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Radio follow-up of the gamma-ray flaring gravitational lens JVAS B0218+357

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Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
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Cristiana Spingola, D. Dallacasa, M. Orienti, M. Giroletti, J. P. McKean, C. C. Cheung, T. Hovatta, S. Ciprini
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F. D'Ammando, E. Falco, S. Larsson, W. Max-Moerbeck, R. Ojha, A. C. S. Readhead, J. L. Richards, J. Scargle

Astrophysics of Galaxies · Submitted 14 Jan 2016

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim The radio light curves did not reveal any significant flux density variability, suggesting that no clear correlation between the high energy and low-energy emission is present.

how it is stated · hedged possibility 0.94 read the record →

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arXiv ID1601.03591 (version 1)
Pith IDTT2TWUM3, Pith's permanent record of this paper and its review
CitationA. C. S. Readhead, C. C. Cheung, Cristiana Spingola, D. Dallacasa, E. Falco, F. D'Ammando, J. L. Richards, J. P. McKean, J. Scargle, M. Giroletti, M. Orienti, R. Ojha, S. Ciprini, S. Larsson, T. Hovatta, W. Max-Moerbeck. "Radio follow-up of the gamma-ray flaring gravitational lens JVAS B0218+357." arXiv:1601.03591 (2016). https://pith.science/paper/TT2TWUM3
Claim paper

The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,059 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.53 · human participants 0.01 · controlled comparison 0.07 · randomized assignment 0.01 · states quantitative result 0.64 · compares with prior results 0.45 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; .

We present results on multifrequency Very Long Baseline Array (VLBA) monitoring observations of the double-image gravitationally lensed blazar JVAS B0218+357. Multi-epoch observations started less than one month after the gamma-ray flare detected in 2012 by the Large Area Telescope on board Fermi, and spanned a 2-month interval. The radio light curves did not reveal any significant flux density variability, suggesting that no clear correlation between the high energy and low-energy emission is present. This behaviour was confirmed also by the long-term Owens Valley Radio Observatory monitoring data at 15 GHz. The milliarcsecond-scale resolution provided by the VLBA observations allowed us to resolve the two images of the lensed blazar, which have a core-jet structure. No significant morphological variation is found by the analysis of the multi-epoch data, suggesting that the region responsible for the gamma-ray variability is located in the core of the AGN, which is opaque up to the highest observing frequency of 22 GHz.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 We present results on multifrequency Very Long Baseline Array (VLBA) monitoring observations of the double-image gravitationally lensed blazar JVAS B0218+357. contribution 0.99 0.94 0.04 asserted 0.97
s1 Multi-epoch observations started less than one month after the gamma-ray flare detected in 2012 by the Large Area Telescope on board Fermi, and spanned a 2-month interval. method 0.95 0.83 0.03 asserted 1.00
s2 The radio light curves did not reveal any significant flux density variability, suggesting that no clear correlation between the high energy and low-energy emission is present. result 0.72 0.94 0.72 hedged possibility 0.94
s3 This behaviour was confirmed also by the long-term Owens Valley Radio Observatory monitoring data at 15 GHz. result 0.92 0.57 0.13 asserted 1.00
s4 The milliarcsecond-scale resolution provided by the VLBA observations allowed us to resolve the two images of the lensed blazar, which have a core-jet structure. result 0.80 0.95 0.06 asserted 1.00
s5 No significant morphological variation is found by the analysis of the multi-epoch data, suggesting that the region responsible for the gamma-ray variability is located in the core of the AGN, which is opaque up to the highest observing frequency of 22 GHz. interpretation 0.94 0.95 0.41 hedged possibility 0.91

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.99.

What was examined, and what was not

sources read
  • arXiv listing abstract v1
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

We present results on multifrequency Very Long Baseline Array (VLBA) monitoring observations of the double-image gravitationally lensed blazar JVAS B0218+357. Multi-epoch observations started less than one month after the gamma-ray flare detected in 2012 by the Large Area Telescope on board Fermi, and spanned a 2-month interval. The radio light curves did not reveal any significant flux density variability, suggesting that no clear correlation between the high energy and low-energy emission is present. This behaviour was confirmed also by the long-term Owens Valley Radio Observatory monitoring data at 15 GHz. The milliarcsecond-scale resolution provided by the VLBA observations allowed us to resolve the two images of the lensed blazar, which have a core-jet structure. No significant morphological variation is found by the analysis of the multi-epoch data, suggesting that the region responsible for the gamma-ray variability is located in the core of the AGN, which is opaque up to the highest observing frequency of 22 GHz.

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