Stanley Smith, G. Godfrey, F. de Palma, T. Glanzman, Benoit Lott, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Fermi-LAT, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Abdo, A. A., Ackermann, M., Ajello, M., Atwood, B., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Bechtol, K., Belfiore, A., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Camilo, F., Caraveo, P. A., Carrigan, S., Casandjian, J. M., Cecchi, C., Celik, O., Charles, E., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Conrad, J., Angelis, A. d., Luca, A. d., Palma, F. d., Digel, S. W., Dormody, M., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Edmonds, Y., Farnier, C., Favuzzi, C., Fegan, S. J., Focke, W. B., Fortin, P., Frailis, M., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giavitto, G., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M. H., Grove, J. E., Guillemot, L., Guiriec, S., Gwon, C., Hadasch, D., Harding, A. K., Hays, E., Horan, D., Hughes, R. E., Jackson, M. S., Johannesson, G., Johnson, A. S., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Kanai, Y., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Knodlseder, J., Kuss, M., Lande, J., Latronico, L., Lemoine Goumard, M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Marelli, M., Mazziotta, M. N., Mcenery, J. E., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce Rollins, M., Pierbattista, M., Piron, F., Porter, T. A., Raino, S., Rando, R., Ransom, S. M., Ray, P. S., Razzano, M., Rea, N., Reimer, A., Reimer, O., Reposeur, T., Rochester, L. S., Rodriguez, A. Y., Romani, R. W., Roth, M., Ryde, F., Sadrozinski, H. F. W., Sander, A., Parkinson, P. M. S., Scargle, J. D., Sgro, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Strickman, M. S., Suson, D. J., Takahashi, H., Tanaka, T., Thayer, J. B., Thayer, J. G., Thompson, D. J., Thorsett, S. E., Tibaldo, L., Tibolla, O., Torres, D. F., Tosti, G., Tramacere, A., Usher, T. L., Etten, A. V., Vasileiou, V., Venter, C., Vilchez, N., Vitale, V., Waite, A. P., Wang, P., Watters, K., Winer, B. L., Wolff, M. T., Wood, K. S., Ylinen, T., Ziegler, M., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Population, Pulsar planet, FOS: Physical sciences, Fermi satellite, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar wind nebula, High Energy Gamma-ray Astronomy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Pulsar, Millisecond pulsar, pulsars: general, 0103 physical sciences, Gamma rays: general, Pulsars: general, pulsars: individual (PSR J1836+5925), 010306 general physics, education, 010303 astronomy & astrophysics, Pulsars, Astrophysics::Galaxy Astrophysics, gamma rays: general, pulsars: individual: PSR J1836+5925, Physics, education.field_of_study, Astronomy, Astronomy and Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Neutron star, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Fermi Gamma-ray Space Telescope
Abstract

The discovery of the gamma-ray pulsar PSR J1836+5925, powering the formerly unidentified EGRET source 3EG J1835+5918, was one of the early accomplishments of the Fermi Large Area Telescope (LAT). Sitting 25 degrees off the Galactic plane, PSR J1836+5925 is a 173 ms pulsar with a characteristic age of 1.8 million years, a spindown luminosity of 1.1$\times10^{34}$ erg s$^{-1}$, and a large off-peak emission component, making it quite unusual among the known gamma-ray pulsar population. We present an analysis of one year of LAT data, including an updated timing solution, detailed spectral results and a long-term light curve showing no indication of variability. No evidence for a surrounding pulsar wind nebula is seen and the spectral characteristics of the off-peak emission indicate it is likely magnetospheric. Analysis of recent XMM observations of the X-ray counterpart yields a detailed characterization of its spectrum, which, like Geminga, is consistent with that of a neutron star showing evidence for both magnetospheric and thermal emission., Accepted to Astrophysical Journal

Published
2010
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42. Discovery of a new soft gamma repeater: SGR J0418 + 5729

Author

Michael S. Briggs, Christopher R. Gelino, Ersin Gogus, E. P. Mazets, P. Oleynik, Scott Barthelmy, David Palmer, Dmitry S. Svinkin, S. V. Golenetskii, Valerie Connaughton, Colleen A. Wilson-Hodge, D. D. Frederiks, Dawn M. Gelino, Hans A. Krimm, Jay Cummings, Charles A. Meegan, Enrico Ramirez-Ruiz, Paul M. Woods, Mark H. Finger, A. J. van der Horst, Yuki Kaneko, Valentin Pal'shin, Anna L. Watts, Stefanie Wachter, M. van der Klis, Chryssa Kouveliotou, Jonathan Granot, Julie McEnery, Neil Gehrels, A. von Kienlin, Kevin Hurley, M. Ulanov, Asaf Pe'er, R. L. Aptekar, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Swift Gamma-Ray Burst Mission, Astrophysics::High Energy Astrophysical Phenomena, Population, Soft gamma repeater, Perseus Arm, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetar, Galaxy, Spitzer Space Telescope, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, education, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

On 2009 June 5, the Gamma-ray Burst Monitor (GBM) onboard the Fermi Gamma-ray Space Telescope triggered on two short, and relatively dim bursts with spectral properties similar to Soft Gamma Repeater (SGR) bursts. Independent localizations of the bursts by triangulation with the Konus-RF and with the Swift satellite, confirmed their origin from the same, previously unknown, source. The subsequent discovery of X-ray pulsations with the Rossi X-ray Timing Explorer (RXTE), confirmed the magnetar nature of the new source, SGR J0418+5729. We describe here the Fermi/GBM observations, the discovery and the localization of this new SGR, and our infrared and Chandra X-ray observations. We also present a detailed temporal and spectral study of the two GBM bursts. SGR J0418+5729 is the second source discovered in the same region of the sky in the last year, the other one being SGR J0501+4516. Both sources lie in the direction of the galactic anti-center and presumably at the nearby distance of ~2 kpc (assuming they reside in the Perseus arm of our galaxy). The near-threshold GBM detection of bursts from SGR J0418+5729 suggests that there may be more such dim SGRs throughout our galaxy, possibly exceeding the population of bright SGRs. Finally, using sample statistics, we conclude that the implications of the new SGR discovery on the number of observable active magnetars in our galaxy at any given time is, 6 pages, 3 figures, 2 tables; accepted for publication in ApJL on 2010 January 8

Published
2010

43. DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OFz= 6.7 GRB 080913,z= 8.2 GRB 090423, AND SOME SHORT/HARD GRBs

Author

En-Wei Liang, Xue-Feng Wu, Neil Gehrels, D. Alexander Kann, Daniel Proga, Kenji Toma, Bing Zhang, Peter Mészáros, Francisco J. Virgili, Hou-Jun Lv, Peter W. A. Roming, Bin-Bin Zhang, and David N. Burrows

Subjects
Physics, education.field_of_study, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Population, GRB 090423, Astronomy and Astrophysics, Observational study, Astrophysics, education, Gamma-ray burst
Abstract

(Abridged) The two high-redshift gamma-ray bursts, GRB 080913 at z=6.7 and GRB 090423 at z=8.3, recently detected by Swift appear as intrinsically short, hard GRBs. They could have been recognized by BATSE as short/hard GRBs should they have occurred at z

Published
2009
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44. ULTRAVIOLET SPECTROSCOPY OF SUPERNOVAE: THE FIRST TWO YEARS OFSWIFTOBSERVATIONS

Author

Filomena Bufano, Massimo Turatto, Stefan Immler, Luca Zampieri, Paolo A. Mazzali, P. W. A. Roming, Neil Gehrels, Stefano Benetti, Peter J. Brown, Stephen T. Holland, Enrico Cappellaro, A. A. Breeveld, Nino Panagia, Wayne B. Landsman, Elena Pian, and Peter A. Milne

Subjects
Swift, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Swift Gamma-Ray Burst Mission, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, medicine.disease_cause, Spectral line, Grism, Supernova, Ultraviolet visible spectroscopy, Space and Planetary Science, medicine, Ejecta, computer, Ultraviolet, Astrophysics - Cosmology and Nongalactic Astrophysics, computer.programming_language
Abstract

We present the entire sample of ultraviolet (UV) spectra of supernovae (SNe) obtained with the Ultraviolet/Optical Telescope (UVOT) on board the Swift satellite during the first 2 years of observations (2005/2006). A total of 29 UV-grism and 22 V-grism spectra of 9 supernovae (SNe) have been collected, of which 6 are thermonuclear (type Ia) and 3 core collapse (type Ibc/II) SNe. All the spectra have been obtained during the photospheric phase. After a comparison of the spectra of our sample with those in the literature (SNe 1992A, 1990N and 1999em), we confirm some degree of diversity in the UV emission of Type Ia SNe and a greater homogeneity in the Type II Plateau SN sample. Signatures of interaction between the ejecta and the circumstellar environment have been found in the UV spectrum of SN 2006jc, the only SN Type Ib/c for which UVOT grism data are available. Currently, Swift UVOT is the best suited instrument for early SN studies in the UV due to its fast response and flexible scheduling capabilities. However, in order to increase the quality of the data and significantly improve our understanding of the UV properties of SNe and to fully maximize the scientific potential of UVOT grism observations, a larger investment in observing time and longer exposures are needed., Comment: 64 pages, 18 figures, accepted to ApJ

Published
2009
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45. Suzaku-WAM, Konus-Wind, and Swift-BAT Observations of Prompt Emission of the High-Redshift GRB 050904

Author

Valentin Pal'shin, T. Sakamoto, Michael Stamatikos, Hans A. Krimm, S. V. Golenetskii, J. R. Cummings, Yujin E. Nakagawa, A. M. Parsons, Yuji Urata, Kazutaka Yamaoka, Neil Gehrels, Masanori Ohno, Makoto Tashiro, Satoshi Sugita, and Scott Barthelmy

Subjects
Physics, Swift, Range (particle radiation), Astronomy, Astronomy and Astrophysics, Astrophysics, Redshift, Luminosity, Wavelength, Space and Planetary Science, Spectral analysis, Gamma-ray burst, computer, computer.programming_language
Abstract

We present the results of the high-redshift GRB 050904 at z = 6.295 from joint spectral analysis among Swift- BAT, Konus-Wind, and Suzaku-WAM, covering a wide energy range of 15-5000 keV. TheFspectrum peak energy, Epeak, was measured at 314 +173 � 89 keV, corresponding to 2291 +1263 � 634 keV in the source frame, and the isotropic equivalent radiated energy, Eiso, was estimated to be 1.04 +0:25 � 0:17 � 10 54 erg. Both are among the highest values that have ever been measured. GRBs with such a high Eiso (� 10 54 erg) might be associated with prompt optical emis- sion. The derived spectral and energetic parameters are consistent with the correlation between the rest-frame Ep;i and the Eiso (Amati relation), but not with the correlation between the intrinsic peak energy Ep;i and the collimation- corrected energy E� (Ghirlanda relation), unless the density of the circumburst environment of this burst is much larger than the nominal value, as suggested by other wavelength observations. We also discuss the possibility that this burst is an outlier in the correlation between Ep;i and the peak luminosity Lp (Yonetoku relation).

Published
2009
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46. THE EVOLUTION OFSWIFT/BAT BLAZARS AND THE ORIGIN OF THE MeV BACKGROUND

Author

Marco Ajello, Andres Escala, Neil Gehrels, Rita M. Sambruna, Jochen Greiner, L. Costamante, Richard Mushotzky, J. V. Wall, Jack Tueller, J. Chiang, and Arne Rau

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), QSOS, Physics, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COSMIC cancer database, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Accretion (astrophysics), Redshift, Space and Planetary Science, Elliptical galaxy, Astrophysics - High Energy Astrophysical Phenomena, Blazar, education, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use 3 years of data from the Swift/BAT survey to select a complete sample of X-ray blazars above 15 keV. This sample comprises 26 Flat-Spectrum Radio Quasars (FSRQs) and 12 BL Lac objects detected over a redshift range of 0.03, Comment: Accepted for publication in The Astrophysical Journal. 59 pages, 18 figures, 5 tables

Published
2009
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47. Gamma-ray telescopes

Author

J. K. Cannizzo and Neil Gehrels

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, Astronomical telescopes, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Blazar, Gamma-ray burst, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract

The last half-century has seen dramatic developments in gamma-ray telescopes, from their initial conception and development through to their blossoming into full maturity as a potent research tool in astronomy. Gamma-ray telescopes are leading research in diverse areas such as gamma-ray bursts, blazars, Galactic transients, and the Galactic distribution of aluminum-26., Comment: 11 pages, 6 figures/ in "400 Years of Astronomical Telescopes: A Review of History, Science and Technology", ed. B.R. Brandl, R. Stuik, & J.K. Katgert-Merkeli (Exp. Astron. 26, 111-122 [2009])

Published
2009
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48. ULTRAVIOLET LIGHT CURVES OF SUPERNOVAE WITH THESWIFTULTRAVIOLET/OPTICAL TELESCOPE

Author

Martin Still, Stefan Immler, Neil Gehrels, Peter J. Brown, Stephen T. Holland, Peter W. A. Roming, Peter Milne, John A. Nousek, Nino Panagia, and Daniel E. Vanden Berk

Subjects
Swift, Physics, Near-infrared spectroscopy, Astronomy and Astrophysics, Astrophysics, Light curve, medicine.disease_cause, Redshift, Supernova, Wavelength, Space and Planetary Science, Ultraviolet light, medicine, computer, Ultraviolet, computer.programming_language
Abstract

We present ultravioliet (UV) observations of supernovae (SNe) obtained with the UltraViolet/Optical Telescope (UVOT) on board the Swift spacecraft. This is the largest sample of UV light curves from any single instrument and covers all major SN types and most subtypes. The UV light curves of SNe Ia are fairly homogenous while SNe Ib/c and IIP show more variety in their light curve shapes. The UV-optical colors clearly differentiate SNe Ia and IIP, particularly at early times. The color evolution of SNe IIP, however, makes their colors similar to SNe Ia at about 20 days after explosion. SNe Ib/c are shown to have varied UV-optical colors. The use of UV colors to help type SNe will be important for high redshift SNe discovered in optical observations. These data can be added to ground based optical and near infrared data to create bolometric light curves of individual objects and as checks on generic bolometric corrections used in the absence of UV data. This sample can also be compared with rest-frame UV observations of high redshift SNe observed at optical wavelengths.

Published
2009
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49. Detection of 16 gamma-ray pulsars through blind frequency searches using the Fermi LAT

Author

A. W. Borgland, W. B. Atwood, S. Germani, Grzegorz Madejski, Nicola Giglietto, A. P. Waite, Denis Bastieri, P. L. Nolan, A. De Luca, A. Reimer, M. N. Lovellette, Jeffrey D. Scargle, P. A. Caraveo, Persis S. Drell, C. Meurer, N. Kawai, R. A. Cameron, P. Fusco, Sylvain Guiriec, Francesco Longo, Carmelo Sgrò, Riccardo Rando, E. Hays, T. H. Burnett, Richard Dubois, Gino Tosti, R. E. Hughes, E. J. Siskind, Joel R. Primack, Claudia Cecchi, Johann Cohen-Tanugi, G.L. Godfrey, Nanda Rea, E. Nuss, P. Giommi, Matthew Kerr, S. J. Fegan, Takaaki Tanaka, Tadayuki Takahashi, W. Mitthumsiri, Paul S. Ray, David Paneque, M. Kuss, S. Rainò, M. S. Strickman, D. J. Thompson, Magnus Axelsson, V. Vasileiou, N. Vilchez, Jonathan F. Ormes, Kent S. Wood, Markus Ackermann, Jean Ballet, M. Lemoine-Goumard, Karen Watters, B. Lott, M. T. Wolff, C. Farnier, H. Tajima, M. Brigida, C. C. Cheung, T. Glanzman, A. Sander, R. Claus, F. Piron, Paul J. Wang, Stefano Ciprini, Jean-Luc Starck, J. M. Casandjian, G. A. Caliandro, A. Brez, Yasunobu Uchiyama, A. van Etten, J. P. Norris, T. Ylinen, Hiromitsu Takahashi, Morihiro Hayashida, Alice K. Harding, P. M. Saz Parkinson, A. Morselli, V. Vitale, A. Chekhtman, Tsunefumi Mizuno, David S. Smith, R. P. Johnson, T. Ohsugi, F. Gargano, Elliott D. Bloom, B. M. Baughman, Nicola Omodei, Luca Latronico, J. Bregeon, L. Guillemot, A. Y. Rodriguez, Brandon Anderson, M. Dormody, C. Monte, A. A. Abdo, E. Orlando, J. E. Grove, Yasushi Fukazawa, P. Spinelli, M. N. Mazziotta, F. Giordano, M. L. Kocian, Stefan Funk, T. A. Porter, Roger W. Romani, M.-H. Grondin, F. de Palma, J. G. Thayer, Seth Digel, Tyrel J. Johnson, A. Makeev, Dario Gasparrini, P. D. Smith, E. Do Couto E Silva, Brian L Winer, M. E. Monzani, P. Lubrano, Luca Baldini, Giovanni F. Bignami, H. F.W. Sadrozinski, Ronaldo Bellazzini, Emanuele Bonamente, M. Pierbattista, I. A. Grenier, Gudlaugur Johannesson, J. Lande, F. Loparco, M. Ziegler, Felix Ryde, A. De Angelis, Jürgen Knödlseder, Y. Hanabata, C. Favuzzi, Gloria Spandre, Guido Barbiellini, B. Giebels, Matthew G. Baring, A. Tramacere, S. Murgia, S. Ritz, Charles D. Dermer, D. Parent, Melissa Pesce-Rollins, O. Tibolla, D. J. Suson, B. Berenji, W. McConville, Pascal Bruel, W. N. Johnson, Peter F. Michelson, Hideaki Katagiri, T. Kamae, Igor V. Moskalenko, Olaf Reimer, Jan Conrad, Diego F. Torres, V. Pelassa, C. Gwon, Julie McEnery, Neil Gehrels, David Sánchez, Marco Ajello, L. Tibaldo, Jun Kataoka, Ö. Çelik, S. Cutini, M. Pepe, D. Dumora, James Chiang, Roger Blandford, M. Marelli, M. Razzano, L.S. Rochester, T. L. Usher, Keith Bechtol, T. Reposeur, Abdo, A. A., Ackermann, M., Ajello, M., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Baughman, B. M., Bechtol, K., Bellazzini, R., Berenji, B., Bignami, G. F., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Celik, O., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Conrad, J., Cutini, S., Dermer, C. D., Angelis, A. d., Luca, A. d., Palma, F. d., Digel, S. W., Dormody, M., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Farnier, C., Favuzzi, C., Fegan, S. J., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giebels, B., Giglietto, N., Giommi, P., Giordano, F., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M. H., Grove, J. E., Guillemot, L., Guiriec, S., Gwon, C., Hanabata, Y., Harding, A. K., Hayashida, M., Hays, E., Hughes, R. E., Johannesson, G., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Knodlseder, J., Kocian, M. L., Kuss, M., Lande, J., Latronico, L., Lemoine Goumard, M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Marelli, M., Mazziotta, M. N., Mcconville, W., Mcenery, J. E., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Parent, D., Pelassa, V., Pepe, M., Pesce Rollins, M., Pierbattista, M., Piron, F., Porter, T. A., Primack, J. R., Raino, S., Rando, R., Ray, P. S., Razzano, M., Rea, N., Reimer, A., Reimer, O., Reposeur, T., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Romani, R. W., Ryde, F., Sadrozinski, H. F. W., Sanchez, D., Sander, A., Parkinson, P. M. S., Scargle, J. D., Sgro, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Starck, J. L., Strickman, M. S., Suson, D. J., Tajima, H., Takahashi, H., Takahashi, T., Tanaka, T., Thayer, J. G., Thompson, D. J., Tibaldo, L., Tibolla, O., Torres, D. F., Tosti, G., Tramacere, A., Uchiyama, Y., Usher, T. L., Etten, A. V., Vasileiou, V., Vilchez, N., Vitale, V., Waite, A. P., Wang, P., Watters, K., Winer, B. L., Wolff, M. T., Wood, K. S., Ylinen, T., Ziegler, M., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Fermi satellite, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, High Energy Gamma-ray Astronomy, Pulsar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, Pulsars, Astrophysics::Galaxy Astrophysics, Physics, Multidisciplinary, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics - Astrophysics of Galaxies, Neutron star, Stars, Supernova, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope, X-ray pulsar
Abstract

Pulsars are rapidly-rotating, highly-magnetized neutron stars emitting radiation across the electromagnetic spectrum. Although there are more than 1800 known radio pulsars, until recently, only seven were observed to pulse in gamma rays and these were all discovered at other wavelengths. The Fermi Large Area Telescope makes it possible to pinpoint neutron stars through their gamma-ray pulsations. We report the detection of 16 gamma-ray pulsars in blind frequency searches using the LAT. Most of these pulsars are coincident with previously unidentified gamma-ray sources, and many are associated with supernova remnants. Direct detection of gamma-ray pulsars enables studies of emission mechanisms, population statistics and the energetics of pulsar wind nebulae and supernova remnants., Comment: Corresponding authors: Michael Dormody, Paul S. Ray, Pablo M. Saz Parkinson, Marcus Ziegler

Published
2009
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50. Detection of high-energy gamma-ray emission from the globular cluster 47 Tucanae with Fermi

Author

I. A. Grenier, Marco Ajello, Francesco Longo, J. B. Thayer, T. H. Burnett, M. Ziegler, A. Sander, N. Kawai, Yasunobu Uchiyama, L. Tibaldo, V. Vasileiou, Kent S. Wood, C. Meurer, Luca Latronico, P. Wang, Hartmut Sadrozinski, Gloria Spandre, Denis Bastieri, N.A. Webb, Alessandro Brez, Gino Tosti, C. C. Cheung, Igor V. Moskalenko, Luca Baldini, R. E. Hughes, Emanuele Bonamente, A. Chekhtman, T. L. Usher, J. Lande, Sylvain Guiriec, Olaf Reimer, D. Horan, Jean Ballet, A. Y. Rodriguez, V. Pelassa, M. Pierbattista, R. Dubois, J. M. Casandjian, P. L. Nolan, L. Guillemot, D. J. Thompson, W. B. Focke, Stefano Ciprini, C. Farnier, B. M. Baughman, Diego F. Torres, P. Spinelli, P. D. Smith, C. Favuzzi, M. Razzano, S. Rainò, Tsunefumi Mizuno, Eric Charles, P. M. Saz Parkinson, C. Monte, T. Ohsugi, D. Parent, S. Murgia, B. Lott, Julie McEnery, Neil Gehrels, Hiromitsu Takahashi, David Sánchez, Elliott D. Bloom, W. B. Atwood, D. J. Suson, F. Piron, Pascal Bruel, Ö. Çelik, A. S. Johnson, S. Cutini, Francesco Giordano, T. Kamae, T. Glanzman, Nicola Giglietto, Jürgen Knödlseder, Nicola Omodei, M. Pepe, W. N. Johnson, W. McConville, Claudia Cecchi, Y. Hanabata, Randall P. Johnson, Carmelo Sgrò, Riccardo Rando, Alice K. Harding, Dario Gasparrini, Peter F. Michelson, M. N. Mazziotta, J. G. Thayer, A. Tramacere, James Chiang, A. A. Abdo, E. Orlando, P. Lubrano, B. Giebels, F. Gargano, Roger Blandford, Roger W. Romani, E. Nuss, G. Godfrey, Sylvain Chaty, M. N. Lovellette, Jean-Luc Starck, T. Reposeur, P. A. Caraveo, J. E. Grove, David Paneque, Takaaki Tanaka, D. Dumora, J. P. Norris, Hideaki Katagiri, A. Morselli, Persis S. Drell, Yasushi Fukazawa, Johann Cohen-Tanugi, Nanda Rea, A. W. Borgland, M. Kuss, J. F. Ormes, M. S. Strickman, V. Vitale, M. Roth, J. Bregeon, E. Hays, Seth Digel, M. Brigida, F. de Palma, F. Kuehn, E. Do Couto E Silva, T. Ylinen, J. H. Panetta, Magnus Axelsson, M. Lemoine-Goumard, Brian L Winer, N. Vilchez, Hiroyasu Tajima, Tyrel J. Johnson, T. A. Porter, Jan Conrad, Markus Ackermann, R. A. Cameron, Morihiro Hayashida, A. A. Moiseev, Keith Bechtol, M. Dormody, R. Claus, P. Fusco, F. Loparco, Gudlaugur Johannesson, A. Makeev, W. Mitthumsiri, Matthew Kerr, Felix Ryde, M. E. Monzani, G. A. Caliandro, S. J. Fegan, Guido Barbiellini, M. Frailis, L. S. Rochester, B. Berenji, Ronaldo Bellazzini, S. Ritz, Charles D. Dermer, David Smith, S. Germani, A. Reimer, Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Baughman, B. M., Bechtol, K., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Celik, O., Charles, E., Chaty, S., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Conrad, J., Cutini, S., Dermer, C. D., Palma, F. d., Digel, S. W., Dormody, M., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Farnier, C., Favuzzi, C., Fegan, S. J., Focke, W. B., Frailis, M., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giebels, B., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Grenier, I. A., Grove, J. E., Guillemot, L., Guiriec, S., Hanabata, Y., Harding, A. K., Hayashida, M., Hays, E., Horan, D., Hughes, R. E., Johannesson, G., Johnson, A. S., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Katagiri, H., Kawai, N., Kerr, M., Knodlseder, J., Kuehn, F., Kuss, M., Lande, J., Latronico, L., Lemoine Goumard, M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Makeev, A., Mazziotta, M. N., Mcconville, W., Mcenery, J. E., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pierbattista, M., Piron, F., Porter, T. A., Raino, S., Rando, R., Razzano, M., Rea, N., Reimer, A., Reimer, O., Reposeur, T., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Romani, R. W., Roth, M., Ryde, F., Sadrozinski, H. F. W., Sanchez, D., Sander, A., Parkinson, P. M. S., Sgro, C., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Starck, J. L., Strickman, M. S., Suson, D. J., Tajima, H., Takahashi, H., Tanaka, T., Thayer, J. B., Thayer, J. G., Thompson, D. J., Tibaldo, L., Torres, D. F., Tosti, G., Tramacere, A., Uchiyama, Y., Usher, T. L., Vasileiou, V., Vilchez, N., Vitale, V., Wang, P., Webb, N., Winer, B. L., Wood, K. S., Ylinen, T., Ziegler, M., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, High Energy Astrophys. & Astropart. Phys (API, FNWI), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -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, Population, Fermi satellite, Astrophysics, 01 natural sciences, High Energy Gamma-ray Astronomy, Globular Clusters, Luminosity, Pulsar, Millisecond pulsar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, Multidisciplinary, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Neutron star, Star cluster, Globular cluster, Fermi Gamma-ray Space Telescope
Abstract

Gamma-Ray Pulsar Bonanza Most of the pulsars we know about were detected through their radio emission; a few are known to pulse gamma rays but were first detected at other wavelengths (see the Perspective by Halpern ). Using the Fermi Gamma-Ray Space Telescope, Abdo et al. (p. 840 , published online 2 July; see the cover) report the detection of 16 previously unknown pulsars based on their gamma-ray emission alone. Thirteen of these coincide with previously unidentified gamma-ray sources, solving the 30-year-old mystery of their identities. Pulsars are fast-rotating neutron stars. With time they slow down and cease to radiate; however, if they are in a binary system, they can have their spin rates increased by mass transfer from their companion stars, starting a new life as millisecond pulsars. In another study, Abdo et al. (p. 845 ) report the detection of gamma-ray emission from the globular cluster 47 Tucanae, which is coming from an ensemble of millisecond pulsars in the cluster's core. The data imply that there are up to 60 millisecond pulsars in 47 Tucanae, twice as many as predicted by radio observations. In a further companion study, Abdo et al. (p. 848 , published online 2 July) searched Fermi Large Area Telescope data for pulsations from all known millisecond pulsars outside of stellar clusters, finding gamma-ray pulsations for eight of them. Their properties resemble those of other gamma-ray pulsars, suggesting that they share the same basic emission mechanism. Indeed, both sets of pulsars favor emission models in which the gamma rays are produced in the outer magnetosphere of the neutron star.

Published
2009
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