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2018•Monthly Notices of the Royal Astronomical SocietyOpen access

Extending Gaia DR2 with HST narrow-field astrometry: the WISE J154151.65−225024.9 test case

L. R. Bedin, C. Fontanive

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Abstract

One field containing WISE J154151.65− 225024.9 was observed by Hubble Space Telescope at three different epochs taken in ∼5 yr. We measured positions of sources in all images and successfully linked these positions to the Gaia DR2 absolute system to derive the astrometric parameters for this faint close-by Y1 brown dwarf. The developed procedure avoids traditional limitations of relative imaging-astrometry with narrow-field cameras, extending Gaia DR2 to fainter magnitudes. We found (μαcos δ, μδ, π) = (−902.62 ± 0.35 mas yr−1, −88.26 ± 0.35 mas yr−1, 168.4 ± 2.2 mas), which represent a sizable improvement over recent determinations in the literature. Applying a correction from relative (π) to absolute parallax (ϖ) we found ϖ = 169 ± 2 mas, corresponding to a distance of 5.9 ± 0.1 pc.

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One field containing WISE J154151.65− 225024.9 was observed by Hubble Space Telescope at three different epochs taken in ∼5 yr. We measured positions of sources in all images and successfully linked these positions to the Gaia DR2 absolute system to derive the astrometric parameters for this faint close-by Y1 brown dwarf. The developed procedure avoids traditional limitations of relative imaging-astrometry with narrow-field cameras, extending Gaia DR2 to fainter magnitudes. We found (μαcos δ, μδ, π) = (−902.62 ± 0.35 mas yr−1, −88.26 ± 0.35 mas yr−1, 168.4 ± 2.2 mas), which represent a sizable improvement over recent determinations in the literature. Applying a correction from relative (π) to absolute parallax (ϖ) we found ϖ = 169 ± 2 mas, corresponding to a distance of 5.9 ± 0.1 pc.

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Available abstract

One field containing WISE J154151.65− 225024.9 was observed by Hubble Space Telescope at three different epochs taken in ∼5 yr. We measured positions of sources in all images and successfully linked these positions to the Gaia DR2 absolute system to derive the astrometric parameters for this faint close-by Y1 brown dwarf. The developed procedure avoids traditional limitations of relative imaging-astrometry with narrow-field cameras, extending Gaia DR2 to fainter magnitudes. We found (μαcos δ, μδ, π) = (−902.62 ± 0.35 mas yr−1, −88.26 ± 0.35 mas yr−1, 168.4 ± 2.2 mas), which represent a sizable improvement over recent determinations in the literature. Applying a correction from relative (π) to absolute parallax (ϖ) we found ϖ = 169 ± 2 mas, corresponding to a distance of 5.9 ± 0.1 pc.

Key concepts: Parallax, Astrometry, Physics, Hubble space telescope, Absolute magnitude, Astrophysics, Proper motion, Field (mathematics)

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