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1. Incremental Fermi Large Area Telescope Fourth Source Catalog

Author

Abdollahi, Soheila, Acero, Fabio, Bloom, Elliott, Orienti, Monica, Orlando, Elena, Paneque, David, Pei, Zhiyuan, Perkins, Jeremy S., Persic, Massimo, Pesce-Rollins, Melissa, Petrosian, Vahe, Pillera, Roberta, Poon, Helen, Bonino, Raffaella, Porter, Troy A., Principe, Giacomo, Raino, Silvia, Rando, Riccardo, Rani, Bindu, Razzano, Massimiliano, Razzaque, Soebur, Reimer, Anita, Reimer, Olaf, Reposeur, Thierry, Brill, Ari, Sanchez-Conde, Miguel A., Saz Parkinson, Pablo M., Scotton, Lorenzo, Serini, Davide, Sgro, Carmelo, Siskind, Eric J., Smith, David A., Spandre, Gloria, Spinelli, Paolo, Sueoka, Kohei, Britto, Richard J., Suson, Dan J., Tajima, Hiro, Tak, Dongguen, Thayer, Jana B., Thompson, David J., Torres, Diego F., Troja, Eleonora, Valverde, Janeth, Wood, Kent, Zaharijas, Gabrijela, Bruel, Philippe, Fermi-LAT Collaboration, Burnett, Toby H., Buson, Sara, Cameron, Rob A., Caputo, Regina, Caraveo, Patrizia A., Baldini, Luca, Castro, Daniel, Chaty, Sylvain, Cheung, Teddy C., Chiaro, Graziano, Cibrario, Nicolo, Ciprini, Stefano, Coronado-Blazquez, Javier, Crnogorcevic, Milena, Cutini, Sara, D'Ammando, Filippo, Ballet, Jean, De Gaetano, Salvatore, Digel, Seth W., Di Lalla, Niccolo, Dirirsa, Feraol F., Di Venere, Leonardo, Dominguez, Alberto, Fallah Ramazani, Vandad, Fegan, Stephen J., Ferrara, Elizabeth C., Fiori, Alessio, Bastieri, Denis, Fleischhack, Henrike, Franckowiak, Anna, Fukazawa, Yasushi, Funk, Stefan, Fusco, Piergiorgio, Galanti, Giorgio, Gammaldi, Viviana, Gargano, Fabio, Garrappa, Simone, Gasparrini, Dario, Bellazzini, Ronaldo, Giacchino, Federica, Giglietto, Nico, Giordano, Francesco, Giroletti, Marcello, Glanzman, Thomas, Green, David, Grenier, Isabelle A., Grondin, Marie-Helene, Guillemot, Lucas, Guiriec, Sylvain, Berenji, Bijan, Gustafsson, Michael, Harding, Alice K., Hays, Liz, Hewitt, John W., Hays, E., Horan, Deirdre, Hou, Xian, Johannesson, Gudlaugur, Karwin, Christopher M., Kayanoki, Taishu, Berretta, Alessandra, Kerr, Matthew T., Kuss, Michael, Landriu, David, Larsson, Stefan, Latronico, Luca, Lemoine-Goumard, Marianne, Li, Jian, Liodakis, Ioannis, Longo, Francesco, Loparco, Francesco, Bissaldi, Elisabetta, Lott, Benoit, Lubrano, Pasquale, Maldera, Simone, Malyshev, Dmitry, Manfreda, Alberto, Marti-Devesa, Guillem, Mazziotta, Mario N., Mereu, Isabella, Meyer, Manuel, Michelson, Peter F., Blandford, Roger D., Mirabal, Nestor, Mitthumsiri, Warit, Mizuno, Tsunefumi, Moiseev, Alex A., Monzani, Maria E., Morselli, Aldo, Moskalenko, Igor V., Negro, Michela, Nuss, Eric, Omodei, Nicola, European Space Agency, National Science Foundation (US), National Aeronautics and Space Administration (US), Department of Energy (US), Agenzia Spaziale Italiana, Institut de recherche en astrophysique et planétologie (IRAP), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, and UAM. Departamento de Física Teórica

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Física, Astronomy and Astrophysics, Galaxies, Astronomi, astrofysik och kosmologi, Space and Planetary Science, BL Lacertae Object, Astronomy, Astrophysics and Cosmology, ddc:520, ddc:530, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Blazars
Abstract

Abdollahi et al., We present an incremental version (4FGL-DR3, for Data Release 3) of the fourth Fermi Large Area Telescope (LAT) catalog of γ-ray sources. Based on the first 12 years of science data in the energy range from 50 MeV to 1 TeV, it contains 6658 sources. The analysis improves on that used for the 4FGL catalog over eight years of data: more sources are fit with curved spectra, we introduce a more robust spectral parameterization for pulsars, and we extend the spectral points to 1 TeV. The spectral parameters, spectral energy distributions, and associations are updated for all sources. Light curves are rebuilt for all sources with 1 yr intervals (not 2 month intervals). Among the 5064 original 4FGL sources, 16 were deleted, 112 are formally below the detection threshold over 12 yr (but are kept in the list), while 74 are newly associated, 10 have an improved association, and seven associations were withdrawn. Pulsars are split explicitly between young and millisecond pulsars. Pulsars and binaries newly detected in LAT sources, as well as more than 100 newly classified blazars, are reported. We add three extended sources and 1607 new point sources, mostly just above the detection threshold, among which eight are considered identified, and 699 have a plausible counterpart at other wavelengths. We discuss the degree-scale residuals to the global sky model and clusters of soft unassociated point sources close to the Galactic plane, which are possibly related to limitations of the interstellar emission model and missing extended sources., The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Études Spatiales in France. This work is performed in part under DOE Contract DE-AC02-76SF00515. This work made extensive use of the ATNF pulsar catalog 102 (Manchester et al. 2005). This research has made use of the NASA/IPAC Extragalactic Database (NED; 2019), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and of archival data, software, and online services provided by the ASI Science Data Center (ASDC) operated by the Italian Space Agency.

Published
2022
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2. Einstein@Home discovers a radio-quiet gamma-ray millisecond pulsar

Author

Clark, Colin J., Pletsch, Holger J., Aulbert, Carsten, Orienti, Monica, Orlando, Elena, Palatiello, Michele, Paliya, Vaidehi S., de Palma, Francesco, Paneque, David, Perkins, Jeremy S., Persic, Massimo, Pesce-Rollins, Melissa, Porter, Troy A., Beer, Christian, Principe, Giacomo, Rainò, Silvia, Rando, Riccardo, Ray, Paul S., Razzano, Massimiliano, Reimer, Anita, Reimer, Olaf, Romani, Roger W., Saz Parkinson, Pablo M., Sgrò, Carmelo, Bock, Oliver, Siskind, Eric J., Smith, David A., Spada, Francesca, Spandre, Gloria, Spinelli, Paolo, Thayer, Jana B., Thompson, David J., Torres, Diego F., Troja, Eleonora, Vianello, Giacomo, Cuéllar, Andres, Wood, Kent, Wood, Matthew, Fermi-LAT Collaboration, Eggenstein, Heinz-Bernd, Fehrmann, Henning, Kramer, Michael, Kwang, Shawn A., Machenschalk, Bernd, Nieder, Lars, Wu, Jason, Ackermann, Markus, Ajello, Marco, Baldini, Luca, Ballet, Jean, Barbiellini, Guido, Bastieri, Denis, Bellazzini, Ronaldo, Bissaldi, Elisabetta, Blandford, Roger D., Bloom, Elliott D., Guillemot, Lucas, Bonino, Raffaella, Bottacini, Eugenio, Brandt, Terri J., Bregeon, Johan, Bruel, Philippe, Buehler, Rolf, Burnett, Toby H., Buson, Sara, Cameron, Rob A., Caputo, Regina, Kerr, Matthew, Caraveo, Patrizia A., Cavazzuti, Elisabetta, Cecchi, Claudia, Charles, Eric, Chekhtman, Alexandre, Ciprini, Stefano, Cominsky, Lynn R., Costantin, Denise, Cutini, Sara, D'Ammando, Filippo, Johnson, Tyrel J., De Luca, Andrea, Desiante, Rachele, Di Venere, Leonardo, Di Mauro, Mattia, Di Lalla, Niccolò, Digel, Seth W., Favuzzi, Cecilia, Ferrara, Elizabeth C., Franckowiak, Anna, Fukazawa, Yasushi, Camilo, Fernando, Funk, Stefan, Fusco, Piergiorgio, Gargano, Fabio, Gasparrini, Dario, Giglietto, Nico, Giordano, Francesco, Giroletti, Marcello, Gomez-Vargas, Germán A., Green, David, Grenier, Isabelle A., Salvetti, David, Guiriec, Sylvain, Harding, Alice K., Hewitt, John W., Horan, Deirdre, Jóhannesson, Guðlaugur, Kensei, Shiki, Kuss, Michael, La Mura, Giovanni, Larsson, Stefan, Latronico, Luca, Allen, Bruce, Li, Jian, Longo, Francesco, Loparco, Francesco, Lovellette, Michael N., Lubrano, Pasquale, Magill, Jeffrey D., Maldera, Simone, Manfreda, Alberto, Mazziotta, Mario N., McEnery, Julie E., Anderson, David, Michelson, Peter F., Mirabal, Nestor, Mitthumsiri, Warit, Mizuno, Tsunefumi, Monzani, Maria Elena, Morselli, Aldo, Moskalenko, Igor V., Nuss, Eric, Ohsugi, Takashi, Omodei, Nicola, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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 Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-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), 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), 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), Fermi-LAT, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-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), ITA, Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), 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 Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-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), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Centre National de la Recherche Scientifique ( CNRS ) -Université d'Orléans ( UO ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Laboratoire Univers et Particules de Montpellier ( LUPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ), 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 ), 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 ), Raunvísindastofnun (HÍ), Science Institute (UI), Verkfræði- og náttúruvísindasvið (HÍ), School of Engineering and Natural Sciences (UI), Háskóli Íslands, University of Iceland, Clark, Colin J., Pletsch, Holger J., Wu, Jason, Guillemot, Luca, Kerr, Matthew, Johnson, Tyrel J., Camilo, Fernando, Salvetti, David, Allen, Bruce, Anderson, David, Aulbert, Carsten, Beer, Christian, Bock, Oliver, Cuéllar, Andre, Eggenstein, Heinz-Bernd, Fehrmann, Henning, Kramer, Michael, Kwang, Shawn A., Machenschalk, Bernd, Nieder, Lar, Ackermann, Marku, Ajello, Marco, Baldini, Luca, Ballet, Jean, Barbiellini, Guido, Bastieri, Deni, Bellazzini, Ronaldo, Bissaldi, Elisabetta, Blandford, Roger D., Bloom, Elliott D., Bonino, Raffaella, Bottacini, Eugenio, Brandt, Terri J., Bregeon, Johan, Bruel, Philippe, Buehler, Rolf, Burnett, Toby H., Buson, Sara, Cameron, Rob A., Caputo, Regina, Caraveo, Patrizia A., Cavazzuti, Elisabetta, Cecchi, Claudia, Charles, Eric, Chekhtman, Alexandre, Ciprini, Stefano, Cominsky, Lynn R., Costantin, Denise, Cutini, Sara, D'Ammando, Filippo, De Luca, Andrea, Desiante, Rachele, Di Venere, Leonardo, Di Mauro, Mattia, Di Lalla, Niccolò, Digel, Seth W., Favuzzi, Cecilia, Ferrara, Elizabeth C., Franckowiak, Anna, Fukazawa, Yasushi, Funk, Stefan, Fusco, Piergiorgio, Gargano, Fabio, Gasparrini, Dario, Giglietto, Nico, Giordano, Francesco, Giroletti, Marcello, Gomez-Vargas, Germán A., Green, David, Grenier, Isabelle A., Guiriec, Sylvain, Harding, Alice K., Hewitt, John W., Horan, Deirdre, Jóhannesson, Guolaugur, Kensei, Shiki, Kuss, Michael, La Mura, Giovanni, Larsson, Stefan, Latronico, Luca, Li, Jian, Longo, Francesco, Loparco, Francesco, Lovellette, Michael N., Lubrano, Pasquale, Magill, Jeffrey D., Maldera, Simone, Manfreda, Alberto, Mazziotta, Mario N., Mcenery, Julie E., Michelson, Peter F., Mirabal, Nestor, Mitthumsiri, Warit, Mizuno, Tsunefumi, Monzani, Maria Elena, Morselli, Aldo, Moskalenko, Igor V., Nuss, Eric, Ohsugi, Takashi, Omodei, Nicola, Orienti, Monica, Orlando, Elena, Palatiello, Michele, Paliya, Vaidehi S., De Palma, Francesco, Paneque, David, Perkins, Jeremy S., Persic, Massimo, Pesce-Rollins, Melissa, Porter, Troy A., Principe, Giacomo, Rainò, Silvia, Rando, Riccardo, Ray, Paul S., Razzano, Massimiliano, Reimer, Anita, Reimer, Olaf, Romani, Roger W., Parkinson, Pablo M. Saz, Sgrò, Carmelo, Siskind, Eric J., Smith, David A., Spada, Francesca, Spandre, Gloria, Spinelli, Paolo, Thayer, Jana B., Thompson, David J., Torres, Diego F., Troja, Eleonora, Vianello, Giacomo, Wood, Kent, and Wood, Matthew

Subjects
Einstein@Home, Gammageislar, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, Computer Science::Hardware Architecture, Bulge, Millisecond pulsar, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, education, 010303 astronomy & astrophysics, Research Articles, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Line-of-sight, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Nifteindastjörnur, Astrophysics::Instrumentation and Methods for Astrophysics, SciAdv r-articles, Computer Science::Computers and Society, Stjörnusjónaukar, Neutron star, ddc:500, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope, Research Article
Abstract

Millisecond pulsars (MSPs) are old neutron stars that spin hundreds of times per second and appear to pulsate as their emission beams cross our line of sight. To date, radio pulsations have been detected from all rotation-powered MSPs. In an attempt to discover radio-quiet gamma-ray MSPs, we used the aggregated power from the computers of tens of thousands of volunteers participating in the Einstein@Home distributed computing project to search for pulsations from unidentified gamma-ray sources in Fermi Large Area Telescope data. This survey discovered two isolated MSPs, one of which is the only known rotation-powered MSP to remain undetected in radio observations. These gamma-ray MSPs were discovered in completely blind searches without prior constraints from other observations, raising hopes for detecting MSPs from a predicted Galactic bulge population., This work was supported by the Max-Planck-Gesellschaft, the Deutsche Forschungsgemeinschaft through an Emmy Noether Research Grant [no. PL 710/1-1 (H.J.P.)], and NSF award 1104902. C.J.C. acknowledges support from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 715051; Spiders). W.M. was partially supported by the Thailand Research Fund (grants TRG5880173 and RTA5980003). M.R. was funded by the Italian Ministry of Education, University and Research (contract no. FIRB-2012-RBFR12PM1F). Work at the Naval Research Laboratory is supported by NASA. The Parkes Observatory is part of the Australia Telescope, funded by the Commonwealth of Australia for operation as a National Facility managed by the Commonwealth Scientific and Industrial Research Organisation (CSIRO). The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT, as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. This work performed in part under DOE Contract DE-AC02-76SF00515.

Published
2018

3. STROBE-X: X-ray Timing and Spectroscopy on Dynamical Timescales from Microseconds to Years

Author

Ray, Paul S., Arzoumanian, Zaven, Ballantyne, David, Bozzo, Enrico, Brandt, Soren, Brenneman, Laura, Chakrabarty, Deepto, Christophersen, Marc, DeRosa, Alessandra, Feroci, Marco, Gendreau, Keith, Goldstein, Adam, Hartmann, Dieter, Hernanz, Margarita, Jenke, Peter, Kara, Erin, Maccarone, Tom, McDonald, Michael, Nowak, Michael, Phlips, Bernard, Remillard, Ron, Stevens, Abigail, Tomsick, John, Watts, Anna, Wilson-Hodge, Colleen, Wood, Kent, Zane, Silvia, Ajello, Marco, Alston, Will, Altamirano, Diego, Antoniou, Vallia, Arur, Kavitha, Ashton, Dominic, Auchettl, Katie, Ayres, Tom, Bachetti, Matteo, Balokovic, Mislav, Baring, Matthew, Baykal, Altan, Begelman, Mitch, Bhat, Narayana, Bogdanov, Slavko, Briggs, Michael, Bulbul, Esra, Bult, Petrus, Burns, Eric, Cackett, Ed, Campana, Riccardo, Caspi, Amir, Cavecchi, Yuri, Chenevez, Jerome, Cherry, Mike, Corbet, Robin, Corcoran, Michael, Corsi, Alessandra, Degenaar, Nathalie, Drake, Jeremy, Eikenberry, Steve, Enoto, Teruaki, Fragile, Chris, Fuerst, Felix, Gandhi, Poshak, Garcia, Javier, Gonzalez, Anthony, Grefenstette, Brian, Grinberg, Victoria, Grossan, Bruce, Guillot, Sebastien, Guver, Tolga, Haggard, Daryl, Heinke, Craig, Heinz, Sebastian, Hemphill, Paul, Homan, Jeroen, Hui, Michelle, Huppenkothen, Daniela, Ingram, Adam, Irwin, Jimmy, Jaisawal, Gaurava, Jaodand, Amruta, Kalemci, Emrah, Kaplan, David, Keek, Laurens, Kennea, Jamie, Kerr, Matthew, van der Klis, Michiel, Kocevski, Daniel, Koss, Mike, Kowalski, Adam, Lai, Dong, Lamb, Fred, Laycock, Silas, Lazio, Joseph, Lazzati, Davide, Longcope, Dana, Loewenstein, Michael, Maitra, Dipankair, Majid, Walid, Maksym, W. Peter, Malacaria, Christian, Margutti, Raffaella, Martindale, Adrian, McHardy, Ian, Meyer, Manuel, Middleton, Matt, Miller, Jon, Miller, Cole, Motta, Sara, Neilsen, Joey, Nelson, Tommy, Noble, Scott, O'Brien, Paul, Osborne, Julian, Osten, Rachel, Ozel, Feryal, Palliyaguru, Nipuni, Pasham, Dheeraj, Patruno, Alessandro, Pelassa, Vero, Petropoulou, Maria, Pilia, Maura, Pohl, Martin, Pooley, David, Prescod-Weinstein, Chanda, Psaltis, Dimitrios, Raaijmakers, Geert, Reynolds, Chris, Riley, Thomas E., Salvesen, Greg, Santangelo, Andrea, Scaringi, Simone, Schanne, Stephane, Schnittman, Jeremy, Smith, David, Smith, Krista Lynne, Snios, Bradford, Steiner, Andrew, Steiner, Jack, Stella, Luigi, Strohmayer, Tod, Sun, Ming, Tauris, Thomas, Taylor, Corbin, Tohuvavohu, Aaron, Vacchi, Andrea, Vasilopoulos, Georgios, Veledina, Alexandra, Walsh, Jonelle, Weinberg, Nevin, Wilkins, Dan, Willingale, Richard, Wilms, Joern, Winter, Lisa, Wolff, Michael, Zand, Jean in 't, Zezas, Andreas, Zhang, Bing, and Zoghbi, Abdu

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We present the Spectroscopic Time-Resolving Observatory for Broadband Energy X-rays (STROBE-X), a probe-class mission concept selected for study by NASA. It combines huge collecting area, high throughput, broad energy coverage, and excellent spectral and temporal resolution in a single facility. STROBE-X offers an enormous increase in sensitivity for X-ray spectral timing, extending these techniques to extragalactic targets for the first time. It is also an agile mission capable of rapid response to transient events, making it an essential X-ray partner facility in the era of time-domain, multi-wavelength, and multi-messenger astronomy. Optimized for study of the most extreme conditions found in the Universe, its key science objectives include: (1) Robustly measuring mass and spin and mapping inner accretion flows across the black hole mass spectrum, from compact stars to intermediate-mass objects to active galactic nuclei. (2) Mapping out the full mass-radius relation of neutron stars using an ensemble of nearly two dozen rotation-powered pulsars and accreting neutron stars, and hence measuring the equation of state for ultradense matter over a much wider range of densities than explored by NICER. (3) Identifying and studying X-ray counterparts (in the post-Swift era) for multiwavelength and multi-messenger transients in the dynamic sky through cross-correlation with gravitational wave interferometers, neutrino observatories, and high-cadence time-domain surveys in other electromagnetic bands. (4) Continuously surveying the dynamic X-ray sky with a large duty cycle and high time resolution to characterize the behavior of X-ray sources over an unprecedentedly vast range of time scales. STROBE-X's formidable capabilities will also enable a broad portfolio of additional science., 50 pages, Probe class mission concept study report submitted to NASA for Astro2020 Decadal Survey

Published
2019

4. The NRL Program in X-ray Navigation

Author

Wood, Kent S. and Ray, Paul S.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

This chapter describes the development of X-ray Navigation at the Naval Research Laboratory (NRL) within its astrophysics research programs. The prospects for applications emerged from early discoveries of X-ray source classes and their properties. Starting around 1988 some NRL X-ray astronomy programs included navigation as one of the motivations. The USA experiment (1999) was the first flight payload with an explicit X-ray navigation theme. Subsequently, NRL has continued to work in this area through participation in DARPA and NASA programs. Throughout, the general concept of X-ray navigation (XRNAV) has been broad enough to encompass many different uses of X-ray source observations for attitude determination, position determination, and timekeeping. Pulsar-based X-ray navigation (XNAV) is a special case., 30 pages, 15 figures, to appear in Proceedings of the 593. WE-Heraeus Seminar on Autonomous Spacecraft Navigation, ed. W. Becker

Published
2017

5. Characterization of Pulsar Sources for X-ray Navigation

Author

Ray, Paul S., Wood, Kent S., and Wolff, Michael T.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The Station Explorer for X-ray Timing and Navigation Technology (SEXTANT) is a technology demonstration enhancement to the Neutron Star Interior Composition Explorer (NICER) mission, which is scheduled to launch in 2017 and will be hosted as an externally attached payload on the International Space Station (ISS). During NICER's 18-month baseline science mission to understand ultra-dense matter through observations of neutron stars in the soft X-ray band, SEXTANT will, for the first-time, demonstrate real-time, on-board X-ray pulsar navigation. Using NICER/SEXTANT as an example, we describe the factors that determine the measurement errors on pulse times of arrival, including source and background count rates, and pulse profile shapes. We then describe properties of the SEXTANT navigation pulsar catalog and prospects for growing it once NICER launches. Finally, we describe the factors affecting the prediction of pulse arrival times in advance, including variable interstellar propagation effect and red timing noise. Together, all of these factors determine how well a particular realization of an X-ray pulsar-based navigation system will perform., Comment: 16 pages, 7 figures, to appear in Proceedings of the 593. WE-Heraeus Seminar on Autonomous Spacecraft Navigation, ed. W. Becker

Published
2017
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6. Looking into the Theory of Pulsar Accretion: Cen X-3 and XTE J1946+274

Author

Marcu, Diana M., Pottschmidt, Katja, Gottlieb, Amy M., Wolff, Michael T., Becker, Peter A., Joern Wilms, Ferrigno, Carlo, and Wood, Kent S.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

This is an overview of pulsar accretion modeling. The physics of pulsar accretion, i.e., the process of plasma flow onto the neutron star surface, can be constrained from the spectral properties of the X-ray source. We discuss a new implementation of the physical continuum model developed by Becker and Wolff (2007, ApJ 654, 435). The model incorporates Comptonized blackbody, bremsstrahlung, and cyclotron emission. We discuss preliminary results of applying the new tool to the test cases of Suzaku data of Cen X-3 and XTE J1946+274. Cen X-3 is a persistent accreting pulsar with an O-star companion observed during a bright period. XTE J1946+274 is a transient accreting pulsar with a Be companion observed during a dim period. Both sources show spectra that are well described with an empirical Fermi Dirac cutoff power law model. We extend the spectral analysis by making the first steps towards a physical description of Cen X-3 and XTE J1946+274., 9 pages, 6 figures, 2014 INTEGRAL Workshop Proceedings. http://pos.sissa.it/archive/conferences/228/065/Integral2014_065.pdf

Published
2015

7. The 1st Fermi Lat Supernova Remnant Catalog

Author

Acero, Fabio, Ackermann, Markus, Ajello, Marco, Baldini, Luca, Ballet, Jean, Barbiellini, Guido, Bastieri, Denis, Bellazzini, Ronaldo, Bissaldi, E., Blandford, Roger, Bloom, E. D., Bonino, Raffaella, Bottacini, Eugenio, Bregeon, J., Bruel, Philippe, Buehler, Rolf, Buson, S., Caliandro, G. A., Cameron, Rob A., Caputo, R., Caragiulo, Micaela, Caraveo, Patrizia A., Casandjian, Jean Marc, Cavazzuti, Elisabetta, Cecchi, Claudia, Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, Stefano, Claus, R., Cohen, J. M., Cohen-Tanugi, Johann, Cominsky, L. R., Condon, B., Conrad, Jan, Cutini, S., D Ammando, F., Angelis, A., Palma, F., Desiante, Rachele, Digel, S. W., Venere, L., Drell, Persis S., Drlica-Wagner, Alex, Favuzzi, C., Ferrara, E. C., Franckowiak, Anna, Fukazawa, Yasushi, Funk, Stefan, Fusco, P., Gargano, Fabio, Gasparrini, Dario, Giglietto, Nicola, Giommi, Paolo, Giordano, Francesco, Giroletti, Marcello, Glanzman, Tom, Godfrey, Gary, Gomez-Vargas, G. A., Grenier, I. A., Grondin, M. -H, Guillemot, L., Guiriec, Sylvain, Gustafsson, M., Hadasch, D., Harding, A. K., Hayashida, M., Hays, Elizabeth, Hewitt, J. W., Adam Hill, Horan, Deirdre, Hou, X., Iafrate, Giulia, Jogler, Tobias, J Ohannesson, G., Johnson, Anthony S., Kamae, T., Katagiri, Hideaki, Kataoka, Jun, Katsuta, Junichiro, Kerr, Matthew, Knodlseder, J., Kocevski, Dale, Kuss, M., Laffon, Helene, Lande, J., Larsson, S., Latronico, Luca, Lemoine-Goumard, Marianne, Li, J., Li, L., Longo, Francesco, Loparco, Francesco, Lovellette, Michael N., Lubrano, Pasquale, Magill, J., Maldera, S., Marelli, Martino, Mayer, Michael, Mazziotta, M. N., Michelson, Peter F., Mitthumsiri, Warit, Mizuno, Tsunefumi, Moiseev, Alexander A., Monzani, Maria Elena, Moretti, E., Morselli, Aldo, Moskalenko, Igor V., Murgia, Simona, Nemmen, Rodrigo, Nuss, Eric, Ohsugi, Takashi, Omodei, Nicola, Orienti, Monica, Orlando, Elena, Ormes, Jonathan F., Paneque, David, Perkins, J. S., Pesce-Rollins, Melissa, Petrosian, Vahe, Piron, Frederic, Pivato, Giovanna, Porter, Troy, Rain O, S., Rando, Riccardo, Razzano, Massimiliano, Razzaque, Soebur, Reimer, Anita, Reimer, Olaf, Renaud, Matthieu, Reposeur, Thierry, Romain Rousseau, Mr., Parkinson, P. M., Schmid, J., Schulz, A., Sgr O, C., Siskind, Eric J., Spada, Francesca, Spandre, Gloria, Spinelli, Paolo, Strong, Andrew W., Suson, Daniel, Tajima, Hiro, Takahashi, Hiromitsu, Tanaka, T., Thayer, Jana B., Thompson, D. J., Tibaldo, L., Tibolla, Omar, Torres, Diego F., Tosti, Gino, Troja, Eleonora, Uchiyama, Yasunobu, Vianello, G., Wells, B., Wood, Kent, Wood, M., Yassine, Manal, and Zimmer, Stephan

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract

To uniformly determine the properties of supernova remnants (SNRs) at high energies, we have developed the first systematic survey at energies from 1 to 100 GeV using data from the Fermi Large Area Telescope. Based on the spatial overlap of sources detected at GeV energies with SNRs known from radio surveys, we classify 30 sources as likely GeV SNRs. We also report 14 marginal associations and 245 flux upper limits. A mock catalog in which the positions of known remnants are scrambled in Galactic longitude, allows us to determine an upper limit of 22% on the number of GeV candidates falsely identified as SNRs. We have also developed a method to estimate spectral and spatial systematic errors arising from the diffuse interstellar emission model, a key component of all Galactic Fermi LAT analyses. By studying remnants uniformly in aggregate, we measure the GeV properties common to these objects and provide a crucial context for the detailed modeling of individual SNRs. Combining our GeV results with multiwavelength (MW) data, including radio, X-ray, and TeV, demonstrates the need for improvements to previously sufficient, simple models describing the GeV and radio emission from these objects. We model the GeV and MW emission from SNRs in aggregate to constrain their maximal contribution to observed Galactic cosmic rays., Comment: Resubmitted to ApJS

Published
2015
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8. High energy $��$-ray emission from PSR B1259$-$63 during 2014 and 2010 periastron passages

Author

Caliandro, G. Andrea, Cheung, C. C. Teddy, Li, Jian, Torres, Diego F., and Wood, Kent

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences
Abstract

PSR B1259$-$63/SS 2883 is a $��$-ray binary system composed of a radio pulsar in a long (1236.7 days) and elliptical ($e\sim0.87$) orbit around a Be star. In its 2010 periastron passage, multiwavelength emission from radio to TeV was observed, and an unexpected GeV flare was detected by the Fermi Large Area Telescope (LAT). Here we present the results of the LAT monitoring of PSR B1259$-$63 during its most recent 2014 periastron passage. We confirm that the GeV flare is recurrent within the orbit. The comparison of the 2014 and 2010 periastron passages shows overall similarities of flare durations, average flux levels, and spectra. In contrast, the detailed time evolutions of the two flares present interesting differences. Indeed, the light curves of the two flares show both a different structure and peak energy flux ($9.6 \pm1.8 \times 10^{-10}$ erg cm$^{-2}$ s$^{-1}$ and $7.1 \pm1.3 \times 10^{-10}$ erg cm$^{-2}$ s$^{-1}$, respectively in 2010 and 2014). While the tail of the 2010 flare the flux decayed exponentially, in 2014 it persisted at a high level. The interpretation of these differences as well as of the flare themselves is subject of debate., Conference proceeding. Swift: 10 Years of Discovery, 2-5 December 2014, La Sapienza University, Rome, Italy. 6 pages, 2 figures

Published
2015
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9. Million Degree Plasmas in Extreme Ultraviolet (EUV) Astrophysics

Author

Kowalski, Michael P., Barstow, Martin, Bruhweiler, Frederick, Cruddace, Raymond, Dupree, Andrea, Holberg, Jay, Howell, Steve, Laming, J. Martin, Linsky, Jeffrey, Sion, Edward, Strohmayer, Tod, Szkody, Paula, Welsh, Barry, Wolff, Michael, and Wood, Kent

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

Million degree plasmas are ubiquitous in the Universe, and examples include the atmospheres of white dwarfs; accretion phenomena in young stars, cataclysmic variables and active galactic nuclei; the coronae of stars; and the interstellar medium of our own galaxy and of others. The bulk of radiation from million degree plasmas is emitted at extreme ultraviolet (EUV) wavelengths, which includes critical spectral features containing diagnostic information often not available at other wavelengths. With underpinning by a mature instrument technology, there is great opportunity here for exciting discoveries., 8 pages, 3 figures; Science White Paper for the Astro2010 decadal review

Published
2009

10. Quantum Dynamics of Small-Size Triplet Superconductors with Broken Time-Reversal Symmetry

Author

Gulian, Armen M. and Wood, Kent S.

Subjects
Superconductivity (cond-mat.supr-con), Condensed Matter - Superconductivity, FOS: Physical sciences
Abstract

Symmetry of the order parameter in some triplet superconductors corresponds to doubly-degenerate chiral states. We predict that in a sufficiently small sample this degeneracy can be lifted via macroscopic quantum tunneling. Moreover, if the initial state is prepared correspondingly, 'instanton'-like quantum behavior is possible in a single-domain sample. In this case coherent oscillations of magnetic momentum should take place, as well as the sign alternations of the boundary currents. In particular, spontaneous Hall-effect recently predicted for ruthenates should posses the oscillating voltage feature., 6 pages, 1 figure, submitted to Phys. Rev. Lett

Published
2002

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