Simultaneous Multiwavelength Spectrum and Variability of 3C 279 from 10 9 to 10 24 Hz

Hartman, R. C.; Webb, J. R.; Marscher, A. P.; Travis, John; Dermer, C. D.; Aller, H. D.; Aller, M. F.; Balonek, T. J.; Bennett, K.; Bloom, S. D.; Fujimoto, R.; Hermsen, W.; Hughes, P. A.; Jenkins, Ṕamela; Kii, T.; Kurfess, J. D.; Makino, F.; Mattox, J. R.; Montigny, C. von; Ohashi, T.; Robson, Ian; Ryan, J.; Sadun, A. C.; Schöenfelder, V.; Smith, Alex; Teraesranta, H.; Tornikoski, M.; Turner, Martin

doi:10.1086/177095

Cited by 116 publications

(89 citation statements)

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“…This includes NLS1 AGNs Mkn 335 (e.g., Grupe et al 2007) and 1H 0707-495 (e.g., Boller et al 2002); one of the least luminous, lowest mass and nearest Seyfert 1 Galaxy NGC4395 (Filippenko & Ho 2003) which has also been classified as a BLS1/S1.9 (Nikołajuk et al 2009), and CGCG 229-10 also called Zw 299-015 which is a Type I Seyfert Galaxy that exhibits broad-line emission (e.g., Barth et al 2011). In addition to these four we also included broad-line Seyfert 1.5 AGN NGC 3227 (see e.g., Markowitz et al 2009, and references therein), high frequency BL Lac blazar PKS 2155-304 (e.g., Zhang et al 1999Zhang et al , 2005, optically violent variable blazars 3c279 (e.g., Hartman et al 1996;Chatterjee et al 2008) and 3c345 (e.g., Kidger & de Diego 1990), and quasars 3c454.3 (e.g., Fuhrmann et al 2006;Giommi et al 2006) and 3c273 (e.g., Kaastra & Roos 1992;Xiong et al 2017). These sources are optimal for our analysis as they have a sufficiently large number of observations such that the emission from these events has a temporal coverage similar to those seen for our TDE sample.…”

Section: Brightness As a Function Of Redshiftmentioning

confidence: 99%

A Comparison of the X-Ray Emission from Tidal Disruption Events with those of Active Galactic Nuclei

Auchettl

Ramírez-Ruiz

Guillochon

2018

ApJ

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One of the main challenges of current tidal disruption events (TDEs) studies is that emission arising from AGN activity may potentially mimic the expected X-ray emission of a TDE. Here we compare the X-ray properties of TDEs and AGN to determine a set of characteristics which would allow us to discriminate between flares arising from these two objects. We find that at peak, TDEs are brighter than AGN found at similar redshifts. However, compared to preflare upperlimits, highly variable AGN can produce flares of a similar order of magnitude as those seen from X-ray TDEs. Nevertheless, TDEs decay significantly more monotonically, and their emission exhibits little variation in spectral hardness as a function of time. We also find that X-ray TDEs are less absorbed, and their emission is much softer than the emission detected from AGN found at similar redshifts. We derive the X-ray luminosity function (LF) for X-ray TDEs using the events from Auchettl et al. (2017). Interestingly, our X-ray LF matches closely the theoretically derived LF by Milosavljević et al. (2006) which assumes a higher TDE rate currently estimated from observations. Using our results and the results of Stone & Metzger (2016), we estimate a TDE rate of (0.7 − 4.7) × 10 −4 yr −1 per galaxy, higher than current observational estimates. We find that TDEs can contribute significantly to the LF of AGN for z 0.4, while there is no evidence that TDEs influence the growth of 10 6−7 M BHs. However, BHs < 10 6 M can grow from TDEs arising from super-Eddington accretion without contributing significantly to the observed AGN LF at z = 0.

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Section: Brightness As a Function Of Redshiftmentioning

confidence: 99%

A Comparison of the X-Ray Emission from Tidal Disruption Events with those of Active Galactic Nuclei

Auchettl

Ramírez-Ruiz

Guillochon

2018

ApJ

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“…So in addition to the already known variability of many sources in the lower energy bands (for a review see Wagner & Witzel 1995), the blazar Mkn 421 was discovered to exhibit TeV flares, the fastest of which had a duration of about 15 minutes (Gaidos et al 1996), while in the case of Mkn 501 the reported variability is about one day (Aharonian et al 1999). More powerful sources, such as 3C 279, have shown variability in the GeV regime of the order of an hour (Hartman et al 1996). These observations put new, interesting constraints on the theoretical models of high energy emission from AGN since one expects the particle cooling times to be of the order of the flare duration itself.…”

Section: Introductionmentioning

confidence: 97%

Models of Variability in Blazar Jets

Mastichiadis

Kirk

2002

Publ. – Astron. Soc. Aust

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During the last decade multiwavelength observations of blazars have revealed many interesting patterns in their emission across the EM spectrum. In the present article we will review the time-dependent one-zone models and the models which advocate an acceleration and a radiation zone, and we will make some comparisons between them, especially in light of recent observations of the so-called TeV blazars.

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“…545 cospatially with c-rays are contaminated by another source of X-rays, possibly located at larger distances along the jet and therefore varying on much longer timescales. Superposition of radiation components produced at lower and higher distances can also explain progressively weaker variability in the synchrotron component at lower frequencies (Brown et al 1989 ;Edelson 1992 ;Hartman et al 1996 ;Ulrich et al 1997). Since both sources located at smaller and larger distances are related to dissipation events presumably triggered by collisions between inhomogeneities propagating down the jet at di †erent velocities, one can expect that the location and strength of these collisions change with time.…”

Section: Introductionmentioning

confidence: 99%

Comptonization of Infrared Radiation from Hot Dust by Relativistic Jets in Quasars

Błażejowski

Sikora

Moderski

et al. 2000

ApJ

412

300

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We demonstrate the importance of near-infrared radiation from hot dust for Compton cooling of electrons/positrons in quasar jets. In our model, we assume that the nonthermal radiation spectra observed in optically violent variable (OVV) quasars are produced by relativistic electrons/positrons accelerated in thin shells that propagate down the jet with relativistic speeds. We show that the Comptonization of the near-IR Ñux is likely to dominate the radiative output of OVV quasars in the energy range from tens of keV up to hundreds of MeV, where it exceeds that produced by Comptonization of the UV radiation reprocessed and rescattered in the broad emission line (BEL) region. The main reason for this lies in the fact that the jet encounters the ambient IR radiation over a relatively large distance as compared to the distance where the energy density of the BEL light peaks. In the soft to mid-energy X-ray band, the spectral component resulting from Comptonization of the near-IR radiation joins smoothly with the synchrotron self-Compton component, which may be responsible for the soft X-ray Ñux. At the highest observed c-ray energies, in the GeV range, Comptonization of broad emission lines dominates over other components.

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Simultaneous Multiwavelength Spectrum and Variability of 3C 279 from 10 9 to 10 24 Hz

Cited by 116 publications

References 0 publications

A Comparison of the X-Ray Emission from Tidal Disruption Events with those of Active Galactic Nuclei

A Comparison of the X-Ray Emission from Tidal Disruption Events with those of Active Galactic Nuclei

Models of Variability in Blazar Jets

Comptonization of Infrared Radiation from Hot Dust by Relativistic Jets in Quasars

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