The Role of Stellar Mass and Star Formation in Shaping X-ray Emission of Radio-Loud and Radio-Quiet AGN

F. Shaban; R. M. Samir; SH. M. Shehata

REVIEW 4 major objections 5 minor 51 references

The Role of Stellar Mass and Star Formation in Shaping X-ray Emission of Radio-Loud and Radio-Quiet AGN

T0 review · 4 major / 5 minor · reviewed 2026-08-05 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Radio-loud AGN in this sample show X-ray luminosity and star formation tightly coupled (Spearman rho=0.79, p=0.036) while stellar mass drops out; radio-quiet AGN correlate across all three properties.

desk verdict The RQ side is a routine but reasonable check; the RL headline is an artifact-prone correlation on 7 objects with an unexplained sign flip. read the letter →

arxiv 2509.00612 v1 pith:I5LWEGFO submitted 2025-08-30 astro-ph.GA astro-ph.HE

SH. M. Shehata , F. Shaban , R. M. Samir This is my paper

classification astro-ph.GAastro-ph.HE

keywords AGNX-rayluminositystarformationratestellarmassradio-loudquasarsradio-quietfeedbackSpearmancorrelation

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Using a sample of 45 radio-quiet and 7 radio-loud quasars with X-ray, optical, and radio data plus SED-derived host properties, the paper tests whether X-ray luminosity, star formation rate, and stellar mass correlate differently by radio class. It finds that radio-loud AGN show a strong positive correlation between X-ray luminosity and star formation rate (Spearman rho = 0.79, p = 0.036) but no significant correlations with stellar mass. Radio-quiet AGN, by contrast, show significant positive correlations among all three quantities. The authors read this as evidence that in radio-loud systems accretion and star formation are coupled through a mechanism independent of host mass, likely tied to jets, while radio-quiet AGN co-evolve with their hosts through a shared cold gas supply. If correct, this means radio-loud AGN may slow or decouple star formation in their galaxies, while radio-quiet AGN grow together with it.

What carries the argument

The analysis is carried by two devices. First, the radio-loudness parameter R, defined as the rest-frame 6 cm flux density divided by the rest-frame 2500 Å flux density, sorts the quasar sample into radio-loud (R ≥ 10) and radio-quiet (R = 0) groups. Second, Spearman rank correlations among log LX, log SFR, and log M* are computed separately for each group. The contrast between the two correlation matrices is the entire argument: no physical model is fitted, so the difference in the correlation patterns does the work of suggesting different fueling and feedback modes. Host stellar masses, SFRs, and AGN fractions come from SED fitting that includes an AGN component.

What would settle it

Compute partial Spearman correlations between log LX and log SFR controlling for redshift in the seven RL sources; if the residual correlation is no longer significant, the central RL claim is a distance artifact. A second check: repeat with a matched larger RL sample to see whether the mass-decoupling persists.

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Extended reading notes

Core claim

The paper's central claim is that radio-loud and radio-quiet AGN occupy two different correlation landscapes. For the 7 radio-loud sources, X-ray luminosity and star formation rate are strongly and significantly correlated (Spearman rho = 0.79, p = 0.036), but X-ray luminosity and stellar mass are not (rho = 0.25, p = 0.59), nor are star formation rate and stellar mass (rho = 0.46, p = 0.29). For the 45 radio-quiet sources, all three pairs show significant positive correlations: LX-SFR rho = 0.55, LX-M* rho = 0.39, SFR-M* rho = 0.42, each p < 0.01. The authors interpret the RL pattern as accretion and star formation being coupled in a way that bypasses host stellar mass, and the RQ pattern a

Load-bearing premise

The whole radio-loud result rests on just seven objects spread over 0.16 < z < 3.00, and because both X-ray luminosity and star formation rate grow with distance, a redshift trend could produce the apparent LX-SFR correlation without any physical coupling.

Editorial extensions

If this is right

For radio-loud AGN, X-ray luminosity can serve as a tracer of ongoing star formation even when host stellar mass is not a controlling factor.
Radio-quiet AGN behave as one coupled system: more massive hosts, higher SFRs, and more luminous X-ray nuclei rise together, consistent with a shared cold gas reservoir feeding both.
The absence of stellar-mass correlations in radio-loud AGN implies that jet-related feedback, not total host mass, is the relevant axis for their co-evolution.
Mixing radio-loud and radio-quiet AGN into a single LX-SFR scaling relation would average away two distinct behaviors.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

If jet emission contributes to the X-ray band in radio-loud sources, part of the LX-SFR correlation may be a jet-star-formation link rather than an accretion link; separating jet and coronal X-ray components would test this.
Recomputing the seven RL correlations as partial Spearman coefficients controlling for redshift is the quickest way to check whether the coupling survives distance effects.
The moderate RQ correlations may be shaped by the Eddington-ratio distribution rather than purely by gas supply; comparing LX/SFR with Eddington ratio would sharpen the interpretation.
A larger radio-loud sample matched in redshift and stellar mass to radio-quiet controls would reveal whether the mass-decoupling is intrinsic or a selection effect of seven sources.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

The one genuinely new thing here is pairing the DESI AGN Host Galaxies VAC with 4XMM/SDSS/FIRST and splitting by radio loudness. That is a reasonable dataset to build, and the RQ subsample (N=45) gives the expected picture: moderate positive correlations among LX, SFR, and M*, consistent with shared cold-gas fueling. If the paper stopped there, it would be a modest but harmless confirmation on a new catalog.

The RL claim is where it falls apart. It rests on 7 objects. The headline LX–SFR Spearman is rho=0.79, p=0.036, just past the N=7 two-tailed 5% threshold (rho≈0.786). There is no partial correlation on redshift, and the sample spans z=0.16–3.0, so distance-based selection is a real confounder. Worse, the same section reports a linear-regression slope of -0.595 for log LX–log SFR while claiming a strong positive monotonic relation. That sign flip is load-bearing and the paper does not even acknowledge it. The non-significant M* correlations in the RL sample are exactly what you expect with N=7; "decoupled from stellar mass" is absence of evidence, not a detection.

There are also reproducibility problems. Section 2.1's numbers do not add up: 811 point-like sources, then "211 source sample," then 8904 objects, then 6353 point sources, then 826 quasars, then 798. The path from 4XMM to the final 52 DESI-matched AGN is not auditable as written. Six Spearman tests are run without multiple-comparison correction; with a Bonferroni threshold of 0.0083, the RL p=0.036 is gone.

Credit where due: the RQ analysis is clean, the literature is cited broadly and appropriately, and the self-citations are methodological rather than result-inflating. The raw data are public, so the analysis is checkable. It is just under-analyzed.

This is not publishable as-is. The RL dichotomy is unsupported and the internal contradiction needs to be resolved before the interpretation is taken seriously. I would not cite it. But it deserves a serious referee, not a desk reject, because the RQ side is usable and the RL pitfalls are instructive. If it lands on your desk, send it to review on condition that the referee pushes hard on the RL analysis; as is, it would need major revision.

Referee Report

4 major / 5 minor

Summary. The paper cross-matches X-ray sources from 4XMM-DR11 with SDSS-DR16 quasars, classifies them as radio-loud (RL) or radio-quiet (RQ) using FIRST, and then matches to the DESI AGN Host Galaxies VAC to obtain physical properties from CIGALE SED fits. The final sample contains 45 RQ-AGN and 7 RL-AGN. Using Spearman rank correlations, the authors report for RL-AGN a strong positive LX?SFR correlation (rho = 0.79, p = 0.036) but no significant correlations with stellar mass, while RQ-AGN show significant positive correlations among LX, SFR, and M*. They interpret this as evidence that RL and RQ systems follow different co-evolution paths, with RL AGN decoupled from host mass and possibly suppressing star formation.

Significance. The question addressed is important: whether radio-loud and radio-quiet AGN differ in how their accretion and host-galaxy star formation are coupled. The use of uniformly derived CIGALE physical properties from the DESI VAC is a positive feature, as is the multi-wavelength cross-matching. However, the central RL result is not statistically robust: it rests on 7 objects, one marginally significant p-value, and no control for redshift or multiple testing. The paper also contains an internal contradiction between the reported linear-regression slope and the Spearman correlation. If the result held, it would be a useful observational constraint, but in its current form the evidence is insufficient to support the abstract's claims.

major comments (4)

[§5.2] The headline RL LX?SFR result (rho = 0.79, p = 0.036) is based on N = 7. For a two-tailed Spearman test at alpha = 0.05, the critical rho for N = 7 is approximately 0.79, so the correlation is only marginally significant. The paper does not apply any multiple-comparison correction despite reporting six Spearman tests in Sections 5.1 and 5.2; a conservative Bonferroni correction would make p = 0.036 non-significant (0.036 x 6 = 0.216). More importantly, the test is performed on raw logLX and logSFR values over 0.16 < z < 3.00 with no partialization on redshift. Both quantities are distance-dependent (LX from flux and luminosity distance, SFR from SED luminosities), and the sample is X-ray flux-selected, so a common redshift trend could induce a positive rank correlation. The homogeneity argument in §4 only shows that the RL and RQ redshift distributions are similar (median 0.80 vs 0.85);
[§4 and Fig. 6 vs §5.2] The paper reports in §4 that the linear regression slope of logLX versus logSFR for RL-AGN is -0.595, while §5.2 reports a positive Spearman rank correlation rho = 0.79 for the same two variables. A strong positive monotonic association cannot generally coexist with a negative linear regression slope, and the paper does not address this contradiction. The explanation may lie in outliers, non-linearity, or a small-sample artifact, but as written the two statements undermine each other. The authors need to reconcile these results or restrict the claims to whichever statistic is actually robust.
[§2.1, §3, §4] The sample construction is internally inconsistent and not reproducible as described. The paper states '211 source sample', then '8904 object', then '6353 point source', then '826 mutual sample', then '798 quasar', then '780 match' with FIRST, then '118 RLQs, 5 RIQs, and the remainder as RQQs' (which would be 657 for the 780 matched, but the final DESI match yields only 45 RQ-AGN and 7 RL-AGN). The selection criteria that reduce 798 quasars to 52 AGN host galaxies are not described in sufficient detail, and the earlier counts do not connect. Since the entire analysis depends on the final sample of 45 RQ and 7 RL objects, the ambiguity in sample selection is a load-bearing issue. The authors should provide a clear, step-by-step table of the sample selection with exact numbers at each stage.
[§5.2] The conclusion that RL-AGN are 'decoupled from stellar mass' is based on non-significant p-values (rho = 0.25, p = 0.59; rho = 0.46, p = 0.29) with N = 7. With such a small sample, the lack of a significant correlation is expected even if a true correlation exists; the statistical power to detect a moderate correlation is very low. Absence of evidence is not evidence of absence. The paper should either report a power analysis or explicitly soften the interpretation to 'we cannot detect a correlation with stellar mass in this small sample' rather than claiming a physical decoupling.

minor comments (5)

[Abstract and §1] The abstract states 'radio-loud AGN might slow down star formation in their galaxies', but the paper does not present evidence for a causal or directional effect. This overreach should be toned down to match the correlational nature of the analysis.
[§2.1] Typographical and numerical inconsistencies: 'total number of point-like sources is 811, out of that, we have 211 source sample' and 'choosing it > 800 counts that allowed estimating 8904 object' should be corrected. The text also says the X-ray analysis covers 0.5?10.0 keV but §6 says 0.3?10.0 keV; please unify.
[Figures] Figures 6 and 7 do not show error bars, and Figure 2 is not referenced in the main text. Adding uncertainties on LX and SFR would help assess the robustness of the correlations.
[§4] The statement that the sample is 'homogeneous' based only on similar median redshifts is misleading; homogeneity in an astrophysical context usually requires similar redshift, luminosity, and mass distributions. Please rephrase.
[References] Some references are cited with incomplete information (e.g., 'Ref (Rosario et al., 2012)' appears without a year-appropriate citation style), and the text contains typographical errors such as 'galaxys´' and 'farction'. A careful proofread is needed.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the correlation results are computed from external catalogs and standard statistics, not derived from the claims themselves.

full rationale

The paper is an observational correlation study. It constructs a sample by cross-matching 4XMM-DR11, SDSS-DR16, FIRST, and the DESI AGN Host Galaxies VAC; fits X-ray spectra with standard models; classifies radio loudness using R = f6cm/f2500; and then computes Spearman rank correlations among log LX, log SFR, and log M*. None of the central results—e.g., the RL LX–SFR correlation (rho = 0.79, p = 0.036)—is defined in terms of the conclusion being drawn. The quantities being correlated come from external catalogs and independent SED fitting, and no fitted parameter is renamed as a prediction. The only self-citations (Shehata et al. 2021 for sample selection criteria; Shaban et al. 2022 for radio classification) are procedural and do not supply the correlation coefficients or the physical interpretation. No uniqueness theorem or ansatz is imported from the authors' prior work to force the choice of correlations. The redshift-mixing and small-N concerns raised in the reader's take are statistical validity issues, not circularity: they do not show that the correlation is equivalent to its input by construction. Therefore the derivation chain is self-contained and the circularity score is 0.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

The paper introduces no new entities or free model parameters. The free-parameter list includes only descriptive regression slopes. The load-bearing assumptions are statistical: no redshift control, and reliance on catalog-derived SFR, M*, and Lx without propagated uncertainties.

free parameters (2)

Linear regression slope for RL Lx-SFR = -0.595
Reported in Figure 6 and used to interpret the RL Lx-SFR relation; descriptive fit, but introduced ad hoc and it contradicts the positive Spearman rho.
Linear regression slope for RQ Lx-SFR = 0.657
Reported in Figure 6 and used to interpret the RQ Lx-SFR relation; descriptive fit for the RQ sample.

assumptions (4)

domain assumption The Spearman correlations are not artifacts of the wide redshift range; no partialization on redshift is applied.
Section 5 computes raw Spearman correlations on a sample spanning 0.16 < z < 3.0. Both Lx and SFR are distance-dependent, so a common redshift trend could produce spurious correlations.
domain assumption The CIGALE SED fits in the DESI VAC provide unbiased SFR and stellar mass for the AGN host galaxies.
The paper adopts the VAC values (Section 4) without checking systematics from AGN contribution or SED-fitting degeneracies.
domain assumption The X-ray spectral fitting with zpowerlaw (plus optional absorption/blackbody) provides unbiased Lx values.
Section 2.2 describes the spectral fitting but does not report uncertainties or cross-checks against other X-ray measurements.
domain assumption The radio loudness classification using R = f6cm/f2500 with a power-law slope of alpha_nu = -0.5 is reliable.
Section 3 assumes alpha_nu = -0.5 to convert 20 cm flux to 6 cm; the classification threshold R >= 10 is standard but depends on this assumption.

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Cite this review

Pith. "Pith review of The Role of Stellar Mass and Star Formation in Shaping X-ray Emission of Radio-Loud and Radio-Quiet AGN." pith.science (2026). https://pith.science/paper/I5LWEGFO

@misc{pith2026250900612,
  author       = {Pith},
  title        = {Pith review of: The Role of Stellar Mass and Star Formation in Shaping X-ray Emission of Radio-Loud and Radio-Quiet AGN},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/I5LWEGFO}},
  note         = {Machine review of arXiv:2509.00612}
}

read the original abstract

Galaxy evolution and extragalactic astronomy research depend on an understanding of the interactions between active galactic nuclei (AGN) and their host galaxies. We investigate the relationships between X-ray luminosity (Lx), star formation rate (SFR), and stellar mass (M) in distinct samples of radio-loud (RL) and radio-quiet (RQ) AGN. Using data from 4XMM-DR11, SDSS-DR16, and the DESI AGN Host Galaxies VAC, we examine how these key properties correlate within each AGN population. Our analysis reveals different behaviors: RL-AGN show a strong, statistically significant Lx-SFR correlation but no significant link with M, suggesting that accretion and star formation are coupled, possibly independent of host mass. In contrast, RQ-AGN display moderate, significant positive correlations across all parameters, consistent with joint growth driven by a shared cold gas supply.These results suggest that radio-loud AGN might slow down star formation in their galaxies, while radio-quiet AGN seem to grow together with it.

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Works this paper leans on

51 extracted references · 25 canonical work pages

[1]

Introduction Active galactic nuclei (AGN) are considered to be one of the most luminous and dynamic objects in the universe, as they are powered by the accumulation of matter onto supermassive black holes. Their emissions cover a wide range of the elec- tromagnetic spectrum, X-ray emission in AGNs arises from the corona near the accretion disk and where h...

work page 2013
[2]

X-ray Observations In this section we will present the sample selection method, the reduction and analysis of the sample. 2.1. Selection Criteria The aim of this section is to construct a sample of common objects between both optical and X-ray. We create an X-ray sample by cross-matching the X-ray catalog (4XMM-DR11) with optical quasar catalog (SDSS-DR16...

work page 2021
[3]

To make a detailed study for our sample, we used multi-wavelength analysis

Radio Classification Our sample is constructed through cross matching quasars from SDSS-DR16 with XMM-Newton. To make a detailed study for our sample, we used multi-wavelength analysis. Since quasars’ high-energy activities are mainly in radio and X-ray bands, we extend our research and include their radio classifi- cation. We matched our 798 sample with ...

work page 1997
[4]

The Sample of AGN Host Galaxies The Dark Energy Spectroscopic Instrument (DESI) (Levi et al., 2013; DESI Collaboration et al., 2016, 2022; Raichoor et al.,

work page 2013
[5]

Spearman test It is essential to models of galaxy evolution to comprehend the interaction between the star formation activity within their host galaxies and the growth of supermassive black holes, as indicated by Active Galactic Nucleus (AGN) luminosity. Key parameters in this investigation include the AGN’s intrinsic power, often probed by X-ray luminosi...

work page 2014
[6]

This yielded 826 initial candidates, refined to 798 quasars after excluding sources with poor data quality (e.g., partial window modes, edge artifacts)

Summary and Discussion In this section, we highlight the significance and innova- tion of our work, as well as its implications for understanding AGN–host galaxy co-evolution: • Sample Construction and Methodology: We constructed an X-ray-selected quasar sample by cross-matching the 4XMM-DR11 catalog with the SDSS-DR16 optical cat- alog within a 5-arcseco...

work page 2025
[9]

Hunter, J.D.,

doi:10.1088/ 0004-637X/782/1/9, arXiv:1306.3218. Hunter, J.D.,

arXiv
[15]

622, A103

CIGALE: a python Code Investigating GALaxy Emission. 622, A103. doi:10.1051/0004-6361/201834156, arXiv:1811.03094. Brinkmann, W., Laurent-Muehleisen, S., Voges, W., Siebert, J., Becker, R., Brotherton, M., White, R., Gregg, M.,

arXiv

Show all 51 references

[18]

449, 373–389

Mapping the average AGN accretion rate in the SFR- M∗ plane for Herschel-selected galaxies at 0 ¡ z ≤ 2.5. 449, 373–389. doi:10.1093/mnras/stv213, arXiv:1501.07602. DESI Collaboration, Abareshi, B., Aguilar, J., Ahlen, S., Alam, S., Alexan- der, D.M., Alfarsy, R., Allen, L., A...

arXiv
[20]

arXiv e-prints , arXiv:1611.00036doi:10.48550/arXiv.1611.00036, arXiv:1611.00036

The DESI Experiment Part I: Science,Targeting, and Survey Design. arXiv e-prints , arXiv:1611.00036doi:10.48550/arXiv.1611.00036, arXiv:1611.00036. Drouart, G., De Breuck, C., Vernet, J., Seymour, N., Lehnert, M., Barthel, P., Bauer, F.E., Ibar, E., Galametz, A., Haas, M., Hat...

doi arXiv
[27]

585, 357–362

Array programming with NumPy. 585, 357–362. doi:10.1038/ s41586-020-2649-2, arXiv:2006.10256. Heinis, S., Gezari, S., Kumar, S., Burgett, W.S., Flewelling, H., Huber, M.E., Kaiser, N., Wainscoat, R.J., Waters, C.,

2006 arXiv
[32]

618, A31

Disentangling the AGN and star formation connec- tion using XMM-Newton. 618, A31. doi:10.1051/0004-6361/ 201833397, arXiv:1807.01723. Miller, B.P., Brandt, W.N., Schneider, D.P., Gibson, R.R., Steffen, A.T., Wu, J.,

arXiv
[33]

(Ed.), The X-ray Universe 2014, p

Radio-loud AGN through the eyes of 3XMM, WISE and FIRST/NVSS, in: Ness, J.U. (Ed.), The X-ray Universe 2014, p

2014
[35]

AGN Main Sequence

The Hidden “AGN Main Sequence”: Evidence for a Universal Black Hole Accretion to Star Formation Rate Ratio since z ˜2 Producing an M BH-M ∗ Relation. 753, L30. doi:10.1088/2041-8205/753/2/L30, arXiv:1204.2824. Raichoor, A., Eisenstein, D.J., Karim, T., Newman, J.A., Moustakas,...

arXiv
[40]

Journal of High Energy Astrophysics 36, 152–161

X-ray properties of high-redshift Radio Loud and Ra- dio Quiet Quasars observed by Chandra. Journal of High Energy Astrophysics 36, 152–161. doi:10.1016/j.jheap.2022.10.002, arXiv:2301.02866. Shehata, S.M., Misra, R., Osman, A., Shalabiea, O., Hayman, Z.,

2022 arXiv
[41]

691, A308

Value-added catalog of physical proper- ties for more than 1.3 million galaxies from the DESI survey. 691, A308. doi:10.1051/0004-6361/202451761, arXiv:2409.19066. Stanley, F., Harrison, C.M., Alexander, D.M., Swinbank, A.M., Aird, J.A., Del Moro, A., Hickox, R.C., Mullaney, J.R.,
[42]

453, 591–604

A remarkably flat re- lationship between the average star formation rate and AGN luminosity for distant X-ray AGN. 453, 591–604. doi:10.1093/mnras/stv1678, arXiv:1502.07756. Stemo, A., Comerford, J.M., Barrows, R.S., Stern, D., Assef, R.J., Griffith, R.L.,

arXiv
[46]

527, 12091–12108

Probing supermassive black hole growth and its dependence on stellar mass and star formation rate in low-redshift galaxies. 527, 12091–12108. doi:10.1093/mnras/stad3965, arXiv:2312.13869. Waskom, M.,

arXiv
[48]

doi:10.3847/1538-4365/ac9ead, arXiv:2209.03987. Ye`che, C., Palanque-Delabrouille, N., Claveau, C.A., Brooks, D.D., Chaus- sidon, E., Davis, T.M., Dawson, K.S., Dey, A., Duan, Y., Eftekharzadeh, S., Eisenstein, D.J., Gaztan˜aga, E., Kehoe, R., Landriau, M., Lang, D., Levi, M.E...

arXiv
[58]

doi:10.3847/ 1538-3881/aca5fb, arXiv:2208.08515. Zhou, R., Newman, J.A., Dawson, K.S., Eisenstein, D.J., Brooks, D.D., Dey, A., Dey, B., Duan, Y., Eftekharzadeh, S., Gaztan˜aga, E., Kehoe, R., Lan- driau, M., Levi, M.E., Licquia, T.C., Meisner, A.M., Moustakas, J., My- ers, A....

arXiv
[62]

Hickox, R.C., Mullaney, J.R., Alexander, D.M., Chen, C.T.J., Civano, F.M., Goulding, A.D., Hainline, K.N.,

doi:10.3847/0004-637X/826/1/62, arXiv:1605.02194. Hickox, R.C., Mullaney, J.R., Alexander, D.M., Chen, C.T.J., Civano, F.M., Goulding, A.D., Hainline, K.N.,

arXiv
[63]

doi:10.1088/0004-637X/771/1/63, arXiv:1302.1202. Ruiz-Macias, O., Zarrouk, P., Cole, S., Norberg, P., Baugh, C., Brooks, D., Dey, A., Duan, Y., Eftekharzadeh, S., Eisenstein, D.J., Forero-Romero, J.E., Gaztan˜aga, E., Hahn, C., Kehoe, R., Landriau, M., Lang, D., Levi, M.E., Lu...

arXiv
[78]

3847/1538-4357/ab5f66, arXiv:1911.07864

doi:10. 3847/1538-4357/ab5f66, arXiv:1911.07864. Taylor, M.,

1911 arXiv
[107]

doi:10.3847/1538-4357/acb3c2, arXiv:2208.08511. Delvecchio, I., Lutz, D., Berta, S., Rosario, D.J., Zamorani, G., Pozzi, F., Gruppioni, C., Vignali, C., Brusa, M., Cimatti, A., Clements, D.L., Cooray, A., Farrah, D., Lanzuisi, G., Oliver, S., Rodighiero, G., Santini, P., Syme-...

arXiv
[123]

Bernhard, E., Grimmett, L.P., Mullaney, J.R., Daddi, E., Tadhunter, C., Jin, S.,

doi:10.3847/1538-3881/aabc4f, arXiv:1801.02634. Bernhard, E., Grimmett, L.P., Mullaney, J.R., Daddi, E., Tadhunter, C., Jin, S.,

arXiv
[126]

Rosario, D., Santini, P., Lutz, D., Shao, L., Maiolino, R., Alexander, D., Altieri, B., Andreani, P., Aussel, H., Bauer, F., et al.,

doi:10.3847/1538-3881/ acb213, arXiv:2208.08513. Rosario, D., Santini, P., Lutz, D., Shao, L., Maiolino, R., Alexander, D., Altieri, B., Andreani, P., Aussel, H., Bauer, F., et al.,

arXiv
[179]

doi:10.3847/2515-5172/abc01a, arXiv:2010.11280. Zhou, R., Dey, B., Newman, J.A., Eisenstein, D.J., Dawson, K., Bailey, S., Berti, A., Guy, J., Lan, T.W., Zou, H., Aguilar, J., Ahlen, S., Alam, S., Brooks, D., de la Macorra, A., Dey, A., Dhungana, G., Fanning, K., Font- Ribera,...

2010 arXiv
[180]

doi:10.3847/2515-5172/abc078, arXiv:2010.11281. Raichoor, A., Moustakas, J., Newman, J.A., Karim, T., Ahlen, S., Alam, S., Bailey, S., Brooks, D., Dawson, K., de la Macorra, A., de Mattia, A., Dey, A., Dey, B., Dhungana, G., Eftekharzadeh, S., Eisenstein, D.J., Fanning, K., Fo...

2010 arXiv
[181]

doi:10.3847/2515-5172/abc0f4, arXiv:2010.11282

2010 arXiv
[187]

Shaban, F., Siemiginowska, A., Suleiman, R.M., El-Nawawy, M.S., Ali, A.,

doi:10.3847/ 2515-5172/abc25a, arXiv:2010.11283. Shaban, F., Siemiginowska, A., Suleiman, R.M., El-Nawawy, M.S., Ali, A.,

2010 arXiv
[207]

doi:10.3847/1538-3881/ac882b, arXiv:2205.10939. DESI Collaboration, Aghamousa, A., Aguilar, J., Ahlen, S., Alam, S., Allen, L.E., Allende Prieto, C., Annis, J., Bailey, S., Balland, C., Ballester, O., Baltay, C., Beaufore, L., Bebek, C., Beers, T.C., Bell, E.F., Bernal, J.L., ...

arXiv
[253]

Hardcastle, M.J., Croston, J.H.,

doi:10.3847/1538-3881/accff8, arXiv:2208.08512. Hardcastle, M.J., Croston, J.H.,

arXiv
[507]

doi:10.1086/173020. Hahn, C., Wilson, M.J., Ruiz-Macias, O., Cole, S., Weinberg, D.H., Mous- takas, J., Kremin, A., Tinker, J.L., Smith, A., Wechsler, R.H., Ahlen, S., Alam, S., Bailey, S., Brooks, D., Cooper, A.P., Davis, T.M., Dawson, K., Dey, A., Dey, B., Eftekharzadeh, S.,...

doi
[2000]

Astronomy and Astrophysics, v

Radio and x-ray bright agn: the rosat-first correlation. Astronomy and Astrophysics, v. 356, p. 445-462 (2000) 356, 445–462. 8 Chaussidon, E., Ye`che, C., Palanque-Delabrouille, N., Alexander, D.M., Yang, J., Ahlen, S., Bailey, S., Brooks, D., Cai, Z., Chabanier, S., Davis, T....

2000
[2007]

Computing in Science and Engineering 9, 90–95

Matplotlib: A 2D Graphics Environment. Computing in Science and Engineering 9, 90–95. doi:10.1109/MCSE.2007.55. Kondapally, R., Best, P.N., Duncan, K.J., Ro¨ttgering, H.J., Smith, D.J., Pran- doni, I., Hardcastle, M.J., Holc, T., Patrick, A.L., Arnaudova, M.I., et al.,

2007 doi
[2009]

396, 1929–1952

The active nuclei of z ¡ 1.0 3CRR radio sources. 396, 1929–1952. doi:10.1111/j.1365-2966. 2009.14887.x, arXiv:0904.1323. Harris, C.R., Millman, K.J., van der Walt, S.J., Gommers, R., Virtanen, P., Cournapeau, D., Wieser, E., Taylor, J., Berg, S., Smith, N.J., Kern, R., Picus, ...

1929
[2012]

found that accretion and SFR are uncorrelated at all redshifts when AGN luminosi- ties are low, which is in line with the hypothesis that secular processes in the host galaxies are the primary source of energy for the majority of low-luminosity AGNs. According to their interpr...

2009
[2013]

48550/arXiv.1308.0847, arXiv:1308.0847

arXiv e-prints , arXiv:1308.0847doi:10. 48550/arXiv.1308.0847, arXiv:1308.0847. Lyke, B.W., Higley, A.N., McLane, J., Schurhammer, D.P., Myers, A.D., Ross, A.J., Dawson, K., Chabanier, S., Martini, P., Des Bourboux, H.D.M., et al.,

doi arXiv
[2014]

566, A53

Rapidly growing black holes and host galaxies in the distant Universe from the Herschel Radio Galaxy Evolution Project. 566, A53. doi:10.1051/0004-6361/201323310, arXiv:1404.1080. Fabian, A.C., Lohfink, A., Kara, E., Parker, M.L., Vasudevan, R., Reynolds, C.S.,

arXiv
[2015]

Also, (Bongiorno et al.,

investigated the connection between stellar mass and X- ray luminosity in a sample of X-ray selected AGN, providing Preprint submitted to High Energy Astrophysics June 23, 2025 2 f insights into how the stellar mass of the host galaxy influences the AGN’s X-ray emission. Also,...

2025
[2016]

Is AGN feedback responsible for the mass-quenching of galaxies? 588, A78

AGN host galaxy mass func- tion in COSMOS. Is AGN feedback responsible for the mass-quenching of galaxies? 588, A78. doi:10.1051/0004-6361/201527436, arXiv:1601.02091. Boquien, M., Burgarella, D., Roehlly, Y., Buat, V., Ciesla, L., Corre, D., In- oue, A.K., Salas, H.,

arXiv
[2017]

arXiv e-prints , arXiv:1707.02160arXiv:1707.02160

TOPCAT: Desktop Exploration of Tab- ular Data for Astronomy and Beyond. arXiv e-prints , arXiv:1707.02160arXiv:1707.02160. Torbaniuk, O., Paolillo, M., Carrera, F., Cavuoti, S., Vignali, C., Longo, G., Aird, J.,

arXiv
[2018]

476, 436–450

Evidence for a mass-dependent AGN Eddington ratio distribution via the flat relationship between SFR and AGN luminosity. 476, 436–450. doi:10.1093/mnras/sty219, arXiv:1801.07717. Bongiorno, A., Schulze, A., Merloni, A., Zamorani, G., Ilbert, O., La Franca, F., Peng, Y., Piconc...

arXiv
[2019]

Monthly Notices of the Royal Astronomical Society: Letters 483, L52–L57

Inferring a difference in the star-forming properties of lower versus higher x-ray luminosity AGNs. Monthly Notices of the Royal Astronomical Society: Letters 483, L52–L57. doi:10.1093/mnrasl/sly217. Bernhard, E., Mullaney, J.R., Aird, J., Hickox, R.C., Jones, M.L., Stan- ley,...

doi
[2020]

88, 101539

Radio galaxies and feedback from AGN jets. 88, 101539. doi:10.1016/j.newar.2020.101539, arXiv:2003.06137. Hardcastle, M.J., Evans, D.A., Croston, J.H.,

2020
[2021]

506, 2619–2637

The connection between star formation and supermassive 10 black hole activity in the local Universe. 506, 2619–2637. doi:10.1093/ mnras/stab1794, arXiv:2106.11079. Torbaniuk, O., Paolillo, M., D’Abrusco, R., Vignali, C., Georgakakis, A., Carrera, F.J., Civano, F.,

arXiv
[2022]

fitted the power-law continuum to the spec- trum to determine the rest-frame 2500 flux density (Wu and Shen, 2022). Then, estimating the quasar radio loudness param- eter (R) defining Radio Loud quasars (RLQs) and Radio Quiet Quasars (RQQs) based on the following equation R = ...

2022
[2023]

survey will measure the distortions of galaxy clus- tering caused by redshift-space effects, as well as the baryon acoustic feature imprinted on the large-scale structure of the universe, with high precision. The survey aims to accom- plish these objectives by performing spect...

2020
[2024]

Astronomy & Astrophysics 683, A172

The link among x-ray spectral prop- erties, agn structure, and the host galaxy. Astronomy & Astrophysics 683, A172. doi:10.1051/0004-6361/202348204. Mullaney, J.R., Daddi, E., Be´thermin, M., Elbaz, D., Juneau, S., Pannella, M., Sargent, M.T., Alexander, D.M., Hickox, R.C.,

doi
[3021]

White, R.L., Becker, R.H., Helfand, D.J., Gregg, M.D.,

doi:10.21105/joss.03021. White, R.L., Becker, R.H., Helfand, D.J., Gregg, M.D.,

doi
[4383]

Haardt, F., Maraschi, L.,

doi:10.1093/mnras/stv1218, arXiv:1505.07603. Haardt, F., Maraschi, L.,

arXiv

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.

[1] [1]

Introduction Active galactic nuclei (AGN) are considered to be one of the most luminous and dynamic objects in the universe, as they are powered by the accumulation of matter onto supermassive black holes. Their emissions cover a wide range of the elec- tromagnetic spectrum, X-ray emission in AGNs arises from the corona near the accretion disk and where h...

work page 2013

[2] [2]

X-ray Observations In this section we will present the sample selection method, the reduction and analysis of the sample. 2.1. Selection Criteria The aim of this section is to construct a sample of common objects between both optical and X-ray. We create an X-ray sample by cross-matching the X-ray catalog (4XMM-DR11) with optical quasar catalog (SDSS-DR16...

work page 2021

[3] [3]

To make a detailed study for our sample, we used multi-wavelength analysis

Radio Classification Our sample is constructed through cross matching quasars from SDSS-DR16 with XMM-Newton. To make a detailed study for our sample, we used multi-wavelength analysis. Since quasars’ high-energy activities are mainly in radio and X-ray bands, we extend our research and include their radio classifi- cation. We matched our 798 sample with ...

work page 1997

[4] [4]

The Sample of AGN Host Galaxies The Dark Energy Spectroscopic Instrument (DESI) (Levi et al., 2013; DESI Collaboration et al., 2016, 2022; Raichoor et al.,

work page 2013

[5] [5]

Spearman test It is essential to models of galaxy evolution to comprehend the interaction between the star formation activity within their host galaxies and the growth of supermassive black holes, as indicated by Active Galactic Nucleus (AGN) luminosity. Key parameters in this investigation include the AGN’s intrinsic power, often probed by X-ray luminosi...

work page 2014

[6] [6]

This yielded 826 initial candidates, refined to 798 quasars after excluding sources with poor data quality (e.g., partial window modes, edge artifacts)

Summary and Discussion In this section, we highlight the significance and innova- tion of our work, as well as its implications for understanding AGN–host galaxy co-evolution: • Sample Construction and Methodology: We constructed an X-ray-selected quasar sample by cross-matching the 4XMM-DR11 catalog with the SDSS-DR16 optical cat- alog within a 5-arcseco...

work page 2025

[7] [9]

Hunter, J.D.,

doi:10.1088/ 0004-637X/782/1/9, arXiv:1306.3218. Hunter, J.D.,

arXiv

[8] [15]

622, A103

CIGALE: a python Code Investigating GALaxy Emission. 622, A103. doi:10.1051/0004-6361/201834156, arXiv:1811.03094. Brinkmann, W., Laurent-Muehleisen, S., Voges, W., Siebert, J., Becker, R., Brotherton, M., White, R., Gregg, M.,

arXiv