Program - Astronomy Development in Vietnam: Challenges and Opportunities

SCIENCE PROGRAM - July 31 to Aug 2, 2016

SUNDAY - July 31, 2016

Time	Duration	Session	Speaker	Title/Abstract
8:45	15		Jean Tran Thanh Van Rencontres du Vietnam	Opening Welcome
Chair: Paul Ho
9:00	60	Science	Masa Hayashi masa.hayashi@nao.ac.jp NAOJ	The History and an Overview of NAOJ (National Astronomical Observatory of Japan) I will present the history of NAOJ together with an overview of its current system. Tokyo Astronomical Observatory (TAO), the previous form of NAOJ, was established as part of the University of Tokyo in 1888. It started modern astronomy (astrophysics) in the late 1950's by inaugurating Norikura Corona Observatory and Okayama Astrophysical Observatory, followed by Kiso Observatory equipped with a Schmidt telescope. The inauguration of Nobeyama Radio Observatory in 1982 was an important milestone for TAO in the sense that TAO's projects became "big science" and a competitive open-use style of operations was first employed. In 1988, TAO and two other institutes were merged into NAOJ, forming an Inter-University Research Institute under direct jurisdiction of the Japanese government. This has so far been the biggest change that made Japanese ground based astronomy grow. Since then, NAOJ has been involved in Subaru, ALMA and TMT, changing the governance style from that of a university to a project-oriented organization. I will discuss a possible future way of Japanese astronomy.
10:00	50	Instrument	Nobuo Arimoto arimoto@naoj.org Subaru Telescope, NAOJ	Subaru Strategy for 2020's, Science Results and Cooperation Plan with Vietnam Recent scientific results of Subaru Telescope will be presented. The strategic plan of Subaru in the era of 2020's will also be introduced. Subaru has decided to invest a large number of nights in wide field surveys with instruments such as HSC, PFS, and Ultimate-Subaru. These surveys are expected not only to reveal the distribution of dark matter, the acceleration of the expanding universe, and the first generation of stars and galaxies, but to provide original targets to TMT. Possible collaborations, such as Subaru School in Vietnam, acceptance of young researchers and PhD students to Subaru, and Subaru-Vietnam joint Subaru projects, will be discussed to seek for collaborative efforts.
10:50	20	Break	Everyone
Chair: Satoru Iguchi
11:10	30	Instrument	Mikio Kurita mikio@kusastro.kyoto-u.ac.jp Kyoto University	Kyoto Optical and Near Infrared 3.8 m Telescope A telescope constructed by joint program among Kyoto university, Hiroshima University,and National Astronomical Observatory Japan is the first segmented telescope in Japan. Construction of an enclosure is undergoing on Okayama Astrophysical Observatory and the telescope will be installed in summer 2017. The project aims not only science goal but also technology development of 18 petal shaped segments for the primary mirror and light-weight structure allowing us to point objects quickly. The key technologies and future potential of the telescope will be introduced in this talk for the group who plan to obtain medium size telescope(s).
11:40	30	Instrument	Đinh Văn Trung IoP/VAST	*Intensity Interferometry with 1-m Optical Telescope* *(A Concept for Collaborative Study)* In this presentation I will review the physical principles of the stellar intensity interferometry, the historical development of the technique by Hanbury Brown and Twiss in the 1950s to measure the diameter of several bright stars. I will discuss the possibility of building a small intensity interferometer using recent advances in technologies, especially high speed electronics and photon counting detectors. Initial development of the single photon detectors based on avalanche photodiodes and high speed correlator will be presented. The intensity interferometer will be based on the 1 meter light weight optical telescope that our group is currently developing. The development of this instrument will serve as good training ground for graduate students in astronomy and physics.
12:10	110	Lunch		WORKSHOP PHOTO
Chair: Eijiro Hiei
14:00	20		Đinh Văn Trung IoP/VAST	*A Brief History of Astronomy in Vietnam*
14:20	40	Viet Rep	Pierre Darriulat pierre.darriulat@gmail.com VNSC	*Development of astronomy and astrophysics in Viet Nam: What is most needed?* *A personal view* After brief comments on the Vietnamese space programme and on outreach activities, I shall focus on research and education in astrophysics: presentation of the research community and of its work; what we need to progress, first from Viet Nam and next from abroad; which instruments do we need.
15:00	30	Viet Rep	Phan Bảo Ngọc HCMIU	*Astrophysics in Viet Nam: Challenges and Opportunities* I present current training programs in Space Science and Engineering of Vietnam National University - HCMC and discuss the impact of these programs on the development of Astrophysics in Viet Nam.
15:30	20	Viet Rep	Nguyễn Quỳnh Lan Hanoi University of Education	*Education Activities of Astrophysics at HNUE* We report education and research activities of astrophysics at HNUE. The contents of astrophysics had been taught at HNUE since 1960's. However the hours for teaching is just enough to teach in basic knowledge. Since we had telescope in 2000, we often organize outreach activities for high school students and public. However recently (about 5 years), the Hanoi sky is not good because the light city and smoke, it is very hard to organize observation events like that often. We also would like to report on research project we work on and future plan for high level training on astrophysics, such as the graduate program.
15:50	20	Viet Rep	Hoàng Chí Thiêm CITA	*Current Status and Perspective for the Development of Theoretical Astronomy in Vietnam* Our solid understanding of the Universe requires precise observations and accurate theoretical models. While Observational Astronomy is expensive and requires big investment into observational facilities, Theoretical Astronomy is very affordable. In this talk, I will first present the current status of research in Theoretical Astronomy in Vietnam. Then I will present several paths to develop the branch of Theoretical Astronomy in Vietnam, through collaboration in training and research with international centers in Theoretical Astronomy. Finally, I will argue that Vietnam possess many excellent opportunities to advance in Theoretical and Computational Astrophysics research.
16:10	20	Break
16:30	60	Panel Discussion	Moderator: Nguyễn Trọng Hiền	*Challenges and Opportunities* Panelists: , Pierre Darriulat, Đinh Văn Trung, Phan Bao Ngoc, Hayashi, Paul Ho, and Young Chol Minh
17:30	30	Break
18:00	90	Dinner

MONDAY - Aug 1, 2016

Time	Duration	Session	Speaker	Title and Abstract
8:50	10			*Quick Announcement (Local Logistics, etc.)*
Chair: Masa Hayashi
9:00	60	Science	Paul Ho pho@asiaa.sinica.edu.tw ASIAA/EAO	*The Development of Radio Astronomy in Taiwan* In this talk, we will review the development of radio astronomy in Taiwan over the past 20 years. We will discuss the rationale behind the choices we made in terms of the projects which we participated in and joined. There were a few important considerations: Identification of a leader(s) in our development. Excellence of science. Possibility of technical developments. Availability of strong partners who will guide our development and provide protection against failure mode. Leverage our investments to ensure the most impact. Potential of future paths of development. These considerations led us to choose interferometry in the submillimeter wavelengths as our focus in development. Today, the research landscape in radio astronomy has changed drastically after these past twenty years. We can discuss how we would make our choices today.
10:00	30	Instrument	Satoru Iguchi s.iguchi@nao.ac.jp NAOJ	*Atacama Large Millimeter/submillimeter Array, ALMA - the Status of Operations and Future Development* The Atacama Large Millimeter/submillimeter Array (ALMA) is an international radio observatory under a global partnership among East Asia (led by Japan), Europe, and North America in cooperation with the Republic of Chile. The array is located at an altitude of about 5000 meters in the Chilean Andes with an operating wavelength range of 0.3 to 9 mm. By using an "Aperture Synthesis Technique," ALMA consists of a homogeneous array of 50 12-m diameter antennas and the Atacama Compact Array (ACA) in order to cover all spatial frequency Fourier components of the brightness distribution of observed sources. ACA is an array composed of 4 12-m diameter antennas in a single-dish mode and a homogeneous array of 12 7-m diameter antennas that has a very compact configuration to take short-baseline data corresponding to the high angular resolution and high sensitivity, and newly achieved the high-fidelity imaging by ALMA. Early science operation started from September 30, 2011 with an initial Call for Proposal (Cycle 0). Second Call for Proposal (Cycle 1), third Call for Proposal (Cycle 2), fourth Call for Proposal (Cycle 3) and fifth Call for Proposal (Cycle 4) were already done on July 12, 2021, December 5, 2013, April 23, 2015, and April 21, 2016, respectively, with the limited number of antennas of less than 66. The observations during these initial stages, however, provided an exciting opportunity for science to utilize this unique world-class facility. The last 66th ALMA antenna arrived at array site on June 16, 2014. This presentation provides an overview of the development of the observatory, the status of its operations, latest results of science observations, and also the future development programs to enhance ALMA.
10:30	30		Break
Chair: Vũ Việt Phương
11:00	30	Instrument	Alvaro Gonzalez Alvaro.Gonzalez@nao.ac.jp NAOJ	*Millimeter and Sub-mm Wave Instrumentation Development for ALMA at NAOJ/Chile Observatory* During ALMA construction, in terms of instrumentation, NAOJ contributed with the design, production and integration of all the receivers for ALMA bands 4 (125-163 GHz), 8 (385-500 GHz) and 10 (787-950 GHz), as well as Holography receivers and an artificial calibration source at 100 GHz based on photonic technologies. After the end of the initial construction phase of ALMA, both the ALMA Science Advisory Committee and the East Asia science community have recommended several instrumentation upgrades to satisfy future ALMA science demands. In that context, the Future Development team at NAOJ Chile Observatory and Advanced Technology Center have started research on new artificial calibration sources, and on advanced receiver technologies which can be included in future upgrades of the ALMA front-end: THz receiver, ultra-wideband RF/IF receivers, and multibeam technologies. In parallel, we have also contributed to the on-going efforts to equip ALMA with the instrumentation for the remaining frequency bands: band 1, 2 and 5. In this talk, I will report on these activities, and try to highlight opportunities for collaboration between Vietnam and NAOJ in this field.
11:30	30	Instrument	Ken'ichi Tatematsu k.tatematsu@nao.ac.jp NAOJ	*Science Operation, Software Development, and Internet Deployment for the International Radio Telescope Project ALMA* I will introduce the software development, remote operation and data transfer, user service for the international radio telescope project ALMA (Atacama Large Millimeter/submillimeter Array). ALMA operates at 5000m site in the northern Chile in Latin America. Twenty-one countries participate its operation. Its construction started in 2002, and we had its inauguration in 2013. ALMA consists of 66 high-precision parabola antennas to observe radio signals with wavelengths down to 0.3 mm. For telescope control, we needed to develop precise software for telescope on real-time OS. The basic assumptions is that observers are not requested to come to Chile for their observation. Then, we needed to develop science operation infrastructure so that observers can create their observing script without faults, programs are optimally carried out through Dynamic Scheduler, and proposers can analyze the data for their sciences. Furthermore, ALMA is the first radio interferometric telescope which was designed so that the observed data is fully quality assured, and calibration and imaging data reduction is done automatically through pipeline software. For operation, we need a stable network from Chile to worldwide, and currently we use international R&E network collaborations. We are continuing efforts for new software requirements for improvement and new functionalities for new telescope capabilities
12:00	20	Instrument	Kohno Kotaro Tokyo University	*Millimeter/Submillimeter galaxy surveys using ALMA and future facilities* Unbiased surveys of galaxies at millimeter and submillimeter wavelengths give unique opportunities for unveiling dust-obscured star-formation and growth of super massive black holes in the early universe, due to the strong negative K-correction. Such surveys will also allow us to uncover millimeter and submillimeter line emitting galaxies and to constrain luminosity functions of CO and [CII] emission lines, which will be essential for understanding the underlying physics which governs the history of cosmic star formation rate density. In this talk, I will describe recent progress of such deep surveys using ALMA and prospects for future possible survey facilities at millimeter and submillimeter wavelengths.
12:20	100	Lunch
Chair: Nobuo Arimoto
14:00	30	Exp Report	Hideo Ogawa Osaka Prefecture University	*Astronomical site testing, atmospheric science, radio lab operation and radio telescope construction*
14:30	20	Viet Report	Đinh Văn Trung IoP/VAST	*Instrumentation Development in Vietnam* In this presentation I will provide an overview of instrumentation projects that I have carried out during the last few years at the Institute of Physics, Vietnam Academy of Science and Technologies. The main drive is to develop tools up to now unavailable in Vietnam to perform highly accurate optical and spectroscopic measurements in the field of atmospheric research and nanoscience. Two specific cases will be shown: the multiwavelength LIDAR system to study atmosphere and the fluorescence correlation spectroscopy apparatus to study single molecules and single nanoparticles. I will discuss the difficulties and challenges encountered during the realisation of these projects.
14:50	20	Viet Report	Phạm Ngọc Điệp VNSC	*A Concept for Collaborative Study: On a possible future national radio astronomy facility* We were asked to make a study on possible radio telescope installations that Vietnam might wish to acquire in the near future. The content of our report: general considerations, the ASEAN and East Asia context, implications for Vietnam and main recommendations will be presented.
15:10	30	Viet Report	Kaz Sekiguchi NAOJ	*Why Vietnam should support astronomy and how the IAU can help* Vietnam is a registered National Member of the International Astronomical Union (IAU). The IAU has set up the Office of Astronomy for Development (OAD) in partnership with the South African National Research Foundation (NRF). The aim of the IAU/OAD is to use astronomy to stimulate development at all levels including primary, secondary and tertiary education, science research and the public understanding of science. I will introduce the activities of the IAU/OAD and other bodies that Vietnam could utilize for its development of Astronomy.
15:40	20	Break
16:00	60	Panel Discussion	Moderator: Satoru Iguchi	*On the science and technical challenges, and promises for international collaboration* Panelists: Arimoto, Hayashi, Ho, Young Chol Minh, Phạm Ngọc Điệp, and Đinh Văn Trung
17:00	60	Visit to ICISE
18:00	90	Dinner

TUESDAY - Aug 2, 2016

Time	Duration	Session	Speaker	Title and Abstract
8:50	10			*Quick Announcement (Local Logistics, etc.)*
Chair: Pierre Darriulat
9:00	60	Science.	Young Chol Minh minh@kasi.re.kr KASI	*Challenge to the mm/Far-IR region and our experience to promote the astronomical activities in Korea* The far-IR and sub-millimeter region is the final frontier still waiting for an exciting challenge. Along the importance of multi-frequency studies, the far-IR/sub-mm region becomes a major part to understand the whole picture of the astronomical phenomena. I plan to give a brief introduction on the characteristic features of this wavelength region, and then another introduction on some of previous Korean experience to promote the astronomical research activities in Korea. I will focus on our radio projects, especially, on the KVN (Korean VLBI Network) project. If I may, I would like to share our experience to provide assistance when Viet Nam launches a new radio project.
10:00	30		Kee-Tae Kim KASI	Korean VLBI Network (KVN) and TRAO 14-m Telescope KASI started to operate the Taeduk Radio Astronomy Observatory 14-m telescope at (85 – 115) GHz in mid 1980’s and recently installed the SEQUOIA, which is a cryogenic focal plane array with 16 pixels. KASI also started to operate the Korean VLBI Network (KVN) in late 2013. The KVN consists of three 21-m telescopes eqiupped with the multi-frequency receiving systems, which allow to observe at 22, 43, 86, 129 GHz simultaneously both in single-dish and VLBI modes. The KVN is often combined with the Japanese VLBI network, VERA, to form the KVN and VERA array (KaVA). I will talk about the performance and ongoing key science projects of the KVN/KaVA and TRAO 14-m telescope.
10:30	30	Instrument	Hiroshi Imai hiroimai@sci.kagoshima-u.ac.jp Kagoshima University	*Planning VLBI in the SKA era* In 2020's, radio astronomy at high and low frequency bands will be increasingly developed by large international facilities such as ALMA and the SKA, respectively. Taking into account the observation conditions and the importance of domestic research activities in the individual nations, exploration of radio astronomy at low frequency bands with their own facilities has great benefits with some sustainability for these issues and expanding the frontier of radio astronomy. The SKA with ultimate sensitivity and wide fields of view is expected to lead the low frequency-band radio astronomy in order to elucidate key questions in astronomy such as cosmic dawn, galaxy evolution, cradle of life, and the general relativity. The SKA is also expected to explore "unknown unknown", such as transient objects. In any key science, high angular resolution and high accuracy astrometry are essential for reliable identification of the discovered sources and their locations in the universe. Although the SKA (especially in phase 1) and its big precursors (e.g. MeerKAT and ASKAP) will be constructed in South Africa and Australia on the western side, their combination with surrounding radio telescopes will provide necessary angular resolution and astrometric accuracy. It is also expected that newly discovered sources with the SKA will be observationally followed by other telescopes through more intensive monitoring campaigns. We have studied possible science cases in such combined observation models. VLBI is one of the greatest scientific applications. We discuss Japanese view points of SKA VLBI, which encourages synergies in VLBI in Africa and Asia-Pacific nations.
11:00	20		Break
11:20	20	Instrument	Eijiro Hiei eijiro.hiei@nao.ac.jp NAOJ	*Ground-based Solar Observation in Japan* The observing instruments and facilities at NAOJ and Hida Observatory will be talked, and the solved and unsolved researches carried on by using these telescopes are summarized.
11:40	20	Instrument	Ryouhei Kano ryouhei.kano@nao.ac.jp NAOJ	*Solar observations in space, and the Hinode results* The solar atmosphere is a highly energetic region, which is occupied with higher-temperature (>1MK at most) plasma than the surface ("photosphere", 6000K), and in which many dynamic phenomena like solar flares frequently happen. Such energetic activities must be caused by the interaction between the plasma and the magnetic fields in it. To understand the entire solar atmosphere consisting of the chromosphere (10000K), the transition region (10000K-1MK) and the corona (>1MK) above the photosphere, UV- or X-ray observations in space are required. In 2006, the 3rd Japanese solar satellite "Hinode" was launched with carrying 3 telescopes: the Solar Optical Telescope (SOT) to observe the photosphere and the chromosphere, especially the photospheric magnetic fields; the X-Ray Telescope (XRT) to observe the corona; and the EUV Imaging Spectrometer (EIS) to observe the dynamics and flows in the solar atmosphere. Hinode is still working well and give us precise magnetic information on the photosphere as well as dynamic plasma phenomena in the upper layers. In the presentation, we will show the solar observations in space which the Japanese solar-physics community conducted or joined, and their investigations with future plans.
12:00	120	Lunch
Chair: Đinh Văn Trung
14:00	30		Toshikazu Onishi Osaka Prefecture University	*Small mm-submm telescopes: Large-scale molecular gas survey in CO lines* In this presentation, I will present a project overview and some of the observational results with the small aperture radio telescopes that I have been involving in; Nagoya 4-m telescopes and Osaka 1.85m telescope. These telescopes were built to reveal the molecular gas distribution extensively in the Galaxy and Magellanic system. The purpose is an elucidation of evolution of interstellar matter and the mechanism of star formation by revealing the distribution, kinematics, and physical conditions of interstellar gas in the molecular phase with the thorough extensive survey.
14:30	20	Exp. Report	Phạm Tuấn Anh VNSC	*Study of the gas and dust components of high redshift galaxies* We present millimetre/sub-millimetre observations of the gravitationally lensed quasar host RX J0911,at redshift ~2.8 corresponding to the epoch of maximal star formation rate. The joint observation of line emission- CO(7-6) measured at IRAM Plateasu de Bure - and continuum emission - 358 GHz measured at ALMA - makes it possible to resolve both the gas and dust components and measure their sizes. We compare the results with galaxies in a similar stage of evolution, when mergers play an important role, and comment on the potential of ALMA in making new observations, using as example the gravitationally lensed galaxy HE 1104 at z~2.3.
14:50	20	Exp Report	Đỗ Thị Hoài VNSC	*Study of the gas envelopes of evolved stars and protostars* We present observations made at the ALMA and IRAM Plateau de Bure interferometers of the CO emission at millimetre/sub-millimetre wavelengths of both evolved stars and stars in formation. In both cases, we model in space the morphology and kinematics of the gas envelopes using simplifying hypotheses such as rotation invariance about an axis. While we have been analysing data on evolved stars for now more than four years our implication in the star formation field is more recent. Examples are presented that illustrate the main results.
15:10	20	Exp Rep	Lê Huy Minh IGP/VAST	Global positioning system and its application for ionospheric study in Vietnam We present briefly the Global positioning system and the continuous GPS network in Vietnam and its application for ionospheric study. The method of calculation of ionospheric total electron content (TEC) from combination of of the carrier phase and pseudorange measurements at the GPS frequencies f1 and f2 is presented. The TEC calculation from the continuous GPS network in Vietnam and in the Southeast Asian region shows that Vietnam is under the equatorial ionization anomaly (EIA), the northern part on the crest and the southern one on the trough region. Time variation of the parameters of the crests of the EIA is analyzed for the period 2006-2013. In both hemispheres, the amplitude of the crest is larger in spring than autumn from 2006 to 2008 and smaller in spring than in autumn from 2009. We also observe an asymmetry between the amplitude and the position of the two crests of ionization anomaly. There is a very high level of correlation between the amplitude of the TEC at the two crests and the sunspot number. During the deep solar minimum 2008-2009, the amplitude of crests of ionization becomes small during several months in summer and winter. The results show that both crests move significantly equatorward in winter than other seasons and there is a tendency for both crests to appear earlier in winter and latter in summer. The TEC variation during the St Patrick Day’s magnetic storm (17 March 2015), the largest magnetic storm during the 24th solar activity cycle is presented in combination with the other magnetic and ionospheric data in Vietnam.
15:30	20	Exp Rep	Nguyễn Trọng Hiền JPL/Caltech	*LIME: Line Intensity Mapping Experiment* LIME is a small and compact optical telescope with spectroscopic capability. I will discuss the science motivation and experimental planning for the instrument.
15:50	60		Workshop	*Summary - Free Discussion*
16:50				*Workshop Adjourns*