COMMISSION J: Radio Astronomy(November 2016 – October 2020)
Edited by Nario Kuno (University of Tsukuba)
Activity of meetingsJapan SKA consortium local meeting for “Development” in Kagoshima
Date: December 17, 2016
Venue: Inamori Hall, Kagoshima University, Kagoshima, Japan
Topics: Technical Development for Square Kilometre Array (SKA)

ALMA/45m/ASTE Users Meeting 2016
Date: December 19-20, 2016
Venue: NAOJ Mitaka, JapanThe users meeting is hosted by the Chile Observatory and Nobeyama Radio Observatory of
the National Astronomical Observatory of Japan (NAOJ).

SKA Workshop “Galaxy Evolution and Distant Universe” 2017
Date: January 7 – 9, 2017
Venue: Arden Hotel Aso, Kumamoto, Japan
Topics: Cosmic Reionization, Cosmology, Galaxy Evolution, and Square Kilometre Array (SKA)

ALMA Band 1 Science Workshop
Date: January 16-18, 2017
Venue: ASIAA, Taipei (Taiwan)
The ALMA Band 1 Science Workshop will take place at the ASIAA (Academia Sinica,
Institute for Astronomy and Astrophysics) in Taipei (Taiwan) from January 16 to 18 2017. It willconsist of a few invited talks on the main scientific goals of ALMA Band 1, plus contributed talks.
We also plan to have poster sessions. The ALMA Band 1 Science workshop will provide the firstopportunity to show the exciting new science ALMA Band 1 can deliver and to start preparing
for the first observing proposals in the ALMA lowest frequency band. The two days after theworkshop, 19-20 January, will be dedicated to the discussion and planning of the upcoming Band
1 Science Verification phase.



ALMA Workshop for Proto-Planetary Disks
1

Date: January 27, 2017
Venue: Mitaka, NAOJ, Tokyo, Japan
Topics: ALMA proposal Cycle 5, Summary of current works


ALMA Workshop “Nearby galaxy M83 2017”
Date: February 20 – 21, 2017
Venue: Mitaka, NAOJ, Japan
Topics: Observation of fine structure of M83, ISM evolution, Chemical evolution, Star formation

Japan Radio Science Forum Symposium 2016
Date: February 22 – 23, 2017
Venue: NAOJ, Mitaka, Japan
Topics: Dialogue between Senior and Young Scientists



17th “Millimeter/Submillimeter Receiver Workshop” and 3rd “RIKEN and NICT Joint THz
Workshop”
Date: February 27 – 28, 2017
Venue: NICT, Koganei, Japana
Topics: Detection Devices, Optics, Antenna, HEMT, Cooling, Integration, Calibration andScience, Future Projects

Workshop: 30m THz telescope in Antarctica
Date: March 2 – 3, 2017
Venue: The National Institute of Polar Research (NIPR), Tachikawa, Japan
Topics: THz astronomy, THz telescope

ALMA Workshop for Solar System
Date: March 6, 2017
Venue: Mitaka, NAOJ, Japan
Topics: Millimeter and Submillimeter observation and Solar System

Workshop “Why does the Universe accelerate? -Exhaustive study and Challenge for the
future”
Dates: March 8 – 10, 2017
Venue: Kobayashi Hall, KEK, Japan
Because gravity is an attractive force, the expansion speed of the Universe should be2

decreasing. However, observational data accumulated over the years strongly support that thepresent Universe is in the phase of the accelerated expansion and there was also another phase of
the accelerated expansion in the very early Universe. The physical mechanism that makes the
Universe undergo the accelerated expansion is not known yet. Some “repulsive force” isnecessary. The purpose of this innovative area is to clarify the origin of the accelerated expansion.
In order to achieve this goal, it is necessary to investigate the interplay between the repulsive
force causing the accelerated expansion and the attractive force sourced by dark matter which
triggers the formation of the cosmic structures such as the galaxies and clusters of galaxies. In
this innovative area, researchers from different fields join together and form nine sub-groups:
inflation in the early Universe (A01), decelerated expansion by dark matter (A02), accelerated
expansion by dark energy in the present Universe (A03), cosmic microwave background (B01),
galaxy imaging (B02), galaxy spectroscopy (B03), direct measurement of the cosmic expansion(B04), ultimate data analysis (D01), and ultimate theory of the Universe (C01). Not only
collaborations within each individual sub-group but also collaborations among the different subgroups are essential to obtain scientific achievements we desire.
East-Asian ALMA Science Workshop 2016-Taiwan
Date: March 10-12, 2017
Venue: National Tsing Hua University, Hsinchu, Taiwan
In the past few cycles of ALMA scientific operations, we see great success from the EA
community in producing remarkable results. We are also excited by the expansion of the ALMA
community into Korea. To maintain the momentum and to promote regional collaboration, wehold regular science workshops in the three EA-ALMA countries. We are pleased to announce
the 2016 East-Asian ALMA Science Workshop, to be held by National Tsing Hua University in
Hsinchu, Taiwan, on March 10-12, 2017. Like the previous EA-ALMA Science Workshops, we
invite ALMA users to present their recent results. Furthermore, we would like to enhance theworkshop functions on promoting discussion and regional collaborations, by adjusting theworkshop format. We will split part of the workshop into two parallel sessions on Galactic andextragalactic studies. We will have special sessions for prospective projects to call forcollaborators, for archival science, and science that require multi-wavelength observations. The
workshop will be timely to develop proposal ideas and form collaborations for the upcoming
Cycle-5 deadline for PI programs. On the other hand, we encourage teams that plan to submit
large proposals to hold meetings in advance, and present their ideas in the EA ALMA Science
Workshop.



ALMA Workshop on Stars： At the Age of Full Band Availability
3

Date: March 24 – 25, 2017
Venue: Okayama University of Science, Okayama, Japan
Topics: Evolved Stars, Molecule/Dust, Full-band observation


Workshop: Black Hole Astrophysics with VLBI: Past, Present, and Future
Date: March 27 - 29, 2017
Venue: Mitaka campus of NAOJ, Tokyo, JapanThe workshop "Black Hole Astrophysics with VLBI: Past, Present, and Future", will be heldin Tokyo next March. We are organizing this workshop on the occasion of Professor Makoto
Inoue's retirement to honor and celebrate his leading and foundational contributions to the field.
We aim to share our fond memories of Professor Inoue's scientific career, and we also intend toencourage the younger generation to succeed and exceed the future prospects in the advancing
field of radio astronomy. Anybody interested in the workshop is welcome.



ALMA Cycle 5 Town Meeting
Date: April 5, 2017
Venue: Mitaka, National Astronomical Observatory of Japan
ALMA Observatory was announced the ALMA Cycle 5 Call for Proposals (CfP) for
scientific observations. We use Observing Tool (OT) for proposal preparation (parameter setting,estimation of observing time etc.) and submit an ALMA proposal. In Town Meeting, we, East
Asia ALMA Regional Center (EAARC), will explain capability of ALMA Cycle 5 and we will
have an opportunity to consult about proposal preparation through Q&A.



The 16th

IVS NICT Technology Development Center Symposium

Date: June 21, 2017
Venue: NICT Kashima Space Technology Center, Main Building
As an activity of Technology Development Center of IVS （International VLBI Service forGeodesy and Astrometry）, NICT has been organizing annual symposium focused on Technology
development related with space geodetic techniques. Proceedings of the symposium have been
published as IVS NICT-TDC News (http://www2.nict.go.jp/sts/stmg/ivstdc/news-index.html)
and delivered to domestic and international institutes and individuals working on VLBI and space
geodesy.
One of the recent research subject of technology development in VLBI and in radio
astronomy is broadband observation. NICT is conducting a new broadband observation technique
named GALA-V for a target of distant frequency comparison. This broadband observation system
is intended to be compatible with the next generation geodetic VLBI system VGOS. The subject
4

of symposium is not limited only VLBI, but also single dish observation technique for radio
astronomy, space geodetic technique and research result including GNSS, SLR and, local tie
observations. We welcome contributions from broad field of view in these research subject.
Symposium "Evolution of Molecules in Space"
Date: June 27-29, 2017
Venue: Institute of Low Temperature Science, Hokkaido University
We try to approach the answer to the question of how the molecule evolved and the planet,
the earth, and the life were formed in the solar system that was born 4.6 billion years ago in theuniverse where various structures were formed since Big Bang. Focusing on ice and organic
matter composed of the most abundant elements (H, C, O, N), the whole picture of molecular
evolution from the interstellar molecular cloud to the protoplanetary system will be explored inboth experiment and theory.

Workshop ‘Formation of high mass star and cluster in Magellanic Clouds’
Date: July 26-27, 2017
Venue: I-site Namba, Osaka
Recent observations of molecular clouds in the Milky Way and Magellanic Clouds revealthat the interaction between molecular clouds has a major influence on the formation of highmass stars and clusters. In this workshop, through the results of detailed observations ofmolecular cloud and HI in the Magellanic clouds where large clusters are still being formed,
through consideration of environmental differences such as heavy element quantity, the formation
process of high mass star formation will be discussed. High resolution observation of nearby
galaxies and comparison with theoretical studies are also important themes.



NRO45m/ASTE Single Dish Science Workshop 2017
Date: August 1-2, 2017
Venue: Nobeyama Radio Observatory
At Nobeyama Radio Observatory, a new phase of 45m radio telescope is going to start. Now,
three legacy program is finishing, and it is expected that world-leading preeminent results will
come. Furthermore, we are entering the phase to achieve cutting-edge scientific output throughnew observations using receivers including FOREST.
In the southern hemisphere, ASTE is offering 345 GHz and 450 GHz receiver capabilities,
and new and unique results are being published, including those leading to ALMA observations.
It is also expected that the new detector Deshima (On-chip Filterbank Spectrometer for
Submillimeter Wave Cosmology) will open our view to high-z universe.
5In this workshop, we focus on scientific results from single-dish radio telescopes. (1) We
introduce up-to-date scientific results with Nobeyama 45 m telescope and ASTE. (2) We discuss
future requirements from the scientific point of view. We invite oral and poster presentations.
Possible topics include; scientific results with Nobeyama 45m telescope, ASTE, or other singledish telescopes, possibilities of new instrumental development, theoretical studies based on
observational results, etc.
Radio Astronomy Forum meeting 2017
Date: September 11, 2017
Venue: Hokkaido University
Topics: Business meeting

Workshop “Star formation with ALMA: Evolution from dense cores to protostars”
Date : October 26, 2017
Venue : National Astronomical Observatory of Japan, Mitaka



15th Mizusawa VLBI observatory Users’ Meeting.
Date : November 3-4, 2017
Venue : Conference Room, Mizusawa Kita HotelEast Asian ALMA Science Workshop 2017
Date : November 27-29, 2017
Venue : Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea



2nd SKA Workshop for Technology
Date : December 18, 2017
Venue : Kagoshima University



NAOJ Science Meeting “A Role of Magnetic Field in Star Formation and Galactic Structure”
Date : December 20-22, 2017
Venue : Kagoshima University



VLBI Consortium Symposium 2017
Date : December 23-25, 2017
Venue : Teikyo University of Science62017 ALMA/45m/ASTE Users Meeting
Date : December 26-27, 2017
Venue : National Astronomical Observatory of Japan, MitakaWorkshop “An overview of achievements and future of radio astronomy”
Date : December 28, 2017
Venue : University of Tokyo, Institute of AstronomyThe 5th Workshop for Supermassive Black Hole
Date : January 8-9, 2018
Venue : Tohoku University, KatahiraWorkshop “Star formation with ALMA: Evolution from dense cores to protostars”
Date : January 17-18, 2018
Venue : I-site Namba (Osaka prefecture university)



ALMA Star Workshop : What can we really do with ALMA?
Date : January 18-19, 2018
Venue : Tohoku University, AobayamaWorkshop on Proto-planetary Disk
Date : February 1, 2018
Venue : National Astronomical Observatory of Japan, MitakaWorkshop for Science Cases with Takahagi/Hitachi 32m Radio Telescopes
Date : February 20-21, 2018
Venue : Ibaraki University



18th millimeter/sub-millimeter receiver workshop
Date : February 22-23, 2018
Venue : National Astronomical Observatory of Japan, Mitaka

Science Workshop 2018 on FUGIN: The Galactic Plane Legacy Survey for Molecular
CloudsDate : February 26-27, 2018
Venue : Nagoya University
7Workshop on the Solar System Science with ALMA
Date : March 7-8, 2018
Venue : National Astronomical Observatory of Japan, MitakaRadio Astronomy Forum of Japan Symposium FY2017 “Development of New Observation
Technology”
Date : March 19-20, 2018
Venue : National Astronomical Observatory of Japan, MitakaWorkshop for High Mass Star Formation 2018 “High Spatial/Time Resolution Observation
for the Study of High Mass Star Formation”
Date : March 22-23, 2018
Venue : Yamaguchi UniversityWorkshop on the Antarctica 30m THz Telescope
Date : March 27, 2018
Venue : Tsukuba UniversityWorkshop "Star Formation Triggered by Cloud-Cloud Collision"
Date : May 28-29, 2018
Venue : Nagoya University



The Power of Faraday Tomography: towards 3D Mapping of Cosmic Magnetic Fields
Date May 28-June 2, 2018
Venue : Seagaia Resort, Miyazaki



VLBI Science in SKA Age
Date: July 22-23, 2018
Venue: NAOJ, Mitaka
Since VLBI observation techniques can achieve ultra-high spatial resolution (micro to
milliarcsecond) that can not be realized with any other method. Many of Scientific results havebeen obtained by VLBI, such as motions of matter around AGN jets, proto-stars or late-type stars
are captured as moving images. On the other hand, they have always been plagued by poorsensitivity. To realize VLBI observation on a global scale by adding a VLBI function to SKA1
(aperture: 0.1 million square meters, construction will start from 2020, scientific verification in
8

2024 and public observation in 2027), it will be possible to far surpass the existing VLBI
observation network in terms of both sensitivity and spatial resolution. Therefore, as part of the
future plan study at the VLBI conference, we will hold a study conference focused on the science
realized by Japan contributing to the addition of the VLBI network to SKA1.
NOEMA/30m Workshop
Date: July 24-25, 2018
Venue: NAOJ, Mitaka
The NOEMA (NOrthern Extended Millimeter Array) interferometer is currently the mostadvanced millimeter array in the Northern Hemisphere. The maximum angular resolution of
NOEMA is ~0.5 arcsecs at an observing wavelength of 1.3 mm (230 GHz), with receivers
operating at 3mm, 2mm, and 1mm. The number of antennas is expected to reach 12, and thesensitivity of the full NOEMA is expected to be 45-65% of ALMA. The 30-meter single dishtelescope is equipped with a series of heterodyne receivers and continuum cameras operating at
3, 2, 1, and 0.9 millimeters. The main goal of this 2-day workshop is to introduce NOEMA/30m
to the Japanese community and to discuss possible science cases through a series ofinvited/contributed talks given by our community members. Speakers are invited to express
their opinion on how NOEMA/30m time will enhance their immediate and long term science
productivity, based on the assumption that NAOJ gains access to NOEMA/30m time in the near
future. We encourage young scientists to take advantage of this opportunity and actively voice
their opinion.



SNR workshop 2018
Date: September 9-10, 2018
Venue: Nagoya University
Supernova remnants (SNRs) are the most energetic objects not only in our Galaxy, but also
in external 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 ~3000-10000 km/s. Recent observations of the shells in X-rays as well as radio
continuum emission have provided a wealth of information on their physical and kinematicalproperties. It is also remarkable that the dense interstellar medium interacting with the shocks islikely playing a key role to produce X- and gamma-rays as shown by comparisons with HI/COand dust emission. Theoretical works on acceleration and escape of cosmic rays in SNRs are
unveiling details of cosmic-ray acceleration/propagation by magneto-hydro-dynamical numericalsimulations, which will be compared with observations. In the present workshop, we invite
observers and theorists to stimulate active interaction and exchange of ideas on SNRs.
9

Science Workshop on the 30-m THz Telescope in the Antarctica ~Star-Planet formation~
Date: September 12, 2018
Venue: NIPR, Tachikawa
The Antarctic Astronomical Consortium is promoting a plan to construct a 30m class THz
telescope in the inland part of Antarctica where the observation conditions are the best on the
ground. For this time, with the support of the National Institute of Polar Research Research
Meeting, we will hold a research meeting focusing on the formation of star and planet systems
with the THz telescope.

General Meeting of the Radio Astronomy Forum
Date: September 19, 2018
Venue: Hosei University, Koganei

16th Mizusawa VLBI Observatory Users Meeting in 2018
Date: September 25-26, 2018
Venue: NAOJ, Mitaka
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 basisof the activity, we have accelerated a development of KaVA (KVN and VERA Array) and EAVN
(East-Asian VLBI Network), and as a result an open-use of EAVN has been initiated since 2018B
semester (observations will be allocated from 2018 September). We emphasize that thedevelopment of EAVN will promote the KaVA Large Programs in research fields of Star, AGN,
and High-mass star formation, which have been initiated since 2016. In this users meeting, we
will discuss about not only exciting scientific results with VERA/KaVA/EAVN but also future
prospects of Mizusawa VLBI Observatory especially in 2022 and beyond. We hope thatreferences below will be helpful to accelerate these discussions: EAVN will be further developedon the basis of future collaborations with JVN (Japanese VLBI Network), FAST 500-m (China),
and TNRT 40-m (Thailand) radio telescopes, leading improvement of sensitivities and observablefrequencies; Synergy with Gaia DR2 (opened in 2018 April) and SKA (now constructed and its
operation will be initiated in 2027) has been expected.

Workshop on Interstellar Matter 2018 (ISM2018)
Date: November 14-16, 2018
Venue: The Institute of Low Temperature Science, Hokkaido University
The aim of this compact workshop is to offer an opportunity for exchange of current research
10results of physics and chemistry of astronomically-relevant atoms, molecules, and ions in both
gas and condensed phases. Toward the development of interactive activation among astronomical
observations, theoretical calculations, and laboratory experiments, participants from wide fields,
physics, chemistry, planetary sciences, and astronomy, are welcome to this workshop.


ALMA Workshop: From Disk to Solar System
Date: November 21-22, 2018
Venue: WTC Conference Center TokyoVLBI Consortium Symposium 2018: VLBI in SKA Age
Date: December 1-2, 2018
Venue: Kumamoto University



19th East Asia Submillimeter-wave Receiver Technology Workshop &5th Riken-NICT Joint Workshop on Terahertz Technology
Date: December 11-13, 2018
Venue: Kwansei Gakuin UniversityEast Asian ALMA Development Workshop 2018
Date: December 14-15, 2018
Venue: Osaka Prefecture University
The main goal of the workshop is to discuss and identify development items that are criticalin the long term development and operation of the ALMA telescope. The topic of this year's
workshop is “wide IF”. Since the hardware/software development is intimately connected tofuture science requirements, active participation by scientists is highly encouraged.

East Asian ALMA Science Workshop 2018
Date: December 17-19, 2018
Venue: I-site Namba (Osaka Prefecture University)
The main aim of this workshop is to continue to promote and stimulate international
collaboration among the researchers in the EA partners, by reviewing and sharing the most recent
ALMA science results in all relevant fields of astronomy. We plan to hold discussion sessions
to promote closer communication among the researchers in related fields.

Radio Astronomy Forum Symposium 2018: Future Science of Radio Astronomy
Date: December 20-21, 201811

Venue: NAOJ, Mitaka
2018 ALMA/45m/ASTE Users Meeting
Date: December 26-27, 2018
Venue: NAOJ, MitakaIbaraki University Workshop: Transient/Variable Event and Radio Follow-up
Date: February 27-28, 2019
Venue: Ibaraki University

First circular of SOKENDAI-UST Asia Winter School (SAWS) 2019: Star and Planet
Formation: Key Questions and Challenges
Date: February 27-March 1, 2019
Venue: NAOJ, MitakaStar formation with ALMA: Evolution from molecular clouds to protostars
Date: March 4-6, 2019
Venue: Nagoya UniversityInternational Workshop on EAO Futures: Future Science and Instrumentation
Date: March 20-23, 2019
Venue: Najing, China
May 20th - 23rd 2019 the East Asian Observatory will host a four day (two half days andtwo full days) meeting looking at the future of science drivers and instrumentation needs of Submm 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 AsianVLBI project, and instrumentation in polar climates. Talks will cover both the technology
involved in these programs and the science cases for such instrumentation.



Workshop: Polarimetry in the ALMA era: a new crossroads of astrophysics
Date: March 25-29, 2019
Venue: NAOJ, MitakaGalactic Center Workshop 2019
Date: June 10, 2019
Venue: Nagoya Univeristy
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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 with large
velocity dispersion. Further, it is said that the magnetic field strength in the central portion is oneorder of magnitude higher than that in the disk region. Research on the star formation process insuch 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-like objects that blowout from the center to the north and south. Therefore, it can be said that the closest core, the centerof the galaxy, is the most important target for understanding the evolution and activity of the core.
In order to study interstellar phenomena and core activity in such a strong magnetic fieldenvironment, theoretical approaches such as magnetohydrodynamic calculations areindispensable. In this study group, observation researchers and theoretical researchers fromvarious wavelengths and research fields will meet together to provide a place for concrete andclose discussions with a view to future observation equipment.


The 17th IVS NICT-Technology Development Center Symposium
Date: June 27, 2019
Venue: 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 the world (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 is conducting
international observations of intercontinental frequency comparisons using wideband small
antennas. At the symposium, we would like to exchange information on VLBI technology, spacesurveying technology such as GNSS, SLR, single radio telescope observation, time / frequency
related technology, and observation results, aiming for further development of the VLBI field.

Sub-mm Spectroscopy and Large-Scale Science with ASTE
Date: August 19, 2019 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 Center13

region, 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 Highredshift 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 astronomicalsources, in both continuum and line emission. In this year, installation and commissioning of a
new receiver with ALMA Band 10 frequency coverage (787-950 GHz) is planned 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 and LargeScale Science with ASTE by our community members. We look forward to the participation byresearchers who are interested in sub-mm astronomy and related fields.
Nobeyama Science Workshop Reiwa 1st
Date: September 4-6, 2019
Venue: Nobeyama Radio Observatory
The Nobeyama 45m radio telescope has been playing an active role as the leading telescopein Japanese 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 4thyear of this year. It even gives the impression that the science itself with single-dish is shirinking.
However, many active users are young researchers who will lead the next generation. This
workshop provides a place for users to gather and discuss about the latest achievements andresearch prospects, and to think about the possibilities of science with a single-dish in the newera.

General Meeting of Japan Radio Astronomy Forum
Date: September 11, 2019
Venue: Kumamoto University

The 1st circular of the next generation VLA workshop
Date: September 17-20, 2019
Venue: 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
14

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 short baselinearray 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 with baselines up to
9000 km, which will translate into unprecedented sensitivity and milli arcsecond angularresolution at frequencies from 1.2 to 116 GHz.
The 12nd East Asia VLBI Workshop
Date: September 24-26, 2019
Venue: 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.



The 10th Galactic Center Workshop (GCWS 2019): New Horizons in Galactic Center
Astronomy and Beyond
Date: October 21 (Monday) to 24 (Thursday), 2019 (Reiwa 1)
Venue: 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 and interstellar
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 abundanceof dense molecular gas; a currently inactive supermassive black hole but rich signatures of pastcentral activities, the high-energy diffuse gamma-ray emission from GeV up to TeV energies, etc.
15

These unsolved issues span wide ranges of spatial scale, time scale, and energy scale and arelikely related to each other. Current key issues in Galactic center studies include: (1) the triggering
mechanism of central activity; (2) the formation process of the central 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 their binaries, which would be gravitational
wave progenitors. These issues are common to studies of extragalactic nuclei.


VLBI Consortium Symposium 2019: VLBI Crosses National Borders
Date: November 23-25, 2019
Venue: 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 a largescale international joint research, and succeeded in shooting a black hole shadow. A 230GHzVLBI 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, is about to start
construction. It can be said that international VLBI collaboration is now providing a new researchframework. Research themes have expanded from classic AGN jets and maser to accretion disks,transient objects, black holes in the galaxy, and further expanded into new areas of multimessenger 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 newresearch framework through international collaboration, entitled "VLBI Crosses Borders." Thepurpose of this is to draw out new research themes of the VLBI community and discuss and sharethe future image.



The ALMA Workshop: Early Planet Formation in Embedded Disks
Date: December 8-10, 2019
Venue: 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 the form 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 thatat 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,16

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, and strategy
how to understand possible early planet formation in embedded disks.


EA ALMA Development Workshop 2019
Date: December 10-11, 2019
Venue: 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 order tomaintain 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, withthe main aim to present the latest technological advancement and exchange 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 scientific communities, 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 is recognized 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 andsoftware development. Apart from this major focus, we will welcome contributions in the fieldsof antennas, front-ends, back-ends, and software development and related talks in science,science operations and/or commissioning of new capabilities.


17th Mizusawa VLBI Observatory Users Meeting in 2019: 1st circularDate: December 13 - 14, 2019
Venue: 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 basisof 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 of17

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 isnecessary that we discuss with community members how efficiently we conduct 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 of Mizusawa VLBI
Observatory especially in 2022 and beyond. EAVN will be further developed on the basis of
future collaborations with JVN (Japanese VLBI Network), FAST 500-m (China), and TNRT 40m (Thailand) radio telescopes, leading improvement of sensitivities and observable frequencies;
Synergy with Gaia DR2 and SKA has been expected.


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 bepresenting the latest science results related to ALMA. Anybody is welcome to join and hear thetalks.
2019 ALMA/45m/ASTE Users Meeting
Date: December 18 - 19 (Wednesday - Thursday), 2019
Venue: National Astronomical Observatory of Japan (Mitaka Campus, Subaru building 1F large
seminar room)

New View of the Universe opened by THz Observation
Date: December 21, 2019
Venue: National Institute of Polar Research
The terahertz band, which is the new horizon of ground observation, is an undeveloped area
and is 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: January 16-17, 202018

Venue: 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 inastronomy. The outer edge of the galaxy is an optimal target that can cover parameter spaces thatcannot be filled by the system alone with high-resolution observations. In particular, observationsof 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 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 a bird's-eye view of theentire 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 energeticallyadvanced, and it is expected that statistical verification of the physical / chemical properties ofmassive star formation in low-heavy element environment will progress.
<<<CHANGED TO VIRTUAL MEETING, OCTOBER 14-16, 2020>>>

SNR Workshop 2020
Date: February 26-27, 2020
Venue: Nagoya University
Supernova remnants (SNRs) are the most energetic objects not only in our Galaxy, but also
in external 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 as radio
continuum emission have provided a wealth of information on their physical and kinematicalproperties. It is also remarkable that the dense interstellar medium interacting with the shocks islikely playing a key role to produce X-rays and gamma-rays as shown by comparisons with
CO/HI and dust emission. Theoretical works on acceleration and escape of cosmic rays in SNRs
are unveiling details of cosmic-ray acceleration/propagation by magneto-hydro-dynamical
numerical simulations, which will be compared with observations. In the present workshop, we
invite observers and theorists to stimulate active interaction and exchange of ideas on SNRs.
<<<CANCELLED>>>

6th Riken-NICT THz Workshop & 20th Millimeter-Submillimeter Receiver Workshop
Date: Mrch 2-3, 2020
Venue: Tohoku University

19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 thesize and structures of protostellar disks, is one of the ultimate goals in star formation studies.
Such diversity should be originated from the natal dense cores. Observational studies of suchdense 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 condition ofstar formation. However, previous ALMA observations have not extensively explored such young
objects but mainly targeted well-known protostellar and T-Tauri sources, which were discovered
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, are trying to find new
exciting objects without any bright infrared sources, such as candidates of the first hydrostaticcore. Although single-dish telescope and other wavelength data still play an essential role as thefirst atlas, the era that ALMA itself can be one of the survey telescopes is likely upcoming. In thisworkshop, we will discuss the observational strategies on how to select the target objects using
ALMA and to optimize the subsequent follow-up observations to reveal the initial condition ofstar formation, also by combining with the related theoretical simulation.
<<<CANCELLED>>>The ALMA 2030 Vision: Design considerations for Digitizers, Backend and Data Transmission
SystemDate: March 11-13, 2020
Venue: 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 of receivers
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.



ALMA Lensing Cluster Survey Workshop
Date: March 13 - 14, 202020

Venue: 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>>>General Meeting of the Japan Radio Astronomy Forum
Date: March 17, 2020
Remote Meeting

Dynamics and physics of outflows in protostellar disks and Active Galactic Nuclei II
Date: March 23-25, 2020
Loation: Kagoshima University

Japan Radio Astronomy Forum Symposium 2019: Radio astronomy that opens up withextreme performance
Date: March 23-25, 2020
Venue: 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 future plans.
At the symposiums of the last two years, we have held multifaceted discussions over two days,
focusing on technological development that will support future radio astronomy and futurescience in collaboration with other wavelengths and fields. Based on these results, this year, we
will focus on various "extreme performances" regardless of projects and existing telescopes, andexplore science that can only be done by radio astronomy and new methods to realize it in theentire community.
<<<CANCELLED>>>IAU Symposium 360: Astronomical Polarimetry 2020 -- New Era of Multi-Wavelength21Polarimetry
Date: March 23-27, 2020
Venue: 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>>>


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, and also
share the related theoretical studies. In addition, we would like to discuss a strategy for the usageof ALMA Band 8 and 10.
<<<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 focuseson the proposal writing with lectures on the tips to write competitive proposals based on thecurrent writing style in EA. In addition, participants bring their own draft proposals and work 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 thisworkshop.
22

<<<SCALE DOWN, REMOTE MEETING>>>ngVLA Science Working Group Kick-off Meeting
Date: March 31, 2020
Remote Meeting

IVS NICT Technology Development Center Symposium
Date: April 24-25, 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 this time, meetingis 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 encourage contribution not
limited only VLBI technology but also observational results on geodesy and radio 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 in2020 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>>>ngVLA Sub-working Group for Planetary Formation and Proto-planetary Disk, 1st Meeting
Date: May 25, 2020
Remote Meeting

New Developments of Planetary Sciences with ALMA in JpGU-AGU Joint Meeting 2020
Date: May 27, 2020
Venue: Makuhari Messe in Chiba
23

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
Messe in Chiba. It has been about 5 years since the series of concentric rings has been discoveredin the protoplanetary disk of HL Tau, and we will review the current understanding of planetarysystem formation in our session. Recent results with ALMA on the Sun, solar-system planets, andextra-solar planetary systems will be presented and discussed among researchers in planetaryscience and astronomy.
ngVLA Sub-working Group for Black Hole Formation and Evolution, Time-domain/Multimessenger Astronomy
Date: May 28, 2020
Remote MeetingngVLA Sub-working Group for Galaxy Evolution in the Cosmic History, 1st Meeting
Date: June 2, 2020
Remote MeetingngVLA Sub-working Group for Star Formation and Astro-chemistry at Multiple Layer
Date: June 11, 2020
Remote MeetingngVLA Sub-working Group for Planetary Formation and Proto-planetary Disk
Date: August 12, 2020
Remote MeetingTechnology for Next Generation Space-Earth Environmental Radio Science, a workshop by
ISEE
Date: August Wednesday 26 and Thursday 27, 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 with manyantennas. Indeed, there are such large radio telescopes and radars for space-earth environmental
sciences. In radio astronomy, transient science attracts much attention due to the discovery of fast
radio bursts, along with developments of new generation receivers such as ASKAP's PAF andParkes' UWL. The construction of the world's largest low-frequency radio interferometer, SKA,
24

will start in 2021. Phased arrays and wideband receivers are very common and applicabletechnologies that benefit various research fields such as space science, geophysics, astronomy,
meteorology, and so on. Meanwhile, such technologies have been developed in each field due toa historical background. Moreover, new problems such as radio frequency interference (RFI) andhigh data rate signal processing emerged along with the improvement of receivers. Therefore, inthis conference, we invite experts of developing low-frequency radio instruments across research
fields. We aim to provide exchange of the latest development information, clarify common
technical elements and problems, and conduct interdisciplinary joint research and collaboration.
ngVLA Sub-working Group for Star Formation and Astro-chemistry at Multiple Layer
Date: September 1, 2020
Remote MeetingngVLA Sub-working Group for Testing Gravitational Theories by Galactic Center Pulsars
Date: September 3, 2020
Remote MeetingngVLA Sub-working Group for Black Hole Formation and Evolution, Time-domain/Multimessenger Astronomy
Date: September 3, 2020
Remote MeetingGeneral Meeting of the Japan Radio Astronomy Forum
Date: September 10, 2020
Remote Meeting25