JWST Detection of Hydrocarbon Ices and Methane Gas on Makemake
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| Format: | Preprint |
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2025
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| author | Protopapa, Silvia Wong, Ian Lellouch, Emmanuel Johnson, Perianne E. Grundy, William M. Glein, Christopher R. Müller, Thomas Kiss, Csaba Emery, Joshua P. Brunetto, Rosario Holler, Bryan J. Parker, Alex H. Stansberry, John A. Hammel, Heidi B. Milam, Stefanie N. Guilbert-Lepoutre, Aurélie Santos-Sanz, Pablo Pinilla-Alonso, Noemí |
| author_facet | Protopapa, Silvia Wong, Ian Lellouch, Emmanuel Johnson, Perianne E. Grundy, William M. Glein, Christopher R. Müller, Thomas Kiss, Csaba Emery, Joshua P. Brunetto, Rosario Holler, Bryan J. Parker, Alex H. Stansberry, John A. Hammel, Heidi B. Milam, Stefanie N. Guilbert-Lepoutre, Aurélie Santos-Sanz, Pablo Pinilla-Alonso, Noemí |
| contents | JWST/NIRSpec observations of Makemake reveal a chemically complex surface and evidence of gaseous CH$_4$. Our spectral modeling indicates a surface composition consisting of CH$_4$, CH$_3$D, and possibly CH$_3$OH, combined with aggregates of C$_2$H$_2$ and C$_2$H$_6$. The presence of C$_2$H$_4$ is also considered given its expected photochemical origin. Both areal and layered configurations reproduce the observed spectrum, with the latter being preferred. This composition confirms earlier hydrocarbon detections and suggests that CH$_4$ photolysis is either ongoing or occurred recently. The detection of CH$_3$D yields a D/H ratio in CH$_4$ ice of $(3.98 \pm 0.34) \times 10^{-4}$, consistent within $2σ$ with previous estimates. We report the first detection of CH$_4$ fluorescence from Makemake, establishing it as only the second trans-Neptunian object$\unicode{x2014}$after Pluto$\unicode{x2014}$with confirmed volatile release. We explore two scenarios consistent with the observed CH$_4$ emission, though neither fully reproduces the data: an expanding coma, yielding production rates of $(0.2\unicode{x2013}1.6) \times 10^{28}$ molecules s$^{-1}$ and a rovibrational temperature of $\sim$35 K, possibly originating from a localized plume, and a gravitationally bound atmosphere, which, if adopted, implies gas kinetic temperatures near 40 K and surface pressures of $\sim$10 pbar$\unicode{x2014}$values consistent with stellar occultation constraints and an atmosphere in equilibrium with surface CH$_4$ ice. Discriminating between these scenarios will require higher spectral resolution and improved signal-to-noise observations. Together, the gas-phase CH$_4$, intermediate D/H ratio between that in water and CH$_4$ in comets, and complex surface composition challenge the traditional view of Makemake as a quiescent, frozen body. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_06772 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | JWST Detection of Hydrocarbon Ices and Methane Gas on Makemake Protopapa, Silvia Wong, Ian Lellouch, Emmanuel Johnson, Perianne E. Grundy, William M. Glein, Christopher R. Müller, Thomas Kiss, Csaba Emery, Joshua P. Brunetto, Rosario Holler, Bryan J. Parker, Alex H. Stansberry, John A. Hammel, Heidi B. Milam, Stefanie N. Guilbert-Lepoutre, Aurélie Santos-Sanz, Pablo Pinilla-Alonso, Noemí Earth and Planetary Astrophysics JWST/NIRSpec observations of Makemake reveal a chemically complex surface and evidence of gaseous CH$_4$. Our spectral modeling indicates a surface composition consisting of CH$_4$, CH$_3$D, and possibly CH$_3$OH, combined with aggregates of C$_2$H$_2$ and C$_2$H$_6$. The presence of C$_2$H$_4$ is also considered given its expected photochemical origin. Both areal and layered configurations reproduce the observed spectrum, with the latter being preferred. This composition confirms earlier hydrocarbon detections and suggests that CH$_4$ photolysis is either ongoing or occurred recently. The detection of CH$_3$D yields a D/H ratio in CH$_4$ ice of $(3.98 \pm 0.34) \times 10^{-4}$, consistent within $2σ$ with previous estimates. We report the first detection of CH$_4$ fluorescence from Makemake, establishing it as only the second trans-Neptunian object$\unicode{x2014}$after Pluto$\unicode{x2014}$with confirmed volatile release. We explore two scenarios consistent with the observed CH$_4$ emission, though neither fully reproduces the data: an expanding coma, yielding production rates of $(0.2\unicode{x2013}1.6) \times 10^{28}$ molecules s$^{-1}$ and a rovibrational temperature of $\sim$35 K, possibly originating from a localized plume, and a gravitationally bound atmosphere, which, if adopted, implies gas kinetic temperatures near 40 K and surface pressures of $\sim$10 pbar$\unicode{x2014}$values consistent with stellar occultation constraints and an atmosphere in equilibrium with surface CH$_4$ ice. Discriminating between these scenarios will require higher spectral resolution and improved signal-to-noise observations. Together, the gas-phase CH$_4$, intermediate D/H ratio between that in water and CH$_4$ in comets, and complex surface composition challenge the traditional view of Makemake as a quiescent, frozen body. |
| title | JWST Detection of Hydrocarbon Ices and Methane Gas on Makemake |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2509.06772 |