Dokumentdetails
ID
oai:arXiv.org:2405.13128
Thema
Astrophysics - Earth and Planetary... Astrophysics - Solar and Stellar A...Autor
Xuan, Jerry W. Hsu, Chih-Chun Finnerty, Luke Wang, Jason J. Ruffio, Jean-Baptiste Zhang, Yapeng Knutson, Heather A. Mawet, Dimitri Mamajek, Eric E. Inglis, Julie Wallack, Nicole L. Bryan, Marta L. Blake, Geoffrey A. Mollière, Paul Hejazi, Neda Baker, Ashley Bartos, Randall Calvin, Benjamin Cetre, Sylvain Delorme, Jacques-Robert Doppmann, Greg Echeverri, Daniel Fitzgerald, Michael P. Jovanovic, Nemanja Liberman, Joshua López, Ronald A. Morris, Evan Pezzato, Jacklyn Sappey, Ben Schofield, Tobias Skemer, Andrew Wallace, James K. Wang, Ji Agrawal, Shubh Horstman, KatelynKategorie
Wissenschaften: Astrophysik
Jahr
2024
Auflistungsdatum
29.05.2024
Schlüsselwörter
level accretion measurements models core solar companions astrophysicsZusammenfassung
Using Keck Planet Imager and Characterizer (KPIC) high-resolution ($R$~35000) spectroscopy from 2.29-2.49 $\mu$m, we present uniform atmospheric retrievals for eight young substellar companions with masses of ~10-30 $M_\textrm{Jup}$, orbital separations spanning ~50-360 au, and $T_\textrm{eff}$ between ~1500-2600 K.
We find that all companions have solar C/O ratios, and metallicities, to within the 1-2$\sigma$ level, with the measurements clustered around solar composition.
Stars in the same stellar associations as our systems have near-solar abundances, so these results indicate that this population of companions is consistent with formation via direct gravitational collapse.
Alternatively, core accretion outside the CO snowline would be compatible with our measurements, though the high mass ratios of most systems would require rapid core assembly and gas accretion in massive disks.
On a population level, our findings can be contrasted with abundance measurements for directly imaged planets with m<10 $M_\textrm{Jup}$, which show tentative atmospheric metal enrichment.
In addition, the atmospheric compositions of our sample of companions are distinct from those of hot Jupiters, which most likely form via core accretion.
For two companions with $T_\textrm{eff}$~1700-2000 K (kap And b and GSC 6214-210 b), our best-fit models prefer a non-gray cloud model with >3$\sigma$ significance.
The cloudy models yield 2-3$\sigma$ lower $T_\textrm{eff}$ for these companions, though the C/O and [C/H] still agree between cloudy and clear models at the $1\sigma$ level.
Finally, we constrain 12CO/13CO for three companions with the highest S/N data (GQ Lup b, HIP 79098 b, and DH Tau b), and report $v$sin($i$) and radial velocities for all companions.
;Comment: Accepted to ApJ, 52 pages, 20 figures
Xuan, Jerry W.,Hsu, Chih-Chun,Finnerty, Luke,Wang, Jason J.,Ruffio, Jean-Baptiste,Zhang, Yapeng,Knutson, Heather A.,Mawet, Dimitri,Mamajek, Eric E.,Inglis, Julie,Wallack, Nicole L.,Bryan, Marta L.,Blake, Geoffrey A.,Mollière, Paul,Hejazi, Neda,Baker, Ashley,Bartos, Randall,Calvin, Benjamin,Cetre, Sylvain,Delorme, Jacques-Robert,Doppmann, Greg,Echeverri, Daniel,Fitzgerald, Michael P.,Jovanovic, Nemanja,Liberman, Joshua,López, Ronald A.,Morris, Evan,Pezzato, Jacklyn,Sappey, Ben,Schofield, Tobias,Skemer, Andrew,Wallace, James K.,Wang, Ji,Agrawal, Shubh,Horstman, Katelyn, 2024, Are these planets or brown dwarfs? Broadly solar compositions from high-resolution atmospheric retrievals of ~10-30 $M_\textrm{Jup}$ companions
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