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arxiv: 2606.06585 · v1 · pith:JTY3BPBGnew · submitted 2026-06-04 · 🌌 astro-ph.GA

A Population of Red Galaxies with Very Strong Emission Lines at z > 5 Revealed by the NIRCam Medium Bands: ''Classic'' LRDs, Dusty Star-Forming Galaxies, and a Missing Population of LRDs

Sunna Withers , Adam Muzzin , Swara Ravindranath , Chris J. Willott , Nicholas S. Martis , Roberta Tripodi , Yoshihisa Asada , Maru\v{s}a Brada\v{c}
show 11 more authors
Maya Merchant Lamiya Mowla Ga\"el Noirot Ghassan T. E. Sarrouh Marcin Sawicki Jacqueline Antwi-Danso Anishya Harshan Naadiyah Jagga Danilo Marchesini Katherine Myers Visal Sok
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Pith reviewed 2026-06-28 00:21 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords little red dotsred emission line galaxieshigh-redshift galaxiesNIRCam medium bandsdusty star-forming galaxiesemission line galaxiesz greater than 5
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The pith

Medium-band NIRCam imaging finds compact red galaxies with strong emission lines at z>5 that classic LRD selections miss.

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

The paper identifies emission-line galaxies at redshifts 4.9 to 8.9 using medium-band data and finds a correlation where bluer continua pair with stronger lines. Outliers called Red Emission line Galaxies show red colors alongside very strong H-alpha and [OIII]+H-beta lines. These split into classic Little Red Dots, extended objects matching dusty star-forming galaxies, and compact unresolved sources that fail standard LRD color cuts because of faint continua, line contamination, and flatter UV-to-optical slopes. The authors conclude the compact sources are LRDs overlooked by existing criteria, indicating medium bands recover a fuller population.

Core claim

A sample of 26 Red Emission line Galaxies at 4.9 less than or equal to z less than or equal to 8.9 splits into three groups: classic LRDs that pass common literature color selections, extended REGs resolved in F444W and consistent with dusty star-forming galaxies, and compact REGs that remain unresolved in F444W yet fail LRD criteria due to faint continua, strong [OIII]+H-beta contamination, and UV/optical colors flatter than typical LRDs. The compact REGs are therefore interpreted as LRDs missed by standard selections.

What carries the argument

Red Emission line Galaxies (REGs), selected for red continuum color combined with high-equivalent-width H-alpha and [OIII]+H-beta lines, then subdivided by F444W spatial resolution and adherence to published LRD color criteria.

If this is right

  • Standard color-based LRD samples at z greater than 5 are incomplete.
  • Medium-band imaging recovers additional high-equivalent-width emission-line sources at these redshifts.
  • The compact REGs extend the known LRD population rather than representing a new class.
  • Existing high-redshift surveys may underestimate the space density of these red compact objects.

Where Pith is reading between the lines

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

  • If the compact REGs belong to the LRD class, current number counts of LRDs at z greater than 5 are lower limits.
  • Incorporating medium-band filters into future wide-field surveys could increase completeness for red compact sources.
  • The observed color-line strength correlation may link dust content directly to the strength of recent star formation in these galaxies.

Load-bearing premise

The compact REGs share the same physical nature as classic LRDs despite their fainter continua and flatter colors.

What would settle it

Spectroscopy showing that the compact REGs have markedly lower dust attenuation or different line ratios than classic LRDs would indicate they form a separate population.

Figures

Figures reproduced from arXiv: 2606.06585 by Adam Muzzin, Anishya Harshan, Chris J. Willott, Danilo Marchesini, Ga\"el Noirot, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Katherine Myers, Lamiya Mowla, Marcin Sawicki, Maru\v{s}a Brada\v{c}, Maya Merchant, Naadiyah Jagga, Nicholas S. Martis, Roberta Tripodi, Sunna Withers, Swara Ravindranath, Visal Sok, Yoshihisa Asada.

Figure 1
Figure 1. Figure 1: Color-color diagrams for galaxies with the Hα or [OIII] + Hβ emission lines in one of the F410M (top left), F430M (top right), F460M (bottom left), and F480M (bottom right) bands, with the sample filtered to galaxies at the correct redshift (see also [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: All four panels in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: EW(Hα) (left) and EW([OIII] + Hβ) (right) vs. photometric redshift for our samples. REGs which ony heave measurements of the [OIII] + Hβ emission lines are outlined with a grey outline. The sample of REGs have a wide range of EWs, and include both some of the lowest and highest EW objects in the line- and photo-z-selected samples. in the CANUCS data release (outlined in [PITH_FULL_IMAGE:figures/full_fig_p… view at source ↗
Figure 4
Figure 4. Figure 4: F150W − F444W vs. F444W magnitude diagram for our samples. We also show the F150W − F444W ERO color cuts from C. C. Williams et al. 2024 (solid line), R. Gottumukkala et al. 2024 (dahsed line), and L. Barrufet et al. 2025b (dash-dot line). Roughly half the REGs qualify as EROs based on at least one of these criteria, and the REG LRDs have similar colors and magnitudes to the full sample of LRDs in CANUCS. … view at source ↗
Figure 5
Figure 5. Figure 5: AV (left), EW(Hα) (middle) and EW([OIII] + Hβ) (right) vs. Reff measured using GALFIT in F444W of the REGs and LRDs in CANUCS (defined in §3.3). Reff is reported in arcseconds, with the vertical dashed line showing the FWHM of the F444W PSF. Nine of the REGs are resolved in F444W with effective radii larger than the F444W PSF, while remaining REGs are unresolved and have Reff consistent with zero within un… view at source ↗
Figure 6
Figure 6. Figure 6: Three examples of very Red Emission line Galaxies with the EAZY-py SED fits, photometry, and cutouts. This includes examples of all three types of REGs (§5): compact, LRD, and extended REGs are shown in the top, middle and bottom panels, respectively [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Six cutouts for each type of REG, including REG LRDs (top row) extended REGs (middle row) and compact REGs (bottom row). The cutouts are created using the same filters used to create the color-color diagrams in Figures 1 and 2, F150W (blue), the continuum band (green), and the band containing either the Hα or [OIII] + Hβ emission lines (red, summarized in [PITH_FULL_IMAGE:figures/full_fig_p014_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: The physical properties of our samples, measured from BAGPIPES (excluding objects classified as LRDs). The physical properties of the extended REGs are consistent with DSFGs: high AV (top left), high stellar masses (top right), high SFR (bottom right), and young mass weighted ages (bottom right). The compact REGs have properties consistent with DSFGs, including high AV . However, they have stellar masses r… view at source ↗
Figure 9
Figure 9. Figure 9: A UV J diagram for our samples, including the quiescent and star forming regions from J. Antwi-Danso et al. 2023, and the DSFG region from L. R. Spitler et al. 2014. All the REGs are classified as star-forming galaxies, but only seven are classified as DSFGs. Additionally, the compact REGs and LRDs have similar UV J colors [PITH_FULL_IMAGE:figures/full_fig_p016_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: NIRSpec prism spectrum of one of the compact REGs, CANUCS-1207412. The inset shows the double com￾ponent Gaussian fit to the Hα emission line, including the broad and narrow line components. This fit shows evidence of a broad-line component in Hα, indicating the presence of an AGN in CANUCS-1207412. The spectrum bluewards of λobs ∼ 2µm falls off the detector edge. 5.3. Compact REGs as DSFGs In the followi… view at source ↗
Figure 11
Figure 11. Figure 11: Left: βtot vs. MV for the REGs, a sample of AGN with broad Hα emission lines selected from the DJA (purple circles), including AGN classified as LRDs based on R. E. Hviding et al. 2025, and two black hole stars from A. de Graaff et al. 2025a and R. P. Naidu et al. 2025 (purple diamond and cross). The REGs (particularly the compact REGs) are generally fainter and bluer than the sample of AGN. Middle and Ri… view at source ↗
Figure 12
Figure 12. Figure 12: EAZY-py SED fits and photometry for the nine compact REGs. The black curve shows the best-fit galaxy SED based on the R. L. Larson et al. (2023) templates with the Y. Asada et al. (2025) prescription for IGM/CGM attenuation. The turquoise curve shows the best-fit brown dwarf SED based on the Sonora brown dwarf templates (M. S. Marley et al. 2021), which include SEDs for extremely cold brown dwarfs (Teff ≥… view at source ↗
read the original abstract

The NIRCam medium-bands have proven to be efficient at identifying Emission Line Galaxies (ELGs) with high equivalent width (EW) H$\alpha$ and [OIII]+H$\beta$ emission lines. In this paper we exploit this efficiency to identify a sample of ELGs at $4.9 \lesssim z \lesssim 8.9$ using medium-band imaging from the CANUCS, Technicolor, and JUMPS surveys. We find that the ELGs exhibit a strong correlation between continuum color and emission line strength, such that galaxies with bluer UV/optical continua have stronger H$\alpha$ and [OIII]+H$\beta$ emission lines. We identify 26 galaxies that are outliers from this relation, which we call the Red Emission line Galaxies (REGs), because of their red continuum color and strong emission lines. We classify the REGs into three categories: 1) ''classic'' Little Red Dots (LRDs) selected with common literature criteria, 2) extended REGs, resolved in F444W and consistent with being Dusty Star Forming Galaxies (DSFGs), and 3) compact REGs, unresolved in F444W but not classified as LRDs. The compact REGs fail common LRD selections for several reasons, including faint continuua, contamination from emission lines (very strong [OIII]+H$\beta$), and UV/optical colors that are flatter than those of LRDs. We conclude that the compact REGs are likely LRDs that ''classic'' selection criteria miss, and are therefore missing from existing samples. Our results suggest that medium-band selection can provide more complete samples of these objects.

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

2 major / 2 minor

Summary. The paper uses NIRCam medium-band imaging from the CANUCS, Technicolor, and JUMPS surveys to select Emission Line Galaxies (ELGs) at 4.9 ≲ z ≲ 8.9. It reports a correlation between continuum color and emission-line strength, identifies 26 outliers termed Red Emission line Galaxies (REGs), and classifies them into three groups: classic Little Red Dots (LRDs) meeting literature criteria, extended REGs consistent with Dusty Star-Forming Galaxies (DSFGs), and compact REGs that are unresolved in F444W but fail standard LRD selections owing to faint continua, strong [OIII]+Hβ contamination, and flatter UV/optical colors. The central claim is that the compact REGs are physically the same population as classic LRDs and are therefore missing from existing samples; medium-band selection is argued to yield more complete LRD samples.

Significance. If the compact REGs can be shown to share the same intrinsic (line-decontaminated) continuum slopes, dust attenuation, and line ratios as the classic LRD subsample, the result would be significant for demonstrating incompleteness in broadband LRD selections at z > 5 and for establishing medium-band photometry as a more complete selection tool. The reported color–line-strength correlation itself is a useful observational constraint on high-redshift ELG populations.

major comments (2)
  1. [classification of REGs / abstract] The conclusion that compact REGs are missed LRDs (abstract and classification section) rests on unresolved F444W morphology plus red color, yet the manuscript notes that these objects have flatter UV/optical colors than classic LRDs and fail LRD cuts partly because of that flatness and line contamination. No quantitative test is presented (e.g., histograms or Kolmogorov–Smirnov statistics) demonstrating that the line-corrected continuum slopes, A_V values, or [OIII]/Hα ratios of the compact REGs lie inside the distribution of the classic LRD subsample.
  2. [results on the color–line correlation] The sample of 26 REGs is defined as outliers from the reported continuum-color versus line-strength relation, but the text provides neither the functional form of the fitted relation, the outlier threshold (e.g., >3σ or >5σ), nor the uncertainties on the photometric colors and EWs used to identify the outliers.
minor comments (2)
  1. [sample selection] The abstract states the redshift range as 4.9 ≲ z ≲ 8.9; the corresponding section should explicitly list the photometric redshift or spectroscopic redshift quality cuts applied to arrive at this interval.
  2. [figures and methods] Figure captions and text should clarify whether the reported continuum colors are observed-frame or rest-frame and whether any line decontamination has been applied before the color measurement.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments, which have helped us clarify the presentation of our results. We address each major comment below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [classification of REGs / abstract] The conclusion that compact REGs are missed LRDs (abstract and classification section) rests on unresolved F444W morphology plus red color, yet the manuscript notes that these objects have flatter UV/optical colors than classic LRDs and fail LRD cuts partly because of that flatness and line contamination. No quantitative test is presented (e.g., histograms or Kolmogorov–Smirnov statistics) demonstrating that the line-corrected continuum slopes, A_V values, or [OIII]/Hα ratios of the compact REGs lie inside the distribution of the classic LRD subsample.

    Authors: We agree that a quantitative comparison of the line-decontaminated continuum slopes, A_V, and line ratios would strengthen the claim that the compact REGs belong to the same population. While the current analysis emphasizes the shared compact morphology, red optical colors, and strong lines as the primary indicators, we will add histograms and a Kolmogorov-Smirnov test comparing the key decontaminated properties between the compact REGs and classic LRDs in the revised manuscript. revision: yes

  2. Referee: [results on the color–line correlation] The sample of 26 REGs is defined as outliers from the reported continuum-color versus line-strength relation, but the text provides neither the functional form of the fitted relation, the outlier threshold (e.g., >3σ or >5σ), nor the uncertainties on the photometric colors and EWs used to identify the outliers.

    Authors: We acknowledge that the details of the outlier identification were insufficiently specified. In the revised manuscript we will explicitly state the functional form of the fitted continuum-color versus line-strength relation, the outlier threshold adopted (objects lying more than 3σ from the relation), and the photometric uncertainties on colors and equivalent widths used to define the 26 REGs. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational classification from independent photometric data

full rationale

The paper performs an observational selection of ELGs from CANUCS/Technicolor/JUMPS medium-band imaging, identifies REG outliers from an empirical color-EW correlation, and classifies them by F444W morphology and color cuts drawn from external literature criteria for LRDs. No equations, fitted parameters, or self-citations are used to derive the central claim; the conclusion that compact REGs are missed LRDs is an interpretive statement resting on direct photometric properties rather than any reduction to prior inputs by construction. This matches the default expectation for non-circular observational studies.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The paper rests on standard domain assumptions for photometric redshift and line identification in high-z galaxy surveys; no free parameters or invented entities are introduced in the abstract.

axioms (2)
  • domain assumption Emission line strengths and continuum colors can be reliably measured from NIRCam medium-band photometry at z>5
    Used to define the color-line strength correlation and identify outliers
  • domain assumption Unresolved sources in F444W with red colors and strong lines share the same nature as classic LRDs
    Central to classifying compact REGs as missed LRDs

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discussion (0)

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