40 research outputs found
Concurrent presentation of cryptococcal meningoencephalitis and systemic lupus erythematosus
金沢大学医薬保健研究域医学系医学教育研究センターCryptococcal meningitis is a recognized complication of systemic lupus erythematosus (SLE), with high mortality rates, particularly in those treated with immunosuppressive agents. We describe a patient diagnosed simultaneously with cryptococcal meningoencephalitis and SLE and reviewed four similar cases reported in the literature. In our case, profound low CD4 lymphocyte count and low complement levels were observed. The patient was treated with prednisolone, fluconazole, and 5-flucytosine and evinced good clinical improvement. This case suggests that intrinsic immunological abnormality related to SLE predisposed to opportunistic infections. © 2010 Japan College of Rheumatology
Improvement of the target sensitivity in DECIGO by optimizing its parameters for quantum noise including the effect of diffraction loss
DECIGO is the future Japanese gravitational wave detector in outer space. We
previously set the default design parameters to provide a good target
sensitivity to detect the primordial gravitational waves (GWs). However, the
updated upper limit of the primordial GWs by the Planck observations motivated
us for further optimization of the target sensitivity. Previously, we had not
considered optical diffraction loss due to the very long cavity length. In this
paper, we optimize various DECIGO parameters by maximizing the signal-to-noise
ratio (SNR), for the primordial GWs to quantum noise including the effects of
diffraction loss. We evaluated the power spectrum density for one cluster in
DECIGO utilizing the quantum noise of one differential Fabry-Perot
interferometer. Then we calculated the SNR by correlating two clusters in the
same position. We performed the optimization for two cases: the constant
mirror-thickness case and the constant mirror-mass case. As a result, we
obtained the SNR dependence on the mirror radius, which also determines various
DECIGO parameters. This result is the first step toward optimizing the DECIGO
design by considering the practical constraints on the mirror dimension and
implementing other noise sources.Comment: 13 pages, 12 figure
First-step experiment in developing optical-spring quantum locking for DECIGO: sensitivity optimization for simulated quantum noise by completing the square
DECi-hertz Interferometer Gravitational Wave Observatory (DECIGO) is a future
mission for a space-borne laser interferometer. DECIGO has 1,000-km-long arm
cavities mainly to detect the primordial gravitational waves (PGW) at lower
frequencies around 0.1 Hz. Observations in the electromagnetic spectrum have
lowered the bounds on the upper limit of PGW energy density (). As a result, DECIGO's target sensitivity, which
is mainly limited by quantum noise, needs further improvement. To maximize the
feasibility of detection while constrained by DECIGO's large diffraction loss,
a quantum locking technique with an optical spring was theoretically proposed
to improve the signal-to-noise ratio of the PGW. In this paper, we
experimentally verify one key element of the optical-spring quantum locking:
sensitivity optimization by completing the square of multiple detector outputs.
This experiment is operated on a simplified tabletop optical setup with
classical noise simulating quantum noise. We succeed in getting the best of the
sensitivities with two different laser powers by the square completion method.Comment: 10 pages, 14 figure
Self-Care of People with Schizophrenia Living in Community -Focus on maintenance of balance of solitude and social interaction-
journal articl
Current status of space gravitational wave antenna DECIGO and B-DECIGO
Deci-hertz Interferometer Gravitational Wave Observatory (DECIGO) is the
future Japanese space mission with a frequency band of 0.1 Hz to 10 Hz. DECIGO
aims at the detection of primordial gravitational waves, which could be
produced during the inflationary period right after the birth of the universe.
There are many other scientific objectives of DECIGO, including the direct
measurement of the acceleration of the expansion of the universe, and reliable
and accurate predictions of the timing and locations of neutron star/black hole
binary coalescences. DECIGO consists of four clusters of observatories placed
in the heliocentric orbit. Each cluster consists of three spacecraft, which
form three Fabry-Perot Michelson interferometers with an arm length of 1,000
km. Three clusters of DECIGO will be placed far from each other, and the fourth
cluster will be placed in the same position as one of the three clusters to
obtain the correlation signals for the detection of the primordial
gravitational waves. We plan to launch B-DECIGO, which is a scientific
pathfinder of DECIGO, before DECIGO in the 2030s to demonstrate the
technologies required for DECIGO, as well as to obtain fruitful scientific
results to further expand the multi-messenger astronomy.Comment: 10 pages, 3 figure
Current status of space gravitational wave antenna DECIGO and B-DECIGO
The Deci-hertz Interferometer Gravitational Wave Observatory (DECIGO) is a future Japanese space mission with a frequency band of 0.1 Hz to 10 Hz. DECIGO aims at the detection of primordial gravitational waves, which could have been produced during the inflationary period right after the birth of the Universe. There are many other scientific objectives of DECIGO, including the direct measurement of the acceleration of the expansion of the Universe, and reliable and accurate predictions of the timing and locations of neutron star/black hole binary coalescences. DECIGO consists of four clusters of observatories placed in heliocentric orbit. Each cluster consists of three spacecraft, which form three Fabry–Pérot Michelson interferometers with an arm length of 1000 km. Three DECIGO clusters will be placed far from each other, and the fourth will be placed in the same position as one of the other three to obtain correlation signals for the detection of primordial gravitational waves. We plan to launch B-DECIGO, which is a scientific pathfinder for DECIGO, before DECIGO in the 2030s to demonstrate the technologies required for DECIGO, as well as to obtain fruitful scientific results to further expand multi-messenger astronomy