XMM-Newton follow-up of two eROSITA X-ray binary candidates

A. Avakyan; A. Santangelo; A. Schwope; A. Zainab; D. Buckley; J. Brink; J. Wilms; V. Doroshenko; V. Suleimanov

REVIEW 3 major objections 5 minor 1 cited by

XMM-Newton follow-up of two eROSITA X-ray binary candidates

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Two eROSITA X-ray binary candidates are reclassified by follow-up: one is an active M-type subgiant, the other a bright novalike cataclysmic variable, and the paper traces the original selection to overestimated fluxes in the early…

desk verdict Solid, workmanlike reclassification of two eROSITA XRB candidates; the CV identification is convincing, the subgiant call has an internal log g/radius tension, and the missing chance-coincidence calculation is the main loose end. read the letter →

arxiv 2507.08592 v1 pith:MZRWUOOE submitted 2025-07-11 astro-ph.HE

A. Avakyan , A. Zainab , V. Doroshenko , J. Wilms , A. Schwope , V. Suleimanov , D. Buckley , J. Brink

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A. Santangelo

This is my paper

classification astro-ph.HE

keywords X-raybinariescataclysmicvariablesactivestarseROSITAsurveyXMM-NewtonopticalspectroscopystarspotsTESSphotometry

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

This paper follows up two sources that the first eROSITA all-sky survey flagged as X-ray binary candidates, and argues that neither is actually an X-ray binary. For 1eRASS J061330.8+160440 it assembles LAMOST spectroscopy, a spectral energy distribution fit, and ZTF/TESS photometry to classify the counterpart as an M0-M2 chromospherically active subgiant whose 7.189-day periodic brightness modulation is likely produced by starspots. For 1eRASS J161201.9-464622 it uses SALT spectroscopy and X-ray spectra to classify the source as a bright novalike cataclysmic variable, the second such system found with eROSITA, with a persistent 4.802-hour signal in three TESS epochs tentatively identified as the orbital period. The paper also concludes that the original X-ray binary selection was driven by overestimated fluxes and spectral hardness in the early eROSITA pipeline. If the classifications hold, they show that eROSITA follow-up can separate real accreting binaries from active stars and cataclysmic variables in the survey sample.

What carries the argument

The argument runs on three identification mechanisms. The first is the astrometric matching of XMM-Newton positions to unique Gaia counterparts through an OM-Gaia cross-correlation, which fixes the optical identification that every later classification step presupposes. The second is the two-temperature optically thin plasma model (apec+apec) for the X-ray spectra, which the paper uses to characterise the sources as coronal emission rather than accretion power, together with the SALT emission-line diagnostics (Balmer lines, He II 4686, the C III/N III Bowen blend, equivalent widths and the He II/H-beta ratio) that separate a non-magnetic novalike CV from a magnetic CV and from an X-ray binary. The third is the period search on de-trended TESS light curves with a Lomb-Scargle periodogram and bootstrap false-alarm thresholds, which recovers the stable 4.802-hour signal in all three epochs; for J061331, the TiO-band spectral type indicators and the ARIADNE SED fit fix the subgiant parameters that make starspot rotation a natural reading of the 7.189-day period.

What would settle it

Compute the expected number of random Gaia matches of the same brightness within the roughly one-arcsecond error circles for the two positions; if the chance-coincidence rate is not well below one, the unique-counterpart assumption on which both classifications rest is not secure.

Watch

Extended reading notes

Core claim

The paper's central claim is that 1eRASS J061330.8+160440 and 1eRASS J161201.9-464622 are unlikely to be X-ray binaries. J061331 is presented as a coronal active subgiant: its X-ray spectrum is a two-temperature optically thin plasma, its optical spectrum shows strong H-$\alpha$ without the He/Balmer accretion signatures typical of accreting binaries, and its SED fit gives an M0-M2 star with radius $R \sim 5\,R_\odot$ and luminosity $L \sim 6\,L_\odot$, with the 7.189-day optical period attributed to starspots. J161201 is presented as a weakly magnetized novalike cataclysmic variable: the SALT spectrum shows a blue continuum, H-Balmer, He I, He II and C III/N III Bowen fluorescence, and broad absorption wings from an optically thick accretion disc, while the X-ray spectrum is a harder two-temperature plasma with an iron line near 6.55 keV; the line ratios and equivalent widths argue against a magnetic CV. A 4.802-hour signal is found in all three TESS observations (2019, 2021, 2023) after de-trending and is tentatively identified as the binary orbital period. The paper further concludes that the original X-ray binary candidacy was mainly an artifact of overestimated flux and hardness in the preliminary eROSITA pipeline, amplified by genuine variability of both objects.

Load-bearing premise

The classifications assume that the single Gaia source found within each roughly one-arcsecond XMM-Newton error circle is the true optical counterpart, since the paper does not compute a chance-coincidence probability; if either association is wrong, every spectral and photometric conclusion for that source attaches to the wrong star.

Editorial extensions

If this is right

J061331 should be treated as a chromospherically active M-type subgiant rather than as an X-ray binary candidate; the 7.189-day period is a rotation and starspot signal, and the broad H-alpha emission implies a co-rotating circumstellar component reaching roughly 8-10 stellar radii.
J161201 joins SRGt 062340.2-265751 as only the second bright novalike cataclysmic variable discovered with eROSITA, showing that the survey can uncover CVs as well as X-ray binaries.
The 4.802-hour signal, if confirmed by high-speed photometry and time-resolved spectroscopy, would be the orbital period of J161201 and would anchor the physical parameters of the binary.
Future eROSITA candidate selection should use the reprocessed pipeline and fluxes derived from spectral fitting rather than count-rate conversion, because the early pipeline overestimated both flux and hardness for these two sources.
Because both sources are intrinsically variable, a low or non-detection in a single eROSITA survey should not by itself rule out a source as a candidate X-ray binary.

Reading between the lines

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

A testable extension would be to compute the chance-coincidence probability for the two Gaia counterparts; the roughly one-arcsecond positional agreement is suggestive, but the local stellar density is not quantified in the paper.
If the 7.189-day modulation is really starspot rotation, one would predict that the X-ray emission of J061331 varies on the same timescale in longer X-ray monitoring, a test the current short exposures cannot perform.
The 4.802-hour photometric signal in a novalike CV could equally be a disc-driven or superhump-like periodicity; only a radial-velocity curve of the emission lines can settle whether it is the true orbital period.
A systematic reclassification of eRASS1 X-ray binary candidates with the updated pipeline would quantify the contamination rate that this two-object study only samples.

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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

Quick take: this is a useful, honest follow-up paper. Both sources get classified as non-XRBs, and the evidence is generally good. The CV classification for J161201 rests on a SALT spectrum with Balmer, He II, Bowen fluorescence, and broad absorption wings—about as solid as it gets from one spectrum. J061331 as an M-type active subgiant is reasonable, though the log g ~4.4 from both LAMOST and the SED fit sits oddly with R ~5 R_sun; that tension should be discussed before the subgiant label sticks. The 7.189 d and 4.802 h periods are interesting but need uncertainties and, for the CV, time-resolved spectroscopy as the authors say.

What's new: first XMM follow-up of these two specific candidates; J161201 becomes the second eROSITA-discovered novalike CV; the paper also documents the earlier pipeline flux overestimate that caused mis-selection. That last point is a real contribution to the eROSITA candidate-selection story.

Soft spots, in order of importance. The counterpart association is the load-bearing hinge: no chance-coincidence probability is computed, just positional offsets of 0.9" and 0.68" against ~1" errors. With 84 and 455 OM/Gaia matches the astrometric correction is likely good, and unique counterparts at those offsets are plausible, but a quick local source-density estimate would remove the doubt. Second, the X-ray spectral fits use large eROSITA cross-normalization constants (2 and 6.6); the thermal-plasma classification for J161201 is supported by the Fe line and optical spectrum, so I'm not worried, but it should be stated more carefully. Third, the period uncertainties are missing, and 'solidly classifies' overreaches for the CV orbital period (not for the CV itself). Minor: the SED fit for J061331 has A_V ~3.3 and some blue excess, but the conclusion doesn't depend on it.

Overall, the central conclusions hold up. The paper deserves a serious referee. For me, it's a cite for the eROSITA false-positive rate, and I'd send it back asking for a chance-coincidence probability, a comment on the log g/radius tension, and period uncertainties.

Referee Report

3 major / 5 minor

Summary. The paper reports XMM-Newton follow-up observations of two X-ray binary candidates from the first eROSITA all-sky survey, 1eRASS J061330.8+160440 and 1eRASS J161201.9-464622. After astrometric correction using XMM-Newton OM/Gaia matches, the authors identify a unique Gaia counterpart for each X-ray source and attach multiwavelength data to those stars. The X-ray spectra of both sources are fitted with a two-temperature thermal plasma model, and no coherent X-ray pulsations are found. For J061331, LAMOST spectroscopy and SED fitting lead to classification as an M0-M2 chromospherically active subgiant with a 7.189 d photometric period attributed to starspots. For J161201, SALT spectroscopy shows Balmer, He I, He II and Bowen emission lines, leading to classification as a weakly magnetized novalike cataclysmic variable; a 4.802 h signal is found in three TESS epochs and tentatively identified as the orbital period. The paper concludes that neither source is an X-ray binary, and attributes the original XRB selection to overestimated fluxes and hardnesses in the preliminary eRASS1 pipeline.

Significance. If the classifications hold, the paper provides a useful demonstration that eROSITA XRB candidate selection can be contaminated by chromospherically active stars and CVs, and it adds a new bright novalike CV to the small sample discovered through eROSITA. The main classifications rest on independent observational diagnostics: the SALT optical spectrum robustly indicates an accreting white dwarf binary, while the LAMOST spectrum and SED strongly support an active subgiant for J061331. The astrometric correction using 84 and 455 OM/Gaia matches is a genuine strength, and the multi-epoch TESS analysis, including several de-trending methods, is a careful approach. The paper is falsifiable and the requested quantitative cross-match and significance values would materially strengthen it.

major comments (3)

[2.2, Table 2] The identification of the optical counterparts is load-bearing for both conclusions, and the paper never computes a chance-coincidence probability. The Gaia counterparts lie at 0.924 arcsec and 0.679 arcsec from the astrometrically corrected XMM-Newton positions, whose 1-sigma uncertainties are 0.98 arcsec and 0.94 arcsec, respectively. Since every subsequent piece of evidence (LAMOST, SALT, SED, TESS/ZTF periods) is attached to these stars, a wrong association would invalidate the central claim for that source. The authors should quantify the local Gaia source density within the XMM-Newton error circles and report the probability that a random background star falls at these separations, or perform an equivalent Bayesian cross-match.
[3.1, Table 4] The combined eROSITA plus XMM-Newton spectral fit uses cross-normalization constants CeROSITA = 2.07^{+1.34}_{-0.93} for J061331 and 6.62^{+1.32}_{-1.10} for J161201, meaning the eROSITA flux exceeds the XMM-Newton flux by factors of roughly two and six. This raises the concern that the thermal-plasma classification and the inferred spectral hardness are driven by eROSITA data whose flux and spectral shape differ substantially from the XMM-Newton observation. Because the conclusion that these objects are unlikely XRBs relies in part on the X-ray spectral shape, the authors should show explicitly that the XMM-Newton data alone are well described by the double-apec model and reject the cutoff power-law and blackbody models, or present a robustness check with eROSITA excluded from the fit.
[3.4, Fig. 10] The paper claims that the 4.802 h signal is persistent across all three TESS epochs, but it reports only the 1% false-alarm probability power levels (0.12, 0.07 and 0.02 for 2019, 2021 and 2023) without giving the peak power and the corresponding false-alarm probability for each epoch. The figure suggests that the 2019 and 2021 peaks may be only marginally above or near their threshold. The authors should report the peak power, the bootstrap false-alarm probability, and the significance for each epoch individually, so that the 'persistent' claim can be evaluated quantitatively.

minor comments (5)

[3.3, Section 4] The H-alpha FWHM of 7.4 ± 0.3 A from LAMOST is not corrected for the instrumental resolution of LAMOST low-resolution spectroscopy (R ~ 1800, corresponding to roughly 3.6 A at 6563 A). The derived width of ~330 km/s therefore overestimates the intrinsic line width, and the interpretation of emission extending to 8-10 stellar radii in Section 4 should be treated as tentative until an instrumental correction is applied.
[Table 3 vs. Table 9] The adopted distance to J061331 from Bailer-Jones et al. is 656.9^{+57.5}_{-40.5} pc, while the SED fit with ariadne returns 787^{+101}_{-71} pc. The paper uses the SED-derived radius to compute the rotational velocity but does not discuss this distance tension; a brief comment on the consistency would be useful.
[Fig. 7] The right panel of Figure 7 shows the J161201 light curve folded at P = 0.937 d, but Section 2.2 mentions a tentative ASAS-SN period of 177.8 d and the text says the periodogram 'does not look very promising.' The caption should clarify which periodogram peak is being folded and why this period was chosen.
[2.1, Fig. 4] There is a typo in the table reference ('Table1' instead of 'Table 1') in Section 2.1, and the legend of Figure 4 mentions 'eRASS1B' without explanation; these should be corrected.
[References] Reference [120] contains a duplicated DOI string; the duplicate should be removed.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the classifications rest on independent X-ray, optical, and photometric fingerprints, and the only self-references are non-load-bearing inputs.

full rationale

The paper's central conclusions — that J061331 is an M0 chromospherically active subgiant and J161201 is a novalike cataclysmic variable — do not reduce to the fitted inputs. The X-ray classification is based on a two-temperature apec spectral fit with a statistically acceptable approximation, whereas cutoff power-law and blackbody models fail; this is an empirical comparison, not a quantity that is then re-derived as a 'prediction'. The optical classifications come from independent SALT and LAMOST spectroscopy (H-alpha, Balmer, He I, He II, Bowen blend, TiO indices) and from an SED fit with ariadne. The 7.189 d and 4.802 h periods are found in external archival photometry (ZTF, TESS, ASAS-SN) and are not defined by any parameter fitted earlier in the paper. The authors' own XRB catalogues (refs [2,3]) are used only for candidate input selection, and the final conclusions would not change if those candidates had been selected differently; the later re-processing with the current eROSITA pipeline independently shows lower fluxes. The one defensible weakness is the lack of a quantitative chance-coincidence probability for the proposed Gaia counterparts, but that is a robustness or correctness risk, not a circularity: a wrong association would invalidate the conclusions empirically, but it would not mean the derivation was equivalent to its inputs by construction. No uniqueness theorem is imported from the authors, no ansatz is smuggled in via citation, and no fitted parameter is renamed as a prediction. The circularity burden is therefore low.

Assumptions & free parameters 6 free parameters · 7 assumptions · 0 invented entities

The central claims rest on standard astrophysical modeling assumptions and on the positional identification of optical counterparts. The most consequential hidden choice is the SED-based subgiant classification despite an internal log g versus radius inconsistency. No new physical entities are introduced.

free parameters (6)

Cross-normalization constants (CeROSITA, CPN, CMOS2) = J061331: 2.07/0.80/0.93; J161201: 6.62/0.99/1.02
Fitted in the combined XMM+eROSITA spectral model (Table 4); they absorb large flux offsets between instruments and epochs, and are central to the claim that both spectra are thermal plasma.
Two-temperature apec parameters (kT1, kT2, norm1, norm2, NH_XMM, NH_eROSITA) = Table 4: e.g., J061331 kT1=0.87 keV, kT2=3.46 keV; J161201 kT1=0.94 keV, kT2=5.84 keV
Model parameters fitted to the combined X-ray spectra; the classification as coronal/CV plasma rather than accretion XRB rests on this model choice.
Fe line parameters for J161201 (E, norm, FWHM) = 6.55 keV, 3.08e-5 ph cm^-2 s^-1, 435 eV
Gaussian fit in the PN spectrum (Table 5); used to infer hard X-ray emission supporting the CV interpretation.
SED fitted parameters for J061331 (Teff, log g, Fe/H, D, R, AV, L, Age) = 3885 K, 4.47, -0.54, 787 pc, 5.07 Rsun, 3.32 mag, 5.88 Lsun, 11.9 Gyr
Outputs of the ARIADNE SED fit (Table 9) that drive the subgiant classification and the rotational velocity estimate.
TESS de-trending cutoff (Savitzky-Golay long-term timescale) = ~1 day
Chosen by hand to isolate the sub-day 4.802 h signal in J161201; the authors verified robustness against other detrending methods (Sect. 3.4).
1% false-alarm probability threshold = 0.01
Used for bootstrap significance of the 4.802 h signal; a standard choice but arbitrary.

assumptions (7)

domain assumption Optical counterparts identified by positional coincidence within ~1 arcsec are the true X-ray sources.
Sect. 2.2: unique Gaia counterparts at 0.9 and 0.68 arcsec; no chance-coincidence probability is quantified, so the association is an assumption.
domain assumption The X-ray spectra of XRBs would show accretion-dominated features (power-law/cutoff or blackbody), while two-temperature apec thermal plasma indicates coronal stars or CVs.
Sect. 3.1 and 4: used to argue the sources are unlikely to be XRBs.
domain assumption The 4.802 h TESS periodicity is the orbital period of J161201.
Sect. 3.4 and 4: labeled tentative; could be a superhump or other timescale, so the orbital-period claim rests on this assumption.
domain assumption The 7.189 d optical period of J061331 is caused by starspots, not orbital motion.
Sect. 3.4 and 4: supported by the single-wave light curve shape and flare, but not directly proven.
ad hoc to paper The SED-derived radius and LAMOST log g for J061331 are both reliable; the star is a subgiant.
Sect. 3.5 and Table 9: the two values are internally inconsistent (log g=4.47 with R=5.07 Rsun implies M~27 Msun), yet the paper proceeds with the subgiant classification without discussing the tension.
domain assumption H-alpha FWHM of 7.4 A corresponds to Doppler broadening of ~330 km/s; emission extended to 8-10 stellar radii in a corotating circumstellar environment.
Sect. 4: used to reconcile rotation velocity with H-alpha width; relies on standard Doppler formula and the corotating envelope model from other active stars.
standard math Lomb-Scargle statistics, bootstrap FAP, Z^2 test, and Bayesian nested sampling are valid for the data cadence and sampling.
Used throughout Sect. 3.2-3.5; these are established statistical tools.

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Cite this review

Pith. "Pith review of XMM-Newton follow-up of two eROSITA X-ray binary candidates." pith.science (2026). https://pith.science/paper/MZRWUOOE

@misc{pith2026250708592,
  author       = {Pith},
  title        = {Pith review of: XMM-Newton follow-up of two eROSITA X-ray binary candidates},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/MZRWUOOE}},
  note         = {Machine review of arXiv:2507.08592}
}

read the original abstract

We report on the follow-up observations with XMM-Newton of two X-ray binary candidates identified in the first eROSITA all-sky survey data (eRASS1), 1eRASS J061330.8+160440 and 1eRASS J161201.9-464622. Based on the obtained results, in particular, the observed X-ray spectra and lack of pulsations, as well as properties of the identified optical counterparts, we conclude that both candidates are unlikely to be XRBs. Based on LAMOST optical spectroscopy and SED fit results for 1eRASS J061330.8+160440 we classify it as an M0 chromospherically active subgiant star. ZTF and TESS photometry reveal highly significant period for this object of 7.189 days, which likely attributed to starspot(s). On the other hand, SALT follow-up spectroscopy of 1eRASS J161201.9-464622 solidly classifies this source as a bright novalike cataclysmic variable (CV), the second discovered with eROSITA. A persistent 4.802 h signal is found across all three available TESS observations, and is tentatively identified as the orbital period of the binary. Follow-up high-speed photometry and time-resolved spectroscopy are required to confirm the derived orbital modulation.

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Forward citations

Cited by 1 Pith paper

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