Polarization microvariability of BL Lacertae objects

Andruchow, I.; Romero, Gustavo E.; Cellone, S. A.

doi:10.1051/0004-6361:20053325

Cited by 78 publications

(73 citation statements)

References 27 publications

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“…The optical observations discussed in the previous paragraph bracket the VHE detections of PG 1553+113 by HESS Aharonian et al (2006) and MAGIC Albert et al (2007) in 2005 …”

Section: Discussionsupporting

confidence: 59%

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High-temporal resolution optical observations of the gamma-ray blazar PG 1553+113

et al. 2010

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Abstract. We present here the results of an observational photo-polarimetry campaign at optical wavelengths of the blazar PG 1553+113, which was recently detected at very high energies (> 100 GeV) by the H.E.S.S and MAGIC γ-ray experiments.Our high-temporal resolution data show significant variations in the linear polarization percentage and position angle at inter-night time-scales, while at shorter (intra-night) time-scales both parameters varied less significantly, if at all. Simultaneous differential photometry (at the B and R bands) shows no significant variability in the total optical flux.

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“…The optical observations discussed in the previous paragraph bracket the VHE detections of PG 1553+113 by HESS Aharonian et al (2006) and MAGIC Albert et al (2007) in 2005 …”

Section: Discussionsupporting

confidence: 59%

“…In the same period, ref. Andruchow et al (2005) followed the source in P (V filter) during two nights. P and θ showed then microvariations with a most likely flickering behaviour.…”

Section: Discussionmentioning

confidence: 99%

High-temporal resolution optical observations of the gamma-ray blazar PG 1553+113

et al. 2010

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“…However, have proposed a new classification based on the broad-line region (BLR) luminosity in units of Eddington luminosity, with FSRQs having higher BLR luminosity (L BLR / L Edd > 5 × 10 −4 ). Both classes share many common properties, such as flat radio spectra (a n < µ n a -0.5; S r ) at GHz frequencies, rapid flux,and polarization variations (Wagner & Witzel 1995;Andruchow et al 2005), and exhibit superluminal patterns at radio wavelengths (Jorstad et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Multi-Wavelength Observations of 3c 279 During the Extremely Bright Gamma-Ray Flare in 2014 March–april

Paliya

Sahayanathan

Stalin

2015

ApJ

110

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The well-studied blazar 3C 279 underwent a giant γ-ray outburst in 2014 March-April. The measured γ-ray flux (1.21 ± 0.10 × 10 −5 --ph cm s 2 1 in a 0.1-300 GeV energy range) is the highest detected from 3C 279 by theFermi Large Area Telescope. Hour-scale γ-ray flux variability is observed, with a flux doubling time as short as 1.19 ± 0.36 hr detected during one flare. The γ-ray spectrum is found to be curved at the peak of the flare, suggesting low probability of detecting very high energy (VHE; E > 100 GeV) emission, which is further confirmed by the VERITAS observations. The γ-ray flux increased by more than an order in comparison to a low-activity state and the flare consists of multiple sub-structures having a fast rise and slow decay profile. The flux enhancement is seen in all the wavebands, though at a lesser extent compared to γ-rays. During the flare, a considerable amount of the kinetic jet power gets converted to γ-rays and the jet becomes radiatively efficient. A one-zone leptonic emission model is used to reproduce the flare and we find increase in the bulk Lorentz factor as a major cause of the outburst. From the observed fast variability, lack of VHE detection, and the curved γ-ray spectrum, we conclude that the location of the emission region cannot be far out from the broadline region (BLR) and contributions from both BLR and torus photons are required to explain the observed γ-ray spectrum.

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“…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). Simultaneously with this γ-ray flare, these authors also found intense variability at optical and radio wavelengths.…”

Section: Pks 1510−089mentioning

confidence: 99%

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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Polarization microvariability of BL Lacertae objects

Cited by 78 publications

References 27 publications

High-temporal resolution optical observations of the gamma-ray blazar PG 1553+113

High-temporal resolution optical observations of the gamma-ray blazar PG 1553+113

Multi-Wavelength Observations of 3c 279 During the Extremely Bright Gamma-Ray Flare in 2014 March–april

Optical flux behaviour of a sample ofFermiblazars

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