{"id":"a9fb3fd4-e15c-43a9-81d5-77fb26663d91","arxiv_id":"2509.02533","paper_version":1,"verdict":"CONDITIONAL","confidence":"HIGH","novelty_score":6.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":4,"one_line_summary":"A simulation study predicts PRIMA will measure interstellar magnetic field orientations to about 6 degrees and resolve magnetic turbulence at 20 parsec scales in nearby galaxies, capabilities SOFIA lacked.","lead":"Using galaxy simulations, this paper predicts that the proposed PRIMA space telescope will measure magnetic field structure in nearby galaxies down to roughly 20 parsec scales, far better than the retired SOFIA observatory. If correct, PRIMA would let astronomers trace turbulence and magnetic alignment in the gas that forms stars.","discovery_kind":"new_application","skeptic_critique":{"model":"deepseek-v4-flash","headline":"PRIMA small-scale precision claims rest on a simulation the authors admit is not converged at 10–20 pc; the 6° precision may be a property of the numerical grid, not of real galaxies.","rationale":"The reader's weakest assumption identifies the simulation resolution/convergence at 10–20 pc as the central risk; I agree. The paper's own Sec. 2.2 contains an explicit admission that convergence may require higher resolution by at least a few dex [30,31] — this is the single largest threat to the headline claims. The '6° precision' result (Sec. 3.3, Fig. 7) is measured against the intrinsic field of this same simulation; if that field is not converged, the precision is a statement about the numerical experiment, not about real galaxies. The P–S relation and polarization-fraction recovery (Sec. 3.4) are equally sensitive because they depend on the degree of small-scale field tangling that feeds beam depolarization. I do not think this requires rejecting the paper: the comparative trends across magnetization models and the PRIMA-vs-SOFIA differences are likely robust, and the paper is transparent about the limitation in Sec. 2.2. However, the abstract and conclusions present the quantitative 10 pc/6° numbers without the caveat, and there is also an internal inconsistency: the abstract says 'about 10 pc' for galaxies up to 0.5 Mpc, while Sec. 2.7 and 3.3 use 20 pc as the PRIMA resolution at 0.5 Mpc. These issues justify maintaining the CONDITIONAL verdict: the qualitative capability claims can stand, but the specific numerical predictions should be accompanied by a resolution-convergence estimate or explicitly labeled as simulation-dependent. No change to the reader's verdict is needed.","tokens_in":18945,"tokens_out":4767,"duration_ms":41581,"concrete_test":"Re-run one representative model (e.g., MB11 or MBinj) with a peak resolution of 5 pc (or 2.5 pc) — or, if that is prohibitive, a zoom-in patch around a star-forming spiral-arm region — and regenerate the PRIMA-like (20 pc) mock observations. Recompute the median Δθ_measurement distribution of Fig. 7 and the 100 pc turbulent magnetic fraction of Fig. 5. If the median separation changes by more than ~2° or the turbulent fraction by more than ~10% relative to the 10 pc run, the 6° precision and 10 pc resolving-power claims are not converged. A cheaper auxiliary check: use the resolution study in [29] to estimate the magnetic power spectrum at the dissipation scale and report the resolved inertial range; if the range at 10 pc is less than an order of magnitude in k, the ground truth is resolution-limited.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The paper's headline quantitative claims — that PRIMA will resolve magnetic observables at ~10 pc and recover intrinsic field orientations to ~6° — presuppose that the simulation's small-scale magnetic field is a reliable ground truth. Section 2.2 states the opposite: 'convergence may still require higher resolution by at least a few dex [30, 31].' If the turbulent magnetic field at 10–20 pc is not converged, then the 'intrinsic' field used as ground truth in Fig. 7 and Sec. 3.3 is a numerical artifact of the grid scale and of numerical resistivity (Sec. 2.1). The 6° median separation could simply reflect an artificially smooth field, not real astrophysical coherence. The same limitation propagates to the P–S relation (Fig. 8) and the recovery of intrinsic polarization fractions, which depend on unresolved tangling and beam depolarization. Because the admitted resolution shortfall is 'a few dex' — orders of magnitude, not a factor of two — the abstract's '~10 pc' and '~6°' statements should not be read as robust predictions about real galaxies until a convergence study demonstrates otherwise. Note also that at 0.5 Mpc, PRIMA's 9.3″ beam gives ~20 pc, not ~10 pc as stated in the abstract; the concrete quantitative claims are therefore both under-resolved and internally inconsistent.","agreement_with_reader":"agree"},"referee_report":{"model":"deepseek-v4-flash","summary":"The paper uses a suite of RAMSES cosmological MHD simulations of a face-on Milky Way-like galaxy with five initial magnetization strengths (MB10, MB11, MB12, MB20, MBinj) to generate synthetic far-infrared dust polarization maps via a geometric dust-alignment model. These maps are processed into SOFIA/HAWC+-like (300 pc) and PRIMA-like (20 pc at 0.5 Mpc) mock observations and compared with the simulation ground truth. The authors analyze the magnetic turbulence fraction at 100 pc scales, the alignment between magnetic fields and density structures, the angular separation between FIR-measured and intrinsic B-fields, the polarization fraction versus angular dispersion relation, and the magnetic alignment parameter ζ. The main claims are that magnetic turbulence increases with weaker magnetization, that PRIMA will recover intrinsic field orientations to roughly 6° precision and resolve observables at about 10 pc for galaxies up to 0.5 Mpc, that beam depolarization is significantly reduced with PRIMA, and that PRIMA will recover the polarization fraction–ζ correlation.","tokens_in":19250,"tokens_out":5157,"duration_ms":45426,"significance":"If the simulation ground truth is reliable, the qualitative trends—stronger magnetization suppressing small-scale magnetic turbulence and reducing alignment with density structures—are physically plausible and provide useful predictions for a proposed instrument. The paper's main strengths are its forward-modeling approach from independent MHD simulations, the use of externally calibrated dust parameters (p0=0.25, dust-to-metal ratio 0.4), and the explicit tests of inclination effects and of the magnetic-turbulence proxy in the appendices. The central limitation is the admitted non-convergence of the simulations at the 10–20 pc scales that the headline quantitative claims depend on; Section 2.2 states that convergence may require higher resolution by at least a few dex. The quantitative predictions (6° precision, 10 pc resolution) are therefore conditional on a numerical ground truth that has not been established, which is a load-bearing issue for the paper's most prominent claims.","major_comments":[{"comment":"The headline claims that PRIMA will measure unresolved intrinsic magnetic field orientations to about 6° precision and resolve observables at about 10 pc rest on a simulation ground truth that the authors themselves state is not converged. Section 2.2 reads: 'convergence may still require higher resolution by at least a few dex [30, 31].' Because the intrinsic POS field used in Fig. 7 is a density-weighted column average of a field whose small-scale structure is not converged, the reported 6° median separation could reflect artificial smoothness introduced by the finite grid and numerical resistivity (Section 2.1) rather than astrophysical coherence. Please either provide a convergence study at higher resolution or explicitly temper the abstract and conclusions so that the 6° and 10 pc statements are presented as conditional on resolution convergence, not as robust predictions for real galaxies.","section":"Abstract; §2.2; §3.3; Fig. 7"},{"comment":"There is an internal inconsistency in the claimed spatial resolution. The abstract says PRIMA will resolve 'down to scales comparable to the resolution of our simulations (about 10 pc) for galaxies up to 0.5 Mpc away,' but Section 2.7 computes the PRIMA beam at 0.5 Mpc as 9.3 arcsec at 100 μm, giving about 20 pc, and Section 3.3 explicitly states 'down to scales of about 20 pc.' At 0.5 Mpc, 9.3 arcsec corresponds to roughly 20 pc, not 10 pc. The abstract overstates the resolution by a factor of two and should be corrected to state ~20 pc, with the ~10 pc figure reserved for the simulation cell size rather than the PRIMA beam.","section":"Abstract vs. §2.7 and §3.3"},{"comment":"The 'intrinsic magnetic field orientation' used as ground truth in Fig. 7 is the gas-density-weighted column-averaged POS field, not the full 3D magnetic field orientation. The 6° precision is therefore a statement about how well the mock pipeline recovers this column-averaged quantity under PRIMA-like smoothing, not a statement about recovery of the true local 3D field. This distinction should be stated explicitly whenever the 6° number is quoted, since the abstract's phrase 'unresolved intrinsic magnetic field orientations' risks overstating what is actually tested.","section":"§3.3; Fig. 7"},{"comment":"The paper reports different values for SOFIA's deviation from ground truth in the turbulence fraction recovery. Section 3.1 states 'the SOFIA case has deviations of up to about 30 percent with respect to ground truth values,' while conclusion item 2 says SOFIA can recover with 'up to about 35 percent deviations.' Please reconcile these numbers or clarify whether they refer to different density ranges or different metrics, so that the conclusions are quantitatively consistent with the body of the paper.","section":"§4, conclusion item 2 vs. §3.1"}],"minor_comments":[{"comment":"The abstract contains a typo: 'magnetic alignment paramater' should be 'parameter'.","section":"Abstract"},{"comment":"The paragraph introducing Fig. 4 repeats itself: 'In Fig. 4 we show the comparison...' is followed immediately by 'To further investigate the turbulence... we show a 2D histogram...'. Please remove the duplicated sentence and merge the two descriptions.","section":"§3.1"},{"comment":"When listing the dispersion radii, the sentence reads '10 pc, 13.6 arcsec (300 pc), and 9.3 arcsec (20 pc) for the simulation, SOFIA, and PRIMA.' Please explicitly state the assumed distances (simulation native resolution, 10 Mpc for SOFIA, 0.5 Mpc for PRIMA) in that sentence for consistency with Section 2.7.","section":"§2.9.2"},{"comment":"Equation (12) appears to have a formatting issue: 'ζ = cos(2Δθ_spiral)' should probably read 'ζ = cos(2 Δθ_spiral)' or a closing parenthesis is missing; please check the typesetting.","section":"Eq. (12)"},{"comment":"The caption states 'Colorscale values are displaced downwards by exactly 1 dex to reduce saturation.' This is unclear; please specify which quantity is displaced and why a one-dex offset is applied, or remove the sentence if it is not essential.","section":"Figure 1 caption"},{"comment":"The description of the 'quasi-asymmetrical binning' method is vague. The text says the highest and lowest bin edges are the maximum and minimum values, but it is not clear how many bins are used or how the low/high edges are set without making the bins pathologically wide. Please give the exact binning prescription.","section":"§2.10"}],"recommendation":"major_revision","confidential_remarks":"The paper is a useful forward-modeling study for a proposed instrument, and the qualitative trends are likely robust, but the abstract and conclusions make quantitative claims (6° precision, 10 pc resolution) that the authors' own resolution-convergence caveat does not support. The internal inconsistency between the abstract's ~10 pc and the body's ~20 pc at 0.5 Mpc is the kind of issue that must be fixed before publication. I do not see a circularity problem: the mock observations are not fitted to the target quantities, and the calibration parameters come from external constraints. The overlap with the SALSA team is a strength rather than a conflict, since it provides direct context for the observational comparison. The paper is within the scope of a general astrophysics journal."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Worth a serious referee. The paper is a clean, well-documented forecast of what PRIMA could do for extragalactic FIR polarimetry, based on a suite of MHD simulations of a Milky-Way-like galaxy with five magnetization models. The genuinely new results are the PRIMA-specific numbers: ~6° recovery of the intrinsic plane-of-sky field orientation, the shallow P-S slope of -0.27 matching the simulation, and the turbulence-fraction recovery within ~4% where SOFIA-era mock observations deviate by ~35%. Those are concrete and not in the prior SOFIA-era literature. The qualitative trends—weaker magnetization giving more magnetic turbulence and lower alignment with density structure—are consistent across models and physically sensible.\n\nThe paper does what a good forecast should: it states the geometric dust polarization model, cites external calibration for p0 and dust-to-metal ratio, makes the mock observational pipeline explicit, and includes inclination and radial checks in appendices. The authors are also honest about the biggest weakness: Section 2.2 admits the simulations 'may still require higher resolution by at least a few dex' at the 10 pc scales that the whole small-scale forecast is about. That is a load-bearing caveat that should be in the abstract, not just in the methods. If the magnetic field structure at 10-20 pc is not converged, the 'intrinsic' field used as ground truth is partly numerical, and the 6° number is a property of the simulated grid, not necessarily of real galaxies.\n\nThere is also a concrete internal inconsistency: the abstract says PRIMA resolves ~10 pc for galaxies up to 0.5 Mpc, but Section 2.7 correctly says 9.3\" at 0.5 Mpc gives ~20 pc. The factor of two is not minor. The paper has no error bars on the headline numbers, though quantile spreads give some sense of robustness. The heavy overlap with the SALSA team is not itself a problem; the cited calibration and comparison papers are real and relevant.\n\nNet: this deserves a serious referee. Not a desk reject. The referee should ask for a corrected abstract, a visible convergence caveat, and ideally one higher-resolution simulation to show the 10-20 pc results do not change qualitatively. I would read this in a journal club and likely cite it in a PRIMA context, but I would not treat the 6° precision as a firm prediction until the convergence question is addressed.","headline":"Solid PRIMA forecast, but the abstract overstates resolution (10 pc vs 20 pc) and the 6° precision claim rests on a simulation the authors concede is not converged at those scales.","tokens_in":19756,"tokens_out":2931,"would_cite":true,"duration_ms":27140,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"PRIMA will resolve magnetic fields in nearby galaxies to 20 pc","keywords":["PRIMA","far-infrared polarimetry","magnetic fields","interstellar medium","magnetohydrodynamics","galaxy simulations","dust polarization","magnetic turbulence"],"falsifier":"Run the same galaxy formation models with peak resolution increased by a few dex (to about 1 pc) and recompute the median $\\Delta\\theta$ between mock-PRIMA and intrinsic field orientations and the 100-pc turbulence fractions; if $\\Delta\\theta$ moves above about $6^\\circ$ or $f_{B,\\mathrm{turb}}$ changes by more than a few percent, the central precision claim fails. Alternatively, a PRIMA observation of a local galaxy at 20-pc resolution whose $P$-$S$ slope matches SOFIA's $-0.52$ rather than the predicted $-0.27$ would show that the beam-depolarization reduction is not as strong as claimed.","tokens_in":18797,"feed_emoji":"🔭","tokens_out":7761,"duration_ms":68273,"temperature":0.7,"pith_summary":"This paper argues that the proposed PRIMA far-infrared space telescope will transform extragalactic magnetic-field studies by resolving the cold, dusty interstellar medium of local galaxies down to about 20 pc, close to the 10-pc resolution of the simulations used as ground truth. It builds synthetic far-infrared polarimetric observations from five magnetohydrodynamical models of a Milky Way-like galaxy, spanning initial magnetic field strengths from $10^{-10}$ to $10^{-20}$ G plus a supernova-seeded case. Against those mock observations, PRIMA-like sensitivity recovers the simulated turbulence fraction at 100-pc scales to within about 4%, measures intrinsic magnetic field orientations to about $6^\\circ$ median precision, and reproduces the intrinsic polarization-dispersion relation, whereas SOFIA-like observations are degraded by roughly 300-pc beams and show deviations up to about 35%. The practical point is that, if these predictions hold, the next far-infrared observatory can turn nearby galaxies into resolved laboratories for interstellar magnetism.","feed_headline":"PRIMA will resolve magnetic fields in nearby galaxies to 20 pc","feed_subtitle":"Simulated observations predict PRIMA will outperform SOFIA on turbulence, alignment, and beam depolarization.","key_machinery":"The load-bearing machinery is the synthetic far-infrared polarimetry pipeline: for each adaptive-mesh cell, a geometric dust-polarization model (Eqs. 1-3) converts gas density, metallicity with an ionization-dependent metal-to-dust ratio, and magnetic field geometry into Stokes $I$, $Q$, and $U$; line-of-sight integration gives face-on maps, and Gaussian smoothing to PRIMA's and SOFIA's beams turns them into mock observations. On top of that, the analysis stack defines the observables that carry the claims: the 100-pc turbulence fraction $f_{B,\\mathrm{turb}}$, the alignment angle $\\Delta\\theta$ between magnetic field and density-gradient orientations, the polarization fraction $P$, the circular-standard-deviation dispersion $S$, and the spiral alignment parameter $\\zeta = \\cos(2\\Delta\\theta_{\\mathrm{spiral}})$. Comparing each observable at simulation resolution, PRIMA resolution, and SOFIA resolution is what converts the simulations' ground truth into instrument-specific predictions.","core_discovery":"On the paper's own terms, the central discovery is a quantified resolution gap: magnetic-field information that SOFIA-era observations could only see as beam-averaged structure becomes individually resolvable with PRIMA's sensitivity. The paper claims that PRIMA will measure the plane-of-sky magnetic field orientation in local galaxies ($\\lesssim 0.5$ Mpc) at about 20-pc resolution with median $\\Delta\\theta \\sim 6^\\circ$ fidelity relative to the intrinsic field, versus about $11^\\circ$ for SOFIA at 300 pc, and about $8^\\circ$ versus $19^\\circ$ in the densest clumps. It also claims that the polarization fraction-angular dispersion relation, which looks steeply depolarized ($P \\propto S^{-0.52}$) in SOFIA-like beams, is recovered at its intrinsic shallower slope ($\\alpha \\simeq -0.27$) by PRIMA, and that the magnetic alignment parameter $\\zeta$ correlates with polarization fraction in dense regions only when small-scale structure is resolved. The underlying physical trends established in the simulations are that 100-pc magnetic turbulence increases with decreasing magnetization and that stronger magnetization weakens the alignment of magnetic fields with density structures.","pith_inferences":["An extension the authors leave implicit: if the simulated anti-correlation between 100-pc turbulence and magnetization is confirmed, observed turbulence fractions could become a statistical estimator of unresolved disk field strength.","Because the ground truth is resolution-limited, PRIMA itself could be used to measure sub-beam field dispersion in real galaxies and check whether the simulated 10-pc structure is realistic.","The inclination correction in Appendix B implies a practical strategy beyond the paper's face-on case: deprojecting observed alignment angles with $\\theta_{\\mathrm{int}} = \\arctan(\\tan\\theta_{\\mathrm{obs}} / \\cos i)$ would let PRIMA recover small-scale alignment signals in inclined galaxies.","A comparative test: galaxies with similar star formation but different mean field strengths, observed by PRIMA, would show whether the magnetization-alignment trend is universal or specific to these initial conditions."],"forward_implications":["PRIMA will recover the 100-pc magnetic turbulence fraction to within about 4% of simulation ground truth, whereas SOFIA-like observations deviate by up to about 35%, especially in dense spiral-arm gas.","PRIMA will nearly double the accuracy of magnetic-field orientation measurements: median $\\Delta\\theta \\sim 6^\\circ$ versus about $11^\\circ$ for SOFIA, and about $8^\\circ$ versus $19^\\circ$ in the densest clumps.","PRIMA will resolve polarized fraction and magnetic alignment down to about 20-pc scales for galaxies out to roughly 0.5 Mpc, sampling the turbulence coherence scale instead of averaging over it.","PRIMA will reproduce the intrinsic polarization-dispersion relation ($\\alpha = -0.27$) rather than SOFIA's beam-depolarized slope ($-0.52$), and will recover a positive $P$-$\\zeta$ correlation in high-density regions that SOFIA flattens."],"supporting_citations":[{"why":"Supplies the geometric FIR polarization model with the Stokes I/Q/U equations and metal-to-dust ratio from which all mock observations are built.","marker":"[10]"},{"why":"Defines the SALSA sample and the roughly 300-pc SOFIA-like resolution used as the observational baseline.","marker":"[12]"},{"why":"Defines the magnetic alignment parameter zeta and the SALSA result that FIR alignment is lower than radio alignment, which PRIMA is predicted to resolve.","marker":"[13]"},{"why":"Supplies the earlier synthetic-polarization comparison for the polarization fraction-dispersion anti-correlation used as a reference in Section 3.4.","marker":"[18]"},{"why":"Supplies PRIMA's sensitivity specifications that drive the mock PRIMA observations and the claimed resolution advantage.","marker":"[21]"},{"why":"Introduces the cosmological initial conditions and supernova-seeded magnetization setup used for the simulations.","marker":"[24]"},{"why":"Sets the maximum polarization fraction p0,FIR = 0.25 in the synthetic emission model from Planck dust polarimetry.","marker":"[42]"},{"why":"Gives HAWC+/SOFIA's point-spread-function width and sensitivity, used to construct the SOFIA-like mock observations and compare with PRIMA.","marker":"[48]"},{"why":"Supplies the roughly 50-100 pc turbulence coherence scale that motivates the 0.5-Mpc distance and 20-pc PRIMA resolution choice.","marker":"[51]"}],"fun_headline_variants":["PRIMA resolves galaxy magnetic fields at 20 pc","PRIMA maps magnetic fields 15x finer than SOFIA","PRIMA to unveil small-scale magnetism in nearby galaxies","PRIMA outperforms SOFIA on magnetic turbulence and alignment"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"The paper's ground truth is a simulation whose magnetic-field structure at 10-20 pc scales is not proven converged; the authors note that convergence may require at least a few orders of magnitude higher resolution, so PRIMA's predicted about 6-degree precision against that ground truth could be optimistic for real galaxies.","fun_headline_variants_meta":{"raw":{"variants":["PRIMA resolves galaxy magnetic fields at 20 pc","PRIMA maps magnetic fields 15x finer than SOFIA","PRIMA to unveil small-scale magnetism in nearby galaxies","PRIMA outperforms SOFIA on magnetic turbulence and alignment"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.00066,"raw_usage":{"total_tokens":3110,"prompt_tokens":1128,"completion_tokens":1982,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":744,"completion_tokens_details":{"reasoning_tokens":1913}},"tokens_in":744,"tokens_out":1982,"duration_ms":14200,"temperature":1.0,"reasoning_tokens":1913,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-15T16:36:48.198800+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Run the same galaxy formation models with peak resolution increased by a few dex (to about 1 pc) and recompute the median $\\Delta\\theta$ between mock-PRIMA and intrinsic field orientations and the 100-pc turbulence fractions; if $\\Delta\\theta$ moves above about $6^\\circ$ or $f_{B,\\mathrm{turb}}$ changes by more than a few percent, the central precision claim fails. Alternatively, a PRIMA observation of a local galaxy at 20-pc resolution whose $P$-$S$ slope matches SOFIA's $-0.52$ rather than the predicted $-0.27$ would show that the beam-depolarization reduction is not as strong as claimed.","supporting_citations":[{"cited_title":"Extragalactic Magnetism with SOFIA (SALSA Legacy Program). VII. A Tomographic View of Far-infrared and Radio Polarimetric Observations through MHD Simulations of Galaxies,","cited_arxiv_id":null,"evidence_quote":"Supplies the geometric FIR polarization model with the Stokes I/Q/U equations and metal-to-dust ratio from which all mock observations are built."},{"cited_title":"Extragalactic Magnetism with SOFIA (SALSA Legacy Program). IV. Program Overview and First Results on the Polarization Fraction*,","cited_arxiv_id":null,"evidence_quote":"Defines the SALSA sample and the roughly 300-pc SOFIA-like resolution used as the observational baseline."},{"cited_title":"Extragalactic Magnetism with SOFIA (SALSA Legacy Program). V. First Results on the Magnetic Field Orientation of Galaxies,","cited_arxiv_id":null,"evidence_quote":"Defines the magnetic alignment parameter zeta and the SALSA result that FIR alignment is lower than radio alignment, which PRIMA is predicted to resolve."},{"cited_title":"Polarised emission from aligned dust grains in nearby galaxies: Predictions from the Auriga simulations,","cited_arxiv_id":null,"evidence_quote":"Supplies the earlier synthetic-polarization comparison for the polarization fraction-dispersion anti-correlation used as a reference in Section 3.4."},{"cited_title":"Unraveling the origin of magnetic fields in galaxies,","cited_arxiv_id":null,"evidence_quote":"Introduces the cosmological initial conditions and supernova-seeded magnetization setup used for the simulations."},{"cited_title":"Planck 2018 results. XII. Galactic astrophysics using polarized dust emission,","cited_arxiv_id":null,"evidence_quote":"Sets the maximum polarization fraction p0,FIR = 0.25 in the synthetic emission model from Planck dust polarimetry."},{"cited_title":"HAWC+, the Far-Infrared Camera and Polarimeter for SOFIA,","cited_arxiv_id":null,"evidence_quote":"Gives HAWC+/SOFIA's point-spread-function width and sensitivity, used to construct the SOFIA-like mock observations and compare with PRIMA."},{"cited_title":"The Outer Scale of Turbulence in the Magnetoionized Galactic Interstellar Medium,","cited_arxiv_id":null,"evidence_quote":"Supplies the roughly 50-100 pc turbulence coherence scale that motivates the 0.5-Mpc distance and 20-pc PRIMA resolution choice."}],"review_version":2}