Pith. sign in

REVIEW 2 major objections 6 minor 116 references

Scattered near-infrared light maps water ice across prestellar cores, and the densest cores show a central absorption drop that simple scattering models cannot explain.

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 ↗

T0 review · grok-4.5

2026-07-31 05:29 UTC pith:NDM74JZG

load-bearing objection First real coreshine ice maps from SPHEREx; the maps and method hold up, but the claim that simple RT excludes a scattering origin for the central dip is not yet numerically secure. the 2 major comments →

arxiv 2607.24934 v1 pith:NDM74JZG submitted 2026-07-27 astro-ph.GA

Using Scattered Near-Infrared Light to Map Water Ice in Prestellar Cores with SPHEREx

Tamojeet Roychowdhury , Jennifer B. Bergner , Jens Kauffmann , Thushara G.S. Pillai , Silvia Spezzano This is my paper
classification astro-ph.GA
keywords coreshinewater iceprestellar coresSPHERExice absorptionnear-infrared scatteringBonnor-Ebert spheremolecular clouds
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.

This paper shows that light scattered inside dense star-forming cores (coreshine) can be turned into spatially resolved maps of the 3 µm water-ice absorption band, using all-sky SPHEREx spectra instead of sparse background stars. In four nearby prestellar cores, ice absorption rises toward the centre in the two lower-density objects, but drops in the innermost regions of the two densest cores. Analytical and Monte Carlo models of a Bonnor-Ebert sphere lit by scattering confirm that coreshine spectra track ice mass fraction when the density structure is known, yet none of the tested geometries, grain-growth cases, ice-formation thresholds, or simple CO–water mixes reproduce the central dip. The result both establishes a uniform-resolution ice probe for many cores and flags an unexplained physical or chemical effect in the densest prestellar gas.

Core claim

Coreshine-derived SPHEREx spectra yield the first uniform, spatially resolved maps of 3 µm H2O ice absorption in four nearby prestellar cores. Two cores show the expected centre-peaked ice absorption; the two densest show a surprising central drop. Models of scattered light in a Bonnor-Ebert sphere demonstrate that such spectra robustly trace spatially varying ice density and composition, but standard geometric, grain-growth, and ice-composition variants cannot produce the reduced central absorption, implying an unexplained effect in the densest regions.

What carries the argument

Coreshine ice-depth maps: pixel-by-pixel continuum-subtracted optical depth of the 3 µm H2O band measured against diffuse scattered Galactic light inside the core, interpreted with single-scattering analytics and 3D Monte Carlo radiative transfer of a Bonnor-Ebert sphere.

Load-bearing premise

That a simple spherical density profile with constant or simply thresholded ice fraction, ordinary grain sizes, and a basic radiation field is a fair null model—so failure to match the central ice dip means real physics or chemistry rather than missing complexity in dust or light.

What would settle it

Deep multi-band ice maps or background-star sightlines through the true centres of the densest cores that either confirm lower central water-ice column than at intermediate radii, or erase the dip once full multi-scattering and anisotropic illumination are included.

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

If this is right

  • Ice absorption can be mapped at roughly thousand-AU resolution across the large share of cores that show coreshine, without needing background stars.
  • When dust or gas tracers fix the density structure, coreshine ice depth can constrain ice mass fraction and column.
  • The unexplained central dip marks densest, evolved prestellar regions as places where ice may not scale linearly with gas.
  • The same scattered-light method can be extended with SPHEREx to other ice bands and much larger core samples.

Where Pith is reading between the lines

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

  • A confirmed central water-ice deficit would tighten links between dense-core freeze-out, oxygen budget, and the inventory of solids that later feed planet-forming disks.
  • A statistical sample of coreshine cores sorted by central density and evolutionary stage could separate local chemistry from illumination geometry as the driver of the dip.
  • Joint coreshine ice maps with gas-phase water and CO freeze-out tracers would test whether oxygen is reallocated among ices rather than simply depleted.

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 / 6 minor

Summary. The authors present the first spatially resolved maps of the 3 µm H2O ice absorption feature measured against coreshine (Galactic radiation scattered by micron-sized grains in dense cores), using SPHEREx spectrophotometry of four nearby prestellar cores (L1544, CrA 151, L260, L1512). The two lower-density cores show ice absorption peaking toward the center, as expected, while the two densest cores show a central drop in tau_ice. The observational pipeline is carefully validated: continuum-fit variants and S/N cuts change tau_ice by ≲10%, foreground subtraction cannot reverse the central-dip trend except at unphysical foreground levels (App. B), and SPHEREx tau_ice for L1544 background stars agrees with Goto et al. (2021) within ~10% (App. A). To interpret the maps, the authors build a single-scattering analytical model and RADMC-3D Monte Carlo models of a Bonnor-Ebert-like sphere; the models reproduce the continuum central dip but not the central tau_ice drop, and variants testing ISRF geometry, grain growth to 100 µm, ice-formation thresholds, and CO–H2O mixing also fail. Only an ad hoc central ice-saturation model reproduces the dip. The authors conclude that an unexplained physical or chemical effect operates in the densest regions, and advertise coreshine spectroscopy as a new probe of ice density and composition.

Significance. If it holds, this is a genuinely useful methodological advance: spatially continuous ice-abundance maps for any coreshine-bright core, rather than maps limited to the sparse set of background-star sightlines — enabling statistically large samples with an all-sky survey. The pipeline is reproducible (public SPHEREx/WISE/Herschel data, public RADMC-3D and OpTool codes), carries an external ~10% cross-calibration against IRTF background-star measurements (App. A), and is tested against foreground and continuum-fitting systematics. The reported central ice-absorption drop in the two densest cores, if confirmed as non-scattering in origin, would be a new and interesting constraint on ice chemistry at n_H2 ~ 10^6-10^7 cm^-3. The proof-of-concept value of the technique stands independently of how the interpretive question resolves.

major comments (2)
  1. [§3.3, App. C (Eq. C1)] §3.3 vs §3.1/App. C: the high-density null tests appear to under-resolve the region that dominates the physics. The BE profile uses r0 = 0.002 pc inside a 0.2 pc truncation radius, so a uniform 40^3 Cartesian grid spanning the cloud gives ~0.01 pc cells — 5x r0 — and an even-numbered grid need not place a cell at the center. App. C itself states that 'the opacity is dominated by the central flat region' (tau ~ kappa rho0 r0) and that the single-scattering assumption fails at n_H2 = 10^7 cm^-3 (tau ~ 10), so the analytical model cannot validate the Monte Carlo result precisely where the claimed discrepancy lives. The statement that the 40^3 grid was 'found sufficient' is asserted without a convergence test. Since the abstract's claim that 'none of these [models] can explain the reduced central absorption' rests entirely on these high-density RADMC-3D runs, a convergence demonstration is n
  2. [Abstract; §5, item 3] Conclusion 3 and the abstract state the null result more strongly than the explored parameter space supports, given the magnitude of the mismatch. In the high-density fiducial model the central tau_ice reaches ~1.5 (Fig. 4, top right), while the observed central values are ~0.6-0.8 with a ring peaking near ~1 (Fig. 2) — a factor ~2 offset, well above the 10-15% measurement errors. The §4 variants test only coarse departures (a sharp 5-to-100 um a_max jump, a single 30 deg cap ISRF orientation, one threshold density). The body text is appropriately hedged ('Other physical explanations... cannot be ruled out', §4.4.1), but the abstract and Conclusions should be brought in line — e.g., 'within the model family tested' — or the variant suite should be broadened (continuous rgrowth, swept ISRF directions combined with the Major-Comment-1 convergence test). As written, a reader could take the
minor comments (6)
  1. [§2.2] §2.2: the 7.2-arcsec grid spacing is justified against the 6.2-arcsec native pixel, but adjacent grid points are not independent given the SPHEREx PSF (~2 pixels); please state the effective spatial resolution of the tau_ice maps and confirm the central dip spans more than one independent beam.
  2. [§3.3] §3.3: please justify the 10^6 photons per wavelength and the 200 MJy/sr flux floor. Photon noise and the floor could both affect the derived central tau_ice in the faint central depression; a brief noise estimate for the simulated images would help.
  3. [Fig. 3, Fig. 5] Fig. 3 legends: the density labels (e.g., '0 = 0.1x10^6') do not state whether the quantity is n_H2 or rho0, nor units; the axis label 'ice' should be tau_ice. Same notation issue in Fig. 5.
  4. [Table 1] Table 1's 'Central Density' column contains 'Low'/'High' rather than densities; either give approximate central densities (with the references already cited in §2.1) or rename the column.
  5. [§2.3, Fig. 2] Fig. 2 radial profiles: describe the annulus binning and how the +/-1 sigma band is constructed (the text mentions only adding 10% to the upper error for the bandpass correction).
  6. [Various] Typos/style: 'gasesous' (§4.4.1), 'upto' (§4.2), 'focussing' (§2.1), 'roughly corresponding' (§2.2); 'megajansky per steradian' in §3.3 without distance scaling makes the absolute flux comparison to data unclear.

Circularity Check

0 steps flagged

No circularity: ice maps are measured independently from SPHEREx photometry; models are null tests that fail to force the central dip.

full rationale

The paper’s load-bearing observational product is τ_ice computed pixel-by-pixel from SPHEREx coreshine spectra via continuum fitting and −ln(F/F_cont) (Eq. 1, §2.2); that quantity is not defined in terms of the Bonnor–Ebert or RADMC-3D models. The models (§3–4) are used as interpretive null tests: they adopt standard domain choices (BE profile, MRN-like grains, η_ice, isotropic/cap ISRF) and are shown to reproduce continuum central dips and monotonic ice profiles, but not the observed central τ_ice drop in the densest cores. Failure of the null models is not a fitted-input-called-prediction, nor is any uniqueness theorem or self-citation chain used to forbid alternatives. Literature central densities are used only to label cores high vs low density, which does not make the measured maps or the model–data mismatch circular. Cross-checks (background-star comparison in App. A, foreground subtraction in App. B, continuum-fit variants) are external consistency tests, not self-referential closures. Score 0 is therefore appropriate.

Axiom & Free-Parameter Ledger

7 free parameters · 7 axioms · 1 invented entities

The observational τ_ice maps rest mainly on standard photometric reductions and continuum-fitting practice. The interpretive claim that the central dip is physical and unexplained rests on a stack of domain modeling choices (BE density law, fixed ice fraction, grain opacities, ISRF geometry) none of which are derived in the paper; free parameters set the null models that fail to match the dip.

free parameters (7)
  • fiducial ice mass fraction η_ice = 0.4 (fiducial)
    Set to 40% in the primary models; varied 0.1–0.9 in sensitivity tests. Controls absolute τ_ice scale and whether ice tracks dust.
  • central flat-density radius r0 = 0.002 pc
    Fixed at 0.002 pc for all models; sets where density (and ice) peaks and how steep the envelope is.
  • core truncation radius R = 0.2 pc
    Set to 0.2 pc to match NIR extent; defines integration domain for scattering.
  • maximum grain size a_max (and rgrowth) = 5 µm fiducial; 100 µm in core for growth tests
    Fiducial a_max = 5 µm; growth tests use 100 µm inside rgrowth ∈ {0.01, 0.03, 0.06, 0.1} pc with a sharp boundary—hand-chosen to test coagulation.
  • ice-threshold density ρt (via n_H2 = 10^4 cm^{-3}) = n_H2 ≈ 10^4 cm^{-3}
    Ad hoc density where ice-to-dust ratio is forced to change in threshold and reduction models; f = ρ/(ρ+ρt) is an arbitrary smooth switch.
  • continuum-fit wavelength windows and spike cut = 1.5× median spike cut; stated windows
    Quadratic fit on 2.4–2.7 and 3.6–4.1 µm; points >1.5× median continuum rejected. Choices affect τ_ice at the ≲10% level by authors’ tests.
  • ISRF geometry (full sphere vs 30° cap) = isotropic ~500-star Fibonacci sphere; 30° cap test
    Illumination anisotropy is chosen by hand to test geometry; not fit to each core’s Galactic environment.
axioms (7)
  • domain assumption Prestellar cores can be approximated as Bonnor-Ebert spheres: constant density for r < r0, ρ ∝ r^{-2} outside.
    Used throughout §3–4 as the sole density structure for analytical and RADMC-3D models.
  • domain assumption Gas-to-dust mass ratio ≈ 100 and DHS porous grains with MRN size distribution generate NIR opacities via OpTool.
    §3.1; standard ISM dust assumptions underlying all scattering/absorption coefficients.
  • domain assumption Single-scattering, forward-dominated transport is adequate for the analytical model at moderate τ (mean free path argument in App. C).
    Authors note it breaks at n_H2 ~ 10^7 cm^{-3}; RADMC-3D is used to go beyond this.
  • domain assumption Quadratic continuum interpolation outside 2.9–3.1 µm yields an unbiased estimate of the H2O ice optical depth at SPHEREx resolution (correction factor ≈1–1.1).
    §2.2; follows Hora et al. 2026 and stellar-ice practice; authors test linear/median variants.
  • domain assumption Thermal NIR emission and Galactic foreground are subdominant to coreshine for these <150 pc cores after off-core checks.
    §2.2 and App. B; load-bearing for interpreting central τ_ice as intrinsic.
  • standard math Ice absorption opacity scales with ice mass on grains; continuum scattering opacity is set by dust size distribution.
    Standard radiative-transfer separation used to define τ_ice = -ln(I_ice/I_cont) in models and data.
  • ad hoc to paper Failure of the tested model suite to produce a central τ_ice dip implies an unexplained physical or chemical effect in the densest regions.
    Abstract and §4–5; this is an inference from negative model results, not a derived necessity.
invented entities (1)
  • Ice-reduction / saturation model (ice density plateaus above n_H2 ~ 10^4 cm^{-3}) no independent evidence
    purpose: Phenomenological density law introduced to try to reproduce the observed central drop in τ_ice.
    Not a new particle or force, but a new postulated radial ice profile without independent microphysical derivation; only partially motivated by oxygen reallocation arguments.

pith-pipeline@v1.2.0-grok45-kimik3 · 29465 in / 4507 out tokens · 83705 ms · 2026-07-31T05:29:02.290579+00:00 · methodology

0 comments
read the original abstract

We present the first coreshine-derived, spatially-resolved maps of the 3 $\mu$m H$_2$O ice absorption feature in four prestellar cores, using SPHEREx spectra. Ices are a key component of dense cores in molecular clouds, playing a central role in the chemistry of planet formation around young stars. However, spatially resolved abundance studies remain limited, typically relying on unevenly distributed background star sightlines. Here, we take advantage of the all-sky spectrophotometric capabilities of SPHEREx to construct ice absorption maps with uniform spatial resolution using the illumination of dense cores by scattered Galactic radiation, or coreshine. To demonstrate proof of concept, we analyse the spatially varying H$_2$O ice absorption in four nearby (~140 pc) prestellar cores - L1544, CrA 151, L260 and L1512. Two cores follow the expected spatial trend of ice absorption peaking at the centre, but the two densest cores show a surprising drop in observed ice absorption in the innermost regions. To interpret the absorption maps, we construct analytical and simulated models of a Bonnor-Ebert sphere illuminated by scattering. We study the effects of different geometric configurations, ice mass fractions, and spatial differences in ice composition. None of these can explain the reduced central absorption, pointing to an unexplained physical or chemical effect operating in the densest prestellar regions. Our simulations further show that spectra derived from coreshine provide a robust tracer of spatially varying ice density and composition, establishing SPHEREx scattered-light spectroscopy as a powerful new probe of ice in dense cores.

Figures

Figures reproduced from arXiv: 2607.24934 by Jennifer B. Bergner, Jens Kauffmann, Silvia Spezzano, Tamojeet Roychowdhury, Thushara G.S. Pillai.

Figure 1
Figure 1. Figure 1: Continuum flux maps and spectra for four prestellar cores. The top row shows the continuum flux at 3.4 µm from WISE, and contours of log10 (NH2 ) estimated using Herschel. In each core, we pick three representative points marked with crosses, starting at the centre (dark red) and going outwards (orange to yellow), chosen as to avoid intersecting background star sightlines. These points probe decreasing NH2… view at source ↗
Figure 2
Figure 2. Figure 2: Ice absorption maps and radial profiles for four prestellar cores. The top row shows the ice absorption depth, τH2O in a spatial grid, with contours marking the increasing levels of τice. The bottom row shows the averaged radial profile of ice absorption depth τice (and ±1σ uncertainty band – upper error including an additional 10% for the unknown τice correction factor) for each core. The lower density co… view at source ↗
Figure 3
Figure 3. Figure 3: Model derived light profile and ice absorption profile as a function of radius for the prestellar core as described in §3.2. Left: continuum profile for varying densities. Middle: ice absorption profile for varying densities. Right: ice absorption profile for varying ice opacities. We present the NIR continuum light profile and the ice absorption map for each of the two central densities in [PITH_FULL_IMA… view at source ↗
Figure 4
Figure 4. Figure 4: Top row: RADMC-3D derived NIR light profile (left), observed ice absorption profile (right) for the dense (central nH2 ≈ 107 ) prestellar core. The central flux dip is reproduced in NIR continuum. We observe the central ice absorption to be very high. All profiles are roughly consistent with the analytical model in [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Left panel: RADMC-3D derived τice as a function of radius for varying central densities. Right panel: RADMC-3D derived τice as a function of radius for varying ice mass fractions ηice. We see a clear difference in the observed τice profile as ηice is varied. As mentioned earlier, these models are intentionally simplified: they do not account for anisotropies in ei￾ther the source of illumination or the clo… view at source ↗
Figure 6
Figure 6. Figure 6: RADMC-3D derived ice absorption map for Top left: the fiducial cloud for a constant ηice = 40%, same as [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Ice density as a function of radius for the canoni￾cal model in § 3.3 in cyan, and for the ice formation threshold and ice reduction models from § 4.3 in brown and indigo re￾spectively Let f be a factor given by f = ρ ρ + ρt (3) such that the effective ice absorption coefficient scales as κabs,ice,eff = f · κabs,ice + (1 − f) · κabs,cont (4) This broadly means that for large densities (closer to the centre… view at source ↗
Figure 8
Figure 8. Figure 8: Water ice absorption toward three background stars in L1544 as studied by Goto et al. (2021). The colour of the circular marker on the WISE image in the left panel corresponds to the colour used to plot the optical depth spectrum on the right panel. Stars marked A, B, C above correspond to stars 1, 3, 5 respectively in Goto et al. (2021), with reported τice of 1.99 ± 0.25, 1.21 ± 0.03 and 0.67 ± 0.15 respe… view at source ↗
Figure 9
Figure 9. Figure 9: Ice absorption spectra at the three points marked in [PITH_FULL_IMAGE:figures/full_fig_p019_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Setup of the analytical model. The background light source is exactly along the line-of-sight. The top blue arrow show the rays of light from the background light source to the infinitesimal element ds (marked in a grey rectangle) at projected radius b and LoS coordinate s. The lower blue arrow shows the ray of light from the same element to the observer at the bottom. The small red rectangle shows an inf… view at source ↗

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

116 extracted references · 11 canonical work pages · 1 internal anchor

  1. [1]

    arXiv e-prints , keywords =

    The SPHEREx Satellite Mission. arXiv e-prints , keywords =. doi:10.48550/arXiv.2511.02985 , archivePrefix =. 2511.02985 , primaryClass =

    doi:10.48550/arxiv.2511.02985

  2. [2]

    Infrared Emission from Interstellar Dust. II. The Diffuse Interstellar Medium. , keywords =. doi:10.1086/323147 , archivePrefix =. astro-ph/0011319 , primaryClass =

    Pith/arXiv arXiv

  3. [3]

    , keywords =

    Is the dust-to-gas ratio constant in molecular clouds?. , keywords =. doi:10.1093/mnrasl/slx096 , archivePrefix =. 1706.05107 , primaryClass =

    Pith/arXiv arXiv

  4. [4]

    , keywords =

    The infrared band strengths of H\_2\_O, CO and CO\_2\_ in laboratory simulations of astrophysical ice mixtures. , keywords =. doi:10.48550/arXiv.astro-ph/9409076 , archivePrefix =. astro-ph/9409076 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9409076

  5. [5]

    Mit 5 Textabbildungen

    \"U ber die Verdichtung von H I-Gebieten. Mit 5 Textabbildungen. , year = 1955, month = jan, volume =

    1955

  6. [6]

    , year = 1956, month = jan, volume =

    Boyle's Law and gravitational instability. , year = 1956, month = jan, volume =. doi:10.1093/mnras/116.3.351 , adsurl =

    doi:10.1093/mnras/116.3.351 1956

  7. [7]

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

  8. [8]

    OpTool: Command-line driven tool for creating complex dust opacities

  9. [9]

    , keywords =

    Modeling optical properties of cosmic dust grains using a distribution of hollow spheres. , keywords =. doi:10.1051/0004-6361:20041920 , archivePrefix =. astro-ph/0503068 , primaryClass =

    Pith/arXiv arXiv

  10. [10]

    , keywords =

    Scattering from dust in molecular clouds: Constraining the dust grain size distribution through near-infrared cloudshine and infrared coreshine. , keywords =. doi:10.1051/0004-6361/201322102 , archivePrefix =. 1310.7105 , primaryClass =

    Pith/arXiv arXiv

  11. [11]

    , keywords =

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

  12. [12]

    , keywords =

    Properties of starless and prestellar cores in Taurus revealed by Herschel: SPIRE/PACS imaging. , keywords =. doi:10.1093/mnras/stu219 , archivePrefix =. 1401.7871 , primaryClass =

    Pith/arXiv arXiv

  13. [13]

    On the internal structure of starless cores. I. Physical conditions and the distribution of CO, CS, N _ 2 H ^ + , and NH _ 3 in L1498 and L1517B. , keywords =. doi:10.1051/0004-6361:20031704 , adsurl =

    work page doi:10.1051/0004-6361:20031704

  14. [14]

    The constant-mass case

    An analytical model for the evolution of starless cores - I. The constant-mass case. , keywords =. doi:10.1093/mnras/stw729 , archivePrefix =. 1603.09591 , primaryClass =

    Pith/arXiv arXiv

  15. [15]

    , keywords =

    Dust opacities for protostellar cores. , keywords =

  16. [16]

    , year = 1941, month = jan, volume =

    Diffuse radiation in the Galaxy. , year = 1941, month = jan, volume =. doi:10.1086/144246 , adsurl =

    doi:10.1086/144246 1941

  17. [17]

    , year = 1965, month = nov, volume =

    Multiple Scattering by Large Particles. , year = 1965, month = nov, volume =. doi:10.1086/148436 , adsurl =

    work page doi:10.1086/148436 1965

  18. [18]

    Multiple Scattering by Large Particles. II. Optically Thick Layers. , year = 1968, month = jun, volume =. doi:10.1086/149598 , adsurl =

    work page doi:10.1086/149598 1968

  19. [19]

    , keywords =

    A note on double Henyey-Greenstein phase function. , keywords =. doi:10.1016/j.jqsrt.2016.06.016 , adsurl =

    work page doi:10.1016/j.jqsrt.2016.06.016 2016

  20. [20]

    Multiple scattering in reflection nebulae. I. A Monte Carlo approach. , keywords =. doi:10.1086/190463 , adsurl =

    work page doi:10.1086/190463

  21. [21]

    , keywords =

    Dust particle size, shape and optical depth during the 2018/MY34 Martian global dust storm retrieved by MSL Curiosity rover Navigation Cameras. , keywords =. doi:10.1016/j.icarus.2020.114021 , archivePrefix =. 2008.01968 , primaryClass =

    arXiv 2018

  22. [22]

    , keywords =

    A three-parameter analytic phase function for multiple scattering calculations. , keywords =. doi:10.1016/0022-4073(75)90095-3 , adsurl =

    doi:10.1016/0022-4073(75)90095-3

  23. [23]

    arXiv e-prints , keywords =

    SPHEREx Wide-Field Infrared Spectral Mapping of Interstellar Ices and Polycyclic Aromatic Hydrocarbons. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.12390 , archivePrefix =. 2603.12390 , primaryClass =

    work page doi:10.48550/arxiv.2603.12390

  24. [24]

    The Central 1000 au of a Pre-stellar Core Revealed with ALMA. I. 1.3 mm Continuum Observations. , keywords =. doi:10.3847/1538-4357/ab0700 , archivePrefix =. 1902.05299 , primaryClass =

    Pith/arXiv arXiv 1902

  25. [25]

    , keywords =

    The Spitzer Ice Legacy: Ice Evolution from Cores to Protostars. , keywords =. doi:10.1088/0004-637X/740/2/109 , archivePrefix =. 1107.5825 , primaryClass =

    Pith/arXiv arXiv

  26. [26]

    , keywords =

    Observations of the icy universe. , keywords =. doi:10.1146/annurev-astro-082214-122348 , archivePrefix =. 1501.05317 , primaryClass =

    Pith/arXiv arXiv

  27. [27]

    , keywords =

    Water in star-forming regions: physics and chemistry from clouds to disks as probed by Herschel spectroscopy. , keywords =. doi:10.1051/0004-6361/202039084 , archivePrefix =. 2102.02225 , primaryClass =

    Pith/arXiv arXiv

  28. [28]

    , keywords =

    Laboratory and Computational Studies of Interstellar Ices. , keywords =. doi:10.1146/annurev-astro-071221-052732 , archivePrefix =. 2407.06657 , primaryClass =

    Pith/arXiv arXiv

  29. [29]

    , keywords =

    An Embedded Disk (eDisk) in the IceAge: Investigating the Jet and Outflow from Ced 110 IRS4. , keywords =. doi:10.3847/1538-3881/adb1ba , archivePrefix =. 2502.00394 , primaryClass =

    Pith/arXiv arXiv

  30. [30]

    Methanol-rich ice in the envelope of Serpens SMM 4

    Mapping ices in protostellar environments on 1000 AU scales. Methanol-rich ice in the envelope of Serpens SMM 4. , keywords =. doi:10.1051/0004-6361:20041276 , archivePrefix =. astro-ph/0407316 , primaryClass =

    Pith/arXiv arXiv

  31. [31]

    Tracing the chemical environment and thermal history of ices in protostellar envelopes

    JWST observations of ^ 13 CO _ 2 ice. Tracing the chemical environment and thermal history of ices in protostellar envelopes. , keywords =. doi:10.1051/0004-6361/202348718 , archivePrefix =. 2402.04314 , primaryClass =

    Pith/arXiv arXiv

  32. [32]

    The c2d Spitzer Spectroscopic Survey of Ices around Low-Mass Young Stellar Objects. I. H _ 2 O and the 5-8 m Bands. , keywords =. doi:10.1086/533425 , archivePrefix =. 0801.1167 , primaryClass =

    Pith/arXiv arXiv

  33. [33]

    The c2d Spitzer Spectroscopic Survey of Ices around Low-Mass Young Stellar Objects. II. CO _ 2. , keywords =. doi:10.1086/533431 , archivePrefix =. 0711.4616 , primaryClass =

    Pith/arXiv arXiv

  34. [34]

    The c2d Spitzer Spectroscopic Survey of Ices around Low-Mass Young Stellar Objects. III. CH _ 4. , keywords =. doi:10.1086/533432 , archivePrefix =. 0801.1223 , primaryClass =

    Pith/arXiv arXiv

  35. [35]

    The c2d Spitzer Spectroscopic Survey of Ices Around Low-mass Young Stellar Objects. IV. NH _ 3 and CH _ 3 OH. , keywords =. doi:10.1088/0004-637X/718/2/1100 , archivePrefix =. 1005.2225 , primaryClass =

    Pith/arXiv arXiv

  36. [36]

    , keywords =

    JWST Observations of Young protoStars (JOYS): Overview of program and early results. , keywords =. doi:10.1051/0004-6361/202554444 , archivePrefix =. 2505.08002 , primaryClass =

    Pith/arXiv arXiv

  37. [37]

    Journal of Korean Astronomical Society , keywords =

    Near- to Mid-Infrared Spectroscopic Study of Ice Analysis Using the AKARI/IRC and Spitzer/IRS Spectra. Journal of Korean Astronomical Society , keywords =. doi:10.5303/JKAS.2025.58.1.111 , archivePrefix =. 2505.05390 , primaryClass =

    Pith/arXiv arXiv 2025

  38. [38]

    , keywords =

    Enhanced formation of interstellar complex organic molecules on carbon monoxide ice. , keywords =. doi:10.1051/0004-6361/202449604 , archivePrefix =. 2405.20707 , primaryClass =

    Pith/arXiv arXiv

  39. [39]

    Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights. , keywords =. doi:10.3847/1538-4365/ac1432 , archivePrefix =. 2109.06268 , primaryClass =

    Pith/arXiv arXiv

  40. [40]

    Protostars and Planets VI , year = 2014, editor =

    Water: From Clouds to Planets. Protostars and Planets VI , year = 2014, editor =. doi:10.2458/azu_uapress_9780816531240-ch036 , archivePrefix =. 1401.8103 , primaryClass =

    Pith/arXiv arXiv 2014

  41. [41]

    Encyclopedia of Astrophysics, Volume 1 , year = 2026, volume =

    Protoplanetary disk chemistry and structure. Encyclopedia of Astrophysics, Volume 1 , year = 2026, volume =. doi:10.1016/B978-0-443-21439-4.00044-4 , archivePrefix =. 2410.23235 , primaryClass =

    Pith/arXiv arXiv 2026

  42. [42]

    , keywords =

    The 3.1 m absorption in molecular clouds is probably due to amorphous H _ 2 O ice. , keywords =

  43. [43]

    , keywords =

    The Wide-field Infrared Survey Explorer (WISE): Mission Description and Initial On-orbit Performance. , keywords =. doi:10.1088/0004-6256/140/6/1868 , archivePrefix =. 1008.0031 , primaryClass =

    Pith/arXiv arXiv

  44. [44]

    Science , keywords =

    The Ubiquity of Micrometer-Sized Dust Grains in the Dense Interstellar Medium. Science , keywords =. doi:10.1126/science.1193211 , archivePrefix =. 1110.4180 , primaryClass =

    Pith/arXiv arXiv

  45. [45]

    , keywords =

    Grain size limits derived from 3.6 m and 4.5 m coreshine. , keywords =. doi:10.1051/0004-6361/201425434 , archivePrefix =. 1508.04691 , primaryClass =

    Pith/arXiv arXiv

  46. [46]

    , keywords =

    Hunting pre-stellar cores with APEX: Corona Australis 151, the densest pre-stellar core or the youngest protostar?. , keywords =. doi:10.1051/0004-6361/202452579 , archivePrefix =. 2502.13745 , primaryClass =

    Pith/arXiv arXiv

  47. [47]

    Monthly Notices of the Royal Astronomical Society , volume =

    Keto, Eric and Rawlings, Jonathan and Caselli, Paola , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2014 , month =. doi:10.1093/mnras/stu426 , url =

    work page doi:10.1093/mnras/stu426 2014

  48. [48]

    , keywords =

    Physical and chemical modeling of the starless core L 1512. , keywords =. doi:10.1051/0004-6361/201936877 , archivePrefix =. 2002.01346 , primaryClass =

    Pith/arXiv arXiv 2002

  49. [49]

    Noble, J. A. and Fraser, H. J. and Pontoppidan, K. M. and Craigon, A. M. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2017 , month =. doi:10.1093/mnras/stx329 , url =

    doi:10.1093/mnras/stx329 2017

  50. [50]

    The Astrophysical Journal Supplement Series , year =

    Murakawa, Koji and Tamura, Motohide and Nagata, Tetsuya , title =. The Astrophysical Journal Supplement Series , year =

  51. [51]

    A direct measurement of CO depletion and the formation of CO\_2

    Spatial mapping of ices in the Ophiuchus-F core. A direct measurement of CO depletion and the formation of CO\_2. , keywords =. doi:10.1051/0004-6361:20065569 , archivePrefix =. astro-ph/0605576 , primaryClass =

    Pith/arXiv arXiv

  52. [52]

    and Neufeld, D

    Sonnentrucker, P. and Neufeld, D. A. and Gerakines, P. A. and Bergin, E. A. and Melnick, G. J. and Forrest, W. J. and Pipher, J. L. and Whittet, D. C. B. , year=. Fully Sampled Maps of Ices and Silicates in Front of Cepheus A East with theSpitzer Space Telescope , volume=. The Astrophysical Journal , publisher=. doi:10.1086/523790 , number=

    doi:10.1086/523790

  53. [53]

    , keywords =

    A Survey of H _ 2 O, CO _ 2 , and CO Ice Features toward Background Stars and low-mass Young Stellar Objects Using AKARI. , keywords =. doi:10.1088/0004-637X/775/2/85 , archivePrefix =. 1307.1527 , primaryClass =

    Pith/arXiv arXiv

  54. [54]

    Nature Astronomy , year = 2025, month = jun, volume =

    Cospatial ice mapping of H _ 2 O with CO _ 2 and CO across a molecular cloud with JWST/NIRCam. Nature Astronomy , year = 2025, month = jun, volume =. doi:10.1038/s41550-025-02511-z , adsurl =

    doi:10.1038/s41550-025-02511-z 2025

  55. [55]

    , keywords =

    Infrared spectroscopy of dust in the Taurus dark clouds : ice and silicates. , keywords =. doi:10.1093/mnras/233.2.321 , adsurl =

    work page doi:10.1093/mnras/233.2.321

  56. [56]

    , keywords =

    Spitzer Mid-Infrared Spectroscopy of Ices toward Extincted Background Stars. , keywords =. doi:10.1086/499584 , archivePrefix =. astro-ph/0511467 , primaryClass =

    Pith/arXiv arXiv

  57. [57]

    , keywords =

    Spitzer Observations of CO _ 2 Ice toward Field Stars in the Taurus Molecular Cloud. , keywords =. doi:10.1086/431932 , archivePrefix =. astro-ph/0505345 , primaryClass =

    Pith/arXiv arXiv

  58. [58]

    , keywords =

    The SPHEREx Target List of Ice Sources (SPLICES). , keywords =. doi:10.3847/1538-4357/acc86b , archivePrefix =. 2501.17797 , primaryClass =

    arXiv

  59. [59]

    , keywords =

    Multi-wavelength observations and modelling of a quiescent cloud LDN1512. , keywords =. doi:10.1051/0004-6361/202038401 , archivePrefix =. 2101.12032 , primaryClass =

    Pith/arXiv arXiv

  60. [60]

    , keywords =

    A survey of magnetic field properties in Bok Globules. , keywords =. doi:10.1093/mnras/staf529 , archivePrefix =. 2412.00201 , primaryClass =

    arXiv

  61. [61]

    The link between water gas and ice in protostellar envelopes

    Water in low-mass star-forming regions with Herschel. The link between water gas and ice in protostellar envelopes. , keywords =. doi:10.1051/0004-6361/201424236 , archivePrefix =. 1409.6473 , primaryClass =

    Pith/arXiv arXiv

  62. [62]

    , year = 2009, month = sep, volume =

    Complex Organic Interstellar Molecules. , year = 2009, month = sep, volume =. doi:10.1146/annurev-astro-082708-101654 , adsurl =

    doi:10.1146/annurev-astro-082708-101654 2009

  63. [63]

    and Williams, David A

    Awad, Zainab and Viti, Serena and Collings, Mark P. and Williams, David A. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2010 , month =. doi:10.1111/j.1365-2966.2010.17077.x , url =

    arXiv 2010

  64. [64]

    , keywords =

    JWST Observations of Young protoStars (JOYS): Overview of gaseous molecular emission and absorption in low-mass protostars. , keywords =. doi:10.1051/0004-6361/202451967 , archivePrefix =. 2410.01636 , primaryClass =

    Pith/arXiv arXiv

  65. [65]

    , keywords =

    An ALMA Survey of H _ 2 CO in Protoplanetary Disks. , keywords =. doi:10.3847/1538-4357/ab64d9 , archivePrefix =. 2002.12525 , primaryClass =

    Pith/arXiv arXiv 2002

  66. [66]

    Survey description and a first look at G9.62+0.19

    ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - I. Survey description and a first look at G9.62+0.19. , keywords =. doi:10.1093/mnras/staa1577 , archivePrefix =. 2006.01549 , primaryClass =

    arXiv 2006

  67. [67]

    The ALMA-QUARKS Survey. I. Survey Description and Data Reduction. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/ad0d5c , archivePrefix =. 2311.08651 , primaryClass =

    Pith/arXiv arXiv

  68. [68]

    , keywords =

    ALMA Observations of Massive Clouds in the Central Molecular Zone: Ubiquitous Protostellar Outflows. , keywords =. doi:10.3847/1538-4357/abde3c , archivePrefix =. 2101.07925 , primaryClass =

    Pith/arXiv arXiv

  69. [69]

    The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview. , keywords =. doi:10.3847/2041-8213/aaf741 , archivePrefix =. 1812.04040 , primaryClass =

    Pith/arXiv arXiv 2041

  70. [70]

    arXiv e-prints , keywords =

    JWST Edge-on Disk Ice (JEDIce): Program overview and ice survey results. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.18163 , archivePrefix =. 2603.18163 , primaryClass =

    doi:10.48550/arxiv.2603.18163

  71. [71]

    , keywords =

    JOYS: MIRI/MRS spectroscopy of gas-phase molecules from the high-mass star-forming region IRAS 23385+6053. , keywords =. doi:10.1051/0004-6361/202348105 , archivePrefix =. 2401.06880 , primaryClass =

    Pith/arXiv arXiv

  72. [72]

    Nature Astronomy , keywords =

    An Ice Age JWST inventory of dense molecular cloud ices. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01875-w , archivePrefix =. 2301.09140 , primaryClass =

    Pith/arXiv arXiv

  73. [73]

    arXiv e-prints , keywords =

    The SPHEREx Ices Investigation: An Overview. arXiv e-prints , keywords =

  74. [74]

    Parallaxes and proper motions of interstellar masers toward the Cygnus X star-forming complex. I. Membership of the Cygnus X region. , keywords =. doi:10.1051/0004-6361/201118211 , archivePrefix =. 1111.7023 , primaryClass =

    Pith/arXiv arXiv

  75. [75]

    arXiv e-prints , keywords =

    The Colors of Ices: Measuring ice column density through photometry. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.00292 , archivePrefix =. 2510.00292 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2510.00292

  76. [76]

    , keywords =

    JWST Reveals Widespread CO Ice and Gas Absorption in the Galactic Center Cloud G0.253+0.016. , keywords =. doi:10.3847/1538-4357/acfc34 , archivePrefix =. 2308.16050 , primaryClass =

    Pith/arXiv arXiv

  77. [77]

    arXiv e-prints , keywords =

    Mapping CO Ice in a Star-Forming Filament in the 3 kpc Arm with JWST. arXiv e-prints , keywords =. doi:10.48550/arXiv.2509.21763 , archivePrefix =. 2509.21763 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2509.21763

  78. [78]

    , keywords =

    Photometric Mapping of Carbonaceous/Siliceous Dust and Water Ice in the ISM with JWST: Applications to the Dense Sightlines. , keywords =. doi:10.3847/1538-3881/adf103 , archivePrefix =. 2507.17550 , primaryClass =

    Pith/arXiv arXiv

  79. [79]

    , keywords =

    Bolometric Temperatures of Young Stellar Objects. , keywords =. doi:10.1086/186956 , adsurl =

    doi:10.1086/186956

  80. [80]

    , keywords =

    Fractionation in young cores: Direct determinations of nitrogen and carbon fractionation in HCN. , keywords =. doi:10.1051/0004-6361/202449344 , archivePrefix =. 2403.04408 , primaryClass =

    Pith/arXiv arXiv

Showing first 80 references.