Molecular evolution throughout planetary system formation: from molecular clouds to comets

Evolution throughout star formation: from molecular clouds to comets Álvaro López-Gallifa Supervisor: Víctor M. Rivilla Centro de Astrobiología (CAB), CSIC-INTA, Spain European Southern Observatory (ESO), Chile This project has received funding from the Comunidad de Madrid through the Atracción de Talento Investigador (Doctores con experiencia) Grant (COOL: Cosmic Origins Of Life; 2019-T1/TIC15379), from the Agencia Estatal de Investigación (AEI) through the Ramón y Cajal programme (grant RYC2020-029387-I) financed by MCIN/AEI /10.13039/501100011033. and from the the Consejo Superior de Investigaciones Científicas (CSIC) and the Centro de Astrobiología (CAB) through the project 20225AT015 (Proyectos intramurales especiales del CSIC). Contact: [email protected] 1 Origin of prebiotic molecules Endogenous synthesis 2 Exogenous delivery Chyba et al. (1990), Cooper et al. (2001), Pearce et al. (2017) •∼330 molecules detected with increasing chemical complexity 3 Chemical complexity in the interstellar medium Courtesy of Brett McGuire The chemical history of star formation •Is there any chemical heritage between phases? 4 BILL SAXTON/NSF/AUI/NRAO Similar chemical content between star-forming regions and comets Bockeleé-Morvan et al. (2000) Drozdovskaya et al. (2019) 5 7 G31.41 core •Hot Molecular Core (HMC) with T>100K. •G31.41 is one of the most chemically rich star-forming regions in the Galaxy (e.g. Beltrán et al. 2009, Rivilla et al. 2017). 8 Massive star-forming region G31.41+0.31 (G31.41) Beltrán et al. 2021 9 Massive star-forming region G31.41+0.31 (G31.41) •GUAPOS: G31.41+0.31 Unbiased ALMA sPectral Observational Survey •This project is devoted to study the chemical inventory of G31 with ALMA covering full band 3 (84-116 GHz). • The spatial resolution is 1.2”x1.2” (4400 au x 4400 au). •The spectral resolution is about 0.5 MHz (1.2-1.8 km s−1) The GUAPOS project Beltrán et al. 2021 •Hot Molecular Core (HMC) with T>100K. •G31.41 is one of the most chemically rich star-forming regions in the Galaxy (e.g. Beltrán et al. 2009, Rivilla et al. 2017). Molecular inventory in G31.41 10 G31.41 shock region G31.41 core •Thermal processing on grains •Hot gas phase chemistry gas phase 17 Fontani et al. 2024 Fontani et al. 2024 G31.41 shock region •The shock region provides us with pristine material of the natal molecular cloud G31.41 core •Thermal processing on grains •Hot gas phase chemistry gas phase 18 30 detected molecules + multiple isotopologues and non-detections G31.41: shock vs core •The molecular abundances are poorly correlated •Possible reprocessing due to the high temperature conditions in G31.41 core Star-forming region (López-Gallifa et al. 2025a, in prep). 20 Low-mass Protostellar outflow e.g. Lefloch et al. 2012, 2016, 2017, 2021 High-mass Protostellar outflow Busch et al. 2024 Galatic center shock-dominated molecular cloud e.g. Zeng et al. 2018, Jiménez-Serra et al. 2020, Rivilla et al. 2022 (López-Gallifa et al. 2025a, in prep). G31.41 shock vs shock-dominated regions 22 •Similar molecular inventory on the 4 shock dominated regions located in different regions of the Galaxy (López-Gallifa et al. 2025a, in prep). G31.41 shock vs shock-dominated regions 23 Low-mass Protostellar outflow e.g. Lefloch et al. 2012, 2016, 2017, 2021 High-mass Protostellar outflow Busch et al. 2024 Galatic center shock-dominated molecular cloud e.g. Zeng et al. 2018, Jiménez-Serra et al. 2020 What about other galaxies? 26 Astrochemistry outside of our Galaxy: ALCHEMI •ALCHEMI: ALMA Comprehensive High-resolution Extragalactic Molecular Inventory (P.I. Sergio Martín) •Study of the CMZ of the nearby starburst galaxy NGC 253 •Frequency Coverage: 84 to 368 GHz (full ALMA Bands 3, 4, 5, 6, and 7) •1.6’’ (25pc) Spatial resolution 28 Comparison of the GMCs of NGC 253 P3 P6 P4 P7 29 Comparison of NGC 253 GMCs •The chemical reservoir is very similar in all the GMCs of the CMZ of NGC 253 P3 P6P4 P7 (López-Gallifa et al. 2025b, in prep). 30 NGC 253 vs Galactic sources (López-Gallifa et al. 2025b, in prep). High-mass star forming region Shock region Galatic center shockdominated molecular cloud 31 GUAPOS full spectrum 38 •GUAPOS I: Mininni et al. 2020 •GUAPOS II: Colzi et al. 2021 39 Comparison results 40 Comparison results 41 S-bearing molecules There is a bump here! Star-forming regions Comets Higher S/O ratio in the comet than in star-forming regions! Sulfur depletion problem? Star-forming regions Comet Correlation tests •In this work we use 3 correlation coeffcients: Spearman, Kendall and Theil-Shen. •Spearman is widely use and known. It is a range correlation test that rearrange the data and calculates the coefficient. •Knedall’s tau is a another coefficient based on the comparison between pairs of data, comparing if x and y are bigger or smaller than the other point. 42 Correlation tests •Theil-Sen´s method make a linear regression. The slope is calculate by doing the median of the slope of all the possible points in pairs. •It is an alternative to Pearsons method, but is more robust. Theil-Sen depends less on outliers. Once the slope is calculated, we make a correlation coefficient as in Pearson linear fit. 43 Comparison with other sources Low-mass star-forming region (hot corino) •Solar-like protostellar system •Chemically rich IRAS 16293-2422 B (IRAS16B), a low-mass proto-star (0.1 M☉) previously studied in detail. •67P/Churyumov-Gerasimenko (67P/CG): visited by the spacecraft Rosetta which provide unique in-situ massspectroscopy data (e.g. Drozdovskaya et al. 2019, and references therein). •46P/Wirtanen (46P/W): molecular inventory from millimeter single-dish observations (Biver et al. 2021). 44 Comets PILS survey (Jorgensen et al. 2016, Calcutt et al. 2018, Coutens et al. 2018, Drozdovskaya et al. 2019, Manigand et al. 2021) and Martín-Doménech et al. 2017 Source B 45 Comparison results (comet) (comet) Previous comparative studies All sources within a ratio of 2! HMSFRs GC Clouds H ot corinos PCs PS shock comets 46 Massive star-forming region G31.41+0.31 (G31.41) •Hot Molecular Core (HMC) with T>100K. •Distance = 3.75 kpc •Mass of 70 M☉. •G31 is one of the most chemically rich star-forming regions in the Galaxy (e.g. Beltrán et al. 2009, Rivilla et al. 2017). 47 Mininni et al. 2020 •4 massive protostars inside the core.