• 대한화학회지
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• 제40권6호
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• pp.427-435
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• 1996

$Ca^{2+}$ 이온과 $Cs^+$ 이온으로 치환되고 완전히 탈수된 제올라이트 X, $Ca_{35}Cs_{22}Si_{100}Al_{92}O_{384}$($Ca_{35}Cs_{22}$-X; a=25.071(1) $\AA)와Ca_{29}Cs_{34}Si_{100}Al_{92}O_{384}$($Ca_{29}Cs_{34}$-X; a=24.949(1) $\AA)$의 두 개의 결정 구조를 $21^{\circ}C$에서 입방공간군 Fd3을 사용하여 단결정 X-선 회절법으로 해석하고 구조를 정밀화하였다. 탈수한 $Ca_{35}Cs_{22}$-X의 구조를 Full-matrix 최소자승법 정밀화 계산에서 $I>3\sigma(I)$인 322개의 독립 반사를 사용하여 최종 오차 인자를 $R_1$=0.051, $R_2$=0.044까지 정밀화 계산하였고, 탈수한 $Ca_{35}Cs_{22}$-X의 구조는 260개의 독립 반사를 사용하여 $R_1$=0.058, $R_2$=0.055까지 정밀화시켰다. 이들 구조에서 $Ca^{2+}$ 이온과 $Cs^+$ 이온은 서로 다른 5개의 결정학적 자리에 위치하고 있다. 탈수한 $Ca_{35}Cs_{22}$-X 구조에서는 16개의 $Ca^{2+}$ 이온은 D6R의 중심, 자리 I에 모두 채워져 있다(Ca-O=2.41(1) $\AA$, $O-Ca-O=93.4(3)^{\circ}).$ 다른 19개의 $Ca^{2+}$ 이온은 자리 II에 (Ca-O=2.29(1) $\AA$, $O-Ca-O=118.7(4)^{\circ})$, 10개의 $Cs^+$ 이온은 큰 공동에서 6-링 맞은편 II에 채워져 있고, 각각 3개의 산소로 만들어지는 산소 평면으로부터 $1.95\AA$ 들어가 위치하고 $있다(Cs-O=2.99(1)\AA$, $O-Cs-O=82.3(3)^{\circ}).$ 3개의 $Cs^+$ 이온은 산소 평면에서 소다라이트 공동쪽으로 $2.27\AA$ 들어간 자리 II'에서 위치하고 $있다(Cs-O=3.23\AA$, $O-Cs-O=75.2(3)^{\circ}).$ 나머지 9개의 $Cs^+$ 이온은 각각 큰 공동내 2회 회전축을 가지고 있는 48(f) 위치인 자리 III에 통계학적으로 분포하고 $있다(Cs-O=3.25(1)\AA$, Cs-O=3.49(1) $\AA).$ 탈수한 $Ca_{29}Cs_{34}$-X에서 16개의 $Ca^{2+}$ 이온은 자리 I에 채워지고 (Ca-O=2.38(1) $\AA$, $O-Ca-O=94.1(4)^{\circ})$ 13개의 $Ca^{2+}$ 이온은 자리 II에 채워져 있다(Ca-O=2.32(2) $\AA$, $O-Ca-O=119.7(6)^{\circ}).$ 다른 12개의 $Cs^+$ 이온은 자리 II에 채워져 있고, 이들은 산소 평면으로부터 각각 $1.93\AA$ 들어가 위치하고 $있다(Cs-O=3.02(1)\AA$, $O-Cs-O=83.1(4)^{\circ}).$ 7개의 $Cs^+$ 이온은 각각 자리 II'에 위치하고 있고, 산소 평면으로부터 소다라이트 공동으로 $2.22\AA$ 들어가 위치하고 있다(Cs-O=3.21(2) $\AA$, $O-Cs-O=77.2(4)^{\circ}).$ 나머지 16개의 $Cs^+$ 이온은 큰 공동내의 자리 III에 있다(Cs-O=3.11(1) $\AA$, Cs-O=3.46(2) $\AA).Ca^{2+}$ 이온은 자리 I과 자리 II에 우선적으로 위치하고 $Cs^+$ 이온은 너무 커서 자리 I에 채워질 수 없으며 나머지 자리에 채워진다.

• 천문학회지
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• 제29권spc1호
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• pp.63-64
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• 1996

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$\~$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 $s^{-l}$), 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$\ast$ 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 $\~$70 km $s^{-l}$ 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 $s^{-l}$) at the > $99\%$ 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 $\~$ 0.25 than their present-day counterparts. 2. What is the nature of the internal kinematics of faint field galaxies? The linewidths of these faint galaxies appear to be dominated by the global disk rotation. The larger galaxies in our sample are about 2"-.5" in diameter so one can get direct insight into the nature of their internal velocity field from the $\~$ I" seeing CTIO Fabry-Perot data. A montage of Fabry-Perot data is shown in Fig. 3. The linewidths are too large (by. $5\sigma$) to be caused by turbulence in giant HII regions.

• Bulletin of the Korean Chemical Society
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• 제30권6호
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• pp.1285-1292
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• 2009

Large single crystals of zeolite, |$Na_{75}$|[$Si_{117}Al_{75}O_{384}$]-FAU (Na-Y, Si/Al = 1.56), were synthesized from gels with composition of 3.58Si$O_2$ : 2.08NaAl$O_2$ : 7.59NaOH : 455$H_2$O : 5.06TEA : 2.23TCl. One of these, a colorless single-crystal was ion exchanged by allowing aqueous 0.02 M CsOH to flow past the crystal at 293 K for 3 days, followed by dehydration at 673 K and 1 ${\times}\;10^{-6}$ Torr for 2 days. The crystal structure of fully dehydrated partially $Cs^+$-exchanged zeolite Y, |$Cs_{45}Na_{30}$|[$Si_{117}Al_{75}O_{384}$]-FAU per unit cell (a = 24.9080(10) $\AA$) was determined by single-crystal X-ray diffraction technique in the cubic space group Fd $\overline{3}$ m at 294(1) K. The structure was refined using all intensities to the final error indices (using only the 877 reflections with $F_o\;>\;4{\sigma}(F_o))\;R_1$ = 0.0966 (Based on F) and $R_2\;=\;0.2641\;(Based\;on\;F^2$). About forty-five $Cs^+$ ions per unit cell are found at six different crystallographic sites. The 2 $Cs^+$ ions occupied at site I, at the centers of double 6-ring (D6Rs, Cs-O = 2.774(10) $\AA$ and O-Cs-O = 88.9(3) and 91.1(3)$^o$). Two $Cs^+$ ions are found at site I’ in the sodalite cavity; the $Cs^+$ ions were recessed 2.05 $\AA$ into the sodalite cavity from their 3-oxygen plane (Cs-O = 3.05(3) $\AA$ and O-Cs-O = 77.4(13)$^o$). Site-II’ positions (opposite single 6-rings in the sodalite cage) are occupied by 7 $Cs^+$ ions, each of which extends 2.04 $\AA$ into the sodalite cage from its 3-oxygen plane (Cs-O = 3.067(11) $\AA$ and O-Cs-O = 80.1(3)$^o$). The 26 $Cs^+$ ions are nearly three-quarters filled at site II in the supercage, being recessed 2.34 $\AA$ into the supercage (Cs-O = 3.273(8) $\AA$ and O-Cs-O = 74.3(3)$^o$). The 4 $Cs^+$ ions are found at site III deep in the supercage (Cs-O = 3.321(19) and 3.08(3) $\AA$), and 4 $Cs^+$ ions at another site III’ (Cs-O = 2.87(4) and 3.38(4) $\AA$). About 30 $Na^+$ ions per unit cell are found at one crystallographic site; The $Na^+$ ions are located at site I’ in the sodalite cavity opposite double 6-rings (Na-O = 2.578(11) $\AA$ and O-Na-O = 97.8(4)$^o$).