WISEPA J041022.71+150248.5

History of observations

Discovery

WISE 0410+1502 was discovered in 2011 from data, collected by Wide-field Infrared Survey Explorer (WISE) Earth-orbiting satellite—NASA infrared-wavelength 40 cm (16 in) space telescope, which mission lasted from December 2009 to February 2011. WISE 0410+1502 has two discovery papers: Kirkpatrick et al. (2011) and Cushing et al. (2011), however, basically with the same authors and published nearly simultaneously.

• Kirkpatrick et al. presented discovery of 98 new found by WISE brown dwarf systems with components of spectral types M, L, T and Y, among which also was WISE 0410+1502.These 98 brown dwarf systems are only among first, not all brown dwarf systems, discovered from data, collected by WISE: six discoveries were published earlier (however, also listed in Kirkpatrick et al. (2011)) in Mainzer et al. (2011) and Burgasser et al. (2011), and the other discoveries were published later.
• Cushing et al. presented discovery of seven brown dwarfs—one of T9.5 type, and six of Y-type—first members of the Y spectral class, ever discovered and spectroscopically confirmed, including "archetypal member" of the Y spectral class WISE 1828+2650, and WISE 0410+1502. These seven objects are also the faintest seven of 98 brown dwarfs, presented in Kirkpatrick et al. (2011).

Distance

Currently the most accurate distance estimate of WISE 0410+1502 is a trigonometric parallax, published in 2021 by Kirkpatrick et al.: , corresponding to a distance , or .

Space motion

WISE 0410+1502 has a large proper motion of milliarcseconds per year. The brown dwarf WISE 0410+1502 lies in local void 6.5 parsecs across, where relatively few stars and brown dwarfs are located.

Physical properties

The object's temperature estimate is . Cushing et al. obtained a low-resolution Magellan/FIRE spectrum and later they obtained a higher quality spectrum with Hubble WFC3, confirming the Y0 spectral type. The fitting of the spectrum with cloudy models produces realistic values and Leggett et al. finds a mass of about 10–15 . The atmosphere is likely in a chemical disequilibrium and a cloud-free disequilibrium model does fit well with the Y- and H-band, but does not fit well with the J-band.

Notes

References

References

1. (2016). "A non-uniform distribution of the nearest brown dwarfs". Astronomy & Astrophysics.
2. (2011). "The Discovery of Y Dwarfs using Data from the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal.
3. (2011). "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)". [[The Astrophysical Journal Supplement]].
4. (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". [[The Astrophysical Journal]].
5. Marsh, Kenneth A.. (2013). "Parallaxes and Proper Motions of Ultracool Brown Dwarfs of Spectral Types Y and Late T". [[The Astrophysical Journal]].
6. (2014). "WISE Y Dwarfs As Probes of the Brown Dwarf-Exoplanet Connection". [[The Astrophysical Journal]].
7. (March 2021). "The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs". [[The Astrophysical Journal Supplement Series]].
8. (2014-05-01). "Three New Cool Brown Dwarfs Discovered with the Wide-field Infrared Survey Explorer (WISE) and an Improved Spectrum of the Y0 Dwarf WISE J041022.71+150248.4". The Astronomical Journal.
9. (2013-02-01). "A Comparison of Near-infrared Photometry and Spectra for Y Dwarfs with a New Generation of Cool Cloudy Models". The Astrophysical Journal.
10. (2019-05-01). "A Uniform Retrieval Analysis of Ultra-cool Dwarfs. III. Properties of Y Dwarfs". The Astrophysical Journal.
11. (2024-12-21). "The Y Dwarf Population with HST: unlocking the secrets of our coolest neighbours -- II. Parallaxes and Proper Motions". Monthly Notices of the Royal Astronomical Society.