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REVIEW 3 major objections 4 minor 116 references

Star-formation rates of two GRB host galaxies at z~2 and a [CII] deficit observed with ALMA

T0 review · 3 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read ALMA far-infrared photometry places two z~2 GRB hosts on the galaxy main sequence and reports the first [C II] 158 micron detection in a GRB host at z>2.

desk verdict Solid FIR-based SFR update for two z~2 GRB hosts; the headline [C II] deficit rests on a S/N~4 line and should be treated as tentative. read the letter →

arxiv 1908.01541 v1 pith:T6JT4BQD submitted 2019-08-05 astro-ph.GA

Tetsuya Hashimoto , Bunyo Hatsukade , Tomotsugu Goto , Seong Jin Kim , Kouji Ohta , Tohru Nagao , Albert K. H. Kong , Kouichiro Nakanishi
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Jirong Mao
This is my paper · ORCID
classification astro-ph.GA
keywords gamma-rayburstsGRBhostgalaxiesstarformationratefar-infraredcontinuum[CII]158micronmainsequenceredshift~2dust-obscured
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

This paper reports millimetre-wavelength observations of two galaxies that hosted long gamma-ray bursts at redshift ~2. Using rest-frame far-infrared emission, which traces dust-obscured star formation without being dimmed by dust, it derives star-formation rates of $49.85^{+72.33}_{-2.86}$ and $123.4^{+25.19}_{-21.78}\,M_\odot\,\mathrm{yr}^{-1}$ for the GRB 070521 and 080207 hosts. These values put the galaxies on the "main sequence" of normal star-forming galaxies at $z\sim2$, far below radio-based estimates of about $800\,M_\odot\,\mathrm{yr}^{-1}$. The paper also reports a marginal detection of the [C II] 158 micron cooling line from the 080207 host, giving a [C II]-to-FIR luminosity ratio of $7.5\times10^{-4}$, among the lowest known at $z\sim1$-$2$ for similar FIR luminosity. If this picture holds, high-redshift GRB hosts can be ordinary star-forming galaxies rather than extreme starbursts, and the [C II] deficit may become a new way to characterise them.

What carries the argument

The argument is carried by rest-frame far-infrared photometry that covers the peak of the dust emission, in combination with an energy-balance SED-fitting model that re-distributes energy absorbed by dust in the UV/optical into mid- and far-infrared dust templates. This yields dust-unbiased obscured star-formation rates. The second device is the [C II] 158 micron fine-structure line, the main coolant of neutral gas: after continuum subtraction, its velocity-integrated flux defines $L_{\rm [C\,II]}$, and the ratio $L_{\rm [C\,II]}/L_{\rm FIR}$, plotted against FIR luminosity and FIR surface density, locates the host on the known [C II] deficit trend. The paper also uses the observed ratio of [N II] 205 micron to [C II] to set a metallicity upper limit of about one solar metallicity for the host.

What would settle it

A longer ALMA observation of the GRB 080207 host reaching S/N > 8 in [C II] 158 micron would settle the matter: reproducing the line flux of $4.4\,\mathrm{Jy\,km\,s^{-1}}$ at the same velocity offset would confirm the deficit, while a non-detection or a much weaker line would refute it.

Watch

Extended reading notes

Core claim

The central claim is that rest-frame far-infrared continuum detections of the GRB 070521 and 080207 host galaxies provide reliable obscured star-formation rates: $49.85^{+72.33}_{-2.86}$ and $123.4^{+25.19}_{-21.78}\,M_\odot\,\mathrm{yr}^{-1}$. These SED-based rates agree with optical estimates, place both systems on the mass--SFR main sequence at $z\sim2$, and are far below the radio-derived rates of about 817 and 846 $M_\odot\,\mathrm{yr}^{-1}$, which the paper argues are inflated by long-lived radio afterglows or by the radio SFR calibration. In addition, a marginal [C II] 158 micron line detection (S/N~4) in the 080207 host, the first for a GRB host at $z>2$, yields $L_{\rm [C\,II]}/L_{\rm FIR}=7.5\times10^{-4}$. That ratio is one of the smallest among galaxies at $z\sim1$-$2$ with the same FIR luminosity, so the host shows a [C II] deficit; the paper identifies metallicity, a top-heavy IMF, and high gas density as possible drivers.

Load-bearing premise

The load-bearing premise is that the marginal [C II] 158 micron detection in the GRB 080207 host is real; if the S/N~4 line is dominated by noise or by continuum-subtraction systematics, the claimed [C II] deficit collapses.

Editorial extensions

If this is right

  • The host galaxies of GRB 070521 and 080207 are consistent with the main sequence of star-forming galaxies at $z\sim2$, so GRB hosts at this redshift do not have to be extreme starbursts.
  • Radio-based star-formation rates for these hosts are overestimated by factors of about 7 to 16, meaning afterglow contamination must be accounted for in GRB host studies that rely on radio continuum.
  • Rest-frame far-infrared observations should become a standard tool for measuring star-formation rates of GRB hosts at $z\sim1$-$2$, because they avoid dust extinction and afterglow contamination.
  • The [C II] deficit, quantified by $L_{\rm [C\,II]}/L_{\rm FIR}=7.5\times10^{-4}$, is a candidate new dust-extinction-free diagnostic of GRB host environments at $z\sim1$-$2$.

Reading between the lines

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

  • If these two hosts are representative of the $z\sim2$ GRB population, GRB event rates may trace ordinary main-sequence star-forming galaxies, which would strengthen the use of long GRBs as tracers of cosmic star-formation history.
  • Because deep ALMA observations favor the detection of faint [C II] emitters, the low $L_{\rm [C\,II]}/L_{\rm FIR}$ ratio found here may turn out to be common among $z\sim2$ galaxies; a complete survey of [C II] in main-sequence galaxies at the same depth could show whether the "deficit" is specific to GRB hosts.
  • The relative roles of metallicity, IMF, and gas density could be separated by measuring [N II] 205 micron and CO line ratios in a larger sample of GRB hosts; the paper provides only an upper limit for one host.
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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 / 4 minor

Summary. The paper reports ALMA band 8/9 rest-frame far-infrared (FIR) continuum observations of two GRB host galaxies at z~2, GRB 070521 and GRB 080207, and a marginal detection of [C ii] 158 μm emission from the latter. The FIR detections are used with the public MAGPHYS high-z SED-fitting code to derive star-formation rates of 49.85(+72.33,-2.86) and 123.4(+25.19,-21.78) M_sun/yr, respectively, which place both hosts on the z~2 main sequence and well below earlier radio-derived SFRs. The paper further reports L[CII]/LFIR = 7.5e-4 for GRB 080207, interprets this as one of the smallest values at z~1-2 and as a possible '[C ii] deficit' characteristic of GRB hosts, and argues that the previous radio SFRs are overestimated by afterglow contamination. The two main scientific claims are therefore (1) that FIR-based SFRs revise these hosts from extreme starbursts to normal star-forming galaxies, and (2) that the first z>2 GRB-host [C ii] detection reveals a strong [C ii] deficit.

Significance. If the FIR-based SFRs hold, the paper makes a useful and timely contribution: it demonstrates that ALMA FIR photometry can correct radio-based SFR estimates that may be biased by afterglow contamination, and it strengthens the view that high-z GRB hosts are not necessarily extreme starbursts. The continuum detections are high signal-to-noise (S/N ~7-19), the SED fitting uses a standard public code, and the authors include several appropriate caveats, including a discussion of observational bias toward low L[CII]/LFIR in deep ALMA observations. The [C ii] deficit claim is novel and potentially important, but it rests on the weakest measurement in the paper, a S/N~4 line detection. The SFR results are largely independent of the [C ii] claim and should survive even if the line is questioned; the deficit interpretation, however, is not on the same footing without a robustness analysis.

major comments (3)
  1. [Section 3, Table 2, Section 5.3] The entire [C ii] deficit claim rests on a single marginal line detection: S/N ~4, velocity-integrated flux 4.4 ± 1.2 Jy km/s, integrated over ±125 km/s after continuum subtraction and at a velocity offset of 155 km/s from the optical redshift (Table 2, Fig. 2). The paper itself calls the detection 'marginal' in Section 3, yet Section 5.3 and the Conclusions treat the resulting L[CII]/LFIR = 7.5e-4 as one of the smallest values at z~1-2. Because this is the paper's most novel claim, I request a quantitative robustness analysis: noise statistics of the continuum-subtracted cube, significance as a function of the chosen integration window, checks for a posteriori selection effects, and a bootstrap or jackknife estimate of the line flux. If the line cannot be established against plausible correlated-noise or continuum-subtraction systematics, the 'first detection' and 'deficit' claims should be explicitly downgraded to tentative. The quoted L[CII]/LFIR ratio also needs a propagated uncertainty.
  2. [Section 5.1.2 vs Abstract/Conclusions] The abstract and Conclusions state that the radio fluxes of both hosts are contaminated by long-lived afterglows, but Section 5.1.2 concludes for GRB 080207 that the radio excess is probably due to an overestimated radio SFR conversion factor, 'rather than the afterglow/AGN contamination.' These statements are contradictory. Because the paper's central message includes the origin of the radio discrepancy, the authors should harmonize the text and state explicitly which host(s) support the afterglow-contamination scenario.
  3. [Section 4, Table 5] For GRB 070521, the SED fit is anchored by a single rest-frame FIR photometric point, and the authors acknowledge in Section 4 that the MAGPHYS dust parameters are likely more uncertain than quoted. The derived SFR 49.85(+72.33,-2.86) M_sun/yr and its placement on the main sequence in Section 5.2 inherit this limitation. The paper should either quantify how the SFR changes under alternative dust-temperature or emissivity assumptions, or explicitly label the 070521 SFR as less secure than the formal MAGPHYS error bars, rather than presenting it in the abstract as a 'reliable' FIR-based SFR.
minor comments (4)
  1. [Sections 5.1.1 and 5.1.2] The FIR flux values are swapped: the GRB 070521 continuum flux is 3.58 ± 0.45 mJy and the GRB 080207 band 9 flux is 11.9 ± 1.7 mJy (Table 2). The sentences citing 11.9 mJy in Section 5.1.1 and 3.58 mJy in Section 5.1.2 should be reversed; the conclusion that afterglow contamination is negligible is unchanged, but the text is internally inconsistent.
  2. [Section 5.3.1, Table 5] The ratio L[CII]/LFIR = 7.5e-4 is quoted without an uncertainty; it should be computed by propagating the errors on L[CII] and LFIR.
  3. [Section 5.3.1] The phrase 'one of the smallest values' should be supported by a quantitative rank or percentile among the comparison sample shown in Fig. 5, rather than left as a visual impression.
  4. [Abstract and Section 5.3.2] There are minor typographical issues: 'an useful' in the abstract should be 'a useful', and 'the the GRB 980425 host' appears in Section 5.3.2.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the SFRs and the [C ii]/FIR ratio are measured outputs fitted to new ALMA photometry and compared with external relations and samples, not re-statements of the paper's own inputs.

full rationale

The paper's central results are measurement-driven rather than definitional. The SFRs (49.85 and 123.4 M_sun/yr) are outputs of MAGPHYS fitted to multi-wavelength photometry that includes new ALMA rest-frame FIR continuum detections; MAGPHYS is an external public code with published assumptions (Bruzual & Charlot 2003 stellar models, Charlot & Fall 2000 attenuation, Chabrier 2003 IMF), and the FIR points are independent observational inputs, not constructed from the claimed SFRs or from the authors' prior conclusions. The main-sequence placement is a comparison against the external Whitaker et al. (2014) relation, so it is not tautological. The claimed L[CII]/LFIR = 7.5e-4 combines a measured [C ii] line flux with an LFIR obtained from the MAGPHYS fit and an external Calzetti et al. (2000) conversion; no equation defines this ratio as its own input. The '[C ii] deficit' label is an application of an established literature phenomenon to a new galaxy, and the authors explicitly discuss a possible ALMA observational bias in Section 5.3.4, which weakens the claim but is not circular. Self-citations (e.g., Hashimoto et al. 2018) are contextual and not load-bearing; the CO data from Hatsukade et al. (2019) are independent observational constraints used only for a secondary gas-density discussion. The marginal S/N~4 [C ii] detection and the apparent swapping of continuum flux values between Sections 5.1.1 and 5.1.2 (11.9 versus 3.58 mJy) are genuine data-quality and presentation concerns, but they do not make the derivation equivalent to its inputs. No circular step or self-citation chain forces any central result.

Assumptions & free parameters 1 free parameters · 6 assumptions · 0 invented entities

The central claims rest on standard modeling assumptions rather than invented entities. The free parameters are those of the public MAGPHYS SED code, and the axioms are external calibration and modeling choices commonly used in galaxy SED fitting. The derived SFRs and deficit ratio inherit these assumptions.

free parameters (1)
  • MAGPHYS SED-fitting parameters = posterior distributions, not reported individually
    The SFRs and FIR luminosities are derived by fitting this public code's adjustable parameters (SFH timescale, age, burst amplitude, stellar metallicity, dust optical depth, ISM fraction, dust emission component fractions) to the observed photometry in Section 4. They count as fitted to the same data used for the central claim.
assumptions (6)
  • domain assumption The MAGPHYS high-z model correctly describes the hosts' UV-to-FIR emission.
    Central SFRs and LFIR are outputs of this model (Section 4). The model has no AGN component; if an AGN heats dust, the derived values would be biased. The authors note possible AGN hints for both hosts in Sections 5.1.1 and 5.3.1.
  • domain assumption The observed FIR continuum is dominated by star-formation-heated dust, with negligible afterglow or AGN contamination at ALMA wavelengths.
    Section 5.1 extrapolates radio afterglow flux to 600 GHz using typical spectral slopes to argue contamination is negligible. For GRB 070521 an AGN radio excess is acknowledged as possible, and for 080207 an AGN contribution is discussed in Section 5.3.1.
  • domain assumption The radio afterglow spectral slopes of Sari et al. (1998) are applicable for extrapolating 5 GHz flux to 600 GHz.
    Used in Sections 5.1.1 and 5.1.2 to show afterglow contamination is negligible. If the true spectral slope lies outside the assumed range, the extrapolation could be wrong, although the margin of safety is large (microJy versus mJy).
  • domain assumption The conversion log(LTIR/LFIR)=0.24 (Calzetti et al. 2000) applies to these galaxies.
    Applied in Section 4 and Table 5 to compute LFIR and the [C II]/FIR ratio. The deficit claim depends on this external conversion.
  • domain assumption The Chabrier (2003) IMF is appropriate for the SFR and stellar-mass calibrations.
    Stated in Section 1. A top-heavy IMF, suggested as a possible cause of the [C II] deficit in Section 5.3.2, would change the SFR calibration.
  • domain assumption The comparison samples in Figures 5-7 are representative and consistently measured.
    The deficit claim compares one host to literature galaxies with heterogeneous SFR and luminosity determinations. The authors discuss a possible ALMA selection bias in Section 5.3.4 but do not quantify it.

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Cite this review

Pith. "Pith review of Star-formation rates of two GRB host galaxies at z~2 and a [CII] deficit observed with ALMA." pith.science (2026). https://pith.science/paper/T6JT4BQD

@misc{pith2026190801541,
  author       = {Pith},
  title        = {Pith review of: Star-formation rates of two GRB host galaxies at z~2 and a [CII] deficit observed with ALMA},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/T6JT4BQD}},
  note         = {Machine review of arXiv:1908.01541}
}
abstract

Event rate of long Gamma-Ray Bursts (GRBs) is expected to be an useful tracer of the cosmic star-formation history. For this purpose, it is necessary to understand what kind of star formations/galaxies are traced by GRBs. Here we report rest-frame far-infrared (FIR) continuum detections of GRB 070521 and 080207 host galaxies at $z\sim2$ with ALMA band 8 and 9. The FIR photometries provide the reliable star-formation rates (SFRs), because FIR emission is free from dust extinction and possible radio contamination from long-lived afterglows of GRBs. The spectral energy distribution fittings indicate 49.85$^{+72.33}_{-2.86}$ and 123.4$^{+25.19}_{-21.78}$ $M_{\odot}$ yr$^{-1}$ for the 070521 and 080207 hosts, respectively. The derived SFRs place them on the \lq \lq main sequence\rq \rq\ of normal star-forming galaxies at $z\sim2$. The derived SFRs are significantly lower than that of radio observations. It is inferred that the observed radio fluxes in a previous study are contaminated by the afterglows. ALMA marginally detected [C~{\sc ii}]\,158\,$\mu$m emission line from the GRB 080207 host galaxy with S/N $\sim$ 4. This is the first detection of [C~{\sc ii}]\,158\,$\mu$m of a GRB host at $z>2$, and the second detection among known GRBs. The luminosity ratio of [C~{\sc~ii}]\,158$\mu$m to FIR is 7.5$\times 10^{-4}$, which is one of the smallest values among galaxies at $z\sim 1-2$ with the same FIR luminosity. The \lq \lq [C~{\sc ii}] deficit\rq \rq\ could be a new physical property to characterise GRB hosts at $z\sim1-2$. Possible parameters controlling the deficit include the metallicity, initial mass function, and gas density.

Figures

Figures reproduced from arXiv: 1908.01541 by the authors.

Figure 1
Figure 1. Rest-frame FIR continuum images obtained with (left) ALMA band 9 for the GRB 070521 host, (middle) band 9 for the GRB 080207 host, and (right) band 8 for the GRB 080207 host. Beam sizes are indicated by ellipses. Colour ranges are between 1 σ noise levels and peak flux densities. (Calzetti et al. 2000). Here LFIR is defined as a luminosity in￾tegrated between rest-frame 40 and 120 µm. We used the de￾convolved physic… view at source ↗
Figure 2
Figure 2. (Top) [C ii] 158 µm spectrum with a spectral resolution of 50 km s−1 at the position of the GRB 080207 host galaxy. The velocity axis is relative to z = 2.0858 measured by [O iii]λ5007 and Hα (Kruhler et al. ¨ 2012). The continuum emission is subtracted from the spectrum. Noise levels, ±1σ, are shown by dashed lines. Red solid line is the best-fit Gaussian function with a central position at 155 km s−1 . (Bottom) [C… view at source ↗
Figure 3
Figure 3. Spectral energy distributions of the GRB 070521 (left) and 080207 (right) host galaxies (black dots). ALMA photometries measured in this work are marked by red stars. Photometies at wavelengths longer than ∼500µm were excluded from the SED fitting analysis to avoid the possible contaminated flux from the long-lived afterglows. Photometries used for the SED fitting analysis are marked by blue circles. The best fit re… view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: Stellar mass as a function of SFR. Red dots high￾lighted by red stars are GRB 070521 and 080207 hosts (this work). Other GRB host galaxies are compiled from GHostS project (http://www.grbhosts.org/) and displayed by coloured dots. Short GRB host galaxies with T90 < 2.0…
Figure 6
Figure 6. Figure 6: L[CII]/LFIR as a function of LFIR surface density, ΣFIR=LFIR/πr 2 FIR. GRB 080207 host (this work) is shown by a red star. A blue star indicates a local GRB 980425 host galaxy, where we used LFIR of 4.83×108 L and size of 2.0 kpc (Micha lowski et al. 2014, 2016) to est…
Figure 7
Figure 7. Figure 7: L[CII]/LFIR as a function of LCO(1−0)/LFIR. GRB 080207 host (this work) is shown by a red star. The CO(1-0) line lu￾minosity of the GRB 080207 host is calculated from the ob￾served CO(1-0) emission-line flux (Hatsukade et al. 2019). A blue star indicates a local GRB 98…

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Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.