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arxiv: 2606.13123 · v1 · pith:U47GAPH7new · submitted 2026-06-11 · 🌌 astro-ph.GA

Grain Alignment and Dust Evolution Physics with Polarisation (GRADE-POL). II. On the physical basis of Serkowski and super-Serkowski polarisation spectra

Le Ngoc Tram , Thiem Hoang , B-G Andersson , Alex Lazarian , Lapo Fanciullo , Bao Truong , Archana Soam This is my paper

Pith reviewed 2026-06-27 06:43 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords grain alignmentpolarisation spectraSerkowski relationsuper-Serkowskiradiative torqueparamagnetic relaxationinterstellar dustUV polarisation
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The pith

Radiative torque alignment boosted by B-star radiation below the Lyman limit accounts for super-Serkowski polarisation spectra.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper examines why some interstellar polarisation spectra deviate from the standard Serkowski curve by showing excess polarisation in the mid-UV. It tests whether the joint action of radiative torque alignment and paramagnetic relaxation can reproduce both standard and super-Serkowski curves when the illuminating radiation field is adjusted. For two stars with super-Serkowski behaviour, radiation from a B-type star shortward of 912 angstroms improves the match when combined with the second mechanism, while standard interstellar radiation suffices for the regular cases. A reader would care because a working physical model for the wavelength shape of polarisation directly constrains the size, composition, and alignment efficiency of interstellar dust grains.

Core claim

For the super-Serkowski spectra of HD 30614 and HD 204827, RAT alignment enhanced by radiation produced from a B-type star below the Lyman limit can reasonably explain the observations and a combination with the DG alignments results in a better fit for λ^{-1} ≥ 5.5 μm^{-1}. For the Serkowski spectra in HD 37903 and HD 161056, only RAT alignment by itself under the typical interstellar radiation field above the Lyman limit, within a typical cold neutral medium, can account for the observed spectra, with a combination of a very inefficient DG alignment.

What carries the argument

The joint effect of paramagnetic relaxation (DG alignment) and radiative torque (RAT alignment) under different radiation fields: either the scaled interstellar radiation field above the Lyman limit or an additional component from a B-type star below 912 Å.

If this is right

  • The model predicts the starlight polarisation spectrum from infrared to far-UV wavelengths.
  • RAT alignment enhanced by B-type star radiation below the Lyman limit explains the super-Serkowski excess at mid-UV wavelengths.
  • A combination with DG alignment provides a better fit for wavelengths shorter than about 0.18 micrometers.
  • Standard interstellar radiation field with inefficient DG alignment accounts for regular Serkowski spectra in a cold neutral medium.

Where Pith is reading between the lines

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

  • Local radiation environments near B-type stars may be responsible for enhanced grain alignment in certain lines of sight.
  • The modelling framework could be tested against future UV spectrophotometry data from space missions.
  • Super-Serkowski features might serve as tracers of specific stellar radiation influences rather than solely grain property variations.

Load-bearing premise

The radiation field incident on the grains is either the standard interstellar radiation field above the Lyman limit or an additional component from a B-type star below 912 Å, adopted as input to match the polarisation data rather than derived from independent observations.

What would settle it

Spectroscopic observations confirming the absence of additional B-type star radiation below 912 Å along the sightlines to HD 30614 and HD 204827, or failure of the predicted spectra to match new UV polarisation measurements.

Figures

Figures reproduced from arXiv: 2606.13123 by Alex Lazarian, Archana Soam, Bao Truong, B-G Andersson, Lapo Fanciullo, Le Ngoc Tram, Thiem Hoang.

Figure 1
Figure 1. Figure 1: The locations of our selections of super-Serkowski po [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 3
Figure 3. Figure 3: The comparison in the timescale between the param [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The comparison between our model and the observed super-Serkowski spectra towards HD 30614 (left column) and HD [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The polarisation spectrum and extinction curve towards super-Serkowski spectra in HD 30614 (p [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Similar to Figure [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The polarisation spectrum towards HD 30614, similar to [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Panel a-b: The distribution of grain mass (top) and the alignment function (bottom) for the HD 30614 (within Per OB3 bubble) and HD 37903. Comparing with HD 39703, the amount of VSGs (a ≤ 10−3 µm) is more abundant, while the values of fmax is lower in HD 30614. The alignment function for a < aalign of HD 30614 is also more complex, in which the resonant alignment for VSGs and paramagnetic alignment for lar… view at source ↗
read the original abstract

Optical-to-near infrared interstellar polarisation, induced by aligned dust grains, generally follows a convex wavelength dependence, known as the Serkowski relation. However, observations in the ultraviolet (UV) and at [mid-]infrared wavelengths indicated that some of the spectra do not follow this relation. Specifically, about 25% show an excess in the degree of polarisation at mid-UV wavelengths ($\lambda^{-1} > 3\,\rm \mu m^{-1}$), referred to as the super-Serkowski polarisation. In this study, we re-examine both the Serkowski and super-Serkowski spectra based on the joint effect of paramagnetic relaxation (DG alignment) and radiative torque (RAT) alignment. We used the observational data for HD 30614, HD 204827, HD 37903 and HD 161056 to constrain our modelling. We examined two types of radiation fields: one derived from the scaled interstellar radiation field and another originating from a B-type star. For the super-Serkowski spectra of HD 30614 and HD 204827, our model demonstrates that RAT alignment enhanced by radiation produced from a B-type star below the Lyman limit ($\lambda=912 \r{A}$) can reasonably explain the observations and that a combination with the DG alignments results in a better fit for $\lambda^{-1}\geq 5.5\,\rm \mu m^{-1}$. For the Serkowski spectra in HD 37903 and HD 161056, only RAT alignment by itself under the typical interstellar radiation field above the Lyman limit, within a typical cold neutral medium, can account for the observed spectra, with a combination of a very inefficient DG alignment. The capacity of our model to predict the starlight polarisation spectrum up to from infrared to far-UV is thus a promising tool for interpreting future missions that observe spectrophotometry in the UV bands.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The manuscript claims that joint radiative torque (RAT) alignment and Davis-Greenstein (DG) paramagnetic relaxation, under either a scaled interstellar radiation field above the Lyman limit or an additional B-type star radiation component below 912 Å, can reproduce both standard Serkowski polarization spectra (HD 37903, HD 161056) and super-Serkowski spectra with UV excess (HD 30614, HD 204827) from IR to far-UV, using observational data from these four stars to constrain the modeling.

Significance. If the radiation fields are independently anchored, the model supplies a physical mechanism for the full wavelength dependence of interstellar polarization, including the ~25% of sightlines showing super-Serkowski behavior. The capacity to predict spectra across IR to far-UV is a clear strength for interpreting future UV spectrophotometry missions.

major comments (2)
  1. [Abstract] Abstract: the claim that RAT alignment enhanced by B-star radiation below the Lyman limit explains the super-Serkowski spectra of HD 30614 and HD 204827 rests on adopting this radiation field as an input chosen to match the polarization data rather than deriving its strength or spectrum from independent sight-line constraints (stellar parameters, distances, or UV photometry/spectroscopy specific to these lines of sight). This renders the explanation post-hoc and non-unique, as the short-wavelength flux can be scaled to fit any observed UV excess.
  2. [Abstract] Abstract and modeling description: the manuscript states that a combination with DG alignment improves the fit for λ^{-1} ≥ 5.5 μm^{-1}, yet provides no quantitative assessment of how many free parameters (RAT efficiency scaling, DG efficiency, radiation scaling factors) are adjusted versus predicted from first principles, leaving the degree of tuning unclear.
minor comments (1)
  1. [Abstract] Abstract: the wavelength threshold for the UV excess is given as λ^{-1} > 3 μm^{-1} while the DG improvement is stated for λ^{-1} ≥ 5.5 μm^{-1}; ensure consistent notation and ranges throughout.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. We address the two major comments below and outline the revisions we will make.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the claim that RAT alignment enhanced by B-star radiation below the Lyman limit explains the super-Serkowski spectra of HD 30614 and HD 204827 rests on adopting this radiation field as an input chosen to match the polarization data rather than deriving its strength or spectrum from independent sight-line constraints (stellar parameters, distances, or UV photometry/spectroscopy specific to these lines of sight). This renders the explanation post-hoc and non-unique, as the short-wavelength flux can be scaled to fit any observed UV excess.

    Authors: We agree that the B-star radiation component is introduced as a scaled input to reproduce the UV excess in the two super-Serkowski sightlines and is not derived from independent constraints specific to HD 30614 and HD 204827. This choice is motivated by the physical expectation that additional short-wavelength flux below 912 Å can enhance RAT alignment at small grain sizes, but we acknowledge the post-hoc character of the scaling. In the revised manuscript we will (i) explicitly state that the scaling factors are fitted rather than predicted a priori, (ii) discuss possible nearby B-type stars or local radiation-field variations that could motivate the enhancement, and (iii) note that the same scaling cannot be applied indiscriminately to all sightlines, as demonstrated by the successful fits to the two Serkowski stars with the standard ISRF alone. revision: partial

  2. Referee: [Abstract] Abstract and modeling description: the manuscript states that a combination with DG alignment improves the fit for λ^{-1} ≥ 5.5 μm^{-1}, yet provides no quantitative assessment of how many free parameters (RAT efficiency scaling, DG efficiency, radiation scaling factors) are adjusted versus predicted from first principles, leaving the degree of tuning unclear.

    Authors: We accept that the current text does not quantify the number of adjusted versus fixed parameters. In the revised version we will add a dedicated paragraph (and, if space permits, a short table) that lists (a) parameters taken directly from theory or prior literature (grain size distribution, magnetic susceptibility for DG, baseline RAT efficiency), (b) parameters that are varied to fit the four sightlines (radiation-field scaling factors for the two super-Serkowski stars, DG efficiency for all stars), and (c) the resulting number of degrees of freedom. This will make the degree of tuning explicit and allow readers to judge the predictive power of the joint RAT+DG framework. revision: yes

Circularity Check

1 steps flagged

Radiation field below Lyman limit selected and scaled to fit super-Serkowski spectra of HD 30614/HD 204827 rather than derived independently

specific steps
  1. fitted input called prediction [Abstract]
    "We used the observational data for HD 30614, HD 204827, HD 37903 and HD 161056 to constrain our modelling. [...] For the super-Serkowski spectra of HD 30614 and HD 204827, our model demonstrates that RAT alignment enhanced by radiation produced from a B-type star below the Lyman limit (λ=912 Å) can reasonably explain the observations and that a combination with the DG alignments results in a better fit for λ^{-1}≥5.5 μm^{-1}."

    The radiation-field type (scaled ISRF vs. B-star spectrum below Lyman limit) and its scaling are chosen among the two examined options specifically to reproduce the observed polarisation curves of the target stars. The 'demonstration' that this choice explains the data is therefore the direct output of the fitting process used to constrain the model, not an independent prediction.

full rationale

The paper constrains its RAT+DG model directly on the polarisation spectra of four named stars and selects the B-star radiation component (below 912 Å) as the input that reproduces the UV excess. This choice is presented as the physical explanation, but the abstract explicitly states the data are used 'to constrain our modelling' and that the chosen field 'can reasonably explain the observations' with a 'better fit' when DG is added. No independent derivation of the field strength or spectrum from stellar parameters, distances or UV photometry of these sight-lines is indicated in the provided text. The central claim therefore reduces to a fitted-input demonstration rather than a first-principles prediction.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Abstract-only; the model necessarily rests on standard assumptions about grain magnetic susceptibility, shape distribution, and the spectral shape of the incident radiation field, none of which are re-derived here.

free parameters (2)
  • RAT alignment efficiency scaling
    Must be adjusted to match observed polarisation amplitude under each radiation field.
  • DG alignment efficiency
    Tuned to improve the fit at λ^{-1} ≥ 5.5 μm^{-1} for the super-Serkowski cases.
axioms (2)
  • domain assumption Grain alignment is governed by the joint action of radiative torques and paramagnetic relaxation.
    Invoked throughout the abstract as the physical basis for the model.
  • domain assumption The radiation field below the Lyman limit can be approximated by scaling a B-star spectrum.
    Used to explain the super-Serkowski excess without independent verification for the sight-lines.

pith-pipeline@v0.9.1-grok · 5920 in / 1467 out tokens · 17028 ms · 2026-06-27T06:43:19.717544+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

288 extracted references · 250 canonical work pages · 87 internal anchors

  1. [1]

    , year =

    Hoang, Thiem and Lazarian, A , title =. , year =

  2. [2]

    2017 , rating =

    Hoang, Thiem , journal =. 2017 , rating =. doi:10.3847/1538-4357/836/1/13 , abstract =

    work page doi:10.3847/1538-4357/836/1/13 2017

  3. [4]

    arXiv preprint arXiv:2412.19701 , year=

    Magnetic fields on different spatial scales of the L328 cloud , author=. arXiv preprint arXiv:2412.19701 , year=

    arXiv

  4. [5]

    , journal =

    Reissl, Stefan and Guillet, Vincent and Brauer, Robert and Levrier, François and Boulanger, François and Klessen, Ralf S. , journal =. 2020 , title =. doi:10.1051/0004-6361/201937177 , eprint =

    work page doi:10.1051/0004-6361/201937177 2020

  5. [6]

    , keywords =

    The Orion molecular cloud and star-forming region. , keywords =. doi:10.1146/annurev.aa.27.090189.000353 , adsurl =

    work page doi:10.1146/annurev.aa.27.090189.000353

  6. [7]

    The Polarizing Power of the Interstellar Medium in Taurus

    The Polarizing Power of the Interstellar Medium in Taurus. ApJl , keywords =. doi:10.1086/311337 , archivePrefix =. astro-ph/9803199 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/311337

  7. [8]

    The Efficiency of Grain Alignment in Dense Interstellar Clouds: A Reassessment of Constraints from Near Infrared Polarization

    The Efficiency of Grain Alignment in Dense Interstellar Clouds: a Reassessment of Constraints from Near-Infrared Polarization. ApJ , keywords =. doi:10.1086/525040 , archivePrefix =. 0711.2536 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/525040

  8. [9]

    Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence. A&A , keywords =. doi:10.1051/0004-6361/201424086 , archivePrefix =. 1405.0872 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201424086

  9. [11]

    ApJ , keywords =

    Comparing Submillimeter Polarized Emission with Near-infrared Polarization of Background Stars for the Vela C Molecular Cloud. ApJ , keywords =. doi:10.3847/1538-4357/aa62a7 , eprint =

    work page doi:10.3847/1538-4357/aa62a7

  10. [12]

    ApJ , keywords =

    The Far-infrared Polarization Spectrum of Ophiuchi A from HAWC+/SOFIA Observations. ApJ , keywords =. doi:10.3847/1538-4357/ab3407 , archivePrefix =. 1905.00705 , primaryClass =

    work page doi:10.3847/1538-4357/ab3407 1905

  11. [13]

    Planck 2018 results. XII. Galactic astrophysics using polarized dust emission. A&A , keywords =. doi:10.1051/0004-6361/201833885 , primaryClass =

    work page doi:10.1051/0004-6361/201833885 2018

  12. [14]

    , keywords =

    HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1. , keywords =. doi:10.3847/1538-4357/aafd37 , primaryClass =

    work page doi:10.3847/1538-4357/aafd37

  13. [15]

    Polarimetry of Stars and Planetary Systems , year = 2015, pages =

    Interstellar Polarization. Polarimetry of Stars and Planetary Systems , year = 2015, pages =

    2015

  14. [16]

    , keywords =

    Tracing magnetic fields with aligned grains. , keywords =. doi:10.1016/j.jqsrt.2007.01.038 , primaryClass =

    work page doi:10.1016/j.jqsrt.2007.01.038 2007

  15. [17]

    ARAA , year = 2015, month = aug, volume =

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

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

  16. [18]

    , keywords =

    Radiative torques: analytical model and basic properties. , keywords =. doi:10.1111/j.1365-2966.2007.11817.x , primaryClass =

    work page doi:10.1111/j.1365-2966.2007.11817.x 2007

  17. [19]

    2009 , Bdsk-Url-1 =

    Radiative torque alignment: essential physical processes. , keywords =. doi:10.1111/j.1365-2966.2008.13249.x , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.13249.x 2008

  18. [20]

    Nature Astronomy , keywords =

    Rotational disruption of dust grains by radiative torques in strong radiation fields. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0763-6 , primaryClass =

    work page doi:10.1038/s41550-019-0763-6

  19. [23]

    A&A , keywords =

    The Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory. A&A , keywords =. doi:10.1051/0004-6361/201014535 , primaryClass =

    work page doi:10.1051/0004-6361/201014535

  20. [24]

    The dust opacity exponent and the gas-to-dust mass ratio g2d

    Gas and dust in the star-forming region Oph A. The dust opacity exponent and the gas-to-dust mass ratio g2d. A&A , keywords =. doi:10.1051/0004-6361/201525641 , primaryClass =

    work page doi:10.1051/0004-6361/201525641

  21. [25]

    ApJ , keywords =

    A Unified Model of Grain Alignment: Radiative Alignment of Interstellar Grains with Magnetic Inclusions. ApJ , keywords =. doi:10.3847/0004-637X/831/2/159 , primaryClass =

    work page doi:10.3847/0004-637x/831/2/159

  22. [26]

    Polarized Far-Infrared and Submillimeter Emission from Interstellar Dust

    Polarized Far-Infrared and Submillimeter Emission from Interstellar Dust. ApJ , keywords =. doi:10.1088/0004-637X/696/1/1 , archivePrefix =. 0809.2094 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/696/1/1 2094

  23. [28]

    Physics of the Interstellar and Intergalactic Medium

  24. [29]

    Determination of the gas-to-dust ratio in nearby dense clouds using X-ray absorption measurements

    Determination of the gas-to-dust ratio in nearby dense clouds using X-ray absorption measurements. A&A , keywords =. doi:10.1051/0004-6361:20030942 , archivePrefix =. astro-ph/0306447 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20030942

  25. [30]

    Dust models compatible with Planck intensity and polarization data in translucent lines of sight

    Dust models compatible with Planck intensity and polarization data in translucent lines of sight. A&A , keywords =. doi:10.1051/0004-6361/201630271 , archivePrefix =. 1710.04598 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201630271

  26. [31]

    ApJ , keywords =

    Modeling Rotational Disruption of Grains and Microwave Emission from Spinning Dust in AGB Envelopes. ApJ , keywords =. doi:10.3847/1538-4357/ab7b5e , archivePrefix =. 1907.10654 , primaryClass =

    work page doi:10.3847/1538-4357/ab7b5e 1907

  27. [32]

    Journal of Astronomical Instrumentation , keywords =

    HAWC+, the Far-Infrared Camera and Polarimeter for SOFIA. Journal of Astronomical Instrumentation , keywords =. doi:10.1142/S2251171718400081 , adsurl =

    work page doi:10.1142/s2251171718400081

  28. [33]

    JOSAA , keywords =

    Discrete-dipole approximation for scattering calculations. JOSAA , keywords =. doi:10.1364/JOSAA.11.001491 , adsurl =

    work page doi:10.1364/josaa.11.001491

  29. [34]

    The discrete dipole approximation for periodic targets I. theory and tests

    Discrete-dipole approximation for periodic targets: theory and tests. JOSAA , keywords =. doi:10.1364/JOSAA.25.002693 , archivePrefix =. 0809.0338 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1364/josaa.25.002693

  30. [35]

    Optics Express , year = 2012, month = jan, volume =

    Fast near field calculations in the discrete dipole approximation for regular rectilinear grids. Optics Express , year = 2012, month = jan, volume =. doi:10.1364/OE.20.001247 , adsurl =

    work page doi:10.1364/oe.20.001247 2012

  31. [36]

    The global dust SED: Tracing the nature and evolution of dust with DustEM

    The global dust SED: tracing the nature and evolution of dust with DustEM. A&A , keywords =. doi:10.1051/0004-6361/201015292 , archivePrefix =. 1010.2769 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201015292

  32. [37]

    A&A , keywords =

    Multicolour photometry of stars in the Ophiuchus dark cloud region. A&A , keywords =

  33. [38]

    A&A , keywords =

    Physical parameters of stars in the Scorpio-Centaurus OB association. A&A , keywords =

  34. [39]

    Interstellar reddening from the HIPPARCOS and TYCHO catalogues. I. Distances to nearby molecular clouds and star forming regions. A&A , keywords =

  35. [40]

    , keywords =

    Stellar Rotation in Young Clusters: The First 4 Million Years. , keywords =. doi:10.1086/380931 , adsurl =

    work page doi:10.1086/380931

  36. [41]

    A Preliminary VLBA Distance to the Core of Ophiuchus, with an Accuracy of 4%

    A Preliminary VLBA Distance to the Core of Ophiuchus, with an Accuracy of 4\. ApJl , keywords =. doi:10.1086/529548 , archivePrefix =. 0801.2192 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/529548

  37. [42]

    Hipparcos distances of Ophiuchus and Lupus cloud complexes

    Hipparcos distance estimates of the Ophiuchus and the Lupus cloud complexes. A&A , keywords =. doi:10.1051/0004-6361:20079110 , archivePrefix =. 0801.3346 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20079110

  38. [43]

    On the Distance to the Ophiuchus Star-Forming Region

    On the distance to the Ophiuchus star-forming region. Astronomische Nachrichten , keywords =. doi:10.1002/asna.200710827 , archivePrefix =. 0709.0505 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1002/asna.200710827

  39. [44]

    ApJ , keywords =

    A Study of the Ophiuchi Cloud: Mapping the Distribution and the Motions of Interstellar Gas. ApJ , keywords =. doi:10.1086/587132 , adsurl =

    work page doi:10.1086/587132

  40. [45]

    The Gould s Belt Distances Survey (GOBELINS). I. Trigonometric Parallax Distances and Depth of the Ophiuchus Complex. ApJ , keywords =. doi:10.3847/1538-4357/834/2/141 , archivePrefix =. 1611.06466 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/834/2/141

  41. [46]

    , keywords =

    Role of magnetic fields in the evolution of five dark cloud complexes. , keywords =. doi:10.1086/112031 , adsurl =

    work page doi:10.1086/112031

  42. [47]

    The Cobwebs of Ophiuchus. I. Strands of 13CO: The Mass Distribution. ApJ , keywords =. doi:10.1086/167244 , adsurl =

    work page doi:10.1086/167244

  43. [48]

    The Cobwebs of Ophiuchus. II. 13CO Filament Kinematics. ApJ , keywords =. doi:10.1086/167245 , adsurl =

    work page doi:10.1086/167245

  44. [49]

    From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt survey

    From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt Survey. A&A , keywords =. doi:10.1051/0004-6361/201014666 , archivePrefix =. 1005.2618 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201014666

  45. [50]

    The Spitzer c2d Legacy Results: Star Formation Rates and Efficiencies; Evolution and Lifetimes

    The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes. ApJs , keywords =. doi:10.1088/0067-0049/181/2/321 , archivePrefix =. 0811.1059 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/181/2/321

  46. [51]

    The James Clerk Maxwell Telescope Legacy Survey of Nearby Star-forming Regions in the Gould Belt

    The James Clerk Maxwell Telescope Legacy Survey of Nearby Star-forming Regions in the Gould Belt. , keywords =. doi:10.1086/521277 , archivePrefix =. 0707.0169 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/521277

  47. [52]

    ApJs , keywords =

    Wide-field Infrared Polarimetry of the Ophiuchi Cloud Core. ApJs , keywords =. doi:10.1088/0067-0049/220/1/17 , adsurl =

    work page doi:10.1088/0067-0049/220/1/17

  48. [53]

    A First Look at BISTRO Observations of The $\rho$ Oph-A core

    A First Look at BISTRO Observations of the Oph-A core. ApJ , keywords =. doi:10.3847/1538-4357/aabd82 , archivePrefix =. 1804.09313 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aabd82

  49. [54]

    RADMC-3D: A multi-purpose radiative transfer tool

  50. [55]

    ApJ , keywords =

    A Young Radio-emitting Magnetic B Star in the Rho Ophiuchi Cloud. ApJ , keywords =. doi:10.1086/166979 , adsurl =

    work page doi:10.1086/166979

  51. [56]

    Chandra Observations of a Young Embedded Magnetic B Star in the rho Ophiuchus Cloud

    Chandra Observations of a Young Embedded Magnetic B Star in the Ophiuchus Cloud. , keywords =. doi:10.1093/pasj/55.5.981 , archivePrefix =. astro-ph/0309164 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/pasj/55.5.981

  52. [57]

    , year = 2012, month = sep, volume =

    Magnetic Fields in Molecular Clouds. , year = 2012, month = sep, volume =. doi:10.1146/annurev-astro-081811-125514 , adsurl =

    work page doi:10.1146/annurev-astro-081811-125514 2012

  53. [58]

    Protostars and Planets IV , year = 2000, editor =

    Polarized Light from Star-Forming Regions. Protostars and Planets IV , year = 2000, editor =

    2000

  54. [59]

    Sensitivity of Polarization to Grain Shape. I. Convex Shapes , author=. The Astrophysical Journal , volume=. 2024 , publisher=

    2024

  55. [60]

    , journal =

    Bianchi, S. , journal =. 2024 , title =. doi:10.1051/0004-6361/202451086 , eprint =

    work page doi:10.1051/0004-6361/202451086 2024

  56. [61]

    A&A , keywords =

    Interstellar radiation field and dust temperatures in the diffuse interstellar matter and in giant molecular clouds. A&A , keywords =

  57. [62]

    arXiv e-prints , keywords =

    Rotational Disruption of Astrophysical Dust and Ice: Theory and Applications. arXiv e-prints , keywords =

  58. [63]

    The evolution of amorphous hydrocarbons in the ISM: dust modelling from a new vantage point

    The evolution of amorphous hydrocarbons in the ISM: dust modelling from a new vantage point. A&A , keywords =. doi:10.1051/0004-6361/201321686 , archivePrefix =. 1411.6293 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321686

  59. [64]

    ApJ , keywords =

    The size distribution of interstellar grains. ApJ , keywords =. doi:10.1086/155591 , adsurl =

    work page doi:10.1086/155591

  60. [65]

    Condition for the formation of micron-sized dust grains in dense molecular cloud cores

    Condition for the formation of micron-sized dust grains in dense molecular cloud cores. , keywords =. doi:10.1093/mnrasl/slt081 , archivePrefix =. 1306.5575 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slt081

  61. [66]

    arXiv e-prints , keywords =

    Modelling Grain Alignment, Disruption, Extinction and Polarization of Active Galactic Nuclei by Dust Grains subject to Radiative Torques. arXiv e-prints , keywords =

  62. [67]

    ApJ , keywords =

    Optical Properties of Interstellar Graphite and Silicate Grains. ApJ , keywords =. doi:10.1086/162480 , adsurl =

    work page doi:10.1086/162480

  63. [68]

    ApJ , keywords =

    Physical Model of Dust Polarization by Radiative Torque Alignment and Disruption and Implications for Grain Internal Structures. ApJ , keywords =. doi:10.3847/1538-4357/ab8e33 , archivePrefix =. 1911.00654 , primaryClass =

    work page doi:10.3847/1538-4357/ab8e33 1911

  64. [70]

    ApJ , keywords =

    Understanding Polarized Dust Emission from Ophiuchi A in Light of Grain Alignment and Disruption by Radiative Torques. ApJ , keywords =. doi:10.3847/1538-4357/abc6fe , primaryClass =

    work page doi:10.3847/1538-4357/abc6fe

  65. [71]

    Galaxies , keywords =

    Rotational Disruption of Astrophysical Dust and Ice Theory and Applications. Galaxies , keywords =. doi:10.3390/galaxies8030052 , primaryClass =

    work page doi:10.3390/galaxies8030052

  66. [72]

    Star formation in 30 Doradus

    Star Formation in 30 Doradus. ApJ , keywords =. doi:10.1088/0004-637X/739/1/27 , archivePrefix =. 1106.2801 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/739/1/27

  67. [73]

    , keywords =

    The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150M _ solar stellar mass limit. , keywords =. doi:10.1111/j.1365-2966.2010.17167.x , archivePrefix =. 1007.3284 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17167.x 2010

  68. [74]

    Velocity profiles of [CII], [CI], CO, and [OI] and physical conditions in four star-forming regions in the Large Magellanic Cloud

    Velocity profiles of [C _ II ], [C _ I ], CO, and [O _ I ] and physical conditions in four star-forming regions in the Large Magellanic Cloud. A&A , keywords =. doi:10.1051/0004-6361/201833398 , archivePrefix =. 1808.08826 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833398

  69. [75]

    Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud. II. 30 Doradus. A&A , keywords =. doi:10.1051/0004-6361/201935215 , archivePrefix =. 1905.10051 , primaryClass =

    work page doi:10.1051/0004-6361/201935215 1905

  70. [76]

    A model for atomic and molecular interstellar gas: The Meudon PDR code

    A Model for Atomic and Molecular Interstellar Gas: The Meudon PDR Code. ApJs , keywords =. doi:10.1086/503252 , archivePrefix =. astro-ph/0602150 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/503252

  71. [77]

    Models of irradiated molecular shocks

    Models of irradiated molecular shocks. A&A , keywords =. doi:10.1051/0004-6361/201834248 , archivePrefix =. 1901.04273 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201834248 1901

  72. [78]

    ApJ , keywords =

    Interstellar shock waves with magnetic precursors. ApJ , keywords =. doi:10.1086/158416 , adsurl =

    work page doi:10.1086/158416

  73. [79]

    Molecular and Ionized Hydrogen in 30 Doradus. I. Imaging Observations. ApJ , keywords =. doi:10.1088/0004-637X/807/2/117 , archivePrefix =. 1504.04951 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/807/2/117

  74. [80]

    A&A , keywords =

    ISO-SWS observations of OMC-1: H\_2 and fine structure lines. A&A , keywords =

  75. [81]

    title Measuring the black hole masses of high-redshift quasars

    New determinations of the critical velocities of C-type shock waves in dense molecular clouds: application to the outflow source in Orion. , keywords =. doi:10.1046/j.1365-8711.2002.05373.x , adsurl =

    work page doi:10.1046/j.1365-8711.2002.05373.x 2002

  76. [83]

    Formation of Massive Molecular Cloud Cores by Cloud-cloud Collision

    Formation of Massive Molecular Cloud Cores by Cloud-Cloud Collision. ApJl , keywords =. doi:10.1088/2041-8205/774/2/L31 , archivePrefix =. 1305.4655 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/774/2/l31 2041

  77. [84]

    A&A , keywords =

    Dense gas formation in the Musca filament due to the dissipation of a supersonic converging flow. A&A , keywords =. doi:10.1051/0004-6361/201937104 , archivePrefix =. 2009.03083 , primaryClass =

    work page doi:10.1051/0004-6361/201937104 2009

  78. [85]

    A&A , keywords =

    Formation of the Musca filament: evidence for asymmetries in the accretion flow due to a cloud-cloud collision. A&A , keywords =. doi:10.1051/0004-6361/202038281 , archivePrefix =. 2010.12479 , primaryClass =

    work page doi:10.1051/0004-6361/202038281 2010

  79. [86]

    First observations of the magnetic field inside the Pillars of Creation: Results from the BISTRO survey

    First Observations of the Magnetic Field inside the Pillars of Creation: Results from the BISTRO Survey. ApJl , keywords =. doi:10.3847/2041-8213/aac771 , archivePrefix =. 1805.11554 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aac771 2041

  80. [87]

    SOFIA Community Science I: HAWC+ Polarimetry of 30 Doradus

Showing first 80 references.