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Significant functionality is under active development, such as a model fitting framework, VO client and server tools, and aperture and point spread function (PSF) photometry tools. The core development team is actively making additions and enhancements to the current code base, and we encourage anyone interested to participate in the development of future Astropy versions.","external_url":"https://arxiv.org/abs/1307.6212","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-07-10T23:57:41.375755+00:00","pith_arxiv_id":"1307.6212","created_at":"2026-05-10T23:25:50.968350+00:00","updated_at":"2026-07-10T23:57:41.375755+00:00","title_quality_ok":true,"display_title":"Astropy: A Community Python Package for Astronomy","render_title":"Astropy: A Community Python Package for Astronomy"},"hub":{"state":{"work_id":"02354d9b-ad6f-4a4e-9720-06d21c2feba5","tier":"super_hub","tier_reason":"100+ Pith inbound or 10,000+ external citations","pith_inbound_count":172,"external_cited_by_count":null,"distinct_field_count":8,"first_pith_cited_at":"2018-11-05T21:35:34+00:00","last_pith_cited_at":"2026-07-09T04:46:17+00:00","author_build_status":"needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-08-21T10:19:24.949369+00:00","tier_text":"super_hub"},"tier":"super_hub","role_counts":[{"context_role":"method","n":7},{"context_role":"background","n":6},{"context_role":"other","n":5},{"context_role":"baseline","n":1},{"context_role":"dataset","n":1},{"context_role":"extension","n":1}],"polarity_counts":[{"context_polarity":"unclear","n":7},{"context_polarity":"use_method","n":7},{"context_polarity":"background","n":4},{"context_polarity":"baseline","n":1},{"context_polarity":"extend","n":1},{"context_polarity":"use_dataset","n":1}],"runs":{"ask_index":{"job_type":"ask_index","status":"succeeded","result":{"title":"Astropy: A Community Python Package for Astronomy","claims":[{"claim_text":"We present the first public version (v0.2) of the open-source and community-developed Python package, Astropy. 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The interactions between these small halos ultimately lead to nonlinear perturbations to the power spectrum, and cause a \"bottom-up\" version of structure formation - large halos containing galaxies are surrounded by smaller \"subhalos\" that contain satellites. 7 10−4 10−2 100 102 k [h/Mpc] 10−3 10−1 101 103 105 P (k) [Mpc 3] CDM WDM IDM 10−2 10−1 100 101 102 k [h/Mpc] 10−3 10−2 10−1 100 101 102 k3P (k)/2π2 Figure 1.1 Left: The linear matter power spectrum atz=0for three different dark matter models. Right: The dimensionless linear matter power spectrum for the same. The dotted vertical line in both panels representskeq= 0.0104Mpc −1. 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IJ acknowledges support from the Research grant TAsP (Theoretical Astroparticle Physics) funded by INFN, and Research grant \"Address- ing systematic uncertainties in searches for dark matter\", Grant No. 2022F2843L funded by the Italian Ministry of University and Research (mur). This work made use of Numpy [201], SciPy [202], astropy [203], matplotlib [204], Jupyter [205], as well as Webplotdigitizer [206]. [1] G. Bertone and D. Hooper, Rev. Mod. Phys. 90, 045002 (2","claim_type":"method","confidence":0.8,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks Astropy: A Community Python Package for Astronomy because it crossed a citation-hub threshold. Current citing contexts most often use it as other evidence (5 contexts).","role_counts":[{"n":5,"context_role":"other"},{"n":4,"context_role":"background"},{"n":4,"context_role":"method"},{"n":1,"context_role":"extension"}]},"error":null,"updated_at":"2026-06-26T03:54:42.089559+00:00"}},"summary":{"title":"Astropy: A Community Python Package for Astronomy","claims":[{"claim_text":"We present the first public version (v0.2) of the open-source and community-developed Python package, Astropy. This package provides core astronomy-related functionality to the community, including support for domain-specific file formats such as Flexible Image Transport System (FITS) files, Virtual Observatory (VO) tables, and common ASCII table formats, unit and physical quantity conversions, physical constants specific to astronomy, celestial coordinate and time transformations, world coordinate system (WCS) support, generalized containers for representing gridded as well as tabular data, a","claim_type":"abstract","evidence_strength":"source_metadata"},{"claim_text":"tidal wraps overlap in certain regions of phase space, making some particles intrinsically more difficult to assign to a unique stripping epoch. By learnings, the network is encouraged to recognize such ambiguous cases and to return appropriately larger predictive uncertainties. We clampsto the interval [−9.2,2.2], which corresponds to confining σ ˆTs to [0.01,3] Gyr, thereby excluding unphysical uncertainty estimates and improving numerical stability during optimization. The loss function adopt","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"With constantly improving detectors and analysis capabilities, we will continue to expand the scope and sensitivity of our tests of GR and our probes of the nature of BHs when analyzing data from O3b and future observing runs. ACKNOWLEDGMENTS Analyses in this paper made use of NumPy[ 271], SciPy [272], Astropy[ 273, 274], IPython[ 275],qnm[ 276], PE- Summary[ 277], and GWpy[ 278]; plots were produced with Matplotlib[ 279], and Seaborn[ 280]. Posteriors were sam- pled with Stan[ 128], CPNest[ 281","claim_type":"other","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"SR/FST/PSII/2021/162(C) awarded to the DAASE, IIT Indore. The authors would like to thank the Square Kilometre Array (SKA) team members for promptly answering queries related to SKA station beam mod- elling.Software: ThisworkisheavilybasedonthePythonprogramminglanguage(https: //www.python.org/). The packages used here areastropy(https://www.astropy. org/, [70, 71] ),numpy(https://numpy.org/), ,h5py(https://www.h5py.org/), matplotlib(https://matplotlib.org/),scipy(https://scipy.org/). A Posterior","claim_type":"method","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"their sensitvity to predictions from specific modified theories of gravity, can play a very important role in constraining beyond- GR physics using future gravitational-wave observations. ACKNOWLEDGMENTS Analyses in this paper made use of NumPy [275], SciPy [276], Astropy [277, 278], IPython [279], qnm [280], PE- Summary [281], and GWpy [282]; plots were produced with Matplotlib[283], and Seaborn [284]. Posteriors were sampled with Stan [285], CPNest [146], PyMultinest [286, 287], Bilby [138, 13","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"(Astropy Collaboration), Astropy: A community Python package for astronomy, Astron. and As- trophys.558, A33 (2013), arXiv:1307.6212 [astro-ph.IM]. [186] A. M. Price-Whelanet al.(Astropy Collaboration), The As- tropy Project: Building an Open-science Project and Status of the v2.0 Core Package, The Astronomical Journal156, 123 (2018), arXiv:1801.02634 [astro-ph.IM]. [187] A. M. Price-Whelanet al.(Astropy Collaboration), The Astropy Project: Sustaining and Growing a Community- oriented Open-sourc","claim_type":"method","confidence":0.85,"evidence_strength":"citation_context"},{"claim_text":"cil under contract 2022-04283. IJ acknowledges support from the Research grant TAsP (Theoretical Astroparticle Physics) funded by INFN, and Research grant \"Address- ing systematic uncertainties in searches for dark matter\", Grant No. 2022F2843L funded by the Italian Ministry of University and Research (mur). This work made use of Numpy [201], SciPy [202], astropy [203], matplotlib [204], Jupyter [205], as well as Webplotdigitizer [206]. [1] G. Bertone and D. Hooper, Rev. Mod. Phys. 90, 045002 (2","claim_type":"method","confidence":0.8,"evidence_strength":"citation_context"}],"why_cited":"Pith tracks Astropy: A Community Python Package for Astronomy because it crossed a citation-hub threshold. 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The interactions between these small halos ultimately lead to nonlinear perturbations to the power spectrum, and cause a \"bottom-up\" version of structure formation - large halos containing galaxies are surrounded by smaller \"subhalos\" that contain satellites. 7 10−4 10−2 100 102 k [h/Mpc] 10−3 10−1 101 103 105 P (k) [Mpc 3] CDM WDM IDM 10−2 10−1 100 101 102 k [h/Mpc] 10−3 10−2 10−1 100 101 102 k3P (k)/2π2 Figure 1.1 Left: The linear matter power spectrum atz=0for three different dark matter models. Right: The dimensionless linear matter power spectrum for the same. The dotted vertical line in both panels representskeq= 0.0104Mpc −1. 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THE KERR NA TURE OF THE REMNANT Identification of two modes in the data can be used to test","citing_arxiv_id":"2509.08054"},{"n":1,"role":"method","polarity":"use_method","paper_title":"INTEGRAL, eROSITA and Voyager Constraints on Light Bosonic Dark Matter: ALPs, Dark Photons, Scalars, $B-L$ and $L_{i}-L_{j}$ Vectors","primary_cat":"hep-ph","context_text":"cil under contract 2022-04283. IJ acknowledges support from the Research grant TAsP (Theoretical Astroparticle Physics) funded by INFN, and Research grant \"Address- ing systematic uncertainties in searches for dark matter\", Grant No. 2022F2843L funded by the Italian Ministry of University and Research (mur). This work made use of Numpy [201], SciPy [202], astropy [203], matplotlib [204], Jupyter [205], as well as Webplotdigitizer [206]. [1] G. Bertone and D. Hooper, Rev. Mod. Phys. 90, 045002 (2018), arXiv:1605.04909 [astro-ph.CO]. [2] G. Bertone and T. Tait, M. P., Nature 562, 51 (2018), arXiv:1810.01668 [astro-ph.CO]. [3] P. 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