# CONSTRUCTING THE ASTRONOMICAL OBSERVATORY AT TAY NGUYEN UNIVERSITY, VIETNAM

Tan LE-MINH  Department of Physics, Faculty of Natural Science and Technology,
Tay Nguyen University,
567 Le Duan street, Buon Ma Thuot city, Dak Lak province, Vietnam  Lam TRAN-
QUOC  Department of Physics, Faculty of Natural Science and Technology, Tay
Nguyen University,
567 Le Duan street, Buon Ma Thuot city, Dak Lak province, Vietnam  Quang
NGUYEN-LUONG  120 Bloor Street East, Toronto, ON, M4Y 1B7, Canada, and at
Nagoya City University

###### Abstract

We are planning to build an observatory that includes a 40 cm optical
telescope at Tay Nguyen University (TNU), Daklak Province, Vietnam. In this
paper, we report the initial activities of our project. First, to prepare for
the scientific exploitation of the observatory, we organized the observational
nights for students at the International Center for Interdisciplinary Science
and Education, Qui Nhon in April 2017 and at the Nha Trang Observatory, Nha
Trang in November 2018. These activities aim to provide students with the
skills of astronomical observations and to create their passion in astronomy
study. Second, we are organizing the annual Exploration Program in
Astrophysics Research (EPAR) at TNU. The goals of EPAR are to promote the
teaching and learning activities at TNU and promoting collaboration between
TNU and other institutes. Finally, we are conducting joint research project
between TNU and Kyoto astronomical observatory of Kyoto university to prepare
for the technical details of the observatory.

##  1 Why do we need an astronomical observatory in Tay Nguyen University?

In 2017-2018, the Vietnam National Space Center (VNSC) installed two 50 cm
optical telescopes in Hanoi and Nha Trang cities. They are about to begin
operations. In addition, the International Center for Interdisciplinary
Science and Education (ICISE) in Quy Nhon city and VNSC held a workshop on
Astronomy Development in Vietnam - Challenges and Opportunities from 31 July
to 2 August, 2016. The purpose of the workshop is “seek to establish a road-
map for the development of astronomy and astrophysics in Vietnam”. Following
this workshop’s goal, Tay Nguyen university (TNU) in Dak Lak province, Vietnam
has held the special programs for astronomy and strives to attract students to
study astronomy.

Dak Lak province is the largest province in the HighLand region in Vietnam.
This province is in one of the mountain region of Vietnam which has an average
high of 400 - 800 m above sea level and the peaks up to 1500 - 2000 m. It has
a high mountain, Chu Yang Sin, with 2442 m high. Dak Lak is about 200 km far
from the sea. The dry season begins from November to April each year with
quite dry weather and many clear nights. The TNU located in Daklak is the
largest university in the region. The TNU has about 12800 students, among
which 600 students are in Faculty of Natural Science and Technology. There are
about 80 students in Physics at Department of Physics. Department of Physics
has two lecturers and one technician in Astronomy. One lecture, Nguyen Dang
Thanh Nhan, now is pursuing a graduate program in Astrophysics at Bonn,
Germany. Astronomy subject is taught for the third-year students. It has three
credits with 25 hours for lecture and 3 days for observational practice.
However, a night-sky observation is still a big gap because we now just have a
small optical telescope with 90 mm in diameter.

Figure 1: Vietnam map shows the location of DakLak province where TNU resides.

We plan to start building an astronomical observatory at TNU which will
contain a 40 cm optical telescope. The main audience of the observatory is the
students to conduct experiments and exercise. In return, the students will
conduct public shows to draw the attention of the public to science and to
increase the awareness of science. Astronomical observation brings the passion
and creativity for students and promote the researching and teaching
activities in Astronomy at TNU. The observatory is also used for research
purpose such as finding the exoplanets, studying planet formation, observing
asteroids, etc. Furthermore, according to the draft of Vietnam High School
Physics curriculum in 2017, the Physics program for the 10th grade has a
subject of the Earth and Sky with the time of 11 hours. Therefore, the
observatory is an ideal destination for High School students in Dak Lak
province to practise this subject. The main goals of our project are as
follows,

Figure 2: Current astronomical instruments at TNU: Very Low Frequency Array
(upper) and 21 cm waveband radio telescope (lower).

  * •

Construct an astronomical observatory for education by 2023

  * •

Build an astronomy hub at TNU for local researchers to meet and exchange
continuously

  * •

Nurture young enthusiasts and encourage students to follow higher degree in
astronomy

##  2 Main current initiative and relevant activities

###  2.1 The main activities

This project will be a long term (3-5 years) project and will be supported by
institutes such as National Astronomical Observatory of Japan (NAOJ), Kyoto
Univeristy, Nishi-Harima Astronomical Observatory (NHAO), etc. The main
activities include three parts including exchange staffs, on-site training,
and building construction.

Exchange staffs: There are two main parts within this activity. First, we will
send TNU staffs to Kyoto university to conduct experimentation and
construction with Kyoto university staff, the cost is covered jointly by TNU
and Kyoto university. Second, Japanese researchers will visit TNU to give
lecture, exchange, promote students. This activity is supported mainly by TNU
fund and NAOJ fund.

On-site training: We are planning for a 1-week school in telescope training
on-site at TNU in 2019 after part of the telescope is finished.

Observatory construction: A building that includes housing for the telescope,
control room, museum room is already planned and will be the responsibility of
TNU. The TNU has agreed to support this activity. Kyoto university will
support with the telescope tube and the overall technical design of the
telescope. The observatory will also host the current existing research and
training instruments at TNU such as Very Low Frequency telescope and 21 cm
waveband radio telescope. We have used these instruments effectively in
research and training in the past years[4,5,6,7,8,9].

###  2.2 Past relevant activities

The following past activities promoted the education and research activities
in Astronomy at TNU,

  * •

First visit of Nguyen Luong Quang (CITA) in 2015 to TNU has promoted students
in astronomy studying

  * •

In December 2015, Le Minh Tan (TNU) visited to Nobeyama Radio Observatory
(NAOJ), Japan for observational practice.

  * •

In July 2016, Professor Masatoshi Ohishi (NAOJ) and Nguyen Luong Quang gave
lectures about a basic of radio astronomy and promoted the observatory
construction project at TNU.

  * •

In March 2017, Nguyen Dang Thanh Nhan (TNU) visited NHAO, University of Hyogo,
Japan to learn how to use the 60 cm optical telescope to conduct telescopes,
observations of asteroids, and analyze the data.

  * •

In July 2017, Professor Neal Evans (The University of Texas at Austin) visited
TNU and gave students the basics of Astrophysics.

  * •

In June 2017, Le Minh Tan (TNU) visited Mitaka (NAOJ), Japan to learn the ALMA
data analysis.

  * •

Tran Quoc Lam (TNU) joined the NARIT Optical Design Summer School 2018 in
Chiang Mai, Thai Land

###  2.3 Educational activities

  * •

Tropical school for undergraduate astronomy at ICISE, Qui Nhon, Vietnam in
April 2017

We were the first university to partner with ICISE to bring students to ICISE
and organize the first hands-on event in ICISE in April, 2017. We are looking
to strengthen this partnership and creating a better model for university and
ICISE collaboration. We created a tropical school series in astronomy with
lectures from ICISE conference attendants. School had 60 attendants (see
Figure 2). We also organized a night-sky observation in ICISE’s garden using a
40 cm telescope and some small telescopes designed by Le Quang Thuy and Nguyen
Anh Tuan (ExploraSciene Center, ICISE) (see Figure 3). Students were very
interested in this activity and really impressed with seeing the bright stars
through the optical telescope.

Figure 3: Dr. Hideaki Fujiwara (NAOJ) and TNU students in the tropical school
for undergraduate astronomy in Qui Nhon university

Figure 4: Students attended the sky observation section at ICISE garden

  * •

Exploration Program in Astrophysics Research (EPAR) at TNU, 2 - 13 July, 2018

Figure 5: Summary of EPAR activities. Logo of EPAR and opening section of EPAR
(upper), student groups were working on their projects (middle lowers), and
results from individual working group (lower): exoplanet transist (left), HR
diagram (middle), and gamma-ray burst (right).

The EPAR at TNU brings astronomers and students together to work on specific
research topics in astrophysics. The program run for 2 weeks, hosted by TNU.
The program welcomed students from all parts of Vietnam who are senior
undergraduate students or graduate students searching for research
experiences. Vietnamese students who are searching for a place to host their
dissertations are also welcomed. Participants can come for a shorter period or
for the whole duration of the program, and are encouraged to come back year
after year. Three visiting scientists and nine students teamed up and conduct
common research projects (see Figure 5). The projects were designed such that
they can be sub-divided into individual sub-projects and tailored to match
with the availability of the supervisor that year. Each week, scientists were
responsible for the scientific theme and student supervision. Students
presented their progress in the two Friday’s afternoons. These projects are
described with the details below,

Project 1: Observing Gamma Ray Burst with James Clerk Maxwell Telescope (JCMT)
(supervisor: Dr. Mark Rawlings, EAO, USA)

Students get to act as members of a GRB monitoring team. The project walks the
students through the notification process for a GRB trigger, encourages them
to check the position with Set of Identifications, Measurements, and
Bibliography for Astronomical Data (SIMBAD), prepare a simple JCMT MSB with
the JCMT Observing Tool, receive the data, examine it, conduct flux
calibration and plot a simple light curve.

Project 2: Radiative Transfer modeling of planet forming core (supervisor: Dr.
Dimitris Stamatellos, UCL, UK)

In this project, students find the temperature of the prestellar cores, do
radiative transfer simulations and test the cores by comparing it with
previous works. Students also study the motion of the exoplanets observed by
the Kepler space telescope using the web browser and directly download the
data of the planet to study. Students look at some of the exoplanets of the K2
mission and determine what kind of planets they are (hot planet, cold planet
or habitable planet) by defining parameters of planets such as radius,
temperature, mass,….Students also calculate the parameters of orbital radius,
orbital period, stellar luminosity.

Project 3: Sciences with sub-1m optical telescopes: stellar evolution and HR
diagram, asteroid light curve (supervisor: Prof. Itoh Yoichi, NHAO, JP)

Real photometric data taken with the 2 m Nayuta Telescope, a 60 cm Nishimura
telescope, and a 30 cm Meade telescope at NHAO will be examined. The exercise
consists of three steps; photometry of open cluster members, time series
photometry of an asteroid, and time series precise photometry of an exoplanet
transit.

  * •

Observational event at Nha Trang Observatory (NTO) from 4 - 7 November 2018

Figure 6: Student activities in observational event at NTO

Figure 6 shows the activities of TNU students at NTO. Students surveyed the
parts of the 50 cm optical telescope to understand how it work and were
provided with the basic knowledge of the sky. The lectures presented by staff
of NTO focused on the basic concepts and guidelines for observing the sky.
Students did the exercises on how to determine the zodiac constellations, and
identify the constellations in the summer triangle and typically bright stars
in particular season. Students also experienced and admired the beauty of the
universe at the planetarium with film “Two small pieces of glass”. In the
evening students experienced the night sky with a small optical telescope to
practice the knowledge which they were learnt in the planetarium.

##  3 Future plan

###  3.1 Strategic plans

  * •

Establish annual EPAR program at TNU and in corporation with other institutes

  * •

Exploit scientific projects that can be done with 40cm telescopes

  * •

Incorporate the hands-on activities with telescopes into astronomy curriculum

  * •

Involve in extended training and research network

###  3.2 Detailed plans

  * •

2019:  We will continue to organize the EPAR at TNU and NTO, in July 2019. It
will run for two weeks. This program will focus on the topics such as basics
of Astrophysics, photometry and spectroscopy. In the second week, the school
will conduct astrophysical observation training for university students and
young scientists using the 50cm optical telescope at NTO. The number of
participants is about 15. The observation targets are the dispersed star and
asteroids. At the end of 2019, we will start to build the observatory. The
site area is about 100 m2 inside TNU campus.

  * •

2020-2021:  Dr. Mikio Kurita, an associate professor at Kyoto University, will
establish a 40-cm telescope at TNU. This telescope will be installed,
operating, and so on, to install CCD cameras and to conduct initial testing
observations. We will organize the Astronomy training. Students will conduct
observation on university students from the previous fiscal year (2019) using
the 50cm optical telescope at NTO. This training was conducted using newly
developed optical spectrometer.

  * •

2022-2023:  Currently, VNSC has two observatories. We hope that we will join
the optical telescope network in Vietnam. In addition, the TNU 40 cm telescope
will be also included in an observation network of Japan to participate in the
observation of unexpected celestial bodies such as supernova explosions and
gravitational waves.

##  4 Summary and Challenges

We plan to build an astronomical observatory at TNU and to design a 40cm
telescope with the new design led by the astronomy lab from Kyoto university.
Land and observatory construction cost is granted by TNU. We successfully
organized “Tropical school for undergraduate astronomy” at ICISE in Qui Nhon
and “Observational event” in NTO. These activities aim to provide students
with the skills of night sky observation and to create their passion in
astronomy study. We successfully organized the EPAR from July 2 to July 13,
2018 at TNU. The goals of this program are to promote the teaching and
learning activities on Astrophysics, and to promote the astronomical
observatory construction project at TNU. We also showed the future plan for
observatory construction.

However, we meet many challenges such as human source, budget and
collaboration. There is a lack of experts in Astronomy in Central Highland,
Vietnam. We are actively looking for financial support to purchase parts of
the observatory and send staffs to visit foreign institutes. We actively need
support from scientific community to come to Daklak to teach and exchange. We
are also looking for support to receive our students for internship or
exchange.

Acknowledgement:  During the course of our work, we appreciate the supports
from individuals such as tropical school lecturers, EPAR lecturers, Kaz
Sekiguchi, Mikio Kurita, Yoichi Itoh, Neal Evans, Yong-Chol Minh, Hyung Mok
Lee, Nguyen Thi Hoang Anh, Pham Ngoc Diep, Nguyen Trong Hien and institutes
such as NAOJ, ICISE, KASI, NHAO, Kyoto University, VNSC, IAU-OAD.

## References

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j^{\prime}}\cdot{\bm{b}^{\prime}}}-\nabla\cdot\overline{{\bf F}},$ (24)

where the first term on the right hand side describes the generation of
magnetic helicity and the second one its resistive destruction, while
$\overline{\bf F}$ is the small-scale helicity flux (see, e.g., Brandenburg
and Subramanian, 2005). If the flux is significant, its divergence should be
dominant over the two other terms during a steady state dynamo. From the
evolution equation for the dynamical $\alpha$ effect, Eq. (19), one would also
expect that the mean field strength would become independent of ${\rm Re}_{\rm
M}$, if the fluxes are efficient.

Del Sordo et al (2013) studied an isothermal plane-wave forced Cartesian
system with a possibility for an imposed wind in one coordinate direction. The
forcing used was helical, producing an equator perpendicular to the wind
direction by changing the sign of helicity across the equatorial plane.
Although simplified, this model has some similarities to a local volume of a
rotating galactic disc subject to a wind. The results show that the wind-like
advection can induce a non-zero magnetic helicity flux, which shows asymptotic
behavior as a function of ${\rm Re}_{\rm M}$. The other terms in Eq.(24) were
larger for ${\rm Re}_{\rm M}<1000$, but for higher ${\rm Re}_{\rm M}$ they
became comparable to the divergence of helicity flux. Moreover, these terms
showed an inverse dependence on $Rm$. However, the MF decreased when the wind
strength increased. Essentially similar results were obtained with a
comparable but incompressible setup without a wind Rincon (2021). Agreeing
with the results of Del Sordo et al (2013) without the wind, Rincon (2021)
found significant helicity fluxes due to the redistribution of helicity
through turbulent flux across the equator. Although promising, these results
do not yet conclusively prove that helicity fluxes can alleviate the
catastrophic quenching scenario. Simulations with higher ${\rm Re}_{\rm M}$
and also including shear and more realistic turbulence driving are required.

##  5 Conclusions

###  5.1 Comparisons with analytic theory

Many aspects of analytic theory appear consistent with numerical simulations,
in particular the existence of both SSD and LSD activity in galaxy models at
different scales. SSD growth rates are strongly dependent on $\rm Re$ (Eq.
23), and thus on numerical resolution if it dominates resistivity over any
physical resistivity implemented. SSD and LSD compete for energy when both are
active, but after SSD saturates, LSD continues to grow MF as predicted
analytically (Sect. 3.3.3). The requirement of helical turbulence for dynamo
activity is verified (Sect. 3.4.2). Parker instability, MBI, and MRI can drive
further dynamo activity, although likely subdominant effects in star-forming
regions of galactic disks (Sect. 3.3.3.

Turbulent transport coefficients derived from the numerical models with
multiple different sets of assumptions show that, although the overall picture
of dynamo behaviour from analytic models does have some resemblance to the
results, there are many inconsistencies (Sect. 4.1). These are most likely due
to the strong, anisotropic turbulent flows produced by the SN driving in
stratified discs. As a result, simple dipolar or quadrupolar field
configurations are likely to be more the exception than the rule (Sect.
3.4.2).

The question of the source of the magnetic fields that grow due to dynamo
activity has been dramatically answered in recent years with the clear
demonstration of dynamo action leading to near-equipartition fields occurring
in plasmas magnetised ab initio by Weibel instability (Sect. 3.1). As this can
occur already in protogalactic accretion flows, galaxies appear likely to be
born magnetised. Fast SSD action in these high Re systems maintains fields
within an order of magnitude of equipartition on less than megayear
timescales. Large-scale MF does take much longer to develop, as it still
relies on LSD activity over far longer timescales comparable to the rotational
periods of galaxies (Sect. 3.3).

Many models suggest that helicity fluxes can prevent catastrophic quenching of
LSD activity by small-scale magnetic fluctuations (Sect. 4.2). However, direct
measurements of helicity fluxes in well-defined numerical experiments will
still be required to conclusively demonstrate that catastrophic quenching does
not occur in galactic dynamos.

###  5.2 Consistency with observations

The observed global structure of magnetic fields has points of contact with
models. The weak correlation of magnetic spiral arms with stars and gas is
seen in models including a circumgalactic medium. Models show a wide variety
of pitch angles, some of which do appear consistent with measurements of
shallow negative values, although even positive values are seen in the models
in perturbed or strongly interacting galaxies (Sect. 3.6).

Simulated maps of Faraday rotation derived from models agree best with
observations if whole galaxy models are combined with a sub-grid model for H
ii regions produced by stellar clusters drawn from a population synthesis
model. High-galactic latitude regions in particular are dominated by structure
within a few kiloparsecs of the Sun, if not the surface of the Local Bubble.
Predictions of rotation measures are consistent with observed upper limits,
but small enough that improved observations will be needed to constrain them
(Sect. 3.6).

###  5.3 Challenges

Starting from the earliest times, models of seed field production and
amplification by Weibel instability need to be extended towards realistic
values of the electron-ion mass ratio, and checked for robustness against
Landau damping. Quantitative demonstration of their applicability to
protogalactic accretion flows will also be valuable.

However, the strong implication of these models that galaxies are born
magnetised suggests that numerical models of galaxy formation and evolution
should not start with infinitesimal fields, but rather with turbulent fields
of some fraction of equipartition, and that those minimum values of the
turbulent field should be somehow maintained even if the numerical resolution
of global or cosmological models is insufficient to directly capture the
relevant fast SSD maintaining the models. Performing simulated observations of
the synchrotron radiation and IR polarisation produced by the MF structure of
galaxies in their cosmological context will ultimately require models of both
magnetic field and cosmic ray evolution. These will allow much better
constraints on the models to be placed by classical observations such as the
pitch angle of spiral arms and field reversals.

Achieving sufficient resolution to measure MF dynamo coefficients in models
that include the necessary physical processes in the ISM is a third challenge,
that offers a potential solution to the second challenge. If dynamo
coefficients can be accurately and self-consistently measured, they can be
used to support the construction of explicit large eddy simulations that
capture the sub-grid dynamo behavior. Although preliminary work indicates
agreement between MF models in some regimes and the DNS-like MHD models from
which they draw their coefficients (Sect. 4.1), much further work needs to be
done to extend this result into saturated regimes. Disentangling the effects
of multiple types of dynamos acting simultaneously remains a major challenge.

Acknowledgments We acknowledge fruitful discussions with Abhijit Bendre,
Matthias Rheinhardt, and Jörn Warnecke on the manuscript. This project has
received funding from the European Research Council (ERC) under the European
Union’s Horizon 2020 research and innovation program (Project UniSDyn, grant
agreement n:o 818665; for MJKL and FAG). M-MML was partly supported by US NSF
grant AST23-07950 and acknowledges Interstellar Institute’s program “II6” and
the Paris-Saclay University’s Institut Pascal for hosting discussions that
nourished the development of some of the ideas behind this work.

##### Disclosure statement

The authors declare that they have no relevant or material financial interests
that relate to the research described in this paper.

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