[en] Two models of the phase rotation channels of the neutrino factory were designed with a solenoid transport system and the induction linac acceleration system. One model has the one stage induction linac channel, and another model has two stages of the induction linac channels and an absorber and drift space in between them. Major figure of merits of the channel are the particle ratio of muons over primary protons, the momentum spread and the muon polarization correlation to the arrival time at the end of the phase rotation channel. The μ/proton ratios were 0.25 and 0.13 for the single stage and the double stage induction linac channels, respectively. The effective muon polarization, radical< helicity²>radical, was 0.16 and the muon polarization correlation was 0.23/(100 ns) for the single stage induction linac model

[en] Two bright galactic H-2 regions, M 17 and Ori A, have been mapped at 3.5 mm wave length (87 GHz) with resolution of 2 min. The features were found, which are not seen in centimeter- and longer millimeter-wave maps. It is possible that these components are very compact H-2 regions with the emission measure of about 10¹¹pc cm^-6. Observations were made from December 1974 to March 1975 with the 6-m millimeter-wave telescope at Tokyo Astronomic Observatory. The data were taken in beam switching mode. Strip maps were made from a set of right ascension scans at 1 min-intervals in declination, and 50 to 150 scans were made at each declination. The scanned area was from -16 deg. 5 min. to -16 deg. 19 min. in the declination for M 17 and from -5 deg. 21 min. to -5 deg. 30 min. for Orion A. The central right ascension was 18 h 17 m 30 s for M 17 and 5 h 32 m 50 s for Orion A, the distance scanned was 100 s in right ascension. In discussion, the dust hypothesis was abandoned, but the thermal bremsstrahlung was adopted as the most probable explanation. In this case, it is possible that M 17 E is a high density ''cocoon star'' though this explanation is not free from difficulty. At the position of M 17 E, no H₂O or OH maser emission has been detected. The exciting star must be very massive and young according to the theoretical consideration. As for the elongation N in Orion A, similar consideration can be applied. (Iwakiri, K.)

[en] Results are presented of both low- and high-resolution molecular-line observations made toward the dark cloud L1287. The cloud appears filamentary in (C-13)O emission and extends over 10 pc along the Galactic plane. At least four separate cores are aligned along the filament. The most intense emission of (C-13)O comes from the L1287 main core. The total mass of the cloud is estimated to be about 240 solar masses. An energetic molecular outflow has been discovered in (C-12)O emission toward the peak of the main cloud core where a cold-type IRAS source, which is suggested to be the driving source of the outflow, is located. The central part of the main (C-13)O core has been mapped in HCN and HCO(+) (J = 1-0) lines. These lines are intense and optically thick, as suggested by the strong self-absorption. Both emission components have sizes of 0.1 pc. The lower limit of the mass of the HCN core is estimated to be 13 solar masses. Bipolar wing emission is also revealed in the HCO(+) spectra. The main (C-13)O core exhibits an unusually high ratio of the luminosity of the central object to the associated (C-13)O core mass in comparison with the typical isolated dark clouds in the solar neighborhood. The stellar wind from the neighboring Be star Kappa Cas is suggested to have played a role. 49 refs

[en] CDF Plug Upgrade(tile-fiber) EM Calorimeter performed resolution of 15%/√(E)+0.7% with non-linearity less than 1% in a energy range of 5-180 GeV at Fermilab Test Beam. Transverse uniformity of inside-tower-response of the EM Calorimeter was 2.2% with 56 GeV positron, which was reduced to 1.0% with response map correction. We observed 300 photo electron/GeV in the EM Calorimeter. Ratios of EM Calorimeter response to positron beam to that to ¹³⁷C_s Source was stable within 1% in the period of 8 months

[en] It has been found from ¹³CO observations using the Nagoya 4-m telescope that the blue- and redshifted contours (e.g., V_LSR ± 0.5 kms^-1) in the ρ Oph streamer (north) are systematically separated from each other, with blue on the north-west side and red on the south-east side of the curved axis of the streamer, respectively. Our interpretation is that the streamer is spinning around its axis. We propose a picture in which the streamer is a 'drain' through which the angular momentum is carried away from a massive cloud of active star formation by the magnetic twist. This draining allows the star-formation process in the massive cloud to occur with an enhanced rate. (author)

[en] The first detection of linear polarization of the semicircular supernova remnant G109.1 - 1.0 is reported. The observations were made at 10 GHz with the Nobeyama 45-m telescope. The degree of polarization typically ranges from several to 30 %. The distribution of the projected magnetic field cannot be simply explained as tangential to the shall of the supernova remnant, but is rather consistent with the general galactic magnetic field. (author)

[en] Inclusive production of rho⁰ (770), ω (783) and f (1270) has been studied in π^-p interactions at 6 GeV/c. The inclusive cross sections for rho⁰ and f are; 2.9 +- 0.3 mb and 0.47 +- 0.07 mb. The semi-inclusive cross section for ω is 0.20 +- 0.03 mb. These cross sections and ratios of rho⁰/π, f/rho⁰ and K*⁺/rho⁰ are compared with higher energy data. The differential cross sections for rho⁰, ω and f are presented as a function of Feynman scaling variable x and squared transverse momentum P sub(T)sup(2). The x distributions for rho⁰ and ω show them to be produced primarily in the forward direction. Inclusive rho⁰, ω and f resonance production in 6 GeV/c π^-p interactions seems to have not yet reached the high energy limiting behavior. (author)

[en] A molecular cloud has been discovered from a large-scale (C-13)0 (J = 1-0) survey in the Cep OB4 region. Detailed properties of this cloud, named as M120.1 + 3.0, are investigated on the basis of molecular-line observations and the IRAS data. The cloud, appearing dense and filamentary, is composed of two parts. Each of the two parts has a size of 6 x 1 pc and a mass of 800 solar mass, similar to dark clouds observed within 500 pc of the solar neighborhood. The cloud is associated with about 12 low-luminosity IRAS sources, and the locations of the sources show remarkable coincidence with the distribution of the dense molecular gas. Two molecular outflows have been discovered toward two of IRAS sources. 27 refs

[en] Radio observations of the ring complex G24.6 + 0.0 or the Scutum ring were made at 10, 5, and 2.7 GHz in continuum and at 115.27 GHz in the CO(J = 1 - 0) line emission. The complex is composed of several compact H_II regions associated with a diffuse extended radio emission centered on l = 24.6, b = 0.0. The spectrum of the diffuse component is flat, indicating its thermal origin. According to the radial velocities of the compact H_II regions they are located in the Scutum arm at 9.1 kpc from the sun, composing a shell-like association of radius 35 pc embedded in an extended H_II region. CO observations have revealed association of an arcshaped molecular cloud of mass 3 x 10⁵ solar mass aligned concentric to the H_II ring having a sharp inner edge, most likely being shock-compressed from inside. This molecular arc is further surrounded by a larger arc of H_I gas of radius 70 pc and a mass of 2 x 10⁴ solar mass. The positional relationship of the H_II, H₂(CO), and H_I gases suggests a typical sequential star formation on a shock-compressed CO shell being sandwitched between an expanding H_II region and the larger H_I cloud. (author)

[en] We designed a muon cooling ring with straight inserts with Lithium lenses and injection and extraction which can be used for the final transverse muon cooling for a Higgs Factory, a low energy version of a μ+μ- collider. We demonstrated the transverse phase space cooling of muon beam with the normalized transverse emittance at 0.3 mm*rad with a tracking simulation of the cooling ring with hard-edged magnetic elements. Work is in progress in using realistic magnetic field for the magnetic elements of the cooling ring