ABSTRACT. TBC

ABSTRACT. We highlight recent scientific results coming from extragalactic HI studies with ASKAP, FAST and MeerKAT. The complementary strengths of ASKAP (high resolution, wide area), FAST (high sensitivity, wide area) and MeerKAT (high resolution, deep fields) are particularly suitable for the exploration of rare phenomena (such as dark galaxies) and the low-column density Universe (such as circumgalactic gas). The ASKAP WALLABY survey has now detected a significant number of extragalactic HI sources without optical counterparts, several of which have now been confirmed with MeerKAT observations (O'Beirne, Staveley-Smith et al. 2024, 2025). Similarly, interacting systems discovered by WALLABY in HI (Staveley-Smith et al. 2025) have been followed up with deep FAST and MeerKAT observations to create images with exquisite spatial resolution and column density sensitivity, nicely demonstrating the gas fragmentation and cooling can occur even in a hot cluster medium.

ABSTRACT. The China-Argentina Radio Telescope (CART) has a diameter of 40 m, and 8 working bands including L, S/X, C, Ku, K, Ka and Q. The S/X dual band cryogenic receivers and the dual beam Q band cryogenic receivers are among the first to be equipped with CART starting from the testing phase. CART is a milestone joint-project between China and Argentina, it is located at the CESCO Observatory of the National University of San Juan of Argentina, and will be the largest single dish and VLBI unit in Latin America. It is expected to have important synergies with LLAMA and AGGO, and will get involved in and contribute to major international VLBI campaigns such as IVS, SKA VLBI and maybe also ALMA in the future.

ABSTRACT. Since 2022, we have conducted water vapor monitoring at the National Astronomical Observatory Ali Station, located at an altitude exceeding 5,000 meters in Ali, Tibet. Beginning in 2024, an additional microwave radiometer was installed at Site B (elevation 5,250 m) to simultaneously monitor atmospheric water vapor. Our monitoring results demonstrate that the precipitable water vapor at Ali Station remains below 1 mm during the observing season, confirming its status as an exceptional site for millimeter and submillimeter wave astronomy. These observational data will provide crucial environmental support for the upcoming Ali primordial gravitational wave detection.

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ABSTRACT. Launched in January 2024, the Einstein Probe (EP) is a space X-ray observatory designed to detect high-energy transients and variables at unprecedented sensitivity and spatial resolution in the soft X-ray band, enabled by the novel lobster-eye micropore optics technology. The transients and variables can be characterized by quick follow-up observations onboard with a dedicated X-ray telescope. Transient alerts can be downlinked quickly to ground to trigger follow-up observations at multi-wavelengths. The Einstein Probe is a project led by the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES. After extensive and elaborative in-orbit calibration and commissioning, EP has started nominal science operations since July 2024. Thanks to the unparalleled capability of the two instruments onboard, EP has so far detected a large sample of X-ray transients of various timescales and physical origins, ranging from collapsars, compact star mergers, tidal disruption events, to stellar super-flares. These EP sources have been extensively followed up and studied by the EP as well as the entire time-domain astronomical communities, providing valuable targets of opportunities for many telescopes, large and small, across the world. In addition, EP has also made remarkable discoveries in non-transient fields across astrophysics. This talk will present the scientific highlights of Einstein Probe achieved in the first two years of operations and will briefly discuss the prospects in its future operations, particularly in the fields of multi-messenger time-domain astrophysics.

ABSTRACT. Compact object mergers are multi-messenger sources and known progenitors of some gamma-ray bursts, bright flashes of high-energy radiation powered by a central engine, either an accreting black hole or a neutron star. Our understanding of these events has so far been shaped primarily by observations in the gamma-ray band, leaving their prompt phase poorly constrained at lower energies. A long-lasting (~100 s) engine-driven X-ray emission was discussed to explain rapidly fading X-ray afterglows following several (~30 %) bursts of short (<~2 s) duration. However, this prompt X-ray component was not directly observed and past candidates were not confirmed. Here we report the discovery of a minutes-long (~560 s) flash of soft (0.5–4 keV) X-rays immediately following the short (~0.4 s) GRB 250704B. The variability and spectral shape of this emission are inconsistent with the canonical picture of a hard, accretion-powered spike followed by a standard external-shock afterglow. Instead, the long-soft bump points to a distinct phase of prompt emission in X-rays, which would not have been detected without the soft X-ray coverage of Einstein Probe. The detection of a prompt soft X-ray counterpart in an otherwise ordinary short GRB shows that long-lasting X-ray emission is likely a common feature of merger-driven bursts and a promising electromagnetic counterpart to gravitational wave sources.

ABSTRACT. Insight-HXMT is the first Chinese X-ray astronomy satellite and was launched to a 550 km orbit on 15th June 2017. The Insight-HXMT consists of three collimated telescopes HE (20-250keV), ME (5-30 keV) and LE (1-15 keV), and is characterized by a broadband energy coverage, where at above 20 keV it has a large detection area and, at below 3 keV it has good energy/time resolution and is free from pile-up problem in observation of the bright source. As one of the core sciences, XRB was explored in depth with over than 200 papers born out of Insight-HXMT observations. Here I will briefly introduce on behalf of the Insight-HXMT team the research progresses achieved upon the X-ray binary systems.

ABSTRACT. Supermassive black holes are ubiquitous in the nearby Universe. Their lifecycle appears to be closely connected to the evolution of galaxies. How and when did these mysterious objects form? What was the first generation of black hole seeds? How did they grow quickly enough to power the most distant quasars? And how precisely do black holes co-evolve with galaxies? I will summarize the demographics of central black holes in the local Universe and recent discoveries made with the James Webb Space Telescope that offer surprising, new insights into the earliest phases of black hole and galaxy formation during the first billion years of cosmic history. I will outline what we know and the much else that still remains uncertain.

ABSTRACT. The Epoch of Reionization and Cosmic Dawn mark the emergence of the first luminous structures and remain among the least constrained phases of cosmic history. This talk explores the prospects for reconstructing the evolution of the early Universe through the joint interpretation of complementary observational probes. We will emphasize the synergy between cosmic microwave background measurements, quasar absorption spectra, the rapidly expanding census of high-redshift galaxies from JWST, and forthcoming observations of the redshifted 21 cm signal. A central theme is the requirement for self-consistent modelling of galaxy formation and the intergalactic medium in order to robustly connect theory with these diverse datasets. We will further discuss the role of advanced statistical and inference frameworks, including machine-learning–based approaches, in mitigating parameter degeneracies and maximizing the information content of multi-probe analyses. Finally, we will highlight how this combined observational program enables stringent constraints on reionization-era astrophysics while providing novel tests of the concordance cosmological model and potential signatures of new physics at high redshift.

ABSTRACT. Dwarf galaxies provide unique laboratories for investigating active galactic nucleus (AGN) activity in low-mass systems, where black hole accretion and feedback may operate under fundamentally different conditions from those in massive galaxies. Their shallow gravitational potentials and relatively unevolved structures are regarded as 'cosmic fossils' of early galaxies, making them valuable local analogues of high-redshift AGN hosts. Moreover, dwarf galaxies are promising sites for hosting intermediate-mass black holes (IMBHs), offering critical constraints on black hole seeding and early growth pathways. However, identifying accreting black holes in these systems is challenging due to contamination from star formation and the limited spatial resolution of conventional surveys. Very long baseline interferometry (VLBI), with milli-arcsecond resolution and high brightness-temperature sensitivity, offers a powerful diagnostic for isolating compact, non-thermal radio cores associated with accretion. In this talk, I will present our systematic VLBI-based selection of AGN candidates in dwarf galaxies, combining spatially resolved MaNGA spectroscopy with high-resolution radio observations to probe nuclear and off-nuclear activity. As a representative example, we highlight MaNGA 12772–12704, where VLBA observations at 1.6 and 4.9 GHz reveal a compact (>10⁹ K) radio core and a ∼2 pc-scale jet, offset by ∼0.94 kpc from the galaxy center. The steep radio spectrum and decade-long variability support sustained accretion rather than stellar processes. Our results demonstrate the effectiveness of VLBI in uncovering AGN activity in dwarf hosts and provide new constraints on the demographics and growth of IMBHs in low-mass galaxies.

ABSTRACT. A significant population of quasars have been found to exist within the first Gyr of cosmic time. Most of them have high black hole (BH) masses (MBH ~ 10^{8-10} Msun) with an elevated BH-to-stellar mass ratio compared to typical local galaxies, posing challenges to our understanding of the formation of supermassive BHs and their coevolution with host galaxies. Here, based on size measurements of [CII] 158um emission for a statistical sample of z ~ 6 quasars, we find that their host galaxies are systematically more compact (with half-light radius Re ~ 1.6 kpc) than typical star-forming galaxies at the same redshifts. Specifically, the sizes of the most compact quasar hosts, which also tend to contain less cold gas than their more extended counterparts, are comparable to that of massive quiescent galaxies at z~4-5. These findings reveal an intimate connection between the formation of massive BHs and compactness of their host galaxies in the early universe. These compact quasar hosts are promising progenitors of the first population of quiescent galaxies.

ABSTRACT. The 2022 Revised National Curriculum of South Korea emphasizes the cultivation of digital literacy and data analysis skills across science education,To keep pace with these shifting educational paradigms, research and training to enhance teacher professionalism have become more critical than ever.

In this study, we developed innovative science educational content that leverages the vast big data and data science methodologies inherent in astronomy. This content is designed to foster students' scientific reasoning, inquiry skills, problem-solving abilities, and active scientific engagement. Key topics include 'Classification of Stars', 'Cosmic Expansion', 'Exoplanets', and 'Space Hazards'—the latter directly linking astronomical phenomena to the broader context of environmental protection and planetary safety.

In this presentation, We will introduce the specific components of the developed educational content and share the outcomes of various teacher training programs conducted to date. Furthermore, we aim to discuss sustainable strategies for integrating astronomy-based educational data into future academic programs, ensuring their long-term viability in the evolving educational landscape.

ABSTRACT. The night sky connects our species through space and time, across rich diverse cultures –under one sky. The awe and wonder of the Cosmos unlocks imaginations and has inspired thinkers and creators to explore some of the most fundamental questions about the Cosmos from various viewpoints. Astronomy gives students a Cosmic Perspective, and provides students with the opportunity to engage with, and appreciate the deep connections between, STEM and non-STEM disciplines. This has implications for supporting students to develop the skills and knowledge to enable them to tackle the challenges humanity will face far into the future.

Over the last few decades, progress in networking and sharing telescope resources has come a long way from dialup modems sharing tiny CCD images across home telephone lines up to the current large-scale telescope networks used for education. It is now the time in the development of these networks that large-scale sharing of resources with reasonable sharing of costs to significant numbers of users from youth up to graduate students and beyond and from simple colour images to long-term research projects like exoplanet monitoring.

This talk will provide a unique perspective of how to tap into the immense potential of robotic telescope access and sharing in the resources for education, outreach and research that it brings, through one of the most advanced and growing network of robotic telescopes for education - www.nextastro.org.

This talk will provide a brief overview of the history of robotic telescopes in education, the current landscape, the range of tools and networks available as well as possibilities and inevitabilities for the future of robotic telescopes, student research and education.

ABSTRACT. In Nepal, girls often receive limited encouragement to pursue scientific subjects, particularly Astronomy, which typically requires evening or nighttime observation. Due to safety concerns, many parents do not permit their daughters to study outside after dark, creating barriers for students genuinely interested in astronomy. This study explores an alternative, daytime-based learning approach designed to sustain and enhance girls’ interest in science. By introducing concepts such as the Sun’s motion, shadow observation, and the construction of sundials, students were able to understand the fundamental idea of determining time using solar shadows. This hands-on, daylight-focused method not only increased their curiosity and participation in astronomy but also helped parents gain confidence in allowing their daughters to engage in scientific learning. The outcomes indicate that such accessible, culturally sensitive teaching strategies can effectively promote scientific interest among girls and positively influence parental attitudes.

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ABSTRACT. Abstract to be provided by the deadline.

ABSTRACT. Introductions of special CSU session

ABSTRACT. Scientific and application support capabilities of China's space station and manned lunar exploration, as well as international cooperation

ABSTRACT. Research achievements on DRO exploration in the Earth-Moon space and international joint observations

ABSTRACT. A new VLBI Global Observing System (VGOS)-compatible radio telescope, namely ITB-Bosscha VLBI Station is currently in phase of completion at Bosscha Observatory, Indonesia, thanks to the partnership between ITB and the SHAO - CAS. The construction of the telescope tower has been finalized, accompanied by a supporting building to facilitate telescope operations. The main reflector disk was successfully hoisted during the Big Lift operation in July 2025, representing a pivotal achievement in the structural assembly of the VGOS antenna system. Subsequently, integration and installation of the signal chain components were completed successfully, initiating the next stage of RF and backend instrumentation deployment in the VGOS system. This achievement was validated by a successful fringe test conducted between Sheshan Station and ITB-Bosscha Station on 28 December 2025. A number of testing, commissioning, and science verification plans are underway to obtain a comprehensive picture of the telescope's operation. This also requires several observation simulations and scheduling plans, which will be conducted in conjunction with several potential telescopes, particularly with the VGOS telescopes in China and Thailand. As is known, Thailand has succeeded in building two radio telescopes in Chiangmai (TNRT 40m and VGOS 13m) and two more are under construction in Walailak and Songkhla in southern Thailand. Obviously, this will form a solid foundation to establish forthcoming regional VLBI networks, which is the Southeast Asia VLBI Network (SEAVN) expected from collaboration with Indonesia, Malaysia, and Vietnam. Eventually, this new expected network can be integrated into a larger network such as East Asia VLBI Network (EAVN) and European VLBI Network (EVN). The potential of scientific return will be presented in this talk.

ABSTRACT. Chinese VLBI Network (CVN) has played an important role for the satellite tracking and achieved a great success in a series of Chinese deep space missions. CVN stations are also active members of international VLBI arrays, e.g. the East Asian VLBI Network, the European VLBI Network, the International VLBI Service for Geodesy and Astrometry. With the development of radio astronomy in China being greatly expanded in last decade, besides of legacy radio telescopes located at Shanghai, Kunming and Urumqi, new radio telescopes geographically distributed across China are built (Changbai Mountain 40-Meter Radio Telescope, Shigatse 40-Meter Radio Telescope) or in-building (Qitai 110-Meter Radio Telescope, Jingdong 120-Meter Radio Telescope). These telescopes with the state of art of modern technology, such as simultaneous multi-band receiver, wideband digital backend, high speed data recording and so on, not only provide the completeness of spatial sampling and boost the sensitivity of CVN, but also benefit for high frequency and high-resolution astronomical observations, which shows great advantage to new discoveries in recent years. In this report, we will introduce some fresh observational results of CVN with the new technology (e.g. simultaneous multi-band receiver), and new telescopes (on microquasars, pulsars, etc). Moreover, joint observations connecting the Asia-Pacific will further improve the resolution and the sensitivity, collaborations in the Asia-Pacific region will also be very important for both instrumental upgrading and scientific observations.

ABSTRACT. Very-long baseline interferometric (VLBI) observations are responsible for achieving some of the highest angular resolution images in astronomy. However, the image reconstruction challenge with VLBI observations, involving corrupted correlations, calibration uncertainties, and sparse sampling of the Fourier domain, is an ill-posed deconvolution problem. Estimates of the source intensity distribution require robust algorithms to overcome the VLBI limitations in aperture coverage and the final image can be sensitive to calibration assumptions. In this work, we present a direct interferometric imaging approach leveraging closure invariants, special interferometric quantities formed from triangular loops of mixed Fourier components which capture calibration-independent information on the source morphology. Our methodology involves a purpose-designed generative deep learning architecture comprised of a conditional diffusion U-Net and a convolutional neural network optimiser, specifically tailored to utilise observable closure invariants for direct image reconstruction. We evaluate our image reconstructions against state-of-the-art VLBI imaging algorithms on Next-Generation Event Horizon Telescope (ngEHT) total intensity imaging challenges, showing how our deep learning approach with closure invariants yields comparable results, independent of arbitrarily large complex station-based corruptions. Moreover, we apply our method to actual EHT observations of blazar 3C 279, Centaurus A, and M87. Crucially, the trained model exhibits generalisability across complex source morphologies and robustness to thermal noise. This framework, which can be further extended for dynamic or polarimetric imaging, offers an additional independent constraint on source morphology, ultimately improving the accuracy and reliability of sparse VLBI imaging results.

ABSTRACT. We present recent VLBI progress on compact radio activity in nearby galaxies based on ongoing high-resolution follow-up observations of the LeMMINGs sample. Our 5 GHz imaging reveals a high detection rate of compact (≤5 pc) synchrotron cores and small-scale jets, demonstrating that weakly accreting supermassive black holes can still launch detectable radio outflows even at extremely low accretion levels. In this talk, I will also highlight two particularly interesting cases that illustrate the diversity of faint nuclear activity. The first is an exceptionally weak nucleus with the lowest known accretion rate in our sample, where VLBI resolves a two-sided sub-parsec jet and an unusually steep frequency-dependent core shift, suggesting strong magnetic–particle non-equipartition and providing rare evidence of jet formation in a nearly dormant SMBH. The second is a sudden 2023–2024 radio outburst discovered in a star-forming galaxy, where new e-MERLIN and VLBI monitoring shows a flux increase by more than a factor of two to three relative to past VLBI measurements and an inverted spectrum at GHz frequencies, indicating a rapidly evolving compact source. I will present the latest observational results and discuss possible interpretations, along with planned VLBI follow-up and prospects for future SKA-VLBI studies of faint nuclear activity in the local Universe.

ABSTRACT. Since its launch in 2008, the Fermi Large Area Telescope (Fermi-LAT) has aided to discover more than half of the known millisecond pulsars (MSPs). Among these are Spider pulsars, which are MSP binaries with main sequence or semi-degenerate stars in tight orbit (orbital periods ≲ 1day). These Spider pulsars are among the fastest-spinning and heaviest pulsars due to the recycling scenario. They provide stringent constraints on the physics of ultra-dense matter in neutron-star interiors. Observing these pulsars in radio wavelengths can be challenging due to eclipses caused by intrabinary material shed away by the companion star which can last up to 70% of the orbit. Optical surveys, on the other hand, offer an alternative channel to search for Spider pulsars. In such tight orbit, the companions are tidally distorted and heavily irradiated by pulsar winds. These effects form unique sinusoidal modulations on optical light curves, distinguishing them from most variable stars. Since 2020, we have been observing unidentified Fermi-LAT sources using the Thai Robotic Telescope, Liverpool Telescope, and New Technology Telescope at La Silla Observatory. Two new black widow PSRs J1544-2555 and J1213-4415 was discovered by the survey and subsequently confirmed by radio follow-up observations using the radio telescope MeerKAT. In the LSST and SKA era, many more spider systems are expected to be uncovered in the southern sky.

ABSTRACT. Black holes and neutron stars are among the most extreme laboratories in the Universe, where gravity, radiation, and magnetic fields interact to shape powerful cosmic outflows. I will present coordinated X-ray, optical, and radio observations that probe variability and jet formation in these systems. Focusing on the black-hole candidate Swift J1357.2–0933, we detected 1–5 mHz X-ray quasi-periodic oscillations accompanied by correlated optical/UV variability, pointing to a low-frequency inner-disc instability; although the system is radio faint, AMI monitoring and ATCA limits place important constraints on jet activity and accretion geometry. I will place these results in the broader context of neutron-star low-mass X-ray binaries, including 4U 1820–30, where X-ray–radio coupling appears linked to changes in boundary-layer size, and XTE J1739–285, where accretion- and nuclear-powered pulsations together with a 0.83 Hz QPO reveal how rotation and accretion rate shape variability. Finally, I will discuss how upcoming time-domain facilities—XRISM, NewAthena, LSST, SKA—and coordinated monitoring with small optical and radio telescopes will enable continuous multi-band coverage, offering transformative insight into disc instabilities and jet launching across the compact-object population.

ABSTRACT. In this talk, I will present results from our study of the connection between quasi-periodic oscillation (QPO) frequencies and spectral parameters in the black hole binary GRS 1915+105, using broadband observations from AstroSat’s LAXPC and SXT instruments. By modeling the spectra across a wide range of X-ray states, we find that the accretion rate varies from ∼0.1 to ∼5.0 × 10¹⁸ g s⁻¹ and that the inner disk truncation radius shifts between ∼1.2 and ∼19 gravitational radii, consistent with a nearly maximally spinning black hole. Despite the large variation in parameters, the observed 2–6 Hz C-type QPOs follow the trend predicted by the relativistic dynamical frequency model, based on sound-crossing timescales at the truncation radius. Interestingly, the ∼70 Hz high-frequency QPO also follows the same trend, indicating a possible common physical origin near the innermost stable circular orbit.

ABSTRACT. Using 7.5 years of data from the Medium Energy X-ray telescope (ME) and High Energy X-ray telescope (HE) onboard the Insight-HXMT satellite, we detected over 90 lightning-induced electron precipitation (LEP) events. These events mainly occurred near the eastern coast of South Africa and North America, distributed broadly within the L-shell range of 1.5 < L < 3. They exhibited seasonal variations and were observed exclusively at nighttime, with a pulse period range of 0.2–0.45 s (peaking at 0.35 s). Our analysis indicated that their occurrence was correlated with solar activity but not with the Dst index. The energy of the precipitating electrons was estimated to be 100–400 keV using the ME data, consistent with the tens to hundreds of keV range observed by the HE. This energy estimate is further supported by GEANT4 simulations. The HE and ME data revealed unusual features in the electron signals, which are attributed to strong electron scattering effects. We also derived that the electron pitch angle distribution is broad, with the majority concentrated between 50◦ and 130◦, and peaking at 90◦.

ABSTRACT. Cataclysmic variables (CVs) are binary systems consisting of a white dwarf and a low-mass main-sequence companion, with accretion onto the white dwarf producing X-ray emission. CVs are among the major Galactic X-ray sources, and the eROSITA survey provides a new opportunity to identify numerous X-ray-emitting CVs and study their Galactic population. In this work, we search for CV candidates by cross-matching sources from four X-ray catalogs—eROSITA, XMM-Newton, Swift, and ROSAT—with Gaia sources located between the main sequence and the white dwarf cooling sequence in the Hertzsprung-Russell diagram. For the selected candidates, we further investigate periodic modulations in ZTF and TESS light curves. We identify 444 X-ray-emitting CV candidates, including 267 previously known CVs. Among the remaining 177 candidates, 56 show potential orbital modulation. Approximately 51% of the candidates are uniquely found in the eROSITA catalog, while 36%, 9%, and 4% are selected from XMM-Newton, Swift, and ROSAT, respectively. Color-color diagrams indicate that most candidates are distinct from active stars, though some may be eclipsing binaries rather than CVs. Our results demonstrate that combining X-ray catalog cross-matching with Gaia selection and time-domain analysis is an effective method to identify X-ray-emitting CVs. eROSITA, in particular, uncovers sources missed by other catalogs thanks to its wide sky coverage and high sensitivity. As eROSITA’s flux limit continues to improve, we expect the known population of Galactic X-ray-emitting CVs to expand significantly.

ABSTRACT. Observational data elucidate key characteristics of SEP populations: (i) multi-component composition, (ii) variable elemental abundances, (iii) isotopic diversity, and (iv) diverse ionization states. Analyzing these species' abundances, charge states, and energy distributions offers critical insights into SEP acceleration dynamics. The multi-component, elemental, and isotopic properties are fundamental to understanding SEP acceleration mechanisms. These properties are typically quantified using elemental ratios (e.g., Fe/O, He/H, C/O), isotopic ratios (e.g., ³He/⁴He), and abundances of elements such as electrons, protons, helium, carbon, and other metals within the simulation domain. This study investigates impulsive SEP events driven by fully coupled hydrodynamic-magnetohydrodynamic-kinetic continuous-scale flare-loop systems characterized by significant temporal-spatial turbulence and magnetic reconnection. These events, distinguished by current sheet thicknesses on the order of characteristic electron length scales, exhibit enhanced electron and heavy-ion populations and are associated with type III radio bursts. We developed the multi-component-abundance-isotope model, incorporating a relativistic algorithm and advancing the Relativistic hybrid Particle-in-Cell Lattice Boltzmann Method code. These advancements provide innovative tools for analyzing Langmuir turbulence acceleration driven by nonlinear resonant wave-particle interactions.

ABSTRACT. We present a novel deep-learning-based method, named Galactic-Seismology Substructures and Streams Hunter (GS3 Hunter), designed to search for substructures and streams in stellar kinematics data. GS3 Hunter combines Siamese neural networks to transform phase space information with the K-means algorithm for clustering. As a validation test, we apply GS3 Hunter to a subset of the Feedback in Realistic Environments (FIRE) cosmological simulations. The stellar streams and substructures identified align well with results previously reported by the FIRE team. In a similar vein, we apply the method to a subset of local halo stars from the Gaia and GALAH datasets, successfully recovering several known dynamical groups, including Thamnos 1+2, the hot thick disk, ED-1, L-RL3, Helmi 1+2, Gaia-Sausage-Enceladus, Sequoia, Virgo Radial Merger, Cronus, and Nereus. To investigate the origin of the Gaia-Sausage-Enceladus (GSE), we conduct a chemical dynamical analysis using APOGEE and DESI data. By incorporating chemical information (e.g., [Mg/Fe], [Al/Fe]), we classify the stars into accreted and in-situ populations, the majority of our sample consists of in-situ stars in the Galactic disk region, with a smaller fraction of accreted stars. Finally, we apply GS3 Hunter, without fine-tuning, to a subset of K giant stars from the LAMOST Data located in the inner halo region. We recover three previously known structures (Sagittarius, Hercules-Aquila Cloud, and the Virgo Overdensity), along with the discovery of several new substructures. Our group anticipate that GS3 Hunter will become a valuable tool for the community in the search for stellar streams and structures within the Milky Way (MW) and the Local Group. It will significantly advance our understanding of the inner and outer halos of the MW, as well as the galaxy’s assembly and tidal stripping history. This contributed talk will also highlight recent progress in the accretion history of the MW.

ABSTRACT. High-redshift (z > 5.5) quasars probe the earliest phases of supermassive black hole (SMBH) growth, when the Universe was less than one billion years old. The existence of billion-solar-mass black holes at such early epochs challenges standard growth models, particularly regarding the formation, collimation, and evolution of relativistic jets in young galaxies. While optical surveys have significantly expanded the census of high-redshift quasars, their radio properties remain poorly constrained, and the diversity of jet activity in the early Universe is still unclear.

We present a multi-scale radio study of Southern Hemisphere quasars at z > 5.5, combining arcsecond-resolution ASKAP observations from the RACS survey with milliarcsecond-resolution VLBA imaging. We focus on three newly identified quasars, J0322–18 (z = 6.09), J1011–01 (z = 5.56), and J0202–17 (z = 5.57), which exhibit distinct manifestations of radio AGN activity. VLBA imaging reveals compact cores and, in some cases, parsec-scale jet structures, providing direct evidence for early relativistic jet formation. ASKAP monitoring further shows variability, suggesting a range of jet orientations and intrinsic powers.

Our results demonstrate significant structural and phenomenological diversity among high-redshift radio quasars, from blazar-like systems to young, compact sources. This diversity challenges the notion of a homogeneous early AGN population and provides new constraints on SMBH growth, jet triggering, and feedback processes in the first Gyr of cosmic history.

ABSTRACT. Strong Gravitational Lensing offers one of the best probes to understand the nature of dark matter. Massive objects like galaxies bend light from distant background bright sources like Type Ia Supernovae and Quasars, resulting in the formation of multiple images of the background source. The positions and magnifications of these images depend on the matter distribution of the lensing object, most of which is dark matter, allowing us to use the images to constrain the lens dark matter profile. In order to do so, we need to construct a model of the matter profile of the lensing object that can accurately predict the observed positions and magnifications of the lensed images. Initially, lens models comprised a single component to model a galaxy's mass. However, such models would leave position and magnification anomalies – meaning they were unable to reproduce the lensed image properties within errors. Thus, models were made with a secondary component – an external shear, meant to account for changes in the lens potential by mass along the line of sight or from a nearby deflector close to the lens. The addition of an external shear often completely resolves position anomalies in almost all lens models. At present, lens models are even more complex, sometimes with four or more components; however, the external shear component remains a commonality. Recent work has shown that the shear strength being implemented across the literature is much stronger than what is expected from weak lensing. Other recent work has demonstrated that the shear being invoked to resolve anomalies in isolated systems is indistinguishable from that of lenses in cluster environments. In this work, we investigate the effect of external shear on lens models using mock strong lenses generated from the IllustrisTNG simulations to understand why shear is able to resolve lensing anomalies so well. We find that the external shear behaves like a fitting function in that it adjusts the macro model component to generate a configuration of lensed images where the external shear perfectly compensates to resolve anomalies. The abnormally large shear strength is because the shear is responsible for much more change in the lens potential than can be physically accounted for. Furthermore, we explore the external shear parameter space and find numerous degeneracies, as well as tight relations between the external shear and macro model parameters. All of this points to the unphysical nature of external shear. This is problematic as all lens models in recent literature include external shear as an ingredient with unphysical shear strengths similar to what we get in this work. This brings into question the validity of all recent lensing studies and reintroduces a problem that was long thought to be solved – that of lensing anomalies.

ABSTRACT. We present an extension of the High-z Evolution of Large and Luminous Objects (HELLO) simulations, designed to investigate the formation and evolution of galaxies up to z \simeq 4.5. Building on the original HELLO framework, this work explores the physical processes that shape the early growth of galaxies, including dark matter assembly, gas accretion, star formation, and feedback. The extended simulations enable a detailed examination of how structural and dynamical properties evolve in the first 1.5 billion years of cosmic history. We analyze the relation between stellar mass, star formation rate (SFR), and halo properties to trace the emergence of scaling relations at high redshift and assess their consistency with ΛCDM predictions. Comparisons with recent JWST observations show strong agreement in stellar mass build-up, SFR evolution, and size–mass relations, indicating that the HELLO framework captures the key mechanisms governing early galaxy formation. This work expands the redshift reach of the HELLO project and provides theoretical insight into the rapid assembly and evolution of massive galaxies in the early Universe.

ABSTRACT. Understanding how galaxies assembled, from the formation of the first stars to the diverse population we observe today, remains one of the central challenges in galaxy evolution. Recent JWST surveys have unveiled a rich population of early star-forming, emission-line galaxies, providing an unprecedented window into the physical conditions of galaxies at high redshift. In this talk, I will present a semi-analytic framework that jointly constrains the ISM pressure ($P_{\mathrm{ISM}}$), ionization parameter ($q$), and gas-phase metallicity ($Z$) for galaxies at $6 \leq z \leq 11$. Our model incorporates turbulence driven by gas accretion and supernova feedback, and is calibrated to reproduce the observed [O\,III] luminosity function. We find that turbulence plays a fundamental role in regulating ISM conditions, driving systematic increases in both $q$ and $P_{\mathrm{ISM}}$ toward earlier cosmic times, while requiring higher metal retention during supernovae to match the relatively elevated metallicities implied by JWST observations.

Building on these results, we use updated stellar evolutionary tracks coupled with the MAPPINGS photoionization code to generate synthetic spectra across the full parameter space inferred from the simulations. With these spectra, we develop new emission-line diagnostics complementary to studies at lower redshift, that probe unexplored regions of $(P_{\mathrm{ISM}}, q, Z)$, calculated from our semi-analytic model. These diagnostics are designed specifically for the extreme conditions of early galaxies and will significantly improve metallicity and ionization estimates for high-redshift sources observed with JWST, and lays the groundwork for future spectroscopic studies enabled by the SKA.

ABSTRACT. The Rubin Observatory’s LSST will deliver ugrizy photometry for an unprecedented number of galaxies, enabling population-scale investigations of galaxy formation and evolution. Extracting robust physical parameters—such as stellar mass, star-formation rate, metallicity, dust content, and star-formation histories—from broad-band data remains challenging, not least because these quantities depend sensitively on modelling assumptions and on the limited wavelength coverage available in LSST alone. In this talk, I will present an assessment of these challenges using a cross-matched sample of approximately ten thousand galaxies from LSST Data Preview 1 and the MUSYC survey, which provides extended optical–near-infrared coverage. The two datasets show excellent photometric consistency, allowing a clean investigation of how far ugrizy photometry alone can constrain fundamental physical properties, and where additional bands or stronger priors become indispensable. I will discuss the stability of inferred quantities under different assumptions, the impact of filter completeness, and the practical limits imposed by broad-band SED fitting. Finally, I will introduce a browser-based interactive SED-grid tool designed for rapid exploration of high-dimensional model spaces, useful both for developing LSST-scale pipelines and for building intuition about parameter sensitivities.

ABSTRACT. The exponential growth of astronomical datasets offers humanity an extraordinary opportunity to deepen our understanding of the Universe. However, the effective analysis of such vast amounts of data poses a considerable challenge. Citizen science initiatives, like those hosted on the Zooniverse platform, provide one potential solution to address this issue. In this presentation, I will introduce China's first citizen science platform for astronomy, which has been launched at the National Astronomical Data Center of China. This platform features approximately ten projects focused on comets, stars, supernovae, the Milky Way, galaxies, and beyond. To enhance citizen engagement, we have also developed a smartphone portal for the platform via the WeChat mini-app. Furthermore, I will discuss the future of citizen science, including its opportunities and challenges, and how it will be enriched by innovative techniques such as Internet of Things, Artificial Intelligence, and Virtual Reality/Augmented Reality/Mixed Reality technologies.

ABSTRACT. As the former Head of the IAU Office for Astronomy Outreach (OAO) who drafted the IAU strategic plan and a current member of the WGSN (Star Names) and CAP (Communicating Astronomy with the Public) Commission, the author occupies a unique position at the intersection of international policy and local practice. This presentation explores the "implementation gap"—the friction that occurs when high-level global resources and naming conventions meet the practical, socio-economic, and cultural realities of a local observatory in a high-density urban environment like Hong Kong.

While the IAU provides robust tools and standardized frameworks, local practitioners often encounter a sense of indifference toward "top-down" initiatives that do not immediately align with local needs. Drawing on recent experiences with STEM education projects and observatory facility upgrades in Hong Kong, this talk will address:

1. The Relevance Gap: Identifying which IAU resources "stick" at the local level and which are perceived as too abstract. 2. Cultural Resonance: How working groups like the WGSN can serve as a bridge by validating local heritage and Chinese astronomical culture, making "global" astronomy feel "personal." 3. The Local Reality: The challenges of hardware upgrades and STEM curriculum integration in a city where light pollution and competitive academic environments dictate public interest.

The session concludes with a call for "Bi-directional Outreach"—moving beyond the dissemination of tools to a model where local obstacles actively reshape global policy.

ABSTRACT. Since 2016, the Overseas Education Support Team of the Korean Astronomical Society has organized seven Astronomy Camps in Cambodia, with a pause during the COVID-19 pandemic (2020–2022). The camps initially targeted students and high school teachers in underserved northern provinces, including Pursat and Banteay Meanchey. Guided by the motto, “Through astronomy, we inspire children with limited access to education to explore new scientific horizons and dream about their future on the scale of the Universe”. Due to its relatively low infrastructure requirements, astronomy offers a unique opportunity to deliver high-impact science education in resource-limited settings, making it a powerful and accessible tool for educational outreach. Since 2023, the initiative has expanded to the Royal University of Phnom Penh, engaging about 40 undergraduate and graduate students annually. This effort supports a long-term goal of establishing formal astronomy courses and a sustainable academic program. We will present the program’s progress, outcomes, and future plans for strengthening astronomy education in Cambodia.

ABSTRACT. The Bosscha Observatory is now more than a century old. At the time of its establishment, it was one of only three astronomical observatories in the Southern Hemisphere. Today, Bosscha Observatory is designated as a national vital object, a national cultural heritage site, and a nationally strategic area. The International Astronomical Union (IAU) has recognized Bosscha Observatory as one of the outstanding sites of astronomical heritage. Light pollution currently represents the dominant threat to the observatory’s continued functionality as an active laboratory for astronomical research, education, and public outreach. Economic pressures for regional development are particularly intense, given that the observatory is located within a major tourism area. Compared with other forms of environmental degradation—such as air, water, soil, or even noise pollution—light pollution remains relatively under-recognized and poorly understood by the general public, including many residents living in the immediate vicinity of Bosscha Observatory. Although various regulations have been issued by governmental authorities, their implementation and enforcement remain weak. Public outreach and education efforts are ongoing; however, it has become increasingly evident that the adopted approaches cannot be centered solely on the interests of the observatory. To secure sustained societal support for its scientific and educational functions, the observatory’s presence must be perceived as delivering tangible benefits to the surrounding communities. This presentation will discuss a range of strategies undertaken to safeguard the role and functions of Bosscha Observatory, with particular emphasis on collaborative initiatives involving schools, the Family Welfare Movement (a community organization that empowers women to participate in Indonesia’s development), environmental activists, and local government.

ABSTRACT. MissionMaker is an AI-based learning platform that helps students create and explore their own space missions in a simple and fun way. Students can choose a planet or moon, design a basic spacecraft, and set the goals for their mission. The platform guides them step by step so they can understand how real missions are planned. A special feature of MissionMaker is that students can also perform analog missions, hands-on activities that match the digital missions they design. They can build small models, plan rover paths, or try simple experiments that imitate space tasks. These activities make learning more engaging and help students understand concepts better. MissionMaker aims to make space education easy, creative, and enjoyable for all learners.

ABSTRACT. Research results and progress in space manufacturing

ABSTRACT. Research progress and achievements in the field of artificial intelligence for space science and applications

ABSTRACT. The SKA Observatory is constructing two next-generation complementary radio telescopes: SKA-Low in Australia (50–350 MHz) and SKA-Mid in South Africa (350 MHz–15.4 GHz). When completed later this decade, they will be the most sensitive facilities in their respective frequency ranges. Both instruments are now entering the science commissioning phase. SKA-Low has achieved its 4-station interferometry milestone and is progressing toward the next phase (16 stations), while SKA-Mid, following the successful detection of its first interferometric fringes and phase closure test earlier this year, is now beginning its 4-dishes interferometry stage. I will outline the science commissioning approach and highlight early technical and scientific results.

The talk will then focus on SKA-Low, a phased aperture array located in the Murchison region of Western Australia that will ultimately comprise 512 stations distributed over baselines up to 74 km. With a ten-station array currently operational, SKA-Low commissioning activities include: system stability, calibration verification, beamforming validation, pulsar detections, sensitivity assessments, first interferometric images, and a calibrator surveys plan. I will highlight commissioning progress and plans for upcoming test phases, that are paving the way toward science verification, early science operations, and SKA-Low’s transformational low-frequency science.

ABSTRACT. The first major scientific milestone of Science Verification, which will provide the first user access to SKA data, is now on the horizon. In this hugely exciting stage, we will be calling for Science Verification target ideas from the community and releasing the datasets publicly to ensure verification of the scientific capability, overall workflow and usability of our systems. In this talk I will discuss everything you need to know about this stage: the expected timelines, availability of modes and capabilities, the process of the call for ideas, details of the datasets and their delivery as well as expected resource availability on the SRCNet.

ABSTRACT. Significant progress is being made with the construction of the SKA-Low telescope in Australia at Inyarrimanha Ilgari Bundara, the CSIRO Murchison Radio-astronomy Observatory site. The current schedule has SKA-Low to be the first SKAO telescope to undergo Science Verification, with a telescope that will surpass current comparable radio astronomy facilities. I will discuss the specifics of SKA-Low Science Verification as relevant to the community, including initial observing targets.

ABSTRACT. When complete, the SKA telescopes will be highly flexible instruments enabling a diverse range of science goals. In this talk, I will present the capabilities of the SKA telescopes in steady-state operations, including array layouts, observing modes, multibeam capabilities, and templates for subarrays and substations. I will also introduce several user-facing tools (like the sensitivity calculator and subarray simulation tool) that SKAO has released to the community.

ABSTRACT. The combination of SKAO and SRCNet will provide users with an end-to-end system spanning the full lifecycle of a project; from proposal preparation through data product delivery to the SRCNet, where users will have access to resources to analyse and create publishable data products. A range of support options will be available to users to aid them at every stage of their project.

The SKA Helpdesk is the cornerstone of the user support model and will serve every aspect of the users needs: a unified Helpdesk where users can access assistance from both the SKAO and the SRCNet. The SKA Helpdesk is supported by the Science Portal, which provides users with a variety of self-service support options, including a thorough documentation library, FAQ, and a range of training materials.

This talk will provide an introduction to and overview of the current and soon-to-be-launched support options available for future SKA users and the wider community.

ABSTRACT. Relativistic jets emanating from active galactic nuclei (AGNs) play a pivotal role as a feedback mechanism in the Universe, and the cosmic rays (CRs) carried by AGN jets can have profound influence on galaxy properties and the circumgalactic medium. Consequently, self-consistent modeling of CR propagation, spectral evolution, and emission mechanisms is imperative for understanding the thermal and non-thermal emissions of galaxies. We employ advanced 3D CR-magnetohydrodynamic simulations to elucidate that the multi-wavelength observations of the Fermi and eRosita bubbles within the Milky Way can be accounted for by past activity of Sgr A*. We investigate the feasibility of generating symmetric bubbles through the interaction of oblique AGN jets with the dense Galactic disk. We posit that, when viewed head-on, AGN jet-inflated bubbles may provide a plausible explanation for the recently identified enigmatic odd radio circles (ORCs). We further test this AGN bubble scenario of ORC formation using semi-analytical models and show that the predicted number of ORCs is consistent with that found by existing surveys. These works advance our understanding of CR jet feedback and their influence on various astrophysical phenomena within our cosmic neighborhood.

ABSTRACT. We investigate binary major mergers of galaxy clusters with mass ratios below 3 using three-dimensional magnetohydrodynamic simulations that include cosmic-ray (CR) electron acceleration through diffusive shock acceleration. In addition to synchrotron, inverse-Compton, and Coulomb cooling, we assess the effects of postshock magnetic turbulence via Fermi-II acceleration, modeled through simplified momentum diffusion. Equatorial shocks prove generally weaker than the two axial shocks and contribute negligibly to the total CR energy. Shock 1, propagating ahead of the heavier subcluster, is more compact yet exhibits a higher mean Mach number and kinetic-energy flux than Shock 2, resulting in greater CR-electron energy density. Consequently, unequal-mass mergers generate asymmetric double relics, with the more compact, stronger Shock 1 appearing brighter than Shock 2 owing to its elevated Mach number and amplified magnetic fields. This asymmetry contrasts with findings from certain cosmological simulations, suggesting that local intracluster medium conditions—such as turbulence and filamentary inflows, plus subsequent minor mergers—profoundly shape shock characteristics. Furthermore, the observed morphology and brightness of radio relics vary sharply with viewing angle, dramatically altering their apparent shape and contrast.

ABSTRACT. Pulsar radio emission exhibits variations over a wide range of timescales, spanning from months down to the nanosecond level. One of the shortest timescale variations among these, known as microstructures (MSs), is a distinctive feature that has been discovered in the emission from a variety of pulsars. While the microstructures manifest as narrow, often quasi-periodic, artifacts in numerous individual pulses of a pulsar, not all pulses exhibit this characteristic. The study of these structures can provide valuable information to understand the pulsar emission mechanism. However, the manual hunt for these structures in a time series containing thousands, and sometimes millions, of pulses is a laborious and time-intensive task. To address this challenge, we have developed QMIST, a Python-based pipeline designed to search for pulses that exhibit quasi-periodic microstructures in pulsar time series data. We provide a comprehensive description of the algorithm used in our pipeline along with its caveats. Using QMIST, we showcase and discuss the results from a survey of microstructures in 26 normal, mostly young, pulsars observed across both northern and southern hemispheres.

ABSTRACT. Fast Radio Bursts (FRBs) offer one of the most compelling astrophysical puzzles of the past decade, yet the key to understanding their origins may lie in the nearby Universe. The growing sample of well-localized FRBs, particularly at distances where host-galaxy environments can be resolved in detail, is transforming our view of their progenitor channels. In this talk, I will present a unified perspective that combines host-galaxy constraints, population-level statistics, targeted searches in local galaxies, and multi-wavelength analogs to illuminate the physical pathways that can give rise to FRBs.

I begin by examining host-galaxy demographics from recent surveys, highlighting trends in stellar mass, metallicity, star-formation activity, and local environment that emerge from CHIME/FRB, ASKAP, and MeerKAT localizations. These observables already point toward diverse formation channels, with evidence for both young magnetars formed in recent core-collapse supernovae and older compact-object populations in more quiescent environments. By explicitly incorporating archival connections with historical supernovae, ultraluminous X-ray sources, and globular cluster catalogues, I will show how multi-wavelength proxies for compact-object activity can be leveraged to place novel constraints on potential FRB progenitors in the nearby Universe.

I will then discuss how complementary searches for FRB emission from known local galaxies—ranging from star-forming spirals to dwarf irregulars and globular cluster systems—set independent limits on burst rates, energetics, and beaming. These searches not only contextualize the environments where FRBs do occur, but also highlight regions of parameter space where they do not, tightening constraints on formation channels and duty cycles.

A key theme of this synthesis is the identification of several missing links that remain inaccessible to current GHz-frequency surveys. Wide-field instruments suffer from scattering biases and limited localization precision, obscuring the role of dense local environments and preventing definitive associations with progenitor signatures. I will highlight how higher-frequency observations, emerging mid-frequency arrays, and next-generation wide-field facilities expected in the Asia-Pacific region can break these degeneracies. These capabilities offer improved sampling of compact, weakly scattered bursts, more precise localization, and the ability to probe fainter and older stellar environments than current surveys.

Finally, I will outline the rapidly expanding multi-messenger potential of local-Universe FRBs. Coordinated optical and X-ray monitoring of bursts from nearby hosts, coupled with synergies with gravitational-wave detectors, provides a realistic pathway for distinguishing between young magnetar, accreting compact-object, and dynamical formation scenarios. These joint approaches bridge the gap between electromagnetic and non-EM probes and will be essential for identifying the true diversity of FRB origins.

Together, these threads demonstrate that the convergence of radio surveys, local-galaxy studies, archival multi-wavelength constraints, and emerging multi-messenger opportunities positions the local Universe as the most powerful laboratory for solving the FRB progenitor problem.

ABSTRACT. This research investigates the relativistic spherical accretion through a dynamical analysis of a generalized Hamiltonian for static, D-dimensional Reissner-Nordström (RN) Black Holes (BH). We consider two different fluid models, namely, an isotropic fluid characterized by a linear equation of state and a non-linear polytropic fluid, to analyze the critical points in a D-dimensional RN BH. The flow dynamics of the fluids are studied in different spacetime dimensions in the framework of Hamiltonian formalism. The isotropic fluid is found to admit both transonic and non-transonic flow behavior, but in the case of polytropic fluid, the flow behavior is found to exhibit only non-transonic flow, determined by a critical point that is related to the local sound speed. A primary focus of this study is the impact of higher spacetime dimensions (D) on accretion processes. The study shows that the critical radius exhibits a non-monotonic behavior: as the dimension increases from D = 4, the critical radius decreases to a minimum at D = 8 or D = 9 (depending upon the state parameter of the fluid) and thereafter increases again. The event horizon radius for the RN BH is also found to follow the same trend. The mass accretion rate also shows different levels of dependency on dimensionality, depending on the state parameter of the fluid. The accretion rate for ultra-stiff fluids (\omega = 1) decreases as dimensions increase, but it rises for ultra-relativistic (\omega = 1/2) and radiation fluids (\omega = 1/3). The flow behavior and mass accretion rate for a change in the BH charge parameter are also studied. An increase in the charge parameter leads to a decrease in the critical radius but an increase in the critical Hamiltonian. It is noted that the maximum mass accretion rate in a higher-dimensional Schwarzschild BH is the lowest, which, however, increases with the increase in charge parameter in a higher-dimensional RN BH. These results highlight the significant impact of extra dimensions and charge on the kinematic and thermodynamic properties of accretion flows.

ABSTRACT. India’s AstroSat UltraViolet Imaging Telescope (UVIT) offers sub-arcsecond ultraviolet imaging, providing a powerful means to trace recent star formation across a wide range of cosmic environments. This talk presents recent UVIT results that examine star formation in secularly evolving spiral galaxies, interacting and merging systems, and dense cluster environments. Spatially resolved UVIT observations of nearby spirals reveal age and stellar mass distributions consistent with inside-out disk growth, while studies of interacting galaxies demonstrate both localized and global star formation enhancements associated with bar dynamics, interaction mass ratios, and merger stage. In cluster galaxies, UVIT observations—combined with PHANGS–HST and ALMA data—probe the onset of ram-pressure stripping and reveal spatial variations in recent star formation histories, and joint analyses with JWST mid-infrared diagnostics link star formation surface density to PAH grain properties and feedback processes. UVIT studies of polar ring galaxies further provide spatially resolved constraints on stellar populations, tracing evolutionary pathways from actively star-forming to transitioning systems, and collectively underscore UVIT’s unique role in tracing star formation across cosmic environments.

ABSTRACT. Recent JWST observations have revealed an unexpected abundance of bright galaxies at z ≳ 12, both in the UV and as Lyman-α emitters, challenging standard galaxy formation models and our theoretical expectation of reionization in the early universe. Using a semi-analytic galaxy formation model, we find that while faint JWST galaxies align with predictions, bright galaxies require enhanced star formation efficiencies or hosting Population-III stars to be reconciled with theory. We also explore the detectability of Lyman-alpha emission from these galaxies by integrating galaxy formation models with IGM reionization simulations. Our results indicate that intrinsic velocity offsets and reionization morphology significantly impact Lyman-alpha visibility, with low-mass galaxies driving reionization boosting detectability, as seen in JADES-GS-z13-1-LA (z = 13). Our findings underscore the need for spectroscopic follow-ups, improved reionization modeling, and refined simulations to accurately interpret JWST’s high-redshift discoveries.

ABSTRACT. Detecting low surface brightness galaxies, such as dwarf ellipticals (dEs), remains one of the most persistent challenges in modern astronomical surveys. Their diffuse morphology and low luminosities often cause them to be missed by traditional source extraction algorithms. We have built a deep learning framework based on a modified region-based convolutional neural network combined with a CNN classifier, designed to robustly detect and classify dEs in wide-field imaging data. As a proof of concept, we apply our method to the Virgo cluster using archival data from the Legacy Survey, generating a homogeneous and statistically significant catalog of dEs across the entire cluster and recover key structural and environmental distinctions between nucleated and non-nucleated dEs, revealing contrasting spatial correlations with massive galaxies and the intracluster medium. We expect that our method is also well-suited for next-generation deep imaging surveys such as Euclid, which will require scalable, morphology-sensitive tools to uncover the low surface brightness universe on cosmological scales.

ABSTRACT. The circumgalactic medium (CGM) surrounding galaxies constitutes ~50% of the baryonic matter within their dark matter haloes, serving as a massive reservoir of star-forming fuel. Studying the distribution and flow of this diffuse gas in and around galaxies is crucial for understanding galaxy evolution and addressing various problems in galactic astrophysics. CGM analyses typically measure the distribution of cool gas using absorption lines in the spectra of bright background sources such as quasars. However, the relatively small cross-section area of quasar sightlines necessitates averaging over multiple quasar-galaxy pairs to study spatial variation, leading to a crude statistical picture of the CGM. Recently, gravitationally lensed images of background galaxies have been used to illuminate the CGM of foreground galaxies along the line of sight. This technique, known as gravitational arc tomography, probes the CGM with a significantly larger cross-section than quasar sightlines, enabling investigation of the spatio-structural and kinematic properties of the CGM at the level of single galaxies.

In this talk, I present the results of an arc tomographic investigation of gas flows in the CGM of an inclined disc-like intervening galaxy at z~0.86 along the line-of-sight to the lens system AGEL152509. Using KCWI integral field spectroscopy, we detect Mg II 2796,2803 and Fe II 2857,2600 absorption lines at z~0.86 in the spectrum of 3 lensed images of a background galaxy and map the metal-enriched gas traced by this absorption at impact parameters of 5 to 25 kpc. I discuss how the anti-correlation between the rest-frame Mg II equivalent width and impact parameter observed in multi-galaxy quasar absorption studies is reproduced with significantly less scatter for a single galaxy. I also discuss the kinematics of the metal absorbers, which reveal circumgalactic gas co-rotating with the absorber galaxy and a flat rotation curve with relatively little scatter. The rotation speed of the CGM gas is consistently lower than the maximum rotation speed extrapolated from morpho-kinematic modelling of the [O II] emission from the galaxy, indicating that the observed co-rotation could be driven by gas accreting onto the galaxy. Finally, I discuss the detection of a blueshifted component in the Mg II absorption profiles of one of the lensed arcs that is kinematically consistent with the Mg II absorption in the down-the-barrel spectrum of the absorber galaxy, and may represent star-formation driven outflows. Through these spatially resolved observations of the CGM made possible by gravitational lensing, I highlight the potential of arc tomography to spatially map inflows and outflows — major processes in the much coveted baryon cycle — around an individual galaxy.

ABSTRACT. The physical conditions of the interstellar medium (ISM) are fundamental to understanding galaxy formation and evolution, as they trace the cumulative history of star formation and gas flows. Bright nebular emission lines serve as powerful diagnostics of these conditions, underpinning key scaling relations such as the mass-metallicity relation and the widely used strong-line calibrations of gas-phase metallicity. However, the underlying nebular physics that governs these relations remains poorly constrained. The Comprehensive IFU Research on Accurate Abundance Studies (CIRAAS) survey utilizes deep integral field spectroscopy (IFS) with Keck/KCWI to map nearby H II regions with unprecedented precision. Combined with complementary far-infrared data from SOFIA and Herschel, CIRAAS provides a unique window into the detailed thermal, ionization, and chemical structure of ionized gas. Early results from Mrk 71, Haro 3, and M42 reveal striking deviations from the classical “gold standard” metallicity diagnostics, suggesting that conventional gas-phase abundance measurements may be systematically biased by as much as a factor of two. The complete CIRAAS sample of 25 nearby star-forming regions and dwarf galaxies spans a wide range of physical environments. It will provide a robust empirical foundation for recalibrating metallicity diagnostics and establishing a truly accurate abundance scale applicable across cosmic epochs.

ABSTRACT. The Hubble Space Telescope Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey(CANDELS) fields offer an exceptional combination of depth, spatial resolution, and area for identifying a shear-selected sample of dark matter overdensities. We present the first infrared weak lensing analysis of the five HST CANDELS fields: COSMOS, UDS, EGS, GOODS-N, and GOODS-S. Our analysis identifies 11 shear-selected overdensities that span masses from M200 = (0.2 – 2.2) × 10^14 M⊙, with a median mass of M200 = 5.0 × 10^13 M⊙. The systems lie at redshifts 0.22 < z < 0.9 with a mean redshift of z = 0.65. Seven of the overdensities have diffuse X-ray emission reported in literature with X-ray centroids that are in spatial agreement with our weak-lensing peaks, which confirms their nature as collapsed structures. By stacking the tangential shear of all detections, we determine the average radial mass density profile and find that it is well-fit by an NFW model with concentration of 4.9 ± 2.11 and M200 = 1.3 ± 0.3 × 10^14 M⊙.

ABSTRACT. TBA

ABSTRACT. Black holes have been the most mysterious objects in the universe. Although people are fascinated about how black holes are formed and how they evolve and why they are related to the origin of the universe, these massive-mass but small-size objects still remain a mystery to the general public. Based on major discoveries in cosmology and astrophysics, this talk will give a brief history of scientific development in black holes. It will cover both theoretical development and observational discoveries as well as major scientific findings related to black holes, for example, the discovery of the cosmic microwave background radiation and the observation of gravitational waves. Built upon the Chandrasekhar limit, this talk will also discuss under what conditions a black hole can be formed and how it will affect the surrounding space and time from the perspective of theory of general relativity. This talk will contribute to Stephen Hawking’s legacy in his groundbreaking scientific research in cosmology and his profound ability to communicate complex ideas to the public, especially his astoundingly successful book "A Brief History of Time" (1988) which was translated into some 40 languages and sold over 25 millions of copies worldwide.

ABSTRACT. The exponential growth of astronomical data from various surveys—spanning images, spectra, and time-domain light curves—presents unprecedented opportunities and challenges for analysis and discovery. Traditional methods, reliant on specialized, siloed rules and models, struggle to integrate these heterogeneous modalities, limiting insights into cosmic phenomena such as stellar variability, and galaxy evolution. To address this, Zhejiang Lab, in collaboration with the National Astronomical Observatories, Chinese Academy of Sciences (NAOC), has developed OneAstronomy, a pioneering AI foundation model ecosystem designed to decode the language of the cosmos through native multimodal understanding and scientific reasoning.

The first version of OneAstronomy, released in April 2025 as a 70-billion-parameter LLM, adopts a hybrid architecture that seamlessly processes natural language, time-domain, and spectral inputs, enabling knowledge and reasoning akin to a PhD-level astronomical assistant. Trained on a curated corpus exceeding 36 billion tokens—including 32 billion astronomical-specific tokens from 300,000 reviewed websites and annotated Common Crawl data, as well as other mathematical, code, and reasoning data—OneAstronomy excels in complex problem-solving, such as FRB energy estimation based on FAST observation. Astronomy-specific benchmarks such as GPQA-astro, SuperGPQA-astro, AstroBench-MCQ, and a carefully curated question set GuoTai-TianYi show that OneAstronomy matches or surpasses frontier general-purpose models in both knowledge and reasoning accuracy with a much smaller model scale. In practice, this allows astronomers to interact with OneAstronomy through natural language for tasks such as problem setup, literature synthesis, hypothesis checking, and quantitative back-of-the-envelope calculations, enabling AI-assisted research workflows. Two additional scientific agents further enhance its capabilities: FALCO, a 1.4-billion-parameter foundation model for light curves, achieves 95% accuracy in stellar variability classification and 87% in flare detection achieved through self-supervised training on ~150,000 Kepler light curves. SpecCLIP, a CLIP-inspired aligner model, bridges the resolution gap between LAMOST and Gaia XP spectra, enabling translation between spectral types and the estimation of stellar parameters, including atmospheric parameters, elemental abundances, and asteroseismic parameters.

Looking ahead, the new OneAstronomy-Omni envisions a unified native multimodal foundation model, embedding unstructured data of different modalities into one token sequence via a universal tokenizer. OneAstronomy-Omni, pretrained on the multimodal dataset from various surveys (Legacy Survey, DESI, SDSS, Gaia, ZTF, etc.), learns the cross-modality relationships and promises data efficiency for regression, segmentation, and retrieval, tackling grand challenges in cosmology, dark matter, and exoplanet evolution. Through multimodal masked encoding and scientific chain-of-thought training, OneAstronomy-Omni adopts the 021 Science Foundation Model and integrates the complex, heterogenous data with scientific reasoning for emergent physical understanding, enabling zero-shot discovery of rare objects like gravitational lenses and generative tasks such as spectral super-resolution.

OneAstronomy is publicly accessible via https://oneastronomy.zero2x.org/. By democratizing AI-driven analysis, OneAstronomy bridges data-driven discovery with theoretical astrophysics, empowering interdisciplinary collaborations for transformative insights into the universe's origins and dynamics.

ABSTRACT. Astronomy education often presents challenges for young learners due to its abstract concepts and reliance on visualization skills, highlighting the need for engaging and accessible teaching tools. To address this issue, this study introduces AL-KAHF, an interactive educational card game designed to enhance interest, understanding, and active participation in astronomy learning. The aim of this article is to examine how the game’s hybrid structure combining traditional card-based mechanics with interactive elements supports conceptual development in astronomy. The problem driving this research is students’ limited exposure to astronomy and their difficulty visualizing celestial phenomena through conventional instruction. Using a qualitative approach, data were collected through facilitator observations, informal feedback sessions, and reflections from participants across primary, secondary, and university levels during structured outreach activities. Analysis focused on behavioural engagement, conceptual responses, and perceived usefulness of the game. Findings indicate that AL-KAHF effectively fosters curiosity, encourages peer collaboration, and simplifies complex ideas through an enjoyable, inquiry-driven experience. Participants valued the game’s interactive format, noting that it made astronomy more relatable and less intimidating compared to textbook-based learning. The study suggests that integrating game-based learning into astronomy education can broaden access, support STEM engagement, and cultivate early scientific interest. Future research should explore long-term retention effects, adaptation of the AL-KAHF framework for other astronomy topics, and scalability of the tool for classroom use. In conclusion, AL-KAHF demonstrates strong potential as an innovative educational resource that bridges conceptual gaps, enhances motivation, and supports meaningful learning in astronomy.

ABSTRACT. Occultation observations, in which the Moon or asteroids hide background stars, have long been a popular activity among amateur astronomers. Recently, however, these observations have also begun to attract the attention of researchers. This is due to the significantly improved accuracy of asteroid occultation predictions for two reasons: First, the Gaia satellite's precise positional measurements of faint stars down to magnitude 16. Second, all-sky surveys with large telescopes increased the orbital accuracy of asteroids. Observing asteroid occultations can directly measure an asteroid's precise shape and size without assumptions or modeling. Occultation observations have contributed significantly to planetary flyby missions such as NASA's New Horizons, Lucy, and JAXA's DESTINY+. Consequently, a global network of researchers and amateur astronomers has formed to observe asteroid occultations. The International Occultation Timing Association-East Asia (IOTA/EA) is part of this network. Because the phenomenon of a star vanishing in front of people's eyes is fascinating, asteroid occultations are ideal targets for public observatories, high school and university stargazing events, and astronomy club meetings. Since the asteroid's occultation path extends into neighboring countries, cross-border collaborative observations are possible. By encouraging everyone to observe, measure, and learn these principles, we hope to promote astronomy education that transcends borders and generations.

I'd like to have a poster presentation.

ABSTRACT. Introduction: Planetary science research provides profound insights into solar system formation, yet its complexity often renders it inaccessible. Bridging this gap requires pedagogical models that maintain scientific authenticity while being adaptable for educational audiences. This work presents a framework for translating primary research data into structured STEM learning experiences. Method: The Research-to-Classroom (R2C) Framework: a three-stage curriculum design model derived from the author's background in mineralogical analysis of carbonaceous chondrites and Martian meteorites is proposed: 1. Core Narrative Identification: Distilling a research project into its fundamental scientific story (e.g., planetary accretion and differentiation). 2. Data Scaffolding: Systematically simplifying complex datasets (e.g., BSE imagery, EPMA maps) into relatable educational tools while preserving evidentiary value. 3. Hypothesis-Driven Engagement: Designing activities where learners act as investigators, building conclusions from scaffolded evidence. Results: The framework is applied to meteorite mineralogy, transforming research on CM carbonaceous chondrites into a "Planetary Detective" activity. Students utilize a scaffolded "Meteorite Mineralogy Kit"—based on authentic mineralogical data—to categorize meteorite samples (e.g., chondrite, achondrite, carbonaceous chondrite) and match them to planetary formation scenarios. This process requires learners to articulate evidence-based reasoning, mirroring the scientific practice of constructing narratives from physical data. Conclusion: The Research-to-Classroom (R2C) Framework effectively transitions students from passive recipients to active investigators. It enhances STEM literacy by modeling the scientific process, fosters critical thinking through evidence-based reasoning, and provides a scalable model for integrating frontier research into educational contexts. This approach demonstrates how authentic data can create a tangible connection between the classroom and the forefront of planetary exploration.

ABSTRACT. The global space sector moves toward the New Space era driven by commercialization and resource exploitation, where AI robotics will play central roles and be directly responsible for meeting stringent requirements in cost, operability, reusability, and sustainability of long-lived assets in the harsh space environments. This talk will present some latest research work and technology development involving robotic vision, machine learning and biomimetic mechanisms, appliable to mission scenarios such as formation flying, on-obit assembly, active debris removal, planetary sample return and ISRU, etc.

ABSTRACT. Space has ceased to be exclusively about rockets, satellites and other hardware. The most valuable product is services (remote sensing data, satellite Internet, navigation, analytics), as well as the ability to provide consumers with products and services with a space component. Today, the organization that wins is not the one with more engineers, but the one where engineering is "stitched" with law, economics and international relations. This is exactly what the global frontier looks like now — from lunar cooperation programs to international missions, where the key role is played not by formal attributes (for example, identification markings), but by compliance with general rules and the quality of services provided. The current development of events may lead to a situation where space debris can become either an apple of discord or a bone of contention. The nuances of the biblical plots are not so important here, because it is important that before we witness the Kessler syndrome, a "domino effect" may begin in the established system of international space law. A specialised international organization similar to the ICAO should be established in order of achieve sustainability in space activities. In the context of the formation of a new multipolar world order, it is necessary to develop comprehensive approaches to the problem of space traffic management and active space debris removal. The system of international law that has been developed over the decades is beginning to be criticized. The policy of sanctions has not spared space either. Pragmatic cooperation, which was characterized by elements of people's diplomacy at the beginning of man's journey into space, is being replaced by a fierce confrontation that requires an understanding of the intricacies of space diplomacy. Formation of interdisciplinary competencies among future specialists in the space industry through the study of economic, legal, political and communication aspects of international cooperation. Involvement of students and young professionals in the development of the technological base for cleaning near-Earth space from debris. Creating conditions for productive interaction between representatives of engineering, technical and humanitarian fields in order to form global initiatives to solve the problems of pollution of the Earth's orbit. Conducting joint research in the fields of space economics and law aimed at expanding professional skills and improving the employment prospects of graduates. Training of qualified personnel capable of responding quickly to changes in global space management practices and effectively integrating new technologies into the national economy.

ABSTRACT. The telescope Zeiss-1000 of the International astronomical observatory Sanglokh (Institute of Astrophysics of NAST, MPC code 193) in Tajikistan was repaired and upgraded in 2016 after a 26-year period. The observatory with coordinates φ=38.3° N, λ=69.2° E, h=2190 m is located at 120 km from Dushanbe. The astroclimate of this place is one of the best in the territory of the former USSR for optical observations of celestial bodies. Such an astroclimate and the proximity of the observatory both to the equator and to the geostationary libration point of 75° E provide excellent conditions for the space debris’ investigation on the geostationary orbit. From August 2016 to October 2023 on Sanglokh a lot of sessions of observations of space debris were performed within the scientific fields maintained in IA NAST. The paper presents the results of studies of translational-rotational motion and of changes in the brightness of several fragments of space debris moving in the libration mode around the libration point 75° E.

ABSTRACT. SRCNet is crucial to the delivery of SKA science, providing key functionality such as delivering SKA data products to scientists, storing SKA data for future use, computer facilities to undertake scientific analysis and local user support. The first user-facing scientific milestone, Science Verification for SKA-Low AA2 will start in 2027, and it is anticipated that some resources will be made available on SRCNet for analysis. The participation of the SRCNet from the very beginning of Science Verification will be hugely valuable, allowing a first test with a diverse set of users at a reasonable scale, using real SKA datasets, testing SRCNet workflows and providing feedback that will guide future development. I will present an overview of the current status and planning towards Science Delivery within the SRCNet and our combined ambition to ensure an accessible and seamless user experience on SRCNet for the first key milestone of Science Verification and beyond.

ABSTRACT. As a sensitive low-frequency aperture array with a large field of view (FoV), the upcoming SKA1-Low AA* will be an efficient facility for pulsar searches, particularly at mid-to-high Galactic latitudes. Using the Murchison Widefield Array (MWA), the Southern-sky MWA Rapid Two-metre (SMART) pulsar survey acts as an important demonstrator survey for SKA1-Low, providing valuable insights into low-frequency pulsar populations and survey strategies. Despite its high survey efficiency (cover the entire Southern sky in just 94 hours), SMART data processing presents significant computational and I/O challenges, requiring the offline formation of thousands of tied-array beams per observation. With currently available software and local HPC resources, fully processing the survey would take more than ten years. To help address this challenge, and as part of a broader distributed-processing strategy, we have started to process SMART raw voltage data using computing resources in China, in collaboration with the Computer Network Information Center of the Chinese Academy of Sciences (CNIC, CAS). This work demonstrates the feasibility of cross-continental raw voltage data transfer and processing for low-frequency radio arrays, and has already resulted in ten new pulsar discoveries. In the talk, I will also present a pulsar-processing demonstration using the current China SRC infrastructure, which is part of the SRCNet. This demonstration focuses on pulsar timing and is based on a selected Detailed Science Case (DSC) from the SKA-Low AA2 DSC list identified by the SRCNet project scientists.

ABSTRACT. The SKA telescopes will soon be the most powerful radio telescopes in the world with very broad scientific objectives. Science is constantly evolving; the SKA pathfinders and precursors are shaping the scientific landscape in which the SKA telescopes will operate. In this talk, I will give an overview of the SKA science objectives and the plans to get to science delivery. I will discuss recent developments from SKA pathfinders and precursors and how they will determine the long-term future of SKA science. This session will also include contributed SKA science talks from the Asia-Pacific region.

ABSTRACT. When pulsars spin down, most of their rotational energy is carried away by relativistic particle outflow known as pulsar wind. The interaction between the wind and the ambient medium results in a termination shock, where the particles are accelerated up to PeV energies. These ultra-relativistic particles then inflate a bubble in the medium and emit synchrotron and inverse-Compton radiation from radio to X-rays to gamma-rays. Such a structure is referred to as a pulsar wind nebula (PWN). These are important high energy sources in the Galaxy that offer the best laboratories for studying relativistic shocks and the production of cosmic rays. In this talk, I will give a general overview of PWN physics and highlight some recent results from multiwavelength observations.

ABSTRACT. We present a search for new spider pulsar candidates through multi-wavelength cross-matching, including $\gamma$-ray, X-ray, and optical data. A search for sinusoidal-like optical modulations in TESS data of 183 eROSITA X-ray sources coincident with unassociated \textit{Fermi}-LAT $\gamma$-ray sources led to the identification of four promising spider pulsar candidates. We found optical variability periods ranging from 5 to 13 hours. All candidates display smooth sinusoidal-like phase light curves, similar to what can be expected from ellipsoidal variation; one shows double-peaked profiles indicative of harmonics. The absence of sharp minima, which are often found in black widow systems due to irradiation, together with their optical magnitudes of about G $\approx$ 14, suggests these sources are more likely redback-type binaries. One of the Fermi-LAT counterparts is included in a machine-learning catalog of unassociated $\gamma$-ray sources, with relatively high pulsar probabilities. We also identify potential Gaia counterparts for several sources and estimate their distances and luminosities where parallax measurements are available. Future observations, including further spectroscopic and multi-wavelength studies, are needed to fully characterize these systems.

ABSTRACT. Nulling pulsars and rotating radio transients (RRATs) differ hugely in detectability and emission patterns. Nulling pulsars exhibit periodic nulls, with the off-pulse fractions ranging from about 10% to 90%, whereas RRATs are characterised by sporadic bursts, and typically display much higher off-pulse fractions, often exceeding 90%. How are their underlying mechanisms differ or similar?

In this talk, we present the simulation of the distributions of the off-pulse fraction for nulling pulsars and RRATs under the same framework. It begins with our recent observations of PSR B0329+54, which suggest that some pulsar radio emission regions may be segmented. For each segment, we identify the following for changes of the visible emission: (i) Two different radio emission states each can be associated with particular plasma density, and (ii) Changes between radio on and off correspond to changes in the plasma density between two emission states. Our results show that the only difference between nulling pulsars and RRATs is in the default emission, implying a similar origin. The underlying mechanism is likely a random process, which implies that the emission can be different for different nulling pulsars and RRATs. We conclude that the emission may change from RRAT to pulse nulling, and vice versa, as a pulsar evolves.

ABSTRACT. We investigate the optical linear polarization caused by Thomson scattering of the stellar radiation for gamma-ray binary LS I + 61°303, which likely contains a young pulsar. Based on the pulsar binary scenario, we model the interaction between the pulsar wind and stellar wind from the massive companion star, which creates a shock. To accurately compute the resulting polarization of the stellar wind, we develop a method for the Thomson scattering that accounts for the finite size of the companion star. By fitting the optical polarization data, we constrain the system parameters, such as eccentricity, the momentum ratio of the two winds, and mass-loss rate from the companion star. We find that (i) the predicted eccentricity e ∼ 0.1 is smaller than the values derived from the radial velocity curve and (ii) the orbital phase of the periastron is νp = 0.5–0.6, which is consistent with the previous polarization study of Kravtsov et al. Additionally, we estimate the mass-loss rate from the companion star and the momentum ratio of two winds as M 2 × 10 6M yr 1 and η > 0.1, respectively. Assuming that the pulsar wind carries the spin-down energy, the spin-down magnetic field of the putative pulsar inferred from these parameters is of the order of B ∼ 1014 G, which may support the highly B pulsar or magnetar scenario for the compact object of LS I + 61°303. We also discuss the dispersion measure under the predicted orbital geometry and provide a corresponding interpretation of the pulsed radio signal detected by FAST.

ABSTRACT. 2003fg-like Type Ia supernovae (03fg-like SNe~Ia) are rare subtype of SNe~Ia, photometrically characterized by broader optical light curves and bluer ultraviolet (UV) colors compared to normal SNe~Ia. In this work, we study four 03fg-like SNe~Ia using \textit{Swift} UltraViolet and Optical Telescope (UVOT) grism observations to understand their unique UV properties and progenitor scenario(s). We report 03fg-like SNe~Ia to have similar UV features and elemental compositions as normal SNe~Ia, but with higher UV flux relative to optical. Previous studies have suggested that the UV flux levels of normal SNe~Ia could be influenced by their progenitor properties, such as metallicity, with metal-poor progenitors producing higher UV flux levels. While 03fg-like SNe were previously reported to occur in low-mass and metal-poor host environments, our analysis indicates that their UV excess cannot be explained by their host-galaxy parameters. Instead, we demonstrate that the addition of a hot blackbody component, likely arising from the interaction with the circumstellar material (CSM), to the normal SN~Ia spectrum, can reproduce their distinctive UV excess. This supports the hypothesis that 03fg-like SNe~Ia could explode in a CSM-rich environment.

ABSTRACT. Located at the centres of supernova remnants, central compact objects (CCOs) are among the most puzzling neutron stars. CCOs are bright in thermal X-rays, yet have evaded detection by major radio telescopes for decades, giving rise to the view that they are intrinsically radio-quiet and possess exceptionally weak magnetic fields. Here we report the discovery of coherent radio emission from the prototypical CCO 1E 1207.4-5209, using the MeerKAT radio telescope. The 424.1 ms radio period matches the known X-ray pulsations, and the dispersion measure of 69 pc cm^-3 is consistent with the distance to its host supernova remnant. The highly linearly polarised emission yields a rotation measure of only 10 rad m^-2, indicating a low-density, weakly magnetized environment. The smooth sweep of the polarisation angle implies that the beam passes close to our line of sight and suggests that CCOs may be intrinsically faint radio sources rather than fundamentally radio-silent. The measured magnetic-field strength of ~10^11G is so low that the neutron star must have been born rotating slowly (~0.4 s) and will take a Gyr to reach a spin period of 1 s at its current spin-down rate. This evolutionary path stands in sharp contrast to that of ordinary radio pulsars, which typically emerge from supernovae as rapidly spinning, high-field objects that shine brightly at birth and fade within a few million years. We believe these results will be of broad interest to the community and open a new observational window on the CCO population.

ABSTRACT. Bow-shock pulsar wind nebulae (BSPWNe) are steady-state synchrotron sources produced when a supersonic pulsar's relativistic wind is confined by the ambient interstellar medium. Isolated from their parent supernova remnants, they serve as efficient particle accelerators and provide a critical laboratory for testing acceleration theories. The Mouse PWN, a prototypical BSPWN, is bright in both the radio and X-ray bands, enabling multi-wavelength spectral modeling. Using data from 16 telescopes, we identify a spectral break at approximately 3.5 GHz. Adopting a steady one-zone model that includes synchrotron cooling, we successfully reproduce the spectral energy distribution from low radio frequencies to X‑rays under different injected particle spectra. The analysis shows that the observed spectral break supports the presence of a low-energy cutoff in the injected particle spectra, an intrinsic feature not explained by synchrotron cooling or self-absorption. This phenomenon may be attributed to the minimum plasma energy threshold required for matter to escape the pulsar magnetosphere, or alternatively, the efficient particle acceleration threshold occurring at the termination shock front.

ABSTRACT. Active galactic nuclei (AGNs) produce luminous X-ray emission. However, some super-Eddington AGNs are X-ray weak, with possible causes including heavy obscuration and intrinsic corona suppression. PHL 1811 was once considered a prototypical intrinsically X-ray weak quasar. But its analogs (94% X-ray weak) are absorption-driven, challenging this interpretation. A 2015 XMM-Newton observation of PHL 1811 showed a >5 keV excess, suggestive of Compton-thick absorption; in 2024, it recovered to an X-ray nominal state briefly, suggesting a normal intrinsic corona. We discuss evidence for the obscuration scenario and aim to unify understanding of X-ray weakness in PHL 1811, its analogs, and super-Eddington AGNs in general.

ABSTRACT. I will present an analysis towards the multiphase (warm+cold molecular and ionized) gas and dust content toward a cool-core brightest cluster galaxy (BCG) at z=0.4, using new JWST observations complemented by ALMA, MUSE, VLA, and Chandra data. The target harbours an AGN and hosts one of the largest known H2 reservoirs and elevated star formation. We obtained new JWST NIRSpec and MIRI MRS observations that detect warm H2 lines, PAH complexes, and ionized nebular lines. The H2 line ratios indicate a different temperature distribution in the circumgalactic medium (CGM) compared to the interstellar medium within the BCG. The strength of the PAH 11 micron complex relative to other PAH features indicates the prevalence of neutral PAH molecules. The PAH complexes are found in the BCG core region, as well as in dense clumps embedded within the more diffuse CGM along the radio synchrotron emission, suggesting shock-driven star formation. We perform resolved stellar population synthesis modelling over the system, as well as photoionization and shock modelling to constrain the metallicity and excitation conditions. I will summarize the implications of this pilot study on the intricate link between the enhanced star formation in this BCG and its CGM, as well as the role of AGN feedback in regulating star formation. This case study serves as a pathfinder for using JWST to unveil the warm molecular gas in galaxies for investigating the energy and mass flows in feedback processes.

ABSTRACT. Gravity and electromagnetic interactions are the only fundamental physical interactions (outside the nuclear domain). In this work, we shall concentrate on Hamiltonians containing gravitational interaction, which according to general relativity must be retarded. In recent years, retarded gravity has explained many of the mysteries surrounding the “missing mass” related to galactic rotation curves, the Tully–Fisher relations, and gravitational lensing phenomena. Indeed, a recent paper analyzing 143 galaxies has demonstrated that retarded gravity will suffice to explain galaxies’ rotation curves without the need to postulate dark matter for multiple types of galaxies. Moreover, it also demystified the “missing mass” related to galactic clusters and elliptic galaxies in which excess matter was derived through the virial theorem. Here, we give a mathematical criterion that specifies the cases in which retardation is important for gravity (and when it is not). The criterion takes the form of an inequality.

Bibliography

Yahalom, A. Gravitational Hamiltonian Systems and the Retarded Gravity Inequality. Entropy 2024, 26, 986. https://doi.org/10.3390/e26110986

ABSTRACT. Mergers represent one of the most critical phases in galaxy evolution, driving morphological transformations and rapid mass build-up at cosmic noon, when galaxies assemble their mass most efficiently. To gain critical insight over these processes, we have used high-resolution ALMA and JWST observations of a major-merger-induced double starburst at z=1.525, resolving scales down to 300 pc. The system reveals diverse structures, including highly obscured starbursting cores, unobscured tidal tails, clumps, tentative molecular outflows, and potential progenitors of stellar halos. VLA data also show radio jets 20 kpc away from the pair, yet we find little evidence for significant AGN impact on their star formation. This multi-wavelength analysis captures the consequences of the first passage of a massive merger: nuclear starbursts efficiently build bulges within gas-rich disks that remain largely intact; tidal tails host newly formed stars, while stripped older stars form a more diffuse component; and AGN activity, possibly triggered by the interaction, may represent a brief episode but can exert long-term influence by heating the halo and suppressing cold gas accretion, potentially leading to quenching. This study extends the legacy of Arp 220 into cosmic noon, revealing how massive galaxies formed their bulges and regulated their growth.

ABSTRACT. Most baryons in present-day galaxy clusters exist as hot gas (>10^7K), forming the intracluster medium (ICM). Cosmological simulations predict that the mass and temperature of the ICM decline towards earlier times, as intracluster gas in younger clusters is still assembling and being heated. To date, hot ICM has been securely detected only in a few systems at or above z≈2, leaving the timing and mechanism of ICM assembly uncertain. In this talk, I will present the direct detection of hot intracluster gas via its thermal Sunyaev–Zeldovich signature in the protocluster SPT2349–56 with the Atacama Large Millimeter/submillimeter Array. SPT2349–56 hosts a large molecular gas reservoir and three radio-loud active galactic nuclei (AGN) within an approximately 100-kpc region at z=4.3. The measurement implies a thermal energy of about 10^61 erg in the core, about 10 times more than gravity alone should produce. Contrary to current theoretical expectations, the hot ICM in SPT2349–56 demonstrates that substantial heating can occur very early in cluster assembly, depositing enough energy to overheat the nascent ICM well before mature clusters become common at z≈2.

ABSTRACT. Recent studies and literature already point to the coevolution of galactic bulges and central supermassive black holes (SMBHs), as well as to active galactic nuclei (AGN) being the transitional stage between star-forming and quiescent phases. In this study, we explore the correlation between the average Sérsic indices of the entire host galaxies and the masses of the central SMBHs to test the effect of the AGN beyond their immediate environment and to examine the evolution of this correlation as a function of redshift. This test can also provide insight into how the morphological development of the stellar components of host galaxies over time increases the probability of AGN triggering and how AGN feedback shapes the accumulation of stellar density in host galaxies. From multi-band photometric data and fiber spectroscopy of more than 10,000 AGN in Sloan Digital Sky Survey Data Release 17, we have found a strong correlation between the average Sérsic indices of the AGN host galaxies and the masses of the central SMBHs. For z<1 low luminosity AGN, we have found positive trends between the Sérsic Indices and SMBH masses. However, the trends become weaker and flatten out at higher redshift bins. This could be due to insufficient time for the morphology to develop and respond to the AGN activity. Nevertheless, the correlation shows the strongest positive trends in the SDSS r’, i’, and z’ bands, providing undeniable evidence of a link between SMBH growth and the structural evolution of host galaxies.

ABSTRACT. We present a multi-wavelength study combining optical r-band data from MegaCam at CFHT with near-infrared (NIR) J and Ks band observations obtained using WIRCam, focusing on a sample of nearby, grand design galaxies. The objective of this program is to perform a robust characterization of fundamental galactic properties by leveraging the differential sensitivity of these bands to stellar populations and interstellar dust attenuation. The Ks band effectively traces the evolved stellar mass backbone of the galaxies, while the r-band highlights younger stellar populations and regions of recent star formation activity.

This comprehensive dataset will enable several key astrophysical investigations. We will produce detailed color maps (e.g. r-Ks, J-K) and color-magnitude diagrams to constrain star formation histories. We will also explore stellar mass maps using mass models and estimate the spatial distribution and amount of dust attenuation within the galaxies. This work is part of a larger program aimed at studying the mass distribution of gas, stars, and dark matter for a statistical reference sample of nearby galaxies, linking stellar and gas mass distributions with kinematical perturbations on local scales (~ 0.1 kpc) to ultimately constrain the evolution of angular momentum within the sample.

ABSTRACT. Observations of the large-scale structure and the spatial distribution of galaxies in the Universe indicate that galaxies are mainly located in the densest regions, such as galaxy clusters. These systems are crucial for investigating the role of environment in galaxy evolution at different epochs. In the early Universe, the progenitors of galaxy clusters are protoclusters. Therefore, the search for and identification of protoclusters is a way to investigate the formation and assembly of clusters. Using lightcone data from the Horizon Run 5 (HR5) simulation, we search for spherical regions that are protocluster candidates and will collapse into clusters by z=0. The HR5 simulation covers a wide volume on Gpc scales, with spatial resolution down to 1 kpc, allowing us to investigate the properties of protoclusters across different scales. The protocluster identification method has been tested using snapshot data and is now applied to lightcone data from HR5, with future applications to observations such as Rubin LSST.

ABSTRACT. Radio astronomy offers some unique opportunities for education programs. Whilst optical astronomy is well-served with a wide range of excellent education programs and facilities such as LCOGTN there are fewer programs utilising radio astronomy. Long running radio astronomy education programs such as CSIRO’s PULSE@Parkes show that radio astronomy can be effectively translated to be engaging, relevant and pedagogically sound for high school students. Although PULSE@Parkes uses Murriyang, the 64m Parkes radio telescope other programs such as the Victorian Space Science Education Centre’s “Radio Astronomy: The Invisible Universe” using a more modest 3m dish antenna also provides an effective education program. Another advantage of these programs is that students can control the telescopes live, remotely and during the daytime and generally independent of the weather, unlike live observing with optical facilities. The advent of Software Defined Radios now mean that the principles of radio astronomy can be demonstrated in schools cheaply with a variety of low-cost instruments around the $200 mark developed by a range of institutions and individuals. The other area in which radio astronomy can have an impact is in the area of data science. Radio astronomy produces some of the largest datasets globally that are freely and publicly available. The advent of new facilities such as the SKA-Low and SKA-Mid currently under construction will lead to even more massive datasets. Already some citizen science projects such as the Zooniverse’s Radio Galaxy Zoo Emu bring radio astronomy data to the public in an engaging and effective manner whilst also producing quality science. There is potential for new software tools and education programs to make this data flood useful and understandable for educators and students. Opportunities for future programs drawing on what we have learnt from existing programs is discussed along with a call for greater collaboration.

ABSTRACT. Since 2007, Nepal Astronomical Society (NASO) has been promoting Astronomy in Nepal with a hope to leap in the Astronomy development in Nepal. Currently it is in a situation where many clubs and societies has been started throughout the country ranging from high school level to local level. As an addition to it, now our motto is to make astronomy accessible to all. Thus, NASO's current work focuses on breaking down the barriers by reaching out to the people who have traditionally been left out of science education. This includes people with physical disabilities including visual and hearing impairments (those who face challenges in regular classrooms), women and girls who are often discouraged from studying science, and communities from different cultural backgrounds who have had little access to scientific learning. Thus, this paper will present about the initiative of NASO in brining astronomy to the wider group of audiences in Nepal and in a regional level. Furthermore, it will also share on the approaches of the impact of taking Office of Astronomy for Education (OAE)'s resources to the classroom and the teaching community in Nepal and the region around Nepal through OAE Node Nepal (first international astronomy office in Nepal that NASO hosts).

ABSTRACT. Conferences are avenues for connecting researchers, initiating new and long-lasting collaborations, and sharing the latest knowledge and findings in their respective fields. These events are especially important for the astronomy community, whose field is ever-changing at an unprecedented rate. It is therefore important to provide a safe, welcoming, and inclusive environment at such events to promote and enhance engagement among participants and organizers. We report on some of the practices and initiatives implemented to promote a diverse and inclusive environment at the Philippine Space Science and Astronomy Research Conference (PSSARC), the first professional astronomy conference in the Philippines, which was held from August 8 to 12, 2025, at Adamson University, Philippines. Participants received stickers based on the color communication badge system as introduced by the Autistic Self Advocacy Network (ASAN), which indicates their communication preference without requiring any initial verbal interaction. Additionally, their preferred gender pronouns (PGPs) were displayed on their name tags. Braille translations of signage posted around the venue were also printed and pasted. Lastly, a sign language interpreter was present during the conference to accommodate deaf participants. Our pre- and post-surveys revealed that most of our participants are senior high school students aged 19-22 years old, reflecting the relatively young age of the Philippine astronomy community. There is a general improvement in the feelings of inclusivity among participants after the distribution of color-coded labels and PGPs. The Braille signage also needed improvement in visibility. However, the sign language interpretation was well received by both deaf and non-deaf participants. We highlight several suggestions and improvements on our initiatives in the future, and strongly advocate for their implementation in other conferences within and outside the country.

ABSTRACT. Hong Kong is rapidly positioning itself within the global NewSpace economy, supported by a new wave of entrepreneurial actors and recent regulatory developments enabling space-related innovation. Research on entrepreneurial ecosystems shows that high-impact entrepreneurship depends on the interaction of culture, networks, finance, policy and human capital rather than isolated firms (Isenberg, 2010; Spigel, 2017; Malecki, 2018; Spigel & Harrison, 2018). More recent work in international business introduces the ideas of ecosystem-specific advantages (ESA) and ecosystem social responsibility (ESR): ESA captures the location- and configuration-bound advantages arising from complementarities among platforms, users and complementors (Li et al., 2019), while ESR highlights the collective, co-created social responsibilities of ecosystem participants (Yi et al., 2023). Yet these insights have rarely been applied to highly regulated frontier sectors such as NewSpace, nor to city-regional contexts like Hong Kong’s NewSpace and low-altitude economy. Building on prior ecosystem mapping in emerging Asian contexts (Borsano, 2022), this study addresses this gap by examining how a NewSpace innovation ecosystem is emerging in Hong Kong, using the Orion Astropreneur Space Academy (OASA) and the city’s broader NewSpace community as an anchor case. Recent policy signals — including Chief Executive John Lee’s 2025 Policy Address commitment to streamline vetting procedures for Low Earth Orbit (LEO) satellite licensing and to expand low-altitude and aerospace technology infrastructure — provide a shifting institutional environment that may unlock new pathways for upstream and downstream space ventures. Using a qualitative methodology, the research draws on semi-structured interviews with ecosystem stakeholders, including founders, policy actors, OASA executives, industry practitioners, and Hong Kong–based legal and regulatory experts specialising in satellite governance and aviation/low-altitude legislation. The study analyzes how entrepreneurial initiatives, talent development programmes, and evolving regulatory frameworks interact to shape early-stage ecosystem formation. Findings will offer actionable insights for policymakers, astronomy partners, and cross-border science–innovation platforms seeking to integrate entrepreneurial ecosystems into space and satellite development agendas. Borsano, P. (2022). Mapping the Thai entrepreneurial ecosystem: Constraints, trends, entrepreneurial intention and initiative. AIP Conference Proceedings, 2644, 020001. Isenberg, D. J. (2010). How to start an entrepreneurial revolution. Harvard Business Review, 88(6), 40–50. Li, J., Chen, L., Yi, J., Mao, J., & Liao, J. (2019). Ecosystem-specific advantages in international digital commerce. Journal of International Business Studies, 50(9), 1448–1463. Malecki, E. J. (2018). Entrepreneurship and entrepreneurial ecosystems. Geography Compass, 12(3), e12359. Spigel, B. (2017). The relational organization of entrepreneurial ecosystems. Entrepreneurship Theory and Practice, 41(1), 49–72. Spigel, B., & Harrison, R. T. (2018). Towards a process theory of entrepreneurial ecosystems. Strategic Entrepreneurship Journal, 12(1), 151–168. Yi, J., Li, J., & Chen, L. (2023). Ecosystem social responsibility in international digital commerce. Journal of International Business Studies, 54(1), 24–41.

ABSTRACT. Astronomy offers a unique and compelling entry point into scientific literacy and broader STEM/STEAM engagement. However, how astronomy education and public engagement (EPE) professionals connect public audiences with scientific knowledge remains understudied, especially within global networks. This contribution presents findings from an interdisciplinary qualitative research. This research examines how the International Astronomical Union (IAU), through its Offices for astronomy education and outreach, as well as the corresponding networks of National Outreach Coordinators (NOCs) and National Astronomy Education Coordinators (NAECs), enacts astronomy EPE across diverse cultural and socio-economic contexts.

Drawing from in-depth interviews with NOCs and NAECs from around the world, the analysis reveals two dominant patterns in how practitioners conceptualise and operationalise astronomy EPE. First, astronomy acts as a boundary-spanning bridge connecting researchers, educators, communicators, and the public through curiosity, shared understanding, and accessible narrative frameworks. Participants describe astronomy as an inherently integrative domain that fosters cognitive competencies such as critical thinking, scientific reasoning, awareness, and evidence-based judgment. Through translation and coordination work, combined with identity-bridging roles, astronomy EPE professionals serve as mediators between science and society. The contextual practices of these boundary spanners show how organisational boundary-spanning, a key role of the IAU Offices, creates the conditions for science literacy to flourish within a globally entangled landscape.

Second, astronomy EPE is portrayed as a catalyst for inspiration, values formation, and global perspectives. Participants also emphasise how experiences such as night-sky observations, localised educational materials, and cross-cultural storytelling can transform initial curiosity into sustained interest, a sense of belonging guided by scientific enterprise, and reflections on planetary interconnectedness. This illustrates the ethical and socio-emotional dimensions of astronomy EPE. The findings further highlight the increasing use of boundary objects, such as astronomical instruments, citizen-science platforms, and indigenous cosmologies, which enable communication across linguistic and cultural divides. Multimodal strategies, including hybrid events, context-sensitive materials, and audience-tailored audio-visual resources, play an undeniable role in linking scientific discoveries with local realities. Participating NOCs and NAECS also stress the importance of expanding astronomy EPE to underserved communities, noting the structural inequities and organisational barriers they face. They argue that tackling these challenges is essential to realising the inspirational and educational potential of astronomy worldwide.

By positioning astronomy EPE within an integrated theoretical lens and drawing on empirical insights from global practitioners, this study provides a nuanced account of how astronomy EPE professionals act as bridge builders across scientific, cultural, and institutional domains. For APRIM 2026, the contribution invites further dialogue on how the Asia-Pacific community can join hands towards a more inclusive, collaborative, and globally informed astronomy EPE in the future.

ABSTRACT. In 2023, leaders of Maunakea Observatories shared their perspective on the historic events surrounding the controversy in Hawaiʻi over the development of astronomical facilities on Maunakea. In this paper, we shared our process of introspection and transformation, our hopes and ambitions for the future of astronomy in Hawaiʻi, as advocated by the U.S. National Academy of Sciences and Engineering's Astro2020 report, which calls on the profession to embrace a community-based model of astronomy. We called on the entire profession, including astronomers, engineers, technicians and administrative staff, to share their thoughts and help us develop this model.

In this paper, we will review the progress of this model, particularly in Hawaiʻi, and reflect on the opportunities and initiatives still to be taken to consolidate and expand it.

ABSTRACT. TBA

ABSTRACT. Accurate centre-of-mass (CoM) alignment is essential for ensuring the validity of air-bearing spacecraft testing facilities used for ground-based verification of Attitude Determination and Control Subsystems (ADCS). Even small CoM offsets relative to the platform’s mechanical rotation axis introduce parasitic torques that distort detumbling and pointing experiments. To address this, we present the design, implementation, and validation of an autonomous mass-balancing system for planar air-bearing spacecraft platforms. The proposed system employs four motorised masses to regulate the CoM in three degrees of freedom. PID controllers independently adjust the X–Y planar mass positions, driving the CoM toward the platform’s rotational centre, while a Batch Least Squares (BLS) estimator identifies Z-axis imbalance and iteratively refines the mass configuration to compensate for out-of-plane disturbance torques. This hybrid PID–BLS approach enables autonomous balancing without iterative manual procedures. Experimental results show that the system reduces planar CoM error to within a millimetre and accurately estimates Z-axis imbalance under sensor noise and small disturbances. When activated, the mass-balancing mechanism significantly improves detumbling repeatability and stabilisation accuracy during ADCS experiments. By providing a low-cost, autonomous means of correcting multi-axis mass imbalance, this work enhances the fidelity of ground-based ADCS verification and supports safer, more reliable development of small-satellite technologies in increasingly congested orbital environments.

ABSTRACT. We present a simulation-driven methodology for the pre-launch development of embedded solar glint detection algorithms, addressing a fundamental constraint in Space Situational Awareness (SSA): no orbital training data exist prior to satellite launch. While ground-based SSA systems require extensive observational datasets, they remain limited in detecting small, fast-moving, and non-cooperative debris in Low Earth Orbit (LEO). We demonstrate that physics-based simulation can substitute for on-orbit data during algorithm development, thereby reducing technical risk for CubeSat SSA missions and enabling real-time satellite-to-satellite monitoring capabilities for in-orbit detection of space objects. Our simulator integrates five modular components: GalSim point spread function modeling, the Gaia DR3 stellar catalog with zodiacal light background, the IMX500 sensor noise chain, bidirectional reflectance distribution function (BRDF) spacecraft material models, and SGP4 orbital propagation with Sun–satellite–target geometry in a satellite-to-satellite monitoring configuration. BRDF reflectance models are validated against laboratory measurements, and sensor parameters are characterized through hardware testing. Parameter uncertainties, particularly Attitude Determination and Control System (ADCS) jitter, which cannot be characterized before flight, are explicitly bounded. The detection algorithm targets a 3U CubeSat in sun-synchronous Low Earth Orbit (LEO) at 500 km, using a Sony IMX500 sensor and a Raspberry Pi Zero 2W processor. Performance validation demonstrates 14 fps throughput and an F1-score of 88.8% for LEO debris detection. Detection is material-dependent: high-albedo debris achieves robust recall, while low-albedo surfaces (e.g., solar panels) produce insufficient flux. Detection performance in GEO/MEO regimes is limited, reflecting system optimization for LEO monitoring scenarios, where debris density and relative motion are most critical. These results demonstrate the feasibility of real-time monitoring of orbiting objects directly from a moving orbital platform, particularly for debris producing observable solar glints. This work establishes a replicable template for future embedded SSA missions at the National Astronomical Research Institute of Thailand (NARIT), and provides a pathway toward distributed, autonomous satellite-to-satellite SSA architectures. Such systems can reduce latency, minimize reliance on ground infrastructure, and contribute directly to space sustainability by enabling real-time monitoring and mitigation of space debris in increasingly congested orbital environments.

ABSTRACT. With the decrease in launch and satellite manufacturing cost, within 10 years the number of active spacecrafts on orbit has reached 12,300 in the beginning of 2026, which is 7-fold increase in the past 10 years. The majority of the spacecrafts are in Low Earth Orbit (LEO), around 500 km altitude, leading to conjunctions between active satellites. Historically, conjunctions have been caused by an accelerating rate of debris generation caused by on-orbit fragmentations from explosions and collisions. Satellite operators reacted to the increasing threat by utilizing Space Situational Awareness (SSA) providers to gain insight and protect their missions by performing collision avoidance maneuvers.

With the trend to utilize the LEO by commercial constellations, new challenges arise due to the need to coordinate between operators. Operators resort to email or other conventional methods to communicate with their conjunction partner, which is prone to miscommunication and loss of mission time, if communication is achieved at all. Space Traffic Management (STM) has been established as discipline to solve this problem by empowering the operators to communicate and share data. As part of STM a common understanding is created including a joint timeline with actions both partners can take and agree on. Transparency from sharing orbital data and understanding each other’s processes leads to building trust between operators and increasing space sustainability.

To ensure the long-term sustainability of space activities, the following measures are needed: • Establish a globally unified STM architecture to promote data sharing and transparency. • Encourage multilateral cooperation all spacefaring nations and private enterprises. • Develop flexible regulatory mechanisms tailored to commercial space, balancing innovation and safety. • Strengthen Space Situational Awareness (SSA) capabilities to improve early warning and response efficiency.

The architecture of an STM system is designed to be SSA provider agnostic and the challenge of data sharing in a global context in mind. The interface allows (a) exchange satellite and orbit information (b) trigger SSA services via APIs. A traceability requirement is applied to document all actions performed by the operators and values provided from the SSA interface. In addition, the system needs to be auditable by a monitoring entity. Similar developments have been seen in the financial and health care sectors. The paper gives an overview of the OKAPI:Astrolabe Space Traffic Coordination platform.

ABSTRACT. This research deals with the development analytical-geometric framework for the prediction of a satellite's entry into and exit from a planet's umbra and penumbra. The core of the method lies in developing the general approach for conic model, the intersection of which with the satellite's orbital plane forms a "shadow ellipse"—a second-order curve. By deriving the parameters of this shadow ellipse and solving for its intersection with the satellite's Keplerian orbit, the problem is reduced to finding the roots of a universal fourth-degree equation. This solution directly yields the true anomalies at the eclipse boundaries, from which the exact eclipse duration can be computed using Kepler's equation.

The method's efficacy is demonstrated through application to a high-eccentricity orbit of a prospective Venus orbiter, relevant to missions like Venera-D. Validation against high-fidelity numerical simulations in a full ephemeris model confirms the approach's accuracy, with results showing close agreement. Furthermore, the concept of an "invariant surface $S(\Delta T_{ED}, \Omega, \omega, i)$ is introduced, providing a powerful tool for visualizing and predicting long-term eclipse dynamics over multiple orbital revolutions.

Beyond calculating eclipses by the solid body, the method is successfully extended to a critical practical application: determining the parameters for atmospheric occultation experiments. It enables the fast and still reliable calculation of the time a satellite spends in the region where the planetary atmosphere occults the Sun, as well as the determination of the latitude and longitude of the perpendicular to the satellite-Sun line on the planet's surface. This demonstrates the versatility and direct utility of the approach in the design and planning of advanced scientific missions to Venus and other planetary bodies.

ABSTRACT. With the rapid development of space activities, the number of space debris is increasing by year, which poses a serious threat to the safety of in-orbit spacecraft and space missions. Optical observation is one of the main ways to detect space debris, but optical images often suffer from problems such as low contrast, serious noise interference, which greatly affect the accuracy and efficiency of debris extraction, linking and identification. To solve these problems, an efficient extraction method of optical observation images for space debris is proposed in this paper. First, the preprocessing operation of the original optical observation image is carried out, including denoising based on improved filtering and enhancement, so as to eliminate noise interference and highlight the target characteristics of space debris. Then, aiming at the characteristics of small size, low grayscale and easy adhesion of space debris in optical images, an object extraction algorithm combining adaptive threshold segmentation and Gabor filtering processing is designed to accurately separate debris targets from complex background. Finally, a large number of simulation experiments and actual optical observation image tests are carried out to verify the performance of the proposed method. The experimental results show that compared with the traditional extraction methods, the proposed method has higher extraction accuracy and faster operation speed, can effectively extract space debris targets from low-quality optical observation images. The method proposed in this paper provides a reliable technical support for the efficient detection and accurate identification of space debris, and has important theoretical significance and engineering application value in the field of space debris optical observation.

ABSTRACT. Optical telescopes can acquire high-precision angular measurement data of space debris; however, their observation window is limited by the solar illumination conditions of space debris and the occlusion of space debris by the Earth's shadow. Therefore, the optical angular measurement data exhibit a significant sparse nature in the temporal distribution for a single space debris. In addition, the angular measurement data lack range-wise constraints on the orbit of space debris, which brings challenges to the stability of precise orbit determination for space debris. This paper presents a precise orbit determination method fits for sparse optical angular measurement data. Compared with traditional methods, the proposed method boasts the advantages of a wide convergence range and stable orbit determination results. The results demonstrate that the method described in this paper can effectively improve the accuracy of precise orbit determination.

ABSTRACT. The main contents and technical methods of the National Standard of the People's Republic of China entitled Space Debris Collision Warning Technical Requirements were elaborated in this report. Implemented on September 1, 2025, the standard was formulated to specify the technical processes and key requirements for space debris collision warning, and it was applicable to the launch and on-orbit collision warning of cataloged space debris for spacecraft and launch vehicles. The responsibilities of space object owners, collision warning providers and monitoring parties were defined in the standard, as well as the interface requirements for data interaction. In addition, the technical requirements for core processes such as dynamic data preparation, orbit screening, orbital conjunction prediction and collision probability calculation were stipulated therein. The calculation and determination methods for orbital errors, collision probability and risk thresholds were detailed in the informative annexes. As a national standard, it standardized the work of space debris collision warning.