Author name code: ueda
ADS astronomy entries on 2022-09-14
author:"Ueda, Kohei"
------------------------------------------------------------------------
Title: Short-wavelength free-electron laser sources and science:
a review
Authors: Seddon, E. A.; Clarke, J. A.; Dunning, D. J.; Masciovecchio,
C.; Milne, C. J.; Parmigiani, F.; Rugg, D.; Spence, J. C. H.; Thompson,
N. R.; Ueda, K.; Vinko, S. M.; Wark, J. S.; Wurth, W.
Bibcode: 2017RPPh...80k5901S
Altcode:
This review is focused on free-electron lasers (FELs) in the hard
to soft x-ray regime. The aim is to provide newcomers to the area
with insights into: the basic physics of FELs, the qualities of the
radiation they produce, the challenges of transmitting that radiation to
end users and the diversity of current scientific applications. Initial
consideration is given to FEL theory in order to provide the foundation
for discussion of FEL output properties and the technical challenges
of short-wavelength FELs. This is followed by an overview of existing
x-ray FEL facilities, future facilities and FEL frontiers. To provide
a context for information in the above sections, a detailed comparison
of the photon pulse characteristics of FEL sources with those of other
sources of high brightness x-rays is made. A brief summary of FEL
beamline design and photon diagnostics then precedes an overview of
FEL scientific applications. Recent highlights are covered in sections
on structural biology, atomic and molecular physics, photochemistry,
non-linear spectroscopy, shock physics, solid density plasmas. A short
industrial perspective is also included to emphasise potential in
this area. Dedicated to John M J Madey (1943-2016) and Rodolfo
Bonifacio (1940-2016) whose perception, drive and perseverance paved
the way for the realisation and development of short-wavelength
free-electron lasers.
Title: Photospheric Properties of Warm EUV Loops and Hot X-Ray Loops
Authors: Kano, R.; Ueda, K.; Tsuneta, S.
Bibcode: 2014ApJ...782L..32K
Altcode:
We investigate the photospheric properties (vector magnetic fields and
horizontal velocity) of a well-developed active region, NOAA AR 10978,
using the Hinode Solar Optical Telescope specifically to determine
what gives rise to the temperature difference between "warm loops"
(1-2 MK), which are coronal loops observed in EUV wavelengths, and
"hot loops" (>3 MK), coronal loops observed in X-rays. We found
that outside sunspots, the magnetic filling factor in the solar network
varies with location and is anti-correlated with the horizontal random
velocity. If we accept that the observed magnetic features consist of
unresolved magnetic flux tubes, this anti-correlation can be explained
by the ensemble average of flux-tube motion driven by small-scale random
flows. The observed data are consistent with a flux tube width of ~77
km and horizontal flow at ~2.6 km s-1 with a spatial scale
of ~120 km. We also found that outside sunspots, there is no significant
difference between warm and hot loops either in the magnetic properties
(except for the inclination) or in the horizontal random velocity
at their footpoints, which are identified with the Hinode X-Ray
Telescope and the Transition Region and Coronal Explorer. The energy
flux injected into the coronal loops by the observed photospheric
motion of the magnetic fields is estimated to be 2 × 106
erg s-1 cm-2, which is the same for both warm and
hot loops. This suggests that coronal properties (e.g., loop length)
play a more important role in giving rise to temperature differences
of active-region coronal loops than photospheric parameters.
Title: A Sounding Rocket Experiment for Spectropolarimetric
Observations with the Lyα Line at 121.6 nm (CLASP)
Authors: Ishikawa, R.; Bando, T.; Fujimura, D.; Hara, H.; Kano,
R.; Kobiki, T.; Narukage, N.; Tsuneta, S.; Ueda, K.; Wantanabe,
H.; Kobayashi, K.; Trujillo Bueno, J.; Manso Sainz, R.; Stepan, J.;
de Pontieu, B.; Carlsson, M.; Casini, R.
Bibcode: 2011ASPC..437..287I
Altcode:
A team consisting of Japan, USA, Spain, and Norway is developing a
high-throughput Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP),
which is proposed to fly with a NASA sounding rocket in 2014. CLASP will
explore the magnetism of the upper solar chromosphere and transition
region via the Hanle effect of the Lyα line for the first
time. This experiment requires spectropolarimetric observations with
high polarimetric sensitivity (∼0.1%) and wavelength resolution
(0.1 Å). The final spatial resolution (slit width) is being discussed
taking into account the required high signal-to-noise ratio. We have
demonstrated the performance of the Lyα polarimeter by
extensively using the Ultraviolet Synchrotron ORbital Radiation Facility
(UVSOR) at the Institute for Molecular Sciences. In this contribution,
we report these measurements at UVSOR together with the current status
of the CLASP project.
Title: The Chromospheric Lyman Alpha SpectroPolarimeter (CLASP)
Authors: Kobayashi, K.; Tsuneta, S.; Trujillo Bueno, J.; Cirtain,
J. W.; Bando, T.; Kano, R.; Hara, H.; Fujimura, D.; Ueda, K.; Ishikawa,
R.; Watanabe, H.; Ichimoto, K.; Sakao, T.; de Pontieu, B.; Carlsson,
M.; Casini, R.
Bibcode: 2010AGUFMSH11B1632K
Altcode:
Magnetic fields in the solar chromosphere play a key role in the
energy transfer and dynamics of the solar atmosphere. Yet a direct
observation of the chromospheric magnetic field remains one of the
greatest challenges in solar physics. While some advances have been
made for observing the Zeeman effect in strong chromospheric lines,
the effect is small and difficult to detect outside sunspots. The
Hanle effect offers a promising alternative; it is sensitive to weaker
magnetic fields (e.g., 5-500 G for Ly-Alpha), and while its magnitude
saturates at stronger magnetic fields, the linear polarization signals
remain sensitive to the magnetic field orientation. The Hanle effect
is not only limited to off-limb observations. Because the chromosphere
is illuminated by an anisotropic radiation field, the Ly-Alpha line is
predicted to show linear polarization for on-disk, near-limb regions,
and magnetic field is predicted to cause a measurable depolarization. At
disk center, the Ly-Alpha radiation is predicted to be negligible
in the absence of magnetic field, and linearly polarized to an order
of 0.3% in the presence of an inclined magnetic field. The proposed
CLASP sounding rocket instrument is designed to detect 0.3% linear
polarization of the Ly-Alpha line at 1.5 arcsecond spatial resolution
(0.7’’ pixel size) and 10 pm spectral resolution. The instrument
consists of a 30 cm aperture Cassegrain telescope and a dual-beam
spectropolarimeter. The telescope employs a ``cold mirror’’ design
that uses multilayer coatings to reflect only the target wavelength
range into the spectropolarimeter. The polarization analyzer consists of
a rotating waveplate and a polarizing beamsplitter that comprises MgF2
plates placed at Brewster’s Angle. Each output beam of the polarizing
beamsplitter, representing two orthogonal linear polarizations, is
dispersed and focused using a separate spherical varied-line-space
grating, and imaged with a separate 512x512 CCD camera. Prototypes
of key optical components have been fabricated and tested. Instrument
design is being finalized, and the experiment will be proposed for a
2014 flight aboard a NASA sounding rocket.
Title: Orientation of X-Ray Bright Points in the Quiet Sun
Authors: Ueda, K.; Kano, R.; Tsuneta, S.; Shibahashi, H.
Bibcode: 2010SoPh..261...77U
Altcode:
Thanks to the high-resolution images from the X-ray telescope (XRT)
aboard the Hinode satellite, X-ray bright points (XBPs) in the quiet
region of the Sun are resolved and can be seen to have complex loop-like
structures. We measure the orientation of such loop structures for 488
XBPs picked up in 26 snapshot X-ray images near the disk center. The
distribution of the orientation is slightly but clearly biased to
the east - west direction: the random distribution is rejected with a
significance level of 1% by the χ2-test. The distribution
is similar to the orientation distribution for the bipolar magnetic
fields. The XBP orientation is, however, much more random than that
of the bipolar magnetic fields with similar size. 24% of the XBPs are
due to emerging bipoles, while the remaining 76% are due to chance
encounters of opposite polarities.
Title: Stellar-Mass Black Holes and Their Progenitors
Authors: Miller, J.; Uttley; Nandra; Barret; Paerels; Mandez;
Diaz; Cappi; Kitamoto; Nowak; Wilms; Rothschild; Smith; Weisskopf;
Teraschima; Ueda
Bibcode: 2009astro2010S.207M
Altcode: 2009arXiv0902.4677M
If a black hole has a low spin value, it must double its mass to
reach a high spin parameter. Although this is easily accomplished
through mergers or accretion in the case of supermassive black holes
in galactic centers, it is impossible for stellar-mass black holes
in X-ray binaries. Thus, the spin distribution of stellar-mass black
holes is almost pristine, largely reflective of the angular momentum
imparted at the time of their creation. This fact can help provide
insights on two fundamental questions: What is the nature of the
central engine in supernovae and gamma-ray bursts? and What was the
spin distribution of the first black holes in the universe?
Title: DECIGO pathfinder
Authors: Ando, M.; Kawamura, S.; Nakamura, T.; Tsubono, K.; Tanaka,
T.; Funaki, I.; Seto, N.; Numata, K.; Sato, S.; Ioka, K.; Kanda,
N.; Takashima, T.; Agatsuma, K.; Akutsu, T.; Akutsu, T.; Aoyanagi,
K. -s.; Arai, K.; Arase, Y.; Araya, A.; Asada, H.; Aso, Y.; Chiba,
T.; Ebisuzaki, T.; Enoki, M.; Eriguchi, Y.; Fujimoto, M. -K.; Fujita,
R.; Fukushima, M.; Futamase, T.; Ganzu, K.; Harada, T.; Hashimoto,
T.; Hayama, K.; Hikida, W.; Himemoto, Y.; Hirabayashi, H.; Hiramatsu,
T.; Hong, F. -L.; Horisawa, H.; Hosokawa, M.; Ichiki, K.; Ikegami, T.;
Inoue, K. T.; Ishidoshiro, K.; Ishihara, H.; Ishikawa, T.; Ishizaki,
H.; Ito, H.; Itoh, Y.; Kamagasako, S.; Kawashima, N.; Kawazoe, F.;
Kirihara, H.; Kishimoto, N.; Kiuchi, K.; Kobayashi, S.; Kohri, K.;
Koizumi, H.; Koima, Y.; Kokeyama, K.; W-Kokuyama; Kotake, K.; Kozai,
Y.; Kudoh, H.; Kunimori, H.; Kuninaka, H.; Kuroda, K.; Maeda, K. -i.;
Matsuhara, H.; Mino, Y.; Miyakawa, O.; Miyoki, S.; Morimoto, M. Y.;
Morioka, T.; Morisawa, T.; Moriwaki, S.; Mukohyama, S.; Musha, M.;
Nagano, S.; Naito, I.; Nakagawa, N.; Nakamura, K.; Nakano, H.; Nakao,
K.; Nakasuka, S.; Nakayama, Y.; Nishida, E.; Nishiyama, K.; Nishizawa,
A.; Niwa, Y.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Okutomi, A.; Onozato,
K.; Oohara, K.; Sago, N.; Saijo, M.; Sakagami, M.; Sakai, S. -i.;
Sakata, S.; Sasaki, M.; Sato, T.; Shibata, M.; Shinkai, H.; Somiya,
K.; Sotani, H.; Sugiyama, N.; Suwa, Y.; Tagoshi, H.; Takahashi, K.;
Takahashi, K.; Takahashi, T.; Takahashi, H.; Takahashi, R.; Takahashi,
R.; Takamori, A.; Takano, T.; Taniguchi, K.; Taruya, A.; Tashiro, H.;
Tokuda, M.; Tokunari, M.; Toyoshima, M.; Tsujikawa, S.; Tsunesada,
Y.; Ueda, K. -i.; Utashima, M.; Yamakawa, H.; Yamamoto, K.; Yamazaki,
T.; Yokoyama, J.; Yoo, C. -M.; Yoshida, S.; Yoshino, T.
Bibcode: 2008JPhCS.120c2005A
Altcode:
DECIGO pathfinder (DPF) is a milestone satellite mission for DECIGO
(DECi-hertz Interferometer Gravitational wave Observatory) which is a
future space gravitational wave antenna. DECIGO is expected to provide
us fruitful insights into the universe, in particular about dark energy,
a formation mechanism of supermassive black holes, and the inflation
of the universe. Since DECIGO will be an extremely large mission which
will formed by three drag-free spacecraft with 1000m separation, it
is significant to gain the technical feasibility of DECIGO before its
planned launch in 2024. Thus, we are planning to launch two milestone
missions: DPF and pre-DECIGO. The conceptual design and current status
of the first milestone mission, DPF, are reviewed in this article.
Title: The Japanese space gravitational wave antenna; DECIGO
Authors: Kawamura, S.; Ando, M.; Nakamura, T.; Tsubono, K.; Tanaka,
T.; Funaki, I.; Seto, N.; Numata, K.; Sato, S.; Ioka, K.; Kanda,
N.; Takashima, T.; Agatsuma, K.; Akutsu, T.; Akutsu, T.; Aoyanagi,
K. -s.; Arai, K.; Arase, Y.; Araya, A.; Asada, H.; Aso, Y.; Chiba,
T.; Ebisuzaki, T.; Enoki, M.; Eriguchi, Y.; Fujimoto, M. -K.; Fujita,
R.; Fukushima, M.; Futamase, T.; Ganzu, K.; Harada, T.; Hashimoto,
T.; Hayama, K.; Hikida, W.; Himemoto, Y.; Hirabayashi, H.; Hiramatsu,
T.; Hong, F. -L.; Horisawa, H.; Hosokawa, M.; Ichiki, K.; Ikegami, T.;
Inoue, K. T.; Ishidoshiro, K.; Ishihara, H.; Ishikawa, T.; Ishizaki,
H.; Ito, H.; Itoh, Y.; Kamagasako, S.; Kawashima, N.; Kawazoe, F.;
Kirihara, H.; Kishimoto, N.; Kiuchi, K.; Kobayashi, S.; Kohri, K.;
Koizumi, H.; Kojima, Y.; Kokeyama, K.; Kokuyama, W.; Kotake, K.; Kozai,
Y.; Kudoh, H.; Kunimori, H.; Kuninaka, H.; Kuroda, K.; Maeda, K. -i.;
Matsuhara, H.; Mino, Y.; Miyakawa, O.; Miyoki, S.; Morimoto, M. Y.;
Morioka, T.; Morisawa, T.; Moriwaki, S.; Mukohyama, S.; Musha, M.;
Nagano, S.; Naito, I.; Nakagawa, N.; Nakamura, K.; Nakano, H.; Nakao,
K.; Nakasuka, S.; Nakayama, Y.; Nishida, E.; Nishiyama, K.; Nishizawa,
A.; Niwa, Y.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Okutomi, A.; Onozato,
K.; Oohara, K.; Sago, N.; Saijo, M.; Sakagami, M.; Sakai, S. -i.;
Sakata, S.; Sasaki, M.; Sato, T.; Shibata, M.; Shinkai, H.; Somiya,
K.; Sotani, H.; Sugiyama, N.; Suwa, Y.; Tagoshi, H.; Takahashi, K.;
Takahashi, K.; Takahashi, T.; Takahashi, H.; Takahashi, R.; Takahashi,
R.; Takamori, A.; Takano, T.; Taniguchi, K.; Taruya, A.; Tashiro, H.;
Tokuda, M.; Tokunari, M.; Toyoshima, M.; Tsujikawa, S.; Tsunesada,
Y.; Ueda, K. -i.; Utashima, M.; Yamakawa, H.; Yamamoto, K.; Yamazaki,
T.; Yokoyama, J.; Yoo, C. -M.; Yoshida, S.; Yoshino, T.
Bibcode: 2008JPhCS.120c2004K
Altcode:
DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the
future Japanese space gravitational wave antenna. DECIGO is expected
to open a new window of observation for gravitational wave astronomy
especially between 0.1 Hz and 10 Hz, revealing various mysteries of
the universe such as dark energy, formation mechanism of supermassive
black holes, and inflation of the universe. The pre-conceptual design
of DECIGO consists of three drag-free spacecraft, whose relative
displacements are measured by a differential Fabry-Perot Michelson
interferometer. We plan to launch two missions, DECIGO pathfinder and
pre-DECIGO first and finally DECIGO in 2024.
Title: The Japanese space gravitational wave antenna - DECIGO
Authors: Kawamura, S.; Ando, M.; Nakamura, T.; Tsubono, K.; Tanaka,
T.; Funaki, I.; Seto, N.; Numata, K.; Sato, S.; Ioka, K.; Kanda,
N.; Takashima, T.; Agatsuma, K.; Akutsu, T.; Akutsu, T.; Aoyanagi,
Koh-Suke; Arai, K.; Arase, Y.; Araya, A.; Asada, H.; Aso, Y.; Chiba,
T.; Ebisuzaki, T.; Enoki, M.; Eriguchi, Y.; Fujimoto, M. -K.; Fujita,
R.; Fukushima, M.; Futamase, T.; Ganzu, K.; Harada, T.; Hashimoto,
T.; Hayama, K.; Hikida, W.; Himemoto, Y.; Hirabayashi, H.; Hiramatsu,
T.; Hong, F. -L.; Horisawa, H.; Hosokawa, M.; Ichiki, K.; Ikegami, T.;
Inoue, K. T.; Ishidoshiro, K.; Ishihara, H.; Ishikawa, T.; Ishizaki,
H.; Ito, H.; Itoh, Y.; Kamagasako, S.; Kawashima, N.; Kawazoe, F.;
Kirihara, H.; Kishimoto, N.; Kiuchi, K.; Kobayashi, S.; Kohri, K.;
Koizumi, H.; Kojima, Y.; Kokeyama, K.; Kokuyama, W.; Kotake, K.; Kozai,
Y.; Kudoh, H.; Kunimori, H.; Kuninaka, H.; Kuroda, K.; Maeda, K. -i.;
Matsuhara, H.; Mino, Y.; Miyakawa, O.; Miyoki, S.; Morimoto, M. Y.;
Morioka, T.; Morisawa, T.; Moriwaki, S.; Mukohyama, S.; Musha, M.;
Nagano, S.; Naito, I.; Nakagawa, N.; Nakamura, K.; Nakano, H.; Nakao,
K.; Nakasuka, S.; Nakayama, Y.; Nishida, E.; Nishiyama, K.; Nishizawa,
A.; Niwa, Y.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Okutomi, A.; Onozato,
K.; Oohara, K.; Sago, N.; Saijo, M.; Sakagami, M.; Sakai, S. -i.;
Sakata, S.; Sasaki, M.; Sato, T.; Shibata, M.; Shinkai, H.; Somiya,
K.; Sotani, H.; Sugiyama, N.; Suwa, Y.; Tagoshi, H.; Takahashi, K.;
Takahashi, K.; Takahashi, T.; Takahashi, H.; Takahashi, R.; Takahashi,
R.; Takamori, A.; Takano, T.; Taniguchi, K.; Taruya, A.; Tashiro, H.;
Tokuda, M.; Tokunari, M.; Toyoshima, M.; Tsujikawa, S.; Tsunesada,
Y.; Ueda, K. -i.; Utashima, M.; Yamakawa, H.; Yamamoto, K.; Yamazaki,
T.; Yokoyama, J.; Yoo, C. -M.; Yoshida, S.; Yoshino, T.
Bibcode: 2008JPhCS.122a2006K
Altcode:
DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the
future Japanese space gravitational wave antenna. The goal of DECIGO
is to detect gravitational waves from various kinds of sources mainly
between 0.1 Hz and 10 Hz and thus to open a new window of observation
for gravitational wave astronomy. DECIGO will consist of three drag-free
spacecraft, 1000 km apart from each other, whose relative displacements
are measured by a Fabry—Perot Michelson interferometer. We plan to
launch DECIGO pathfinder first to demonstrate the technologies required
to realize DECIGO and, if possible, to detect gravitational waves from
our galaxy or nearby galaxies.
Title: Joint LIGO and TAMA300 search for gravitational waves from
inspiralling neutron star binaries
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Ageev, A.; Agresti, J.;
Ajith, P.; Allen, B.; Allen, J.; Amin, R.; Anderson, S. B.; Anderson,
W. G.; Araya, M.; Armandula, H.; Ashley, M.; Asiri, F.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Balasubramanian, R.; Ballmer, S.; Barish,
B. C.; Barker, C.; Barker, D.; Barnes, M.; Barr, B.; Barton, M. A.;
Bayer, K.; Beausoleil, R.; Belczynski, K.; Bennett, R.; Berukoff,
S. J.; Betzwieser, J.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.;
Black, E.; Blackburn, K.; Blackburn, L.; Bland, B.; Bochner, B.;
Bogue, L.; Bork, R.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau,
J. E.; Brown, D. A.; Bullington, A.; Bunkowski, A.; Buonanno, A.;
Burgess, R.; Busby, D.; Butler, W. E.; Byer, R. L.; Cadonati, L.;
Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.;
Cao, J.; Cardenas, L.; Carter, K.; Casey, M. M.; Castiglione, J.;
Chandler, A.; Chapsky, J.; Charlton, P.; Chatterji, S.; Chelkowski,
S.; Chen, Y.; Chickarmane, V.; Chin, D.; Christensen, N.; Churches,
D.; Cokelaer, T.; Colacino, C.; Coldwell, R.; Coles, M.; Cook, D.;
Corbitt, T.; Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Crooks,
D. R. M.; Csatorday, P.; Cusack, B. J.; Cutler, C.; Dalrymple, J.;
D'Ambrosio, E.; Danzmann, K.; Davies, G.; Daw, E.; Debra, D.; Delker,
T.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar, S.; di Credico,
A.; Díaz, M.; Ding, H.; Drever, R. W. P.; Dupuis, R. J.; Edlund,
J. A.; Ehrens, P.; Elliffe, E. J.; Etzel, T.; Evans, M.; Evans, T.;
Fairhurst, S.; Fallnich, C.; Farnham, D.; Fejer, M. M.; Findley, T.;
Fine, M.; Finn, L. S.; Franzen, K. Y.; Freise, A.; Frey, R.; Fritschel,
P.; Frolov, V. V.; Fyffe, M.; Ganezer, K. S.; Garofoli, J.; Giaime,
J. A.; Gillespie, A.; Goda, K.; Goggin, L.; González, G.; Goßler, S.;
Grandclément, P.; Grant, A.; Gray, C.; Gretarsson, A. M.; Grimmett,
D.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, E.; Gustafson,
R.; Hamilton, W. O.; Hammond, M.; Hanna, C.; Hanson, J.; Hardham,
C.; Harms, J.; Harry, G.; Hartunian, A.; Heefner, J.; Hefetz, Y.;
Heinzel, G.; Heng, I. S.; Hennessy, M.; Hepler, N.; Heptonstall, A.;
Heurs, M.; Hewitson, M.; Hild, S.; Hindman, N.; Hoang, P.; Hough, J.;
Hrynevych, M.; Hua, W.; Ito, M.; Itoh, Y.; Ivanov, A.; Jennrich, O.;
Johnson, B.; Johnson, W. W.; Johnston, W. R.; Jones, D. I.; Jones, G.;
Jones, L.; Jungwirth, D.; Kalogera, V.; Katsavounidis, E.; Kawabe,
K.; Kells, W.; Kern, J.; Khan, A.; Killbourn, S.; Killow, C. J.;
Kim, C.; King, C.; King, P.; Klimenko, S.; Koranda, S.; Kötter,
K.; Kovalik, J.; Kozak, D.; Krishnan, B.; Landry, M.; Langdale,
J.; Lantz, B.; Lawrence, R.; Lazzarini, A.; Lei, M.; Leonor, I.;
Libbrecht, K.; Libson, A.; Lindquist, P.; Liu, S.; Logan, J.; Lormand,
M.; Lubiński, M.; Lück, H.; Luna, M.; Lyons, T. T.; Machenschalk,
B.; Macinnis, M.; Mageswaran, M.; Mailand, K.; Majid, W.; Malec,
M.; Mandic, V.; Mann, F.; Marin, A.; Márka, S.; Maros, E.; Mason,
J.; Mason, K.; Matherny, O.; Matone, L.; Mavalvala, N.; McCarthy,
R.; McClelland, D. E.; McHugh, M.; McNabb, J. W. C.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki, E.; Messenger,
C.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.;
Mittleman, R.; Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.;
Mueller, G.; Mukherjee, S.; Murray, P.; Myers, E.; Myers, J.; Nagano,
S.; Nash, T.; Nayak, R.; Newton, G.; Nocera, F.; Noel, J. S.; Nutzman,
P.; Olson, T.; O'Reilly, B.; Ottaway, D. J.; Ottewill, A.; Ouimette,
D.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah,
V.; Parameswariah, C.; Pedraza, M.; Penn, S.; Pitkin, M.; Plissi,
M.; Prix, R.; Quetschke, V.; Raab, F.; Radkins, H.; Rahkola, R.;
Rakhmanov, M.; Rao, S. R.; Rawlins, K.; Ray-Majumder, S.; Re, V.;
Redding, D.; Regehr, M. W.; Regimbau, T.; Reid, S.; Reilly, K. T.;
Reithmaier, K.; Reitze, D. H.; Richman, S.; Riesen, R.; Riles, K.;
Rivera, B.; Rizzi, A.; Robertson, D. I.; Robertson, N. A.; Robinson,
C.; Robison, L.; Roddy, S.; Rodriguez, A.; Rollins, J.; Romano, J. D.;
Romie, J.; Rong, H.; Rose, D.; Rotthoff, E.; Rowan, S.; Rüdiger, A.;
Ruet, L.; Russell, P.; Ryan, K.; Salzman, I.; Sandberg, V.; Sanders,
G. H.; Sannibale, V.; Sarin, P.; Sathyaprakash, B.; Saulson, P. R.;
Savage, R.; Sazonov, A.; Schilling, R.; Schlaufman, K.; Schmidt, V.;
Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Seader, S. E.; Searle, A. C.; Sears, B.; Seel, S.; Seifert, F.;
Sellers, D.; Sengupta, A. S.; Shapiro, C. A.; Shawhan, P.; Shoemaker,
D. H.; Shu, Q. Z.; Sibley, A.; Siemens, X.; Sievers, L.; Sigg, D.;
Sintes, A. M.; Smith, J. R.; Smith, M.; Smith, M. R.; Sneddon, P. H.;
Spero, R.; Spjeld, O.; Stapfer, G.; Steussy, D.; Strain, K. A.; Strom,
D.; Stuver, A.; Summerscales, T.; Sumner, M. C.; Sung, M.; Sutton,
P. J.; Sylvestre, J.; Tanner, D. B.; Tariq, H.; Tarallo, M.; Taylor,
I.; Taylor, R.; Taylor, R.; Thorne, K. A.; Thorne, K. S.; Tibbits,
M.; Tilav, S.; Tinto, M.; Tokmakov, K. V.; Torres, C.; Torrie, C.;
Traylor, G.; Tyler, W.; Ugolini, D.; Ungarelli, C.; Vallisneri,
M.; van Putten, M.; Vass, S.; Vecchio, A.; Veitch, J.; Vorvick, C.;
Vyachanin, S. P.; Wallace, L.; Walther, H.; Ward, H.; Ward, R.; Ware,
B.; Watts, K.; Webber, D.; Weidner, A.; Weiland, U.; Weinstein, A.;
Weiss, R.; Welling, H.; Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.;
Whitcomb, S. E.; Whiting, B. F.; Wiley, S.; Wilkinson, C.; Willems,
P. A.; Williams, P. R.; Williams, R.; Willke, B.; Wilson, A.; Winjum,
B. J.; Winkler, W.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.;
Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yoshida,
S.; Zaleski, K. D.; Zanolin, M.; Zawischa, I.; Zhang, L.; Zhu, R.;
Zotov, N.; Zucker, M.; Zweizig, J.; Akutsu, T.; Akutsu, T.; Ando, M.;
Arai, K.; Araya, A.; Asada, H.; Aso, Y.; Beyersdorf, P.; Fujiki, Y.;
Fujimoto, M. -K.; Fujita, R.; Fukushima, M.; Futamase, T.; Hamuro, Y.;
Haruyama, T.; Hayama, K.; Iguchi, H.; Iida, Y.; Ioka, K.; Ishitsuka,
H.; Kamikubota, N.; Kanda, N.; Kaneyama, T.; Karasawa, Y.; Kasahara,
K.; Kasai, T.; Katsuki, M.; Kawamura, S.; Kawamura, M.; Kawazoe, F.;
Kojima, Y.; Kokeyama, K.; Kondo, K.; Kozai, Y.; Kudoh, H.; Kuroda,
K.; Kuwabara, T.; Matsuda, N.; Mio, N.; Miura, K.; Miyama, S.; Miyoki,
S.; Mizusawa, H.; Moriwaki, S.; Musha, M.; Nagayama, Y.; Nakagawa, K.;
Nakamura, T.; Nakano, H.; Nakao, K.; Nishi, Y.; Numata, K.; Ogawa, Y.;
Ohashi, M.; Ohishi, N.; Okutomi, A.; Oohara, K.; Otsuka, S.; Saito,
Y.; Sakata, S.; Sasaki, M.; Sato, N.; Sato, S.; Sato, Y.; Sato, K.;
Sekido, A.; Seto, N.; Shibata, M.; Shinkai, H.; Shintomi, T.; Soida,
K.; Somiya, K.; Suzuki, T.; Tagoshi, H.; Takahashi, H.; Takahashi,
R.; Takamori, A.; Takemoto, S.; Takeno, K.; Tanaka, T.; Taniguchi,
K.; Tanji, T.; Tatsumi, D.; Telada, S.; Tokunari, M.; Tomaru, T.;
Tsubono, K.; Tsuda, N.; Tsunesada, Y.; Uchiyama, T.; Ueda, K.; Ueda,
A.; Waseda, K.; Yamamoto, A.; Yamamoto, K.; Yamazaki, T.; Yanagi,
Y.; Yokoyama, J.; Yoshida, T.; Zhu, Z. -H.
Bibcode: 2006PhRvD..73j2002A
Altcode: 2005gr.qc....12078L
We search for coincident gravitational wave signals from inspiralling
neutron star binaries using LIGO and TAMA300 data taken during
early 2003. Using a simple trigger exchange method, we perform an
intercollaboration coincidence search during times when TAMA300 and
only one of the LIGO sites were operational. We find no evidence of
any gravitational wave signals. We place an observational upper limit
on the rate of binary neutron star coalescence with component masses
between 1 and 3M⊙ of 49 per year per Milky Way equivalent
galaxy at a 90% confidence level. The methods developed during this
search will find application in future network inspiral analyses.
Title: Upper limits from the LIGO and TAMA detectors on the rate of
gravitational-wave bursts
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Ageev, A.; Agresti, J.;
Ajith, P.; Allen, B.; Allen, J.; Amin, R.; Anderson, S. B.; Anderson,
W. G.; Araya, M.; Armandula, H.; Ashley, M.; Asiri, F.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Balasubramanian, R.; Ballmer, S.; Barish,
B. C.; Barker, C.; Barker, D.; Barnes, M.; Barr, B.; Barton, M. A.;
Bayer, K.; Beausoleil, R.; Belczynski, K.; Bennett, R.; Berukoff,
S. J.; Betzwieser, J.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.;
Black, E.; Blackburn, K.; Blackburn, L.; Bland, B.; Bochner, B.;
Bogue, L.; Bork, R.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau,
J. E.; Brown, D. A.; Bullington, A.; Bunkowski, A.; Buonanno, A.;
Burgess, R.; Busby, D.; Butler, W. E.; Byer, R. L.; Cadonati, L.;
Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.;
Cao, J.; Cardenas, L.; Carter, K.; Casey, M. M.; Castiglione, J.;
Chandler, A.; Chapsky, J.; Charlton, P.; Chatterji, S.; Chelkowski,
S.; Chen, Y.; Chickarmane, V.; Chin, D.; Christensen, N.; Churches,
D.; Cokelaer, T.; Colacino, C.; Coldwell, R.; Coles, M.; Cook, D.;
Corbitt, T.; Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Crooks,
D. R. M.; Csatorday, P.; Cusack, B. J.; Cutler, C.; Dalrymple, J.;
D'Ambrosio, E.; Danzmann, K.; Davies, G.; Daw, E.; Debra, D.; Delker,
T.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar, S.; di Credico,
A.; Díaz, M.; Ding, H.; Drever, R. W. P.; Dupuis, R. J.; Edlund,
J. A.; Ehrens, P.; Elliffe, E. J.; Etzel, T.; Evans, M.; Evans, T.;
Fairhurst, S.; Fallnich, C.; Farnham, D.; Fejer, M. M.; Findley, T.;
Fine, M.; Finn, L. S.; Franzen, K. Y.; Freise, A.; Frey, R.; Fritschel,
P.; Frolov, V. V.; Fyffe, M.; Ganezer, K. S.; Garofoli, J.; Giaime,
J. A.; Gillespie, A.; Goda, K.; Goggin, L.; González, G.; Goßler, S.;
Grandclément, P.; Grant, A.; Gray, C.; Gretarsson, A. M.; Grimmett,
D.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, E.; Gustafson,
R.; Hamilton, W. O.; Hammond, M.; Hanna, C.; Hanson, J.; Hardham,
C.; Harms, J.; Harry, G.; Hartunian, A.; Heefner, J.; Hefetz, Y.;
Heinzel, G.; Heng, I. S.; Hennessy, M.; Hepler, N.; Heptonstall, A.;
Heurs, M.; Hewitson, M.; Hild, S.; Hindman, N.; Hoang, P.; Hough, J.;
Hrynevych, M.; Hua, W.; Ito, M.; Itoh, Y.; Ivanov, A.; Jennrich, O.;
Johnson, B.; Johnson, W. W.; Johnston, W. R.; Jones, D. I.; Jones, G.;
Jones, L.; Jungwirth, D.; Kalogera, V.; Katsavounidis, E.; Kawabe,
K.; Kells, W.; Kern, J.; Khan, A.; Killbourn, S.; Killow, C. J.;
Kim, C.; King, C.; King, P.; Klimenko, S.; Koranda, S.; Kötter,
K.; Kovalik, J.; Kozak, D.; Krishnan, B.; Landry, M.; Langdale,
J.; Lantz, B.; Lawrence, R.; Lazzarini, A.; Lei, M.; Leonor, I.;
Libbrecht, K.; Libson, A.; Lindquist, P.; Liu, S.; Logan, J.; Lormand,
M.; Lubiński, M.; Lück, H.; Luna, M.; Lyons, T. T.; Machenschalk,
B.; Macinnis, M.; Mageswaran, M.; Mailand, K.; Majid, W.; Malec,
M.; Mandic, V.; Mann, F.; Marin, A.; Márka, S.; Maros, E.; Mason,
J.; Mason, K.; Matherny, O.; Matone, L.; Mavalvala, N.; McCarthy,
R.; McClelland, D. E.; McHugh, M.; McNabb, J. W. C.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki, E.; Messenger,
C.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.;
Mittleman, R.; Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.;
Mueller, G.; Mukherjee, S.; Murray, P.; Myers, E.; Myers, J.; Nagano,
S.; Nash, T.; Nayak, R.; Newton, G.; Nocera, F.; Noel, J. S.; Nutzman,
P.; Olson, T.; O'Reilly, B.; Ottaway, D. J.; Ottewill, A.; Ouimette,
D.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah,
V.; Parameswariah, C.; Pedraza, M.; Penn, S.; Pitkin, M.; Plissi,
M.; Prix, R.; Quetschke, V.; Raab, F.; Radkins, H.; Rahkola, R.;
Rakhmanov, M.; Rao, S. R.; Rawlins, K.; Ray-Majumder, S.; Re, V.;
Redding, D.; Regehr, M. W.; Regimbau, T.; Reid, S.; Reilly, K. T.;
Reithmaier, K.; Reitze, D. H.; Richman, S.; Riesen, R.; Riles, K.;
Rivera, B.; Rizzi, A.; Robertson, D. I.; Robertson, N. A.; Robinson,
C.; Robison, L.; Roddy, S.; Rodriguez, A.; Rollins, J.; Romano, J. D.;
Romie, J.; Rong, H.; Rose, D.; Rotthoff, E.; Rowan, S.; Rüdiger, A.;
Ruet, L.; Russell, P.; Ryan, K.; Salzman, I.; Sandberg, V.; Sanders,
G. H.; Sannibale, V.; Sarin, P.; Sathyaprakash, B.; Saulson, P. R.;
Savage, R.; Sazonov, A.; Schilling, R.; Schlaufman, K.; Schmidt, V.;
Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Seader, S. E.; Searle, A. C.; Sears, B.; Seel, S.; Seifert, F.;
Sellers, D.; Sengupta, A. S.; Shapiro, C. A.; Shawhan, P.; Shoemaker,
D. H.; Shu, Q. Z.; Sibley, A.; Siemens, X.; Sievers, L.; Sigg, D.;
Sintes, A. M.; Smith, J. R.; Smith, M.; Smith, M. R.; Sneddon, P. H.;
Spero, R.; Spjeld, O.; Stapfer, G.; Steussy, D.; Strain, K. A.; Strom,
D.; Stuver, A.; Summerscales, T.; Sumner, M. C.; Sung, M.; Sutton,
P. J.; Sylvestre, J.; Tanner, D. B.; Tariq, H.; Tarallo, M.; Taylor,
I.; Taylor, R.; Taylor, R.; Thorne, K. A.; Thorne, K. S.; Tibbits,
M.; Tilav, S.; Tinto, M.; Tokmakov, K. V.; Torres, C.; Torrie, C.;
Traylor, G.; Tyler, W.; Ugolini, D.; Ungarelli, C.; Vallisneri,
M.; van Putten, M.; Vass, S.; Vecchio, A.; Veitch, J.; Vorvick, C.;
Vyachanin, S. P.; Wallace, L.; Walther, H.; Ward, H.; Ward, R.; Ware,
B.; Watts, K.; Webber, D.; Weidner, A.; Weiland, U.; Weinstein, A.;
Weiss, R.; Welling, H.; Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.;
Whitcomb, S. E.; Whiting, B. F.; Wiley, S.; Wilkinson, C.; Willems,
P. A.; Williams, P. R.; Williams, R.; Willke, B.; Wilson, A.; Winjum,
B. J.; Winkler, W.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.;
Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yoshida,
S.; Zaleski, K. D.; Zanolin, M.; Zawischa, I.; Zhang, L.; Zhu, R.;
Zotov, N.; Zucker, M.; Zweizig, J.; Akutsu, T.; Akutsu, T.; Ando, M.;
Arai, K.; Araya, A.; Asada, H.; Aso, Y.; Beyersdorf, P.; Fujiki, Y.;
Fujimoto, M. -K.; Fujita, R.; Fukushima, M.; Futamase, T.; Hamuro, Y.;
Haruyama, T.; Hayama, K.; Iguchi, H.; Iida, Y.; Ioka, K.; Ishizuka,
H.; Kamikubota, N.; Kanda, N.; Kaneyama, T.; Karasawa, Y.; Kasahara,
K.; Kasai, T.; Katsuki, M.; Kawamura, S.; Kawamura, M.; Kawazoe, F.;
Kojima, Y.; Kokeyama, K.; Kondo, K.; Kozai, Y.; Kudoh, H.; Kuroda,
K.; Kuwabara, T.; Matsuda, N.; Mio, N.; Miura, K.; Miyama, S.; Miyoki,
S.; Mizusawa, H.; Moriwaki, S.; Musha, M.; Nagayama, Y.; Nakagawa, K.;
Nakamura, T.; Nakano, H.; Nakao, K.; Nishi, Y.; Numata, K.; Ogawa, Y.;
Ohashi, M.; Ohishi, N.; Okutomi, A.; Oohara, K.; Otsuka, S.; Saito,
Y.; Sakata, S.; Sasaki, M.; Sato, N.; Sato, S.; Sato, Y.; Sato, K.;
Sekido, A.; Seto, N.; Shibata, M.; Shinkai, H.; Shintomi, T.; Soida,
K.; Somiya, K.; Suzuki, T.; Tagoshi, H.; Takahashi, H.; Takahashi,
R.; Takamori, A.; Takemoto, S.; Takeno, K.; Tanaka, T.; Taniguchi,
K.; Tanji, T.; Tatsumi, D.; Telada, S.; Tokunari, M.; Tomaru, T.;
Tsubono, K.; Tsuda, N.; Tsunesada, Y.; Uchiyama, T.; Ueda, K.; Ueda,
A.; Waseda, K.; Yamamoto, A.; Yamamoto, K.; Yamazaki, T.; Yanagi,
Y.; Yokoyama, J.; Yoshida, T.; Zhu, Z. -H.
Bibcode: 2005PhRvD..72l2004A
Altcode: 2005gr.qc.....7081L
We report on the first joint search for gravitational waves by the TAMA
and LIGO collaborations. We looked for millisecond-duration unmodeled
gravitational-wave bursts in 473 hr of coincident data collected during
early 2003. No candidate signals were found. We set an upper limit of
0.12 events per day on the rate of detectable gravitational-wave bursts,
at 90% confidence level. From software simulations, we estimate that our
detector network was sensitive to bursts with root-sum-square strain
amplitude above approximately 1-3×10-19Hz-1/2
in the frequency band 700-2000 Hz. We describe the details of this
collaborative search, with particular emphasis on its advantages
and disadvantages compared to searches by LIGO and TAMA separately
using the same data. Benefits include a lower background and longer
observation time, at some cost in sensitivity and bandwidth. We also
demonstrate techniques for performing coincidence searches with a
heterogeneous network of detectors with different noise spectra and
orientations. These techniques include using coordinated software
signal injections to estimate the network sensitivity, and tuning
the analysis to maximize the sensitivity and the livetime, subject to
constraints on the background.
Title: Present status of large-scale cryogenic gravitational wave
telescope
Authors: Uchiyama, T.; Kuroda, K.; Ohashi, M.; Miyoki, S.; Ishitsuka,
H.; Yamamoto, K.; Hayakawa, H.; Kasahara, K.; Fujimoto, M. -K.;
Kawamura, S.; Takahashi, R.; Yamazaki, T.; Arai, K.; Tatsumi, D.;
Ueda, A.; Fukushima, M.; Sato, S.; Tsunesada, Y.; Zhu, Zong-Hong;
Shintomi, T.; Yamamoto, A.; Suzuki, T.; Saito, Y.; Haruyama, T.;
Sato, N.; Higashi, Y.; Tomaru, T.; Tsubono, K.; Ando, M.; Numata, K.;
Aso, Y.; Ueda, K. -I.; Yoneda, H.; Nakagawa, K.; Musha, M.; Mio, N.;
Moriwaki, S.; Somiya, K.; Araya, A.; Takamori, A.; Kanda, N.; Telada,
S.; Tagoshi, H.; Nakamura, T.; Sasaki, M.; Tanaka, T.; Ohara, K. -I.;
Takahashi, H.; Nagano, S.; Miyakawa, O.; Tobar, M. E.
Bibcode: 2004CQGra..21S1161U
Altcode: 2004CQGra..21.1161U
The large-scale cryogenic gravitational wave telescope (LCGT) is the
future project of the Japanese gravitational wave group. Two sets of 3
km arm length laser interferometric gravitational wave detectors will
be built in a tunnel of Kamioka mine in Japan. LCGT will detect chirp
waves from binary neutron star coalescence at 240 Mpc away with a S/N
of 10. The expected number of detectable events in a year is two or
three. To achieve the required sensitivity, several advanced techniques
will be employed such as a low-frequency vibration-isolation system,
a suspension point interferometer, cryogenic mirrors, a resonant side
band extraction method, a high-power laser system and so on. We hope
that the beginning of the project will be in 2005 and the observations
will start in 2009.
Title: Determination of iron(III)- complexing ligands originated
from marine phytoplankton using cathodic stripping voltammetry
Authors: Hiroshi, H.; Maki, T.; Asano, K.; Ueda, K.; Ueda, K.
Bibcode: 2003GeCAS..67R.137H
Altcode:
No abstract at ADS
Title: Current status of large-scale cryogenic gravitational wave
telescope
Authors: Kuroda, K.; Ohashi, M.; Miyoki, S.; Uchiyama, T.; Ishitsuka,
H.; Yamamoto, K.; Kasahara, K.; Fujimoto, M. -K.; Kawamura, S.;
Takahashi, R.; Yamazaki, T.; Arai, K.; Tatsumi, D.; Ueda, A.;
Fukushima, M.; Sato, S.; Nagano, S.; Tsunesada, Y.; Zhu, Zong-Hong;
Shintomi, T.; Yamamoto, A.; Suzuki, T.; Saito, Y.; Haruyama, T.; Sato,
N.; Higashi, Y.; Tomaru, T.; Tsubono, K.; Ando, M.; Takamori, A.;
Numata, K.; Aso, Y.; Ueda, K. -I.; Yoneda, H.; Nakagawa, K.; Musha,
M.; Mio, N.; Moriwaki, S.; Somiya, K.; Araya, A.; Kanda, N.; Telada,
S.; Tagoshi, H.; Nakamura, T.; Sasaki, M.; Tanaka, T.; Oohara, K.;
Takahashi, H.; Miyakawa, O.; Tobar, M. E.
Bibcode: 2003CQGra..20S.871K
Altcode:
The large-scale cryogenic gravitational wave telescope (LCGT) project
is the proposed advancement of TAMA, which will be able to detect the
coalescences of binary neutron stars occurring in our galaxy. LCGT
intends to detect the coalescence events within about 240 Mpc, the rate
of which is expected to be from 0.1 to several events in a year. LCGT
has Fabry Perot cavities of 3 km baseline and the mirrors are cooled
down to a cryogenic temperature of 20 K. It is planned to be built in
the underground of Kamioka mine. This paper overviews the revision of
the design and the current status of the R&D.
Title: Detection of bacterial population contributing to organoarsenic
decomposition
Authors: Maki, T.; Hasegawa, H.; Wachi, S.; Ueda, K.
Bibcode: 2003GeCAS..67Q.269M
Altcode:
No abstract at ADS
Title: LCGT Project Observing Gravitational Wave Events at 240 Mpc
Authors: Kuroda, K.; Ohashi, M.; Miyoki, S.; Uchiyama, T.; Ishitsuka,
H.; Yamamoto, K.; Hayakawa, H.; Kasahara, K.; Fujimoto, M. K.;
Kawamura, S.; Takahashi, R.; Yamazaki, T.; Arai, K.; Tatsumi, D.;
Ueda, A.; Fukushima, M.; Sato, S.; Nagano, S.; Tsunesada, Y.; Zhu,
Z. H.; Shintomi, T.; Yamamoto, A.; Suzuki, T.; Saito, Y.; Haruyama,
T.; Sato, N.; Higashi, Y.; Tomaru, T.; Tsubono, K.; Ando, M.; Takamori,
A.; Numata, K.; Aso, Y.; Ueda, K. I.; Yoneda, H.; Nakagawa, K.; Musha,
M.; Mio, N.; Moriwaki, S.; Somiya, K.; Araya, A.; Kanda, N.; Telada,
S.; Tagoshi, H.; Nkakmura, T.; Sasaki, M.; Tanaka, T.; Ohara, K.;
Takahashi, H.; Miyakawa, O.; Tobar, M. E.
Bibcode: 2003ICRC....5.3103K
Altcode: 2003ICRC...28.3103K
The large-scale cryogenic gravitational wave telescope (LCGT) project
was originally planned in 1998 and was revised in 2002. The design
concept of the LCGT was to raise the baseline of TAMA by one order and
to decrease the thermal noise of the mirrors by one order by using
cryogenics and by locating LCGT at an underground site in Kamioka
mine. Two sets of interferometers will be constructed in the same
tunnel in order to reject possible fake events.
Title: Japanese large-scale interferometers
Authors: Kuroda, K.; Ohashi, M.; Miyoki, S.; Ishizuka, H.; Taylor,
C. T.; Yamamoto, K.; Miyakawa, O.; Fujimoto, M. -K.; Kawamura,
S.; Takahashi, R.; Yamazaki, T.; Arai, K.; Tatsumi, D.; Ueda,
A.; Fukushima, M.; Sato, S.; Shintomi, T.; Yamamoto, A.; Suzuki,
T.; Saito, Y.; Haruyama, T.; Sato, N.; Higashi, Y.; Uchiyama, T.;
Tomaru, T.; Tsubono, K.; Ando, M.; Takamori, A.; Numata, K.; Ueda,
K. -I.; Yoneda, H.; Nakagawa, K.; Musha, M.; Mio, N.; Moriwaki, S.;
Somiya, K.; Araya, A.; Kanda, N.; Telada, S.; Sasaki, M.; Tagoshi,
H.; Nakamura, T.; Tanaka, T.; Ohara, K.
Bibcode: 2002CQGra..19.1237K
Altcode:
No abstract at ADS
Title: Combined half-collision approach to the nonadiabatic
transitions in the Hg(6s6p3P2)-N2,
CO cold and thermal quasimolecules
Authors: Ohmori, K.; Kurosawa, T.; Amano, K.; Chiba, H.; Okunishi,
M.; Ueda, K.; Sato, Y.; Devdariani, A. Z.; Nikitin, E. E.
Bibcode: 1999AIPC..467..389O
Altcode: 1999sls..conf..389O
No abstract at ADS
Title: First observation of the bound Hg-rare-gas complex in the
dark c-state using free-bound-bound 2-step laser excitation
Authors: Amano, K.; Ohmori, K.; Kurosawa, T.; Chiba, H.; Okunishi,
M.; Ueda, K.; Sato, Y.; Devdariani, A. Z.; Nikitin, E. E.
Bibcode: 1999AIPC..467..390A
Altcode: 1999sls..conf..390A
No abstract at ADS
Title: Far-wing line-shape study of the inter-excited-state
transitions of the Hg-Ar and Hg-Ne collisional quasimolecules
Authors: Amano, K.; Ohmori, K.; Okunishi, M.; Chiba, H.; Ueda, K.;
Sato, Y.
Bibcode: 1999AIPC..467..391A
Altcode: 1999sls..conf..391A
No abstract at ADS
Title: Far-wing line-shape study of the collision-induced c<--X
transition in Hg-rare-gas quasimolecules
Authors: Sato, Y.; Kurosawa, T.; Ohmori, K.; Chiba, H.; Okunishi,
M.; Ueda, K.; Devdariani, A. Z.; Nikitin, E. E.
Bibcode: 1999AIPC..467..388S
Altcode: 1999sls..conf..388S
No abstract at ADS
Title: Accurate measurement of the radius of curvature of a concave
mirror and the power dependence in a high-finesse Fabry-Perot
interferometer
Authors: Uehara, N.; Ueda, K.
Bibcode: 1995ApOpt..34.5611U
Altcode:
We describe the accurate measurement of the radius of curvature of
a concave mirror in a Fabry-Perot interferometer with a finesse of
78,100. The radius of curvature of the concave mirror is determined
by measuring the free spectral range and the transverse-mode range
with the frequency response functions. The radii of curvature at two
orthogonal (x and y) axes on the mirror surface resulting from the
polishing nonisotropy were accurately measured to be rx
= 1008.46 mm and ry = 1006.94 mm, respectively, with an
accuracy of 8 \times 10 -5. This accuracy is the best
to our knowledge. The power dependence of the radii of curvature to
the cavity internal intensity at a steady state was measured to be
drx/dI c = +60 mu m/(MW/cm2) at the x axis
and dr<sub>y/dI<sub>c = +47 mu m/(MW/cm/2)
at the y axis to an intensity of 2.1 MW/cm2.
Title: Behavior of Japanese tree frogs under microgravity on MIR
and in parabolic flight
Authors: Izumi-Kurotani, A.; Yamashita, M.; Kawasaki, Y.; Kurotani, T.;
Mogami, Y.; Okuno, M.; Oketa, A.; Shiraishi, A.; Ueda, K.; Wassersug,
R. J.; Naitoh, T.
Bibcode: 1994AdSpR..14h.419I
Altcode: 1994AdSpR..14..419I
Japanese tree frogs (Hyla japonica) were flown to the space station
MIR and spent eight days in orbit during December, 1990/1/. Under
microgravity, their postures and behaviors were observed and
recorded. On the MIR, floating frogs stretched four legs out,
bent their bodies backward and expanded their abdomens. Frogs on a
surface often bent their neck backward and walked backwards. This
behavior was observed on parabolic flights and resembles the retching
behavior of sick frogs on land- a possible indicator of motion
sickness. Observations on MIR were carried out twice to investigate
the frog's adaptation to space. The frequency of failure in landing
after a jump decreased in the second observation period. After the
frogs returned to earth, readaptation processes were observed. The
frogs behaved normally as early as 2.5 hours after landing.
Title: High power LD-pumped solid-state laser.
Authors: Ueda, K.
Bibcode: 1991AstHe..84..126U
Altcode:
No abstract at ADS