The Third Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope M
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Arxiv:1705.04776V1 [Astro-Ph.HE] 13 May 2017 Aaua M
White Paper on East Asian Vision for mm/submm VLBI: Toward Black Hole Astrophysics down to Angular Resolution of 1 RS Editors Asada, K.1, Kino, M.2,3, Honma, M.3, Hirota, T.3, Lu, R.-S.4,5, Inoue, M.1, Sohn, B.-W.2,6, Shen, Z.-Q.4, and Ho, P. T. P.1,7 Authors Akiyama, K.3,8, Algaba, J-C.2, An, T.4, Bower, G.1, Byun, D-Y.2, Dodson, R.9, Doi, A.10, Edwards, P.G.11, Fujisawa, K.12, Gu, M-F.4, Hada, K.3, Hagiwara, Y.13, Jaroenjittichai, P.15, Jung, T.2,6, Kawashima, T.3, Koyama, S.1,5, Lee, S-S.2, Matsushita, S.1, Nagai, H.3, Nakamura, M.1, Niinuma, K.12, Phillips, C.11, Park, J-H.15, Pu, H-Y.1, Ro, H-W.2,6, Stevens, J.11, Trippe, S.15, Wajima, K.2, Zhao, G-Y.2 1 Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan 2 Korea Astronomy and Space Science Institute, Daedukudae-ro 776, Yuseong-gu, Daejeon 34055, Republic of Korea 3 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan 4 Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China 5 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, D-53121 Bonn, Germany 6 University of Science and Technology, 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of Korea 7 East Asian Observatory, 660 N. -
Fermi Large Area Telescope Second Source Catalog the Fermi LAT Collaboration
Revision: 3455: Last update: 2011-07-09 23:47:14 - 0700 Fermi Large Area Telescope Second Source Catalog The Fermi LAT Collaboration ABSTRACT This is a pre-submission draft of the paper provided to document the public release of the 2FGL catalog through the FSSC. The draft will be replaced soon by the version that is submitted to ApJS and posted on the arXiv. We present the second catalog of high-energy γ-ray sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi),derivedfromdatatakenduringthefirst 24 months of the science phase of the mission, which began on 2008 August 4. Source detection is based on the average flux over the 24-monthperiod.The Second Fermi-LAT catalog (2FGL) includes source location regions, defined in terms of elliptical fits to the 95% confidence regions and spectral fits in terms of power-law, power-law-with-exponential-cutoff, or log-normal forms. Also in- cluded are flux measurements in 5 energy bands for each source and monthly light curves. Twelve sources in the catalog are modeled as spatially extended. We provide a detailed comparison of the results from this catalog with those from the first Fermi-LAT catalog (1FGL). Although the diffuse Galactic and isotropic models used in the 2FGL analysis are improved compared to the 1FGL catalog, we attach caution flags to 162 of the sources to indicate possible confusion with residual imperfections in the diffuse model. The 2FGL catalogcontains1873 sources detected and characterized in the 100 MeV to 100 GeV range of which we consider 127 as being firmly identified and 1174 as being reliably associated with counterparts of known or likely γ-ray-producing source classes. -
The B3-VLA CSS Sample⋆
A&A 528, A110 (2011) Astronomy DOI: 10.1051/0004-6361/201015379 & c ESO 2011 Astrophysics The B3-VLA CSS sample VIII. New optical identifications from the Sloan Digital Sky Survey The ultraviolet-optical spectral energy distribution of the young radio sources C. Fanti1,R.Fanti1, A. Zanichelli1, D. Dallacasa1,2, and C. Stanghellini1 1 Istituto di Radioastronomia – INAF, via Gobetti 101, 40129 Bologna, Italy e-mail: [email protected] 2 Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy Received 12 July 2010 / Accepted 22 December 2010 ABSTRACT Context. Compact steep-spectrum radio sources and giga-hertz peaked spectrum radio sources (CSS/GPS) are generally considered to be mostly young radio sources. In recent years we studied at many wavelengths a sample of these objects selected from the B3-VLA catalog: the B3-VLA CSS sample. Only ≈60% of the sources were optically identified. Aims. We aim to increase the number of optical identifications and study the properties of the host galaxies of young radio sources. Methods. We cross-correlated the CSS B3-VLA sample with the Sloan Digital Sky Survey (SDSS), DR7, and complemented the SDSS photometry with available GALEX (DR 4/5 and 6) and near-IR data from UKIRT and 2MASS. Results. We obtained new identifications and photometric redshifts for eight faint galaxies and for one quasar and two quasar candi- dates. Overall we have 27 galaxies with SDSS photometry in five bands, for which we derived the ultraviolet-optical spectral energy distribution (UV-O-SED). We extended our investigation to additional CSS/GPS selected from the literature. -
Counting Gamma Rays in the Directions of Galaxy Clusters
A&A 567, A93 (2014) Astronomy DOI: 10.1051/0004-6361/201322454 & c ESO 2014 Astrophysics Counting gamma rays in the directions of galaxy clusters D. A. Prokhorov1 and E. M. Churazov1,2 1 Max Planck Institute for Astrophysics, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany e-mail: [email protected] 2 Space Research Institute (IKI), Profsouznaya 84/32, 117997 Moscow, Russia Received 6 August 2013 / Accepted 19 May 2014 ABSTRACT Emission from active galactic nuclei (AGNs) and from neutral pion decay are the two most natural mechanisms that could establish a galaxy cluster as a source of gamma rays in the GeV regime. We revisit this problem by using 52.5 months of Fermi-LAT data above 10 GeV and stacking 55 clusters from the HIFLUCGS sample of the X-ray brightest clusters. The choice of >10 GeV photons is optimal from the point of view of angular resolution, while the sample selection optimizes the chances of detecting signatures of neutral pion decay, arising from hadronic interactions of relativistic protons with an intracluster medium, which scale with the X-ray flux. In the stacked data we detected a signal for the central 0.25 deg circle at the level of 4.3σ. Evidence for a spatial extent of the signal is marginal. A subsample of cool-core clusters has a higher count rate of 1.9 ± 0.3 per cluster compared to the subsample of non-cool core clusters at 1.3 ± 0.2. Several independent arguments suggest that the contribution of AGNs to the observed signal is substantial, if not dominant. -
Cfa in the News ~ Week Ending 3 January 2010
Wolbach Library: CfA in the News ~ Week ending 3 January 2010 1. New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 2. 2009 in science and medicine, ROGER SCHLUETER, Belleville News Democrat (IL), Sunday, January 3, 2010 3. 'Science, celestial bodies have always inspired humankind', Staff Correspondent, Hindu (India), Tuesday, December 29, 2009 4. Why is Carpenter defending scientists?, The Morning Call, Morning Call (Allentown, PA), FIRST ed, pA25, Sunday, December 27, 2009 5. CORRECTIONS, OPINION BY RYAN FINLEY, ARIZONA DAILY STAR, Arizona Daily Star (AZ), FINAL ed, pA2, Saturday, December 19, 2009 6. We see a 'Super-Earth', TOM BEAL; TOM BEAL, ARIZONA DAILY STAR, Arizona Daily Star, (AZ), FINAL ed, pA1, Thursday, December 17, 2009 Record - 1 DIALOG(R) New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 TEXT: "In this paper we report on testing the 'rolen model' and 'opportunity-structure' hypotheses about the parents whom scientists mentioned as career influencers. According to the role-model hypothesis, the gender match between scientist and influencer is paramount (for example, women scientists would disproportionately often mention their mothers as career influencers)," scientists writing in the journal Social Studies of Science report (see also ). "According to the opportunity-structure hypothesis, the parent's educational level predicts his/her probability of being mentioned as a career influencer (that ism parents with higher educational levels would be more likely to be named). The examination of a sample of American scientists who had received prestigious postdoctoral fellowships resulted in rejecting the role-model hypothesis and corroborating the opportunity-structure hypothesis. -
Second AGILE Catalogue of Gamma-Ray Sources?
A&A 627, A13 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834143 & c ESO 2019 Astrophysics Second AGILE catalogue of gamma-ray sources? A. Bulgarelli1, V. Fioretti1, N. Parmiggiani1, F. Verrecchia2,3, C. Pittori2,3, F. Lucarelli2,3, M. Tavani4,5,6,7 , A. Aboudan7,12, M. Cardillo4, A. Giuliani8, P. W. Cattaneo9, A. W. Chen15, G. Piano4, A. Rappoldi9, L. Baroncelli7, A. Argan4, L. A. Antonelli3, I. Donnarumma4,16, F. Gianotti1, P. Giommi16, M. Giusti4,5, F. Longo13,14, A. Pellizzoni10, M. Pilia10, M. Trifoglio1, A. Trois10, S. Vercellone11, and A. Zoli1 1 INAF-OAS Bologna, Via Gobetti 93/3, 40129 Bologna, Italy e-mail: [email protected] 2 ASI Space Science Data Center (SSDC), Via del Politecnico snc, 00133 Roma, Italy 3 INAF-Osservatorio Astronomico di Roma, Via di Frascati 33, 00078 Monte Porzio Catone, Italy 4 INAF-IAPS Roma, Via del Fosso del Cavaliere 100, 00133 Roma, Italy 5 Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy 6 INFN Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy 7 Consorzio Interuniversitario Fisica Spaziale (CIFS), Villa Gualino - v.le Settimio Severo 63, 10133 Torino, Italy 8 INAF–IASF Milano, Via E. Bassini 15, 20133 Milano, Italy 9 INFN Pavia, Via Bassi 6, 27100 Pavia, Italy 10 INAF–Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Selargius, CA, Italy 11 INAF–Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate, LC, Italy 12 CISAS, University of Padova, Padova, Italy 13 Dipartimento di Fisica, University of Trieste, Via Valerio 2, 34127 Trieste, Italy 14 INFN, sezione di Trieste, Via Valerio 2, 34127 Trieste, Italy 15 School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein stateJohannesburg 2050, South Africa 16 ASI, Via del Politecnico snc, 00133 Roma, Italy Received 27 August 2018 / Accepted 12 March 2019 ABSTRACT Aims. -
An Optical Spectroscopic Survey of the 3CR
A&A 560, A81 (2013) Astronomy DOI: 10.1051/0004-6361/201322842 & c ESO 2013 Astrophysics An optical spectroscopic survey of the 3CR sample of radio galaxies with z < 0.3 V. Implications for the unified model for FR IIs Ranieri D. Baldi1, Alessandro Capetti2, Sara Buttiglione3, Marco Chiaberge4,5,6, and Annalisa Celotti1,7,8 1 SISSA-ISAS, via Bonomea 265, 34136 Trieste, Italy e-mail: [email protected] 2 INAF − Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Italy 3 INAF − Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 5 INAF − Istituto di Radio Astronomia, via P. Gobetti 101, 40129 Bologna, Italy 6 Center for Astrophysical Sciences, Johns Hopkins University, 3400 N. Charles Street Baltimore, MD 21218, USA 7 INAF − Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate, Italy 8 INFN − Sezione di Trieste, via Valerio 2, 34127 Trieste, Italy Received 14 October 2013 / Accepted 30 October 2013 ABSTRACT We explore the implications of our optical spectroscopic survey of 3CR radio sources with z < 0.3 for the unified model (UM) for radio-loud AGN, focusing on objects with a “edge-brightened” (FR II) radio morphology. The sample contains 33 high ionization galaxies (HIGs) and 18 broad line objects (BLOs). According to the UM, HIGs, the narrow line sources, are the nuclearly obscured counterparts of BLOs. The fraction of HIGs indicates a covering factor of the circumnuclear matter of 65% that corresponds, adopting a torus geometry, to an opening angle of 50◦ ± 5. -
Revealing Hidden Substructures in the $ M {BH} $-$\Sigma $ Diagram
Draft version November 14, 2019 A Typeset using L TEX twocolumn style in AASTeX63 Revealing Hidden Substructures in the MBH –σ Diagram, and Refining the Bend in the L–σ Relation Nandini Sahu,1,2 Alister W. Graham2 And Benjamin L. Davis2 — 1OzGrav-Swinburne, Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia 2Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia (Accepted 2019 October 22, by The Astrophysical Journal) ABSTRACT Using 145 early- and late-type galaxies (ETGs and LTGs) with directly-measured super-massive black hole masses, MBH , we build upon our previous discoveries that: (i) LTGs, most of which have been 2.16±0.32 alleged to contain a pseudobulge, follow the relation MBH ∝ M∗,sph ; and (ii) the ETG relation 1.27±0.07 1.9±0.2 MBH ∝ M∗,sph is an artifact of ETGs with/without disks following parallel MBH ∝ M∗,sph relations which are offset by an order of magnitude in the MBH -direction. Here, we searched for substructure in the MBH –(central velocity dispersion, σ) diagram using our recently published, multi- component, galaxy decompositions; investigating divisions based on the presence of a depleted stellar core (major dry-merger), a disk (minor wet/dry-merger, gas accretion), or a bar (evolved unstable 5.75±0.34 disk). The S´ersic and core-S´ersic galaxies define two distinct relations: MBH ∝ σ and MBH ∝ 8.64±1.10 σ , with ∆rms|BH = 0.55 and 0.46 dex, respectively. We also report on the consistency with the slopes and bends in the galaxy luminosity (L)–σ relation due to S´ersic and core-S´ersic ETGs, and LTGs which all have S´ersic light-profiles. -
NASA Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, Maryland 20771
1 NASA Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, Maryland 20771 This report covers the period from July 1, 2002 to June Stephen Henderson, Hans Krimm, John Krizmanic, Jeongin 30, 2003. Lee, John Lehan, James Lochner, Thomas McGlynn, Paul This Laboratory’s scientific research is directed toward McNamara, Alex Moiseev, Koji Mukai, James Reeves, Na- experimental and theoretical investigations in the areas of dine Saudraix, Chris Shrader, Steven Snowden, Yang Soong, X-ray, gamma-ray, gravitational wave and cosmic-ray astro- Martin Still, Steve Sturner, and Vigdor Teplitz. physics. The range of interests of the scientists includes the The following investigators are University of Maryland Sun and the solar system, stellar objects, binary systems, Scientists: Drs. Keith Arnaud, David Band ͑UMBC͒, Simon neutron stars, black holes, the interstellar medium, normal Bandler, Patricia Boyd ͑UMBC͒, John Cannizzo ͑UMBC͒, and active galaxies, galaxy clusters, cosmic ray particles, David Davis ͑UMBC͒, Ian George ͑UMBC͒, Masaharu gravitational wave astrophysics, extragalactic background ra- Hirayama ͑UMBC͒, Una Hwang, Yasushi Ikebe ͑UMBC͒, diation, and cosmology. Scientists and engineers in the Kip Kuntz ͑UMBC͒, Mark Lindeman, Michael Loewenstein, Laboratory also serve the scientific community, including Craig Markwardt, Julie McEnery ͑UMBC͒, Igor Moskalenko project support such as acting as project scientists and pro- ͑UMBC͒, Chee Ng, Patrick Palmeri, Dirk Petry ͑UMBC͒, viding technical assistance for various space missions. Also Christopher Reynolds, Ian Richardson, and Jane Turner at any one time, there are typically between ten and fifteen ͑UMBC͒. graduate students involved in Ph.D. research work in this Visiting scientists from other institutions: Drs. Hilary Laboratory. -
00E the Construction of the Universe Symphony
The basic construction of the Universe Symphony. There are 30 asterisms (Suites) in the Universe Symphony. I divided the asterisms into 15 groups. The asterisms in the same group, lay close to each other. Asterisms!! in Constellation!Stars!Objects nearby 01 The W!!!Cassiopeia!!Segin !!!!!!!Ruchbah !!!!!!!Marj !!!!!!!Schedar !!!!!!!Caph !!!!!!!!!Sailboat Cluster !!!!!!!!!Gamma Cassiopeia Nebula !!!!!!!!!NGC 129 !!!!!!!!!M 103 !!!!!!!!!NGC 637 !!!!!!!!!NGC 654 !!!!!!!!!NGC 659 !!!!!!!!!PacMan Nebula !!!!!!!!!Owl Cluster !!!!!!!!!NGC 663 Asterisms!! in Constellation!Stars!!Objects nearby 02 Northern Fly!!Aries!!!41 Arietis !!!!!!!39 Arietis!!! !!!!!!!35 Arietis !!!!!!!!!!NGC 1056 02 Whale’s Head!!Cetus!! ! Menkar !!!!!!!Lambda Ceti! !!!!!!!Mu Ceti !!!!!!!Xi2 Ceti !!!!!!!Kaffalijidhma !!!!!!!!!!IC 302 !!!!!!!!!!NGC 990 !!!!!!!!!!NGC 1024 !!!!!!!!!!NGC 1026 !!!!!!!!!!NGC 1070 !!!!!!!!!!NGC 1085 !!!!!!!!!!NGC 1107 !!!!!!!!!!NGC 1137 !!!!!!!!!!NGC 1143 !!!!!!!!!!NGC 1144 !!!!!!!!!!NGC 1153 Asterisms!! in Constellation Stars!!Objects nearby 03 Hyades!!!Taurus! Aldebaran !!!!!! Theta 2 Tauri !!!!!! Gamma Tauri !!!!!! Delta 1 Tauri !!!!!! Epsilon Tauri !!!!!!!!!Struve’s Lost Nebula !!!!!!!!!Hind’s Variable Nebula !!!!!!!!!IC 374 03 Kids!!!Auriga! Almaaz !!!!!! Hoedus II !!!!!! Hoedus I !!!!!!!!!The Kite Cluster !!!!!!!!!IC 397 03 Pleiades!! ! Taurus! Pleione (Seven Sisters)!! ! ! Atlas !!!!!! Alcyone !!!!!! Merope !!!!!! Electra !!!!!! Celaeno !!!!!! Taygeta !!!!!! Asterope !!!!!! Maia !!!!!!!!!Maia Nebula !!!!!!!!!Merope Nebula !!!!!!!!!Merope -
FY13 High-Level Deliverables
National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2013 (1 October 2012 – 30 September 2013) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 13 December 2013 Revised 18 September 2014 Contents NOAO MISSION PROFILE .................................................................................................... 1 1 EXECUTIVE SUMMARY ................................................................................................ 2 2 NOAO ACCOMPLISHMENTS ....................................................................................... 4 2.1 Achievements ..................................................................................................... 4 2.2 Status of Vision and Goals ................................................................................. 5 2.2.1 Status of FY13 High-Level Deliverables ............................................ 5 2.2.2 FY13 Planned vs. Actual Spending and Revenues .............................. 8 2.3 Challenges and Their Impacts ............................................................................ 9 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 11 3.1 Cerro Tololo Inter-American Observatory ....................................................... 11 3.2 Kitt Peak National Observatory ....................................................................... 14 3.3 Gemini Observatory ........................................................................................ -
IAU Symp 269, POST MEETING REPORTS
IAU Symp 269, POST MEETING REPORTS C.Barbieri, University of Padua, Italy Content (i) a copy of the final scientific program, listing invited review speakers and session chairs; (ii) a list of participants, including their distribution on gender (iii) a list of recipients of IAU grants, stating amount, country, and gender; (iv) receipts signed by the recipients of IAU Grants (done); (v) a report to the IAU EC summarizing the scientific highlights of the meeting (1-2 pages). (vi) a form for "Women in Astronomy" statistics. (i) Final program Conference: Galileo's Medicean Moons: their Impact on 400 years of Discovery (IAU Symposium 269) Padova, Jan 6-9, 201 Program Wednesday 6, location: Centro San Gaetano, via Altinate 16.0 0 – 18.00 meeting of Scientific Committee (last details on the Symp 269; information on the IYA closing ceremony program) 18.00 – 20.00 welcome reception Thursday 7, morning: Aula Magna University 8:30 – late registrations 09.00 – 09.30 Welcome Addresses (Rector of University, President of COSPAR, Representative of ESA, President of IAU, Mayor of Padova, Barbieri) Session 1, The discovery of the Medicean Moons, the history, the influence on human sciences Chair: R. Williams Speaker Title 09.30 – 09.55 (1) G. Coyne Galileo's telescopic observations: the marvel and meaning of discovery 09.55 – 10.20 (2) D. Sobel Popular Perceptions of Galileo 10.20 – 10.45 (3) T. Owen The slow growth of human humility (read by Scott Bolton) 10.45 – 11.10 (4) G. Peruzzi A new Physics to support the Copernican system. Gleanings from Galileo's works 11.10 – 11.35 Coffee break Session 1b Chair: T.