The Report of The National Astronomical Observatory of Japan for Visiting Review Committee

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Forword

Overview
of
The National Astronomical Observatory
of Japan (NAOJ)

As an inter-university research institute for astronomy,
the National Astronomical Observatory of Japan (NAOJ) actively
promotes open-use of observing facilities, joint research and
instrument development programs, and international cooperative
researches.

1.1 History
NAOJ was established in 1988, integrating the Tokyo
Astronomical Observatory of the University of Tokyo, the
International Latitude Observatory of Mizusawa, and the
solar radio group of the Research Institute of Atmospherics,
Nagoya University. In order to promote open-use of the
observatory facilities for country-wide researchers, these
three research centers were reorganized as NAOJ.

(1) The Tokyo Astronomical Observatory, the University of Tokyo
The antecedent of the Tokyo Astronomical Observatory started
as a small observatory in the Science Department, the University
of Tokyo in 1878. The observatory became a university's research
institute in 1888 and was moved to Mitaka City in 1924. In 1949,
the observatory was reorganized as the Tokyo Astronomical
Observatory. As a center of astronomical research in Japan,
the observatory had promoted wide-range observational and
theoretical research; it established the Norikura Solar
Observatory in 1949, the Okayama Astrophysical Observatory
in 1960, the Dodaira Astronomical Observatory in 1962, the
Nobeyama Radio Observatory (Solar Radio Observing Facilities)
in 1970, the Kiso Optical Astronomical Observatory in 1974,
and the Nobeyama Radio Observatory (Cosmic Radio Observing
Facilities) in 1978. In addition, it played an important
role in astronomical computation and data analysis by
implementing a computer center in 1978. It had also
compiled Calendar and Ephemeris information and officially
determined the Japanese Standard Time.

(2) The International Latitude Observatory of Mizusawa
The International Latitude Observatory was tentatively
established under the program of the International Latitude
Service in 1899. The Observatory became an institute in 1920
for the continuation of this service. It started time and
latitude observations in 1956 and earth tides observations
in 1967. With rapid progress in astronomy and its related
sciences, the observatory was anticipated to play new and
more demanding roles by introducing new techniques such as
VLBI.

(3) The Research Institute of Atmospherics, Nagoya University
This institute was established in 1949, aiming to conduct
research in atmospherics. In 1952, a radio astronomy group
started research on solar and cosmic radio emission. This
group made great contributions to solar observations by
developing grating interferometer systems. This group joined
the solar radio astronomy group in NAOJ in 1988.

(4) The Establishment of NAOJ
Before the establishment of the NAOJ, detailed discussions
were made in 1984 at the Committee of Astronomy in the Science
Council of Japan. The main topics were reviews of astronomy in
Japan, future development plans including big projects such as
the Subaru project, and reorganization of research institutes.
Since then, detailed discussions were organized in the three
institutes mentioned above as well as beyond institutional
framework. As a result, the NAOJ was established in 1988 as an
inter-university research institute for astronomy. The NAOJ at
the time of establishment had 6 divisions (22 research sections*1
and 2 guest research sections) and 8 research facilities.
(Three research sections and one observatory facility were
moved from the Tokyo Astronomical Observatory to the Institute
of Astronomy, the University of Tokyo for continuity of
astronomical education in the University.)
In 1991, the construction of the 8-m telescope Subaru
started at the summit area of Mauna Kea, Hawaii. In 1993,
the Advanced Technology Center was established as a center
for the development of the instruments to be used for Subaru.
In 1997, Subaru Telescope Hawaii Facility, which is the first
Japanese, large-scale research facility located outside Japan,
was opened in Hilo City. In order to promote the Subaru project,
the seventh research division was established as Division of
Large Optical-Infrared Telescope during 1992-1996.
In order to observe solar active phenomena at radio wavelengths,
the Nobeyama Radioheliograph was completed in 1992. Supercomputers
were introduced in the Astronomical Data Analysis Center in 1996;
they are used by researchers inside and outside of NAOJ.
Currently the NAOJ consists of 6 research divisions and the
Subaru Telescope Hawaii Facility (containing 29 research sections
and 9 guest research sections) and 9 other research facilities,
located at Mitaka, Mizusawa, Dodaira, Nobeyama, Norikura, and
Okayama.
Since April 1992 NAOJ has been participating in Department of
Astronomical Science, School of Mathematical and Physical Science,
the Graduate University for Advanced Studies, and fulfilling the
responsibilities of doctor course education. The NAOJ has been
performing educational duties including observations, instrument
developments, and astronomical data analysis.

1.2 Present Status of NAOJ

(1) Organization
NAOJ consists of a Research Department, an Engineering
Support Department, and an Administration Department. The
Director General represents NAOJ with the assistance of
Associate Director. The Director General is elected by a
Board of Councillors, while an Advisory Council for Research
and Management is responsible for the personnel selection of
scientific staff individuals and for management.

(2) Structure
The structure of NAOJ is shown in Table 1.2.1. The numbers
of staff in individual departments are summarized in Table 1.2.2
and Figure 1.2.1.

1.3 Research Department

The NAOJ Research Department consists of 6 research divisions
and 10 observatory facilities, as shown below. Many of the
facilities are open for astronomers throughout the world.

Division of Optical and Infrared Astronomy
7 research sections + 2 guest research sections (1 for domestic, 1 for foreign)
Perticipates in the 8-m optical-infrared telescope (Subaru)
project; observes various phenomena ranging from the solar
system, stars and stellar systems, galaxies, and the Universe;
also develops observational hardware and software for the
Subaru project.
Okayama Astrophysical Observatory
Operates 188-cm, 91-cm, and 65-cm optical telescopes for
open use.
Dodaira Astronomical Observatory
Operates a 91-cm reflector and a spectro-polarimeter for
open use.

Subaru Telescope Hawaii Facility
3 research sections
Is the main body responsible for the construction of the
8-m optical-infrared telescope, Subaru, on the 4200-m high
summit of Mauna Kea, Hawaii.

Division of Solar Physics
2 research sections + 1 domestic guest research section
Conducts observational and theoretical research on the
solar magnetic fields, the solar atmosphere, various
solar activity phenomena, and the interior structure
of the Sun.
Norikura Solar Observatory
Located at the altitude of 2876 m. A 25-cm coronagraph
has been used for spectroscopic studies of the Sun.
World Data Center for Solar Activities
Compiles and publishes solar activity data from around
the world.

Division of Astrometry and Celestial Mechanics
3 research sections
Conducts research on reference frames based on precise
measurements with the Tokyo Meridian Circle.
Started construction of TAMA300, a gravitational wave
detector.

Division of Theoretical Astrophysics
2 research sections + 2 guest research sections (1 for domestic, 1 for foreign)
Conducts theoretical research on various cosmic phenomena,
such as the large-scale structure of the Universe,
the formation process of galaxies, stars and planets,
the structure and evolution of rotating celestial bodies.

Division of Radio Astronomy
7 research sections + 2 guest research sections (1 for domestic, 1 for foreign)
Promotes astronomical observations using radio waves
and conducts research on various cosmic phenomena,
such as the formation of stars, active phenomena in
active galaxies, explosive phenomena on the solar surface.

Cosmic Radio Observing Facilities of NRO
Operate a 45-m telescope and an interferometer array of
six 10-m telescopes. Open for astronomers around the world.
Solar Radio Observing Facilities of NRO
Obtain high space- and time-resolution images of the
radio Sun with a radioheriograph. It has been upgraded
into a dual-frequency system at 17 and 34 GHz.

Division of Earth Rotation
5 research sections + 2 guest research sections (1 for domestic, 1 for foreign)
Makes precise measurements of the Earth's variable rotation,
of tidal and crustal deformations, and of gravity changes;
and investigates the dynamics and internal structure of
the Earth.
Mizusawa Astrogeodynamics Observatory
Operates a 10-m VLBI radio telescope,
Earth tides station at Esashi, etc.

Astronomical Data Analysis Center
Is utilized for performing huge numerical simulations,
analyzing and archiving a vast amount of observational
data from telescopes inside and outside Japan.

Advanced Technology Center
Promotes development of astronomical observing instruments.

Office for Public Relations
and Identification of New Astronomical Objects,
Office for Calendar and Ephemeris, and Office for Standard Time
Actively provide the general public with latest astronomical
information, including responses to requests from
mass-media etc. Help identifying discoveries of new
astronomical objects by amateur astronomers. Determine
Calendar, Ephemeris and Japan Standard Time.

The number of staff in each research division is shown in
Figure 1.3.1. There has been a sharp increase in the number
of staff in the Division of Optical and Infrared Astronomy,
owing to the Subaru project. Also there is a slight increase
in the Division of Radio Astronomy, because of expansion of
new frontiers such as VLBI astronomy and sub-millimeter astronomy.

1.4 Facilities and Instruments of NAOJ

Location of Facilities

Subaru Telescope Hawaii Facility

Established in 1997, this facility takes responsibility in
the construction of the 8-m optical-infrared telescope (Subaru)
on the Mauna Kea summit, and in related research, and development
of hardware and software, etc. The Subaru aims at exploring the
first galaxy formation at a distance of 15 billion light-years,
planetary systems in our galaxy, and yet unknown outer regions
of the solar system. The First Light and test observations are
scheduled in the middle of 1998 and the full operation by 2000.

NRO: Cosmic Radio Observing Facilities

The NRO Cosmic Radio Observing Facilities have a 45-m
telescope and an interferometer array of six 10-m telescopes
(Nobeyama Millimeter Array: NMA), both of which are the
largest-scale millimeter telescopes today. The facilities
are open for research use by astronomers throughout the world.
The 45-m telescope and the NMA are, owing to high sensitivity
and image resolution,

advancing our knowledge on the interstellar matter, on the
formation of stars and protoplanetary systems, and on the
structure and evolution of galaxies as well as those of our
Milky Way Galaxy.

NRO: Solar Radio Observing Facilities

The Nobeyama Radioheliograph was completed in 1992 March
and started routine observations at 17 GHz in 1992 June.
High-spatial (10 arcsec) and temporal (up to 50 ms) resolution
imaging of the radio Sun has revealed many new and interesting
phenomena occurring in the solar atmosphere. In autumn 1995
frequency-selective subreflectors and 34-GHz receivers were
installed and dual-frequency observations started.

Norikura Solar Observatory

The Norikura Solar Observatory is located in Northern
Japan Alps, at an altitude of 2876 m above sea level. The
oldest 10-cm coronagraph has been used to measure the
brightness of the corona since 1950. A 25-cm coronagraph
with a coude focus is equipped with a large spectrograph
and a CCD detector system and has been used for spectroscopic
studies of the Sun. The newest 10-cm fully-automated coronagraph
takes digitized images of the solar corona continuously.

Okayama Astrophysical Observatory

The Okayama Astrophysical Observatory has been the center
of optical observations in Japan, operating 188-cm, 91-cm, and
65-cm telescopes. The largest reflector has been used to make
spectroscopic and photometric observations of galaxies, stars,
and solar-system objects. Photometric and spectroscopic
monitoring of variable celestial objects are carried out
using the 91-cm reflector. Solar magnetic fields are routinely
measured with the magnetograph of the 65-cm solar telescope.

Dodaira Astronomical Observatory

The Dodaira Astronomical Observatory has been used to study
variability and polarization of galaxies and stars, by using
a 91-cm reflector.Transient events like comets, novae, and
supernovae are also observed.

Mizusawa Astrogeodynamics Observatory

Observational research is made on the Earth's variable
rotation and deformation, in time scales ranging from a few
minutes to several decades, with VLBI, gravimeters, strain
meters, and tilt meters. The VLBI is also used for radio
astrometry. Theoretical studies of geodynamics are made
from VLBI, atmospheric and oceanographic data.

Advanced Technology Center

The Advanced Technology Center promotes development of
observing instruments by utilizing modern designing, measuring,
and machining facilities, with contributions by scientists
and engineers from both inside and outside NAOJ. This center
was established in 1993 on the recognition that research
and development of advanced instruments are of crucial
importance for the progress of astronomy and astrophysics.

Astronomical Data Analysis Center

Various kinds of computers (from personal- to
supercomputers) are available in the Astronomical Data
Analysis Center at Mitaka. This center has been used for
performing huge numerical simulations, and for analyzing
and archiving a vast amount of observational
data from telescopes inside and outside Japan. It also aims
at serving an important role as the center of computational
astronomy in Japan.

World Data Center for Solar Activities

The main activity of this World Data Center is to issue
the Quarterly Bulletin of Solar Activity (QBSA) based on solar
observations around the world. They include sunspot numbers,
solar flares, coronal brightness, magnetic field on the solar
surface, and radio fluxes from the Sun. Publications are
distributed to solar researchers around the world. This is
a part of the activities of the International Astronomical
Union (IAU/ICSU). Also published are solar data obtained at
NAOJ.

Facilities at Mitaka

Automatic Photoelectric Meridian Circle

A meridian circle is used to observe absolute positions
of celestial objects. The automatic photoelectric meridian
circle at Mitaka accurately measures positions of solar system
objects and of many stars in our Galaxy.It has contributed and
is still contributing to establishing the standard astronomical
coordinate systems in the framework of long-term international
cooperation.It also determines movement of celestial objects
in our Galaxy.The observation of very faint stars is performed
with a special purpose CCD camera.

Very Long Baseline Interferometry (VLBI) Correlation Center

This Center is for correlation processing of data from
the Space-VLBI
mission (VLBI Space Observatory Program: VSOP) . The VSOP
satellite was successfully launched into space in February
1997 by the Institute of Space and Astronautical Science,and
became the world-first satellite for VLBI. With superior angular
resolution, images taken with the VSOP program will be used to
investigate among others, massive black holes in active galactic
nuclei.

Solar Optical Observing Facilities

The main solar instrument at Mitaka is the Solar Flare
Telescope, which observes magnetic and velocity fields as
well as H-alpha and continuum images of the Sun's active
regions simultaneously. A new instrument for the measurement
of magnetic and velocity fields of the full solar disk was
built in 1993.As a long-term monitoring program of solar
activity, H-alpha flare patrol and visual observations of
sunspots have been conducted for more than 40 years.

Gravitational Wave Laboratory

Detection of gravitational waves will reveal new aspects
of the Universe such as the primordial cosmos, core dynamics
of the supernovae, and the surface behavior of black holes.
These cannot be observed by other means. Laser inter-
ferometric gravitational wave detectors are being developed
in this lab for the purpose of opening this new window into
the Universe. TAMA-300, an L-shaped laser interferometer with
arms 300 m long, is now under construction as shown in the
photograph.This photo shows a view of ongoing subsystem
experiment and an installed vacuum pipe (bottom left).
Experimental research is also carried out by operating a
prototype detector with 20-m long arms.

Educational Telescope for the General Public

A 50-cm reflector with a fork mount is mainly used for
public gatherings to view astronomical objects. It is operated
by the Office for Public Relations. The public gatherings are
held twice a month. It is also used for practice of astronomical
observations in university classes, visits for extracurricular
activities, and adult education classes on demand.

1.5 Recent Major Research Results in NAOJ

(1) Massive Black Hole in NGC 4258
A massive black hole, 36 million times more massive than
the Sun, has been found in the center of the spiral galaxy M106
(also known as NGC4258). This is the first and most reliable
evidence for the existence of a massive black hole.
An extremely high velocity (about 1000 km/s) water vapor
maser emission was discovered with the Nobeyama 45-m telescope
(Nakai et al., 1993). The research group used the VLBA,
collaborating with the U.S. group, to image the central
few parsecs of the nucleus of the galaxy, and found a rapidly
rotating gas disk of very small radius (0.2 pc)
(Miyoshi et al., 1995). By Keplerian rotation, the central
mass was derived. The results provided the best evidence to
date suggesting a massive black hole.
In addition, the distance to the galaxy has been measured
directly to be 6.4 Megaparsecs (21 million light years) using
the acceleration of the maser spots. This new method uses only
the Newtonian gravitation law and simple geometry in obtaining
accurate cosmical distances and is very helpful to reveal the
large scale structure of the Universe.
M. Miyoshi, N. Nakai, and M. Inoue were awarded the Nishina
Prize, the highest prize in physics in Japan.

1) Nakai, N., Inoue, M. and Miyoshi, M., "Extremely-High-Velocity
H2O Maser Emission in the Galaxy NGC4258," Nature 361 (1993) 45
2) Miyoshi, M., Moran, J., Herrnstein, J., Greenhill, L., Nakai,
N., Diamond, P. and Inoue, M., "Evidence for a Black Hole from
High Rotation Velocities in a Sub-Parsec Region of NGC4258,"
Nature 373 (1995) 127

(2) Near-IR Imaging Observations
of the Impact of the Comet Shoemaker-Levy 9 into Jupiter
The Impact of the comet Shoemaker-Levy 9 into Jupiter
in July 1994 was observed at the Okayama Astrophysical
Observatory. Using an infrared camera 'OASIS' attached
to the 188-cm telescope, a mushroom cloud after the impact
was detected successfully. Figure 1.5.2 shows that a mushroom
cloud which was bright in the near-IR appears after the impact
of fragment C (the third fragment) and then it disappeared.
Due to strong absorption by methane at low-to-middle latitudes,
Jupiter can be recognized as two arcs at the polar regions.
This detection gave very important information about gas
and dust components of the Jovian atmosphere. Since such
a clear image of the impact in the infrared light was very few,
this picture was published on many newspapers throughout the world.
The satellite in the left-hand side is Europa.

1) Takeuchi, S., Hasegawa, H., Watanabe, J., Yamashita, T.,
Abe, M., Hirota, Y., Nishihara, E., Okumura, S. and Mori, A.,
"Near-IR Imaging Observations of the Cometary Impact
into Jupiter," Geophys. Res. Letters 22 (1995) 581

(3) A Loop-Top Hard X-ray Source in a Compact Solar Flare
Yohkoh is a satellite for solar observations, launched
by the Institute of Space and Astro- nautical Science in 1991.
The solar physics group of NAOJ played a major role in instrument
development and has been actively participating in researches
based on Yohkoh data, as well as in the operation of the satellite.
One of the new findings from Yohkoh is shown in Figure 1.5.3,
in which a hard X-ray image (in contours) of a flare of 1992
January 13 is superposed on a soft X-ray image (in false color).
The solar limb is indicated with a nearly straight line.
The two hard X-ray sources are located on the limb, i.e. at
the feet of a flaring magnetic loop. In addition, one can see
another hard X-ray source above the soft X-ray loop.
This newly-discovered source can be nicely interpreted as
a result of magnetic reconnection which is believed
to be responsible for the energy release in solar flares.
The model predicts a high-speed plasma jet coming out from
the region of magnetic field reconnection, and the jet will
collide with an underlying magnetic loop and will heat the
plasma and accelerate the particles there. This discovery
has given strong evidence for the reconnection model of
solar flares.

1) Masuda, S., Kosugi, T., Hara, H., Tsuneta, S.
and Ogawara, Y., "A Loop-Top Hard X-Ray Source in a
Compact Solar Flare as Evidence
for Magnetic Reconnection," Nature 371 (1994) 495

(4) Discovery of a Silent Earthquake
One can measure slow movements of tectonic plates covering
the Earth's surface with space geodetic techniques, i.e.,
by performing precise measurements over the reference frame
composed of celestial bodies. Past observations have revealed
the velocities of such plates. However, the numbers and magnitudes
of the actual earthquakes have been pointed out to fall seriously
short of those predicted by the plate velocities. It was a serious
problem unresolved.
It was found that, for a year after the 1994 Dec. 28
Sanriku-Haruka-Oki earthquake, the GPS (Global Positioning System)
points in the northeastern Japan had undergone slow eastward
movements in addition to a sudden jump at the time of the
earthquake occurrence. This finding suggests possible existence
of silent (i.e. without earthquakes) fault slip, as large in energy
as the high-speed rupture that caused damages over the wide area
around Hachinohe city. Such a slow fault slip that is difficult
to be detected by conventional seismometric observations, might
give overall understanding about the relation between the
energy accumulated by plate motion and the energy released by
earthquake.
This work was a joint research between NAOJ and Geographical
Survey Institute.

1) Heki, K., Miyazaki, S. and Tsuji, H., "Silent Fault Slip
Following an Interplate Thrust Earthquake at the Japan Trench,"
Nature 386 (1997) 595

(5) Detection of Molecular Gas in the Quasar BR1202-0725 at Redshift z=4.69
Although great efforts have been made to locate molecular
gas -- the material out of which stars form -- in the early
Universe, there have been only two firm detections at high
redshift. Both are gravitationally lensed objects at redshift
z=2.5. Recently, CO emission from the radio-quiet quasar
BR1202-9725 at redshift z=4.96 was detected and imaged with
the Nobeyama Millimeter Array (Ohta et al., 1996).
From the observed CO luminosity, it is estimated that
molecular hydrogen of almost one hundred billion solar masses
is associated with the quasar; this is comparable to the stellar
mass of a present-day luminous galaxy. This results suggest that
BR1202-0725 is a massive galaxy, in which the gas is largely
concentrated in the central region, and that it is currently
undergoing a large burst of star formation.
This discovery provides very prominent progress in
understanding the formation and evolution of galaxies at
cosmological distances.

1) Ohta, K., Yamada, T., Nakanishi, K., Kohno, K., Akiyama, M.
and Kawabe, R., "Detection of Molecular Gas in the Quasar
BR1202 - 0725 at Redshift z = 4.69," Nature 382 (1996) 426

(6) Magnetichydrodynamic Numerical Simulation of Solar Coronal X-ray Jets
Coronal X-ray jets (sudden ejection of X-ray emitting
plasma in the solar corona) were discovered by the soft X-ray
telescope of Yohkoh. A theoretical model for the jet phenomena
in terms of the magnetic reconnection has been constructed in
the following way. A magnetic flux tube lying in the solar
convection zone becomes buoyant because of instability and
emerges into the solar atmosphere. Then the magnetic loop
may interact with the pre-existing magnetic field, and the
magnetic energy can be converted into heat and kinetic energy
of plasma by the magnetic reconnection process. The hot plasma
thus created (exceeding a few million degrees) can be identified
with the observed X-ray jets. Figure 1.5.6 shows the simulated
distribution of temperature and density resulting from the
reconnection. Superposed are magnetic field lines and velocities.
The vertical axes are heights measured from the photosphere,
in units of 200 km.

1) Yokoyama, T. and Shibata, K., "Magnetic Reconnection as the
Origin of X-Ray Jets and H-alpha Surges on the Sun,"
Nature 375 (1995) 42.

(7) Discovery of a Rotating Protoplanetary Gas Disk around the Young Star GG Tauri
Many T Tauri stars were known to be accompanied by dust
disks of 100 AU size from various observations. It is also
theoretically predicted that a planetary system forms in a
gas disk rotating around a young star. The size, however,
is very small and it has been very difficult to detect the
proto-planetary gas disks. Using the Nobeyama 45-m telescope,
Strutskie et al. (1993) observed the CO (J=1-0) emission from
a T Tauri star, GG Tauri, and found a twin-peaked line profile
which can be naturally inferred from a rotating gas disk around
the star.
Aperture synthesis CO observations of GG Tauri were made using
the Nobeyama Millimeter Array (NMA), and a rotating gas disk
having a radius of about 500 AU around the star was discovered
(Kawabe et al., 1993). The rotation velocity is 0.8 km/s at
the radius, which is roughly consistent with a Kepler rotation
around the central star. The figure indicates the rotating gas
disk; the red part indicates approaching gas, while the blue
part receding gas. These results gave a constraint to the theory
of planetary formation.

1) Strutskie, M.F., et al., "Detection of Circumstellar Gas
Associated with GG Tauri," Astrophys. J. 409 (1993) 422.
2) Kawabe, R., Ishiguro, M., Omodaka, T., Kitamura, Y.
and Miyama, S.M. "Discovery of A Rotating Protoplanetary
Gas Disk Around the Young Star GG Tauri," Astrophys. J.
Letters, 404 (1993) L63.

1.6 Statistics of Research Results

Figure 1.6.1 shows the number of papers from NAOJ. On average,
about 120 papers are published in refereed journals every year by
the scientific staff. Since many scientists in the Division of
Optical and Infrared Astronomy are now working for the
construction of Subaru, the output from this group does not
catch up with the increasing number of scientists. Among the
eight groups, the Division of Solar Physics yields a relatively
large number of papers these years, by virtue of the success of
the Yohkoh project.
Figure 1.6.2 summarizes the total number of papers between
1988 and 1996.
As shown in Figure 1.6.3, papers from NAOJ mainly appear in
international journals. Only less than a third of them are
published in domestic journals.
The number of proceedings are summarized in Figure 1.6.4.

1.7 Personnel in NAOJ

(1) Permanent Staff

(1-A) Number of Staff Members

The yearly variation of staff members in total number is
shown in Figure 1.7.1. Also shown in Figure 1.7.2 is a composition
in the research department. Since 1988 when NAOJ was established,
7 research sections have been added. An accelerated increase
since 1991 is due to the Subaru project.

(1-B) Age Distribution of Scientific and Engineering Staff

The age distribution in NAOJ has drastically changed since 1988,
as shown in Figures 1.7.3 and Figures 1.7.4. At the establishment
of NAOJ, a remarkable peak was seen in the age group of 40's.
It has now disappeared; a flat, favorable distribution has
been achieved due partially to outward movement of staff members.

(1-C) Personnel Changes

Changes of scientific staff in number is shown in
Figure 1.7.5. The plus side means movement from other
institutes and new adoption, while the minus side retirement
and movement to other institutes. On average, five members move
in every year; approximately 5% of the scientific staff members
are renewed in a year. It follows that NAOJ constantly changes
scientific staff members, suggesting that NAOJ is rather active
in personnel exchanges.

Figure 1.7.6 shows the personnel changes for promotions to
professors and associate professors. About 25 % of professors
and 33 % of associate professors are promoted from outside of
NAOJ. In the Japanese astronomical community, there are only 3
universities that have graduate courses in astronomy and
astrophysics; the number of research sections there is only
about 20. On the other hand, NAOJ has 29 research sections.
Thus the promotions to professors and associate professors
of NAOJ from outside have contributed to activate personnel
exchanges in the Japanese astronomical community.

(2) Domestic and Foreign Guest Scientists

(2-A) Domestic Guest Professors

NAOJ has 5 domestic guest research sections, which include
positions for 5 guest professors and 3 guest associate professors.
These positions are open to university professors and associate
professors, respectively. Those who are selected as guest
(associate) professors conduct research in collaboration with
NAOJ scientific staff for a term of one year. Moreover, they
sometimes contribute to graduate course education in NAOJ.

The numbers of guest (associate) professors are shown in
Figure 1.7.7; the red bar indicates those of domestic ones,
while the blue bar those of foreign ones.
There are two kinds of foreign guest scientists in NAOJ:
foreign guest professors and Center of Excellence (COE) foreign
researchers.

(2-B) Foreign Guest Professors
In 4 guest research sections for foreigners, 4 foreign
professors stay for 3-12 months and conduct research in NAOJ.

(2-C) Center of Excellence (COE) Foreign Researchers
NAOJ is regarded as a Center of Excellence institute by
the Ministry of Education and several positions for foreign
researchers are assigned to NAOJ. The salary for the COE
foreign researcher is the same as for the foreign guest
professor. COE foreign researchers also stay for 3-12
months and study in NAOJ.
The number of COE foreign researchers is shown in Figure 1.7.8.
To provide guests with comfortable stay, NAOJ has made
efforts in various fields such as assistance in the immigration
procedure, accommodations, insurance, and research environments.
Still in some cases, they meet troubles and we need further
efforts.

(3) Post Doctoral Fellows
In NAOJ, there are the following 4 categories of PDFs. The PDFs
described below are indispensable for research activities in NAOJ.
The number of PDFs is shown in Figure 1.7.9.

(3-A) Center Of Excellence (COE) Research Fellows
NAOJ has 7 COE research fellows positions. The salary of the
COE Research Fellow is comparable with that of the part-time
lecturer. Foreigners are adoptable but their air fares are not
supported. Selection of COE Research Fellows is made on an AO
(Announcement of Opportunity) basis. They participate in various
projects as do tenure-track research associates. The maximum
term is 3 years.

(3-B) NAOJ Research Fellows
Twelve positions are assigned internally in NAOJ to post-doc
researchers under the authorization by the Advisory Council for
Research and Management. Selection of NAOJ Research Fellows is
made in the individual divisions on an AO basis. The term is 2
years, extendable.

(3-C) Japan Society for the Promotion of Science (JSPS) Domestic Post Doctoral Fellows
These are the PDF of the JSPS. The total number is not fixed.
Professors or associate professors in related field individually
accept the fellows for the term of two or three years.

(3-D) JSPS Foreign Post Doctoral Fellows
The JSPS also accept PDFs from oversea. In this case,
the term is one or two years. Air fares and living expenses
in Japan are supported.

Since 1996, a new scholarship named Research Assistant has
been introduced for excellent graduate students. These assistants
are expected to conduct research under supervision of professors
or associate professors.

(4) Part-time Employees

The responsibilities of NAOJ have been increased year by year.
The Subaru and other projects have demanded many administrative
and research jobs. Owing to the limited number of permanent
positions, NAOJ has recently employed an increasing number
of part-timers, as shown in Figure 1.7.10. An urgent increase
of permanent positions is strongly desired.

1.8 Budget for NAOJ

The basic budget of NAOJ comes from the Ministry of Education.
Since 1991 when the Subaru project started, the budget has
drastically increased as shown in Figure 1.8.1. However,
the increase has not been so large in budget spent for
operations and maintenance for existing facilities as
well as for their development. The budget spent for these
amounts to about 3 billion yen, 37 % of which is for
operating and maintaining the Nobeyama Radio Observatory.

There are two other sources of research funds: Grants-in-Aid
for Scientific Research of the Ministry of Education (Fig. 1.8.2)
and scholarship donation from private companies and organizations
(Figure 1.8.3). In the past few years, the construction of 300-m
gravitational wave detector using laser interferometry has been
in progress with a big amount of newly-founded Grant-in-Aid for
a big project.

Scholarship donation from private companies is used for
hosting international conferences and for air fares to those
who attend oversea conferences and go abroad for observations.
The total amount of the donation is insufficient compared with
the demands; more efforts to obtain donation have to be made
in the future.

1.9 Administration of NAOJ

University scientists participate in the research and
management of NAOJ as summarized in Table 1.9.1.

(1) Election of Director General
The Board of Councillors elects the Director General,
taking into account advices from the Advisory Council for
Research and Management.

(2) Selection of Scientific Staff Members
New adoption and promotion of scientific staff members
are made on an AO (Announcement of Opportunity) basis and
decided by the Advisory Council for Research and Management,
based upon in-depth review in a subcommittee for personnel
selection, organized by the Advisory Council. Scientific
staff members are often adopted from outside NAOJ (e.g.,
see Figure 1.7.6).

(3) Promotion of Open Use and Joint Research
Most of the NAOJ facilities, listed below, are open
for research use by astronomers outside NAOJ: (a) radio
telescopes at Nobeyama, (b) optical-infrared telescopes
at Okayama, (c) supercomputers in Astronomical Data Analysis
Center, and so on.
Those who want to use these facilities submit proposals
to each facility, and the proposals are screened by a committee
for observation programming, which is organized for each facility
with participation of members from outside NAOJ.
The Committee for Collaborative Research is responsible for
promoting joint research programs with researchers outside NAOJ
and supporting development of technology in universities, as well
as selection of guest (associate) professors, COE Foreign
Researchers, COE Research Fellows, and NAOJ Research Fellows.
The Committee distributes three categories of subsidy on an AO
basis for domestic and international research use as follows:

1) Subsidy of collaborative development research
Researchers in universities participate in various
collaborative development researches and provide NAOJ
with resultant hardware and/or software.
2) Collaborative research
Researchers in universities conduct researches jointly
with NAOJ scientific staff members. Transportation fares
are supported.
3) Workshops (small meetings) at NAOJ
Organization of scientific meetings are financially supported.

Table 1.9.1 Organization Structure of NAOJ
(4) Internal Review and Development Planning
Research activities of individual fields and their development
plans are reviewed by the Advisory Committees, while development
plans concerning the NAOJ as a whole are reviewed by the Committee
for General Planning, as well as by the Advisory Council and the
Board of Councillors. The Phase-II Development Plan has been
prepared by taking into account discussions at and advices from
these committees.

(5) NAOJ Internal Management
The Steering Committee is organized under the Director General,

and handles daily management of NAOJ, such as budgetary issues
and settlement of internal regulations. The Committee members
are directors of individual divisions, supplemented by several
(associate) professors selected by the Faculty Council.
The Committee is held every two weeks.
The Faculty Council, consisting of professors and associate
professors, discusses and decides important internal issues such
as future plans of NAOJ, graduate course education, and budgetary
requests to the Ministry of Education. Also it selects Associate
Director, Directors of individual divisions, and so on among
the members. It meets three times a year.

2. Activities of NAOJ

2.1 Activities as an Open-Use Institute for Universities

(1) Nobeyama Radio Observatory: Cosmic Radio Observing Facilities

The open-use of the 45-m telescope began in December 1982
for 10-GHz and 40-GHz bands. A total of 52 observing proposals
were accepted for the period until March 1983. From the second
observing period (1983-1984), millimeter wave band became
available. The telescope has been widely used by foreign
researchers from its early stage.
The open use continued steadily since then, with the
telescope time for the open use increasing from 650 hours
in 1982-1983 to 2700 hours in 1987-1988 (Fig. 2.1.2.). On the
average, 45-60 proposals were accepted (Fig. 2.1.1) and 200-300
observers (including co-investigators) use the telescope
(Fig. 2.1.3) each year. Star formation and galaxies have
been the most popular research fields (Fig. 2.1.4).
A new style of observation called 'long-term observation'
was introduced in 1991-1992, and 200 hours each were allocated
for the two accepted proposals as a first step. It is for key
science programs that requires a long telescope time. It has
resulted in the discoveries of proto-planetary disks and
Galactic bulge structure.
The open use of the Nobeyama Millimeter Array (NMA)
started in 1986-1987 for 22-GHz continuum observations.
The millimeter wave open use began in 1988-1989 for 40-GHz
and 100-GHz bands with 4 array configurations. The NMA was
opened to foreign observers from 1989-1990. The number of
proposals from oversea exceeded that from inside Japan at
the beginning (Fig. 2.1.5), which is due to the fact that
the performance of NMA was the best in the world at that
time. The open use peaked in 1990-1991 with about 130
man-day (Fig. 2.1.6). In 1991 the 150-GHz band was opened
for the first time in the world at this wavelength.
(The 40-GHz band was closed, instead.)
The NMA improved by installing a new 10-m antenna;
the efficiency of aperture synthesis has greatly improved
because of the increasing number of baselines from 10 to 15.
The new NMA restarted in 1994.
The NMA has been used by researchers from oversea more
extensively than the 45-m telescope. The usage has been
declining since 1992, however. This is probably because
the performances of IRAM, OVRO, and BIMA have been greatly
improved.
The results from open use of NRO Cosmic Radio Observing
Facilities are published in scientific journals as shown
in Figure 2.1.8. On the average, including proceedings papers,
about 60 papers are published each year; the total number of
publications has amounted to 800 up to 1996.

Fig. 2.1.7

(2) Okayama Astrophysical Observatory

As an open-use optical-infrared observatory, the Okayama
Astrophysical Observatory (OAO) had been operating three
telescopes and developing observational facilities for 30
years from its foundation. Figure 2.1.9 shows the number
of observation programs using the 188-cm telescope, which
is most frequently used. The yearly average
of researchers who visit OAO is about 400 (Figure 2.1.10).
Figure 2.1.11 shows celestial objects observed with the 180-cm
telescope; stars, galaxies, and clusters of galaxies are the
most popular research fields. Scientific publications from
the open use of OAO are summarized in Figure 2.1.12, which
indicates that OAO, as the currently largest optical-infrared
observatory in Japan, has been producing a large amount of
scientific results.

(3) Nobeyama Radio Observatory: Solar Radio Observing Facilities

From June 1992, the Nobeyama Radioheliograph has been in routine
operation and obtained solar images at 17 GHz, and also at 34 GHz
since November 1996. The heliograph is fully automated. Daily
images of the radio Sun is made public through the Internet.
An on-lined data-archive service is now under construction.
From 1996, the observatory has been accepting open-use proposals
for analyzing data with a long-term stay by foreign researchers.
The number of scientific papers using data from the Nobeyama
Radioheliograph is shown in Figure 2.1.13.

(4) Norikura Solar Observatory

At the establishment of NAOJ, the open use of the 25-cm
coronagraph was not made on an AO basis, though used by
nation-wide solar physicists (Figure 2.1.14). The observatory has
made efforts to enlarge the open use by establishing a proposal
system.

(5) Mizusawa Astrogeodynamics Observatory

The Advisory Committee for Astrometry, Celestial Mechanics and
Earth Rotation selects the proposals. The number of open use is
shown in Figure 2.1.15. Details of individual open-use programs are
summarized in Figure 2.1.16. The open use of computers is the most popular.
The Esashi Earth Tides Observing Station and the Japanese VLBI network
(J-NET) are also frequently used. The Mizusawa Observatory has been
serving as the correlation center for J-NET consisting of Mizusawa
10-m telescope, Kagoshima 6-m telescope, Nobeyama 45-m telescope,
and other domestic telescopes.
The number of scientific papers from the Observatory is shown
in Figure 2.1.17.

(6) Astronomical Data Analysis Center

Astronomical Data Analysis Center was established at the same
time as NAOJ itself. Its aim is to promote the open-use of
computational facilities for researchers country-wide.
This Center is used for numerical simulations and analysis of
astronomical data. Figure 2.1.18 shows the number of researchers
that register to the Center. In the early days, a main frame
computer was a major computing facility in the Center.
Eventually workstations have become more widely used.
In 1996, a supercomputer running on the same UNIX system as
workstations was introduced; as a result, the registration has
been unified.
Figure 2.1.19 indicates the rapid increase of computational
time in 1996. This is caused by introduction of the supercomputer
system with parallel processors. Proposals requesting computational
time are screened by referees and computational time is allocated to
accepted proposals.
Many graduate students write master's and doctoral theses by
using the workstations in the Center. The number of scientific
papers and theses, to which the usage of computational facilities in
the Center has played a dominant role, is shown in Figure 2.1.20.

(7) Advanced Technology Center

With modern designing, measuring, and machining facilities,
the Advanced Technology Center promotes development of astronomical
observing instruments with contributions by scientists and engineers
from both inside and outside NAOJ. The facilities in the Center can
be open-used as follows.
(A) One may register a new project and can obtain certain space
in the Center building. The users can have access to most of the
facilities. This style (for users in Tokyo area) is most popular
(Figure 2.1.21).
(B) One may apply for specific facilities under the open-use
program of the Center.
(C) The approved users can use the workshops by themselves.

(8) Joint Development of Observing Instruments, Joint Research, and Workshop Meetings

In addition to the open use of observing facilities and
computers, NAOJ supports joint development of observing
instruments at universities, joint researches, and organization of
workshops or small scientific meetings on various themes. Proposals
of these collaborative activities are received openly and reviewed
by the Committee for Collaborative Research.
The budget for joint developments of observing instruments is
shown in Figure 2.1.22. This budget has been spent, e.g., for
the development of GRAPE, a special-purpose computer for
gravitational N-body problems, at the University of Tokyo,
and also for the development of infrared detectors at Kyoto
University. The amount of this budget has not been enough,
however.
Figure 2.1.23 shows the number of accepted proposals for
the three types of collaborative research opportunities.

2.2 Graduate Education

(1) Graduate Students in NAOJ

The NAOJ accepts the following kinds of graduate students.

(1-A) PhD Students in the Graduate University for Advanced Studies
The NAOJ has participated in the Graduate University for
Advanced Studies since 1992 as one of its fundamental research
institutes and accepted doctor course students. The number of
students in each grade is about 6, as shown by red bars in
Figure 2.2.1 and by a blue part in Figure 2.2.2.

(1-B) Graduate Students from Other Universities (Special Research Fellows)
Some of graduate students belonging to universities, shown
by yellow bars in Figure 2.2.1 and by a purple part in Figure 2.2.2,
are supervised by NAOJ (associate) professors. From a historical reason,
more than 50% of these students are from the Department of Astronomy,
the University of Tokyo.

(1-C) Research Students in the Graduate University for Advanced Studies
After awarded master's or doctor's degrees, some students
study in NAOJ as research students of the Graduate University
for Advanced Studies (shown by blue bars in Figure 2.2.1).

A total of 111 graduate students (including PDFs) stay and
conduct research in NAOJ, the composition of which is shown in
Figure 2.2.2.
Figure 2.2.3 shows the number of students who have obtained
degrees by their research work conducted with the facilities of
or data from NAOJ. The number has been increasing year by year,
a tendency caused by an increasing number of graduate students
in the Graduate University of Advanced Studies as well as in
the Department of Astronomy, the University of Tokyo.
Issues on graduate education are the responsibility of
the Committee for Graduate Education. Individual graduate
students are supervised by faculty members of the Graduate
University for Advanced Studies or the school of Science,
the University of Tokyo.

2.3 Contribution of NAOJ to Universities, Other Research Institutes, and Astronomical Societies

(1) Contribution to Universities and Other Research Institutes
Scientific staff members in NAOJ give lecture not only in
NAOJ but also in many universities as guest lecturers. This
activity is of essential importance because most of universities
in Japan lack astronomers and astrophysicists in their own
teaching staff. Also this activity helps encouraging young
undergraduate or graduate students who are interested in
astronomy and astrophysics. The lectures are mainly based
upon new results obtained by using NAOJ facilities such
as large observing telescopes and supercomputers. The number
of such lectures is shown in Figure 2.3.1.
Scientific staff members also participate in activities
in other research institutes as well as in various advisory
committees such as organized by the Ministry of Education
and by related research organizations (shown by blue bars
in Figure 2.3.2). Recently contributions to observatories
founded by local governments and by public service corporations
for promoting astronomy education to the general public have
been increasing (shown by red and green bars in Figure 2.3.2).

(2) Contribution to Astronomical Societies
The NAOJ has contributed to the development of domestic
and international astronomical societies, as the center of
astronomical research in Japan.
Scientific staff members of NAOJ have contributed in
various ways to the management of the Astronomical Society of
Japan, the Geodetic Society of Japan, and the Physical Society
of Japan. In particular, in the Astronomical Society of Japan,
they have taken responsibilities of, e.g., director, council
members, editors of the Publications of the Astronomical Society
of Japan (PASJ; an English scientific journal), and editors of
the Astronomical Herald ("Tenmon Geppou"; a Japanese journal for
the society members).
Most of scientific staff members of NAOJ are also members of
the International Astronomical Union (IAU). The IAU is composed of
many commissions, in some of which Japanese astronomers have
taken roles of presidents or vice-presidents (Figure 2.3.3).
Note that more than half of Japanese presidents or vice-presidents
have been from NAOJ. During the period of 1985-1988, Yoshihide Kozai,
former Director General of NAOJ, served as General President of IAU.
Currently for the period of 1997-2000, Norio Kaifu, Director of the
Subaru Telescope Hawaii Facilities, serves as Vice-President of IAU.

2.4 International Collaborations

The NAOJ has contributed actively to international
collaborations through various ways. Many international
conferences have been organized with participation of NAOJ
scientific staff members as scientific as well as local
organizing committee members.
Figure 2.4.1 shows the number of international conferences
in which the role of chairperson(s) was taken by NAOJ members.
Some of them were held in Japan with NAOJ as a host institute.

Figure 2.4.2 shows the sums of participants to the international
conferences held by NAOJ as a host institute.

2.5 Public Relations Activities of NAOJ

(1) Various Services for Public Relations

As the center of astronomical research in Japan, NAOJ has
been also playing a core role in introducing the Japanese
astronomical community to the general public. At the time of
establishment of NAOJ, an office of public relations was started
to take this role. This office is a small one, consisting of only
3 scientific staff members, but has conducted extensive services
by organizing observatory-wide cooperation, as mentioned below.

(1-A) Open Days for the General Public

Major campuses of NAOJ are opened to the general pubic at
least once a year.

Mitaka Campus

At the Mitaka campus, an open-house day is held on one Saturday
in the autumn. The main activities include general lectures on a
certain topic, display of panels showing latest scientific results
from NAOJ as well as from the world, and open-night for the public,
usually showing nearby celestial objects such as Moon and other
planets. Usually more than 3000 people visit the Mitaka campus on
this open-house day. (The open-house activities are a joint effort
with the Institute of Astronomy, the University of Tokyo, which
shares the same Mitaka campus with NAOJ.).
In addition, the office for public relations hosts a series
of open-nights (star watching parties; twice a month) for the
general public from April 1996, by using a new 50-cm telescope.
This series helps giving frequent opportunities to the general
public, especially to children, to enjoy watching astronomical
objects. There are about 50-150 participants every time.

Nobeyama Site

This site is open to the general public with outdoor
exhibition panels from 9:00 to 17:00 everyday. In total about
a hundred thousand people visit this site each year. Since
research facilities in buildings are closed to the general
public on usual days, an open-house day is specially held
on September 23, one of the national holidays. Public
lectures are given on this occasion. Scientific staff members,
research fellows, and graduate students respond to questions
from visitors.(Fig. 2.5.1)

Okayama Site

This site is usually open to the general public from 9:00
to 16:30 every day. Visitors can see the largest telescope from
a visitor's room next to the main dome. An astronomical museum,
which is next to this Observatory, is run by the local government.
There are many cooperative efforts for exhibitions and public
lectures between our observatory and the museum.

Mizusawa Site

An open-house day is usually held in the autumn together
with public lectures. Guided tours in the campus, including
the memorial building for Prof. Hisashi Kimura, famous for
his discovery of the Z-term in the Earth rotation from
latitudinal observation.

(1-B) Series of Public Lectures

Mitaka Public Lecture Series "Exploring the Universe"

Cooperative with the Mitaka-city education section,
a series of lectures entitled "Exploring the Universe"
has been held once a year. About 60 participants, limited by
the number of seats of NAOJ's lecture room, visit the Mitaka
campus, receive half-day lectures on recent topics in astronomy,
and enjoy a star-watching party with the 50-cm telescope in the
evening, if possible.

Public Lecture Series "Studying Astronomy"

Cooperating with the Science Museum of Tama Six Cities, a
series of lectures entitled "Studying Astronomy" is held for
children once a year. About 60-80 participants, mainly from
junior high schools, visit the Museum, have a half-day class
of elementary astronomy, and enjoy a planetarium program.

(1-C) Responses to Inquiries

Telephone Inquiries

Various questions and inquiries arrive at NAOJ from the
general public, mass-media, or official institutions by
telephone as shown in Figures 2.5.2 and 2.5.3. The Office of
Public Relations responds such calls from 9:00 to 18:00.
Since more than 9000 calls arrive at NAOJ a year, two part-time
consultants work exclusively for the response to telephone calls.

Letter Inquiries

Similarly to telephone inquiries, many inquiry letters
arrive at NAOJ, requesting answers. The Office of Public
Relations writes answers to all inquiry letters. The number of
such letters has recently increased up to about 350 a year.

Official Correspondences

The NAOJ receives official inquiries from various
organizations such as police, investigation and prosecution
office, and lawyers' offices. Most of these inquiries are
related to the time of sunrise, sunset, moonrise, moonset,
and twilight. Official correspondence has been made from
Director General with the assistance of adequate sections of
NAOJ. The number of such inquiries also increases year by year,
exceeding 50 in 1996, as shown in Fig. 2.5.4.

(1-D) Information Service

In response to strong requests from the general public,
the Office of Public Relations has recently established
information services as mentioned below.

Internet Services

The "NAO Astronews" are circulated to many institutes via
the Internet. Also the homepage service at http://www.nao.ac.jp/
began on March 21, 1996. This homepage provides information on
the NAOJ facilities and research activities, together with the
"NAO Astronews." In addition, it provides many astronomical
images that can be freely used for the educational purpose.
The images are frequently updated in the case of varying
astronomical objects such as comets. Because of this, the
homepage service is one of the most heavily accessed; the
number of hits per day is 10 thousand on the average, with
the maximum, recorded in the closest approach of comet Hale Bop,
exceeding 100 thousand (Figure 2.5.5).

Telephone and Fax Services

For science museums, public astronomical observatories,
planetariums, and high-level amateurs, we release "NAO Astronews"
every Thursday. This newsletter contains high-level science news
in the field of astronomy. When interesting new objects are found,
extra newsletters are released at a timely manner.
In cooperation with the Mitaka station of Nippon
Telecommunication & Telegram Company (NTT), the Office of
Public Relations provides voice news service. It is updated
twice a month.

(1-E) PAONET

The PAONET (Public Astronomical Observatory NETwork) was
started on November 28, 1995. The newest and most exciting
images in astronomy are supplied through this network to most
of public observatories, science museums, planetariums, and
educational centers throughout Japan. The host machine of the
PAONET, located at Mitaka, collects astronomical images from
domestic observatories and institutes as well as from foreign
sites. There are 8 sites of sub-host machines spread over Japan;
each sub-host machine obtains these images from the host machine
and provides information for the general public. By PAONET,
public observatory staffs can access most up-to-dated astronomical
images. At present 98 public observatories and institutes are
linked with PAONET.

(2) Office for Identification of New Astronomical Objects

The NAOJ receives about 60 reports a year on possible
discovery of yet unknown astronomical objects. 5-10% of them are
really identified as newly-found objects, such as comets, novae,
and supernovae. The Office for Identification of New Astronomical
Objects works for reports 24 hours a day. Figure 2.5.6 shows the
number of reports made in night-time.

(3) Office for Calendar and Ephemeris

This office compiles Calendar and Ephemeris information,
which is then made available to the general public. This office
also carries out theoretical studies of the motions of celestial
bodies in the solar system and historical studies of old Japanese
Ephemerides. Scientific staff members in the Division of
Astrometry and Celestial Mechanics are in charge of this office.

(4) Office for Standard Time

This office contributes to the maintenance of International
Atomic Time and to the determination of world-wide standard time.
In addition, it develops techniques for the precise determination
of time, and provides precise times for astronomical observations.
This office is now located in the Mizusawa campus.

2.6 Publications of NAOJ

circulation
Publications of the NAOJ Annual 1,100
NAOJ Reprint Occasional 100
Report of NAOJ* Twice a year 600
Annual Report on NAOJ* Annual 900
Overview of NAOJ* Annual 1,100
Pamphlet for NAOJ (Japanese) Annual 3,100
Pamphlet for NAOJ (English) Occasional 1,650
NAOJ News* Monthly 1,400
Annual Ephemerides* Annual 2,000
Chronological Scientific Tables* Annual 1,000 for free distribution

Mitaka Campus
Solar Vector Magnetograms Annual 150
Solar & Plasma Astrophysics Preprint Series
Occasional 250
Theoretical Astrophysics Preprint Series
Occasional 200
Technical Report on Subaru* Occasional 300
Subaru NEWS LETTER Occasional 1,500

Nobeyama Radio Observatory
NRO Report Occasional 350
NRO Technical Report (English/Japanese)
Occasional 200

Mizusawa Astrogeodynamics Observatory
Ann. Rep. Mizusawa Astrogeodyn. Obs.
Annual 300
Annual Report on Meteorology* Annual 200
Technical Report in Mizusawa Center*
Annual 300
Mizusawa News* Thrice a year 600

World Data Center for Solar Activities
Airglow Data in Japan Occasional 100
I.A.U. Quarterly Bulletin on Solar Activity
4 times a year 500
Monthly Bulletin on Solar Phenomena
Monthly 100

Astronomical Data Analysis Center
Ann. Rep. Astron. Data Analysis Center*
Annual 400

(* In Japanese; otherwise in English)

3. Present Status of Japanese Astronomy

Modern astronomy and astrophysics, which aim to understand
the universe, are sometimes compared with industrial science
directly related to production activities. From ancient times,
the universe has been stimulating an intellectual interest of
human kind. In modern societies, new understandings and concepts
brought by astronomy are acknowledged by general republic. In fact,
in newspapers and other mass-media, articles concerned with the
Universe are appearing frequently. In addition, through the
studies of the early universe and cosmic-rays, astronomy gave
strong impact on basic physics such as elementary particle
physics. Furthermore, development of astronomical observing
facilities supported by high-technology will possibly find
a new path for future investigation.

3.1 International Trend of Astronomical Research

For astronomy, the latter half of the 20th century has
been an 'era of discovery' in which new discoveries such as
the large-scale structure of the Universe, cosmic background
radiation, QSOs, black holes and so on have deepened our
understandings of the Universe. With the aid of another new
discoveries in the coming century, we will have the whole
image of the Universe and our cosmological history of human
beings. The main research targets and related research themes
are given below:

(1) The early universe and large-scale structure of the universe
Understanding the large-scale structure of the universe as
a whole. Detection of the first -generation objects in the
expanding universe. Revealing the nature of the dark matter.
Precise observation of age and expansion of the universe.

(2) Formation and evolution of Galaxies
Discovery and understandings of galaxy formation. Physical
understanding of scenarios of galaxy formation and evolution,
and active galactic nuclei.

(3) Interstellar matter and star- and planet-formation
Understandings of the formation and evolution of interstellar
matter. Revealing the process of star- and planet- formation.
Discovery of planets in other stellar systems. Understandings
of the origin and evolution of the solar system as well as the
origin of life.

(4) The late stage of evolved stars and compact objects
Understandings of supernova explosions and the formation
of neutron stars and black holes. Development of new astronomy
with neutrinos, gamma-rays, and gravitational waves.

To achieve the aims mentioned above, there seems to be the
following international trend of the development of new observing
facilities:

(1) Large ground-based observing facilities
Japan, the United States and European countries are
constructing 8-m class telescopes in optical and infrared bands.
As future plans, large radio interferometers of very high-resolution
are discussed (Japan: LMSA, USA: MMA, Europe: LSA). Furthermore,
large gravitational wave detectors are under construction (LIGO,
VIRGO).

(2) Space astronomy missions
Japan, the United States, European countries and Russia have
developed space observing facilities in gamma-rays, X-rays,
far-infrared, and submillimeter bands. In the near future, the
technologies are expected to extend to the construction of space
stations and lunar observatories. The development plan for next
generation space telescopes is under examination.

(3) Middle- and small-size observing facilities
To fulfill individual research interests, unique observing
facilities such as SDSS are under examination. In many
universities and research institutes, various middle- and
small-size observing facilities are planned, constructed, and used.

The United States and European countries promote astronomical
researches under the following circumstances:
(1) Astronomy is well recognized as a major position in
fundamental research.
(2) Many universities have small and middle-scale observing
facilities. Occasionally their scientific results are competing
with those from large-scale observing facilities.
(3) There are observational centers established independently
for each research field such as for radio astronomy, optical/IR
astronomy, and astrometry.
(4) In these research institutes, the number of engineering
staff usually exceeds scientific staff. This allows the
institutes to promote their own engineering development
without strong association with industries.
(5) In each observatory, there are enough number of
technical/engineering staff who can operate and maintain
telescopes or other kind of facilities.
(6) Public relations with observatories are intensified by
setting up museums or visitor rooms supported by dedicated staff.

3.2 Present Status of Astronomical Research in Japan

In radio astronomy, the Nobeyama Radio Observatory has been
contributing in researches on star-forming regions, galactic
structure and super-massive black hole. Groups in Nagoya
University and the University of Tokyo are promoting the
observations of northern and southern skies with small
millimeter telescopes. VLBI researches are also expanding
recently among Japanese radio astronomy communities to be
able to launch a space VLBI satelight, the first attempt
in the world, in collaboration with world-wide researchers.
In the optical-infrared wavelengths, the construction of
Subaru telescope has been the major project. Moreover, the
University of Tokyo is constructing a middle-size telescope
(MAGNUM) overseas. There is another plan of a survey telescope
in collaboration with several universities. An infrared
interferometer is now under construction at Mitaka.
The ISAS X-ray missions, although they are relatively
small scale, have been achieved many outstanding discoveries;
the Japanese researches are playing a leading role in the field
of X-ray astronomy for long periods. The solar observing satellite,
Yohkoh, together with the Nobeyama Radioheliograph, have produced
excellent results in solar plasma physics. The next-generation
solar observing satellite is now under development.
In theoretical astronomy, researchers in NAOJ and other
universities are studying in collaboration with researchers
in observational astronomy. The success of the development of
GRAPE, a special purpose computer for gravitational N-body
problems, and the recent installation of parallel supercomputers
in NAOJ would accelerate further progress in the astronomical
simulations.
NAOJ is also developing gravitational-wave detector based
on laser interferometry in collaboration with university groups.

It should be noticed that the number of astronomers amounts
to only 3 persons per 1 million population in Japan, which is
unfortunately ranked at 24th in the world (Fig. 3.2.1). The
number is too small considering the above mentioned large-scale
activities in Japan. If there are sufficient educational
courses to produce astronomers and more number of positions
for astronomical scientists in universities, the more outcomes
in the field of astronomy and astrophysics are expected. Therefore,
it should be emphasized that we need to increase the number of
researchers.
Nevertheless there are only four universities that have more
than two astronomy or astrophysical divisions (in the University
of Tokyo and in Kyoto University, six divisions; in Tohoku and
Nagoya Universities, four divisions). Osaka, Hokkaido, Ibaraki,
Tokyo Metropolitan, Niigata, Rikkyo, and Waseda Universities have
one division; however, most of them are theoretical groups. In
Japan, as a whole, the number of organizations and researchers
in astronomy is extremely small compared with the nation's
interest for the universe, with other scientific research fields
in Japan, and with the situation of astronomical research in the
world.

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