A Wide Planetary Mass Companion Discovered through the Citizen Science Project Backyard Worlds: Planet 9

December 2021 • 2021ApJ...923...48F

Authors • Faherty, Jacqueline K. • Gagné, Jonathan • Popinchalk, Mark • Vos, Johanna M. • Burgasser, Adam J. • Schümann, Jörg • Schneider, Adam C. • Kirkpatrick, J. Davy • Meisner, Aaron M. • Kuchner, Marc J. • Bardalez Gagliuffi, Daniella C. • Marocco, Federico • Caselden, Dan • Gonzales, Eileen C. • Rothermich, Austin • Casewell, Sarah L. • Debes, John H. • Aganze, Christian • Ayala, Andrew • Hsu, Chih-Chun • Cooper, William J. • Smart, R. L. • Gerasimov, Roman • Theissen, Christopher A. • Backyard Worlds: Planet 9 Collaboration

Abstract • Through the Backyard Worlds: Planet 9 citizen science project we discovered a late-type L dwarf co-moving with the young K0 star BD+60 1417 at a projected separation of 37″ or 1662 au. The secondary-CWISER J124332.12+600126.2 (W1243)-is detected in both the CatWISE2020 and 2MASS reject tables. The photometric distance and CatWISE proper motion both match that of the primary within ~1σ and our estimates for a chance alignment yield a zero probability. Follow-up near-infrared spectroscopy reveals W1243 to be a very red 2MASS (J-K _s = 2.72), low surface gravity source that we classify as L6-L8γ. Its spectral morphology strongly resembles that of confirmed late-type L dwarfs in 10-150 Myr moving groups as well as that of planetary mass companions. The position on near- and mid-infrared color-magnitude diagrams indicates the source is redder and fainter than the field sequence, a telltale sign of an object with thick clouds and a complex atmosphere. For the primary we obtained new optical spectroscopy and analyzed all available literature information for youth indicators. We conclude that the Li I abundance, its loci on color-magnitude and color-color diagrams, and the rotation rate revealed in multiple TESS sectors are all consistent with an age of 50-150 Myr. Using our re-evaluated age of the primary and the Gaia parallax, along with the photometry and spectrum for W1243, we find T _eff = 1303 ± 31 K, log g = 4.3 ± 0.17 cm s^-2, and a mass of 15 ± 5 M _Jup. We find a physical separation of ~1662 au and a mass ratio of ~0.01 for this system. Placing it in the context of the diverse collection of binary stars, brown dwarfs, and planetary companions, the BD+60 1417 system falls in a sparsely sampled area where the formation pathway is difficult to assess.

Links

• PREPRINT http://arxiv.org/abs/2112.04678
• ELECTR https://doi.org/10.3847%2F1538-4357%2Fac2499
• SIMBAD http://simbad.u-strasbg.fr/simbo.pl?bibcode=2021ApJ...923...48F
• PDF https://iopscience.iop.org/article/10.3847/1538-4357/ac2499/pdf
• DATA http://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/923/48
• DATA https://archive.stsci.edu/mastbibref.php?bibcode=2021ApJ...923...48F
• DATA https://irsa.ipac.caltech.edu/bibdata/2021/F/2021ApJ...923...48F.html