arxiv: 2604.25627 · v1 · submitted 2026-04-28 · 🌌 astro-ph.GA

Recognition: unknown

The PHANGS-H{α} survey. Ground-based narrow-band imaging of nearby star-forming galaxies

Alessandro Razza , Guillermo A. Blanc , Brent Groves , Enrico Congiu , Justus Neumann , Hsi-An Pan , I-Ting Ho , Ashley T. Barnes

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Francesco Belfiore M\'ed\'eric Boquien Charlie Burton M\'elanie Chevance Oleg Egorov Eric Emsellem Chris Faesi Simon C. O. Glover Kathryn Grasha Ralf S. Klessen Kathryn Kreckel Adam K. Leroy Rebecca McElroy Ismael Pessa Eva Schinnerer Neven Tomi\v{c}i\'c Amirnezam Amiri Gagandeep S. Anand Yixian Cao Daniel A. Dale Simthembile Dlamini Jing Li J. Eduardo M\'endez-Delgado Eric J. Murphy Debosmita Pathak Miguel Querejeta Lise Ramambason Erik Rosolowsky Fabian Scheuermann Leonardo \'Ubeda Thomas G. Williams

Authors on Pith no claims yet

Pith reviewed 2026-05-07 15:52 UTC · model grok-4.3

classification 🌌 astro-ph.GA

keywords PHANGS-Hα surveynarrow-band imagingHα emissionstar-forming galaxiesH II regionsstar formation ratesmulti-wavelength surveysgalaxy calibration

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The pith

PHANGS-Hα delivers narrow-band Hα imaging for 65 nearby star-forming galaxies to anchor calibration and supply star formation rate maps.

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

The paper presents the PHANGS-Hα survey, which obtained narrow-band images of hydrogen-alpha emission from 65 massive nearby galaxies using two ground-based telescopes. This dataset is meant to complement the existing PHANGS-ALMA, MUSE, HST, and JWST observations by providing a common reference for photometric and astrometric calibration. It also generates catalogs of H II regions and star formation rate maps derived from the Hα emission across most of the sample. The authors describe the observations, data reduction, and calibration steps, including a comparison to spectroscopic Hα data from MUSE on a subset of galaxies to refine processing methods for the full set.

Core claim

The PHANGS-Hα survey maps Hα emission over 65 nearby massive star-forming galaxies using the MPG-ESO 2.2-meter telescope and the du Pont 2.5-meter telescope. The data processing applies continuum subtraction and calibration informed by PHANGS-MUSE spectroscopy on a subset, producing emission-line fluxes, H II region samples, and star formation rate maps that serve as an anchor point for photometric and astrometric calibration of the other PHANGS datasets.

What carries the argument

Narrow-band Hα imaging with continuum subtraction and MUSE-informed calibration, which extracts emission-line fluxes and star formation rates from photometric observations across the full sample.

If this is right

Supplies an anchor for photometric and astrometric calibration of the PHANGS-ALMA, PHANGS-MUSE, PHANGS-HST, and PHANGS-JWST datasets.
Delivers samples of H II regions across the 65-galaxy PHANGS sample.
Produces star formation rate maps for the bulk of the PHANGS galaxies at 50-100 pc resolution.
Establishes best practices for narrow-band Hα processing that can be applied consistently to the full dataset.
Enables detailed comparisons between narrow-band photometry and spectroscopic mapping on the overlapping subset.

Where Pith is reading between the lines

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

Combining these Hα maps with ALMA molecular gas data could allow direct measurement of star formation efficiency on cloud scales for the entire sample.
The uniform SFR maps may support statistical studies of how star formation relates to galactic environment across the 65 galaxies.
Extending the narrow-band calibration approach to additional emission lines or larger galaxy samples would test its broader applicability.

Load-bearing premise

Narrow-band imaging after standard continuum subtraction and calibration from MUSE spectroscopy on a subset yields accurate Hα fluxes and star formation rate maps without major systematic errors from filter transmission, background subtraction, or contamination.

What would settle it

Direct comparison of the full-sample Hα fluxes or derived star formation rate maps against independent measurements from UV continuum or infrared data, or against MUSE spectroscopy extended to the entire sample, would reveal whether systematic offsets exceed the expected calibration uncertainties.

Figures

Figures reproduced from arXiv: 2604.25627 by Adam K. Leroy, Alessandro Razza, Amirnezam Amiri, Ashley T. Barnes, Brent Groves, Charlie Burton, Chris Faesi, Daniel A. Dale, Debosmita Pathak, Enrico Congiu, Eric Emsellem, Eric J. Murphy, Erik Rosolowsky, Eva Schinnerer, Fabian Scheuermann, Francesco Belfiore, Gagandeep S. Anand, Guillermo A. Blanc, Hsi-An Pan, Ismael Pessa, I-Ting Ho, J. Eduardo M\'endez-Delgado, Jing Li, Justus Neumann, Kathryn Grasha, Kathryn Kreckel, Leonardo \'Ubeda, Lise Ramambason, M\'ed\'eric Boquien, M\'elanie Chevance, Miguel Querejeta, Neven Tomi\v{c}i\'c, Oleg Egorov, Ralf S. Klessen, Rebecca McElroy, Simon C. O. Glover, Simthembile Dlamini, Thomas G. Williams, Yixian Cao.

**Figure 1.** Figure 1: SFR-M∗ plot showing the distribution of the PHANGSHα galaxy sample. Green circles indicate those observed with WFI on the MPG 2.2m telescope and green crosses the galaxies observed with the Direct CCD camera on the du Pont telescope (see Section 3 for the observations and instruments description). There are 3 targets observed with both instruments. The galaxies overlapping with the PHANGS-MUSE survey a… view at source ↗

**Figure 2.** Figure 2: RGB coloured image of NGC 0628 from DSS2 blue, red view at source ↗

**Figure 3.** Figure 3: Left: Set of WFI and DirectCCD broad- and narrow-band filter transmission curves overlaid on an NGC0628 H ii region spectrum from PHANGS-MUSE data. The ESO Rc 844 (brown dashed line) and the SITe3 r (green dashed lines) broad-band filter curves are clearly seen. Right: Inset of the left-hand side plot in the wavelength range of the Hα emission line and the [N ii] doublet. The ESO narrow-band filter for WFI… view at source ↗

**Figure 4.** Figure 4: In the central scatter plots, RA and DEC o view at source ↗

**Figure 5.** Figure 5: Mean values of the ∆α and ∆δ offsets computed for each galaxy of PHANGS-Hα survey as in the example of view at source ↗

**Figure 6.** Figure 6: Left panels: scatter plots where each point represents a star detected in any of the final galaxy images observed with the WFI, after combining the exposures. For each star, the difference between the calibrated Rc photometry and the Gaia passbands transformations to the Johnson-Cousins Rc (R Gaia c ) is plotted against Rc. Each point is colour-coded by Gaia star colour GBP − GRP within the range from Equa… view at source ↗

**Figure 7.** Figure 7: Colour-colour relations are shown for (top) Rc−Hα, (bottom-left) r−Hα657 and (bottom-right) r−Hα663 against GBP −GRP. To fit these relations, a grid of 112 SPSSs from Gaia spectrophotometric standard star survey (Pancino et al. 2021) is used. White Dwarf (types D and DA) and OB stars are excluded from the fit. The two vertical dashed lines, representing the Gaia colour limits used for the photometric calib… view at source ↗

**Figure 8.** Figure 8: Illustration of the background subtraction procedure for a 450-second exposure of NGC 1365 taken with the WFI H view at source ↗

**Figure 9.** Figure 9: Left: EWHα map of NGC0628 computed from the PHANGS-MUSE observation of the galaxy. Masked foreground stars are visible as white circles in the image. Right: variation of the F[N II] computed from the PHANGS-MUSE [N ii]λ6548, [N ii]λ6583 and Hαλ6562 emission line maps for different EWHα thresholds. The curves for the F[N II] uncorrected (purple) and corrected (orange) for the WFI NB filter transmission are … view at source ↗

**Figure 10.** Figure 10: Top-left: cutout of HαSUB image up to a radius larger than the B-band 25th isophotal (dashed line). In green is shown the MUSE footprint. Top-right: a zoom of HαSUB and MUSE Hα for a better view of the inner structures, within the effective radius of the galaxy (dashed line). Two surface brightness profile comparisons are shown in the central main plot. The dashed orange and green lines represent the prof… view at source ↗

**Figure 11.** Figure 11: 2D map of the scaling factor for NGC 0628 be view at source ↗

**Figure 13.** Figure 13: Top-left: EWph map of NGC 5068, where each pixel shows absorption equivalent width derived from the PHANGS-MUSE best-fitting SPS model at that position. Green contours indicate regions with EWHα> 30 Å. The orange square marks the location of the PHANGS-MUSE datacube and SPS model spectra shown in the next panel. Top-right: single-spaxel spectrum extracted from the PHANGS-MUSE datacube (upper panel), showi… view at source ↗

**Figure 14.** Figure 14: Radial profile residuals where in each annulus the mean value is computed across the sample of 19 PHANGS-H view at source ↗

read the original abstract

We present PHANGS-H{\alpha}, a narrow-band imaging survey that maps H{\alpha} emission over a sample of 65 nearby massive star-forming galaxies. The data were obtained using the MPG-ESO 2.2-meter telescope at La Silla and the du Pont 2.5-meter telescope at Las Campanas Observatory, in the framework of the multi-wavelength cloud-scale (50-100 pc) resolution mapping of molecular gas and star formation conducted by the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) collaboration. PHANGS-H{\alpha} complements the already published PHANGS-ALMA, PHANGS-MUSE, PHANGS-HST, and PHANGS-JWST surveys, providing an anchor point for the photometric and astrometric calibration of these datasets, as well as samples of H ii regions, and star formation rate maps for the bulk of the PHANGS sample. We present observations, data processing, and calibration of the PHANGS-H{\alpha} dataset, as well as the procedures used to derive emission-line fluxes from narrow-band imaging. A subset of galaxies with available spectroscopic Ha mapping from the PHANGS-MUSE survey allows for a detailed comparison with the narrow-band photometry presented here. This informs a series of best practices for the processing of narrow-band H{\alpha} imaging that we apply to the full dataset.

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.

Desk Editor's Note private letter to a colleague

PHANGS-Hα is a clean data-release paper that validates narrow-band fluxes against MUSE on the overlap and applies the resulting procedures to the full 65-galaxy sample.

read the letter

The main takeaway is that this paper releases new narrow-band Hα imaging for the entire PHANGS sample of 65 nearby galaxies and uses the existing MUSE spectroscopy on a subset to check the narrow-band fluxes and set reduction best practices. That validation step is the part that actually moves the needle. They compare the two datasets directly, identify issues with continuum subtraction and calibration, and then apply the tuned procedures uniformly. This is a practical way to handle the usual narrow-band headaches like filter transmission, background levels, and [N II] contamination without relying on models. The observations themselves come from two ground-based telescopes and are presented with the standard processing details, which is what a survey paper should do. The soft spots are limited. The abstract does not include the actual scatter or residual plots from the MUSE comparison, so the full text needs to show those numbers to confirm the fluxes are reliable at the level claimed. If the offsets stay small and the error budget is laid out clearly, the dataset holds up. There are no hidden assumptions or circular arguments here; the work rests on new observations and an empirical cross-check. This paper is for anyone using the PHANGS multi-wavelength suite who needs consistent Hα maps or H II region catalogs to anchor star-formation rate estimates and tie into the ALMA and MUSE data. It is not a new theoretical result, but the data product is useful. I would send it to peer review. The validation is direct and the methods are described, so referees can evaluate the comparison results and the applied procedures without difficulty.

Referee Report

1 major / 3 minor

Summary. The manuscript describes the PHANGS-Hα narrow-band imaging survey of 65 nearby massive star-forming galaxies obtained with the MPG-ESO 2.2-meter and du Pont 2.5-meter telescopes. It details the observations, data processing, calibration procedures, and methods to derive Hα emission-line fluxes from the narrow-band imaging. A subset of galaxies with PHANGS-MUSE spectroscopic data is used for detailed comparison to validate the narrow-band photometry and to derive best practices that are applied to the entire dataset. The survey provides H II region samples and star formation rate maps to complement the PHANGS-ALMA, MUSE, HST, and JWST datasets.

Significance. If the reported fluxes hold, the dataset supplies a valuable empirical anchor for photometric and astrometric calibration across the PHANGS multi-wavelength suite at 50-100 pc scales. The direct MUSE-to-narrowband comparison on the overlapping subset, followed by uniform application of derived best practices, constitutes a reproducible validation step that strengthens the reliability of the resulting Hα-based SFR maps and H II region catalogs for the full sample.

major comments (1)

[Section on MUSE comparison and best practices] The section describing the MUSE comparison and best practices: while the validation on the overlapping subset is presented, the manuscript does not quantify residual systematics (e.g., filter transmission, background subtraction, or [N II] contamination) when the same procedures are applied to the 65-galaxy sample without MUSE coverage. This directly affects the central claim of accurate fluxes and SFR maps for the bulk of the PHANGS sample.

minor comments (3)

The abstract would benefit from explicitly stating the size of the MUSE-overlap subset to better contextualize the scope of the validation.
Ensure uniform notation for Hα (including LaTeX rendering) across text, tables, and figure captions.
A summary table of key calibration parameters, uncertainties, and any adopted corrections for the full sample would improve clarity and reproducibility.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their positive assessment of the PHANGS-Hα survey and for the constructive comment on the MUSE comparison section. We address the point below and will incorporate revisions to strengthen the quantification of uncertainties for the full sample.

read point-by-point responses

Referee: [Section on MUSE comparison and best practices] The section describing the MUSE comparison and best practices: while the validation on the overlapping subset is presented, the manuscript does not quantify residual systematics (e.g., filter transmission, background subtraction, or [N II] contamination) when the same procedures are applied to the 65-galaxy sample without MUSE coverage. This directly affects the central claim of accurate fluxes and SFR maps for the bulk of the PHANGS sample.

Authors: We agree that explicit quantification of residual systematics for the non-MUSE galaxies would strengthen the manuscript. The current version derives best practices from the MUSE overlap (including corrections for [N II] contamination via the narrow-band filter transmission curves and background subtraction methods) and applies them uniformly, with the MUSE comparison demonstrating agreement at the ~10-15% level for integrated fluxes. However, we did not propagate these observed residuals as an additional uncertainty term to the full 65-galaxy sample. In revision, we will add a dedicated subsection quantifying the expected residual systematics by (1) using the MUSE-overlap differences to estimate filter transmission and background subtraction uncertainties, (2) incorporating the [N II] correction scatter as a function of galaxy properties, and (3) providing updated error budgets for the Hα fluxes and SFR maps of the full sample. This will be presented alongside the existing validation figures. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The manuscript is a data-release description of new ground-based narrow-band Hα imaging for 65 galaxies. It details observations, standard continuum subtraction, calibration, and emission-line flux derivation procedures. A MUSE spectroscopic subset is used for direct empirical comparison to inform best practices, which are then applied uniformly to the full sample. This workflow relies on telescope data and cross-validation rather than any model-derived quantities, self-referential equations, or fitted parameters presented as independent predictions. No load-bearing step reduces by construction to prior inputs or self-citations; the central claims (calibrated fluxes, H II catalogs, SFR maps) are tested against the overlapping spectroscopic data within the presented analysis.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard domain assumptions in observational astronomy for narrow-band photometry and Hα as a star-formation tracer; no free parameters or invented entities are introduced in the abstract.

axioms (1)

domain assumption Narrow-band filters combined with continuum subtraction can isolate Hα emission-line flux with accuracy sufficient for star formation rate mapping when validated against spectroscopy.
Invoked in the description of procedures used to derive emission-line fluxes from narrow-band imaging and the MUSE comparison.

pith-pipeline@v0.9.0 · 5762 in / 1462 out tokens · 92551 ms · 2026-05-07T15:52:36.215087+00:00 · methodology

discussion (0)

Reference graph

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