Galaxies

Editorial

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2 pages, 161 KiB

Open AccessEditorial

The Conference Blazars through Sharp Multi-Wavelength Eyes

by Alan P. Marscher^1,*

, Jose L. Gómez² and Svetlana G. Jorstad^1,3

¹ Institute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA

² Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080, Granada, Spain

³ Astronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, Russia

Galaxies 2016, 4(3), 21; https://doi.org/10.3390/galaxies4030021 - 1 Sep 2016

Cited by 1 | Viewed by 2897

Abstract

Blazars are active, galactic nuclei with jets of magnetized, high-energy plasma that ﬂow outward from the center of the host galaxy at near-light speeds.[...] Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

Research

Jump to: Editorial, Review

8 pages, 659 KiB

Open AccessArticle

The Disk-Driven Jet of Cygnus A

by Bia Boccardi^*, Thomas P. Krichbaum

and Uwe Bach

Max-Planck-Institut für Radioastronomie, 53121 Bonn, Germany

Galaxies 2017, 5(2), 22; https://doi.org/10.3390/galaxies5020022 - 28 Apr 2017

Cited by 1 | Viewed by 4256

Abstract

Recently published results from VLBI observations at 3 and 7 millimeters of the radio galaxy Cygnus A are reviewed in this article, and discussed within the model of a prominently stratified jet outflow. At the source redshift (

z =

0.056), mm-VLBI allows [...] Read more.

Recently published results from VLBI observations at 3 and 7 millimeters of the radio galaxy Cygnus A are reviewed in this article, and discussed within the model of a prominently stratified jet outflow. At the source redshift (

z =

0.056), mm-VLBI allows a spatial resolution down to 200 Schwarzschild radii to be achieved, providing an extremely detailed view of the two-sided jet base. Through a study of the kinematic properties of the flow and of its transverse structure, it is shown that the radio emission is produced by an accelerating, mildly relativistic, parabolically expanding disk-wind. The observed transverse stratification, both of the flux density and of the bulk speed, supports the presence of an invisible faster spine close to the jet axis, powered either by the inner regions of the accretion disk or by the spinning black hole. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 1528 KiB

Open AccessArticle

Gaussian Processes for Blazar Variability Studies

by Vassilis Karamanavis

Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany

Galaxies 2017, 5(1), 19; https://doi.org/10.3390/galaxies5010019 - 17 Mar 2017

Cited by 4 | Viewed by 4433

Abstract

This article briefly introduces Gaussian processes as a new approach for modelling time series in the field of blazar physics. In the second part of the paper, recent results from an application of GP modelling to the multi-wavelength light curves of the blazar [...] Read more.

This article briefly introduces Gaussian processes as a new approach for modelling time series in the field of blazar physics. In the second part of the paper, recent results from an application of GP modelling to the multi-wavelength light curves of the blazar PKS 1502+106 are discussed. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 2713 KiB

Open AccessArticle

Long-Term Monitoring of Bright Blazars in the Multi-GeV to TeV Range with FACT

by Fabian Temme^1,*, Jan Adam¹, Max L. Ahnen², Dominik Baack¹, Matteo Balbo³, Matthias Bergmann⁴, Adrian Biland², Michael Blank⁴, Thomas Bretz²

, Kai A. Brügge¹, Jens Buss¹, Anton Dmytriiev³, Daniela Dorner⁴

, Sabrina Einecke¹, Christina Hempfling⁴, Dorothee Hildebrand², Gareth Hughes², Lena Linhoff¹, Karl Mannheim⁴, Sebastian Müller²

, Dominik Neise², Andrii Neronov³, Max Nöthe¹, Aleksander Paravac⁴, Felicitas Pauss², Wolfgang Rhode¹, Amit Shukla², Julia Thaele¹ and Roland Walter³ Show full author list Hide full author list

¹ TU Dortmund, Experimental Physics 5, Otto-Hahn-Str. 4, 44221 Dortmund, Germany

² ETH Zurich, Institute for Particle Physics, Otto-Stern-Weg 5, 8093 Zurich, Switzerland

³ ISDC Data Center for Astrophysics, University of Geneva, Chemin d’Ecogia 16, 1290 Versoix, Switzerland

⁴ Institute for Theoretical Physics and Astrophysics, Universität Würzburg, Emil-Fischer-Str. 31, 97074 Würzburg, Germany

Galaxies 2017, 5(1), 18; https://doi.org/10.3390/galaxies5010018 - 20 Feb 2017

Cited by 4 | Viewed by 6754

Abstract

Blazars like Markarian 421 or Markarian 501 are active galactic nuclei (AGN), with their jets orientated towards the observer. They are among the brightest objects in the very high energy (VHE) gamma ray regime (>100 GeV). Their emitted gamma-ray fluxes are extremely variable, [...] Read more.

Blazars like Markarian 421 or Markarian 501 are active galactic nuclei (AGN), with their jets orientated towards the observer. They are among the brightest objects in the very high energy (VHE) gamma ray regime (>100 GeV). Their emitted gamma-ray fluxes are extremely variable, with changing activity levels on timescales between minutes, months, and even years. Several questions are part of the current research, such as the question of the emission regions or the engine of the AGN and the particle acceleration. A dedicated longterm monitoring program is necessary to investigate the properties of blazars in detail. A densely sampled and unbiased light curve allows for observation of both high and low states of the sources, and the combination with multi-wavelength observation could contribute to the answer of several questions mentioned above. FACT (First G-APD Cherenkov Telescope) is the first operational telescope using silicon photomultiplier (SiPM, also known as Geigermode—Avalanche Photo Diode, G-APD) as photon detectors. SiPM have a very homogenous and stable longterm performance, and allow operation even during full moon without any filter, leading to a maximal duty cycle for an Imaging Air Cherenkov Telescope (IACT). Hence, FACT is an ideal device for such a longterm monitoring of bright blazars. A small set of sources (e.g., Markarian 421, Markarian 501, 1ES 1959+650, and 1ES 2344+51.4) is currently being monitored. In this contribution, the FACT telescope and the concept of longterm monitoring of bright blazars will be introduced. The results of the monitoring program will be shown, and the advantages of densely sampled and unbiased light curves will be discussed. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 474 KiB

Open AccessArticle

The Statistical Study of the Daily Fermi Light Curves of 130 Sources

by Wei Cai^1,2, Yi Liu^1,2,*

and Jun H. Fan^1,2

¹ Center for Astrophysics, Guangzhou University, Guangzhou 510006, China

² Department of Education, Astronomy Science and Technology Research Laboratory, Guangdong Province, Guangzhou 510006, China

Galaxies 2017, 5(1), 14; https://doi.org/10.3390/galaxies5010014 - 11 Feb 2017

Cited by 1 | Viewed by 4453

Abstract

Blazars show rapid and high amplitude variability. It is interesting to question what kind of process the variability corresponds to. Maybe it is a result of the instability of the accretion flows. In this work, Fermi daily light curves of 130 sources are [...] Read more.

Blazars show rapid and high amplitude variability. It is interesting to question what kind of process the variability corresponds to. Maybe it is a result of the instability of the accretion flows. In this work, Fermi daily light curves of 130 sources are analyzed, and the distributions of daily variability are compared by using a Kolmogorov–Smirnov (K-S) test. The results can be summarized as follows:(1) in most cases, the distributions are not Gaussian; (2) some pairs of the distributions are similar. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 898 KiB

Open AccessArticle

Study of the Time-Series of Microvariability in Kepler Blazar W2R 1926+42

by Mahito Sasada^1,*

, Shin Mineshige², Shinya Yamada³ and Hitoshi Negoro⁴

¹ Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA

² Department of Astronomy, Graduate School of Science, Kyoto University, Kyoto 606-8502, Japan

³ Department of Physics, Tokyo Metropolitan University, Tokyo 192-0397, Japan

⁴ Department of Physics, Nihon University, Tokyo 101-8308, Japan

Galaxies 2017, 5(1), 13; https://doi.org/10.3390/galaxies5010013 - 8 Feb 2017

Viewed by 3317

Abstract

One of the remarkable features of blazars is violent variability over a wide wavelength range. The variation mechanism causing the observed complex behavior is still under debate. The variability timescales range from less than a day to decades. Variation on timescales less than [...] Read more.

One of the remarkable features of blazars is violent variability over a wide wavelength range. The variation mechanism causing the observed complex behavior is still under debate. The variability timescales range from less than a day to decades. Variation on timescales less than a day is known as “microvariability.” Such short-term variations can provide insights regarding the origin of the variability after they are distinguished from longer-term variational components. We select about 195 microvariability events from the continuous light curve of blazar W2R 1926+42 with 1-min time resolution obtained by the Kepler spacecraft, and estimate the timescale and amplitude of each event. The rise and decay timescales of the events reveal random variations over short timescales less than a day, but they indicate systematic variations on timescales longer than several days. This result implies that the events are not independent, but rather mutually correlated. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 1910 KiB

Open AccessArticle

OJ 287 as a Rotating Helix

by Marshall H. Cohen

Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA

Galaxies 2017, 5(1), 12; https://doi.org/10.3390/galaxies5010012 - 8 Feb 2017

Cited by 28 | Viewed by 5861

Abstract

We present preliminary data from high-cadence 15-GHz VLBA images of OJ 287 from 1995 to 2015. The ridgelines suggest that the jet is rotating, perhaps with a period of∼30 years. The EVPA of the core rotated by 240° in 2001–2002 and decreased slowly [...] Read more.

We present preliminary data from high-cadence 15-GHz VLBA images of OJ 287 from 1995 to 2015. The ridgelines suggest that the jet is rotating, perhaps with a period of∼30 years. The EVPA of the core rotated by 240° in 2001–2002 and decreased slowly after that. The inner jet apparently moved to a new direction after the rotation,as shown by the emergence of a new component at a new PA at 43 GHz, in 2004. This was presaged by a strong rise in the ﬂux density of the core, and then its sudden fall as the new component was identiﬁed. The equivalent sequence of events took place about 5 years later at 15 GHz, but in addition the core EVPA had a step in 2006 and moved to be aligned with the new 43-GHz component. The 15-GHz core became optically thin in 2006, but the angular resolution was insufﬁcient to separate the new component from the core until 2010 Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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10 pages, 1834 KiB

Open AccessArticle

The Origin and Structure of the Magnetic Fields and Currents of AGN Jets

by Denise Gabuzda

Physics Department, University College Cork, Cork, Ireland

Galaxies 2017, 5(1), 11; https://doi.org/10.3390/galaxies5010011 - 2 Feb 2017

Cited by 8 | Viewed by 6532

Abstract

This paper reviews observational evidence obtained to date about the overall structure of the magnetic ﬁelds in the jets of Active Galactic Nuclei (AGN). Because they are sensitive to the line-of-sight magnetic-ﬁeld component, Faraday rotation observations of AGN jets provide an effective tool [...] Read more.

This paper reviews observational evidence obtained to date about the overall structure of the magnetic ﬁelds in the jets of Active Galactic Nuclei (AGN). Because they are sensitive to the line-of-sight magnetic-ﬁeld component, Faraday rotation observations of AGN jets provide an effective tool for searching for toroidal jet magnetic ﬁelds, whose line-of-sight component changes systematically across the jet. Transverse Faraday rotation measure (RM) gradients providing direct evidence for helical/toroidal magnetic ﬁelds have been reliably detected in nearly 40 AGN on parsec scales. Helical magnetic ﬁelds are believed to form due to the combined action of the rotation of the central black hole and accretion disk, and these observations demonstrate that at least some of this helical ﬁeld survives to distances well beyond the Very Long Baseline Interferometry (VLBI) core. Observations of reversals in the direction of the transverse RM gradients in a number of AGN provide evidence for a“return”magnetic ﬁeld forming a nested helical-ﬁeld structure with oppositely directed azimuthal components in the inner and outer regions of the helical magnetic ﬁeld. The collected data now provide ﬁrm evidence for a predominance of inward jet currents on parsec scales and outward currents on scales greater than a few tens of parsecs. This suggests a global pattern of magnetic ﬁelds and currents with an inward current near the jet axis and an outward current farther from the jet axis, with these currents closing in the accretion disk and far out in the radio lobes, forming a self-consistent set of ﬁelds and currents together with the implied nested helical-ﬁeld structure. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 2675 KiB

Open AccessArticle

The Power of (Near) Simultaneous Multi-Frequency Observations for mm-VLBI and Astrometry

by María J. Rioja^1,2,3,*,†

, Richard Dodson^1,†, José L. Gómez^4,†, Sol N. Molina^4,†

, Taehyun Jung^5,† and Bong Won Sohn^5,†

¹ International Centre for Radio Astronomy, M468, University of Western Australia, 35 Stirling Hwy, 6009 Perth, Australia

² Commonwealth Scientific and Industrial Research Organisation Astronomy and Space Science, 26 Dick Perry Avenue, 6151 Kensington, Australia

³ Observatorio Astronómico Nacional-IGN, Alfonso XII, 3 y 5, 28014 Madrid, Spain

⁴ Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, E-18008 Granada, Spain

⁵ Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, 305-348 Daejeon, Korea

^† These authors contributed equally to this work.

Galaxies 2017, 5(1), 9; https://doi.org/10.3390/galaxies5010009 - 24 Jan 2017

Cited by 7 | Viewed by 4244

Abstract

Simultaneous or near-simultaneous observations at multiple frequency bands have the potential to overcome the fundamental limitation imposed by the atmospheric propagation in mm-VLBI observations. The propagation effects place a severe limit in the sensitivity achievable in mm-VLBI, reducing the time over which the [...] Read more.

Simultaneous or near-simultaneous observations at multiple frequency bands have the potential to overcome the fundamental limitation imposed by the atmospheric propagation in mm-VLBI observations. The propagation effects place a severe limit in the sensitivity achievable in mm-VLBI, reducing the time over which the signals can be coherently combined, and preventing the use of phase referencing and astrometric measurements. We present two demonstrations of the power of (near) simultaneous multi-frequency observations with the KVN and VLBA, and our recently developed analysis strategies to enable new measurements at mm-VLBI. The first case comprises simultaneous observations at 22, 43, 87 and 130 GHz of a group of five AGNs, the weakest of which is ∼200 mJy at 130 GHz, with angular separations ranging from 3.6 to 11 degrees, using the KVN. We analysed this data using the Frequency Phase Transfer (FPT) and the Source Frequency Phase Referencing (SFPR) techniques, which use the observations at a lower frequency to correct those at a higher frequency. The results of the analysis provide an empirical demonstration of the increase in the coherence times at 130 GHz from a few tens of seconds to about twenty minutes, with FPT, and up to many hours with SFPR. Moreover the astrometric analysis provides high precision relative position measurements between two frequencies, including, for the first time, astrometry at 130 GHz. The second case is a variation of the above, whereby adding dedicated wide-band cm-wavelength observations to measure the ionosphere eliminates the need for a second, calibrator, source. This addresses the scarcity of calibrators at mm-VLBI. We dubbed this technique Multi Frequency Phase Referencing (MFPR). We present bona fide astrometrically aligned VLBA images of BL Lacertae at 22 and 43 GHz using MFPR, which, combined with results from conventional phase referencing at cm-wavelengths, suggests the VLBI core has a recollimation shock that is revealed at mm-wavelengths. These shocks could be responsible for the γ-ray emission in blazar jets. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 3063 KiB

Open AccessArticle

Proper Motions of Jets on the Kiloparsec Scale: New Results with HST

by Eileen T. Meyer^1,*

, William B. Sparks², Markos Georganopoulos¹, Roeland Van der Marel², Jay Anderson², Sangmo T. Sohn², John Biretta², Colin Norman², Marco Chiaberge² and Eric Perlman³

¹ Department of Physics, University of Maryland, Baltimore County, Baltimore, MD 20742, USA

² Space Telescope Science Institute, Baltimore, MD 21218, USA

³ Florida Institute of Technology, Melbourne, FL 32901, USA

Galaxies 2017, 5(1), 8; https://doi.org/10.3390/galaxies5010008 - 20 Jan 2017

Cited by 19 | Viewed by 4456

Abstract

The Hubble Space Telescope recently celebrated 25 years of operation. Some of the first images of extragalactic optical jets were taken by HST in the mid-1990s; with time baselines on the order of 20 years and state-of-the-art astrometry techniques, we are now able [...] Read more.

The Hubble Space Telescope recently celebrated 25 years of operation. Some of the first images of extragalactic optical jets were taken by HST in the mid-1990s; with time baselines on the order of 20 years and state-of-the-art astrometry techniques, we are now able to reach accuracies in proper-motion measurements on the order of a tenth of a milliarcsecond per year. We present the results of a recent HST program to measure the kiloparsec-scale proper motions of eleven nearby optical jets with Hubble, the first sample of its kind. When paired with VLBI proper-motion measurements on the parsec scale, we are now able to map the full velocity profile of these jets from near the black hole to the final deceleration as they extend out into and beyond the host galaxy. We see convincing evidence that weak-flavor jets (i.e., FR Is) have a slowly increasing jet speed up to 100 pc from the core, where superluminal components are first seen. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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4 pages, 885 KiB

Open AccessArticle

Optical and Gamma-Ray Variability of the vRL NLSy1 Galaxy, 1H 0323+342

by Hugh R. Miller^*, Clay. S. Turner, Jeremy D. Maune and Joseph R. Eggen

Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30302-3965, USA

Galaxies 2017, 5(1), 7; https://doi.org/10.3390/galaxies5010007 - 20 Jan 2017

Cited by 3 | Viewed by 3635

Abstract

1H 0323+342 was one of the first vRLNLSy1 galaxies detected at gamma-rays with the Fermi-LAT and is one of the brightest of this class observed at optical wavelengths. We report the results of monitoring the optical flux, polarization and the gamma-ray flux of [...] Read more.

1H 0323+342 was one of the first vRLNLSy1 galaxies detected at gamma-rays with the Fermi-LAT and is one of the brightest of this class observed at optical wavelengths. We report the results of monitoring the optical flux, polarization and the gamma-ray flux of 1H 0323+342 during the past ~5 years. In some cases, the optical flux has been monitored on timescales as short as ~minutes simultaneously with two telescopes, demonstrating, for the first time, the reality of microvariability events with durations as short as ~15 min for this object. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 234 KiB

Open AccessArticle

Multifrequency Study of the Blazar 3C 454.3

by Ilhuiyolitzin Villicaña-Pedraza^1,*, Francisco Carreto-Parra^2,3

, Alberto Carramiñana⁴ and Julio Saucedo-Morales⁵

¹ Departamento de Física Teórica, Universidad Autónoma de Madrid, Madrid 28049, Spain

² Science Department, New Mexico State University, Las cruces, NM 88003, USA

³ Departament of science VV, El Paso Community College, El Paso, TX 79915, USA

⁴ Coordinación de Astrofísica, Instituto Nacional de Astrofísica, Óptica y Electrónica, Puebla 72840, México

⁵ Departamento de Investigación en Física, Universidad de Sonora, Hermosillo Sonora 83000, México

Galaxies 2017, 5(1), 3; https://doi.org/10.3390/galaxies5010003 - 30 Dec 2016

Cited by 2 | Viewed by 4575

Abstract

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 [...] Read more.

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 [2800 Angstroms] and FeII emission line features. We have obtained optical magnitudes and color indices of the quasar and performed a correlation between the optical, IR, and gamma-ray light curves. We have found statistically significant correlations between the light curves at different wavelengths. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 1402 KiB

Open AccessArticle

A New Statistical Approach to the Optical Spectral Variability in Blazars

by Jose A. Acosta-Pulido^1,2,*, Noel Castro Segura^1,2, Maria Isabel Carnerero^2,3 and Claudia M. Raiteri³

¹ Instituto de Astrofisica de Canarias-Spain, La Laguna E38205, Spain

² Dpto de Astrofisica, University La Laguna-Spain, La Laguna E38206, Spain

³ INAF-Osservatorio Astrofisico di Torino, Pino Torinese (TO) 10025, Italy

Galaxies 2017, 5(1), 1; https://doi.org/10.3390/galaxies5010001 - 28 Dec 2016

Cited by 5 | Viewed by 4403

Abstract

We present a spectral variability study of a sample of about 25 bright blazars, based on optical spectroscopy. Observations cover the period from the end of 2008 to mid 2015, with an approximately monthly cadence. Emission lines have been identified and measured in [...] Read more.

We present a spectral variability study of a sample of about 25 bright blazars, based on optical spectroscopy. Observations cover the period from the end of 2008 to mid 2015, with an approximately monthly cadence. Emission lines have been identified and measured in the spectra, which permits us to classify the sources into BL Lac-type or FSRQs, according to the commonly used EW limit. We have obtained synthetic photometry and produced colour-magnitude diagrams which show different trends associated with the object classes: generally, BL Lacs tend to become bluer when brighter and FSRQs become redder when brighter, although several objects exhibit both trends, depending on brightness. We have also applied a pattern recognition algorithm to obtain the minimum number of physical components which can explain the variability of the optical spectrum. We have used NMF (Non-Negative Matrix Factorization) instead of PCA (Principal Component Analysis) to avoid un-realistic negative components. For most targets we found that 2 or 3 meta-components are enough to explain the observed spectral variability. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 822 KiB

Open AccessArticle

The Structure and Propagation of the Misaligned Jet M87

by Kazuhiro Hada

Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan

Galaxies 2017, 5(1), 2; https://doi.org/10.3390/galaxies5010002 - 26 Dec 2016

Cited by 28 | Viewed by 7285

Abstract

Due to its proximity, M87 is a prime target for next-generation high-resolution VLBI at short millimeter wavelengths, by which the jet launching region and the black hole shadow are expected to be resolved and imaged sometime soon. Along with this situation, high-quality VLBI [...] Read more.

Due to its proximity, M87 is a prime target for next-generation high-resolution VLBI at short millimeter wavelengths, by which the jet launching region and the black hole shadow are expected to be resolved and imaged sometime soon. Along with this situation, high-quality VLBI imaging and monitoring at lower frequencies play an important role in complementing the high-frequency data. Here, we present our recent and ongoing observational studies of the M87 jet on pc-to-subpc scales based on ultra-deep VLBI imaging programs at 86 GHz and 15 GHz. The high-dynamic-range images have allowed us to obtain some remarkably improved views on this jet. We also introduce the KVN and VERA Array (KaVA), a new regularly-operating VLBI network in East Asia, which is quite suitable for studying the structure and propagation of relativistic jets. Some early results from our pilot study for M87—including the detection of superluminal motions near the jet base—implying an efficient magnetic-to-kinetic conversion at these scales, are reported. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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5 pages, 1175 KiB

Open AccessArticle

Conical Stream of the Two-Sided Jets in NGC 4261 over the Range of 10³–10⁹ Schwarzschild Radii

by Satomi Nakahara^1,2,*, Akihiro Doi^1,2, Yasuhiro Murata^1,2, Kazuhiro Hada³

, Masanori Nakamura⁴ and Keiichi Asada⁴

¹ Department of Space and Astronautical Science, The Graduate University for Advanced Studies, 3-1-1 Yoshinodai, Chuou-ku, Sagamihara, Kanagawa 252-0222, Japan

² The Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuou-ku, Sagamihara, Kanagawa 252-5210, Japan

³ National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

⁴ Institute of Astronomy & Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan

Galaxies 2016, 4(4), 80; https://doi.org/10.3390/galaxies4040080 - 20 Dec 2016

Cited by 1 | Viewed by 5067

Abstract

We report the jet width profile of of the nearby (

\sim 30 Mpc

) AGN NGC 4261 for both the approaching jet and the counter jet at radial distances ranging from

\sim 10^{3}

–

10^{9}

Schwarzschild radius ( [...] Read more.

We report the jet width profile of of the nearby (

\sim 30 Mpc

) AGN NGC 4261 for both the approaching jet and the counter jet at radial distances ranging from

\sim 10^{3}

–

10^{9}

Schwarzschild radius (

R_{S}

) from the central engine. Our Very Large Array (VLA) and Very Long Baseline Array (VLBA) observations reveal that the jets maintain a conical structure on both sides over the range

10^{3}

–

10^{9} R_{S}

without any structural transition (i.e., parabolic to conical) like in the approaching jet in M87. Thus, NGC 4261 will provide a unique opportunity to examine the conical jet hypothesis in blazars, while it may require some additional consideration on the acceleration and collimation process in AGN jets. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 887 KiB

Open AccessArticle

Emission Knots and Polarization Swings of Swinging Jets

by Maxim Lyutikov^1,* and Evgeniya Kravchenko²

¹ Department of Physics, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907-2036, USA

² Lebedev Physical Institute, Astro Space Center, Profsoyuznaya 84/32, Moscow 117997, Russia

Galaxies 2016, 4(4), 75; https://doi.org/10.3390/galaxies4040075 - 7 Dec 2016

Viewed by 3438

Abstract

Knots (emission features in jets of active galactic nuclei) often show non-ballistic dynamics and variable emission/polarization properties. We model these features as emission pattern propagating in a jet that carries a helical magnetic field and is launched along a changing direction. The model [...] Read more.

Knots (emission features in jets of active galactic nuclei) often show non-ballistic dynamics and variable emission/polarization properties. We model these features as emission pattern propagating in a jet that carries a helical magnetic field and is launched along a changing direction. The model can reproduce a wide range of phenomena observed in the motion of knots: non-ballistic motion (both smooth and occasional sudden change of direction, and/or oscillatory behavior), variable brightness, and confinement of knots’ motion within an overlaying envelope. The model also reproduces smooth large polarization angle swings, and at the same time allows for the seemingly random behavior of synchrotron fluxes, polarization fraction, and occasional

π / 2

polarization jumps. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 1446 KiB

Open AccessArticle

Multi-Frequency Monitoring of the Flat Spectrum Radio Quasar PKS 1222+216 in 2008–2015

by Ivan Troitskiy^1,*, Daria Morozova¹

, Svetlana Jorstad^1,2

, Valery Larionov¹

, Alan Marscher²

, Ivan Agudo³, Dmitry Blinov^1,4, Paul Smith⁵ and Yuliya Troitskaya¹

¹ Astronomical Institute, St. Petersburg State University, Universitetsky Prospekt, 28, Peterhof, St. Petersburg 198504, Russia

² Institute for Astrophysical Research, Boston University, 725 Commonwealth Ave., Boston, MA 02215, USA

³ Instituto de Astrofisíca de Andalucía, CSIC, Glorieta de la Astronomía, Granada E-18008, Spain

⁴ Department of Physics, Institute for Plasma Physics, University of Crete, Heraklion GR-71003, Greece

⁵ Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721, USA

Galaxies 2016, 4(4), 72; https://doi.org/10.3390/galaxies4040072 - 28 Nov 2016

Cited by 5 | Viewed by 4053

Abstract

We analyze the broadband activity of the flat spectrum radio quasar PKS 1222+216 from 2008 to 2015 using multi-frequency monitoring which involves γ-ray data from the Fermi Large Area Telescope, total intensity and linear polarization observations from different optical telescopes in R [...] Read more.

We analyze the broadband activity of the flat spectrum radio quasar PKS 1222+216 from 2008 to 2015 using multi-frequency monitoring which involves γ-ray data from the Fermi Large Area Telescope, total intensity and linear polarization observations from different optical telescopes in R band, and imaging of the inner jet structure with the Very Long Baseline Array (VLBA) at 43 GHz. During the observations, the source showed several dramatic flares at γ rays and optical bands, with the rising branch of a γ-ray flare accompanied by a rapid rotation of the polarization position angle (EVPA), a fast increase of the degree of polarization in the optical band, brightening of the VLBI core, and appearance of a new superluminal component in the parsec-scale jet. The rapid variability of the optical linear polarization may be explained by a strong turbulence in the jet plasma. We find a correlation between the γ rays, optical R band, and 43 GHz variability on a long-term scale (months and years), and a good general alignment between EVPAs in R band and at 43 GHz, while the correlation between short-term variations (days and weeks) is weaker. Synchronous activity across the bands supports the idea that the emission regions responsible for the γ-ray and optical flares are co-spatial and located in the vicinity of the mm-wave core of the parsec-scale jet. However, these connections do not completely explain the challenging behaviour of PKS 1222+216, since there are some γ-ray flares which are not accompanied by jet events, and vice versa. We need a continuation of multi-frequency monitoring along with high resolution imaging of the parsec-scale jet to understand in detail the origin of high energy emission in blazars. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 2387 KiB

Open AccessArticle

Direct Imaging of a Toroidal Magnetic Field in the Inner Jet of NRAO 150

by Sol N. Molina^1,*

, Iván Agudo¹, José L. Gómez¹, Thomas P. Krichbaum²

, Iván Martí-Vidal³ and Alan L. Roy²

¹ Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080 Granada, Spain

² Max-Planck-Institut für Radioastronomie, auf dem Hugel, 69, 53121 Bonn, Germany

³ Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 43992 Onsala, Sweden

Galaxies 2016, 4(4), 70; https://doi.org/10.3390/galaxies4040070 - 24 Nov 2016

Cited by 2 | Viewed by 4149

Abstract

Most formation models and numerical simulations cause a helical magnetic field to form, accelerate and collimate jets in active galactic nuclei (AGN). For this reason, observational direct evidence for the existence of these helical magnetic fields is of special relevance. In this work, [...] Read more.

Most formation models and numerical simulations cause a helical magnetic field to form, accelerate and collimate jets in active galactic nuclei (AGN). For this reason, observational direct evidence for the existence of these helical magnetic fields is of special relevance. In this work, we present ultra- high-resolution observations of the innermost regions of the jet in the quasar NRAO150. We study the polarization structure and report evidence of a helical magnetic field. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 8740 KiB

Open AccessArticle

Multiwavelength Picture of the Blazar S5 0716+714 during Its Brightest Outburst

by Marina Manganaro^1,*, Giovanna Pedaletti², Marlene Doert³, Denis Bastieri⁴, Vandad Fallah Ramazani⁵, Dario Gasparrini⁶, Elina Lindfors⁵, Benoit Lott⁷, Mireia Nievas⁸

, Bindu Rani⁹, David J. Thompson⁹

, Emmanouil Angelakis¹⁰

, George Borman¹¹, Mark Gurwell¹², Talvikki Hovatta¹³, Ryosuke Itoh¹⁴, Svetlana Jorstad¹⁵

, Alex Kraus¹⁰, Thomas P. Krichbaum¹⁰

, Paul Kuin¹⁶, Anne Lähteenmäki^13,17, Valeri Larionov¹⁸

, Amy Yarleen Lien⁹, Ioannis Myserlis¹⁰, Merja Tornikoski¹³, Ivan Troitsky¹⁸, J. Anton Zensus¹⁰ and The MAGIC and -LAT Collaborations¹ Show full author list Hide full author list

¹ Inst. de Astrofísica de Canarias, E-38200 La Laguna, and Universidad de La Laguna, Dpto. Astrofísica, E-38206 La Laguna, Tenerife, Spain

² Deutsches Elektronen-Synchrotron (DESY), D-15738 Zeuthen, Germany

³ Department of Physics, Technical University of Dortmund, Dortmund D-44221, Germany

⁴ INFN Padova, I-35131 Padova, Italy

⁵ Department of Physics and Astronomy, University of Turku, 20500 Turku, Finland

⁶ ASI Science Data Center and INFN, 06123 Perugia, Italy

⁷ CEN Bordeaux-Gradignan, 33170 Gradignan, France

⁸ Department of Atomic Molecular and Nuclear Physics, Universidad Complutense, E-28040 Madrid, Spain

⁹ NASA’s Goddard Space Flight Center, Greenbelt, MD 20771, USA

¹⁰ Max Planck Institut für Radioastronomie (MPIfR), 53121 Bonn, Germany

¹¹ Crimean Astrophysics Observatory, 98409 Nauchny, Crimea, Russia

¹² Harvard-Smithsonian CfA, Cambridge, MA 02138, USA

¹³ Metsähovi Radio Observatory, Aalto University, FI-02540 Kylmälä, Finland

¹⁴ Department of Physical Science, Hiroshima University, Higashi-hiroshima 739-8526, Japan

¹⁵ Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA

¹⁶ Mullard Space Science Lab., University College London, RH5 6NT Dorking, UK

¹⁷ Department of Radio Science and Engineering, Aalto University, FI-00076 Aalto, Finland

¹⁸ Astronomical Institute, St.-Petersburg State University, St.-Petersburg 198504, Russia

Show full affiliation list Hide full affiliation list

Galaxies 2016, 4(4), 69; https://doi.org/10.3390/galaxies4040069 - 24 Nov 2016

Cited by 3 | Viewed by 5120

Abstract

S5 0716+714 is a well known BL Lac object, and one of the brightest and most active blazars. The discovery in the Very High Energy band (VHE, E > 100 GeV) by MAGIC happened in 2008. In January 2015, the source went through [...] Read more.

S5 0716+714 is a well known BL Lac object, and one of the brightest and most active blazars. The discovery in the Very High Energy band (VHE, E > 100 GeV) by MAGIC happened in 2008. In January 2015, the source went through the brightest optical state ever observed, triggering MAGIC follow-up and a VHE detection with ∼

13 σ

significance (ATel

♯ 6999

). Rich multiwavelength coverage of the flare allowed us to construct the broad-band spectral energy distribution of S5 0716+714 during its brightest outburst. In this work, we will present the preliminary analysis of MAGIC and Fermi-LAT data of the flaring activity in January and February 2015 for the HE (0.1 < HE < 300 GeV) and VHE band, together with radio (Metsähovi, OVRO, VLBA, Effelsberg), sub-millimeter (SMA), optical (Tuorla, Perkins, Steward, AZT-8+ST7, LX-200, Kanata), X-ray and UV (Swift-XRT and UVOT), in the same time-window and discuss the time variability of the multiwavelength light curves during this impressive outburst. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 980 KiB

Open AccessArticle

JVLA Wideband Polarimetry Observations on a Sample of High Rotation Measure Sources

by Alice Pasetto^1,*, Carlos Carrasco-González², Gabriele Bruni¹

, Aritra Basu¹

, Shane O’Sullivan³, Alex Kraus¹ and Karl-Heinz Mack⁴

¹ Max-Planck Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, D-53121 Bonn, Germany

² Instituto de Radioastronomía y Astrofísica (IRyA-UNAM), Antigua Carretera a Pátzcuaro 8701, 58089 Morelia, Michoacán, Mexico

³ Instituto de Astronomía (IA-UNAM), Circuito Exterior, área de la Investigación Científica, Ciudad Universitaria, Ciudad de México C.P. 04510 , México

⁴ Istituto di Radioastronomia (IRA-INAF), Via Gobetti 101, I-40129 Bologna, Italy

Galaxies 2016, 4(4), 66; https://doi.org/10.3390/galaxies4040066 - 24 Nov 2016

Cited by 4 | Viewed by 4699

Abstract

We present preliminary results of JVLA wideband full polarization observations of a sample of Active Galactic Nuclei (AGN) with very high Rotation Measure (RM) values, a sign of extreme environment. Polarization properties show a complex behaviour such that the polarization angle (PA) and [...] Read more.

We present preliminary results of JVLA wideband full polarization observations of a sample of Active Galactic Nuclei (AGN) with very high Rotation Measure (RM) values, a sign of extreme environment. Polarization properties show a complex behaviour such that the polarization angle (PA) and fractional polarization (fp) change dramatically within the wide band. The measured RM is not constant within the wide band. Its complex behaviour reflects the complexity of the medium with the presence of several Faraday components. The depolarization has been studied by modelling the variations of the Stokes parameters Q and U together with the polarization parameters (PA and fp) with wavelength using combinations of the simplest existing depolarization models. With this JVLA study we could spectrally resolve multiple polarized components of unresolved AGN. These preliminary results reveal the complexity of these objects, but improvements to the depolarization modelling are needed to better understand the polarization structure of these sources. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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5 pages, 611 KiB

Open AccessArticle

Multiwavelength Monitoring of the Gamma-Bright Blazar Mkn 421

by Yulia Troitskaya^1,*, Valeri Larionov¹

, Vladimir Hagen-Thorn¹, Daria Morozova¹

, Dmitry Blinov^1,2, George Borman³, Tatiana Grishina¹, Natalia Efimova^1,4, Evgenia Kopatskaya¹, Liudmila Larionova¹, Elena Larionova¹, Ivan Troitsky¹ and Anna Mokrushina^1,4

¹ St. Petersburg State University, Universitetsky Prospekt, 28, Peterhof, St. Petersburg 198504, Russia

² Department of Physics, Institute for Plasma Physics, University of Crete, Heraklion GR-71003, Greece

³ Crimean Astrophysical Observatory, P/O Nauchny, Crimea 298409, Russia

⁴ Pulkovo Observatory of Russian Academy of Sciences, Pulkovskoye Chaussee 65, Saint-Petersburg 196140, Russia

Galaxies 2016, 4(4), 67; https://doi.org/10.3390/galaxies4040067 - 23 Nov 2016

Viewed by 4101

Abstract

We present the results of photo-polarimetric monitoring observations of the blazar Markarian 421 carried out with different telescopes (the 0.4 m telescopes of St. Petersburg State University and the Pulkovo Observatory, the 0.7 m telescope of the Crimean Astrophysical Observatory) during 2008–2015. We [...] Read more.

We present the results of photo-polarimetric monitoring observations of the blazar Markarian 421 carried out with different telescopes (the 0.4 m telescopes of St. Petersburg State University and the Pulkovo Observatory, the 0.7 m telescope of the Crimean Astrophysical Observatory) during 2008–2015. We analyse the optical data as well as gamma-ray ligh t curves obtained with the Fermi Large Area Telescope. The multiwavelength flux variations are discussed. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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0 pages, 1890 KiB

Open AccessArticle

Recent Progress in Understanding the Large Scale Jets of Powerful Quasars

by Markos Georganopoulos^1,*, Eileen T. Meyer¹

and Eric S. Perlman²

¹ Department of Physics, University of Maryland, Baltimore County, MD 21250, USA

² Department of Physics, Florida Institute of Technology, Melbourne, FL 32901, USA

Galaxies 2016, 4(4), 65; https://doi.org/10.3390/galaxies4040065 - 23 Nov 2016

Cited by 17 | Viewed by 4665

Abstract

Our understanding of the physics of kpc-scale quasar jets had seemed to converge to a paradigm in which these jets are as highly relativistic on the kpc scale as they are on sub-pc scales close to the central black hole. Retaining bulk Lorentz [...] Read more.

Our understanding of the physics of kpc-scale quasar jets had seemed to converge to a paradigm in which these jets are as highly relativistic on the kpc scale as they are on sub-pc scales close to the central black hole. Retaining bulk Lorentz factors (Γ) on the order of 10–20 at these distances implies a jet power comparable to or higher than their Eddington luminosity. We recently started challenging this paradigm, which was put in place to explain the surprisingly bright X-ray emission of the knots of many quasar jets as inverse Compton scattering off the cosmic microwave background (IC/CMB). We have shown that the knot X-ray emission of the archetypical jets 3C 273 and PKS 0637-752 is not due to IC/CMB. With IC/CMB disfavored, an alternative interpretation for the X-rays is synchrotron radiation from a second population of electrons accelerated in situ up to ∼100 TeV. These results are the first step towards resolving the long-standing issue of the nature of the X-ray emission in powerful quasar jets. Comprehensive observational and theoretical work on essentially all X-ray-detected large-scale quasar jets to test the IC/CMB model over a much larger population needs to be done to examine the implications of slower jets that are extremely efficient accelerators. A fascinating case can be made that—contrary to popular belief—the total radiative power of the large-scale jet of these sources is comparable to that of the quasar core. Even more so, the angle-integrated TeV output of these (previously thought TeV-quiet) quasar jets likely makes them the dominant class among active galactic nuclei (AGN), exceeding the TeV production of so-called TeV blazars. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 1265 KiB

Open AccessArticle

Correlation Analysis of Delays between Variations of Gamma-Ray and Optical Light Curves of Blazars

by Karen E. Williamson^1,*, Svetlana G. Jorstad^1,2

, Alan P. Marscher¹

, Valeri M. Larionov^2,3,4, Iván Agudo^1,5, Arkady A. Arkharov³, Dmitry A. Blinov^2,6, Carolina Casadio⁵, José L. Gómez⁵, Vladimir A. Hagen-Thorn^2,4, Manasvita Joshi¹, Tatiana S. Konstantinova², Evgenia N. Kopatskaya², Elena G. Larionova², Liudmilla V. Larionova², Michael P. Malmrose¹, Ian M. McHardy⁷, Sol N. Molina⁵

, Daria A. Morozova²

, Brian W. Taylor^1,8 and Ivan S. Troitsky² Show full author list Hide full author list

¹ Institute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA

² Astronomical Institute, St. Petersburg State University, Universitetskij Pr. 28, Petrodvorets, 198504 St. Petersburg, Russia

³ Main (Pulkovo) Astronomical Observatory of RAS, Pulkovskoye shosse, 60, 196140 St. Petersburg, Russia

⁴ Isaac Newton Institute of Chile, St. Petersburg Branch, 198504 St. Petersburg, Russia

⁵ Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080 Granada, Spain

⁶ Department of Physics, University of Crete, 71003 Heraklion, Greece

⁷ Department of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK

⁸ Lowell Observatory, Flagstaff, AZ 86001, USA

Galaxies 2016, 4(4), 64; https://doi.org/10.3390/galaxies4040064 - 23 Nov 2016

Cited by 3 | Viewed by 3699

Abstract

We have been performing multi-wavelength monitoring of a sample of

γ

-ray blazars since the launch of the Fermi Gamma-ray Space Telescope in 2008. We present

γ

-ray and optical light curves for several quasars and BL Lac objects from the sample to [...] Read more.

We have been performing multi-wavelength monitoring of a sample of

γ

-ray blazars since the launch of the Fermi Gamma-ray Space Telescope in 2008. We present

γ

-ray and optical light curves for several quasars and BL Lac objects from the sample to illustrate different patterns of variability. We investigate correlations between

γ

-ray and R-band light curves and, if these are statistically significant, determine delays between variations at the two wavebands. Such time delays can reveal the relative locations of the emitting regions in AGN jets and the origin of the high-energy photons. We present preliminary results of this analysis. Of the 29 blazars with sufficient time coverage, 17 display a significant, singular, correlated time lag when tested over the entire 7-year period. Of these sources, the six that exhibit a consistent time lag across a majority of epochs of high activity have lags of 0 ± 7 days; the 11 without consistency across epochs of high activity generally display longer mean lags, with

γ

-ray leading optical. Eleven sources display no significant singular correlation over either the entire 7-year period or across shorter intervals. No significant difference is apparent between the BL Lac objects and FSRQs. Even after 7 years of monitoring, our correlation analysis remains plagued with uncertainties due to insufficient data. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 334 KiB

Open AccessArticle

AP Librae: The Extended Jet as the Source of VHE Emission?

by Michael Zacharias^*

and Stefan J. Wagner

Landessternwarte, Universität Heidelberg, D-69117 Heidelberg, Germany

Galaxies 2016, 4(4), 63; https://doi.org/10.3390/galaxies4040063 - 15 Nov 2016

Cited by 3 | Viewed by 3688

Abstract

The LBL AP Librae has been detected in the TeV gamma-ray range, which is unexpected for this kind of blazar. The broad-band SED cannot be explained by a one-zone model, and especially fails in the TeV domain. An extended jet has been detected [...] Read more.

The LBL AP Librae has been detected in the TeV gamma-ray range, which is unexpected for this kind of blazar. The broad-band SED cannot be explained by a one-zone model, and especially fails in the TeV domain. An extended jet has been detected on arcsec scales both in radio and X-ray frequencies. The spectral index of the X-ray band indicates an inverse Compton origin. Using an IC/CMB model, the TeV emission can be successfully modeled as originating in the extended jet. Several arguments in favor of this model, as well as observational tests, will be presented. The observations suggest that acceleration of particles to very high energies is still efficient at large distances from the core. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 2059 KiB

Open AccessArticle

Investigating the Puzzling Synchrotron Behaviour of Mrk 421

by Maria I. Carnerero^1,*, Claudia M. Raiteri¹, Massimo Villata¹, Jose A. Acosta Pulido^2,3, Paul S. Smith⁴, Valeri M. Larionov^5,6 and The WEBT Collaboration¹

¹ INAF, Osservatorio Astrofisico di Torino, via Osservatorio 20, I-10025 Pino Torinese, Italy

² Instituto de Astrofisica de Canarias (IAC). E-38205 La Laguna, Tenerife, Spain

³ Departamento de Astrofisica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain

⁴ Steward Observatory, University of Arizona, Tucson, AZ 85721, USA

⁵ Astronomical Institute, St. Petersburg State University, St. Peterburg 198504, Russia

⁶ Pulkovo Observatory, St.-Petersburg 196140, Russia

Galaxies 2016, 4(4), 61; https://doi.org/10.3390/galaxies4040061 - 4 Nov 2016

Cited by 2 | Viewed by 3984

Abstract

We investigate the multiwavelength behaviour of the high-energy peaked BL Lac object (HBL) Mrk 421 at redshift

z = 0.031

in the period 2007–2015. We use optical photometric, spectroscopic, and polarimetric data and near-infrared data obtained by 35 observatories participating in [...] Read more.

We investigate the multiwavelength behaviour of the high-energy peaked BL Lac object (HBL) Mrk 421 at redshift

z = 0.031

in the period 2007–2015. We use optical photometric, spectroscopic, and polarimetric data and near-infrared data obtained by 35 observatories participating in the GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT), as well as by the Steward Observatory Support of the Fermi Mission. We also employ high-energy data from the Swift (UV and X-rays) satellite to study correlations among emission in different bands. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 465 KiB

Open AccessArticle

Physical Conditions and Variability Processes in AGN Jets through Multi-Frequency Linear and Circular Radio Polarization Monitoring

by Ioannis Myserlis^*, Emmanouil Angelakis

, Alex Kraus, Lars Fuhrmann, Vassilis Karamanavis

and J. Anton Zensus

Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

Galaxies 2016, 4(4), 58; https://doi.org/10.3390/galaxies4040058 - 2 Nov 2016

Cited by 7 | Viewed by 4471

Abstract

Radio polarimetry is an invaluable tool to investigate the physical conditions and variability processes in active galactic nuclei (AGN) jets. However, detecting their linear and circular polarization properties is a challenging endeavor due to their low levels and possible depolarization effects. We have [...] Read more.

Radio polarimetry is an invaluable tool to investigate the physical conditions and variability processes in active galactic nuclei (AGN) jets. However, detecting their linear and circular polarization properties is a challenging endeavor due to their low levels and possible depolarization effects. We have developed an end-to-end data analysis methodology to recover the polarization properties of unresolved sources with high accuracy. It has been applied to recover the linear and circular polarization of 87 AGNs measured by the F-GAMMA program from July 2010 to January 2015 with a mean cadence of 1.3 months. Their linear polarization was recovered at four frequencies between 2.64 and 10.45 GHz and the circular polarization at 4.85 and 8.35 GHz. The physical conditions required to reproduce the observed polarization properties and the processes which induce their variability were investigated with a full-Stokes radiative transfer code which emulates the synchrotron emission of modeled jets. The model was used to investigate the conditions needed to reproduce the observed polarization behavior for the blazar 3C 454.3, assuming that the observed variability is attributed to evolving internal shocks propagating downstream. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 976 KiB

Open AccessArticle

Investigating the Innermost Jet Structures of Blazar S5 0716+714 Using Uniquely Dense Intra-day Photo-polarimetric Observations

by Gopal Bhatta

Astronomical Observatory of Jagiellonian University, ul. Orla 171, 30-244 Krakow, Poland

Galaxies 2016, 4(4), 56; https://doi.org/10.3390/galaxies4040056 - 27 Oct 2016

Cited by 2 | Viewed by 3853

Abstract

The sub-hour timescale variability commonly observed in blazars—widely known as intra-day or microvariability—has been extensively studied in optical photo-polarimetric bands over the past 25–30 years. In addition, there have been comprehensive theoretical discussions on the topic, with various models and scenarios proposed; [...] Read more.

The sub-hour timescale variability commonly observed in blazars—widely known as intra-day or microvariability—has been extensively studied in optical photo-polarimetric bands over the past 25–30 years. In addition, there have been comprehensive theoretical discussions on the topic, with various models and scenarios proposed; however, the phenomenon still remains relatively poorly understood. Here we present the summary of our optical microvariability studies over the past few years based on multi-frequency photo-polarimetric Whole Earth Blazar Telescope (WEBT) observation campaigns. The primary objective of the study was to explore the characteristics of the source microvariability on timescales of a few minutes to a few days using exceptionally dense photo-polarimetric observations. The results show that the source often displays fast variability with an amplitude as large as 0.3 mag within a few hours, as well as color variability on similar time scales often characterized by “bluer-when-brighter” trend. Similarly, the correlation between variability in flux and polarization appears to depend upon the configuration of the optical polarization angle relative to the positional angle of the innermost radio core of the jet. Other fascinating observations include a sudden and temporary disappearance in the observed variability lasting for ∼6 h. In addition, the modeling of individual microflares strongly suggests that the phenomenon of microvariability can be best explained by convolved emission from compact emission sites distributed stochastically in the turbulent jet. Besides, analysis of some of the well resolved micro-flares exhibiting high degrees of polarization points towards a complex magnetic geometry pervading the jet with the possible presence of small-scale regions of highly ordered and enhanced magnetic field similar to so-called “magnetic islands”. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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4 pages, 262 KiB

Open AccessArticle

The RadioAstron Dedicated DiFX Distribution

by Gabriele Bruni^1,*

, James M. Anderson², Walter Alef¹, Helge Rottmann¹, Andrei P. Lobanov^1,3 and J. Anton Zensus¹

¹ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

² Deutsches GeoForschungsZentrum GFZ, Telegrafenberg A6, 14473 Potsdam, Germany

³ Institut für Experimentalphysik, Universität Hamburg, Luruper Chaussee 149, 22761 Hamburg, Germany

Galaxies 2016, 4(4), 55; https://doi.org/10.3390/galaxies4040055 - 27 Oct 2016

Cited by 18 | Viewed by 4747

Abstract

Distributed FX-architecture (DiFX) is a software Very Long Baseline Interferometry (VLBI) correlator currently adopted by several main correlation sites around the globe. After the launch of the RadioAstron Space-VLBI mission in 2011, an extension was necessary to handle processing of an orbiting antenna, [...] Read more.

Distributed FX-architecture (DiFX) is a software Very Long Baseline Interferometry (VLBI) correlator currently adopted by several main correlation sites around the globe. After the launch of the RadioAstron Space-VLBI mission in 2011, an extension was necessary to handle processing of an orbiting antenna, to be correlated with supporting ground arrays. Here, we present a branch of the main DiFX distribution (2.4), uploaded on the publicly available repository during July 2016, that the Max Planck Institute for Radio Astronomy (MPIfR) developed to process data of the three key active galactic nuclei (AGN)-imaging RadioAstron science projects, as well as part of the AGN survey project, and General Observing Time (GOT) projects proposed since Announcement of Opportunity 2 (AO-2, July 2014–July 2015). It can account for general relativistic correction of an orbiting antenna with variable position/velocity, providing a routine to convert the native RadioAstron Data Format (RDF) format to the more common Mark5 B (M5B). The possibility of introducing a polynomial clock allows one to mitigate the effects of spacecraft acceleration terms in near-perigee observations. Additionally, since for the first time polarimetry on space-baselines is available thanks to RadioAstron, this DiFX branch allows one to include the spacecraft orientation information at the correlation stage, in order to perform proper polarization calibration during data reduction. Finally, a fringe-finding algorithm able to manage an arbitrarily large fringe-search window is included, allowing one to increase the search space normally adopted by common software packages like HOPS. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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11 pages, 3054 KiB

Open AccessArticle

Observing—and Imaging—Active Galactic Nuclei with the Event Horizon Telescope

by Vincent L. Fish^1,*

, Kazunori Akiyama^1,2, Katherine L. Bouman³, Andrew A. Chael⁴, Michael D. Johnson⁴, Sheperd S. Doeleman⁴, Lindy Blackburn⁴, John F. C. Wardle⁵, William T. Freeman^3,6 and The Event Horizon Telescope Collaboration¹

¹ Massachusetts Institute of Technology, Haystack Observatory, Westford, MA 01886, USA

² Japan Society for the Promotion of Science, Chiyoda (Tokyo) 102-0083, Japan

³ Massachusetts Institute of Technology, Computer Science and Artificial Intelligence Laboratory, Cambridge, MA 02139, USA

⁴ Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA

⁵ Physics Department, Brandeis University, Waltham, MA 02453, USA

⁶ Google Inc., 1600 Amphitheatre Parkway, Mountain View, CA 94043, USA

Galaxies 2016, 4(4), 54; https://doi.org/10.3390/galaxies4040054 - 27 Oct 2016

Cited by 64 | Viewed by 14116

Abstract

Originally developed to image the shadow region of the central black hole in Sagittarius A* and in the nearby galaxy M87, the Event Horizon Telescope (EHT) provides deep, very high angular resolution data on other active galactic nucleus (AGN) sources too. The challenges [...] Read more.

Originally developed to image the shadow region of the central black hole in Sagittarius A* and in the nearby galaxy M87, the Event Horizon Telescope (EHT) provides deep, very high angular resolution data on other active galactic nucleus (AGN) sources too. The challenges of working with EHT data have spurred the development of new image reconstruction algorithms. This work briefly reviews the status of the EHT and its utility for observing AGN sources, with emphasis on novel imaging techniques that offer the promise of better reconstructions at 1.3 mm and other wavelengths. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 720 KiB

Open AccessArticle

Ringo2 Optical Polarimetry of Blazars

by Helen Jermak^1,2,*

, Iain Steele¹

, Elina Lindfors³, Talvikki Hovatta³, Kari Nilsson⁴, Gavin Lamb¹

, Carole Mundell⁵, Ulisses Barres De Almeida⁶

, Andrei Berdyugin³, Ville Kadenius³, Riho Reinthal³ and Leo Takalo³

¹ Astrophysics Research Institute, Liverpool John Moores University, Brownlow Hill, Liverpool L3 5RF, UK

² Department of Physics, Lancaster University, Bailrigg Campus, Lancaster LA1 4YW, UK

³ Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland

⁴ Finnish Center for Astrophysics with ESO, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland

⁵ Department of Physics, Bath University, Bath BA2 7AY, UK

⁶ Centro Brasileiro de Pesquisas Fisicas, Rua Dr. Xavier Sigaud 150, Rio de Janeiro, RJ 22290-180, Brazil

Galaxies 2016, 4(4), 52; https://doi.org/10.3390/galaxies4040052 - 26 Oct 2016

Viewed by 4085

Abstract

We present polarimetric and photometric observations from a sample of 15 γ-ray bright blazars with data from the Tuorla blazar monitoring program (KVA DIPOL) and Liverpool Telescope (LT) Ringo2 polarimeters (supplemented with γ-ray data from Fermi-LAT). We find that (1) The [...] Read more.

We present polarimetric and photometric observations from a sample of 15 γ-ray bright blazars with data from the Tuorla blazar monitoring program (KVA DIPOL) and Liverpool Telescope (LT) Ringo2 polarimeters (supplemented with γ-ray data from Fermi-LAT). We find that (1) The optical magnitude and γ-ray flux are positively correlated; (2) electric vector position angle rotations can occur in any blazar subclass; (3) there is no difference in the γ-ray flaring rates in the sample between subclasses; flares can occur during and outside of rotations with no preference for this behaviour; (4) the average degree of polarisation (P), optical magnitude and γ-ray flux are lower during a rotation compared with during non-rotation; (5) the number of observed flaring events and optical polarisation rotations are correlated and (6) the maximum observed P increases from ∼10% to ∼30% to ∼40% for subclasses with synchrotron peaks at high, intermediate and low frequencies respectively. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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14 pages, 2245 KiB

Open AccessArticle

Probing the Internal Structure of Magnetized, Relativistic Jets with Numerical Simulations

by José-María Martí

Departament d’Astronomia i Astrofísica and Observatori Astronòmic, Universitat de València, 46100 Burjassot (València), Spain

Galaxies 2016, 4(4), 51; https://doi.org/10.3390/galaxies4040051 - 26 Oct 2016

Cited by 2 | Viewed by 3737

Abstract

From an observational point of view, unveiling the physical processes behind the nature of the jets emanating from radio-loud AGN demands the resolution of the structure across the jet with the highest angular resolutions. Relying on a magneto-fluid dynamical description, numerical simulations can [...] Read more.

From an observational point of view, unveiling the physical processes behind the nature of the jets emanating from radio-loud AGN demands the resolution of the structure across the jet with the highest angular resolutions. Relying on a magneto-fluid dynamical description, numerical simulations can help to characterize the internal structure of jets (transversal structure, magnetic field structure, internal shocks, etc.). In the first part of the paper, we shall discuss equilibrium models of magnetized, relativistic, infinite, axisymmetric jets with rotation propagating through a homogeneous, static, unmagnetized ambient medium. Then, these transversal equilibrium profiles will be used to build steady models of overpressured, superfast-magnetosonic, relativistic jets, with the aim of characterizing their internal structure in connection with their dominant type of energy (internal energy: hot jets; rest-mass energy: kinetically-dominated jets; magnetic energy: Poynting-flux-dominated jets). Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 1282 KiB

Open AccessArticle

Through the Looking Glass: Faraday Conversion in Turbulent Blazar Jets

by Nicholas Roy MacDonald

Institute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA

Galaxies 2016, 4(4), 50; https://doi.org/10.3390/galaxies4040050 - 25 Oct 2016

Cited by 4 | Viewed by 3465

Abstract

Faint levels of circular polarization (Stokes V) have been detected in several relativistic jets. While typically less than a few percent, circular polarization can give us critical insight into the underlying nature of the jet plasma. Circular polarization can be produced through [...] Read more.

Faint levels of circular polarization (Stokes V) have been detected in several relativistic jets. While typically less than a few percent, circular polarization can give us critical insight into the underlying nature of the jet plasma. Circular polarization can be produced through a process known as linear birefringence, in which initially linearly polarized emission produced in one region of the jet is altered by Faraday rotation as it propagates through other regions of the jet with distinct magnetic field orientations. Recently, Marscher has developed the Turbulent Extreme Multi-Zone (TEMZ) model for blazar emission, in which turbulent plasma crossing a standing shock in the jet is represented by a collection of thousands of individual plasma cells, each with distinct magnetic field orientation. In order to test whether the TEMZ model can reproduce circularly polarized radiation at levels comparable to those observed in blazars, I have developed a numerical algorithm to solve the full Stokes equations of polarized radiative transfer. I have embedded this algorithm into the ray-tracing code RADMC3D (http://ascl.net/1202.015). RADMC3D was originally developed to model continuum radiative transfer in dusty media. This code, however, has been written in a modularized fashion that allows the user to specify the physics that is incorporated into the radiative transfer. I have replaced RADMC3D’s thermal emission and absorption coefficients with non-thermal coefficients pertaining to polarized synchrotron emission. This code is applied to ray-tracing through the 3-D TEMZ computational grid. Here I present a suite of synthetic polarized emission maps that highlight the effect that thousands of distinct cells of plasma within a jet can have on the observed linear and circular polarization. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 750 KiB

Open AccessArticle

Millimeter VLBI of NGC 1052: Dynamics

by Anne-Kathrin Baczko^1,2,3,*, Robert Schulz^1,2,4, Eduardo Ros^3,5

, Matthias Kadler², Manel Perucho⁵ and Jörn Wilms¹

¹ Dr. Remeis-Sternwarte & ECAP, University Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, Germany

² Institut für Th. Physik und Astrophysik, University Würzburg, Emil-Fischer-Str. 31, 97074 Würzburg, Germany

³ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

⁴ Netherlands Institute for Radio Astronomy (ASTRON), PO Box 2, 7990 AA Dwingeloo, The Netherlands

⁵ Obs. Astronòmic & Department d’As. i Astr., University de València, E-46071 València, Spain

Galaxies 2016, 4(4), 48; https://doi.org/10.3390/galaxies4040048 - 20 Oct 2016

Cited by 4 | Viewed by 4084

Abstract

The LINER galaxy NGC 1052 is an ideal target to study the innermost regions of active galactic nuclei (AGN), given its close distance of about 20 Mpc. The source was observed at 29 epochs from 2005 to 2009 with the Very Long Baseline [...] Read more.

The LINER galaxy NGC 1052 is an ideal target to study the innermost regions of active galactic nuclei (AGN), given its close distance of about 20 Mpc. The source was observed at 29 epochs from 2005 to 2009 with the Very Long Baseline Array (VLBA) at 43 GHz. Here, we present a kinematic study of its twin-jet system from a subset of 9 epochs at 43 GHz carried out in 2005 and 2006, finding a bright central feature as the dynamic center. The resulting mean velocities of

β = v / c = 0.46 \pm 0.08

and

β = 0.69 \pm 0.02

for the western and eastern jet, respectively, give hints towards higher velocities in the eastern jet. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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10 pages, 1037 KiB

Open AccessArticle

The VLBA-BU-BLAZAR Multi-Wavelength Monitoring Program

by Svetlana Jorstad^1,2,*,†

and Alan Marscher^1,†

¹ Institute for Astrophysical Research, Boston University, 725 Commonwealth Ave, Boston, MA 02215, USA

² Astronomical Institute, St.Petersburg State University, Universitetsky prospekt, 28, St. Petersburg 198504, Russia

^† These authors contributed equally to this work.

Galaxies 2016, 4(4), 47; https://doi.org/10.3390/galaxies4040047 - 20 Oct 2016

Cited by 75 | Viewed by 7218

Abstract

We describe a multiwavelength program of monitoring of a sample of bright γ-ray blazars, which the Boston University (BU) group has being carrying out since June 2007. The program includes monthly monitoring with the Very Long Baseline Array at 43 GHz, optical [...] Read more.

We describe a multiwavelength program of monitoring of a sample of bright γ-ray blazars, which the Boston University (BU) group has being carrying out since June 2007. The program includes monthly monitoring with the Very Long Baseline Array at 43 GHz, optical photometric and polarimetric observations, construction and analysis of UV and X-ray light curves obtained with the Rossi X-ray Timing Explorer (RXTE) and Swift satellites, and construction and analysis of γ-ray light curves based on data provided by the Large Area Telescope of the Fermi Gamma-ray Space Telescope. We present general results about the kinematics of parsec-scale radio jets, as well as the connection between γ-ray outbursts and jet events. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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10 pages, 3031 KiB

Open AccessArticle

Observations of the Structure and Dynamics of the Inner M87 Jet

by R. Craig Walker^1,*, Philip E. Hardee², Fred Davies³, Chun Ly⁴, William Junor⁵, Florent Mertens^6,7 and Andrei Lobanov^6,8

¹ National Radio Astronomy Observatory, Socorro, NM 87801, USA

² Department of Physics & Astronomy, The University of Alabama, Tuscaloosa, AL 35487, USA

³ MPIA, 69117 Heidelberg, Germany

⁴ Goddard Space Flight Center, Astrophysics Science Division, 8800 Greenbelt Road, Greenbelt, MD 20771, USA

⁵ ISR-2, MS-D436, Los Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545, USA

⁶ Max Plank Institute für Radioastronomie, Auf dem Huegel 69, 53121 Bonn, Germany

⁷ Kapteyn Astronomical Institute, PO Box 800, 9700 AV Groningen, The Netherlands

⁸ Institut für Experimentalphysik, Universität Hamburg, Luruper Chaussee 149, 22761 Hamburg, Germany

Galaxies 2016, 4(4), 46; https://doi.org/10.3390/galaxies4040046 - 18 Oct 2016

Cited by 22 | Viewed by 5207

Abstract

M87 is the best source in which to study a jet at high resolution in gravitational units because it has a very high mass black hole and is nearby. The angular size of the black hole is second only to Sgr A*, which [...] Read more.

M87 is the best source in which to study a jet at high resolution in gravitational units because it has a very high mass black hole and is nearby. The angular size of the black hole is second only to Sgr A*, which does not have a strong jet. The jet structure is edge brightened with a wide opening angle base and a weak counterjet. We have roughly annual observations for 17 years plus intensive monitoring at three week intervals for a year and five day intervals for 2.5 months made with the Very Long Baseline Array (VLBA) at 43 GHz. The inner jet shows very complex dynamics, with apparent motions both along and across the jet. Speeds from zero to over 2c are seen, with acceleration observed over the first 3 milli-arcseconds. The counterjet decreases in brightness much more rapidly than the main jet, as is expected from relativistic beaming in an accelerating jet oriented near the line-of-sight. Details of the structure and dynamics are discussed. The roughly annual observations show side-to-side motion of the whole jet with a characteristic time scale of about 9 years. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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Graphical abstract

9 pages, 1068 KiB

Open AccessArticle

Theoretical Study of the Effects of Magnetic Field Geometry on the High-Energy Emission of Blazars

by Manasvita Joshi^1,*, Alan Marscher¹

and Markus Böttcher^2,3

¹ Insitute for Astrophysical Research, Boston University, Boston, MA 02215, USA

² Centre for Space Research, North-West University, Potchefstroom 2520, South Africa

³ Department of Physics and Astronomy, Ohio University, Athens, OH 45701, USA

Galaxies 2016, 4(4), 45; https://doi.org/10.3390/galaxies4040045 - 14 Oct 2016

Cited by 8 | Viewed by 3928

Abstract

The knowledge of the structure of the magnetic field inside a blazar jet, as deduced from polarization observations at radio to optical wavelengths, is closely related to the formation and propagation of relativistic jets that result from accretion onto supermassive black holes. However, [...] Read more.

The knowledge of the structure of the magnetic field inside a blazar jet, as deduced from polarization observations at radio to optical wavelengths, is closely related to the formation and propagation of relativistic jets that result from accretion onto supermassive black holes. However, a largely unexplored aspect of the theoretical understanding of radiation transfer physics in blazar jets has been the magnetic field geometry as revealed by the polarized emission and the connection between the variability in polarization and flux across the spectrum. Here, we explore the effects of various magnetic geometries that can exist inside a blazar jet: parallel, oblique, toroidal, and tangled. We investigate the effects of changing the orientation of the magnetic field, according to the above-mentioned geometries, on the resulting high-energy spectral energy distributions (SEDs) and spectral variability patterns (SVPs) of a typical blazar. We use the MUlti-ZOne Radiation Feedback (MUZORF) model of Joshi et al. (2014) to carry out this study and to relate the geometry of the field to the observed SEDs at X-ray and γ-ray energies. One of the goals of the study is to understand the relationship between synchrotron and inverse Compton peaks in blazar SEDs and the reason for the appearance of γ-ray “orphan flares” observed in some blazars. This can be associated with the directionality of the magnetic field, which creates a difference in the radiation field as seen by an observer versus that seen by the electrons in the emission region. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 806 KiB

Open AccessArticle

Parsec-Scale Structure and Kinematics of Faint TeV HBLs

by B. Glenn Piner¹ and Philip G. Edwards^2,*

¹ Department of Physics and Astronomy, Whittier College, Whittier, CA 90608, USA

² CSIRO Astronomy and Space Science, Epping 2121, Australia

Galaxies 2016, 4(4), 44; https://doi.org/10.3390/galaxies4040044 - 11 Oct 2016

Cited by 2 | Viewed by 3077

Abstract

We present new multi-epoch Very Long Baseline Array (VLBA) observations of a set of TeV blazars drawn from our VLBA program to monitor all TeV-detected high-frequency peaked BL Lac objects (HBLs) at parsec scales. Most of these sources are faint in the radio, [...] Read more.

We present new multi-epoch Very Long Baseline Array (VLBA) observations of a set of TeV blazars drawn from our VLBA program to monitor all TeV-detected high-frequency peaked BL Lac objects (HBLs) at parsec scales. Most of these sources are faint in the radio, so they have not been well observed with VLBI by other surveys. Our previous measurements of apparent jet speeds in TeV HBLs showed apparent jet speeds that were subluminal or barely superluminal, suggesting jets with velocity structures at the parsec-scale. Here we present apparent jet speed measurements for eight new TeV HBLs, which for the first time show a superluminal tail to the apparent speed distribution for the TeV HBLs. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 3663 KiB

Open AccessArticle

Polarization Vector Rotations: Real, Spurious, Hidden and Imaginary

by Valeri M. Larionov^1,*

, Svetlana G. Jorstad^1,2

, Alan P. Marscher²

and Paul S. Smith³

¹ Astronomical Institute, St.-Petersburg State University, St.-Petersburg 198504, Russia

² Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA

³ Steward Observatory, University of Arizona, Tucson, AZ 85721, USA

Galaxies 2016, 4(4), 43; https://doi.org/10.3390/galaxies4040043 - 11 Oct 2016

Cited by 12 | Viewed by 4236

Abstract

Large and variable polarization is an inherent property of a majority of blazars. Systematic rotations of the polarization vector have been claimed for several blazars. In some cases, however, the reality of these rotations may be questionable. We suggest an additional method for [...] Read more.

Large and variable polarization is an inherent property of a majority of blazars. Systematic rotations of the polarization vector have been claimed for several blazars. In some cases, however, the reality of these rotations may be questionable. We suggest an additional method for the verification of the reality of polarization position angle rotations based on the correlation of the normalized Stokes parameters. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 969 KiB

Open AccessArticle

Radio-to-γ-Ray, Broadband Variability Study of the Classical BL Lac Object PKS 0735+178

by Arti Goyal^1,*, Łukasz Stawarz¹, Michal Ostrowski¹ and Valeri Larionov²

¹ Astronomical Observatory, Jagiellonian University, ul. Orla 171, Krakow 30-244, Poland

² Astronomical Institute of St. Petersburg State University, Petrodvorets 198504, Russia

Galaxies 2016, 4(4), 42; https://doi.org/10.3390/galaxies4040042 - 10 Oct 2016

Cited by 1 | Viewed by 3477

Abstract

The power-law shape of the power spectral density (PSD) of blazar light curves—

P (ν_{k}) \propto ν_{k}^{- β}

, where

ν_{k}

is the temporal frequency—indicates that blazar variability is, in general, of the colored-type noise ( [...] Read more.

The power-law shape of the power spectral density (PSD) of blazar light curves—

P (ν_{k}) \propto ν_{k}^{- β}

, where

ν_{k}

is the temporal frequency—indicates that blazar variability is, in general, of the colored-type noise (

β ≃ 1 - 3

). A precise characterisation of PSD slopes, normalizations, or characteristic timescales (if any) manifesting as distinct features in the power spectra of blazars is important for constraining the physics of the emission and energy dissipation processes in relativistic jets. Here we present the results of the PSD analysis for the BL Lac object PKS 0735+178 at GeV (Fermi-LAT), optical (R-band), and radio (GHz band from UMRAO and OVRO programmes) frequencies, covering a broad range in variability timescales. The novelty of our approach is that in the optical regime, by combining the long-term and densely sampled R-band intra-night light curves, we constructed the PSD for time periods ranging from 23 years down to minutes. Our analysis reveals that: (1) the nature of processes generating flux variability at optical and radio frequencies is different from those operating at GeV photon energies (

β \sim

2 and 1, respectively); (2) the main driver behind the optical variability is the same on timescales of years, months, days, and hours (a single power-law with

β \sim

2). We discuss our findings in the framework of a model where the overall blazar variability is generated by an underlying single stochastic process (radio and optical frequencies), or a linear superposition of such processes (γ-ray regime). Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 2524 KiB

Open AccessArticle

A Search for QPOs in the Blazar OJ287: Preliminary Results from the 2015/2016 Observing Campaign

by S. Zola^1,2,*

, M. Valtonen^3,4, G. Bhatta¹

, A. Goyal¹, B. Debski¹, A. Baran², J. Krzesinski², M. Siwak², S. Ciprini^5,6, A. Gopakumar⁷, H. Jermak⁸, K. Nilsson⁴, D. Reichart⁹, K. Matsumoto¹⁰, K. Sadakane¹⁰, K. Gazeas¹¹, M. Kidger¹², V. Piirola^3,4, F. Alicavus^13,14, K. S. Baliyan¹⁵, A. Berdyugin⁴, D. Boyd¹⁶, M. Campas Torrent¹⁷, F. Campos¹⁸, J. Carrillo Gómez¹⁹, D. B. Caton²⁰, V. Chavushyan²¹, J. Dalessio²², D. Dimitrov²³, M. Drozdz², H. Er²⁴, A. Erdem^13,14, A. Escartin Pérez²⁵, V. Fallah Ramazani⁴, A. V. Filippenko²⁶, F. Garcia²⁷, F. Gómez Pinilla²⁸, M. Gopinathan²⁹, J. B. Haislip³⁰, J. Harmanen⁴, R. Hudec^31,32, G. Hurst³³, K. M. Ivarsen³⁰, M. Jelinek³¹, A. Joshi³⁴, M. Kagitani³⁵, N. Kaur¹⁵, W. C. Keel³⁶, A. P. LaCluyze³⁰, B. C. Lee³⁷, E. Lindfors⁴, J. Lozano de Haro³⁸, J. P. Moore³⁰, M. Mugrauer³⁹, R. Naves Nogues¹⁷, A. W. Neely⁴⁰, R. H. Nelson⁴¹, W. Ogloza², S. Okano³⁵, J. C. Pandey³⁴, M. Perri^5,42, P. Pihajoki⁴³, G. Poyner⁴⁴, J. Provencal²², T. Pursimo⁴⁵, A. Raj⁴⁶, R. Reinthal⁴, S. Sadegi⁴, T. Sakanoi³⁵, Sameer¹⁵, J.-L. Salto González⁴⁷, T. Schweyer^48,49, F. C. Soldán Alfaro⁵⁰, N. Karaman⁵¹, E. Sonbas⁵¹, I. Steele⁸, J. T. Stocke⁵², J. Strobl³¹, L. O. Takalo⁴, T. Tomov⁵³, L. Tremosa Espasa⁵⁴, J. R. Valdes²¹, J. Valero Pérez⁵⁵, F. Verrecchia^5,42, J. R. Webb⁵⁶, M. Yoneda⁵⁷, M. Zejmo⁵⁸, W. Zheng²⁶, J. Telting⁴⁵, J. Saario⁴⁵, T. Reynolds⁴⁵, A. Kvammen⁴⁵, E. Gafton⁴⁵, R. Karjalainen⁵⁹ and P. Blay⁶⁰ Show full author list Hide full author list

¹ Astronomical Observatory, Jagiellonian University, ul. Orla 171, Krakow 30-244, Poland

² Mt. Suhora Observatory, Pedagogical University, ul. Podchorazych 2, Krakow 30-084, Poland

³ Finnish Centre for Astronomy with ESO, University of Turku, Turku F-21500, Finland

⁴ Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Turku F-21500, Finland

⁵ Agenzia Spaziale Italiana (ASI) Science Data Center, Roma I-00133, Italy

⁶ Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, Perugia I-06123, Italy

⁷ Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Mumbai 400005, India

⁸ Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, Brownlow Hill L3 5RF, UK

⁹ Departmentof Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599, USA

¹⁰ Astronomical Institute, Osaka Kyoiku University, 4-698 Asahigaoka, Kashiwara, Osaka 582-8582, Japan

¹¹ Department of Astrophysics, Astronomy and Mechanics, National & Kapodistrian University of Athens, Zografos GR-15784, Athens, Greece

¹² Herschel Science Centre, ESAC, European Space Agency, C/Bajo el Castillo, s/n, Villanueva de la Cañada, Madrid E-28692, Spain

¹³ Department of Physics, Faculty of Arts and Sciences, Canakkale Onsekiz Mart University, Canakkale TR-17100, Turkey

¹⁴ Astrophysics Research Center and Ulupinar Observatory, Canakkale Onsekiz Mart University, Canakkale TR-17100, Turkey

¹⁵ Physical Research Laboratory, Ahmedabad 380009, India

¹⁶ 5, Silver Lane, West Challow, Wantage, Oxon OX12 9TX, UK

¹⁷ C/Jaume Balmes No 24, Cabrils, Barcelona E-08348, Spain

¹⁸ C/.Riera, 1, 1^o 3^a B, Vallirana, Barcelona E-08759, Spain

¹⁹ Carretera de Martos 28 primero Fuensanta, Jaen E-23001, Spain

²⁰ Dark Sky Observatory, Department of Physics and Astronomy, Appalachian State University, Boone, NC 28608, USA

²¹ Instituto Nacional de Astrofisica, Óptica y Electrónica, Apartado Postal 51-216, Puebla 72000, Mexico

²² Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA

²³ Institute of Astronomy and NAO, Bulgarian Academy of Science, 72 Tsarigradsko Chaussee Blvd., Sofia 1784, Bulgaria

²⁴ Department of Physics, Faculty of Science, Atatürk University, Erzurum 25240, Turkey

²⁵ Aritz Bidea No 8 4 B, Mungia, Bizkaia E-48100, Spain

²⁶ Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA

²⁷ Muñas de Arriba La Vara, Valdés E-33780, Spain

²⁸ C/Concejo de Teverga 9, 1 C, Madrid E-28053, Spain

²⁹ Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital 263002, India

³⁰ Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599, USA

³¹ Astronomical Institute, The Czech Academy of Sciences, Ondřejov 25165, Czech Republic

³² Faculty of Electrical Engineering, Czech Technical University, Prague 74864, Czech Republic

³³ 16 Westminster Close, Basingstoke, Hampshire RG22 4PP, UK

³⁴ Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital 263002, India

³⁵ Planetary Plasma and Atmospheric Research Center, Tohoku University, Sendai 980-8578, Japan

³⁶ Department of Physics and Astronomy and SARA Observatory, University of Alabama, Box 870324, Tuscaloosa, AL 35487, USA

³⁷ Korea Astronomy and Space Science Institute, 776, Daedeokdae-Ro, Youseong-Gu, Daejeon 305-348, Korea

³⁸ Partida de Maitino, Pol. 2 Num. 163, Elche E-03206, Spain

³⁹ Astrophysikalisches Institut und Universitäts-Sternwarte, Schillergäßchen 2-3, Jena D-07745, Germany

⁴⁰ NF/Observatory, Silver City, NM 88041, USA

⁴¹ 1393 Garvin Street, Prince George, BC V2M 3Z1, Canada

⁴² INAF—Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio Catone I-00040, Italy

⁴³ Department of Physics, University of Helsinki, P.O. Box 64, Helsinki FI-00014, Finland

⁴⁴ BAA Variable Star Section, 67 Ellerton Road, Kingstanding, Birmingham B44 0QE, UK

⁴⁵ Nordic Optical Telescope, Apartado 474, Santa Cruz de La Palma E-38700, Spain

⁴⁶ Indian Institute of Astrophysics, II Block Koramangala, Bangalore 560 034, India

⁴⁷ Observatori Cal Maciarol Módul 8. Masia Cal Maciarol, Camí de l’Observatori s/n, Ager, Lerida E-25691, Spain

⁴⁸ Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, Garching D-85748, Germany

⁴⁹ Physik Department, Technische Universität München, James-Franck-Str., Garching D-85748, Germany

⁵⁰ C/Petrarca 6 1^a Sevilla E-41006, Spain

⁵¹ Department of Physics, University of Adiyaman, Adiyaman 02040, Turkey

⁵² Department of Astrophysical and Planetary Sciences, Center for Astrophysics and Space Astronomy, University of Colorado, Box 389, Boulder, CO 80309, USA

⁵³ Centre for Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, ul. Grudziadzka 5, Torun 87-100, Poland

⁵⁴ C/Cardenal Vidal i Barraquee No 3, Cambrils, Tarragona E-43850, Spain

⁵⁵ C/Matarrasa 16, Ponferrada, León E-24411, Spain

⁵⁶ Florida International University and SARA Observatory, University Park Campus, Miami, FL 33199, USA

⁵⁷ Kiepenheuer-Institut fur Sonnenphysik, Freiburg D-79104, Germany

⁵⁸ Janusz Gil Institute of Astronomy, University of Zielona Góra, Szafrana 2, Zielona Góra PL-65-516, Poland

⁵⁹ Isaac Newton Group of Telescopes, Apartado 321, Santa Cruz de La Palma E-38700, Spain

⁶⁰ IAC-NOT, C/Via Lactea, S/N, La Laguna E-38205, Spain

Show full affiliation list Hide full affiliation list

Galaxies 2016, 4(4), 41; https://doi.org/10.3390/galaxies4040041 - 9 Oct 2016

Cited by 17 | Viewed by 6343

Abstract

We analyse the light curve in the R band of the blazar OJ287, gathered during the 2015/2016 observing season. We did a search for quasi-periodic oscillations (QPOs) using several methods over a wide range of timescales. No statistically significant periods were found in [...] Read more.

We analyse the light curve in the R band of the blazar OJ287, gathered during the 2015/2016 observing season. We did a search for quasi-periodic oscillations (QPOs) using several methods over a wide range of timescales. No statistically significant periods were found in the high-frequency domain both in the ground-based data and in Kepler observations. In the longer-period domain, the Lomb–Scargle periodogram revealed several peaks above the 99% significance level. The longest one—about 95 days—corresponds to the innermost stable circular orbit (ISCO) period of the more massive black hole. The 43-day period could be an alias, or it can be attributed to accretion in the form of a two-armed spiral wave. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 1049 KiB

Open AccessArticle

Magnetic Dissipation in Relativistic Jets

by Yosuke Mizuno^1,*

, Jose L. Gómez², Ken-Ichi Nishikawa³, Athina Meli⁴, Philip E. Hardee⁵, Luciano Rezzolla^1,6, Chandra B. Singh⁷ and Elisabete M. de Gouveia Dal Pino⁷

¹ Institute for Theoretical Physics, Goethe University, D-60438 Frankfurt am Main, Germany

² Instituto de Astrofísica de Andalucía (CSIC), 18080 Granada, Spain

³ Department of Physics, University of Alabama in Huntsville, Huntsville, AL 35899, USA

⁴ Department of Physics and Astronomy, University of Gent, B-9000 Gent, Belgium

⁵ Department of Physics and Astronomy, The University of Alabama, Tuscaloosa, AL 35487, USA

⁶ Frankfurt Institute for Advanced Studies, D-60438 Frankfurt am Main, Germany

⁷ Department of Astronomy (IAG-USP), University of São Paulo, São Paulo SP 05508-090, Brazil

Galaxies 2016, 4(4), 40; https://doi.org/10.3390/galaxies4040040 - 7 Oct 2016

Cited by 3 | Viewed by 4439

Abstract

The most promising mechanisms for producing and accelerating relativistic jets, and maintaining collimated structure of relativistic jets involve magnetohydrodynamical (MHD) processes. We have investigated the magnetic dissipation mechanism in relativistic jets via relativistic MHD simulations. We found that the relativistic jets involving a [...] Read more.

The most promising mechanisms for producing and accelerating relativistic jets, and maintaining collimated structure of relativistic jets involve magnetohydrodynamical (MHD) processes. We have investigated the magnetic dissipation mechanism in relativistic jets via relativistic MHD simulations. We found that the relativistic jets involving a helical magnetic field are unstable for the current-driven kink instability, which leads to helically distorted structure in relativistic jets. We identified the regions of high current density in filamentary current sheets, indicative of magnetic reconnection, which are associated to the kink unstable regions and correlated to the converted regions of magnetic to kinetic energies of the jets. We also found that an over-pressured relativistic jet leads to the generation of a series of stationary recollimation shocks and rarefaction structures by the nonlinear interaction of shocks and rarefaction waves. The differences in the recollimation shock structure due to the difference of the magnetic field topologies and strengths may be observable through mm-VLBI observations and space-VLBI mission. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 1526 KiB

Open AccessArticle

Resolving the Base of the Relativistic Jet in M87 at 6R_sch Resolution with Global mm-VLBI

by Jae-Young Kim^1,*, Ru-Sen Lu¹, Thomas P. Krichbaum¹

, Michael Bremer², J. Anton Zensus¹, R. Craig Walker³ and The M87 collaboration¹

¹ Max Planck Institut für Radioastronomie, Auf dem Hügel 69, Bonn D-53121, Germany

² Institut de Radio Astronomie Millimétrique, 300 rue de la Piscine, Domaine Universitaire, Saint Martin d’Héres 38406, France

³ National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801, USA

Galaxies 2016, 4(4), 39; https://doi.org/10.3390/galaxies4040039 - 30 Sep 2016

Cited by 18 | Viewed by 4653

Abstract

M87 is one of the nearest radio galaxies with a central Super-Massive Black Hole (SMBH) and a prominent relativistic jet. Due to its close distance to the observer and the large SMBH mass, the source is one of the best laboratories to obtain [...] Read more.

M87 is one of the nearest radio galaxies with a central Super-Massive Black Hole (SMBH) and a prominent relativistic jet. Due to its close distance to the observer and the large SMBH mass, the source is one of the best laboratories to obtain strong observational constraints on the theoretical models for the formation and evolution of the AGN jets. In this article, we present preliminary results from our ongoing observational study about the innermost jet of M87 at an ultra-high resolution of ∼50

μ

as achieved by the Global Millimeter-Very Long Baseline Interferometry Array (GMVA). The data obtained between 2004 and 2015 clearly show limb-brightened jets at extreme resolution and sensitivity. Our preliminary analysis reveals that the innermost jet expands in an edge-brightened cone structure (parabolic shape) but with the jet expansion profile slightly different from the outer regions of the jet. Brightness temperatures of the Very Long Baseline Interferometry (VLBI) core obtained from cm- to mm-wavelengths show a systematic evolution, which can be interpreted as the evolution as a function of distance from the BH. We also adopt an alternative imaging algorithm, Bi-Spectrum Maximum Entropy Method (BSMEM), to test reliable imaging at higher angular resolution than provided by the standard CLEAN method (i.e., super-resolution). A demonstration with a VLBA 7 mm example data set shows consistent results with a near-in-time 3 mm VLBI image. Application of the method to the 2009 GMVA data yields an image with remarkable fine-scale structures that have been never imaged before. We present a brief interpretation of the complexity in the structure. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 8405 KiB

Open AccessArticle

Microscopic Processes in Global Relativistic Jets Containing Helical Magnetic Fields

by Ken-Ichi Nishikawa^1,*

, Yosuke Mizuno²

, Jacek Niemiec³, Oleh Kobzar³

, Martin Pohl^4,5, Jose L. Gómez⁶, Ioana Duţan⁷, Asaf Pe’er⁸, Jacob Trier Frederiksen⁹

, Åke Nordlund⁹, Athina Meli¹⁰, Helene Sol¹¹, Philip E. Hardee¹² and Dieter H. Hartmann¹³

¹ Department of Physics, University of Alabama in Huntsville, ZP12, Huntsville, AL 35899, USA

² Institute for Theoretical Physics, Goethe University, Frankfurt am Main D-60438, Germany

³ Institute of Nuclear Physics PAN, ul. Radzikowskiego 152, Kraków 31-342, Poland

⁴ Institut fur Physik und Astronomie, Universität Potsdam, Potsdam-Golm 14476, Germany

⁵ DESY, Platanenallee 6, Zeuthen 15738, Germany

⁶ Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, Granada 18080, Spain

⁷ Institute of Space Science, Atomistilor 409, Bucharest-Magurele RO-077125, Romania

⁸ Physics Department, University College Cork, Cork T12 YN60, Ireland

⁹ Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, Copenhagen DK-2100, Denmark

¹⁰ Department of Physics and Astronomy, University of Gent, Proeftuinstraat 86, Gent B-9000, Belgium

¹¹ LUTH, Observatore de Paris-Meudon, 5 place Jules Jansen, Meudon CEDEX 92195, France

¹² Department of Physics and Astronomy, The University of Alabama, Tuscaloosa, AL 35487, USA

¹³ Department of Physics and Astronomy, Clemson University, Clemson, SC 29634, USA

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Galaxies 2016, 4(4), 38; https://doi.org/10.3390/galaxies4040038 - 29 Sep 2016

Cited by 12 | Viewed by 4839

Abstract

In the study of relativistic jets one of the key open questions is their interaction with the environment on the microscopic level. Here, we study the initial evolution of both electron–proton (

e^{-}

–

p^{+}

) and electron–positron ( [...] Read more.

In the study of relativistic jets one of the key open questions is their interaction with the environment on the microscopic level. Here, we study the initial evolution of both electron–proton (

e^{-}

–

p^{+}

) and electron–positron (

e^{\pm}

) relativistic jets containing helical magnetic fields, focusing on their interaction with an ambient plasma. We have performed simulations of “global” jets containing helical magnetic fields in order to examine how helical magnetic fields affect kinetic instabilities such as the Weibel instability, the kinetic Kelvin-Helmholtz instability (kKHI) and the Mushroom instability (MI). In our initial simulation study these kinetic instabilities are suppressed and new types of instabilities can grow. In the

e^{-}

–

p^{+}

jet simulation a recollimation-like instability occurs and jet electrons are strongly perturbed. In the

e^{\pm}

jet simulation a recollimation-like instability occurs at early times followed by a kinetic instability and the general structure is similar to a simulation without helical magnetic field. Simulations using much larger systems are required in order to thoroughly follow the evolution of global jets containing helical magnetic fields. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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10 pages, 7659 KiB

Open AccessArticle

The Blazar Sequence 2.0

by Gabriele Ghisellini

INAF—Osservatorio Astronomico di Brera, Merate I–23807, Italy

Galaxies 2016, 4(4), 36; https://doi.org/10.3390/galaxies4040036 - 27 Sep 2016

Cited by 30 | Viewed by 7402

Abstract

This paper discusses the spectral energy distribution (SED) of all blazars with redshift detected by the Fermi satellite and listed in the 3LAC catalog. The so called “blazar sequence” from the phenomenological point of view will be updated, with no theory or modelling. [...] Read more.

This paper discusses the spectral energy distribution (SED) of all blazars with redshift detected by the Fermi satellite and listed in the 3LAC catalog. The so called “blazar sequence” from the phenomenological point of view will be updated, with no theory or modelling. It will be shown that: (i) pure data show that jet and accretion power are related; (ii) the updated blazar sequence maintains the properties of the old version, albeit with a less pronounced dominance of the γ-ray emission; (iii) at low bolometric luminosities, two different types of objects have the same high energy power: low black hole mass flat spectrum radio quasars and high mass BL Lacs. Therefore, at low luminosities, there is a very large dispersion of SED shapes; (iv) in low power BL Lacs, the contribution of the host galaxy is important. Remarkably, the luminosity distribution of the host galaxies of BL Lacs are spread in a very narrow range; (v) a simple sum of two smoothly joining power laws can describe the blazar SEDs very well. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 3069 KiB

Open AccessArticle

The Connection between the Radio Jet and the γ-ray Emission in the Radio Galaxy 3C 120 and the Blazar CTA 102

by Carolina Casadio^1,*

, José L. Gómez², Svetlana G. Jorstad^3,4

, Alan P. Marscher³

, Paola Grandi⁵, Valeri M. Larionov^4,6, Matthew L. Lister⁷, Paul S. Smith⁸, Mark A. Gurwell⁹, Anne Lähteenmäki^6,10, Iván Agudo², Sol N. Molina²

, Vishal Bala³, Manasvita Joshi³, Brian Taylor³, Karen E. Williamson³, Yuri Y. Kovalev^1,11, Tuomas Savolainen^1,6, Alexander B. Pushkarev^1,12,13, Arkady A. Arkharov¹³, Dmitry A. Blinov^4,14, George A. Borman¹², Andrea Di Paola¹⁵, Tatiana S. Grishina⁴, Vladimir A. Hagen-Thorn⁴, Ryosuke Itoh¹⁶, Evgenia N. Kopatskaya⁴, Elena G. Larionova⁴, Liudmila V. Larionova⁴, Daria A. Morozova⁴

, Elizaveta Rastorgueva-Foi^6,17

, Sergey G. Sergeev¹², Merja Tornikoski⁶, Ivan S. Troitsky⁴, Clemens Thum¹⁸ and Helmut Wiesemeyer¹ Show full author list Hide full author list

¹ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

² Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía, s/n, 18008 Granada, Spain

³ Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA

⁴ Astronomical Institute, St. Petersburg State University, 198504 St. Petersburg, Russia

⁵ Istituto Nazionale di Astrofisica-IASFBO, 40127 Bologna, Italy

⁶ Aalto University Metsähovi Radio Observatory, FI-02540 Kylmälä, Finland

⁷ Department of Physics, Purdue University, 610 Purdue Mall, West Lafayette, IN 47907, USA

⁸ Steward Observatory, University of Arizona, Tucson, AZ 85721, USA

⁹ Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA

¹⁰ Aalto University Department of Radio Science and Engineering, FI-00076 Aalto, Finland

¹¹ Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, 117810 Moscow, Russia

¹² Crimean Astrophysical Observatory, 98409 Nauchny, Crimea, Russia

¹³ Pulkovo Observatory, 196140 St. Petersburg, Russia

¹⁴ Department of Physics and Institute for Plasma Physics, University of Crete, GR-71003 Heraklion, Greece

¹⁵ INAF, Osservatorio Astronomico di Roma, 00136 Roma, Italy

¹⁶ Department of Physical Sciences, Hiroshima University, Hiroshima Prefecture 739-8511, Japan

¹⁷ School of Maths and Physics, University of Tasmania, Australia, Private Bag 37, TAS 7001 Hobart, Australia

¹⁸ Instituto de Radio Astronomía Milimétrica, 18012 Granada, Spain

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Galaxies 2016, 4(4), 34; https://doi.org/10.3390/galaxies4040034 - 27 Sep 2016

Cited by 3 | Viewed by 4877

Abstract

We present multi-wavelength studies of the radio galaxy 3C 120 and the blazar CTA 102 during unprecedented γ-ray flares for both sources. In both studies the analysis of γ-ray data has been compared with a series of 43 GHz VLBA images [...] Read more.

We present multi-wavelength studies of the radio galaxy 3C 120 and the blazar CTA 102 during unprecedented γ-ray flares for both sources. In both studies the analysis of γ-ray data has been compared with a series of 43 GHz VLBA images from the VLBA-BU-BLAZAR program, providing the necessary spatial resolution to probe the parsec scale jet evolution during the high energy events. To extend the radio dataset for 3C 120 we also used 15 GHz VLBA data from the MOJAVE sample. These two objects which represent very different classes of AGN, have similar properties during the γ-ray events. The γ-ray flares are associated with the passage of a new superluminal component through the mm VLBI core, but not all ejections of new components lead to γ-ray events. In both sources γ-ray events occurred only when the new components are moving in a direction closer to our line of sight. We locate the γ-ray dissipation zone a short distance from the radio core but outside of the broad line region, suggesting synchrotron self-Compton scattering as the probable mechanism for the γ-ray production. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 288 KiB

Open AccessArticle

Broad Band Observations of Gravitationally Lensed Blazar during a Gamma-Ray Outburst

by Julian Sitarek^1,*

, Josefa Becerra González^2,3,4, Sara Buson^2,5, Dijana Dominis Prester⁶

, Marina Manganaro^7,8, Daniel Mazin^9,10, Kari Nilsson¹¹, Mireia Nievas¹²

, Antonio Stamerra¹³, Fabrizio Tavecchio¹³ and Ievgen Vovk¹⁰

¹ Department of Astrophysics, University of Łódź, PL-90236 Lodz, Poland

² Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

³ Department of Physics, University of Maryland, College Park, MD 20742, USA

⁴ Department of Astronomy, University of Maryland, College Park, MD 20742, USA

⁵ Center for Research and Exploration in Space Science and Technology (CRESST), University of Maryland Baltimore County, Baltimore, MD 21250, USA

⁶ Department of Physics, University of Rijeka, Radmile Matejčić 2, 51000 Rijeka, Croatia

⁷ Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain

⁸ Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain

⁹ Institute for Cosmic Ray Research, University of Tokyo, Kashiwa-no-ha 5-1-5, Kashiwa-shi, 277-8582 Chiba, Japan

¹⁰ Max-Planck-Institut für Physik, D-80805 München, Germany

¹¹ Tuorla Observatory, Astronomy Division, University of Turku, FI-21500 Piikkiö, Finland

¹² Department of Atomic, Molecular and Nuclear Physics, Universidad Complutense de Madrid, E-28040 Madrid, Spain

¹³ INAF National Institute for Astrophysics, I-00136 Rome, Italy

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Galaxies 2016, 4(4), 31; https://doi.org/10.3390/galaxies4040031 - 27 Sep 2016

Viewed by 4423

Abstract

QSO B0218+357 is a gravitationally lensed blazar located at a cosmological redshift of 0.944. In July 2014 a GeV flare was observed by Fermi-LAT, triggering follow-up observations with the MAGIC telescopes at energies above 100 GeV. The MAGIC observations at the expected [...] Read more.

QSO B0218+357 is a gravitationally lensed blazar located at a cosmological redshift of 0.944. In July 2014 a GeV flare was observed by Fermi-LAT, triggering follow-up observations with the MAGIC telescopes at energies above 100 GeV. The MAGIC observations at the expected time of arrival of the trailing component resulted in the first detection of QSO B0218+357 in Very-High-Energy (VHE, >100 GeV) gamma rays. We report here the observed multiwavelength emission during the 2014 flare. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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10 pages, 4656 KiB

Open AccessArticle

Radiative Transfer Modeling of Radio-Band Linear Polarization Observations as a Probe of the Physical Conditions in the Jets of γ-Ray Flaring Blazars

by Margo F. Aller^1,*, Philip A. Hughes¹, Hugh D. Aller¹, Talvikki Hovatta^2,3 and Venkatessh Ramakrishnan²

¹ Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1107, USA

² Aalto Observatory, Metsähovi Radio Observatory, Kylmälä 02540, Finland

³ Department of Radio Science and Engineering, Aalto University, P.O. Box 13000, FI-00076, Aalto, Espoo 02150, Finland

Galaxies 2016, 4(4), 35; https://doi.org/10.3390/galaxies4040035 - 26 Sep 2016

Cited by 5 | Viewed by 3864

Abstract

Since the mid-1980s, the shock-in-jet model has been the preferred paradigm to explain radio-band flaring in blazar jets. We describe our radiative transfer model incorporating relativistically-propagating shocks, and illustrate how the 4.8, 8, and 14.5 GHz linear polarization and total flux density data [...] Read more.

Since the mid-1980s, the shock-in-jet model has been the preferred paradigm to explain radio-band flaring in blazar jets. We describe our radiative transfer model incorporating relativistically-propagating shocks, and illustrate how the 4.8, 8, and 14.5 GHz linear polarization and total flux density data from the University of Michigan monitoring program, in combination with the model, constrain jet flow conditions and shock attributes. Results from strong Fermi-era flares in 4 blazars with widely-ranging properties are presented. Additionally, to investigate jet evolution on decadal time scales we analyze 3 outbursts in OT 081 spanning nearly 3 decades and find intrinsic changes attributable to flow changes at a common spatial location, or, alternatively, to a change in the jet segment viewed. The model’s success in reproducing these data supports a scenario in which relativistic shocks compress a plasma with an embedded passive, initially-turbulent magnetic field, with additional ordered magnetic field components, one of which may be helical. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 1612 KiB

Open AccessArticle

Exploring the Magnetic Field Configuration in BL Lac Using GMVA

by Bindu Rani^1,2,*,†, Thomas Krichbaum²

, Jeff A. Hodgson³, Shoko Koyama², Anton J. Zensus², Lars Fuhramnn², Alan Marscher⁴

and Svetlana Jorstad⁴

¹ NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

² Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, Bonn 53121, Germany

³ Korea Astronomy and Space Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Korea

⁴ Institute for Astrophysical Research, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA

Galaxies 2016, 4(3), 32; https://doi.org/10.3390/galaxies4030032 - 20 Sep 2016

Cited by 5 | Viewed by 4933

Abstract

The high radio frequency polarization imaging of non-thermal emission from active galactic nuclei (AGN) is a direct way to probe the magnetic field strength and structure in the immediate vicinity of supermassive black holes (SMBHs) and is crucial in testing the jet-launching scenario. [...] Read more.

The high radio frequency polarization imaging of non-thermal emission from active galactic nuclei (AGN) is a direct way to probe the magnetic field strength and structure in the immediate vicinity of supermassive black holes (SMBHs) and is crucial in testing the jet-launching scenario. To explore the the magnetic field configuration at the base of jets in blazars, we took advantage of the full polarization capabilities of the Global Millimeter VLBI Array (GMVA). With an angular resolution of ∼50 micro-arcseconds (μas) at 86 GHz, one could resolve scales up to ∼450 gravitational radii (for a

10^{9}

solar mass black hole at a redshift of 0.1). We present here the preliminary results of our study on the blazar BL Lac. Our results suggest that on sub-mas scales the core and the central jet of BL Lac are significantly polarized with two distinct regions of polarized intensity. We also noted a great morphological similarity between the 7 mm/3 mm VLBI images at very similar angular resolution. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 772 KiB

Open AccessArticle

The Radio/Gamma-Ray Connection from 120 MHz to 230 GHz

by Marcello Giroletti^1,*

, Filippo D’Ammando^1,2, Monica Orienti¹, Rocco Lico^1,2

and The Fermi-LAT Collaboration¹

¹ INAF Istituto di Radioastronomia, via Gobetti 101, Bologna I-40129, Italy

² Dipartimento di Fisica e Astronomia, Università di Bologna, via Ranzani 1, Bologna 40127, Italy

Galaxies 2016, 4(3), 30; https://doi.org/10.3390/galaxies4030030 - 13 Sep 2016

Cited by 2 | Viewed by 4701

Abstract

Radio loud active galactic nuclei are composed of different spatial features, each one characterized by different spectral properties in the radio band. Among them, blazars are the most common class of sources detected at gamma-rays by Fermi, and their radio emission is [...] Read more.

Radio loud active galactic nuclei are composed of different spatial features, each one characterized by different spectral properties in the radio band. Among them, blazars are the most common class of sources detected at gamma-rays by Fermi, and their radio emission is dominated by the flat spectrum compact core. In this contribution, we explore the connection between emission at high energy revealed by Fermi and at radio frequencies. Taking as a reference the strong and very highly significant correlation found between gamma rays and cm-λ radio emission, we explore the different behaviours found as we change the energy range in gamma rays and in radio, therefore changing the physical parameters of the zones involved in the emitted radiation. We find that the correlation weakens when we consider (1) gamma rays of energy above 10 GeV (except for high synchrotron peaked blazars) or (2) low frequency radio data taken by the Murchison Widefield Array; on the other hand, the correlation strengthens when we consider mm-λ data taken by Atacama Large Millimeter Array (ALMA). Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 992 KiB

Open AccessArticle

AGN Jet Kinematics on Parsec-Scales: The MOJAVE Program

by Matthew Lister^* and The MOJAVE Collaboration

Department of Physics and Astronomy, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USA

Galaxies 2016, 4(3), 29; https://doi.org/10.3390/galaxies4030029 - 9 Sep 2016

Cited by 9 | Viewed by 4837

Abstract

Very long baseline interferometry offers the best means of investigating the complex dynamics of relativistic jets powered by active galactic nuclei, via multi-epoch, sub-milliarcsecond, full-polarization imaging at radio wavelengths. Although targeted studies have yielded important information on the structures of individual AGN jets, [...] Read more.

Very long baseline interferometry offers the best means of investigating the complex dynamics of relativistic jets powered by active galactic nuclei, via multi-epoch, sub-milliarcsecond, full-polarization imaging at radio wavelengths. Although targeted studies have yielded important information on the structures of individual AGN jets, the strong selection effects associated with relativistically beaming imply that general aspects of the flows can only be determined via large statistical studies. In this review I discuss major results from the Monitoring of Jets in Active Galactic Nuclei With VLBA Experiments (MOJAVE) program, which has gathered multi-epoch Very Long Baseline Array (VLBA) data at 15 GHz on over 400 AGN jets over the course of two decades. The sample is large enough to encompass a range of AGN optical class, radio luminosity and synchrotron peak frequency, and has been used to show that within a particular jet, individual bright features have a spread of apparent speed and velocity vector position angle about a characteristic value. We have found that in some cases there is a secular evolution of launch angle direction over time, indicative of evolving narrow energized channels within a wider outflow. The majority of the jet features are superluminal and accelerating, with changes in speed more common than changes in direction. Within approximately 100 pc of the AGN, the flows are generally accelerating, while beyond this distance the flows begin to decelerate or remain nearly constant in speed. We also find evidence for a maximum bulk flow Lorentz factor of 50 in the pc-scale radio regime, and a trend of higher jet speeds in lower-synchrotron peaked and gamma-ray-loud blazars. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 220 KiB

Open AccessArticle

Applying Relativistic Reconnection to Blazar Jets

by Krzysztof Nalewajko

Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, Warsaw 00-716, Poland

Galaxies 2016, 4(3), 28; https://doi.org/10.3390/galaxies4030028 - 8 Sep 2016

Cited by 12 | Viewed by 3426

Abstract

Rapid and luminous flares of non-thermal radiation observed in blazars require an efficient mechanism of energy dissipation and particle acceleration in relativistic active galactic nuclei (AGN) jets. Particle acceleration in relativistic magnetic reconnection is being actively studied by kinetic numerical simulations. Relativistic reconnection [...] Read more.

Rapid and luminous flares of non-thermal radiation observed in blazars require an efficient mechanism of energy dissipation and particle acceleration in relativistic active galactic nuclei (AGN) jets. Particle acceleration in relativistic magnetic reconnection is being actively studied by kinetic numerical simulations. Relativistic reconnection produces hard power-law electron energy distributions

N (γ) \propto γ^{- p} \exp (- γ / γ_{\max})

with index

p \to 1

and exponential cut-off Lorentz factor

γ_{\max} \sim σ

in the limit of magnetization

σ = B^{2} / (4 π w) ≫ 1

(where w is the relativistic enthalpy density). Reconnection in electron-proton plasma can additionally boost

γ_{\max}

by the mass ratio

m_{p} / m_{e}

. Hence, in order to accelerate particles to

γ_{\max} \sim 10^{6}

in the case of BL Lacs, reconnection should proceed in plasma of very high magnetization

σ_{\max} ≳ 10^{3}

. On the other hand, moderate mean jet magnetization values are required for magnetic bulk acceleration of relativistic jets,

σ_{mean} \sim Γ_{j} ≲ 20

(where

Γ_{j}

is the jet bulk Lorentz factor). I propose that the systematic dependence of

γ_{\max}

on blazar luminosity class—the blazar sequence—may result from a systematic trend in

σ_{\max}

due to homogeneous loading of leptons by pair creation regulated by the energy density of high-energy external radiation fields. At the same time, relativistic AGN jets should be highly inhomogeneous due to filamentary loading of protons, which should determine the value of

σ_{mean}

roughly independently of the blazar class. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

9 pages, 4828 KiB

Open AccessArticle

Sharp Polarimetric Eyes: More Trees than Forest?

by Paul S. Smith

Steward Observatory, University of Arizona, Tucson, AZ 85721, USA

Galaxies 2016, 4(3), 27; https://doi.org/10.3390/galaxies4030027 - 7 Sep 2016

Cited by 11 | Viewed by 3936

Abstract

The Fermi Gamma-ray Space Telescope (Fermi) has focused the intensive multi-wavelength and international observational effort on blazars since it was launched in 2008. Part of this effort involves systematic monitoring of the highly variable polarization of the continuum emission from these [...] Read more.

The Fermi Gamma-ray Space Telescope (Fermi) has focused the intensive multi-wavelength and international observational effort on blazars since it was launched in 2008. Part of this effort involves systematic monitoring of the highly variable polarization of the continuum emission from these objects. These observations are valuable in that they provide direct information on the degree of ordering and orientation on the sky of the magnetic field within the non-thermal emission region(s). Unfortunately, it is not yet possible to measure the polarization of the inverse-Compton continuum, only that of the lower-energy synchrotron emission. The inability to directly compare the polarization of the two dominant continuum sources in blazars is a drawback and leads to more ambiguities in determining their relative locations. There are many compelling examples of strong connections between γ-ray, X-ray, UV/optical/IR, and radio behavior in blazars that suggest the same region produces much of the observed emission at all wavelengths at least some of the time. However, the wealth of polarization behavior seen relative to flux changes invariably results in a complex situation that is difficult to interpret and model. The long-term blazar monitoring program undertaken at Steward Observatory is designed to primarily obtain accurate optical polarimetry of γ-ray-bright blazars during the Fermi mission with the goal of gaining important insights into the jet structure and physics of these objects. Data from this program are available to all researchers as soon as reductions are completed. I briefly detail the current status and progress of the program and the data products available. Although the wide variety of polarization behavior in blazars adds another layer of complexity to an already difficult problem, I summarize several important conclusions that can be drawn from the polarization information gathered during the Fermi era. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 732 KiB

Open AccessArticle

Flaring γ-Ray Emission from High Redshift Blazars

by Monica Orienti^1,*, Filippo D’Ammando^1,2, Marcello Giroletti¹

, Justin Finke³ and Daniele Dallacasa^1,2

¹ INAF - Istituto di Radioastronomia, Via Gobetti 101, Bologna I-40129, Italy

² Dipartimento di Fisica e Astronomia, Universitá degli Studi di Bologna, Viale Berti Pichat, 6/2, Bologna I-40127, Italy

³ U.S. Naval Research Laboratory, Code 7653, 4555 Overlook Ave SW, Washington, DC 20375-5352, USA

Galaxies 2016, 4(3), 26; https://doi.org/10.3390/galaxies4030026 - 6 Sep 2016

Cited by 2 | Viewed by 3939

Abstract

High redshift blazars are among the most powerful objects in the Universe. Although they represent a significant fraction of the extragalactic hard X-ray sky, they are not commonly detected in γ-rays. High redshift (

z > 2

) objects represent [...] Read more.

High redshift blazars are among the most powerful objects in the Universe. Although they represent a significant fraction of the extragalactic hard X-ray sky, they are not commonly detected in γ-rays. High redshift (

z > 2

) objects represent

< 10

per cent of the active galactic nuclei (AGN) population observed by Fermi so far, and γ-ray flaring activity from these sources is even more uncommon. The characterization of the radio-to-γ-ray properties of high redshift blazars represents a powerful tool for the study of the energetics of such extreme objects and the Extragalactic Background Light. This contribution will present results of multi-band campaigns, from radio to γ-rays, on PKS 0836+710, PKS 2149−306, and TXS 0536+145. The latter is the highest redshift detection of a flaring γ-ray blazar so far. At the peaks of their respective flares these sources reached an apparent isotropic gamma-ray luminosity of about 10

^{50}

erg·s

^{- 1}

, which is comparable with the luminosity observed from the most powerful blazars. The physical properties derived from the multi-wavelength observations of these sources are then compared with those shown by the high redshift population. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 1349 KiB

Open AccessArticle

Intra-Day Simultaneous Optical Monitoring of S5 0716+714

by Xiaoyuan Zhang¹, Jianghua Wu^1,* and Zhongyi Man^2,3

¹ Department of Astronomy, Beijing Normal University, Beijing 100875, China

² Department of Astronomy, Physics School, Peking University, Beijing 100871, China

³ Kavli Institute for Astronomy and Astrophysics (KIAA), Peking University, Beijing 100871, China

Galaxies 2016, 4(3), 25; https://doi.org/10.3390/galaxies4030025 - 6 Sep 2016

Cited by 6 | Viewed by 3510

Abstract

We present the results of simultaneous optical multi-color observations of BL Lac object 0716+714 in November 2014 and February 2016. The intra-day variability (IDV) varies from 0.04 to 0.3 mags. Both achromatic and bluer-when-brighter (BWB) color behaviors were detected. A probable quasi-periodic oscillation [...] Read more.

We present the results of simultaneous optical multi-color observations of BL Lac object 0716+714 in November 2014 and February 2016. The intra-day variability (IDV) varies from 0.04 to 0.3 mags. Both achromatic and bluer-when-brighter (BWB) color behaviors were detected. A probable quasi-periodic oscillation overlapping on a significant flare was also observed. We used the interpolated cross-correlation function to calculate time lags between light curves in different bands. Variations in the B and R lagging behind that in the I band were found, which corresponds with anti-clockwise loops on the color-magnitude diagrams. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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5 pages, 2145 KiB

Open AccessArticle

Optical Outburst of the Blazar S4 0954+658 in Early 2015

by Daria Morozova^1,*

, Valeri Larionov¹

, Svetlana Jorstad^1,2

, Alan Marscher²

, Yulia Troitskaya¹, Ivan Troitskiy¹, Dmitriy Blinov^1,3, Georg Borman⁴ and Mark Gurwell⁵

¹ Department of Astrophysics, St. Petersburg State University, Universitetsky Prospekt, 28, Peterhof, St. Petersburg 198504, Russia

² Institute for Astrophysical Research, Boston University, 725 Commonwealth Ave., Boston, MA 02215, USA

³ Department of Physics, Institute for Plasma Physics, University of Crete, Heraklion GR-71003, Greece

⁴ Crimean Astrophysical Observatory, P/O Nauchny, Crimea 298409, Russia

⁵ Harvard-Smithsonian CfA, Cambridge, MA 02138, USA

Galaxies 2016, 4(3), 24; https://doi.org/10.3390/galaxies4030024 - 3 Sep 2016

Cited by 2 | Viewed by 3878

Abstract

We analyze the behavior of the BL Lac object S4 0954+658 during an unprecedented bright optical flare in early 2015. The optical flare was accompanied by a powerful

γ

-ray flare and the detection of very-high-energy

γ

-ray emission. We analyze total and [...] Read more.

We analyze the behavior of the BL Lac object S4 0954+658 during an unprecedented bright optical flare in early 2015. The optical flare was accompanied by a powerful

γ

-ray flare and the detection of very-high-energy

γ

-ray emission. We analyze total and polarized intensity images obtained with the VLBA at 43 GHz and discover a new bright polarized superluminal knot, which was ejected from the VLBI-core during the peak of the flare. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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Graphical abstract

9 pages, 1844 KiB

Open AccessArticle

TimeTubes: Visualization of Polarization Variations in Blazars

by Makoto Uemura^1,*, Ryosuke Itoh², Longyin Xu³, Masanori Nakayama³, Hsiang-Yun Wu³

, Kazuho Watanabe⁴

, Shigeo Takahashi⁵ and Issei Fujishiro³

¹ Hiroshima Astrophysical Science Center, Hiroshima University, Kagamiyama 1-3-1, Higashi-Hiroshima 739-8526, Japan

² Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan

³ Department of Information and Computer Science, Keio University, 3-14-1 Hiyoshi, Kohoku-ku, Yokohama 223-8522, Japan

⁴ Toyohashi University of Technology, 1-1 Hibarigaoka, Tempaku-cho, Toyohashi 441-8580, Japan

⁵ Department of Computer Science and Engineering, University of Aizu, Tsuruga, Ikki-machi, Aizu-Wakamatsu 965-8580, Japan

Galaxies 2016, 4(3), 23; https://doi.org/10.3390/galaxies4030023 - 3 Sep 2016

Cited by 9 | Viewed by 5025

Abstract

Optical polarization provides important clues to the magnetic field in blazar jets. It is easy to find noteworthy patterns in the time-series data of the polarization degree (PD) and position angle (PA). On the other hand, we need to see the trajectory of [...] Read more.

Optical polarization provides important clues to the magnetic field in blazar jets. It is easy to find noteworthy patterns in the time-series data of the polarization degree (PD) and position angle (PA). On the other hand, we need to see the trajectory of the object in the Stokes

Q U

plane when the object has multiple polarized components. In this case, ironically, the more data we have, the more difficult it is to gain any knowledge from it. Here, we introduce TimeTubes, a new visualization scheme to explore the time-series data of polarization observed in blazars. In TimeTubes, the data is represented by tubes in 3D (Q, U, and time) space. The measurement errors of Q and U, color, and total flux of objects are expressed as the size, color, and brightness of the tubes. As a result, TimeTubes allows us to see the behavior of six variables in one view. We used TimeTubes for our data taken by the Kanata telescope between 2008 and 2014. We found that this tool facilitates the recognition of the patterns in blazar variations; for example, favored PA of flares and PA rotations associated with a series of flares. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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Graphical abstract

9 pages, 2709 KiB

Open AccessArticle

Spectral and Polarization Signatures of Relativistic Shocks in Blazars

by Markus Böttcher^1,2

¹ Centre for Space Research, North-West University, Potchefstroom 2520, South Africa

² Department of Physics and Astronomy, Ohio University, Athens, OH 45701, USA

Galaxies 2016, 4(3), 22; https://doi.org/10.3390/galaxies4030022 - 2 Sep 2016

Cited by 3 | Viewed by 4623

Abstract

Relativistic shocks are one of the most plausible sites of the emission of strongly variable, polarized multi-wavelength emission from relativistic jet sources such as blazars, via the diffusive shock acceleration (DSA) of relativistic particles. This paper summarizes recent results on a self-consistent coupling [...] Read more.

Relativistic shocks are one of the most plausible sites of the emission of strongly variable, polarized multi-wavelength emission from relativistic jet sources such as blazars, via the diffusive shock acceleration (DSA) of relativistic particles. This paper summarizes recent results on a self-consistent coupling of diffusive shock acceleration and radiation transfer in blazar jets. We demonstrate that the observed spectral energy distributions (SEDs) of blazars strongly constrain the nature of hydromagnetic turbulence responsible for pitch-angle scattering by requiring a strongly energy-dependent pitch-angle mean free path. The prominent soft X-ray excess (“Big Blue Bump”) in the SED of the BL Lac object AO 0235+164 can be modelled as the signature of bulk Compton scattering of external radiation fields by the thermal electron population, which places additional constraints on the level of hydromagnetic turbulence. It has further been demonstrated that internal shocks propagating in a jet pervaded by a helical magnetic field naturally produce polarization-angle swings by 180

^{\circ}

, in tandem with multi-wavelength flaring activity, without requiring any helical motion paths or other asymmetric jet structures. The specific application of this model to 3C279 presents the first consistent simultaneous modeling of snap-shot SEDs, multi-wavelength light curves, and time-dependent polarization signatures of a blazar during a polarization-angle (PA) rotation. This model has recently been generalized to a lepto-hadronic model, in which the high-energy emission is dominated by proton synchrotron radiation. It is shown that in this case, the high-energy (X-ray and γ-ray) polarization signatures are expected to be significantly more stable (not showing PA rotations) than the low-energy (electron-synchrotron) signatures. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 629 KiB

Open AccessArticle

Gamma-Ray Variability Induced by Microlensing on Intermediate Size Structures in Lensed Blazars

by Julian Sitarek^*

and Włodek Bednarek

Department of Astrophysics, University of Łódź, Lodz PL-90236, Poland

Galaxies 2016, 4(3), 20; https://doi.org/10.3390/galaxies4030020 - 31 Aug 2016

Viewed by 3021

Abstract

Changes of the magnification ratio of images in a lensed blazar, caused by microlensing on individual stars, have been proposed as a probe of the size and velocity of the emission region in the lensed source. We study whether similar changes in the [...] Read more.

Changes of the magnification ratio of images in a lensed blazar, caused by microlensing on individual stars, have been proposed as a probe of the size and velocity of the emission region in the lensed source. We study whether similar changes in the magnification ratio can be caused by the microlensing on the intermediate size structures in the lensing galaxy, namely stellar clusters and giant molecular clouds. Our numerical simulations show that changes in the magnification ratio of two images with similar time scales (as seen in QSO B0218+357) can be obtained for relativistically-moving emission regions with sizes up to 0.01 pc in the case of microlensing on clumps in giant molecular clouds. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 260 KiB

Open AccessArticle

Time-Dependent Injection as a Model for Rapid Blazar Flares

by Michael Zacharias

Landessternwarte, Universität Heidelberg, Heidelberg D-69117, Germany

Galaxies 2016, 4(3), 19; https://doi.org/10.3390/galaxies4030019 - 31 Aug 2016

Viewed by 3041

Abstract

Time-dependent injection can cause non-linear cooling effects, which lead to a faster energy loss of the electrons in jets. The most obvious result is the appearance of unique breaks in the SED, which would normally be attributed to a complicated electron distribution. Knowledge [...] Read more.

Time-dependent injection can cause non-linear cooling effects, which lead to a faster energy loss of the electrons in jets. The most obvious result is the appearance of unique breaks in the SED, which would normally be attributed to a complicated electron distribution. Knowledge of the observation time and duration is important for the interpretation of the observed spectra, because of the non-trivial evolution of the spectral energy distributions (SED). Intrinsic gamma–gamma absorption processes in the emission region are only of minor importance. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 575 KiB

Open AccessArticle

18–22 cm VLBA Observational Evidence for Toroidal B-Field Components in Six AGN Jets

by Juliana Cristina Motter^1,2,* and Denise Carmen Gabuzda²

¹ Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, São Paulo 05508-090, Brasil

² Physics Department, University College Cork, Cork, Ireland

Galaxies 2016, 4(3), 18; https://doi.org/10.3390/galaxies4030018 - 30 Aug 2016

Cited by 2 | Viewed by 3926

Abstract

The formation of relativistic jets in Active Galactic Nuclei (AGN) is related to accretion onto their central supermassive black holes, and magnetic (B) fields are believed to play a central role in launching, collimating, and accelerating the jet streams from very [...] Read more.

The formation of relativistic jets in Active Galactic Nuclei (AGN) is related to accretion onto their central supermassive black holes, and magnetic (B) fields are believed to play a central role in launching, collimating, and accelerating the jet streams from very compact regions out to kiloparsec scales. We present results of Faraday rotation studies based on Very Long Baseline Array (VLBA) data obtained at 18–22 cm for six well known AGN (OJ 287, 3C 279, PKS 1510-089, 3C 345, BL Lac, and 3C 454.3), which probe projected distances out to tens of parsecs from the observed cores. We have identified statistically significant, monotonic, transverse Faraday rotation gradients across the jets of all but one of these sources, indicating the presence of toroidal B fields, which may be one component of helical B fields associated with these AGN jets. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 1295 KiB

Open AccessArticle

The Optical Variability of the BL Lac AO 0235+164

by Junhui Fan^1,2,*, Omar Kurtanidze^3,4, Yi Liu^1,2

, Xiang Liu⁵

, Gotthard M. Richter⁶, Maria G. Nikolashvili³, Sophia O. Kurtanidze³, Revaz Chanishvili³, Hongtao Wang⁷, Mahito Sasada⁸, Aiying Zhou⁹, Chao Lin^1,2 and Yuhai Yuan^1,2

¹ Center for Astrophysics, Guangzhou University, Guangzhou 510006, China

² Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province, Guangzhou 510006, China

³ Abastumani Observatory, Mt. Kanobili, Abastumani 0301, Georgia

⁴ Engelhardt Astronomical Observatory, Kazan Federal University, Tatarstan 420000, Russia

⁵ Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China

⁶ Astrophysikalisches Institut Potsdam, An der Sternwarte 16, Potsdam 14482, Germany

⁷ Faculty of Physics and Electronic Information, LangFang Teacher’s College, China

⁸ Department of Astronomy, Boston University, Boston, MA 02215, USA

⁹ National Astronomical Observatory, Chinese Academy of Sciences, Beijing 100864, China

Galaxies 2016, 4(3), 17; https://doi.org/10.3390/galaxies4030017 - 30 Aug 2016

Cited by 1 | Viewed by 3839

Abstract

In this work, we present optical R band observations of AO 0235+164 carried out during the period of November 2006 to December 2012 using the Ap6E CCD camera attached to the primary focus of the 70 cm meniscus telescope at Abastumani Observatory, Georgia. [...] Read more.

In this work, we present optical R band observations of AO 0235+164 carried out during the period of November 2006 to December 2012 using the Ap6E CCD camera attached to the primary focus of the 70 cm meniscus telescope at Abastumani Observatory, Georgia. It shows a large variation of

Δ R

= 4.88 mag (14.19–19.07 mag) and a short time scale of

Δ T_{v}

= 73.5 min during our monitoring period. When periodicity analysis methods are applied to the R-band data from both historic and our observations, periods

P_{1}

= 8.26 yr and

P_{2}

= 0.54 yr are found. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 1430 KiB

Open AccessArticle

The Classifications and Some Correlations for Fermi Blazars

by Junhui Fan^1,2,*, Yi Liu^1,2

, Jianghe Yang³, Chao Lin^1,2, Jingmeng Hao^1,2 and Hubing Xiao^1,2

¹ Center for Astrophysics, Guangzhou University, Guangzhou 510006, China

² Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province, Guangzhou 510006, China

³ Department of Physics and Electronics Science, Hunan University of Arts and Science, Changde 415000, China

Galaxies 2016, 4(3), 16; https://doi.org/10.3390/galaxies4030016 - 29 Aug 2016

Cited by 2 | Viewed by 3912

Abstract

In a recent paper, we constructed the spectral energy distributions (SEDs) for 1425 Fermi blazars. We classify them as low synchrotron peak sources (LSPs) if log

ν_{p} (Hz) \leq

14.0, intermediate synchrotron peak sources (ISPs) if [...] Read more.

In a recent paper, we constructed the spectral energy distributions (SEDs) for 1425 Fermi blazars. We classify them as low synchrotron peak sources (LSPs) if log

ν_{p} (Hz) \leq

14.0, intermediate synchrotron peak sources (ISPs) if

14.0 < \log ν_{p} (Hz) \leq 15.3

, and high synchrotron peak sources (HSPs) if

\log ν_{p} (Hz) > 15.3

. We obtain an empirical relation to estimate the synchrotron peak frequency,

ν_{p}^{Eq .}

from effective spectral indexes

α_{o x} and α_{r o}

as

\log ν_{p}^{Eq .} = 16 + 4.238 X

if

X < 0

, and

\log ν_{p}^{Eq .} = 16 + 4.005 Y

if

X > 0

, where

X = 1.0 - 1.262 α_{r o} - 0.623 α_{o x}

and

Y = 1.0 + 0.034 α_{r o} - 0.978 α_{o x}

. In the present work, we investigate the correlation between the peak frequency and the radio-to-X-ray spectral index, between peak luminosity (bolometric luminosity) and γ-ray/optical luminosity, and between peak luminosity and bolometric luminosity. Some discussion is presented. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 5857 KiB

Open AccessArticle

Multi-Frequency Blazar Micro-Variability as a Tool to Investigate Relativistic Jets

by James R. Webb

Department of Physics, Florida International University, Miami, FL 33199, USA

Galaxies 2016, 4(3), 15; https://doi.org/10.3390/galaxies4030015 - 29 Aug 2016

Cited by 10 | Viewed by 4567

Abstract

For the past 12 years we have been studying optical micro-variability of a sample of 15 Blazars. We summarize the results of this study and draw some basic conclusions about the characteristics of micro-variability. The intermittency, the stochastic nature, and the similar profile [...] Read more.

For the past 12 years we have been studying optical micro-variability of a sample of 15 Blazars. We summarize the results of this study and draw some basic conclusions about the characteristics of micro-variability. The intermittency, the stochastic nature, and the similar profile shapes seen in micro-variations at different times and in different objects have led us to a possible model to explain the observed micro-variations. The model is based on a strong shock propagating down a relativistic jet and encountering turbulence which causes density or magnetic field enhancements. We use the theory of Kirk, Reiger, and Mastichiadis (1998) to describe the pulse of synchrotron emission emanating from individual density enhancements energized by the shock. By fitting these “pulses” to micro-variability observations, we obtain excellent fits to actual micro-variations. The model predicts that the spectral index changes as a function of pulse duration. This effect should be observable in multi-frequency micro-variability data. We present the theoretical model, model fits of our micro-variability light curves, and preliminary multi-frequency micro-variability observations that support this model. A further test that has yet to be carried out involves observing polarization changes in different pulses. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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7 pages, 1022 KiB

Open AccessArticle

Search for High-Confidence Blazar Candidates and Their MWL Counterparts in the Fermi-LAT Catalog Using Machine Learning

by Sabrina Einecke

Institute of Physics, Technische Universität Dortmund, Dortmund, D-44221, Germany,

Galaxies 2016, 4(3), 14; https://doi.org/10.3390/galaxies4030014 - 26 Aug 2016

Cited by 8 | Viewed by 3880

Abstract

A large fraction of the gamma-ray sources presented in the Third Fermi-LAT source catalog (3FGL) is affiliated with counterparts and source types, but 1010 sources remain unassociated and 573 sources are associated with active galaxies of uncertain type. The purpose of this [...] Read more.

A large fraction of the gamma-ray sources presented in the Third Fermi-LAT source catalog (3FGL) is affiliated with counterparts and source types, but 1010 sources remain unassociated and 573 sources are associated with active galaxies of uncertain type. The purpose of this study is to assign blazar classes to these unassociated and uncertain sources, and to link counterparts to the unassociated. A machine learning algorithm is used for the classification, based on properties extracted from the 3FGL, an infrared and an X-ray catalog. To estimate the reliability of the classification, performance measures are considered through validation techniques. The classification yielded purity values around 90% with efficiency values of roughly 50%. The prediction of high-confidence blazar candidates has been conducted successfully, and the possibility to link counterparts in the same procedure has been proven. These findings confirm the relevance of this novel multiwavelength approach. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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5 pages, 439 KiB

Open AccessArticle

The Extremes in Intra-Night Blazar Variability: The S4 0954+65 Case

by Rumen Bachev^*, Anton Strigachev, Evgeni Semkov, Rosa Victoria Muñoz Dimitrova, Georgi Latev, Borislav Spassov and Blagovest Petrov

Institute of Astronomy, Bulgarian Academy of Sciences, 72 Tsarigradsko Shosse Blvd, Sofia 1784, Bulgaria

Galaxies 2016, 4(3), 13; https://doi.org/10.3390/galaxies4030013 - 26 Aug 2016

Cited by 2 | Viewed by 3609

Abstract

We present results of optical observations of the extremely violently variable blazar S4 0954+65 on intra-night time scales. The object showed flux changes of up to 100% within a few hours. Time delays between optical bands, color changes and “rms-flux” relations are investigated [...] Read more.

We present results of optical observations of the extremely violently variable blazar S4 0954+65 on intra-night time scales. The object showed flux changes of up to 100% within a few hours. Time delays between optical bands, color changes and “rms-flux” relations are investigated and the results are discussed in terms of existing models of blazar variability. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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8 pages, 477 KiB

Open AccessArticle

Powers and Magnetization of Blazar Jets

by Marek Sikora

Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences/Bartycka 18, 00-716 Warsaw, Poland

Galaxies 2016, 4(3), 12; https://doi.org/10.3390/galaxies4030012 - 26 Aug 2016

Cited by 18 | Viewed by 3670

Abstract

In this work I review the observational constraints imposed on the energetics and magnetisation of quasar jets, in the context of theoretical expectations. The discussion is focused on issues regarding the jet production efficiency, matter content, and particle acceleration. I show that if [...] Read more.

In this work I review the observational constraints imposed on the energetics and magnetisation of quasar jets, in the context of theoretical expectations. The discussion is focused on issues regarding the jet production efficiency, matter content, and particle acceleration. I show that if the ratio of electron-positron-pairs to protons is of order 15, as is required to achieve agreement between jet powers computed using blazar spectral fits and those computed using radio-lobe calorimetry, the magnetization of blazar jets in flat-spectrum-radio-quasars (FSRQ) must be significant. This result favors the reconnection mechanism for particle acceleration and explains the large Compton-dominance of blazar spectra that is often observed, without the need to postulate very low jet magnetization. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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11 pages, 916 KiB

Open AccessArticle

A Panchromatic View of Relativistic Jets in Narrow-Line Seyfert 1 Galaxies

by Filippo D’Ammando^1,2,*, Monica Orienti², Justin Finke³, Josefin Larsson⁴

, Marcello Giroletti²

and Claudia M. Raiteri⁵

¹ Dipartimento di Fisica e Astronomia, Universitá degli Studi di Bologna, Viale Berti Pichat 6/2, Bologna 40127, Italy

² INAF - Istituto di Radioastronomia, Via Gobetti 101, Bologna 40129, Italy

³ U.S. Naval Research Laboratory, Code 7653, 4555 Overlook Ave. SW, Washington, DC 20375-5352, USA

⁴ KTH, Department of Physics, and the Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden

⁵ INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025 Pino Torinese (TO), Italy

Galaxies 2016, 4(3), 11; https://doi.org/10.3390/galaxies4030011 - 25 Aug 2016

Cited by 24 | Viewed by 5195

Abstract

The discovery by the Large Area Telescope on board Fermi of variable γ-ray emission from radio-loud narrow-line Seyfert 1 (NLSy1) galaxies revealed the presence of a possible third class of Active Galactic Nuclei (AGN) with relativistic jets in addition to blazars and [...] Read more.

The discovery by the Large Area Telescope on board Fermi of variable γ-ray emission from radio-loud narrow-line Seyfert 1 (NLSy1) galaxies revealed the presence of a possible third class of Active Galactic Nuclei (AGN) with relativistic jets in addition to blazars and radio galaxies. Considering that NLSy1 are usually hosted in spiral galaxies, this finding poses intriguing questions about the nature of these objects and the formation of relativistic jets. We report on a systematic investigation of the γ-ray properties of a sample of radio-loud NLSy1, including the detection of new objects, using 7 years of Fermi-LAT data with the new Pass 8 event-level analysis. In addition we discuss the radio-to-very-high-energy properties of the γ-ray emitting NLSy1, their host galaxy, and black hole mass in the context of the blazar scenario and the unification of relativistic jets at different scales. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 690 KiB

Open AccessArticle

Precessing Jet in the High-Redshift Blazar J0017+8135

by Kristóf Rozgonyi¹

and Sándor Frey^2,*

¹ Department of Physics of Complex Systems, Eötvös Loránd University, Pázmány P. sétány 1/A, Budapest H-1117, Hungary

² FÖMI Satellite Geodetic Observatory, P.O. Box 585, Budapest H-1592, Hungary

Galaxies 2016, 4(3), 10; https://doi.org/10.3390/galaxies4030010 - 24 Aug 2016

Cited by 5 | Viewed by 4268

Abstract

The prominent flat-spectrum radio quasar J0017+8135 (S5 0014+81) at z = 3.366 is one of the most luminous active galactic nuclei (AGN) known. Its milliarcsecond-scale radio jet structure has been studied with very long baseline interferometry (VLBI) since the 1980s. The quasar was [...] Read more.

The prominent flat-spectrum radio quasar J0017+8135 (S5 0014+81) at z = 3.366 is one of the most luminous active galactic nuclei (AGN) known. Its milliarcsecond-scale radio jet structure has been studied with very long baseline interferometry (VLBI) since the 1980s. The quasar was selected as one of the original defining objects of the International Celestial Reference Frame, but left out from its current second realization (ICRF2) because of systematic long-term positional variations. Here we analyse archival 8.6- and 2.3-GHz VLBI imaging data collected at nearly 100 different epochs during more than 20 years, to obtain information about the kinematics of jet components. Because of the cosmological time dilation, extensive VLBI monitoring data are essential to reveal changes in the jet structure of high-redshift AGN. In the case of J0017+8135, the data can be described with a simple kinematic model of jet precession with a 12-year periodicity in the observer’s frame. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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Graphical abstract

Review

Jump to: Editorial, Research

10 pages, 1547 KiB

Open AccessReview

A Search for Blazar-Like Radio-Loud Narrow-Line Seyfert 1 Galaxies

by Hugh R. Miller^1,*, Jeremy D. Maune¹, Joseph R. Eggen¹

, Clay S. Turner¹, Elizabeth C. Ferrara¹, Diana O. Gudkova¹ and Amy M. Battles²

¹ Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30302, USA

² Department of Physics, Georgia Gwinnett College, 1000 University Center Ln, Lawrenceville, GA 30043, USA

Galaxies 2017, 5(1), 20; https://doi.org/10.3390/galaxies5010020 - 21 Mar 2017

Cited by 6 | Viewed by 3994

Abstract

We report the results of an observational program to investigate the gamma-ray and optical variability properties of the vRL NLSY1 galaxies listed in the Yuan et al. sample. We have identified 17 members of the Yuan et al. sample possibly associated with gamma-ray [...] Read more.

We report the results of an observational program to investigate the gamma-ray and optical variability properties of the vRL NLSY1 galaxies listed in the Yuan et al. sample. We have identified 17 members of the Yuan et al. sample possibly associated with gamma-ray sources based on a combination of their optical polarization and optical variability and their gamma-ray properties. Eight have previously been associated with gamma-ray sources. We find nine additional members that we predict are excellent candidates to be associated with gamma-ray sources in the future. All 17 sources have many properties in common with flat spectrum radio quasars (FSRQs), suggesting that they may, in fact, constitute a new subclass of FSRQs. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 3194 KiB

Open AccessReview

Interstellar Scintillation and Scattering of Micro-arc-second AGN

by David L. Jauncey^1,2,*, Hayley E. Bignall³

, Lucyna Kedziora-Chudczer^4,5, Jun Yi Koay⁶, James E. J. Lovell⁷

, Jean-Pierre Macquart^8,9, Roopesh Ojha^10,11,12, Tapio Pursimo¹³

, Cormac Reynolds³ and Barney J. Rickett¹⁴

¹ CSIRO Astronomy and Space Science, Epping 1710, Australia

² Research School of Astronomy and Astrophysics, Australian National University, Canberra 2611, Australia

³ CSIRO Astronomy and Space Science, Kensington 6151, Australia

⁴ School of Physics, The University of New South Wales, Sydney 2052, Australia

⁵ Australian Centre for Astrobiology, The University of New South Wales, Sydney 2052, Australia

⁶ Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen ∅, Denmark

⁷ University of Tasmania, School of Physical Sciences, Private Bag 37, Hobart 7001, Australia

⁸ ICRAR/Curtin University, Curtin Institute of Radio Astronomy, Perth 6845, Australia

⁹ ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), The University of Sydney, Sydney 2006, Australia

¹⁰ NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA

¹¹ Center for Space Science and Technology, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA

¹² Department of Physics, The Catholic University of America, 620 Michigan Ave NE, Washington, DC 20064, USA

¹³ Nordic Optical Telescope, La Palma, Canary Islands 3537, Spain

¹⁴ ECE Department, University of California San Diego, La Jolla, CA 92093, USA

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Galaxies 2016, 4(4), 62; https://doi.org/10.3390/galaxies4040062 - 14 Nov 2016

Cited by 12 | Viewed by 4260

Abstract

The discovery of the first quasar 3C 273 led directly to the discovery of their variability at optical and radio wavelengths. We review the radio variability observations, in particular the variability found at frequencies below 1 GHz, as well as those exhibiting intra-day [...] Read more.

The discovery of the first quasar 3C 273 led directly to the discovery of their variability at optical and radio wavelengths. We review the radio variability observations, in particular the variability found at frequencies below 1 GHz, as well as those exhibiting intra-day variability (IDV) at cm wavelengths. Observations have shown that IDV arises principally from scintillation caused by scattering in the ionized interstellar medium of our Galaxy. The sensitivity of interstellar scintillation towards source angular sizes has provided a powerful tool for studying the most compact components of radio-loud AGN at microarcsecond and milliarcsecond scale resolution. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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9 pages, 424 KiB

Open AccessReview

Consequences of Proton Acceleration in Blazar Jets

by Apostolos Mastichiadis

Physics Department, National and Kapodistrian University of Athens, Athens 10679, Greece

Galaxies 2016, 4(4), 59; https://doi.org/10.3390/galaxies4040059 - 2 Nov 2016

Cited by 2 | Viewed by 4380

Abstract

Hadronic models of blazar emission constitute an interesting alternative to the more popular leptonic ones. Using the BL Lac object Mrk 421 as a characteristic example, we present two distinct ways of modeling the spectral energy distribution of blazars in the hadronic context, [...] Read more.

Hadronic models of blazar emission constitute an interesting alternative to the more popular leptonic ones. Using the BL Lac object Mrk 421 as a characteristic example, we present two distinct ways of modeling the spectral energy distribution of blazars in the hadronic context, and we discuss the predictions of each variant on the spectral shape, the multi-wavelength variability, the cosmic-ray flux, and the high-energy neutrino emission. Focusing on the latter, we then present an application of the hadronic model to individual BL Lacs that were recently suggested to be the counterparts of some of the IceCube neutrinos. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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6 pages, 216 KiB

Open AccessReview

Multifrequency Studies of Active Galactic Nuclei in the Planck Satellite Era

by Anne Lähteenmäki^* and The Planck Collaboration

Aalto University Metsähovi Radio Observatory & Department of Radio Science and Engineering, P.O. Box 13000, FI-00076 AALTO, Finland

Galaxies 2016, 4(4), 49; https://doi.org/10.3390/galaxies4040049 - 21 Oct 2016

Cited by 1 | Viewed by 2897

Abstract

The multi-epoch single-survey Planck satellite data have given a rare glimpse into how the radio spectra of active galactic nuclei (AGN) evolve in time. Using Planck and simultaneous auxiliary radio data ranging from 1 GHz to 857 GHz, spectra for 104 bright northern [...] Read more.

The multi-epoch single-survey Planck satellite data have given a rare glimpse into how the radio spectra of active galactic nuclei (AGN) evolve in time. Using Planck and simultaneous auxiliary radio data ranging from 1 GHz to 857 GHz, spectra for 104 bright northern extragalactic radio sources (most of them AGN) have been assembled; in these, the various stages of flare development can be identified. The results are compared with theoretical models describing relativistic jets. Evidence for particularly flat high-frequency radio spectra is found, indicating a harder accelerated electron energy spectrum than usually assumed. A set of sources also shows signs of intrinsic cold dust. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

12 pages, 1457 KiB

Open AccessFeature PaperReview

Variability of Blazars and Blazar Models over 38 Years

by Alan P. Marscher

Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA

Galaxies 2016, 4(4), 37; https://doi.org/10.3390/galaxies4040037 - 27 Sep 2016

Cited by 40 | Viewed by 6565

Abstract

Since 1978, when BL Lac objects and violently variable quasars were married to become “blazars”, physical interpretations of the phenomenon have evolved. Remarkably, though, the general picture of relativistic jets beaming their radiation in our direction, proposed that year by Blandford and Rees, [...] Read more.

Since 1978, when BL Lac objects and violently variable quasars were married to become “blazars”, physical interpretations of the phenomenon have evolved. Remarkably, though, the general picture of relativistic jets beaming their radiation in our direction, proposed that year by Blandford and Rees, remains intact. The main stress on theoretical models has come from observations that reveal ever more extreme variability requiring rampant particle acceleration on time-scales of minutes, often parsecs away from the central black hole. Here the author reviews many of the observations and theoretical ideas that have shaped his studies of blazars over about 40 years. This leads to his preferred scenario that blazar jets contain a helical magnetic field close to the black hole, turbulent plasma on parsecs scales, and both standing and moving shock waves. Particle acceleration can then occur in multiple stages involving the second-order Fermi process, magnetic reconnections, and modest jumps in energy at shock fronts. The most extreme variability, as well as brightness temperatures ~100 times the inverse Compton limit, probably require occasional exceptionally high bulk Lorentz factors. These can result, for example, from supersonic, relativistic turbulence, or ultra-relativistic flows propelled from sites of magnetic reconnection. Future efforts in these and other areas can determine whether these potential solutions are valid. Full article

(This article belongs to the Special Issue Blazars through Sharp Multi-wavelength Eyes)

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