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18 results on '"UNIFIED SCHEMES"'

1. MAGIC observations of the giant radio galaxy M 87 in a low-emission state between 2005 and 2007

Author

Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Nieto, Daniel, Satalecka, Konstanzja, Scapin, Valeria, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, López Moya, Marcos, Miranda Pantoja, José Miguel, Nieto, Daniel, Satalecka, Konstanzja, and Scapin, Valeria

Abstract

© ESO 2012. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESSMAGIC/2010/0., Context. We present the results of a long M 87 monitoring campaign in very high energy.-rays with the MAGIC-I Cherenkov telescope. Aims. We aim to model the persistent non-thermal jet emission by monitoring and characterizing the very high energy gamma-ray emission of M 87 during a low state. Methods. A total of 150 h of data were taken between 2005 and 2007 with the single MAGIC-I telescope, out of which 128.6 h survived the data quality selection. We also collected data in the X-ray and Fermi-LAT bands from the literature (partially contemporaneous). Results. No flaring activity was found during the campaign. The source was found to be in a persistent low-emission state, which was at a confidence level of 7 sigma. We present the spectrum between 100 GeV and 2 TeV, which is consistent with a simple power law with a photon index Gamma = 2.21 +/- 0.21 and a flux normalization at 300GeV of (7.7 +/- 1.3) x 10(-8) TeV-1 s(-1) m(-2). The extrapolation of the MAGIC spectrum into the GeV energy range matches the previously published Fermi-LAT spectrum well, covering a combined energy range of four orders of magnitude with the same spectral index. We model the broad band energy spectrum with a spine layer model, which can satisfactorily describe our data., German BMBF, German MPG, Italian INFN, Swiss National Fund SNF, Spanish MICINN, Spanish Consolider-Ingenio 2010 programme, Bulgarian NSF, Academy of Finland, DFG Cluster of Excellence “Origin and Structure of the Universe”, DFG Collaborative Research Centers, Polish MNiSzW, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

2. The 2010 very high energy gamma-ray flare and 10 years of multi-wavelength observations of M 87

Author

Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, and Miranda Pantoja, José Miguel

Abstract

© The American Astronomical Society. The H.E.S.S. Collaboration acknowledges support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S., as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment.The MAGIC Collaboration thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the Marie Curie program, by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the YIP of the Helmholtz Gemeinschaft, by the DFG Cluster of Excellence "Origin and Structure of the Universe," by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.The VERITAS Collaboration acknowledges support from the US Department of Energy Office of Science, the US National Science Foundation, and the Smithsonian Institution, from NSERC in Canada, from Science Foundation Ireland (SFI 10/RFP/AST2748), and from STFC in the UK. We acknowledge the excellent work of the technical, The giant radio galaxy M 87 with its proximity (16 Mpc), famous jet, and very massive black hole ((3-6) x 10(9) M-circle dot) provides a unique opportunity to investigate the origin of very high energy (VHE; E > 100 GeV) gamma-ray emission generated in relativistic outflows and the surroundings of supermassive black holes. M 87 has been established as a VHE gamma-ray emitter since 2006. The VHE gamma-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M 87 by the MAGIC and VERITAS instruments in 2010 are reported. During the campaign, a flare at VHE was detected triggering further observations at VHE (H.E.S.S.), X-rays (Chandra), and radio (43 GHz Very Long Baseline Array, VLBA). The excellent sampling of the VHE gamma-ray light curve enables one to derive a precise temporal characterization of the flare: the single, isolated flare is well described by a two-sided exponential function with significantly different flux rise and decay times of tau(rise)(d) = (1.69 +/- 0.30) days and tau(decay)(d) = (0.611 +/- 0.080) days, respectively. While the overall variability pattern of the 2010 flare appears somewhat different from that of previous VHE flares in 2005 and 2008, they share very similar timescales (similar to day), peak fluxes (Phi(>0.35 TeV) similar or equal to (1-3) x 10(-11) photons cm(-2) s(-1)), and VHE spectra. VLBA radio observations of 43 GHz of the inner jet regions indicate no enhanced flux in 2010 in contrast to observations in 2008, where an increase of the radio flux of the innermost core regions coincided with a VHE flare. On the other hand, Chandra X-ray observations taken similar to 3 days after the peak of the VHE gamma-ray emission reveal an enhanced flux from the core (flux increased by factor similar to 2; variability timescale <2 days). The long-term (2001-2010) multi-wavelength (MWL) light curve of M 87, spanning from radio to VHE and including data from Hubb, Facilities Council (STFC), IPNP of the Charles University, Polish Ministry of Science and Higher Education, South African Department of Science and Technology, National Research Foundation, University of Namibia, German BMBF, German MPG, Italian INFN, Swiss National Fund SNF, Spanish MICINN, Bulgarian NSF, Academy of Finland, YIP of the Helmholtz Gemeinschaft, DFG Cluster of Excellence "Origin and Structure of the Universe", DFG Collaborative Research Centers, Polish MNiSzW, US Department of Energy Office of Science, US National Science Foundation, Smithsonian Institution, NSERC in Canada, Science Foundation Ireland (SFI), STFC in the UK, Istituto Nazionale di Astrofisica in Italy, Centre National d'Etudes Spatiales in France, NASA, Associated Universities, Inc., European Community, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

3. Generalized Family of Approximating Schemes based on Newton Interpolating Polynomials and its Error Analysis.

Author

Khan, Faheem, Omar, Muhammad, and Mustafa, Ghulam

Subjects
POLYNOMIALS, ERROR analysis in mathematics, COMPUTER-generated imagery, DIFFERENTIAL equations, NUMERICAL analysis
Abstract

A generalized family of (2j + 2)-point n-ary approximating subdivision schemes by using Newton interpolating polynomials is presented for the generation of curves and surfaces, where j≥ 0 and n≥ 2. This family unifies some well known curve and surface schemes. Furthermore, the error bound evaluation technique for the proposed schemes is also discussed. [ABSTRACT FROM AUTHOR]

Published
2019

4. Jets in Active Galaxies.

Author

Saikia, D. J.

Subjects
ACTIVE galaxies, ELECTROMAGNETIC spectrum, ASTROPHYSICS, RADIO galaxies, SUPERMASSIVE black holes
Abstract

Jets in active galaxies are signatures of energy supply via collimated beams of plasma from the galactic nucleus to the extended regions of emission. These jets, which occur across the electromagnetic spectrum, are powered by supermassive black holes in the centres of the host galaxies. Jets are seen on the scale of parsecs in the nuclear regions to those which power the giant radio sources extending over several megaparsecs. These jets raise many challenging astrophysical questions. This article explores some aspects of jets in radio galaxies and quasars, which are amongst the most powerful active galaxies. [ABSTRACT FROM AUTHOR]

Published
2018
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6. Investigating the unification of LOFAR-detected powerful AGN in the Boötes field

Author

Gianfranco Brunetti, Isabella Prandoni, George K. Miley, Wendy L. Williams, Matt J. Jarvis, Martin J. Hardcastle, A. Saxena, Jeremy J. Harwood, D. Engels, Kenneth Duncan, Timothy W. Shimwell, Huub Röttgering, Cyril Tasse, Leah K. Morabito, Philip Best, Marcus Brüggen, Krzysztof T. Chyzy, Aleksandar Shulevski, Peter Barthel, Elizabeth K. Mahony, Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Galaxies, Etoiles, Physique, Instrumentation (GEPI), 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 Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, Active galactic nucleus, UNIFIED SCHEMES, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], galaxies: active, jets [galaxies], SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7C REDSHIFT SURVEY, 01 natural sciences, 0103 physical sciences, BLACK-HOLES, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, radio continuum: galaxies, 010308 nuclear & particles physics, RADIO-SOURCE SURVEY, Astronomy and Astrophysics, Quasar, BOOTES, LOFAR, galaxies: jets, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, galaxies [radio continuum], GALAXIES, UMINOSITY FUNCTION, Space and Planetary Science, active [galaxies], Radio frequency, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], COMPLETE QUASAR SAMPLE, Astrophysics - Cosmology and Nongalactic Astrophysics, OPTICAL SPECTROSCOPY
Abstract

Low radio frequency surveys are important for testing unified models of radio-loud quasars and radio galaxies. Intrinsically similar sources that are randomly oriented on the sky will have different projected linear sizes. Measuring the projected linear sizes of these sources provides an indication of their orientation. Steep-spectrum isotropic radio emission allows for orientation-free sample selection at low radio frequencies. We use a new radio survey of the Bo\"otes field at 150 MHz made with the Low Frequency Array (LOFAR) to select a sample of radio sources. We identify 44 radio galaxies and 16 quasars with powers $P>10^{25.5}$ W Hz$^{-1}$ at 150 MHz using cross-matched multi-wavelength information from the AGN and Galaxy Evolution Survey (AGES), which provides spectroscopic redshifts. We find that LOFAR-detected radio sources with steep spectra have projected linear sizes that are on average 4.4$\pm$1.4 larger than those with flat spectra. The projected linear sizes of radio galaxies are on average 3.1$\pm$1.0 larger than those of quasars (2.0$\pm$0.3 after correcting for redshift evolution). Combining these results with three previous surveys, we find that the projected linear sizes of radio galaxies and quasars depend on redshift but not on power. The projected linear size ratio does not correlate with either parameter. The LOFAR data is consistent within the uncertainties with theoretical predictions of the correlation between the quasar fraction and linear size ratio, based on an orientation-based unification scheme., Comment: 14 pages, accepted for publication in MNRAS

Published
2017
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7. THE ORIGIN OF THE INFRARED EMISSION IN RADIO GALAXIES. II. ANALYSIS OF MID- TO FAR-INFRAREDSPITZEROBSERVATIONS OF THE 2JY SAMPLE

Author

Clive Tadhunter, Brent Groves, Katherine J. Inskip, R. Morganti, D. Dicken, Joanna Holt, R. M. González Delgado, David J. Axon, and Kapteyn Astronomical Institute

Subjects
ACTIVE GALACTIC NUCLEI, UNIFIED SCHEMES, Radio galaxy, Infrared, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, ENERGY-DISTRIBUTIONS, infrared: galaxies, STAR-FORMATION, Far infrared, Weak line, Thermal, Emission spectrum, Astrophysics::Galaxy Astrophysics, Physics, Astrophysics (astro-ph), Astronomy and Astrophysics, 3CR QUASARS, YOUNG STELLAR POPULATIONS, NARROW-LINE REGION, ULIRG EVOLUTION, Space and Planetary Science, OPTICAL CONTINUUM, Optical emission spectroscopy, Detection rate, OBSCURING DUST TORI
Abstract

We present an analysis of deep mid- to far-infrared (MFIR) Spitzer photometric observations of the southern 2Jy sample of powerful radio sources (0.05 < z < 0.7), conducting a statistical investigation of the links between radio jet, AGN, starburst activity and MFIR properties. This is part of an ongoing extensive study of powerful radio galaxies that benefits from both complete optical emission line information and a uniquely high detection rate in the far-infrared (far-IR). We find tight correlations between the MFIR and [OIII] emission luminosities, which are significantly better than those between MFIR and extended radio luminosities, or between radio and [OIII] luminosities. Since [OIII] is a known indicator of intrinsic AGN power, these correlations confirm AGN illumination of the circum-nuclear dust as the primary heating mechanism for the dust producing thermal MFIR emission at both 24 and 70 microns. We demonstrate that AGN heating is energetically feasible, and identify the narrow line region clouds as the most likely location of the cool, far-IR emitting dust. Starbursts make a major contribution to the heating of the cool dust in only 15-28% of our targets. We also investigate the orientation dependence of the continuum properties, finding that the broad- and narrow-line objects in our sample with strong emission lines have similar distributions of MFIR luminosities and colours. Therefore our results are entirely consistent with the orientation-based unified schemes for powerful radio galaxies. However, the weak line radio galaxies (WLRG) form a separate class of objects with intrinsically low luminosity AGN in which both the optical emission lines and the MFIR continuum are weak., 29 pages, 5 figures, Accepted for publication in The Astrophysical Journal

Published
2009
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8. Radio galaxies

Author

Pieter Barthel, I.M. van Bemmel, and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, Unification, UNIFIED SCHEMES, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, galaxies : active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, CENTAURUS-A, Astrophysics::Galaxy Astrophysics, Physics, quasars : general, FR-I, infrared : galaxies, Astrophysics (astro-ph), Astronomy and Astrophysics, 3CR QUASARS, HOST GALAXIES, CONTINUUM, Space and Planetary Science, VIEWING-ANGLE, EMISSION, radio continuu : galaxies, CYGNUS-A
Abstract

The 2002 status of unification models for extragalactic radio sources is examined, with particular emphasis on the dust properties of these objects., Comment: 9 pages, no figures, in Proceedings Radio Galaxy Workshop, Leiden, 11-15 November 2002

Published
2003

9. EVN observations of low-luminosity flat-spectrum active galactic nuclei

Author

A. Caccianiga, A. Thean, M. J. M. Marchã, J. Dennett-Thorpe, and Kapteyn Astronomical Institute

Subjects
UNIFIED SCHEMES, Astrophysics::High Energy Astrophysical Phenomena, galaxies : active, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, LINE REGION, Lower limit, Radio spectrum, IDENTIFICATIONS, Luminosity, galaxies : Seyfert, radio continuum : galaxies, Very-long-baseline interferometry, Emission spectrum, RESOLUTION RADIO OBSERVATIONS, QUIET QUASARS, Astrophysics::Galaxy Astrophysics, Physics, Spectrum (functional analysis), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, LOUD, Space and Planetary Science, JET, Brightness temperature, ALL-SKY SURVEY, SEYFERT-GALAXY, MARKARIAN-3
Abstract

We present and discuss the results of very-long baseline interferometry (VLBI, EVN) observations of three low-luminosity (P-5GHz

Published
2001
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10. Flat radio-spectrum galaxies and BL Lacs I. Core properties

Subjects
ACTIVE GALACTIC NUCLEI, POLARIZATION, UNIFIED SCHEMES, galaxies : active, BLAZARS, galaxies : jets, BANK VLBI SURVEY, radio continuum : galaxies, galaxies : nuclei, galaxies : BL Lacertae objects : general, PHASE CALIBRATION SOURCES, RELATIVISTIC JETS, COMPLETE SAMPLE, SCALE STRUCTURE, LACERTAE OBJECTS
Abstract

This paper concerns the relationship of BL Lacs and flat-spectrum weak emission-line galaxies. We compare the weak emission-line galaxies and the BL Lacs in a sample of 57 flat-spectrum objects (Marcha et al. 1996), using high-frequency radio and non-thermal optical flux densities, spectral indices and polarization properties. We consider whether objects which are not 'traditional' BL Lacs - due to their larger emission line strengths, and larger Ca II spectral breaks - are simply starlight diluted BL Lacs. Their broad-band spectral properties are consistent with this interpretation, but their radio polarization may indicate more subtle effects.. Comparison of the weak emission-line galaxies and the BL Lacs shows that, on average, the former have steeper spectra between 8 and 43 GHz, and are less polarized at 8.4 GHz. This is consistent with many of the weak-lined objects being at larger angles to the line of sight than the BL Lacs. In addition to this population, we indicate a number of the weak emission-line galaxies which may be 'hidden BL Lacs': relativistically boosted objects very close to the line of sight with an apparently weak AGN.

Published
2000

11. Extreme host galaxy growth in powerful early-epoch radio galaxies

Author

Christian Leipski, Belinda Jane Wilkes, Peter Barthel, Martin Haas, and Astronomy

Subjects
Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), UNIFIED SCHEMES, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, galaxies: starburst, DUST, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, infrared: galaxies, STAR-FORMATION, galaxies: high-redshift, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, AGN, Astrophysics::Galaxy Astrophysics, Physics, Solar mass, Epoch (reference date), 3CR SOURCES, Astronomy and Astrophysics, Quasar, Galaxy, Redshift, Black hole, QUASARS, Space and Planetary Science, X-RAY, Astrophysics::Earth and Planetary Astrophysics, HIGH-REDSHIFT, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

During the first half of the universe's age, a heyday of star-formation must have occurred because many massive galaxies are in place after that epoch in cosmic history. Our observations with the revolutionary Herschel Space Observatory reveal vigorous optically obscured star-formation in the ultra-massive hosts of many powerful high-redshift 3C quasars and radio galaxies. This symbiotic occurrence of star-formation and black hole driven activity is in marked contrast to recent results dealing with Herschel observations of X-ray selected active galaxies. Three archetypal radio galaxies, at redshifts 1.132,1.575, and 2.474 are presented here, with inferred star-formation rates of hundreds of solar masses per year. A series of spectacular coeval AGN/starburst events may have formed these ultra-massive galaxies and their massive central black holes during their relatively short lifetimes., Comment: To appear in Astrophysical Journal Letters

Published
2012
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12. The 2010 very high energy γ-ray flare and 10 years of multi-wavelength observations of M 87

Author

Abramowski, A[, 1, 20, ], Acero, F[ 2 ], Aharonian, F[, 3, 5 ], 4, Akhperjanian, Ag[, 5, 6, ], Anton, G[ 7 ], Balzer, A[ 7 ], Barnacka, A[, 8, 9, ], de Almeida, UB[ 10 ], Becherini, Y[, 11, 12, ], Becker, J[ 13 ], Behera, B[ 14 ], Bernlohr, K[, 3, 15, ], Birsin, E[ 15 ], Biteau, J[ 12 ], Bochow, A[ 3 ], Boisson, C[ 16 ], Bolmont, J[ 17 ], Bordas, P[ 18 ], Brucker, J[ 7 ], Brun, F[ 12 ], Brun, P[ 9 ], Bulik, T[ 19 ], Busching, I[, 13, Carrigan, S[ 3 ], Casanova, S[ 13 ], Cerruti, M[ 16 ], Chadwick, PM[ 10 ], Charbonnier, A[ 17 ], Chaves, RCG[ 3 ], Cheesebrough, A[ 10 ], Clapson, AC[ 3 ], Coignet, G[ 21 ], Cologna, G[ 14 ], Conrad, J[ 22 ], Dalton, M[ 15 ], Daniel, MK[ 10 ], Davids, ID[ 23 ], Degrange, B[ 12 ], Deil, C[ 3 ], Dickinson, HJ[ 22 ], Djannati Atai, A[ 11 ], Domainko, W[ 3 ], Drury, LO[ 4 ], Dubus, G[ 24 ], Dutson, K[ 25 ], Dyks, J[ 8 ], Dyrda, M[ 26 ], Egberts, K[ 27 ], Eger, P[ 7 ], Espigat, P[ 11 ], Fallon, L[ 4 ], Farnier, C[ 2 ], Fegan, S[ 12 ], Feinstein, F[ 2 ], Fernandes, MV[ 1 ], Fiasson, A[ 21 ], Fontaine, G[ 12 ], Forster, A[ 3 ], Fussling, M[ 15 ], Gallant, YA[ 2 ], Gast, H[ 3 ], Gerard, L[ 11 ], Gerbig, D[ 13 ], Giebels, B[ 12 ], Glicenstein, JF[ 9 ], Gluck, B[ 7 ], Goret, P[ 9 ], Goring, D[ 7 ], Haffner, S[ 7 ], Hague, JD[ 3 ], Hampf, D[ 1 ], Hauser, M[ 14 ], Heinz, S[ 7 ], Heinzelmann, G[ 1 ], Henri, G[ 24 ], Hermann, G[ 3 ], Hinton, JA[ 25 ], Hoffmann, A[ 18 ], Hofmann, W[ 3 ], Hofverberg, P[ 3 ], Holler, M[ 7 ], Horns, D[ 1 ], Jacholkowska, A[ 17 ], de Jager, OC[ 20 ], Jahn, C[ 7 ], Jamrozy, M[ 28 ], Jung, I[ 7 ], Kastendieck, MA[ 1 ], Katarzynski, K[ 29 ], Katz, U[ 7 ], Kaufmann, S[ 14 ], Keogh, D[ 10 ], Khangulyan, D[ 3 ], Khelifi, B[ 12 ], Klochkov, D[ 18 ], Kluzniak, W[ 8 ], Kneiske, T[ 1 ], Komin, N[ 21 ], Kosack, K[ 9 ], Kossakowski, R[ 21 ], Laffon, H[ 12 ], Lamanna, G[ 21 ], Lennarz, D[ 3 ], Lohse, T[ 15 ], Lopatin, A[ 7 ], CC[ 3 ], Lu, Marandon, V[ 11 ], Marcowith, A[ 2 ], Masbou, J[ 21 ], Maurin, D[ 17 ], Maxted, N[ 30 ], 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Montpellier (LUPM), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Unité Scientifique de la Station de Nançay (USN), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-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), HESS, 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), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Univers et Théories (LUTH (UMR_8102)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), APC - Astrophysique des Hautes Energies (APC - AHE), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), 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)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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), Abramowski A., Acero F., Aharonian F., Akhperjanian A. G., Anton G., Balzer A., Barnacka A., Barres de Almeida U., Becherini Y., Becker J., Giovannini G., and and 436 coauthors.

Subjects
High energy, UNIFIED SCHEMES, Radio galaxy, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], VHE [gamma ray], jets [galaxies], nuclei [galaxies], Astrophysics, 7. Clean energy, 01 natural sciences, Spectral line, LARGE-AREA TELESCOPE, law.invention, ACTIVE GALACTIC NUCLEI, SUPERMASSIVE BLACK-HOLE, RADIO GALAXY M87, BASE-LINE ARRAY, TEV EMISSION, CRAB-NEBULA, SCALE JETS, INNER JET, Raigs gamma, law, HESS, flux [gamma ray], black hole, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], MAGIC (telescope), 010303 astronomy & astrophysics, Physics, [PHYS]Physics [physics], flux [X-ray], Gamma ray, radioastronomia, non-thermal [radiation mechanisms], active [galaxies], galaxies [gamma rays], VERITAS, Electrónica, Física nuclear, Electricidad, Flare, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: individual (M 87), Astrophysics::High Energy Astrophysical Phenomena, radio wave [galaxy], galaxies: active, gamma rays: observations, galaxies: jets, radiation mechanisms: non-thermal, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray astronomy, Cosmic rays, IMAGING CHERENKOV DETECTOR, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], individual: M 87 [galaxies], emission [gamma ray], 0103 physical sciences, gamma rays: galaxies, Astrophysics::Galaxy Astrophysics, galaxies: active , galaxies: individual (M 87) , galaxies: jets , galaxies: nuclei , gamma rays: galaxies , radiation mechanisms: non-thermal, 010308 nuclear & particles physics, Gamma rays, Institut für Physik und Astronomie, Astronomy and Astrophysics, Light curve, Galaxies, MAGIC, Galàxies, Black hole, Space and Planetary Science, ddc:520, time dependence, galaxies: nuclei, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

著者人数: 444名, Accepted: 2011-11-18, 資料番号: SA1003024000

Published
2012
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13. The asymmetric radio structure and record jet of giant quasar 4C 34.47

Author

S. Hocuk, P. D. Barthel, and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, SAMPLE, UNIFIED SCHEMES, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, SPECTRAL INDEX, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Asymmetry, DEPOLARIZATION ASYMMETRY, quasars: individual: 4C 34.47, Astrophysics::Galaxy Astrophysics, media_common, Physics, Line-of-sight, Astronomy and Astrophysics, Quasar, 3CR QUASARS, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Galaxy, STATISTICS, GALAXIES, DEFINITION, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Aspect angle, POLARIZATION PROPERTIES, Halo
Abstract

Giant double-lobed radio source 4C34.47 displays a straight one-sided jet, measuring a record length of 380kpc, in its double-lobed radio structure. Assuming an intrinsically symmetric two-sided jet structure the radio source jet axis must be at least 33 degrees away from the sky plane, that is within 57 degrees from the line of sight. The radio polarization properties indicate that this giant source has largely outgrown the depolarizing halo generally associated with the host galaxies of powerful radio sources. The measured small depolarization asymmetry is nevertheless in accordance with its inferred orientation. All data for this giant radio source are in agreement with its preferred orientation as predicted within the unification scheme for powerful radio sources. Seen under a small aspect angle the radio source is large but not excessively large. The global properties of 4C34.47 do not differ from other giant (old) FR2 radio sources: it is a slowly expanding low-luminosity radio source., Accepted for publication in Astronomy and Astrophysics

Published
2010

14. Dust tori in radio galaxies

Author

Reynier Peletier, Pieter Barthel, J. W. Pel, G. van der Wolk, and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, UNIFIED SCHEMES, Radio galaxy, Point source, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, infrared: galaxies, symbols.namesake, FR-II DICHOTOMY, HIGH-RESOLUTION MAPS, Emission spectrum, Astrophysics::Galaxy Astrophysics, Physics, LAC UNIFYING MODEL, BLACK-HOLE MASSES, Astronomy and Astrophysics, Quasar, SOURCE COUNTERPARTS, HUBBLE-SPACE-TELESCOPE, galaxies: jets, radiation mechanisms: non-thermal, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Redshift, Galaxy, radiation mechanisms: thermal, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Eddington luminosity, symbols, COMPLETE SAMPLE, galaxies: nuclei, EMISSION-LINE
Abstract

We investigate the validity of the quasar - radio galaxy unification scenario and detect dust tori within radio galaxies of various types. Using VISIR on the VLT, we acquired sub-arcsecond (~0.40") resolution N-band images, at a wavelength of 11.85 micron, of the nuclei of a sample of 27 radio galaxies of four types in the redshift range z=0.006-0.156. The sample consists of 8 edge-darkened, low-power Fanaroff-Riley class I (FR-I) radio galaxies, 6 edge-brightened, class II (FR-II) radio galaxies displaying low-excitation optical emission, 7 FR-IIs displaying high-excitation optical emission, and 6 FR-II broad emission line radio galaxies. Out of the sample of 27 objects, 10 nuclei are detected and several have constraining non-detections at sensitivities of 7 mJy, the limiting flux a point source has when detected with a signal-to-noise ratio of 10 in one hour of source integration. On the basis of the core spectral energy distributions of this sample we find clear indications that many FR-I and several low-excitation FR-II radio galaxies do not contain warm dust tori. At least 57+-19 percent of the high-excitation FR-IIs and almost all broad line radio galaxies display excess infrared emission, which must be attributed to warm dust reradiating accretion activity. The FR-I and low-excitation FR-II galaxies all possess low efficiencies, calculated as the ratio of bolometric and Eddington luminosity log (L_bol/L_Edd) < -3. This suggests that thick tori are absent at low accretion rates and/or low efficiencies. We argue that the unification viewing angle range 0-45 degrees of quasars should be increased to ~60 degrees, at least at lower luminosities., 17 pages, 9 figures, published in Astronomy and Astrophysics. Version 2 matches published version.

Published
2010

15. Mid-infrared spectroscopy of high-redshift 3CRR sources

Author

C. Leipski, Belinda Jane Wilkes, Peter Barthel, P. M. Ogle, M. L. N. Ashby, Steven P. Willner, M. Haas, R. Chini, Giovanni G. Fazio, F. Heymann, Ralf Siebenmorgen, Robert Antonucci, and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), UNIFIED SCHEMES, Radio galaxy, KECK SPECTROPOLARIMETRY, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, INFRARED OBSERVATIONS, FOS: Physical sciences, Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, SILICATE FEATURES, Spectral line, infrared: galaxies, chemistry.chemical_compound, POWERFUL RADIO GALAXIES, Spitzer Space Telescope, galaxies: high-redshift, Astrophysics::Galaxy Astrophysics, SPITZER-SPACE-TELESCOPE, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Quasar, Rest frame, Silicate, Redshift, INTERSTELLAR EXTINCTION LAW, chemistry, Space and Planetary Science, 8.0 MU-M, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using the Spitzer Space Telescope, we have obtained rest frame 9-16mu spectra of 11 quasars and 9 radio galaxies from the 3CRR catalog at redshifts 1.0, Comment: 16 pages, 8 Figures, accepted for ApJ

Published
2010
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16. Observation of gamma‐ray emission from the galaxy m87 above 250 gev with veritas1

Author

V. A. Acciari, M. Beilicke, G. Blaylock, S. M. Bradbury, J. H. Buckley, V. Bugaev, Y. Butt, O. Celik, A. Cesarini, L. Ciupik, P. Cogan, P. Colin, W. Cui, M. K. Daniel, C. Duke, T. Ergin, A. D. Falcone, S. J. Fegan, J. P. Finley, G. Finnegan, P. Fortin, L. F. Fortson, K. Gibbs, G. H. Gillanders, J. Grube, R. Guenette, G. Gyuk, D. Hanna, E. Hays, J. Holder, D. Horan, S. B. Hughes, M. C. Hui, T. B. Humensky, A. Imran, P. Kaaret, M. Kertzman, D. B. Kieda, J. Kildea, A. Konopelko, H. Krawczynski, F. Krennrich, M. J. Lang, S. LeBohec, K. Lee, G. Maier, A. McCann, M. McCutcheon, J. Millis, P. Moriarty, R. Mukherjee, T. Nagai, R. A. Ong, D. Pandel, J. S. Perkins, M. Pohl, J. Quinn, K. Ragan, P. T. Reynolds, H. J. Rose, M. Schroedter, G. H. Sembroski, A. W. Smith, D. Steele, S. P. Swordy, A. Syson, J. A. Toner, L. Valcarcel, V. V. Vassiliev, S. P. Wakely, J. E. Ward, T. C. Weekes, A. Weinstein, R. J. White, D. A. Williams, S. A. Wissel, M. D. Wood, and B. Zitzer

Subjects
unified schemes, Active galactic nucleus, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies : individual (m87, ngc 4486, virgo a), 01 natural sciences, Observatory, jet, 0103 physical sciences, gamma rays : observations, crab-nebula, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, tev emission, 010308 nuclear & particles physics, variability, Gamma ray, telescope observations, Astronomy and Astrophysics, Radius, Cherenkov Telescope Array, lac objects, Galaxy, x-ray, 13. Climate action, Space and Planetary Science, markarian-421, High Energy Physics::Experiment, Radio wave, supermassive black-hole
Abstract

The multiwavelength observation of the nearby radio galaxy M87 provides a unique opportunity to study in detail processes occurring in Active Galactic Nuclei from radio waves to TeV gamma-rays. Here we report the detection of gamma-ray emission above 250 GeV from M87 in spring 2007 with the VERITAS atmospheric Cherenkov telescope array and discuss its correlation with the X-ray emission. The gamma-ray emission is measured to be point-like with an intrinsic source radius less than 4.5 arcmin. The differential energy spectrum is fitted well by a power-law function: dPhi/dE=(7.4+-1.3_{stat}+-1.5_{sys})(E/TeV)^{-2.31+-0.17_{stat}+-0.2_{sys}} 10^{-9}m^{-2}s^{-1}TeV^{-1}. We show strong evidence for a year-scale correlation between the gamma-ray flux reported by TeV experiments and the X-ray emission measured by the ASM/RXTE observatory, and discuss the possible short-time-scale variability. These results imply that the gamma-ray emission from M87 is more likely associated with the core of the galaxy than with other bright X-ray features in the jet.

Published
2008

17. FERMI LARGE AREA TELESCOPE GAMMA-RAY DETECTION OF THE RADIO GALAXY M87

Author

Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Axelsson, Magnus, Johannesson, G., Johnson, A. S., Ryde, Felix, Conrad, Jan, Ylinen, Tomi, Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Axelsson, Magnus, Johannesson, G., Johnson, A. S., Ryde, Felix, Conrad, Jan, and Ylinen, Tomi

Abstract

We report the Fermi Large Area Telescope (LAT) discovery of high-energy (MeV/GeV) gamma-ray emission positionally consistent with the center of the radio galaxy M87, at a source significance of over 10 sigma in 10 months of all-sky survey data. Following the detections of Cen A and Per A, this makes M87 the third radio galaxy seen with the LAT. The faint point-like gamma-ray source has a >100 MeV flux of 2.45 (+/-0.63) x 10(-8) photons cm(-2) s(-1) (photon index = 2.26 +/- 0.13) with no significant variability detected within the LAT observation. This flux is comparable with the previous EGRET upper limit (<2.18 x 10-8 photons cm(-2) s(-1), 2 sigma), thus there is no evidence for a significant MeV/GeV flare on decade timescales. Contemporaneous Chandra and Very Long Baseline Array data indicate low activity in the unresolved X-ray and radio core relative to previous observations, suggesting M87 is in a quiescent overall level over the first year of Fermi-LAT observations. The LAT gamma-ray spectrum is modeled as synchrotron self-Compton (SSC) emission from the electron population producing the radio-to-X-ray emission in the core. The resultant SSC spectrum extrapolates smoothly from the LAT band to the historical-minimum TeV emission. Alternative models for the core and possible contributions from the kiloparsec-scale jet in M87 are considered, and cannot be excluded., QC 20100525

Published
2009
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18. Flat radio-spectrum galaxies and BL Lacs I. Core properties

Author

Dennett-Thorpe, J, Marcha, MJ, and Kapteyn Astronomical Institute

Subjects
ACTIVE GALACTIC NUCLEI, POLARIZATION, UNIFIED SCHEMES, Astrophysics::High Energy Astrophysical Phenomena, galaxies : active, Astrophysics::Cosmology and Extragalactic Astrophysics, BLAZARS, galaxies : jets, BANK VLBI SURVEY, radio continuum : galaxies, galaxies : nuclei, galaxies : BL Lacertae objects : general, PHASE CALIBRATION SOURCES, RELATIVISTIC JETS, COMPLETE SAMPLE, SCALE STRUCTURE, Astrophysics::Galaxy Astrophysics, LACERTAE OBJECTS
Abstract

This paper concerns the relationship of BL Lacs and flat-spectrum weak emission-line galaxies. We compare the weak emission-line galaxies and the BL Lacs in a sample of 57 flat-spectrum objects (Marcha et al. 1996), using high-frequency radio and non-thermal optical flux densities, spectral indices and polarization properties. We consider whether objects which are not 'traditional' BL Lacs - due to their larger emission line strengths, and larger Ca II spectral breaks - are simply starlight diluted BL Lacs. Their broad-band spectral properties are consistent with this interpretation, but their radio polarization may indicate more subtle effects.. Comparison of the weak emission-line galaxies and the BL Lacs shows that, on average, the former have steeper spectra between 8 and 43 GHz, and are less polarized at 8.4 GHz. This is consistent with many of the weak-lined objects being at larger angles to the line of sight than the BL Lacs. In addition to this population, we indicate a number of the weak emission-line galaxies which may be 'hidden BL Lacs': relativistically boosted objects very close to the line of sight with an apparently weak AGN.

Published
2000

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