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REVIEW 2 major objections 5 minor 231 references

An automated Python pipeline recovers reliable stellar polarization from dual-beam images for both isolated stars and crowded fields.

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 →

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T0 review · grok-4.5

2026-07-12 04:16 UTC pith:MTZUTTQX

load-bearing objection Solid, usable AIMPOL pipeline with multi-epoch validation and public code; incremental but fills a real gap for that community. the 2 major comments →

arxiv 2607.03185 v1 pith:MTZUTTQX submitted 2026-07-03 astro-ph.IM

DHARA: Data Handling and Automated Reduction pipeline for AIMPOL

Namita Uppal , Shashikiran Ganesh , Santosh Joshi , Dmitry Blinov , Konstantinos Tassis , Sadhana Singh This is my paper
classification astro-ph.IM
keywords techniques: polarimetricmethods: observationalinstrumentation: polarimetersdata reduction pipelinedual-beam polarimetryStokes parametersAIMPOL
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.

DHARA is an end-to-end reduction pipeline for dual-beam optical polarimeters that turns raw CCD frames into Stokes parameters, polarization degree, and position angle with uncertainties. Built for AIMPOL on a 1-m telescope, it first calibrates and stacks frames by half-wave-plate angle, then pairs each star’s ordinary and extraordinary images—interactively for single sources, via a one-time offset plus Gaia astrometry for crowded fields—and performs aperture photometry that can choose the least-contaminated radius from a curve of growth. Instrumental polarization and angle zero-point are removed using standard stars observed each run. On 26 polarized standards spanning 2017–2025 and on stars in the Alessi 1 open cluster, the pipeline values match published results within 2σ. The authors argue that this removes the bottleneck of manual reduction and makes dual-beam polarimetry practical for larger surveys of the northern Galactic disk and similar instruments that place both beams on one detector.

Core claim

The paper establishes that a single automated workflow—bias calibration, half-wave-plate-aware stacking, fixed-offset e/o-ray pairing, multi-aperture photometry, and instrumental Stokes correction—yields polarization parameters for AIMPOL data that agree with literature values for both isolated standard stars and stars in a crowded open-cluster field within 2σ uncertainties.

What carries the argument

Constant e-ray/o-ray image separation (~30 pixels, stable to ±1 pixel across the CCD), measured once from a single pair and applied field-wide (with optional re-centering), so that relative photometry and the modulation factor R(α) can be computed automatically for every star.

Load-bearing premise

The ordinary and extraordinary images of every star stay a fixed number of pixels apart across the whole detector, so one measured offset can safely pair all sources.

What would settle it

Measure e/o separations across a dense open-cluster field under changed focus or temperature; if many pairs deviate by more than ~1–2 pixels from the adopted constant offset, the automated pairing fails and Stokes parameters become systematically biased.

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

If this is right

  • Crowded dual-beam fields that previously required manual star-by-star selection can now be reduced in minutes to science-ready catalogs.
  • Any dual-channel polarimeter that records both beams on one CCD with a stable spatial offset can reuse the same pairing-plus-photometry core.
  • Uniform, reproducible Stokes catalogs become feasible for multi-epoch campaigns that previously suffered user-dependent reductions.
  • Future versions that add PSF photometry can recover stars currently discarded because of aperture overlap.

Where Pith is reading between the lines

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

  • The same constant-offset pairing idea could be ported to other small-aperture dual-beam systems that currently lack public pipelines, accelerating northern-sky polarization mapping.
  • Because instrumental Stokes terms and angle zero-points must still be re-measured each run, the pipeline does not remove the need for regular standard-star observations; it only standardizes their application.
  • If field-dependent optical distortions grow with aging optics or a future detector swap, the constant-offset assumption would need to be replaced by a position-dependent distortion map.

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

2 major / 5 minor

Summary. The manuscript presents DHARA, a Python-based automated reduction pipeline for dual-beam optical linear polarimetry with AIMPOL. It performs bias calibration, optional frame alignment/stacking, e/o-ray pair identification (interactive for single sources; astrometry.net + Gaia + fixed separation for crowded fields), aperture photometry (fixed 3 imes FWHM or multi-aperture curve-of-growth), Stokes-parameter fitting via the modulation factor R(α), instrumental polarization and zero-angle corrections, Ricean debiasing of P, and angle-uncertainty treatment following standard prescriptions. Validation uses 26 polarized standards observed 2017–2025 (Table 1) and a re-reduction of the published Alessi 1 open-cluster field; both agree with literature values within 2σ. Source code is released on GitHub/Zenodo. The pipeline is stated to be adaptable to any dual-channel imager that records e- and o-rays on a single CCD.

Significance. Automated, reproducible reduction for dual-beam polarimeters remains scarce, especially for instruments used by the Indian community. DHARA fills a practical gap for AIMPOL and similar systems, with multi-epoch standard-star validation, an independent crowded-field test, explicit instrumental-correction protocol, and public code. These strengths make the work useful for ongoing and future stellar-polarization surveys of the northern Galactic disk. The constant e/o-separation assumption is load-bearing but is already tested on a dense field (Appendix C) and supported by the absence of systematic outliers in the validation samples.

major comments (2)
  1. The Alessi 1 comparison (Sect. 4.2, Fig. 5) applies a uniform 0.05% zero-point shift to the pipeline results before fitting. While the authors attribute this to differences in instrumental-polarization estimation, the unshifted residuals and the origin of the offset should be shown explicitly (or the shift omitted) so that the reader can judge the raw agreement. After that clarification the 1σ consistency claim remains defensible.
  2. Sect. 3.2 / Appendix C: the constant e/o separation (mean 30.59 pix, ±1 pix, no radial trend) is validated on one open-cluster field. Because residual field-dependent distortions or focus changes larger than this bound would systematically mis-pair sources, a brief statement of the tested range of seeing/focus conditions (or a second field) would strengthen the claim that the assumption holds for typical AIMPOL data.
minor comments (5)
  1. Eq. (6) writes the instrumental Stokes vector as [q_inst, u_inst] but the surrounding text twice uses “qinst, qinst”; correct the typo.
  2. Fig. 3 caption and body refer to HD 344776 / HD 322776 inconsistently; standardize the object name.
  3. Table 1 header uses ψ_inst while the continuation page uses Δθ; unify the column label and clarify that the quantity is the measured zero-angle offset for that epoch.
  4. The abstract and introduction state that the pipeline is “readily adaptable” to any dual-channel imager; a short paragraph listing the configuration parameters a new user must supply (HWP sequence, plate scale, typical e/o separation) would make that claim more concrete.
  5. A few typographical issues remain (e.g., “di fferent”, “e ffective”, “o ffset”, missing spaces after periods in the abstract footnote). A careful copy-edit pass is recommended.

Circularity Check

0 steps flagged

No circularity: pipeline validation against external standards and prior reductions is independent of the reduction equations themselves.

full rationale

DHARA is a methodological software paper whose load-bearing claim is empirical agreement (within 2σ) of its output Stokes parameters, P and θ with literature values for 26 polarized standards and with a prior reduction of the same Alessi 1 frames. The Stokes reduction follows the standard dual-beam formalism of Ramaprakash et al. (1998) (Appendix A, Eqs. A1–A6 and pipeline Eqs. 1–11); instrumental q_inst, u_inst and ψ_inst are measured each epoch from independent unpolarized and polarized standards and then applied (Sect. 3.4). No equation defines a quantity in terms of itself, no fitted free parameter is re-labeled a “prediction,” and no uniqueness theorem or ansatz is imported via self-citation to force the result. The Alessi 1 comparison uses the identical raw data previously reduced by a co-author with IRAF, but the paper reports the 0.05 % zero-point offset explicitly and tests slope consistency after the shift; this is ordinary pipeline cross-check, not circular derivation. The constant e/o-ray separation assumption is independently verified on a dense field (Appendix C). The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 0 invented entities

The central claim rests on standard dual-beam polarimetry mathematics (Ramaprakash et al. 1998), the empirically verified constant e/o separation, nightly instrumental-polarization measurements from standards, and conventional aperture-photometry and Ricean-debiasing practices. No new physical entities are postulated; free parameters are the usual per-epoch instrumental corrections and user-chosen photometric apertures.

free parameters (4)
  • q_inst, u_inst (instrumental Stokes parameters) = epoch-dependent (typically few ×0.1 %)
    Measured each night from unpolarized standards and subtracted in q–u space; values are epoch-dependent free parameters supplied as pipeline presets.
  • ψ_inst (zero-angle offset) = epoch-dependent (≈70–90° range in Table 1)
    Average difference between measured and literature polarization angles of polarized standards; applied as a rotation matrix each epoch.
  • aperture radius (or curve-of-growth selection) = 1–3 × FWHM
    Chosen as 3× FWHM or the radius where polarization saturates; user- or algorithm-selected free parameter that affects final P and θ.
  • e/o separation vector = ≈30.59 pixels
    Measured once from a bright pair and applied field-wide; treated as constant but is an empirical free parameter of the instrument configuration.
axioms (4)
  • domain assumption The dual-beam modulation factor R(α) = (I_e/I_o – 1)/(I_e/I_o + 1) equals p cos(2θ – 4α) after response-factor correction (Eqs. A3–A6).
    Taken directly from Ramaprakash et al. (1998) and used throughout Sect. 3.4 and Appendix A; standard for Wollaston-prism polarimeters.
  • domain assumption e-ray and o-ray images of every source are separated by a fixed vector (within ±1 pixel) across the entire CCD.
    Invoked in Sect. 3.2 for crowded-field pairing; empirically checked in Appendix C but remains an instrument-specific assumption.
  • domain assumption Flat-field correction is unnecessary because pixel-to-pixel sensitivity is absorbed into the Fo/Fe response ratio measured from the four HWP positions.
    Stated in Sect. 3.1; follows the classic dual-beam design but is not re-derived here.
  • standard math Ricean bias is adequately removed by the asymptotic estimator P = sqrt(p_obs² – σ_p²) and angle uncertainties follow Naghizadeh-Khouei & Clarke (1993).
    Standard statistical corrections applied in Sect. 3.4; not re-proved.

pith-pipeline@v1.1.0-grok45 · 26486 in / 2986 out tokens · 31272 ms · 2026-07-12T04:16:15.626068+00:00 · methodology

0 comments
read the original abstract

We present an automated data-reduction and analysis for optical linear polarimetric data obtained from a dual-beam polarimeter. The pipeline is optimized for observations acquired with the ARIES Imaging POLarimeter mounted at the Cassegrain focus of the 1.04-m Sampurnanand Telescope at ARIES. It is implemented using interactive Python routines that process raw images to derive the Stokes parameters, from which the degree of polarization and polarization angle are computed along with their uncertainties. The pipeline framework is designed to handle the reduction of both single-source and crowded-field observations. The identification of extraordinary (e-ray) and ordinary (o-ray) image pairs is a crucial step and is performed using different strategies for single-source and crowded-field data, while subsequent stages, such as photometric and polarimetric analysis, follow a common procedure. We validate the pipeline using observations of polarized standard stars acquired over multiple epochs between 2017 to 2025, and compare the results with values reported in the literature. To demonstrate the applicability of the pipeline to crowded-field observations, we apply it to polarimetric data of the Alessi~1 open cluster and compare with previously published results derived using traditional reduction methods. In both cases, the polarization parameters derived using the pipeline agree with literature values within $2\sigma$ uncertainties. Although developed for AIMPOL, the pipeline is readily adaptable to any dual-channel imaging polarimeter in which the e-ray and o-ray images are recorded in a FITS image from a single CCD.

Figures

Figures reproduced from arXiv: 2607.03185 by Dmitry Blinov, Konstantinos Tassis, Namita Uppal, Sadhana Singh, Santosh Joshi, Shashikiran Ganesh.

Figure 2
Figure 2. Figure 2: The detailed descriptions of the different tasks are provided in the following subsections. 3.1 CCD frame calibration The basic CCD calibration procedure begins with the construction of a master bias frame. All bias (zero￾exposure) images were median-combined to generate the master bias, which is then subtracted from each science frame. Flat-field correction is not required for AIMPOL observations, as the … view at source ↗

discussion (0)

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Reference graph

Works this paper leans on

231 extracted references · 80 canonical work pages · 52 internal anchors

  1. [1]

    Polarization of active galactic nuclei with significant VLBI-Gaia displacements

    Polarization of active galactic nuclei with significant VLBI-Gaia displacements. A&A , keywords =. doi:10.1051/0004-6361/202451186 , archivePrefix =. 2409.12226 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202451186

  2. [2]

    Discovery of X-ray polarization angle rotation in the jet from blazar Mrk 421. Nat. Astron. , keywords =. doi:10.1038/s41550-023-02032-7 , archivePrefix =. 2305.13497 , primaryClass =

    Pith/arXiv arXiv doi:10.1038/s41550-023-02032-7

  3. [3]

    Optical polarization from colliding stellar stream shocks in a tidal disruption event

    Optical polarization from colliding stellar stream shocks in a tidal disruption event. Science , keywords =. doi:10.1126/science.abj9570 , archivePrefix =. 2208.14465 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.abj9570

  4. [4]

    The Guitar's Magnetic Field Revealed by Starlight Polarization

    The Guitar Filament's Magnetic Field Revealed by Starlight Polarization. ApJ , keywords =. doi:10.3847/1538-4357/adafa8 , archivePrefix =. 2501.07577 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/adafa8

  5. [5]

    PRIMA General Observer Science Book Volume 2 , year = 2025, editor =

    Tracing Cloud Formation and Evolution Through 3D Magnetic Field Mapping. PRIMA General Observer Science Book Volume 2 , year = 2025, editor =

    2025

  6. [6]

    Astronomy Letters , keywords =

    Nature of the Eclipsing Polar 1RXS J184542.4+483134. Astronomy Letters , keywords =. doi:10.1134/S1063773723110051 , adsurl =

    work page doi:10.1134/s1063773723110051

  7. [7]

    Optical Linear Polarization toward the Open Star Cluster Casado Alessi 1

    Optical Linear Polarization toward the Open Star Cluster Casado Alessi 1. AJ , keywords =. doi:10.3847/1538-3881/ab6608 , archivePrefix =. 2001.11227 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/ab6608 2001

  8. [8]

    Magnetic Seismology of Interstellar Gas Clouds: Unveiling a Hidden Dimension

    Magnetic seismology of interstellar gas clouds: Unveiling a hidden dimension. Science , keywords =. doi:10.1126/science.aao1185 , archivePrefix =. 1805.03664 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.aao1185

  9. [9]

    AJ , keywords =

    Mimir: A Near-Infrared Wide-Field Imager, Spectrometer and Polarimeter. AJ , keywords =. doi:10.1086/524775 , adsurl =

    work page doi:10.1086/524775

  10. [10]

    The Galactic Plane Infrared Polarization Survey (GPIPS): Data Release 4

    The Galactic Plane Infrared Polarization Survey (GPIPS): Data Release 4. ApJS , keywords =. doi:10.3847/1538-4365/ab9f30 , archivePrefix =. 2006.15203 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ab9f30 2006

  11. [11]

    Ground-based and Airborne Instrumentation for Astronomy X , year = 2024, editor =

    Improving polarimetric accuracy of RoboPol to < 0.05 \. Ground-based and Airborne Instrumentation for Astronomy X , year = 2024, editor =. doi:10.1117/12.3021523 , adsurl =

    work page doi:10.1117/12.3021523 2024

  12. [12]

    ApJ , keywords =

    Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds. ApJ , keywords =. doi:10.1086/305772 , archivePrefix =. astro-ph/9710327 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/305772

  13. [13]

    ApJ , keywords =

    Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination. ApJ , keywords =. doi:10.3847/1538-4357/acf4a1 , archivePrefix =. 2306.03926 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/acf4a1

  14. [14]

    A new, large-scale map of interstellar reddening derived from HI emission

    A New, Large-scale Map of Interstellar Reddening Derived from H I Emission. ApJ , keywords =. doi:10.3847/1538-4357/aa84af , archivePrefix =. 1706.00011 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa84af

  15. [15]

    Planck intermediate results. XLVIII. Disentangling Galactic dust emission and cosmic infrared background anisotropies. A&A , keywords =. doi:10.1051/0004-6361/201629022 , archivePrefix =. 1605.09387 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201629022

  16. [16]

    VLT Spectropolarimetry of the optical transient in NGC300. Evidence for asymmetry in the circumstellar dust

    VLT spectropolarimetry of the optical transient in NGC 300. Evidence of asymmetry in the circumstellar dust. A&A , keywords =. doi:10.1051/0004-6361/200913083 , archivePrefix =. 0908.0942 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200913083

  17. [17]

    ApJS , keywords =

    The Galactic Plane Infrared Polarization Survey (GPIPS). ApJS , keywords =. doi:10.1088/0067-0049/200/2/19 , adsurl =

    doi:10.1088/0067-0049/200/2/19

  18. [18]

    The astrometric solution

    Gaia Early Data Release 3. The astrometric solution. A&A , keywords =. doi:10.1051/0004-6361/202039709 , archivePrefix =. 2012.03380 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202039709 2012

  19. [19]

    Tracing the asymmetry across the disc

    The Outer spiral arm of the Milky Way using red clump stars. Tracing the asymmetry across the disc. A&A , keywords =. doi:10.1051/0004-6361/202244548 , adsurl =

    doi:10.1051/0004-6361/202244548

  20. [20]

    Summary of the contents and survey properties

    Gaia Data Release 2. Summary of the contents and survey properties. A&A , keywords =. doi:10.1051/0004-6361/201833051 , archivePrefix =. 1804.09365 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201833051

  21. [21]

    Summary of the content and survey properties

    Gaia Data Release 3. Summary of the content and survey properties. A&A , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202243940

  22. [22]

    Estimating Distance from Parallaxes. IV. Distances to 1.33 Billion Stars in Gaia Data Release 2. AJ , keywords =. doi:10.3847/1538-3881/aacb21 , archivePrefix =. 1804.10121 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-3881/aacb21

  23. [23]

    Estimating Distances from Parallaxes. V. Geometric and Photogeometric Distances to 1.47 Billion Stars in Gaia Early Data Release 3. AJ , keywords =. doi:10.3847/1538-3881/abd806 , archivePrefix =. 2012.05220 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-3881/abd806 2012

  24. [24]

    A&A , keywords =

    Gaia-2MASS 3D maps of Galactic interstellar dust within 3 kpc. A&A , keywords =. doi:10.1051/0004-6361/201834695 , archivePrefix =. 1902.04116 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201834695 1902

  25. [25]

    A&A , keywords =

    Updated Gaia-2MASS 3D maps of Galactic interstellar dust. A&A , keywords =. doi:10.1051/0004-6361/202142846 , archivePrefix =. 2203.01627 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202142846

  26. [26]

    A&A , keywords =

    Three-dimensional extinction maps: Inverting inter-calibrated extinction catalogues. A&A , keywords =. doi:10.1051/0004-6361/202243319 , archivePrefix =. 2205.09087 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202243319

  27. [27]

    ApJ , keywords =

    A 3D Dust Map Based on Gaia, Pan-STARRS 1, and 2MASS. ApJ , keywords =. doi:10.3847/1538-4357/ab5362 , archivePrefix =. 1905.02734 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/ab5362 1905

  28. [28]

    A&A , keywords =

    A parsec-scale Galactic 3D dust map out to 1.25 kpc from the Sun. A&A , keywords =. doi:10.1051/0004-6361/202347628 , archivePrefix =. 2308.01295 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202347628

  29. [29]

    Two-component Magnetic Field along the Line of Sight to the Perseus Molecular Cloud: Contribution of the Foreground Taurus Molecular Cloud

    Two-component Magnetic Field along the Line of Sight to the Perseus Molecular Cloud: Contribution of the Foreground Taurus Molecular Cloud. ApJ , keywords =. doi:10.3847/1538-4357/abfcc5 , archivePrefix =. 2104.11932 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/abfcc5

  30. [30]

    Detailed 3D structure of OrionA in dust with Gaia DR2

    Detailed 3D structure of Orion A in dust with Gaia DR2. A&A , keywords =. doi:10.1051/0004-6361/202038708 , archivePrefix =. 2007.01331 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202038708 2007

  31. [31]

    Orion A's complete 3D magnetic field morphology

    Orion A's complete 3D magnetic field morphology. A&A , keywords =. doi:10.1051/0004-6361/202243322 , archivePrefix =. 2203.08763 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202243322

  32. [32]

    Mapping the Magnetic Interstellar Medium in Three Dimensions Over the Full Sky with Neutral Hydrogen

    Mapping the Magnetic Interstellar Medium in Three Dimensions over the Full Sky with Neutral Hydrogen. ApJ , keywords =. doi:10.3847/1538-4357/ab5803 , archivePrefix =. 1909.11673 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab5803 1909

  33. [33]

    JCMT BISTRO Observations: Magnetic Field Morphology of Bubbles Associated with NGC 6334

    JCMT BISTRO Observations: Magnetic Field Morphology of Bubbles Associated with NGC 6334. ApJ , keywords =. doi:10.3847/1538-4357/acac81 , archivePrefix =. 2212.10884 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/acac81

  34. [34]

    Protostars and Planets VII , year = 2023, editor =

    Magnetic Fields in Star Formation: from Clouds to Cores. Protostars and Planets VII , year = 2023, editor =. doi:10.48550/arXiv.2203.11179 , archivePrefix =. 2203.11179 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2203.11179 2023

  35. [35]

    Starlight-polarization-based tomography of the magnetized interstellar medium: PASIPHAE's line-of-sight inversion method

    Starlight-polarization-based tomography of the magnetized ISM: PASIPHAE's line-of-sight inversion method. A&A , keywords =. doi:10.1051/0004-6361/202244625 , archivePrefix =. 2208.02278 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202244625

  36. [36]

    Magnetic fields in spiral galaxies. A&A Rev. , keywords =. doi:10.1007/s00159-015-0084-4 , archivePrefix =. 1509.04522 , primaryClass =

    Pith/arXiv arXiv doi:10.1007/s00159-015-0084-4

  37. [37]

    A&A , keywords =

    Radio observational constraints on Galactic 3D-emission models. A&A , keywords =. doi:10.1051/0004-6361:20078671 , archivePrefix =. 0711.1572 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361:20078671

  38. [38]

    Planets, Stars and Stellar Systems

    Magnetic Fields in Galaxies. Planets, Stars and Stellar Systems. Volume 5: Galactic Structure and Stellar Populations , year = 2013, editor =. doi:10.1007/978-94-007-5612-0_13 , adsurl =

    doi:10.1007/978-94-007-5612-0_13 2013

  39. [39]

    Antisymmetry in the Faraday Rotation Sky Caused by a Nearby Magnetized Bubble

    Antisymmetry in the Faraday Rotation Sky Caused by a Nearby Magnetized Bubble. ApJL , keywords =. doi:10.1088/2041-8205/724/1/L48 , archivePrefix =. 1011.0341 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/724/1/l48 2041

  40. [40]

    ApJS , keywords =

    Arecibo 430 MHz Pulsar Polarimetry: Faraday Rotation Measures and Morphological Classifications. ApJS , keywords =. doi:10.1086/379802 , archivePrefix =. astro-ph/0310073 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/379802

  41. [41]

    A new method to determine the line-of-sight magnetic field structure in molecular clouds

    Helical magnetic fields in molecular clouds?. A new method to determine the line-of-sight magnetic field structure in molecular clouds. A&A , keywords =. doi:10.1051/0004-6361/201732219 , archivePrefix =. 1802.07831 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201732219

  42. [42]

    Structure in the Magnetic Field of the Milky Way Disk and Halo traced by Faraday Rotation

    Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation. ApJ , keywords =. doi:10.3847/1538-4357/ac94ce , archivePrefix =. 2209.10819 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac94ce

  43. [43]

    Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust. A&A , keywords =. doi:10.1051/0004-6361/201424082 , archivePrefix =. 1405.0871 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201424082

  44. [44]

    Science , year = 1949, month = feb, volume =

    Polarization of Light from Distant Stars by Interstellar Medium. Science , year = 1949, month = feb, volume =. doi:10.1126/science.109.2825.165 , adsurl =

    doi:10.1126/science.109.2825.165 1949

  45. [45]

    Science , year = 1949, month = feb, volume =

    Observations of the Polarized Light from Stars. Science , year = 1949, month = feb, volume =. doi:10.1126/science.109.2825.166 , adsurl =

    doi:10.1126/science.109.2825.166 1949

  46. [46]

    ARA&A , year = 2015, month = aug, volume =

    Interstellar Dust Grain Alignment. ARA&A , year = 2015, month = aug, volume =. doi:10.1146/annurev-astro-082214-122414 , adsurl =

    doi:10.1146/annurev-astro-082214-122414 2015

  47. [47]

    ApJ , keywords =

    A New Model of the Galactic Magnetic Field. ApJ , keywords =. doi:10.1088/0004-637X/757/1/14 , archivePrefix =. 1204.3662 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/757/1/14

  48. [48]

    Galaxies , keywords =

    Practical Modeling of Large-Scale Galactic Magnetic Fields: Status and Prospects. Galaxies , keywords =. doi:10.3390/galaxies7020052 , archivePrefix =. 1904.12689 , primaryClass =

    Pith/arXiv arXiv doi:10.3390/galaxies7020052 1904

  49. [49]

    Linear polarization study of open clusters towards the anticenter direction: Signature of the spiral arms

    Linear polarization study of open clusters in the anticenter direction: Signature of the spiral arms. A&A , keywords =. doi:10.1051/0004-6361/202449537 , archivePrefix =. 2408.05603 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202449537

  50. [50]

    The annals of statistics , pages=

    Estimating the dimension of a model , author=. The annals of statistics , pages=. 1978 , publisher=

    1978

  51. [51]

    IEEE Transactions on Automatic Control , keywords =

    A New Look at the Statistical Model Identification. IEEE Transactions on Automatic Control , keywords =

  52. [52]

    MNRAS , keywords =

    DYNESTY: a dynamic nested sampling package for estimating Bayesian posteriors and evidences. MNRAS , keywords =. doi:10.1093/mnras/staa278 , archivePrefix =. 1904.02180 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/staa278 1904

  53. [53]

    Observational Constraints on the Physical Properties of Interstellar Dust in the Post-Planck Era

    Observational Constraints on the Physical Properties of Interstellar Dust in the Post-Planck Era. ApJ , keywords =. doi:10.3847/1538-4357/abc8f1 , archivePrefix =. 2009.00018 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/abc8f1 2009

  54. [54]

    The first degree-scale starlight-polarization-based tomography map of the magnetized interstellar medium

    The first degree-scale starlight-polarization-based tomography map of the magnetized interstellar medium. A&A , keywords =. doi:10.1051/0004-6361/202349015 , archivePrefix =. 2404.10821 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202349015

  55. [55]

    ApJ , keywords =

    Demonstration of Magnetic Field Tomography with Starlight Polarization toward a Diffuse Sightline of the ISM. ApJ , keywords =. doi:10.3847/1538-4357/aafdb2 , archivePrefix =. 1809.09804 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aafdb2

  56. [56]

    Tomographic Imaging of the Sagittarius Spiral Arm's Magnetic Field Structure

    Tomographic Imaging of the Sagittarius Spiral Arm's Magnetic Field Structure. ApJ , keywords =. doi:10.3847/1538-4357/ad0fe2 , archivePrefix =. 2311.13054 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ad0fe2

  57. [57]

    Interstellar Polarization Survey. V. Galactic Magnetic Field Tomography of the Spiral Arms Using Optical and Near-infrared Starlight Polarization. AJ , keywords =. doi:10.3847/1538-3881/addecc , archivePrefix =. 2506.01564 , primaryClass =

    doi:10.3847/1538-3881/addecc

  58. [58]

    A compilation of optical starlight polarization catalogs

    A Compilation of Optical Starlight Polarization Catalogs. ApJS , keywords =. doi:10.3847/1538-4365/ad8b21 , archivePrefix =. 2307.05752 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/ad8b21

  59. [59]

    Interstellar Polarization Survey. II. General Interstellar Medium. AJ , keywords =. doi:10.3847/1538-3881/aca8fd , archivePrefix =. 2212.05985 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aca8fd

  60. [60]

    arXiv e-prints , keywords =

    PASIPHAE: A high-Galactic-latitude, high-accuracy optopolarimetric survey. arXiv e-prints , keywords =. doi:10.48550/arXiv.1810.05652 , archivePrefix =. 1810.05652 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1810.05652

  61. [61]

    Astronomical Polarimetry: Current Status and Future Directions , year = 2005, editor =

    A Southern Optical/Infrared Survey of Interstellar Polarization. Astronomical Polarimetry: Current Status and Future Directions , year = 2005, editor =

    2005

  62. [62]

    A Comparative Study of Dust Grain Polarisation Efficiencies in the Interstellar and Intracluster Mediums towards Anti-Center Galaxy

    A comparative study of dust grain polarization efficiencies in the interstellar and intracluster mediums towards anticentre galaxy. MNRAS , keywords =. doi:10.1093/mnras/stae749 , archivePrefix =. 2404.01169 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stae749

  63. [63]

    MNRAS , keywords =

    The linear polarization of Southern bright stars measured at the parts-per-million level. MNRAS , keywords =. doi:10.1093/mnras/stv2185 , archivePrefix =. 1509.07221 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv2185

  64. [64]

    Epsilon Sagittarii: An Extreme Rapid Rotator with a Decretion Disk

    ϵ Sagittarii: An Extreme Rapid Rotator with a Decretion Disk. ApJ , keywords =. doi:10.3847/1538-4357/ad630b , archivePrefix =. 2407.11352 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ad630b

  65. [65]

    AJ , keywords =

    Using Red Clump Stars to Decompose the Galactic Magnetic Field with Distance. AJ , keywords =. doi:10.1088/0004-6256/148/3/49 , archivePrefix =. 1407.7268 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-6256/148/3/49

  66. [66]

    The O - C (observed-calculated) technique reconsidered

    The analysis of indexed astronomical time series - II. The O - C (observed-calculated) technique reconsidered. MNRAS , keywords =. doi:10.1093/mnras/263.2.309 , adsurl =

    work page doi:10.1093/mnras/263.2.309

  67. [67]

    MNRAS , keywords =

    A method of detecting radio transients. MNRAS , keywords =. doi:10.1111/j.1365-2966.2010.17346.x , archivePrefix =. 1008.3152 , primaryClass =

    doi:10.1111/j.1365-2966.2010.17346.x 2010

  68. [68]

    Poisson-FOCuS: An efficient online method for detecting count bursts with application to gamma ray burst detection

    Poisson-FOCuS: An efficient online method for detecting count bursts with application to gamma ray burst detection. arXiv e-prints , keywords =. doi:10.48550/arXiv.2208.01494 , archivePrefix =. 2208.01494 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2208.01494

  69. [69]

    Testing and dating of structural changes in practice , volume =

    Zeileis, Achim and Kleiber, Christian and Kr\". Testing and dating of structural changes in practice , volume =. Computational Statistics &amp; Data Analysis , publisher =. 2003 , month = oct, pages =. doi:10.1016/s0167-9473(03)00030-6 , number =

    work page doi:10.1016/s0167-9473(03)00030-6 2003

  70. [70]

    strucchange: AnRPackage for Testing for Structural Change in Linear Regression Models , volume =

    Zeileis, Achim and Leisch, Friedrich and Hornik, Kurt and Kleiber, Christian , year =. strucchange: AnRPackage for Testing for Structural Change in Linear Regression Models , volume =. Journal of Statistical Software , publisher =. doi:10.18637/jss.v007.i02 , number =

    work page doi:10.18637/jss.v007.i02

  71. [71]

    Estimating and Testing Linear Models with Multiple Structural Changes , volume =

    Bai, Jushan and Perron, Pierre , year =. Estimating and Testing Linear Models with Multiple Structural Changes , volume =. Econometrica , publisher =. doi:10.2307/2998540 , number =

    doi:10.2307/2998540

  72. [72]

    Computation and analysis of multiple structural change models , volume =

    Bai, Jushan and Perron, Pierre , year =. Computation and analysis of multiple structural change models , volume =. Journal of Applied Econometrics , publisher =. doi:10.1002/jae.659 , number =

    doi:10.1002/jae.659

  73. [73]

    The Generalization of Student’s Ratio , ISBN =

    Hotelling, Harold , year =. The Generalization of Student’s Ratio , ISBN =. doi:10.1007/978-1-4612-0919-5_4 , booktitle =

    work page doi:10.1007/978-1-4612-0919-5_4

  74. [74]

    Pingouin: statistics in Python , volume =

    Vallat, Raphael , year =. Pingouin: statistics in Python , volume =. Journal of Open Source Software , publisher =. doi:10.21105/joss.01026 , number =

    doi:10.21105/joss.01026

  75. [75]

    Modeling the magnetized Local Bubble from dust data

    Modeling the magnetized Local Bubble from dust data. A&A , keywords =. doi:10.1051/0004-6361/201937157 , archivePrefix =. 1911.09691 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201937157 1911

  76. [76]

    Local Bubble contribution to the 353-GHz dust polarized emission

    Local Bubble contribution to the 353-GHz dust polarized emission. A&A , keywords =. doi:10.1051/0004-6361/201936547 , archivePrefix =. 1908.08706 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201936547 1908

  77. [77]

    ApJ , keywords =

    The Coherent Magnetic Field of the Milky Way. ApJ , keywords =. doi:10.3847/1538-4357/ad4a54 , archivePrefix =. 2311.12120 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/ad4a54

  78. [78]

    A&A , keywords =

    The coherent magnetic field of the Milky Way halo, the Local Bubble, and the Fan region. A&A , keywords =. doi:10.1051/0004-6361/202451440 , archivePrefix =. 2407.02148 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202451440

  79. [79]

    An analytical model for the magnetic field in the thick shell of Galactic bubbles with uniform initial conditions

    An analytical model for the magnetic field in the thick shell of Galactic bubbles with uniform initial conditions. A&A , keywords =. doi:10.1051/0004-6361/202452943 , archivePrefix =. 2411.06277 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202452943

  80. [80]

    MNRAS , keywords =

    A high sampling-density polarization study of the Southern Coalsack. MNRAS , keywords =. doi:10.1111/j.1365-2966.2004.08538.x , adsurl =

    doi:10.1111/j.1365-2966.2004.08538.x 2004

Showing first 80 references.