MASCA is a conference aimed at sharing findings on AGN on 0.1-100 pc spatial scales at any wavelength, from x-ray to the VLBI. We aim to focus on:

• the subparsec scales and jets;
• the Broad Line Region;
• parsec scale structure, composition, and kinematics;
• the link with the central host galaxy <100 pc bulge region;
• the use of AGN information on a cosmic scale, which includes galactic evolution and contribution to the cosmological tension problem;
• and the instrumentation that we require to address the above points.

For additional questions, please see the conference website.

Winds are produced by nearly all stars, including hot stars on the main sequence to stellar remnants, and supermassive black holes. Conditions in the wind launching zone range from the extremely hot corona of our own Sun, to extreme magnetic-field dominated magnetospheres of isolated neutron stars, to transient flows of hot gas around merging neutron stars and supermassive black holes with recently tidally disrupted stars. On larger scales, winds driven by stellar processes and supermassive black holes interact with the surrounding interstellar medium and likely affect the subsequent evolution of the host galaxies. Multiple new observational probes have recently emerged to probe these outflows, among which are the Parker Solar Probe providing an extremely detailed look at the solar wind, observations of radioactively powered transients (“kilonovae’’) produced by accretion disc winds following a neutron star merger, and the James Webb Space Telescope which now allows to study winds in galaxies with unprecedented precision. The future also looks very promising with the upcoming launch of XRISM, which will provide a powerful new tool to study hot winds driven by individual stars and stellar clusters as well as supermassive black holes.

The 2023 JSI conference will bring together experts in theory, modeling, and observations of multiple astrophysical systems to discuss recent progress, as well as outline new frontiers in our understanding and exploration of winds in the Universe. The workshop will be divided into six sessions: Our Sun, other stars, stellar remnants, supermassive black holes, a panel discussion, and a session on future directions.

Attendance will be limited to 60-70 participants.

For additional questions, please see the conference website.

The advent of gravitational-wave and particle detectors, which now routinely observe events through new windows upon our dynamic Universe, has ushered in the era of Multi-messenger Astronomy (MMA). With a diverse and powerful network of ground- and space-based instruments and facilities, we now have advanced resources to both identify the electromagnetic counterparts of Multi-messenger events, and to monitor and characterize their evolution. This activity requires coordination of the full range of available telescopes and their capabilities. While the scientific potential is staggering, future campaigns will be resource-intensive, expensive, and require considerable coordination, collaboration, and communication among the communities in order to deliver effective science.

To foster the infrastructure for a vibrant and collaborative MMA ecosystem, NSF's NOIRLab, in partnership with NSF and NASA, invites the international community to participate in a workshop in Tucson, AZ during October 16–18, 2023. The workshop goals are to identify pathways that increase the coordination of observational MMA campaigns and reduce operational redundancy across the network of ground- and space-based observatories. We invite the community to review the current state of resources for MMA, report on existing collaborations and partnerships, and identify potential obstacles to success. We ask the workshop participants to conceptualize community strategies and methods of tackling data sharing, such as telescope pointings, both planned and executed, observation outcomes, and calibrated data. Furthermore, we ask the workshop participants to identify pathways which will incentivize coordination, collaboration, partnership, and collegiality within the MMA community.

Key Questions to Address:

• What are the main challenges to perform successful MMA campaigns and to maximize their scientific potential?
• How should we coordinate MMA follow-up to reduce operational redundancy across the network of ground and space-based observatories?
• How should we foster collaboration in the MMA community?
• How can we ensure that the MMA field reaches its full potential over the next decade?

For additional questions, please see the conference website.

Young Astronomers on Galactic Nuclei (YAGN) is an annual series of informal meetings of Ph.D. students and postdocs working on supermassive black holes and active galactic nuclei in general, with the aim of promoting exchanges of ideas and new collaborations amongst young scientists.

If you are interested in giving a talk, please fill this form by May 31, 2023. The speakers will be selected in June 2023. For any inquiries, please send an e-mail to yagn2023@gmail.com.

SOC: Pedro R. Capelo (Universität Zürich), Massimo Dotti (Università degli Studi di Milano-Bicocca), and Ciro Pinto (Istituto di Astrofisica Spaziale e Fisica Cosmica)

For additional questions, please see the conference website.

The High Energy Phenomena in Relativistic Outflows (HEPRO) conferences are a cycle of biennial events devoted to the discussion of the most recent developments, either theoretical, phenomenological, or observational, on the major themes of high-energy and multi-messenger astrophysics associated with relativistic winds and jets, on all scales.

This cycle of conferences has been spurred by Felix Aharonian, Josep Maria Paredes, and Gustavo Romero, and the previous editions were held in Dublin (2007), Buenos Aires (2009), Barcelona (2011), Heidelberg (2013), La Plata (2015), Moscow (2017) and Barcelona (2019).

The HEPRO VIII edition will be held in Paris (France), on the campus of Institut d'Astrophysique de Paris and Observatoire de Paris, from October 23 to October 26, 2023. Some specific themes that will be addressed at HEPRO VIII include the physics, dynamics and multi-wavelength signatures of jets, the production of cosmic-rays, gamma-rays and neutrinos in relativistic outflows, the environments of compact objects, the physics of relativistic sources, including pulsar wind nebulae, binary systems, gamma-ray bursts and blazars, and particle acceleration.

The sessions will be held in the main lecture hall ("Amphithéâtre") of Institut d'Astrophysique de Paris. The number of participants will be limited to 130.

The scientific program leaves ample room for oral contributions and posters, so do not hesitate to contribute!

Financial support: a limited amount of external funding is available to provide financial support for some participants. If you wish to benefit from such financial support, please do the following: first register to the conference and suggest an oral or poster-type contribution, by May 15 at the latest; then, send an email to hepro8[AT]sciencesconf[DOT]org to detail your request for support. We will collect and process all requests for funding and provide a reply by June 1st. Note that we may be unable to meet all requests.

PRELIMINARY LIST OF INVITED SPEAKERS:

• Mitchell Begelman (U. Colorado - Boulder, USA -- TBC)
• Andrei Beloborodov (Columbia U., USA)
• Valentì Bosch-Ramon (U. Barcelona, Spain)
• Zeljka Bosnjak (U. Zagreb, Croatia)
• Jonathan Ferreira (U.Grenoble, France)
• Eduardo Gutiérrez (Penn. State U., USA)
• Shigeo Kimura (Tohoku U., Japan)
• Astrid Lamberts (Obs. Nice, France)
• Eileen Meyer (U. Maryland Baltimore County, USA)
• Barbara Olmi (Obs. Arcetri, Italy)
• Alexander Philippov (U. Maryland College Park -- TBC)
• Fabrizio Tavecchio (Obs. Brera, Italy)
• Arno Vanthieghem (Princeton U., USA)
• Frédéric Vincent (Obs. Paris, France)
• Xiang-Yu Wang (Nanjing U., China)
• Walter Winter (DESY Zeuthen, Germany)

LOCAL ORGANIZING COMMITTEE

Sandy Artero (IAP); Frédéric Daigne (IAP); Kumiko Kotera (IAP); Martin Lemoine (IAP); Hélène Sol (Obs. Paris-Meudon)

SCIENTIFIC ORGANIZING COMMITTEE

Felix Aharonian (DIAS, Ireland - MPIK, Germany); Elena Amato (INAF - Osservatorio Astrofisico di Arcetri, Italy); Katsuaki Asano (ICRR, U. Tokyo); Marcia Branchesi (GSSI, Italy); Paolo Coppi (Yale University, USA); Francis Halzen (U. Wisconsin - Madison, USA); Jim Hinton (MPIK, Heidelberg, Germany); Martin Lemoine (IAP, France -- Chair); Reshmi Mukherjee (Columbia U.,USA); Josep M. Paredes (Universitat de Barcelona, Spain); Anita Reimer (U. Innsbruck, Austria); Frank Rieger (Heidelberg U. - MPIK, Germany); Gustavo Romero (IAR - FCAG, Argentina); Samar Safi-Harb (U. Manitoba, Canada) Hélène Sol (Obs. Paris-Meudon, France) Dmitri Uzdensky (U. Colorado Boulder, USA); Xiang-Yu Wang (Nanjing University, China); Eli Waxman (Weizmann Inst., Israel); Andreas Zech (Obs. Paris-Meudon, France)

For additional questions, please see the conference website.

Scientific Topic In this meeting we aim to explore the various observational and theoretical aspects of intermediate-mass black holes, and their unique role in: (1) Cosmology and galaxy evolution; (2) Formation of gravitational wave sources; (3) Accretion, tidal disruption events, and high-energy phenomena. The workshop aims to serve as a focal point for researchers working on intermediate-mass black holes on all scales, to connect theorists and observers, and to link together and share knowledge and tools between groups working on similar questions.

Meeting Format The meeting will consist of contributed talks and active discussion, for about 6 hours per day from Saturday 2 December through Tuesday 5 December 2023. Plenty of time will be dedicated to fruitful discussions and interactions among the participants, and to enjoy the beautiful venue of Belize.

Pre-Registration If you plan to attend the meeting, we kindly ask you to pre-register. Pre-registration is not mandatory, and it will only be used to have an estimate of the number of possible participants and of the number of people that need a reduced conference fee. Registration and abstract submission will open at the end of May.

Social Events We are planning to have plenty of time for social interactions among the participants. Social events will include a guided historical tour, the social dinner, scuba diving, and much more!

For additional questions, registration, anstract submission and updates, please visit the conference website.

With galaxy formation simulations pushing to the sub-parsec regime and beyond, this workshop will bring together the small-scale and large-scale simulation communities to review simulating AGN across all aspects: seeding, accretion, feedback, and dynamics. The key conference goal is to generate discussion and facilitate new collaborations across the scales, with a focus on four key questions:

• How do we implement the different theoretical seeding models into galaxy formation simulations, and can we use these to make testable predictions for future (and current) observational facilities?
• How will the next generation of large-scale models bridge the gap between black hole accretion discs and galaxies?
• How can we self-consistently model accretion and feedback across a range of regimes and scales?
• How can we accurately model black hole dynamics in galaxy formation
simulations given the advent of multi-messenger astronomy?

We expect to announce the contributed talk selections by the end of July.

Confirmed invited speakers:

Elisa Bortolas; Tiago Costa; Shane Davis; Melanie Habouzit

SOC:

Yan-Fei Jiang (CCA, Flatiron Institute); Sophie Koudmani (CCA, Flatiron Institute, SOC/LOC co-chair); Doug Rennehan (CCA, Flatiron Institute, SOC/LOC co-chair); Chris Reynolds (IoA, Cambridge); Rachel Somerville (CCA, Flatiron Institute); Marta Volonteri (IAP, Paris)

For additional questions, please see the conference website.

Since 1963, the Texas Symposium on Relativistic Astrophysics has been one of the most important international conferences in astronomy and physics. Traditionally, it moves around the globe and takes place in different cities every two years. The 32nd Texas Symposium on Relativistic Astrophysics will take place in Shanghai, China, from December 11 to 15,2023. It will be hosted by Tsung-Dao Lee Institute, Shanghai Jiao Tong University.

Shanghai, situated on the estuary of Yangtze River, serves as the most influential economic, financial, international trade, and cultural center in East China. It is also a popular destination for travelers seeking to experience the country's dynamic development. In addition to its modernization, the city's multicultural flair endows it with a unique charm. New skyscrapers and old Shikumen together draw the skyline of the city. Western customs and Chinese traditions intertwine, making any visit to Shanghai a memorable experience.

Tsung-Dao Lee Institute (TDLI), initiated by Tsung-Dao Lee, a prominent Chinese-American physicist and Nobel laureate in Physics, was established in 2016 with strong support from various Chinese government agencies. The goal of TDLI is to develop into a top-level physics-astronomy research institute in the world, and to boost research and develop talents in basic sciences in China. Professor Frank Wilczek was the founding director, and Professor Jie Zhang is the current director.

The symposium will cover all major topics on high-energy and particle astrophysics, cosmology and relativity. It will include morning plenary sessions and afternoon parallel sessions which will function as mini-symposia in each sub-field. The plenary sessions will consist of 30-45 min review talks. The afternoon sessions will feature oral talks (about 20-30 min) and poster contributions.

We look forward to welcoming hundreds of international astronomers and physicists to Shanghai in December 2023!

To stay informed about the meeting details and future announcements, please pre-register by providing your name and email.

For additional questions, please see the conference website.

Transient astronomy has seen accelerated growth and progress in the last two decades that has led to a more complete understanding of known transient phenomena and the discovery of new event classes at all wavelengths and messengers. These data have provided new insight into stellar evolution, cosmology, condensed matter, extreme energy physics, heavy element creation, cosmic chemical enrichment, the evolution of structure formation and ionised content of the Universe, among other things. Transient astronomy is time-sensitive and requires the capabilities and coordination of various observational facilities worldwide. Transients exhibit a wide range of physical processes and the wholesale discovery of transients and the discovery of new classes feed and challenge theoretical models and place unique demands on current and future instrumentation, data handing, processing, and analysis. As a result, international collaborations are essential to acquire and interpret the data to progress the field and our understanding of the Universe.

Transients Down Under brings together researchers from around the world working in transient astronomy to share ideas and recent progress in theoretical research and data collection, processing and analysis strategies, tools, and techniques. Conference topics include cataclysmic events at all wavelengths, messengers, and durations spanning observation, theory, data science, instrumentation, and cultural astronomy.

Confirmed Invited Speakers in alphabetical order (as of July 29):

Gemma Anderson (Curtin, Australia); Ghillar Michael Anderson (Euahlayi Elder, Australia); Iair Arcavi (Tel Aviv, Israel); Stéphane Basa (LAM/AMU/CNRS/CNES, France); David Buckley (SAAO, South Africa); Manisha Caleb (U Sydney, Australia); Tamara Davis (U Queensland, Australia); Orsola De Marco (Macquarie, Australia); Laura Driessen (U Sydney, Australia); Jan Eldridge (Auckland, New Zealand); Francisco Förster (Universidad de Chile, Chile); Duncan Galloway (Monash, Australia); Jarita Holbrook (Edinburgh, UK); Thomas Janka (MPA, Germany); Manoj Kovalam (UWA, Australia); Keiichi Maeda (Kyoto U, Japan); Anais Möller (Swinburne, Australia); Friedrich Röpke (HITS/Heidelberg University, Germany); Ken Shen (Berkeley, USA); Lilli Sun (ANU, Australia); Tony Travouillon (ANU, Australia)

SOC:

Ashley Ruiter (UNSW Canberra, co-chair) Jeff Cooke (Swinburne, co-chair); Brad Tucker (ANU); Karelle Seillez (UTas); Stuart Ryder (Macquarie); Christopher Lidman (ANU); Duane Hamacher (Melbourne); Ryosuke Hirai (Monash); Ivo Seitenzahl (UNSW Canberra); Alex Heger (Monash); Evgeni Grishin (Monash); Linqing Wen (UWA); Tony Travouillon (ANU); Lilia Ferrario (ANU); Nicolas Rodriguez-Segovia (UNSW Canberra)

LOC:

Jeff Cooke (Swinburne); Jade Powell (Swinburne); Simon Stevenson (Swinburne); Alex Heger (Monash); Ryosuke Hirai (Monash); Evgeni Grishin (Monash); Duane Hamacher (Melbourne); Katie Auchettl (Melbourne); Karelle Seillez (UTas)

For additional questions, please see the conference website or email to transientsdownunder2024 [at] gmail [dot] com.

This conference brings together the communities of white dwarf modelers and dense matter physicists to foster new collaborations and identify astrophysical problems that can be addressed with advanced physical theories, simulations, and experiments.

SCIENTIFIC MOTIVATION

White dwarf stars represent the end stage of the life of the vast majority of stars, including our Sun. These common stars are the sites of exotic physical conditions that are not encountered in other stars. Matter in such extreme conditions is beginning to be probed experimentally. Historically, theoretical work in dense plasma physics has found fertile applications in white dwarf models. The astrophysics of white dwarfs is a mature field, yet modern observations challenge many aspects of the models in regimes ranging from the relatively low-density gas at the observable surface through the deeper regions of partial ionization to the dense core. In many instances, modern physical theories, simulation methods and experimental techniques can be fruitfully applied to drive the field to a new level of understanding and resolve outstanding astrophysical problems.

Topics to be covered include:

• Astrophysics of white dwarf stars
• Physical processes in white dwarf stars
• Radiative opacities in dense gases and plasmas
• Equation of state and transport coefficients
• Magnetic fields
• Crystallization and phase diagrams
• Models and simulations of warm dense plasmas
• Experimental measurements

The workshop is intended to foster exchanges between different communities with the goal of identifying problems ripe for investigation. The program will consist of a limited number of invited overview talks on key topics in white dwarf astrophysics, matched with presentations of the relevant current physics methods. Scheduled group discussions will explore selected topics in greater details. Contributed posters will be up during the entire workshop and there will be ample time for discussions. We encourage the participation of young researchers. A limited number of travel grants will be available to assist students and postdocs.

WORKSHOP ORGANIZERS

Didier Saumon (Los Alamos National Laboratory, USA, co-chair); Jerome Daligault (Los Alamos National Laboratory, USA, co-chair); Simon Blouin (U. Victoria, Canada); Stephanie Hansen (Sandia National Laboratories, USA); Amy Lazicki (Lawrence Livermore National Laboratory, USA); Nicole Reindl (Zentrum für Astronomie der Universität Heidelberg, Germany)

For additional questions, please see the conference website.

Save the date! Note: The Horseshoe Bay Resort is near the centerline of the 2024 Total Solar Eclipse on Monday April 8, 2024.

Check the website for more information.

Tidal disruption events (TDEs), which occur when a star is destroyed by the immense tidal field of a supermassive black hole, fuel luminous accretion flares that provide unique insight into the properties of galactic nuclei and their central black holes. The detection rate of these events has accelerated in recent years thanks to advances in wide-field survey capabilities across the electromagnetic spectrum. Nonetheless, there remain theoretical uncertainties in the modeling of TDEs that obfuscate understanding in the face of observations, and our ability to use TDEs as a collective Rosetta Stone for deciphering black hole demographics across cosmic time remains elusive. To bridge theory and observation and to start to tap the wealth of understanding contained within TDE observations, this conference aims to unite the diverse field of astronomers working on TDEs and the related fields of variable Active Galactic Nuclei (AGN) and X-ray binaries. This conference will highlight the recent advances that have been made in understanding TDEs, make connections to related astrophysical phenomena, and elucidate the most outstanding questions in TDE theory and observation.

For additional questions, please see the conference website.

The exchange of mass, energy, and metals between galaxies, their surrounding circum-galactic medium (CGM), and the gas permeating halos at larger scale represents a fundamental part of the modern astrophysics. Both components still elude our knowledge. Indeed, we are very far from having a census of the CGM properties in the bulk of the galaxy population. Furthermore, the halo gas is well known at large scale only in the most massive halos of our Universe, the galaxy clusters (intra-cluster medium, ICM), but it is still very elusive in the bulk of the virtualized halo population at the group mass scale (Intra-group medium IGrM).

For this reason, so far, the study of such baryon cycle has been linked almost exclusively to galaxy evolution in a so called "streetlight bias". Albeit more difficult to detect, the IGrM and the CGM are the other two key players on the stage, and their evolution across cosmic time is linked to the baryon exchange as much as the galactic component. Due to the substantial lack of information on the nature of the CGM and IGrM at large scales, many key questions remain unanswered. For instance, how is the IGrM affected at large scales by the feedback imparted energy? In other words, how does the baryon cycle affect the large-scale structure of our Universe? How much energy, momentum and entropy are released to the still elusive CGM hot component around galaxies? What is the main mechanism of interplay between CGM and central galaxy?

With the advent of instrument such as eROSITA, XRISM and JWST, and the enormous variety of results collected by Alma, MUSE, KCWI and LOFAR, it is time to review the state of the art of this research field. The final goal of this workshop is to fill the knowledge gap and review in an unbiased way all the key aspects of the baryon cycle: from the hot IGrM enclosed in the bulk of the virtualized halo population, to the CGM at hundreds of kpc from the central galaxy, and down to the main mechanisms in act at the galaxy center able to trigger the baryonic exchange.

For additional questions, please see the conference website.

A tidal disruption event (TDE) occurs when a star is pulled apart by the gravitational field of a supermassive black hole (SMBH), transforming the star into a stream of stellar debris. In a matter of months, a fraction of this debris stream returns to the SMBH and ignites an accretion flare in the nucleus of the galaxy where it resides. TDEs have been observed in great detail across the electromagnetic spectrum; from the initial rise in flux to the decay back to quiescence. Such observations may enable an inference of the SMBH and disrupted star properties, while also providing a unique window into poorly understood aspects of accretion theory, such as the nature of super-Eddington flows and the production of jets and outflows. The large increase in observational data for TDEs will provide an unprecedented census of the low-mass end of the SMBH population, but to take full advantage of this influx of data, we need robust and predictive theoretical models for the radiation from these events. The goal of this program is to bring theorists and observers together to answer some of the most pressing questions on the physics of TDEs. From the processes that generate stars on fateful orbits toward the SMBH, to the initial destruction of the star and the formation of an accretion flow, to the production of high-energy radiation and outflows, this program aims to test, revise and extend our current understanding of TDEs.

For additional questions, please see the program website. See also the associated conference information.

We are on the cusp of significant advancements to our understanding of the origins and early growth of massive black holes with current and near-future electromagnetic observations by JWST and other upcoming missions which will be complemented by gravitational wave detections with LISA in the coming decade. The focus of this conference is on recent advancements in both observations and theory on the origin, growth and dynamics of MBHs in the early Universe. Follow the pre-registration link above to let us know you are interested and you will receive an email when abstract submission is open!

Topics of interest:

• Observations and predicted properties of AGN and their hosts at early times
• Constraining MBH formation mechanisms with multimessenger observations at low and high redshift
• Predictions for MBH seed masses from low redshift observations of dwarf galaxies
• Challenges (both theoretical and observational) to observing and interpreting data on early MBHs
• MBH-galaxy co-evolution and feedback in the early universe
• Dynamics of MBHs and MBH binaries in the early Universe
• How can we connect current and near-future E-M observations to future GW detections to do astrophysics?
• Understanding the environment of high redshift MBHs and AGN and how it affects their early evolution

Extreme galaxies and extreme environments have long served as key benchmarks for models of galaxy formation. The mere existence of such galaxies and environments creates significant challenges to physical models of galaxy formation, as such models must be able to explain the formation of “normal galaxies” in “normal environments” as well as the extreme tail of the galaxy and environmental distribution. For example, massive and quenched/strongly star-forming galaxies have long placed significant constraints on quenching models. Likewise, the existence of proto-clusters containing both strongly starbursting and quenched galaxies are forcing us to reevaluate the effect of environment on galaxy evolution at high redshift. Studies at 1 < z < 2 have raised a host of new questions about galaxy evolution that can only be answered by turning our gaze to even higher redshift. Fortuitously, the coming of observatories such as JWST, ALMA and the upcoming Euclid and Roman Missions are opening up the study of the z > 2 universe with large surveys that make possible the study of extreme galaxies and extreme environments at the very highest redshifts. The goal of this meeting is to bring together theoreticians and observational astronomers working on extreme galaxies in extreme environments at z > 2 to summarize the state of these fields and discuss how they are pushing forward our understanding of the physics of galaxy formation.

This 5-day meeting will focus on 4 key themes under the general topic of extreme objects. The four topics that will be discussed in the meeting are:

1. Extreme galaxies: Massive galaxies, dusty-star-forming galaxies, high/low mass quiescent galaxies, AGN, and other extreme objects
2. Extreme environments: Proto-clusters, galaxy overdensities, and voids
3. Extreme galaxies in extreme environments: Is the evolution of extreme galaxies and environment linked at high-redshift and if so, how?
4. The evolution with time of extreme galaxies and environments: How do these extreme environments/objects connect to lower-redshift descendants (z < 2) and what does this tell us about the physics of galaxy formation?

Benedetta Vulcani, INAF OaPD (chair); Adam Muzzin, York University (co-chair); Greg Rudnick, University of Kansas (co-chair) Scientific organizing committee (SOC):

Gabriella De Lucia; Michele Fumagalli; Nina Hatch; Jackie Hodge; Adam Muzzin; Greg Rudnick; Rhea-Silvia Remus; Sandro Tacchella; Benedetta Vulcani; Kate Whitaker

For additional questions, please see the conference website.

The X-ray emission from neutron stars and white dwarfs has been a subject of extensive research, unveiling unique insights into the high-energy phenomena occurring within these compact stellar remnants. In this meeting, we gather experts from various disciplines to delve into the latest advancements in understanding the X-ray emission processes, its origin, and the astrophysical implications associated with neutron stars and white dwarfs.

We will explore the diverse X-ray emission mechanisms, ranging from thermal emission due to accretion processes, magnetic fields, and nuclear reactions, to non-thermal emission originating from particle acceleration and magnetic reconnection events. These mechanisms provide crucial insights into the physical conditions and dynamics present in the extreme environments surrounding neutron stars and white dwarfs.

The X-ray spectra and timing properties will be discussed in detail, enabling a deeper understanding of the underlying emission mechanisms and the associated astrophysical phenomena. Spectral analysis techniques will shed light on the composition, temperature distribution, and physical parameters of the emitting regions. Furthermore, timing studies will reveal periodic and aperiodic variability, aiding in the characterization of rotational dynamics, accretion phenomena, and potential gravitational wave signatures.

In addition, we will explore the role of X-ray emission in the context of binary systems, investigating the interactions between compact objects and their stellar companions. X-ray binaries, including pulsars and cataclysmic variables, provide unique opportunities to study the accretion processes and the influence of intense magnetic fields on the X-ray emission.

Finally, we will discuss the implications of X-ray studies for our broader understanding of astrophysics. The X-ray emission from neutron stars and white dwarfs offers invaluable insights into compact object formation, stellar evolution, and the interplay between magnetic fields, radiation, and matter in extreme conditions. Synergies with radio, infrared, optical, gamma-rays and multi-messenger studies will be looked at, fostering interdisciplinary discussions and collaborations, encouraging the exchange of ideas. By collectively unraveling the high-energy mysteries, we strive to advance our understanding of these enigmatic stellar remnants and their impact on the cosmos as a whole.

For additional questions, please see the conference website or email to xmmws2024 [at] esa [ dot] int.

ollowing the success of the previous two conferences on supernova remnants in 2016 and 2019, a consensus was reached to hold regular meetings on the topic. Following delays due to COVID-19 pandemic, the Institute for Astronomy, Astrophysics, Space Applications & Remote Sensing of the National Observatory of Athens is happy to invite you to “Supernova Remnants III: An Odyssey in Space after Stellar death” on the beautiful island of Crete, the home of the mythical inventor and artisan Deadalus, as well as Icarus, Theseus and the Minotaur.

The conference will build upon spectral and imaging observations from radio to gamma-ray wavelengths of SNR blast waves, pulsar wind nebulae and SN ejecta and their interpretation through theoretical models and numerical simulations. The goals of the meeting are understanding the evolution of SNe, SNRs and their interaction with interstellar gas, elucidating the physical processes that govern shock waves and relativistic plasmas, and inferring characteristics of supernova explosions from SNR observations.

We will focus on narrowing the gap between observations and theories with the help of powerful new observing facilities and increasingly detailed and realistic numerical simulations. New understanding of the nature of supernova remnants and processes that occur there offers new insights into the role of SNRs in the structure and evolution of galaxies and the nature of supernova explosions.

Looking forward to seeing you in Crete!

For additional questions, please see the conference website.

This scientific workshop will explore current understanding of AGN populations, with a particular focus on current and future observational surveys. The primary scientific questions to be addressed are:

1. How can we establish a complete census of black hole growth across cosmic time (including the highest redshift AGN) and what does this tell us about how and when supermassive black holes form and grow?
2. What can multi-wavelength surveys tell us about different physical components of AGN and what implications does this have for a standard/unified model or evolutionary model of AGN? For example: obscured vs. unobscured AGN; red vs. blue quasars; `radio quiet’ vs. `radio loud’ AGN. This could include understanding the information we need from the different physical components of an AGN (e.g., obscuring torus, narrow line region, broad line region, jets, etc.).
3. What are the properties of the host galaxies of different AGN populations and what does this tell us about how galaxies and AGN influence each other?
4. What are the different data, observational techniques, and analysis methods we need to accelerate progress in answering these questions over the coming decade? This could include: exploiting SKA and its pathfinders; utilising current and forthcoming large-scale photometric/spectroscopic surveys; placing new constraints on magnetic fields; and applications of machine learning.

A parallel objective to the scientific content, is to build research connections between the European and African continents. Towards this, there will be substantial financial support to enable participation from astronomers based in Africa, who might otherwise be unable to attend the workshop. In conjunction with the scientific programme, we will hold dedicated activities before, during, and after the workshop to develop collaboration between the different scientific communities, and provide early career researchers with peer networking opportunities.

We anticipate a strong showcase of work that is of strong interest to both the European and African communities. For example, results from SKA pathfinder telescopes such as LOFAR, e-MERLIN, JVLA, and MeerKAT, in addition to telescopes such SALT in South Africa and H.E.S.S. in Namibia. Whilst the focus is on European-African collaboration, scientists from everywhere are welcome to participate.

The workshop will be limited to around 80 participants. Selection will be based on the quality of abstract submissions for talks or posters, and their alignment to the focus of the meeting. Consideration will also be made to a strong representation from African astronomers, to ensure a balanced view of AGN science across the continents.

Costs and Financial Support

The anticipated conference fee is around £350 (details to be confirmed later).

We have a substantial (but finite) budget to support scientists coming from Africa. This could cover, up to and including all travel and accommodation costs, plus a fee waiver. Preference for financial support will be given to those most in need, and to early career researchers. Applicants should indicate in their form, the level of financial support they would require to attend the workshop (e.g., travel, accommodation, fee waiver, complete costs, etc.).

SOC/LOC

Scientific Organising Committee:

Chris Harrison (UK) - Co-Chair; Leah Morabito (UK) - Co-Chair; Mirjana Pović (Ethiopia); James Chibueze (South Africa); Cristina Ramos Almeida (Spain); Zara Randriamanakoto (South Africa); Eli Kasai (Namibia); James Aird (UK); Brooke Simmons (UK)

Local Organising Committee:

Nicole Thomas (Durham); Ann Njeri (Newcastle); Houda Haidar (Newcastle); Emmanuel Bempong-Manful (Manchester); Leah Morabito (Durham); Chris Harrison (Newcastle)

For additional questions, please see the conference website.