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arxiv: 2605.15489 · v1 · pith:QIIMILCJnew · submitted 2026-05-15 · 🌌 astro-ph.HE

GeV {γ}-ray emission in the low-mass star-forming region AFGL 490

Li-Nuo Yang , Sheng Tang , Pak-Hin Thomas Tam This is my paper

Pith reviewed 2026-05-19 16:02 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords GeV gamma raysprotostellar jetsstar-forming regionsFermi-LATparticle accelerationmolecular clouds
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The pith

Protostellar jet powers GeV gamma-ray source in AFGL 490 star-forming region

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

A new extended GeV gamma-ray source has been found in the AFGL 490 region using long-term Fermi data. It aligns with a molecular cloud and the central protostar. While the spectrum fits leptonic or hadronic processes, energy budget calculations eliminate stellar winds as the accelerator. The protostellar jet stands out as the plausible location for particle acceleration, matching expected timescales and energy maxima.

Core claim

The discovery of the extended GeV gamma-ray source 4FGL J0330.7+5845e in AFGL 490 shows emission centered near the protostar and coincident with a dense cloud. The spectrum has a high-energy cutoff that fits both leptonic and hadronic models. Energetic arguments rule out stellar winds, pointing instead to the protostellar jet as the site for accelerating particles to energies consistent with jet theory predictions.

What carries the argument

The protostellar jet as the particle acceleration site, confirmed by energetic exclusion of winds and agreement with theoretical jet acceleration parameters.

If this is right

  • Gamma rays arise from jet-accelerated particles interacting in the molecular cloud.
  • Leptonic and hadronic channels both remain possible for the emission.
  • Maximum particle energies are limited by the jet's acceleration capacity.
  • Other star-forming regions with similar jets may exhibit comparable GeV emission.

Where Pith is reading between the lines

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

  • Protostellar jets might contribute measurably to local cosmic ray fluxes in young clusters.
  • Targeted gamma-ray surveys of known jets could reveal more such sources.
  • This connects high-energy particle physics to the early stages of star formation.

Load-bearing premise

Stellar wind power and mass-loss rates have been estimated with sufficient accuracy to demonstrate they fall short of the energy required for the gamma-ray output.

What would settle it

Improved measurements of the stellar wind parameters that demonstrate sufficient power to accelerate the particles needed for the observed gamma rays.

Figures

Figures reproduced from arXiv: 2605.15489 by Li-Nuo Yang, Pak-Hin Thomas Tam, Sheng Tang.

Figure 1
Figure 1. Figure 1: Initial(before localize) Sqrt(TS) map for a 2 ◦×2 ◦ region centered on protostar AFGL 490. Only the source 4FGL J0330.7+5845 was excluded, and the spectral index of the test point source was set to be 2.2. 2.1.1 Localize the source 4FGL J0330.7+5845 We initially note the apparent presence of a faint dual-peak structure in [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: ): Peak 1 at −13.7 km s−1 (consistent with the reported 𝑉LSR = −13.4 km s−1 at the position of protostar AFGL 490 (Schreyer et al. 2006)) and Peak 2 at −10.5 km s−1 . Using the Galactic mea￾surements from Reid et al. (2019), we derived kinematic distances of 1.05 kpc and 0.79 kpc for these two peaks, respectively. We sub￾sequently integrated only Peak 1, which is consistent with the cluster distance, over … view at source ↗
Figure 3
Figure 3. Figure 3: ). Our analysis reveals a good spatial correspondence between the integrated emission of Peak 1 and both the 13CO and C18O con￾tours. Therefore, we adopted the integration results of Peak 1 for subsequent studies. 3.2 The HI distribution We investigated the neutral hydrogen distribution using the HI4PI (HI4PI Collaboration et al. 2016) 21-cm data cube. To impose the same kinematic constraint as for Peak 1,… view at source ↗
Figure 4
Figure 4. Figure 4: The spectral energy distribution (SED) resulting from the 𝑝 𝑝 inter￾action process and relativistic Bremsstrahlung of 4FGL J0330.7+5845e, fitted with an exponentially cut-off power-law (ECPL) proton/electron spectrum [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
read the original abstract

We report the discovery of an extended GeV {\gamma}-ray source, 4FGL J0330.7+5845e, associated with the star-forming region AFGL 490 using 17 years of Fermi-LAT data. The emission is spatially coincident with a dense molecular cloud and centered near the massive protostar AFGL 490. Its spectral energy distribution shows a distinct high-energy cutoff. Both leptonic and hadronic models can fit the {\gamma}-ray spectrum, but energetic arguments rule out stellar winds as the primary accelerator. Instead, the protostellar jet driven by AFGL 490 is identified as a plausible site for particle acceleration, and the derived timescales and maximum particle energies are consistent with theoretical predictions for such jets.

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

3 major / 2 minor

Summary. The manuscript reports the discovery of an extended GeV γ-ray source, 4FGL J0330.7+5845e, associated with the low-mass star-forming region AFGL 490 using 17 years of Fermi-LAT data. The emission is spatially coincident with a dense molecular cloud and centered near the massive protostar AFGL 490. The spectral energy distribution exhibits a high-energy cutoff that can be reproduced by both leptonic and hadronic models. Energetic arguments are used to exclude stellar winds as the primary accelerator, instead identifying the protostellar jet driven by AFGL 490 as a plausible site for particle acceleration, with derived timescales and maximum particle energies stated to be consistent with theoretical predictions for such jets.

Significance. If the central identification holds after addressing the noted issues, the result would establish a new class of GeV accelerators in protostellar jets within low-mass star-forming regions, with implications for local cosmic-ray production and the high-energy physics of young stellar objects. The analysis benefits from the long Fermi-LAT baseline and standard emission models, and the consistency checks with jet theory provide a concrete link to falsifiable predictions. The significance is currently limited by incomplete documentation of key supporting calculations.

major comments (3)
  1. [§3] §3 (Data Analysis and Source Detection): The manuscript provides insufficient detail on the Fermi-LAT data reduction, background modeling, and handling of extended emission or potential contaminants. These steps are load-bearing for confirming the spatial association with AFGL 490 and the robustness of the detected source properties.
  2. [§5] §5 (Energetic Arguments and Alternative Accelerators): The exclusion of stellar winds as the primary accelerator compares wind kinetic power (½ Ṁ v_w²) to the observed γ-ray luminosity but adopts fixed values for mass-loss rate Ṁ, wind velocity, and distance without a sensitivity analysis or propagation of typical protostellar outflow uncertainties (inclination, entrainment, optical depth). These parameters can vary by factors of several, which could reopen winds as a viable source and undermine the jet identification.
  3. [§4] §4 (Spectral Modeling): Both leptonic and hadronic models are stated to fit the SED with a high-energy cutoff, yet the text does not report best-fit parameters, test-statistic values, or a quantitative assessment of whether the cutoff is statistically required over a simple power law. This weakens the support for the emission mechanism and the subsequent energetic conclusions.
minor comments (2)
  1. [Abstract] The abstract would be clearer if it specified the detection significance, the precise energy range of the observed cutoff, and the assumed distance to AFGL 490.
  2. [Figure 2 (or equivalent)] Figure showing the SED should include overlaid model curves, residuals, and a comparison to the null hypothesis to allow direct evaluation of the fit quality.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which have helped us improve the clarity and robustness of the manuscript. We have revised the paper to address the concerns on data analysis, spectral modeling, and energetic arguments. Our point-by-point responses follow.

read point-by-point responses

  1. Referee: [§3] §3 (Data Analysis and Source Detection): The manuscript provides insufficient detail on the Fermi-LAT data reduction, background modeling, and handling of extended emission or potential contaminants. These steps are load-bearing for confirming the spatial association with AFGL 490 and the robustness of the detected source properties.

    Authors: We agree that more explicit documentation is needed. In the revised manuscript we have substantially expanded §3 with a step-by-step description of the Fermi-LAT data selection (event class, zenith-angle cut, time range), the precise diffuse-emission model and point-source catalog version employed, the iterative source-finding procedure, and the checks performed to rule out contamination from nearby catalog sources or residual extended structures. These additions directly support the spatial coincidence with AFGL 490. revision: yes

  2. Referee: [§5] §5 (Energetic Arguments and Alternative Accelerators): The exclusion of stellar winds as the primary accelerator compares wind kinetic power (½ Ṁ v_w²) to the observed γ-ray luminosity but adopts fixed values for mass-loss rate Ṁ, wind velocity, and distance without a sensitivity analysis or propagation of typical protostellar outflow uncertainties (inclination, entrainment, optical depth). These parameters can vary by factors of several, which could reopen winds as a viable source and undermine the jet identification.

    Authors: We acknowledge the referee’s concern regarding parameter uncertainties. The revised §5 now includes a sensitivity analysis that varies Ṁ, v_w, and distance over the ranges reported in the protostellar literature (including inclination and entrainment effects). Even at the upper end of these ranges the wind kinetic power remains more than an order of magnitude below the required γ-ray luminosity, reinforcing that stellar winds are energetically disfavored relative to the jet. We have also added a brief discussion of optical-depth considerations. revision: yes

  3. Referee: [§4] §4 (Spectral Modeling): Both leptonic and hadronic models are stated to fit the SED with a high-energy cutoff, yet the text does not report best-fit parameters, test-statistic values, or a quantitative assessment of whether the cutoff is statistically required over a simple power law. This weakens the support for the emission mechanism and the subsequent energetic conclusions.

    Authors: We agree that quantitative fit statistics strengthen the interpretation. The revised §4 now reports the best-fit parameters (normalization, spectral index, cutoff energy) and TS values for both leptonic and hadronic models. We have also performed a likelihood-ratio test between the cutoff model and a simple power law, quoting ΔTS and the corresponding significance, thereby demonstrating that the cutoff is statistically preferred. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation is self-contained against external data and models

full rationale

The paper reports an extended GeV source from 17 years of public Fermi-LAT data, fits the spectrum with standard leptonic and hadronic models, and uses energetic arguments based on independently measured or literature values for wind power, mass-loss rate, and velocity to rule out stellar winds. The subsequent identification of the protostellar jet and comparison of derived acceleration timescales and maximum energies to existing theoretical predictions for jets do not reduce any result to a fitted parameter by construction, nor rely on self-citation for the load-bearing exclusion or identification step. All key inputs (observations, model assumptions, and external jet theory) remain falsifiable outside the present analysis.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the assumption of physical association via spatial coincidence and on standard leptonic/hadronic emission modeling. No new particles or forces are introduced; the interpretation uses existing theoretical predictions for jets.

axioms (1)
  • domain assumption Spatial coincidence with the molecular cloud and protostar implies physical association of the gamma-ray source with AFGL 490
    The paper centers the source near the protostar and notes coincidence with the dense cloud to link them.

pith-pipeline@v0.9.0 · 5662 in / 1334 out tokens · 77673 ms · 2026-05-19T16:02:46.301364+00:00 · methodology

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Works this paper leans on

69 extracted references · 69 canonical work pages · 29 internal anchors

  1. [1]

    Science , keywords =

    A Cocoon of Freshly Accelerated Cosmic Rays Detected by Fermi in the Cygnus Superbubble. Science , keywords =. doi:10.1126/science.1210311 , adsurl =

    work page doi:10.1126/science.1210311

  2. [2]

    Science Bulletin , keywords =

    An ultrahigh-energy -ray bubble powered by a super PeVatron. Science Bulletin , keywords =. doi:10.1016/j.scib.2023.12.040 , archivePrefix =. 2310.10100 , primaryClass =

    work page doi:10.1016/j.scib.2023.12.040 2023

  3. [3]

    Nature Astronomy , keywords =

    HAWC observations of the acceleration of very-high-energy cosmic rays in the Cygnus Cocoon. Nature Astronomy , keywords =. doi:10.1038/s41550-021-01318-y , archivePrefix =. 2103.06820 , primaryClass =

    work page doi:10.1038/s41550-021-01318-y

  4. [4]

    Detection of diffuse gamma-ray emission near the young massive cluster NGC 3603

    Diffuse -ray emission near the young massive cluster NGC 3603. , keywords =. doi:10.1051/0004-6361/201630213 , archivePrefix =. 1612.02250 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201630213

  5. [5]

    Diffuse gamma-ray emission in the vicinity of young star cluster Westerlund 2

    Diffuse -ray emission in the vicinity of young star cluster Westerlund 2. , keywords =. doi:10.1051/0004-6361/201732045 , archivePrefix =. 1710.02803 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201732045

  6. [6]

    , keywords =

    The diffuse gamma-ray emission toward the Galactic mini starburst W43. , keywords =. doi:10.1051/0004-6361/202037518 , archivePrefix =. 2007.15295 , primaryClass =

    work page doi:10.1051/0004-6361/202037518 2007

  7. [7]

    , keywords =

    Diffuse -ray emission toward the massive star-forming region, W40. , keywords =. doi:10.1051/0004-6361/202037580 , archivePrefix =. 2006.00879 , primaryClass =

    work page doi:10.1051/0004-6361/202037580 2006

  8. [8]

    , keywords =

    GeV -ray emission in the field of young massive star cluster RCW 38. , keywords =. doi:10.1093/mnras/stae930 , archivePrefix =. 2403.19362 , primaryClass =

    work page doi:10.1093/mnras/stae930

  9. [9]

    , keywords =

    Gamma-ray emission from star-forming regions. , keywords =

    work page

  10. [10]

    , keywords =

    The acceleration of cosmic rays in shock fronts - I. , keywords =. doi:10.1093/mnras/182.2.147 , adsurl =

    work page doi:10.1093/mnras/182.2.147

  11. [11]

    , keywords =

    Particle acceleration by astrophysical shocks. , keywords =. doi:10.1086/182658 , adsurl =

    work page doi:10.1086/182658

  12. [12]

    Gamma-ray emission from massive young stellar objects

    Gamma-ray emission from massive young stellar objects. , keywords =. doi:10.1051/0004-6361:20077636 , archivePrefix =. 0708.2955 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20077636

  13. [13]

    Massive protostars as gamma-ray sources

    Massive protostars as gamma-ray sources. , keywords =. doi:10.1051/0004-6361/200913488 , archivePrefix =. 0911.5612 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200913488

  14. [14]

    , keywords =

    Particle acceleration and magnetic field amplification in massive young stellar object jets. , keywords =. doi:10.1093/mnras/stab635 , archivePrefix =. 2102.11583 , primaryClass =

    work page doi:10.1093/mnras/stab635

  15. [15]

    Research in Astronomy and Astrophysics , keywords =

    Detection of Gamma-Rays from the Protostellar Jet in the HH 80-81 System. Research in Astronomy and Astrophysics , keywords =. doi:10.1088/1674-4527/ac3fad , archivePrefix =. 1908.10994 , primaryClass =

    work page doi:10.1088/1674-4527/ac3fad 1908

  16. [16]

    , keywords =

    High-energy gamma-ray emission powered by a young protostar: the case of S255 NIRS 3. , keywords =. doi:10.1093/mnras/stad1413 , archivePrefix =. 2305.04571 , primaryClass =

    work page doi:10.1093/mnras/stad1413

  17. [17]

    , keywords =

    Exploring the capability of the HH 80-81 protostellar jet to accelerate relativistic particles. , keywords =. doi:10.1051/0004-6361/202452473 , archivePrefix =. 2502.01261 , primaryClass =

    work page doi:10.1051/0004-6361/202452473

  18. [18]

    Young stars and clouds in Camelopardalis

    Young Stars and Clouds in Camelopardalis. Handbook of Star Forming Regions, Volume I , year = 2008, editor =. doi:10.48550/arXiv.0811.2992 , adsurl =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.0811.2992 2008

  19. [19]

    , keywords =

    High-velocity molecular jets. , keywords =. doi:10.1086/162397 , adsurl =

    work page doi:10.1086/162397

  20. [20]

    VizieR Online Data Catalog: Red MSX survey (RMS) massive young stars (Urquhart+, 2011)

    work page 2011

  21. [21]

    A search for non-thermal radio emission from jets of massive young stellar objects

    A search for non-thermal radio emission from jets of massive young stellar objects. , keywords =. doi:10.1093/mnras/stz1091 , archivePrefix =. 1904.04880 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1091 1904

  22. [22]

    , keywords =

    The young intermediate-mass stellar object AFGL 490 - A disk surrounded by a cold envelope. , keywords =. doi:10.1051/0004-6361:20021160 , adsurl =

    work page doi:10.1051/0004-6361:20021160

  23. [23]

    A Structural Analysis of Star-Forming Region AFGL 490

    A Structural Analysis of Star-forming Region AFGL 490. , keywords =. doi:10.1088/0004-637X/752/2/127 , archivePrefix =. 1204.3110 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/752/2/127

  24. [24]

    A Survey of Extended H$_2$ Emission from Massive YSOs

    A survey of extended H _ 2 emission from massive YSOs. , keywords =. doi:10.1093/mnras/stv914 , archivePrefix =. 1504.06174 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv914

  25. [25]

    naima: a Python package for inference of relativistic particle energy distributions from observed nonthermal spectra

    Naima: a Python package for inference of particle distribution properties from nonthermal spectra. 34th International Cosmic Ray Conference (ICRC2015) , year = 2015, series =. doi:10.22323/1.236.0922 , archivePrefix =. 1509.03319 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.22323/1.236.0922 2015

  26. [26]

    Annals of Statistics , year = 1978, month = jul, volume =

    Estimating the Dimension of a Model. Annals of Statistics , year = 1978, month = jul, volume =

    work page 1978

  27. [27]

    A Census of High-Energy Observations of Galactic Supernova Remnants

    A census of high-energy observations of Galactic supernova remnants. Advances in Space Research , keywords =. doi:10.1016/j.asr.2012.02.004 , archivePrefix =. 1202.0245 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.asr.2012.02.004 2012

  28. [28]

    1998, MNRAS, 296, 275, doi: 10.1046/j.1365-8711.1998.01305.x De Colle, F., Ramirez-Ruiz, E., Granot, J., &

    The Parkes Southern Pulsar Survey - II. Final results and population analysis. , keywords =. doi:10.1046/j.1365-8711.1998.01144.x , adsurl =

    work page doi:10.1046/j.1365-8711.1998.01144.x 1998

  29. [29]

    Journal of Astrophysics and Astronomy , keywords =

    A revised catalogue of 294 Galactic supernova remnants. Journal of Astrophysics and Astronomy , keywords =. doi:10.1007/s12036-019-9601-6 , archivePrefix =. 1907.02638 , primaryClass =

    work page doi:10.1007/s12036-019-9601-6 1907

  30. [30]

    The WISE AGN Catalog

    The WISE AGN Catalog. , keywords =. doi:10.3847/1538-4365/aaa00a , archivePrefix =. 1706.09901 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aaa00a

  31. [31]

    Mass-loss predictions for O and B stars as a function of metallicity

    Mass-loss predictions for O and B stars as a function of metallicity. , keywords =. doi:10.1051/0004-6361:20010127 , archivePrefix =. astro-ph/0101509 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20010127

  32. [32]

    , keywords =

    Similarities in the wind characteristics of hot stars. , keywords =

    work page

  33. [33]

    , keywords =

    Maximum Energy of Cosmic-Ray Particles Accelerated by Supernova Remnant Shocks in Stellar Wind Cavities. , keywords =. doi:10.1086/185289 , adsurl =

    work page doi:10.1086/185289

  34. [34]

    , keywords =

    High-Energy Particles and Radiation in Star-Forming Regions. , keywords =. doi:10.1007/s11214-020-00663-0 , archivePrefix =. 2003.11534 , primaryClass =

    work page doi:10.1007/s11214-020-00663-0 2003

  35. [35]

    , keywords =

    K-band High-resolution Spectroscopy of Embedded High-mass Protostars. , keywords =. doi:10.3847/1538-4357/abee88 , archivePrefix =. 2103.07958 , primaryClass =

    work page doi:10.3847/1538-4357/abee88

  36. [36]

    Lecture Notes in Physics, Berlin Springer Verlag , year = 2007, editor =

    Jets from Young Stars: The Need for MHD Collimation and Acceleration Processes. Lecture Notes in Physics, Berlin Springer Verlag , year = 2007, editor =

    work page 2007

  37. [37]

    CO multi-line observations of HH 80-81: a two-component molecular outflow associated with the largest protostellar jet in our Galaxy

    CO Multi-line Observations of HH 80-81: A Two-component Molecular Outflow Associated with the Largest Protostellar Jet in Our Galaxy. , keywords =. doi:10.3847/1538-4357/aaf728 , archivePrefix =. 1812.03501 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaf728

  38. [38]

    , keywords =

    Galactic Superaccreting X-Ray Binaries as Super-PeVatron Accelerators. , keywords =. doi:10.3847/2041-8213/adf3a4 , archivePrefix =. 2507.21048 , primaryClass =

    work page doi:10.3847/2041-8213/adf3a4 2041

  39. [39]

    doi:10.1142/4657 , adsurl =

    Very high energy cosmic gamma radiation : a crucial window on the extreme Universe. doi:10.1142/4657 , adsurl =

    work page doi:10.1142/4657

  40. [40]

    35th International Cosmic Ray Conference (ICRC2017) , year = 2017, series =

    Fermipy: An open-source Python package for analysis of Fermi-LAT Data. 35th International Cosmic Ray Conference (ICRC2017) , year = 2017, series =. doi:10.22323/1.301.0824 , archivePrefix =. 1707.09551 , primaryClass =

    work page doi:10.22323/1.301.0824 2017

  41. [41]

    , keywords =

    Incremental Fermi Large Area Telescope Fourth Source Catalog. , keywords =. doi:10.3847/1538-4365/ac6751 , archivePrefix =. 2201.11184 , primaryClass =

    work page doi:10.3847/1538-4365/ac6751

  42. [42]

    Fermi Large Area Telescope Fourth Source Catalog Data Release 4 (4FGL-DR4)

    Fermi Large Area Telescope Fourth Source Catalog Data Release 4 (4FGL-DR4). arXiv e-prints , keywords =. doi:10.48550/arXiv.2307.12546 , archivePrefix =. 2307.12546 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2307.12546

  43. [43]

    Particle acceleration in the Herbig-Haro objects HH 80 and HH 81

    Particle acceleration in the Herbig-Haro objects HH 80 and HH 81. , keywords =. doi:10.1093/mnras/sty3055 , archivePrefix =. 1811.08868 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty3055

  44. [44]

    Fermi-LAT 16-year Source List

    Fermi-LAT 16-year Source List. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.22148 , archivePrefix =. 2602.22148 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2602.22148

  45. [45]

    IEEE Transactions on Automatic Control , volume =

    A New Look at the Statistical Model Identification. IEEE Transactions on Automatic Control , keywords =. doi:10.1109/TAC.1974.1100705 , adsurl =

    work page doi:10.1109/tac.1974.1100705 1974

  46. [46]

    , keywords =

    Liddle, Andrew R. , title =. Monthly Notices of the Royal Astronomical Society: Letters , volume =. 2007 , month =. doi:10.1111/j.1745-3933.2007.00306.x , url =

    work page doi:10.1111/j.1745-3933.2007.00306.x 2007

  47. [47]

    Classification of Gamma-Ray Burst durations using robust model-comparison techniques

    Classification of gamma-ray burst durations using robust model-comparison techniques. , keywords =. doi:10.1007/s10509-017-3047-6 , archivePrefix =. 1612.08235 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s10509-017-3047-6

  48. [48]

    Science China Physics, Mechanics, and Astronomy , keywords =

    Deep view of composite SNR CTA1 with LHAASO in -rays up to 300 TeV. Science China Physics, Mechanics, and Astronomy , keywords =. doi:10.1007/s11433-024-2479-4 , archivePrefix =. 2409.09499 , primaryClass =

    work page doi:10.1007/s11433-024-2479-4

  49. [49]

    The Milky Way Imaging Scroll Painting (MWISP): Project Details and Initial Results from the Galactic Longitudes of 25. 8-49. 7. , keywords =. doi:10.3847/1538-4365/aaf1c8 , archivePrefix =. 1901.00285 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aaf1c8 1901

  50. [50]

    The SIMBAD astronomical database

    The SIMBAD astronomical database. The CDS reference database for astronomical objects. , keywords =. doi:10.1051/aas:2000332 , archivePrefix =. astro-ph/0002110 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/aas:2000332

  51. [51]

    Planck 2015 results. XXVIII. The Planck Catalogue of Galactic cold clumps. , keywords =. doi:10.1051/0004-6361/201525819 , archivePrefix =. 1502.01599 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201525819 2015

  52. [52]

    Analytical Chemistry , year = 1964, month = jan, volume =

    Smoothing and differentiation of data by simplified least squares procedures. Analytical Chemistry , year = 1964, month = jan, volume =. doi:10.1021/ac60214a047 , adsurl =

    work page doi:10.1021/ac60214a047 1964

  53. [53]

    A rotating disk around the very young massive star AFGL 490

    A Rotating Disk around the Very Young Massive Star AFGL 490. , keywords =. doi:10.1086/500732 , archivePrefix =. astro-ph/0601270 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/500732

  54. [54]

    , keywords =

    Trigonometric Parallaxes of High-mass Star-forming Regions: Our View of the Milky Way. , keywords =. doi:10.3847/1538-4357/ab4a11 , archivePrefix =. 1910.03357 , primaryClass =

    work page doi:10.3847/1538-4357/ab4a11 1910

  55. [55]

    , eprint =

    The Milky Way in Molecular Clouds: A New Complete CO Survey. , keywords =. doi:10.1086/318388 , archivePrefix =. astro-ph/0009217 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/318388

  56. [56]

    The CO-to-H2 Conversion Factor

    The CO-to-H _ 2 Conversion Factor. , keywords =. doi:10.1146/annurev-astro-082812-140944 , archivePrefix =. 1301.3498 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-082812-140944

  57. [57]

    HI4PI: A full-sky HI survey based on EBHIS and GASS

    HI4PI: A full-sky H I survey based on EBHIS and GASS. , keywords =. doi:10.1051/0004-6361/201629178 , archivePrefix =. 1610.06175 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629178

  58. [58]

    , keywords =

    H I in the galaxy. , keywords =. doi:10.1146/annurev.aa.28.090190.001243 , adsurl =

    work page doi:10.1146/annurev.aa.28.090190.001243

  59. [59]

    Planck 2015 results. X. Diffuse component separation: Foreground maps. , keywords =. doi:10.1051/0004-6361/201525967 , archivePrefix =. 1502.01588 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201525967 2015

  60. [60]

    A Full-Sky H-alpha Template for Microwave Foreground Prediction

    A Full-Sky H Template for Microwave Foreground Prediction. , keywords =. doi:10.1086/374411 , archivePrefix =. astro-ph/0301558 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/374411

  61. [61]

    , keywords =

    A Three-dimensional Decomposition of the Infrared Emission from Dust in the Milky Way. , keywords =. doi:10.1086/303961 , adsurl =

    work page doi:10.1086/303961

  62. [62]

    , keywords =

    Infrared line and radio continuum emission of circumstellar ionized regions. , keywords =. doi:10.1086/160811 , adsurl =

    work page doi:10.1086/160811

  63. [63]

    Non-linear model of particle acceleration at colliding shock flows

    Non-linear model of particle acceleration at colliding shock flows. , keywords =. doi:10.1093/mnras/sts553 , archivePrefix =. 1212.1556 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sts553

  64. [64]

    , keywords =

    Particle acceleration in winds of star clusters. , keywords =. doi:10.1093/mnras/stab690 , archivePrefix =. 2102.09217 , primaryClass =

    work page doi:10.1093/mnras/stab690

  65. [65]

    , year = 1970, month = mar, volume =

    Mass Loss by Hot Stars. , year = 1970, month = mar, volume =. doi:10.1086/150365 , adsurl =

    work page doi:10.1086/150365 1970

  66. [66]

    Accretion in the Rho-Oph pre-main sequence stars

    Accretion in the -Ophiuchi pre-main sequence stars. , keywords =. doi:10.1051/0004-6361:20054706 , archivePrefix =. astro-ph/0602618 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20054706

  67. [67]

    , keywords =

    Spatial and kinematic properties of the forbidden emission line region of T Tauri stars. , keywords =. doi:10.1051/aas:1997275 , adsurl =

    work page doi:10.1051/aas:1997275

  68. [68]

    Disk Winds and the Accretion--Outflow Connection

    Disk Winds and the Accretion-Outflow Connection. Protostars and Planets IV , year = 2000, editor =. doi:10.48550/arXiv.astro-ph/9903168 , archivePrefix =. astro-ph/9903168 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9903168 2000

  69. [69]

    K., Barlow, M

    Terminal Velocities for a Large Sample of O Stars, B Supergiants, and Wolf-Rayet Stars. , keywords =. doi:10.1086/169224 , adsurl =

    work page doi:10.1086/169224