IPA: Class 0 Protostars Viewed in CO Emission Using JWST
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arXiv
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| Auteurs principaux: | , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2023
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| author | Rubinstein, Adam E. Evans II, Neal J. Tyagi, Himanshu Narang, Mayank Nazari, Pooneh Gutermuth, Robert Federman, Samuel Manoj, P. Green, Joel D. Watson, Dan M. Megeath, S. Thomas Rocha, Will R. M. Brunken, Nashanty G. C. Slavicinska, Katerina van Dishoeck, Ewine F. Beuther, Henrik Bourke, Tyler L. Garatti, Alessio Caratti o Hartmann, Lee Klaassen, Pamela Linz, Hendrik Looney, Leslie W. Muzerolle, James Stanke, Thomas Tobin, John J. Wolk, Scott J. Yang, Yao-Lun |
| author_facet | Rubinstein, Adam E. Evans II, Neal J. Tyagi, Himanshu Narang, Mayank Nazari, Pooneh Gutermuth, Robert Federman, Samuel Manoj, P. Green, Joel D. Watson, Dan M. Megeath, S. Thomas Rocha, Will R. M. Brunken, Nashanty G. C. Slavicinska, Katerina van Dishoeck, Ewine F. Beuther, Henrik Bourke, Tyler L. Garatti, Alessio Caratti o Hartmann, Lee Klaassen, Pamela Linz, Hendrik Looney, Leslie W. Muzerolle, James Stanke, Thomas Tobin, John J. Wolk, Scott J. Yang, Yao-Lun |
| contents | We investigate the bright CO fundamental emission in the central regions of five protostars in their primary mass assembly phase using new observations from JWST's Near-Infrared Spectrograph (NIRSpec) and Mid-Infrared Instrument (MIRI). CO line emission images and fluxes are extracted for a forest of $\sim$150 ro-vibrational transitions from two vibrational bands, $v=1-0$ and $v=2-1$. However, ${}^{13}$CO is undetected, indicating that ${}^{12}$CO emission is optically thin. We use H$_2$ emission lines to correct fluxes for extinction and then construct rotation diagrams for the CO lines with the highest spectral resolution and sensitivity to estimate rotational temperatures and numbers of CO molecules. Two distinct rotational temperature components are required for $v=1$ ($\sim600$ to 1000 K and 2000 to $\sim 10^4$ K), while one hotter component is required for $v=2$ ($\gtrsim 3500$ K). ${}^{13}$CO is depleted compared to the abundances found in the ISM, indicating selective UV photodissociation of ${}^{13}$CO; therefore, UV radiative pumping may explain the higher rotational temperatures in $v=2$. The average vibrational temperature is $\sim 1000$ K for our sources and is similar to the lowest rotational temperature components. Using the measured rotational and vibrational temperatures to infer a total number of CO molecules, we find that the total gas masses range from lower limits of $\sim10^{22}$ g for the lowest mass protostars to $\sim 10^{26}$ g for the highest mass protostars. Our gas mass lower limits are compatible with those in more evolved systems, which suggest the lowest rotational temperature component comes from the inner disk, scattered into our line of sight, but we also cannot exclude the contribution to the CO emission from disk winds for higher mass targets. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2312_07807 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | IPA: Class 0 Protostars Viewed in CO Emission Using JWST Rubinstein, Adam E. Evans II, Neal J. Tyagi, Himanshu Narang, Mayank Nazari, Pooneh Gutermuth, Robert Federman, Samuel Manoj, P. Green, Joel D. Watson, Dan M. Megeath, S. Thomas Rocha, Will R. M. Brunken, Nashanty G. C. Slavicinska, Katerina van Dishoeck, Ewine F. Beuther, Henrik Bourke, Tyler L. Garatti, Alessio Caratti o Hartmann, Lee Klaassen, Pamela Linz, Hendrik Looney, Leslie W. Muzerolle, James Stanke, Thomas Tobin, John J. Wolk, Scott J. Yang, Yao-Lun Solar and Stellar Astrophysics Astrophysics of Galaxies We investigate the bright CO fundamental emission in the central regions of five protostars in their primary mass assembly phase using new observations from JWST's Near-Infrared Spectrograph (NIRSpec) and Mid-Infrared Instrument (MIRI). CO line emission images and fluxes are extracted for a forest of $\sim$150 ro-vibrational transitions from two vibrational bands, $v=1-0$ and $v=2-1$. However, ${}^{13}$CO is undetected, indicating that ${}^{12}$CO emission is optically thin. We use H$_2$ emission lines to correct fluxes for extinction and then construct rotation diagrams for the CO lines with the highest spectral resolution and sensitivity to estimate rotational temperatures and numbers of CO molecules. Two distinct rotational temperature components are required for $v=1$ ($\sim600$ to 1000 K and 2000 to $\sim 10^4$ K), while one hotter component is required for $v=2$ ($\gtrsim 3500$ K). ${}^{13}$CO is depleted compared to the abundances found in the ISM, indicating selective UV photodissociation of ${}^{13}$CO; therefore, UV radiative pumping may explain the higher rotational temperatures in $v=2$. The average vibrational temperature is $\sim 1000$ K for our sources and is similar to the lowest rotational temperature components. Using the measured rotational and vibrational temperatures to infer a total number of CO molecules, we find that the total gas masses range from lower limits of $\sim10^{22}$ g for the lowest mass protostars to $\sim 10^{26}$ g for the highest mass protostars. Our gas mass lower limits are compatible with those in more evolved systems, which suggest the lowest rotational temperature component comes from the inner disk, scattered into our line of sight, but we also cannot exclude the contribution to the CO emission from disk winds for higher mass targets. |
| title | IPA: Class 0 Protostars Viewed in CO Emission Using JWST |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2312.07807 |