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arxiv: 2606.24159 · v1 · pith:L26LT7GZnew · submitted 2026-06-23 · 🌌 astro-ph.GA · astro-ph.CO

A First Measurement of Circumgalactic Dust Reddening from Only 4.6 deg² of the Rubin Observatory's DP1

John Franklin Crenshaw , Matthew McQuinn , Jessica K. Werk This is my paper

Pith reviewed 2026-06-26 00:06 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords circumgalactic dustreddeningextinctiongalaxy halosLSSTRubin Observatoryphotometric redshiftsdust budget
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The pith

Circumgalactic dust reddening measured from just 4.6 square degrees of Rubin Observatory data matches results from much larger surveys.

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

The paper stacks colors of background galaxies around foreground galaxies using photometric redshifts in a small patch of early Rubin data. This reveals a reddening signal from 10 kpc to 1 Mpc, which they convert to visual extinction using a Milky Way curve. The resulting profile agrees in amplitude and slope with previous measurements despite the tiny survey area and a sample of much fainter, lower-mass galaxies. A sympathetic reader would care because it shows that LSST can deliver precise galaxy-dust maps even early on, and it hints at substantial dust in halos of typical galaxies.

Core claim

The authors detect a chromatic reddening profile by stacking background galaxy colors around foreground galaxy positions. Interpreting the average E(g-z) with a Milky Way extinction curve, they measure A_V = (1.2 ± 0.4) × 10^{-1} (r_⊥ / 20 kpc)^{-1.8 ± 0.4} within 120 kpc. This profile extends the measurement to lower stellar mass galaxies and shows that the innermost regions reach A_V around 0.3 magnitudes, comparable to Milky Way disk extinction.

What carries the argument

Stacking of background-galaxy colors around foreground-galaxy positions using photometric redshifts to extract the chromatic reddening profile.

If this is right

  • The steep power-law slope of -1.8 implies the dust distribution does not simply trace the halo-gas profile.
  • Redder foreground galaxies exhibit stronger reddening within 50 kpc, suggesting a dust-to-stellar-mass ratio near 1 percent.
  • The measurement reaches comparable precision to prior work with 1000 times less area, demonstrating LSST's capability for such studies.
  • Splitting the sample shows potential color dependence, though the blue subsample remains noisy.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the Milky Way curve applies, the high dust content in lower-mass halos suggests efficient dust production or retention in these systems.
  • Full LSST coverage could allow mapping how dust content varies with galaxy environment and redshift.
  • The agreement with larger surveys validates the photometric redshift approach for future wide-field dust measurements.

Load-bearing premise

The observed color excess is due to dust reddening rather than photometric redshift errors, galaxy clustering biases, or other systematics, and the Milky Way extinction curve applies to circumgalactic dust.

What would settle it

Repeating the analysis with a sample of galaxies having spectroscopic redshifts that shows no significant color excess signal.

Figures

Figures reproduced from arXiv: 2606.24159 by Jessica K. Werk, John Franklin Crenshaw, Matthew McQuinn.

Figure 1
Figure 1. Figure 1: Foreground (background) galaxies are green (purple). Left: LePhare vs FlexZBoost photo-z estimates. We remove galaxies for which the two estimates differ by more than 0.1(1 +zphot). For the remainder, we assign the inverse variance-weighted mean of the two methods for our photo-z estimate. Middle: photo-z vs spec-z for galaxies with spectroscopy. Right: photo-z and spec-z histograms. These distributions de… view at source ↗
Figure 2
Figure 2. Figure 2: Upper: rest-frame color-magnitude diagram for the foreground sample. We use a cut of g − r = 0.5 to split the foreground sample into red and blue subsamples. Left: observed-frame apparent r-band magnitudes. Dashed lines and arrows mark magnitude limits from previous studies. Middle: estimated stellar masses. The red sample is more massive than the blue sample; dashed lines and arrows mark lower mass limits… view at source ↗
Figure 3
Figure 3. Figure 3: Observed extinction relative to the r band, compared with standard extinction curves for the Milky Way (blue; E. L. Fitzpatrick 1999 with RV = 3.1) and the SMC bar (red; K. D. Gordon et al. 2003). Each panel shows one radial bin. The MW and SMC normalizations are fit independently in each bin; the corresponding χ 2 per degree of freedom is shown in the upper right. We then estimate the radial profile of th… view at source ↗
Figure 4
Figure 4. Figure 4: Top left: average projected AV reddening from our stacking analysis using Rubin DP1 E(g − z), compared to previous measurements from SDSS (B. M´enard et al. 2010b), KiDS (E. Genc et al. 2025), and DES (J. E. McCleary et al. 2026). Top right: AV measurements from each of the twelve jackknife samples, where the legend indicates which jackknife region was excluded. Bottom left: AV for the red and blue foregro… view at source ↗
Figure 5
Figure 5. Figure 5: Stacked reddening profiles with jackknife uncertainties for several analysis variants. With the exception of the estimator that omits the flipped-stack correction, the variants remain consistent with the fiducial measurement, indicating that the DP1 signal is not driven by any single analysis choice. Note all analyses use the same radial binning; the offsets in r⊥ are for visibility. C. VALIDATING THE ROBU… view at source ↗
Figure 6
Figure 6. Figure 6 [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
read the original abstract

We present the first measurement of circumgalactic dust reddening from the Vera C. Rubin Observatory, using only 4.6 deg$^2$ of ComCam Data Preview 1 - roughly $0.03\%$ of the final LSST footprint. Using photometric redshifts, we stack background-galaxy colors around foreground-galaxy positions and detect a chromatic reddening profile from $r_\perp \simeq 10$ kpc to $1$ Mpc. Interpreting average $E(g-z)$ with a Milky Way extinction curve, we find $A_V = (1.2 \pm 0.4) \times 10^{-1} (r_\perp / 20\,\mathrm{kpc})^{-1.8 \pm 0.4}$ within $120$ kpc. The amplitude and radial dependence agree with earlier SDSS, KiDS, and DES results despite the $\sim1000\times$ smaller survey area and a foreground sample extending 3-6 mag fainter and 1-2 dex lower in stellar mass. The innermost 10-15 kpc bin reaches $A_V \simeq 0.3$ mag, comparable to high-latitude extinction through the Milky Way disk near the Solar circle; the steep power-law slope implies a dust distribution that does not simply trace the halo-gas profile. Splitting by rest-frame $g-r$ shows stronger extinction around red foreground galaxies (rest-frame $g-r > 0.5$), although the blue subsample is too noisy to establish a significant color dependence. This red sample, with median halo mass $5 \times 10^{11}\,M_\odot$, shows substantially more reddening within 50 kpc than previously measured around more massive LRGs and implies a dust-to-stellar-mass ratio of $\sim 1\%$, nearly saturating the dust budget allowed by stellar metal yields. These pathfinder data demonstrate LSST's promise for high-precision galaxy-dust measurements across galaxy mass, environment, and redshift.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The paper presents the first measurement of circumgalactic dust reddening from 4.6 deg² of Rubin Observatory ComCam DP1 data. Using photometric redshifts, background galaxy colors are stacked around foreground galaxy positions to detect a chromatic reddening signal from ~10 kpc to 1 Mpc. Interpreting the average E(g-z) with a Milky Way extinction curve yields the power-law A_V = (1.2 ± 0.4) × 10^{-1} (r_⊥ / 20 kpc)^{-1.8 ± 0.4} within 120 kpc, with amplitude and slope consistent with prior SDSS/KiDS/DES results despite the ~1000× smaller area and fainter, lower-mass foreground sample. Additional findings include stronger reddening around red galaxies and implications for dust-to-stellar-mass ratios.

Significance. If robust, the result is significant as a pathfinder demonstrating LSST's capability for high-precision CGM dust measurements with limited data, extending prior work to lower-mass halos (~5×10^{11} M_⊙) and providing a steep radial profile that does not trace halo gas. The agreement with independent surveys and the detection in a small footprint are strengths.

major comments (3)
  1. [Methods (background selection and photo-z validation)] The central interpretation that the stacked E(g-z) arises from dust reddening (rather than photo-z errors, clustering biases, or selection effects) is load-bearing for the A_V profile and all downstream claims, yet the methods provide no quantitative validation of photometric redshift quality for the background sample or explicit tests (e.g., null tests with randomized positions or color-selected subsamples) to rule out these systematics. This is especially relevant given the foreground sample is 3-6 mag fainter than prior LRG studies.
  2. [Results (interpretation of E(g-z) and A_V fit)] The conversion of measured E(g-z) to A_V assumes a Milky Way extinction curve applies to CGM dust at these radii and galaxy masses; no justification, alternative curves, or sensitivity test is provided, directly affecting the quoted normalization and the comparison to prior work.
  3. [Results (power-law fit and error budget)] The power-law fit within 120 kpc reports uncertainties on amplitude and index, but the text does not detail how the covariance matrix incorporates the small survey area, sample variance, or potential systematics from the 4.6 deg² footprint; this undermines the claimed consistency with SDSS/KiDS/DES results.
minor comments (2)
  1. [Abstract and Introduction] The abstract and text use 'first measurement' without clarifying how it differs in methodology or sample from the cited SDSS/KiDS/DES works beyond area and depth.
  2. [Figures and Results] Figure captions and text should explicitly state the number of foreground/background pairs per radial bin to allow assessment of the innermost bin's A_V ~0.3 mag claim.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive comments, which highlight important areas for clarification in our pathfinder analysis. We address each major comment below with honest responses and commit to revisions that strengthen the manuscript without overstating the current data.

read point-by-point responses

  1. Referee: The central interpretation that the stacked E(g-z) arises from dust reddening (rather than photo-z errors, clustering biases, or selection effects) is load-bearing for the A_V profile and all downstream claims, yet the methods provide no quantitative validation of photometric redshift quality for the background sample or explicit tests (e.g., null tests with randomized positions or color-selected subsamples) to rule out these systematics. This is especially relevant given the foreground sample is 3-6 mag fainter than prior LRG studies.

    Authors: We agree this is a valid concern for a pathfinder result using fainter samples. The current manuscript relies on the detection significance and consistency with prior surveys for validation, but lacks explicit metrics. In revision we will add quantitative photo-z validation (e.g., outlier fractions and bias estimates from available spec-z overlaps) plus null tests with randomized foreground positions and color-selected background subsamples. These will be presented in a new methods subsection to directly rule out the listed systematics. revision: yes

  2. Referee: The conversion of measured E(g-z) to A_V assumes a Milky Way extinction curve applies to CGM dust at these radii and galaxy masses; no justification, alternative curves, or sensitivity test is provided, directly affecting the quoted normalization and the comparison to prior work.

    Authors: The manuscript adopts the MW curve for direct comparability with SDSS/KiDS/DES results but provides no explicit justification or alternatives. We will revise by adding a short justification paragraph citing prior CGM dust studies that support MW-like curves at these radii, plus a sensitivity test showing A_V changes under SMC/LMC curves. This will quantify the impact on normalization while preserving the core radial profile result. revision: yes

  3. Referee: The power-law fit within 120 kpc reports uncertainties on amplitude and index, but the text does not detail how the covariance matrix incorporates the small survey area, sample variance, or potential systematics from the 4.6 deg² footprint; this undermines the claimed consistency with SDSS/KiDS/DES results.

    Authors: The uncertainties are derived from bootstrap resampling over the 4.6 deg² footprint, which captures some sample variance, but the text indeed omits a full description of the covariance construction. We will expand the methods to detail the bootstrap procedure, its limitations for cosmic variance on this scale, and why the detected signal amplitude remains comparable to larger surveys. We maintain that the consistency claim is still supported by the high-significance detection, but the added text will make the error budget transparent. revision: partial

Circularity Check

0 steps flagged

No circularity: direct empirical stack and fit to observed colors

full rationale

The paper measures E(g-z) by stacking background galaxy colors around foreground positions in 4.6 deg² data, then converts the measured excess to A_V via an external Milky Way extinction curve and fits a power-law radial profile to the data. No step equates a claimed prediction or first-principles result to its own inputs by construction; the power-law parameters are fitted rather than presupposed, and no self-citations close any loop on the core measurement or interpretation. The derivation is self-contained against the observed photometry.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claim rests on fitting two parameters to the stacked color-excess profile and on the assumption that a standard Milky Way extinction law converts the observed E(g-z) into A_V; no new entities are postulated.

free parameters (2)
  • power-law index = -1.8
    Fitted exponent of the radial A_V profile
  • normalization amplitude = 0.12
    Fitted prefactor of the A_V profile at 20 kpc
axioms (1)
  • domain assumption Milky Way extinction curve applies to circumgalactic dust
    Invoked when converting measured E(g-z) to A_V

pith-pipeline@v0.9.1-grok · 5927 in / 1480 out tokens · 18093 ms · 2026-06-26T00:06:57.646803+00:00 · methodology

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