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1968년 ~ 2024년까지 1,211 건의 한국천문학회지를 격월간 확인하실 수 있습니다.
- The Korean Astronomical Society (The Korean Astronomical Society)
- 계간 (Quarterly)
- ISSN : 1225-4614 (ISSN : 1225-4614)
1225-4614
- DB구축현황 : 1,211건 (DB Construction : 1,211 Articles)
총 게시글 1,211건
페이지 97/122
961
- NEIZVESTNY S. I.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.77-78
- 1996
- 원문 바로보기
We perfom a large project for complex study of Blue Compact Galaxies (BCGs) with strong star formation, which includes optical spectroscopy, BVR CCD photometry and HI 21 cm radio survey. The most interesting galaxies are studied also with HST and VLA. In the frame of this project we began the study of H<TEX>$\alpha$</TEX> morphology of BCGs with 6-m telescope. We present and discuss here the results for the first 6 galaxies. We found the noticeable variety of forms for H<TEX>$\alpha$</TEX> morphology comparing to broad band images: from very compact HII region in very center of stellar body (Mark 996, possible dwarf post-merger, old galaxy experiencing strong star formation burst), to very extended gas emission encompassing the whole area traced by stars (SBS 0335-052, the most probable young galaxy in formation).
962
- KIM SANG-JOON
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.347-350
- 1996
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Spectroscopic data between 7 and 15 microns obtained in 1979 by Voyager 1 and 2 Infrared Interferometer Spectrometer (IRIS) have been revisited. Using the spectral data, Jupit.er images have been constructed at the emission bands of hydrocarbons, such as methane, ethane, and acetylene. The resultant. images show differences in emission intensities in the polar regions, suggesting inhomogeneous distributions of the hydrocarbons over the auroral regions of Jupiter.
963
- KOO BON-CHUL
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.183-186
- 1996
- 원문 바로보기
We report the results of H I 21-cm and molecular line studies of the shocked interstellar gas in the W51 complex. We present convincing evidences suggesting that the shocked gas has been produced by the interaction of the W51C supernova remant (SNR) with a large molecular cloud, Our results show that W51C is the second SNR with direct evidences for the shocked cloud material.
964
- LEE Y.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.173-174
- 1996
- 원문 바로보기
We have mapped <TEX>$17 deg^2$</TEX> region toward Galactic anticenter in <TEX>$^{12}CO$</TEX> J = 1 - 0 using the 3 mm SIS receiver on the 14 m telescope at Taeduk Radio Astronomy Observatory (TRAO). The region mapped in this paper is the first target of the Galactic AntiCenter CO Survey Project (GACCOS) and was selected comparing with IRAS Sky Survey Atlas (ISSA) images at 100<TEX>${\mu}m$</TEX>. Molecular emission of the target area is found to be very extended and is well matching with the FIR emission boundary. There are several pieces of clouds, and as some of spectra show several peaks, there seem to be several clouds overlapped in some directions. The Velocity of Local Standard of Rest (<TEX>$V_{LSR}$</TEX>) of the CO emission of the mapped region ranges from -20 to +10 km/s. It is also found that the two cloudlets located around I = <TEX>$180^{\circ}$</TEX> have <TEX>$V_{LSR}$</TEX> = -20 km/s, which is very abnormal. The peak antenna temperature of 13 K arises near the H II Region S241.
965
- KUBOTA JUN
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.329-330
- 1996
- 원문 바로보기
966
- WU XUEJUN
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.41-42
- 1996
- 원문 바로보기
A possible cosmic X-ray background(XRB) radiation related to original antimatter is considered. If the universe is made of separating domains of antimatter and matter, the photons produced by the annihilation of electron-positron and proton-antiproton on the last scattering surface would reach us in the energy <TEX>$\~$</TEX>0.45 keV and <TEX>$\~$</TEX>60 keV respectively because of the redshift. The spectrums of X-ray radiation from annihilation are deduced and a possible observational figure is described also.
967
- ZHU XINGFEN
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.109-110
- 1996
- 원문 바로보기
968
- GUHATHAKURTA PURAGRA
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.63-64
- 1996
- 원문 바로보기
The nature of distant faint blue field galaxies remains a mystery, despite the fact that much attention has been devoted to this subject in the last decade. Galaxy counts, particularly those in the optical and near ultraviolet bandpasses, have been demonstrated to be well in excess of those expected in the 'no-evolution' scenario. This has usually been taken to imply that galaxies were brighter in the past, presumably due to a higher rate of star formation. More recently, redshift surveys of galaxies as faint as B<TEX>$\~$</TEX>24 have shown that the mean redshift of faint blue galaxies is lower than that predicted by standard evolutionary models (de-signed to fit the galaxy counts). The galaxy number count data and redshift data suggest that evolutionary effects are most prominent at the faint end of the galaxy luminosity function. While these data constrain the form of evolution of the overall luminosity function, they do not constrain evolution in individual galaxies. We are carrying out a series of observations as part of a long-term program aimed at a better understanding of the nature and amount of luminosity evolution in individual galaxies. Our study uses the luminosity-linewidth relation (Tully-Fisher relation) for disk galaxies as a tool to study luminosity evolution. Several studies of a related nature are being carried out by other groups. A specific experiment to test a 'no-evolution' hypothesis is presented here. We have used the AUTOFIB multifibre spectro-graph on the 4-metre Anglo-Australian Telescope (AAT) and the Rutgers Fabry-Perot imager on the Cerro Tolalo lnteramerican Observatory (CTIO) 4-metre tele-scope to measure the internal kinematics of a representative sample of faint blue field galaxies in the red-shift range z = 0.15-0.4. The emission line profiles of [OII] and [OIII] in a typical sample galaxy are significantly broader than the instrumental resolution (100-120 km <TEX>$s^{-l}$</TEX>), and it is possible to make a reliable de-termination of the linewidth. Detailed and realistic simulations based on the properties of nearby, low-luminosity spirals are used to convert the measured linewidth into an estimate of the characteristic rotation speed, making statistical corrections for the effects of inclination, non-uniform distribution of ionized gas, rotation curve shape, finite fibre aperture, etc.. The (corrected) mean characteristic rotation speed for our distant galaxy sample is compared to the mean rotation speed of local galaxies of comparable blue luminosity and colour. The typical galaxy in our distant sample has a B-band luminosity of about 0.25 L<TEX>$\ast$</TEX> and a colour that corresponds to the Sb-Sd/Im range of Hub-ble types. Details of the AUTOFIB fibre spectroscopic study are described by Rix et al. (1996). Follow-up deep near infrared imaging with the 10-metre Keck tele-scope+ NIRC combination and high angular resolution imaging with the Hubble Space Telescope's WFPC2 are being used to determine the structural and orientation parameters of galaxies on an individual basis. This information is being combined with the spatially resolved CTIO Fabry-Perot data to study the internal kinematics of distant galaxies (Ing et al. 1996). The two main questions addressed by these (preliminary studies) are: 1. Do galaxies of a given luminosity and colour have the same characteristic rotation speed in the distant and local Universe? The distant galaxies in our AUTOFIB sample have a mean characteristic rotation speed of <TEX>$\~$</TEX>70 km <TEX>$s^{-l}$</TEX> after correction for measurement bias (Fig. 1); this is inconsistent with the characteristic rotation speed of local galaxies of comparable photometric proper-ties (105 km <TEX>$s^{-l}$</TEX>) at the > <TEX>$99\%$</TEX> significance level (Fig. 2). A straightforward explanation for this discrepancy is that faint blue galaxies were about 1-1.5 mag brighter (in the B band) at z <TEX>$\~$</TEX> 0.25 than their present-day counterparts. 2. What i
969
- YERSHOV V. N.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.427-428
- 1996
- 원문 바로보기
The Struve astrometric satellite which is being developed at Pulkovo Observatory in cooperation with Krasno-yarsk Institute of Applied Mechanics, S.I. Vavilov's State Optical Institute and some others space instrumentation institutes, will produce observations of a second epoch for the Hipparcos stars. The project is devoted to maintaining the Hipparcos coordinate system as well as extending it to a density of <TEX>$\approx$</TEX> 100 stars per square degree. Possibilities of submilliarcsecond accuracy of observations with single aperture on-board telescopes are discussed. Requirements to the optical scheme and to the dynamic properties of the spacecraft are formulated. CCD and microchannel plates are discussed as a focal assembly detectors.
970
- LIU HANPING
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.175-176
- 1996
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