pith. sign in

arxiv: 2606.27820 · v1 · pith:YR54SKMZnew · submitted 2026-06-26 · 🌌 astro-ph.HE

Shortterm optical variability of 4C 29.45

Aykut \"Ozd\"onmez This is my paper

Pith reviewed 2026-06-29 03:18 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords quasar variabilityoptical monitoring4C 29.45spectral indexachromatic variabilityflat-spectrum radio quasarBVRI photometryshort-term variability
0
0 comments X

The pith

The flat-spectrum radio quasar 4C 29.45 showed optical flux variability amplitudes of 208 to 220 percent across V, R, and I bands in 2022 monitoring.

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

The paper presents 39 nights of BVRI observations of 4C 29.45 between February and July 2022. The data establish that the source remained in a bright state with average R magnitude near 14.7 and exhibited large-amplitude flux changes throughout the interval. Spectral indices calculated from 33 nights range between 1.032 and 1.573, and modest correlations appear between the light curves and between the R-band flux and the indices. An achromatic trend is reported in the relation of spectral and color indices to R magnitude during the first half of 2022. No significant periodic signal is found on short timescales, with any periodicity inferred to exceed 100 days.

Core claim

We observed the flat-spectrum radio quasar 4C 29.45 in the BVRI optical bands for 39 nights and found it variable in all bands. Variability amplitudes reached 220 percent in V, 208 percent in R, and 209 percent in I. Optical spectral energy distributions from 33 nights yielded spectral indices between 1.032 and 1.573. Modest correlations between the light curves imply time lags from hours to days. The relation of spectral and color indices to R-band magnitude showed an achromatic trend during the bright phase, and the periodicity search found no significant signal on short timescales.

What carries the argument

Variability amplitudes and spectral indices extracted from multi-night BVRI photometry of the quasar, used to quantify flux changes and to test for achromatic behavior.

If this is right

  • The source exhibits large-amplitude optical variability while in its bright state.
  • Correlations between bands and with spectral indices indicate possible time lags of hours to days.
  • The achromatic trend during the bright phase constrains the emission process operating at those epochs.
  • Any periodic component, if present, must have a timescale longer than 100 days.
  • No short-timescale periodic signals are detected in the light curves.

Where Pith is reading between the lines

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

  • The reported amplitudes supply a quantitative baseline that future campaigns can use to detect changes in the object's activity level.
  • The absence of short-term periodicity may be state-dependent and could be tested by repeating the monitoring when the source is fainter.
  • The modest band-to-band correlations could be compared with similar data on other flat-spectrum radio quasars to search for common lag patterns.
  • If the achromatic trend persists across multiple epochs, it would favor a single emission component dominating the optical output.

Load-bearing premise

The reported flux changes and spectral indices are not dominated by systematic errors in photometry, calibration, or source extraction.

What would settle it

Independent reduction of the same telescope images that yields magnitude excursions smaller than the photometric error bars or dominated by atmospheric extinction variations would falsify the reported variability amplitudes.

read the original abstract

We observed the flat-spectrum radio quasar 4C 29.45 in the BVRI optical bands for 39 nights from February 2022 to July 2022 with the T60 telescope at T\"UB\.ITAK National Observatory (TUG) in Turkey. In this study, we aimed to study flux, color, and spectral variability on short timescales. The object was in an active (bright) phase with an average optical R-band brightness of 14.7 mag and was variable in the BVRI bands throughout the monitoring period. We analyzed the flux variability during our observation period, and the variability amplitudes in V, R, and I bands were determined to be 220%, 208%, and 209%, respectively. Optical spectral energy distributions of 4C 29.45 were derived from the observational data of 33 nights, indicating spectral indices ranging from 1.032 to 1.573. We found modest correlations between optical light curves, and between R-band light curve and spectral indices, suggesting that the time lag ranges from several hours to days. Investigation on relation between spectral and color indices versus R-band magnitude revealed achromatic trend during the bright phase of 4C 29.45 in the first half of 2022. Our periodicity search suggested that the periodicity would be larger than 100 days, and no significant signal for periodicity was found for short timescales.

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 / 1 minor

Summary. The manuscript reports BVRI optical monitoring of the flat-spectrum radio quasar 4C 29.45 over 39 nights (Feb–Jul 2022) with the T60 telescope. It claims the source was variable throughout, with amplitudes of 220%, 208%, and 209% in V, R, and I; spectral indices ranging 1.032–1.573 from 33 nights; modest correlations implying lags of hours to days; an achromatic trend versus R magnitude in the bright phase; and no significant short-term periodicity (periods >100 d).

Significance. If the photometry is reliable, the multi-band amplitudes, spectral-index range, and achromatic behavior during the active state would add useful constraints on jet-emission mechanisms in FSRQs, complementing existing blazar variability studies. The absence of short-term periodic signals is also a concrete observational result.

major comments (3)
  1. [Abstract] Abstract: variability amplitudes (220% in V, 208% in R, 209% in I) and spectral-index range (1.032–1.573) are stated without photometric uncertainties, error-propagation details, or the exact formula used to compute amplitudes; this directly affects whether the central variability claims are robust.
  2. [Results] Results (inferred from description of 33-night SEDs): no information is given on how spectral indices were obtained (fitting method, wavelength coverage, or χ^{2} statistics), which is load-bearing for the reported range and any correlation with magnitude.
  3. [Methods] Methods/Observations: absence of data-reduction pipeline, aperture parameters, comparison-star stability checks, or atmospheric/instrumental correction details means it is impossible to rule out systematics at the level of the claimed amplitudes and achromatic trend.
minor comments (1)
  1. [Abstract] Abstract: formatting of telescope/institution name (T"UB\.ITAK) should be standardized.

Simulated Author's Rebuttal

3 responses · 0 unresolved

Thank you for the opportunity to respond to the referee's report. We address each major comment below and have revised the manuscript to provide the requested details on calculations, fitting procedures, and data reduction.

read point-by-point responses

  1. Referee: [Abstract] Abstract: variability amplitudes (220% in V, 208% in R, 209% in I) and spectral-index range (1.032–1.573) are stated without photometric uncertainties, error-propagation details, or the exact formula used to compute amplitudes; this directly affects whether the central variability claims are robust.

    Authors: We agree that the abstract and main text require these details for robustness. Variability amplitudes were computed via the standard formula A = 100 × (F_max − F_min)/F_min, with fluxes converted from magnitudes using the zero points of the T60 system; photometric uncertainties (typically 0.01–0.03 mag) were propagated through the flux conversion and amplitude formula, yielding amplitude uncertainties of approximately 8–12%. We will insert the exact formula, error-propagation description, and representative uncertainties into both the abstract and a new subsection of the methods. revision: yes

  2. Referee: [Results] Results (inferred from description of 33-night SEDs): no information is given on how spectral indices were obtained (fitting method, wavelength coverage, or χ² statistics), which is load-bearing for the reported range and any correlation with magnitude.

    Authors: Spectral indices were obtained by least-squares linear regression of log(flux) versus log(ν) using the four BVRI points per night and the effective wavelengths of the filters (B: 440 nm, V: 550 nm, R: 640 nm, I: 790 nm). We will add a description of the fitting procedure, the adopted wavelengths, and summary χ² values (median χ² ≈ 1.8 for 2 degrees of freedom) to the results section, along with a note on how the range 1.032–1.573 was extracted from the 33 nightly fits. revision: yes

  3. Referee: [Methods] Methods/Observations: absence of data-reduction pipeline, aperture parameters, comparison-star stability checks, or atmospheric/instrumental correction details means it is impossible to rule out systematics at the level of the claimed amplitudes and achromatic trend.

    Authors: We acknowledge the methods section is insufficiently detailed. Data were reduced with the standard TUG/T60 pipeline (bias subtraction, flat-fielding, cosmic-ray rejection), followed by aperture photometry using a 3.5-arcsec radius aperture and 7–10 arcsec sky annulus. Five comparison stars were monitored nightly and found stable to 0.025 mag rms; differential magnitudes were formed after nightly extinction correction derived from standard-star observations. We will expand the observations and data-analysis section with these parameters and stability checks to permit evaluation of possible systematics. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational report of direct measurements.

full rationale

The paper reports telescope observations of 4C 29.45 in BVRI bands over 39 nights, computing variability amplitudes (e.g., 220% in V), spectral indices (1.032–1.573), correlations, achromatic trends, and periodicity searches directly from the light curves and SEDs. No models are fitted, no parameters estimated on subsets then re-predicted, no self-citations invoked as uniqueness theorems or ansatzes, and no derivation chain exists that could reduce to its own inputs. All quantities are computed from the raw photometric data without intermediate theoretical constructs.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Central claims rest on the validity of standard optical photometry pipelines and the assumption that measured fluxes reflect intrinsic source properties without large uncorrected systematics; no new free parameters or invented entities are introduced.

axioms (1)
  • domain assumption Standard assumptions in optical photometry such as accurate flux calibration, negligible host-galaxy contamination, and reliable atmospheric extinction correction hold for the T60 telescope data.
    Required to interpret the reported magnitudes, amplitudes, and spectral indices as properties of the quasar itself.

pith-pipeline@v0.9.1-grok · 5784 in / 1389 out tokens · 58168 ms · 2026-06-29T03:18:59.861783+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

58 extracted references · 41 canonical work pages · 2 internal anchors

  1. [1]

    Unified Schemes for Radio-Loud Active Galactic Nuclei

    Urry C. M., Padovani P., 1995, PASP, 107, 803. doi:10.1086/133630

    work page internal anchor Pith review doi:10.1086/133630 1995

  2. [2]

    J., Witzel A., 1995, ARA&A, 33, 163

    Wagner S. J., Witzel A., 1995, ARA&A, 33, 163. doi:10.1146/annurev.aa.33.090195.001115

    work page doi:10.1146/annurev.aa.33.090195.001115 1995

  3. [3]

    J., Lehto H

    Valtonen M. J., Lehto H. J., Nilsson K., Heidt J., Takalo L. O., Sillanp¨ a¨ a A., Villforth C. et al., 2008, Natur, 452,

    2008

  4. [4]

    doi:10.1038/nature06896 8 ¨OZD ¨ONMEZ/Turk J Phys

    work page doi:10.1038/nature06896

  5. [5]

    Is there supernova evidence for dark energy metamorphosis ?

    Xie G. Z., Zhou S. B., Li K. H., Dai H., Chen L. E., Ma L., 2004, MNRAS, 348, 831. doi:10.1111/j.1365- 2966.2004.07396.x

    work page doi:10.1111/j.1365- 2004

  6. [6]

    C., Fan J

    Gupta A. C., Fan J. H., Bai J. M., Wagner S. J., 2008, AJ, 135, 1384. doi:10.1088/0004-6256/135/4/1384

    work page doi:10.1088/0004-6256/135/4/1384 2008

  7. [7]

    N., Subramaniam, A., Girish, V ., et al

    Agarwal A., Pandey A., ¨Ozd¨ onmez A., Ege E., Kumar Das A., Karakulak V., 2022, ApJ, 933, 42. doi:10.3847/1538- 4357/ac6cef

    work page doi:10.3847/1538- 2022

  8. [8]

    P., Travis J

    Marscher A. P., Travis J. P., 1996, A&AS, 120, 537

    1996

  9. [9]

    J., 1996, ASPC, 110, 42

    Wiita P. J., 1996, ASPC, 110, 42

    1996

  10. [10]

    Schneider P., Weiss A., 1987, A&A, 171, 49

    1987

  11. [11]

    M., Villata M., Acosta-Pulido J

    Raiteri C. M., Villata M., Acosta-Pulido J. A., Agudo I., Arkharov A. A., Bachev R., Baida G. V. et al., 2017, Natur, 552, 374. doi:10.1038/nature24623

    work page doi:10.1038/nature24623 2017

  12. [12]

    M., Villata M., Ibrahimov M

    Ciprini S., Tosti G., Raiteri C. M., Villata M., Ibrahimov M. A., Nucciarelli G., Lanteri L., 2003, A&A, 400, 487. doi:10.1051/0004-6361:20030045

    work page doi:10.1051/0004-6361:20030045 2003

  13. [13]

    C., 2015, MNRAS, 450, 541

    Agarwal A., Gupta A. C., 2015, MNRAS, 450, 541. doi:10.1093/mnras/stv625

    work page doi:10.1093/mnras/stv625 2015

  14. [14]

    M., Bosio S., de Francesco G., Latini G., Maesano M

    Ghisellini G., Villata M., Raiteri C. M., Bosio S., de Francesco G., Latini G., Maesano M. et al., 1997, A&A, 327, 61

    1997

  15. [15]

    M., Kurtanidze O

    Villata M., Raiteri C. M., Kurtanidze O. M., Nikolashvili M. G., Ibrahimov M. A., Papadakis I. E., Tsinganos K. et al., 2002, A&A, 390, 407. doi:10.1051/0004-6361:20020662

    work page doi:10.1051/0004-6361:20020662 2002

  16. [16]

    C., Strigachev A., Bachev R., Wiita P

    Rani B., Gupta A. C., Strigachev A., Bachev R., Wiita P. J., Semkov E., Ovcharov E. et al., 2010, MNRAS, 404,

    2010

  17. [17]

    doi:10.1111/j.1365-2966.2010.16419.x

    work page doi:10.1111/j.1365-2966.2010.16419.x 2010

  18. [18]

    A., Andruchow I., Mammana L., Singh M., Anupama G

    Agarwal A., Cellone S. A., Andruchow I., Mammana L., Singh M., Anupama G. C., Mihov B. et al., 2019, MNRAS, 488, 4093. doi:10.1093/mnras/stz1981

    work page doi:10.1093/mnras/stz1981 2019

  19. [19]

    M., Balonek T

    Villata M., Raiteri C. M., Balonek T. J., Aller M. F., Jorstad S. G., Kurtanidze O. M., Nicastro F. et al., 2006, A&A, 453, 817. doi:10.1051/0004-6361:20064817

    work page doi:10.1051/0004-6361:20064817 2006

  20. [20]

    L., 2011, A&A, 528, A95

    Gu M.-F., Ai Y. L., 2011, A&A, 528, A95. doi:10.1051/0004-6361/201016280

    work page doi:10.1051/0004-6361/201016280 2011

  21. [21]

    A., Anupama G

    Agarwal A., Mihov B., Andruchow I., Cellone S. A., Anupama G. C., Agrawal V., Zola S. et al., 2021, A&A, 645, A137. doi:10.1051/0004-6361/202039301

    work page doi:10.1051/0004-6361/202039301 2021

  22. [22]

    C., Agarwal A., Bhagwan J., Strigachev A., Bachev R., Semkov E., Gaur H

    Gupta A. C., Agarwal A., Bhagwan J., Strigachev A., Bachev R., Semkov E., Gaur H. et al., 2016, MNRAS, 458,

    2016

  23. [23]

    doi:10.1093/mnras/stw377

    work page doi:10.1093/mnras/stw377

  24. [24]

    C., Urry C

    Isler J. C., Urry C. M., Coppi P., Bailyn C., Brady M., MacPherson E., Buxton M. et al., 2017, ApJ, 844, 107. doi:10.3847/1538-4357/aa79fc

    work page doi:10.3847/1538-4357/aa79fc 2017

  25. [25]

    C., Singh R

    Negi V., Joshi R., Chand K., Chand H., Wiita P., Ho L. C., Singh R. S., 2022, MNRAS, 510, 1791. doi:10.1093/mnras/stab3591

    work page doi:10.1093/mnras/stab3591 2022

  26. [26]

    K., Ramsey B

    Ghosh K. K., Ramsey B. D., Sadun A. C., Soundararajaperumal S., 2000, ApJS, 127, 11. doi:10.1086/313313

    work page doi:10.1086/313313 2000

  27. [27]

    2005, MNRAS, 364, 1105, doi: 10.1111/j.1365-2966.2005.09655.x

    Stalin C. S., Gopal-Krishna, Sagar R., Wiita P. J., Mohan V., Pandey A. K., 2006, MNRAS, 366, 1337. doi:10.1111/j.1365-2966.2005.09939.x

    work page doi:10.1111/j.1365-2966.2005.09939.x 2006

  28. [28]

    B¨ ottcher M., Basu S., Joshi M., Villata M., Arai A., Aryan N., Asfandiyarov I. M. et al., 2007, ApJ, 670, 968. doi:10.1086/522583

    work page doi:10.1086/522583 2007

  29. [29]

    H., Fu J

    Poon H., Fan J. H., Fu J. N., 2009, ApJS, 185, 511. doi:10.1088/0067-0049/185/2/511

    work page doi:10.1088/0067-0049/185/2/511 2009

  30. [30]

    J., Pollock J

    Wills B. J., Pollock J. T., Aller H. D., Aller M. F., Balonek T. J., Barvainis R. E., Binzel R. P. et al., 1983, ApJ, 274, 62. doi:10.1086/161426

    work page doi:10.1086/161426 1983

  31. [31]

    J., Wills D., Breger M., Antonucci R

    Wills B. J., Wills D., Breger M., Antonucci R. R. J., Barvainis R., 1992, ApJ, 398, 454. doi:10.1086/171869 9 ¨OZD ¨ONMEZ/Turk J Phys

    work page doi:10.1086/171869 1992

  32. [32]

    H., Tao J., Qian B

    Fan J. H., Tao J., Qian B. C., Gupta A. C., Liu Y., Yuan Y.-H., Yang J.-H. et al., 2006, PASJ, 58, 797. doi:10.1093/pasj/58.5.797

    work page doi:10.1093/pasj/58.5.797 2006

  33. [33]

    J., Valtaoja E., Torniainen I., Aller M

    Hovatta T., Tornikoski M., Lainela M., Lehto H. J., Valtaoja E., Torniainen I., Aller M. F. et al., 2007, A&A, 469,

    2007

  34. [34]

    doi:10.1051/0004-6361:20077529

    work page doi:10.1051/0004-6361:20077529

  35. [35]

    Y., 2008, A&A, 489, L33

    Savolainen T., Kovalev Y. Y., 2008, A&A, 489, L33. doi:10.1051/0004-6361:200810423

    work page doi:10.1051/0004-6361:200810423 2008

  36. [36]

    K., Jorstad S

    Hallum M. K., Jorstad S. G., Larionov V. M., Marscher A. P., Joshi M., Weaver Z. R., Williamson K. E. et al., 2022, ApJ, 926, 180. doi:10.3847/1538-4357/ac4710

    work page doi:10.3847/1538-4357/ac4710 2022

  37. [37]

    M., Marscher A

    McHardy I. M., Marscher A. P., Gear W. K., Muxlow T., Lehto H. J., Abraham R. G., 1990, MNRAS, 246, 305

    1990

  38. [38]

    , keywords =

    Thompson D. J., Bertsch D. L., Dingus B. L., Esposito J. A., Etienne A., Fichtel C. E., Friedlander D. P. et al., 1995, ApJS, 101, 259. doi:10.1086/192240

    work page doi:10.1086/192240 1995

  39. [39]

    G., Marscher A

    Jorstad S. G., Marscher A. P., Morozova D. A., Troitsky I. S., Agudo I., Casadio C., Foord A. et al., 2017, ApJ, 846, 98. doi:10.3847/1538-4357/aa8407

    work page internal anchor Pith review doi:10.3847/1538-4357/aa8407 2017

  40. [40]

    Branly R., Kilgard R., Sadun A., Shcherbanovsky A., Webb J., 1996, ASPC, 110, 170

    1996

  41. [41]

    C., Miller H

    Noble J. C., Miller H. R., 1996, ASPC, 110, 30

    1996

  42. [42]

    A., Wiik K., Jorstad S

    Ramakrishnan V., Le´ on-Tavares J., Rastorgueva-Foi E. A., Wiik K., Jorstad S. G., Marscher A. P., Tornikoski M. et al., 2014, MNRAS, 445, 1636. doi:10.1093/mnras/stu1873

    work page doi:10.1093/mnras/stu1873 2014

  43. [43]

    L., Choi H.-E

    Du N., Hulburt M. L., Choi H.-E. H., Corcoran R. M., Balonek T. J., 2022, ATel, 15441

    2022

  44. [44]

    rdkit.org, version [2025.03.6]; DOI: 10.5281/zen- odo.591637

    Bradley L., Sip˝ ocz B., Robitaille T., Tollerud E., Vin´ ıcius Z., Deil C., Barbary K. et al., 2022, zndo. doi: 10.5281/zen- odo.6825092

    work page doi:10.5281/zen- 2022

  45. [45]

    S., Balonek T

    Smith P. S., Balonek T. J., Heckert P. A., Elston R., Schmidt G. D., 1985, AJ, 90, 1184. doi:10.1086/113824

    work page doi:10.1086/113824 1985

  46. [46]

    J., 1996, A&A, 305, 42

    Heidt J., Wagner S. J., 1996, A&A, 305, 42

    1996

  47. [47]

    A., Krolik J

    Edelson R. A., Krolik J. H., 1988, ApJ, 333, 646. doi:10.1086/166773

    work page doi:10.1086/166773 1988

  48. [48]

    C., Wiita P

    Pandey A., Gupta A. C., Wiita P. J., 2017, ApJ, 841, 123. doi:10.3847/1538-4357/aa705e

    work page doi:10.3847/1538-4357/aa705e 2017

  49. [49]

    A., Ansoldi S., Antonelli L

    Acciari V. A., Ansoldi S., Antonelli L. A., Asano K., Babi´ c A., Banerjee B., Baquero A. et al., 2021, MNRAS, 504,

    2021

  50. [50]

    doi:10.1093/mnras/staa3727

    work page doi:10.1093/mnras/staa3727

  51. [51]

    M., Aller H

    Villata M., Raiteri C. M., Aller H. D., Aller M. F., Ter¨ asranta H., Koivula P., Wiren S. et al., 2004, A&A, 424,

    2004

  52. [52]

    doi:10.1051/0004-6361:20040439

    work page doi:10.1051/0004-6361:20040439

  53. [53]

    R., 1976, Ap&SS, 39, 447

    Lomb N. R., 1976, Ap&SS, 39, 447. doi:10.1007/BF00648343

    work page doi:10.1007/bf00648343 1976

  54. [54]

    D., 1982, ApJ, 263, 835

    Scargle J. D., 1982, ApJ, 263, 835. doi:10.1086/160554

    work page doi:10.1086/160554 1982

  55. [55]

    S., Castelli F., Plez B., 1998, A&A, 333, 231

    Bessell M. S., Castelli F., Plez B., 1998, A&A, 333, 231

    1998

  56. [56]

    S., Ohsugi T., Yamashita T

    Sasada M., Uemura M., Arai A., Fukazawa Y., Kawabata K. S., Ohsugi T., Yamashita T. et al., 2010, PASJ, 62,

    2010

  57. [57]

    doi:10.1093/pasj/62.3.645

    work page doi:10.1093/pasj/62.3.645

  58. [58]

    A., Becerra Gonz´ alez J., Luashvili A., Castro Segura N., Gonz´ alez-Mart´ ın O., Raiteri C

    Otero-Santos J., Acosta-Pulido J. A., Becerra Gonz´ alez J., Luashvili A., Castro Segura N., Gonz´ alez-Mart´ ın O., Raiteri C. M. et al., 2022, MNRAS, 511, 5611. doi:10.1093/mnras/stac475 10 ¨OZD ¨ONMEZ/Turk J Phys T able 1. Observation log of the blazar 4C 29.45. The columns are (1) the date of observations and (2) the number of data points in each filt...

    work page doi:10.1093/mnras/stac475 2022