Symposium S11  3-4 July 2024

Once upon a time... our astrochemical history

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Aims and scope

   In the beginning, the Solar System was ''just'' a cloud of interstellar dust and gas, like many other molecular clouds in the Milky Way. About 4.6 billion years ago, however, this cloud started to contract, leading to the formation of the Sun and the Earth and triggering the emergence of life on our planet. In order to investigate our origins, we need to answer some fundamental questions related to this process: Can we reconstruct the history of our Solar System? Did the chemical complexity, which ultimately led to life, emerge during this process? These questions, apparently impossible to tackle for many years, are now part of the most exciting challenges of modern astrochemical research and are within reach to being addressed observationally, theoretically and experimentally.
   Astrochemistry is a powerful tool for reconstructing the history of our chemical origins, as molecular tracers are excellent probes of the physical and chemical evolution from prestellar cores to protoplanetary discs. Given the growing evidence that our Solar System formed in a cluster that contained both low- and high-mass stars, it is also crucial to study how irradiation with energetic photons and particles from nearby stars, formed close to the protosun, affected the chemical history of the Solar System.
   Large observational campaigns with (sub-)mm telescopes such as IRAM 30m, APEX, NOEMA and ALMA, as well as the new results from JWST in the mid-IR, provide a wealth of information about the molecular content of star-forming gas and about the composition of the icy mantles in protostellar objects. On the other hand, the current astrochemical models include physical and chemical processes that are now well-constrained thanks to the new results from laboratory experiments and theoretical calculations.
   The aim of this symposium is to foster new collaborations between experts in astrochemical observations and modelling to build a coherent picture of the emergence and evolution of molecular complexity during the star formation process. We aim to bring together the communities working on high-mass and low-mass star-forming regions and protoplanetary discs to build a global picture of star formation using astrochemistry.


The symposium is divided into three sessions:

  • Session I: Disks & Protoplanets
  • Session II: Low-mass star-forming regions & Sun-like protostars
  • Session III: High-mass star-forming regions & clusters
More specifically, the symposium aims to foster discussion and exchange in the following key areas:
  1. The exploitation of the huge datasets of molecular line observations from radio to infrared wavelengths (e.g. IRAM 30m, APEX, NOEMA ALMA, JWST, SKA and ngVLA), to characterise the chemical composition and evolution of star-forming regions and Sun-like planetary systems under different environmental conditions.
  2. State-of-the-art astrochemical models and toolkits, which include advanced techniques to predict the chemical composition of forming planetary systems, to develop a new model of the proto-Sun nebula.
The Symposium will include a selection of invited review speakers (20+5mins), contributed talks (12+3mins) and ePosters.

Invited speakers

  • Ashley T. Barnes (ESO, Garching; Germany)
  • ``Astrochemical fingerprint of high-mass star formation from the Galactic Center to the outer Galaxy''
  • Marta De Simone (ESO, Garching; Germany)
  • ``Chemical complexity in Sun-like star-forming regions on different spatial scales"
  • Stefano Facchini (Università degli Studi di Milano; Italy)
  • ``The chemical and dynamical interplay between disks and nascent planets "
  • Caroline Gieser (MPE, Center for Astrochemical Studies; Germany)
  • ``Modelling the physical and chemical structure of high-mass star-forming regions"
  • Inga Kamp (University of Groningen; The Netherlands)
  • ``Modelling the dynamical and chemical evolution from protostellar discs to protoplanets "
  • Alessandro Lupi (Università degli Studi dell'Insubria, Italy)
  • `The state-of-the-art of astrochemical models: What can be improved?`"

Scientific organisers

  • Giovanni Sabatini (Chair; INAF - Osservatorio Astrofisico di Arcetri; Italy)
  • Eleonora Bianchi (Co-Chair; Excellence Cluster ORIGINS; Germany)
  • Catherine Walsh (Co-Chair; University of Leeds; United Kingdom)
  • Alice S. Booth (Leiden Observatory; The Netherlands)
  • Stefano Bovino (Dipartimento di Chimica - Sapienza, Università di Roma; Italy)
  • Claudio Codella (INAF - Osservatorio Astrofisico di Arcetri; Italy)
  • Izaskun Jiménez-Serra (Centro de Astrobiología; Spain)
  • Linda Podio (INAF - Osservatorio Astrofisico di Arcetri; Italy)
  • Elena Redaelli (Max Planck Institute for extraterrestrial Physics; Germany)
  • Dmitry Semenov (Max-Planck-Institut für Astronomie; Germany)
  • Benoît Tabone (CNRS - Institut d'Astrophysique Spatiale; France)
  • Friedrich Wyrowski (Max-Planck-Institut für Radioastronomie; Germany)
The SOC acknowledge support from: the Science and Technology Facilities Council and UK Research and Innovation (grants ST/X001016/1 & MR/T040726/1); the Italian PRIN-MUR 2020 BEYOND-2p (Prot. 2020AFB3FX) and PRIN MUR 2022 FOSSILS (Prot. 2022JC2Y93); the project ASI-Astrobiologia 2023 MIGLIORA (F83C23000800005); the INAF-GO 2023 fundings PROTO-SKA (C13C23000770005); the INAF Mini-Grants (2022) ``Chemical Origins'' and (2023) TRIESTE (``TRacing the chemIcal hEritage of our originS: from proTostars to planEts'').


Updated on Wed May 08 15:30:50 CEST 2024