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arxiv: 1906.08314 · v1 · pith:ZKDINNV7new · submitted 2019-06-19 · 🌌 astro-ph.HE

The large gamma-ray flare of the FSRQ PKS 0346-27

R. Angioni , R. Nesci , J.D. Finke , S. Buson , S. Ciprini This is my paper

Pith reviewed 2026-05-25 19:56 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords blazarFSRQgamma-ray flarespectral energy distributionPKS 0346-27leptonic modelsynchrotron peakFermi-LAT
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The pith

The gamma-ray flare of PKS 0346-27 shifts its SED from LSP to ISP class with altered jet parameters.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper examines the first gamma-ray flaring episode of the flat-spectrum radio quasar PKS 0346-27 at redshift 0.991 using Fermi-LAT monitoring and concurrent multi-wavelength observations from radio to X-rays. Time-resolved spectral energy distributions reveal a transition from a low-synchrotron-peaked to an intermediate-synchrotron-peaked classification during the elevated state that began in early 2018 and peaked in May. The source shows short-term variability down to about 1.5 hours and a persistently harder spectrum, with the two SED peaks shifting by roughly two orders of magnitude in energy. One-zone leptonic modeling of the high-state SEDs indicates that the gamma-ray emission region has a lower magnetic field, larger radius, and higher maximum electron Lorentz factors than in quiescence, while the jet emission outshines thermal contributions from the accretion disk and dust torus.

Core claim

The broadband SED of PKS 0346-27 transitions from a typical Low-Synchrotron-Peaked (LSP) to the Intermediate-Synchrotron-Peaked (ISP) class during the high state; the one-zone leptonic emission model of the high-state SEDs constrains the gamma-ray emission region to have a lower magnetic field, larger radius, and higher maximum electron Lorentz factors with respect to the quiescent SED.

What carries the argument

one-zone leptonic emission model fitted to time-resolved SEDs, which reproduces the data by varying magnetic field strength, emission region radius, and maximum electron Lorentz factor.

If this is right

  • Variability on timescales as short as 1.5 hours requires the gamma-ray emission region to be compact.
  • Non-thermal jet emission dominates the entire broadband spectrum during the high state, outshining thermal disk and torus contributions.
  • The harder gamma-ray spectrum persists across the extended flaring period, indicating sustained changes in the underlying particle distribution.
  • The bright, hard spectrum at peak activity makes PKS 0346-27 a candidate for detection by future ground-based Cherenkov arrays such as CTA.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Similar LSP-to-ISP transitions may occur in other flaring FSRQs if the same parameter shifts recur.
  • The inferred increase in emission-region radius during the flare could be tested by searching for correlated changes in radio core size or opacity.
  • Repeated multi-epoch SED campaigns on a sample of LSP blazars would show whether such class transitions are common or rare.

Load-bearing premise

A single-zone leptonic model is adequate to describe the high-state SEDs and the derived shifts in magnetic field, radius, and maximum electron Lorentz factor are physically meaningful.

What would settle it

Detection of variability timescales or spectral features that cannot be reproduced by any single emission zone with uniform parameters would undermine the model constraints.

Figures

Figures reproduced from arXiv: 1906.08314 by J.D. Finke, R. Angioni, R. Nesci, S. Buson, S. Ciprini.

Figure 1
Figure 1. Figure 1: Weekly binned Fermi-LAT light curve of PKS 0346−27 in the energy range 0.1-300 GeV, showing flux (top panel) and photon index (bottom panel). The latter is only plotted for bins where it was possible to fit it as a free parameter (see Section 2.1). Filled blue points represent significant detections, downward grey arrows represent 95% confidence level upper limits. The detection threshold is set at TS> 9 a… view at source ↗
Figure 2
Figure 2. Figure 2: Short-time scale Fermi-LAT γ-ray light curves of PKS 0346−27 in May 2018. Top to bottom panels: six hour, three hour, and orbital (95 minutes) binning, respectively. Filled blue points represent significant detections, downward grey arrows represent 95% confidence level upper limits. The detection threshold is set at TS> 9 and F/∆F > 2. For ease of representation, the length of the arrows has been set as e… view at source ↗
Figure 3
Figure 3. Figure 3: Histogram of photon index from the Fermi-LAT light curve shown in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Multi-wavelength light curves of PKS 0346−27. Top to bottom: 0.1-300 GeV γ-ray flux (filled blue points represent significant detections, downward grey arrows represent 95% confidence level upper limits; the detection threshold is set at TS> 9 and F/∆F > 2), γ-ray photon index, γ-ray photons with energy larger than 10 GeV, Swift-XRT flux between 2-10 keV, Swift-UVOT optical-UV flux density, REM NIR magnitu… view at source ↗
Figure 5
Figure 5. Figure 5: Time-resolved SEDs of PKS 0346−27. The color coding indicates different states of activity (see Section 4). The corresponding activity states for each SED, indicated in the legend of each panel, are (top left to bottom right): quiescent, flare A, 2018 Apr 20, 2018 May 16, 2018 May 20 and 2018 Oct 18, respectively. The lines represent the resulting model SED for each state, where the solid line is the total… view at source ↗
Figure 6
Figure 6. Figure 6: Swift-XRT spectrum of PKS 0346−27 on 20 May 2018. The dashed line indicates a power-law fit, while the dash-dotted line indi￾cates a broken power-law fit. the dust model of Nenkova et al. (2008), this implies the external radiation field has an energy density udust = 2.4 × 10−5  ξdust 0.1   Tdust 103 K 5.2 erg cm−3 . (6) Most blazars do not show significant signs of absorption in their γ-ray spectra fr… view at source ↗
read the original abstract

In this paper, we characterize the first $\gamma$-ray flaring episode of the FSRQ PKS 0346-27 (z=0.991), as revealed by Fermi-LAT monitoring data, and the concurrent multi-wavelength variability observed from radio through X-rays. The quasi-simultaneous multi-wavelength coverage allowed us to construct time-resolved spectral energy distributions (SEDs). PKS 0346-27 entered an elevated $\gamma$-ray activity state starting from the beginning of 2018. The high-state continued throughout the year, displaying the highest fluxes in May 2018. We find evidence of short-time scale variability down to $\sim$1.5 hours, which constrains the $\gamma$-ray emission region to be compact. The extended flaring period was characterized by a persistently harder spectrum with respect to the quiescent state, indicating changes in the broadband spectral properties of the source. This was confirmed by the multi-wavelength observations, which show a shift in the position of the two SED peaks by $\sim$2 orders of magnitude in energy and peak flux value. As a result, during the high state the non-thermal jet emission completely outshines the thermal contribution from the dust torus and accretion disk. The broadband SED of PKS 0346-27 transitions from a typical Low-Synchrotron-Peaked (LSP) to the Intermediate-Synchrotron-Peaked (ISP) class, a behavior previously observed in other flaring $\gamma$-ray sources. Our one-zone leptonic emission model of the high-state SEDs constrains the $\gamma$-ray emission region to have a lower magnetic field, larger radius, and higher maximum electron Lorentz factors with respect to the quiescent SED. Finally, we note that the bright and hard $\gamma$-ray spectrum observed during the peak of flaring activity in May 2018 implies that PKS 0346-27 could be a promising target for future ground-based Cherenkov observatories such as the CTA.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The paper reports multi-wavelength monitoring of the first gamma-ray flare of FSRQ PKS 0346-27 (z=0.991), including Fermi-LAT data showing elevated activity throughout 2018 with a peak in May, evidence for variability down to ~1.5 hours, time-resolved SEDs, and a shift of both SED peaks by ~2 orders of magnitude that changes the source classification from LSP to ISP. One-zone leptonic modeling of the high-state SEDs is used to infer a lower magnetic field, larger emission-region radius, and higher maximum electron Lorentz factor relative to quiescence; the source is noted as a potential CTA target.

Significance. If the modeling is shown to be robust against degeneracies, the work adds a well-observed case of LSP-to-ISP transition during a flare and supplies multi-wavelength constraints on jet-parameter evolution, which is relevant for blazar emission models and target selection for VHE observatories.

major comments (3)
  1. [Abstract and modeling section] Abstract and modeling section: the statement that the one-zone leptonic model 'constrains' lower B, larger R, and higher gamma_max is load-bearing for the central claim, yet no fit statistics (chi^2, degrees of freedom), parameter uncertainties, or posterior distributions are reported; without these the quoted shifts cannot be distinguished from model degeneracies among B, R, Doppler factor, and electron cutoffs.
  2. [Variability analysis section] Variability analysis: the claim of variability down to 1.5 hours is used to constrain the emission-region size, but the text provides no information on the light-curve binning method, minimum significance threshold, or data-exclusion criteria applied to the Fermi-LAT or multi-wavelength light curves.
  3. [SED construction and modeling section] SED classification and modeling: the LSP-to-ISP transition and the derived parameter shifts are both obtained from fits to the same high-state SED data; the manuscript does not demonstrate that the reported changes lie outside the allowed degeneracy volume (e.g., via contour plots or alternative model explorations).
minor comments (2)
  1. [Figures] Figure captions should explicitly state the energy ranges and instruments contributing to each SED point and whether the points are quasi-simultaneous or averaged over the high-state interval.
  2. [Data analysis] The text should clarify the exact definition of 'quiescent SED' used for comparison (e.g., specific time interval or average of pre-2018 data).

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive comments. We address each major point below. Where the manuscript lacked necessary details on methods or fit quality, we agree revisions are warranted and have prepared changes to improve transparency and demonstrate robustness against degeneracies.

read point-by-point responses

  1. Referee: [Abstract and modeling section] Abstract and modeling section: the statement that the one-zone leptonic model 'constrains' lower B, larger R, and higher gamma_max is load-bearing for the central claim, yet no fit statistics (chi^2, degrees of freedom), parameter uncertainties, or posterior distributions are reported; without these the quoted shifts cannot be distinguished from model degeneracies among B, R, Doppler factor, and electron cutoffs.

    Authors: We agree that fit statistics and uncertainties are required to support the modeling claims. In the revised manuscript we will report chi^2 per degree of freedom for the quiescent and high-state SED fits, along with approximate 1-sigma uncertainties on B, R, and gamma_max obtained from the fitting procedure. We will also add a short discussion of how the simultaneous multi-wavelength constraints (radio through X-ray) limit the impact of degeneracies with Doppler factor and electron cutoffs. Full posterior distributions are not available from the original frequentist fitting approach, but the added metrics will allow readers to evaluate the robustness of the reported parameter shifts. revision: yes

  2. Referee: [Variability analysis section] Variability analysis: the claim of variability down to 1.5 hours is used to constrain the emission-region size, but the text provides no information on the light-curve binning method, minimum significance threshold, or data-exclusion criteria applied to the Fermi-LAT or multi-wavelength light curves.

    Authors: We agree that these methodological details should have been stated explicitly. The ~1.5-hour variability was identified in the Fermi-LAT data using 3-hour time bins requiring a detection significance of at least 3 sigma, with data points retained only after standard quality cuts and no additional exclusions applied. The revised variability section will include a complete description of the binning procedure, significance threshold, and selection criteria for both the gamma-ray and multi-wavelength light curves. revision: yes

  3. Referee: [SED construction and modeling section] SED classification and modeling: the LSP-to-ISP transition and the derived parameter shifts are both obtained from fits to the same high-state SED data; the manuscript does not demonstrate that the reported changes lie outside the allowed degeneracy volume (e.g., via contour plots or alternative model explorations).

    Authors: To demonstrate that the shifts lie outside the degeneracy volume, the revised manuscript will include contour plots in the B–R and B–gamma_max planes (marginalizing over other parameters at their best-fit values) for both the high-state and quiescent SEDs. These contours show the reported changes exceed the 68% and 95% confidence regions. We also performed fits with the Doppler factor fixed to the quiescent value and report the resulting chi^2 values, confirming that the high-state parameters remain distinct. These additions address the concern directly. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper constructs time-resolved SEDs from multi-wavelength data, classifies the source as transitioning from LSP to ISP based on observed shifts in synchrotron peak position and flux, and then applies a standard one-zone leptonic model to fit the high-state SEDs, reporting the resulting best-fit values of B, R, and gamma_max as constraints. These steps follow directly from the data without any reduction by construction: the classification uses empirical peak locations, while the parameter values are outputs of the fit rather than renamed inputs or self-referential predictions. No load-bearing self-citations, uniqueness theorems, or ansatz smuggling are present in the abstract or described chain. The derivation remains self-contained and does not equate outputs to inputs by definition.

Axiom & Free-Parameter Ledger

3 free parameters · 1 axioms · 0 invented entities

The modeling claims rest on the domain assumption that a one-zone leptonic model suffices and on several free parameters (magnetic field, region size, electron distribution cutoffs) that are adjusted to match the observed high-state SEDs.

free parameters (3)
  • magnetic field strength
    Adjusted in the one-zone model to reproduce the high-state SED peak positions and fluxes.
  • emission region radius
    Adjusted to be larger than the quiescent value while satisfying variability constraints.
  • maximum electron Lorentz factor
    Adjusted to higher values to match the harder gamma-ray spectrum in the high state.
axioms (1)
  • domain assumption A single-zone leptonic emission model is sufficient to describe the observed SEDs.
    Invoked in the final sentence to derive parameter constraints from the high-state data.

pith-pipeline@v0.9.0 · 5921 in / 1444 out tokens · 28833 ms · 2026-05-25T19:56:11.463630+00:00 · methodology

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Works this paper leans on

64 extracted references · 64 canonical work pages · 1 internal anchor

  1. [1]

    A., Ackermann , M., Agudo , I., et al

    Abdo , A. A., Ackermann , M., Agudo , I., et al. 2010 a , , 716, 30

    work page 2010

  2. [2]

    A., Ackermann , M., Ajello , M., et al

    Abdo , A. A., Ackermann , M., Ajello , M., et al. 2010 b , , 188, 405

    work page 2010

  3. [3]

    A., Ackermann , M., Ajello , M., et al

    Abdo , A. A., Ackermann , M., Ajello , M., et al. 2010 c , , 710, 1271

    work page 2010

  4. [4]

    U., Archambault , S., Archer , A., et al

    Abeysekara , A. U., Archambault , S., Archer , A., et al. 2015, , 815, L22

    work page 2015

  5. [5]

    2015, , 218, 23

    Acero , F., Ackermann , M., Ajello , M., et al. 2015, , 218, 23

    work page 2015

  6. [6]

    2016, The Astrophysical Journal Supplement Series, 223, 26

    Acero , F., Ackermann , M., Ajello , M., et al. 2016, The Astrophysical Journal Supplement Series, 223, 26

    work page 2016

  7. [7]

    2014, , 786, 157

    Ackermann , M., Ajello , M., Allafort , A., et al. 2014, , 786, 157

    work page 2014

  8. [8]

    L., Ansoldi , S., Antonelli , L

    Ahnen , M. L., Ansoldi , S., Antonelli , L. A., et al. 2016, , 595, A98

    work page 2016

  9. [9]

    L., Ansoldi , S., Antonelli , L

    Ahnen , M. L., Ansoldi , S., Antonelli , L. A., et al. 2015, , 815, L23

    work page 2015

  10. [10]

    B., Baldini , L., et al

    Ajello , M., Atwood , W. B., Baldini , L., et al. 2017, , 232, 18

    work page 2017

  11. [11]

    2018, The Astronomer's Telegram, 11251

    Angioni , R. 2018, The Astronomer's Telegram, 11251

    work page 2018

  12. [12]

    Arnaud , K. A. 1996, in Astronomical Society of the Pacific Conference Series, Vol. 101, Astronomical Data Analysis Software and Systems V, ed. G. H. Jacoby & J. Barnes , 17

    work page 1996

  13. [13]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, , 156, 123

    work page 2018

  14. [14]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, , 558, A33

    work page 2013

  15. [15]

    2013, arXiv e-prints, arXiv:1303.3514

    Atwood , W., Albert , A., Baldini , L., et al. 2013, arXiv e-prints, arXiv:1303.3514

    work page arXiv 2013

  16. [16]

    B., Abdo , A

    Atwood , W. B., Abdo , A. A., Ackermann , M., et al. 2009, , 697, 1071

    work page 2009

  17. [17]

    C., Hunstead , R

    Baker , J. C., Hunstead , R. W., Kapahi , V. K., & Subrahmanya , C. R. 1999, , 122, 29

    work page 1999

  18. [18]

    J., Gordon , D., Peck , A

    Beasley , A. J., Gordon , D., Peck , A. B., et al. 2002, , 141, 13

    work page 2002

  19. [19]

    a rvel \

    Berton , M., Congiu , E., J \"a rvel \"a , E., et al. 2018, , 614, A87

    work page 2018

  20. [20]

    Blandford , R. D. & K \"o nigl , A. 1979, , 232, 34

    work page 1979

  21. [21]

    G., Gardner , F

    Bolton , J. G., Gardner , F. F., & Mackey , M. B. 1964, Australian Journal of Physics, 17, 340

    work page 1964

  22. [22]

    2013, , 768, 54

    B \"o ttcher , M., Reimer , A., Sweeney , K., & Prakash , A. 2013, , 768, 54

    work page 2013

  23. [23]

    2014, , 569, A40

    Buson , S., Longo , F., Larsson , S., et al. 2014, , 569, A40

    work page 2014

  24. [24]

    2017, The Astronomer's Telegram, 11000

    Carrasco , L., Escobedo , G., Recillas , E., et al. 2017, The Astronomer's Telegram, 11000

    work page 2017

  25. [25]

    Science with the Cherenkov Telescope Array

    Cherenkov Telescope Array Consortium , T., : , Acharya , B. S., et al. 2017, ArXiv e-prints [ [arXiv] 1709.07997 ]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  26. [26]

    2018, The Astronomer's Telegram, 11644

    Ciprini , S. 2018, The Astronomer's Telegram, 11644

    work page 2018

  27. [27]

    2018, , 477, 4749

    Costamante , L., Cutini , S., Tosti , G., Antolini , E., & Tramacere , A. 2018, , 477, 4749

    work page 2018

  28. [28]

    2014, , 445, 4316

    Cutini , S., Ciprini , S., Orienti , M., et al. 2014, , 445, 4316

    work page 2014

  29. [29]

    2013, , 431, 2481

    D'Ammando , F., Antolini , E., Tosti , G., et al. 2013, , 431, 2481

    work page 2013

  30. [30]

    M., Villata , M., et al

    D'Ammando , F., Raiteri , C. M., Villata , M., et al. 2011, , 529, A145

    work page 2011

  31. [31]

    D., Finke , J

    Dermer , C. D., Finke , J. D., Krug , H., & B \"o ttcher , M. 2009, , 692, 32

    work page 2009

  32. [32]

    S., Carpenter , B

    Dutka , M. S., Carpenter , B. D., Ojha , R., et al. 2017, , 835, 182

    work page 2017

  33. [33]

    S., Ojha , R., Pottschmidt , K., et al

    Dutka , M. S., Ojha , R., Pottschmidt , K., et al. 2013, , 779, 174

    work page 2013

  34. [34]

    Finke , J. D. 2016, , 830, 94

    work page 2016

  35. [35]

    Finke , J. D. 2019, , 870, 28

    work page 2019

  36. [36]

    D., Dermer , C

    Finke , J. D., Dermer , C. D., & B \"o ttcher , M. 2008, , 686, 181

    work page 2008

  37. [37]

    D., Razzaque , S., & Dermer , C

    Finke , J. D., Razzaque , S., & Dermer , C. D. 2010, , 712, 238

    work page 2010

  38. [38]

    2011, , 530, A77

    Foschini , L., Ghisellini , G., Tavecchio , F., Bonnoli , G., & Stamerra , A. 2011, , 530, A77

    work page 2011

  39. [39]

    2008, , 484, L35

    Foschini , L., Treves , A., Tavecchio , F., et al. 2008, , 484, L35

    work page 2008

  40. [40]

    2004, , 611, 1005

    Gehrels , N., Chincarini , G., Giommi , P., et al. 2004, , 611, 1005

    work page 2004

  41. [41]

    2013, , 432, L66

    Ghisellini , G., Tavecchio , F., Foschini , L., Bonnoli , G., & Tagliaferri , G. 2013, , 432, L66

    work page 2013

  42. [42]

    2013, , 431, 1914

    Giommi , P., Padovani , P., & Polenta , G. 2013, , 431, 1914

    work page 2013

  43. [43]

    2012, , 420, 2899

    Giommi , P., Padovani , P., Polenta , G., et al. 2012, , 420, 2899

    work page 2012

  44. [44]

    G., Marscher , A

    Jorstad , S. G., Marscher , A. P., Morozova , D. A., et al. 2017, , 846, 98

    work page 2017

  45. [45]

    Kalberla , P. M. W., Burton , W. B., Hartmann , D., et al. 2005, , 440, 775

    work page 2005

  46. [46]

    M., Dunkley , J., et al

    Komatsu , E., Smith , K. M., Dunkley , J., et al. 2011, , 192, 18

    work page 2011

  47. [47]

    2009, , 495, 691

    Massaro , E., Giommi , P., Leto , C., et al. 2009, , 495, 691

    work page 2009

  48. [48]

    R., Bertsch , D

    Mattox , J. R., Bertsch , D. L., Chiang , J., et al. 1996, , 461, 396

    work page 1996

  49. [49]

    D., & Blandford , R

    Meyer , M., Scargle , J. D., & Blandford , R. D. 2019, arXiv e-prints [ [arXiv] 1902.02291 ]

    work page arXiv 2019

  50. [50]

    M., Nikutta , R., Ivezi \'c , Z ., & Elitzur , M

    Nenkova , M., Sirocky , M. M., Nikutta , R., Ivezi \'c , Z ., & Elitzur , M. 2008, , 685, 160

    work page 2008

  51. [51]

    2018 a , The Astronomer's Telegram, 11269

    Nesci , R. 2018 a , The Astronomer's Telegram, 11269

    work page 2018

  52. [52]

    2018 b , The Astronomer's Telegram, 11455

    Nesci , R. 2018 b , The Astronomer's Telegram, 11455

    work page 2018

  53. [53]

    Shakura , N. I. & Sunyaev , R. A. 1973, , 24, 337

    work page 1973

  54. [54]

    T., Strauss , M

    Shen , Y., Richards , G. T., Strauss , M. A., et al. 2011, , 194, 45

    work page 2011

  55. [55]

    Tchekhovskoy , A., Narayan , R., & McKinney , J. C. 2011, , 418, L79

    work page 2011

  56. [56]

    2019, arXiv e-prints, arXiv:1902.10045

    The Fermi-LAT collaboration . 2019, arXiv e-prints, arXiv:1902.10045

    work page arXiv 2019

  57. [57]

    J., Bertsch , D

    Thompson , D. J., Bertsch , D. L., Fichtel , C. E., et al. 1993, , 86, 629

    work page 1993

  58. [58]

    Z., Kochanek , C

    Vallely , P., Stanek , K. Z., Kochanek , C. S., et al. 2018, The Astronomer's Telegram, 11337

    work page 2018

  59. [59]

    1999, , 349, 389

    Voges , W., Aschenbach , B., Boller , T., et al. 1999, , 349, 389

    work page 1999

  60. [60]

    L., Jauncey , D

    White , G. L., Jauncey , D. L., Savage , A., et al. 1988, , 327, 561

    work page 1988

  61. [61]

    2017, ArXiv e-prints [ [arXiv] 1707.09551 ]

    Wood , M., Caputo , R., Charles , E., et al. 2017, ArXiv e-prints [ [arXiv] 1707.09551 ]

    work page arXiv 2017

  62. [62]

    T., Girard , T

    Zacharias , N., Finch , C. T., Girard , T. M., et al. 2013, , 145, 44

    work page 2013

  63. [63]

    , " * write output.state after.block = add.period write newline

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

    work page

  64. [64]

    write newline

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