Overview of the complex chemistry in starless and prestellar cores

ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Overview of the complex chemistry in starless and prestellar cores Samantha Scibelli Jansky Fellow, NRAO Charlottesville, Virginia, USA A Complex Molecular Universe Known Interstellar Molecules Created with ASTROMOL v2021.9.1 bmcguir2.github.io/astromol McGuire 2022 ApJS 259, 30 2 Atoms CH CN CH+ OH CO H2 SiO CS SO SiS NS C2 NO HCl NaCl AlCl KCl AlF PN SiC CP NH SiN SO+ CO+ HF N2 CF+ PO O2 AlO CNOH+ SH+ HCl+ SH TiO ArH+ NS+ HeH+ VO PO+ SiP FeC 3 Atoms H2O HCO+ HCN OCS HNC H2S N2H+ C2H SO2 HCO HNO HCS+ HOC+ SiC2 C2S C3 CO2 CH2 C2O MgNC NH2 NaCN N2O MgCN H3+ SiCN AlNC SiNC HCP CCP AlOH H2O+ H2Cl+ KCN FeCN HO2 TiO2 CCN SiCSi S2H HCS HSC NCO CaNC NCS MgC2 HSO CaC2 4 Atoms NH3 H2CO HNCO H2CS C2H2 C3N HNCS HOCO+ C3O l-C3H HCNH+ H3O+ C3S c-C3H HC2N H2CN SiC3 CH3 C3NPH3 HCNO HOCN HSCN HOOH l-C3H+ HMgNC HCCO CNCN HONO MgCCH HCCS HNCN H2NC HCCS+ CH3+ HCNS HOCS+ HNSO 5 Atoms HC3N HCOOH CH2NH NH2CN H2CCO C4H SiH4 c-C3H2 CH2CN C5 SiC4 H2CCC CH4 HCCNC HNCCC H2COH+ C4HCNCHO HNCNH CH3O NH3D+ H2NCO+ NCCNH+ CH3Cl MgC3N HC3O+ NH2OH HC3S+ H2CCS C4S CHOSH HCSCN HC3O NaCCCN MgC3N+ C2H3+ NCCHS 6 Atoms CH3OH CH3CN NH2CHO CH3SH C2H4 C5H CH3NC HC2CHO H2C4 C5S HC3NH+ C5N HC4H HC4N c-H2C3O CH2CNH C5NHNCHCN SiH3CN MgC4H CH3CO+ H2CCCS CH2CCH HCSCCH C5O HCCNCH+ C5H+ c-C5H HC4S HMgCCCN MgC4H+ H2C3H+ HOCOOH H2C3N H2CNCN 7 Atoms CH3CHO CH3CCH CH3NH2 CH2CHCN HC5N C6H c-C2H4O CH2CHOH C6HCH3NCO HC5O HOCH2CN HC4NC HC3HNH c-C3HCCH MgC5N CH2C3N l-H2C5 NC4NH+ MgC5N+ 8 Atoms HCOOCH3 CH3C3N C7H CH3COOH H2C6 CH2OHCHO HC6H CH2CHCHO CH2CCHCN NH2CH2CN CH3CHNH CH3SiH3 NH2CONH2 HCCCH2CN CH2CHCCH MgC6H C2H3NH2 HOCHCHOH HCCCHCCC C7NCH3CHCO MgC6H+ 9 Atoms CH3OCH3 CH3CH2OH CH3CH2CN HC7N CH3C4H C8H CH3CONH2 C8HCH2CHCH3 CH3CH2SH HC7O CH3NHCHO H2CCCHCCH HCCCHCHCN H2CCHC3N 10 Atoms CH3COCH3 HOCH2CH2OH CH3CH2CHO CH3C5N CH3CHCH2O CH3OCH2OH H2CCCHC3N C6H4 C2H5NCO HC7NH+ CH3CHCHCN CH2CCH3CN CH2CHCH2CN NH2COCH2OH CH3CH2CCH 11 Atoms HC9N CH3C6H C2H5OCHO CH3COOCH3 CH3COCH2OH C5H6 NH2CH2CH2OH CH2CCHC4H C10HC4H5CN 12 Atoms C6H6 n-C3H7CN i-C3H7CN C2H5OCH3 1-C5H5CN 2-C5H5CN n-CH3CH2CH2OH i-CH3CH2CH2OH i-C4H8 13+ Atoms C6H5CN HC11N 1-C5H5CCH 2-C5H5CCH c-C5H4CCH2 CH3OCH2CH2OH c-C6H5CCH 1-C10H7CN 2-C10H7CN C9H8 2-C9H7CN C60 C60+ C70 307 Molecules Last Updated: 31 Dec 2024 McGuire 2022 ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] A Complex Molecular Universe Known Interstellar Molecules Created with ASTROMOL v2021.9.1 bmcguir2.github.io/astromol McGuire 2022 ApJS 259, 30 2 Atoms CH CN CH+ OH CO H2 SiO CS SO SiS NS C2 NO HCl NaCl AlCl KCl AlF PN SiC CP NH SiN SO+ CO+ HF N2 CF+ PO O2 AlO CNOH+ SH+ HCl+ SH TiO ArH+ NS+ HeH+ VO PO+ SiP FeC 3 Atoms H2O HCO+ HCN OCS HNC H2S N2H+ C2H SO2 HCO HNO HCS+ HOC+ SiC2 C2S C3 CO2 CH2 C2O MgNC NH2 NaCN N2O MgCN H3+ SiCN AlNC SiNC HCP CCP AlOH H2O+ H2Cl+ KCN FeCN HO2 TiO2 CCN SiCSi S2H HCS HSC NCO CaNC NCS MgC2 HSO CaC2 4 Atoms NH3 H2CO HNCO H2CS C2H2 C3N HNCS HOCO+ C3O l-C3H HCNH+ H3O+ C3S c-C3H HC2N H2CN SiC3 CH3 C3NPH3 HCNO HOCN HSCN HOOH l-C3H+ HMgNC HCCO CNCN HONO MgCCH HCCS HNCN H2NC HCCS+ CH3+ HCNS HOCS+ HNSO 5 Atoms HC3N HCOOH CH2NH NH2CN H2CCO C4H SiH4 c-C3H2 CH2CN C5 SiC4 H2CCC CH4 HCCNC HNCCC H2COH+ C4HCNCHO HNCNH CH3O NH3D+ H2NCO+ NCCNH+ CH3Cl MgC3N HC3O+ NH2OH HC3S+ H2CCS C4S CHOSH HCSCN HC3O NaCCCN MgC3N+ C2H3+ NCCHS 6 Atoms CH3OH CH3CN NH2CHO CH3SH C2H4 C5H CH3NC HC2CHO H2C4 C5S HC3NH+ C5N HC4H HC4N c-H2C3O CH2CNH C5NHNCHCN SiH3CN MgC4H CH3CO+ H2CCCS CH2CCH HCSCCH C5O HCCNCH+ C5H+ c-C5H HC4S HMgCCCN MgC4H+ H2C3H+ HOCOOH H2C3N H2CNCN 7 Atoms CH3CHO CH3CCH CH3NH2 CH2CHCN HC5N C6H c-C2H4O CH2CHOH C6HCH3NCO HC5O HOCH2CN HC4NC HC3HNH c-C3HCCH MgC5N CH2C3N l-H2C5 NC4NH+ MgC5N+ 8 Atoms HCOOCH3 CH3C3N C7H CH3COOH H2C6 CH2OHCHO HC6H CH2CHCHO CH2CCHCN NH2CH2CN CH3CHNH CH3SiH3 NH2CONH2 HCCCH2CN CH2CHCCH MgC6H C2H3NH2 HOCHCHOH HCCCHCCC C7NCH3CHCO MgC6H+ 9 Atoms CH3OCH3 CH3CH2OH CH3CH2CN HC7N CH3C4H C8H CH3CONH2 C8HCH2CHCH3 CH3CH2SH HC7O CH3NHCHO H2CCCHCCH HCCCHCHCN H2CCHC3N 10 Atoms CH3COCH3 HOCH2CH2OH CH3CH2CHO CH3C5N CH3CHCH2O CH3OCH2OH H2CCCHC3N C6H4 C2H5NCO HC7NH+ CH3CHCHCN CH2CCH3CN CH2CHCH2CN NH2COCH2OH CH3CH2CCH 11 Atoms HC9N CH3C6H C2H5OCHO CH3COOCH3 CH3COCH2OH C5H6 NH2CH2CH2OH CH2CCHC4H C10HC4H5CN 12 Atoms C6H6 n-C3H7CN i-C3H7CN C2H5OCH3 1-C5H5CN 2-C5H5CN n-CH3CH2CH2OH i-CH3CH2CH2OH i-C4H8 13+ Atoms C6H5CN HC11N 1-C5H5CCH 2-C5H5CCH c-C5H4CCH2 CH3OCH2CH2OH c-C6H5CCH 1-C10H7CN 2-C10H7CN C9H8 2-C9H7CN C60 C60+ C70 307 Molecules Last Updated: 31 Dec 2024 McGuire 2022 Acetaldehyde CH3CHO Methanol CH3OH Interstellar “Complex” Organic Molecules “COMs” or “iCOMs” •Contains at least 6 or more atoms •Contains at least one carbon atom Herbst & van Dishoeck 2009; Ceccarelli et al. 2017 Acetone (CH3)2CO ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] A Complex Molecular Universe Known Interstellar Molecules Created with ASTROMOL v2021.9.1 bmcguir2.github.io/astromol McGuire 2022 ApJS 259, 30 2 Atoms CH CN CH+ OH CO H2 SiO CS SO SiS NS C2 NO HCl NaCl AlCl KCl AlF PN SiC CP NH SiN SO+ CO+ HF N2 CF+ PO O2 AlO CNOH+ SH+ HCl+ SH TiO ArH+ NS+ HeH+ VO PO+ SiP FeC 3 Atoms H2O HCO+ HCN OCS HNC H2S N2H+ C2H SO2 HCO HNO HCS+ HOC+ SiC2 C2S C3 CO2 CH2 C2O MgNC NH2 NaCN N2O MgCN H3+ SiCN AlNC SiNC HCP CCP AlOH H2O+ H2Cl+ KCN FeCN HO2 TiO2 CCN SiCSi S2H HCS HSC NCO CaNC NCS MgC2 HSO CaC2 4 Atoms NH3 H2CO HNCO H2CS C2H2 C3N HNCS HOCO+ C3O l-C3H HCNH+ H3O+ C3S c-C3H HC2N H2CN SiC3 CH3 C3NPH3 HCNO HOCN HSCN HOOH l-C3H+ HMgNC HCCO CNCN HONO MgCCH HCCS HNCN H2NC HCCS+ CH3+ HCNS HOCS+ HNSO 5 Atoms HC3N HCOOH CH2NH NH2CN H2CCO C4H SiH4 c-C3H2 CH2CN C5 SiC4 H2CCC CH4 HCCNC HNCCC H2COH+ C4HCNCHO HNCNH CH3O NH3D+ H2NCO+ NCCNH+ CH3Cl MgC3N HC3O+ NH2OH HC3S+ H2CCS C4S CHOSH HCSCN HC3O NaCCCN MgC3N+ C2H3+ NCCHS 6 Atoms CH3OH CH3CN NH2CHO CH3SH C2H4 C5H CH3NC HC2CHO H2C4 C5S HC3NH+ C5N HC4H HC4N c-H2C3O CH2CNH C5NHNCHCN SiH3CN MgC4H CH3CO+ H2CCCS CH2CCH HCSCCH C5O HCCNCH+ C5H+ c-C5H HC4S HMgCCCN MgC4H+ H2C3H+ HOCOOH H2C3N H2CNCN 7 Atoms CH3CHO CH3CCH CH3NH2 CH2CHCN HC5N C6H c-C2H4O CH2CHOH C6HCH3NCO HC5O HOCH2CN HC4NC HC3HNH c-C3HCCH MgC5N CH2C3N l-H2C5 NC4NH+ MgC5N+ 8 Atoms HCOOCH3 CH3C3N C7H CH3COOH H2C6 CH2OHCHO HC6H CH2CHCHO CH2CCHCN NH2CH2CN CH3CHNH CH3SiH3 NH2CONH2 HCCCH2CN CH2CHCCH MgC6H C2H3NH2 HOCHCHOH HCCCHCCC C7NCH3CHCO MgC6H+ 9 Atoms CH3OCH3 CH3CH2OH CH3CH2CN HC7N CH3C4H C8H CH3CONH2 C8HCH2CHCH3 CH3CH2SH HC7O CH3NHCHO H2CCCHCCH HCCCHCHCN H2CCHC3N 10 Atoms CH3COCH3 HOCH2CH2OH CH3CH2CHO CH3C5N CH3CHCH2O CH3OCH2OH H2CCCHC3N C6H4 C2H5NCO HC7NH+ CH3CHCHCN CH2CCH3CN CH2CHCH2CN NH2COCH2OH CH3CH2CCH 11 Atoms HC9N CH3C6H C2H5OCHO CH3COOCH3 CH3COCH2OH C5H6 NH2CH2CH2OH CH2CCHC4H C10HC4H5CN 12 Atoms C6H6 n-C3H7CN i-C3H7CN C2H5OCH3 1-C5H5CN 2-C5H5CN n-CH3CH2CH2OH i-CH3CH2CH2OH i-C4H8 13+ Atoms C6H5CN HC11N 1-C5H5CCH 2-C5H5CCH c-C5H4CCH2 CH3OCH2CH2OH c-C6H5CCH 1-C10H7CN 2-C10H7CN C9H8 2-C9H7CN C60 C60+ C70 307 Molecules Last Updated: 31 Dec 2024 McGuire 2022 Interstellar “Complex” Organic Molecules “COMs” or “iCOMs” •Contains at least 6 or more atoms •Contains at least one carbon atom Herbst & van Dishoeck 2009; Ceccarelli et al. 2017 Precursor “Prebio,c” Species (“CHNOPS”) •Believed to be involved in the processes leading to the origin of life PO Amino Acetonitrile HCN SO2 E.g., Baross et al., 2020, Sasselov et al., 2020, Krijt et al., 2022 ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] A Complex Molecular Universe Known Interstellar Molecules Created with ASTROMOL v2021.9.1 bmcguir2.github.io/astromol McGuire 2022 ApJS 259, 30 2 Atoms CH CN CH+ OH CO H2 SiO CS SO SiS NS C2 NO HCl NaCl AlCl KCl AlF PN SiC CP NH SiN SO+ CO+ HF N2 CF+ PO O2 AlO CNOH+ SH+ HCl+ SH TiO ArH+ NS+ HeH+ VO PO+ SiP FeC 3 Atoms H2O HCO+ HCN OCS HNC H2S N2H+ C2H SO2 HCO HNO HCS+ HOC+ SiC2 C2S C3 CO2 CH2 C2O MgNC NH2 NaCN N2O MgCN H3+ SiCN AlNC SiNC HCP CCP AlOH H2O+ H2Cl+ KCN FeCN HO2 TiO2 CCN SiCSi S2H HCS HSC NCO CaNC NCS MgC2 HSO CaC2 4 Atoms NH3 H2CO HNCO H2CS C2H2 C3N HNCS HOCO+ C3O l-C3H HCNH+ H3O+ C3S c-C3H HC2N H2CN SiC3 CH3 C3NPH3 HCNO HOCN HSCN HOOH l-C3H+ HMgNC HCCO CNCN HONO MgCCH HCCS HNCN H2NC HCCS+ CH3+ HCNS HOCS+ HNSO 5 Atoms HC3N HCOOH CH2NH NH2CN H2CCO C4H SiH4 c-C3H2 CH2CN C5 SiC4 H2CCC CH4 HCCNC HNCCC H2COH+ C4HCNCHO HNCNH CH3O NH3D+ H2NCO+ NCCNH+ CH3Cl MgC3N HC3O+ NH2OH HC3S+ H2CCS C4S CHOSH HCSCN HC3O NaCCCN MgC3N+ C2H3+ NCCHS 6 Atoms CH3OH CH3CN NH2CHO CH3SH C2H4 C5H CH3NC HC2CHO H2C4 C5S HC3NH+ C5N HC4H HC4N c-H2C3O CH2CNH C5NHNCHCN SiH3CN MgC4H CH3CO+ H2CCCS CH2CCH HCSCCH C5O HCCNCH+ C5H+ c-C5H HC4S HMgCCCN MgC4H+ H2C3H+ HOCOOH H2C3N H2CNCN 7 Atoms CH3CHO CH3CCH CH3NH2 CH2CHCN HC5N C6H c-C2H4O CH2CHOH C6HCH3NCO HC5O HOCH2CN HC4NC HC3HNH c-C3HCCH MgC5N CH2C3N l-H2C5 NC4NH+ MgC5N+ 8 Atoms HCOOCH3 CH3C3N C7H CH3COOH H2C6 CH2OHCHO HC6H CH2CHCHO CH2CCHCN NH2CH2CN CH3CHNH CH3SiH3 NH2CONH2 HCCCH2CN CH2CHCCH MgC6H C2H3NH2 HOCHCHOH HCCCHCCC C7NCH3CHCO MgC6H+ 9 Atoms CH3OCH3 CH3CH2OH CH3CH2CN HC7N CH3C4H C8H CH3CONH2 C8HCH2CHCH3 CH3CH2SH HC7O CH3NHCHO H2CCCHCCH HCCCHCHCN H2CCHC3N 10 Atoms CH3COCH3 HOCH2CH2OH CH3CH2CHO CH3C5N CH3CHCH2O CH3OCH2OH H2CCCHC3N C6H4 C2H5NCO HC7NH+ CH3CHCHCN CH2CCH3CN CH2CHCH2CN NH2COCH2OH CH3CH2CCH 11 Atoms HC9N CH3C6H C2H5OCHO CH3COOCH3 CH3COCH2OH C5H6 NH2CH2CH2OH CH2CCHC4H C10HC4H5CN 12 Atoms C6H6 n-C3H7CN i-C3H7CN C2H5OCH3 1-C5H5CN 2-C5H5CN n-CH3CH2CH2OH i-CH3CH2CH2OH i-C4H8 13+ Atoms C6H5CN HC11N 1-C5H5CCH 2-C5H5CCH c-C5H4CCH2 CH3OCH2CH2OH c-C6H5CCH 1-C10H7CN 2-C10H7CN C9H8 2-C9H7CN C60 C60+ C70 307 Molecules Last Updated: 31 Dec 2024 McGuire 2022 New complex molecules added frequently! Dimethyl sulfide! CH3SCH3 Sanz-Novo et al., 2025 (see Sanz-Novo & San Andrés posters! ) High-mass G+0.69 Cloud ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] A Complex Molecular Universe Known Interstellar Molecules Created with ASTROMOL v2021.9.1 bmcguir2.github.io/astromol McGuire 2022 ApJS 259, 30 2 Atoms CH CN CH+ OH CO H2 SiO CS SO SiS NS C2 NO HCl NaCl AlCl KCl AlF PN SiC CP NH SiN SO+ CO+ HF N2 CF+ PO O2 AlO CNOH+ SH+ HCl+ SH TiO ArH+ NS+ HeH+ VO PO+ SiP FeC 3 Atoms H2O HCO+ HCN OCS HNC H2S N2H+ C2H SO2 HCO HNO HCS+ HOC+ SiC2 C2S C3 CO2 CH2 C2O MgNC NH2 NaCN N2O MgCN H3+ SiCN AlNC SiNC HCP CCP AlOH H2O+ H2Cl+ KCN FeCN HO2 TiO2 CCN SiCSi S2H HCS HSC NCO CaNC NCS MgC2 HSO CaC2 4 Atoms NH3 H2CO HNCO H2CS C2H2 C3N HNCS HOCO+ C3O l-C3H HCNH+ H3O+ C3S c-C3H HC2N H2CN SiC3 CH3 C3NPH3 HCNO HOCN HSCN HOOH l-C3H+ HMgNC HCCO CNCN HONO MgCCH HCCS HNCN H2NC HCCS+ CH3+ HCNS HOCS+ HNSO 5 Atoms HC3N HCOOH CH2NH NH2CN H2CCO C4H SiH4 c-C3H2 CH2CN C5 SiC4 H2CCC CH4 HCCNC HNCCC H2COH+ C4HCNCHO HNCNH CH3O NH3D+ H2NCO+ NCCNH+ CH3Cl MgC3N HC3O+ NH2OH HC3S+ H2CCS C4S CHOSH HCSCN HC3O NaCCCN MgC3N+ C2H3+ NCCHS 6 Atoms CH3OH CH3CN NH2CHO CH3SH C2H4 C5H CH3NC HC2CHO H2C4 C5S HC3NH+ C5N HC4H HC4N c-H2C3O CH2CNH C5NHNCHCN SiH3CN MgC4H CH3CO+ H2CCCS CH2CCH HCSCCH C5O HCCNCH+ C5H+ c-C5H HC4S HMgCCCN MgC4H+ H2C3H+ HOCOOH H2C3N H2CNCN 7 Atoms CH3CHO CH3CCH CH3NH2 CH2CHCN HC5N C6H c-C2H4O CH2CHOH C6HCH3NCO HC5O HOCH2CN HC4NC HC3HNH c-C3HCCH MgC5N CH2C3N l-H2C5 NC4NH+ MgC5N+ 8 Atoms HCOOCH3 CH3C3N C7H CH3COOH H2C6 CH2OHCHO HC6H CH2CHCHO CH2CCHCN NH2CH2CN CH3CHNH CH3SiH3 NH2CONH2 HCCCH2CN CH2CHCCH MgC6H C2H3NH2 HOCHCHOH HCCCHCCC C7NCH3CHCO MgC6H+ 9 Atoms CH3OCH3 CH3CH2OH CH3CH2CN HC7N CH3C4H C8H CH3CONH2 C8HCH2CHCH3 CH3CH2SH HC7O CH3NHCHO H2CCCHCCH HCCCHCHCN H2CCHC3N 10 Atoms CH3COCH3 HOCH2CH2OH CH3CH2CHO CH3C5N CH3CHCH2O CH3OCH2OH H2CCCHC3N C6H4 C2H5NCO HC7NH+ CH3CHCHCN CH2CCH3CN CH2CHCH2CN NH2COCH2OH CH3CH2CCH 11 Atoms HC9N CH3C6H C2H5OCHO CH3COOCH3 CH3COCH2OH C5H6 NH2CH2CH2OH CH2CCHC4H C10HC4H5CN 12 Atoms C6H6 n-C3H7CN i-C3H7CN C2H5OCH3 1-C5H5CN 2-C5H5CN n-CH3CH2CH2OH i-CH3CH2CH2OH i-C4H8 13+ Atoms C6H5CN HC11N 1-C5H5CCH 2-C5H5CCH c-C5H4CCH2 CH3OCH2CH2OH c-C6H5CCH 1-C10H7CN 2-C10H7CN C9H8 2-C9H7CN C60 C60+ C70 307 Molecules Last Updated: 31 Dec 2024 McGuire 2022 New complex molecules added frequently! Cyclopropenethione! c-C3H2S Remijan et al., 2025 Low-mass TMC-1 Cloud ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] A Complex Molecular Universe Known Interstellar Molecules Created with ASTROMOL v2021.9.1 bmcguir2.github.io/astromol McGuire 2022 ApJS 259, 30 2 Atoms CH CN CH+ OH CO H2 SiO CS SO SiS NS C2 NO HCl NaCl AlCl KCl AlF PN SiC CP NH SiN SO+ CO+ HF N2 CF+ PO O2 AlO CNOH+ SH+ HCl+ SH TiO ArH+ NS+ HeH+ VO PO+ SiP FeC 3 Atoms H2O HCO+ HCN OCS HNC H2S N2H+ C2H SO2 HCO HNO HCS+ HOC+ SiC2 C2S C3 CO2 CH2 C2O MgNC NH2 NaCN N2O MgCN H3+ SiCN AlNC SiNC HCP CCP AlOH H2O+ H2Cl+ KCN FeCN HO2 TiO2 CCN SiCSi S2H HCS HSC NCO CaNC NCS MgC2 HSO CaC2 4 Atoms NH3 H2CO HNCO H2CS C2H2 C3N HNCS HOCO+ C3O l-C3H HCNH+ H3O+ C3S c-C3H HC2N H2CN SiC3 CH3 C3NPH3 HCNO HOCN HSCN HOOH l-C3H+ HMgNC HCCO CNCN HONO MgCCH HCCS HNCN H2NC HCCS+ CH3+ HCNS HOCS+ HNSO 5 Atoms HC3N HCOOH CH2NH NH2CN H2CCO C4H SiH4 c-C3H2 CH2CN C5 SiC4 H2CCC CH4 HCCNC HNCCC H2COH+ C4HCNCHO HNCNH CH3O NH3D+ H2NCO+ NCCNH+ CH3Cl MgC3N HC3O+ NH2OH HC3S+ H2CCS C4S CHOSH HCSCN HC3O NaCCCN MgC3N+ C2H3+ NCCHS 6 Atoms CH3OH CH3CN NH2CHO CH3SH C2H4 C5H CH3NC HC2CHO H2C4 C5S HC3NH+ C5N HC4H HC4N c-H2C3O CH2CNH C5NHNCHCN SiH3CN MgC4H CH3CO+ H2CCCS CH2CCH HCSCCH C5O HCCNCH+ C5H+ c-C5H HC4S HMgCCCN MgC4H+ H2C3H+ HOCOOH H2C3N H2CNCN 7 Atoms CH3CHO CH3CCH CH3NH2 CH2CHCN HC5N C6H c-C2H4O CH2CHOH C6HCH3NCO HC5O HOCH2CN HC4NC HC3HNH c-C3HCCH MgC5N CH2C3N l-H2C5 NC4NH+ MgC5N+ 8 Atoms HCOOCH3 CH3C3N C7H CH3COOH H2C6 CH2OHCHO HC6H CH2CHCHO CH2CCHCN NH2CH2CN CH3CHNH CH3SiH3 NH2CONH2 HCCCH2CN CH2CHCCH MgC6H C2H3NH2 HOCHCHOH HCCCHCCC C7NCH3CHCO MgC6H+ 9 Atoms CH3OCH3 CH3CH2OH CH3CH2CN HC7N CH3C4H C8H CH3CONH2 C8HCH2CHCH3 CH3CH2SH HC7O CH3NHCHO H2CCCHCCH HCCCHCHCN H2CCHC3N 10 Atoms CH3COCH3 HOCH2CH2OH CH3CH2CHO CH3C5N CH3CHCH2O CH3OCH2OH H2CCCHC3N C6H4 C2H5NCO HC7NH+ CH3CHCHCN CH2CCH3CN CH2CHCH2CN NH2COCH2OH CH3CH2CCH 11 Atoms HC9N CH3C6H C2H5OCHO CH3COOCH3 CH3COCH2OH C5H6 NH2CH2CH2OH CH2CCHC4H C10HC4H5CN 12 Atoms C6H6 n-C3H7CN i-C3H7CN C2H5OCH3 1-C5H5CN 2-C5H5CN n-CH3CH2CH2OH i-CH3CH2CH2OH i-C4H8 13+ Atoms C6H5CN HC11N 1-C5H5CCH 2-C5H5CCH c-C5H4CCH2 CH3OCH2CH2OH c-C6H5CCH 1-C10H7CN 2-C10H7CN C9H8 2-C9H7CN C60 C60+ C70 307 Molecules Last Updated: 31 Dec 2024 McGuire 2022 Today, most new detections come from dark clouds! 2021 2025 Percentage of known molecules that were detected for the first time in carbon stars, dark clouds, Line-of-sight (LOS) clouds, and Star Forming Regions (SFR) ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Rich chemistry throughout! NASA and the Night Sky Network Molecular Life Cycle There is a rich complex chemistry throughout the interstellar medium (ISM), from the beginning to the end stages of both low-mass and highmass star formation The natal molecular cloud environment where stars begin their life-cycle sets constraints on initial conditions that get influence the later stages ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Rich chemistry throughout! Molecular Life Cycle There is a rich complex chemistry throughout the interstellar medium (ISM), from the beginning to the end stages of both low-mass and highmass star formation The natal molecular cloud environment where stars begin their life-cycle sets constraints on initial conditions that get influence the later stages +Planets, Comets, Meteorites +Disks NASA and the Night Sky Network ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] (+ see Jenson & Colzi talk! + Andras-Letanovszky, Giers, & Steffes posters!) 1. Cold and Dense: dense gas tracers such as NH3 (also a temperature probe) and N2H+ closely match that of sub-millimeter con>nuum 2. Quiescent: no violent ou?lows or energe>c mo>ons, “sharp” molecular line profiles and close-to-thermal linewidths - Occasionally Infall: observa>ons of op>cally thick, selfabsorbed asymmetric line profiles for species such as CS, H2CO, HCN, or HCO+ can trace inward mo>on of the gas 3. Chemical depleEon: Atoms and molecules in the gas-phase freezeout onto the cold (~10 K) surfaces of the sub-micron dust grains, forming the so-called icy grain mantles - Leading to Isotopic FracEonaEon: sensi>ve to either photon flux, or gas or grain temperatures, the D/H, 13C/12C, 15N/14N, and 18O/16O ra>os in molecules can be used to pinpoint when and where they formed ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Caselli & Ceccarelli 2012 Aikawa et al. 2001 Starless and Prestellar Core Characteristics + See also: Dalgarno & Lepp 1984; Roberts & Millar 2000; Caselli et al., 1999; Bacmann et al., 2002; Tafall a et al. , 2002, 2006; Pagani et al., 2005 Crapsi et al., 2005; Lippok et al., 2013, etc., CCS (greyscale) N2H+ (contours) Adapted from Scibelli Thesis, 2023 Starless and Prestellar Core Classifications Dense Core Classification Evolutionary Stages Definitions Examples Starless Core Chemically Young • Low CO depletion • “Earlytime” molecules (CS, CCS, etc.) peak on core • “Late-time” molecules (NH3, N2H+) very weak •Weak deuterated molecules Dynamically Young • No evidence in kinematics of collapse • Lower volume densities (n) Prestellar Core Chemically Evolved • High CO depletion • “Late-time” molecules (NH3, N2H+) bright and centrally concentrated • Bright deuterated molecules Dynamically Evolved • Kinematic collapse is evident (i.e., HCN, HCO+ profiles) • High volume densities (n) More Evolved n ~ 3 × 105 cm−3 n ~ a few × 106 cm−3 L1521E L1544 n ~ a few × 105 cm−3 L1498 Tafalla & Santiago 2004 Jiménez-Serra et al., 2021 Shirley et al., 2000 ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Dense Core Classification Evolutionary Stages Definitions Examples Starless Core Chemically Young • Low CO depletion • “Earlytime” molecules (CS, CCS, etc.) peak on core • “Late-time” molecules (NH3, N2H+) very weak •Weak deuterated molecules Dynamically Young • No evidence in kinematics of collapse • Lower volume densities (n) Prestellar Core Chemically Evolved • High CO depletion • “Late-time” molecules (NH3, N2H+) bright and centrally concentrated • Bright deuterated molecules Dynamically Evolved • Kinematic collapse is evident (i.e., HCN, HCO+ profiles) • High volume densities (n) More Evolved n ~ 3 × 105 cm−3 n ~ a few × 106 cm−3 L1521E L1544 n ~ a few × 105 cm−3 L1498 Tafalla & Santiago 2004 Jiménez-Serra et al., 2021 Shirley et al., 2000 Where do we see complex chemistry? Starless and Prestellar Core Classifications Adapted from Scibelli Thesis, 2023 ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] http://www.esa.int/spaceinimages/Images/2001/05/Astrobiology Complex Chemistry in Starless and Prestellar Cores Key question: What is the ‘limit’ of chemical complexity at this earliest stage of star formation and how widespread is it? ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] http://www.esa.int/spaceinimages/Images/2001/05/Astrobiology Complex Chemistry in Starless and Prestellar Cores Key question: How do large molecules form and get destroyed in such cold (10K) and isolated environments, and what role do external factors such as radiation play? Key question: What is the ‘limit’ of chemical complexity at this earliest stage of star formation and how widespread is it? ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] http://www.esa.int/spaceinimages/Images/2001/05/Astrobiology Complex Chemistry in Starless and Prestellar Cores Key question: What is the degree of inheritance? Do the organic molecules synthesized in cold starless and prestellar cores contribute to the chemical evolu7on needed for the emergence of life on Earth? Key question: What is the ‘limit’ of chemical complexity at this earliest stage of star formation and how widespread is it? Key question: How do large molecules form and get destroyed in such cold (10K) and isolated environments, and what role do external factors such as radiation play? ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] I. Laboratory studies + Computational Chemistry II. Theoretical Models III. Observations E.g., Carl, T. et al., 2023 (+see Mazurek and Carl talks!) E.g., Riedel, W. et al., 2023 (+see Riedel talk!) E.g., Santos, J. et al., 2022, 2024 (+ see Santos talk!); Kruczkiewicz et al., 2024 (+ see Kruczkiewicz talk!) -Tell us what molecules to observe and can identify new species! -Provide insight into the reaction networks (get binding energies, collisional rates, reaction rates, etc.,) -Tell us about the likely chemical formation pathways -Tell us if that molecule is present in an object and how much of it is along our line-of-sight See Reviews: Caselli & Ceccarelli 2012; Jørgensen et al. 2020; Öberg & Bergin et al. 2021; Ceccarelli et al., 2023 (PPVII) The three ‘pillars’ of astrochemistry allow us to study COMs in starless and prestellar cores, and can help answer our key questions: ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Deuterated Methyl Mercaptan (CH2DSH)! Bunn et al., 2025 I. Laboratory studies + Computational Chemistry II. Theoretical Models III. Observations E.g., Carl, T. et al., 2023 (+see Mazurek and Carl talks!) E.g., Riedel, W. et al., 2023 (+see Riedel talk!) E.g., Santos, J. et al., 2022, 2024 (+ see Santos talk!); Kruczkiewicz et al., 2024 (+ see Kruczkiewicz talk!) -Tell us what molecules to observe and can identify new species! -Provide insight into the reaction networks (get binding energies, collisional rates, reaction rates, etc.,) -Tell us about the likely chemical formation pathways -Tell us if that molecule is present in an object and how much of it is along our line-of-sight See Reviews: Caselli & Ceccarelli 2012; Jørgensen et al. 2020; Öberg & Bergin et al. 2021; Ceccarelli et al., 2023 (PPVII) The three ‘pillars’ of astrochemistry allow us to study COMs in starless and prestellar cores, and can help answer our key questions: ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Adapted from Jørgensen et al. 2020 Chemical models predict abundances of COMs which can be constrained with observa8ons, e.g., Vasyunin et al., 2017 CH3OCH3 Core: L1544 I. Laboratory studies + Computational Chemistry II. Theoretical Models III. Observations E.g., Carl, T. et al., 2023 (+see Mazurek and Carl talks!) E.g., Riedel, W. et al., 2023 (+see Riedel talk!) E.g., Santos, J. et al., 2022, 2024 (+ see Santos talk!); Kruczkiewicz et al., 2024 (+ see Kruczkiewicz talk!) -Tell us what molecules to observe and can identify new species! -Provide insight into the reaction networks (get binding energies, collisional rates, reaction rates, etc.,) -Tell us about the likely chemical formation pathways -Tell us if that molecule is present in an object and how much of it is along our line-of-sight See Reviews: Caselli & Ceccarelli 2012; Jørgensen et al. 2020; Öberg & Bergin et al. 2021; Ceccarelli et al., 2023 (PPVII) The three ‘pillars’ of astrochemistry allow us to study COMs in starless and prestellar cores, and can help answer our key questions: ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Birthplace of low-mass stars (M ≤ a few M¤) Dense (104 - 105 cm-3) & cold (≤ 10K ) Birthplace of low-mass stars (M ≤ a few M¤) Dense (104 - 105 cm-3) & cold (≤ 10K ) Starless Core B68 Visible light Image I. Laboratory studies + Computational Chemistry II. Theoretical Models III. Observations E.g., Carl, T. et al., 2023 (+see Mazurek and Carl talks!) E.g., Riedel, W. et al., 2023 (+see Riedel talk!) E.g., Santos, J. et al., 2022, 2024 (+ see Santos talk!); Kruczkiewicz et al., 2024 (+ see Kruczkiewicz talk!) -Tell us what molecules to observe and can identify new species! -Provide insight into the reaction networks (get binding energies, collisional rates, reaction rates, etc.,) -Tell us about the likely chemical formation pathways -Tell us if that molecule is present in an object and how much of it is along our line-of-sight See Reviews: Caselli & Ceccarelli 2012; Jørgensen et al. 2020; Öberg & Bergin et al. 2021; Ceccarelli et al., 2023 (PPVII) The three ‘pillars’ of astrochemistry allow us to study COMs in starless and prestellar cores, and can help answer our key questions: ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] 780 752 747 709 715 768 746 739 615 627 642 B5 NGC1333 B1-E 543 491 504 413 479 414 317 355 67 54 B1 339 321 326 264 344 398 256 231 130 L1455 IC348 657 658 656 799 800 Per6 L1451 HPZ6 Perseus Molecular Cloud ~ 300 pc The Prevalence of COMs in Starless and Prestellar Cores B7 B10 B211 B213 B218 B216 17 14 13 12 10 11 9 76 8 5 2 4 27 30 33 32 21 28 24 26 20 16 15 39 37 35 36 29 31 22 Taurus Molecular Cloud L1495-B218 ~ 135 pc Observa(ons with the Arizona Radio Observatory (ARO) 12 m show COMs are prevalent in > 60 ‘typical’ starless and prestellar cores – methanol (CH3OH) found in 100% & acetaldehyde (CH3CHO) found in > 50%! Scibelli & Shirley 2020 3mm Scibelli et al., 2024 Arizona 12m Dish Herschel core catalog: Marsh et al. 2016 NH3 observations: Seo et al., 2015 Within the last 5 years, we now know that complex molecules in starless and prestellar cores are not unique to only a handful of objects, there is a prevalence of COMs in other more ‘typical’ cores in low-mass environments! LaJanzi et al. 2020; Scibelli & Shirley 2020; Scibelli et al., 2021; Jiménez-Sera et al. 2021; Megías et al. 2023; Scibelli et al., 2024; Taniguchi et al., 2025; Scibelli et al., in review; Steffes et al., in prep; +Orion cores (ALMASOP Team) Liu+, in prep; Hsu+ in prep ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Herschel core catalogs: Pezzuto et al. 2021 NH3 observations: Rosolowsky et al. 2008 780 752 747 709 715 768 746 739 615 627 642 B5 NGC1333 B1-E 543 491 504 413 479 414 317 355 67 54 B1 339 321 326 264 344 398 256 231 130 L1455 IC348 657 658 656 799 800 Per6 L1451 HPZ6 Perseus Molecular Cloud ~ 300 pc The Prevalence of COMs in Starless and Prestellar Cores Herschel core catalogs: Pezzuto et al. 2021 NH3 observations: Rosolowsky et al. 2008 Scibelli et al., 2024 Yebes 40m Dish 7mm Detection Percentages: 80 % 60 % 93 % 34 % 27 % + Yebes 40m Observa>ons w/ 18.5 GHz of instantaneous bandwidth allowed for the detec>on of other COMs! Within the last 5 years, we now know that complex molecules in starless and prestellar cores are not unique to only a handful of objects, there is a prevalence of COMs in other more ‘typical’ cores in low-mass environments! LaJanzi et al. 2020; Scibelli & Shirley 2020; Scibelli et al., 2021; Jiménez-Sera et al. 2021; Megías et al. 2023; Scibelli et al., 2024; Taniguchi et al., 2025; Scibelli et al., in review; Steffes et al., in prep; +Orion cores (ALMASOP Team) Liu+, in prep; Hsu+ in prep ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Scibelli et al., 2024 Booth et al., 2021; Evans et al., 2025 (see Evans poster!) CH3OH is a good tracer molecule to compare abundances against because it forms on the grains and believed to survive the disk formation process Seeded Chemical Complexity ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Pueng these observaEons together, we plot COM abundances with respect to methanol across different stages of low-mass star formaEon à Seeded Chemical Complexity Pueng these observaEons together, we plot COM abundances with respect to methanol across different stages of low-mass star formaEon à ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] + Megías et al. 2023, Nagy et al. 2019; Scibelli et al. 2021, Scibelli & Shirley 2020, Jiménez-Serra et al. 2016, 2021, Vastel et al. 2014; Lattanzi et al. 2020, Bacmann et al. 2012; Yoshida et al. 2019, Yan g et al. 2021, Graninger et al. 2016; Bergner et al. 2017, van Gelder et al. 2020; Nazari et al. 2021, Calcutt et al. 2018; Jørgensen et al. 2018. Walsh et al. 2016; Loomis et al. 2018; Favre et al. 2018, Biver & Bockelée-Morvan 2019, Hänni et al. 2023 Scibelli et al., 2024 Seeded Chemical Complexity + Megías et al. 2023, Nagy et al. 2019; Scibelli et al. 2021, Scibelli & Shirley 2020, Jiménez-Serra et al. 2016, 2021, Vastel et al. 2014; Lattanzi et al. 2020, Bacmann et al. 2012; Yoshida et al. 2019, Yan g et al. 2021, Graninger et al. 2016; Bergner et al. 2017, van Gelder et al. 2020; Nazari et al. 2021, Calcutt et al. 2018; Jørgensen et al. 2018. Walsh et al. 2016; Loomis et al. 2018; Favre et al. 2018, Biver & Bockelée-Morvan 2019, Hänni et al. 2023 Scibelli et al., 2024 ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] +V883 Ori; Jeong et al., 2025 Pueng these observaEons together, we plot COM abundances with respect to methanol across different stages of low-mass star formaEon à Seeded Chemical Complexity Similari>es in abundances across stages and environments provides evidence that at least some of the COMS observed in later stages of star and planet forma>on were inherited from the cold prestellar core phase +V883 Ori; Jeong et al., 2025 ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Pueng these observaEons together, we plot COM abundances with respect to methanol across different stages of low-mass star formaEon à + Megías et al. 2023, Nagy et al. 2019; Scibelli et al. 2021, Scibelli & Shirley 2020, Jiménez-Serra et al. 2016, 2021, Vastel et al. 2014; Lattanzi et al. 2020, Bacmann et al. 2012; Yoshida et al. 2019, Yan g et al. 2021, Graninger et al. 2016; Bergner et al. 2017, van Gelder et al. 2020; Nazari et al. 2021, Calcutt et al. 2018; Jørgensen et al. 2018. Walsh et al. 2016; Loomis et al. 2018; Favre et al. 2018, Biver & Bockelée-Morvan 2019, Hänni et al. 2023 Scibelli et al., 2024 Seeded Chemical Complexity A nice ‘global view’… but it is s>ll unclear if more substan>al differences in abundances from core to core are due to: -SpaEal variaEons -Different chemical condiEons/processes -Different evoluEon histories ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] +V883 Ori; Jeong et al., 2025 + Megías et al. 2023, Nagy et al. 2019; Scibelli et al. 2021, Scibelli & Shirley 2020, Jiménez-Serra et al. 2016, 2021, Vastel et al. 2014; Lattanzi et al. 2020, Bacmann et al. 2012; Yoshida et al. 2019, Yan g et al. 2021, Graninger et al. 2016; Bergner et al. 2017, van Gelder et al. 2020; Nazari et al. 2021, Calcutt et al. 2018; Jørgensen et al. 2018. Walsh et al. 2016; Loomis et al. 2018; Favre et al. 2018, Biver & Bockelée-Morvan 2019, Hänni et al. 2023 Scibelli et al., 2024 Pueng these observaEons together, we plot COM abundances with respect to methanol across different stages of low-mass star formaEon à Spatial Distribution of COMs CH3OH detected at as low as Av ~ 3-4 mag! Dust peak CH3OH C4H Dust peak L1544 ALMA Field Spezzano et al., 2017 Cernicharo et al., 2023 C6H5CN Dust peak TMC-1 Taurus Molecular Cloud L1495-B218 Scibelli & Shirley 2020 (+ see also Spezzano et al., 2021, Punanova et al., 2022) ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] There has been effort to map simpler COMs (mostly CH3OH) in dense cores with single-dish radio telescopes, which show: -Chemical differenEaEon, i.e., differences in spaEal distribuEon, column densiEes, and temperatures between species -COMs trace filaments, at low Av, as well as dense cores (Bizzocchi et al. 2014; Soma et al. 2015; Spezzano et al., 2016, 2017, 2020, Nagy et al., 2019, Scibelli & Shirley 2020, Punanova et al., 2022, 2025; Cernicharo et al., 2023) Spatial Distribution of COMs CH3OH detected at as low as Av ~ 3-4 mag! Dust peak CH3OH C4H Dust peak L1544 ALMA Field Spezzano et al., 2017 Cernicharo et al., 2023 C6H5CN Dust peak TMC-1 Taurus Molecular Cloud L1495-B218 Scibelli & Shirley 2020 (+ see also Spezzano et al., 2021, Punanova et al., 2022) S>ll unknown is the spa>al distribu>on of larger COMs to high sensi>vity for a variety of cores, par>cularly prestellar ones! ALMA Band 1 can help? ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] There has been effort to map simpler COMs (mostly CH3OH) in dense cores with single-dish radio telescopes, which show: -Chemical differenEaEon, i.e., differences in spaEal distribuEon, column densiEes, and temperatures between species -COMs trace filaments, at low Av, as well as dense cores (Bizzocchi et al. 2014; Soma et al. 2015; Spezzano et al., 2016, 2017, 2020, Nagy et al., 2019, Scibelli & Shirley 2020, Punanova et al., 2022, 2025; Cernicharo et al., 2023) Modeling the Radial Abundance of COMs ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Scibelli et al., 2021 Core: L1498 Methanol peak Jiménez-Serra et al. 2021 (w/ MONACO code: Vasyunin & Herbst 2013; Vasyunin et al. 2017) Ongoing chemical modeling efforts aimed at reproducing COM abundances in starless and prestellar cores, in order to dis,nguish between COM forma,on pathways, suggest, -Gas-phase and grain surface chemistry is needed to enhance COM abundances at cold (10 K) temperatures -Models with different mechanisms for geeng molecules off grains into the gas-phase (e.g., chemical desorpEon, cosmic rays) can (for the most part) reproduce O-bearing COM abundances (Vasyunin & Herbst 2013; Ruaud et al., 2015; Vasyunin et al. 2017; Shingledecker & Herbst 2018; Shingledecker et al., 2018; Jin & Garrod 2020; Wakelam et al., 2021; Garrod et al., 2022; Kalvāns & Silsbee 2022; Paulive, Carder & Herbst 2022) Scibelli et al., 2021 Complex Chemistry in Starless and Prestellar Cores: Summary and Important Takeaways “Answered” “Unanswered” - COMs are prevalent in numerous starless and prestellar cores in different low-mass molecular clouds - Both gas-phase and grain-surface reacIons play a key role (e.g., desorp(on and nondiffusive surface chemistry) - Strong evidence to suggest that at least some of the organics observed in later stages was inherited from the prestellar phase - What causes varia(ons in COM detec(ons and abundances? - What is the spaIal (+kinemaIc!) distribuIon of large COMs in prestellar core(s) – can it help us constrain models? - Modeling nitrogenbearing COM formaIon at this early stage is needed! - What is the degree of inheritance? How can we test this? ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Key question: What is the ‘limit’ of chemical complexity at this earliest stage of star formation and how widespread is it? Key question: What is the degree of inheritance? Do the organic molecules synthesized in cold starless and prestellar cores contribute to the chemical evolu7on needed for the emergence of life on Earth? Key question: How do large molecules form and get destroyed in such cold (10K) and isolated environments, and what role do external factors such as radiation play? * ‘Starless core’ is a generic 'dense core’ (traced by species such as NH3 and N2H+) with no protostar present, whereas ‘prestellar core’ is a term designated to a dense core that is dynamically evolved and will collapse due to gravity and external pressure and form a protostar, protoplanetary disk, etc., Complex Chemistry in Starless and Prestellar Cores: Summary and Important Takeaways Thank you for your a,en.on! Looking forward to a great week of science! J ESO “Towards New Frontiers” 10-14 March 2025 Contact: [email protected] Key question: What is the ‘limit’ of chemical complexity at this earliest stage of star formation and how widespread is it? Key question: What is the degree of inheritance? Do the organic molecules synthesized in cold starless and prestellar cores contribute to the chemical evolu7on needed for the emergence of life on Earth? Key question: How do large molecules form and get destroyed in such cold (10K) and isolated environments, and what role do external factors such as radiation play? * ‘Starless core’ is a generic 'dense core’ (traced by species such as NH3 and N2H+) with no protostar present, whereas ‘prestellar core’ is a term designated to a dense core that is dynamically evolved and will collapse due to gravity and external pressure and form a protostar, protoplanetary disk, etc., “Answered” “Unanswered” - COMs are prevalent in numerous starless and prestellar cores in different low-mass molecular clouds - Both gas-phase and grain-surface reacIons play a key role (e.g., desorp(on and nondiffusive surface chemistry) - Strong evidence to suggest that at least some of the organics observed in later stages was inherited from the prestellar phase - What causes varia(ons in COM detec(ons and abundances? - What is the spaIal (+kinemaIc!) distribuIon of large COMs in prestellar core(s) – can it help us constrain models? - Modeling nitrogenbearing COM formaIon at this early stage is needed! - What is the degree of inheritance? How can we test this?