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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2409.16355 |
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| _version_ | 1866909325223526400 |
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| author | Thao, Pa Chia Mann, Andrew W. Feinstein, Adina D. Gao, Peter Thorngren, Daniel Rotman, Yoav Welbanks, Luis Brown, Alexander Duvvuri, Girish M. France, Kevin Longo, Isabella Sandoval, Angeli Schneider, P. Christian Wilson, David J. Youngblood, Allison Vanderburg, Andrew Barber, Madyson G. Wood, Mackenna L. Batalha, Natasha E. Kraus, Adam L. Murray, Catriona Anne Newton, Elisabeth R. Rizzuto, Aaron Tofflemire, Benjamin M. Tsai, Shang-Min Bean, Jacob L. Berta-Thompson, Zachory K. Evans-Soma, Thomas M. Froning, Cynthia S. Kempton, Eliza M. -R. Miguel, Yamila Pineda, J. Sebastian |
| author_facet | Thao, Pa Chia Mann, Andrew W. Feinstein, Adina D. Gao, Peter Thorngren, Daniel Rotman, Yoav Welbanks, Luis Brown, Alexander Duvvuri, Girish M. France, Kevin Longo, Isabella Sandoval, Angeli Schneider, P. Christian Wilson, David J. Youngblood, Allison Vanderburg, Andrew Barber, Madyson G. Wood, Mackenna L. Batalha, Natasha E. Kraus, Adam L. Murray, Catriona Anne Newton, Elisabeth R. Rizzuto, Aaron Tofflemire, Benjamin M. Tsai, Shang-Min Bean, Jacob L. Berta-Thompson, Zachory K. Evans-Soma, Thomas M. Froning, Cynthia S. Kempton, Eliza M. -R. Miguel, Yamila Pineda, J. Sebastian |
| contents | The characterization of young planets (< 300 Myr) is pivotal for understanding planet formation and evolution. We present the 3-5$μ$m transmission spectrum of the 17 Myr, Jupiter-size ($R$ $\sim$10$R_{\oplus}$) planet, HIP 67522 b, observed with JWST/NIRSpec/G395H. To check for spot contamination, we obtain a simultaneous $g$-band transit with SOAR. The spectrum exhibits absorption features 30-50% deeper than the overall depth, far larger than expected from an equivalent mature planet, and suggests that HIP 67522 b's mass is $<$20 $M_{\oplus}$ irrespective of cloud cover and stellar contamination. A Bayesian retrieval analysis returns a mass constraint of $13.8\pm1.0M_{\oplus}$. This challenges the previous classification of HIP 67522 b as a hot Jupiter and instead, positions it as a precursor to the more common sub-Neptunes. With a density of $<$0.10g/cm$^{3}$, HIP 67522 b is one of the lowest density planets known. We find strong absorption from H$_{2}$O and CO$_{2}$ ($\ge7σ$), a modest detection of CO (3.5$σ$), and weak detections of H$_2$S and SO$_2$ ($\simeq2σ$). Comparisons with radiative-convective equilibrium models suggest supersolar atmospheric metallicities and solar-to-subsolar C/O ratios, with photochemistry further constraining the inferred atmospheric metallicity to 3$\times$10 Solar due to the amplitude of the SO$_2$ feature. These results point to the formation of HIP 67522 b beyond the water snowline, where its envelope was polluted by icy pebbles and planetesimals. The planet is likely experiencing substantial mass loss (0.01-0.03 M$_{\oplus}$ Myr$^{-1}$), sufficient for envelope destruction within a Gyr. This highlights the dramatic evolution occurring within the first 100 Myr of its existence. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_16355 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST Thao, Pa Chia Mann, Andrew W. Feinstein, Adina D. Gao, Peter Thorngren, Daniel Rotman, Yoav Welbanks, Luis Brown, Alexander Duvvuri, Girish M. France, Kevin Longo, Isabella Sandoval, Angeli Schneider, P. Christian Wilson, David J. Youngblood, Allison Vanderburg, Andrew Barber, Madyson G. Wood, Mackenna L. Batalha, Natasha E. Kraus, Adam L. Murray, Catriona Anne Newton, Elisabeth R. Rizzuto, Aaron Tofflemire, Benjamin M. Tsai, Shang-Min Bean, Jacob L. Berta-Thompson, Zachory K. Evans-Soma, Thomas M. Froning, Cynthia S. Kempton, Eliza M. -R. Miguel, Yamila Pineda, J. Sebastian Earth and Planetary Astrophysics The characterization of young planets (< 300 Myr) is pivotal for understanding planet formation and evolution. We present the 3-5$μ$m transmission spectrum of the 17 Myr, Jupiter-size ($R$ $\sim$10$R_{\oplus}$) planet, HIP 67522 b, observed with JWST/NIRSpec/G395H. To check for spot contamination, we obtain a simultaneous $g$-band transit with SOAR. The spectrum exhibits absorption features 30-50% deeper than the overall depth, far larger than expected from an equivalent mature planet, and suggests that HIP 67522 b's mass is $<$20 $M_{\oplus}$ irrespective of cloud cover and stellar contamination. A Bayesian retrieval analysis returns a mass constraint of $13.8\pm1.0M_{\oplus}$. This challenges the previous classification of HIP 67522 b as a hot Jupiter and instead, positions it as a precursor to the more common sub-Neptunes. With a density of $<$0.10g/cm$^{3}$, HIP 67522 b is one of the lowest density planets known. We find strong absorption from H$_{2}$O and CO$_{2}$ ($\ge7σ$), a modest detection of CO (3.5$σ$), and weak detections of H$_2$S and SO$_2$ ($\simeq2σ$). Comparisons with radiative-convective equilibrium models suggest supersolar atmospheric metallicities and solar-to-subsolar C/O ratios, with photochemistry further constraining the inferred atmospheric metallicity to 3$\times$10 Solar due to the amplitude of the SO$_2$ feature. These results point to the formation of HIP 67522 b beyond the water snowline, where its envelope was polluted by icy pebbles and planetesimals. The planet is likely experiencing substantial mass loss (0.01-0.03 M$_{\oplus}$ Myr$^{-1}$), sufficient for envelope destruction within a Gyr. This highlights the dramatic evolution occurring within the first 100 Myr of its existence. |
| title | The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2409.16355 |