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arXiv 2017年

作者： Donley, J.L. Kartaltepe, J. Kocevski, D. Salvato, M. Santini, P. Suh, H. Civano, F. Koekemoer, A.M. Trump, J. Brusa, M. Cardamone, C. Castro, A. Cisternas, M. Conselice, C. Croton, D. Hathi, N. Liu, C. Lucas, R.A. Nair, P. Rosario, D. Sanders, D. Simmons, B. Villforth, C. Alexander, D.M. Bell, E.F. Faber, S.M. Grogin, N.A. Lotz, J. McIntosh, D.H. Nagao, T. Los Alamos National Laboratory P.O. Box 1663 Los AlamosNM87545 United States Rochester Institute of Technology RochesterNY United States Colby College WatervilleME04901 United States Max Planck Institut für extraterrestrische Physik Giessenbachstrasse 1 Garching bei MünchenD-85748 Germany INAF-Osservatorio Astronomico di Roma via di Frascati 33 Monte Porzio Catone RomaI-00040 Italy Subaru Telescope National Astronomical Observatory of Japan 650 A’ohoku place HiloHI96720 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States University of Connecticut 2152 Hillside Road U-3046 StorrsCT06269 United States INAF-Osservatorio Astronomico di Bologna via Ranzani 1 BolognaI-40127 Italy Department of Math & Science Wheelock College 200 Riverway BostonMA02215 United States Instituto de Astronomía Observatorio Astronómico Nacional. A.P. 877 EnsenadaBC22800 Mexico Universidad Autónoma de Ciudad Juárez Instituto de Ingeniería y Tecnología 1210 Plutarco Elias Calles Cd. Juarez CH32310 Mexico Instituto de Astrofisica de Canarias E-38205 La Laguna Tenerife Spain School of Physics & Astronomy University of Nottingham NottinghamNG7 2RD United Kingdom Centre for Astrophysics & Supercomputing Swinburne University of Technology P.O. Box 218 HawthornVIC3122 Australia UMR 7326 Marseille13388 France Astrophysical Observatory Department of Engineering Science and Physics City University of New York College of Staten Island 2800 Victory Boulevard Staten IslandNY10314 United States Department of Astrophysics and Hayden Planetarium American Museum of Natural History New YorkNY10024 United States Physics Program Graduate Center CUNY New YorkNY10016 United States Department of Physics and Astronomy University of Alabama Box 870324 TuscaloosaAL35487-0324 United States Institute for Astronomy Universit

While major mergers have long been proposed as a driver of both AGN activity and the MBH − σbulge relation, studies of moderate to high redshift Seyfert-luminosity AGN hosts have found little evidence for enhanced rates of interactions. However, both theory and observation suggest that while these AGN may be fueled by stochastic accretion and secular processes, high-luminosity, high-redshift, and heavily obscured AGN are the AGN most likely to be merger-driven. To better sample this population of AGN, we turn to infrared selection in the CANDELS/COSMOS field. Compared to their lower-luminosity and less obscured X-ray–only counterparts, IR-only AGN (luminous, heavily obscured AGN) are more likely to be classified as either irregular (Formula presented) or asymmetric (Formula presented) and are less likely to have a spheroidal component (Formula presented). Furthermore, IR-only AGN are also significantly more likely than X-ray–only AGN (75+−813% vs. 31+−66%) to be classified either as interacting or merging in a way that significantly disturbs the host galaxy or disturbed though not clearly interacting or merging, which potentially represents the late stages of a major merger. This suggests that while major mergers may not contribute significantly to the fueling of Seyfert luminosity AGN, interactions appear to play a more dominant role in the triggering and fueling of high-luminosity heavily obscured AGN. Copyright © 2017, The Authors. All rights reserved.

关键词： Merging

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Dark energy survey year 1 results: Methodology and projections for joint analysis of galaxy Clustering, galaxy lensing, and CMB lensing two-point functions

arXiv

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arXiv 2018年

作者： Baxter, E.J. Omori, Y. Chang, C. Giannantonio, T. Kirk, D. Krause, E. Blazek, J. Bleem, L. Choi, A. Crawford, T.M. Dodelson, S. Gruen, D. Holder, G.P. Jain, B. Jarvis, M. MacCrann, N. Nicola, A. Pandey, S. Prat, J. Samuroff, S. Sánchez, C. Sheldon, E. Troxel, M.A. Zuntz, J. Abbott, T.M.C. Abdalla, F.B. Annis, J. Avila, S. Bechtol, K. Bertin, E. Brooks, D. Buckley-Geer, E. Burke, D.L. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Castander, F.J. Cawthon, R. Cunha, C.E. D'Andrea, C.B. Da Costa, L.N. Davis, C. De Vicente, J. DePoy, D.L. Diehl, H.T. Doel, P. Eifler, T.F. Estrada, J. Evrard, A.E. Flaugher, B. Fosalba, P. Frieman, J. García-Bellido, J. Gaztanaga, E. Gerdes, D.W. Gruendl, R.A. Gschwend, J. Gutierrez, G. Hartley, W.G. Hollowood, D. Hoyle, B. James, D.J. Kent, S. Kuehn, K. Kuropatkin, N. Lahav, O. Lima, M. Maia, M.A.G. March, M. Marshall, J.L. Melchior, P. Menanteau, F. Miquel, R. Plazas, A.A. Roodman, A. Rykoff, E.S. Sanchez, E. Schindler, R. Schubnell, M. Sevilla-Noarbe, I. Smith, M. Smith, R.C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M.E.C. Tarle, G. Walker, A.R. Weller, J. Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall StanfordCA94305 United States Dept. of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States Department of Physics McGill Space Institute McGill University MontrealQCH3A 2T8 Canada Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Universitäts-Sternwarte Fakultät für Physik Ludwig-Maximilians Universität München Scheinerstr. 1 München81679 Germany Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Department of Astronomy/Steward Observatory 933 North Cherry Avenue TucsonAZ85721-0065 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Dr. PasadenaCA91109 United States Center for Cosmology and Astro-Particle Physics Ohio State University ColumbusOH43210 United States Observatoire de Sauverny Versoix1290 Switzerland Department of Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Scottish Universities Physics Alliance Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Center for Cosmology and AstroParticle Physics Ohio State University 191 West Woodruff Avenue ColumbusOH43210 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Observatories of the Carnegie Institution of Washington 813 Santa Barbara St. PasadenaCA91101 United States Kavli Institute for Particle

Optical imaging surveys measure both the galaxy density and the gravitational lensing-induced shear fields across the sky. Recently, the Dark Energy Survey (DES) collaboration used a joint fit to two-point correlations between these observables to place tight constraints on cosmology (DES Collaboration et al. 2018). In this work, we develop the methodology to extend the DES year one joint probes analysis to include cross-correlations of the optical survey observables with gravitational lensing of the cosmic microwave background (CMB) as measured by the South Pole Telescope (SPT) and Planck. Using simulated analyses, we show how the resulting set of five two-point functions increases the robustness of the cosmological constraints to systematic errors in galaxy lensing shear calibration. Additionally, we show that contamination of the SPT+Planck CMB lensing map by the thermal Sunyaev-Zel'dovich effect is a potentially large source of systematic error for two-point function analyses, but show that it can be reduced to acceptable levels in our analysis by masking clusters of galaxies and imposing angular scale cuts on the two-point functions. The methodology developed here will be applied to the analysis of data from the DES, the SPT, and Planck in a companion work. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

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Instrumentation development for space debris optical observation system in Indonesia: Preliminary results

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AIP Conference Proceedings 2015年第1期1677卷

作者： Tiar Dani Abdul Rachman Rhorom Priyatikanto Bahar Religia ∗Space Science Center Indonesian National Institute of Aeronautics and Space (LAPAN) Indonesia †Astronomy Program Bandung Institute of Technology (ITB) Indonesia

An increasing number of space junk in orbit has raised their chances to fall in Indonesian region. So far, three debris of rocket bodies have been found in Bengkulu, Gorontalo and Lampung. LAPAN has successfully developed software for monitoring space debris that passes over Indonesia with an altitude below 200 km. To support the software-based system, the hardware-based system has been developed based on optical instruments. The system has been under development in early 2014 which consist of two systems: the telescopic system and wide field system. The telescopic system uses CCD cameras and a reflecting telescope with relatively high sensitivity. Wide field system uses DSLR cameras, binoculars and a combination of CCD with DSLR Lens. Methods and preliminary results of the systems will be presented.

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Cosmic-ray electron-positron spectrum from 7 GeV to 2 TeV with the Fermi Large Area Telescope

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Physical Review D 2017年第8期95卷 082007-082007页

作者： S. Abdollahi M. Ackermann M. Ajello W. B. Atwood L. Baldini G. Barbiellini D. Bastieri R. Bellazzini E. D. Bloom R. Bonino T. J. Brandt J. Bregeon P. Bruel R. Buehler R. A. Cameron R. Caputo M. Caragiulo D. Castro E. Cavazzuti C. Cecchi A. Chekhtman S. Ciprini J. Cohen-Tanugi F. Costanza A. Cuoco S. Cutini F. D’Ammando F. de Palma R. Desiante S. W. Digel N. Di Lalla M. Di Mauro L. Di Venere P. S. Drell A. Drlica-Wagner C. Favuzzi W. B. Focke S. Funk P. Fusco F. Gargano D. Gasparrini N. Giglietto F. Giordano M. Giroletti D. Green L. Guillemot S. Guiriec A. K. Harding T. Jogler G. Jóhannesson T. Kamae M. Kuss G. La Mura L. Latronico F. Longo F. Loparco P. Lubrano S. Maldera D. Malyshev A. Manfreda M. N. Mazziotta P. F. Michelson N. Mirabal W. Mitthumsiri T. Mizuno A. A. Moiseev M. E. Monzani A. Morselli I. V. Moskalenko M. Negro E. Nuss E. Orlando D. Paneque J. S. Perkins M. Pesce-Rollins F. Piron G. Pivato T. A. Porter G. Principe S. Rainò R. Rando M. Razzano A. Reimer O. Reimer C. Sgrò D. Simone E. J. Siskind F. Spada G. Spandre P. Spinelli H. Tajima J. B. Thayer L. Tibaldo D. F. Torres E. Troja M. Wood A. Worley G. Zaharijas S. Zimmer Department of Physical Sciences Hiroshima University Higashi-Hiroshima Hiroshima 739-8526 Japan Deutsches Elektronen Synchrotron DESY D-15738 Zeuthen Germany Department of Physics and Astronomy Clemson University Kinard Lab of Physics Clemson South Carolina 29634-0978 USA Santa Cruz Institute for Particle Physics Department of Physics and Department of Astronomy and Astrophysics University of California at Santa Cruz Santa Cruz California 95064 USA Università di Pisa and Istituto Nazionale di Fisica Nucleare Sezione di Pisa I-56127 Pisa Italy Istituto Nazionale di Fisica Nucleare Sezione di Trieste I-34127 Trieste Italy Dipartimento di Fisica Università di Trieste I-34127 Trieste Italy Istituto Nazionale di Fisica Nucleare Sezione di Padova I-35131 Padova Italy Dipartimento di Fisica e Astronomia “G. Galilei ” Università di Padova I-35131 Padova Italy Istituto Nazionale di Fisica Nucleare Sezione di Pisa I-56127 Pisa Italy W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics and SLAC National Accelerator Laboratory Stanford University Stanford California 94305 USA Istituto Nazionale di Fisica Nucleare Sezione di Torino I-10125 Torino Italy Dipartimento di Fisica Università degli Studi di Torino I-10125 Torino Italy NASA Goddard Space Flight Center Greenbelt Maryland 20771 USA Laboratoire Univers et Particules de Montpellier Université Montpellier CNRS/IN2P3 F-34095 Montpellier France Laboratoire Leprince-Ringuet École polytechnique CNRS/IN2P3 F-91128 Palaiseau France Dipartimento di Fisica “M. Merlin” dell’Università e del Politecnico di Bari I-70126 Bari Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari I-70126 Bari Italy Agenzia Spaziale Italiana (ASI) Science Data Center I-00133 Roma Italy Istituto Nazionale di Fisica Nucleare Sezione di Perugia I-06123 Perugia Italy Dipartimento di Fisica Università degli Studi di Perugia I-06123 Perugia Italy College of Science

We present a measurement of the cosmic-ray electron+positron spectrum between 7 GeV and 2 TeV performed with almost seven years of data collected with the Fermi Large Area Telescope. We find that the spectrum is well fit by a broken power law with a break energy at about 50 GeV. Above 50 GeV, the spectrum is well described by a single power law with a spectral index of 3.07±0.02(stat+syst)±0.04(energy measurement). An exponential cutoff lower than 1.8 TeV is excluded at 95% CL.

关键词： Cosmic ray & astroparticle detectors Cosmic ray composition & spectra Cosmic ray sources Particle astrophysics

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Baryon content in a sample of 91 galaxy clusters selected by the south pole telescope at 0.2 < z < 1.25

arXiv

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arXiv 2017年

作者： Chiu, I. Mohr, J.J. McDonald, M. Bocquet, S. Desai, S. Klein, M. Israel, H. Ashby, M.L.N. Stanford, A. Benson, B.A. Brodwin, M. Abbott, T.M.C. Abdalla, F.B. Allam, S. Annis, J. Bayliss, M. Benoit-Lévy, A. Bertin, E. Bleem, L. Brooks, D. Buckley-Geer, E. Bulbul, E. Capasso, R. Carlstrom, J.E. Carnero Rosell, A. Carretero, J. Castander, F.J. Cunha, C.E. D'Andrea, C.B. da Costa, L.N. Davis, C. Diehl, H.T. Dietrich, J.P. Doel, P. Drlica-Wagner, A. Eifler, T.F. Evrard, A.E. Flaugher, B. García-Bellido, J. Garmire, G. Gaztanaga, E. Gerdes, D.W. Gonzalez, A. Gruen, D. Gruendl, R.A. Gschwend, J. Gupta, N. Gutierrez, G. Hlavacek, J.-L. Honscheid, K. James, D.J. Jeltema, T. Kraft, R. Krause, E. Kuehn, K. Kuhlmann, S. Kuropatkin, N. Lahav, O. Lima, M. Maia, M.A.G. Marshall, J.L. Melchior, P. Menanteau, F. Miquel, R. Murray, S. Nord, B. Ogando, R.L.C. Plazas, A.A. Rapetti, D. Reichardt, C.L. Romer, A.K. Roodman, A. Sanchez, E. Saro, A. Scarpine, V. Schindler, R. Schubnell, M. Sharon, K. Smith, R.C. Smith, M. Soares-Santos, M. Sobreira, F. Stalder, B. Stern, C. Strazzullo, V. Suchyta, E. Swanson, M.E.C. Tarle, G. Vikram, V. Walker, A.R. Weller, J. Zhang, Y. 11F of AS/NTU Astronomy-Mathematics Building No.1 Sec. 4 Roosevelt Rd Taipei10617 Taiwan Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich81679 Germany Excellence Cluster Universe Boltzmannstr. 2 Garching85748 Germany Max Planck Institute for Extraterrestrial Physics Giessenbachstrasse Garching85748 Germany Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology 77 Massachusetts Avenue CambridgeMA02139 United States Argonne National Laboratory High-Energy Physics Division 9700 S. Cass Avenue ArgonneIL60439 United States Department of Physics IIT Hyderabad Kandi Telangana502285 India Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Physics Department University of California DavisCA95616 United States Fermi National Accelerator Laboratory BataviaIL60510-0500 United States Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics and Astronomy University of Missouri 5110 Rockhill Road Kansas CityMO64110 United States Cerro Tololo Inter-American Observatory National Optical Astronomy Observatory Casilla 603 La Serena Chile Department of Physics and Electronics Rhodes University PO Box 94 Grahamstown6140 South Africa Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology 77 Massachusetts Avenue CambridgeMA02139 United States Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d'Astrophysique de Paris ParisF-75014 France CNRS UMR 7095 Institut d'Astrophysique de Paris ParisF-75014 France Argonne National

We estimate total mass (M500), intracluster medium (ICM) mass (MICM) and stellar mass (M*) in a Sunyaev-Zel'dovich effect (SZE) selected sample of 91 galaxy clusters with masses M500 2.5 × 1014M☉ and redshift 0.2 2 South Pole Telescope SPT-SZ survey. The total masses M500 are estimated from the SZE observable, the ICM masses MICM are obtained from the analysis of Chandra X-ray observations, and the stellar masses M* are derived by fitting spectral energy distribution templates to Dark Energy Survey (DES) griz optical photometry and WISE or Spitzer near-infrared photometry. We study trends in the stellar mass, the ICM mass, the total baryonic mass and the cold baryonic fraction with cluster halo mass and redshift. We find significant departures from self-similarity in the mass scaling for all quantities, while the redshift trends are all statistically consistent with zero, indicating that the baryon content of clusters at fixed mass has changed remarkably little over the past ≈ 9 Gyr. We compare our results to the mean baryon fraction (and the stellar mass fraction) in the field, finding that these values lie above (below) those in cluster virial regions in all but the most massive clusters at low redshift. Using a simple model of the matter assembly of clusters from infalling groups with lower masses and from infalling material from the low density environment or field surrounding the parent halos, we show that the measured mass trends without strong redshift trends in the stellar mass scaling relation could be explained by a mass and redshift dependent fractional contribution from field material. Similar analyses of the ICM and baryon mass scaling relations provide evidence for the so-called "missing baryons" outside cluster virial regions. Copyright © 2017, The Authors. All rights reserved.

关键词： Hadrons

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Realization of Single-Qubit Positive-Operator-Valued Measurement via a One-Dimensional Photonic Quantum Walk

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Physical Review Letters 2015年第20期114卷 203602-203602页

作者： Zhihao Bian Jian Li Hao Qin Xiang Zhan Rong Zhang Barry C. Sanders Peng Xue Department of Physics Southeast University Nanjing 211189 China Hefei National Laboratory for Physical Sciences at Microscale and Department of Modern Physics University of Science and Technology of China Hefei Anhui 230026 China Shanghai Branch CAS Center for Excellence and Synergetic Innovation Center in Quantum Information and Quantum Physics University of Science and Technology of China Shanghai 201315 China Institute for Quantum Science and Technology University of Calgary Alberta T2N 1N4 Canada Program in Quantum Information Science Canadian Institute for Advanced Research Toronto Ontario M5G 1Z8 Canada State Key Laboratory of Precision Spectroscopy East China Normal University Shanghai 200062 China Beijing Institute of Mechanical and Electrical Space Beijing 100094 China

We perform generalized measurements of a qubit by realizing the qubit as a coin in a photonic quantum walk and subjecting the walker to projective measurements. Our experimental technique can be used to realize, photonically, any rank-1 single-qubit positive-operator-valued measure via constructing an appropriate interferometric quantum-walk network and then projectively measuring the walker’s position at the final step.

关键词： PHOTONS POSITIVE operators LIGHT quantization LINEAR operators QUANTUM theory

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Characterizing the population of pulsars in the inner galaxy with the fermi large area telescope

arXiv

引用

arXiv 2017年

作者： Ajello, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Blandford, R.D. Bloom, E.D. Bottacini, E. Bregeon, J. Bruel, P. Buehler, R. Cameron, R.A. Caputo, R. Caragiulo, M. Caraveo, P.A. Cavazzuti, E. Cecchi, C. Charles, E. Chekhtman, A. Chiaro, G. Ciprini, S. Costantin, D. Costanza, F. D’Ammando, F. Palma, F.D.E. Desiante, R. Digel, S.W. Lalla, N.D.I. Mauro, M.D.I. Venere, L.D.I. Favuzzi, C. Ferrara, E.C. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Green, D. Guillemot, L. Guiriec, S. Harding, A.K. Horan, D. Jóhannesson, G. Kuss, M. Mura, G.L.A. Larsson, S. Latronico, L. Li, J. Longo, F. Loparco, F. Lovellette, M.N. Lubrano, P. Maldera, S. Malyshev, D. Marcotulli, L. Martin, P. Mazziotta, M.N. Meyer, M. Michelson, P.F. Mirabal, N. Mizuno, T. Monzani, M.E. Morselli, A. Moskalenko, I.V. Nuss, E. Omodei, N. Orienti, M. Orlando, E. Palatiello, M. Paliya, V.S. Paneque, D. Perkins, J.S. Persic, M. Pesce-Rollins, M. Piron, F. Principe, G. Rainò, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Parkinson, P.M. Saz Sgrò, C. Siskind, E.J. Smith, D.A. Spada, F. Spandre, G. Spinelli, P. Tajima, H. Thayer, J.B. Thompson, D.J. Tibaldo, L. Torres, D.F. Troja, E. Vianello, G. Wood, K. Wood, M. Zaharijas, G. Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Laboratoire AIM CEA-IRFU CNRS Université Paris Diderot Service d’Astrophysique CEA Saclay Gif sur YvetteF-91191 France Istituto Nazionale di Fisica Nucleare Sezione di Trieste TriesteI-34127 Italy Dipartimento di Fisica Università di Trieste TriesteI-34127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Padova PadovaI-35131 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università di Padova PadovaI-35131 Italy Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Dipartimento di Fisica "M. Merlin" dell’Università e del Politecnico di Bari BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Laboratoire Univers et Particules de Montpellier Université Montpellier CNRS/IN2P3 MontpellierF-34095 France Laboratoire Leprince-Ringuet École polytechnique CNRS/IN2P3 PalaiseauF-91128 France Deutsches Elektronen Synchrotron DESY ZeuthenD-15738 Germany NASA Goddard Space Flight Center GreenbeltMD20771 United States INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano via E. Bassini 15 MilanoI-20133 Italy Italian Space Agency Via del Politecnico snc Roma00133 Italy Istituto Nazionale di Fisica Nucleare Sezione di Perugia PerugiaI-06123 Italy Dipartimento di Fisica Università degli Studi di Perugia PerugiaI-06123 Italy College of Science George Mason University Fairfax Naval Research DC20375 United States ASI Space Science Data Center Via del Politecnico snc Roma00133 Italy INAF Istituto di Radioastronomia BolognaI-40129 Italy Dipartimento di Ast

An excess of γ-ray emission from the Galactic Center (GC) region with respect to predictions based on a variety of interstellar emission models and γ-ray source catalogs has been found by many groups using data from the Fermi Large Area Telescope (LAT). Several interpretations of this excess have been invoked. In this paper we search for members of an unresolved population of γ-ray pulsars located in the inner Galaxy that are predicted by the interpretation of the GC excess as being due to a population of such sources. We use cataloged LAT sources to derive criteria that efficiently select pulsars with very small contamination from blazars. We search for point sources in the inner 40◦ × 40◦ region of the Galaxy, derive a list of approximately 400 sources, and apply pulsar selection criteria to extract pulsar candidates among our source list. We performed the entire data analysis chain with two different interstellar emission models (IEMs), and found a total of 135 pulsar candidates, of which 66 were selected with both IEMs. Copyright © 2017, The Authors. All rights reserved.

关键词： Pulsars

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space telescope and optical reverberation mapping project : VII. Understanding the ultraviolet anomaly in NGC 5548 with X-ray spectroscopy

arXiv

引用

arXiv 2017年

作者： Mathur, S. Gupta, A. Page, K. Pogge, R.W. Krongold, Y. Goad, M.R. Adams, S.M. Anderson, M.D. Arévalo, P. Barth, A.J. Bazhaw, C. Beatty, T.G. Bentz, M.C. Bigley, A. Bisogni, S. Borman, G.A. Boroson, T.A. Bottorff, M.C. Brandt, W.N. Breeveld, A.A. Brown, J.E. Brown, J.S. Cackett, E.M. Canalizo, G. Carini, M.T. Clubb, K.I. Comerford, J.M. Coker, C.T. Corsini, E.M. Crenshaw, D.M. Croft, S. Croxall, K.V. Dalla Bontà, E. Deason, A.J. Denney, K.D. de Lorenzo-Cáceres, A. de Rosa, G. Dietrich, M. Edelson, R. Ely, J. Eracleous, M. Evans, P.A. Fausnaugh, M.M. Ferland, G.J. Filippenko, A.V. Flatland, K. Fox, O.D. Gates, E.L. Gehrels, N. Geier, S. Gelbord, J.M. Gorjian, V. Greene, J.E. Grier, C.J. Grupe, D. Hall, P.B. Henderson, C.B. Hicks, S. Holmbeck, E. Holoien, T.W.-S. Horenstein, D. Horne, Keith Hutchison, T. Im, M. Jensen, J.J. Johnson, C.A. Joner, M.D. Jones, J. Kaastra, J. Kaspi, S. Kelly, B.C. Kelly, P.L. Kennea, J.A. Kim, M. Kim, S. Kim, S.C. King, A. Klimanov, S.A. Kochanek, C.S. Korista, K.T. Kriss, G.A. Lau, M.W. Lee, J.C. Leonard, D.C. Li, M. Lira, P. Ma, Z. MacInnis, F. Manne-Nicholas, E.R. Malkan, M.A. Mauerhan, J.C. McGurk, R. McHardy, I.M. Montouri, C. Morelli, L. Mosquera, A. Mudd, D. Muller-Sanchez, F. Musso, R. Nazarov, S.V. Netzer, H. Nguyen, M.L. Norris, R.P. Nousek, J.A. Ochner, P. Okhmat, D.N. Ou-Yang, B. Pancoast, A. Papadakis, I. Parks, J.R. Pei, L. Peterson, B.M. Pizzella, A. Poleski, R. Pott, J.-U. Rafter, S.E. Rix, H.-W. Runnoe, J. Saylor, D.A. Schimoia, J.S. Schnülle, K. Sergeev, S.G. Shappee, B.J. Shivvers, I. Siegel, M. Simonian, G.V. Siviero, A. Skielboe, A. Somers, G. Spencer, M. Starkey, D. Stevens, D.J. Sung, H.-I. Tayar, J. Tejos, N. Turner, C.S. Uttley, P. van Saders, J. Vestergaard, M. Vican, L. Villanueva, S. Villforth, C. Weiss, Y. Woo, J.-H. Yan, H. Young, S. Yuk, H. Zheng, W. Zhu, W. Zu, Y. Department of Astronomy Ohio State University 140 W 18th Ave ColumbusOH43210 United States Center for Cosmology and AstroParticle Physics Ohio State University 191 West Woodruff Ave ColumbusOH43210 United States Department of Biological and Physical Sciences Columbus State Community College ColumbusOH43215 United States Department of Physics and Astronomy University of Leicester LeicesterLE1 7RH United Kingdom Instituto de Astronomia Universidad Nacional Autonoma de Mexico Cuidad de Mexico Mexico Cahill Center for Astrophysics California Institute of Technology PasadenaCA91125 United States Department of Physics and Astronomy Georgia State University 25 Park Place Suite 605 AtlantaGA30303 United States Instituto de Física y Astronomía Facultad de Ciencias Universidad de Valparaíso Gran Bretana N 1111 Playa Ancha Valparaíso Chile Department of Physics and Astronomy 4129 Frederick Reines Hall University of California IrvineCA92697 United States Department of Astronomy and Astrophysics Eberly College of Science Pennsylvania State University 525 Davey Laboratory University ParkPA16802 United States Center for Exoplanets and Habitable Worlds Pennsylvania State University University ParkPA16802 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Osservatorio Astrofisico di Arcetri largo E. Fermi 5 Firenze50125 Italy Crimean Astrophysical Observatory P/O Nauchny Crimea298409 Russia Las Cumbres Observatory Global Telescope Network 6740 Cortona Drive Suite 102 GoletaCA93117 United States Fountainwood Observatory Department of Physics FJS 149 Southwestern University 1011 E. University Ave. GeorgetownTX78626 United States Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Department of Physics 104 Davey Laboratory Pennsylvania State University University ParkPA16802 United States Mullard Space Science Laboratory University Col

During the space Telescope and Optical Reverberation Mapping Project (STORM) observations of NGC 5548, the continuum and emission-line variability became decor-related during the second half of the 6-month-long observing campaign. Here we present Swift and Chandra X-ray spectra of NGC 5548 obtained as a part of the campaign. The Swift spectra show that excess flux (relative to a power-law continuum) in the soft X-ray band appears before the start of the anomalous emission-line behavior, peaks during the period of the anomaly, and then declines. This is a model-independent result suggesting that the soft excess is related to the anomaly. We divide the Swift data into on- and off-anomaly spectra to characterize the soft excess via spectral fitting. The cause of the spectral differences is likely due to a change in the intrinsic spectrum rather than to variable obscuration or partial covering. The Chandra spectra have lower signal-to-noise ratios, but are consistent with the Swift data. Our preferred model of the soft excess is emission from an optically thick, warm Comptonizing corona, the effective optical depth of which increases during the anomaly. This model simultaneously explains all three observations: the UV emission-line flux decrease, the soft-excess increase, and the emission-line anomaly. Copyright © 2017, The Authors. All rights reserved.

关键词： Galaxies

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A Measurement of CMB Cluster Lensing with SPT and DES Year 1 Data

arXiv

引用

arXiv 2017年

作者： Baxter, E.J. Raghunathan, S. Crawford, T.M. Fosalba, P. Hou, Z. Holder, G.P. Omori, Y. Patil, S. Rozo, E. Abbott, T.M.C. Annis, J. Aylor, K. Benoit-Lévy, A. Benson, B.A. Bertin, E. Bleem, L. Buckley-Geer, E. Burke, D.L. Carlstrom, J. Carnero Rosell, A. Carrasco Kind, M. Walker, A.R. Williamson, R. Zhang, Y. Zuntz, J. Carretero, J. Chang, C.L. Cho, H.-M. Crites, A.T. Crocce, M. Cunha, C.E. da Costa, L.N. Marrone, D.P. Marshall, J.L. Martini, P. McMahon, J.J. Melchior, P. Menanteau, F. Meyer, S.S. Miller, C.J. Miquel, R. Mocanu, L.M. Mohr, J.J. Natoli, T. Nord, B. Ogando, R.L.C. Sevilla-Noarbe, I. Shirokoff, E. Smith, M. Smith, R.C. Soares-Santos, M. Sobreira, F. Staniszewski, Z. D’Andrea, C.B. Davis, C. de Haan, T. Desai, S. Dietrich, J.P. Dobbs, M.A. Dodelson, S. Doel, P. Drlica-Wagner, A. Estrada, J. Everett, W.B. Fausti Neto, A. Flaugher, B. Frieman, J. García-Bellido, J. George, E.M. Gaztanaga, E. Giannantonio, T. Gruen, D. Gruendl, R.A. Gschwend, J. Gutierrez, G. Halverson, N.W. Harrington, N.L. Hartley, W.G. Holzapfel, W.L. Honscheid, K. Hrubes, J.D. Jain, B. James, D.J. Jarvis, M. Jeltema, T. Knox, L. Krause, E. Kuehn, K. Kuhlmann, S. Kuropatkin, N. Lahav, O. Lee, A.T. Leitch, E.M. Li, T.S. Lima, M. Luong-Van, D. Manzotti, A. March, M. Padin, S. Plazas, A.A. Pryke, C. Rapetti, D. Reichardt, C.L. Romer, A.K. Roodman, A. Ruhl, J.E. Rykoff, E. Sako, M. Sanchez, E. Sayre, J.T. Scarpine, V. Schaffer, K.K. Schindler, R. Schubnell, M. Stark, A. Story, K. Suchyta, E. Tarle, G. Thomas, D. Troxel, M.A. Vanderlinde, K. Vieira, J.D. Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States School of Physics University of Melbourne ParkvilleVIC3010 Australia Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Institute of Space Sciences IEEC-CSIC Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Canadian Institute for Advanced Research CIFAR Program on Gravity and the Extreme Universe TorontoONM5G 1Z8 Canada Astronomy Department University of Illinois at Urbana Champaign 1002 W. Green Street UrbanaIL61801 United States Department of Physics University of Illinois Urbana Champaign 1110 W. Green Street UrbanaIL61801 United States Department of Physics McGill University 3600 rue University MontrealQCH3A 2T8 Canada Department of Physics University of Arizona TucsonAZ85721 United States Cerro Tololo Inter-American Observatory National Optical Astronomy Observatory Casilla 603 La Serena Chile Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Department of Physics University of California DavisCA95616 United States CNRS UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Department of Physics & Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Department of Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Enrico Fermi Institute University of Chicago ChicagoIL60637 United States Laboratório Interi

Clusters of galaxies gravitationally lens the cosmic microwave background (CMB) radiation, resulting in a distinct imprint in the CMB on arcminute scales. Measurement of this effect offers a promising way to constrain the masses of galaxy clusters, particularly those at high redshift. We use CMB maps from the South Pole Telescope Sunyaev-Zel’dovich (SZ) survey to measure the CMB lensing signal around galaxy clusters identified in optical imaging from first year observations of the Dark Energy Survey. The cluster catalog used in this analysis contains 3697 members with mean redshift of z¯ = 0.45. We detect lensing of the CMB by the galaxy clusters at 8.1σ significance. Using the measured lensing signal, we constrain the amplitude of the relation between cluster mass and optical richness to roughly 17% precision, finding good agreement with recent constraints obtained with galaxy lensing. The error budget is dominated by statistical noise but includes significant contributions from systematic biases due to the thermal SZ effect and cluster miscentering. Copyright © 2017, The Authors. All rights reserved.

关键词： Cosmology

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3FHL: The Third Catalog of Hard Fermi-LAT Sources

arXiv

引用

arXiv 2017年

作者： Ajello, M. Atwood, W.B. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Blandford, R.D. Bloom, E.D. Bonino, R. Bregeon, J. Britto, R.J. Bruel, P. Buehler, R. Buson, S. Cameron, R.A. Caputo, R. Caragiulo, M. Caraveo, P.A. Cavazzuti, E. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C.C. Chiaro, G. Ciprini, S. Cohen, J.M. Costantin, D. Costanza, F. Cuoco, A. Cutini, S. D’Ammando, F. de Palma, F. Desiante, R. Digel, S.W. Di Lalla, N. Di Mauro, M. Di Venere, L. Domínguez, A. Drell, P.S. Dumora, D. Favuzzi, C. Fegan, S.J. Ferrara, E.C. Fortin, P. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Green, D. Grenier, I.A. Grondin, M.-H. Grove, J.E. Guillemot, L. Guiriec, S. Harding, A.K. Hays, E. Hewitt, J.W. Horan, D. Jóhannesson, G. Kensei, S. Kuss, M. la Mura, G. Larsson, S. Latronico, L. Lemoine-Goumard, M. Li, J. Longo, F. Loparco, F. Lott, B. Lubrano, P. Magill, J.D. Maldera, S. Manfreda, A. Mazziotta, M.N. McEnery, J.E. Meyer, M. Michelson, P.F. Mirabal, N. Mitthumsiri, W. Mizuno, T. Moiseev, A.A. Monzani, M.E. Morselli, A. Moskalenko, I.V. Negro, M. Nuss, E. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Palatiello, M. Paliya, V.S. Paneque, D. Perkins, J.S. Persic, M. Pesce-Rollins, M. Piron, F. Porter, T.A. Principe, G. Rainò, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reposeur, T. Saz Parkinson, P.M. Sgrò, C. Simone, D. Siskind, E.J. Spada, F. Spandre, G. Spinelli, P. Stawarz, L. Suson, D.J. Takahashi, M. Tak, D. Thayer, J.G. Thayer, J.B. Thompson, D.J. Torres, D.F. Torresi, E. Troja, E. Vianello, G. Wood, K. Wood, M. Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States Santa Cruz Institute for Particle Physics Department of Physics Department of Astronomy and Astrophysics University of California at Santa Cruz Santa CruzCA95064 United States Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Laboratoire AIM CEA-IRFU CNRS Université Paris Diderot Service d’Astrophysique CEA Saclay Gif sur YvetteF-91191 France Istituto Nazionale di Fisica Nucleare Sezione di Trieste TriesteI-34127 Italy Dipartimento di Fisica Università di Trieste TriesteI-34127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Padova PadovaI-35131 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università di Padova PadovaI-35131 Italy Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Dipartimento di Fisica "M. Merlin" dell’Università e del Politecnico di Bari BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy Laboratoire Univers et Particules de Montpellier Université Montpellier CNRS/IN2P3 MontpellierF-34095 France Department of Physics University of the Free State P.O. Box 339 Bloemfontein9300 South Africa Laboratoire Leprince-Ringuet École polytechnique CNRS/IN2P3 PalaiseauF-91128 France Deutsches Elektronen Synchrotron DESY ZeuthenD-15738 Germany NASA Goddard Space Flight Center GreenbeltMD20771 United States NASA Postdoctoral Program Fellow United States NASA Goddard Space Flight Center GreenbeltMD20771 United States INAF-Istituto di As

We present a catalog of sources detected above 10 GeV by the Fermi Large Area Telescope (LAT) in the first 7 years of data using the Pass 8 event-level analysis. This is the Third Catalog of Hard Fermi-LAT Sources (3FHL), containing 1556 objects characterized in the 10 GeV–2 TeV energy range. The sensitivity and angular resolution are improved by factors of 3 and 2 relative to the previous LAT catalog at the same energies (1FHL). The vast majority of detected sources (79%) are associated with extragalactic counterparts at other wavelengths, including 16 sources located at very high redshift (z > 2). Eight percent of the sources have Galactic counterparts and 13% are unassociated (or associated with a source of unknown nature). The high-latitude sky and the Galactic plane are observed with a flux sensitivity of 4.4 to 9.5 ×10−11 ph cm−2 s−1, respectively (this is approximately 0.5 % and 1 % of the Crab Nebula flux above 10 GeV). The catalog includes 214 new γ-ray sources. The substantial increase in the number of photons (more than 4 times relative to 1FHL and 10 times to 2FHL) also allows us to measure significant spectral curvature for 32 sources and find flux variability for 163 of them. Furthermore, we estimate that for the same flux limit of 10−12 erg cm−2 s−1, the energy range above 10 GeV has twice as many sources as above 50 GeV, highlighting the importance, for future Cherenkov telescopes, of lowering the energy threshold as much as possible. Copyright © 2017, The Authors. All rights reserved.

关键词： Gamma rays

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