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28 April 2024 |
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Assessing the C/O Ratio Formation Diagnostic: A Potential Trend with Companion Mass | | Kielan K. W. Hoch
; Quinn M. Konopacky
; Christopher A. Theissen
; Jean-Baptiste Ruffio
; Travis S. Barman
; Marshall D. Perrin
; Bruce Macintosh
; Christian Marois
; | | Date: |
8 Dec 2022 | | Abstract: | The carbon-to-oxygen (C/O) ratio in an exoplanet atmosphere has been
suggested as a potential diagnostic of planet formation. Now that a number of
exoplanets have measured C/O ratios, it is possible to examine this diagnostic
at a population level. Here, we present an analysis of currently measured C/O
ratios of directly imaged and transit/eclipse planets. First, we derive
atmospheric parameters for the substellar companion HD 284149 b using data that
were taken with the OSIRIS integral field spectrograph at the W.M. Keck
Observatory and report two non-detections from our ongoing imaging spectroscopy
survey of exoplanetary atmospheres with Keck/OSIRIS. We find an effective
temperature of $T_mathrm{eff} = 2502$~K, with a range of 2291--2624~K, $log
g=4.52$, with a range of 4.38--4.91, and [M/H] = 0.37, with a range of
0.10--0.55. These values are in agreement with previous studies done by
Bonavita et al. (2014, 2017). We derive a C/O of 0.589$^{+0.148}_{-0.295}$ for
HD 284149 b. We then add this measurement to the growing list of C/O ratios for
directly imaged planets from the literature, and compare them with those
available from a sample of transit/eclipse planets. There is a trend in C/O
ratio with companion mass (M$_{mathrm{Jup}}$), with a break seen around 4
M$_{mathrm{Jup}}$. We run a Kolmogorov-Smirnov and an Anderson-Darling test on
planets above and below this mass boundary, and find that they are two distinct
populations. This could be additional evidence of two distinct populations
possibly having two different formation pathways, with companion mass as a
primary indicator of most likely formation scenario. | | Source: | arXiv, 2212.04557 | | Services: | Forum | Review | PDF | Favorites | |
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