The low luminosity end of Galactic HMXBs with eROSITA: Establishing a luminosity floor for accreting BeXRBs

Aafia Zainab; Alicia Rouco Escorial; Artur Avakyan; Christian Kirsch; Ekaterina Sokolova-Lapa; Galina Lipunova; Jakob Stierhof; Joel Coley; Joern Wilms; Katja Pottschmidt

REVIEW 3 major objections 5 minor 279 references

The low luminosity end of Galactic HMXBs with eROSITA: Establishing a luminosity floor for accreting BeXRBs

T0 review · 3 major / 5 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read Most Be X-ray binaries are accreting even when not in outburst

desk verdict A careful eROSITA population study that extends the HMXB luminosity function to 10^32 erg/s and makes a credible but slightly over-stated case that most BeXRBs accrete outside outburst; the measurement is solid, the Be-star baseline needs work. read the letter →

arxiv 2608.13259 v1 pith:OEZJSXUG submitted 2026-08-13 astro-ph.HE astro-ph.GA

Aafia Zainab , Philipp Thalhammer , Nico Zalot , Artur Avakyan , Jakob Stierhof , Ekaterina Sokolova-Lapa , Victor Doroshenko , Victoria Grinberg

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Peter Kretschmar Galina Lipunova Nazma Islam Matthias R. Schreiber Christian Kirsch Steven Hämmerich Philipp Weber Ralf Ballhausen Alicia Rouco Escorial Joel Coley Richard Rothschild Katja Pottschmidt Joern Wilms

This is my paper · ORCID

classification astro-ph.HEastro-ph.GA

keywords high-massX-raybinariesBeluminosityfunctionlogN-logLaccretionpropellereffecteROSITAsurveys

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

The paper uses the first four all-sky surveys of the eROSITA X-ray telescope to measure the X-ray luminosities of every known high-mass X-ray binary in the Western Galactic hemisphere down to about $10^{32}\,\mathrm{erg}\,\mathrm{s}^{-1}$, the deepest wide-area census of these objects yet made. At these luminosities the sample is dominated by Be X-ray binaries — systems in which a neutron star orbits a Be-type star with a circumstellar disk. The central finding is that the vast majority, more than 80 percent once the four surveys are combined, are detected in a random snapshot at luminosities of $10^{33}$ to $10^{35}\,\mathrm{erg}\,\mathrm{s}^{-1}$, at least an order of magnitude above what their Be star donors alone emit. The authors interpret this excess as ongoing accretion onto the neutron star outside of outburst, meaning the long-standing picture of BeXRBs as 'off' between rare outbursts is wrong for most systems, and establishing a de facto luminosity floor for accreting BeXRBs around $10^{32}$ to $10^{33}\,\mathrm{erg}\,\mathrm{s}^{-1}$. The result matters because the low-luminosity end of the Milky Way's HMXB luminosity function was previously inaccessible, and it suggests that some X-ray-luminous 'isolated' Be stars may in fact be hidden accreting binaries.

What carries the argument

The argument is carried by a comparison of two logN-logL distributions: the BeXRBs detected by eROSITA versus the eROSITA-detected Be stars drawn from a catalog of 832 Gaia quality-cut stars in the Western hemisphere (170 detected), where a 500 pc volume-limited subsample stands in lieu of a volume-corrected distribution. The physical interpretation is anchored to two analytic thresholds: the cold disk accretion luminosity, $L_{\rm cold} \sim 9\times10^{33}\,k^{1.5} B_{12}^{0.86} M_{1.4}^{0.28} R_6^{1.57}\,\mathrm{erg}\,\mathrm{s}^{-1}$, below which a poorly ionized disk can still sustain accretion, and the propeller limit, $L_{\rm prop} \sim 4\times10^{37}\, k^{7/2} B_{12}^{2} P^{-7/3} M_{1.4}^{-2/3} R_6^{5}\,\mathrm{erg}\,\mathrm{s}^{-1}$, below which the rotating magnetosphere is expected to inhibit accretion; plotting each system's spin period against its eROSITA luminosity places most BeXRBs between these two limits. On the data side, the load-bearing elements are the four stacked eROSITA surveys (eRASS1–4), the updated HMXB catalog of 72 Western-hemisphere systems, and fluxes from absorbed power-law and blackbody fits corrected for pile-up, complete to about $10^{-13}\,\mathrm{erg}\,\mathrm{s}^{-1}\,\mathrm{cm}^{-2}$.

What would settle it

A decisive test would be a volume-complete comparison: select BeXRBs and isolated Be stars to the same distance limit (say, 3 kpc using Gaia parallaxes), correct both samples for absorption, and compare their hard 2–10 keV luminosity distributions; if the BeXRB excess over the isolated Be-star distribution disappears, the accretion-outside-outburst conclusion would be undermined. A complementary check is to monitor the few BeXRBs with stringent upper limits below about $10^{32}\,\mathrm{erg}\,\mathrm{s}^{-1}$ (such as AX J1700.2−4220 and Ginga 0834−430) for months to years with a sensitive instrument: if any of them is caught in a bright outburst after a long quiet period, the propeller picture would have to accommodate a genuine 'off' state, whereas if they are always detected at or above $10^{32}\,\mathrm{erg}\,\mathrm{s}^{-1}$ whenever sufficient exposure is accumulated, the inferred luminosity floor would be confirmed.

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Extended reading notes

Core claim

The paper's central claim is that the low-luminosity regime of the Galactic HMXB population belongs to the Be X-ray binaries, and that these systems are, in a random snapshot of the sky, most often found accreting rather than quiescent. Using the eRASS1–4 data, the authors extend the HMXB logN-logL from around $10^{35}$ down to $10^{32}\,\mathrm{erg}\,\mathrm{s}^{-1}$, and show that the distribution requires a broken power law in this range, with the lower-luminosity slope dominated by BeXRBs and the bright end by supergiant systems. Comparing the BeXRB distribution with the eROSITA-detected isolated Be star population — including a volume-limited 500 pc subsample used as a donor baseline — over 80 percent of the BeXRBs lie at luminosities at least an order of magnitude above what their Be donors would produce, in a regime consistent with cold disk accretion onto the neutron star. The four eROSITA scans also reveal a large scatter in the overall logN-logL due to source-intrinsic variability, which the variability-resampled RXTE/ASM and MAXI distributions above $10^{35}\,\mathrm{erg}\,\mathrm{s}^{-1}$ confirm is consistent with previous monitoring, while below that level the monitors suffer incompleteness. A small number of bright, hard X-ray 'isolated' Be stars reach luminosities comparable to the faintest BeXRBs, which the authors propose as candidate quiescent or low-luminosity accreting systems.

Load-bearing premise

The argument that BeXRBs are accreting outside outburst assumes that the luminosity distribution of isolated Be stars, especially the 500 pc volume-limited subsample, is an unbiased baseline for the X-ray output of the Be donor inside a binary, so if binary interactions brighten the donor or the BeXRB distances and absorbing columns differ systematically, the order-of-magnitude excess attributed to accretion could be inflated.

Editorial extensions

If this is right

The Milky Way HMXB luminosity function is time-dependent: the four eROSITA scans differ substantially in shape and break luminosity depending on which sources are flaring, so single-epoch XLFs come with large intrinsic scatter that must be propagated when comparing with external galaxies.
All-sky monitors that only reach $\gtrsim 10^{35}\,\mathrm{erg}\,\mathrm{s}^{-1}$ (RXTE/ASM, MAXI) are strongly biased toward supergiant HMXBs; the dominant BeXRB population is essentially invisible to them outside outburst, which explains the longstanding 'transient' classification.
The propeller mechanism is constrained to at most ~20% of the BeXRB population: most systems are detected in the cold-disk luminosity band, and only a handful of short-spin systems sit near or below the propeller limit with stringent upper limits.
With more than 80% of BeXRBs detected in eRASS1:4 at $10^{33}{-}10^{35}\,\mathrm{erg}\,\mathrm{s}^{-1}$, the eROSITA data indicate that stable low-luminosity accretion rather than quiescence is the typical state of these binaries.
The logN-logL of the known sample requires a broken power law with the low-luminosity part dominated by BeXRBs, so extrapolating a single power law from outburst-censored samples would misrepresent both the shape and the subclass composition of the Milky Way HMXB population.

Reading between the lines

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

If accretion outside outburst is the norm, the transient/quiescent distinction for BeXRBs is largely an observational bias of monitoring instruments; population synthesis and binary evolution models should treat most BeXRBs as quasi-persistent low-luminosity accretors with outburst duty cycles superimposed, which would change estimates of the integrated accretion luminosity of the Galaxy.
The $10^{32}$–$10^{33}\,\mathrm{erg}\,\mathrm{s}^{-1}$ overlap between the most luminous isolated Be stars and the faintest BeXRBs suggests luminosity alone cannot identify hidden compact companions; the discriminating observables are hard-band spectral shape (power-law tail versus purely thermal) and timing (pulsations), a testable prediction for follow-up campaigns with sensitive hard X-ray inst
Correlating eROSITA luminosities with optical measurements of the Be star's circumstellar disk state across the eRASS1–4 sample would test the cold-disk interpretation: if X-rays persist when the disk is depleted, the low-luminosity accretion must be fed by a different reservoir than the classic decretion disk.

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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

You should know two things about this paper. First, the central measurement is real and valuable: it is the first wide-area logN-logL for known Galactic HMXBs reaching down to about 10^32 erg/s, three orders of magnitude fainter than what RXTE/ASM or MAXI could do. Second, the headline claim that accretion outside outburst is “likely the norm” for >80% of BeXRBs is plausible but less firmly established than the abstract suggests, because it leans on a small, volume-limited sample of Be stars that is not demonstrably unbiased.

The paper is genuinely well done. The cross-matching, pile-up corrections, and upper-limit treatment are careful. The consistency check against RXTE/ASM and MAXI, using random sampling of the monitoring lightcurves to match eROSITA's snapshot nature, is a thoughtful and convincing way to validate the bright end. The subclass-resolved distributions, with SgXBs populating the high-luminosity end and BeXRBs the low end, are a useful step beyond earlier averaged XLFs. The catalog release is a plus.

The soft spot is exactly where the stress-test note lands. The “order of magnitude above the most X-ray luminous Be stars” baseline is the 500 pc volume-limited Be-star subsample, which contains only a few hundred stars and ends near 10^32 erg/s. The full (non-volume-corrected) Be-star sample extends above 10^33 erg/s and overlaps the faint BeXRBs. If the true Be-star luminosity function has a tail to 10^33 erg/s, then the 80% detection fraction at luminosities “10x above the Be-star max” would drop. The authors do acknowledge the overlap and use spectral hardness as a discriminator, and they have some NuSTAR follow-up, but the luminosity-only excess is still a load-bearing part of their argument. They should either quantify the uncertainty in the Be-star maximum (e.g., via a luminosity function model or a bootstrap) or soften the specific 80%/10x claim.

Other concerns are minor: the sample is half the sky, distances for some systems are poorly constrained, and the faint-source fluxes assume fixed spectral parameters. None of this breaks the measurement.

Bottom line: this paper deserves a serious referee. The logN-logL extension and the snapshot-detection statistics are important and likely correct. The accretion interpretation is probably right, but the Be-star baseline comparison needs strengthening before the headline claim is published as stated.

Recommendation: send it to peer review, but ask the authors to make the Be-star comparison robust and to restrain the abstract until they do.

Referee Report

3 major / 5 minor

Summary. The paper presents eROSITA eRASS1-4 observations of 72 known HMXBs in the Western Galactic hemisphere, measuring 0.2-10 keV fluxes and luminosities down to ~10^32 erg/s, with careful pile-up corrections, fixed/modeled spectral parameters, and upper limits for non-detections. It constructs logN-logL distributions for the full sample and for subclasses (BeXRBs, SgXBs, SFXTs), compares them with variability-aware resamplings of RXTE/ASM and MAXI light curves, and compares BeXRB luminosities with those of isolated Be stars. The paper reports that BeXRBs dominate the low-luminosity end, that combining the four eRASS surveys yields a detection fraction of about 80% for known BeXRBs, and interprets the luminosity excess over isolated Be stars as evidence that low-luminosity accretion outside outburst is likely the norm, discussing cold-disk accretion and the propeller mechanism.

Significance. If the central claim is robust, this is an important result: it is the first wide-area survey characterization of Galactic HMXBs at 10^32-10^34 erg/s, with implications for the HMXB XLF, the quiescent behavior of BeXRBs, and accretion theory at low mass-accretion rates. The paper's strengths include a carefully vetted and reclassified HMXB catalog, explicit treatment of pile-up, cross-instrument consistency checks against RXTE/ASM and MAXI, and the release of a source catalog as auxiliary material. However, the headline accretion conclusion rests on a statistically fragile comparison to a small volume-limited Be-star sample and, for most sources, on luminosity arguments rather than direct spectral or timing diagnostics; the significance is therefore conditional on a more robust statistical treatment of the Be-star baseline.

major comments (3)

[Sect. 4, Fig. 6] The load-bearing comparison for the abstract's claim that more than 80% of BeXRBs exceed the most X-ray luminous Be stars by an order of magnitude uses the 500 pc volume-limited Be-star subsample as the baseline. This sample contains only of order 10^2 Be stars, so its observed upper end near 10^32 erg/s is a noisy extreme-order statistic; the non-volume-limited Be-star sample in the same figure extends above 10^33 erg/s and overlaps the BeXRB locus, as the paper itself acknowledges. If the intrinsic Be-star X-ray luminosity function has a tail to about 10^33 erg/s, the 'order of magnitude' threshold becomes about 10^34 erg/s, and most eROSITA BeXRB detections, which cluster at 10^33-10^34 erg/s, would no longer exceed it. The manuscript needs a quantitative treatment of this baseline, for example a bootstrap or order-statistics analysis, or a completeness-corrected Be-star XLF, before the headline claim can be supported.
[Sect. 5.2, Fig. 8] The central physical conclusion that accretion outside outburst is the norm is an extrapolation from snapshot detections for most sources. The paper states in Sect. 5.2 that eROSITA does not provide enough statistics for detailed spectral or timing studies, and the spectral discrimination between a Be star and a low-luminosity BeXRB (Fig. 7) is available for only a minority of sources. Hard X-ray confirmation, shown as blue points in Fig. 8, covers roughly 20% of the sample (Zalot et al. 2026). For the remaining detections, the luminosity excess over isolated Be stars could also be produced by binary-enhanced donor emission, gamma-Cas-like activity, or magnetospheric emission, alternatives that the paper itself discusses for bright Be stars. The conclusion should be reworded as a hypothesis with supporting evidence, and the fraction of sources with direct accretion signatures should be stated separately from the fraction detected at elevated luminosity.
[Sect. 3.1, Sect. 5.2] The flux and luminosity calibration carries an acknowledged systematic uncertainty of up to a factor of 10 from geometrical and other effects (Sect. 5.2), which is comparable to the 'order of magnitude' excess that underpins the central claim. In addition, fluxes for sources with fewer than about 50 counts are derived by fixing Gamma=1 or kT=1 keV and N_H at catalog values, and upper limits are sensitive to the assumed absorption. Since many sources lie near the 10^33 erg/s threshold used to define the >80% fraction, the authors should propagate these uncertainties into the reported detection fraction and the order-of-magnitude excess fraction, for example by varying spectral parameters and N_H within plausible ranges.

minor comments (5)

[Abstract] The abstract refers to 'the Galactic population' and 'known HMXBs' without noting that the analysis covers only the Western Galactic hemisphere; this limitation should be stated explicitly in the abstract.
[Table C.1] The column labeled 'KS-Test probability' reports values such as 19.32 and 6.82, which cannot be probabilities; this is likely the KS statistic or a scaled D value, and the column should be relabeled or converted to p-values.
[Sect. 5.1, Abstract] The text states that the detection fraction increases to 80% when combining eRASS1:4, while the abstract claims that more than 80% of BeXRBs are detected at luminosities at least an order of magnitude higher than the most X-ray luminous Be stars; these are different statements, and not all sources in Table E.1 have minimum luminosities above 10^33 erg/s, so the wording should be reconciled.
[Fig. 6] Please clarify whether the red dashed curve for undetected BeXRBs is constructed from flux upper limits and how upper limits enter the N(>L) counting; the current description is ambiguous.
[Sect. 4] The phrase 'in lieu of a volume-corrected distribution' highlights a limitation of the Be-star comparison; at minimum, the discussion should address how the distance and absorption distributions of the BeXRB sample differ from those of the 500 pc Be-star sample, since these differences could bias the inferred luminosity excess.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the eROSITA detection claim and the physical thresholds are externally anchored; self-citations are supportive, not load-bearing.

full rationale

The paper's central claim is observational: eROSITA detects most known BeXRBs at 10^33-10^35 erg/s, and this is above the bright end of the volume-limited 500 pc Be-star sample. This is not a fitted prediction. The Be-star baseline is an independently constructed eROSITA logN-logL from the BeSS catalog; it is not a parameter fit to BeXRB data, and no equation defining the BeXRB excess in terms of the Be-star baseline is introduced. The paper explicitly notes the overlap between the total Be-star sample and the least luminous BeXRBs (Sect. 4, Fig. 6), so the comparison is not disguised as a separation. The fragility of the 500 pc bright end is a statistical-robustness concern about a small-sample maximum used 'in lieu of a volume-corrected distribution,' not a circular reduction: the threshold is not chosen to make the 80% statement true. The physical interpretation uses external thresholds (Tsygankov et al. 2017a for cold disk; Illarionov & Sunyaev 1975 for propeller; Corbet et al. 1997 for magnetospheric accretion), with parameter ranges for B and spin stated; these are not fitted to the eROSITA data. The paper's own caveats (Sect. 5.2 factor-of-10 luminosity uncertainties; Sect. 5.3 that non-detections cannot be interpreted without absorption information) are honest limitations that lower the strength of the inference but do not constitute circularity. Self-citations appear (Zalot et al. 2026 for NuSTAR hard X-ray detections; Weber et al. 2026 for eROSITA completeness; Stierhof et al. 2025 for characteristic radii), but the detection claim is established by the eROSITA measurements themselves and checked against external RXTE/ASM and MAXI distributions, so these citations are supportive rather than load-bearing. No equation reduces to its own input, no fitted parameter is renamed as a prediction, and no uniqueness theorem is imported. Therefore no significant circularity; score 2 reflects only the presence of minor supportive self-citations.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The central observational result depends mainly on survey completeness, catalog completeness, distances, and spectral assumptions. The physical interpretation additionally depends on external accretion theory. There are no new particles or forces; the only speculative population is hidden BeXRB companions among isolated Be stars, which is not an invented entity.

free parameters (4)

Broken power law parameters (K, Gamma_1, Gamma_2, L_break) = Table 2, varies per eRASS and subclass
Fitted to the eROSITA logN-logL distributions to describe their shape; they do not enter the physical accretion claim directly but show the data require a break.
Photon index Gamma for the power law spectral model = Fitted for sources with more than 50 counts, fixed to 1 for faint sources
Used to convert count rate to flux; the choice affects derived luminosities and upper limits (Sect. 3.1).
Blackbody temperature kT = Fitted for bright sources, fixed to 1 keV for faint sources
Alternative spectral model used for Be stars and low-count HMXBs; affects flux estimates (Sects. 3.1 and 4).
Absorption column N_H = Fixed from XRBcats or HI4PI, not fitted
Fixed to literature or Galactic values; highly absorbed sources may have underestimated flux if intrinsic absorption is variable (Sect. 3.1).

assumptions (5)

domain assumption eROSITA is complete to 10^-13 erg/s/cm^2, and effective exposures of 400 to 1400 s are sufficient to treat non-detections above this limit as source-intrinsic.
The paper relies on this to convert detection fractions into statements about intrinsic behavior (Sect. 3.1, Fig. 1, Sect. 5.1).
domain assumption The known HMXB catalog from XRBcats and Fortin et al. is representative of the true Galactic HMXB population in the Western hemisphere.
All population fractions and logN-logL shapes are computed from this known sample, not a complete survey sample (Sect. 2.1).
domain assumption Gaia DR3 and XRBcat distances are accurate enough for luminosity estimates.
Luminosities scale as distance squared; distance uncertainty is not propagated into the logN-logL (Sect. 3.2).
domain assumption The eROSITA detected Be-star sample, especially the 500 pc volume-limited subsample, provides the correct baseline for the Be donor X-ray luminosity in BeXRBs.
The central accretion-is-the-norm argument compares BeXRB luminosities to this baseline (Sect. 4, Fig. 6).
domain assumption The cold disk accretion and propeller threshold formulas from Tsygankov et al. 2017a and Illarionov and Sunyaev 1975 apply to these systems with the assumed magnetic field range of 10^12 to 10^13 G.
Used to classify sources as accreting, propelling, or transitional in Fig. 8 (Sect. 5.2, Eqs. 2 and 3).

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Cite this review

Pith. "Pith review of The low luminosity end of Galactic HMXBs with eROSITA: Establishing a luminosity floor for accreting BeXRBs." pith.science (2026). https://pith.science/paper/OEZJSXUG

@misc{pith2026260813259,
  author       = {Pith},
  title        = {Pith review of: The low luminosity end of Galactic HMXBs with eROSITA: Establishing a luminosity floor for accreting BeXRBs},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OEZJSXUG}},
  note         = {Machine review of arXiv:2608.13259}
}

abstract

We present a first look at the Galactic population of heretofore known HMXBs as observed by SRG/eROSITA during its first four surveys. eROSITA's sensitivity of $\sim10^{-13}\,\mathrm{erg}\,\mathrm{s}^{-1}\,\mathrm{cm}^{-2}$, translating to $10^{32}$-$10^{34},\mathrm{erg}\,\mathrm{s}^{-1}$ in luminosity for most known HMXBs in the Milky Way, has thus far never been reached by any wide-area survey instrument. We present the extended log N-log L distribution of known HMXBs reaching down to $10^{32}\,\mathrm{erg}\,\mathrm{s}^{-1}$ using eROSITA, and show the large scatter that can be induced by source intrinsic variability. We present sub-type resolved luminosity distributions, showing that the Supergiant X-ray binaries (SgXBs) and Be X-ray binaries (BeXRBs) occupy different parts of the overall distribution, and reanalyse RXTE/ASM data and MAXI for comparison to eROSITA. The luminosity regime uncovered by eROSITA allows a systematic study of the "transient" BeXRBs, which are typically below the detection threshold of monitors outside of outburst, and whose low luminosity behavior has been a longstanding question. Signatures of stable accretion at low luminosities have been observed with pointed instruments for a fraction of the overall sample, so far. With the eROSITA results, we posit that accretion outside of outburst is likely the norm, since a vast majority (> 80%) of BeXRBs are detected at luminosities at least an order of magnitude higher than expected for the most X-ray luminous Be stars. We discuss the observed luminosity in the context of cold disk accretion and the "propeller" mechanism. We highlight a small subpopulation of "isolated" Be-stars that reach luminosities comparable to the least luminous BeXRBs, hinting at the presence of compact object companions.

Figures

Figures reproduced from arXiv: 2608.13259 by the authors.

**Figure 1.** Known HMXBs in the Western hemisphere depicted with the effective exposure time at their corresponding sky position, shown in a Hammer projection of the Galactic plane. All sources in our sample are within 5◦ latitude of the galactic plane. They each get effective exposure of ∼400–1400 s in the combined eRASS1:4 data. to increase the number of known HMXBs in the Galaxy by a factor 2 (Doroshenko et al. 2014). Confirm… view at source ↗

**Figure 2.** The log N-log S distribution computed using eROSITA fluxes obtained according to Sect. 3.1 in eRASS1:4. The eROSITA log Nlog S distribution reaches down to fluxes of 10−13 erg cm−2 s −1 , which is where eROSITA is complete up to 99% (Weber et al. 2026). 0 5 10 15 20 Distance [kpc] 0 5 10 15 20 Number 1031 1032 1033 1034 Llim erg s − Distance unknown 1 flim = 10−13 cgs flim = 6 × 10−14 cgs [PITH_FULL_IMAGE:figures/… view at source ↗

**Figure 3.** Left hand axis and histogram: Number of sources in a given distance range (teal) and number of sources with unknown distances (grey). Right hand axis: Limiting luminosity to which eROSITA is complete within a sensitivity limit of 10−13erg s cm−2 marked for the 0.2– 10.0 keV (solid) and the 0.2–2.3 keV (dashed) bands. eROSITA is complete down to a 0.2–10.0 keV luminosity of 1033 erg s−1 within ∼ 10 kpc. istically l… view at source ↗

Figures from the paper (5 more)

**Figure 4.** Figure 4: Left: The log N-log L distributions of HMXBs and their subclasses as detected by eROSITA in eRASS1 to eRASS4, multiplied by 2 to project to the whole sky. The subclasses show marked variability in eRASS1–4, depending on the flaring states of individual sources. Right: …

**Figure 5.** Figure 5: RXTE/ASM (left) and MAXI (right) log N-log L taking variability into account by random sampling from the monitoring lightcurves of each source, along with the eRASS1–4 distributions. RXTE/ASM is sensitive up to 1036 erg s−1 , while MAXI reaches a few 1035 erg s−1 . Bot…

**Figure 6.** Figure 6: eROSITA log N-log L distributions of BeXRBs (red) shown alongside that of Be stars (teal), using eRASS1 as a representative case. A volume-limited sample of Be stars within 500 pc (teal, dashed) is also shown in lieu of a volume-corrected distribution. BeXRBs are evide…

**Figure 7.** Figure 7: Comparison of a typical spectrum of an isolated Be star, and a BeXRB at low luminosity. The Be star spectrum is purely thermal and drops off after 1 keV. The BeXRB on the other hand, is significantly harder, and prominent above 1 keV. the luminosity to be expected of t…

**Figure 8.** Figure 8: Luminosities and NS spins of Galactic BeXRBs. Points from each eRASS scan are connected for readability. A separate panel shows luminosities of systems without a known spin period. The transition luminosities towards cold disk accretion according to Tsygankov et al. (2…

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