text:
Contact@springfieldministerialalliance.org
2019 Annual Dr. Martin Luther King, Jr. Service – January 30 at Zion Baptist Church
Let Us R.I.S.E.
Annual Martin Luther King, Jr. Day Service Honors Civil Rights Icon
The Ministerial Alliance of Springfield and Vicinity
Advancing the Kingdom of God in Springfield, Illinois
Officers & Members
Annual Alliance Events
Member Churches Events
THE MINISTERIAL ALLIANCE OF SPRINGFIELD AND VICINITY, INC
The following By-laws of the 'Ministerial Alliance of Springfield and Vicinity' include the most recent revisions that were previously submitted and subsequently ratified in January of 2018.They are presented here for the benefit of those ministers who are considering aligning themselves with this fellowship.
In order to secure a more direct understanding on our related objectives, we, the Christian Ministers of Springfield and Vicinity, have agreed and set forth in the following declaration, the purpose of this organized body hereby known as The Ministerial Alliance of Springfield and Vicinity, Inc.
ARTICLE I – NAME
The name of this organization shall be The Ministerial Alliance of Springfield and Vicinity, Inc.
ARTICLE II – PURPOSE
The major purpose of the alliance is to promote the spread of the Gospel Message and principles of Jesus Christ throughout Springfield and Vicinity. The organization is organized exclusively for charitable, religious, educational, and/or social service purposes under Section 501(c)3 of the Internal Revenue code.
ARTICLE III – NATURE
The Alliance is a NOT-FOR-PROFIT-BODY, which serves as a medium through which the Christian Churches in this area may work in harmony and cooperation with one another, promoting the work of the Kingdom. The Alliance has not, and it shall never have, any ecclesiastical authority over any Church.
ARTICLE IV – OBJECTIVES
The Alliance shall develop and implement its efforts to achieve the following objectives:
To serve as an advocate for the religious community of Springfield and Vicinity.
To promote the improvement of social, political, educational and health conditions, for all citizens of Springfield and Vicinity.
To promote scholastic excellence among the youth of our member Churches.
To promote harmonious efforts among the Pastors and Churches in fellowship, witness, and other Ministries engaged in by this Alliance.
ARTICLE V – MEMBERSHIP
This body shall consist of Christian Pastors and Ministers who are active in their respective Churches.
SECTION 1: All members shall endorse and support the purpose and objectives of the Alliance.
SECTION 2: All members shall regularly attend and participate in the scheduled meetings and activities of the Alliance.
SECTION 3: All members shall maintain their financial obligations to the Alliance.
SECTION 4: All members shall conform to Sections 1, 2, and 3 of Article V of these Bylaws in order to remain in good standing with this Alliance.
SECTION 5: The Alliance retains the right to expel any member, by two-thirds votes of the membership present at a regular meeting, for failure to comply with Section 4 of Article V.
ARTICLE VI – OFFICERS
The Officers of this Alliance shall be President, Vice President, Secretary, Assistant Secretary, Treasurer, Chaplain, and Parliamentarian.
SECTION 1: These Officers shall comprise the Executive Committee.
SECTION 2: All Officers shall be elected every two (2) years.
SECTION 3: There are no term limits.
SECTION 4: Only Ministers of the Alliance who are ordained in or by their respective denomination and who have been active members of the Alliance for the last one (1) year or more shall be eligible to hold the office of President or Vice President. Those who run for the offices of President and/or Vice-President must submit evidence of their ordination to the Alliance.
SECTION 5: In the event a vacancy should occur in any office, other than the President's office, the President shall be authorized to appoint a temporary replacement who shall serve the remainder of the term of that office. The Vice-President will automatically assume the role of President should that office come vacant.
SECTION 6: Any person filling an appointed office may be eligible for election to that office for its full term after completing the appointed term of office.
ARTICLE VII – DUTIES OF OFFICERS
SECTION 1: The President shall preside at all meetings. He/she shall appoint all committee chairpersons; and serve as the chair of the Executive Committee. The President shall also be an ex-officio member of all other committees, and shall set the Agenda for all Alliance meetings.
SECTION 2: The Vice President shall assist the President as assigned and shall perform the duties of the President as needed. If the Vice-President is unable to preside at a meeting in the absence of the President, the task shall go to another Alliance Officer in the following order: Secretary, Treasurer, Assistant Secretary, Chaplain, Parliamentarian.
SECTION 3: The Secretary shall keep accurate minutes of all meetings. He/she shall forward copies of the minutes of each meeting to the active members of this Alliance. Officers and other members of the Alliance shall turn over to the Treasurer all monies received by the Alliance.
SECTION 4: The Assistant Secretary shall perform the duties of the Secretary as needed.
SECTION 5: The Treasurer shall deposit all monies of the Alliance in appropriate accounts as deemed by the Alliance. He/she shall disburse monies by check as authorized by the Alliance. All checks shall have two (2) signatures, which must be signed by the Treasurer, Secretary, President or Senior Advisor of the Alliance.
SECTION 6: The Chaplain shall be responsible for the Devotions and the selections of the speaker for the meditation of the regular meetings of the Alliance.
SECTION 7: The Parliamentarian shall maintain proper decorum during all meetings and shall keep the body informed of the constitutionality of all proceedings.
ARTICLE VIII – FINANCIAL OBLIGATIONS
Each member shall contribute an annual membership fee and any other special offerings as determined by the Alliance.
SECTION 1: The annual membership fee must be paid by the First Saturday in April.
SECTION 2: New members joining after the March meeting will pay a proration of the annual membership fee by the following meeting date.
ARTICLE IX – MEETINGS
The Alliance shall meet on the first (1st) Saturday of each month with the exception of July.
SECTION 1: Biblical principles and Robert's Rules of Order shall guide the proceedings of each meeting. The Parliamentarian shall bring a copy of Robert's Rules to each official Alliance business meeting.
SECTION 2: The regular meetings shall provide time for Devotion, Breakfast, Business, Invited Guests, instructional period and any other matters as shall be considered appropriate by the body.
SECTION 3: The meetings shall begin with a Devotion at 8:00 a.m.
SECTION 4: Members in good standing who currently meet the criteria for membership as defined in Article V of these Bylaws shall be eligible to vote on any business matters pertaining to the Alliance. "Good standing" includes those members who have been exempted from paying dues to the Alliance.
SECTION 5: The calendar year January 1 through December 31 shall constitute the fiscal year of the Alliance.
SECTION 6: A quorum consisting of one-third of the members in good standing must be present in order to conduct official business. The President, or other person presiding, will see to it that a Quorum is present (through roll-call or other means) before conducting official business.
ARTICLE X – ELECTIONS
SECTION 1: Officer Elections shall be held on the First Saturday in May at the end of every two (2) years. The elective year shall begin on the First Saturday of June.
SECTION 2: A nominating committee, appointed by the President in March shall present the nominees in April, and shall oversee the Officer Elections.
SECTION 3: All nominees must be in good standing pursuant to Article V of these Bylaws.
SECTION 4: Nominations may be made from the floor at the time of the elections.
SECTION 5: Officer Elections shall be made by secret ballot. A simple majority of those voting shall be sufficient for elections.
SECTION 6: Absentee votes will be accepted by the nominating committee up to the day of the election.
ARTICLE XI – INSTALLLATIONS
Installation services for the newly elected officers shall be held immediately following the conclusion of business, on the same day of the election.
ARTICLE XII – STANDING COMMITTEES
SECTION 1: The functions of these Committees are:
1. PROGRAM: Be responsible for all Special Services that the Alliance chooses to sponsor.
2. SOCIAL ACTION: Pursue ways to maintain communication with social agencies to insure that the Alliance is responsive to the needs of the people. Keep the Alliance advised of the current social needs and available resources.
3. HEALTH/WELFARE: Be responsible for referring disadvantaged persons to the appropriate agency for assistance.
4. PUBLIC RELATIONS: Be responsible for informing the media and other appropriate persons or organizations of matters authorized by the Alliance.
5. EDUCATION: Be responsible for the presentation of non-denominational topics during our educational period. Such topics to include: A review of the Bible; Ministerial Ethics, Greek and Hebrew Word Studies. Monitor selected issues of parochial and public schools. Coordinate the Alliance's Scholarship program as directed by the body.
6. ENTERTAINMENT: Be responsible for planning and implementing whatever social functions the Alliance chooses to sponsor.
7. POLITICAL CONCERNS: Strive to create an atmosphere where there is mutual exchange of ideas in the political arena, while monitoring the moral and ethical issues confronting the community and remaining responsive to the needs of the people. Shall try to create an environment that insures that the conduct of opposing parties in any election reflects the highest ethical standards. Shall maintain neutral on political party affiliation and shall not endorse or support any political candidate for local, state or national election.
8. BUDGET & FINANCE: Shall be responsible for developing an annual fiscal year budget for approval by the First Saturday in December of each year.
ARTICLE XIII – AMENDMENTS
These Bylaws may only be amended at a regular meeting or a special call meeting of the Alliance.
SECTION 1: Any proposed amendment of these Bylaws requires a two-thirds majority vote by the membership.
SECTION 2: Proposed amendments must be presented in writing to the President at least two (2) months prior to the meeting at which the amendment is to be considered.
SECTION 3: Written copies of any proposed amendments, shall be forwarded by the President to the members of the Alliance at least one (1) month prior to the meeting at which the amendment is to be considered.
ARTICLE XIV – DISSOLUTION/POWERS CLAUSE
1. "Upon the dissolution of your organization, assets will be distributed for one or more exempt Purposes within the meaning of Section 501(c) 3 of the Internal Revenue Code, or corresponding section of any future Federal tax code or shall be distributed to the Federal government, or the state or local government for public purposes."
2. We agree that no part of the net earnings of the organization will inure to the benefit of, or be distributable to its members, trustees, officers, or other private persons, except that the organization shall be authorized to pay reasonable compensation for services rendered and to make payments and distributions in furtherance of the purposes set forth in our organizing document and our application for federal tax exemption. Notwithstanding any other provision of these articles, the corporation shall not carry on any other activities not permitted to be carried on (a) by a corporation exempt from federal income tax and under section 501(c)3 of the Internal Revenue Code, or the corresponding section of any future federal tax code, or (b) by a corporation, contributions to which are deductible under section 170( c)2 of the Internal Revenue Code, or the corresponding section of any future federal tax code."
Copyright © 2020 The Ministerial Alliance of Springfield and Vicinity. All rights reserved.
Education Hub Pro by WEN Themes


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René Swennen, né le  à Jemeppe-sur-Meuse et décédé le  à Liège, est un écrivain belge de langue française.

Biographie

Il est avocat et l'auteur de romans et de pièces de théâtre.

Il obtient le prix Victor-Rossel en 1987 pour Les Trois Frères.

Œuvres
 Dom Sébastien, roi de Portugal, Paris, Éditions Julliard, 1979, 181 p.
 - Prix Max Barthou de l'Académie française 1979
 Belgique requiem, Paris, Éditions Julliard, 1980, 157 p.  - rééd. Paris, La Table ronde, 2007
 Palais-Royal, Paris, Éditions Julliard, 1983, 243 p.
 - Prix Paul Flat de l'Académie française 1984
 La Nouvelle Athènes, Paris, Éditions Grasset et Fasquelle, 1985, 251 p.
 Les Trois Frères, Paris, Éditions Grasset et Fasquelle, 1987, 264 p.
 - Prix Victor-Rossel 1987
 Le Roman du linceul, Paris, Éditions Gallimard, 1991, 152 p.
 Belgique requiem, suite et fin ?, Bruxelles, Belgique, Éditions Complexe, 1999, 106 p.
 Le Soleil et le Mousquetaire, suivi de La Nuit de la Saint-Nicolas, Liège, Belgique, Éditions du Céfal, 1999, 152 p.
 Cinq nô occidentaux, Liège, Belgique, Éditions du Céfal, 1999, 91 p.
 Belgique requiem. Suite et fin ?, Paris, Éditions Complexe, 2009, 106 p.
 La Disparition de John, Bruxelles, Belgique, Éditions du Grand Miroir, coll. « Roman », 2008, 112 p.
 L'Ombre de Palerme, Neufchateau, Belgique, Weyrich Édition, coll. « Plumes du coq », 2012, 196 p.

Notes et références

Liens externes

Écrivain belge du XXe siècle
Écrivain belge du XXIe siècle
Romancier belge
Dramaturge belge du XXe siècle
Dramaturge belge du XXIe siècle
Naissance en janvier 1942
Naissance à Seraing
Décès en janvier 2017
Décès à Liège
Décès à 75 ans

redpajama_set_name: RedPajamaWikipedia


This presentation is based on our experience with building and using data and time-series analytics tools for F#. We look at two projects that have been developed by BlueMountain Capital: the R type provider allows analysts to access R packages and functions directly from the F# environment while Deedle is a time-series and data manipulation library implementing operations such as data alignment, joining and handling of missing values. In the talk, we would like to discuss two interesting questions that arise from the projects.
Firstly, the R type provider discovers R packages and functions and makes them accessible via the F# type system. This raises interesting questions about the interoperability between statically-typed and dynamically-typed languages. How much information can we obtain from dynamic runtime like R? And what features did we propose for F# to make the interoperability between static and dynamic languages easier?
Secondly, the Deedle library raises similar interoperability questions, but at the boundary between functional-first F# and object-oriented C#. Our design goal has been to make the library usable from both languages - what is the right balance between object-oriented and functional API design? We'll also discuss finding the right balance between immutable and mutable data structures in this project.


TSYS (NYSE:TSS) today announced the publication, in association with FICO (NYSE:FICO) , of a new report titled "Engaging Customers: Why Should Financial Institutions Move Toward a 'Bring Your Own Persona' Approach." The report explains that with the growing consumer adoption of mobile devices, social media and improved user interfaces, financial institutions can differentiate themselves by understanding their customers' preference for digital communication and their degree of trust in sharing financial information through digital channels.
Most financial institutions are leveraging "Know Your Customer" (KYC), traditionally a risk-management tactic and regulatory compliance obligation, as an approach that allows customers to elect their preferred channel of communication. The report suggests, however, that this approach is no longer adequate. A "Bring Your Own Persona" approach, according to the report, allows new segments to be identified and categorised by their level of digital engagement and trust in sharing information.
"Financial institutions now recognise that the traditional approach to communicating with customers is no longer adequate. Relying solely on data such as income, age and geography isn't enough In the digital age, customers expect banks to understand their preferred communications channels, willingness to share personal data in various scenarios and ability to transact," said Bruno Courbage, senior director of Product Management for Customer Management at FICO.
"Financial institutions' relationships with their customers are changing, largely driven by two key influencers – the adoption of enabling technology and the insight available from big data. Banks that embrace big data, use it to better understand their customers' habits and preferences and combine it with the user experience will have a true strategic advantage," said John Goodale, group executive, product and market development, TSYS International.
The report looks at the findings from the 2015 TSYS U.K. Consumer Payments Engagement Survey, which identified key consumer preferences around engaging with financial institutions. The report concludes by providing four prescriptions for financial institutions that intend to use a "Bring Your Own Persona" approach to engage customers.
FICO (NYSE:FICO) is a leading analytics software company, helping businesses in 90+ countries make better decisions that drive higher levels of growth, profitability and customer satisfaction. The company's groundbreaking use of Big Data and mathematical algorithms to predict consumer behavior has transformed entire industries. FICO provides analytics software and tools used across multiple industries to manage risk, fight fraud, build more profitable customer relationships, optimize operations and meet strict government regulations. Many of our products reach industry-wide adoption. These include the FICO(R) Score, the standard measure of consumer credit risk in the United States. FICO solutions leverage open-source standards and cloud computing to maximize flexibility, speed deployment and reduce costs. The company also helps millions of people manage their personal credit health. FICO: Make every decision countTM. Learn more at www.fico.com.


We are very excited to announce that we will be returning to the Elm Tree Ringwood on Friday the 14th of December!
We love this venue and are looking forward to performing a 1 hour set of original music from 8:30pm.
Pop on down for what should be a great evening of live music!


text:
Lawmakers still haven't finished up
While celebrating many gains for the disability community in the 2021 special legislative session, some eyes are on the calendar. […]
While celebrating many gains for the disability community in the 2021 special legislative session, some eyes are on the calendar.
The Minnesota Legislature will gavel back into session in September. The main topic on the agenda is to make decisions on bonus pay for essential workers who toiled on the front lines of the COVID-19 pandemic. Lawmakers in June passed a measure to pay $250 million to potentially thousands of front-line essential workers. That could include nurses, long-term care workers, grocery store workers, small business owners and many others. A nine-member committee is to decide how the money will be allocated. Three members will be appointed by Gov. Tim Walz, three by the Republican-controlled Senate and three by the DFL-controlled House. A seven-member majority vote is needed to allocate the money. Their recommendations are due by September 6, when lawmakers will meet again in a special session.
Action on bonding is also possible in September.
The 2021 special session, which extended into July, was highlighted by a compromise the state budget. Disability advocates and their organizations saw many gains, especially on the personal care attended compensation front.
Federal assistance and higher-than-anticipated tax revenues made many gains possible. Here's a look at other highlights of the 2021 session and links to additional information. In recent weeks groups have been posting legislative updates on their web pages. Self-advocates should check the web pages of the groups they are involved with.
One of the most detailed legislative wrap-ups is provided by the Minnesota Council on Disability. https://www.disability.state.mn.us/public-policy/legislative-update/#7-7-21 The council is also sending out updates on individual bills.
Many gains were made in mental health, and have been outlined by National Alliance for the Mentally ill (NAMI) Minnesota. One big step is to expand the mental health workforce, increase its diversity and have it be more culturally informed. Gains include a funding increase for loan forgiveness programs and expanding it to licensed alcohol and drug counselors, cultural and regional diversity standards for licensing boards, including cultural competency in continuing education standards for mental health professionals, paying for BIPOC mental health professionals to become supervisors, creating a culturally informed and culturally responsive mental health task force, and other key items. Wilder Foundation also worked closely on this effort.
Another positive measure is in alternate pathway to children's residential treatment. Legislation from NAMI Minnesota and Aspire Minnesota was passed, that develops an alternative pathway for children voluntarily accessing residential mental health treatment without entering the child protection system.
Legislation was also passed that expands eligibility for Youth ACT services for children as young as eight and adults up to age 25. This will ensure that more children can obtain needed intensive mental health supports.
Another win centered on the CADI (Community Access for Disability Inclusion) waiver: NAMI's bill to suspend, not terminate, the CADI waiver when someone is hospitalized or in residential treatment passed.
Read more about mental health measures and next steps at https://namimn.org/
Another emphasis during the session was to support programs for the homeless and programs to prevent more people from becoming homeless. Minnesota will be transitioning out of the eviction moratorium this summer. The state's housing crisis has had a huge impact of people with disabilities.
Education also saw a lot of disability-related changes, including funding for suicide prevention training, and increased funding for school-linked mental health. State lawmakers are putting $1.2 billion more into the state's classrooms over the next four years, the largest increase in more than a decade. Special education and individualized education plans or IEPs also got needed attention.
Health care was also a big focus. The state's reinsurance plan will continue through at least 2022. The program gets deserved credit for keeping premiums low, and for serving as a financial backstop for insurers who encounter enrollees with costly health conditions. The program, which has been a boon to many people with disabilities, has often gotten caught in the crosshairs over single-payer health care for Minnesotans.
Another focus was telehealth, which became even more of a lifeline for many people during the pandemic. A big change was to remove the weekly visits cap that public health programs struggled under. Minnesotans can access telehealth services by phone or audio-only means through July 1, 2023. Telehealth services are reimbursed at the same rate as in person treatment.
The July issue of Access Press extensively covered the changes to the personal care attendant program, as well as public safety and other changes. Read more at www.accesspress.org
This information was compiled by Managing Editor Jane McClure.

redpajama_set_name: RedPajamaCommonCrawl


text:
\section{Introduction}
\label{sec:Introduction}

The very long baseline interferometry (VLBI) technique enables us to obtain extremely high angular resolution of milliarcsecond (mas) to microarcsecond ($\mu$as) scales \cite{Thompson17}.
In VLBI, higher angular resolution can be achieved by employing longer baseline length between each telescope or by conducting an observation at higher observing frequency.
Longer baseline lengths can be obtained with global-scale VLBI array such as, for example, the European VLBI Network (EVN) \cite{Zensus15}, the Long Baseline Array (LBA) in Australia \cite{Edwards15}, the Very Long Baseline Array (VLBA) \cite{Napier94}, and the Global Millimeter-VLBI Array \mbox{(GMVA) \cite{Hodgson12}}, or can also be achieved with so-called `space VLBI' technique by employing one (or more) satellite(s) and conducting a VLBI observation using a satellite and ground-based radio telescopes.
Space VLBI observations were realized by the VLBI experiment with the Tracking and Data Relay Satellite System (TDRSS) \cite{Levy86,Linfield89,Linfield90}, the VLBI Space Observatory Programme (VSOP) with the HALCA spacecraft \cite{Hirabayashi98,Hirabayashi00}, and the RadioAstron project \cite{Kardashev13}.
On the other hand, one of the ultimate goals in the angular resolution with higher observing frequency was accomplished by a series of VLBI observations of a black hole shadow in our Galactic center Sgr A$^*$ and a nearby active galaxy M87 at 230~GHz led by the Event Horizon Telescope (EHT) project with its angular resolution of about 25~$\mu$as \cite{EHT19a,EHT22a}.

VLBI is an important tool for studying Galactic and extragalactic astrophysical phenomena mainly on the basis of mas- to $\mu$as-scale images \cite{Verschuur88}, while it also has various applications in geophysics, such as, for example, measurement of the Earth orientation parameter (EOP; \cite{Schuh12,Nothnagel17} and references therein), determination of the International Celestial Reference Frame (ICRF; \cite{Ma98,Fey15,Charlot20,Witt22}) and the International Terrestrial Reference Frame (\mbox{ITRF; \cite{Altamimi16}} and references therein), and study on the Earth's tectonic plate (\cite{Sovers98} and references therein).
Capabilities of these applications can be developed in terms of an accuracy of measurement by conducting high-cadence monitoring with high angular resolution by employing intercontinental VLBI observations (e.g., \cite{Ghaderpour21}).
These examples thus indicate the importance of close international collaboration in VLBI.

Since the first success of a VLBI experiment in 1967 \cite{Broten67,Kellermann01}, a lot of domestic and international VLBI networks have been developed and it is also the case in East Asian countries.
In Japan, pioneering domestic VLBI experiments were carried out using Kashima 34~m and Nobeyama 45~m telescopes called as `the Kashima--Nobeyama Interferometer' (KNIFE) at 22 and 43~GHz early in 1990s \cite{Miyoshi93}.
Nobeyama also joined the intercontinental millimeter-wavelength VLBI experiment at 100~GHz \cite{Baath92}.
Series of VLBI experiments with KNIFE led launch of the first Japanese-domestic VLBI array entitled `the Japanese VLBI Network' (J-Net) in 1994 consisting of four telescopes (Kashima 34~m, Nobeyama 45~m, Mizusawa 10~m, and Kagoshima 6~m).
J-Net made couple of new findings in its kinematics with observations of water-vapor masers in and around star-forming regions and protostars (e.g., \cite{Omodaka99,Imai99}) and evolved stars (e.g., \cite{Imai97,Ishitsuka01}).
J-Net also took an important role in a Galactic-plane survey of extragalactic radio sources for a positional reference of Galactic maser sources \cite{Honma00a} as a pathfinder of the VLBI Exploration of Radio Astrometry (VERA) \cite{Honma00b,Kobayashi03}.
VERA is also a key partner of `the (renewed) Japanese VLBI Network' (JVN) \cite{Doi06} consisting of several telescopes operated by universities and institutes in which each telescope is located (Tomakomai 11~m operated by Hokkaido University \cite{Sorai08}; Hitachi 32~m and Takahagi 32~m operated by Ibaraki University \cite{Yonekura16}; Tsukuba 32~m operated by Geospatial Information Authority of Japan (GSI) \cite{Kokado08}; Kashima 34~m operated by the National Institute of Information and Communications Technology (NICT), Usuda 64~m operated by Japan Aerospace Exploration Agency (JAXA), Gifu 11~m operated by Gifu University, and Yamaguchi 32~m operated by Yamaguchi University \cite{Fujisawa02})\endnote{Tomakomai 11~m, Tsukuba 32~m, and Kashima 34~m telescopes have already been deconstructed.}.

China participated in international VLBI experiments in 1980s.
The first radio telescope in China was constructed at Sheshan, a suburban area of Shanghai, with its diameter of 25~m in 1987 \cite{Liang89}.
Sheshan is a telescope which participated in EVN as a full member at an early stage of EVN in 1990.
After that many telescopes in China started participation in EVN, Nanshan 25~m in 1994 (main reflector of the telescope has been refurbished with its diameter of 26~m in 2015) \cite{Zhang19}, Kunming 40~m in 2009 \cite{Hao10}, and Tianma 65~m in \mbox{2015 \cite{Bolli19}}.
These telescopes constitute `the Chinese VLBI Network' (CVN) \cite{Li08} with the longest baseline length of 3300~km between Sheshan and Nanshan telescopes.
In addition to astronomical VLBI observations, CVN is utilized for determining an orbit of a series of Chang'E lunar explorers (\cite{Liu21} and references therein) and the Tianwen-1 Mars \mbox{explorer \cite{Yang22}}, and for making a precise position determination of landers for these spacecrafts \cite{Klopotek19}.

The first radio telescope in Korea, Taeduk Radio Astronomy Observatory (TRAO) 14-m telescope, was constructed in 1986 with its major observing frequencies of around and greater than 100~GHz \cite{Jeong19}.
TRAO 14~m conducted the first astronomical VLBI observation with Nobeyama 45~m at 86~GHz in 2001 and successful fringe detection of SiO $v$ = 1, $J$ = 2--1 maser emission was made toward an evolved star VY Canis Majoris \cite{Shibata04}.
This experiment was an important demonstration for the construction of a domestic VLBI array `the Korean VLBI Network' (KVN) from \mbox{2001 \cite{Wajima05,Lee11,Lee14}}.
One of the most unique capabilities of KVN is simultaneous multifrequency data receiving system for four observing frequencies (22, 43, 86, and 129~GHz), which is the world's first system equipped in a radio \mbox{telescope \cite{Han13}}.
Antenna's basic performance of KVN telescopes, including the pointing accuracy and beam pattern measurement, was confirmed using a temporary receiver at 100~GHz before starting the open-use program of KVN in 2013 \cite{Kim11}.
KVN started participation in EVN as an associate member in 2014.

As mentioned above, domestic VLBI arrays in each country in East Asia have their own geographical uniqueness.
Japan (VERA and JVN) shows a wide distribution of a lot of radio telescopes in the country with the maximum baseline length of 2300~km, whereas KVN is a compact array with the range of its baseline length of 305--480~km, resulting in making very high-sensitive array with shorter baseline lengths.
Some of CVN telescopes locate at the near-Easternmost and near-Westernmost parts of its very big country.
The features found in each VLBI array are complementary in terms of an angular resolution and an imaging quality.
Those situations motivate us to launch a new international VLBI array in East Asia called `the East Asian VLBI Array' (EAVN) \cite{Wajima16,An18}.
The very early concept of EAVN, however, was discussed in the mm-VLBI workshop held in 2003 in China and the committee of the East Asian VLBI Consortium was established at the 6th East Asian Meeting on Astronomy (EAMA) in 2004 \cite{Inoue05}.
This consortium was transferred to a task force for EAVN as one of working groups under the East Asian Core Observatories Association (EACOA)\endnote{\url{https://www.eacoa.net/}, accessed on 1 December 2022} in 2005 and started its practical activity from 2013 including creation of a governing body of EAVN and evaluation of EAVN's array capability.
Prior to launch of EAVN, bilateral VLBI array between Korea and Japan, the KVN and VERA Array (KaVA; e.g., \cite{Matsumoto14,Niinuma14}), has been started its operation in 2013 and its open-use program in 2014.
KaVA has conducted more than 650 observing sessions with the total observing time of about 4700 hours by the middle of 2018.
After completing a series of fringe test observations \cite{Wajima16}, evaluation of data calibration capability \cite{Cho17}, and pioneering scientific experiments with EAVN (e.g., \cite{Fujisawa14,Sugiyama16}), open-use program of EAVN has been launched in the second half of 2018.

This paper provides basic information on the overall observing system of EAVN and reviews major scientific results obtained by EAVN to date.
EAVN is a unique VLBI array not only for filling a geographical gap between existing VLBI arrays on the Earth but also for providing an opportunity to conduct an observation using the multi-frequency simultaneous data reception system with global-scale VLBI for the first time, both of which are described in Section~\ref{sec:Overview of the Array}.
Astronomers all over the world can utilize these capabilities through the EAVN open-use program, which is described in Section~\ref{sec:Summary of the EAVN Open-Use Program}.
Thanks to the unique capabilities mentioned above, EAVN has made scientific findings toward active galactic nuclei (AGNs), evolved stars, and star-forming regions, as well as various Galactic and extragalactic radio sources, on the basis of high-cadence VLBI monitoring and simultaneous data reception of two or more radio signals at cm- to mm-wavelength regime, which are shown in Section~\ref{sec:Scientific Accomplishments by EAVN}.
EAVN is also grown as one of the key VLBI arrays in terms of future international collaboration and those activities are summarized in Section~\ref{sec:Future Growth into the Global VLBI}.
Note that part of scientific results shown in this paper are derived with not only EAVN but also bilateral VLBI collaboration between East Asian countries, such as KaVA.

\section{Overview of the Array}
\label{sec:Overview of the Array}

This section describes an overview of the observation system of EAVN.
The system is always updated and its detailed specifications can be found in `the EAVN Status Report' on the EAVN website\endnote{\url{https://eavn.kasi.re.kr/}, accessed on 1 December 2022}.

\subsection{Telescope}
\label{subsec:Telescope}

Figure~\ref{fig:EAVN-map} shows the location map for each participating telescope in EAVN which consists of 16 radio telescopes and three correlator sites located in each East Asian country (Daejeon in Korea, Shanghai in China, and Mizusawa in Japan).
EAVN composes of several independent VLBI arrays and radio telescopes.
VERA consists of four telescopes (Iriki, Ishigakijima, Mizusawa, and Ogasawara) and is a core VLBI array in Japan.
Other Japanese telescopes except Nobeyama are joint partners for JVN.
Four Chinese telescopes (Kunming, Nanshan, Sheshan, and Tianma) constitute CVN.
KVN consists of three telescopes (Seoul, Ulsan, and Jeju).
Sejong 22-m telescope has been constructed in 2013 with space geodetic survey being as a main task, while the telescope joined the open-use program for both KVN and EAVN in 2022.

\begin{figure}[H]
\includegraphics[width=12.5 cm]{EAVN-map.png}
\caption{Concept map of EAVN including 16 active telescopes listed in Table~\ref{tbl:EAVN-List}, three potential
telescopes (Miyun 50~m in China, Gifu 11~m, and Usuda 64~m in Japan), and three correlator sites in China, Japan,
and Korea.
Photographs of each radio telescope and correlator site are overlaid on `the Blue Marble' image (credit of the ground image: NASA Earth Observatory (\url{https://earthobservatory.nasa.gov/}, accessed on 1 December 2022).
\label{fig:EAVN-map}}
\end{figure}

Figure~\ref{fig:EAVN-UV} shows examples of the spatial frequency coverage (($u$, $v$) coverage) of EAVN at each observing frequency.
The maximum baseline length of EAVN is composed of Nanshan and VERA-Ogasawara stations with its baseline length of 5078~km, corresponding to an angular resolution of 1.82, 0.55, and 0.28~mas at 6.7, 22, and 43~GHz, respectively.

\begin{figure}[H]
\includegraphics[width=13.5 cm]{EAVN_UV_Coverage.png}
\caption{Examples of the ($u$, $v$) coverage for an EAVN observation with full array configuration at 6.7 (upper panels), 22 (middle panels), and 43~GHz (lower panels) with the source's declination of $+60^{\circ}$ (left panels), $+20^{\circ}$ (center panels), and $-20^{\circ}$ (right panels).
$\lambda$ represents the observing wavelength.
Total observing duration of 10 hours and the antenna's lower elevation limit of $15^{\circ}$ are assumed for all cases.
\label{fig:EAVN-UV}}
\end{figure}

Table~\ref{tbl:EAVN-List} indicates basic observing parameters for participating telescopes of EAVN.
EAVN is operated using 11, 12, and 11 telescopes at three frequency bands, 6.7, 22, and 43~GHz, respectively.
The number of participating telescopes shown above includes Nanshan at 6.7 and 43~GHz in which performance of the cooled receiver at these frequencies is under evaluation.
The system equivalent flux density (SEFD) shown in Table~\ref{tbl:EAVN-List} is defined as follows;
\begin{equation}
SEFD = \frac{2 k_{\rm B} T_{{\rm sys}, \nu}}{A_{{\rm e}, \nu}},
\label{eqn:SEFD}
\end{equation}
where $k_{\rm B}$ is Boltzmann's constant, $T_{{\rm sys}, \nu }$ and $A_{{\rm e}, \nu}$ are the system noise temperature and the effective aperture area at an observing frequency $\nu$, respectively.

\begin{table}[H]
\caption{Participating arrays and telescopes in EAVN.
\label{tbl:EAVN-List}}
\tablesize{\endnotesize}
\setlength{\tabcolsep}{1.4mm}{\begin{tabular}{llcccccc}
\toprule
\textbf{Country} & \textbf{Array/Telescope}	& \textbf{Enrollment} \boldmath{$^a$} & \textbf{Diameter [m]} & \multicolumn{3}{c}{\textbf{SEFD \boldmath{$^b$} [Jy]}} \\
                 &                          &                     &                       & \textbf{6.7~GHz} & \textbf{22~GHz} & \textbf{43~GHz} \\
\midrule
China            & Kunming                  & 2021                & ~~~~~~~40             &  ~~307      &--      &--        \\
                 & Nanshan                  & 2018                & ~~~~~~~26             & *** $^d$    & ~~364  & *** $^d$ \\
                 & Sheshan                  & 2021                & ~~~~~~~25             &   1740      &--      &--        \\
                 & Tianma                   & 2018                & ~~~~~~~65             & ~~~~55      & ~~100  & ~~122    \\
Japan            & Hitachi                  & 2021                & ~~~~~~~32             &  ~~158      &--      &--        \\
                 & Nobeyama                 & 2018                & ~~~~~~~45             &--           & ~~285  & ~~655    \\
                 & Takahagi                 & 2020                & ~~~~~~~32             &--           & ~~343  &--        \\
                 & VERA                     & 2018                & $4 \times 20$         &   2155      &  2110  &  4393    \\
                 & Yamaguchi                & 2021                & ~~~~~~~32             &  ~~286      &--      &--        \\
Korea            & KVN                      & 2018                & $3 \times 21$         &   4241 $^c$ &  1328  &  1992    \\
                 & Sejong                   & 2022                & ~~~~~~~22             &--           &  1231  &  2055    \\
\bottomrule
\end{tabular}}

\noindent{\footnotesize{Note. $^a$ Year of enrolment in EAVN. $^b$ The system equivalent flux density (SEFD) for VERA and KVN is a value for a single antenna. $^c$ Only Ulsan station can conduct an observation at 6.7~GHz. $^d$ The system performance is under evaluation.}}
\end{table}

\subsection{Overview of Data Acquisition Flow}
\label{subsec:Overview of Data Acquisition Flow}

Figure~\ref{fig:EAVN-Data-Flow} shows a schematic diagram of data flow of an EAVN observation.
Radio signal received is digitized and formatted using digital signal processing (DSP) system, and recorded with a disk storage at each telescope.
Recorded data are transferred to the Korea--Japan Correlation Center (KJCC), in which the main correlator for EAVN is equipped, via FTP.
Data at Nobeyama and three JVN stations (Hitachi, Takahagi, and Yamaguchi) are recorded by the OCTADISK recorder \cite{Oyama12} and those data are once transferred to the digital baseband converter (DBBC) at Mizusawa VLBI Observatory to perform digital filtering before sending them to KJCC.
Details of this process are mentioned in Section~\ref{subsec:Digital Signal Processing and Recorder}, while note that the process becomes unnecessary for future EAVN observations with the data recording rate of 2~Gbps or higher.

\begin{figure}[H]
\includegraphics[width=13.5 cm]{EAVN-Data-Flow.png}
\caption{Schematic diagram of data flow of current EAVN observations. `DAS' represents data acquisition system.
\label{fig:EAVN-Data-Flow}}
\end{figure}

\subsection{Frontend}
\label{subsec:Frontend}

Receiver noise temperature of EAVN telescopes for each observing frequency is shown in Table~\ref{tbl:EAVN-Backend}.
Cooled HEMT receiver for all observing frequencies of EAVN is equipped at all EAVN telescopes, except a 6.7~GHz receiver at all VERA stations, KVN-Ulsan, and Sheshan being operated under a room temperature.
Data reception with dual polarization is available for all receivers except a 6.7~GHz receiver at VERA and KVN-Ulsan and a 43~GHz receiver at Nobeyama being available for only left-hand circular polarization.

One of the most unique capabilities of EAVN is a multi-frequency data receiving system in which an observation data can be obtained at two or more frequencies simultaneously.
Currently such system is installed at nine stations, KVN (22, 43, 86, and 129~GHz), VERA (22 and 43~GHz), Sejong (22 and 43~GHz), and Nobeyama (22, 43, and 86~GHz).
This unique capability enables us to obtain better baseline sensitivity by employing the `frequency phase transfer' (FPT) technique \cite{Algaba15,Zhao18}, and to determine a relative position between target and reference source by employing the `source-frequency phase-referencing' (SFPR) \mbox{technique \cite{Dodson14,Zhao19}}.
Details of the system installed at Nobeyama, the HINOTORI (Hybrid Installation Project in Nobeyama, Triple-band Oriented) system, is provided by another paper \cite{Okada20}.

It is also important not only to equip a high-performance receiver but to provide a source catalog optimized for an observation at 22~GHz or higher, which are main observing frequency with EAVN, in order to raise the detectability of target sources and to provide an appropriate environment for calibration of the data obtained by EAVN since VLBI calibrators at higher frequency of greater than 20~GHz are less known compared to those at lower frequency.
A series of VLBI calibrator survey containing more than 1500 extragalactic radio sources with its declination of higher than $-32.5^{\circ}$ are carried out using KVN at 22 and 43~GHz, resulting in providing an important information for calibration of the flux density with KaVA and EAVN \cite{Lee17}.

\begin{table}[H]
\caption{Performance of the receiver and the data acquisition system at each EAVN station.
\label{tbl:EAVN-Backend}}
\tablesize{\endnotesize}

\begin{adjustwidth}{-\extralength}{0cm}
\setlength{\tabcolsep}{4.3mm}{\begin{tabular}{llcccccc}
\toprule
\textbf{Array/Telescope} & \multicolumn{3}{c}{\boldmath{$T_{\rm RX}$}} & \textbf{DSP} & \textbf{Recorder} \\
                         & \textbf{6.7~GHz} & \textbf{22~GHz} & \textbf{43~GHz}                 &              & \\
\midrule
Kunming                  & ~~20     & ---    & ---                    &  DBBC, CDAS  & Mark 5B, Mark 6   \\
Nanshan                  & *** $^a$ & 15     & *** $^a$               &  DBBC, CDAS  & Mark 5B, Mark 6   \\
Sheshan                  & 100      & ---    & ---                    &  DBBC, CDAS  & Mark 5B, Mark 6   \\
Tianma                   & ~~20     & 35     & ~~50                   &  DBBC, CDAS  & Mark 5B, Mark 6   \\
Hitachi                  & ~~20     & ---    & ---                    &  ADS3000+    & OCTADISK          \\
Nobeyama                 & ---      & 85     & 110                    &  ADS3000+    & OCTADISK          \\
Takahagi                 & ---      & 30     & ---                    &  ADS3000+    & OCTADISK          \\
VERA                     & 100      & 50     & ~~90                   &  VERA, OCTAD & OCTADISK          \\
Yamaguchi                & ~~20     & ---    & ---                    &  ADS3000+    & OCTADISK          \\
KVN                      & 300      & 40     & ~~50                   &  VERA, OCTAD & Mark 5B, Mark 6, OCTADISK \\
Sejong                   & ---      & 30     & ~~90                   &  DBBC        & Mark 6            \\
\bottomrule
\end{tabular}}
\end{adjustwidth}
\noindent{\footnotesize{Note. $^a$ The system performance is under evaluation.}}
\end{table}

\subsection{Digital Signal Processing and Recorder}
\label{subsec:Digital Signal Processing and Recorder}

Table~\ref{tbl:EAVN-Backend} shows an equipment for DSP and a recorder used at each telescope.
EAVN is currently operated with the data recording rate of 1024~Mbps, corresponding to the total bandwidth of 256~MHz for 2-bit sampling.
Due to a difference in the historical background of each VLBI array constituting EAVN, DSP and recorder installed are somewhat different.

To keep compatibility of digital data sequence between KVN and VERA for conducting joint observations with KaVA, similar type of digital data acquisition system \cite{Iguchi05} is introduced at KVN stations \cite{Oh11}.
CVN telescopes, on the other hand, introduce the DBBC system partly because they have started participation in EVN prior to EAVN.
Another type of DSP system, the Chinese VLBI Data Acquisition System (CDAS), is developed uniquely in China and installed at all CVN telescopes \cite{Zhang10}.

Observation data at four Japanese telescopes (Hitachi, Nobeyama, Takahagi, and Yamaguchi) are digitized by the ADS3000+ sampler \cite{Takefuji10} and recorded using the OCTADISK system \cite{Oyama16}, both of which were developed uniquely in Japan, while ADS3000+ does not have a same digital filter mode to that of VERA DAS and DBBC.
Data obtained at these telescopes are thus recorded by OCTAD with the data output rate of 2~Gbps and transferred to the Mizusawa VLBI Observatory to convert the data output rate (1~Gbps) and the channel assignment of the data suitable for correlation with other telescopes' data.
Note that EAVN is planning to move to regular operation with the data recording rate of 2~Gbps or higher in the near future, data processing at Mizusawa, shown in Figure~\ref{fig:EAVN-Data-Flow}, will thus become unnecessary.

\subsection{Correlator}
\label{subsec:Correlator}

EAVN is operated using correlators located in China, Japan, and Korea, as shown in Table~\ref{tbl:EAVN-Correlator}.
All correlators are utilized for examining data quality and various observing modes of EAVN, whereas all observation data on the open-use program are correlated using the Daejeon Correlator, which is hardware-based, at the headquarters of Korea Astronomy and Space Science Institute (KASI).
DiFX correlator at Daejeon and Shanghai is mainly used for correlation of data obtained by KVN and CVN, respectively.
The 'SoftCos' correlator was assembled by National Astronomical Observatory of Japan (NAOJ) \cite{Oyama16} on the basis of the GICO3 software correlator as a main engine which was developed by \mbox{NICT \cite{Kimura02}.}

\begin{table}[H]
\caption{Correlators used for EAVN observations.
\label{tbl:EAVN-Correlator}}
\setlength{\tabcolsep}{9.05mm}{\begin{tabular}{llcccccc}
\toprule
\textbf{Site}      & \textbf{Correlator}      & \textbf{Reference}      \\
\midrule
Daejeon (KASI)     & Daejeon Correlator, DiFX & \cite{Lee15,Deller07}   \\
Shanghai (SHAO)    & DiFX                     & \cite{Deller07,Jiang18}         \\
Mizusawa (NAOJ)    & SoftCos                  & \cite{Kimura02,Oyama16} \\
\bottomrule
\end{tabular}}
\end{table}

Table~\ref{tbl:Daejeon Correlator} represents basic specifications of the Daejeon Correlator.
Results of performance evaluation of the Daejeon Correlator can be found in the literature \cite{Lee15}.
The Daejeon Correlator has 16 data input ports, named as the antenna unit, corresponding to a single polarization (right-hand circular polarization (RHCP) or left-hand circular polarization (LHCP)) at a single frequency for one telescope.
This results in the maximum number of telescopes for data correlation at a single path being 16 for an observation with a single polarization at a single frequency, or 8 for an observation with dual polarization at a \mbox{single frequency.}

\begin{table}[H]
\caption{Basic specifications of the Daejeon Correlator.
\label{tbl:Daejeon Correlator}}
\setlength{\tabcolsep}{8.4mm}{\begin{tabular}{llcccccc}
\toprule
Maximum number of stations & 16                         \\
Maximum delay compensation & $\pm 36000$~km            \\
Maximum fringe tracking    & 1.075~kHz                  \\
Maximum data input rate    & 2048~Mbps                  \\
Maximum number of spectral points per IF channel & 8192 \\
Integration time           & 25.6~ms--10.24~s         \\
\bottomrule
\end{tabular}}
\end{table}

\section{Summary of the EAVN Open-Use Program}
\label{sec:Summary of the EAVN Open-Use Program}

As mentioned in Sections~\ref{sec:Introduction} and \ref{sec:Overview of the Array}, a domestic VLBI array is operated in each East Asian country, JVN and VERA in Japan, CVN in China, and KVN in Korea, and the open-use program is also carried out by each VLBI array.
Although each VLBI array has its own advantage in both scientific and technical point of view, it is a natural expansion to constitute a larger VLBI network by combining adjacent domestic VLBI arrays.
On the basis of scientific and technical accomplishments with KaVA and initial performance evaluation with EAVN shown in Section~\ref{sec:Introduction}, the EAVN open-use program has been started from the second half of 2018.

EAVN consists of 16 telescopes in East Asian countries, while the observation time for EAVN to be provided by each telescope time is different between each other, as shown in Table~\ref{tbl:EAVN Telescope Time}.
Proposers can choose any combination of an array configuration so that the configuration becomes a suitable one for their scientific purposes, although KaVA shall participate in all EAVN observations in principle.

\begin{table}[H]
\caption{Total observation time of EAVN provided by each telescope for the open-use program in the 2022B semester.
\label{tbl:EAVN Telescope Time}}
\setlength{\tabcolsep}{8.5mm}{\begin{tabular}{llcccccc}
\toprule
\textbf{Country} & \textbf{Array/Telescope} & \textbf{Observing Time for EAVN [h]}  \\
\midrule
China            & Kunming                  & ~~50 \\
                 & Nanshan                  &  150 \\
                 & Tianma/Sheshan           &  150 \\
Japan            & VERA                     &  500 \\
                 & Hitachi                  & ~~50 \\
                 & Nobeyama                 & ~~48 \\
                 & Takahagi                 & ~~50 \\
                 & Yamaguchi                & ~~50 \\
Korea            & KVN                      &  500 \\
                 & Sejong                   &  100 \\
\bottomrule
\end{tabular}
}
\end{table}

Table~\ref{tbl:EAVN Statistics} represents the total observing time of EAVN for each semester.
EAVN offers opportunities of a VLBI observation to astronomers all over the world from September 1 to June 15 with 2.5 months of the system maintenance, while the term of observation shown above is divided into two semesters from September 1 to January 15 next year (the `B' semester) and from January 16 to June 15 (the `A' semester).
As shown in Table~\ref{tbl:EAVN Statistics}, EAVN is providing the observing time of about 1100 hours during two adjacent semesters.
The observing session of EAVN is basically allocated every two weeks with the total observing term of one week each.
EAVN thus provides opportunities of VLBI observations with the total observing duration of two weeks per month from September to June, {while note that EAVN observations are not always allocated to whole observing term tightly since the total observing time provided by each telescope is limited, as shown in Table~\ref{tbl:EAVN Telescope Time}, and target sources tend to concentrate on a particular right ascension range.
These result in the total observing time for a year ($\sim$ 1100~h) shown in Table~\ref{tbl:EAVN Statistics} being much smaller than the total potential observing time ($\sim$ 3000~h) of EAVN.}

\begin{table}[H]
\caption{Total observing time of EAVN for each semester.
\label{tbl:EAVN Statistics}}
\tablesize{\endnotesize}

\begin{adjustwidth}{-\extralength}{0cm}
\setlength{\tabcolsep}{2.6mm}{\begin{tabular}{ccccccccc}
\toprule
\textbf{Semester} & \textbf{GOT \boldmath{$^a$} [h]} & \textbf{Session} & \textbf{ToO \boldmath{$^b$} [h]} & \textbf{Session} & \textbf{PE \boldmath{$^c$} [h]} & \textbf{Session} & \textbf{Total Time [h]} & \textbf{Total Session}  \\
\midrule
2018B             & ~~487.5              & ~~78             & ---                  & ---              & ~~32.0            & ~~2              & ~~519.5                 & ~~80 \\
2019A             & ~~439.5              & ~~66             & ~~116.0              & 16               & ~~75.0            & ~~7              & ~~630.5                 & ~~89 \\
2019B             & ~~472.0              & ~~70             & ~~~~~~0.0            & ~~0              & ~~55.0            & ~~6              & ~~527.0                 & ~~76 \\
2020A             & ~~539.5              & ~~79             & ~~~~24.0             & ~~3              & ~~63.0            & ~~6              & ~~626.5                 & ~~88 \\
2020B             & ~~327.5              & ~~58             & ~~~~44.0             & 10               & ~~71.5            & 10               & ~~443.0                 & ~~78 \\
2021A             & ~~581.0              & ~~94             & ~~~~16.0             & ~~2              & ~~26.5            & ~~5              & ~~623.5                 & 101  \\
2021B             & ~~483.5              & ~~72             & ~~~~15.5             & 10               & ~~49.0            & ~~7              & ~~548.0                 & ~~89 \\
2022A             & ~~522.0              & ~~84             & ~~~~13.0             & 11               & ~~34.0            & ~~2              & ~~569.0                 & ~~97 \\
\midrule
Total             & 3852.5               & 601              & 228.5                & 52               & 406.0             & 45               & 4481.0                  & 698  \\
\bottomrule
\end{tabular}}
\end{adjustwidth}
\noindent{\footnotesize Note. $^a$ General observing time. $^b$ Target of opportunity. $^c$ Performance evaluation.}
\end{table}

As of the 2022B semester, EAVN open-use program provides opportunities of observations at 6.7, 22, and 43~GHz with single polarization and with the data recording rate of 1~Gbps.
Dual-polarization capability is opened for the open-use program from the 2023A semester.
EAVN also provides opportunities of the dual-frequency simultaneous data recording mode at 22 and 43~GHz for 9 telescopes (KaVA, Nobeyama, and Sejong), as mentioned in Section~\ref{subsec:Frontend}.
The `multi-frequency data recording mode', on the other hand, is also offered as one of the most distinct modes of EAVN in which KVN records the data of not only 22 and 43~GHz but also 86 and 129~GHz simultaneously.
This mode thus enables us to compare the data at different frequencies directly.

From the 2019A semester, EAVN offers a director's discretionary time for target of opportunity (ToO) observations to track transient or unexpected phenomena swiftly.
As of the 2022A semester, we have conducted 52 ToO sessions with the total observing time of 228.5 hours with maser bursts associated with star-forming regions, Galactic black hole binary, and gamma-ray-emitted extragalactic objects being major targets.

Part of EAVN observations were conducted with non-EAVN telescopes in a framework of EAVN open-use program.
As of the 2022A semester, following non-EAVN telescopes have participated in EAVN observation one or more sessions; Hobart 26~m, Tidbinbilla 70~m (Australia), Effelsberg 100~m (Germany), Noto 32~m, Medicina 32~m, Sardinia 64~m (Italy), Badary 32~m, Svetloe 32~m, Zelenchukskaya 32~m (Russia), and Yebes 40~m (Spain).
These are also a good demonstration for promoting global VLBI activities, such as the EATING VLBI or the Global VLBI Alliance, both of which are explained in Section~\ref{sec:Future Growth into the Global VLBI}.

\section{Scientific Accomplishments by EAVN}
\label{sec:Scientific Accomplishments by EAVN}

Thanks to its high angular resolution at multiple frequencies and plenty of observing time of more than 1100 hours in a year, EAVN is a suitable array to conduct high-cadence and long-term VLBI monitoring toward particular targets.
To make full use of the capabilities of EAVN for deriving initial scientific results and for considering future potential science cases with EAVN, three science working groups (SWGs), AGNs, evolved stars, and star-forming regions, were organized in 2011 before launching KaVA's operation and the large observing programs led by these SWGs have been conducted using KaVA and EAVN from 2015 to 2019 by providing about 50\% of whole observing time of KaVA/EAVN.
Galactic Astrometry SWG was also organized in 2017 for promoting astrometric VLBI observations to investigate dynamics of our galaxy.
In this section, let us introduce overview of activities and scientific achievements to date led by these SWGs.

\subsection{Active Galactic Nuclei}
\label{subsec:Active Galactic Nuclei}

Key issues in AGN science are to investigate the accretion process of the matter onto supermassive black holes (SMBHs), and physical processes on the mechanism of jet formation and its collimation and acceleration in the vicinity of SMBHs.
To approach these important subjects, EAVN AGN SWG is focusing on two targets, our Galactic center Sagittarius A$^*$ which contains a SMBH with its BH mass of $\approx 4.0 \times 10^6 M_{\odot}$ (e.g., \cite{Do19,EHT22a}), and a nearby radio galaxy M87 with its BH mass of $\approx 6.5 \times 10^9 M_{\odot}$ (e.g., \cite{Gebhardt11,EHT19b}), both of which are main targets of the EHT project.

The first-epoch observation of M87 was conducted in 2013 using KaVA as a pilot experiment of the large program of KaVA and the monitoring program was continued with the observing interval of two or three weeks.
The first 10-epoch observations in 2013 and 2014 revealed superluminal motions and a trend of gradual acceleration of multiple jet components with its physical scale of 0.1--2~pc, corresponding to 140--2800 Schwarzschild radii \cite{Hada17}.
M87 has been continuously monitored through a large program of KaVA and EAVN since then and those observations revealed the kinematics of the M87 jet on the basis of a detailed velocity profile of the apparent jet speed ($v_{\rm app}$) from the vicinity of the jet base ($\approx 0.5$~mas) with $v_{\rm app} \approx 0.3c$ to $v_{\rm app} \approx 2.7c$ at $\approx 20$~mas from the jet base (\cite{Park19}, see also Figure~\ref{fig:Park_2019_ApJ}).
EAVN observations also reconstructed the fine structure of both approaching and receding jets of M87 with the image dynamic range of around 4000 at both 22 and \mbox{43~GHz \cite{Cui21}}.
EAVN observing campaign of M87 in 2017 spring was carried out as part of quasi-simultaneous multi-wavelength campaign from radio to TeV $\gamma$-ray, which was conducted concurrently with the EHT campaign.
EAVN provided clear images showing knotty jet structure \cite{EHT21}, as well as the flux information at \mbox{cm-wavelengths \cite{EHT19b}.}
Dense monitoring of M87 with five consecutive month in 2016 by KaVA at 22 and 43~GHz quasi-simultaneously could also estimate the magnetic field strength along the jet precisely at an angular scale of 2--10~mas (or 900--4500 Schwarzschild radii for M87) from the core on the basis of detailed determination of the spectral index between two observing \mbox{frequencies \cite{Ro22}}.

\begin{figure}[H]

\includegraphics[width=6 cm]{Park_2019_ApJ_Figure2-1.png}
\includegraphics[width=6 cm]{Park_2019_ApJ_Figure7-1.png}
\caption{({\bf Left}) CLEAN images of M87 obtained with KaVA at 22~GHz.
The images are obtained at eight epochs from 2016 February 26 to June 15.
Circular Gaussian components obtained by the modelfit analysis are overlaid on the images.
({\bf Right}) Apparent jet speed as a function of projected distance from the core of M87.
Symbols shown with magenta and blue colors represent the data obtained at 22 and 43~GHz, respectively.
Adapted from the work in \cite{Park19} with permission from the American Astronomical Society (AAS).
\label{fig:Park_2019_ApJ}}
\end{figure}

Another major target of the EHT project, Sgr A$^*$, is also one of the best laboratories for investigating mass accretion processes and time variability of physical properties in the vicinity of SMBH thanks to its proximity.
EAVN AGN SWG is conducting a long-term monitoring of Sgr A$^*$, including an intensive observation program during the EHT campaign every year as another target of the large program of KaVA and EAVN.
Radio emission from Sgr A$^*$ is affected by interstellar scattering effect, resulting in scatter-broadening of its size as the square of the observing wavelength.
This becomes a disadvantage of an observation at a frequency of, e.g., 22~GHz or lower.
Detection of Sgr A$^*$, on the other hand, is also difficult at 43~GHz or higher due to its lower flux density, although Sgr A$^*$ still has a rising spectrum at 43~GHz.
In this point, KaVA is a suitable array for observing Sgr A$^*$ since KaVA can provide a denser ($u$, $v$) coverage corresponding to the significant radio structure thanks to its compact array configuration with the baseline length of 300--2300~km.
Moreover, KaVA has a better angular resolution in the north--south direction at 43~GHz than that of VLBA, thus KaVA can estimate the minor axis size of Sgr A$^*$ more precisely.
On the basis of these advantages, results of precise size measurements of Sgr A$^*$ with its major-axis angular size of $704 \pm 102$~$\upmu$as and $300 \pm 25$~$\upmu$as at 22 and 43~GHz, respectively, can be obtained by KaVA and EAVN \cite{Johnson18,Cho22}.
Those results enable us to compare with the accretion flow dominated model in terms of the distribution of thermal/non-thermal electron and the viewing angle of Sgr A$^*$, both of which can be determined by a theoretical prediction.
EAVN also provided results of the flux density measurement of Sgr A$^*$ at 22 and 43~GHz through the multi-wavelength observation campaign from radio to X-ray, which was conducted concurrently with the EHT campaign in 2017 \cite{EHT22b}.

KaVA/EAVN is participating in an international multi-frequency observing campaign of AGNs besides the EHT campaign mentioned above.
Multi-frequency monitoring of a gravitationally lensed blazar B0218+357, for example, was performed during 2016 and 2020 from radio to GeV $\gamma$-ray and KaVA provided clear images and flux density information at 22 and 43~GHz for the monitoring, in which two lensed images show clear core-jet structure although a distinct jet motion cannot be seen \cite{Hada20,Acciari22}.

KaVA/EAVN is carrying out individual proposal-based observations toward various AGNs as well.
A series of KaVA observations of a nearby bright radio galaxy 3C~84 have revealed the existence and its structure of a circumnuclear plasma disk \cite{Wajima20} and strong jet--cloud interaction on pc-scales \cite{Kino18,Kino21}.
Short- and long-term monitoring observations with KaVA/EAVN show new findings in physical properties of the jet structure and its motion toward several AGNs, e.g., confirming a clear connection between $\gamma$-ray flare and the ejection of a new jet component in the flat spectrum radio quasar 4C+21.35 at 22 and 43~GHz \cite{Lee19}, determining the rebrightened regions in the jet of a nearby radio galaxy NGC~315 at 22~GHz, which is similar to M87 \cite{Park21}, detecting a misaligned jet component in a transient GeV $\gamma$-ray blazar J1544$-$0649 with its maximum viewing angle of 7.4$^{\circ}$ at 6.7~GHz suggesting the misaligned blazar scenario for this source \cite{Shao22}, and finding a tight linear relation between accretion luminosity and jet luminosity in a sample of the {\it Swift} BAT (Burst Alert Telescope)-detected local AGNs with their redshift of smaller than \mbox{0.05 \cite{Baek19}}.
It should also be notable that EAVN is conducting observations toward extragalactic radio sources which are non-traditional VLBI targets, such as a cluster galaxy \cite{Baek22} and a gamma-ray burst object \cite{An20}, thanks to an excellent imaging sensitivity of EAVN although the gamma-ray burst object 190114C could not be detected with EAVN, maybe due to rapid decay of the radio flux.

\subsection{Evolved Stars}
\label{subsec:Evolved Stars}

Evolved stars tend to show strong maser emission of the hydroxyl radical (OH), water vapor (H$_2$O), and silicon monoxide (SiO) at the circumstellar envelope in the asymptotic giant branch (AGB) and post-AGB phases.
Those masers are associated with gas and dust clumps around an evolved star and, thus, a useful tool to reveal the mass loss processes of evolved stars, although its motion is very complex.
To conduct high-cadence VLBI monitoring of a sample of evolved stars for approaching those issues, EAVN Evolved Stars SWG has launched the `ESTEMA' (Expanded Study on Stellar Masers) project using KaVA \cite{Oyadomari16} and the `(renewed) ESTEMA' (EAVN Synthesis of Stellar Maser Animations) project using EAVN.
The most distinguishing strategy of ESTEMA for approaching various scientific objects is to conduct (quasi-)simultaneous observation at 22, 43, 86, and 129~GHz, corresponding to maser emission H$_2$O maser at 22~GHz, and SiO $J$ = 1--0, 2--1, and 3--2 maser at 43, 86, and 129~GHz, respectively, thanks to a unique capability of multi-frequency simultaneous data reception at KaVA, Sejong, and Nobeyama.

ESTEMA aims to produce animations of circumstellar H$_2$O and SiO masers toward 10 variable stars by dense monitoring during its pulsation period ($P$) of 1--3 years to investigate three-dimensional kinematics of maser gas clumps, while they are focusing on two objects, a Mira variable BX Cam ($P = 486$~days) and a red supergiant NML Cyg ($P \sim 1000$~days), as a first step.
Prior to launch of ESTEMA, pilot observations of several evolved stars showing distinct maser features at different maser species were conducted using KaVA.
For one of those samples, an OH/IR star WX Psc, single-epoch KaVA observation could reconstruct superposed images of the $v = 1$ and 2, $J$ = 1--0 SiO masers with keeping its relative position by employing astrometric analysis.
Those images clearly show a typical ring-like structure in both SiO masers and the difference in their distribution with $v = 2$ masers being located in an inner region of about 0.5~mas compared to $v = 1$ masers (\cite{Yun16}, see also Figure~\ref{fig:Yun_2016_ApJ}).
As for one of the major targets of ESTEMA, BX Cam, long-term monitoring with EAVN from 2018 May to 2021 June, including 37 epochs clearly described three-dimensional kinematics of H$_2$O masers associated with the circumstellar envelope with providing the animation of H$_2$O masers.
These results help us to understand the mechanism of the propagation of shock waves around evolved stars \cite{Xu22}.

Long-term monitoring of those masers will be a good tool for revealing the physical environments of the circumstellar environment and the pumping mechanism of SiO maser.
Simultaneous observations of H$_2$O and SiO masers at four frequencies (22, 43, 86, and 129~GHz) toward several evolved stars, which are not included in the target of ESTEMA, have also conducted using KVN, with EAVN Evolved Stars SWG being collaborated \mbox{(e.g., \cite{Yoon18,Kim19,Yang20}).}

\begin{figure}[H]

\includegraphics[width=6.7 cm]{Yun_2016_ApJ_Figure3.png}
\includegraphics[width=6.8 cm]{Yun_2016_ApJ_Figure6.png}
\caption{({\bf Left}) Spatial distribution of the SiO masers around WX Psc on 2012 April 1.
Blue and red colors represent the $v = 1$ and 2, $J$ = 1--0 SiO maser.
({\bf Right}) Superposed map of SiO masers for $v = 1$ and 2, $J$ = 1--0 in blue and red colors, respectively.
Dashed circles show the average size of the ring-like structure for each SiO maser spot.
Adapted from the work in \cite{Yun16} with permission from AAS.
\label{fig:Yun_2016_ApJ}}
\end{figure}

Some of evolved stars in AGB or post-AGB phases are identified as showing fast bipolar outflows traced by H$_2$O masers, called water fountain sources (e.g., \cite{Imai02}).
EAVN Evolved Stars SWG is carrying out follow-up KaVA observations of a sample of ESTEMA targets in which high-velocity components of H$_2$O masers are detected by Nobeyama 45~m telescope in order to confirm the spatial distribution of H$_2$O masers.
They found that H$_2$O masers in IRAS~18286$-$0959, one of the ESTEMA targets, show a symmetric spatial distribution with extremely high expansion velocities of greater than 200~km~s$^{-1}$, suggesting that H$_2$O masers are associated with the bipolar outflow \cite{Imai20}.

\subsection{Star-Forming Regions}
\label{subsec:Star-Forming Regions}

To reveal the process of massive star formation with its mass of greater than 8$M_{\odot}$ is an important issue for understanding basic astrophysics, such as formation of heavy elements and galaxy formation, while it is still poorly understood mainly because of large distance from us and relatively short evolutionary timescale.
Large number of high-mass young stellar objects (HMYSOs) are known to associate strong emission of class I and II methanol (CH$_3$OH) masers at 44 and 6.7~GHz, respectively, and water vapor (H$_2$O) maser at 22~GHz.
Those masers are associated with various scales of structures in HMYSOs, such as outflows, disks, and H\,II regions, VLBI is thus one of the best tools for investigating the process related to high-mass star formation since VLBI can directly obtain images of HMYSOs and trace three-dimensional motions of masers.

EAVN Star-Forming Regions SWG has started large program for long-term monitoring of H$_2$O masers at 22~GHz and class I CH$_3$OH masers at 44~GHz for a sample of HMYSOs containing 25 primary candidates \cite{Kim18}.
The project was conducted mainly using KaVA since target masers tend to resolve with longer baseline lengths by EAVN than that by KaVA, instead the project contains follow-up observations with JVN, VERA, JVLA (Karl G.\ Jansky Very Large Array), and ALMA (Atacama Large Millimeter/submillimeter Array).
Prior to launch of EAVN, imaging test observations of EAVN (VERA + JVN + Sheshan) at 6.7~GHz had been conducted toward 36 HMYSOs which emit class II CH$_3$OH masers in 2010 and 2011.
These observations provide us a basic information on maser distribution and its morphology (elliptical, arched, linear, paired, and complex) for a sample of \mbox{HMYSOs \cite{Fujisawa14,Sugiyama16}.}
It is also notable that a KaVA observation of a high-mass star-forming region IRAS~18151$-$1208 detected class I CH$_3$OH methanol masers with the baseline lengths of shorter than 650~km, suggesting that the maser component has an extended structure with its angular size of larger than 4~mas or $\sim$12~AU in the linear size of the source \cite{Matsumoto14}.
This is the first detection of class I CH$_3$OH maser at 44~GHz with VLBI, indicating that KaVA is a powerful instrument to study physical properties of HMYSOs.

Another good example for studying the process of high-mass star formation with KaVA and ALMA was demonstrated toward a high-mass cluster-forming region G25.82$-$0.17, detecting continuum emission showing a velocity gradient indicating a rotating disk by ALMA at 230~GHz and strong H$_2$O maser sources associated with the root of bipolar outflows in the continuum source by KaVA at 22~GHz.
These results suggest a similar star-formation process between low-mass and high-mass stars (\cite{Kim20}, see also Figure~\ref{fig:Kim_2020_ApJ}).
KaVA also provides precise measurements of proper motion of H$_2$O masers associated with bipolar outflows toward several HMYSOs and high-mass star-forming regions \mbox{(e.g., \cite{Chibueze21,Trinidad21})} thanks to a capability of dense monitoring by KaVA.
These results are of help to us for understanding basic physical processes of HMYSOs.

\begin{figure}[H]
\includegraphics[width=10 cm]{Kim_2020_ApJ_Figure7.png}
\caption{Spatial distribution of H$_2$O masers obtained with KaVA, which are shown in colored points.
Blue and red contours indicate the integrated intensity map of the SiO 5--4 line and and gray scale represents the continuum emission at 230~GHz, both of which were obtained with ALMA Band 6.
Adapted from the work in \cite{Kim20} with permission from AAS.
\label{fig:Kim_2020_ApJ}}
\end{figure}

\subsection{Astrometry}
\label{subsec:Astrometry}

Precise astrometric measurement for detecting parallax is one of the most distinct features in VLBI thanks to its high angular resolution \cite{Reid14}.
In East Asia, various studies on measurement of distance to Galactic H$_2$O and SiO maser sources, and the three-dimensional structure and dynamics of the Milky Way have been accomplished (\cite{VERA20} and references therein) based on astrometric measurements with VERA, which is a dedicated VLBI array for Galactic astrometry with the unique capability of the dual-beam system \cite{Honma03}.
On the basis of accomplishments made mainly by VERA, EAVN Galactic Astrometry SWG examined the capability of astrometric measurements and EAVN opened the astrometry mode for measuring parallax using KaVA 7 telescopes for the open-use program in the 2019B semester.
Station coordinates of KaVA have been monitored by 22-GHz geodetic VLBI observations since 2014 and individual baseline lengths are determined with an accuracy of $\sim$3~mm \cite{Jike18,Xu21}.
For atmospheric calibration of KaVA astrometry mode (i.e., estimation of zenith wet excess path delays), the data provided by GPS and JMA (Japan Meteorological Agency meso-scale analysis data for numerical weather prediction\endnote{\url{https://www.jma.go.jp/jma/jma-eng/jma-center/nwp/outline2019-nwp/index.htm}, accessed on 1 December 2022}) are applied.
Those examinations result in suppressing the tropospheric zenith delay residual ($c\Delta \tau_{\rm{trop}}$) of less than $\sim$2~cm \cite{Nagayama15}.

To demonstrate the capability of the astrometry mode, Galactic trigonometric parallax measurement of 22~GHz H$_2$O maser sources associated with a famous star-forming region W3(OH) was conducted with KaVA.
The resultant parallax is measured to be \mbox{$0.460 \pm 0.035$~mas}, which is consistent with a result of $0.489 \pm 0.017$~mas measured by VLBA \cite{Hachisuka06} within the margin of error (see Figure~\ref{fig:EAVN_Parallax}).
More than 10 proposals with the total observing time of greater than 300 hours have already been accepted for astrometric study with KaVA, which covers a wide range of scientific topics including studies of the structure of extreme outer Galaxy \cite{Sakai22}, microquasars, jet swinging in AGN, astrometry of radio stars, and geodetic VLBI observations with simultaneous data reception at 22 and 43~GHz.

\begin{figure}[H]
\includegraphics[width=10 cm]{EAVN_Parallax.png}
\caption{Results of parallax measurement and proper-motion fitting for a star-forming region W3(OH). The position offsets of W3(OH) are plotted with respect to the background quasar J0244+6228 in the east ($\alpha$cos$\delta$) and north ($\delta$) directions as a function of time. For clarity, the north direction data is plotted offset from the east direction data.
({\bf Left}) The best-fit models in the east and north directions are shown as continuous and dashed curves, respectively. ({\bf Right}) Same as the left panel, but the component of proper motion is removed.
\label{fig:EAVN_Parallax}}
\end{figure}

\section{Future Growth into the Global VLBI}
\label{sec:Future Growth into the Global VLBI}

As mentioned in Section~\ref{sec:Introduction}, higher angular resolution can be obtained by employing longer baseline length between each telescope.
It is also important to expand the array capability of EAVN by, for example, inviting telescopes and existing VLBI arrays located near and far from EAVN.
International collaboration in VLBI is thus a natural extension to obtain better array capability and we enhance international collaboration in VLBI research with non-EAVN facilities as shown below as examples.

\subsection{Collaboration with Southeast Asian Countries}
\label{subsec:Collaboration with Southeast Asian Countries}

Radio telescope facilities and the radio astronomy community are spreading not only in East Asia but also in Southeast Asia.
In Thailand, construction of 40 m radio telescope (Thai National Radio Telescope; TNRT) has been completed in Chiang Mai led by National Astronomical Research Institute of Thailand (NARIT) and will be operational at 1.0--1.8 and 18.0--26.5~GHz in 2022, while an observable frequency range will be expanded to be 300~MHz--115~GHz in the future \cite{Jaroenjittichai18}.
Key science topics to be achieved with TNRT are summarized in the white paper \cite{Jaroenjittichai22}.
Two new radio telescopes with {their} diameter of 13~m are also under construction in Chiang Mai and Songkhla, both of which conform to the specifications of the VLBI Global Observing System (VGOS).
For another 32 m telecommunication antenna at the campus of CAT Telecom Public Company Limited in Chonburi, the conversion into a radio telescope is also being considered.
These telescopes will constitute the Thai VLBI Network (TVN) with the longest baseline length of 1330~km.
Indonesia plans to convert a 32 m telecommunication antenna into radio telescope.
A new 7 m radio telescope is operated by the Universiti Pendidikan Sultan Idris (UPSI)--Universiti Malaya (UM) Radio Astronomical Observatory in Malaysia.
These are potential telescopes of EAVN for developing array capabilities thanks to its unique location.

For future development in radio astronomy and VLBI in Southeast Asian countries and for close collaboration in these fields between EAVN and those countries, a new memorandum of understanding (MoU) for EAVN has been concluded on 2021 October 1 by inviting NARIT, as well as Yunnan Observatories (YNAO) in China, and National Geographic Information Institute (NGII) in Korea, as a new member institute of EAVN.
This MoU is a renewal of existing one which had been concluded on 2018 September 6 between KASI, NAOJ, Shanghai Astronomical Observatory (SHAO), and Xinjiang Astronomical Observatory (XAO), and will accelerate further practical collaboration in wide fields of VLBI sciences in Asian region.

\subsection{EATING VLBI}
To further connect EAVN to global baselines, let us introduce an example of a practical collaborative VLBI project entitled `East Asia To Italy: Nearly Global VLBI' (EATING VLBI).
Project overview and initial scientific results of EATING VLBI is provided in another review paper in this Special Issue.

EATING VLBI was launched as a trilateral collaborative project between Italy, Japan, and Korea in 2012 and became a regular session of KVN open-use program in 2020.
Current EATING VLBI consists of three Italian telescopes, Medicina 32~m, Noto 32~m, and Sardinia 64~m, and EAVN telescopes shown in Table~\ref{tbl:EAVN-List}, while it operates with the observing frequency of 22~GHz which is a common one for all Italian telescopes and many EAVN telescopes.
The maximum baseline length of EATING VLBI is composed of Sardinia and VERA-Ogasawara stations with its baseline length of 11164~km, corresponding to an angular resolution of 0.25~mas at 22~GHz.
Although a big geographical gap in a ($u$, $v$) plane appears for the original trilateral EATING VLBI, better image sensitivity and ($u$, $v$) coverage can be obtained for renewed EATING VLBI thanks to a big telescope and a unique location in China, such as Tianma 65~m and Nanshan 26~m, respectively.

As of the first half of 2022, EAVN has conducted EATING VLBI observations with the number of sessions of 37 and with the total observing time of 275 hours since the launch of EAVN open-use program in 2018.
About 49\% (135 hours) of those observations involved any of Italian telescopes so that they can secure the common sky coverage with EAVN.
It should also be noted that part of the EATING VLBI sessions were conducted in conjunction with the Quasar network (Badary 32~m, Svetloe 32~m, and Zelenchukskaya 32~m) in Russia \cite{Shuygina19}.
Major targets of EATING VLBI conducted to date are M87 and the nearest gamma-ray emitting narrow-line Seyfert 1 (NLS1) galaxy 1H~0323+342.
It is notable that a series of EATING VLBI observations could provide images with the highest angular resolution to date toward 1H~0323+342 compared to previous studies with VLBI (e.g., \cite{Wajima14,Fuhrmann16,Doi18,Hada18}), which enable us to investigate a gamma-ray emission mechanism of NLS1.
Imaging capability and initial scientific results of these targets are shown in another review paper of this Special Issue.

Three Italian telescopes are planning installation of a new compact triple-band receiver (CTR) \cite{Han17}, in which simultaneous reception of radio signal at 22, 43, and 86~GHz is available.
Design of the quasi-optics and assembly of CTR is carried out at KASI and installation to each telescope will be conducted in 2023.

\subsection{Global VLBI Alliance}

The open-use program is operated by a lot of domestic and international VLBI arrays besides EAVN, such as EVN, LBA, and VLBA, as mentioned in Section~\ref{sec:Introduction}.
It is thus a natural extension of VLBI array capability by integrating these arrays into a single VLBI array to obtain 100~$\mu$as-scale angular resolution at cm- to mm-wavelengths.
This motivates us to set up an idea of the Global VLBI Alliance (GVA)\endnote{See also the following site for more details of GVA: \url{http://gvlbi.evlbi.org/}, accessed on 1 December 2022} \cite{Colomer21}.
GVA aims not only providing an opportunity of obtaining access to the global VLBI array but also sharing various knowledge related to VLBI, such as scientific strategies, technical developments between each VLBI array, and discussion on observational campaigns using GVA.
The official working group for GVA has already been established under the commission B4 (radio astronomy) of the International Astronomical Union in 2020\endnote{\url{https://www.iau.org/science/scientific_bodies/working_groups/324/}, accessed on 1 December 2022} and started practical discussion with four VLBI arrays shown above (EAVN, EVN, LBA, and VLBA) being currently a regular member \mbox{of GVA}.

\section{Conclusions}
\label{sec:Conclusions}

The paper describes overview of the observing system of the East Asian VLBI Network (EAVN) and brief summary of scientific accomplishments to date with EAVN.
EAVN is currently operated using 16 radio telescopes and three correlators located in China, Japan, and Korea, with the longest baseline length of 5078~km, corresponding to the highest angular resolution of 1.82, 0.55, and 0.28~mas at 6.7, 22, and 43~GHz, respectively.
EAVN is offering a total observing time of about 1100 hours in a year for the open-use program and occasional observations using the director's discretionary time to astronomers all over the world.
Although EAVN is operated with limited number of observing frequencies, EAVN provides opportunities of VLBI observations with dual-frequency data receiving system at 22 and 43~GHz, which is one of the most unique capabilities of EAVN, enabling us to obtain better baseline sensitivity and to determine a relative source position by employing the frequency phase transfer technique and the source-frequency phase-referencing technique, respectively.
EAVN conducts VLBI observations toward various Galactic and extragalactic radio sources, while EAVN provides observing opportunities to three major scientific objectives, active galactic nucleus, evolved star, and star-forming region, through the large program of KaVA/EAVN.
EAVN will become one of the most important VLBI facilities for future global VLBI thanks to its unique location and unique capability of multi-frequency simultaneous data receiving system.

\vspace{6pt}

\authorcontributions{{The corresponding} author (K.W.) wrote all the manuscript.
Each author contributes to EAVN operation and scientific activities as shown below:
EAVN director (M.H., K.-T.K., Z.-Q.S., N.W.), EAVN AGN Science Working Group (K.A. (Kazunori Akiyama), J.-C.A., T.A., K.A. (Keiichi Asada), Z.C., X.C., I.C., Y.C., A.D., J.D., W.G. (Wei Gou), W.G. (Wen Guo), K.H., Y.H., J.A.H., Y.J. (Yongbin Jiang), Y.J. (Yongchen Jiang), N.K., M.K., S.K., J.-W.L., J.A.L., S.-S.L., B.L., X.L. (Xiaofei Li), R.-S.L., M.N., K.N., J.O., T.O., J.P., H.R., S.S.-S., B.W.S., Y.S., M.T., F.T., S.T., J.W., X.W., W.Y., K.Y., L.Y., Y.Z., G.-Y.Z., R.Z., W.Z.), EAVN Evolved Stars Science Working Group (J.O.C., S.-H.C., H.I., D.-J.K., J.K., Y.Y. (Youngjoo Yun)), EAVN Star-Forming Regions Science Working Group (K.A. (Kitiyanee Asanok), D.-Y.B., T.H., K.S.), EAVN Galactic Astrometry Science Working Group (T.J. (Taehyun Jung), S.-W.K., C.O., N.S., S.X., B.Z.), management and operation of the Korea-Japan Correlation Center (D.-K.J., H.-R.K., S.-J.O., D.-G.R., J.-H.Y.), EAVN site operation and management (W.C., H.-S.C., L.C., K.F., W.J., T.J. (Takaaki Jike), J.-S.K., H.K., S.W.L., G.L., Z.L., Q.L., X.L. (Xiang Liu), K.M., H.O., K.M.S., Y.T., S.W., B.X., H.Y. (Hao Yan), S.-O.Y., Y.Y. (Yoshinori Yonekura), H.Y. (Hasu Yoon), J.Y., H.Z.), collaboration between EAVN and Southeast Asia (T.C., P.J., B.H.K., S.P., W.R., B.S.), overall coordination of EAVN (K.W.). All authors have read and agreed to the published version of the manuscript.
}

\funding{
This work is funded by following: JSPS (Japan Society for the Promotion of Science) Grant-in Aid for Scientific Research (KAKENHI) (S) 18H05222 (T.H.), (A) 16H02167 (H.I.), 18H03721 (K.N.), 21H04524 (H.I.), 22H00157 (K.H.), (B) 18KK0090 (K.H.), 21H01120 (Y.Y.\ (Yoshinori Yonekura)), (C) 17K05398 (T.H.), 19K03921 (K.S.), 21K03628 (S.S-S.),
JSPS Grant-in-Aid for Scientific Research on Innovative Areas (Research in a proposed research area) 21H00032 (Y.Y.\ (Yoshinori Yonekura)), 21H00047 (H.I.),
JSPS Grant-in-Aid for Transformative Research Areas (A) 20H05845 (T.H.),
the Grant of PIIF Heiwa Nakajima Foundation in 2019 (K.S.),
and the Mitsubishi Foundation 201911019 (K.H.).
K.A.\ (Kazunori Akiyama) is financially supported by grants from the National Science Foundation (AST-1935980, AST-2034306, AST-2107681, AST-2132700,  OMA-2029670).
L.C.\ is supported by the Chinese Academy of Sciences (CAS) 'Light of West China' Program (No.\ 2021-XBQNXZ-005) and the National Science Foundation of China (NSFC; No.\ U2031212 and 61931002).
W.C.\ is supported by NSFC (No.\ 11903079).
Z.C.\ is supported by NSFC (No.\ U1931135).
W.J.\ is supported by NSFC (No.\ 12173074).
R.-S.L.\ is supported by the Max Planck Partner Group of the MPG and the CAS, the Key Program of the NSFC (No.\ 11933007), the Key Research Program of Frontier Sciences, CAS (No.\ ZDBS-LY-SLH011), and the Shanghai Pilot Program for Basic Research - CAS, Shanghai Branch (No.\ JCYJ-SHFY-2022-013).
S.T.\ acknowledges financial support from the National Research Foundation of Korea (NRF) through grant no.\ 2022R1F1A1075115.
B.Z.\ is supported by the NSFC (No.\ U1831136 and U2031212) and Shanghai Astronomical Observatory (N-2020-06-09-005).
}

\dataavailability{
All observing data obtained by EAVN (including KaVA), except the data in the term of right of occupation by a principal investigator, are archived via the following website. \\
\url{https://radio.kasi.re.kr/kvn_arch/kvn_search.php}
}

\acknowledgments{
This work is made use of the East Asian VLBI Network (EAVN), which is operated under cooperative agreement by National Astronomical Observatory of Japan (NAOJ), Korea Astronomy and Space Science Institute (KASI), Shanghai Astronomical Observatory (SHAO), Xinjiang Astronomical Observatory (XAO), Yunnan Observatories (YNAO), National Geographic Information Institute (NGII), and National Astronomical Research Institute of Thailand (Public Organization) (NARIT), with the operational support by Ibaraki University, Yamaguchi University, and Kagoshima University.
Operation of Hitachi 32~m, Takahagi 32~m, and Yamaguchi 32~m telescopes is partially supported by the inter-university collaborative project `Japanese VLBI Network (JVN)' of NAOJ.}

\conflictsofinterest{The authors declare no conflicts of interest.}

\abbreviations{Abbreviations}{
The following abbreviations are used in this manuscript:\\

\noindent
\begin{tabular}{@{}ll}
AGB         & Asymptotic Giant Branch \\
AGN         & Active Galactic Nucleus \\
CTR         & Compact Triple-Band Receiver \\
CVN         & Chinese VLBI Network \\
DAS         & Data Acquisition System \\
DBBC        & Digital Base Band Converter \\
DSP         & Digital Signal Processing \\
EACOA       & East Asian Core Observatories Association \\
EAMA        & East Asian Meeting on Astronomy \\
EATING VLBI & East Asia To Italy: Nearly Global VLBI \\
EAVN        & East Asian VLBI Network \\
EHT         & Event Horizon Telescope \\
EOP         & Earth Orientation Paraeter \\
ESTEMA      & Expanded Study on Stellar Masers / EAVN Synthesis of Stellar Maser Animations \\
EVN         & European VLBI Network \\
FPT         & Frequency Phase Transfer \\
GMVA        & Global Millimeter-VLBI Array \\
\end{tabular}}

{\noindent \small
\begin{tabular}{@{}ll}
GVA         & \hspace{10mm} Global VLBI Alliance \\
HINOTORI    & \hspace{10mm} Hybrid Installation Project in Nobeyama, Triple-Band Oriented \\
HMYSO       & \hspace{10mm} High-Mass Young Stellar Object \\
ICRF        & \hspace{10mm} International Celestial Reference Frame \\
ITRF        & \hspace{10mm} International Terrestrial Reference Frame \\
J-Net       & \hspace{10mm} Japanese VLBI Network \\
JVN         & \hspace{10mm} Japanese VLBI Network \\
KaVA        & \hspace{10mm} KVN and VERA Array \\
KJCC        & \hspace{10mm} Korea-Japan Correlation Center \\
KNIFE       & \hspace{10mm} Kashima--Nobeyama Interferometer \\
KVN         & \hspace{10mm} Korean VLBI Network \\
LBA         & \hspace{10mm} Long Baseline Array \\
LHCP        & \hspace{10mm} Left-Hand Circular Polarization \\
RHCP        & \hspace{10mm} Right-Hand Circular Polarization \\
SEFD        & \hspace{10mm} System Equivalent Flux Density \\
SFPR        & \hspace{10mm} Source-Frequency Phase-Referencing \\
SMBH        & \hspace{10mm} Supermassive Black Hole \\
TDRSS       & \hspace{10mm} Tracking and Data Relay Satellite System \\
TNRT        & \hspace{10mm} Thai National Radio Telescope \\
ToO         & \hspace{10mm} Target of Opportunity \\
TRAO        & \hspace{10mm} Taeduk Radio Astronomy Observatory \\
TVN         & \hspace{10mm} Thai VLBI Network \\
VERA        & \hspace{10mm} VLBI Exploration of Radio Astrometry \\
VGOS        & \hspace{10mm} VLBI Global Observing System \\
VLBA        & \hspace{10mm} Very Long Baseline Array \\
VLBI        & \hspace{10mm} Very Long Baseline Interferometry \\
VSOP        & \hspace{10mm} VLBI Space Observatory Programme
\end{tabular}}

\begin{adjustwidth}{-\extralength}{0cm}
\printendnotes[custom]
\reftitle{References}

redpajama_set_name: RedPajamaArXiv


text:
Q: Microsoft 365. SMTP. Возможно ли использовать PAT? Мы используем smtp.office365.com для отправки писем. Мы делаем следуеще:
  var smtp = new SmtpClient("smtp.office365.com", smtpServerPort);
  smtp.DeliveryMethod = SmtpDeliveryMethod.Network;
  smtp.Credentials = new NetworkCredential(smtpServerUsername, smtpServerPassword);
  smtp.EnableSsl = smtpServerSSL;

Возможно ли как то использовать не smtpServerUsername и smtpServerPassword, а например как в Azure DevOps Service использовать PAT?

redpajama_set_name: RedPajamaStackExchange


BGA glider data sheet Index Page 5 AC4c Page 6 AC5t (Not BGA approved) (Partial data only) Page 102 Jantar Std 3 (SZD48) (Partial data only) Page 103 Janus A Page 104 Janus B Page 130 Libelle Standard (201) Page 131 Libelle Std (201B) Page 132 Libelle 301& 301B Page 133 Lo100 The SZD41 Jantar Standard was a Standard Class glider designed and produced in Poland from 1973.
Download scientific diagram Layout of sailplane SZD 483 Jantar Std. 3 from publication: Flight Testing of DBD Plasma Separation Control SystemThe SZD48 Jantar Standard 2 is a Standard Class glider that was designed and produced in The manually retractable main undercarriage is composed of a single 350 x 135mm diameter wheel Duo Flight Manual Complete. pdf 1278k 20 de nov de 2014 04: 13 por Fbio Luis Visualizar Download: Manual de vo Planador Jantar Standard 2 Manual de vo Planador Jantar Standard 3 Parte 22 Media in category" Cockpits of gliders" The following 51 files are in this category, out of 51 total.
Amazing feel of flight due to the advanced flight dynamics model. Jantar Standard 3: Libelle: RolladenSchneider LS 4: Multiplayer. The most recent version of the Condor manual is available for download here: Manual. pdf. Tips CondorTips by Paul Remde. New Virtualsoaring. eu red skins for Club Class Plane Pack (PP2) are ready for you for download and 1click install.
Skins for ASG29, ASW15, ASW19, Jantar Standard 3, Libelle and LS4. " Nov lak" pre Plane Pack 2 (klubovky) formou intalku repaintov vo" firemnch" farbch Virtualsoaring. eu. Download as PDF, TXT or read online from Scribd. Flag for inappropriate content This document Temporary Revision to Rev 18 of the DA202 Flight Manual Maximum Cylinder Head Temperature Temporary Revision to Rev 6 of the DA Flight Manual Maximum Cylinder Head Temperature Documents Similar To Publication list for Access to all folders is public, however some documents are only available for downloading to registered Geelong GC members.
Please contact GGC Webmaster if you have a query with regard to any document stored on the website. All GGC documents are copyrighted (unless stated otherwise). The SZD48 Jantar Standard 2 is a Standard Class glider that was designed and produced in Poland starting in 1977. Tweet Download PDF See full screen Report a web site issue Report a Flight Crew Operating Manual A318A319A320A321 FMGS Pilot's Guide Vol 4 Print; A319A320A321 Flight Crew Training Manual Vol1 Airbus A FCOM Flight Operations vol 3 back to top Login.
Username. Password. Remember me Forgot SZD 481 Jantar Standard 2 flight manual. Powered by Phoca Download. About GGC Documents Repository. Access to all folders is public, however some documents are only available for downloading to registered Geelong GC members. Please contact GGC Webmaster if you have a query with regard to any document stored on the website.


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Q: Java 7 on Mac OS X 10.6.8 I've tried everything but I cannot get java 7 on mac os x 10.6.8.
This one didn't work either:
How to install java jdk 7 on Snow Leopard
The file in the Java folder is called 1.7 but it is in fact 1.6.
What's the best way to install Java 7 on my OS?


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Frauenhofen ist ein Ortsteil des Marktes Markt Indersdorf und eine Gemarkung im oberbayerischen Landkreis Dachau.

Geographie
Der Weiler Frauenhofen liegt circa zwei Kilometer südlich von Indersdorf und ist über die Staatsstraße 2050 zu erreichen. Die Gemarkung Frauenhofen liegt mit ihrem Gemarkungsteil 0 in Markt Indersdorf und mit Gemarkungsteil 1 in Weichs.

Geschichte
Der Ort wurde 1260 als "Laushoven" erstmals erwähnt. 1374 ist er als "Frawenhoffen de Babaria" bezeugt. 1429 wird er als "Fraunhoven" überliefert.

Im Zuge der Gebietsreform in Bayern wurde die mit dem Gemeindeedikt von 1818 begründete Gemeinde Frauenhofen aufgelöst und zum 1. April 1971 von deren 130 Einwohnern die insgesamt 90 Einwohner der Gemeindeteile Frauenhofen, Häusern und Straßbach in den Markt Markt Indersdorf und die 40 Einwohner der Gemeindeteile Breitenwiesen, Daxberg und Zillhofen in die Gemeinde Weichs eingegliedert.

Weblinks

 Gemeinde Markt Indersdorf

Einzelnachweise

Ort im Landkreis Dachau
Weiler in Oberbayern
Ehemalige Gemeinde (Landkreis Dachau)
Gemeindeauflösung 1971
Ersterwähnung 1260
Geographie (Markt Indersdorf)
Gemarkung in Oberbayern


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Where memory detains itself
The punitive expedition of Decimus Junius Brutus to the Hispanias arrived to the southern bank of river Lima in the summer of 135 b.C.. The weather would be unusually warm. And the soldiers profoundly weary. There was a rumour among the legion: that river was the river of oblivion – the one who would cross it would lose remembrance of all things lived and learned. The Lethes river.
S. would say: whenever I think of forgetting what I want and what I need to forget, the retainment of what I want to forget grows bigger and becomes stronger. Slowly, my memory turns into a patchwork of recollections over recollections of oblivion attempts. It is as if even more sand would run in my veins, draining them of blood. And the memory of remembrance defeats the science of forgetfulness.
All the legion of Decimus Junius Brutus refused to cross the river. Nobody wanted to forget. At the general's command, not a single soldier moved forward. Some went back. Brutus then had the troops observe what he would set himself to do. He crossed the river and from the other bank he called his men by their names, one by one.
In the summer of 2006, N. destroyed 5000 hours of video tape where, for six years, he had recorded the time of the places he lived in or went through. I want to document the history of my time, and memory is the only way of going back - he wrote, as he began his vast collection. By having disposed of everything he recorded, N. dived into Lethes. He anticipated the moment when everything is forgotten, when the memory is erased in the world disintegration.
At the slow instant in which Decimus Junius Brutus let himself be bathed by the Lethes water, as he started his crossing of the river, he thought: what does await me on the other side of memory?
Auggie Wren is the owner of a tobacco shop in New York. Everyday at 7 a.m. sharp he photographs the corner of 7th Ave. and 3rd St.. We are inside Smoke, the film by Wayne Wang. Throughout dozens of years, Auggie filed and catalogued more than 4000 photographs of that very place, filled with thousands of people on the move. When he shows his collection of images to Paul Benjamin, the latter glances through it in a fast, almost automatic motion. Auggie says: you'll never get it if you don't slow down, my friend.