Announcements of Upcoming Meetings

When the Neil Gehrels Swift Observatory was launched on November 20, 2004, its prime objective was to chase Gamma-Ray Bursts. Since then, the mission has far exceeded its original scientific goals. Swift discovered the first afterglows and host galaxies of short-hard GRBs, and a growing sample of events from the local Universe to the epoch of reionization, providing arcsecond positions, light curves, and spectra for more than 1,500 events.

Over time, Swift has become an unequalled Target of Opportunity machine for the astronomical community, thanks to a unique combination of sensitive instrumentation and operational flexibility that provides unprecedented observational capabilities: rapid response coupled with multi-wavelength monitoring of any class of transient/variable object.

After almost 20 years of operations, we think it a fitting occasion to revisit Swift's achievements and to put our mission in the context of the rapidly evolving fields of time-domain and multi-messenger astrophysics. Therefore, we are organizing the meeting "Celebrating 20 years of Swift Discoveries", to be held on March 24-28, 2025, in Florence, Italy, at the Firenze Fiera conference center.

Please mark your calendar to save the date!

Please visit our webpage for details, including upcoming deadlines.

Meeting Dates: 2025 Apr 01 - 03

Meeting Location: Virtual

Registration Deadline: TBA

Jointly with our ESA partners, we will be holding a 3-day virtual data analysis workshop on April 1-3 2025. It will focus on the basics of XMM data analysis with pySAS in the python environment, in the cloud: data processing and storage will be handled remotely via SciServer.

More information, including how to register, can be found here.

Meeting Dates: 2025 Apr 01 - 04

Meeting Location: Padova, Italy

Abstract submission and Registration opens: 2024 Oct 21

Abstract submission closes: 2024 Dec 15

Abstract selection: 2025 Feb 1

Registration closes: 2025 Mar 1

A conference in honour of Enrico Cappellaro, Massimo Della Valle, Laura Greggio, Massimo Turatto

We are delighted to announce the conference: "An extraordinary journey into the Transient Sky: from restless progenitor stars to explosive multi-messenger signals. A conference in honour of Enrico Cappellaro, Massimo Della Valle, Laura Greggio and Massimo Turatto", which will be held from 1st to 4th April 2025, in Padua (Italy).

Supernovae play a key role in various issues in modern astronomy and cosmology. Current surveys have given an enormous boost to the study of transients and supernovae in particular, and it is essential to discuss the state-of-the-art before entering a golden age of the study of the transient Universe. Thanks to the synoptic surveys that will monitor every night the entire visible sky, from optical to radio, and the new-generation instrumentation that will make it possible to observe all the messengers associated with supernova explosions, from photons to neutrinos, from high-energy particles to gravitational waves, it will finally be possible to have both a statistically significant sample of events and a very detailed overview of individual events.

The study of supernovae in the Italian scientific community began in the 1960s with the work of Leonida Rosino and Roberto Barbon and subsequently received a great impulse thanks to Enrico Cappellaro, Massimo Della Valle, Laura Greggio and Massimo Turatto, who studied in Padua in the same years. With this international conference, we intend to celebrate their retirement by recalling their important contribution to the study of supernovae and discussing the still open challenges that we are ready to take up.

Reviewing the trajectory of our honorees, we will touch on topics such as the progenitors of supernovae, the search for supernovae and their rates, the supernova class zoo, supernovae in connection with gamma-ray bursts, and supernova observations in the age of multi-messenger Astronomy.

For additional questions, please see the conference website.

Meeting Dates: 2025 Apr 07 - 11

Meeting Location: Oxford, UK

Abstract submission opens: 2024 October 18

Abstract submission closes: 2024 December 20

Registration closes: 2025 Mar 1

The unparalleled near-infrared capabilities of the James Webb Space Telescope (JWST) allow us to study distant galaxies in remarkable detail. This has ushered in a new era of galaxy evolution studies. With new knowledge of the properties of the stars, gas and dust that make up these early galaxies, we can now start to gain insights into the physical processes driving the assembly of the earliest galaxies, and how they evolve into their lower redshift descendants.

This conference will be an opportunity to highlight recent observational and theoretical results shedding new light on the detailed properties of the stellar populations and interstellar medium (ISM) of galaxies through the early phases of cosmic history. It will also serve as a forum for discussing how new JWST results are transforming our understanding of the formation and evolution of galaxies from early times through to the present day.

Scientific Focus:

Nature of stellar populations in distant galaxies
Properties of the interstellar medium across redshifts
Chemical enrichment and build-up of dust across cosmic time
Spatially resolved studies of galaxies and their environments
Impact of galaxies on cosmic reionization
How can simulations and theory help interpret the latest observations
Feedback and regulating galaxy growth

SOC:

Rebecca Bowler (Manchester); Andy Bunker (Oxford, co-chair); Alex Cameron (Oxford, co-chair); Emma Curtis-Lake (Hertfordshire); Richard Ellis (UCL); Laura Pentericci (INAF-Rome); Aayush Saxena (Oxford, co-chair); Stephen Wilkins (Sussex)

LOC:

Kit Boyett; Andy Bunker; Alex Cameron; Leanne O'Donnell; Gareth Jones; Aayush Saxena

For additional questions, please see the conference website.

Meeting Dates: 2025 Apr 07 - 11

Meeting Location: L'Aquila, Italy

Application Deadline: 2025 Feb 28

The academy focuses on state-of-the-art X-ray and Gamma polarimetry and hosts many experts in the field. The program comprises morning lectures by world-renowned scientists offering an overview of experimental techniques, theoretical aspects, and possible astrophysical observations with current and future mission opportunities. Participants will engage in hands-on exercises emphasizing methodologies, including dedicated sessions to help attendees get acquainted with IXPE data and analyses.

The target audience is PhD students and postdoctoral researchers working on X-ray and Gamma polarimetry or entering the field.

Participants are invited to engage in discussions actively and may have the opportunity to present their research during dedicated poster sessions of the academy.

Registration for the academy is free. Accommodation, travel, and other expenses have to be covered by the participants.

A limited number of grants will be awarded to the most deserving students to cover full expenses, including accommodation and travel.

Application Requirements:

Curriculum Vitae (CV)
Motivational Letter (up to 500 words) detailing your interest in X-ray polarimetry and how the FiXP Academy will benefit your research
Letter of Recommendation from your academic supervisor or professional mentor

Confirmed Speakers and Affiliations:

Marica Branchesi - GSSI; Fiamma Capitanio - INAF/IAPS; Enrico Costa - INAF/IAPS; Casey T. DeRoo - Iowa University; Ettore Del Monte - INAF/IAPS; Alessandro di Giovanni - GSSI; Sergio Fabiani - INAF/IAPS; Riccardo Ferrazzoli - INAF/IAPS; Giorgio Galanti - INAF/IASF; Giancarlo Ghirlanda - INAF/OAB; Herman Marshall - MIT; Giorgio Matt - Università Roma Tre; Fabio Muleri - INAF/IAPS; Mark Pearce - KTH; Nicole Rodriguez Cavero - WashU; Paolo Soffitta - INAF/IAPS; John Tomsick - UC Berkeley;

A detailed list of invited speakers and the full program schedule will be published soon along with the school website.

For additional questions, please see the conference website.

Meeting Dates: 2025 May 14 - 16

Meeting Location: Annapolis, MD, USA

Registration Deadline: TBA

The Advanced X-ray Imaging Satellite (AXIS) will bring X-ray astronomy back to the forefront of modern mainstream astrophysics, working alongside other major facilities of the 2030s (e.g., JWST, Roman, Rubin, ngVLA, LISA) to address some of the most important questions identified by the Astro2020 Decadal Survey. With a single instrument design, AXIS will offer superb arcsecond-resolution and high-sensitivity imaging in the 0.3—10 keV band. AXIS is an excellent facility for transient science, with a two-hour response time to alerts and onboard rapid transient detection.

The AXIS Team will be hosting an AXIS Community Science Conference at The Graduate Hotel, Annapolis, MD. The purpose of the conference is to discuss the major topics driving X-ray astronomy today and the scientific opportunities presented by AXIS in the 2030s. Topics of discussion include:

Seeding and growth of supermassive black holes
Stellar and AGN feedback on galaxy and cluster scales
Stellar activity and the influence on exoplanets
Compact objects and stellar remnants
X-ray transients and multi-messenger landscape of the 2030s
Astrophysical constraints on fundamental physics
Synergies of facilities and opportunities in the 2030s

For additional questions, please see the workshop website.

Meeting Dates: 2025 May 19 - 22

Meeting Location: Baltimore, MD, USA

Abstract Deadline (for contributed talks): 2025 Apr 11

Registration Opens: 2025 ~ Apr 4

Registration Deadline: 2025 ~Apr 25

Abstract Deadline (for posters): 2025 May 7

This conference will celebrate 25 years since the mission's first light in early 2000. Conference topics will cover the wide breadth of XMM science, including but not limited to:

Time domain science
Exoplanet habitability and stellar science
Active galactic nuclei, starburst, and outflows
Clusters and groups of galaxies
Supernova remnants
Solar System science
X-ray binaries, compact objects, and ultra-luminous X-ray sources

Additionally, there will be sessions devoted to the history of XMM-Newton, its synergy with current and future multi-wavelength missions, and its role as a pathfinder for future missions such as NewAthena and AXIS.

Important Note for NASA Civil Servants: Attendees planning to participate in this NASA-sponsored domestic event must register in NCTS by COB March 14, 2025 (NCTS # 51864-25).

Information including registration and hotel room blocks will be updated in the coming weeks. Additionally, if you'd like to be notified directly when registration opens, please register your interest here

This conference will provide an opportunity for the X-ray community to come together and celebrate the many exciting discoveries made by, and yet to come from, one of our flagship missions. We look forward to seeing you there!

Please visit the webpage for details, including upcoming deadlines.

Meeting Dates: 2025 May 19 - 23

Meeting Location: Lowell, MA, USA

Abstract Deadline (for contributed talks): 2025 Apr 11

Registration Opens: 2025 ~ Apr 4

Registration Deadline: 2025 ~Apr 25

Abstract Deadline (for posters): 2025 May 7

Join experts from the Chandra X-ray Center and UMass Lowell for an engaging, hands-on workshop exploring the Chandra X-ray Observatory, X-ray astronomy, and data analysis. This week-long event features science talks, presentations, and practical sessions using real X-ray data — designe for undergraduates and graduate students, as well as early-career scientists in astronomy, physics, and other STEM fields.

Members of the Chandra X-ray Center, CfA and MIT, will join the staff at the University of Massachusetts Lowell for a week long workshop focused on Chandra data analysis. The workshop will include presentations, science talks, and ample time for hands-on learning.

The final program will be tailored to the interests of the attendees. Topics may include:

Introduction to Chandra and CIAO
Spectral analysis

Low resolution CCD spectra
High resolution grating spectra

Spatial analysis

Source Detection
Extended sources

Timing analysis
Sherpa
CIAO in Python
Calibration topics
Statistics
Using SAOImageDS9
Using the Chandra Source Catalog and TGCat

Topics in AI/ML

Registration must be complete by 25 April 2025. Registration is limited to 30 participants. The workshop is open to everyone; however, priority will be given to U. Mass. Lowell students. Registrants will be notified by 30 April 2025 if they have been accepted into the program.

Final arrangements are in progress, but we anticipate that accommodations and meals will be provided at little to no cost for all participants.

Please visit the webpage for details, including upcoming deadlines.

Meeting Dates: 2025 Jun 09 - 13

Meeting Location: Naples, Italy

The aim of this international conference is to bring together observers and theorists to discuss the formation and cosmic evolution of the most massive galaxies in the Universe, focusing on their mass and luminous structure, stellar populations, and the environments in which they live. The most massive M* > 10¹¹ and oldest galaxies account for more than half of the total stellar mass in the local Universe. Their formation and evolution still represent an open contentious question in present-day astrophysics and cosmology. Recent observations have revealed the presence of massive quiescent galaxies even in the first cosmic epochs (out to z>4), representing a challenge for galaxy formation models: it is unclear how they became so massive over such short timescales, how their stellar metallicity grew so fast to solar or supersolar values and, finally, what quenched these objects so quickly and efficiently.

The main aim of this symposium is twofold: Review results from the latest observations of massive quiescent galaxies in the Universe, from high-z to z~0; then, critically analyze to what extent state-of-the-art theoretical models of galaxy formation and evolution can reproduce observations. Key Topics

Physical processes driving the early phases of massive galaxies formation
Metal enrichment, abundances, star formation and the ISM in massive galaxies
Stellar population properties of massive galaxies
The stellar Initial Mass Function in massive galaxies
Influence of internal and external physical processes, and of environment on the evolution of massive galaxies
The co-evolution between black holes and hosting galaxies
Kinematics and dark matter content in massive galaxies, 3D structure of DM halos

Scientific Organising Committee (SOC):

Felipe Barrientos (Universidad Catolica di Chile); Davide Bevacqua (INAF IT, PhD); Paula Coelho (University of São Paulo, Brazil); Roberto de Propris (FINCA, Turku, FI & BIUST Botswana); Anna Ferré-Mateu (IAC, Tenerife, ES); Ignacio Ferreras (IAC, Tenerife, ES); Karl Glazebrook (Swinburne University, AUS); Johanna Hartke (FINCA, Turku, FI); Michaela Hirschmann (CH); Mariska Kriek (NL) Wang Lan (Academy of Sciences, China); Michalina Maksymowicz-Maciata (Bristol UK, PhD); Danilo Marchesini (USA)Nicola Napolitano (Univ. Federico II, IT); Anna Pasquali (Universität Heidelberg, DE); Rosalind Skelton (South Africa Astronomical Observatory); Paolo Saracco (Chair; INAF, Brera); Chiara Spiniello (Co-chair; Oxford University, UK); Masayuki Tanaka (National Astronomical Observatory of Japan); Daniel Thomas (Univerasity of Portsmouth, UK)

Local Organising Committee (LOC):

Gabriella De Lucia (INAF); Fabio Fontanot (INAF); Anna Gallazzi (INAF); Adriana Gargiulo (INAF); Francesco La Barbera (INAF); Amata Mercurio (Univ. Fisciano); Nicola Napolitano (Univ. Federico II); Maurizio Paolillo (Univ. Federico II); Paolo Saracco (INAF); Crescenzo Tortora (INAF); Stefano Zibetti (INAF)

The symposium will take place in Naples, a beautiful and attractive city by the sea in the south of Italy. Naples is home to the Capodimonte Astronomical Observatory, belonging to the National Institute of Astrophysics (INAF), and the Federico II University which hosts a department of Physics and Astrophysics. The city is easily reachable, being served by an international airport and a fast railway.

For additional questions, please see the conference website.

Meeting Dates: 2025 Jun 16 - 19

Meeting Location: Madrid, Spain

Abstract and Registration Opens: 2025 Jan 13

Abstract Submission Deadline: 2025 Feb 28

Accepted Abstract Notices: 2025 March

Registration closes: 2025 May 2

A series of extreme-variability phenomena associated with supermassive black holes (SMBHs) in galactic nuclei are being revealed with increasing frequency in recent years thanks to enhanced survey capabilities across the electromagnetic spectrum. The observation of these extreme phenomena has opened the way to the study of the physics of SMBHs in real time - something that, until a decade ago, was exclusively associated with stellar-mass black holes. As the baseline of follow-up observations extends, repeating events have gathered more and more observational evidence in the recent past.

Understanding the diverse phenomena presented by multi-wavelength observations - a non-exhaustive list of which is given below - is challenging and competing interpretations are being actively debated. With this workshop, we aim at providing an environment where observers and theorists can gather together to investigate whether a detailed look at individual sources, and the broader characteristics of source samples, can reveal common threads which will enable us to advance our understanding of the dynamic and complex environments which exist in galactic nuclei.

Topics:

Full and partial Tidal Disruption Events
Multi-wavelength emission and outflows in nuclear transients
X-ray Quasi-Periodic Eruptions in galactic nuclei
Quasi-Periodic Oscillations from supermassive black holes
Changing-look and changing-state Active Galactic Nuclei
Supermassive black hole binaries, Extreme Mass-Ratio Inspirals, Gravitational Waves
Theory and numerical simulations

SOC: Riccardo Arcodia, Alessia Franchini, Suvi Gezari, Erin Kara, Itai Linial, Giovanni Miniutti (co-chair), Richard Saxton (co-chair), Norbert Schartel, Natalie Webb

LOC: Lucia Ballo, Ignacio de la Calle, Jacobo Ebrero, Margherita Giustini (co-chair), Aitor Ibarra Ibaibarriaga, Jose López Miralles, Erwan Quintin (co-chair), Juan Pablo Vega González

Further information: The workshop is intended to be in-person to ease productive discussion and will lead to the publication of conference proceedings.

For additional questions, please see the workshop website.

Meeting Dates: 2025 Jun 16 - 20

Meeting Location: Sexten, Italy

Abstract submission and Registration opening: 2024 Nov 27

Registration-only opening: 2025 Jan 24

Registration-only closing: 2025 Apr 30

The formation and evolution of galaxies is a complex sequence of physical processes leading to the sources we observe across different epochs of the Universe. Among these processes, mergers play a crucial role. Whether simple accretion events or minor and major mergers, these interactions can dramatically influence the nature, shape, and physical properties of the resulting galaxies, making them vastly different from their progenitors.

Mergers can change the morphology of galaxies, for example, transforming a spiral galaxy into an elliptical galaxy, and altering the distribution of stars and gas within them. Another consequence is that these violent interactions can compress gas clouds, triggering intense starburst periods and enriching the remnant with new stars. Moreover, gas funnelled to the galaxy's core during mergers can fuel the central engine, igniting an active galactic nucleus (AGN), which can significantly influence galaxy evolution by either inhibiting or promoting star formation. Lastly, merger events affect the distribution of dark matter, reorganising the surrounding dark matter halo and modifying their internal dynamics and rotation.

In the beautiful setting of the Dolomites where Haus Sexten is located, we will discuss how galaxies continuously evolve through these processes, contributing to the diversity of shapes and characteristics observed in the Universe over cosmic time. In the following, we list some fundamental questions we aim to address during the conference.

What is our current understanding of how mergers change the morphology of the galaxies we observe in the present-day Universe?
To what extent do mergers contribute to new star formation and alter the chemical distribution in galaxies at different epochs?
How is the supermassive black hole (SMBH) of galaxies affected by accretion events and mergers? Furthermore, how do mergers influence SMBH-galaxy co-evolution and establish the observed scaling relations?
How does our ability to determine the rate of galaxy mergers across different epochs and environments impact our understanding of cosmic structure formation?
What role do mergers play in the evolution of the size, velocity dispersion and other physical properties of galaxies?
Can our current approaches to studying galaxy evolution, whether they are physically motivated high-resolution cosmological simulation, semi-analytical models, or semi-empirical methods, faithfully reproduce the assembly history of galaxies at different epochs?
What are the most plausible scenarios for assembling the massive galaxies that telescopes such as JWST are observing early in the history of the Universe?
How can diverse mergers be most effectively identified across various cosmic epochs through machine learning, visual classification, or morphological statistics?

Invited Speakers (in alphabetic order):

Mariangela Bernardi (University of Pennsylvania); Caitlin Casey (TBC, University of California Santa Barbara); Christopher Conselice (University of Manchester); Victor Debattista (TBC, University of Central Lancashire); Helena Domínguez Sánchez (Instituto de Física de Cantabria); Sara Ellison (University of Victoria); Anna Ferré-Mateu (Instituto de Astrofísica de Canarias); Marc Huertas-Company (Instituto de Astrofísica de Canarias); Peter Johansson (University of Helsinki); Jennifer Lotz (Space Telescope Science Institute); Rhea-Silvia Remus (Ludwig Maximilian University of Munich); Katherine Suess (University of Colorado Boulder)

Scientific Organising Committee (in alphabetic order): Carlo Cannarozzo (chair, New York University Abu Dhabi); Benjamin Davis (New York University Abu Dhabi); Thales Gutcke (University of Hawaii); Susan Kassin (Space Telescope Science Institute); Claudia Lagos (University of Western Australia); Andrea Macciò (New York University Abu Dhabi); Mireia Montes (Instituto de Ciencias del Espacio); Carlo Nipoti (Università di Bologna); Salvatore Quai (Università di Bologna); Aldo Rodriguez-Puebla (Universidad Nacional Autónoma de México)

Local Organising Committee (in alphabetic order):

Bianca Arkeen, Carlo Cannarozzo, Benjamin Davis, Gabriella Deconi, Andrea Macciò, Mandy Mudhar.

For any questions regarding the conference, please visit the conference website or send an email to carlo[DOT]cannarozzo[AT]nyu[DOT]edu with the subject line "Dancing in the Dark - Question" .

Meeting Dates: 2025 Jun 23 - 27

Meeting Location: EAS 2025 Cork, Ireland

Globular clusters provide a powerful tool for decoding the Milky Way?s history, offering a direct link between large-scale galactic structures and the life cycles of individual stars. Their chemical and dynamical properties preserve vital clues about the formation and evolution of the Galaxy, shedding light on the processes that have shaped its structure over billions of years. As some of the oldest and most massive stellar systems, globular clusters serve as stellar fossils, preserving crucial insights into the Milky Way early epochs. Many stars in the Galactic halo are thought to have originated in globular clusters that dissolved over time, highlighting their significant contribution to the Galaxy's assembly.

Recent discoveries have revealed that globular clusters are far more complex than once thought. It is now widely accepted that multiple stellar populations (MPs) in globular clusters reflect intricate star-formation histories, where second-generation stars, enriched in helium and light elements such as sodium and nitrogen, formed from material processed by the first generation. The discovery of MPs has fundamentally changed our understanding of stellar formation and evolution, uncovering physical processes that occur only in the dense and extreme environments of globular clusters. Understanding their origin and evolution is key to reconstructing the role of globular clusters in shaping the Milky Way and its stellar populations.

This session aims to bring together researchers from various disciplines to discuss the latest advances in the study of globular clusters, focusing on their formation, evolution, and the presence of multiple stellar populations.

The session will explore how observations using techniques such as spectroscopy, photometry, and dynamics, combined with theoretical modeling, can connect scientists from different fields and offer new insights into how globular clusters have shaped the universe we observe today.

Program:

The role of stellar dynamics in cluster evolution
Globular clusters and the Milky Way evolution
Understanding the origin of multiple populations
Synergy between spectroscopy, photometry, and dynamics
Globular clusters and multiple populations in extraGalactic environments Insights from young star clusters
Future prospects and surveys

Scientific organisers:

Giacomo Cordoni (Chair, Australian National University, AUS), Emanuele Dondoglio (co-Chair, INAF-Padova, IT), Amanda Karakas (Monash University, AU), Mattia Libralato (INAF-Padova, IT), Anna Marino (INAF-Padova, IT), Davide Massari (INAF-Bologna, IT), Alessandra Mastrobuono-Battisti (University of Padova, IT), Madeleine McKenzie (Carnegie Observatories, US)

For additional questions, please see the conference website.

Meeting Dates: 2025 Jul 01 - 04

Meeting Location: Keele University, Staffordshire, UK

The study of binary stars is one of the oldest areas of astrophysics. Results from binary stars are fundamental to our understanding of how stars form and evolve, galactic stellar populations, chemical evolution, and the cosmological distance scale. Wide binaries allow us to probe the properties of normal stars, including direct measurements of their masses. Eclipsing binaries are the only stars whose masses and radii can be measured to high precision. Close binaries can be used to study the physics of mass transfer, mass loss, accretion discs and how stars evolve. Binary star evolution is critical to the formation of cataclysmic variables, novae, supernovae, X-ray binaries, millisecond pulsars, gamma-ray bursts and gravitational wave events. Planets are found in binary star systems in both S-type and P-type orbits.

We are now firmly in the space-photometry era, with observations of binary stars available from the WIRE, MOST, BRITE, CoRoT, Kepler, TESS and CHEOPS satellites. In the near future PLATO will offer another leap forward in the quality of photometric data, and binary stars will in turn provide crucial information for the interpretation of the many planetary systems it will find. What legacy of achievements can we attribute to the study of binary systems? What is the current state of this area of astrophysics? What problems are still to be solved? How can we further improve our understanding of normal stars? What new analyses are now possible with Kepler, TESS and CHEOPS data? What more will PLATO allow us to do? How should we prepare? The aim of this conference is to bring together observational and theoretical astrophysicists to critique the past, understand the present, and organise the future of binary star research.

The intended sessions are:

Space photometry
Modelling binary systems
Spectroscopic binaries
Astrometric binaries / Gaia
Pulsations in binaries (observations)
Pulsations in binaries (theory and modelling)
Benchmark binaries
Binaries and planets
Interacting binaries and mergers
Binary formation
Binary evolution
Binary populations
Comparison to theoretical models
Looking forward to PLATO

The current list of invited speakers is:

Poojan Agrawal (Leuven, Belgium); Dominic Bowman (Newcastle, UK); Paul Clark (Cardiff, UK); Dariusz Graczyk (CAMK, Toru&nacute;, Poland); Kelly Hambleton Prša (Villanova, US); Cole Johnston (Surrey, UK); Krzysztof Hełminiak (NCAC, Toru&nacute;, Poland); Pierre Kervella (Paris, France); Nikki Miller (Uppsala, Sweden); Maxwell Moe (Wyoming, US); Andrej Prša (Villanova, US); John Southworth (Keele, UK); Elizabeth Stanway (Warwick, UK); Andrew Tkachenko (Leuven, Belgium)

Scientific Organising Committee (SOC):

John Southworth (Keele University, UK); Conny Aerts (KU Leuven, Belgium) ; Jan Eldridge (University of Auckland, NZ); Kareem El-Badry (California Institute of Technology, US); Pierre Maxted (Keele University, UK); Nikki Miller (University of Uppsala, Sweden)

Local Organising Committee (LOC):

Pierre Maxted (Keele University, UK); John Southworth (Keele University, UK); Barry Smalley (Keele University, UK); Ayush Moharana (Keele University, UK); Steve Overall (Keele University, UK); Lex Griffiths (Keele University, UK)

For additional questions, please see the conference website.

EXCOSM Summer School: Large-scale structure of the Universe: from galaxies to cosmology: 2025 Jul 07 - 11

Meeting Dates: 2025 Jul 14 - 18

Meeting Location: Baltimore, MD

Abstract Opens: 2025 Feb 03

Registration Opens: 2025 Apr 14

Registration Deadline: 2025 Jun 09

The Nancy Grace Roman Space Telescope, planned to launch in late 2026, will be capable of surveying the sky 1000 times faster than the Hubble Space Telescope with similar sensitivity and resolution. A combination of near-infrared imaging and spectroscopic surveys, designed by Roman's community-defined Core Community Surveys and General Astrophysics Survey programs, will generate unique data-sets and large-area maps of the sky that will catalyze scientific discovery across all of astrophysics. Roman's accurate mapping of stars, galaxies, and galaxy clusters will offer the unique ability to map our Universe, both the seen and the unseen.

This conference aims to focus on the intersection of galaxy formation and evolution with dark matter and dark energy. It will explore the novel research that is possible only with large cosmic surveys and simulations and discuss how the community will be able to optimize scientific output with Roman in the future. Topics of discussion will include, but are not limited to, the expected impacts from Roman observations of galaxy clustering, baryon acoustic oscillations, weak lensing, galaxy clusters, supernova cosmology, stellar streams, and dwarf galaxies. The conference will also strive to foster synergies between contemporaneous experiments to Roman, such as Euclid, Rubin's LSST, DESI, and Simons Observatory. The schedule will feature invited talks, contributed talks, posters, discussion panels, and fun social activities.

Attendance: The workshop will be a hybrid event (in-person and virtual). To maximize engagement, in-person attendance is encouraged for all participants, especially speakers.

SOC

Ami Choi (NASA Goddard Space Flight Center; Co-Chair), Javier Sanchez (STScI; Co-Chair), Alexandra Amon (Princeton University), Ori Fox (STScI), Konrad Kuijken (Leiden University), Patricia Larsen (Argonne National Laboratory), Lado Samushia (Kansas State University), Yun Wang (Caltech/IPAC), Yuanyuan Zhang (NOIRLab)

LOC

Leslie Beauchamp (STScI), Annalisa Calamida (STScI), Samantha Hoffmann (STScI), Max Mutchler (STScI), Cristina Oliveira (STScI), Melissa Shahbandeh (STScI), Shemiah Smith (STScI)

Further information:

The workshop is intended to be in-person to ease productive discussion and will lead to the publication of conference proceedings.

For additional questions, please see the workshop website.

Meeting Dates: 2025 Jul 14 - 18

Meeting Location: Glasgow, UK

Abstract Deadline: 2025 Mar 21

Early Registration Deadline: 2025 May 9

Registration Deadline: 2025 Jun 29

The International Conference on General Relativity and Gravitation is organised every three years under the guidance of the International Society on General Relativity and Gravitation. It is the principal international meeting for scientists working in all areas of relativity and gravitation.

The Edoardo Amaldi Conference on Gravitational Waves is organised every two years under the guidance of the Gravitational Wave International Committee. It is the principal international meeting for scientists working in all areas of gravitational-wave science.

In 2025, the 24th International Conference on General Relativity and Gravitation (GR24) and the 16th Edoardo Amaldi Conference on Gravitational Waves (Amaldi16) will be held together as a joint meeting, bringing together experts from across classical and quantum gravity, mathematical and applied relativity, gravitational-wave instrumentation and data-analysis, and multimessenger astronomy.

The GR24-Amaldi Meeting will be held as a primarily in-person event at the Scottish Event Campus, Glasgow. Online resources will be made freely available after the event. Meeting organisation is led by the Institute for Gravitational Research at the University of Glasgow and the Institute of Physics.

For additional questions, please see the conference website.

Meeting Dates: 2025 Jul 28 - 31

Meeting Location: Washington D.C., USA

Abstract Deadline: 2025 Feb 21

Registration Deadline: 2025 Jan 31

We are pleased to announce the inaugural open community conference for NASA's Habitable Worlds Observatory, to be held at the Johns Hopkins Bloomberg Center in Washington, DC, from July 28 - 31, 2025. This milestone event will bring together scientists, engineers, industry and community stakeholders to propel the development of HWO, a mission expected to usher in a new era of astrophysics discovery and address one of humanity's oldest questions "Are we alone?"

The Habitable Worlds Observatory is NASA Astrophysics' next flagship mission, and builds on the heritage of the Hubble, Webb, and Roman Space Telescopes. It will deploy advanced ultraviolet, optical, and infrared technologies to identify potentially habitable worlds and analyze their atmospheres for signs of life. This same technology will empower astronomers to address fundamental, persistent questions in cosmology, galaxy evolution, the origins of elements, and our Solar System's place in the universe.

HWO has made significant progress in the past year, with NASA establishing a dedicated Technology Maturation Project Office at Goddard Space Flight Center, working in close collaboration with the Jet Propulsion Laboratory, Ames Research Center, and Marshall Space Flight Center. This initiative advances critical technologies and science cases, and fosters collaboration across government, academia, and industry. Results of HWO working groups will be showcased together with contributions from the global astronomy and engineering communities.

Topics of interest include, but are not limited to:

Science:

Galaxy Growth: Cosmic Web (Intergalactic & Circumgalactic Medium), Active Galactic Nuclei & Black Holes, Galaxy Evolution
Evolution of the Elements: Stars & Stellar Populations, Star Formation & Interstellar Medium, Cosmic Explosions
Cosmology: Nature of Dark Matter & Dark Energy, Distance Scale, Hubble Tension
Planetary Systems: Formation, Evolution, Architectures, Our Solar System, Exoplanet Demographics
Search for Life: Target Stars & Systems, Biosignatures, Habitability

Technology:

Starlight Suppression: Contrast Technology & Methods
Ultrastable Telescope and Observatory Technology
Ultraviolet, Optical, & Near-Infrared Instrument Technologies: mirror coatings, gratings, detectors, spectroscopic multiplexing technologies
L2 Servicing technology and commercial synergies
Emerging Technologies: photonics, quantum sensing
Artificial Intelligence & Machine Learning for mission development, engineering, science research

Accepted presenters will be invited to contribute to the HWO25 conference proceedings, which will serve as the foundation for the first HWO Community Science Book.

For additional questions, please see the conference website.

JWST Summer School: High Redshift Transients with JWST: 2025 Aug 04 - 15

Meeting Dates: 2025 Aug 04 - 08

Meeting Location: Rio de Janeiro

Registration opens: 2025 Jan 17

Abstract submission Deadline: 2025 May 15

Deadline for Early Registration: 2025 Jun 15

The High Energy Phenomena in Relativistic Outflows (HEPRO) conferences are a series of biennial meetings devoted to the discussion of the most recent theoretical, phenomenological, and observational developments in the field of high-energy phenomena associated with relativistic winds and jets. Previous editions were held in Dublin (2007), Buenos Aires (2009), Barcelona (2011), Heidelberg (2013), La Plata (2015), Moscow (2017), Barcelona (2019), and Paris (2023).

The HEPRO IX edition will be held in Rio de Janeiro, Brazil, from August 4 to August 8, 2025. Some specific topics covered during the meeting will be gamma-ray and neutrino production in relativistic outflows, multi-wavelength jet emission, formation and propagation of relativistic jets on different scales, PeVatron sources, and particle acceleration in various relativistic contexts.

The sessions will be held in "Casa de Rui Barbosa" in Botafogo, Rio de Janeiro, Brazil.

For additional questions, please see the conference website.

Meeting Dates: 2025 Aug 24 - 30

Meeting Location: Lijiang, China

Binary stars lie at the heart of many key astrophysical phenomena. Various explosive cosmic events result from binary stars, as do close double black holes/neutron stars/white dwarfs, type Ia supernovae, X-ray binaries, millisecond pulsars etc. Relying on existing large scientific facilities, classical optical, radio and X-ray observations are discovering increasingly large numbers of such binary stars. A decade ago, the ground-based LIGO/Virgo detected the merging of two stellar-mass binary black holes, opening a new window in gravitational wave astronomy. In the future, with the support of next-generation astronomical instruments, we shall discover many more binary-related celestial objects. Against this backdrop, we convene this conference, inviting all international observers and theoreticians in the field of stellar science to participate in and exchange recent progress related to binary stars and to look forward to future collaboration and development of new directions for research.

Topics:

Binary star interactions: from mass transfer to common envelope evolution.
Supernovae: from progenitor modeling to explosion simulation.
Gravitational wave sources: from double black holes to white dwarfs.
Exotic stars: X-ray binaries, binary pulsars, luminous red novae, hot subdwarfs, cataclysmic variables, symbiotic stars, etc.
Binary population synthesis studies on binary objects.
Binary star observations from large facilities: Gaia, TESS, LAMOST, JWST, FAST, etc.

Scientific Organizing Committee:

Floor Broekgaarden; Xuefei Chen; Hongwei Ge (Chair); Zhanwen Han; Natalia Ivanova; Christopher Adam Tout

Local Organizing Committee:

Hailiang Chen; Hongwei Ge; Yanjun Guo; Wenyan Ji (Secretary); Shi Jia; Dengkai Jiang; Jiangdan Li; Jiao Li; Zhenwei Li; Zhengwei Liu (Chair); Xiangcun Meng; Bo Wang; Jianping Xiong; Lifu Zhang

For additional questions, please see the conference website.

Meeting Dates: 2025 Aug 25 - 29

Meeting Location: Nagoya, Japan

Registration opens: 2025 Jan 17

Abstract submission Opens: 2025 Mar 18 (link to submission page)

Abstract submission Deadline: 2025 May 11

Deadline Opens: 2025 Apr 15 (link to registration page)

Deadline for Early Registration: 2025 Jul 25

Understanding the evolution of the interstellar medium (ISM) is essential for comprehending star formation and galaxy evolution. Galaxies are composed primarily of stars and the ISM, and the physical properties of the ISM—such as density, temperature, and kinematics—serve as the initial conditions for star formation, making them fundamental to understanding galactic evolution. The ISM encompasses various physical states, from hydrogen gas (atomic and molecular) to hot plasma and high-energy particles. These states span several orders of magnitude in density (10^-4—10³ cm^-3), temperature (10^–1 billions of Kelvins), and spatial scale (parsecs to hundreds of kiloparsecs), each governed by distinct radiative processes and interacting dynamically with one another. Therefore, it is crucial to investigate the multi-phase structure of the ISM across various wavelengths. This includes cold gas, which is the bulk of the ISM mass, diffuse hot plasma, and high-energy processes that dominate volume and energy. A comprehensive understanding requires a multi-wavelength approach, capturing the ISM's evolution over its wide temperature and density range. However, such multi-faceted studies remain challenging due to the diverse observational techniques and limitations across wavelengths. This symposium invites observational and theoretical researchers interested in the evolution of the ISM through multi-wavelength analyses. It will also explore the prospects of employing next-generation telescopes to advance multi-wavelength studies and aim to foster new collaborations.

While the following topics are expected to be central themes, we strongly encourage contributions on any related subjects to foster broad and inclusive discussions.

Impact of Galaxy Interactions on the ISM and Star Formation (Large-Scale Impact)

How do large-scale gas flows triggered by galaxy interactions drive star formation?
What are the observable signatures in gases and dust?
How do tidal interactions and mergers heat the interstellar gas?

The Impact of Stellar Feedback on the ISM (Medium-Scale Impact)

How does gas heating and ionization occur due to stellar radiation?
How do cosmic rays contribute to ISM ionization and heating?
What is the impact on subsequent star formation?

Shock-Cloud Interactions and Cosmic Ray Acceleration (Small-Scale Impact)

How do shock-cloud interactions induce turbulence?
What gamma-ray signatures originate from high-energy interactions, such as particle acceleration and cosmic-ray interactions with gas?
How do shocks contribute to cosmic ray acceleration and impact the surrounding medium?

Scientific Organizing Committee:

Aya Bamba (The University of Tokyo); Yasuo Fukui (Nagoya University); Kathryn Kreckel (Heidelberg Unviersity); Knox Long (Space Telescope Science Institute); Martin Pohl (Deutsches Elektronen-Synchrotron DESY); Manami Sasaki (Friedrich-Alexander University Erlangen-Nürnberg); Kengo Tachihara (Nagoya University); Kisetsu Tsuge (Gifu University; SOC/LOC chair) 　

For additional questions, please see the conference website.

Meeting Dates: 2025 Sep 01 - 05

Meeting Location: Matera (Italy)

Observations of the local and high-z Universe confirm that star formation is an inherently clumpy and clustered process and, as a consequence, the physical properties of star clusters are expected to be intimately linked with those of their hosts. In particular, the long-lived massive star clusters can be used to trace galaxy assembly and the gas properties at the time of their formation, and they may be one of the primary sources of reionization of the Universe. This field is currently undergoing a revolutionizing phase. Large surveys carried out with ground and space based telescopes (such as Gaia, HST, Euclid, ALMA, ESO/VLT) have enabled unprecedented photometric and spectroscopic studies in the Local Universe and the JWST's access to rest-frame optical wavelengths at z>3 along with the magnification power of gravitational lensing are opening a new era in the study of the star-forming modes well within the reionization epoch allowing us to directly probe star cluster formation and constrain unprecedented/unexpectedly dense stellar systems as possible sites of GC formation.

The formation and evolution of star clusters is inherently a multi-physics and multi-scale problem, involving star formation and feedback, galaxy formation and evolution, N-body dynamics, stellar and binary evolution. As a consequence, the broad range of interconnected issues concerning the study of star clusters and their host galaxies can be addressed only with an interdisciplinary approach.

In this exciting and rapidly changing context, we aim at bringing together observers and theorists from both the local and high-z Universe communities. The goal is to inspire discussions and exchange ideas about how to perform a transformative leap in the field, build a comprehensive picture of star cluster formation and evolution, explore the link between old massive, young star clusters and high-z proto-globular clusters, their connection to galaxy formation and their potential role in the reionization of the Universe. Focus will be given to how efficiently leverage available observations spanning different spatial, temporal and physical scales, along with those that will be soon on-line thanks to the several upcoming new giant facilities (such as E-ELT, Vera Rubin Telescope, Nancy Grace Roman Space Telescope, GMT), and the new generations of dynamical and cosmological hydro-dynamical simulations at spatial scales suitable to resolve stellar clusters.

Confirmed Invited Speakers:

Angela Adamo (Stockholm University); Oscar Gonzalez (STFC UKRI); Sebastian Kamann (Liverpool LJMU); Natalia Lahén (Max Planck Institute); Hui Li (Tsinghua University); Matteo Messa (INAF Bologna); Massimo Ricotti (Maryland University); Elena Sabbi (NOIRLab)

Scientific Organizing Committee:

Emanuele Dalessandro (INAF Bologna; co-Chair); Alison Sills (McMaster University; co-Chair); Mario Cadelano (University of Bologna); Michela Mapelli (Heidelberg University); Florent Renaud (Observatoire Astronomique de Strasbourg); Eros Vanzella (INAF Bologna); Enrico Vesperini (Indiana University)

Local Organizing Committee:

Emanuele Dalessandro (INAF Bologna); Greta Ettorre (INAF Bologna); Alessandro della Croce (INAF Bologna); Mario Cadelano (University of Bologna); Cristiano Fanelli (INAF Bologna); Silvia Leanza (University of Bologna); Raffaele Pascale (INAF Bologna)

For additional questions, please see the conference website.

Meeting Dates: 2025 Sep 08 - 12

Meeting Location: Cambridge, England

Abstract Deadline: 2025 Feb (TBA)

Registration Deadline: 2025 Jun (TBA)

The decisive role of massive black holes in galaxy evolution is implied through scaling relations with galaxy properties and observations of ubiquitous nuclear outflows across a wide redshift range. In simulations, accretion onto black holes is a key ingredient in matching observed galaxy mass functions. Recently, the surprisingly high abundance of AGN at z>4 revealed through JWST observations has sparked renewed interest in massive black hole seeding and growth during the first billion years from both observational and theoretical sides.

The conference aims at bringing together researchers studying massive black holes across and beyond the electromagnetic spectrum, as well as theorists and simulators to discuss recent advances in the research of massive black hole growth, evolution, demographics, and impact across cosmic time.

We will focus on the following key themes:

Observational indicators of massive black holes across cosmic time
Observational constraints on black hole masses through a variety of techniques and across wavelengths (including stellar dynamics, reverberation mapping, single-epoch virial relations, scaling relations, and gravitational waves)
Black hole demographics as a function of redshift through simulationsConstraints on massive black hole formation (including seeding models) and growth pathways through theory, and in combination with observations
Impact of black holes on galaxy evolution evidenced through feedback and scaling relations in observations and simulations

Scientific Organising Committee:

Xiaohui Fan (University of Arizona); Jenny Greene (Princeton University); Sophie Koudmani (Herts/KICC); Roberto Maiolino (KICC, co-chair); Chris Moore (KICC/IoA/DAMPT); Priyamvada Natarajan (Yale University); Debora Sijacki (KICC); Hannah &Ueml;bler (MPE, co-chair)

Local Organising Committee:

Sophie Koudmani(Co-chair); Jan Scholtz(Co-chair); Leah Bigwood; Steve Brereton(admin); Stephanie Buttigieg; Sophia Geris; Lucy Ivey; Xihan Ji; Ignas Juodžbalis; Roberto Maiolino; Eun-jin Shin; Debora Sijacki; Alison Wilson (admin)

For additional questions, please see the conference website.

Meeting Dates: 2025 Sep 22 - 26

Meeting Location: Tomakomai, Hokkaido, Japan

A working model for outbursts in dwarf novae was proposed by Prof. Yoji Osaki in 1974, which is currently known as the disk instability model. We are celebrating the 50th anniversary of the invention of this model by organizing an international workshop.

This workshop aims to review the history of the development of the disk instability model, understand the essential physics, and share the latest research results with participants.

We hope that this workshop will help young researchers set the direction for future research. Also, this workshop will provide smooth communication between senior leading researchers and young researchers & students.

For additional questions, please see the conference website.

Meeting Dates: 2025 Oct 06 - 10

Meeting Location: Olbia, Italy

Abstract submission and registration opening: 2025 Feb 28

Abstract submission deadline: 2025 Apr 30

Program announcement: 2025 Jun 7

Registration Deadline: 2025 Jul 15

MMC2025: Multi-phase, Multi-temperature, and Complex. How Feedback Shapes the Nature of the CGM, Halo Gas, and Galaxies from Galaxy Groups to Clusters

The mechanisms driving galaxy evolution — AGN and stellar feedback — remain central to our understanding of how baryons are redistributed in collapsed structures. Despite significant progress, our theoretical models continue to diverge, particularly when predicting the gas content and star formation activity in low-mass halos, the circum-galactic medium (CGM), and the evolution of central galaxies across different environments. Feedback processes, in particular, play a critical role, with varying effects depending on the scale of the system, from individual galaxies in low-mass halos to massive galaxy clusters.

MMC2025 will bring together experts to address these challenges, focusing on the latest observational results and state-of-the-art hydrodynamic simulations. We will explore the multi-phase, multi-temperature nature of the CGM and its complex interplay with AGN feedback, gas inflow, and star formation across diverse environments —from bright clusters at high redshifts to low-mass halos. The workshop will highlight key observational datasets, including X-ray, SZ, and IFU data, as well as advancements in radio and submillimeter observations, offering fresh insights into the gas and feedback processes shaping galaxies.

Join us in Olbia, Italy, to discuss how these feedback mechanisms drive the evolution of galaxies and clusters, with a special focus on the role of AGN feedback in low-mass halos and its effect on gas content and star formation. MMC2025 will be a unique opportunity to combine cutting-edge observational data with theoretical models to advance our understanding of large-scale structure and galaxy formation and evolution.

We look forward to your participation in this exciting scientific event!

SOC:

Paola Popesso (chair); Ilaria Marini; Marcella Brusa; Dylan Nelson; Klaus Dolag; Paolo Tozzi; Stefano Ettori; Esra Bulbul; Veronica Biffi; Veronica Strazzullo; Eleonora Sani; Silvia Bonoli; Lorenzo Lovisari; Celine Peroux; Celine Gouin; Fabio Gastaldello

LOC:

Ilaria Marini; Paola Popesso; Denisa Tako; Victoria Toptun; Natan de Isidio; Daudi Mazengo

For additional questions, please see the conference website.

Meeting Dates: 2025 Oct 20 - 24

Meeting Location: Kyoto, Japan

Abstract submission and registration opening: 2025 mid-April

Registration Deadline: TBA

The X-Ray Imaging and Spectroscopy Mission (XRISM), launched on September 7th, 2023, is a collaborative mission between JAXA and NASA, with contributions from over 70 institutions in Japan, the U.S., Canada, and Europe. With the successful combination of high-resolution spectroscopy and wide-field imaging, XRISM has provided us with an unprecedented view of the Universe, opening a new era of high-energy astronomy.

This conference will highlight the scientific achievements from the first two years of XRISM and identify key issues we should address in the next observation cycles. Conference topics also cover theoretical studies related to XRISM observations and synergies with other observatories, including future missions.

This is the first international conference for XRISM, launched in September 2023. Conference topics will include:

Formation of the largest structures in the Universe
Chemical evolution of the Universe
Active galactic nuclei and their environment
Endpoints of stellar evolution
Accretion and outflow in compact objects
New physics with high-resolution X-ray spectroscopy
XRISM for multi-wavelength/multi-messenger astronomy

Currently, only the homepage of the conference website is available, but more information including a registration fee/procedure will be available shortly. Registration will open in mid-April.

October is a good season in Kyoto with nice weather and full of tourists, so please make your hotel reservations as early as possible if you are planning to attend. The venue is within walking distance of Kyoto Station.

We look forward to seeing you there. Save the date!

For additional questions, please see the conference website.

Meeting Dates: 2025 Oct 27 - 30

Meeting Location: Huntsville, AL, USA

*** SAVE THE DATE ***

We are pleased to announce the 4th TDAMM Workshop: Advancing Community Observing Plans for Rapid Follow-Up of Explosive Transients will be held October 27-30, 2025 in Huntsville, Alabama.

NASA's new Astrophysics Cross-Observatory Science Support (ACROSS) initiative is organizing the 4th Time Domain and Multi-Messenger Astrophysics (TDAMM) Workshop. This workshop will focus on developing community observing plans to enable the rapid and coordinated follow-up of explosive transients by space-based and ground-based observatories. NASA invites US and international members of the ground and space science communities to attend the workshop and contribute to its final product, a publicly available white paper with findings for relevant agencies and the broader astrophysics community.

If you are interested in attending and/or would like to be on our email list to receive further updates please fill out the following Google form here.

Please visit the website for additional information.

Meeting Dates: 2025 Dec 01 - 05

Meeting Location: Santiago, Chile

Active galactic nuclei (AGN) are among the most dynamic and powerful sources in the universe, powered by supermassive black holes (SMBHs) through mass accretion. The accretion rate influences many AGN properties, with high accretion rates playing a key role in growing black holes and launching outflows that may shape the host galaxy's growth. Highly accreting AGN, particularly at low redshift, offer a benchmark to understand the rapid growth of the first SMBHs in the early Universe, which remains a mystery to be solved.

Significant theoretical and observational advancements have been made in understanding fast-accreting systems, thanks to long-running observatories like VLT, ALMA, JVLA, Chandra, XMM, HST, and NuSTAR, as well as the recently launched JWST, Euclid, and IXPE. With the first light of the ELT on the horizon and the recent results from JWST on the growth of SMBH at high redshift, now is the ideal time to convene and share insights on highly accreting SMBHs. The workshop will gather astronomers to summarize the field's current status, bridging the accretion history from the early to the local Universe, and explore the mechanisms driving their growth and impact on the Universe.

This workshop will focus on the following key themes:

NLS1s and other low-z highly accreting AGN and their cosmological implications;
Outflows, jets, feedback in highly accreting sources from the nearby Universe to cosmic dawn;
Surrounding environment and host galaxy properties of highly accreting AGN at all epochs;
Theoretical and observational advances in the nuclear properties of extreme accreting AGN from low-z to high-z;
Changing-look, tidal disruption event and their implication in changing the accretion state of AGN;
Recent progress in the study of QSOs at high-z and AGN evolution;
Recent observations with state-of-the-art facilities (JWST, ALMA, XMM-Newton), future observations with new facilities (Vera Rubin, Athena, ELT, SKA, 4MOST, AXIS, PRIMA), theoretical modeling and AI.

The workshop will be held in person at the ESO premises in Santiago, Chile, with remote participation available via MS Teams.

For additional questions, please email to agn2025_loc[AT]eso[DOT]org or check out the conference website.

Other Astronomy, Physics and Space Sciences

Meeting Dates: 2025 May 19 - 21

Meeting Location: Pasadena, CA, USA (Hybrid)

Abstract Deadline: 2025 Mar 28

Registration Deadline: 2025 Mar 28

We are pleased to announce a working meeting on "PRIMA and the Future of Far-infrared Science" to be held May 19-21, 2025, on the Caltech campus in Pasadena, CA. This workshop is organized by IPAC, which is part of Caltech.

Far-infrared (FIR) wavelengths are essential to addressing some of the astronomy's highest-priority science topics, from identifying the origins of planetary systems, to understanding the buildup of galaxies. By filling a critical gap in capabilities between wavelengths accessible to ALMA and JWST, FIR wavelengths provide an unparalleled window into the obscured universe and access key tracers of star formation, black hole growth, and planet formation.

PRIMA (the PRobe far-Infrared Mission for Astrophysics), is a mission concept proposed to NASA's Astrophysics Probe Explorer (APEX) line. An observatory for the community, PRIMA will have 75% of its time dedicated to guest observer science. PRIMA is currently in a Phase A study period, with final mission selection expected in 2026. We invite the future user community to this open working meeting which is designed to better define the pressing science cases driving the need for a FIR observatory.

Topics will include:

Protoplanetary disks and planet formation
Transients and other time domain science
AGN across cosmic time
Star formation and feedback in galaxies
The buildup of dust and metals in galaxies
Star formation and magnetic fields in the Milky Way and Local Universe
Solar System science
Other science topics uniquely enabled by PRIMA

Registration and Hybrid Format We strongly encourage in-person participation. We can accommodate up to 64 people. We will also enable online participation.

Registration is free. To register, both for in-person and virtual attendance, please go to: registration site.

For additional questions, please check out the conference website.

Meeting Dates: 2025 Jul 28 - Aug 1

Meeting Location: Acadia National Park, Maine, USA

Abstract Deadline: 2025 Mar 7

Registration Deadline: 2025 May 1

From the production of the first dust grains to the growth of supermassive black holes, paradigms of galaxy evolution in the z>1 cosmos that were once thought fixed are now contested. Our goal is to reconceptualize our long held assumptions in light of new observations and theory. As galaxy evolution is revitalized, so too is the culture of astronomy through ways of creating, collaborating, and sharing knowledge. This workshop places equal emphasis on challenging scientific paradigms and critically inspecting and bettering our ways of doing science. Participants will be empowered to lead workshops, hacks, and discussions dedicated to topics such as inclusion, advocacy, justice, climate change, science communication, and more.

FINANCIAL COST To make this conference broadly accessible we are fully covering the costs of housing and meals for all participants. These will be included in the conference fee which is still TBD but is expected to be between $100 - $300 USD. We will also provide targeted travel grants to further offset costs for select participants.

LAND Schoodic Institute is Acadia National Park's primary partner in science and education and is located on the homeland of the Wabanaki, People of the Dawn. Participants are encouraged to learn about Wabanaki sovereignty at wabanakialliance.com/sovereignty and the Wabanaki Studies Law at wabanakialliance.com/wabanaki-studies-law.

We are collaborating with the Wabanaki people on activities for the unconference.

Organizing Committee Arianna Long, Erini Lambrides, Gourav Khullar, Jed McKinney, Jonathan Cohn, Lindsay House, Olivia Cooper, Sinclaire Manning, Taylor Hutchison on behalf of the choir collaboration.

Further details and updates on the program and the logistics will be provided on the conference website.

Astronomy-related Technology and Instrumentation

Astronomy-related Physics, Computational, Data Analysis, Software or Statistics

Meeting Dates: 2025 Jul 28 - Aug 1

Meeting Location: Traverse City, MI, USA

Registration Opens: 2025 ~ Apr

Radioactive nuclei play a significant role in many current astrophysical pursuits, from the origin of the elements to the driving of emissions from supernovae (⁵⁶Ni) and kilonovae (r-process radioactivity). Radioactive nuclei are crucial for direct studies of galactic enrichment (⁷Be, ²⁶Al, ⁴⁴Ti, ⁶⁰Fe, ⁹⁹Tc, ²⁴⁴Pu) and stellar explosions (⁵⁶Ni,⁴⁴Ti). Stars and their explosions, galaxies and their evolving interstellar medium, and the origin of the solar system are among the targeted astrophysical objects. Stardust, meteorites, ocean floor deposits, cosmic-rays, and gamma-ray spectroscopy provide a rich variety of astronomy to exploit the inherent power of radioactivity. Investigation tools range from numerical models, astronomical instrumentation, and laboratory experiments to derive material compositions and nuclear reaction rates.

The aim of the conference is to bring together researchers interested in the significant role radioactive nuclei play in the cosmos and particularly with respect to questions in astrophysics. The scientific program will cover topics related to the role of radioactivity within galactic chemical evolution, cosmochemistry, the origin of elements, and multi-messenger astronomy.

This is the latest in a series of conferences organized every couple of years and is open to researchers in the various relevant fields including nuclear physics experiment and theory, astronomy, and astrophysics. The purpose of the conference is to provide all participants and particularly early-career researchers with an opportunity to present their work. The format of the meeting will be designed to foster exchange of ideas, learning, and discussion among participants.

Travel support will be available for a number of participants thanks to sponsorship from IReNA.

For additional questions, check out the conference website.

Meeting Dates: 2025 Aug 25 - 29

Meeting Location: Boston, MA, USA

Registration Deadline: 2025 Aug 1

The ninth AtomDB Workshop and Workweek will be from August 25th-29th at the Center for Astrophysics | Harvard & Smithsonian, in Cambridge, Massachussetts. The AtomDB Workweek runs from Monday to Wednesday, and is an opportunity to come and work at the CfA in depth on projects related to AtomDB, atomic physics, and spectroscopy, or just to become familiar with AtomDB and spectroscopic techniques.

The workshop will run from 1.5 days, Thursday afternoon and Friday, and will be a presentation of recent updates to AtomDB, progress during the workweek, and broader updates and discussions on atomic data and spectroscopy. Students and Post Docs are encouraged to attend and present.

Registration is now open for the meeting, and will remain open until August 1st.

Contact

If you have any questions or need letters of invitation, please contact the Organizing Committee: Adam Foster afoster[AT]cfa[DOT]harvard[DOT]edu +1-617-496-3203 and Priyanka Chakraborty priyanka.chakraborty[AT]cfa[DOT]harvard[DOT]edu.

Venue

The meeting will take place at the Center for Astrophysics, 60 Garden St, Cambridge, Massachusetts. The nearest airport is Boston Logan (BOS) with flights from all over the world. Parking is limited at the CfA so we recommend using taxis or public transportation once in the area, details are available at the above link.

Accommodation

Please see here for list of hotels near the CfA. Late August can bebusy so we recommend booking accommodation early.

For additional questions, please email to agn2025_loc[AT]eso[DOT]org or check out the conference website.

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