Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05

We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H _2 CO, CH _...
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Autor*in:	Prasanta Gorai [verfasserIn] Chi-Yan Law [verfasserIn] Jonathan C. Tan [verfasserIn] Yichen Zhang [verfasserIn] Rubén Fedriani [verfasserIn] Kei E. I. Tanaka [verfasserIn] Mélisse Bonfand [verfasserIn] Giuliana Cosentino [verfasserIn] Diego Mardones [verfasserIn] Maria T. Beltrán [verfasserIn] Guido Garay [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2024

Schlagwörter:	Star formation Astrochemistry Complex organic molecules Spectral line identification Massive stars Interstellar medium

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 960(2024), 2, p 127
Übergeordnetes Werk:	volume:960 ; year:2024 ; number:2, p 127

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/ad09bb

Katalog-ID:	DOAJ097864749

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650		4	\|a Star formation
650		4	\|a Astrochemistry
650		4	\|a Complex organic molecules
650		4	\|a Spectral line identification
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allfields	10.3847/1538-4357/ad09bb doi (DE-627)DOAJ097864749 (DE-599)DOAJ89a2e5fc85de4155925c881cd9de815e DE-627 ger DE-627 rakwb eng QB460-466 Prasanta Gorai verfasserin aut Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H _2 CO, CH _3 OH, CH _3 OCH _3 ), sulfur-bearing (SO _2 , H _2 S), and nitrogen-bearing (e.g., HNCO, NH _2 CHO, C _2 H _3 CN, C _2 H _5 CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm ^−2 ), number densities ( n _H ∼ 10 ^9 cm ^−3 ), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M _⊙ , which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry. Star formation Astrochemistry Complex organic molecules Spectral line identification Massive stars Interstellar medium Astrophysics Chi-Yan Law verfasserin aut Jonathan C. Tan verfasserin aut Yichen Zhang verfasserin aut Rubén Fedriani verfasserin aut Kei E. I. Tanaka verfasserin aut Mélisse Bonfand verfasserin aut Giuliana Cosentino verfasserin aut Diego Mardones verfasserin aut Maria T. Beltrán verfasserin aut Guido Garay verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2024), 2, p 127 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2024 number:2, p 127 https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/article/89a2e5fc85de4155925c881cd9de815e kostenfrei https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 960 2024 2, p 127
spelling	10.3847/1538-4357/ad09bb doi (DE-627)DOAJ097864749 (DE-599)DOAJ89a2e5fc85de4155925c881cd9de815e DE-627 ger DE-627 rakwb eng QB460-466 Prasanta Gorai verfasserin aut Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H _2 CO, CH _3 OH, CH _3 OCH _3 ), sulfur-bearing (SO _2 , H _2 S), and nitrogen-bearing (e.g., HNCO, NH _2 CHO, C _2 H _3 CN, C _2 H _5 CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm ^−2 ), number densities ( n _H ∼ 10 ^9 cm ^−3 ), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M _⊙ , which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry. Star formation Astrochemistry Complex organic molecules Spectral line identification Massive stars Interstellar medium Astrophysics Chi-Yan Law verfasserin aut Jonathan C. Tan verfasserin aut Yichen Zhang verfasserin aut Rubén Fedriani verfasserin aut Kei E. I. Tanaka verfasserin aut Mélisse Bonfand verfasserin aut Giuliana Cosentino verfasserin aut Diego Mardones verfasserin aut Maria T. Beltrán verfasserin aut Guido Garay verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2024), 2, p 127 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2024 number:2, p 127 https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/article/89a2e5fc85de4155925c881cd9de815e kostenfrei https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 960 2024 2, p 127
allfields_unstemmed	10.3847/1538-4357/ad09bb doi (DE-627)DOAJ097864749 (DE-599)DOAJ89a2e5fc85de4155925c881cd9de815e DE-627 ger DE-627 rakwb eng QB460-466 Prasanta Gorai verfasserin aut Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H _2 CO, CH _3 OH, CH _3 OCH _3 ), sulfur-bearing (SO _2 , H _2 S), and nitrogen-bearing (e.g., HNCO, NH _2 CHO, C _2 H _3 CN, C _2 H _5 CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm ^−2 ), number densities ( n _H ∼ 10 ^9 cm ^−3 ), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M _⊙ , which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry. Star formation Astrochemistry Complex organic molecules Spectral line identification Massive stars Interstellar medium Astrophysics Chi-Yan Law verfasserin aut Jonathan C. Tan verfasserin aut Yichen Zhang verfasserin aut Rubén Fedriani verfasserin aut Kei E. I. Tanaka verfasserin aut Mélisse Bonfand verfasserin aut Giuliana Cosentino verfasserin aut Diego Mardones verfasserin aut Maria T. Beltrán verfasserin aut Guido Garay verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2024), 2, p 127 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2024 number:2, p 127 https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/article/89a2e5fc85de4155925c881cd9de815e kostenfrei https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 960 2024 2, p 127
allfieldsGer	10.3847/1538-4357/ad09bb doi (DE-627)DOAJ097864749 (DE-599)DOAJ89a2e5fc85de4155925c881cd9de815e DE-627 ger DE-627 rakwb eng QB460-466 Prasanta Gorai verfasserin aut Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H _2 CO, CH _3 OH, CH _3 OCH _3 ), sulfur-bearing (SO _2 , H _2 S), and nitrogen-bearing (e.g., HNCO, NH _2 CHO, C _2 H _3 CN, C _2 H _5 CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm ^−2 ), number densities ( n _H ∼ 10 ^9 cm ^−3 ), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M _⊙ , which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry. Star formation Astrochemistry Complex organic molecules Spectral line identification Massive stars Interstellar medium Astrophysics Chi-Yan Law verfasserin aut Jonathan C. Tan verfasserin aut Yichen Zhang verfasserin aut Rubén Fedriani verfasserin aut Kei E. I. Tanaka verfasserin aut Mélisse Bonfand verfasserin aut Giuliana Cosentino verfasserin aut Diego Mardones verfasserin aut Maria T. Beltrán verfasserin aut Guido Garay verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2024), 2, p 127 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2024 number:2, p 127 https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/article/89a2e5fc85de4155925c881cd9de815e kostenfrei https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 960 2024 2, p 127
allfieldsSound	10.3847/1538-4357/ad09bb doi (DE-627)DOAJ097864749 (DE-599)DOAJ89a2e5fc85de4155925c881cd9de815e DE-627 ger DE-627 rakwb eng QB460-466 Prasanta Gorai verfasserin aut Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H _2 CO, CH _3 OH, CH _3 OCH _3 ), sulfur-bearing (SO _2 , H _2 S), and nitrogen-bearing (e.g., HNCO, NH _2 CHO, C _2 H _3 CN, C _2 H _5 CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm ^−2 ), number densities ( n _H ∼ 10 ^9 cm ^−3 ), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M _⊙ , which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry. Star formation Astrochemistry Complex organic molecules Spectral line identification Massive stars Interstellar medium Astrophysics Chi-Yan Law verfasserin aut Jonathan C. Tan verfasserin aut Yichen Zhang verfasserin aut Rubén Fedriani verfasserin aut Kei E. I. Tanaka verfasserin aut Mélisse Bonfand verfasserin aut Giuliana Cosentino verfasserin aut Diego Mardones verfasserin aut Maria T. Beltrán verfasserin aut Guido Garay verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 960(2024), 2, p 127 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:960 year:2024 number:2, p 127 https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/article/89a2e5fc85de4155925c881cd9de815e kostenfrei https://doi.org/10.3847/1538-4357/ad09bb kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 960 2024 2, p 127
language	English
source	In The Astrophysical Journal 960(2024), 2, p 127 volume:960 year:2024 number:2, p 127
sourceStr	In The Astrophysical Journal 960(2024), 2, p 127 volume:960 year:2024 number:2, p 127
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Star formation Astrochemistry Complex organic molecules Spectral line identification Massive stars Interstellar medium Astrophysics
isfreeaccess_bool	true
container_title	The Astrophysical Journal
authorswithroles_txt_mv	Prasanta Gorai @@aut@@ Chi-Yan Law @@aut@@ Jonathan C. Tan @@aut@@ Yichen Zhang @@aut@@ Rubén Fedriani @@aut@@ Kei E. I. Tanaka @@aut@@ Mélisse Bonfand @@aut@@ Giuliana Cosentino @@aut@@ Diego Mardones @@aut@@ Maria T. Beltrán @@aut@@ Guido Garay @@aut@@
publishDateDaySort_date	2024-01-01T00:00:00Z
hierarchy_top_id	269019219
id	DOAJ097864749
language_de	englisch
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callnumber-first	Q - Science
author	Prasanta Gorai
spellingShingle	Prasanta Gorai misc QB460-466 misc Star formation misc Astrochemistry misc Complex organic molecules misc Spectral line identification misc Massive stars misc Interstellar medium misc Astrophysics Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05
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topic_title	QB460-466 Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05 Star formation Astrochemistry Complex organic molecules Spectral line identification Massive stars Interstellar medium
topic	misc QB460-466 misc Star formation misc Astrochemistry misc Complex organic molecules misc Spectral line identification misc Massive stars misc Interstellar medium misc Astrophysics
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title	Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05
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title_full	Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05
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author_browse	Prasanta Gorai Chi-Yan Law Jonathan C. Tan Yichen Zhang Rubén Fedriani Kei E. I. Tanaka Mélisse Bonfand Giuliana Cosentino Diego Mardones Maria T. Beltrán Guido Garay
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title_sort	astrochemical diagnostics of the isolated massive protostar g28.20-0.05
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title_auth	Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05
abstract	We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H _2 CO, CH _3 OH, CH _3 OCH _3 ), sulfur-bearing (SO _2 , H _2 S), and nitrogen-bearing (e.g., HNCO, NH _2 CHO, C _2 H _3 CN, C _2 H _5 CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm ^−2 ), number densities ( n _H ∼ 10 ^9 cm ^−3 ), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M _⊙ , which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry.
abstractGer	We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H _2 CO, CH _3 OH, CH _3 OCH _3 ), sulfur-bearing (SO _2 , H _2 S), and nitrogen-bearing (e.g., HNCO, NH _2 CHO, C _2 H _3 CN, C _2 H _5 CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm ^−2 ), number densities ( n _H ∼ 10 ^9 cm ^−3 ), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M _⊙ , which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry.
abstract_unstemmed	We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H _2 CO, CH _3 OH, CH _3 OCH _3 ), sulfur-bearing (SO _2 , H _2 S), and nitrogen-bearing (e.g., HNCO, NH _2 CHO, C _2 H _3 CN, C _2 H _5 CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm ^−2 ), number densities ( n _H ∼ 10 ^9 cm ^−3 ), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M _⊙ , which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry.
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title_short	Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05
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Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05

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