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    "title": "Astrometric microlensing measures the mass of white dwarf Stein 2051 B",
    "summary": "Sahu and colleagues used Hubble observations of the apparent positional shift of a background star as the nearby white dwarf Stein 2051 B passed in front of it. Fitting the astrometric microlensing model and parallax gave a lens mass of 0.675 ± 0.051 solar masses, providing a comparison point for white-dwarf mass–radius models.",
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    "area": "Gravitational lensing and stellar physics",
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        "title": "Relativistic deflection of background starlight measures the mass of a nearby white dwarf star",
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            "citation": "Relativistic deflection of background starlight measures the mass of a nearby white dwarf star",
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          "name": "Andrea Bellini",
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            "citation": "Relativistic deflection of background starlight measures the mass of a nearby white dwarf star",
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      "scope": {
        "description": "The lensing mass uses general relativity and modeled source/lens motion and distances; this is not an independent measurement of the relativistic deflection coefficient or a proof of every white-dwarf mass–radius relation. Of eight observing epochs, only four entered the deflection fit because glare and diffraction compromised source measurements close to the white dwarf. Point-spread-function subtraction and the astrometric reference frame contribute uncertainty. The radius comparison uses photometry and a helium-atmosphere model. The supplementary text prints 52 pc where the main text gives 5.52 pc and the quoted 181 mas parallax implies approximately 5.52 pc; this apparent typo is retained for review. The astrometric result relies on the authors’ image reduction; independent reanalysis would be needed to test it.",
        "domain": "Gravitational lensing and stellar physics"
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      "statement": "# Astrometric microlensing measures the mass of white dwarf Stein 2051 B\n\nSahu and colleagues used Hubble observations of the apparent positional shift of a background star as the nearby white dwarf Stein 2051 B passed in front of it. Fitting the astrometric microlensing model and parallax gave a lens mass of 0.675 ± 0.051 solar masses, providing a comparison point for white-dwarf mass–radius models.\n\n## Scientific scope\n\nThe lensing mass uses general relativity and modeled source/lens motion and distances; this is not an independent measurement of the relativistic deflection coefficient or a proof of every white-dwarf mass–radius relation. Of eight observing epochs, only four entered the deflection fit because glare and diffraction compromised source measurements close to the white dwarf. Point-spread-function subtraction and the astrometric reference frame contribute uncertainty. The radius comparison uses photometry and a helium-atmosphere model. The supplementary text prints 52 pc where the main text gives 5.52 pc and the quoted 181 mas parallax implies approximately 5.52 pc; this apparent typo is retained for review. The astrometric result relies on the authors’ image reduction; independent reanalysis would be needed to test it.\n\n## Reading status\n\nThis is a source-linked WRS catalogue note. A full explanatory guide and independent scientific reconstruction have not been completed for this entry. Read the identified original work for its complete narrative and arguments.\n\n## People and systems\n\nKailash C. Sahu; Jay Anderson; Stefano Casertano; Howard E. Bond; Pierre Bergeron; Edmund P. Nelan; Laurent Pueyo; Thomas M. Brown; Andrea Bellini; Zoltan G. Levay; Joshua Sokol; Martin Dominik; Annalisa Calamida; Noé Kains; Mario Livio\n\nThese are the listed authors of the cited contribution sources. Paper authorship does not quantify individual effort. An incomplete list is explicitly marked; same names are not automatically merged.\n\n\n\n## Original sources\n\n- [Relativistic deflection of background starlight measures the mass of a nearby white dwarf star](https://arxiv.org/pdf/1706.02037v1)\n",
      "summary": "Sahu and colleagues used Hubble observations of the apparent positional shift of a background star as the nearby white dwarf Stein 2051 B passed in front of it. Fitting the astrometric microlensing model and parallax gave a lens mass of 0.675 ± 0.051 solar masses, providing a comparison point for white-dwarf mass–radius models.",
      "title": "Astrometric microlensing measures the mass of white dwarf Stein 2051 B"
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    "title": "Astrometric microlensing measures the mass of white dwarf Stein 2051 B",
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    "what_changed": "Sahu and colleagues used Hubble observations of the apparent positional shift of a background star as the nearby white dwarf Stein 2051 B passed in front of it. Fitting the astrometric microlensing model and parallax gave a lens mass of 0.675 ± 0.051 solar masses, providing a comparison point for white-dwarf mass–radius models.",
    "scope": "Sahu and colleagues used Hubble observations of the apparent positional shift of a background star as the nearby white dwarf Stein 2051 B passed in front of it. Fitting the astrometric microlensing model and parallax gave a lens mass of 0.675 ± 0.051 solar masses, providing a comparison point for white-dwarf mass–radius models. The lensing mass uses general relativity and modeled source/lens motion and distances; this is not an independent measurement of the relativistic deflection coefficient or a proof of every white-dwarf mass–radius relation. Of eight observing epochs, only four entered the deflection fit because glare and diffraction compromised source measurements close to the white dwarf. Point-spread-function subtraction and the astrometric reference frame contribute uncertainty. The radius comparison uses photometry and a helium-atmosphere model. The supplementary text prints 52 pc where the main text gives 5.52 pc and the quoted 181 mas parallax implies approximately 5.52 pc; this apparent typo is retained for review. The astrometric result relies on the authors’ image reduction; independent reanalysis would be needed to test it.",
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        "title": "Relativistic deflection of background starlight measures the mass of a nearby white dwarf star",
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