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BEGIN:VEVENT
SUMMARY:Report from the French Polar Institute
DTSTART:20210910T122000Z
DTEND:20210910T123500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7813@events.icecube.wisc.edu
DESCRIPTION:Speakers: Jerome  Chapellaz (Insitut Polair Francais)\n\nhttps
 ://events.icecube.wisc.edu/event/144/contributions/7813/
URL:https://events.icecube.wisc.edu/event/144/contributions/7813/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Superb Astronomical Seeing at Dome A
DTSTART:20210909T133000Z
DTEND:20210909T134500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7731@events.icecube.wisc.edu
DESCRIPTION:Speakers: Bin Ma (Sun Yat-sen University)\n\nFollowing the ins
 tallation of two DIMMs at Kunlun Station\, Dome A in early 2019\, we were 
 able to directly measure astronomical seeing through the winter for the fi
 rst time.  At a height of just 8 meters\,  the seeing was detected as good
  as 0.13 arcsec. For 31% time\, it was free of boundary layer turbulence\,
  and consequently was the free-atmosphere seeing only\, with a median of 0
 .31 arcsec.   We also find that the seeing and boundary layer thickness ar
 e correlated with local temperature inversion which is monitored by KLAWS\
 , a multi-layer automatic weather station.  Then we confirm that the media
 n boundary-layer thickness is about 14 m\, while it is 30 m at Dome C. The
 se results further support Dome A to have the best conditions for optical/
 infrared astronomy.\n\nhttps://events.icecube.wisc.edu/event/144/contribut
 ions/7731/
URL:https://events.icecube.wisc.edu/event/144/contributions/7731/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Progress Report of Antarctic 30cm submm telescope
DTSTART:20210908T124500Z
DTEND:20210908T130000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7738@events.icecube.wisc.edu
DESCRIPTION:Speakers: Nario Kuno\, Antarctic Astronomy Consortium of Japan
 \n\nWe have developed a 30-cm submm telescope which was designed to be ope
 rated in Antarctica (Ishii et al. 2014). We are planning to transport the 
 telescope to Dome Fuji in Antarctic plateau to make a survey of the Galact
 ic plane in CO(J=4-3) and $[$CI$](^3P_1-^3P_0$). $[$CI$](^3P_1-^3P_0$) is 
 a good tracer of diffuse molecular gas\, while CO(J=4-3) is a good tracer 
 of warm and dense molecular gas associated with star forming regions. Sinc
 e the beam size is ~9’ which is comparable to that of the Columbia-CfA 1
 .2m survey in CO(J=1-0)\, we can make direct comparisons with the lower ex
 citation CO line to investigate the physical condition of molecular gas. W
 e are updating the 500 GHz SIS receiver using state of the art SIS mixer d
 eveloped by ATC of NAOJ. The mixer enables us to observe the two lines sim
 ultaneously. We also have developed an optical pointing system which can b
 e used in summer of Antarctica\, that is\, daytime. We will apply for gene
 ral observational research of National Institute of Polar Research of Japa
 n.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/7738/
URL:https://events.icecube.wisc.edu/event/144/contributions/7738/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Unveiling Our Dynamic Infrared Sky
DTSTART:20210910T115000Z
DTEND:20210910T120500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7740@events.icecube.wisc.edu
DESCRIPTION:Speakers: Tony Travouillon\, Tristan Guillot\, Roger Smith\, D
 on Figer\, Mansi Kasliwal (Caltech)\, Anna Moore\, Michael Ashley\n\nMany 
 astronomical events shine the brightest in the infrared due to atomic opac
 ity\, self enshrouding\, dust extinction\, or low temperature. When we saw
  the first electromagnetic counterpart to gravitational waves from a binar
 y neutron star merger\, it was the rapid reddening due to bound-bound opac
 ity and infrared spectral features that confirmed the synthesis of heavy e
 lements by the r-process. Unveiling infrared counterparts to neutron star 
 black hole mergers requires sensitive wide-field infrared surveyors. The b
 est place to build a sensitive infrared surveyor is the Antarctic given th
 e extremely low sky background in the K-dark bandpass. Here\, we present a
  fully cryogenic Antarctic concept for such a dream infrared surveyor that
  leverages the lower background\, advances in detector technology and prog
 ress from pathfinder experiments. A companion talk by Roger Smith will des
 cribe the enabling technologies in more detail.\n\nhttps://events.icecube.
 wisc.edu/event/144/contributions/7740/
URL:https://events.icecube.wisc.edu/event/144/contributions/7740/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The radio detection of neutrinos in polar ice
DTSTART:20210909T120000Z
DTEND:20210909T121500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7743@events.icecube.wisc.edu
DESCRIPTION:Speakers: Eric Oberla\n\nThe low expected flux of cosmic neutr
 inos drives the need for neutrino experiments with large exposures and low
 er thresholds. Radio experiments can achieve such large exposures by takin
 g advantage of the coherent broadband radio emission resulting from ultra-
 high-energy (E>10^16 eV) neutrino interactions. In this talk\, I will revi
 ew the status of existing Antarctic radio experiments and discuss the new 
 Radio Neutrino Observatory in Greenland (RNO-G)\, which completed the firs
 t season of detector installation in the summer of 2021. The outlook for t
 he IceCube-Gen2 radio array will also be briefly presented.\n\nhttps://eve
 nts.icecube.wisc.edu/event/144/contributions/7743/
URL:https://events.icecube.wisc.edu/event/144/contributions/7743/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Science Overview for the IceCube Neutrino Observatory and Future G
 en2
DTSTART:20210909T110000Z
DTEND:20210909T111500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7747@events.icecube.wisc.edu
DESCRIPTION:Speakers: Lu Lu (University of Wisconsin–Madison)\n\nThe Ice
 Cube Neutrino Observatory is the largest neutrino telescope in the world a
 nd uses clear Antarctic ice to detect neutrinos and cosmic rays over an in
 credibly wide range of energies. The multifaceted experiment runs with ove
 r 99% uptime and has been taking high-quality data for over a decade. In m
 y talk I will give a brief overview of IceCube science including real-time
  efforts in\npartnership with multi-messenger observatories\, the possible
  first identification of astrophysical tau neutrinos and the recent result
  of the detection of W boson (Glashow) resonance at the energy beyond reac
 h of the currently operating and future planned particle accelerators. The
  next generation detector\, IceCube Gen2\, is designed to do precision neu
 trino astronomy at high energies. I will briefly discuss the science gain 
 with Gen2.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/7747
 /
URL:https://events.icecube.wisc.edu/event/144/contributions/7747/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Limits on cosmological b-mode polarization from Spider
DTSTART:20210908T113000Z
DTEND:20210908T114500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7728@events.icecube.wisc.edu
DESCRIPTION:Speakers: william jones (Princeton University)\n\nSpider is a 
 CMB polarimeter designed for the Antarctic Long Duration Balloon platform.
   Spider has completed one flight of the two-flight program.  In the first
  flight\, Spider has mapped the astrophysical linear polarization over abo
 ut 10% of the full sky\, with significantly greater sensitivity than Planc
 k HFI in the same region.  We report limits to the cosmological B-mode pol
 arization that are derived from a subset of these data\, corresponding to 
 about 6% of the full sky\, and discuss the plans and prospects for the upc
 oming flight.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/7
 728/
URL:https://events.icecube.wisc.edu/event/144/contributions/7728/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Sky brightness evaluation at Concordia Base\, Antarctica
DTSTART:20210908T123000Z
DTEND:20210908T124500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7730@events.icecube.wisc.edu
DESCRIPTION:Speakers: Gianalfredo Nicolini (INAF)\, Silvano Fineschi (INAF
 )\, Luca Zangrilli (INAF)\, Giuseppe Massone (INAF)\, Gerardo Capobianco (
 INAF)\, Alessandro Liberatore (Istituto Nazionale di Astrofisica (INAF))\,
  Roberto Susino (INAF)\n\nThe study of the sky characteristics plays a fun
 damental role for many astrophysical experiments and on-ground observation
 s. In the field of solar physics\, in particular for the observation of th
 e solar corona\, it is required to have a very low sky brightness value. \
 nCurrently the only place on Earth with the sky characteristics that allow
  a continuous coronagraphic measurements is at the Mauna Loa Observatory -
  MLO (Hawaii\, ~3400m a.s.l.). \nIn the following\, we show the results ob
 tained as part of the ESCAPE project in Antarctica. In particular\, some o
 f the outcome obtained during the XXXIV and XXXV Italian missions in Antar
 ctica at the Concordia Base (Dome C\, ~ 3300m a.s.l.) are presented. The l
 ocal sky brightness was one of the measured quantities. These data were ca
 rried out with a coronagraph (AntarctiCor) designed and built for Antarcti
 c environments and able of capturing\, at the same time\, images with 4 di
 fferent polarizations.\n\nhttps://events.icecube.wisc.edu/event/144/contri
 butions/7730/
URL:https://events.icecube.wisc.edu/event/144/contributions/7730/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Progress of Antarctic Survey Telescopes(AST3) project
DTSTART:20210909T131500Z
DTEND:20210909T133000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7727@events.icecube.wisc.edu
DESCRIPTION:Speakers: Xiaoyan Li\n\nThe trio Antartica Survey Telescopes(A
 ST3) project is the second generation optical telescopes designed to run o
 n Dome A. The first two telescopes have deployed and operated at Dome A si
 nce 2012 and 2015. The third one is now at domestic commissioning stage at
  Yaoan observatory in Yunnan province\, China. This talk will give some de
 tails about the latest progress of the project.\n\nhttps://events.icecube.
 wisc.edu/event/144/contributions/7727/
URL:https://events.icecube.wisc.edu/event/144/contributions/7727/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A New Seeing Monitor and Profiler for Eureka\, on Ellesmere Island
DTSTART:20210910T124500Z
DTEND:20210910T130000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7729@events.icecube.wisc.edu
DESCRIPTION:Speakers: Eric Steinbring (NRC Canada\, Herzberg Astronomy and
  Astrophysics)\n\nAlthough operations at the Polar Environment Atmospheric
  Research Laboratory (PEARL) nearby Eureka on Ellesmere Island (80 degrees
  North) have lately been paused\, there is renewed interest in the site fo
 r astrophysical observations. I will briefly review known PEARL site condi
 tions\, and describe the status of a planned compact instrument for charac
 terization of seeing near the ground\, of particular interest for continuo
 usly observing low-elevation targets.\n\nhttps://events.icecube.wisc.edu/e
 vent/144/contributions/7729/
URL:https://events.icecube.wisc.edu/event/144/contributions/7729/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The Greenland Telescope – Thule Extended Operations
DTSTART:20210910T130000Z
DTEND:20210910T131500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7734@events.icecube.wisc.edu
DESCRIPTION:Speakers: Ming-Tang Chen (Academia Sinica Institute of Astrono
 my and Astrophysics)\n\nI will report the progress and the status of the G
 reenland Telescope in Thule\, Greenland. The telescope was commissioned in
  the spring of 2018\, and it had since participated in the global VLBI obs
 ervation campaign in millimeter and submillimeter wavelengths. The GLT has
  been a partner station in the Even Horizon Telescope since 2018 for the 2
 30 GHz VLBI observation. In 2021\, we have also confirmed the fringe detec
 tion with ALMA at 345 GHz.  Besides the science observations\, the operati
 ons in Thule allow us to test many new functions\, especially those design
 ed to protect the hardware from the harsh cold environment of the GLT befo
 re the telescope is deployed to its final destination near the summit of G
 reenland. The GLT is to achieve two primary scientific goals: To image/stu
 dy the shadow of the supermassive black hole in M87 [1] and conduct astron
 omy research in terahertz frequencies. Since the 12-m ALMA North America P
 rototype Antenna was awarded to our team\, the Academia Sinica Institute o
 f Astronomy & Astrophysics (ASIAA) and the Smithsonian Astrophysical Obser
 vatory have entirely rebuilt the antenna from the ground up for operation 
 in the extreme arctic conditions of northern Greenland [2]. The Thule site
  is our first staging area before moving to Greenland’s high site\, and 
 we have conducted a comprehensive set of technical tests on the telescope 
 in Thule. We have attained the first light at 230 GHz at the end of 2017 a
 nd subsequently participated in global VLBI observations at 86 GHz and 230
  GHz. While conducting system verifications and some specific science obse
 rvations\, we have explored and studied moving the antenna to its final de
 stination. The final stage of the project will bring the antenna and equip
 ment 1100 km inland to the 3216m summit of the Greenland ice sheet\, where
  the antenna will be reassembled\, tested\, and commissioned to take advan
 tage of the arid climate and the northern latitude.\nCredits:\nThe Greenla
 nd Telescope Project is led by the Academia Sinica Institute of Astronomy 
 and Astrophysics and the Smithsonian Astrophysical Observatory\n\nhttps://
 events.icecube.wisc.edu/event/144/contributions/7734/
URL:https://events.icecube.wisc.edu/event/144/contributions/7734/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Report of progress on the instalation of an optical robotic observ
 atory at the argentine base Belgrano II
DTSTART:20210910T131500Z
DTEND:20210910T133000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7735@events.icecube.wisc.edu
DESCRIPTION:Speakers: Mario Melita (CONICET)\, Adriana Gulisano (Instituo 
 Antártico Argentino)\n\nOur objective is the development of a robotic opt
 ical observatory designed to house a 20" telescope with a low focal ratio 
 of abou f/3. Naturally\, this project will take advantage of observing at 
 very high latitudes during the southern night. The scientific objectives w
 ill be focused on high brightness point sources with valuable information 
 for various areas of astronomy such as Planetary Sciences or Stellar Astro
 physics and also on Planetary and Space Defense through the detection of p
 otentially dangerous objects in the Solar System and space junk .  This pr
 oject is part of the National Antarctic Plan\, has passed the environmenta
 l impact requirements and was elevated to the Antarctic Treaty countries. 
 In this presentation we will detail the characteristics of the observatory
  and its fundamental motivations\, the current state of development\, the 
 difficulties encountered in the process and the missing tasks for completi
 on.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/7735/
URL:https://events.icecube.wisc.edu/event/144/contributions/7735/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The impact of the COVID-19 pandemic on ECRs
DTSTART:20210909T124500Z
DTEND:20210909T130000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7737@events.icecube.wisc.edu
DESCRIPTION:Speakers: Jennifer Cooper\n\nThis presentation will broadly co
 ver the impacts of the COVID-19 pandemic on students and early career rese
 archers (ECRs) in the Antarctic and Astronomical fields over the past 1.5 
 years. I will highlight the obstacles many have faced such as graduation/r
 esearch delays\, as well as some new policies that have been introduced th
 at improve access and collaboration. Finally\, I will briefly discuss a *N
 ature* article published in July 2021 on the wider impact to Polar Researc
 hers.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/7737/
URL:https://events.icecube.wisc.edu/event/144/contributions/7737/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A Decade of Astronomy at Dome A
DTSTART:20210909T140000Z
DTEND:20210909T141500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7741@events.icecube.wisc.edu
DESCRIPTION:Speakers: Zhaohui Shang (National Astronomical Observatories\,
  CAS)\n\nAstronomy work has been carried out at Dome A for more than ten y
 ears.  The efforts have greatly advanced our knowledge in understanding th
 e site conditions for astronomical observations\, the instrumentation unde
 r extreme Antarctica conditions\, and the research in time-domain astronom
 y. A complete review is available in Research in Astronomy and Astrophysic
 s (Shang 2020\, RAA\, 20\, 168).  We will highlight the major work and res
 ults in this presentation.\n\nhttps://events.icecube.wisc.edu/event/144/co
 ntributions/7741/
URL:https://events.icecube.wisc.edu/event/144/contributions/7741/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Advantage of Space Debris Observation in Antarctica
DTSTART:20210909T130000Z
DTEND:20210909T131500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7751@events.icecube.wisc.edu
DESCRIPTION:Speakers: Zhengyang Li (Nanjing Institute of Astronomical Opti
 cs and Technology )\, Chenwei Yang (Polar Research Institute of China)\, P
 eng Jiang (Polar Research Institute of China)\n\nIncreasing space debris h
 as seriously threatened the safety of spacecraft of various countries. The
  Pole regions are the most densely distributed regions of Low-Earth orbit 
 space debris\, and are ideal sites for observing LEO space debris. Investi
 gating Antarctica as a window to the skies for satellite traffic managemen
 t has been identified as an important goal for Antarctic Astronomy in the 
 proposal of ASTRO Sciences to SCAR. For the first step\, we systematically
  evaluated the performance of space debris observation at Kunlun Station i
 n Antarctica by revisiting archived data taken in polar night\, yielding h
 igh detection capability and efficiency in comparison with and numerical s
 imulations. In this year\, we plan to deploy small telescope array and car
 ry on small scale survey of space debris as further experiment at Zhongsha
 n Station in Antarctica. In this talk\, we will also report the preliminar
 y results of site testing taken at Taishan Station\, which is almost in ha
 lfway from Zhongshan to Kunlun Station\, and the development of logistics 
 in CHINARE.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/775
 1/
URL:https://events.icecube.wisc.edu/event/144/contributions/7751/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Wind turbines for the high Antarctic plateau
DTSTART:20210910T134500Z
DTEND:20210910T140000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7750@events.icecube.wisc.edu
DESCRIPTION:Speakers: Matthew Gerges (University of New South Wales)\, Mic
 hael Ashley (University of New South Wales)\n\nAt the University of New So
 uth Wales we are designing a wind turbine for the conditions found at Chin
 a's Kunlun Station at Dome A in Antarctica. While Dome A is the least wind
 y place on Earth\, renewable energy from the wind is still possible and ha
 s many advantages over the diesel engines that are typically used: for exa
 mple\, wind energy reduces the need to transport and store fuel while redu
 cing pollution and lowering maintenance requirements. Our baseline design 
 is a horizontal axis wind turbine with three 6m long fixed-pitch blades an
 d a 21m monopole tower.  A 10kW alternator is driven directly from the hub
 . We anticipate a yearly average power of 1kW. Both the tower and blades w
 ill be made of carbon fibre due to its excellent structural properties eve
 n at low temperature. All components must be chosen to work at low tempera
 ture and optimised for the low wind speeds that are found at Dome A. We ar
 e also considering ease of construction\, installation\, and maintenance.\
 n\nhttps://events.icecube.wisc.edu/event/144/contributions/7750/
URL:https://events.icecube.wisc.edu/event/144/contributions/7750/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Instrumentation and Polar Infrastructure Development Supporting th
 e BICEP Array Telescope
DTSTART:20210908T114500Z
DTEND:20210908T120000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7749@events.icecube.wisc.edu
DESCRIPTION:Speakers: Benjamin L. Schmitt (Harvard-Smithsonian Center for 
 Astrophysics)\, For The BICEP Array Collaboration\n\nMeasurement of the po
 larized Cosmic Microwave Background (CMB) over the past few decades has en
 abled precision probes of the evolutionary history\, composition\, and dyn
 amics of the primordial Universe.  Next-generation CMB experiments will e
 xtend this scientific reach\, allowing for tests of the inflationary theor
 y of the early Universe\, driven through constraints on the tensor-scalar 
 ratio “r” via the search for primordial B-mode polarization.  The BIC
 EP Array telescope program is targeting observation of B-modes at large an
 gular scales\, building on constraints already placed by the BICEP/Keck pr
 ogram. BICEP Array comprises four BICEP3-class receivers which will operat
 e in conjunction with BICEP3 at 30/40\, 95\, 150\, and 220/270 GHz. The 30
 /40 GHz receiver was deployed to the Amundsen-Scott South Pole Station dur
 ing the 2019-2020 Austral summer. With all receivers deployed\, BICEP Arra
 y will measure primordial gravitational waves to a precision of σ(r) betw
 een 0.002 and 0.004 after a full three years of observations\, with over 3
 0\,000 detectors on the sky.  This talk will provide an overview of the i
 nstrumentation design of the BICEP Array telescope\, and infrastructure in
  development that will enable a sustainable future for BICEP Array and nex
 t-generation CMB science at the South Pole.\n\nhttps://events.icecube.wisc
 .edu/event/144/contributions/7749/
URL:https://events.icecube.wisc.edu/event/144/contributions/7749/
END:VEVENT
BEGIN:VEVENT
SUMMARY:China's Kunlun Station is an extraordinarily good site for deep in
 frared surveys
DTSTART:20210909T134500Z
DTEND:20210909T140000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7760@events.icecube.wisc.edu
DESCRIPTION:Speakers: Michael Ashley (University of New South Wales)\n\nAt
  any infrared/THz wavelength longer than about 2.3 microns\, China's Kunlu
 n Station in Antarctica has very possibly the darkest sky and best conditi
 ons  - seeing\, cloud coverage\, atmospheric stability\, transparency -  o
 f any site on Earth. This directly translates into dramatic improvements i
 n survey speed and depth. In the near-infrared\, the Kdark region just lon
 gward of 2.3 microns is particularly favourable\, with flux from the night
  sky and telescope being factors of around 50 times less that temperate-la
 titude observatories. The Nanjing Institute of Astronomical Optics and Tec
 hnology has an Antarctic-rated 0.5m telescope ready to go\, the Australian
  Astronomical Observatory is building the camera cryostat\, the UK Astrono
 mical Technology Centre is integrating the detector system\, and the Unive
 rsity of New South Wales is designing the support electronics and power su
 pplies. Together\, these contributions form the Kunlun Infrared Sky Survey
 \, which will explore new regions of parameter space and act as a pathfind
 er for even more ambitious projects that can be undertaken nowhere else on
  Earth.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/7760/
URL:https://events.icecube.wisc.edu/event/144/contributions/7760/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The micrometeorite flux at Dome C (Antarctica) with the CONCORDIA 
 collection
DTSTART:20210908T131500Z
DTEND:20210908T133000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7752@events.icecube.wisc.edu
DESCRIPTION:Speakers: Juan Diego Carrillo-Sánchez (Department of Physics\
 , Catholic University of America)\, Cécile Engrand (Université Paris-Sac
 lay\, CNRS/IN2P3\, IJCLab)\, Lucie Delauche (Université Paris-Saclay\, CN
 RS/IN2P3\, IJCLab)\, Petr Pokorný (Department of Physics\, Catholic Unive
 rsity of America)\, Marie Godard (ISMO\, CNRS\, Univ. Paris Saclay)\, Juli
 en Rojas Arispe (IJCLab/Université Paris-Saclay)\, Emmanuel Dartois (ISMO
 \, CNRS\, Univ. Paris Saclay)\, John M.C. Plane (School of Chemistry\, Uni
 v. of Leeds)\, Jean Duprat (CNRS-MNHN)\, Matthieu Gounelle (IMPMC\, CNRS-M
 NHN-Sorbonne Universités)\n\nThe flux of extraterrestrial material on Ear
 th is dominated by sub-millimeter particles\, however the mass distributio
 n and absolute value of this cosmic dust flux at the Earth surface is stil
 l uncertain due to the difficulty to monitor both the collection efficienc
 y and the exposure parameter (*i.e.* the area-time product in m$^2$.yr). T
 hanks to the exceptional conditions encountered in central Antarctic regio
 ns\, we recently succeeded to measure there the micrometeorite flux down t
 o 30 µm (Rojas et al.\, 2021). \n\nDuring the last 2 decades\, we perform
 ed several field trips at Dome C to recover micrometeorites by melting and
  sieving large volume of ultra-clean snow using a dedicated protocol (IPEV
  program #1120\, Duprat et al. (2010)\; Duprat et al. (2007)). The CONCORD
 IA station is operated by the French and Italian polar institutes (IPEV an
 d PNRA) at Dome C (Antarctica). The regular precipitation rate and the exc
 eptional cleanliness of the snow at Dome C allow a unique control on both 
 the exposure parameter and the collection efficiency\, mandatory to derive
  the micrometeorite flux.\n\nThe thorough inspection of the filters for ma
 ny years allowed us to recover thousands of particles. Each one was indivi
 dually imaged by Secondary Electron Microscopy and its bulk composition wa
 s determined by Energy-Dispersive X-ray spectra. Micrometeorites were clas
 sified in two main types: the unmelted micrometeorites (uMM) that went thr
 ough the atmosphere without melting and the cosmic spherules (CSs) that ha
 ve totally melted during the atmospheric entry. Based on the inferred size
 /mass distribution\, we derived the statistical uncertainties expected for
  collections with exposure parameters ranging from 0.1 up to 10$^5$ m$^2$.
 yr. Within the 30-350 µm diameter range\, we measured mass fluxes of 3.0 
 µg.m$^{-2}$.yr$^{-1}$ for uMMs and 5.6 µg.m$^{-2}$.yr$^{-1}$ for CSs. Ex
 trapolated to the global flux of particles in the 12-700 µm diameter rang
 e\, the corresponding annual mass flux of extraterrestrial dust at Earth s
 urface is 5\,200 tons.yr$^{-1}$ (1\,600 and 3\,600 tons.yr$^{-1}$ of uMMs 
 and CSs\, respectively). The flux of altered and unaltered carbon carried 
 by heated and un-heated particles at Earth surface is estimated to range f
 rom 20 to 100 tons.yr$^{-1}$. The results obtained in this study allow to 
 put constraints on the origin of the micrometeorite mass flux (Plane\, 201
 2). \n\n**References:**\n\nDuprat\, J.\, Dobrică\, E.\, Engrand\, C.\, Al
 éon\, J.\, Marrocchi\, Y.\, Mostefaoui\, S.\, Meibom\, A.\, Leroux\, H.\,
  Rouzaud\, J.-N.\, Gounelle\, M.\, Robert\, F.\, 2010. Extreme Deuterium E
 xcesses in Ultracarbonaceous Micrometeorites from Central Antarctic Snow. 
 Science 328\, 742-745 \n\nDuprat\, J.\, Engrand\, C.\, Maurette\, M.\, Kur
 at\, G.\, Gounelle\, M.\, Hammer\, C.\, 2007. Micrometeorites from Central
  Antarctic snow: The CONCORDIA collection. Adv. Space Res. 39\, 605-611.\n
 \nPlane\, J.M.C.\, 2012. Cosmic dust in the earth's atmosphere. Chemical S
 ociety Reviews 41\, 6507-6518.\n\nRojas\, J.\, Duprat\, J.\, Engrand\, C.\
 , Dartois\, E.\, Delauche\, L.\, Godard\, M.\, Gounelle\, M.\, Carrillo-S
 ánchez\, J.D.\, Pokorný\, P.\, Plane\, J.M.C.\, 2021. The micrometeorite
  flux at Dome C (Antarctica)\, monitoring the accretion of extraterrestria
 l dust on Earth. Earth Planet. Sci. Lett. 560\, 116794.\n\nhttps://events.
 icecube.wisc.edu/event/144/contributions/7752/
URL:https://events.icecube.wisc.edu/event/144/contributions/7752/
END:VEVENT
BEGIN:VEVENT
SUMMARY:RESOURCE Radio Sciences Research on AntarCtic AtmosphEre
DTSTART:20210908T133000Z
DTEND:20210908T134500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7756@events.icecube.wisc.edu
DESCRIPTION:Speakers: Lucilla Alfonsi (INGV)\, Nicolas Bergeot\n\nWe repor
 t the establishment of a Programme Planning Group for developing a SCAR (S
 cientific Committee on Antarctic Research) Scientific Research Programme (
 SRP) entitled “Radio Sciences Research on AntarCtic AtmosphEre” (RESOU
 RCE). The proposed SRP aims to gather the communities that investigate the
  polar atmosphere\, with particular reference to Antarctica but with a bi-
 polar perspective\, by means of radio probes into a common shared initiati
 ve. The scope is to improve the current understanding of the Antarctic atm
 osphere by sharing the expertise and the experience achieved by several sc
 ientific teams in the world\, thus facilitating the advancement in the fie
 ld and avoiding any duplication of activities already in action. SCAR is t
 he best platform to create the necessary environment to assess the actual 
 current understanding and to address the efforts to fill the gaps. The rad
 io techniques enabled by ground and satellite-based sensors have proved to
  be very effective when probing the lower\, middle and upper atmosphere. I
 n parallel\, several scientific communities using radio techniques spent s
 ignificant efforts to remove (what they consider) “atmospheric noise” 
 to extract the desired information from their measurements (as in the case
  of geodesy).  However\, these communities do not sufficiently interact. T
 he RESOURCE SRP aims to take advantage of the experience of the SCAR Exper
 t Group GRAPE (GNSS Research and Application for Polar Environment). The p
 roposed SCAR scientific programme RESOURCE will build upon this important 
 legacy by enhancing interactions between the scientists who measure and ut
 ilise the entire radio spectrum\, either as an auxiliary or principal obse
 rvation\, to study the atmosphere\, the ionosphere\, the ocean\, the solid
  earth and outer space as well as ancillary measurements such as from magn
 etometers which provide supporting data on the solar-terrestrial relations
 hip. Moving from the radio probing of the atmosphere\, the proposed SRP ai
 ms to encompass the ICESTAR (past SCAR SRP) heritage to fill the current g
 ap of SRPs dedicated to the study of the atmosphere\, the upper atmosphere
  and the solar-terrestrial relationship. Additionally\, RESOURCE is design
 ed to support the SERSE SRP\, as a continuation of the experience matured 
 within the GRAPE EG\, and the AAA EG to facilitate the interaction between
  researchers in the fields of Astronomy\, Astrophysics\, Atmosphere and Io
 nosphere. RESOURCE outcomes are relevant for global change studies\, contr
 ibuting to the investigation of the coupling between the neutral and ioniz
 ed atmosphere and supporting a correct evaluation of the atmospheric impac
 t on the measurements of geophysical parameters.\nRESOURCE aspires to purs
 ue three main scientific objectives: \n1.	To monitor the polar atmosphere\
 ;\n2.	To investigate the polar atmosphere\; \n3.	To support the sciences i
 nterested in removing the atmospheric contribution from their observations
  or mitigating the negative impact of atmospheric contributions to their o
 bservations.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/77
 56/
URL:https://events.icecube.wisc.edu/event/144/contributions/7756/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Rare Transits Observed by ASTEP from Antarctica
DTSTART:20210910T112000Z
DTEND:20210910T113500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7754@events.icecube.wisc.edu
DESCRIPTION:Speakers: Abdelkrim Agabi\, Georgina Dransfield (University of
  Birmingham)\, Djamel Mékarnia\, Lyu Abe (OCA)\, Nicholas Crouzet\, Amaur
 y Triaud\, Tristan Guillot\, François-Xavier Schmider\, Philippe Bendjoya
 \, Olga Suarez\n\nThe Transiting Exoplanet Survey Satellite was launched i
 n 2018 to search the sky for planetary candidates. Of the 870+ southern pl
 anetary candidates from TESS currently awaiting confirmation\, roughly 10%
  have transit durations longer than five hours\; a further third of these 
 have orbital periods longer than 20 days. Systems like these could fall in
 to the sparsely populated parameter space of long-period gas giants\; but 
 long transits that happen infrequently present an observational challenge 
 from the ground. Not so for ASTEP\, a 40cm telescope installed at Dome C i
 n Antarctica. ASTEP’s proximity to the South Pole means that it enjoys o
 utstanding photometric conditions\, as well exceptional phase coverage due
  to uninterrupted observing during the Austral Winter. In this talk I will
  share some results from ASTEP’s first seasons of SG1 observing\, includ
 ing uninterrupted 10 hour-long transits\, TTV monitoring\, and the first e
 ver ground-based transit of a circumbinary planet. I will also show that A
 STEP has the potential to make a significant contribution to ephemeris ref
 inement for upcoming missions such as JWST and Ariel.\n\nhttps://events.ic
 ecube.wisc.edu/event/144/contributions/7754/
URL:https://events.icecube.wisc.edu/event/144/contributions/7754/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The One-meter Polar Large Telescope (PLT)  prototype for Concordia
DTSTART:20210910T113500Z
DTEND:20210910T115000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7755@events.icecube.wisc.edu
DESCRIPTION:Speakers: Isabelle Vauglin (CRAL/CNRS - Observatoire de Lyon)\
 , Gil Moretto (CRAL)\n\nFollowing the ANGISS 2.5m off-axis telescope proje
 ct\, presented at the AAA-2015 conference\, we propose to build a 1m proto
 type for 2.5m PLT. Such an optical design is based on a common 2.5m off-ax
 is primary mirror delivering two science cases modes: (1) two mirror corre
 ctor optimized to a wide FOV (1Deg) for IR survey and (2) one mirror corre
 ctor optimized for a narrow FOV for direct exoplanet detection. This 1-m p
 roof-of-concept prototype will access and validate the off-axis PLT techni
 cal feasibility and IPEV logistics for larger telescope.\n\nhttps://events
 .icecube.wisc.edu/event/144/contributions/7755/
URL:https://events.icecube.wisc.edu/event/144/contributions/7755/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Technical Advances towards the IceCube-Gen2 Neutrino Observatory
DTSTART:20210909T113000Z
DTEND:20210909T114500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7758@events.icecube.wisc.edu
DESCRIPTION:Speakers: Carsten Rott (University of Utah)\n\nIceCube-Gen2 is
  a planned extension of the IceCube Neutrino Observatory at the geographic
  South Pole. Gen2 is optimized to search for sources of astrophysical neut
 rinos from TeV to EeV energies. IceCube-Gen2 builds on a successful decade
  of scientific observations with IceCube. The observatory will utilize opt
 ical sensor modules integrated into the deep ultra-clear Antarctic ice for
  the detection of Cherenkov light from neutrino interactions\, surface det
 ectors on the ice for the detection of cosmic-ray air showers\, and an ext
 ended radio array for sensing of ultra-high-energy neutrinos. The presenta
 tion will review future IceCube technologies and infrastructure. Technolog
 ies for the construction and operations of the Gen2 detector will be descr
 ibed\, with a particular emphasis on sustainability and resource optimizat
 ion.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/7758/
URL:https://events.icecube.wisc.edu/event/144/contributions/7758/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Cosmic Ray Intensity and Spectral Changes during 27-day Variations
  Compared with Heliospheric Parameters Using Time-Delay Measurements from 
 Antarctic Neutron Monitor Stations
DTSTART:20210909T121500Z
DTEND:20210909T123000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7757@events.icecube.wisc.edu
DESCRIPTION:Speakers: Paul Evenson (University of Delaware)\, Pradiphat Mu
 angha (Mahidol University)\, John E. Humble (University of Tasmania)\, Suy
 eon Oh (Chonnam National University)\, Alejandro Sáiz (Mahidol University
 )\, Surujhdeo Seunarine (University of Wisconsin-River Falls)\, Jongil Jun
 g (Chungnam National University)\, Marc L. Duldig (University of Tasmania)
 \, Chanoknan Banglieng (Rajamangala University of Technology Thanyaburi)\,
  David Ruffolo (Mahidol University)\n\nNeutron monitors (NMs) are ground-b
 ased detectors of the secondary particles produced in atmospheric cascades
  from primary cosmic rays.  Using neutron time-delay data from neutron mon
 itors (NMs)\, we can extract the leader fraction\, *L*\, of neutron counts
  that do not follow a previous neutron count in the same counter tube due 
 to the cosmic ray shower.  *L* is the inverse of the neutron multiplicity 
 and serves as a proxy of the cosmic ray spectral index over the rigidity r
 ange of the NM response function.  We present a comparative analysis of *L
 * from four Antarctic NM stations outfitted with special electronics to co
 llect neutron time-delay distributions: South Pole (SP)\, McMurdo (MC)\, J
 ang Bogo (JB) and Mawson (MA).  To first order *L* varies in concert with 
 the count rate *C*\, reflecting unrolling of the GeV-range Galactic cosmic
  ray (GCR) spectrum as part of solar modulation during the declining phase
  of solar cycle 24 and during solar minimum.  We use wavelet analysis to s
 tudy the periodicity of *L*\, the count rate *C*\, and heliospheric parame
 ters to consider their relationship with the 27-day variations.  Variation
  in *C* was much more variable over 27 days due to high-speed solar wind s
 treams (HSSs) and corotating interaction regions (CIRs)\, also in strong c
 ombination with the higher harmonics\, while *L* usually had a very weak v
 ariation.  Near the solar minimum of 2019-2020\, we observed essentially n
 o 27-day variation in *C*. In contrast\, during 2015-2016\, near solar max
 imum\, the 27-day variation in *L* and *C* was much stronger and fluctuati
 ng.  Our results indicate weak GeV-range GCR spectral variation due to HSS
 s and CIRs\, relative to the flux variation\, in contrast with the strong 
 observed spectral variation due to solar modulation.  We acknowledge logis
 tical support from Australia’s Antarctic Program and support from the Na
 tional Astronomical Research Institute of Thailand\, grant RTA6280002 from
  Thailand Science Research and Innovation\, and US NSF Office of Polar Pro
 grams Award No. 1341312.\n\nhttps://events.icecube.wisc.edu/event/144/cont
 ributions/7757/
URL:https://events.icecube.wisc.edu/event/144/contributions/7757/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The Analysis of the Snow Mechanics and the Survey Telescopes Tower
  in Dome A
DTSTART:20210910T133000Z
DTEND:20210910T134500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7736@events.icecube.wisc.edu
DESCRIPTION:Speakers: haikun Wen (Niaot)\, Xuefei Gong (NIAOT)\n\nAbstract
 :\nLocated in the highest point of Antarctic ice cap\, Dome A has been con
 sidered as one of the best astronomical observatory sites in the world. So
 me survey telescopes is planning to be installed in Dome A. Unlike any oth
 er areas\, these telescopes have to be settled on the snow ground. In that
  case\, it is very important to analyze the Snow mechanics\,and the deform
 ation of the telescope pier that mostly is truss tower in Dome A. The pres
 entation firstly introduced the analysis of the snow strength and elastic 
 modulus in Dome A. Secondly\,the dynamic and statics analysis of the teles
 cope tower and the dome tower will be shown in this presentation. Based on
  the design of the towers\, the snow treatment and strength test method wi
 ll be introduced at last.\nKey words: Dome A\; Snow Mechanics\; Truss Towe
 r\n\nhttps://events.icecube.wisc.edu/event/144/contributions/7736/
URL:https://events.icecube.wisc.edu/event/144/contributions/7736/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Response Functions of a Semi-Leaded Neutron Monitor from Latitude 
 Surveys during 2018 - 2020
DTSTART:20210908T130000Z
DTEND:20210908T131500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7744@events.icecube.wisc.edu
DESCRIPTION:Speakers: Alejandro Sáiz (Mahidol University)\, Pierre-Simon 
 Mangeard (University of Delaware)\, Achara Seripienlert (National Astronom
 ical Research Institute of Thailand (NARIT)\, Chiang Mai 50180\, Thailand)
 \, Siramas Komonjinda (Chiang Mai University)\, Jim Madsen (University of 
 Wisconsin–Madison)\, Kanokkarn Fongsamut (Chiang Mai Universit)\, Kazuok
 i Munakata (Shinshu University)\, Waraporn Nuntiyakul (Chiang Mai Universi
 ty)\, David Ruffolo (Mahidol University)\, Pongpichit Chuanraksasat (Natio
 nal Astronomical Research Institute of Thailand (NARIT))\, Boonraksa Soont
 hornthum (National Astronomical Research Institute of Thailand (NARIT))\, 
 Paul Evenson (University of Delaware)\, Sidarat Khamphakdee (Chiang Mai Un
 iversity)\, Jiang Peng (Polar Research Institute of China)\n\nWe have deve
 loped a mobile neutron monitor (“Changvan”) with three neutron counter
 s to investigate cosmic ray spectral variations via ship-borne latitude su
 rveys. Because Earth’s magnetic field excludes cosmic rays below the loc
 al geomagnetic cutoff rigidity\, which depends on magnetic latitude\, the 
 count rate due to atmospheric neutrons from cosmic ray showers vs. cutoff 
 rigidity (i.e.\, the response function) is directly related to the cosmic 
 ray spectrum.  Repeated measurements with the same detector over different
  solar cycle phases can provide precise information about cosmic ray spect
 ral variations.  The Changvan uses the NM64 design\, except that the centr
 al counter lacks the lead producer\, so we call this a “semi-leaded” n
 eutron monitor. The Changvan was operated on two voyages on the Chinese ic
 ebreaker “Xue Long” between Shanghai and Antarctica during 2018 – 20
 20\, from which we have measured the response function of each counter.  W
 e present a preliminary comparison of response functions from Monte Carlo 
 simulation and Changvan measurements. We find that the leaded/unleaded cou
 nt rate ratio is sensitive to the cutoff rigidity\, and the maximum differ
 ence between simulated and experimental ratios was less than 8%. This lead
 s to a promising spectral indicator that could be used to determine the sp
 ectral index of relativistic solar ions or Galactic cosmic rays with a sin
 gle detector. The research is supported in part by Thailand Science Resear
 ch and Innovation via Research Team Promotion Grant RTA6280002.\n\nhttps:/
 /events.icecube.wisc.edu/event/144/contributions/7744/
URL:https://events.icecube.wisc.edu/event/144/contributions/7744/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Cryoscope\, a technology pathfinder for time domain astronomy in t
 he NIR
DTSTART:20210910T120500Z
DTEND:20210910T122000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7739@events.icecube.wisc.edu
DESCRIPTION:Speakers: Roger Smith (Caltech)\, Mansi Kasliwal (Caltech)\n\n
 The convergence of many new technologies will soon enable high cadence sur
 veys of the infrared sky for the first time.   We describe a pathfinder te
 lescope currently under construction\, which will demonstrate imaging over
  a field of view two orders of magnitude greater than previously achieved 
 in the thermal infrared.  The novel optical design not only delivers diffr
 action limited image quality over larger fields\, but its double meniscus 
 corrector serves as the entrance window to a fully cryogenic optical path 
 that assures low thermal background.   We describe the window manufacturin
 g and support strategies which allow scaling to apertures larger than a me
 ter\, and the various methods to prevent ice precipitation.  A new\, cheap
 er\, growth process for large format infrared detectors is showing promise
  of making a 600 megapixel NIR focal plane feasible.   High speed direct d
 rive telescope mounts\, now commercially available\, will be upgraded to p
 rovide the vibration isolation necessary to take advantage of the exquisit
 e seeing.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/7739/
URL:https://events.icecube.wisc.edu/event/144/contributions/7739/
END:VEVENT
BEGIN:VEVENT
SUMMARY:CMB spectral distortions from Antarctica with COSMO: performance f
 orecast
DTSTART:20210908T110000Z
DTEND:20210908T111500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7732@events.icecube.wisc.edu
DESCRIPTION:Speakers: Fabio Columbro (Sapienza University of Rome)\, Giamp
 aolo Pisano (Sapienza University of Rome)\, Cristian Franceschet (Universi
 tà degli studi di Milano)\, Aniello Mennella (Università degli studi di 
 Milano)\, Silvia Masi (Sapienza University\, Rome Italy)\, Lucio Piccirill
 o (School of Physics and Astronomy - University of Manchester)\, Sabrina R
 ealini (Università degli studi di Milano)\, Marco De Petris (Sapienza Uni
 versity of Rome)\, Elisabetta Marchitelli (Sapienza University of Rome)\, 
 Mario Zannoni (Università di Milano Bicocca)\, Francesco Piacentini (Sapi
 enza University of Rome)\, Giuseppe D'Alessandro (Sapienza University of R
 ome)\, Gabriele Coppi (Università di Milano Bicocca)\, Elenia Manzan (Uni
 versità degli studi di Milano)\, Giorgio Pettinari (Istituto di fotonica 
 e nanotecnologie - CNR)\, Alessandro Coppolecchia (Sapienza University of 
 Rome)\, Lorenzo Mele (Sapienza University of Rome)\, Andrea Limonta (Unive
 rsità di Milano Bicocca)\, Alessandro Paiella (Sapienza University of Rom
 e)\, Carole Tucker (Cardiff University)\, Luca Lamagna (Sapienza Universit
 y of Rome)\, Federico Nati (Università di Milano Bicocca)\, Paolo de Bern
 ardis (Dipartimento di Fisica\, Sapienza Università di Roma)\, Elia Stefa
 no Battistelli (Sapienza\, University of Rome)\, Massimo Gervasi (Universi
 tà di Milano Bicocca)\, Marco Bersanelli (Università degli studi di Mila
 no)\n\nCOSMO (COSmic Monopole Observer) is a ground based differential Fou
 rier transform spectrometer\, to be operated at Dome-C\, Antarctica\, whic
 h aims at measuring the isotropic y-distortion of the Cosmic Microwave Bac
 kground (CMB). \nThe current upper-limit on $y$ is dated back to 1990 by C
 OBE-FIRAS to $|y|<1.5 \\cdot 10^{-5}$.\nCOSMO will measure the absolute br
 ightness of the sky in the 120-280GHz range in comparison with a reference
  blackbody calibrator and will monitor and remove the atmospheric emission
 \, with its fluctuations\, by performing extremely fast sky dips while sca
 nning the interferogram. \nWe assess the performance of the instrument via
  ILC-based simulations: input multi-frequency maps\, deprived of the atmos
 pheric contribution after the procedure\, include CMB anisotropy\, thermal
  dust as the main Galactic foreground\, and the isotropic y-distortion as 
 $y=1.77 \\cdot 10^{-6}$. The ILC machinery returns the Comptonization para
 meter as $y=(1.82\\pm0.31)\\cdot 10^{-6}$ when a noise realization\, limit
 ed by the photon noise from the atmosphere and the cryostat window emissio
 n\, is included.\n\nhttps://events.icecube.wisc.edu/event/144/contribution
 s/7732/
URL:https://events.icecube.wisc.edu/event/144/contributions/7732/
END:VEVENT
BEGIN:VEVENT
SUMMARY:CMB spectral distortions measurements at Dome-C: the antenna syste
 m of COSMO
DTSTART:20210908T120000Z
DTEND:20210908T121500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7753@events.icecube.wisc.edu
DESCRIPTION:Speakers: Elisabetta Marchitelli (Sapienza\, University of Rom
 e)\, Massimo Gervasi (Università di Milano Bicocca)\, Aniello Mennella (U
 niversità degli studi di Milano)\, Gabriele Coppi (Università di Milano 
 Bicocca)\, Marco De Petris (Sapienza University of Rome)\, Sabrina Realini
  (Università degli studi di Milano)\, Lucio Piccirillo (School of Physics
  and Astronomy - University of Manchester)\, Giorgio Pettinari (Istituto d
 i fotonica e nanotecnologie - CNR)\, Alessandro Coppolecchia (Physics Depa
 rtment\, University of Rome Sapienza\, P.le Aldo Moro 5\, 00185\, Roma\,It
 aly)\, Lorenzo Mele (Sapienza University of Rome)\, Luca Lamagna (Sapienza
  University of Rome)\, Giampaolo Pisano (Sapienza University of Rome)\, Al
 essandro Paiella (Sapienza University of Rome)\, Elenia Manzan (University
  of Milan Statale)\, Francesco Piacentini (Sapienza University of Rome)\, 
 Paolo de Bernardis (Dipartimento di Fisica\, Sapienza Università di Roma)
 \, Carole Tucker (Cardiff University)\, Marco Bersanelli (Università degl
 i studi di Milano)\, Andrea Limonta (Università di Milano Bicocca)\, Silv
 ia Masi (Sapienza University\, Rome Italy)\, Cristian Franceschet (Univers
 ità degli studi di Milano)\, Giuseppe D'Alessandro (Sapienza University o
 f Rome)\, Elia Stefano Battistelli (Sapienza\, University of Rome)\, Mario
  Zannoni (Università di Milano Bicocca)\, Federico Nati (Università di M
 ilano Bicocca)\, Fabio Columbro (Sapienza University of Rome)\n\nIn this w
 ork I present the design and forecasted performance of the multimoded feed
 -horns system of the COSmic Monopole Observer (COSMO). COSMO is a pathfind
 er experiment that aims at measuring the isotropic y-type spectral distort
 ion of the Cosmic Microwave Background from Dome-C\, Antarctica. The curre
 nt upper limit on the y-distortion is $<10^{-5}$ (COBE-FIRAS and TRIS).\n\
 nCOSMO exploits a cryogenic Martin-Puplett Fourier Transform Spectrometer 
 to measure the difference in brightness between the radiation collected fr
 om the sky and from an internal\, cryogenic reference blackbody. To reduce
  the atmospheric contribution\, fast sky-dips at varying elevation are per
 formed through a spinning wedge mirror while the interferogram is scanned 
 by fast\, low-noise Kinetic Inductance detectors.\n\nThe radiation is coup
 led to the detectors by two arrays of nine smooth-walled feed-horns workin
 g in the $120-180$ GHz and $210-300$ GHz range\, respectively. The feed-ho
 rns are multimoded to provide a greater throughput and a higher signal-to-
 noise level than a traditional single-mode receiver\, thus increasing the 
 instrumental sensitivity without extending the focal plane.\n\nThe antenna
  design is a trade-off between the multimode requirement on the antenna wa
 veguide\, the mechanical constraint on the antenna aperture and the optimi
 zation of the antenna directivity within the cryostat aperture window. The
  arrays are obtained by superimposing aluminum plates made with CNC millin
 g\, which is a relatively fast and low-cost manufacturing technique.\n\nht
 tps://events.icecube.wisc.edu/event/144/contributions/7753/
URL:https://events.icecube.wisc.edu/event/144/contributions/7753/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Observing transiting exoplanets in colors with ASTEP+
DTSTART:20210910T110500Z
DTEND:20210910T112000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7746@events.icecube.wisc.edu
DESCRIPTION:Speakers: Anne-Marie Lagrange (Obs. Paris)\, Amaury Triaud (Un
 iv. Birmingham)\, François-Xavier Schmider (OCA)\, Abdelkrim Agabi (OCA)\
 , Nicolas Crouzet (ESA)\, Philippe Bendjoya (OCA)\, Tristan Guillot (OCA)\
 , Djamel Mékarnia (OCA)\, Georgina Dransfield (Univ. Birmingham)\, Lyu Ab
 e (OCA)\, Olga Suarez (OCA)\n\nThe ASTEP telescope has begun since 2019 an
  active program to confirm and monitor long-period transiting exoplanets. 
 Its unique localisation at the Concordia station\, Antarctica\, allows the
  observation of targets difficult to observe from other latitudes\, in par
 ticular when close to the celestial South pole or for long-duration transi
 ts. This is ideal to follow-up TESS exoplanetary candidates (in majority n
 ear the poles) but also for the preparation of JWST and ARIEL as this corr
 esponds to their continuous viewing zones. By following-up exoplanet candi
 dates found by the NASA TESS mission\, ASTEP has enabled the confirmation 
 of exciting exoplanets\, including the observations of transits lasting mo
 re than 8 hours (a first from the ground) and the participation to the dis
 covery of the temperate Neptune-size exoplanet TOI-1231 b. At the end of 2
 021\, a new camera box will be installed\, enabling simultaneous observati
 ons in two colors. This effectively new instrument\, ASTEP+\, will thus ha
 ve the capability to efficiently separate false positive from bona fide ex
 oplanets\, in addition to a much increased sensitivity. I will discuss the
  perspectives of this evolution.\n\nhttps://events.icecube.wisc.edu/event/
 144/contributions/7746/
URL:https://events.icecube.wisc.edu/event/144/contributions/7746/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Measuring spectral distortions of the CMB: the COSMO experiment
DTSTART:20210908T111500Z
DTEND:20210908T113000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7733@events.icecube.wisc.edu
DESCRIPTION:Speakers: Andrea Limonta (Università di Milano Bicocca)\, Ele
 nia Manzan (Università degli studi di Milano)\, Giuseppe D'Alessandro (Sa
 pienza University of Rome)\, Lucio Piccirillo (School of Physics and Astro
 nomy - University of Manchester)\, Gabriele Coppi (Università di Milano B
 icocca)\, Aniello Mennella (Università degli studi di Milano)\, Silvia Ma
 si (Sapienza University\, Rome Italy)\, Federico Nati (Università di Mila
 no Bicocca)\, Mario Zannoni (Università di Milano Bicocca)\, Francesco Pi
 acentini (Sapienza University of Rome)\, Elisabetta Marchitelli (Sapienza\
 , University of Rome)\, Marco De Petris (Sapienza University of Rome)\, Lu
 ca Lamagna (Sapienza University of Rome)\, Fabio Columbro (Sapienza Univer
 sity of Rome)\, Alessandro Paiella (Sapienza University of Rome)\, Massimo
  Gervasi (Università di Milano Bicocca)\, Lorenzo Mele (Sapienza Universi
 ty of Rome)\, Cristian Franceschet (Università degli studi di Milano)\, S
 abrina Realini (Università degli studi di Milano)\, Giampaolo Pisano (Sap
 ienza University of Rome)\, Marco Bersanelli (Università degli studi di M
 ilano)\, Giorgio Pettinari (Istituto di fotonica e nanotecnologie - CNR)\,
  Carole Tucker (Cardiff University)\, Paolo de Bernardis (Dipartimento di 
 Fisica\, Sapienza Università di Roma)\, Elia Stefano Battistelli (Sapienz
 a\, University of Rome)\, Alessandro Coppolecchia (Physics Department\, Un
 iversity of Rome Sapienza\, P.le Aldo Moro 5\, 00185\, Roma\,Italy)\n\nThe
  COsmic Monopole Observer (COSMO) is a pathfinder\, ground-based experimen
 t\, designed for the detection of the isotropic $y$-distortion of the Cosm
 ic Microwave Background (CMB). Deviations from a pure blackbody are expect
 ed as an evidence of all the interactions that CMB photons undergo along t
 he thermal history of the Universe. Their observation provides an insight 
 into processes involving CMB photons that took place both before and after
  recombination.The upper limit on the $y$-distortion is still the one from
  the COBE-FIRAS mission ($y<10^{-5}$) due to the extreme accuracy required
  for spectral distortions measurements.\nCOSMO exploits a cryogenic Martin
 -Puplett Fourier Transform Spectrometer\, comparing the radiation collecte
 d from the sky to the one from an internal\, cryogenic blackbody reference
  with high emissivity. All the optical elements of the FTS are maintained 
 at a temperature of 2.7 K to minimize instrument emission. The interferogr
 am is obtained modulating the optical path difference (OPD) with cryogenic
 \, frictionless linear motion of one of the two roof-mirrors. The maximum 
 mirror displacement is $\\pm 25$ mm\, and it is measured with a resolution
  of $10 \\mu $m. This provides a spectral resolution around 5 GHz. A flat 
 spinning wedge mirror\, at room temperature\, allows to perform fast sky d
 ips along $20^{\\circ}$ diameter circle in the sky while scanning the inte
 rferogram. This strategy enables to measure and remove most of the atmosph
 eric emission and its slow fluctuations. Fast detectors are required\, so 
 small multi-mode Kinetic Inductance Detectors (KIDs) arrays ($\\tau \\sim 
 50\\mu$s)\, operating in the 120-280 GHz range\, will equip the two focal 
 planes.\nCOSMO will operate from the Concordia station\, at Dome-C\, in An
 tarctica\, arguably the best site on Earth  for this kind of measurements.
 \n\nhttps://events.icecube.wisc.edu/event/144/contributions/7733/
URL:https://events.icecube.wisc.edu/event/144/contributions/7733/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A proxy for decadal solar cycles from AD 1600 to 1900 based on nit
 rate concentrations in a Dome Fuji (Antarctica) ice core
DTSTART:20210908T134500Z
DTEND:20210908T140000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7759@events.icecube.wisc.edu
DESCRIPTION:Speakers: Takashi Imamura (National Institute for Environmenta
 l Studies)\, Kazuya Takahashi (RIKEN)\, Yoichi Nakai (RIKEN)\, Hideaki  Mo
 toyama (National Institute of Polar Research)\, Yuko Motizuki (RIKEN)\n\nI
 ce cores yield information about astronomical phenomena as well as informa
 tion about climate changes of the past. We applied time-series analyses to
  variations in nitrate ion concentrations in one segment of an ice core dr
 illed at the Dome Fuji station in East Antarctica\, corresponding to the h
 istorical period from AD 1600 to 1900. Our analyses revealed clear evidenc
 e of periodicities of ~ 11 years\, ~ 22 years\, and ~ 90 years\, comparabl
 e to the 11-year Schwabe\, 22-year Hale\, and to the ~ 90-year Gleissburg 
 solar cycles\, respectively. Our result thereby shows for the first time t
 hat nitrate ion variations in an ice core can certainly be used as a proxy
  for past solar activity on a decadal time scale. This finding may be attr
 ibuted to the advantage of precipitation environment of the Dome Fuji site
 . Furthermore\, we found an 11-year periodicity in the nitrate ion variati
 ons even during AD 1645 – 1715\, the period of the grand Maunder minimum
  when sunspots were almost not observed. Although our evidence for an 11-y
 ear periodicity during the Maunder minimum is less strong statistically th
 an that for the periods from AD 1600 to 1645 and from AD 1715 to 1900\, th
 e discovery of the 11-year periodicity during the Maunder minimum was unex
 pected. This discovery may indicate that an 11-year periodicity existed in
  solar UV radiation even during the Maunder minimum and reconfirms the obs
 ervation that the solar dynamo retains cyclic behavior even during grand s
 olar minima\, as suggested by studies of 10Be content in ice cores.\n\nhtt
 ps://events.icecube.wisc.edu/event/144/contributions/7759/
URL:https://events.icecube.wisc.edu/event/144/contributions/7759/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The IceCube Surface Array Enhancement - A comprehensive overview o
 f the planned cosmic-ray surface detector at the South Pole
DTSTART:20210909T114500Z
DTEND:20210909T120000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7748@events.icecube.wisc.edu
DESCRIPTION:Speakers: Roxanne Turcotte (Karlsruhe Institute of Technology)
 \n\nThe IceCube Neutrino Observatory is a Cherenkov light detector located
  deep in the Antarctic ice. A cosmic-ray detector at the surface\, named I
 ceTop\, composed of Ice-Cherenkov tanks complements the in-ice detector. A
  Surface Array Enhancement for the IceCube Neutrino Observatory is planned
  to be deployed in the near future at the South Pole. It will consist of 3
 2 hybrid stations positioned within the current IceTop footprint. Each sta
 tion of the surface enhancement has one central hybrid DAQ connecting 8 sc
 intillator panels and 3 radio antennas\, all elevated to avoid snow covera
 ge. The surface enhancement will considerably increase the detection sensi
 tivity to air showers in the ~100 TeV to EeV primary energy range\, mitiga
 te the effects of snow accumulation on the existing IceTop tanks\, and be 
 the first step of a future large-scale surface array of IceCube-Gen2 using
  the same technology. The DAQ and its related components are designed to b
 e easily integrated into the already existing computing\, timing\, and com
 munication infrastructure of IceCube. In January 2020\, a complete prototy
 pe station comprising 8 scintillator panels and 3 antennas was deployed an
 d is continuously operating.  In this talk\, we will try to give a compre
 hensive view of the development\, deployment\, and maintenance of a remote
 ly accessible detector and will present some results of the first cosmic-r
 ay induced air-showers detected by the prototype station. We will conclude
  with an outlook on the scientific prospects of the IceCube-Gen2 surface a
 rray whose design builds on the successful experience with the prototype s
 tation and extends the planned surface enhancement of IceTop.\n\nhttps://e
 vents.icecube.wisc.edu/event/144/contributions/7748/
URL:https://events.icecube.wisc.edu/event/144/contributions/7748/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Cosmic Ray Flux Correlation between McMurdo and Jang Bogo Stations
DTSTART:20210910T140000Z
DTEND:20210910T141500Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7745@events.icecube.wisc.edu
DESCRIPTION:Speakers: Paul Evenson (University of Delaware)\, Waraporn Nun
 tiyakul (Chiang Mai University)\, Suyeon Oh (Department of Earth Science E
 ducation\, Chonnam National University\, Gwangju 61186\, South Korea)\, Da
 vid Ruffolo (Mahidol University)\, Achara Seripienlert (National Astronomi
 cal Research Institute of Thailand (NARIT)\, Chiang Mai 50180\, Thailand)\
 , Ekawit Kittiya (Department of Physics and Material Science\, Faculty of 
 Science\, Chiang Mai University)\, Alejandro Sáiz (Mahidol University)\n\
 nA neutron monitor is a large ground-based detector responding to the flux
  of cosmic ray particles in space by measuring atmospheric secondary neutr
 ons. Any ground-based detector is sensitive to cosmic rays from a certain 
 range of directions in space. In particular\, a particle arriving from a s
 pecific sky direction with a specific rigidity (momentum per unit charge) 
 was necessarily moving in a certain direction in space\, called the asympt
 otic direction outside the geomagnetic field. McMurdo and Jang Bogo neutro
 n monitor stations are Antarctic stations with similar geomagnetic latitud
 e but slightly different geomagnetic longitude. From December 2015 to Octo
 ber 2016\, we had transferred six of the eighteen neutron counters from Mc
 Murdo to Jang Bogo\, with full transfer to Jang Bogo completed in December
  2017. We present an analysis of the correlation of the cosmic ray flux be
 tween the McMurdo and Jang Bogo stations\, during the time when both were 
 operating\, with ten-second time resolution. Although highly correlated\, 
 there are significant differences\, including systematic time lags\, in th
 e data from the two stations. Since McMurdo observes a similar asymptotic 
 direction to Jang Bogo with a time delay of approximately 13 minutes\, the
  joint observations reveal structure in the interplanetary cosmic ray dens
 ity at a unique distance and angular scales. The research is supported in 
 part by TA/RA scholarship (active recruitment) of Chiang Mai University an
 d Thailand Science Research and Innovation via Research Team Promotion Gra
 nt RTA6280002.\n\nhttps://events.icecube.wisc.edu/event/144/contributions/
 7745/
URL:https://events.icecube.wisc.edu/event/144/contributions/7745/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Update on the IceCube Upgrade Project
DTSTART:20210909T111500Z
DTEND:20210909T113000Z
DTSTAMP:20260412T162100Z
UID:indico-contribution-7767@events.icecube.wisc.edu
DESCRIPTION:Speakers: Kael Hnason (UW-Madison)\n\nThe IceCube Neutrino Obs
 ervatory at the South Pole is the leading facility\nworldwide for scientif
 ic exploration in the field of neutrino astrophysics.\nA more densely inst
 rumented infill array\, IceCube DeepCore\, was added during\nconstruction 
 to lower IceCube's energy threshold where it could exploit the\nmassive vo
 lume of exceptionally clear ice at the bottom of IceCube to enable\ncompet
 etive measurements of neutrino oscillation parameters. More than ten\nyear
 s after the last IceCube string was deployed\, the IceCube Collaboration\n
 has embarked on a further Upgrade to the detector consisting of seven more
 \nstrings of advanced photodetectors to infill DeepCore\, with sensitivity
 \ngreater than current and near future experiments to detect hints of new\
 nphysics beyond the best model of elementary particles that has stood for\
 nover a half a century. Exploiting the opportunity provided by a restart o
 f\ndeep-ice drilling at the site\, new calibration devices will accompany 
 this\ninstrumentation and will provide data for better modeling of the opt
 ics of\nthe deep glacial ice. Incomplete current knowledge of the ice intr
 oduces\nsystematics in IceCube that limit its precision for neutrino astro
 physics.\nImproved ice models can be fed back into reprocessing more than 
 a decade and\na half of archived data to provide neutrino skymaps and othe
 r data products\nwith significantly improved resolution.\n\nhttps://events
 .icecube.wisc.edu/event/144/contributions/7767/
URL:https://events.icecube.wisc.edu/event/144/contributions/7767/
END:VEVENT
END:VCALENDAR