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FAST H I 21 cm study of blueberry galaxies

T0 review · 3 major / 3 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read Blueberry galaxies appear nearly devoid of atomic hydrogen: FAST detects H I in only 2 of 28 targets, and the remaining upper limits imply depletion times around 0.5 Gyr.

desk verdict First real H I census of blueberries finds a low detection rate, but the size of the gas-poor offset rests on an unvalidated 50 km/s line-width assumption. read the letter →

arxiv 2411.13527 v1 pith:GVE4BR67 submitted 2024-11-20 astro-ph.GA

Yogesh Chandola , Chao-Wei Tsai , D.J. Saikia , Guodong Li , Di Li , Yin-Zhe Ma This is my paper · ORCID
classification astro-ph.GA
keywords blueberrygalaxiesHI21cmlineatomicgasfractiondepletiontimeGreenPeasO32ionizationparameterFASTtelescopestarburstdwarf
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

Blueberry galaxies are tiny, intensely star-forming systems in the nearby universe ($z\lesssim0.05$), often used as local stand-ins for the galaxies that populated the early universe. This paper tries to establish that these galaxies carry surprisingly little atomic hydrogen, the fuel for future star formation. Using FAST's 21 cm observations of 28 blueberries, the authors detect H I in only two targets; for the other 26, the median $3\sigma$ upper limit on H I mass is about $2\times10^{8}\,M_\odot$. From these limits they derive a median upper limit on H I depletion time of about 0.5 Gyr, roughly an order of magnitude shorter than in local main-sequence galaxies, meaning these starbursts are burning through their atomic gas reservoirs very quickly. If true, this would show that the most extreme nearby star-forming dwarfs are gas-poor systems whose starbursts must either be short-lived or depend on external gas replenishment, with direct implications for how we interpret high-redshift analogs.

What carries the argument

The central object is the H I 21 cm line as a tracer of the cold atomic gas reservoir, observed with the Five-hundred-meter Aperture Spherical radio Telescope. The load-bearing step is the conversion of nondetection noise into a $3\sigma$ H I mass upper limit, Equation (6), which assumes a 50 km/s line width for every source; that limit, combined with stellar masses and SFRs from the parent sample, gives the gas fraction $f_{\rm HI}=M_{\rm HI}/M_\ast$ and depletion time $\tau_{\rm HI}=M_{\rm HI}/{\rm SFR}$ plotted against main-sequence relations. The O32 ratio, defined as O[III] $\lambda$5007 / O[II] $\lambda$3727, organizes the sample and connects the low detection rate to the high-O32 Green Pea population, where earlier work also found few H I detections.

What would settle it

A targeted interferometric H I survey of the 26 nondetections reaching $M_{\rm HI}<2\times10^{8}\,M_\odot$ would settle it: recovering emission in more than a few percent of targets, or showing that the assumed 50 km/s line width is too narrow by a factor of several, would overturn the conclusion that blueberries are systematically gas-poor.

Watch

Extended reading notes

Core claim

The central claim is that blueberry galaxies at $z\lesssim0.05$ have H I contents well below what main-sequence scaling relations predict for their stellar masses and star-formation rates. Only two of 28 targets (J1026+0426 and J1132+0809) show significant H I emission, and those detections are entangled with neighboring galaxies in FAST's 3-arcmin beam; if the H I is apportioned by stellar-mass ratio, the blueberries themselves hold roughly $5.4\times10^{7}\,M_\odot$ and $1.7\times10^{8}\,M_\odot$, respectively. For the 26 nondetections, the median $3\sigma$ upper limit on H I mass is $2.0\times10^{8}\,M_\odot$, the gas fraction $f_{\rm HI}=M_{\rm HI}/M_\ast$ lies below the $f_{\rm HI}$--$M_\ast$ and $f_{\rm HI}$--sSFR relations for main-sequence galaxies, and the median $3\sigma$ upper limit on H I depletion time $\tau_{\rm HI}=M_{\rm HI}/{\rm SFR}$ is 0.53 Gyr, about an order of magnitude shorter than typical local main-sequence values. The resulting H I detection rate is only 7.1%, and the paper interprets this as evidence that blueberries, like high-O32 Green Peas, exhaust their atomic gas on short timescales and are likely seen in a brief, gas-hungry starburst phase.

Load-bearing premise

The quantitative conclusions hinge on treating the $3\sigma$ upper limits, computed with an assumed 50 km/s line width, as accurate proxies for the true H I content of the nondetections, and on attributing the two detected profiles to the blueberries rather than to neighboring galaxies inside FAST's large beam.

Editorial extensions

If this is right

  • Blueberry starbursts cannot be sustained by their present atomic reservoirs for more than about 0.5 Gyr; either the star formation is short-lived or the gas must be accreted or recycled from the surroundings.
  • In these low-mass, high-sSFR systems atomic gas is not the dominant baryonic component, breaking the usual expectation that dwarf galaxies are H I-dominated.
  • The low detection rate at high O32 means that selecting galaxies by extreme ionization parameter efficiently picks out galaxies with little neutral gas, strengthening O32-based searches for Lyman-continuum leaker candidates.
  • The H I content must be mapped at higher angular resolution before the detected systems can be used to constrain where LyC photons escape, since the FAST beam blends the blueberries with neighbors.
  • Molecular gas follow-up is needed because the standard H I-to-H2 conversion for main-sequence galaxies may not apply in these low-metallicity, high-density starbursts.

Reading between the lines

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

  • Going beyond the paper, the same upper-limit method could be tested statistically: if the true H I line widths of nondetected dwarfs follow the roughly 20-30 km/s widths typical of dwarf galaxies, the 50 km/s assumption is conservative and the low gas fractions are robust; if they are broader, the offset from main-sequence relations shrinks.
  • The paper's logic implies that the fraction of O32 greater than or similar to 10 dwarfs with detectable H I should drop sharply with decreasing stellar mass; future wide-field H I surveys could map this boundary and predict which systems are most likely to leak Lyman-continuum radiation.
  • If these galaxies are really depleting their gas in about 0.5 Gyr, they may be caught in the final, gas-poor phase of a merger-driven starburst, connecting the short depletion times to the disturbed H I morphologies seen in interferometric images of individual Green Peas and blueberries.
  • A direct measurement of molecular gas in a handful of blueberries would test whether the atomic reservoir is small because it has already been converted into H2, which would make the low H I content a sign of rapid fuelling rather than of genuinely little gas.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 3 minor

Summary. This Letter reports FAST H I 21 cm observations of 28 blueberry galaxies, a class of low-redshift, compact, high-sSFR starbursts considered local analogs of high-redshift Lyα emitters. The authors detect H I toward two objects, J1026+0426 and J1132+0809, and derive 3σ upper limits for the remaining 26 galaxies. Using Equation (6), which assumes a 50 km/s line width for nondetections, they obtain a median 3σ upper limit on H I mass of about 2.0×10^8 M_sun, a median f_HI upper limit of 10.2, and a median τ_HI upper limit of 0.53 Gyr. They compare these values with the f_HI-sSFR and f_HI-M* relations for main-sequence galaxies and conclude that blueberries have low atomic gas fractions and depletion times roughly an order of magnitude below local main-sequence values, with a low detection rate of 2/28 (7.1%).

Significance. If the quantitative conclusions hold, this paper would strengthen the emerging picture that extremely compact, high-sSFR dwarf galaxies such as blueberries are gas-poor, depleting their atomic gas reservoirs on sub-Gyr timescales. The main strengths are the large sample of blueberries observed in H I, the use of the standard H I mass formula, explicit discussion of neighbor contamination, and comparison with external relations from Catinella et al. (2018) and Kanekar et al. (2021). The low detection rate itself is likely robust to many caveats. However, the quantitative offsets in f_HI and τ_HI rest on an assumed line width that is not supported by the detected profiles, and on uncertain attribution of the two detections; these need to be addressed before the central quantitative claims can be accepted.

major comments (3)
  1. [§3, Eq. (6) and Table 1] The upper limits on M_HI, and hence the median f_HI and τ_HI claims, assume a fixed line width of 50 km/s for all nondetections. This assumption is not supported by the two detected profiles, whose FWHMs are 148.8±4.4 and 124.4±7.3 km/s (Table 1 notes). Because the 3σ integrated-flux limit scales as sqrt(W/50), a realistic W≈150 km/s raises every upper limit by a factor of 1.73: the median M_HI upper limit becomes ~3.5×10^8 M_sun, the median log f_HI upper limit moves from ~1.00 to ~1.25, above the extrapolated main-sequence value of ~1.16 at log M*=7.3, and the median τ_HI upper limit rises from 0.53 to ~0.92 Gyr. The claimed order-of-magnitude deficit in τ_HI is therefore not robust to the line-width prior. Please justify the 50 km/s choice using measured widths from BBs, GPs, or low-mass BCDs, or present the upper limits as a function of assumed line width.
  2. [§3, Table 1 notes, Fig. 3] Both detections carry substantial attribution uncertainty. For J1026+0426, the quoted log M_HI=7.73 is obtained by assuming that the BB-to-neighbor H I mass ratio equals their stellar mass ratio, while the neighboring Sbc galaxy's optical velocity is closer to the detected V_HI than the BB's optical velocity is. For J1132+0809, the lower value log M_HI=8.24 assumes the 12″ companion is at the H I velocity, and the alternative with no companion at that redshift gives log M_HI=9.56 (Table 1 note d). Because only two detections are reported, both scenarios should be propagated through the f_HI and τ_HI comparisons in Fig. 3 and the summary, not only in table notes; otherwise the reader cannot determine how much of the 'gas-poor blueberries' conclusion depends on a specific assumption about the neighbors.
  3. [§3.1, Fig. 3(a)] The conclusion that BBs have lower f_HI than main-sequence relations relies on comparing the median 3σ upper limit (10.2) with the extrapolated expected value (14.6). A 3σ upper limit is not a measurement, and the difference of only ~0.16 dex is small; many individual upper limits in Table 1 are above the expected M_HI at their stellar mass, e.g., J0820+5431 has log M_HI<7.94 against an expected log M_HI≈7.76. The claim that BBs 'tend to have lower f_HI' needs a proper upper-limit treatment, such as a Kaplan-Meier or survival-analysis estimate of the median, or a binomial test of the fraction of limits below the expected relation, before it can be regarded as established.
minor comments (3)
  1. [§3.1] In the paragraph discussing f_HI for the detected sources, 'J1123+0809' should be 'J1132+0809'; J1123+2050 is a nondetection and the text is about the detected source with a neighboring blue galaxy.
  2. [§3.3] The statement that 'all 26 BBs have an O32 ratio greater than 8.3' would be clearer if it specified that this refers to the 26 sources with available O[II] fluxes; Table 1 lists two sources (J1136+3427 and J1323−0132) with no O32 value.
  3. [Eq. (6)] The line-width dependence in Equation (6) is presented as a fixed numerical factor with Δv; please state explicitly whether the 50 km/s width is intended as a boxcar, Gaussian FWHM, or other profile shape, since the conversion from per-channel noise to integrated-flux limit depends on this choice.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the H I mass and upper-limit calculations use standard formulae with an explicit line-width prior, comparisons rely on external galaxy relations, and the only self-citation is a comparison sample, not load-bearing.

full rationale

The paper's central claims are observational: a 2/28 detection rate, median 3-sigma H I mass upper limits, and gas fractions and depletion times derived from those limits. The H I mass formula (Eq. 4) is the standard relation. The nondetection upper limits (Eq. 6) adopt an explicit 50 km/s line-width assumption; this is an analysis prior, not a parameter fitted to the target result. Changing the assumed width scales the upper limits, but that is a robustness concern about the sensitivity estimate, not a circular reduction of the conclusion to its input. The comparisons to f_HI-sSFR and f_HI-M* relations use external benchmarks from Catinella et al. (2018) and Kanekar et al. (2021), and the depletion-time comparison to main-sequence galaxies uses Saintonge et al. (2016) and Catinella et al. (2018). The Chandola et al. (2024) self-citation appears as a comparison sample for BCDs and for the method of estimating stellar masses of neighbors; it does not supply the central 'low gas fraction' or 'short depletion time' result. The paper does not invoke any uniqueness theorem, smuggle in an ansatz by citation, or rename a known result. The two detections are deblended from neighboring galaxies using an explicit stellar-mass-ratio assumption, which is a stated model choice rather than a forced equivalence. Overall, the derivation chain is self-contained against external data, and no step reduces to its own input by construction. The single point of caution is the 50 km/s line-width prior for nondetections, but this is an assumption with stated sensitivity implications, not circularity.

Assumptions & free parameters 1 free parameters · 5 assumptions · 0 invented entities

The central claims rest on standard radio astronomy formulas plus two nontrivial assumptions about how to divide H I flux between blueberries and neighboring galaxies. The 50 km/s line width is a chosen analysis parameter that affects all nondetection upper limits. No new physical entities are introduced.

free parameters (1)
  • Assumed H I line width = 50 km/s
    Adopted in Equation (6) for all nondetections to convert per-channel 3 sigma noise into an H I mass upper limit. The mass limit scales as sqrt(W/50), so a different width changes the median f_HI and tau_HI claims.
assumptions (5)
  • domain assumption The 50 km/s line width approximates the true H I profiles of blueberries.
    Equation (6). If real line widths are broader, the nondetection upper limits, median gas fractions, and median depletion times are underestimated.
  • ad hoc to paper For J1026+0426, the H I mass ratio of the blueberry to its companion equals their stellar mass ratio.
    Table 1 note b. This assumption determines the reported detected H I mass for J1026+0426 and has no independent verification.
  • ad hoc to paper The photometric redshift of the companion to J1132+0809 is not at the H I velocity, so most of the detected H I belongs to the blueberry.
    Section 3. The paper also gives the alternative value assuming the companion is at the H I velocity, but the lower BB H I mass is used in the main figures.
  • domain assumption The FAST 3-arcmin beam cannot spatially separate the blueberry from nearby galaxies, so all line flux within the beam is attributed using the mass-ratio and redshift assumptions.
    Section 3. This is the reason the detected H I masses are model dependent.
  • standard math The standard H I mass formula and the ON-OFF calibration equations are valid.
    Equations (1) through (4). These are standard single-dish radio astronomy conversions.

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Cite this review

Pith. "Pith review of FAST H I 21 cm study of blueberry galaxies." pith.science (2026). https://pith.science/paper/GVE4BR67

@misc{pith2026241113527,
  author       = {Pith},
  title        = {Pith review of: FAST H I 21 cm study of blueberry galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GVE4BR67}},
  note         = {Machine review of arXiv:2411.13527}
}
abstract

Green Peas (GPs) and blueberry galaxies (BBs) are thought to be local analogs ($z<$0.1) of high redshift Ly$\alpha$ emitters. H I study of these can help us understand the star formation in the primordial Universe. In this Letter, we present the results of H I 21 cm study of 28 high specific star formation rate (sSFR $\gtrsim$10$^{-8}$ yr$^{-1}$) BBs at $z\lesssim$0.05 with the Five-hundred-meter Aperture Spherical radio Telescope. We report significant H I detection towards two BBs namely J1026+0426 and J1132+0809, and discuss possible H I contribution from neighboring galaxies. The median 3$\sigma$ upper limit of $\sim$2.0$\times$10$^{8}$ M$_{\odot}$ was obtained on H I mass for galaxies with nondetections. We find BBs tend to have lower H I-to-stellar mass ratio or gas fraction ($f_{\rm HI}$) than expected from $f_{\rm HI}$-sSFR and $f_{\rm HI}$-$M_{\ast}$ relations for main-sequence galaxies. The BBs also have a median 3$\sigma$ upper limit on H I gas depletion time scale ($\tau_{\rm HI}$) $\sim$0.5 Gyr, about 1 order of magnitude lower than $\tau_{\rm HI}$ for local main-sequence galaxies. We find a significantly low H I detection rate of 2/28 (7.1$^{+9.4}_{-4.6}$ \%) towards these galaxies, which is similar to previous H I studies of low redshift GPs of high ionization parameter indicator, O32 $\equiv$O[{\sc iii}]$\lambda$5007/O[{\sc ii}]$\lambda$3727 ratios $\gtrsim$10.

Figures

Figures reproduced from arXiv: 2411.13527 by the authors.

Figure 1
Figure 1. 21 cm emission spectra of blueberry galaxies with Hi detections. The X-axes show the velocity relative to opti￾cal systemic velocity (cz) at the heliocentric frame in km s−1 . The Y-axes show the flux density in mJy. Blue shades mark the 3σ noise levels. Red vertical dashed lines mark the zero relative velocity corresponding to the optical redshift of the blueberry galaxies. Green vertical dashed lines mark the Hi v… view at source ↗
Figure 2
Figure 2. Spectra of blueberry galaxies with Hi nondetections. The symbols mean the same as in [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. (a): fHI vs. M∗. BBs observed with the FAST are shown with blue-colored circles. Gray-colored circles represent GPs with Hi study by Kanekar et al. (2021). Filled and empty circles represent detections and nondetections, respectively. Median values of log fHI for respective median log M∗ values for main-sequence galaxies from Catinella et al. (2018) are shown with black connected dots. Similarly, gray connected erro… view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: Top panel:MHI vs. O32 ≡ O[iii]λ5007/O[ii]λ3727 ratio. Middle panel:fHI vs. O32 ≡ O[iii]λ5007/O[ii]λ3727 ratio. Bottom panel: τHI vs. O32 ≡ O[iii]λ5007/O[ii]λ3727 ratio. The symbols mean the same as in [PITH_FULL_IMAGE:figures/full_fig_p008_4.png]

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    Physics, Mechanics, and Astronomy, 62, 959506, doi: 10.1007/s11433-019-9383-y

    doi

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.