What is recorded here?
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.
Source-linked catalogue note. A detailed explanatory guide has not yet been prepared for this entry.
Scientific scope
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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People and systems
Kailash 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
These 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.
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English catalogue narrative
Astrometric microlensing measures the mass of white dwarf Stein 2051 B
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.
Scientific scope
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.
Reading status
This 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.
People and systems
Kailash 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
These 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.