Constraining the Milky Way's Dispersion Measure Using FRB and X-ray Data

Jiale Wang; Taotao Fang; Xiaochuan Jiang; Zheng Zhou

REVIEW 5 major objections 5 minor 72 references

Constraining the Milky Way's Dispersion Measure Using FRB and X-ray Data

T0 review · 5 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read O VII X-ray absorption tracks the Milky Way component of FRB dispersion, giving an empirical DM-MW estimator.

desk verdict New empirical correlation between O VII absorption and Milky Way DM, but the latitude confound is unaddressed and the estimator is not yet trustworthy. read the letter →

arxiv 2501.16770 v1 pith:HUR4ZRDB submitted 2025-01-28 astro-ph.GA astro-ph.HE

Jiale Wang , Zheng Zhou , Xiaochuan Jiang , Taotao Fang This is my paper · ORCID

classification astro-ph.GAastro-ph.HE

keywords Galaxy:haloX-rays:diffusebackgroundradiocontinuum:transientsfastburstsdispersionmeasureOVIIabsorptionhotgasmissingbaryons

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 claims that the Milky Way's contribution to fast radio burst dispersion can be estimated from X-ray absorption by hot gas, specifically the O VII line. Using 47 localized FRBs and the Macquart relation to subtract intergalactic and host-galaxy contributions, it finds a positive correlation between DM_MW and the average O VII equivalent width within 10 degrees of each FRB, with Pearson r = 0.8636 and p = 3.35e-5 on 15 data points. The authors derive an empirical linear relation between DM_MW and O VII equivalent width and argue that O VII absorption traces both the disk and halo components of Galactic hot gas. If correct, O VII absorption gives a practical foreground correction for FRB cosmology and a probe of the temperature structure of the Milky Way's hot gas.

What carries the argument

The load-bearing object is the equivalent width of the O VII K-$\alpha$ absorption line from AGN sightlines, used as a column tracer of million-degree gas. For each FRB, the paper averages the O VII equivalent widths of absorption sources inside a 10-degree angular circle around the FRB's Galactic coordinates, then fits DM_MW against that average with a Markov-chain Monte Carlo procedure. On the other side of the argument, the Macquart relation supplies the intergalactic DM estimate, and a host-galaxy contribution of 30/(1+z) pc $cm^{-3}$ is subtracted, so the DM_MW values are the residual that O VII absorption must explain.

What would settle it

Take a larger sample of localized FRBs with O VII absorption sightlines inside 10 degrees, split it by Galactic latitude (for example, |b| > 30 degrees versus |b| < 30 degrees), and test whether the DM_MW versus O VII equivalent-width relation persists within each latitude bin; if it disappears or flips sign within bins, the claimed correlation is driven by the latitude dependence of both quantities rather than by the hot-gas column.

Watch

Extended reading notes

Core claim

The central discovery is an empirical relationship: DM_MW = (288.71 ± 73.93)(EW_O_VII / 20 mÅ) − (141.17 ± 50.34) pc $cm^{-3}$, based on 15 FRB sightlines that have O VII absorption measurements within 10 degrees. The authors interpret this as evidence that the hot gas traced by O VII K-$\alpha$ absorption is the same ionized medium that contributes to the dispersion of extragalactic FRBs, with both the disk and halo contributing. Supporting evidence comes from two directions: there is no reliable correlation between DM_MW and O VII or O VIII emission, which mostly traces dense disk gas, and the derived DM_MW values match electron-density models that include a halo but significantly exceed disk-only models such as NE2001 and YMW16. The lack of a strong O VIII absorption correlation further suggests that the dominant hot-gas temperature is near 2 × $10^{6}$ K, with hotter gas present but less abundant.

Load-bearing premise

The correlation rests on the assumption that the average O VII absorption equivalent width measured from AGN sightlines within a 10-degree circle around each FRB represents the hot-gas column that actually contributes to that FRB's dispersion measure.

Editorial extensions

If this is right

If O VII absorption traces the same hot gas that disperses FRBs, future FRB surveys can use nearby AGN absorption sightlines to estimate and subtract the Milky Way foreground, reducing systematic error in intergalactic and host-galaxy DM studies.
The empirical formula gives a way to predict the Milky Way DM contribution without relying only on electron-density models like NE2001 and YMW16, which the paper finds underestimate high-latitude DM.
The correlation implies a substantial, direction-dependent hot-halo contribution to DM, so cosmological baryon counts using FRBs must treat the Galactic halo as a real foreground component rather than a constant offset.
The inferred dominant temperature near 2 × 10^6 K, traced by O VII rather than O VIII, is a testable statement about the Milky Way's hot-gas phase structure.
A larger localized-FRB sample, such as the one expected from current and future CHIME-era surveys, can sharpen the coefficients of the empirical relation and map how the correlation changes with sky position.

Reading between the lines

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

If the correlation holds, maps of O VII absorption column density could be converted into an all-sky DM foreground map, a directly testable product once hundreds of localized FRBs and dense O VII sightline coverage exist.
A testable extension is to check nearby, low-redshift FRBs with small intergalactic DM scatter: those with large O VII equivalent widths should show systematically larger DM residuals than those with small equivalent widths.
The apparent correlation may partly reflect Galactic latitude, since both DM and O VII column decline away from the plane; controlling for latitude in a larger sample would separate path-length geometry from a true column-density relation.
A randomized-sky control, shuffling FRB coordinates while keeping the O VII sightline positions fixed, would quantify how often a correlation as strong as r = 0.86 arises by chance given the sparse 15-point sample.

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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: the genuine new item is the explicit correlation test between FRB-derived DMMW and O VII absorption equivalent width, leading to the empirical relation in Eq. 2. The paper does this with 47 localized FRBs and existing X-ray data, and it runs sensible robustness checks on DM_host assumptions and the four unusual FRBs. Those checks show the 10-degree correlation survives reasonable variations.

The soft spot is the latitude confound, and it is as soft as the stress-test note says. The headline r=0.86 at a 10-degree search radius collapses to r=0.34 at 20 degrees and r=0.10 at 30 degrees. That is the signature of a common |b| dependence: both DMMW and O VII EW fall with Galactic latitude, and the paper's own Figure 4 shows DMMW declining with |b|. The authors never control for |b|, so Eq. 2 is not established as an independent tracer. The relation may be a proxy for latitude.

Two more issues, smaller. The DMMW values carry no error bars, so the Pearson p-value overstates significance given the real scatter in DM_host and DM_IGM. And the temperature conclusion rests on O VIII non-detections in only three sightlines; that is too thin to support the claim that the hot gas is mostly 2 x 10^6 K.

The model comparison in Section 4.2 is partially circular, since the halo models were calibrated on the same O VII data. That comparison is not the core of the paper, so it is a minor concern.

The authors are appropriately cautious. They explicitly say the result 'merely suggests a potential connection' and note the small sample. That is honest.

Verdict: a serious editor should send this to review rather than desk-reject. The question is important, the data are public, and a reviewer can ask for a partial correlation control. But as it stands, Eq. 2 is not a calibrated estimator. I would not use it in my own work yet. The paper is useful as a prompt to test the latitude confound with the next CHIME sample.

Referee Report

5 major / 5 minor

Summary. The paper uses 47 localized FRBs to derive Milky Way dispersion measures (DM_MW) by subtracting an IGM term from the Macquart relation and an assumed host-galaxy term of 30/(1+z) pc cm^-3. It then compares these DM_MW values with O VII and O VIII absorption equivalent widths and emission intensities in angular neighborhoods around each FRB. The central claim is a strong positive correlation between DM_MW and O VII absorption EW within a 10-degree search radius, expressed as an empirical relation (Eq. 2), which the authors propose as a practical tracer of the Milky Way's hot-gas contribution to FRB dispersion measures. Supporting claims are that DM_MW is better matched by disk-plus-halo electron density models than by disk-only models, and that the absence of an O VIII correlation implies a hot-gas temperature around 2 x 10^6 K or less.

Significance. If the claimed correlation is physically real and stable, the paper offers a new observational proxy for the Galactic DM contribution to FRBs, which would be valuable for FRB cosmology and for studies of the Milky Way circumgalactic medium. The paper is transparent in using public data, reports multiple robustness checks in Table 2, and includes a candid caveat in Section 4.1 that the results merely suggest a connection. However, the headline correlation is sensitive to the chosen angular radius and is not tested against the strong |b|-dependence shared by both quantities, so the practical utility of Eq. (2) is not yet established.

major comments (5)

[Table 2, Section 3.1] The headline correlation r = 0.8636 is obtained only for the 10-degree search radius; the same analysis at 20 and 30 degrees gives r = 0.3436 and r = 0.1029, respectively. This strong dependence on the averaging radius suggests that the 10-degree result may be driven by a small number of sightlines or by the specific averaging procedure, and it undermines the claim that Eq. (2) is a general empirical tracer. The authors should justify the 10-degree choice, report the number of O VII sources per FRB at each radius, and show that the correlation is not dominated by one or two high-EW points.
[Section 3.1, Figure 2, Figure 4] No control is performed for Galactic latitude |b|, despite the fact that both DM_MW (Figure 4) and O VII absorption EW are expected to decrease with increasing |b|. If the 15 FRBs with O VII sources within 10 degrees span a range of |b|, the positive correlation could arise entirely from this common latitude trend, without requiring that the AGN sightlines probe the same gas as the FRB line of sight. A partial correlation of DM_MW and EW_O_VII controlling for |b|, or a regression that includes |b| as a covariate, is needed before Eq. (2) can be interpreted as a physical tracer relation.
[Table 1, Section 2.2, Table 2] The derived DM_MW values in Table 1 are quoted without uncertainties, and the Pearson p-values in Table 2 do not propagate errors from the Macquart-relation DM_IGM estimate, the assumed DM_host, or the special treatment of the four high-DM FRBs. The alternative analyses in Table 2 vary these assumptions one at a time, but they do not perform a joint Monte Carlo or bootstrap that includes these uncertainties; such an exercise is necessary to support the quoted p = 3.35e-5 and the error bars on the slope and intercept of Eq. (2).
[Section 4.2] The comparison with electron density models is partly circular for the halo-component claim: the F13 model was calibrated using O VII absorption data from the same group's earlier work, so agreement between FRB-derived DM_MW and F13 does not independently confirm the halo's contribution. The authors should explicitly acknowledge this dependence and identify which aspects of the comparison (e.g., the excess over NE2001/YMW16 at |b| > 20 degrees) remain informative despite it.
[Section 3.2, Section 5] The inference that the lack of O VIII correlation implies a primary hot-gas temperature near 2 x 10^6 K is based on only three FRBs with O VIII absorption data within 10 degrees (r = -0.2255, p = 0.8552). With n = 3, no meaningful correlation can be established or excluded; this statement should be removed or substantially tempered in the abstract and summary.

minor comments (5)

[Equation (2)] The units of the slope and intercept in Eq. (2) are unclear: the slope should be in pc cm^-3 per unit of (EW_O_VII / 20 mA), and the intercept in pc cm^-3; please write the units explicitly.
[Table 1] The column header 'cm -3 pc' should be 'pc cm^-3', and the header 'DM MW' is inconsistent with the notation DM_MW used elsewhere.
[Figure 2] The labels 'D21 b = 50 km/s' and 'D21 b = 100 km/s' refer to the Doppler parameter b from Das et al. (2021), but the figure caption should state this explicitly since 'b' is also used for Galactic latitude.
[Section 4.1] The text says the O VIII data points are 'within a 5-degree region', but Table 2 and Figure 2 report O VIII absorption for 10-, 20-, and 30-degree regions; clarify which region is being discussed.
[References] Reference [20] for the ADS has an incorrect DOI (it points to an Astronomy and Computing article); the ADS overview paper's DOI should be corrected.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the DMMW-O VII correlation uses independent datasets, but one supporting model comparison relies on a same-author halo model.

full rationale

The central derivation chain is not circular. The paper computes DMMW from DMobs by subtracting a Macquart-relation DMIGM and an assumed host DM (Eq. 1 and Section 2.2), then compares these values with O VII and O VIII equivalent widths from independent AGN absorption catalogs. The Pearson r = 0.8636 and MCMC relation Eq. (2) are empirical calibrations, not predictions recycled from the same input; no equation is defined in terms of the quantity it is used to estimate. Section 4.1's comparison with Das et al.'s formula is an external check, and the paper's own limitation statement (Section 4.1) correctly notes the small 15-point sample. The only concern is Section 4.2, where agreement with the F13 halo model is cited as supporting evidence; F13 shares an author with this paper (Fang et al. 2012) and is a model of the same hot-gas component traced by O VII absorption, so it does not provide fully independent confirmation. This self-citation is not load-bearing for the main empirical correlation, which stands on the direct data comparison, so it is a minor issue rather than a circular derivation.

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

The central claim depends on the assumed host DM and the Macquart relation for DM_IGM subtraction, plus the angular averaging of O VII data; none of these are derived in the paper. The slope and intercept of Eq. 2 are fitted to the same 15 data points used to claim the correlation, making them empirical parameters rather than predictions.

free parameters (4)

DM_host normalization = 30 pc cm^-3
The assumed host galaxy DM contribution 30/(1+z) pc cm^-3 is applied to all FRBs lacking localization-paper DM_host values; it enters every derived DM_MW value and therefore the correlation. Alternatives of 60 and 100 pc cm^-3 are tested.
Equation 2 slope = 288.71 ± 73.93 pc cm^-3 per (EW/20 mÅ)
Fitted via MCMC to the 15 FRB-O VII pairs in the 10-degree region.
Equation 2 intercept = -141.17 ± 50.34 pc cm^-3
Fitted simultaneously with the slope by the same MCMC fit.
Angular search radius = 10 degrees (primary), 20 and 30 degrees (robustness)
The headline correlation uses the 10-degree radius; wider radii give much weaker correlations. The radius is chosen by the authors, not derived from theory.

assumptions (4)

domain assumption O VII absorption traces the Milky Way's hot gas that contributes to DM_MW.
Invoked throughout Sections 3 and 4; standard in the X-ray literature but not proven within this paper.
domain assumption The Macquart relation provides an unbiased average DM_IGM(z).
Used in Section 2.2 to subtract DM_IGM; scatter and cosmic variance are not propagated into DM_MW uncertainties.
domain assumption Collisional ionization equilibrium and solar abundance assumptions hold when converting between O VII column, equivalent width, and DM.
Inherited from Das et al. (2021), used for the b=50 and b=100 km/s comparison lines in Figure 2 and the model comparison in Section 4.
standard math Pearson correlation and MCMC linear fitting are appropriate for the data.
Standard statistics used in Section 3; no distributional checks are reported.

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Cite this review

Pith. "Pith review of Constraining the Milky Way's Dispersion Measure Using FRB and X-ray Data." pith.science (2026). https://pith.science/paper/HUR4ZRDB

@misc{pith2026250116770,
  author       = {Pith},
  title        = {Pith review of: Constraining the Milky Way's Dispersion Measure Using FRB and X-ray Data},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HUR4ZRDB}},
  note         = {Machine review of arXiv:2501.16770}
}

read the original abstract

The dispersion measures (DMs) of fast radio bursts (FRBs) are a valuable tool for probing the baryonic content of the intergalactic and the circumgalactic medium of the intervening galaxies along the sightlines. However, interpreting the DMs is complicated by the contributions from the hot gas in and around our Milky Way. This study examines the relationship between DM_MW, derived from localized FRBs, and the Galaxy's hot gas, using X-ray absorption and emission data from O VII and O VIII. We find evidence for a positive correlation between DM_MW and O VII absorption, reflecting contributions from both the disk and halo components. This conclusion is supported by two lines of evidence: (1) No correlation between DM_MW and O VII/O VIII emission, which primarily traces dense disk regions; and (2) the comparison with electron density models, where DM_MW aligns with models that incorporate both disk and halo components but significantly exceeds predictions from pure disk-only models, emphasizing the halo's role. Furthermore, the lack of correlation with O VIII absorption suggests that the primary temperature of the Galaxy's hot gas is likely around 2 x 10^6 K or less, as traced by O VII absorption, while gas at higher temperatures (~3 x 10^6 K to 5 x 10^6 K) is present but less abundant. Our findings provide insights into the Milky Way's gas distribution and improve DM_MW estimates for future cosmological studies.

Figures

Figures reproduced from arXiv: 2501.16770 by the authors.

**Figure 1.** Left: Sky distributions in celestial coordinates of 47 localized FRBs analyzed in this work. The color represents the magnitude of their observed DM (DMobs). Right: DM as a function of redshift for these FRBs, with four unusually high-DM FRBs highlighted. Notably, this approach yielded unusually high DMMW values (exceeding 500 pc cm-3) for FRB 190520B, FRB 210117A, FRB 220610A, and FRB 220914A. Since these FRBs are … view at source ↗

**Figure 2.** The correlation between DMMW and the equivalent width (EW) of O VII (left) and O VIII (right) absorption lines. For each FRB, black circles, blue squares, and light orange triangles represent the average equivalent width of sources found within 10, 20, and 30-degree angular regions centered on the FRB’s Galactic coordinates (l, b). The solid lines show the best-fit results obtained from the 10-degree region data for… view at source ↗

**Figure 3.** The correlation between DMMW and the emission intensities of O VII (left) and O VIII (right) measured in Line Units (L.U.). For each FRB, black circles and blue triangles represent the average emission intensities within 5-degree and 10-degree angular regions centered on the FRB’s Galactic coordinates (l, b), respectively. The solid lines show the best-fit results obtained from the 5-degree region data for both O VI… view at source ↗

Figures from the paper (1 more)

**Figure 4.** Figure 4: illustrates the relationship between DM and Galactic latitude |b|. The lines in the figure represent various models of the Milky Way’s electron density distribution. YMW16 and NE2001, as the most widely used disk electron density models, are also shown as lower limits.…

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Pith tools

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