Pith. sign in

REVIEW 3 major objections 5 minor 166 references

PRIMAger, a proposed far-infrared polarimetry imager, can map magnetic fields across entire nearby molecular clouds in 170 hours of observing time.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

A proposed PRIMAger survey would map magnetic fields across 160 square degrees of nearby molecular clouds in polarized far-infrared light, resolving cloud-to-core magnetic field structure for the first time.

T0 review reviewed 2026-08-05 challenge →

load-bearing objection A clear, honest survey proposal for PRIMAger whose headline 170-hour estimate is plausible but depends on an under-specified ETC and an optimistic 20% cirrus polarization fraction; worth a serious referee, but the sensitivity claim needs hardening. the 3 major comments →

arxiv 2509.01796 v1 pith:LTUQ2T2H submitted 2025-09-01 astro-ph.GA astro-ph.IM

Mapping Magnetic Fields from Clouds to Cores with PRIMAger

Kate Pattle , Janik Karoly , Lorna Buhil Findlay , Simon Coud\'e , Brandon S. Hensley , Paulo C. Cortes , James Di Francesco , Valentin J. M. Le Gouellec
show 2 more authors
Enrique Lopez-Rodriguez Fabien Louvet
This is my paper
classification astro-ph.GA astro-ph.IM
keywords magnetic fieldsmolecular cloudsfar-infrared polarimetryPRIMAgerdust grain alignmentstar formationcirrus confusion limitGould Belt Survey
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

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 argues that PRIMAger, the polarimetry imager on the proposed PRIMA far-infrared space telescope, can for the first time map magnetic fields continuously from whole molecular clouds down to the individual filaments and cores inside them. The central estimate is that mapping the 160 square degrees covered by the Herschel Gould Belt Survey down to the cirrus confusion limit (the brightness floor set by diffuse galactic dust) in polarized light would take about 170 hours, giving a 5-sigma detection of 20% polarized cirrus at polarized intensities near 1 MJy/sr in the longest-wavelength band. If that holds, PRIMAger would resolve magnetic field structure at roughly 10^3-10^4 au scales across entire clouds, a resolution improvement of over an order of magnitude over Planck and a mapping-speed gain of about 10,000 times over the SOFIA/HAWC+ polarimeter. The survey would turn magnetic field geometry in star-forming clouds into a statistical, population-wide measurement rather than a set of scattered core-scale snapshots, and would simultaneously deliver multi-wavelength polarization spectra that test dust grain alignment models. The time estimate depends on the PRIMAger exposure-time calculator and on the assumption that diffuse cirrus is 20% polarized; both are stated openly and can be checked before launch.

Core claim

The paper's claim, on its own terms, is that PRIMAger will map the plane-of-sky magnetic field geometry of all star-forming molecular clouds within 0.5 kpc, in four far-infrared bands (PPI1-PPI4, 96-235 micron), at linear resolutions of about 10^-3 to 10^-2 pc. Taking Herschel 250 micron data as a stand-in for PPI4, the authors estimate that 170 hours of observing time, 1.1 hours per square degree including overheads, yields a 5-sigma detection of 20% polarized cirrus at 1.0 MJy/sr in polarized intensity, with the same exposure reaching 2.52, 1.94, and 1.37 MJy/sr in the three shorter bands. Because polarization fraction in the diffuse ISM peaks near 20% and declines with extinction, a detec

What carries the argument

Dust-grain alignment is the physical mechanism: interstellar dust grains align with their minor axes perpendicular to the local magnetic field, so their thermal far-infrared emission is linearly polarized perpendicular to the plane-of-sky field direction, and mapping polarized intensity maps the field. The calculation that carries the argument is the exposure-time chain: the Herschel 250 micron cirrus confusion level (5 MJy/sr) is taken as the PPI4 Stokes I floor; assuming 20% polarization sets a polarized-intensity target of 1.0 MJy/sr; and the PRIMAger exposure-time calculator converts that target into 1.1 hours per square degree, or 170 hours for the full 160 square degree Gould Belt foot

Load-bearing premise

The 170-hour estimate rests entirely on the PRIMAger exposure-time calculator's claim that PPI4 reaches a 5-sigma polarized-intensity sensitivity of 1.0 MJy/sr in 1.1 hours per square degree, together with the assumption that the faintest cirrus the survey targets is genuinely 20% polarized.

What would settle it

Two checks would settle it: (1) scale HAWC+ measured sensitivities to PRIMAger's aperture, wavelengths, and bandwidths and compare against the exposure-time calculator's prediction; (2) measure the actual polarization fraction of cirrus at the 1-5 MJy/sr brightness level using Planck 353 GHz polarization maps of low-column-density fields. If the scaled sensitivity is more than roughly twice the ETC value, or the cirrus polarization fraction comes in below about 10 percent, the 170-hour, 160-square-degree survey time is not achievable as stated.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

  • The entire Gould Belt sample of clouds within 0.5 kpc can be mapped in polarized light in about a week of observing time, making an unbiased statistical survey of magnetic field morphologies practical for the first time.
  • The same image connects scales: magnetic fields in diffuse cloud envelopes and in individual filaments and cores (0.006-0.06 pc resolution) are traced in one dataset, allowing the cloud-to-core field transition to be measured directly.
  • Multi-wavelength polarization spectra across entire clouds would test radiative-alignment and grain-disruption models and map how dust properties change from cirrus to dense cores.
  • A uniform, large-area sample lets field-strength estimators such as the Davis-Chandrasekhar-Fermi method, histogram-of-relative-orientation analyses, and comparisons with magnetized star-formation simulations be applied statistically rather than on a handful of regions.
  • The survey's deep total-intensity maps enable auxiliary science beyond polarimetry, such as censuses of candidate pre-brown-dwarf cores and studies of extragalactic background sources.

Where Pith is reading between the lines

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

  • The same scaling extends beyond 0.5 kpc: mapping more distant, higher-mass star-forming regions would take proportionally longer but remains practical, so this survey is a template for a wider high-mass program that the paper mentions but does not cost out.
  • The 250 micron-to-PPI4 intensity transfer is a bandpass assumption, not a measured equivalence; cold versus warm cirrus will shift it. A pre-launch check comparing Herschel 250 and 350 micron maps in the same fields could bracket this conversion uncertainty.
  • If real cirrus polarization at 235 micron is below the assumed 20%, the survey time scales roughly as the inverse square of the polarization fraction, so 10% polarization would multiply the 170 hours by about four, a straightforward rescaling of the paper's own formula.
  • The paper notes synergies with radio Zeeman and Faraday-rotation instruments; if the survey flies, its wide-area plane-of-sky maps would provide the targeting and prior geometry needed to turn those line-of-sight measurements into three-dimensional field reconstructions.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper proposes an unbiased survey of nearby molecular clouds (within 0.5 kpc) in polarized far-infrared light with the PRIMAger Polarimetry Imager, aiming to map magnetic fields from whole-cloud scales (~10 pc) down to core scales (~10^-2 pc). The central quantitative claim is that mapping the 160 deg^2 covered by the Herschel Gould Belt Survey to the cirrus confusion limit in polarized intensity would require 170 hours of PRIMAger time, yielding 5-sigma detections of 20% polarized cirrus at 1.0-2.4 MJy/sr in PPI1-PPI4. The estimate is obtained by scaling the PRIMAger Exposure Time Calculator (ETC) to the assumed cirrus confusion level, using Herschel 250 micron data as a proxy for PPI4 (235 micron) Stokes I. The paper also presents illustrative model PRIMAger maps of Ophiuchus, compares resolution and mapping speed with Planck and HAWC+, and outlines the scientific analyses enabled by such a survey.

Significance. If the sensitivity estimate is correct, the proposed survey would be transformative: it would provide the first unbiased, high-resolution FIR polarization maps of entire molecular clouds, with >10x better angular resolution than Planck and ~10,000x higher mapping speed than HAWC+, while spanning the peak of the dust SED in four bands. The paper is clearly written, and the model magnetic-field maps in Section 5 are explicitly labeled as illustrative rather than predictions, which is appropriate. The ETC is an independent instrument model, so there is no circularity in the central estimate. However, the 170-hour headline is load-bearing and currently rests on a small number of stated assumptions (notably the 20% cirrus polarization fraction and a unit conversion) and on unstated ETC inputs. The science case is strong, but the feasibility number needs to be made reproducible and robust before the central claim can be accepted.

major comments (3)
  1. [§4, Table 1] The stated conversion '1 MJy/sr = 14.1 mJy/beam' for a PPI4 beam FWHM of 27.6'' is inconsistent with the standard Gaussian-beam solid angle: Omega = 1.133 theta^2 = 2.03e-8 sr, which gives 1 MJy/sr = 20.3 mJy/beam. The value 14.1 mJy/beam corresponds to a top-hat beam of the same FWHM. If the ETC assumes a Gaussian beam, the target polarized flux should be 20.3 mJy/beam, not 14.1 mJy/beam, which increases the required integration time by a factor of (20.3/14.1)^2 ~ 2.1 (i.e., 170 h -> ~350 h). Please state the beam-solid-angle convention used in the ETC and verify the conversion.
  2. [§4, Table 1] The 170-hour estimate is not reproducible from the information given. The paper cites the PRIMAger ETC but does not list its input parameters: detector NEP or NEFD, bandwidth, optical throughput, telescope temperature/emissivity, assumed astrophysical and telescope backgrounds, and the overhead fraction. Table 1 states 'including overheads' but no overhead breakdown is provided. Since integration time scales as (NEFD)^2, a 40% NEFD error changes the required time by a factor of ~2, and a factor-2 error changes it by 4x. Please provide the full ETC inputs, or a table of the assumed instrument parameters, so that the calculation can be independently checked. The PPI1-PPI3 sensitivities in Table 1 (2.52, 1.94, 1.37 MJy/sr) inherit the same fragility, and without the per-band ETC outputs it is not clear that these bands reach the claimed 1.0-2.4 MJy/sr range in the same 170 h.
  3. [§4] The assumed 20% polarization fraction for cirrus is the maximum value seen in the diffuse ISM (Planck XIX), not a typical value. If the typical polarization fraction at the cirrus confusion level is 10%, the polarized intensity is 0.5 MJy/sr, and the time required for a 5-sigma detection quadruples (600+ hours). The sentence 'will ensure detection of polarized emission at all higher column densities' relies on the empirical trend p proportional to I^{-alpha} with 0<alpha<1; this trend is plausible but the specific exponent range should be referenced, and the statement should be explicitly conditional on p=20%. Please present the time estimate as a function of assumed polarization fraction (e.g., 10-20%) and adjust the abstract and summary language accordingly.
minor comments (5)
  1. [§4] Typo: 'sensitvity' should be 'sensitivity'.
  2. [§5] Typo: 'oberservations' should be 'observations'.
  3. [Figure 1 caption] 'Planck plane-of sky magnetic field vectors' should be 'plane-of-sky'.
  4. [§4/Table 1] The text says the estimate is for 'the most stringent case' and Table 1 says 'including overheads', but the overhead fraction is never defined. Please specify what overheads are included (e.g., slewing, calibration, sky subtraction).
  5. [§4] The use of Herschel 250 micron brightness as a proxy for PPI4 235 micron Stokes I is reasonable given the close wavelengths, but the difference in dust emissivity and the SPIRE vs PPI4 beam sizes should be noted as a source of systematic uncertainty in the confusion-level calibration.

Circularity Check

1 steps flagged

One target-restated-as-outcome; the central 170-hour estimate rests on an external ETC, so overall circularity is minimal.

specific steps
  1. self definitional [Section 4 (Time estimate), Table 1; echoed in the Abstract]
    "Assuming 20% polarization in the most diffuse regions of molecular clouds, we expect that the cirrus confusion limit in total intensity (5 MJy/sr) will have a surface brightness in polarized intensity of 1 MJy/sr. Our target is thus to achieve a good detection in polarized intensity where P = 1MJy/sr. ... The time required to map the area observed by the Herschel Gould Belt Survey (160 deg2) to the cirrus confusion limit in polarized light is 170 hours. This will give a 5-sigma detection of 20% polarized low-density cirrus emission"

    The claimed outcome (a 5-sigma detection of 20% polarized cirrus at P = 1.0 MJy/sr) is exactly the input sensitivity target: 1.0 MJy/sr is set by construction as 0.2 × 5 MJy/sr, and the ETC time is chosen so that the 5-sigma P sensitivity in PPI4 equals 1.0 MJy/sr. The Abstract then restates that chosen target as a result that the survey 'will give'. This is a definitional restatement rather than an independent prediction. However, the 170-hour number itself is not forced by this definition alone; it is obtained from the external PRIMAger Exposure Time Calculator, so the circularity is minor and does not drive the central derivation.

full rationale

The central chain is: Herschel/SPIRE cirrus confusion at 250 µm (5 MJy/sr, external) is taken as the PPI4 Stokes I confusion level; Planck XIX supplies the ~20% maximum polarization fraction in diffuse ISM (external); the product gives the PPI4 polarized-intensity target of 1 MJy/sr; the PRIMAger ETC (an external instrument model, not derived in this paper) then yields 1.1 h per square degree and 170 h for 160 deg². None of these inputs is defined in terms of the final claim, and the 170-hour estimate would be an independent sensitivity calculation even if the abstract's phrasing weakly collapses the target and the outcome. The model magnetic-field maps in Section 5 are explicitly described as 'not a prediction' and are only illustrative, so they do not constitute a fitted-input-called-prediction step. No load-bearing self-citation chain or uniqueness argument is used to force the result. The only circular flavor is the target-restated-as-outcome for the 5-sigma detection statement, which justifies a low nonzero score but not a finding of substantive circularity.

Axiom & Free-Parameter Ledger

3 free parameters · 3 axioms · 0 invented entities

No new physical entities are introduced. The free parameters are the assumed polarization fraction and the illustrative transition surface brightness in the model field maps. The 170-hour estimate is built on two explicit domain assumptions: 250 micron brightness maps to PPI4 Stokes I, and 20% polarization in cirrus.

free parameters (3)
  • Cirrus polarization fraction = 0.2 (20%)
    Assumed polarization fraction for low-density cirrus emission, based on Planck diffuse ISM measurements (Section 4). The target detection is defined as 5-sigma detection of 20% polarized cirrus. If the true cirrus polarization is lower, the required time increases.
  • Transition column density between parallel and perpendicular field alignment = 950 MJy/sr at 250 micron
    The center of the sigmoid function that sets the artificial magnetic field geometry in the model Ophiuchus maps (Section 5). Chosen arbitrarily to demonstrate capability, not to match observations. This parameter does not affect the 170-hour estimate but is a free parameter in the demonstration figures.
  • Sigmoid smoothing width for field transition = not specified
    The sigmoid function used to smooth the parallel-to-perpendicular transition in the model field geometry is described but its width is not given. A free choice in constructing the illustrative maps.
axioms (3)
  • domain assumption Herschel SPIRE 250 micron brightness is comparable to PRIMAger PPI4 (235 micron) Stokes I.
    Explicitly stated in Section 4. The entire time estimate converts 5 MJy/sr at 250 micron to a requirement at 235 micron without a spectral correction. Reasonable for a cold dust SED, but the colors of cirrus and cloud material vary.
  • standard math Dust polarization traces the plane-of-sky magnetic field direction with a well-established grain alignment mechanism.
    Standard astrophysics assumption cited to refs 9, 128-130. The survey's scientific value depends on this. Not controversial in this subfield, but it is an unproven background assumption in the strict sense.
  • domain assumption Maximum polarization fraction in diffuse ISM is about 20%.
    Taken from Planck results (ref 10, Section 4). This sets the target polarized intensity of 1 MJy/sr. If the cirrus confusion limit is 5 MJy/sr but polarization is lower than 20%, the detection threshold rises.

reviewed 2026-08-05 · how reviews work

0 comments
Cite this review

Pith. "Pith review of Mapping Magnetic Fields from Clouds to Cores with PRIMAger." pith.science (2026). https://pith.science/paper/LTUQ2T2H

@misc{pith2026250901796,
  author       = {Pith},
  title        = {Pith review of: Mapping Magnetic Fields from Clouds to Cores with PRIMAger},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/LTUQ2T2H}},
  note         = {Machine review of arXiv:2509.01796}
}
Share X Bluesky LinkedIn Reddit HN
abstract

High-resolution, wide-area mapping of magnetic field geometries within molecular clouds, and the star-forming filaments and cores within them, is crucial in order to understand the role of magnetic fields in the star formation process. We therefore propose an unbiased survey of star-forming molecular clouds within 0.5 kpc of the Earth in polarized light with the PRIMAger Polarimetry Imager. We will map magnetic fields over entire molecular clouds at linear resolutions of $\sim10^{-3}-10^{-2}$ pc ($\sim10^{3}-10^{4}$ au) in PRIMAger Bands PPI1 - PPI4, thereby resolving magnetic field structure both within individual star-forming filaments and cores, and in the most diffuse regions of molecular clouds. These multi-wavelength polarimetric observations will allow us to systematically investigate both the wide range of open questions about the role of magnetic fields in star formation and the evolution of the interstellar medium, and interstellar dust grain properties. The time required to map the area observed by the \textit{Herschel} Gould Belt Survey (160 deg$^{2}$) to the cirrus confusion limit in polarized light is 170 hours. This will give a 5-$\sigma$ detection of 20% polarized low-density cirrus emission, with surface brightnesses in polarized intensity of 1.0-2.4\,MJy/sr across the PRIMAger bands, and will ensure detection of polarized emission at all higher column densities. This time estimate can be simply scaled up in order to map magnetic fields in a larger sample of molecular clouds, including more distant regions of higher-mass star formation.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

166 extracted references · 76 canonical work pages · 2 internal anchors

  1. [1]

    Pattle , L

    K. Pattle , L. Fissel , M. Tahani , et al. , `` Magnetic Fields in Star Formation: from Clouds to Cores ,'' in Protostars and Planets VII , S. Inutsuka , Y. Aikawa , T. Muto , et al. , Eds., Astronomical Society of the Pacific Conference Series 534 , 193 (2023)

    2023

  2. [2]

    Beck , A

    R. Beck , A. Brandenburg , D. Moss , et al. , `` Galactic Magnetism: Recent Developments and Perspectives ,'' 34 , 155--206 (1996)

    1996

  3. [3]

    Tsukamoto , A

    Y. Tsukamoto , A. Maury , B. Commercon , et al. , `` The Role of Magnetic Fields in the Formation of Protostars, Disks, and Outflows ,'' in Protostars and Planets VII , S. Inutsuka , Y. Aikawa , T. Muto , et al. , Eds., Astronomical Society of the Pacific Conference Series 534 , 317 (2023)

    2023

  4. [4]

    J. D. Soler , `` Using Herschel and Planck observations to delineate the role of magnetic fields in molecular cloud structure ,'' 629 , A96 (2019)

    2019

  5. [5]

    P. C. Myers and S. Basu , `` Magnetic Properties of Star-forming Dense Cores ,'' 917 , 35 (2021)

    2021

  6. [6]

    T. C. Ching , D. Li , C. Heiles , et al. , `` An early transition to magnetic supercriticality in star formation ,'' 601 , 49--52 (2022)

    2022

  7. [7]

    Palmeirim , P

    P. Palmeirim , P. Andr \'e , J. Kirk , et al. , `` Herschel view of the Taurus B211/3 filament and striations: evidence of filamentary growth? ,'' 550 , A38 (2013)

    2013

  8. [8]

    T. G. S. Pillai , D. P. Clemens , S. Reissl , et al. , `` Magnetized filamentary gas flows feeding the young embedded cluster in Serpens South ,'' Nature Astronomy 4 , 1195--1201 (2020)

    2020

  9. [9]

    B. G. Andersson , A. Lazarian , and J. E. Vaillancourt , `` Interstellar Dust Grain Alignment ,'' 53 , 501--539 (2015)

    2015

  10. [10]

    Planck Collaboration , P. A. R. Ade , N. Aghanim , et al. , `` Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust ,'' 576 , A104 (2015)

    2015

  11. [11]

    Friberg , P

    P. Friberg , P. Bastien , D. Berry , et al. , `` POL-2: a polarimeter for the James-Clerk-Maxwell telescope ,'' in Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII , W. S. Holland and J. Zmuidzinas , Eds., Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series 9914 , 991403 (2016)

    2016

  12. [12]

    Ward-Thompson , K

    D. Ward-Thompson , K. Pattle , P. Bastien , et al. , `` First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt ,'' 842 , 66 (2017)

    2017

  13. [13]

    J. Liu , K. Qiu , D. Berry , et al. , `` The JCMT BISTRO Survey: The Magnetic Field in the Starless Core Ophiuchus C ,'' 877 , 43 (2019)

    2019

  14. [14]

    Coud \'e , P

    S. Coud \'e , P. Bastien , M. Houde , et al. , `` The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region ,'' 877 , 88 (2019)

    2019

  15. [15]

    Eswaraiah , D

    C. Eswaraiah , D. Li , R. S. Furuya , et al. , `` The JCMT BISTRO Survey: Revealing the Diverse Magnetic Field Morphologies in Taurus Dense Cores with Sensitive Submillimeter Polarimetry ,'' 912 , L27 (2021)

    2021

  16. [16]

    Karoly , D

    J. Karoly , D. Ward-Thompson , K. Pattle , et al. , `` The JCMT BISTRO Survey: Studying the Complex Magnetic Field of L43 ,'' 952 , 29 (2023)

    2023

  17. [17]

    Pattle , D

    K. Pattle , D. Ward-Thompson , D. Berry , et al. , `` The JCMT BISTRO Survey: The Magnetic Field Strength in the Orion A Filament ,'' 846 , 122 (2017)

    2017

  18. [18]

    Y. Doi , T. Hasegawa , R. S. Furuya , et al. , `` The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333 ,'' 899 , 28 (2020)

    2020

  19. [19]

    Kwon , K

    W. Kwon , K. Pattle , S. Sadavoy , et al. , `` B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main ,'' 926 , 163 (2022)

    2022

  20. [20]

    Arzoumanian , R

    D. Arzoumanian , R. S. Furuya , T. Hasegawa , et al. , `` Dust polarized emission observations of NGC 6334. BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network ,'' 647 , A78 (2021)

    2021

  21. [21]

    Hwang , J

    J. Hwang , J. Kim , K. Pattle , et al. , `` The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2 ,'' 941 , 51 (2022)

    2022

  22. [22]

    Ching , K

    T.-C. Ching , K. Qiu , D. Li , et al. , `` The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament ,'' 941 , 122 (2022)

    2022

  23. [23]

    The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center

    J. Karoly , D. Ward-Thompson , K. Pattle , et al. , `` The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center ,'' arXiv e-prints , arXiv:2502.11552 (2025)

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  24. [24]

    The JCMT BISTRO Survey: Unveiling the Magnetic Fields around Galactic Center

    M.-Z. Yang , S.-P. Lai , J. Karoly , et al. , `` The JCMT BISTRO Survey: Unveiling the Magnetic Fields around Galactic Center ,'' arXiv e-prints , arXiv:2503.05198 (2025)

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  25. [25]

    Tang , P

    Y.-W. Tang , P. T. P. Ho , P. M. Koch , et al. , `` Evolution of Magnetic Fields in High-Mass Star Formation: Linking Field Geometry and Collapse for the W51 e2/e8 Cores ,'' 700 , 251--261 (2009)

    2009

  26. [26]

    Zhang , K

    Q. Zhang , K. Qiu , J. M. Girart , et al. , `` Magnetic Fields and Massive Star Formation ,'' 792 , 116 (2014)

    2014

  27. [27]

    Ching , S.-P

    T.-C. Ching , S.-P. Lai , Q. Zhang , et al. , `` Magnetic Fields in the Massive Dense Cores of the DR21 Filament: Weakly Magnetized Cores in a Strongly Magnetized Filament ,'' 838 , 121 (2017)

    2017

  28. [28]

    S. I. Sadavoy , P. C. Myers , I. W. Stephens , et al. , `` Dust Polarization toward Embedded Protostars in Ophiuchus with ALMA. I. VLA 1623 ,'' 859 , 165 (2018)

    2018

  29. [29]

    Fern \'a ndez-L \'o pez , P

    M. Fern \'a ndez-L \'o pez , P. Sanhueza , L. A. Zapata , et al. , `` Magnetic Fields in Massive Star-forming Regions (MagMaR). I. Linear Polarized Imaging of the Ultracompact H II Region G5.89-0.39 ,'' 913 , 29 (2021)

    2021

  30. [30]

    Sanhueza , J

    P. Sanhueza , J. M. Girart , M. Padovani , et al. , `` Gravity-driven Magnetic Field at 1000 au Scales in High-mass Star Formation ,'' 915 , L10 (2021)

    2021

  31. [31]

    L. M. Fissel , P. A. R. Ade , F. E. Angil \`e , et al. , `` The balloon-borne large-aperture submillimeter telescope for polarimetry: BLAST-Pol ,'' in Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V , W. S. Holland and J. Zmuidzinas , Eds., Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Serie...

    2010

  32. [32]

    N. N. Gandilo , P. A. R. Ade , F. E. Angil \`e , et al. , `` Submillimeter Polarization Spectrum in the Vela C Molecular Cloud ,'' 824 , 84 (2016)

    2016

  33. [33]

    L. M. Fissel , P. A. R. Ade , F. E. Angil \`e , et al. , `` Relative Alignment between the Magnetic Field and Molecular Gas Structure in the Vela C Giant Molecular Cloud Using Low- and High-density Tracers ,'' 878 , 110 (2019)

    2019

  34. [34]

    Reinacher , F

    A. Reinacher , F. Graf , B. Greiner , et al. , `` The SOFIA Telescope in Full Operation ,'' Journal of Astronomical Instrumentation 7 , 1840007 (2018)

    2018

  35. [35]

    D. A. Harper , M. C. Runyan , C. D. Dowell , et al. , `` HAWC+, the Far-Infrared Camera and Polarimeter for SOFIA ,'' Journal of Astronomical Instrumentation 7 , 1840008--1025 (2018)

    2018

  36. [36]

    D. T. Chuss , B. G. Andersson , J. Bally , et al. , `` HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1 ,'' 872 , 187 (2019)

    2019

  37. [37]

    F. P. Santos , D. T. Chuss , C. D. Dowell , et al. , `` The Far-infrared Polarization Spectrum of Ophiuchi A from HAWC+/SOFIA Observations ,'' 882 , 113 (2019)

    2019

  38. [38]

    I. W. Stephens , P. C. Myers , C. Zucker , et al. , `` The Magnetic Field in the Milky Way Filamentary Bone G47 ,'' 926 , L6 (2022)

    2022

  39. [39]

    Andr \'e , A

    P. Andr \'e , A. Men'shchikov , S. Bontemps , et al. , `` From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt Survey ,'' 518 , L102 (2010)

    2010

  40. [40]

    K \"o nyves , P

    V. K \"o nyves , P. Andr \'e , A. Men'shchikov , et al. , `` A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey ,'' 584 , A91 (2015)

    2015

  41. [41]

    Ladjelate , P

    B. Ladjelate , P. Andr \'e , V. K \"o nyves , et al. , `` The Herschel view of the dense core population in the Ophiuchus molecular cloud ,'' 638 , A74 (2020)

    2020

  42. [42]

    Schneider , P

    N. Schneider , P. Andr \'e , V. K \"o nyves , et al. , `` What Determines the Density Structure of Molecular Clouds? A Case Study of Orion B with Herschel ,'' 766 , L17 (2013)

    2013

  43. [43]

    Kwon , Y

    J. Kwon , Y. Doi , M. Tamura , et al. , `` A First Look at BISTRO Observations of the Oph-A core ,'' 859 , 4 (2018)

    2018

  44. [44]

    Zucker , J

    C. Zucker , J. S. Speagle , E. F. Schlafly , et al. , `` A Large Catalog of Accurate Distances to Local Molecular Clouds: The Gaia DR2 Edition ,'' 879 , 125 (2019)

    2019

  45. [45]

    J. E. Pineda , D. Arzoumanian , P. Andre , et al. , `` From Bubbles and Filaments to Cores and Disks: Gas Gathering and Growth of Structure Leading to the Formation of Stellar Systems ,'' in Protostars and Planets VII , S. Inutsuka , Y. Aikawa , T. Muto , et al. , Eds., Astronomical Society of the Pacific Conference Series 534 , 233 (2023)

    2023

  46. [46]

    Motte , A

    F. Motte , A. Zavagno , S. Bontemps , et al. , `` Initial highlights of the HOBYS key program, the Herschel imaging survey of OB young stellar objects ,'' 518 , L77 (2010)

    2010

  47. [47]

    Molinari , E

    S. Molinari , E. Schisano , D. Elia , et al. , `` Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues. First data release for the inner Milky Way: +68 l -70 ,'' 591 , A149 (2016)

    2016

  48. [48]

    Zucker , C

    C. Zucker , C. Battersby , and A. Goodman , `` Physical Properties of Large-scale Galactic Filaments ,'' 864 , 153 (2018)

    2018

  49. [49]

    J. F. C. Wardle and P. P. Kronberg , `` The linear polarization of quasi-stellar radio sources at 3.71 and 11.1 centimeters. ,'' 194 , 249 (1974)

    1974

  50. [50]

    Montier , S

    L. Montier , S. Plaszczynski , F. Levrier , et al. , `` Polarization measurement analysis. II. Best estimators of polarization fraction and angle ,'' 574 , A136 (2015)

    2015

  51. [51]

    ``Commission 40: Radio astronomy (radio astronomie),'' Transactions of the International Astronomical Union 15 (2), 165–167 (1973)

    1973

  52. [52]

    Pattle , S.-P

    K. Pattle , S.-P. Lai , T. Hasegawa , et al. , `` JCMT BISTRO Survey Observations of the Ophiuchus Molecular Cloud: Dust Grain Alignment Properties Inferred Using a Ricean Noise Model ,'' 880 , 27 (2019)

    2019

  53. [53]

    D. C. B. Whittet , J. H. Hough , A. Lazarian , et al. , `` The Efficiency of Grain Alignment in Dense Interstellar Clouds: a Reassessment of Constraints from Near-Infrared Polarization ,'' 674 , 304--315 (2008)

    2008

  54. [54]

    J. D. Soler , P. Hennebelle , P. G. Martin , et al. , `` An Imprint of Molecular Cloud Magnetization in the Morphology of the Dust Polarized Emission ,'' 774 , 128 (2013)

    2013

  55. [55]

    L \^e , L

    N. L \^e , L. N. Tram , A. Karska , et al. , `` Mapping and characterizing magnetic fields in the Rho Ophiuchus-A molecular cloud with SOFIA/HAWC+ ,'' 690 , A191 (2024)

    2024

  56. [56]

    Reissl , S

    S. Reissl , S. Wolf , and R. Brauer , `` Radiative transfer with POLARIS. I. Analysis of magnetic fields through synthetic dust continuum polarization measurements ,'' 593 , A87 (2016)

    2016

  57. [57]

    Palau , N

    A. Palau , N. Hu \'e lamo , D. Barrado , et al. , `` Observations of pre- and proto-brown dwarfs in nearby clouds: Paving the way to further constraining theories of brown dwarf formation ,'' 99 , 101711 (2024)

    2024

  58. [58]

    Di Francesco , J

    J. Di Francesco , J. Keown , C. Fallscheer , et al. , `` Herschel Gould Belt Survey Observations of Dense Cores in the Cepheus Flare Clouds ,'' 904 , 172 (2020)

    2020

  59. [59]

    Davis , `` The Strength of Interstellar Magnetic Fields ,'' Physical Review 81 , 890--891 (1951)

    L. Davis , `` The Strength of Interstellar Magnetic Fields ,'' Physical Review 81 , 890--891 (1951)

    1951

  60. [60]

    Chandrasekhar and E

    S. Chandrasekhar and E. Fermi , `` Magnetic Fields in Spiral Arms. ,'' 118 , 113 (1953)

    1953

  61. [61]

    R. H. Hildebrand , L. Kirby , J. L. Dotson , et al. , `` Dispersion of Magnetic Fields in Molecular Clouds. I ,'' 696 , 567--573 (2009)

    2009

  62. [62]

    Houde , J

    M. Houde , J. E. Vaillancourt , R. H. Hildebrand , et al. , `` Dispersion of Magnetic Fields in Molecular Clouds. II. ,'' 706 , 1504--1516 (2009)

    2009

  63. [63]

    Lazarian , K

    A. Lazarian , K. H. Yuen , and D. Pogosyan , `` Magnetic Field Strength from Turbulence Theory. I. Using Differential Measure Approach ,'' 935 , 77 (2022)

    2022

  64. [64]

    Skalidis and K

    R. Skalidis and K. Tassis , `` High-accuracy estimation of magnetic field strength in the interstellar medium from dust polarization ,'' 647 , A186 (2021)

    2021

  65. [65]

    J. Liu , Q. Zhang , B. Commer c on , et al. , `` Calibrating the Davis-Chandrasekhar-Fermi Method with Numerical Simulations: Uncertainties in Estimating the Magnetic Field Strength from Statistics of Field Orientations ,'' 919 , 79 (2021)

    2021

  66. [66]

    P. S. Li , E. Lopez-Rodriguez , H. Ajeddig , et al. , `` Mapping the magnetic field in the Taurus/B211 filamentary cloud with SOFIA HAWC + and comparing with simulation ,'' 510 , 6085--6109 (2022)

    2022

  67. [67]

    Pillai , J

    T. Pillai , J. Kauffmann , J. C. Tan , et al. , `` Magnetic Fields in High-mass Infrared Dark Clouds ,'' 799 , 74 (2015)

    2015

  68. [68]

    Cho and H

    J. Cho and H. Yoo , `` A Technique for Constraining the Driving Scale of Turbulence and a Modified Chandrasekhar-Fermi Method ,'' 821 , 21 (2016)

    2016

  69. [69]

    Hwang , J

    J. Hwang , J. Kim , K. Pattle , et al. , `` The JCMT BISTRO Survey: The Distribution of Magnetic Field Strengths toward the OMC-1 Region ,'' 913 , 85 (2021)

    2021

  70. [70]

    R. M. Crutcher , D. J. Nutter , D. Ward-Thompson , et al. , `` SCUBA Polarization Measurements of the Magnetic Field Strengths in the L183, L1544, and L43 Prestellar Cores ,'' 600 , 279--285 (2004)

    2004

  71. [71]

    Chen , P

    C.-Y. Chen , P. K. King , Z.-Y. Li , et al. , `` A new method to trace three-dimensional magnetic field structure within molecular clouds using dust polarization ,'' 485 , 3499--3513 (2019)

    2019

  72. [72]

    Hu and A

    Y. Hu and A. Lazarian , `` Probing 3D magnetic fields - I. Polarized dust emission ,'' 519 , 3736--3748 (2023)

    2023

  73. [73]

    P. M. Koch , Y.-W. Tang , and P. T. P. Ho , `` Magnetic Field Strength Maps for Molecular Clouds: A New Method Based on a Polarization-Intensity Gradient Relation ,'' 747 , 79 (2012)

    2012

  74. [74]

    P. M. Koch , Y.-W. Tang , P. T. P. Ho , et al. , `` The Importance of the Magnetic Field from an SMA-CSO-combined Sample of Star-forming Regions ,'' 797 , 99 (2014)

    2014

  75. [75]

    di Francesco , N

    J. di Francesco , N. J. Evans , II, P. Caselli , et al. , `` An Observational Perspective of Low-Mass Dense Cores I: Internal Physical and Chemical Properties ,'' in Protostars and Planets V , B. Reipurth , D. Jewitt , and K. Keil , Eds., 17 (2007)

    2007

  76. [76]

    E. C. Ostriker , J. M. Stone , and C. F. Gammie , `` Density, Velocity, and Magnetic Field Structure in Turbulent Molecular Cloud Models ,'' 546 , 980--1005 (2001)

    2001

  77. [77]

    A. J. Rigby , T. J. T. Moore , R. Plume , et al. , `` CHIMPS: the ^ 13 CO/C ^ 18 O (J = 3 2) Heterodyne Inner Milky Way Plane Survey ,'' 456 , 2885--2899 (2016)

    2016

  78. [78]

    Schuller , T

    F. Schuller , T. Csengeri , J. S. Urquhart , et al. , `` SEDIGISM: Structure, excitation, and dynamics of the inner Galactic interstellar medium ,'' 601 , A124 (2017)

    2017

  79. [79]

    J. R. Goicoechea , C. H. M. Pabst , S. Kabanovic , et al. , `` Molecular globules in the Veil bubble of Orion. IRAM 30 m ^ 12 CO, ^ 13 CO, and C ^ 18 O (2-1) expanded maps of Orion A ,'' 639 , A1 (2020)

    2020

  80. [80]

    Park , M

    G. Park , M. J. Currie , H. S. Thomas , et al. , `` ^ 12 CO (3-2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release ,'' 264 , 16 (2023)

    2023

Showing first 80 references.

This paper was first reviewed by deepseek-v4-flash on August 5, 2026.