We present 12CO and 13CO molecular line observations of some pre-main sequence stars associated with cometary nebulae and attempt to unravel their detailed structure.

We have carried out an extensive survey of Hα emission stars in the Orion region over an area of about 100 deg2. We present the results for the areas A-0975 and A-0976 of about 25 deg2 each.

We have measured the annual parallax of the water maser source associated with star forming region NGC2264 from observations with VLBI Exploration of Radio Astrometry (VERA). We detected masers at VLSR = 7.2 km s−1. We discussed its driving sources of detected maser spots. One of the maser spots was associated with a centimeter continuum source observed with VLA. Neither optical, infrared nor X-ray sources is catalogued near the spot. The other maser spot is located close to an X-ray source, although there is no optical or infrared counterpart. The proper motion of the former spot was (μα, μδ) = (23.91 ± 4.29, −29.81 ± 4.27) and the proper motion of latter spot was (μα, μδ) = (−0.96 ± 0.58, −6.05 ± 3.06). For the latter spot, the peculiar motion is ∼ 150 km s−1 and it has the high velocity and this may be a jet or an outflow from a young star. The observed parallax is 1.365 ± 0.098 mas, corresponding to the distance of 738+57−50 pc. This value is constant with the photometric distance of NGC2264 previously measured. The fitting result of the parallax is shown in figure 1. We also observed in NH3 (1,1), (2,2), (3,3) lines of NGC2264 with the Kashima 34m telescope. We estimated the star formation efficiency (SFE) of NGC2264 from the dense molecular mass of NH3 and the stellar mass calculated by Teixeira et al. (2012). The SFE is 9 – 12% which is consistent with previous results.

Some composite materials of poly (lactic acid) (PLA) with organophilic clays and an organic crystal accelerator (OCA) were prepared by melt compounding method to improve the rate of crystallization and mechanical properties, especially heat distortion temperature (HDT). The PLA/clay nanocomposite with 2.9wt% of finely dispersed organophilic clay and 1wt% of the OCA showed an exothermic peak corresponding to its crystallization at 1.9 minutes in the isothermal measurement of DSC at 100°C from its molten state, although PLA itself did not show a clear peak in the same procedure. Crystallized specimens of the nanocomposite were well obtained by injection molding when the hold time was set at more than 90 seconds. The HDT of the specimens that were held for more than 120 seconds in the mold exceeded 120°C. It is about 65°C higher than amorphous PLA. The crystallized specimen with 1wt% of the clay showed higher tensile modulus and Izod impact strength than the amorphous one.

Ionic mechanisms and signal transduction underlying noradrenaline (NA)-induced depolarization in single smooth muscle cells of guinea-pig vas deferens were studied. NA caused depolarization followed by action potentials through activation of α1-adrenoceptors. In the presence of nifedipine, no action potential was generated, and the magnitude of the depolarization depended on the concentration of NA (0.1-100 µm). NA, through α1-adrenoceptor activation, reduced the magnitude of membrane currents in response to voltage ramp pulses from -90 to -30 mV in a concentration-dependent manner. The reversal potential of the current inhibited by NA changed proportionally to the change in the equilibrium potential of K+, suggesting that NA inhibited K+ channel activity. Treatment of cells with GDPβS, an inhibitor of G proteins, or bisindolylmaleimide (BIM), a selective protein kinase C (PKC) inhibitor, prevented the NA inhibition of the currents. Application of 12-O-tetradecanoylphorbol 13-acetate (TPA), an activator of PKC, mimicked the effect of NA. It is suggested that in the smooth muscle of guinea-pig vas deferens, activation of α1-adrenoceptors and the subsequent activation of PKC led to inhibition of K+ currents, which is responsible for the depolarization induced by NA.

We report the result of our survey observations in the outer part of the Orion star-forming region which consists of six Kiso sky areas (150 square degrees). In total, we detected only 48 emission line stars. The low surface density suggests that the Orion star-forming region probably terminates around these areas.

In a series of emission-line star survey programs we have conducted wide and deep survey observations for Hα emission stars in the Orion star-forming region. The first result for the Kiso area A-0904 (5°x5°, centered at α = 5h40m and δ = +0°) was presented in Paper I (Wiramihardja et al., 1989), followed by Paper II (Kogure et al., 1989) for the area A-0903 (α = 5h20m, δ = −5° and A-0976 (α = 5h40m, δ = −5°). In Paper IV the results for the areas A-1047 (α = 5h20m, δ = −10° and A-1048 (α = 5h40m, δ = −10°) are given.

Near-infrared photometry is reported for 76 emission-line stars in outer regions of the Orion molecular cloud complex. Most of our program stars are selected from the Hα emission-line star catalog of the large-scale Kiso Schmidt survey of the Orion region. We confirm that most of the emission-line stars with strong emission detected in the Kiso survey are typical T Tauri stars with masses in the range 0.5 to 2 M⊙. Low mass stars have therefore continued to form in the outer parts of the Orion region, away from present day massive molecular clouds, until at least as recently as a few million year ago.

We have reported NMA observations of HH83 with CS (J=2-l) line. The interacton between the outflow and the molecluar cloud is found.

We have made a survey of Hα-emission stars in the CMa R1 region with the 105cm Schmidt telescope at the Kiso Observatory. In an area of about 37 square degrees, a total of 107 Hα-emission stars (V = 6-15 mag.) was found, and, for all of them, the photographic photometry in the UBV system has been carried out.

A cometary globule in IC1396 named ”comet tail 6” by Osterbrock (1957), has been observed at CO and 13CO (J = 1-0) lines with a high spatial resolution, 14″, with the 45-m radio telescope at the Nobeyama Radio Observatory. The resolution corresponds to a linear size of 0.05 pc at the distance of 750 pc (Matthews 1979). Two possible pre-main sequence stars, LkHα 349 and LkHα 349/c (Cohen and Kuhi 1979), associated with small nebulosities nestle in the central part of the globule. We have obtained CO and 13CO spectra long NS and EW strips which cross each other at the position of LkHα 349 and have mapped a 1.5′x1.5′ area around the globule center at 13CO. Results from the observations are summarized as follows: