資料12-J

Activity Report of Commission J
April 26, 2019 to September 18, 2020
September 30, 2020
Kenta Fujisawa (Yamaguchi University)

ALMA project⚫

ALMA press release (September 15, 2020)

Phosphine on Venus - A step forward to understand biomarker molecule
An international team of astronomers detected phosphine (PH3) in the atmosphere ofVenus. They studied the origin of phosphine, but no inorganic processes, including supply
from volcanos and atmospheric photochemistry can explain the detected amount ofphosphine. The phosphine is believed to originate from unknown photochemistry orgeochemistry, but the team does not completely reject the possibility of biological origin.
This discovery is crucial to examine the validity of phosphine as a biomarker.

ALMA image of Venus, superimposed with spectra of phosphine observed with ALMA (in white) and
JCMT (in grey). As molecules of phosphine float in the high clouds of Venus, they absorb some of themillimeter waves that are produced at lower altitudes. When observing the planet in the millimeter
wavelength range, astronomers can pick up this phosphine absorption signature in their data as a dip in
the light from the planet.
Credit: ALMA (ESO/NAOJ/NRAO), Greaves et al. & JCMT (East Asian Observatory)

資料12-J

Activities of meetings⚫

International Workshop on EAO Futures: Future Science and Instrumentation
Date: Mar 20th-23rd, 2019
Location: Najing, China
May 20th - 23rd 2019 the East Asian Observatory will host a four day (two half days and two
full days) meeting looking at the future of science drivers and instrumentation needs of Sub-mm
EAO astronomers. The meeting will discuss a range of topics including the Namakanui
instrument at JCMT, the design of a new 850 micron camera for use at the JCMT, the East
Asian VLBI project, and instrumentation in polar climates. Talks will cover both the technology
involved in these programs and the science cases for such instrumentation.

⚫

The 10th Galactic Center Workshop (GCWS 2019): New Horizons in Galactic Center
Astronomy and Beyond
October 21 (Monday) to 24 (Thursday), 2019 (Reiwa 1)
Keio University Hiyoshi campus
The central few hundred parsecs of the Milky Way Galaxy, which is often referred to as thecentral molecular zone (CMZ), is characterized by a strong concentration of stars andinterstellar matter. Many surveys in various wavelengths, from radio to gamma-rays, as well as
pointed observations have revealed a variety of astrophysical phenomena, most of which
remain elusive: i.e., the three-dimensional distribution of gas; suppressed star formation despite
the abundance of dense molecular gas; a currently inactive supermassive black hole but richsignatures of past central activities, the high-energy diffuse gamma-ray emission from GeV up
to TeV energies, etc. These unsolved issues span wide ranges of spatial scale, time scale, andenergy scale and are likely related to each other. Current key issues in Galactic center studies
include: (1) the triggering mechanism of central activity; (2) the formation process of thecentral supermassive black hole; (3) existence proof of the supermassive black hole at Sgr A*;(4) star formation properties in the CMZ; and (5) the properties of stellar remnants and theirbinaries, which would be gravitational wave progenitors. These issues are common to studies ofextragalactic nuclei.

⚫

Nobeyama Science Workshop Reiwa 1st
Date: 2019/9/4-6
Location: Nobeyama Radio Observatory
The Nobeyama 45m radio telescope has been playing an active role as the leading telescope inJapanese radio astronomy since 1982. Since then, it has brought many important results, but
due to changes in the environment and needs, open use observation will be finished by March
4th year of this year. It even gives the impression that the science itself with single-dish isshirinking. However, many active users are young researchers who will lead the next generation.

資料12-J

This workshop provides a place for users to gather and discuss about the latest achievements
and research prospects, and to think about the possibilities of science with a single-dish in the
new era.
⚫

Galactic Center Workshop 2019
Date: 2019/6/10
Location: Nagoya Univeristy
The galactic center is a unique region of the galaxy where stars and gases are densely packed.
The gas in this region shows non-circular motion at high temperature and high density withlarge velocity dispersion. Further, it is said that the magnetic field strength in the central portionis one order of magnitude higher than that in the disk region. Research on the star formation
process in such a peculiar environment is an important subject of star formation research. In
recent years, sensitive X-ray and gamma-ray observations have revealed several outflow-likeobjects that blow out from the center to the north and south. Therefore, it can be said that theclosest core, the center of the galaxy, is the most important target for understanding theevolution and activity of the core. In order to study interstellar phenomena and core activity insuchastrongmagnetic

field

environment,

theoretical

approaches

such

as

magnetohydrodynamic calculations are indispensable. In this study group, observation
researchers and theoretical researchers from various wavelengths and research fields will meet
together to provide a place for concrete and close discussions with a view to future observationequipment.
⚫

The 12nd East Asia VLBI Workshop
Date: Sep 24 - Sep 26, 2019
Location: Mito Campus, Ibaraki University
Since the release of the first EAVN call for proposal in April 2018, the EAVN array is now in its
real operation with 10 stations (KaVA, Tianma, Nanshan and Nobeyama). The EAVW-2019
will be the first meeting after this milestone, while an increasing number of exciting results arecoming out with KaVA, the core array of EAVN. We will discuss and highlight various science
topics studied by EAVN/KaVA as well as by individual VLBI facilities VERA/KVN/CVN/JVN.
This will include active galactic nuclei, star formation, evolved stars, astrometry, micro quasars,
pulsars, transients, multi-messenger science etc. We will also highlight various ongoingdevelopments of the array capability and instruments as well as the near-future expansion of the
network into Ibaraki, Yamaguchi, Kunming, Thailand, Italy, Australia etc. Moreover, the VLBI
community in East Asia is increasingly involved with EHT and SKA. Therefore, we will also
discuss how EAVN can play a unique role in the era of such huge facilities. This will include"EAVN-high" that includes JCMT/GLT and "EAVN-low" that includes FAST, as well as joining
a global VLBI network.

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The 1st circular of the next generation VLA workshop
Date: September 17-20, 2019
Location: NAOJ, Mitaka, JapanThe next generation Very Large Array (ngVLA) project, which is led by the National Radio
Astronomy Observatory in the USA, is one of the most ambitious on-ground radio astronomy
projects for the next decades. This new on-ground cm/mm-wave radio telescope will becomposed of 214 18-m antennas placed around the current VLA site in New Mexico andextending into other states in the US, and even into Mexico, complemented with a shortbaseline array composed of 6-m and Total Power antennas, and a long baseline array extending
from Hawaii to the US Virgin Islands. This will provide a large collecting surface withbaselines up to 9000 km, which will translate into unprecedented sensitivity and milli arcsecond
angular resolution at frequencies from 1.2 to 116 GHz.

⚫

The 17th IVS NICT-Technology Development Center Symposium
Date: 2019/6/27
Location: NICT Kashima Space Center
We will hold a symposium on research and development of VLBI technology and space
geodesy technology, so we would like to invite you to participate. In the field of geodetic VLBI,IVS (International VLBI Service for Geodesy & Astrometry), which leads the international
geodetic VLBI, is a next-generation wideband geodetic VLBI system that enables
ultra-wideband observation of 2-14 GHz. (VGOS) is being promoted, and countries around theworld (US, Germany, Spain, Japan, Russia, China, South Africa, Norway, etc.) have installed
new antennas and observation systems, and observations have begun. NICT has developed a
3-14GHz wideband VLBI observation system along with the guideline of VGOS, and isconducting international observations of intercontinental frequency comparisons using
wideband small antennas. At the symposium, we would like to exchange information on VLBI
technology, space surveying technology such as GNSS, SLR, single radio telescope observation,
time / frequency related technology, and observation results, aiming for further development of
the VLBI field.

⚫

EA ALMA Development Workshop 2019
Date: December 10-11, 2019
Location: Large Seminar Room, NAOJ, Mitaka
The Atacama Large Millimeter/Submillimeter Array (ALMA) is now routinely producing
groundbreaking scientific results in almost all fields of astronomy and astrophysics. In orderto maintain ALMA as the most advanced (sub)mm-wave array in the coming decades, all
ALMA partners are now striving to realize the goals presented in the ALMA Development
Roadmap. The East Asian ALMA has been holding the EA ALMA Development Workshop
every year, with the main aim to present the latest technological advancement and exchange

資料12-J

ideas which are relevant to the upgrade of ALMA. This annual workshop is intended to become
an effective forum for interaction and discussion between the technical and scientificcommunities, and the input from the community is key in the establishment of the EA ALMA
Development Program. Last year, the main focus of the workshop was “wide IF”, which isrecognized as the highest priority in the ALMA Development Roadmap. This year, we would
like to invite talks and discussion related to high frequency (bands 8, 9 and 10) observations of
ALMA and related hardware and software development. Apart from this major focus, we will
welcome contributions in the fields of antennas, front-ends, back-ends, and softwaredevelopment and related talks in science, science operations and/or commissioning of newcapabilities.
⚫

Sub-mm Spectroscopy and Large-Scale Science with ASTE
Date: 2019/08/19 10:30-17:30
Place: Lecture Room at NAOJ Mitaka Campus
ASTE is a 10-m class submillimeter-wave single-dish telescope which enables to carry out
large programs and surveys with its operational flexibility and superb atmospheric conditions.
There are demands on large scale [CI] and CO (3-2) and (4-3) mapping of the Galactic Centerregion, Galactic Plane, molecular clouds in the far outer galaxy, high-latitude molecular clouds,
LMC/SMC and local group galaxies.
ASTE also serves as a test bench of astronomical instrumentation to explore new areas oftechnology with an expected positive impact on science. DESHIMA (Deep Spectroscopic
High-redshift Mapper) is a new type of submillimeter wave spectrometer, which uses a
superconducting filterbank on a chip to achieve a very wide instantaneous bandwidth.
DESHIMA prototype was installed on the ASTE in 2017 and has successfully detected multiple
astronomical sources, in both continuum and line emission. In this year, installation andcommissioning of a new receiver with ALMA Band 10 frequency coverage (787-950 GHz) isplanned including pilot observations to obtain [CI] (2-1) and CO (7-6) and (8-7) lines.
Therefore, there is no doubt that ASTE can proceed its own unique science in the ALMA era.
The main objective of this workshop to discuss and identify future Sub-mm Spectroscopy andLarge-Scale Science with ASTE by our community members. We look forward to theparticipation by researchers who are interested in sub-mm astronomy and related fields.

⚫

2019 ALMA/45m/ASTE Users Meeting
Date: December 18 - 19 (Wednesday - Thursday), 2019
Location: National Astronomical Observatory of Japan (Mitaka Campus, Subaru building 1F
large seminar room)⚫

General Meeting of Japan Radio Astronomy Forum
Date: 9/11, 2019

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Location: Kumamoto University⚫

VLBI Consortium Symposium 2019: VLBI Crosses National Borders
Date: 2019/11/23-25
Location: Otsuma Women’s University
The VERA project, which has been the core of Japan's astronomical VLBI observations, hasreached the stage of compiling the results, the number of users of EAVN, in which VERA / JVN,
Nobeyama, South Korea, and China participate, is increasing, and results are being produced.
Joint experimental observations with Italy are under active research in both astronomy andgeodetic / time transmission VLBI. A Japanese group also contributed to EHT, which is alarge-scale international joint research, and succeeded in shooting a black hole shadow. A
230GHz VLBI experimental observations in East Asia are also being conducted through joint
research by Japan, Taiwan, South Korea, and China. SKA, which is closely related to VLBI, isabout to start construction. It can be said that international VLBI collaboration is now providing
a new research framework. Research themes have expanded from classic AGN jets and maser
to accretion disks, transient objects, black holes in the galaxy, and further expanded into newareas of multi-messenger astronomy and time domain astronomy through multi-wavelength
collaboration. At the VLBI Consortium Symposium 2019, we plan to focus on discussions
aimed at building a new research framework through international collaboration, entitled"VLBI Crosses Borders." The purpose of this is to draw out new research themes of the VLBI
community and discuss and share the future image.

⚫

17th Mizusawa VLBI Observatory Users Meeting in 2019: 1st circularDate: December 13 - 14, 2019
Location: Mizusawa VLBI observatory, NAOJ
Mizusawa VLBI Observatory has proceeded astrometric observations with VERA to unveil 3-D
spatial/velocity structures in the Milky Way Galaxy and its dynamical evolution. On the basis of
the activity, we have accelerated a development of KaVA (KVN and VERA Array) and EAVN
(East-Asian VLBI Network). As a result an open-use of EAVN has been initiated since 2018B
semester (observations will be allocated from 2018 September). From 2019B semester,
astrometric mode of KaVA open-use has been opened. We emphasize that the development of
EAVN will promote the KaVA Large Programs in research fields of Star, AGN, and High-massstar formation, which have been initiated since 2016. On the other hand, Budget cut for
Mizusawa VLBI Observatory will be expected based on the long term plan of NAOJ
management. It is necessary that we discuss with community members how efficiently weconduct observational research in such situation. Based on that situation, we will discuss about
not only exciting scientific results with VERA/KaVA/EAVN but also future prospects ofMizusawa VLBI Observatory especially in 2022 and beyond. EAVN will be further developedon the basis of future collaborations with JVN (Japanese VLBI Network), FAST 500-m (China),資料12-Jand TNRT 40-m (Thailand) radio telescopes, leading improvement of sensitivities andobservable frequencies; Synergy with Gaia DR2 and SKA has been expected.
⚫

The ALMA Workshop: Early Planet Formation in Embedded Disks
Date: December 8-10, 2019
Location: University of Tokyo.
Previous high-resolution ALMA observations of protoplanetary disks around Class II sources,
such as DSHARP, have shown that substructures in those disks are ubiquitous, mostly in theform of concentric rings and gaps, implying the presence of planets in these disks. The
ubiquitous detection of substructures in protoplanetary disks raises the intriguing possibility
that at least some planet formation may have started already during the embedded stages ofprotostellar evolution. In order to address exactly how and when planet formation might begin,we will start an ALMA large program to systematically observe a large sample of Class 0 and I
objects with an angular resolution of 0.04" (5 au) in 1.3 mm dust continuum and CO emission
lines at 230 GHz to investigate how early substructures indicative of planet formation arise indisks in the evolution of young stars. In the workshop, we will invite several overseas experts inthis field, and will review recent observations of disks around protostars as well as class II
sources. We will also discuss data analysis technique of disks at high angular resolutions, andstrategy how to understand possible early planet formation in embedded disks.

⚫

New View of the Universe opened by THz Observation
Date: 2019/12/21
Location: National Institute of Polar Research
The terahertz band, which is the new horizon of ground observation, is an undeveloped area andis expected to develop significantly in the future. Currently, site survey and equipment
development are underway to open up terahertz astronomy. The purpose of this study group is
to discuss what kind of new science can be developed by utilizing the terahertz band, which is
the only wavelength region that large terrestrial telescopes have not been able to reach.

⚫

Molecular gas observations toward the Local Group and the outer Milky Way
Date: 2020/1/16 – 17
Location: Nagoya University
Research of the formation and evolution of astronomical objects (molecular gas, stars / clusters,
galaxies) from the early universe to the present is one of the greatest challenges in astronomy.
The outer edge of the galaxy is an optimal target that can cover parameter spaces that cannot be
filled by the system alone with high-resolution observations. In particular, observations of low
heavy-element content environments are very useful for understanding the formation andevolution of celestial bodies in the early universe. From recent observations of the large
Magellan cloud and M33, gas motion on the kpc scale due to galaxy interaction and spiral arm

資料12-J

motion may create a molecular cloud filaments width of about 0.1 pc. The possibility of
inducing formation is being clarified, and it is rapidly becoming more important to have abird's-eye view of the entire galaxy with a high spatial dynamic range using multiple devices
such as ALMA. Observations of outflows to primordial stars and surveys of hot cores are also
being energetically advanced, and it is expected that statistical verification of the physical /chemical properties of massive star formation in low-heavy element environment will progress.
⚫

ALMA Grant Fellow Symposium 2019
Date: December 17, 2019
Venue: NAOJ Lecture Room
The NAOJ ALMA project will host the “ALMA Grant Fellow Symposium 2019” on December
17, 2019 at the NAOJ Lecture Room in Mitaka. The symposium will host 12 researchers
hired through the ALMA Joint Scientific Research Program, and they will be presenting thelatest science results related to ALMA. Anybody is welcome to join and hear the talks.

⚫

The ALMA 2030 Vision: Design considerations for Digitizers, Backend and Data Transmission
SystemDate: March 11-13
Location: NAOJ, Mitaka, Japan
The ALMA Development Roadmap has identified the multiplication of the IF bandwidth of
ALMA (at least by a factor 2) as one of the main priorities for ALMA upgrades in the 2020s.
This increase of the instantaneous bandwidth will be realized with the coordinated upgrade ofreceivers in the Front End, the correlators, and last but not least, all electronics between them:
digitizers, backend and Data Transmission System (DTS). This meeting aims to bring together
experts on the ALMA system and digitizer, backend and data transmission system technologies,
from within ALMA and from the community.
<<<CHANGED TO VIRTUAL MEETING, OCTOBER 14-16, 2020>>>⚫

6th Riken-NICT THz Workshop & 20th Millimeter-Submillimeter Receiver Workshop
Date: 2020/3/2 – 3
Location: Tohoku University⚫

Star formation with ALMA 2020: Tracing pre/proto-stellar core evolution in nearby
molecular clouds
Date: March 5 (Thu) 13:00- 6 (Fri) 17:00, 2020
Venue: Rinko-shitsu (C5-112), NAOJ Mitaka champus
Understanding the origin of diversity in star formation, from the initial mass function to the sizeand structures of protostellar disks, is one of the ultimate goals in star formation studies. Suchdiversity should be originated from the natal dense cores. Observational studies of such dense資料12-J

cores harboring Class 0/I objects, i.e., protostellar cores, or even cores before protostellar
formation, prestellar cores, should provide us with crucial information on the initial conditionof star formation. However, previous ALMA observations have not extensively explored suchyoung objects but mainly targeted well-known protostellar and T-Tauri sources, which werediscovered before the ALMA era using, e.g., other wavelength telescopes and low-resolution
mm/sub-mm single-dishes. ALMA has the potential to improve this situation; for example,
recent ALMA surveys, including the ACA (Atacama Compact Array) stand-alone mode, aretrying to find new exciting objects without any bright infrared sources, such as candidates of thefirst hydrostatic core. Although single-dish telescope and other wavelength data still play anessential role as the first atlas, the era that ALMA itself can be one of the survey telescopes islikely upcoming. In this workshop, we will discuss the observational strategies on how to selectthe target objects using ALMA and to optimize the subsequent follow-up observations to reveal
the initial condition of star formation, also by combining with the related theoretical simulation.
<<<CANCELLED>>>⚫

Dynamics and physics of outflows in protostellar disks and Active Galactic Nuclei II
Date: 2020/3/23 – 25
Loation: Kagoshima University⚫

Japan Radio Astronomy Forum Symposium 2019: Radio astronomy that opens up withextreme performance
Date: 2020/3/23 – 25
Location: NAOJ, Mitaka
The Japan Radio Astronomy Forum is an organization that represents the Japanese radio
astronomy community. As part of its activities, a symposium is held every year for the purposeof sharing the science and observation technology of radio astronomy and discussing futureplans. At the symposiums of the last two years, we have held multifaceted discussions over twodays, focusing on technological development that will support future radio astronomy andfuture science in collaboration with other wavelengths and fields. Based on these results, thisyear, we will focus on various "extreme performances" regardless of projects and existingtelescopes, and explore science that can only be done by radio astronomy and new methods torealize it in the entire community.
<<<CANCELLED>>>⚫

New Developments of Planetary Sciences with ALMA in JpGU-AGU Joint Meeting 2020
Date: 27 May, 2020
Location: Makuhari Messe in Chiba
We would like to invite contributed talks for the session of "New Developments of Planetary
Sciences with ALMA" in JpGU-AGU Joint Meeting 2020 held on 27 May, 2020, at Makuhari資料12-J

Messe in Chiba. It has been about 5 years since the series of concentric rings has been
discovered in the protoplanetary disk of HL Tau, and we will review the current understandingof planetary-system formation in our session. Recent results with ALMA on the Sun,solar-system planets, and extra-solar planetary systems will be presented and discussed among
researchers in planetary science and astronomy.
⚫

ALMA Lensing Cluster Survey Workshop
Date: March 13 - 14, 2020
Location: Institute of Astronomy (IoA), University of Tokyo
ALMA lensing cluster survey (ALCS) is one of the cycle-6 large programs to observe highmagnification regions of 33 lensing clusters spending 95 hrs. The ALCS covers 88 arcmin^2 intotal, to a depth of ~60 uJy (1.2mm, 1 sigma), achieved by using a 15-GHz-wide spectral scan,
to enlarge the survey volume of line-emitting galaxies. The sample comes from the best-studied
massive clusters also imaged in HST programs, i.e., CLASH, HFF, and RELICS. The goals of
the workshop are (1) to share the latest outcomes from ALCS and ALMA observations of blankfields, clusters/proto-clusters, and high-redshift lensed galaxies, and (2) to develop next ALMA
(large) proposals and related multi-wavelengths follow-up plans using e.g., JWST. You areencouraged to join if you are interested in any of the topics below.
<<<CANCELLED>>>⚫

IAU Symposium 360: Astronomical Polarimetry 2020 -- New Era of Multi-Wavelength
Polarimetry
Date: March 23 -- 27, 2020
Location: Hiroshima, Japan
Astronomical Polarimetry 2020 (Astropol 2020) is the next in a series of international
conferences. The aim of this series of conferences is to bring researchers interested in
astronomical polarimetry together to share and discuss recent results and advances in technicaland scientific aspects in all relevant astronomical fields. This will be the first time that an
Astropol symposium will take place in Asia.
<<<POSTPONED TO 2021 March 22-26>>>⚫

SNR Workshop 2020
Date: February 26-27, 2020
Location: Nagoya University
Supernova remnants (SNRs) are the most energetic objects not only in our Galaxy, but also inexternal galaxies, and have been observed at various wavelengths from radio to gamma-rays.
One of the most spectacular features of SNRs is the fast moving expanding shells whose
velocity is measured as up to ~10,000 km/s. Recent observations of shells in X-rays as well asradio continuum emission have provided a wealth of information on their physical and資料12-J

kinematical properties. It is also remarkable that the dense interstellar medium interacting withthe shocks is likely playing a key role to produce X-rays and gamma-rays as shown bycomparisons with CO/HI and dust emission. Theoretical works on acceleration and escape ofcosmic rays in SNRs are unveiling details of cosmic-ray acceleration/propagation bymagneto-hydro-dynamical numerical simulations, which will be compared with observations.
In the present workshop, we invite observers and theorists to stimulate active interaction andexchange of ideas on SNRs.
<<<CANCELLED>>>⚫

Workshop on Carbon Observations - Toward understanding how to use Carbon Date: March 25-26, 2020
Venue: The University of Tokyo
Atomic carbon observations have been started by using the Mt.Fuji Submillimeter-wave
telescope in Japan. They have continuously been carried out by using ASTE and are now
progressing toward various targets by using ALMA. In this workshop, we will share the recent
results of carbon observations in galaxies, interstellar medium and star/planet formation, andalso share the related theoretical studies. In addition, we would like to discuss a strategy for theusage of ALMA Band 8 and 10.
<<<CANCELLED>>>⚫

IVS NICT Technology Development Center Symposium
Date: 24-25 April 2020
Venue: Kashima Space Technology Center of NICT
Since IVS (International VLBI Service for Geodesy and Astrometry) was established, NCIT
(former name CRL: Communications Research Laboratory) has been designated as one of thetechnology development centers (TDCs) of IVS. As one of the activities of TDC, we haveregularly organized NICT-TDC symposium. Purpose of the symposium is exchanging
information on activities and status on research & developments of VLBI technology,
application, and radio observing techniques among individual researchers and institutes. In thistime, meeting is going to be held as the international symposium with inviting IVS chairman
Axel Nothnagel, Network station Coordinator Ed Himwich, Weimin Zheng and Fengchun Shu
of Shanghai Astronomical Observatory, and Kosuke Heki of Hokkaido Univ. We encouragecontribution not limited only VLBI technology but also observational results on geodesy andradio astronomy, status updates of radio telescope, observing system, and data processing
system.
Closing Ceremony of Kashima 34m Antenna
Kashima 34m antenna was damaged by typhoon No.15(Faxai) on 9th Sep. 2019, and mainreflector panels are removed in the same month to avoid extension of damage to surroundings
by next coming typhoons. Dismantle of the Kashima 34m antenna was decided to be performed資料12-J

in 2020 not only by this damage, but also due to degradation of the multiple components of theantenna. We will have closing ceremony of Kashima 34m station in the afternoon of 25th April.
Please feel free to contact LOC for inquiry on this ceremony.
<<<CANCELLED>>>⚫

ALMA Cycle 8 Proposal Preparation Workshop on March 26
Date: Thursday, March 26, 2020, 11: 00-17: 00 JST
Place: ALMA Building 1F Room102 at National Astronomical Observatory of Japan, Mitaka
CampusA Call for Proposals on ALMA Cycle 8 (Main Call) will be issued on March 17 and thedeadline for proposal submission will be on April 15, 2020. East Asia ALMA Regional Center(EA-ARC) will hold a Proposal Preparation Workshop for the ALMA Cycle 8 Main Call at the
Mitaka Campus of National Astronomical Observatory of Japan on March 26. The morning
session consists of explanatory talks such as on the schedule, new capabilities, Observing Toolfor proposal preparation and submission for the Cycle 8 Main Call. The afternoon session
focuses on the proposal writing with lectures on the tips to write competitive proposals basedon the current writing style in EA. In addition, participants bring their own draft proposals andwork on improving them with experienced tutors and an English editor in the hands-on session.
We would like to recommend participants to roughly finish up the draft proposals before joining
this workshop.
<<<SCALE DOWN, REMOTE MEETING>>>⚫

General Meeting of the Japan Radio Astronomy Forum
Date: 3/17, 2020
Remote Meeting⚫

ngVLA Science Working Group Kick-off Meeting
Date: 2020/3/31
Remote Meeting⚫

ngVLA Sub-working Group for Planetary Formation and Proto-planetary Disk, 1st
Meeting
Date: 2020/5/25
Remote Meeting

⚫

ngVLA

Sub-working

Group

for

Black

Time-domain/Multi-messenger Astronomy
Date: 2020/5/28
Remote Meeting

Hole

Formation

andEvolution,

資料12-J⚫

ngVLA Sub-working Group for Galaxy Evolution in the Cosmic History, 1st Meeting
Date: 2020/6/2
Remote Meeting⚫

ngVLA Sub-working Group for Star Formation and Astro-chemistry at Multiple Layer
Date: 2020/6/11
Remote Meeting⚫

Technology for Next Generation Space-Earth Environmental Radio Science, a workshop
by ISEE
Date: Wednesday 26 and Thursday 27, August, 2020
Venue: Full remote conference using the Zoom system
Low frequency radio observations are used as one of the main research tools in space-earth
environmental sciences and astronomy. Low-frequency radio observation devices are able toeffectively obtain a large collecting area and a wide field of view by forming an array withmany antennas. Indeed, there are such large radio telescopes and radars for space-earth
environmental sciences. In radio astronomy, transient science attracts much attention due to thediscovery of fast radio bursts, along with developments of new generation receivers such as
ASKAP's PAF and Parkes' UWL. The construction of the world's largest low-frequency radio
interferometer, SKA, will start in 2021. Phased arrays and wideband receivers are very common
and applicable technologies that benefit various research fields such as space science,geophysics, astronomy, meteorology, and so on. Meanwhile, such technologies have beendeveloped in each field due to a historical background. Moreover, new problems such as radio
frequency interference (RFI) and high data rate signal processing emerged along with the
improvement of receivers. Therefore, in this conference, we invite experts of developing
low-frequency radio instruments across research fields. We aim to provide exchange of thelatest development information, clarify common technical elements and problems, and conduct
interdisciplinary joint research and collaboration.

⚫

ngVLA Sub-working Group for Planetary Formation and Proto-planetary Disk
Date: 2020/8/12
Remote Meeting⚫

ngVLA Sub-working Group for Star Formation and Astro-chemistry at Multiple Layer
Date: 2020/9/1
Remote Meeting⚫

ngVLA Sub-working Group for Galaxy Evolution in the Cosmic History, 1st Meeting資料12-J

Date: 2020/6/2
Remote Meeting⚫

ngVLA Sub-working Group for Testing Gravitational Theories by Galactic Center Pulsars
Date: 2020/9/3
Remote Meeting

⚫

ngVLA

Sub-working

Group

for

Black

Hole

Time-domain/Multi-messenger Astronomy
Date: 2020/9/3
Remote Meeting⚫

General Meeting of the Japan Radio Astronomy Forum
Date: 2020/9/10
Remote Meeting

Formation

andEvolution,