A Study of the Accretion–Jet Coupling of Black Hole Objects at Different Scales
Round 1
Reviewer 1 Report
Comments and Suggestions for AuthorsSee a separate report.
Comments for author File: 
Comments.pdf
Please check grammar, sentences and proofread in the end.
Author Response
Please see the attachment.
Author Response File: Author Response.pdf
Reviewer 2 Report
Comments and Suggestions for AuthorsAbstract:
Mention the uncertainties in the exponents in peak radio correlations for AGN and XRBs both in radiatively efficient and inefficient sources. It appears that the correlation will be similar within the uncertainties for AGN and XRBs. Then you can probably give the mean value, claiming that XRB and AGN follow the same correlation. This would indeed be a significant result.
Introduction:
In the introduction, you need to briefly mention the origin of radio emission in AGN. Radio emission could originate from star formation, radio corona, disk wind, and jets.
X-ray emission, on the other hand, originates from the corona, accretion disk, and jets. See: https://ui.adsabs.harvard.edu/abs/2019NatAs...3..387P/abstract
Even jets could be present in highly accreting AGN which could be radio-quiet: https://arxiv.org/abs/2309.16926
https://ui.adsabs.harvard.edu/abs/2019A%26A...627A..53H/abstract
Now, the corona and the jets could have some sort of connection: https://arxiv.org/abs/2302.04007
https://arxiv.org/abs/2203.02963, https://arxiv.org/abs/2206.10424, https://arxiv.org/abs/1708.07011
Some people thinks, there is no connection: https://arxiv.org/abs/1606.06736
This will help the reader understand the context of your work.
Line 47-51: For XRBs, the thermal emission from the thin disc peaks in 47
soft X-rays with a peak luminosity roughly around 1 keV, and since the black hole mass 48
affects the temperature of the accretion disc emission, the disks temperature in AGNs are 49
cooler compared to that of the XRBs, and thus the disc spectrum of AGNs shifts towards 50
lower energies, resulting in the peak of the AGNs disc appearing in the optical/UV band 51
[3,15], with a peak luminosity roughly around 2500 A ̊ luminosity.
This sentence is too long. Please split it into 2 sentences.
Now people are claiming that even at 1 keV, the X ray emission could be from an coronal outflow: https://ui.adsabs.harvard.edu/abs/2022ApJ...934...35M/abstract
It is worth mentioning that even at 1 keV the coronal emission could contribute.
Line 57: “The aims of our work is to use the luminosity near the peak of the black body radiation 57
of the AGNs and XRBs to replace the 2-10 keV luminosity.”. Unclear sentence. Replace the 2-10 keV luminosity with what?
Line 63-65:”In terms of the masses of black hole objects, 63
XRBs are homogeneous, with masses of about 3-20 M⊙, while AGNs have a broad mass 64
range, with masses of about 10^(6−10) M⊙.”. An immediate question is why are you leaving out the intermediate mass black holes? They are a bridge between AGN and stellar mass black holes? Is it due to lack of observational studies? At least provide a good justification.
Sample: Line 96: “The 2-10 keV X-ray luminosities are converted to 1 keV X-ray luminosities by assuming a typical value of the X-ray spectrum of AGNs. “ Why did you convert it into 1 keV X-ray luminosity? Then in equation (3), you convert that into 2 keV X-ray luminosity? Why at such specific energy? You need to justify it. Otherwise, that will severely affect your results.
Results: Line 126: “To reduce the impact of MBH, we use LR/LEdd and Lpeak/LEdd to examine the radio/peak correlation”. Why do you want to reduce the impact of the black hole mass? What is the reason? Why is it an issue to reduce the impact of black hole mass?
Line 155: “Considering the T ∝ MBH^(1/4) scaling of the black hole accretion disk temperature with the black hole mass, the peak luminosity of the blackbody radiation of the AGN is 2500 A ̊ when the AGN mass is MBH ≈ 10^9 M⊙. “ Could you comment, what would be the case for super-Eddington sources? Would the slim disk model still hold true? This is important as a lot of XRBs are actually super-Eddington accretors.
Discussion: Line 195: “The fundamental plane of black hole activity provides a direct evidence on disk-jet coupling [1,7], and previous work has mainly investigated the fundamental plane of black 196
hole activity using 5 GHz radio luminosities, 2-10 keV X-ray luminosities, and black hole 197
masses.” Maybe it is true. But often, jets could be launched utilizing black hole spin (https://academic.oup.com/mnras/article/179/3/433/962905. So, you need to tone down the language.
Also, you need to cite Blindfold & Payne 1982: https://ui.adsabs.harvard.edu/abs/1982MNRAS.199..883B/abstract since they are one of the first people to bring this idea.
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The introduction is sometimes a little difficult to follow. A little proofreading would enhance the quality of the paper.
Author Response
Please see the attachment.
Author Response File: Author Response.pdf
Reviewer 3 Report
Comments and Suggestions for AuthorsIn this paper, the authors investigate the accretion-jet coupling of black hole objects at different scales. It addressed the foundamental plane of black hole activity by modelling the radio-peak luminosity correlations for AGNs and XRBs.
The topic is original and relevant in the field, however, I don't think it addressed the gap in the field.
Compared to Ref[1],[7] and [16], this paper employs the modified peak luminosities to examine the radio-peak correlations.
Based on the numerical results of the model parameters, the conclusions are consistent with the evidence.
The references are appropriate.
The work is well-written and presents some interesting and valuable discussions. I recommend the draft for publication, however, I have one concern:
In equations (3),(6),(7),(11),(12), the numbers following the $\pm$ symbol represent the errors and should be enclosed in parentheses.
Author Response
Comments 1:In this paper, the authors investigate the accretion-jet coupling of black hole objects at different scales. It addressed the foundamental plane of black hole activity by modelling the radio-peak luminosity correlations for AGNs and XRBs.
The topic is original and relevant in the field, however, I don't think it addressed the gap in the field.
Compared to Ref[1],[7] and [16], this paper employs the modified peak luminosities to examine the radio-peak correlations.
Based on the numerical results of the model parameters, the conclusions are consistent with the evidence.
The references are appropriate.
The work is well-written and presents some interesting and valuable discussions. I recommend the draft for publication, however, I have one concern:
In equations (3),(6),(7),(11),(12), the numbers following the $\pm$ symbol represent the errors and should be enclosed in parentheses.
Response 1:I express my sincerest gratitude for your exceptionally thorough and meticulous review of my manuscript, "A study of the accretion-jet coupling of black hole objects at different scales". In the new revised manuscript, we have been corrected in equations (3), (4), (7), (8), (12), (13).
Round 2
Reviewer 1 Report
Comments and Suggestions for AuthorsPlease see my report in attachment.
Comments for author File: Comments.pdf
Improved.
Author Response
Please see the attachment.
Author Response File: Author Response.pdf
Round 3
Reviewer 1 Report
Comments and Suggestions for AuthorsI recommend publication.
Comments on the Quality of English LanguageI recommend publication.
