SCAR AAA 2025

15 Sep 2025, 08:30 → 19 Sep 2025, 17:30 Asia/Bangkok

The 8th Workshop of SCAR AAA 2025
September 15 - 19, 2025
Phuket, Thailand

Astronomy & Astrophysics from Antarctica (AAA) is an Expert Group of SCAR, the Scientific Committee on Antarctic Research. The objectives of AAA are to provide a venue to discuss, promote and coordinate astronomical and astrophysical activities in Antarctica to optimize outcomes from international investments, and to maximize the opportunities for productive interactions with other disciplines.

This is the eighth meeting in the series. Prior meetings include AAA2011 in Sydney, Australia; AAA2013 at the Certosa di Pontignano, Italy; AAA2015 in Hawaii, USA; AAA2017 in Chiang Mai, Thailand; AAA2019 in the Aosta Valley, Italy; AAA2021 held remotely and hosted by the University of Wisconsin–Madison, USA; and AAA2023 in Svalbard, Norway. Building on the success of these prior SCAR AAA meetings, and the XXXV SCAR Biennial Meeting Open Science Conference theme ("Where the Poles come together"), those with interest in either the Arctic or Antarctic research are encouraged to attend. 

The workshop will take place at Dusit Thani Laguna Phuket in Phuket, Thailand.

The abstract submission deadline was July 15 and is now closed.

Virtual attendance is available, and also has a registration fee.

The registration deadline has been extended to August 15.

Registration fee payments are due by August 15.

---

Scientific Organizing Committee

• Adriana Gulisano (Argentina)

• Michael Ashley (Australia)

• Silvia Masi (Italy)

• Peng Jiang (China)

• Xuefei Gong (China)

• Zhaohui Shang (China)

• Waraporn Nuntiyakul (Thailand)

• Achara Seripienlert (Thailand)

• Albrecht Karle (United States)

---

Executive Advisory Committee

• Prof. Dr. Pongruk Sribanditmongkol (CMU)
• Prof. Dr. Pairash Thajchayapong (Princess-IT)
• Dr. Chadamas Thuvasethakul (Princess-IT)
• Assoc. Prof. Boonrucksar Soonthornthum (NARIT)
• Prof. Dr. Suchana Chavanich (CU)
• Assoc. Prof. Dr. Winita Punyodom (CMU)
• Assoc. Prof. Dr. Duangmanee Wongratanaphisan (ThEP)

---

Local Organizing Committee

• Asst. Prof. Dr. Siramas Komonjinda – Chair
• Assoc. Prof. Dr. Waraporn Nuntiyakul – Co-Chair
• Asst. Prof. Dr. Suwicha Wannawichian – Member
• Dr. Chana Sinsabvarodom – Member
• Dr. Achara Seripienlert – Member
• Mr. Thirasak Panyaphirawat – Member & Secretary
• Ms. Kotchanipa Chainoi – Assistant Secretary

Monday, 15 September

15:00 → 20:00 Check-In Begins at Dusit Thani Laguna Phuket Hotel

Tuesday, 16 September

08:30 → 09:00 Opening: Registration

(Draft) SCAR AAA 2025 Programs 11sep25.pdf

09:00 → 09:10 Opening: Welcome Remarks and Report on the Organization of the 8th SCAR AAA Workshop

Convener: Prof. Siramas Komonjinda (Chiang Mai University)

(Draft) SCAR AAA 2025 Programs 11sep25.pdf

09:10 → 09:20 Opening: Remarks by Assoc. Prof. Dr. Duangmanee Wongratanaphisan, Director of Thailand Center of Excellence in Physics

(Draft) SCAR AAA 2025 Programs 11sep25.pdf

09:20 → 09:30 Opening: Remarks by Dr.Jitti Mungkalasiri, Deputy Director of Program Management Unit for Human Resources & Institutional Development, Research, and Innovation (PMU-B)

(Draft) SCAR AAA 2025 Programs 11sep25.pdf

09:30 → 09:35 Opening: Welcome Address: Assoc. Prof. Dr.Piyapong Niamsup, Dean of the Faculty of Science at Chiang Mai University

(Draft) SCAR AAA 2025 Programs 11sep25.pdf

09:35 → 09:45 Opening: Opening Address: Prof. Dr. Adriana Gulisano, Chair of the Expert Group on Astronomy and Astrophysics from Antarctica, SCAR

Convener: Adriana Maria Gulisano (IAA/DNA, IAFE(CONICET-UBA), UBA FCEyN DF)

(Draft) SCAR AAA 2025 Programs 11sep25.pdf

09:45 → 10:20 Special Talk: Scientific Research in Polar Regions under the Royal Initiative of Her Royal Highness Princess Maha Chakri Sirindhorn: Prof. Dr. Pairash Thajchayapong and and Prof. Dr. Suchana Chavanich

20250916 Talk.pdf

มูลนิธิเทคโนโลยีสารสนเทศตามพระราชดำริ สม.mp4

10:20 → 10:40 Coffee Break

10:40 → 12:00 Overview/Summary

10:40 Chiang Mai University’s Role in Advancing Polar Science

Chiang Mai University (CMU) has contributed significantly to polar research through three core domains: scientific research, engineering and data infrastructure, and education and outreach. These efforts have resulted in the development of an integrated operations hub—or “war room”—which supports real-time data handling and coordination across multiple research programs, including but not limited to polar missions. CMU’s contributions include high-energy astrophysics studies, support for field deployments, and long-term partnerships with international collaborators. This talk also outlines Thailand’s future role in the SCAR Astronomy & Astrophysics from Antarctica (AAA) initiative, emphasizing strategic investment in workforce development and national readiness in polar science.

Speaker: Prof. Waraporn Nuntiyakul (Chiang Mai University)

ChiangMaiUniv_WarapornNuntiyakul_AAA2025.pdf

11:00 Work and Recent Developments of AASWO (Argentinean Antarctic Space Weather Observatory)

The Argentinean Antarctic Space Weather Observatory (AASWO) continues to play a leading role in advancing the understanding of space weather phenomena from high-latitude environments. Since the establishment of its first node at Marambio Base in February 2019, AASWO has operated a cutting-edge laboratory designed and maintained by the Argentine Space Weather Laboratory (LAMP, Laboratorio Argentino de Meteorología del esPacio), a collaborative initiative of IAFE (Institute for Astronomy and Space Physics), IAA (Instituto Antártico Argentino) and DCAO (Departamento de Ciencias de la Atmósfera y los Océanos de la Universidad de Buenos Aires).
This Marambio facility hosts a suite of scientific instruments, including a cosmic ray detector, high-sensitivity magnetometers, and a meteorological station. Engineered specifically to endure the harsh Antarctic climate, the infrastructure incorporates materials and systems capable of withstanding extremely low temperatures and sustained high winds. Redundant power supplies based on gel batteries and precise GPS time synchronization ensure reliable, high-resolution data acquisition. Real-time data transmission to LAMP's central servers in Buenos Aires supports the continuous generation of operational space weather products, accessible via the laboratory’s online platform.
As part of its strategic expansion, AASWO has recently completed the installation of its second observational node at the General San Martín Base, within the framework of the 2024 Austral Summer Campaign. The San Martín node is now fully operational, and initial space weather events have already been successfully recorded at both Antarctic sites. This expanded observational capability significantly enhances the spatial coverage of space weather monitoring in the Southern Hemisphere, contributing to the global effort to understand high-latitude space weather dynamics.
Efforts are also underway to integrate the data collected by AASWO’s Cherenkov detectors into the Neutron Monitor Database (NMDB). This process, currently in the testing and calibration phase, aims to ensure the reliability and consistency of the measurements before their inclusion. The integration will provide valuable high-latitude datasets to the international scientific community and promote broader collaboration in space weather research.

Speaker: Dr Adriana Maria Gulisano (Instituto Antártico Argentino (IAA) /Dirección Nacional del Antártico (DNA) , CONICET - Universidad de Buenos Aires, Instituto de Astronomía y Física del Espacio (IAFE), Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales, Departamento de Física, Laboratorio Argentino de Meteorología del esPacio (LAMP))

Work and Recent Developments of AASWO (Argentinean Antarctic Space Weather Observatory).pptx.pdf

11:20 Activities on Antarctic Astronomy in Japan

The Antarctica plateau is the best site for submm-terahertz observations in Astronomy on the earth. Taking the advantages of the Antarctic plateau, we are conducting the Antarctic 30-cm submm telescope project. The 30-cm submm telescope will be transported to Dome Fuji II in 2026. The scientific purpose is to understand the evolutionary process of interstellar gas from diffuse gas to dense gas by observing [CI]$(^3P_1-^3P_0)$ (492 GHz) and CO(J = 4-3) (461 GHz) lines simultaneously. [CI]$(^3P_1-^3P_0)$, fine structure line of atomic carbon, is considered as a good tracer of the diffuse molecular gas which cannot be observed by CO lines because of the photodissociation of CO molecule (CO-dark gas). On the other hand, CO(J = 4-3) is a good tracer of warm and dense molecular gas associated with star forming regions. We will conduct a Galactic plane survey in these two lines until 2029. As the next step, we are planning Antarctic 12-m Terahertz Telescope project (ATT12). The telescope is designed to have very wide field of view for the survey of distant dark-galaxies which can be found only with dust thermal emission. MKID arrays with wide field of view will be installed for the survey. Heterodyne receivers whose observing frequencies are matched to the atmospheric windows up to 2 THz will be also installed. We will introduce these activities on Antarctic astronomy in Japan.

Speaker: Prof. Nario Kuno (University of Tsukuba)

Kuno.pdf

11:40 NIAOT update on Antarctic telescope projects

This talk will introduce the Antarctic Telescope projects that NIAOT has updated and upgraded since 2019, which mainly include Antarctic Survey Telescopes , Kunlun Infrared telescope, Zhongshan Multi-band survey telescopes, etc. AST3-2 has restarted observation since January 2024 which was unmaintained for nearly five years from 2019 due to Covid-19 and some other reasons. AST3-3, which is designed for near-infrared astronomy in Antarctica, is expected to start domestic commissiong at K-band in the northern winter in 2025. Kunlun Near-Infrared telescope with aperture of 15cm and band of 1.1-1.4μm was installed in January 2024. It has measured near-infrared sky light background brightness of the entire sky at Dome A. Besides the telescopes at Kunlun station mentioned above, a number of some telescopes has been deployed at Chinese Zhongshan station in Antarctica, which will be provided some details in this talk.

Speaker: Xiaoyan Li

SCAR2025-9.16-LiXiaoyan-NIAOT.pptx

12:00 → 13:20 Lunch Break

13:20 → 13:40 Overview/Summary

13:20 Introduction of the Latest 41th CHINARE Astronomical Tasks

On December 31, 2024, the 41st China National Antarctic Research Expedition （CHINARE） team arrived at the highest point of the Antarctic Plateau, Dome A. As a member of the Inland Team, I will introduce the progress of our team's mission in the astronomy field.

Speaker: CHAO CHEN (Nanjing Institute of Astronomical Optics & Technology ,National Astronomical Observatories ,CAS)

41st南极科考汇报-NIAOT - SCARAAA.pptx

13:40 → 14:40 High-Energy/Neutrino Science/IceCube

13:40 Exploring High-Energy Neutrino Universe from the South Pole with IceCube

The Amundsen-Scott South Pole Station is an ideal location for studying the universe of high-energy particles by detecting neutrinos. The IceCube Neutrino Observatory measures neutrinos emitted from sources of cosmic rays, which are the most energetic background radiation in the universe. In this talk, we present our latest findings on the neutrino sky, covering a broad range of energies from EeV to TeV using IceCube. We highlight the updated measurements of the high-energy neutrino spectrum in the cosmic background radiation. We also introduce the recent endeavours initiating multi-messenger observations to probe the origins of cosmic-rays.

Speaker: Shigeru Yoshida (Chiba University)

IceCubeSCARAAA2025.pdf

14:00 Advancing Neutrino Astrophysics with the IceCube Upgrade

The IceCube Neutrino Observatory at the geographic South Pole has achieved major milestones in neutrino astrophysics, including the discovery of a high-energy astrophysical neutrino flux and correlations with flaring blazars and Seyfert galaxies. Building on this success, the IceCube Upgrade is scheduled for completion during the 2025/26 Antarctic summer season. This upgrade will deploy seven new strings of densely instrumented optical sensors, primarily near the bottom of the detector, substantially enhancing event reconstruction and improving the selection efficiency of atmospheric and astrophysical neutrinos down to a few GeV. These advancements will enable unique opportunities to study neutrino oscillations, conduct high-precision measurements of tau neutrino appearance, and detect GeV-scale neutrinos from astrophysical transients.
This contribution will present the current status of the IceCube Upgrade ahead of the upcoming construction season, with a focus on its scientific capabilities and its extensive calibration program.

Speaker: Aya Ishihara (Chiba University)

SCAR_Upgrade_v2.pdf

14:20 Developing the next generation of IceCube: IceCube-Gen2

Building on the success of IceCube, and the upcoming deployment of the IceCube Upgrade, the IceCube collaboration is planning for a next phase of upgrade of the detector, IceCube-Gen2. Over the past decade, the IceCube-Gen2 Collaboration has been designing a detector that would provide an order of magnitude greater sensitivity to high- and ultra-high-energy neutrinos, increasing the volume of instrumented ice from 1km3 to 8km3 and adding a large radio component covering TeV to EeV energies. This effort has culminated in a comprehensive three volume Technical Design Report. To further support this expansion, IceCube-Gen2 is planning a comprehensive design phase over the next three years to finalize the detector design, geometries, simulated sensitivities, and logistics needs. In this talk, we will present the motivation, current status, and plans for the development of the IceCube-Gen2 detector.

Speaker: Vivian O'Dell (University of Wisconsin–Madison)

SCAR_IceCubeGen2_v2.pdf

14:40 → 15:00 Coffee Break

15:00 → 16:30 Panel Discussion: AAA SWOT ANALYSIS and alignment with SCAR strategic plan

18:00 → 20:00 Special Events: Welcome Dinner

Wednesday, 17 September

09:00 → 09:20 High-Energy/Neutrino Science/IceCube

09:00 Neutron Monitor Response Functions from the 2023–24 Latitude Survey aboard the Araon Icebreaker

Ground-based cosmic ray observations from polar regions are key to understanding the modulation of galactic cosmic rays and their interactions with Earth’s magnetic environment. In this study, we present results from a latitude survey using the Changvan neutron monitor aboard the South Korean icebreaker Araon, which traversed from Antarctic to Arctic latitudes during its 2023–24 voyages. The survey provides unique data for characterizing geomagnetic effects on cosmic ray access across a broad range of cutoff rigidities.

The Changvan monitor is configured as a semi-leaded neutron detector comprising three proportional counters: a leaded BF₃ tube, an unleaded BP28 tube, and a leaded BP28 tube arranged linearly. The absence of lead rings around the center tube distinguishes the system from standard 3NM64 models. Using geomagnetic cutoff rigidities calculated via the IGRF-14 model, we derive the response functions of each tube type and assess their performance under varying polar conditions.

These observations from both the Antarctic and Arctic reinforce the role of mobile neutron monitors in advancing high-latitude cosmic ray studies and highlight their potential contributions to interdisciplinary Antarctic research. The results will serve as a baseline for future comparisons, including annual solar modulation effects. This project exemplifies international cooperation and the expanding utility of polar platforms in astroparticle physics.

Speaker: Achara Seripienlert

ARAON Voyages

LatitudeSurvey_AcharaSeripienlert.pdf

09:20 → 10:20 Optical/Infrared

09:20 Measure the vertical turbulence profile at Dome A with KLTP

Seeing measured by DIMM reflects the adverse effect on observations from the total atmospheric turbulence above the instrument. After seeing has been monitored at Dome A for a few years, we plan to measure the vertical turbulence profile, which enables us to understand the observing conditions better and is essential for the development and operation of future adaptive optics instruments. A lunar scintillometer, named KunLun Turbulence Profiler (KLTP), was built and deployed to Dome A in early 2025. Details of the KLTP and preliminary results will be presented.

Speaker: Zhaohui Shang (National Astronomical Observatories, CAS)

20250916.Phuket.8th.SCAR.AAA.shang.v1.2.pptx

09:40 Astrometry and Photometry for Images of All-sky Cameras with KLCAM

All-sky cameras are widely used in site testing, fireball triangulation, meteorite recovery, and time-domain astronomy. However, they intrinsically require optics with nonlinear projections, making it challenging to use traditional astrometric and photometric methods. Based on the all-sky camera KunLun Cloud and Aurora Monitor (KLCAM) in Dome-A, we have developed a method to analyse cloud cover and aurora contamination using extinction and sky brightness from photometry. The photometry accuracy we achieve is typically 0.1 mag for stars < 4.5 mag and 0.2 mag for stars < 5.5 mag, while the astrometry accuracy is 0.4 pixels in (x, y). We automate the process that allows us to monitor the real-time distribution of cloud and aurora. Our astrometric method has been generalised and applicable to images of super-wide fields of view.

Speaker: Xu Yang (National Astronomical Observatories, Chinese Academy of Sciences)

YANG Xu-Astrometry and Photometry for Images of All-sky Cameras with KLCAM.pdf

10:00 The 1.4 μm water-vapor-absorption band imaging from Dome A

The light at wavelength around 1.4 μm is heavily absorbed by water vapor in the atmosphere， creating a spectral gap between the J and H bands. However, Dome A’s exceptionally dry conditions provide a unique opportunity for observations in this band. We developed a custom 1.4 μm filter (1.34 to 1.48 μm), similar to JWST’s F140M filter. After initial testing in Daocheng, China, the filter was installed on the Antarctica InfraRed Binocular Telescope (AIRBT) in January 2025. AIRBT consists of two identical 15 cm aperture, f/3 optical-tube-assemblies (OTAs), each equipped with an InGaAs camera (640512 pixels, 15 μm pixel size). This configuration yields a pixel scale of 6.9 arcsec and a field-of-view of 1.2 deg * 1 deg. AIRBT enables simultaneous observations in both J* and 1.4 μm bands. The scientific goal is to search for and study cool stars by detecting their water-vapor-absorption features. AIRBT had monitored some bright stars during polar day, and surveyed the Galactic plane during night-time. It had successfully detected water-vapor-absorption features in some late type stars. This talk will present the instrument design, observational strategy, data analysis, and preliminary results.

Speaker: Bin Ma (Sun Yat-sen University)

20250917.AIRBT 1.4.SCAR AAA.pdf

10:20 → 10:40 Coffee Break

10:40 → 11:20 Optical/Infrared

10:40 Cryoscope Pathfinder: cold telescope for the cold continent

Antarctica is the perfect site for infrared (IR) astronomy, especially at inland sites. At Concordia station, previous observations have shown that the air is cold and dry, such that the IR background at 2.4 micron is only 1% compared to sites at temperate latitudes. Leveraging this "K dark" window unique to Antarctica, we are planning to install a 26-cm fully cryogenic wide-field (16 sq deg) telescope, Cryoscope Pathfinder, at Concordia. Cryoscope Pathfinder has a novel optical design, with a front corrector plate serving as a dewar window, allowing the interior to be pumped to vacuum and kept at a cryogenic temperature using a cryocooler. Cryoscope Pathfinder will perform a time-domain survey of the entire Southern sky in the K dark band. We will provide an overview of the plan and current status of the pathfinder and expected science results. We will also discuss the plan for the full-scale 50 sq deg 1-meter Cryoscope, and its powerful surveying capabilities.

Speaker: Samaporn Tinyanont (National Astronomical Research Institute of Thailand)

Cryoscope_AAA2025.pptx

11:00 Cryoscope: the Antarctic infrared surveyor.

The quarter scale prototype of the ultra-wieldfield infrared surveyor is curently in the later part of its construction at Caltech and on track for deployment in 2026. We report on the instrument design, capability and status.

Speaker: Tony Travouillon

cryoscope SCAR 2025.pptx

11:20 → 12:00 Sub-mm/mm

11:20 First Onsite Activities at Dome Fuji II for 30-cm Sub-millimeter Telescope Installation

Dome Fuji II is located at an altitude of approximately 3,810 m in inland Antarctica, one of the best sites on Earth for sub-millimeter astronomical observations, owing to its extremely low atmospheric water vapor content and cold temperatures. The Consortium of Antarctic Astronomy of Japan is developing a 30-cm sub-millimeter telescope for deployment at Dome Fuji II. In the receiver, the two double-sideband superconductor-insulator-superconductor (SIS) mixers are coupled to a corrugated horn with RF/IF hybrids. The simultaneous survey observations of the two molecular emission lines, ${\rm CO}(J=4\text{-}3)$ and $[{\rm CI}](^3P_1 \text{-} ^3P_0)$, are achieved in the 500-GHz band. The receiver system and telescope are progressing in preparation for upcoming transportation towards Antarctica this year by evaluating the performance measurements in a cold environment around $-20$ to $-30\rm ^\circ C$. From October 2024 to February 2025, two people joined the 66th Japanese Antarctic Research Expedition (JARE-66) to carry out site preparation and infrastructure development for telescope operation at Dome Fuji II, as the first visit from our team. To mitigate the impact of exhaust emissions from snow vehicles and generators, a power cable was buried approximately 250 m upwind from the living facilities. Afterwards, the observation point was decided at the edge of the power cable. In the observation area, the telescope mounting base and power supply enclosure were constructed using a combination of styrofoam blocks and wooden materials for their durability in the harsh Antarctic environment. In this presentation, onsite activities as well as highlights of performance evaluations before shipping to Antarctica will be shown.

Speaker: Shunsuke Honda (University of Tsukuba)

250917_shonda_scaraaa.pdf

11:40 Probing the Origins of the Universe from the South Pole: An Overview of the BICEP Experiment

The BICEP experiment is a series of ground-based cosmic microwave background (CMB) telescopes located at the Amundsen–Scott South Pole Station, designed to detect the faint polarization patterns in the CMB that may provide evidence for inflationary gravitational waves. Over the past two decades, the BICEP collaboration has played a central role in observational cosmology by developing increasingly sensitive instruments and deploying them in the uniquely stable and dry environment of the Antarctic Plateau. Today, our experiment covers a wide frequency range from 30 to 270 GHz to better characterize foregrounds and improve overall sensitivity.
In this talk, I will outline the scientific goals, instrument designs, and recent results from the BICEP program, including updated constraints on the tensor-to-scalar ratio. I will touch on how the South Pole’s atmospheric conditions and logistical support have made these observations possible. I will also share an update on ongoing developments with the BICEP Array, including the recent deployment of the 220/270 GHz receivers, which add more sensitivity at these higher frequencies. I will close with exploring the potential for future cosmology experiments at the South Pole.

Speaker: Howard Hui (Caltech)

202509_SPO_SCAR.pptx

12:00 → 13:20 Lunch Break

13:20 → 15:00 Miscellaneous Topics

13:20 COSMO: Beyond the black-body Cosmic Microwave Background, towards the detection of spectral distortions

The Cosmic Microwave Background (CMB) provides a window into the thermal history of the early Universe. Deviations from a perfect black-body spectrum, known as spectral distortions, carry unique signatures of early physical processes. Yet, despite their significance, no primordial spectral distortions have been detected to date, and the most stringent limits remain those set by the COBE/FIRAS mission in the 1990s. However, technological advancements over the last 30 years now make the first direct measurement of these distortions an achievable milestone.

The Cosmic Monopole Observer (COSMO) instrument is a ground-based experiment
designed to measure tiny spectral distortions in the isotropic component of the Cosmic Microwave Background radiation. COSMO is a Differential Fourier Transform
Spectrometer (DFTS) in the Martin-Pupplet configuration, operating at cryogenic
temperature (lower than 4K). Two input ports compare the emission of the sky to the emission of an internal black-body calibrator, producing an interferogram thanks to a movable roof mirror, which is actuated by a cryogenic Mirror Transfer Mechanism (MTM). This is designed to be effective at cryogenic temperatures while minimizing the heat load on the cryostat. Each of the two output of the DFTS is equipped with an array of multimode Lumped Element Kinetic Inductance Detectors (LEKIDs). The detector arrays operate in two frequency bands centered at 150 GHz and 250 GHz. They are cooled to T ≃ 150mK using a dilution refrigerator, while the optical components are also maintained at cryogenic temperatures to minimize their thermal emission.

COSMO will be operated from the Italian-French Concordia station at Dome-C on the
Antarctic plateau. Extremely cold and dry, this is one of the best sites on Earth for astronomical observations in mm-waves. Nevertheless, the atmosphere is still present so COSMO will use fast elevation scans to separate the atmospheric emission and its longterm fluctuations from the monopole of the sky brightness. This requires very fast detectors, a task well-suited to LEKIDs.

In this talk, I will review the COSMO experiment, focusing on the laboratory
characterization of the black-body calibrator, as well as the design and recent results of the characterization of the 150 GHz LEKID array and the results about the first cryogenic test of the MTM.

Speaker: Alessandro Capponi (Ca' Foscari University of Venice, Sapienza University of Rome, INFN - Sez. Roma)

scar_capponi.pptx

13:40 (Talk Canceled) Kinematics of Coronal Mass Ejections: Leveraging Antarctic Observational Platforms for Enhanced Space Weather Monitoring.

Coronal Mass Ejections (CMEs) are large-scale solar eruptions capable of triggering severe space weather events, particularly impacting high-latitude regions such as the polar zones. Accurate determination of CME kinematics—velocity, acceleration, and trajectory—is critical for early warning systems and for understanding the solar-terrestrial interaction. In this study, I analyze the kinematic profiles of selected CME events using coronagraph data from SOHO/LASCO, applying height-time analysis and polynomial fitting techniques to derive their propagation characteristics.

My ongoing research explores how incorporating ground-based observational data from polar regions—particularly from Antarctica—can improve the temporal resolution and continuity of CME tracking. The Antarctic environment offers distinct advantages for solar observations, including extended daylight periods, low atmospheric disturbance, and minimal radio frequency interference. I propose that integrating data from Antarctic observatories with space-based missions could refine heliospheric models and enhance real-time space weather forecasting, especially for systems vulnerable to solar activity in polar latitudes.

This study supports the broader objective of the SCAR AAA initiative to optimize astronomical research infrastructure in extreme environments. Preliminary findings highlight the value of Antarctic observational platforms in strengthening global CME monitoring networks and advancing our understanding of solar eruptive phenomena.

Speaker: NEELISHA JAKATE (Swami Ramanand Teerth Marathwada University, Nanded)

14:00 Optimization Design of the telescope tower structure for weak snow foundation in Dome A, Antarctica

In light of the available evidence, Dome A is known as one of the best ground-based observatory sites in the world. In order to leverage the advantages offered by the atmospheric boundary layer, which has an average height of 13.9 meters, for enhanced observation capabilities, a tower is to be constructed with a height of 15 meters above ground level to elevate the telescope. Nevertheless, the particular geographical positioning of Dome A and the harsh climatic conditions that prevail on the site necessitated the overcoming of significant transportation and construction challenges in order to build the tower on the 3000 meters weak snow foundation. To ensure that the tower meets the requisite precision conditions for telescope observation, it is essential to design and optimize the strength structure of the tower in accordance with the permissible value of foundation bearing pressure. In this paper, the strength of the snow foundation was gauged and analyzed by field experiment, and the RMS value of foundation strength was 1.962 𝑀𝑃𝑎. Based on the analysis, a tower is designed and optimize to satisfy the requirements of a 2m-class telescope including the stiffness and the displacement of the top under a wind speed of 10 𝑚·𝑠-1. After optimizing the tower structure, the maximum stress of the tower is 16.703𝑀𝑃𝑎, and the maximum stress of the snow foundation is only 0.047𝑀𝑃𝑎. A line pressure is applied on the tower to simulate 10 𝑚·𝑠-1 wind pressure, which carries out a result that the maximum displacement is the angle in the direction, with a magnitude of 0.04″. The analyses presented in this paper show the result can meet the requirement of telescope observation, which also help to inform the future use of the large-scale, high-precision telescopes and other large-scale equipment at Dome A.

Speaker: haikun Wen (Niaot)

Optimization Design of the telescope tower structure for weak snow foundation in Dome A, Antarctica.pptx

14:20 Investigating Ice Drilling Performance in the Firn Layer at the South Pole

This research aims to assess the effectiveness of ice drilling operations within the firn layer at the South Pole for the IceCube Upgrade Project to install neutrino detectors below the Antarctic ice. This firn drill consists of a melting probe of 60 cm diameter. Field experiments carried out during the 2024–2025 summer season highlighted the importance of maintaining a balance between the drill head load and the drilling depth, as this balance greatly influences borehole deviation and the overall success of the drilling process. Careful management of standing load and vertical drill speed was found to reduce borehole misalignment and prevent the drill head from getting stuck, particularly in the porous firn. The study showed that uneven loading can cause the drill to tilt and make retraction more challenging. To improve efficiency, the research recommends strategies such as balancing load and depth, selecting the best drilling windows according to the combining mechanical and thermal drilling methods. These findings offer practical advice to enhance firn drilling under harsh polar conditions, thereby supporting progress in neutrino research.

Speaker: Dr Chana Sinsabvarodom (Chiang Mai University)

Ice_Drilling_Presentation_v4.pptx

14:40 The Antarctic Geospace and ATmosphere reseArch (AGATA SCAR Scientific Research Programme) and their links with the Astronomy community

The AGATA programme is a newly endorsed SCAR initiative aimed at advancing the understanding of Sun–Earth interactions and polar atmosphere dynamics through coordinated international research. After more than a decade without a dedicated SCAR programme in this area, AGATA addresses key questions in space and atmospheric physics, including atmospheric coupling, ionospheric response to geomagnetic activity, and the use of GNSS and radar observations.
AGATA brings together experts from over 40 institutions, leveraging infrastructure in both Antarctica and the Arctic. It promotes a bipolar approach to studying interhemispheric asymmetries and fosters collaboration across disciplines.
Crucially, AGATA is building connections with the astronomy and astrophysics community, seeking synergies in radio propagation studies, satellite data usage, and site-based observations in polar environments. This abstract highlights AGATA’s scientific goals and its commitment to engaging new researchers and fostering cross-disciplinary cooperation.

Speaker: Adriana Maria Gulisano (IAA/DNA, IAFE(CONICET-UBA), UBA FCEyN DF)

AGATA_Gulisanoetal_2025.pptx.pdf

15:00 → 15:35 Coffee Break + U-Shape Table Setup

15:35 → 17:00 Brainstorm & Discussion for the next OSC in Oslo and possible venues for the AAA Workshop 2027

Thursday, 18 September

09:00 → 11:30 Topic Discussion: AAA involvement in IPY 2033

IPY5-meeting topics-Sc1ar AAA Sep 18 -at- 9-11 am (1).pdf

11:30 → 12:30 Lunch Break

12:30 → 16:30 Business Meeting

Friday, 19 September

08:30 → 12:30 Special Events: Excursion