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Blazar 3c454 3

3c 454.

Infrared polarisation of blazar 3C454

Fast Flare of 3C454.3 in the NIR : 3041 : Fermi LAT detection of a rapid and extraordinary GeV outburst from 3C 454.3 : 3034 : AGILE detects another extraordinary gamma-ray flare from the blazar 3C 454.3 : 3005 : Optical follow-up observations of blazar 3C 454.3 : 3003 : Optical and NIR activity of blazars 3C454.3 and 3C66a : 2988 : NIR Flaring. With reference to ATels #2988, #2995 we report that blazar 3C454.3 shows prominent activity in optical and NIR bands (R~13.5 and J~11.5 on November 2, brightening by ~1.5 mag within ~10 days). These values are close to the brightest states of 2008 July and 2009 December outbursts (see ATels #1625 and #2325). Simultaneously R band polarization reached a level of 30%

3c454.

(PDF) INTEGRAL observations of the blazar 3C454

3C454.3 is a widely studied and monitored flat spectrum radio quasar. We use the observations from the Small and Moderate Aperture Research Telescope System (SMARTS) to analyze the long-term optical and spectral variabilities of 3C454.3 at B, V, R, J, and K (BVRJK) bands. Based on the relation: , we calculate the multiband spectral indices. A blazar is an active galactic nucleus (AGN) with a relativistic jet (a jet composed of ionized matter traveling at nearly the speed of light) directed very nearly towards an observer. Relativistic beaming of electromagnetic radiation from the jet makes blazars appear much brighter than they would be if the jet were pointed in a direction away from Earth In Spring 2005, the blazar 3C454.3 underwent a dramatic outburst at all wavelengths from mm to X-rays. This prompted INTEGRAL observations, accomplished in 15-18 May 2005. The source was detected by the INTEGRAL instruments from 3 to 200 keV in a bright state (~5 x 10E-10 cgs), at least a factor of 2-3 higher than previously observed Following a major outburst at radio wavelengths in the quasar 3C454.3, observations by means of very long baseline interferometry have revealed a superluminal increase in the size of the compact. The blazar 3C 454.3 was found to be in a high flux state in 2009 November-December. We performed correlations in optical observations made at three telescopes, along with X-ray data from the MAXI camera and public release 3C454.3 (PKS 2251+158).

3C 454.3 — Wikipédi

The GLAST Large Area Telescope AGN science group is starting a multiwavelength campaign for blazar 3C454.3 (2251+158), effective immediately and continuing through the middle of August. This Ad-Hoc Intensive Campaign (AIC) is prompted by brightening in the radio, optical and X-ray How do you say Blazar 3C454.3? Listen to the audio pronunciation of Blazar 3C454.3 on pronouncekiw Fermi LAT Multiwavelength Coordinating Group; July, 2007, Multiwavelength Campaign on 3C454.3; Browse page BibTeX @MISC{Sikora7113c454.3reveals, author = {Marek Sikora and Greg M. Madejski}, title = {3C454.3 reveals the structure and physics of its 'blazar zone'.}, year = {711}

This work is devoted to multi-frequency studying of the blazar 3C 454.3. The study includes spectroscopic and photometric observations in the optical, IR, and gamma-ray bands. We investigate whether a correlation exists in the light curves at different wavelengths. We have carried out observations of the optical spectrum (from 4000 to 7000 Angstroms) between 2007 and 2009, and identified MgII. Blazar 3C 454.3 is considered one of the brightest and most persistent gamma-ray sources in the sky and can be found in the immediate vicinity of Markab (α-Peg, mag 2.45) where it forms a tight visual double with GSC 1698-0718 (mag 13.1). Further details in relation to blazar 3C 454.3 are available on Simbad and NASA's NED database

The Extraordinary Gamma-Ray Flare of the Blazar 3C 454.3 3C454.3 during the γ-ray outburst in November 2010 the activity (blazar) zone at distances corresponding with those postulated to explain the 2009 optical polarization-swing-event in terms of the scenario of a source propagating along the curved trajectory (Abdo et al. 2010)

3C454.3 Quasar/Blazar/AGN in Pegasus - Deep Sky Observing ..

3C454.3. November 18, 2010: Blazar 3C 454.3 sharply increasing in brightness. which was taken on 2010-11-10 was used to perform the photometry and has been annotated to show the location of 3C 454.3 as well as the comparison and check stars. Five 60 second exposures were average stacked to produce the resulting image We are not allowed to display external PDFs yet. You will be redirected to the full text document in the repository in a few seconds, if not click here.click here

ATel #2330: Swift/BAT detects flaring activity from 3C 454

Optical and NIR activity of blazars 3C454

Fourth project: Multi-wavelength study of the blazar 3C454.3: Swift and Agile (Stefano Vercellone and Patrizia Romano) (PDF,PPT unavailable) Fifth project: Neutron star low mass X-ray binaries seen by INTEGRAL: High energy behaviour (Antonella Tarano) (PDF, Sixth project: Diffuse emission in galactic disks (Kip Kuntz) (PDF, PPT) Tuesday 2 Outburst del cuasar 3C454.3 Maehara-san (VSNET) reporta que el blazar 3C 454.3 esta en outburst (1.2 mag (V) más brillante que en Septiembre de 2006. Las observaciones reportadas son las siguientes. 3C454.3 20060728.706 16.12Rc (Hiroyuki Maehara .VSNET ) 3C454.3 20060923.596 15.36Rc (Hiroyuki Maehara . VSNET). polarization variability observed in the prototype blazar 3C454.3 between MJD ˘55400 and ˘55800. A number of physical properties were constrained, such as the jet plasma density, the coherence length of the magnetic field as well as the compression and Doppler factors of the propagating shocked regions

Crab Nebula Blazar 3C454.3 Comptonisation A population of photons that encounters a region containing free electrons will find its spectrum modified as a result of inverse Compton scattering given sufficient optical depth. If the electrons are on average more energetic than photons then the photons will on average be up-scattered to higher energie We propose a model to explain the ultra-bright GeV gamma-ray flares observed from the blazar 3C454.3. The model is based on the concept of a relativistic jet interacting with compact gas condensations produced when a star (a red giant) crosses the jet close to the central black hole. The study includes an analytical treatment o We propose a model to explain the ultra-bright GeV gamma-ray flares observed from the blazar 3C454.3. The model is based on the concept of a relativistic jet interacting with compact gas condensations produced when a star (red giant) crosses the jet close to the central black hole 3C454.3 during three gamma-ray outbursts • The FSRQ 3C454.3 had three big gamma-ray flares in 2009-10 (Ackermann et al. 2010, Abdo et al. 2011) • L~1049 erg s-1, δ>15 • Jorstad et al. (2013) report on 35 observations between 2009 April and 2011 August, with VLBA @43 GHz • 0.3 mas x 0.1 ma

Detailed map showing the location of the blazar 3C 454.3. I've drawn a small asterism using a group of brighter stars with their magnitudes marked. A scale showing 30 arc minutes (1/2 degree) is. Blazar: 3C454.3 M ~ 109 M Sun time flux index Same anti-correlation as AO0235+164 The rise time and burst periods a lot longer (by an order of magnitude) Quantitative agreement and correct scaling with Blazar mass with (broader sense of) Wakefield theory (Ebisuzaki/Tajima) period ~ M ; luminosity ~M Again, Anti-correlation even in a bigger blazar Title: Interpretation of the development of flare phenomena 2004-2007 in the blazar 3C454.3 Authors: Volvach, A. E. & Larionov, M. G. Journal: Memorie della Societa Astronomica Italiana, v.82, p.165 (2011) Bibliographic Code: 2011MmSAI..82..165 A sample of a full SED movie of the blazar 3C454.3 is currently available on-line and can be seen at the main page of the current version of the ASDC SED tool (V3.0). Usually blazar SED data is compared to theoretical models that are based on the current best understanding of the physical processes responsible for the emission of the multi. The blazar 3C454.3 exhibited a strong flare seen in gamma-rays, X-rays, and optical/NIR bands during 3--12 December 2009. Emission in the V and J bands rose more gradually than did the gamma-rays an

Tracing the peculiar jet kinematics of 3C45

Multiwavelength Campaign for blazar 3C454.3. From: Dave Thompson <David.J.Thompson@nasa.gov> Re: Multiwavelength Campaign for blazar 3C454.3. From: Eric Perlman <perlman@jca.umbc.edu> Re: Multiwavelength Campaign for blazar 3C454.3. From: Neil Gehrels <gehrels@milkyway.gsfc.nasa.gov> Re: Multiwavelength Campaign for blazar 3C454.3 2 modelling blazar emission the 2005/06 are of 3C454.3 physics implications 3 results from the Planck / F-GAMMA collaboration the F-GAMMA project aring around the ERCSC: 3C454.3 and BL Lac 4 the potential of Planck blind search pipeline for variable sources 5 summary a collaboration of J org Rachen Max H aberlein Lars Fuhrmann Emmanouil. 3c454.3というブレーザーは、72憶光年もの遠方にある天体であるが、9月頃から明るくなり始め、12月に入ってから急激に明るくなった。そして、一時的にガンマ線の空では最も明るい天体になったこともあり、今も明るい状態が続いている Fermi以前は, PulsarまたはBlazar以外はほとんど (または全く)知られていなか た種族 今日の主役 Vela Geminga または全く知られていなかった種族: 今日の主役 Radio-quiet PSR SNR Globular Cluster etc. 3c454.3 Non-Blazar AGN Crab Normal Galaxy etc T. Mizuno et al. 6 >1400 sources (Abdo+10, ApJS 188, 405)

VRI Photometry and Polarimetry of 3C454

  1. 3C454.3, PKS 0235+164 and PKS 2155-304 Even for Blazars of similar type, slopes and average flux ratios are different. With fixed observing band, slopes and ratios depend on relative locations of bands w.r.t. peaks within SED
  2. 3. Concurrent -ray, UV, optical, and IR variability of 3C454.3 Recently, Bonning et al. (2009) performed a multi-wavelength monitoring campaign on the blazar, 3C454.3, using IR and optical obser-vations from the SMARTS telescopes, optical, UV and X-ray data from the Swift satellite, and public-release -ray data from the Fermi Space Telescope
  3. osti.gov journal article: star-jet interactions and gamma-ray outbursts from 3c454.3 Title: STAR-JET INTERACTIONS AND GAMMA-RAY OUTBURSTS FROM 3C454.3 Full Recor
  4. An analysis of periodic components of flux variability was carried out based on the long-term monitoring of the nuclei of active galaxies 3C454.3, 1633+382, and 3C120, performed in the Crimean Astrophysical Observatory from 1985 to 2008 at 22.2 and 36.8 GHz. Long-period components of the variability (12-14 yrs) were detected and interpreted in terms of the precessional motion of the central.
  5. Multiwavelength Campaign for Blazar 3C454.3 (2251+158), z = 0.86 News September 1 The 3C454.3 campaign ends on Sep 1; observers are asked to send data to the campaign managers (awehrle_ssi@earthlink.net or Matthias.Kadler@nasa.gov) by Fri, Sep 28, 2007.
  6. For 3C454.3, the monitoring time is in the range from June 23, 2008 to November 30, 2015, and the observations cover five optical and near-IR bands, B, V, R, J, and K bands. The BVRJK lightcurves have been shown in Figure 1, which are built b
  7. g up blazar spectra There is a situation when a sum of different spectra gives more information than individual spectra: A stable emission or absorption feature. The sample: - 1-st Fermi catalog. Flat spectrum radio quasars or low peak BL Lacs

AGILE rivela il Blazar 3C454.3 in uno stato iperattivo. Il satellite AGILE, ancora nella fase di test preliminari, ha osservato i la regione di cielo contenente il Blazar 3C454.3 dal 24 al 30 luglio 2007. AGILE ha rivelato il Blazar in uno stato iper attivo The blazar 3C454.3 underwent a flaring episode in July 2007 during which it was detected in high energy gamma-rays by AGILE. We report on infrared polarimetric observations taken a few days after the last AGILE observation. The source was still in flare with a near-infrared flux more than ten times brighter than during quiescence periods In one of the first published reports using data from Fermi, Yale post-doctoral associate Erin Bonning, together with Charles Bailyn, Meg Urry and other Yale astronomers, showed that the gamma-ray and optical emission from the blazar 3C454.3 varied together. When the blazar shines brightly in gamma-rays, the optical light is also at its brightest

In an effort to provide additional capabilities we are working on a new version that will support polarization data at any frequency. We expect that this version (V4.0) will be released later this year. An animated movie illustrating the temporal evolution of the SED of the blazar 3C454.3 is also available as example Blazar jet physics in the age of Fermi - Volume 6 Issue S27

(PDF) INTEGRAL observation of the blazar 3C454

3C 454.3 es un blazar (un tipo de cuásar con un jet orientado hacia la Tierra) localizado fuera del plano galáctico.Está situado en la constelación de Pegaso.Es una de las fuentes de rayos-gamma más brillantes del firmamento, el más llameante, el doble que el púlsar de la Vela en nuestra galaxia. [2] Es muy brillante a las radio-frecuencias Hi i would like to give some ideias of some problemes that i think affect the server like the spawners i hate de fact that we need a creeper egg to.. The flat-spectrum radio quasar 3C454.3 underwent an extraordinary 5 day γ -ray outburst in 2010 November when the daily flux measured with the Fermi Large Area Telescope (LAT) at photon energies E > 100 MeV reached (66 ± 2) × 10−6 photons cm−2 s−1. This is a factor of three higher than its previous maximum flux recorded in 2009 December and 5 times brighter than the Vela pulsar, which. NASA's Gamma-ray Large Area Space Telescope (GLAST) was launched on 11 June and turned on its main telescope two weeks later. It was immediately blasted with gamma-rays from blazar 3C454.3. Academia.edu is a platform for academics to share research papers

peculiar multiwavelength flare in the blazar 3C 454

  1. During the flight were made coordinated observations between HEFT and NASA's Swift x-ray telescope wich simultaneously observed the extragalactic blazar 3C454.3. Because the blazar was under eruption [...] during th e HEFT f li ght, it was one o f the b rightest active galactic n uc lei i n the s ky
  2. blazar 3C454.3 seen in γ-rays, X-rays, and optical/NIR bandsduring3−12December2009.Theemissioninthe V and J bands increased more gradually than did the γ-rays and soft X-rays, however all peaked at nearly the same time. Optical polarization changed largely during the flare, with a strong anti-correlation between opti
  3. During the flight were made coordinated observations between HEFT and NASA's Swift x-ray telescope wich simultaneously observed the extragalactic blazar 3C454.3. Because the blazar was under eruption during the HEFT flight, it was one of the brightest active galactic nuclei in the sky
  4. ute exposure windows shown in the boaom graph, properly taking into account the variaon in exposure during the window

[1903.04587] The June 2016 Optical and Gamma-Ray Outburst ..

Figure 3. The optical light curve of 3C454.3 around the time of the INTEGRAL AO-3 ToO observation tion started 2005 May 15, at 18:40 UT, with exposure of 200 ksec. The source was clearly detected by IBIS/ISGRI in the 20-40 and 40-100 keV energy bands, with a signifi-cance of 20 and 15 sigma. This confirm the importance o CHAMANI -- Time Variability of the Core-Shift Effect in the Blazar 3C454.3. COSTAMANTE -- To BLR or not to BLR ? The Fermi-LAT view . COVINO -- Year-long quasi-periodicities of gamma-ray blazars: A cautious approach. D'AMMANDO -- Jet physics of blazar-like narrow-line Seyfert 1 galaxies in the Fermi era And its blazar 3C454.3 that clocked in the greatest brightness ever observed, it registered with an absoloute magnitude of -31.4! To put the brightness of quasars into yet another perspective, let me tell you about the 100,000th picture taken by the Hubble telescope Snímka v nepravých farbách vznikla kombináciou pozorovaní za štyri dni. Medzi najvýraznejšie zdroje gama žiarenia na snímke patria Mliečna cesta, pulzary a blazary, zvlášť blazar 3C454.3. apod; 16. august: Nastalo čiastočné zatmenie Mesiaca, pričom celý priebeh úkazu bol pozorovateľný zo územia Slovenska

new metagalactic sources 1739+522, z=1.375 and 3c454.3, z=0.859 with fluxes (0.43±0.17)•10−12 and (0.47±0.18)•10−12 accordingly. The energy spectra at energy region from 0.8 to 10 TeV were measured and the source images are pre-sented (Fig. 1). The galactic source Cygnus X-3 known more than for 10 years a Quelques sources extragalactiques sont également détectées, dont le blazar 3C454.3. 2. Le 16 septembre 2008, pendant une centaine de seconde, dans la direction du ciel indiquée par un petit rond blanc sur la carte, une source est soudainement apparue, qui était plus brillante que tout le reste du ciel : c'était le sursaut gamma GRB 080916C Large VLBA Project BEAM-ME (successor to VLBA-BU-BLAZAR): Total & Polarized Intensity Images of Gamma-Ray Bright Blazars at 43 & 86 GHz. Above left: Movie of the jet of gamma-ray bright quasar 1222+216 (or 4C21.35), at a redshift of 0.435 (distance of 3.8 billion light-years), so that 0.5 mas (milli-arcseconds) corresponds to 9.2 light-years.

Clues on high-energy emission mechanism from blazar 3C 454

CHAPTER 3: RADIO MONITORING OF SOUTHERN BLAZARS 51 Table 3.2: The ATCA blazar monitoring observations. Day numbering begins on January 1, 1997. Start date Epoch MJD-50450 Duration (h) 1997-May-08 1997.35 128 24 1997-Jul-04 1997.51 185 24 1997-Sep-02 1997.67 245 27 1997-Oct-31 1997.83 304 28.5 1998-Jan-02 1998.01 367 24.5 1998-Jan-27 1998.07 392. The mission's First Light image shows blazar 3C454.3, the brightest blazar in the sky during the early months of the mission. SSI's Senior Research Scientist Ann Wehrle (LaCanada, CA Office) and colleagues simultaneously observed the blazar with the Spitze blazar, 3C454.3, using IR and optical obser-vations from the SMARTS telescopes, optical, UV and X-ray data from the Swift satellite, and public-release -ray data from the Fermi Space Telescope. They find an excellent correlation between the IR, optical, UV and gamma-ray light curves, with a time lag of less than one day Application to the FSRQ 3C454.3 (GeV blazar, not TeV!) I External photon eld considered: dust torus + combination of emission lines I SED well reproduced in two di erent ux states I Break in the Fermi/LAT spectrum well reproduced (due to : intrinsic curved particle population, transition to Klein-Nishina regime, superposition of EIC on di eren

3C454.3 reveals the structure and physics of its 'blazar zone

Blazar 3C454.3 Vercellone et al. 2011. F.Longo et al. -- 45 Gamma Ray Bursts GRB 100724B GRB 090510 Del Monte et al. 2011 Giuliani et al. 2010. F.Longo et al. -- 46 Upper limits in GRB Longo et al. 2012. F.Longo et al. -- 47 Galactic Transients: Cygnus X3 Tavani et al. 2009 3C454.3: In 2009 and 2010, Fermi's LAT recorded a series of flares from the blazar 3C 454.3. In November 2010, 3C454.3 briefly was the brightest object in the gamma-ray sky. The source is a particle jet powered by the galaxy's supermassive black hole. This blazar is 7 billion light-years away, but i Blazar 3C 454.3 in outburst and quiescence during 2005-2007: Two Variable Synchrotron Emission Peaks, Patrick M. Ogle, Ann E. Wehrle, Thomas Balonek, Mark A. Gurwell, The Astrophysical Journal Supplement, 195, Issue 2, article id. 19, 20 pp (2011) Photopolarimetry of Blazar 3C454. 3 from MIRO more by Kiran Baliyan The Blazar 3C 454.3 has been active in Gamma-rays, optical and X- rays since Sept. 2009 ( Atel #2181, #2200, #2201) The core shift effect in the blazar 3C 454.3 3397 Figure 1. Naturally weighted total intensity CLEAN images of 3C 454.3. The image peaks are 3.3, 3.4, 6.3, 12.0, 15.8 and 23.5 Jy beam−1,forthe4.6,5.0, 8.4, 15.4, 23.8 and 43.2GHz frequencies, respectively. The contours starting at 6 mJy beam−1 are plotted with a factor of 4 steps at all.

and X-minimaps of the blazar 3C454.3, a source which was extremely variable dur-ing the Planck mission (see, e.g., Fuhrmann et al. 2014), and the similarly bright FR-II radio galaxy Cygnus A, where we also see bright extended emission from the Galaxy. While 3C454.3 reveals its variability by an ex-tremely large value X max = 458:3, the emis Blazar 3C454.3の観測 8月のフレアの国際キャンペーンに参加 11月下旬:AGILE衛星によるGeVγ線フレア検出 再び国際キャンペーン,Suzaku(ToO)との同時観測 Suzak Blazar 3C454.3 merupakan Blazar yang bisa diamati dari bumi yang mana mempunya magnitudo mutlak sebesar -31.4. Spoiler for Blazar 3C454.3: Quote: Untuk melihat perspektif lain dari quasar, silahkan agan dan aganwati lihat dari foto yang dihasilkan dari teleskop hubble di bawah ini 3/17. Calorimetric neutrino expectations from bright blazars Motivation Short Blazar Flares Track-like •Short blazar flares yield only a small (calorimetric) neutrino detection probability 1 3C454.3 1.36 × 10−4 3.25 ± 0.15 × 10−9 5.48 13.1 The friction in the disc creates a quasar which shine thousands of times more brightly than galaxies containing billions of stars. And, if a large portion of the quasar's energy is ejected towards Earth, it's known as a blazar. And the brightest known object is Blazar 3C454.3

NASA - Fermi Sees Brightest-Ever Blazar FlareImages gamma de l&#39;Univers

シナリオ1と3は 常に同じ方向の偏光面回転を予測するがシナリオ1と3は、 常に同じ方向の偏光面回転を予測するが 、 3C279では過去に逆方向の回 転が観測されている (Larionov+08).3C454.3でも観測されている(Sasada+10) 3). Absolute position offsets between optical observations and radio positions need to be measured on the ~10-50 µas level. This requires a stable, space-based optical interferometer and contemporaneous VLBI measurements. Figure 3. Overlay of a 3 mm radio image of the blazar 3C454.3 (Krichbaum, et al. 1999) on Flaring Blazars: 3C454.3 (Abdo et al. 2009) ¥ Well-known blazar, at z = 0.859. Detected by EGRET, AGILE. Very active (bright, rapidly variable) since 2000 ¥Fermi-LAT data show rapid, quasi-symmetric, flares on a time scale of ~3 days ¥First observation of a spectral break in the spectrum of a high luminosity blazar above 100MeV

Blazar! As#of#today,#about3,150# blazars#are#known#(Bzcat,edi(on#4.1, Massaro#etal.#2012).## # This#number#is#increasing#rapidly#butitremains#asmall#percentage FOAqr Star 3.9⋅10 −143.9⋅10 —— 3C454.3 Blazar 2.9⋅10 −142.9⋅10 1.2⋅10−14 4.5⋅10−14 EVLac Star 1.8⋅10 −141.8⋅10. The gamma-ray spectra and uxes of known blazar s Mkn421, Mkn501 as the spectrum of NGC1275 and distant at-spectrum radio quasars 1739+522 and 3c454.3 are presented: for NGC 1275(z=0.0179) k = 2:25 0:10 , k on = 2:13 0:09 , k off = 1:72 0:09 ; for Mkn 421 (z=0.031) Quasars: 2 (blazar 3c454.3, QSO 0957+561) Protoplanetaire schijfen: 1 (m42) Nova's in extra galactische stelsels: 4 (m31), 1(m81) Hanny's voorwerp. SiriusB (witte dwerg) B324 ster in extra galactisch stelsel M33. M87 de Jet van de Black Hole . Het verste waargenomen object: NGC 4290 afstand 144 miljoen lichtjaar

the case of 3c454.3 Francesco Longo (University of Trieste and INFN Trieste) Material from P.Bruel, M.Razzano, S.Buson and R.Desiante PhD course 2017 - Padova 2 Outline • Overview of the Fermi Large AreaTelescope ! How it works ! LAT data ! LAT performance • Fermi Science Tools ! General Introductio OBJECT (SHV): TYP: GALAXY: RA DE: MAX: MIN: OBOR: NOTE: 1: 3C 66A (And) blazar: unknown: 02 22 39.6115 +43 02 07.799: 13: 15: V: z = 0.444 long term monitoring one. Blazar 3c454.3 quasar. 7.000.000.000 lichtjaar . Hanny's Voorwerp. Het voorwerp is zichtbaar omdat het aan gestraalt word door IC 2497. Sirius B. Is een witte dwerg die een sterk elliptische baan heeft rond Sirius. Protoplanetaire schijf in Messier 42. Een protoplanetair stelsel is een zonnestelsel in wording Blazar 3C 454.3 . Brightest extragalactic source In the FERMI-LAT catalog blazar 3C454.3 z=0.859. Cumulative Flux (1015 sources) Gamma Rays in [1-100 GeV] energy interval. Resolved flux Unresolved flux . Gamma Rays in [1-100 GeV] energy interval. Resolved flux Unresolved flu 1. Blazar gamma-ray duty-cycle Stecker and Salamon, 1996 Vercellone et al., 2004 2. Radio - gamma-ray relationship Padovani et al., 1993 Y Dondi & Ghisellini, 1996 Y Mucke et al., 1997 N Jorstad et al., 2001 Y 3. Lorentz factor and Doppler factor Kellermann et al., 2004 4. Structured Jets (radio galaxies) Ghisellini et al., 200

Invited talk titled Accretion Disk-Jet Connection in the Blazar Mrk 421 at the AstroSat View of AGN Central Engines, IUCAA, Pune, India. 2017 eptember Invited talk titled Characteristic Timescale in the X-Ray Variabil-ity of the Blazar Mrk 421 at the Astrosat Science Meet, ISRO Headquarters, Bengaluru, India Outburst of 3C 454.3 in 2009 December, Publications of the Astronomical Society of Japan(査読あり), Vol.64, 2012, Article No.58, 8, DOI: 10.1093/pasj/64.3.58 12. Ackermann, et al.(219 人中196番目), Multi-wavelength Observations of Blazar AO 0235+164 in the 2008-2009 Flaring State, The Astrophysica

The detection of the blazar S4 0954+65 at very-high-energy with the MAGIC telescopes during an exceptionally high optical state: Magic Collaboration: Ahnen, M.L. Jorstad, S.G., Marscher, A.P., et al. 2018: Astronomy & Astrophysics: 617: A30 (15 pages) Multiwavelength observations of the blazar BL Lacertae: a new fast TeV gamma-ray flar Een blazar is een zeer compacte quasar (quasi-stellaire radiobron) die geassocieerd is met een superzwaar zwart gat in het centrum van een actief reusachtig elliptisch sterrenstelsel.Ze bezitten een relativistische jet die ongeveer gericht is naar de Aarde. Blazars behoren tot de meest energetische bronnen in het heelal en zijn een belangrijk onderzoeksobject in de extragalactische astronomie In Chapter 5 I describe the analysis and interpretation of the data from the blazar 3C454.3, which is one of the farthest sources observed by MAGIC. Even though we just obtained an upper limit on the emission flux, this can constrain theoretical models. Par bla·zar (blā′zär′, -sär′, -zər, -sər) n. A compact, extremely bright, active galactic nucleus characterized by strong and rapid changes in the intensity of electromagnetic radiation emitted over a very broad range of frequencies ranging from radio waves to gamma rays. Although the source of blazar energy is the material surrounding a super. 3$ 2030 2040 2050 2060 1013$ 1014$ 1015$ ILC$!!!!Suzuki's!Challenge:!When!can!we!reach!1!PeV? $ Laser plasma accelerator experiments$ V. Yakimenko (BNL) and R. Ischebeck (SLAC), AAC2006 Summary report of WG