REVIEW 3 major objections 1 minor 63 references
Generalized Few-Shot Out-of-Distribution Detection
T0 review · 3 major / 1 minor · reviewed 2026-08-05 · deepseek-v4-flash
Pith's one-line read Few-shot OOD detection can be provably improved by balancing general and task-specific knowledge.
desk verdict The abstract promises a provable generalization bound for few-shot OOD detection via a general knowledge model, but the supplied full text is an unrelated astro-ph paper, so the central claim is not reviewable. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
The central objects are the General Knowledge Model (GKM), a pre-trained model whose output distribution serves as a proxy for general knowledge of the open world, and the GS-balance, a derived condition that balances this general knowledge against the specificity of the few-shot data. Knowledge Dynamic Embedding (KDE) is the mechanism that dynamically aligns the OOD detector's output distribution to the GKM based on the GKM's Generalized Belief (G-Belief); this alignment is what the paper claims realizes the GS-balance and tightens the generalization bound.
What would settle it
Train GOOD with a GKM whose pretraining data has no overlap with either the few-shot classes or the OOD test distribution; if the promised generalization-error reduction and benchmark gains persist despite this total mismatch, the transferability assumption behind GS-balance is not doing the work claimed. Alternatively, compute the claimed upper bound for a family of GKMs with increasing miscalibration and test whether the bound tightens or loosens as predicted.
Extended reading notes
Core claim
The central claim is that few-shot OOD detection can be formulated as a trade-off between general knowledge, what a large pre-trained model knows about the open world, and task-specific knowledge, what the few support examples say, and that balancing these two provably reduces the generalization-error upper bound. The paper introduces the GOOD framework, which uses an auxiliary General Knowledge Model (GKM) instead of direct few-shot learning, derives the GS-balance condition from a generalization perspective, and implements it with Knowledge Dynamic Embedding (KDE). KDE dynamically aligns the OOD detector's output distribution to the general knowledge model based on the Generalized Belief (
Load-bearing premise
The load-bearing premise is that the General Knowledge Model's output distribution is a trustworthy proxy for genuinely general knowledge about the open world, so aligning the few-shot model to it reduces bias rather than injecting it.
Editorial extensions
If this is right
- If correct, few-shot OOD detectors can be built by transferring knowledge from a large pre-trained model rather than relying on the scarce support set alone.
- The GS-balance gives a principled target: detector outputs should sit at the equilibrium between general and task-specific knowledge, not at either extreme.
- KDE provides a concrete, adaptive way to reach that target by weighting general-knowledge guidance according to the GKM's belief.
- The framework should transfer across different few-shot regimes and OOD benchmarks if the theoretical bound is the active mechanism.
- The GS-balance could serve as a design criterion for choosing or fine-tuning the auxiliary general knowledge model.
Reading between the lines
- The framework's success likely depends on the choice of GKM; a model whose pretraining distribution excludes the deployment domain could turn alignment into a source of bias rather than a cure.
- The same GS-balance argument could be transposed to other few-shot tasks such as open-set recognition, novelty detection, or few-shot calibration, since the formal object is a balance between general and specific knowledge.
- A natural ablation is to replace the dynamic G-Belief weighting with a fixed, non-adaptive alignment strength; if performance does not drop, the dynamics of KDE are not the active ingredient.
- The manuscript body supplied with this record is an unrelated astronomy study, so the claims above rest on the abstract alone and the proof and full text should be verified before treating the theoretical bound as established.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The submission is an abstract for a paper titled 'Generalized Few-Shot Out-of-Distribution Detection' (arXiv:2508.05732, cs.CV), which claims to propose a GOOD framework that augments a few-shot OOD detector with a General Knowledge Model (GKM), a Knowledge Dynamic Embedding (KDE) mechanism, and a theoretically derived GS-balance that provably reduces a generalization-error upper bound. Experiments on real-world OOD benchmarks are asserted to show superiority. However, the supplied full text is not this paper; it is an unrelated astrophysics manuscript (arXiv:2508.05742, astro-ph) on binary supermassive black holes and Rubin LSST. Consequently, none of the technical content claimed in the abstract—derivation of GS-balance, definition of G-Belief, the KDE mechanism, or experimental tables—is present in the material provided for review.
Significance. If the claims in the abstract were substantiated, the work could be significant: a principled generalization bound for few-shot OOD detection, a theoretically motivated alignment with a general knowledge model, and strong empirical results on real-world benchmarks would be a valuable contribution to the field. The paper would also be notable for attempting to bridge few-shot learning and OOD detection with a provable bound. However, because the submitted full text does not contain the described method, theory, or experiments, the significance cannot be assessed. The potential significance is real but entirely conditional on content that is absent from the review package.
major comments (3)
- [Full Text (entire submission)] The supplied full text is not the manuscript described in the abstract. It is arXiv:2508.05742, an astro-ph paper titled 'The Consequences of Rubin Observatory Time-Domain Survey Design and Host-Galaxy Contamination on the Identification of Binary Supermassive Black Holes.' There is no overlap with few-shot OOD detection. Thus, the core artifacts needed to evaluate the paper—the GS-balance derivation, the KDE mechanism, the G-Belief definition, and the experimental comparisons—are entirely missing. This is a load-bearing deficiency: the central claim cannot be checked in any form.
- [Abstract: 'provably reduces the upper bound of generalization error'] The abstract asserts a mathematical theorem, but no theorem statement, proof, or even a definition of the GS-balance or the generalization error bound appears anywhere in the supplied text. A necessary condition for accepting such a claim is a precise statement of the assumptions under which the bound is reduced, and an explanation of how the alignment with the GKM enters the bound. Moreover, because the G-Belief is said to be computed from the GKM's outputs, there is a risk of circularity: if the bound is stated 'with a general knowledge model' and the same model's outputs are used to define the alignment, the bound might be reduced by construction rather than by substantive generalization. Without the derivation, this risk cannot be resolved.
- [Abstract: 'Experiments on real-world OOD benchmarks demonstrate our superiority'] No experiments, benchmark descriptions, baselines, evaluation metrics, or numerical results are provided. The empirical claim is therefore unsupported. A reviewer cannot assess whether the method outperforms existing few-shot OOD detectors, what datasets are used, or whether the comparisons are fair. As with the theoretical claim, the absence of this content is a fundamental reviewability failure.
minor comments (1)
- [Abstract] The abstract mentions 'Codes will be available' but provides no link or repository identifier. This is not a blocking issue, but it is customary to include a URL or specify that code will be released upon publication.
Circularity Check
No circularity can be established: the supplied full text is an unrelated astro-ph paper, and the target abstract contains no derivation chain to audit.
full rationale
The only in-scope text from the target paper is its abstract, which asserts that the authors 'theoretically derive the Generality-Specificity balance' and propose KDE/G-Belief, but it provides no equations, no definitions of G-Belief, and no experimental details. The supplied 'FULL TEXT' is arXiv:2508.05742, an entirely different astro-ph paper on binary supermassive black holes, not the cs.CV manuscript under review. Under the hard rule that circularity can only be claimed when the paper's own equations or explicit self-citations exhibit a reduction to inputs, there is no quotable derivation chain to walk. The reader's suggestion that GS-balance might be self-referential because G-Belief is computed from the same GKM's outputs is plausible-sounding but unsupported by any concrete equation or definition in the provided material. Likewise, the transferability concern about GKM's 'general knowledge' is a substantive correctness risk, not a demonstrated circularity. Therefore the honest finding is no significant circularity on the evidence available, with score 0.
Assumptions & free parameters
free parameters (1)
- GS-balance weighting coefficient (inferred) =
not stated in abstract
assumptions (4)
- domain assumption A pre-trained General Knowledge Model provides transferable, reliable knowledge about the open world that is informative for the target few-shot OOD task.
- domain assumption The generalization error upper bound derived (GS-balance) is non-vacuous and its terms are computable from few-shot data.
- domain assumption The few-shot support set and the test-time OOD distribution satisfy standard distributional assumptions needed for a PAC-style generalization bound.
- domain assumption The real-world OOD benchmarks used in the experiments are a faithful proxy for open-world deployment.
invented entities (2)
-
General Knowledge Model (GKM)
-
G-Belief (Generalized Belief)
Cite this review
Pith. "Pith review of Generalized Few-Shot Out-of-Distribution Detection." pith.science (2026). https://pith.science/paper/OUQIZMEE
@misc{pith2026250805732,
author = {Pith},
title = {Pith review of: Generalized Few-Shot Out-of-Distribution Detection},
year = {2026},
howpublished = {\url{https://pith.science/paper/OUQIZMEE}},
note = {Machine review of arXiv:2508.05732}
}
read the original abstract
Few-shot Out-of-Distribution (OOD) detection has emerged as a critical research direction in machine learning for practical deployment. Most existing Few-shot OOD detection methods suffer from insufficient generalization capability for the open world. Due to the few-shot learning paradigm, the OOD detection ability is often overfit to the limited training data itself, thus degrading the performance on generalized data and performing inconsistently across different scenarios. To address this challenge, we proposed a Generalized Few-shot OOD Detection (GOOD) framework, which empowers the general knowledge of the OOD detection model with an auxiliary General Knowledge Model (GKM), instead of directly learning from few-shot data. We proceed to reveal the few-shot OOD detection from a generalization perspective and theoretically derive the Generality-Specificity balance (GS-balance) for OOD detection, which provably reduces the upper bound of generalization error with a general knowledge model. Accordingly, we propose a Knowledge Dynamic Embedding (KDE) mechanism to adaptively modulate the guidance of general knowledge. KDE dynamically aligns the output distributions of the OOD detection model to the general knowledge model based on the Generalized Belief (G-Belief) of GKM, thereby boosting the GS-balance. Experiments on real-world OOD benchmarks demonstrate our superiority. Codes will be available.
Reference graph
Works this paper leans on
-
[1]
Agazie, G., Anumarlapudi, A., Archibald, A. M., et al. 2023a, ApJL, 952, L37, doi: 10.3847/2041-8213/ace18b —. 2023b, ApJL, 951, L8, doi: 10.3847/2041-8213/acdac6
-
[2]
Allam, T., & McEwen, J. D. 2021, Paying Attention to Astronomical Transients: Introducing the Time-series Transformer for Photometric Classification, arXiv, doi: 10.48550/ARXIV.2105.06178
-
[3]
2017, Laser Interferometer Space Antenna, arXiv, doi: 10.48550/ARXIV.1702.00786
Amaro-Seoane, P., Audley, H., Babak, S., et al. 2017, Laser Interferometer Space Antenna, arXiv, doi: 10.48550/ARXIV.1702.00786
- [4]
-
[5]
Artymowicz, P., & Lubow, S. H. 1996, ApJL, 467, L77, doi: 10.1086/310200
doi:10.1086/310200 1996
-
[6]
Barth, A. J., & Stern, D. 2018, The Astrophysical Journal, 859, 10, doi: 10.3847/1538-4357/aab3c5
-
[7]
Bianco, F. B., Ivezi´ c,ˇZ., Jones, R. L., et al. 2022, ApJS, 258, 1, doi: 10.3847/1538-4365/ac3e72 Bogdanovi´ c, T., Miller, M. C., & Blecha, L. 2022, Living Reviews in Relativity, 25, 3, doi: 10.1007/s41114-022-00037-8
-
[8]
Cackett, E. M., Bentz, M. C., & Kara, E. 2021, iScience, 24, 102557, doi: 10.1016/j.isci.2021.102557
arXiv 2021
Show all 63 references
-
[9]
2016, MNRAS, 463, 2145, doi: 10.1093/mnras/stw1838
Charisi, M., Bartos, I., Haiman, Z., et al. 2016, MNRAS, 463, 2145, doi: 10.1093/mnras/stw1838
2016 doi
-
[10]
Trump, J. R. 2022, MNRAS, 510, 5929, doi: 10.1093/mnras/stab3713
2022 doi
-
[11]
2020, Monthly Notices of the Royal Astronomical Society, 499, 2245, doi: 10.1093/mnras/staa2957
Chen, Y.-C., Liu, X., Liao, W.-T., et al. 2020, Monthly Notices of the Royal Astronomical Society, 499, 2245, doi: 10.1093/mnras/staa2957
2020 doi
-
[12]
2024, MNRAS, 527, 12154, doi: 10.1093/mnras/stad3981
Chen, Y.-J., Zhai, S., Liu, J.-R., et al. 2024, MNRAS, 527, 12154, doi: 10.1093/mnras/stad3981
2024 doi
-
[13]
2018, Reports on Progress in Physics, 82, 016903, doi: 10.1088/1361-6633/aae6b5
Christensen, N. 2018, Reports on Progress in Physics, 82, 016903, doi: 10.1088/1361-6633/aae6b5
2018 doi
-
[14]
2018, The Astrophysical Journal, 867, 66, doi: 10.3847/1538-4357/aae2b4
Comerford, J., Nevin, R., Stemo, A., et al. 2018, The Astrophysical Journal, 867, 66, doi: 10.3847/1538-4357/aae2b4
2018 doi
-
[15]
C., Grace, K
Davis, M. C., Grace, K. E., Trump, J. R., et al. 2024, The Astrophysical Journal, 965, 34, doi: 10.3847/1538-4357/ad276e De Rosa, A., Vignali, C., Bogdanovi´ c, T., et al. 2019, NewAR, 86, 101525, doi: 10.1016/j.newar.2020.101525 D’Orazio, D. J., & Charisi, M. 2023, arXiv e-pr...
2024
- [16]
-
[17]
J., Djorgovski, S
Graham, M. J., Djorgovski, S. G., Stern, D., et al. 2015, Monthly Notices of the Royal Astronomical Society, 453, 1562–1576, doi: 10.1093/mnras/stv1726
2015 doi
-
[18]
F., Richards, G
Hopkins, P. F., Richards, G. T., & Hernquist, L. 2007, ApJ, 654, 731, doi: 10.1086/509629
2007 doi
-
[19]
Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90, doi: 10.1109/MCSE.2007.55 Ivezi´ c,ˇZ. 2017, in New Frontiers in Black Hole Astrophysics, ed. A. Gomboc, Vol. 324, 330–337, doi: 10.1017/S1743921316012424 Ivezi´ c,ˇZ., Kahn, S. M., Tyson, J. A., et al. 2019, ApJ, ...
2007 doi
- [20]
-
[21]
Z., D’Orazio, D
Kelley, L. Z., D’Orazio, D. J., & Di Stefano, R. 2021, MNRAS, 508, 2524, doi: 10.1093/mnras/stab2776
2021 doi
-
[22]
Z., Haiman, Z., Sesana, A., & Hernquist, L
Kelley, L. Z., Haiman, Z., Sesana, A., & Hernquist, L. 2019, Monthly Notices of the Royal Astronomical Society, 485, 1579, doi: 10.1093/mnras/stz150
2019 doi
-
[23]
C., Bechtold, J., & Siemiginowska, A
Kelly, B. C., Bechtold, J., & Siemiginowska, A. 2009, ApJ, 698, 895, doi: 10.1088/0004-637X/698/1/895
2009 doi
-
[24]
C., Becker, A
Kelly, B. C., Becker, A. C., Sobolewska, M., Siemiginowska, A., & Uttley, P. 2014, ApJ, 788, 33, doi: 10.1088/0004-637X/788/1/33
2014 doi
-
[25]
C., & Shen, Y
Kelly, B. C., & Shen, Y. 2013, The Astrophysical Journal, 764, 45, doi: 10.1088/0004-637X/764/1/45
2013 doi
-
[26]
J., Treister, E., Kakkad, D., et al
Koss, M. J., Treister, E., Kakkad, D., et al. 2023, The Astrophysical Journal Letters, 942, L24, doi: 10.3847/2041-8213/aca8f0 Koz lowski, S. 2016, Monthly Notices of the Royal Astronomical Society, 459, 2787, doi: 10.1093/mnras/stw819 16 Davis et al. Koz lowski, S., Kochanek,...
2023 doi
-
[27]
Kulkarni, G., Worseck, G., & Hennawi, J. F. 2019, MNRAS, 488, 1035, doi: 10.1093/mnras/stz1493
2019 doi
-
[28]
I.-H., Shen, Y., Ho, L
Li, J. I.-H., Shen, Y., Ho, L. C., et al. 2023, The Astrophysical Journal, 954, 173, doi: 10.3847/1538-4357/acddda
2023 doi
-
[29]
2019, ApJ, 884, 36, doi: 10.3847/1538-4357/ab40cb
Liu, T., Gezari, S., Ayers, M., et al. 2019, ApJ, 884, 36, doi: 10.3847/1538-4357/ab40cb
2019 doi
- [30]
-
[31]
I., & Milosavljevi´ c, M
MacFadyen, A. I., & Milosavljevi´ c, M. 2008, The Astrophysical Journal, 672, 83, doi: 10.1086/523869
2008 doi
-
[32]
L., Ivezi´ c,ˇZ ., Kochanek, C
MacLeod, C. L., Ivezi´ c,ˇZ ., Kochanek, C. S., et al. 2010, The Astrophysical Journal, 721, 1014, doi: 10.1088/0004-637x/721/2/1014
2010 doi
-
[33]
L., Ivezi´ c,ˇZ., Sesar, B., et al
MacLeod, C. L., Ivezi´ c,ˇZ., Sesar, B., et al. 2012, ApJ, 753, 106, doi: 10.1088/0004-637X/753/2/106
2012 doi
-
[34]
McLaughlin, M. A. 2013, Classical and Quantum Gravity, 30, 224008, doi: 10.1088/0264-9381/30/22/224008
2013 doi
-
[35]
2013, MNRAS, 432, 1203, doi: 10.1093/mnras/stt536
McQuillan, A., Aigrain, S., & Mazeh, T. 2013, MNRAS, 432, 1203, doi: 10.1093/mnras/stt536
2013 doi
-
[36]
2009, The Astrophysical Journal, 708, 137, doi: 10.1088/0004-637X/708/1/137
Merloni, A., Bongiorno, A., Bolzonella, M., et al. 2009, The Astrophysical Journal, 708, 137, doi: 10.1088/0004-637X/708/1/137
2009 doi
-
[37]
T., Shannon, R
Miles, M. T., Shannon, R. M., Reardon, D. J., et al. 2025, MNRAS, 536, 1489, doi: 10.1093/mnras/stae2571
2025 doi
-
[38]
F., Edelson, R., Baumgartner, W., & Gandhi, P
Mushotzky, R. F., Edelson, R., Baumgartner, W., & Gandhi, P. 2011, The Astrophysical Journal, 743, L12, doi: 10.1088/2041-8205/743/1/l12
2011 doi
-
[39]
B., & Ingargiola, A
Newville, M., Stensitzki, T., Allen, D. B., & Ingargiola, A. 2014, LMFIT: Non-Linear Least-Square Minimization and Curve-Fitting for Python, 0.8.0, Zenodo, doi: 10.5281/zenodo.11813
2014 doi
-
[40]
Y., Ho, L
Peng, C. Y., Ho, L. C., Impey, C. D., & Rix, H.-W. 2010, AJ, 139, 2097, doi: 10.1088/0004-6256/139/6/2097
2010 doi
-
[41]
Peterson, B. M. 1993, PASP, 105, 247, doi: 10.1086/133140 Planck Collaboration, Aghanim, N., Akrami, Y., et al. 2018, Astronomy & Astrophysics, 641, A6, doi: 10.1051/0004-6361/201833910
1993 doi
- [42]
-
[43]
J., Zic, A., Shannon, R
Reardon, D. J., Zic, A., Shannon, R. M., et al. 2023a, The Astrophysical Journal Letters, 951, L6, doi: 10.3847/2041-8213/acdd02
-
[44]
E., Charisi, M., et al
Robnik, J., Bayer, A. E., Charisi, M., et al. 2024, MNRAS, 534, 1609, doi: 10.1093/mnras/stae2220
2024 doi
-
[45]
Scargle, J. D. 1982, ApJ, 263, 835, doi: 10.1086/160554
1982 doi
-
[46]
Sesana, A., Haiman, Z., Kocsis, B., & Kelley, L. Z. 2018, The Astrophysical Journal, 856, 42, doi: 10.3847/1538-4357/aaad0f
2018 doi
-
[47]
Sesana, A., Vecchio, A., & Colacino, C. N. 2008, Monthly Notices of the Royal Astronomical Society, 390, 192, doi: 10.1111/j.1365-2966.2008.13682.x
2008
-
[48]
F., Faucher-Gigu` ere, C.-A., et al
Shen, X., Hopkins, P. F., Faucher-Gigu` ere, C.-A., et al. 2020, Monthly Notices of the Royal Astronomical Society, 495, 3252, doi: 10.1093/mnras/staa1381
2020 doi
-
[49]
2013, WFIRST-2.4: What Every Astronomer Should Know
Spergel, D., Gehrels, N., Breckinridge, J., et al. 2013, WFIRST-2.4: What Every Astronomer Should Know. https://arxiv.org/abs/1305.5425
2013 arXiv
-
[50]
2015, Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report
Spergel, D., Gehrels, N., Baltay, C., et al. 2015, Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report. https://arxiv.org/abs/1503.03757
2015 arXiv
-
[51]
L., Ivezi´ c,ˇZ., & MacLeod, C
Suberlak, K. L., Ivezi´ c,ˇZ., & MacLeod, C. 2021, ApJ, 907, 96, doi: 10.3847/1538-4357/abc698 van der Walt, S., Colbert, S. C., & Varoquaux, G. 2011, Computing in Science Engineering, 13, 22 Van Wassenhove, S., Volonteri, M., Mayer, L., et al. 2012, ApJL, 748, L7, doi: 10.108...
2021 doi
-
[52]
2012, in Conference on Intelligent Data Understanding (CIDU), 47 –54, doi: 10.1109/CIDU.2012.6382200
Vanderplas, J., Connolly, A., Ivezi´ c,ˇZ., & Gray, A. 2012, in Conference on Intelligent Data Understanding (CIDU), 47 –54, doi: 10.1109/CIDU.2012.6382200
2012
-
[53]
VanderPlas, J. T. 2018, The Astrophysical Journal Supplement Series, 236, 16, doi: 10.3847/1538-4365/aab766
2018 doi
-
[54]
G., et al
Vaughan, S., Uttley, P., Markowitz, A. G., et al. 2016, MNRAS, 461, 3145, doi: 10.1093/mnras/stw1412
2016 doi
-
[55]
E., et al
Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, 17, 261, doi: https://doi.org/10.1038/s41592-019-0686-2
2020 doi
-
[56]
2022, PhRvD, 106, 103010, doi: 10.1103/PhysRevD.106.103010
Haiman, Z. 2022, PhRvD, 106, 103010, doi: 10.1103/PhysRevD.106.103010
2022 doi
-
[57]
C., Brunner, R
Wilhite, B. C., Brunner, R. J., Grier, C. J., Schneider, D. P., & Vanden Berk, D. E. 2008, Monthly Notices of the Royal Astronomical Society, 383, 1232, doi: 10.1111/j.1365-2966.2007.12655.x
2008
-
[58]
A., Charisi, M., Taylor, S
Witt, C. A., Charisi, M., Taylor, S. R., & Burke-Spolaor, S. 2022, The Astrophysical Journal, 936, 89, doi: 10.3847/1538-4357/ac8356 Rubin Survey Design Consequences for Binary SMBHs 17
2022 doi
-
[59]
2021, Monthly Notices of the Royal Astronomical Society, 506, 2408, doi: 10.1093/mnras/stab1856
Xin, C., & Haiman, Z. 2021, Monthly Notices of the Royal Astronomical Society, 506, 2408, doi: 10.1093/mnras/stab1856
2021 doi
-
[60]
Graham, M. J. 2022, ApJ, 936, 132, doi: 10.3847/1538-4357/ac8351
2022 doi
-
[61]
2020, ApJ, 900, 117, doi: 10.3847/1538-4357/abac5a
Zhu, X.-J., & Thrane, E. 2020, ApJ, 900, 117, doi: 10.3847/1538-4357/abac5a
2020 doi
-
[62]
J., Hobbs, G., Wen, L., et al
Zhu, X. J., Hobbs, G., Wen, L., et al. 2014, MNRAS, 444, 3709, doi: 10.1093/mnras/stu1717
2014 doi
-
[63]
S., Koz lowski, S., & Udalski, A
Zu, Y., Kochanek, C. S., Koz lowski, S., & Udalski, A. 2013, The Astrophysical Journal, 765, 106, doi: 10.1088/0004-637X/765/2/106
2013 doi
Reviewed August 5, 2026 · model on record in the stance chip above.
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