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Early-Time Observations of the GRB 050319 Optical Transient

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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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R. M. Quimby, E. S. Rykoff, S. A. Yost, F. Aharonian, C. W. Akerlof, K. Alatalo, M. C. B. Ashley, E. Goegues
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T. Guever, D. Horns, R. L. Kehoe, Ue. Kiziloglu, T. A. McKay, M. Oezel, A. Phillips, B. E. Schaefer, D. A. Smith, H. F. Swan, W. T. Vestrand, J. C. Wheeler, J. Wren

Astrophysics · Submitted 15 Nov 2005

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

The authors' main claim We discuss the fit results with emphasis placed on the importance of knowing the true start time of the optical transient for this multi-peaked burst.

how it is stated · asserted 0.77 read the record →

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arXiv IDastro-ph/0511421 (version 1)
Pith IDYG2AAXH2, Pith's permanent record of this paper and its review
CitationA. Phillips, B. E. Schaefer, C. W. Akerlof, D. A. Smith, D. Horns, E. Goegues, E. S. Rykoff, F. Aharonian, H. F. Swan, J. C. Wheeler, J. Wren, K. Alatalo, M. C. B. Ashley, M. Oezel, R. L. Kehoe, R. M. Quimby, S. A. Yost, T. A. McKay, T. Guever, Ue. Kiziloglu, W. T. Vestrand. "Early-Time Observations of the GRB 050319 Optical Transient." arXiv:astro-ph/0511421 (2005). https://pith.science/paper/YG2AAXH2
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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, 4,598 input tokens.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.37 · human participants 0.02 · controlled comparison 0.09 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.84 · 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 the unfiltered ROTSE-III light curve of the optical transient associated with GRB 050319 beginning 4 s after the cessation of gamma-ray activity. We fit a power-law function to the data using the revised trigger time given by Chincarini et al. (2005), and a smoothly broken power-law to the data using the original trigger disseminated through the GCN notices. Including the RAPTOR data from Wozniak et al. (2005), the best fit power-law indices are alpha=-0.854 (+/- 0.014) for the single power-law and alpha_1=-0.364 (+/- 0.020), alpha_2= -0.881 (+/- 0.030), with a break at t_b = 418 (+/- 30) s for the smoothly broken fit. We discuss the fit results with emphasis placed on the importance of knowing the true start time of the optical transient for this multi-peaked burst. As Swift continues to provide prompt GRB locations, it becomes more important to answer the question, "when does the afterglow begin" to correctly interpret the light curves.

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 the unfiltered ROTSE-III light curve of the optical transient associated with GRB 050319 beginning 4 s after the cessation of gamma-ray activity. contribution 0.98 0.95 0.07 asserted 1.00
s1 We fit a power-law function to the data using the revised trigger time given by Chincarini et al. (2005), and a smoothly broken power-law to the data using the original trigger disseminated through the GCN notices. method 0.98 0.88 0.05 asserted 0.99
s2 Including the RAPTOR data from Wozniak et al. (2005), the best fit power-law indices are alpha=-0.854 (+/- 0.014) for the single power-law and alpha_1=-0.364 (+/- 0.020), alpha_2= -0.881 (+/- 0.030), with a break at t_b = 418 (+/- 30) s for the smoothly broken fit. result 1.00 0.86 0.16 asserted 1.00
s3 We discuss the fit results with emphasis placed on the importance of knowing the true start time of the optical transient for this multi-peaked burst. interpretation 0.96 0.60 0.28 asserted 0.77
s4 As Swift continues to provide prompt GRB locations, it becomes more important to answer the question, "when does the afterglow begin" to correctly interpret the light curves. interpretation 0.45 0.07 0.27 asserted 0.85

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.57.

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 the unfiltered ROTSE-III light curve of the optical transient associated with GRB 050319 beginning 4 s after the cessation of gamma-ray activity. We fit a power-law function to the data using the revised trigger time given by Chincarini et al. (2005), and a smoothly broken power-law to the data using the original trigger disseminated through the GCN notices. Including the RAPTOR data from Wozniak et al. (2005), the best fit power-law indices are alpha=-0.854 (+/- 0.014) for the single power-law and alpha_1=-0.364 (+/- 0.020), alpha_2= -0.881 (+/- 0.030), with a break at t_b = 418 (+/- 30) s for the smoothly broken fit. We discuss the fit results with emphasis placed on the importance of knowing the true start time of the optical transient for this multi-peaked burst. As Swift continues to provide prompt GRB locations, it becomes more important to answer the question, "when does the afterglow begin" to correctly interpret the light curves.

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