Multiwavelength monitoring of the BL Lacertae object PKS 2155-304. 4: Multiwavelength analysis

Edelson, R.; Krolik, Julian H.; Madejski, G. M.; Maraschi, L.; Pike, G.; Urry, C. Megan; Brinkmann, W.; Courvoisier, T. J. L.; Ellithorpe, J. D.; Horne, K.; Treves, A.; Wagner, S. J.; Wamsteker, W.; Warwick, R. S.; Aller, H. D.; Aller, M. F.; Ashley, M. C. B.; Blecha, A.; Bouchet, P.; Bratschi, P.; Bregman, Joel N.; Carini, M. T.; Celotti, A.; Donahue, M.; Feigelson, E.; Filippenko, A. V.; Fink, H. H.; George, I. M.; Glass, I.; Heidt, J.; Hewitt, Jennifer; Hughes, P. A.; Kollgaard, R. I.; Kondo, Y.; Koratkar, Anuradha; Leighly, K. M.; Marscher, A. P.; Martín, P. G.; Matheson, T.; Miller, H. R.; Noble, J. C.; O’Brien, P. T.; Pian, E.; Reichert, G. A.; Saken, Jon M.; Shull, J. M.; Sitko, Michael L.; Smith, Paul S.; Sun, WH; Tagliaferri, G.

doi:10.1086/175059

Cited by 66 publications

(58 citation statements)

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“…Similar delays were noticed in 3C 279 (IR leads X-ray by 0.75±0.25 day) and in PKS 2155−304 (a day between EUV and X-rays, 2 days between UV and X-rays) and of the order of few hours between these (Edelson et al 1995) as well. Frequency stratification and different time scales for the duration of these flares (shorter times for higher frequencies) are possible with the shock-in-jet model (Marscher 1996 and references therein).…”

Section: Discussionsupporting

confidence: 76%

“…Since UV and gamma-ray data was less, so its reliability is doubtful. Edelson et al (1995) have reported correlated emission between X-ray, UV and optical emissions from PKS 2155-304 (an HBL BL Lac object). In another multi-wavelength campaign of PKS 2155-304 from 10 days data, Urry et al 1997 have reported X-ray flare leading EUV flare by one day and UV flare by two days.…”

Section: Discussionmentioning

confidence: 99%

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Simultaneous Multi-Wavelength Observations of the TeV Blazar Mrk 421 during February–March, 2003: X-Ray and NIR Correlated Variability

Gupta

Acharya

Bose

et al. 2008

Chin. J. Astron. Astrophys.

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In the present paper, we have reported the result of simultaneous multi-wavelength observations of the TeV blazar Mrk 421 during February − March 2003. In this period, we have observed Mrk 421 using Pachmarhi Array ofČerenkov Telescopes (PACT) of Tata Institute of Fundamental Research at Pachmarhi, India. Other simultaneous data were taken from the published literature and public data archives. We have analyzed the high quality X-ray (2-20 keV) observations from the NASA Rossi X-Ray Timing Explorer (RXTE). We have seen a possible correlated variability between X-ray and J band (1.25 µ) near infrared (NIR) wavelength. This is the first case of X-ray and NIR correlated variability in Mrk 421 or any high energy peaked (HBL) blazar. The correlated variability reported here is indicating a similar origin for NIR and X-ray emission. The emission is not affected much by the environment of the surrounding medium around the central engine of the Mrk 421. The observations are consistent with the shock-in-jet model for the emission of radiations.

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Section: Discussionsupporting

confidence: 76%

Section: Discussionmentioning

confidence: 99%

Simultaneous Multi-Wavelength Observations of the TeV Blazar Mrk 421 during February–March, 2003: X-Ray and NIR Correlated Variability

Gupta

Acharya

Bose

et al. 2008

Chin. J. Astron. Astrophys.

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“…Note that the relativistic jet is probably still required to explain the rapid variability, polarization, and other blazar characteristics of FSRQ, although microlensing could account for some lowamplitude, approximately achromatic, variability in BL Lac objects (Urry et al 1993;Edelson et al 1995).…”

Section: Bl Lac Objects As Gravitationally Microlensed Fsrqmentioning

confidence: 99%

Unified Schemes for Radio-Loud Active Galactic Nuclei

Urry¹,

Padovani²

1995

PASP

4,788

149

4,274

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ABSTRACT. The appearance of active galactic nuclei (AGN) depends so strongly on orientation that our current classification schemes are dominated by random pointing directions instead of more interesting physical properties. Light from the centers of many AGN is obscured by optically thick circumnuclear matter, particularly at optical and ultraviolet wavelengths. In radio-loud AGN, bipolar jets emanating from the nucleus emit radio through gamma-ray light that is relativistically beamed along the jet axes. Understanding the origin and magnitude of radiation anisotropies in AGN allows us to unify different classes of AGN; that is, to identify each single, underlying AGN type that gives rise to different classes through different orientations. This review describes the unification of radio-loud AGN, which include radio galaxies, quasars, and blazars. We describe the classification and general properties of AGN. We summarize the evidence for anisotropic emission caused by circumnuclear obscuration and relativistic beaming. We outline the two most plausible unified schemes for radio-loud AGN, one linking the high-luminosity sources (quasars and luminous radio galaxies) and one the low-luminosity sources (BL Lac objects and less luminous radio galaxies). Using the formalism appropriate to samples biased by relativistic beaming, we show that the population statistics for two schemes are in accordance with available data. We analyze the possible connections between low-and high-luminosity radio-loud AGN and conclude they probably are powered by similar physical processes, at least within the relativistic jet. We review potential difficulties with unification and conclude that none currently constitutes a serious problem. We discuss likely complications to unified schemes that are suggested by realistic physical considerations; these will be important to consider when more comprehensive data for larger complete samples become available. We conclude with a list of the ten questions we believe are the most pressing in this field.

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“…Its extreme TeV variability seems to demand an ultra-relativistic flow (bulk Lorentz factor ∼50) in at least portions of the jet that is believed to dominate the emission from this and other BL Lacs and blazars (Ghisellini & Tavecchio 2008). This BL Lac has been the target of several simultaneous multi-wavelength monitoring campaigns (e.g., Urry et al 1993;Brinkmann et al 1994;Edelson et al 1995;Courvoisier et al 1995;Urry et al 1997;Pian et al 1997;Pesce et al 1997;Foschini et al 2007Foschini et al , 2008. PKS 2155−304 is among the few blazars for which claims of an apparent QPO have been made, with UV and optical monitoring (from IUE) over five days possibly having a ∼0.7 d periodicity (Urry et al 1993).…”

Section: Introductionmentioning

confidence: 99%

A ~4.6 h quasi-periodic oscillation in the BL Lacertae PKS 2155-304?

Lachowicz

Gupta²,

Gaur³

et al. 2009

A&A

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We report a possible detection of an ∼4.6-h quasi-periodic oscillation (QPO) in the 0.3-10 keV emission of the high-energy peaked blazar PKS 2155−304 from a 64 ks observation by the XMM-Newton EPIC/pn detector. We identify a total modulation of ∼5% in the light curve and confirm that nominal period by periodogram, structure function, and wavelet analyses. The limited light curve duration allows the capture of only 3.8 cycles of this oscillation and thus precludes a very strong claim for this QPO, despite a nominally high ( 3σ) statistical significance. We briefly discuss models capable of producing an X-ray QPO of such a period in a blazar.

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Multiwavelength monitoring of the BL Lacertae object PKS 2155-304. 4: Multiwavelength analysis

Cited by 66 publications

References 0 publications

Simultaneous Multi-Wavelength Observations of the TeV Blazar Mrk 421 during February–March, 2003: X-Ray and NIR Correlated Variability

Simultaneous Multi-Wavelength Observations of the TeV Blazar Mrk 421 during February–March, 2003: X-Ray and NIR Correlated Variability

Unified Schemes for Radio-Loud Active Galactic Nuclei

A ~4.6 h quasi-periodic oscillation in the BL Lacertae PKS 2155-304?

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