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REVIEW 3 major objections 4 minor 131 references

QUIJOTE scientific results - XX. Commissioning and First Results from the Thirty and Forty Gigahertz Instrument (TFGI)

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

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Pith's one-line read TFGI's two 31 GHz detectors already deliver about 8.3 microkelvin per degree polarization sensitivity, nearly matching WMAP with a third of the integration time, and the full array is forecast to reach 1 microkelvin per degree in 5.7 years.

desk verdict Solid commissioning paper with a credible sensitivity measurement; the 5.7-year full-array forecast for 41 GHz is not supported by the only measured FGI pixel and should be presented as conditional. read the letter →

arxiv 2608.08579 v1 pith:4DRTJITH submitted 2026-08-09 astro-ph.IM astro-ph.CO

M. Fernández-Torreiro , J. A. Rubiño-Martín , R. T. Génova-Santos , G. Pascual-Cisneros , A. Fasano , F. J. Casas , R. J. Hoyland , M. W. Peel
show 11 more authors
C. H. López-Caraballo U. Bose R. Rebolo K. Aryan R. B. Barreiro R. Cepeda-Arroita D. Herranz E. Martínez-González F. Poidevin R. Puddu P. Vielva
This is my paper · ORCID
classification astro-ph.IMastro-ph.CO
keywords CosmicmicrowavebackgroundradiationObservationalcosmologyDiffuseRadiocontinuumemissionMilkyWaydiskPolarimetryinstrumentcommissioningpolarizationsensitivity
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 the commissioning of TFGI, a 31/41 GHz polarimeter on the second QUIJOTE telescope, and argues that the instrument has already reached a polarization sensitivity of about 8.3 microkelvin per degree using only two 31 GHz detectors after 0.57 hours per square degree. That is comparable to WMAP's polarization noise in the same region, which used almost three times more integration time per area. Extrapolating from these two detectors to the planned 29-detector array, the paper forecasts that TFGI will reach its survey target of about 1 microkelvin per degree over 3600 square degrees in 5.7 years, enough to constrain the tensor-to-scalar ratio at the $r\le0.05$ level from the Northern sky. The claim matters because it says a comparatively small ground-based Northern-hemisphere instrument can deliver polarization maps competitive with space missions, provided the remaining detectors perform like the three analysed pixels.

What carries the argument

The load-bearing mechanism is the electronic phase-switch polarimeter. TFGI switches its polarization phase states at up to 160 kHz (cycling 16 states at 4 kHz), and forms Stokes $Q$ and $U$ from differences between phase states separated by $180^\circ$, so correlated $1/f$ noise and atmospheric signal cancel within each detector rather than between detectors with different bandpasses. The paper's quantitative engine is the half-mission difference map (HMDM): scans are split chronologically into two halves, the weighted difference is a noise map whose RMS in a $3^\circ$ radius aperture gives the sensitivity in $\mu\mathrm{K}\,\mathrm{deg}^{-1}$. This map-based sensitivity, together with the assumption that sensitivity scales as the inverse square root of detector number and time, produces the 5.7-year forecast.

What would settle it

After one year with the 10 TGI pixels now being installed, construct the half-mission difference maps of a $3^\circ$-radius aperture in the Galactic-plane field and measure the RMS: if the $Q/U$ sensitivity is not close to the projected $\sim 2.9\,\mu\mathrm{K}\,\mathrm{deg}^{-1}$, the detector-count scaling that underlies the 5.7-year forecast is wrong. The same maps will show whether the calibration diode has reduced polarization-angle scatter to the sub-degree level needed to keep the additional detectors from cancelling in $Q$ and $U$.

Watch

Extended reading notes

Core claim

The central discovery is that the TFGI polarization channel works as designed: half-mission difference maps of Galactic plane fields, made with two 31 GHz detectors (plus a 41 GHz check), give $\sim 8.3\,\mu\mathrm{K}\,\mathrm{deg}^{-1}$ in Stokes $Q/U$ at an effective depth of $0.57\,\mathrm{h}\,\mathrm{deg}^{-2}$. This is only about 20 percent worse than WMAP's 33 GHz polarization sensitivity in the same region, despite WMAP having almost three times the integration per unit area. The paper then scales this number linearly with detector count and observing time: 10 TGI pixels would need almost 9 years to reach $1\,\mu\mathrm{K}\,\mathrm{deg}^{-1}$, while the full 29-detector configuration (15 TGI plus 14 FGI) would need 5.7 years over three $1200\,\mathrm{deg}^2$ fields. Along the way it verifies the beam shapes, gain stability, polarization efficiency, intensity-to-polarization leakage below about 0.4 percent, and consistency of W44's intensity and polarization spectral energy distributions with previous data.

Load-bearing premise

The 5.7-year forecast assumes the remaining detectors will perform like the three good pixels analysed here, and that the new calibration diode will fix the unstable polarization angles that degraded three of the seven commissioned pixels.

Editorial extensions

If this is right

  • If the forecast is correct, TFGI's 31 GHz maps reach $\sim 1\,\mu\mathrm{K}\,\mathrm{deg}^{-1}$ over 3600 deg$^2$ after 5.7 years, enough to put an upper limit of $r \le 0.05$ from the Northern sky.
  • With the 10 TGI detectors now installed, reaching the same 31 GHz goal would take almost 9 years; the remaining detectors reduce this to 5.7 years, assuming equal performance per detector.
  • The instantaneous white-noise levels measured from skydips (314–376 $\mu\mathrm{K}\,\mathrm{s}^{1/2}$) match the design value of 350 $\mu\mathrm{K}\,\mathrm{s}^{1/2}$, so per-detector sensitivity is already at the level the forecast assumes.
  • The intensity-to-polarization leakage upper limits (below 0.19 percent for TGI pixels and below 0.36 percent for the FGI pixel) support the assumption that the deep polarization maps will not be dominated by leaked total intensity.

Reading between the lines

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

  • If the detector-scaling model is right, the 2026 19-detector configuration should reach about $2.9\,\mu\mathrm{K}\,\mathrm{deg}^{-1}$ on the 31 GHz TGI map after one year; measuring the HMDM noise in that configuration would test the forecast long before the full array is built.
  • Even with the target sensitivity reached, the reported 4–6 degree polarization-angle calibration uncertainty is far above the sub-degree accuracy future B-mode searches will need, so the calibration diode's angle-tracking performance, not raw sensitivity, is the real constraint on using these maps for cosmology.
  • The comparison with WMAP suggests that fast electronic phase-switching can let a small ground-based telescope compete with a space mission in polarization mapping; the same architecture could be tested at other Northern-hemisphere sites with comparable precipitable water vapour.
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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 the commissioning and first science verification of QUIJOTE-TFGI, a 31/41 GHz polarimeter on the second QUIJOTE telescope, using data from November 2021 to May 2022 with seven installed receivers (four TGI at 31 GHz, three FGI at 41 GHz). It characterizes pointing, beams, gain calibration via Tau A and Cas A, polarization efficiency and angle calibration, instantaneous white-noise levels, intensity-to-polarization leakage, and map-making performance on Cygnus and Galactic-plane fields (W43, W44, W47). The central quantitative result is the half-mission difference-map polarization sensitivity: about 8.3 microK deg^-1 from the two usable TGI pixels at an effective depth of 0.57 h deg^-2, already comparable to WMAP's polarized sensitivity in the same region. The paper then extrapolates this sensitivity to the full 29-detector array and claims that 1 microK deg^-1 over 3600 deg^2 at both 31 and 41 GHz can be reached after 5.7 effective years, enabling a target r <= 0.05.

Significance. If the measured sensitivity holds, this is a valuable result for ground-based CMB polarimetry: it demonstrates that a small Northern-hemisphere telescope with only two 31 GHz detectors can achieve polarization sensitivity comparable to space-based WMAP, and it validates the instrumental chain (phase-switching polarimetry, differential map-making, calibration strategy) with on-sky data. The paper is strong on the measurement side: the HMDM construction is clearly described, the comparison with WMAP and Planck is done on matched maps, the calibrations use external models (Tau A, Cas A), and the SED fits provide independent cross-checks. The main weakness is not the measurement but the forecasting step, which extrapolates from the two best 31 GHz pixels to 29 unmeasured detectors and, in particular, assumes that the 41 GHz channel will match TGI performance despite the only measured FGI pixel being substantially less sensitive.

major comments (3)
  1. [Section 5, Table 8, Eq. (11), Fig. 16] The 41 GHz forecast is not supported by the on-sky data. Pixel 63, the only FGI pixel retained in the analysis, gives sigma_Q = sigma_U = 16.4 microK deg^-1 with one detector at 0.57 h deg^-2, after correcting for its measured 73% polarization efficiency. Scaling this single detector to 14 identical FGI detectors gives (16.4^2 x 0.57)/14 = 10.9 years to reach 1 microK deg^-1, not 5.7 years. Even under a hypothetical 90% polarization efficiency the time would be about 7 years; matching the TGI claim requires that the unmeasured FGI detectors perform at the level of the two best TGI pixels rather than at the level of the only FGI pixel actually measured. The text's statement that 'the FGI map would take a bit longer' understates this by roughly a factor of two, and the abstract's claim of reaching 1 microK deg^-1 at both 31 and 41 GHz after 5.7 years is therefore not established by the commissioning data.
  2. [Section 2.1, Section 3.4, Section 5] The sensitivity estimate and the forecast rest on a post-hoc selection of pixels. Three of the seven installed pixels (TGI pixel 5, FGI 41, FGI 42) were excluded because of time-varying polarization angles and low on-sky polarization efficiency; the 8.3 microK deg^-1 figure uses the best two TGI pixels. The full-array forecast assumes that the calibration diode will repair exactly this failure mode, but no on-sky commissioning measurement demonstrates that convergence. The Conclusions state that the forecasts 'should be interpreted as conservative scenarios', which is difficult to sustain: the 5.7-year number assumes all 29 detectors behave like the best measured subset, and the diode correction is a planned hardware upgrade, not a measured property of the present data. The forecast should be presented as conditional on the diode and on unverified detector yield.
  3. [Section 4, Fig. 11, Appendix D] The W44 polarized SED indicates that pixel 63's polarized signal is lower than expected even after the Tau-A-derived polarization efficiency correction, which the paper attributes to time variations of the polarization angle over the longer W44 dataset. This is directly relevant to the forecast: the 16.4 microK deg^-1 noise value in Table 8 is a valid noise measurement, but if slow polarization-angle drifts suppress the polarized signal on survey timescales, the usable scientific sensitivity is worse than the raw HMDM noise implies. The forecast in Fig. 16 should either account for this signal-recovery loss or explicitly state the assumption that the diode eliminates it.
minor comments (4)
  1. [Section 2.3, Eq. (12)] The two lines defining h1 both use 'h1'; the second line should assign the odd-index scans to h2.
  2. [Section 3.4.2 and Section 6] The text refers to 'TGI pixel 25' as one of the unstable pixels, but Table 1 lists the unstable TGI pixel as pixel 5; the numbering should be made consistent.
  3. [Fig. 16 caption] The label '29 TGI pixels (equivalent to full-TGI configuration)' could mislead readers, since the full TFGI configuration is 15 TGI plus 14 FGI detectors; the curve is a hypothetical all-31-GHz array and should be labeled as such.
  4. [Section 5] The 5.7-year forecast assumes a 50% observing efficiency, whereas the commissioning campaign reports a 35% efficiency (Section 2.3). The paper notes that 50% may be optimistic, but the sensitivity of the headline number to this assumption should be stated explicitly in the main text.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the sensitivity measurement is a direct HMDM noise product, and the 5.7-year forecast is an explicitly stated radiometer-scaling extrapolation.

full rationale

The headline sensitivity in Table 8 is a direct noise product: Eq. 11 forms half-mission difference maps from the observed scans, and the quoted 8.3 uK deg^-1 is the RMS of those HMDMs in a 3-degree aperture. No model parameter fitted to the target claim enters that calculation. Gain calibration (Sect. 3.3) uses external Tau A and Cas A source models, and the polarization-efficiency correction (Sect. 3.4.1) uses the external Tau A polarization fraction from Ritacco et al. (2018); neither is defined in terms of the sensitivity being reported. The array forecast in Sect. 5 and Fig. 16 is an explicit N_det^{-1/2} t^{-1/2} radiometer scaling from the measured white-noise level, with stated assumptions of 18 h/day, 50% observing efficiency, and comparable performance of the remaining detectors; the paper itself flags this as an assumption and notes that the FGI map 'would take a bit longer', with the 41 GHz forecast depending on the calibration diode bringing FGI to TGI-level performance. That is an extrapolation assumption about future hardware, not a circular reduction by construction. The external benchmarks (WMAP, Planck) are independent of the TFGI data, and the self-citations (e.g., Fasano et al. 2026 for laboratory efficiencies and polarization-angle methodology) are ancillary rather than load-bearing for the central sensitivity claim. The abstract's 'at both 31 and 41 GHz ... after 5.7 years' slightly overstates the body text's qualified FGI expectation; that is an internal-consistency or correctness concern, not circularity.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

The paper's central claims are measurements, so the ledger is dominated by calibration parameters fitted to Tau A data. The main axiom that carries the forecast is that future detectors will perform like the three usable ones; this is stated explicitly in Sect. 5.

free parameters (3)
  • Monthly gain calibration factors (mV/K) per pixel and channel = e.g., pixel 23 CH1 ranges 20.96 to 36.54 mV/K (Table 11)
    Absolute calibration of the time-ordered data to kelvin; all quoted sensitivities and flux densities depend on these factors.
  • Polarization efficiency correction per pixel = 96, 85, 38, and 73 percent for pixels 23, 26, 63 pre and post BEM change (Table 5)
    Polarized data are rescaled on a monthly basis by these values to recover the expected Tau A polarization fraction; the W44 polarized SED and the polarization sensitivity estimates depend on them.
  • Polarization angle calibration per month and channel = 4 to 30 degree uncertainties (Tables 6, 14, 15)
    Rotation angle used to map instrument Q and U to sky Q and U; unstable angles reduce the polarization response and are the main cause of the excluded pixels.
assumptions (4)
  • domain assumption Tau A flux model S_nu = 358.3 (nu/22.8 GHz)^-0.297 Jy at t0 = 2016.3, with -0.218 percent per year secular decrease
    Used for absolute gain calibration in Sect. 3.3 (Eq. 6); taken from previous QUIJOTE-MFI work and Weiland et al. (2011).
  • domain assumption Tau A polarization fraction p = 6.95 plus or minus 0.03 percent is constant between 20 and 350 GHz
    Used to derive polarization efficiencies in Sect. 3.4.1; sourced from Ritacco et al. (2018).
  • domain assumption The PICASSO destriper transfer function validated for MFI maps also applies to TFGI maps on scales larger than 20 arcmin
    Invoked in Sect. 2.3 to justify no additional transfer-function correction; based on numerical simulations, but details are deferred to future work.
  • ad hoc to paper Future TFGI detectors will have comparable noise and polarization performance to pixels 23 and 26
    The 5.7-year, 1 microkelvin per degree forecast in Sect. 5 and Fig. 16 scales measured sensitivity as the inverse square root of the detector count and assumes no performance degradation for the remaining detectors.

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Pith. "Pith review of QUIJOTE scientific results - XX. Commissioning and First Results from the Thirty and Forty Gigahertz Instrument (TFGI)." pith.science (2026). https://pith.science/paper/4DRTJITH

@misc{pith2026260808579,
  author       = {Pith},
  title        = {Pith review of: QUIJOTE scientific results - XX. Commissioning and First Results from the Thirty and Forty Gigahertz Instrument (TFGI)},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/4DRTJITH}},
  note         = {Machine review of arXiv:2608.08579}
}
abstract

We present the commissioning and first results of the Thirty and Forty Gigahertz Instrument (TFGI), which observes the sky at 31 and 41 GHz with angular resolutions of 21' and 18' from the second QUIJOTE telescope at the Teide Observatory. Its primary goal is to conduct a deep cosmological survey in selected regions of the Northern sky with high-sensitivity polarization measurements. The commissioning phase covered Nov2021-Oct2022, during which the instrument operated with a configuration of 7 receivers, 4 at 31 GHz and 3 at 41 GHz. Over this period, approximately 1200 h of data were acquired. Of these, 380 h were dedicated to calibration sources, used to characterize the instrumental properties of TFGI, including the pointing model, beam response, gain stability, polarimetric performance, and instantaneous sensitivity. We provide a detailed characterization of these properties and describe how they are being improved for future observing runs. We use 230 h of observations from bright Galactic regions (Cygnus, W43, W44, and W47) to further validate the instrument performance. As an illustrative example, we present the intensity and polarization spectral energy distributions of W44, finding good agreement with existing measurements. From the noise map of these observations, we measure a polarization sensitivity of ~8.3 $\mu$K deg$^{-1}$ after an effective observing depth of 0.57 h deg$^{-2}$. This performance, achieved considering only 2 detectors at 31 GHz, is already comparable to that achieved by WMAP (with almost 3 times the integration time per unit area, 1.61 h deg$^{-2}$). Extrapolating these results to the full TFGI array, with up to 29 detectors, we show that the instrument is expected to reach the target sensitivity of ~ 1 $\mu$K deg$^{-1}$ at both 31 and 41 GHz over three cosmological fields covering a total area of 3600 deg$^2$ after an effective integration time of 5.7 years.

Figures

Figures reproduced from arXiv: 2608.08579 by the authors.

Figure 1
Figure 1. Left column: Maps of Tau A obtained by combining all observations from November 2021 to May 2022. Right column: Best-fitting elliptical beam model. From top to bottom, pixels 23, 26 and 63, computed as the average of their four channels. The beam is slightly narrower for FGI pixel 63 because of its higher frequency, as expected. visible for pixels 23 and 63. The corresponding fitted ellipticities from these maps are… view at source ↗
Figure 2
Figure 2. Monthly Tau A maps from November 2021 to May 2022 used to study the temporal gain variations of the instrument. The maps correspond to channel 1 of pixel 23 at 31 GHz. They are shown in voltage units (µV), as no absolute calibration has been applied here. the gain was stable during these monthly periods. A more precise gain model will be elaborated in future observations once the calibration diode is in place. We wo… view at source ↗
Figure 3
Figure 3. Dependence of the gain with time for the first channel of TGI pixel 23 (left panel) and FGI pixel 63 (right panel). We show the gain value computed from the Tau A map taking into account all monthly measurements (after flagging) as dashed horizontal bars. The colored points show the values computed from data split maps for Tau A (see text), while the filled black regions show the standard deviation from those points… view at source ↗
Figures from the paper (16 more)
Figure 4
Figure 4. Figure 4: Example of Tau A Stokes I, Q, and U maps (top, middle, and bottom rows) before (left) and after (right) applying the ϕc rotation as described in Eq. 7 to recover the expected polarization angle of Tau A, γTau A. After applying the rotation, most of the polarized signal…
Figure 5
Figure 5. Figure 5: Stokes I, Q, and U maps (top, middle, and bottom rows respectively) for the Cygnus region, as observed with TGI pixels 23 (left), 26 (center) and FGI pixel 63 (right column). We clearly see the lower intensity at 41 GHz (pixel 63), because of the decreasing spectral in…
Figure 6
Figure 6. Figure 6: Intensity maps of the Cygnus region with QUIJOTE-TFGI, WMAP and Planck. Top (from left to right): TGI combined map from two detectors (31 GHz), Planck (28.4 GHz), WMAP (33 GHz). Bottom (from left to right): FGI (41 GHz), Planck (44.1 GHz), WMAP (40.7 GHz). We computed …
Figure 7
Figure 7. Figure 7: Power spectra from one skydip observation for the first channel of pixels 23, 26 and 63 (from left to right), both in intensity (top) and polarization (bottom). The measured data (computed as the Fourier transform of the TOD considered) is depicted in grey, while we sh…
Figure 8
Figure 8. Figure 8: (Left) Top: SED of W44 in intensity derived from maps at 1 degree resolution. The photometry is computed using an aperture of radius r = 1◦ . The TFGI measurements are consistent with those from other experiments. The model includes synchrotron, free-free, AME, thermal…
Figure 9
Figure 9. Figure 9: Details of the intensity maps centred on W44 from the two TGI pixels (left), FGI (middle), and Planck-HFI 857 GHz (right), all shown at their native angular resolutions. Circular apertures with r = 30′ are overlaid to illustrate the integration regions used for the pho…
Figure 10
Figure 10. Figure 10: Intensity (I, top) and polarized intensity (P, bottom) maps at 31 GHz (from pixel 23 of the TGI) for the W44 Galactic plane region, both at 30′ (left) and 1◦ (right) scales, with the apertures used for photometry overlaid. Finally, we study the Stokes parameters Q and…
Figure 11
Figure 11. Figure 11: SED for W44 in polarization, extracted from the 1 degree maps. From left to right: Stokes Q, Stokes U and the polarization angle. The polarized intensity, P, is shown in Appendix D. The TGI (pixels 23 & 26) measurements are consistent with previous experiments, simila…
Figure 12
Figure 12. Figure 12: Left: Stokes I, Q, and U maps (from top to bottom) of the region l ∈ (25◦ , 50◦ ) obtained with TGI pixel 23. Small residuals associated with the strong unpolarized emission from W43 are visible in the Q and U maps, displaying the characteristic cloverleaf pattern pro…
Figure 13
Figure 13. Figure 13: Same as [PITH_FULL_IMAGE:figures/full_fig_p021_13.png]
Figure 14
Figure 14. Figure 14: Same as [PITH_FULL_IMAGE:figures/full_fig_p021_14.png]
Figure 15
Figure 15. Figure 15: From top to bottom, maps for Stokes parameters I, Q and U. Left: HMDM from the two TGI pixels combined. Middle: similar plot for WMAP Ka HMDM (subtracting maps from years 1–4 and 5–9). Right: similar plot for Planck 28.4 GHz (ringhalf halfmaps). We note that the achie…
Figure 16
Figure 16. Figure 16: Dependence on the polarization sensitivity of the TFGI with time. We have considered three different instrument configurations: that presented in this paper, with only 2 TGI pixels; one with the next ring of pixels already installed in the instrument, with 10 TGI pixe…
Figure 17
Figure 17. Figure 17: Left: intensity SED for W43 at 1◦ resolution. Right: same SED, now at 30′ resolution [PITH_FULL_IMAGE:figures/full_fig_p030_17.png]
Figure 18
Figure 18. Figure 18: Left: intensity SED for W47 at 1◦ resolution. Right: same SED, now at 30′ resolution. 10 0 10 1 10 2 Frequency (GHz) 10 0 10 1 F l u x d e n s i t y - P ( J y ) W44 - 1 deg - pol MFI WMAP Planck TFGI 10 0 10 1 10 2 Frequency (GHz) 10 0 10 1 F l u x d e n s i t y - P (…
Figure 19
Figure 19. Figure 19: Polarized intensity (P) SED for W44: left 1 degree, right 30 arcmin. Data below 10 GHz were not used in any of the fits due to it being affected by Faraday rotation. The lack of data with resolution ≤ 30′ implies an increased importance of FGI pixel 63 point in the mo…

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