5th Astro-COLIBRI multi-messenger astrophysics workshop

12 oct. 2026, 00:00 → 16 oct. 2026, 18:00 Europe/Paris

Amphitheater + Cathedrale+ Offices (Institut Pascal)

Fabian Schussler (IRFU / CEA Paris-Saclay), Patrick Reichherzer (University of Oxford), Ilja Jaroschewski (CEA - IRFU - DPhP), Bernardo Cornejo Avila (CEA IRFU/DPhP), Sofia Bisero (IRFU / CEA Paris-Saclay)

The key objective of this workshop is to discuss and develop a research agenda on interconnecting software tools for real-time multi-messenger astronomy. This international workshop provides a forum for leading scientists and young researchers to foster communication between developers and users covering a large range of expertise in the production and use of software tools that make life easier in the rapidly evolving domain of real-time multi-messenger astronomy.

The workshop will also be a F2F meeting of members of the working group on realtime multi-messenger observations within the ACME project. 

 

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Funding and support from :

 

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lun. 12 octobre

09:00 → 10:00 Arrival at Insitut Pascal

10:00 → 12:30 Introduction: Keynotes

10:00 Welcome

Orateur: Fabian Schüssler (IRFU / CEA Paris-Saclay)

11:00 From ZTF to LSST

Orateur: Igor Andreoni

11:45 The Eric and Wendy Schmidt Observatory System

Orateur: Thomas Wevers (Schmidt Sciences)

12:30 → 14:00 Buffet lunch

14:00 → 15:40 Messengers: Neutrinos + Cosmic Rays

14:00 The KM3NeT transients and alert program

Orateur: Massimiliano Lincetto (CPPM)

14:20 IceCube: alerts and time domain searches

Orateur: Angela Zegarelli (Ruhr Universität Bochum (RUB), Germany)

14:40 NuTS and the EUSO ballon program

Orateur: Claire Guépin (LUPM)

15:00 The Pierre Auger Observatory in ACME: Expansion of Open Data Access and Development of Real-Time Multi-Messenger Alert Capabilities

The Pierre Auger Observatory, the world’s largest extensive air-shower detector array, is optimized for the measurement of ultra-high-energy cosmic rays (UHECRs) and also provides sensitivity to ultra-high-energy neutrinos via detection of neutrino-induced air showers. Since the start of full operations in 2004, the Observatory has delivered key results in UHECR physics, including constraints on the energy spectrum, mass composition, and arrival direction anisotropies, and has become an important component of the multi-messenger astrophysics landscape.

The Observatory is integrated within the Astrophysical Center for Multi-messenger in Europe (ACME), an infrastructure initiative focused on enabling interoperable data access and enhancing coordination between major astroparticle facilities for time-domain and multi-messenger studies.

Within the ACME framework, the Pierre Auger Collaboration is currently expanding its open data strategy by increasing the accessibility of its archival datasets and developing capabilities for near-real-time analysis. In particular, ongoing developments target the implementation of a real-time alert system based on the identification of neutrino-induced and other highly inclined air-shower signatures, with the goal of enabling rapid multi-wavelength and multi-messenger follow-up observations.

This contribution will present the current status of ACME-related activities within the Pierre Auger Observatory, with emphasis on the extension of the public data infrastructure and the development and commissioning of the real-time alert pipeline.

Orateur: Srijan Sehgal (Bergische Universität Wuppertal)

15:20 LVK alert program + IR run update

Orateur: Barbara Patricelli (University of Pisa and INFN - Pisa)

15:40 → 16:00 Coffee break

16:00 → 17:00 Messengers: Gamma Rays

16:00 LHAASO + LACT

Orateur: Min ZHA

16:20 CTAO ToO program and transient handling

Orateur: Tiffany Collins (Universität Potsdam)

16:40 Time domain programs at the ASTRI mini-array

Transient sources such as gamma-ray bursts (GRBs), gravitational-wave (GW) events and their electromagnetic counterparts, high-energy neutrino counterparts, and Galactic transients such as recurrent novae, have attracted increasing attention in gamma-ray astronomy. The detection of these events at energies around and above 1 TeV has provided new insights into hadronic and leptonic emission processes, highlighting the need for refined theoretical models to complement multiwavelength and multimessenger observations. Observations of transient sources in the TeV and multi-TeV energy range constitute a pillar science programs of the ASTRI Mini-Array. Currently being deployed at the Observatorio del Teide, it consists of an array of nine dual-mirror Schwarzschild–Couder Cherenkov telescopes. Featuring an exceptionally wide field of view (~10°), the array is uniquely suited to scan large localization uncertainty regions typical of GW alerts, while its 3-arcminute angular resolution and 10% energy resolution ensure precise morphological and spectral characterization of complex or crowded fields. To maximize scientific return, the ASTRI transient program is driven by a dedicated, fully automated transient handling system designed to rapidly trigger observations upon receiving and selecting external alerts. Currently in its commissioning phase, the first deployed telescopes are already demonstrating the array’s operational readiness and scientific potential.

Orateur: Antonio Stamerra (INAF-OAR and SNS-Pisa)

17:00 → 17:20 Coffee break

17:20 → 18:00 Messengers: Radio

17:20 Fast Radio Bursts

Orateur: Jason Hessels

17:40 Transients and alert programs in the radio domain

Orateur: Lauren Rhodes

18:00 → 18:40 Platforms: ACME

18:00 The European Broker Initiative

Orateur: Marek Kowalski

18:20 BHTOM

Orateur: Lukasz Wyrzykowski

mar. 13 octobre

09:00 → 10:15 Contributed talks

09:00 A real-time photon candidate event stream with AugerPrime data

Implementation of the ultra-high energy photon candidate data stream to AMON using AugerPrime data will benefit from our design of such a data stream, which has been approved by the Pierre Auger Collaboration for the implementation. The design is based on the analysis developed in a PhD thesis by Lukas Zehrer (2021) and supplied by an internal document (GAP2021_012) describing the data stream handling workflow. Using the photon search optimization results, I will develop and apply, in coordination with the Pierre Auger Collaboration, a photon candidate data stream including the Auger Phase II (WCD/SSD/RD) data. The current surface detector (SD) array data file at the Auger data acquisition center in Malargue contains the latest (small amount of) reconstructed SD events and is updated every few minutes. This latency, similar to the one of the existing Auger data stream to AMON (see e.g. "MM Physics with Auger" paper, by Karl-Heinz et al.), is mostly due to the fully calibrated event reconstruction and analysis steps. I will use this SD data file as an input for the ROOT TMVA toolkit for the MVA analysis of the event parameters. Event selection is applied at this step. Since the goal of the proposed photon candidate data stream is to select sub-threshold events, rather loose cuts will be applied. While the analysis training will be done at a computer of the University of Nova Gorica, the classification of the Auger events will take place on the computer in Malargue. The data file, after applying the cuts, will be combined with the MVA file resulting from the training. The MVA creates a new file containing all the results. Events that have been classified in the MVA as photons (for which the MVA variable value > MVA-cut-value) will be selected with a script and written into a photon candidate event list. The format of this output event list (ASCII text, root, FITS, etc.) to be sent to AMON can be changed easily in the future if needed.

Orateur: Anastasia Baluta (University of Nova Gorica)

09:15 Multi-messenger astronomy with the Hybrid Elevated Radio Observatory for Neutrinos (HERON)

The Hybrid Elevated Radio Observatory for Neutrinos, or HERON, is a proposed detector concept for ultrahigh energy (E > 100 PeV) neutrinos. HERON consists of 24 compact phased radio arrays embedded within a larger sparse array of 360 standalone antennas, deployed along the side of a ~100 km mountain range in Argentina. Due to the high elevation observation sites and the long propagation length of radio, HERON achieves a very large instantaneous effective area towards the horizon, as well as a deep sensitivity thanks to phasing. The excellent pointing resolution provided by the sparse array will make HERON well suited for the detection and localization of astrophysical transient events, paving the way for ultra-high-energy neutrino astronomy. As part of the global multi-messenger network, HERON could both exploit real-time alerts from brokers such as Astro-COLIBRI to perform targeted searches and issue neutrino alerts to trigger follow-up observations across complementary observatories. Here, we present the HERON concept and outline a first multi-messenger observational strategy for its operation. We estimate the angular resolution required to associate transient ultra-high-energy neutrino events with their astrophysical sources, based on population models and external alert networks, focusing on candidate source classes such as gamma-ray bursts. We further evaluate the expected number of potential sources within HERON’s instantaneous field of view to inform detector design and optimization.

Orateur: Paul Minodier (Institut d'Astrophysique de Paris)

09:30 RubiCube: searching for counterparts of high-energy neutrino alerts with Rubin

We are working on a framework to search for optical counterparts of high-energy neutrino alerts from IceCube in realtime. We will take a bayesian approach, where we will use photometric classifiers to identify the transient types and evaluate the probability of a source class emitting a neutrino. We believe this will help us identify the most likely counterpart of the neutrino so for ToO observations.

Orateur: Cristobal Zilleruelo (DESY)

09:45 Gravitational wave detectability range informed by external messengers

A rapid estimate of the detectability of gravitational waves (GWs) associated with astronomical transients is essential for optimizing multi-messenger follow-up observations and for understanding the physical origin of the transient. We introduce the Targeted Detectability Range (TDR), a method designed to rapidly evaluate the detection probability of compact binary coalescences under the assumption that they are associated with an external messenger, such as an electromagnetic or neutrino signal. Unlike the standard GW range, which averages over generic source properties, the TDR incorporates prior information inferred from the external observation, including sky position, binary inclination, and physically motivated constraints on the component masses. We compute the TDR for all gamma-ray bursts, both short and long duration, observed during the first three observing runs of the LIGO–Virgo–KAGRA collaboration. Finally, we validate the method through a systematic comparison with the 90% exclusion distances obtained from modelled targeted GW searches. The tool is publicly available online and a short overview of the web interface will be given.

Orateur: Samuele Ronchini (Gran Sasso Science Institute)

10:00 How to turn alerts into forecasts using plasma physics

Orateur: Patrick Reichherzer (University of Oxford)

10:15 → 10:45 Coffee break

10:45 → 12:30 Contributed talks

10:45 First twenty minutes of GRB afterglows in autonomous telescopes

Robotic telescope networks equipped with next-generation automated follow-up pipelines are enabling systematic exploration of gamma-ray burst afterglows during the first 20 minutes after trigger, a regime that has historically remained sparsely sampled. High-cadence optical observations obtained in the earliest post-trigger seconds reveal temporal and spectral features inaccessible to later or lower-cadence measurements, including evidence of a thermally distributed electron population in events such as GRB 250702F and newly identified correlations between spectral and temporal afterglow properties. The rapid transient-detection and photometric analysis techniques developed for these observations may prove applicable to a broader range of fast astrophysical transients.

Orateur: Filip Novotný (Masaryk University)

11:00 Sixteen Months of EP follow-up at Wendelstein Observatory

We followed up on over 40 EP events between October 2024 and February 2026. Based on our observations and in combination with multi-wavelength data, we derive constraints on the energetics of the events.

Orateur: Malte Busmann (University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München)

11:15 A hidden population of long gamma-ray bursts from compact object mergers

Gamma-ray bursts (GRBs) are powerful, brief flashes of gamma-rays produced either by the merger of two compact objects (Type-I) or by the core-collapse of some kind of massive star (Type-II). While short-duration GRBs have traditionally been associated with mergers and long GRBs with collapsars, an increasing number of long-duration events, such as GRB 230307A associated with kilonovae emission, show robust evidence for a compact object merger origin. These discoveries challenge traditional classification schemes and demand new methods to reliably identify GRB progenitors from their prompt emission. In this talk, I will review existing techniques aimed at identifying GRB progenitors from their prompt emission and present a recent work in which we identified a set of distinctive temporal features in the light curve of GRB 230307A. A similar behaviour is observed in other long merger candidates, such as GRB 211211A, whereas it is not observed in any long GRBs associated with a Ic-BL SN. Extending this study to the whole Fermi/GBM catalogue, we identified 9 additional GRBs with unknown redshift, showing a similar behaviour. Using their tracks in the E_{p,i}-E_{iso} plane, we showed that at least two of these GRBs are outliers of the Amati relation for Type-II GRBs, aligning instead with Type-I GRBs, a conclusion that is also supported by their short minimum variability timescales. Finally, I will outline the usefullness of these signatures to promptly identify long Type-I GRBs directly from their light curves and the implications for their multi-wavelength follow-up campaigns.

Orateur: Romain Maccary

11:30 The Upper Limit on Synchrotron Photon Energies in GRBs"

Within the standard synchrotron model, electrons are typically accelerated by shock waves through the Fermi mechanism and subsequently gyrate around magnetic field lines, emitting photons. Nevertheless, a fundamental limit exists regarding the maximum energy an electron can acquire before it is entirely lost to radiation. We explore several models to estimate the Maximum energy radiated by the synchrotron.

Orateur: Jesus Fernando Ramirez Hernandez

11:45 Probing particle acceleration in Gamma-ray Bursts through MeV afterglows

Orateur: Shraddha Mohnani

12:00 A multiwavelength view of a puzzling dragon.

In this contribution, I will present a comprehensive multiwavelength study of SN 2024jlc, a superluminous supernova (SLSN) that exploded on 2024 May 25 at a redshift of z = 0.039. With a peak g-band absolute magnitude of only −19.38 mag, it is among the least luminous SLSNe ever discovered. As one of the nearest SLSNe exploded in recent years, and among the closest ever observed, SN 2024jlc provided a unique opportunity to investigate the diversity of this class through an extensive multiwavelength campaign. Our analysis combines optical and UV photometry and spectroscopy with observations in soft and hard X-rays, as well as high-energy gamma-rays. We investigate the physical mechanisms powering the light curve, constrain the properties of the circumstellar environment, and explore the similarities and differences between SN 2024jlc and stripped-envelope supernovae (SE-SNe). Our results suggest that SN 2024jlc bridges the gap between SLSN-I and broad-light-curve SE-SNe. Its emission can be explained by either ejecta–circumstellar medium interaction or magnetar spin-down, with a significant contribution from radioactive nickel decay. We also report a suggestive 3.6σ hint of gamma-ray emission, representing the most significant evidence for gamma-ray emission from a SLSN since the confirmed detection of SN 2017egm. I will discuss the implications of this result for the powering mechanism of SLSNe and the prospects for future gamma-ray observations of these remarkable transients.

Orateur: Andrea Simongini

12:15 Real-time detection of lfaring states of blazars for an optical-gamma-ray connection

Blazars are among the most violent non-thermal sources in the universe, exhibiting dramatic variability across the electromagnetic spectrum. Yet, a fundamental question remains unanswered: how tightly coupled are their optical and gamma-ray emissions, and what does this tell us about the physical engines powering these objects? In this talk, I will present a multi-year study of optical and gamma-ray correlations in blazars using data from Fermi-LAT and the ZTF optical survey. By developing a similarity metric to quantify cross-band correlations and a robust flare detection algorithm, we find that ~20% of blazars in our sample show >3σ correlation hints with remarkably short or absent time lags, a possible evidence for co-spatial emission. Moreover, we examine the possibility of distinguishing between emission processes from the optical-gamma-ray correlation signature. We implement a real-time flare detection algorithm that achieves 72% purity in identifying gamma-ray flares and 98% in detecting optical low states, when compared with the gamma-ray high states detected following the former algorithm - demonstrating that optical surveys can serve as high-fidelity triggers for high-energy observations. This capability will be timely with the start of the Rubin Observatory, transmitting alerts through Fink. I will present the implementation of this methodology to detect and trigger observations on high or low blazar states in real time, providing a complement to the triggers from Fermi-LAT and, critically, enabling target-of-opportunity observations with the Cherenkov Telescope Array Observatory (CTAO).

Orateur: Julian Hamo (IJCLab)

12:30 → 14:00 Lunch break

14:00 → 15:00 Contributed talks

14:00 CanDIAPL - Enabling Data-Intensive, Multi-Messenger Astronomy at Scale

The Canadian Data-Intensive Astrophysics Platform (CanDIAPL) aims to develop scalable cloud-based computing infrastructure and specialized software frameworks to enable the processing of petabyte-scale datasets generated by next-generation facilities such as the Vera C. Rubin Observatory and Square Kilometre Array (SKA) precursors. This initiative will include Realtime Analysis pipelines to identify and classify time-critical astrophysical events, enabling rapid discovery and follow-up. It will also develop infrastructure for Dynamic Datasets that processes static sky observations across facilities while supporting queries on time-varying data. Ultimately, it will provide a multi-messenger portal that integrates data across the electromagnetic spectrum and from gravitational-wave detectors, accessible through a single interface for researchers. We present here an overview of the project, describing its infrastructure for ingesting and processing alert streams and large scale databases. We highlight the software tools under development and discuss the successful contributions of the team in providing data support to existing radio surveys involving SKA pathfinders. Finally, we welcome input from the astronomy community on potential features and use cases to guide the development of the platform.

Orateur: Ketan Sand (McGill University)

14:15 AstroGenesis: A Domain-Aware Multi-Agent Model for Data-Driven Astrophysics

Orateur: Narek Sahakyan (ICRANet Armenia IO)

14:30 PyLMT: A transient detection pipeline for the 4-m International Liquid Mirror Telescope

The 4m International Liquid Mirror Telescope (ILMT) is India's first optical survey telescope, which uses a spinning mercury mirror as its primary reflector. It is the only operational liquid mirror telescope globally, with a 22.3' FoV and limiting magnitude of g-mag ~22. The ILMT captures ~15 GB of imaging data per night, producing nearly 30 science frames. A key goal is discovering optical transients and variables, which is facilitated by an automated detection pipeline called the PyLMT. The pipeline employs image subtraction to generate difference frames, followed by a CNN-based classifier to distinguish real sources from artefacts in the resulting images. A second CNN classifies real sources based on host morphology, and known asteroids and solar system objects are identified for rejection. In a recent modification to the pipeline, new CNN models for transient detection and classification were trained using the transfer learning technique, employed between images from the Zwicky Transient Facility and the ILMT. Operational since November 2023, the pipeline has identified various transients and variables, including AGNs, asteroids, T Tauri outbursts, RR Lyrae, Eclipsing Binaries, and 22 supernova-like transient candidates. Six of the detected supernova candidates, viz. AT 2023yjc, 2024fxn, 2024zsm, 2024agkc, 2024aifv, and 2024aiha were reported to the transient name server (TNS) as new discoveries.

Orateur: Kumar Pranshu

14:45 A Real-Time Scheduling Framework for Maximizing the Detection Probability of High-Energy Transients with Gamma-Ray Observatories

Real-time follow-up of high-energy transients requires rapid decisions under uncertainty: the source position, temporal evolution, spectrum, and detectability are often only partially constrained when an alert is received. This is particularly challenging for VHE gamma-ray observatories such as H.E.S.S. and CTAO. Existing follow-up strategies often do not fully account for source time evolution, spectral properties, instrument specific constraints, and real-time updates. The proposed framework starts from an incoming alert, such as a GRB, gravitational-wave event, or high-energy neutrino alert, and extracts the relevant event context. It then performs feasibility and visibility filtering, source hypothesis sampling, and evaluates the expected detectability using a machine learning model trained on simulated transient observations. Finally, the pipeline estimates the detection probability for candidate positions within the uncertainty region, ranks them, and uses this ranking to construct an executable follow-up strategy for observatories. This work aims to develop a framework to enhance the detection of gamma-ray transients with CTAO. The successful implementation of this framework promises to provide deeper insights into high-energy astrophysical phenomena and enhance the scientific return from CTAO observations.

Orateur: Yifan Tian (DESY)

15:00 → 16:00 Messengers: Optical

15:00 Las Cumbres Observatory (LCO)

15:20 Wide-field Spectroscopic Telescope (WST)

Unlocking the Dynamic Universe: The Case for WST as a Spectroscopic Time-Domain Machine

The dynamic universe is one of the defining scientific frontiers of the coming decades, yet our ability to fully explore it is fundamentally constrained by a spectroscopic bottleneck that will only deepen in the 2040s. Photometric surveys such as LSST and Gaia, and multi-messenger observatories including gravitational-wave detectors, will deliver unprecedented volumes of transient discoveries, but they can only tell part of the story. Photometric classification remains ambiguous, gravitational-wave localizations are coarse, and neither can unlock the physical information encoded in spectra. Answering the key scientific questions of the 2040s — spanning Solar System bodies and minor planets, stellar formation and evolution, variable and transient events, black hole demographics from stellar-mass to supermassive, AGN activity across cosmic time, and the electromagnetic characterization of gravitational-wave sources — demands a massively multiplexed wide-field spectroscopic facility designed with time-domain operations at its heart. The Wide-Field Spectroscopic Telescope (WST), with its combination of a large collecting area, wide field of view, and massive multiplex capability across both MOS and IFU modes, is uniquely positioned to serve as this facility. A critical component of the WST design is a spectroscopic alert system: one capable of ingesting photometric and multi-messenger alert streams, autonomously classifying and prioritizing targets, triggering alerts when spectroscopic variations are detected across the multi-epoch survey, and delivering science-ready spectra in near real time. Far from being simply a more efficient follow-up machine, WST equipped with such capabilities opens an entirely new observational window. The ability to obtain spectra of large numbers of variable and transient events immediately and without prior photometric selection breaks the classification bias inherent to all current approaches, creating the conditions for discovering entirely new classes of phenomena. Serendipity, in this regime, becomes systematic. In this talk, I will present the time-domain science cases that define the requirements for WST's spectroscopic alert capabilities, and argue that embedding these capabilities into the WST design from the outset is essential to realize its full potential as a transformational facility for ground-based astronomy in the 2040s.

Orateur: Paula Sanchez Saez (ESO)

15:40 Time Domain Telescope (TDT)

16:00 → 16:20 Coffee break

16:20 → 18:00 Platforms

16:20 NMMA

Orateur: Ramodgwendé Weizmann KIENDREBEOGO (CEA-Irfu)

16:40 Redback

17:00 SCIMMA and its role in Time-Domain Astrophysics

Within minutes of a neutron-star merger, a gravitational-wave trigger, a gamma-ray burst, and an optical kilonova surface in separate data streams — and the discovery exists only if those streams can be joined fast enough to point telescopes before the source fades. SCIMMA, the Scalable Cyberinfrastructure for Multi-Messenger Astrophysics, builds and operates that connective layer; its Kafka-based Hopskotch platform already distributes LIGO, Virgo, and KAGRA alerts to follow-up teams worldwide. The scale is about to grow by orders of magnitude. The Schmidt Sciences Observatory System alone brings three facilities online this decade: the all-sky Argus Array on second cadences, the Deep Synoptic Array localizing thousands of fast radio bursts per year, and the Lazuli space telescope responding to targets of opportunity in under four hours. These arrive alongside Rubin's ten million alerts per night, the gravitational-wave and neutrino networks, Euclid's deep imaging, and the Sino-French SVOM's real-time gamma-ray burst triggers. None is useful in isolation; the physics lives in the coincidences between them. I will describe SCIMMA as an end-to-end stack: Hopskotch routes the alerts, HERMES gives people and machines access to the streams, DASH classifies supernova spectra in real time, BLAST characterizes host galaxies, and HEROIC coordinates follow-up across facilities. With the AI methods of the NSF-Simons SkAI Institute and platforms such as Astro-COLIBRI, these tools turn heterogeneous streams into discoveries within seconds. The telescopes of the next decade are being built now; the infrastructure that lets them act as on observatory has to be built alongside them.

Orateur: Gautham Narayan (University of Illinois Urbana-Champaign)

17:20 GCN

17:40 Astrosky Ecosystem + AT Protocol

In this talk, I will present the Authenticated Transfer (AT) Protocol, a recently debuted internet protocol that enables low-latency, decentralized, global data transfer. Although originally intended as a building block for the social web, the AT Protocol has recently been generating interest as a tool for sharing data. I will present our project - The Astrosky Ecosystem - which has been working to benefit astronomers on the AT Protocol, both by enabling discovery of astronomy content online and through investigations of data streaming on the protocol. I will discuss how data can be streamed and provide examples, such as our efforts over the last months to provide an alternative to the NASA GCNS transient stream, or the matadisco project that has been reposting ESA image and data metadata. Finally, I will outline how the protocol could be used to decentralize and streamline how astronomical transients and data are shared.

Orateur: Emily Hunt

18:00 → 18:20 Citizen science + Community

18:00 How can amateur astronomers contribute to follow-up observations?

Orateur: Bernd Christensen

18:20 → 19:00 Astro-COLIBRI

18:20 Astro-COLIBRI: overview + Q&A

19:00 → 20:00 Sciathon: introduction

Président de session: Fabian Schüssler (IRFU / CEA Paris-Saclay)

19:00 → 20:55 Social events: Beer + chips

mer. 14 octobre

09:30 → 12:30 Sciathon

12:30 → 14:00 Lunch

14:00 → 18:00 Sciathon

jeu. 15 octobre

09:30 → 12:30 Sciathon

12:30 → 14:00 Lunch

14:00 → 19:00 Sciathon

19:30 → 22:30 Social events: Dinner

ven. 16 octobre

10:00 → 12:00 Sciathon: Project presentations

12:00 → 12:30 General: Closing

Closing_4thAstro-COLIBRI_workshop.pdf

12:30 → 14:00 Lunch

14:00 → 16:30 Astro-COLIBRI: ACME WP-5 discussions + free brainstorming