Long-term optical behavior of 144 compact extragalactic objects - 1969-1988

Pica, A. J.; Smith, Alex; Webb, J. R.; Leacock, R. J.; Clements, S. D.; Gombola, P. P.

doi:10.1086/114875

Cited by 102 publications

(131 citation statements)

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“…CTA 102 also shows a jet with superluminal motions of up to 21 c, derived from VLBI observations (see, Jorstad et al 2001;Rantakyrö et al 2003;Jorstad et al 2005). Its history of optical variability can be tracked back to 1973 (Pica et al 1988), with sporadic detections afterwards (see, for example, Wilkes et al 1994;Ghosh et al 2000;Véron-Cetty & Véron 2001;Romero et al 2002). We report here a clear internight variability in both R and V bands.…”

Section: Pks 1510−089supporting

confidence: 51%

“…A tentative value of z ≈ 0.63 was estimated (Rector & Stocke 2001) and then confirmed at z = 0.635 (Landoni et al 2012). This BLLac object, as most of its kind, shows variability at almost every wavelength range, from radio to optical bands (Pica et al 1988). It has also been detected in X-rays (Brinkmann et al 2000).…”

Section: Resultsmentioning

confidence: 87%

“…Its long-term variability at optical bands can be traced back to 1980 (e.g. Baumert 1980;Pica et al 1988;Sillanpaa et al 1991;Katajainen et al 2000). Infrared variations were detected by Fan & Lin (1999), as well as a radio flare by Nieppola et al (2009).…”

Section: Resultsmentioning

confidence: 97%

“…Its emission spans from radio wavelengths to gamma-rays, including optical and X-ray bands (Kataoka et al 2008;Cusumano et al 2010). This quasar has an extensive history of long and short-term variability at optical bands (see, for example, Liller & Liller 1975;Pica et al 1988;Villata et al 1997;Romero et al 2002;Cellone et al 2007), with continuous changes in brightness over long periods of time. Moreover, optical polarization has been detected with variability both in P and in position angle θ (Andruchow et al 2005), as well as a rapid variation in γ-rays (D' Ammando et al 2009).…”

Section: Pks 1510−089mentioning

confidence: 99%

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Optical flux behaviour of a sample ofFermiblazars

Marchesini

Andruchow

Cellone

et al. 2016

A&A

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Aims. We aim at investigating the time-behaviour of a sample of gamma-ray blazars. We present the results from a 13 monthlong optical photometry monitoring campaign of the blazars PKS 0048−097, PKS 0754+100, [HB89] 0827+243, PKS 0851+202, PKS 1253−055, PKS 1510−089, PKS 1749+096, PKS 2230+114 and PKS 2251+158. Methods. We analyse the variability of each object, focusing on different time-scales (long term, short term, and microvariability), in an attempt to achieve a statistical comparison of the results. Results. After applying a geometric model to explain the variability results, we found that it is possible that a slight change in the direction of the jet generates the variations detected in some objects during this campaign.

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Section: Pks 1510−089supporting

confidence: 51%

Section: Resultsmentioning

confidence: 87%

Section: Resultsmentioning

confidence: 97%

Section: Pks 1510−089mentioning

confidence: 99%

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Optical flux behaviour of a sample ofFermiblazars

Marchesini

Andruchow

Cellone

et al. 2016

A&A

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“…(1) Griffiths et al (1979); (2) Griffiths et al (1979), (3) Miller & McAlister (1983), (4) Brindle et al (1986), (5) Hamuy & Maza (1987), (6) Pica et al (1988), (7) Treves et al (1989), (8) Mead et al (1990), (9) Smith & Sitko (1991), (10) Carini & Miller (1992), (11) Smith et al (1992), (12) Jannuzi et al (1993) and (13) Urry et al (1993) as collected in Zhang & Xie (1996); (14) Campbell (2004), (15) Courvoisier et al (1995) and (16) Pesce et al (1997) as collected in Osterman et al (2007); (17) Tommasi et al (2001). Table 1 shows statistics of the data on PKS 2155-304.…”

Section: Summary Of Observationsmentioning

confidence: 99%

Long-term optical variability of PKS 2155-304

Kastendieck

Ashley

Horns

2011

A&A

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Aims. The optical variability of the blazar PKS 2155-304 is investigated to characterise the red noise behaviour at largely different time scales from 20 days to O(>10 yrs). Methods. The long-term optical light curve of PKS 2155-304 is assembled from archival data as well as from so-far unpublished observations mostly carried out with the ROTSE-III and the ASAS robotic telescopes. A forward folding technique is used to determine the best-fit parameters for a model of a power law with a break in the power spectral density function (PSD). The best-fit parameters are estimated using a maximum-likelihood method with simulated light curves in conjunction with the Lomb-Scargle periodogram and the first-order structure function (SF). In addition, a new approach based upon the so-called multiple fragments variance function (MFVF) is introduced and compared to the other methods. Simulated light curves have been used to confirm the reliability of these methods as well as to estimate the uncertainties of the best-fit parameters. Results. The light curve is consistent with the assumed broken power-law PSD. All three methods agree within the estimated uncertainties with the MFVF providing the most accurate results. The red-noise behaviour of the PSD in frequency f follows a power law with f −β , β = 1.8 +0.1 −0.2 and a break towards f 0 at frequencies lower than f min = (2.7 +2.2 −1.6 yrs) −1 .

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Introduction

Fromm¹

2014

Spectral Evolution in Blazars

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Long-term optical behavior of 144 compact extragalactic objects - 1969-1988

Cited by 102 publications

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Optical flux behaviour of a sample ofFermiblazars

Optical flux behaviour of a sample ofFermiblazars

Long-term optical variability of PKS 2155-304

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