http://chineseinput.net/에서 pinyin(병음)방식으로 중국어를 변환할 수 있습니다.
변환된 중국어를 복사하여 사용하시면 됩니다.
ADVANCED DEVICE ISOLATION FOR VLSI-A REVIEW
Pogge, H. Bernhard 대한전자공학회 1989 ICVC : International Conference on VLSI and CAD Vol.1 No.1
Device-isolation concepts and methods have changed over the years, each new approach typically requiring various elements of process development. The ultimate device isolation is one in which the devices can be separated from each other by a dielectric region that reaches down past the active device areas and occupies minimal real estate. The device elements in such a case could all be butted against the isolation region. This process, in principle, becomes lithography limited and is extendible with future lithography improvements. Device scaling is, therefore, assured. It also permits some process technologies, such as fewer masks, elimination of lateral autodoping and Si3N4 films, as well as improved surface planarities. The process technologies required to achieve this form of device isolation (generally termed trench isolation) relate mainly to reactive ion etching (RIE) and chemical vapor deposition (CVD) techniques. In both instances, extensions of current process capabilities and process understanding had to be developed in order to accommodate the various isolation requirements dictated by different device design configurations. Elements of these processes will be discussed, along with examples of associated process difficulties and accomplishments.
LONG-TERM VARIATION OF THE SHUTTER DELAY TIME OF Y4KCAM OF THE CTIO 1.0 M TELESCOPE
Jae-Woo Lee,Richard Pogge 한국천문학회 2016 Journal of The Korean Astronomical Society Vol.49 No.6
We investigate the long-term spatial drift of the center and the temporal variation of the shutter delay time map of Y4KCam mounted on the CTIO 1.0~m telescope. We have collected shutter delay time maps over eight years as a part of our long-term survey program. We find that the center of the shutter delay time map can drift up to 450 $\mu$m, equivalent to $\approx$ 30 pixels, on the CCD. This effect can result in a small amount of error in integration time without the proper shutter delay time correction, but it does not appear to cause any significant problems in photometric measurements. We obtain a mean shutter delay time of 69.1 $\pm$ 0.8 ms and find no temporal variation of the shutter delay time of Y4KCam over eight years, indicative of the mechanical stability of the shutter. We suggest that using a master shutter delay time correction frame would be sufficient to achieve high precision photometry, which does not exceed photometric errors $\approx$ 1.7 mmag across the CCD frame for exposure times longer than 1 s.
Mathur, S.,Gupta, A.,Page, K.,Pogge, R. W.,Krongold, Y.,Goad, M. R.,Adams, S. M.,Anderson, M. D.,Aré,valo, P.,Barth, A. J.,Bazhaw, C.,Beatty, T. G.,Bentz, M. C.,Bigley, A.,Bisogni, S.,Borman, G. American Astronomical Society 2017 The Astrophysical Journal Vol.846 No.1
<P>During the Space Telescope and Optical Reverberation Mapping Project observations of NGC 5548, the continuum and emission-line variability became decorrelated during the second half of the six-month-long observing campaign. Here we present Swift and Chandra X-ray spectra of NGC 5548 obtained as part of the campaign. The Swift spectra show that excess flux (relative to a power-law continuum) in the soft X-ray band appears before the start of the anomalous emission-line behavior, peaks during the period of the anomaly, and then declines. This is a model-independent result suggesting that the soft excess is related to the anomaly. We divide the Swift data into on-and off-anomaly spectra to characterize the soft excess via spectral fitting. The cause of the spectral differences is likely due to a change in the intrinsic spectrum rather than to variable obscuration or partial covering. The Chandra spectra have lower signal-to-noise ratios, but are consistent with the Swift data. Our preferred model of the soft excess is emission from an optically thick, warm Comptonizing corona, the effective optical depth of which increases during the anomaly. This model simultaneously explains all three observations: the UV emission-line flux decrease, the soft-excess increase, and the emission-line anomaly.</P>
THE FIRST NEPTUNE ANALOG OR SUPER-EARTH WITH A NEPTUNE-LIKE ORBIT: MOA-2013-BLG-605LB
Sumi, T.,Udalski, A.,Bennett, D. P.,Gould, A.,Poleski, R.,Bond, I. A.,Skowron, J.,Rattenbury, N.,Pogge, R. W.,Bensby, T.,Beaulieu, J. P.,Marquette, J. B.,Batista, V.,Brillant, S.,Abe, F.,Asakura, Y.,B American Astronomical Society 2016 The Astrophysical journal Vol.825 No.2
<P>We present the discovery of the first Neptune analog exoplanet or super-Earth with a Neptune-like orbit, MOA-2013-BLG-605Lb. This planet has a mass similar to that of Neptune or a super-Earth and it orbits at 9 similar to 14 times the expected position of the snow line, a(snow), which is similar to Neptune's separation of 11 a(snow) from the Sun. The planet/host-star mass ratio is q = (3.6 +/- 0.7) x 10(-4) and the projected separation normalized by the Einstein radius is s = 2.39 +/- 0.05. There are three degenerate physical solutions and two of these are due to a new type of degeneracy in the microlensing parallax parameters, which we designate 'the wide degeneracy.' The three models have (i) a Neptune-mass planet with a mass of M-p = 21(-7)(+6)M(circle plus) orbiting a low-mass M-dwarf with a mass of M-h = 0.19(-0.06)(+0.05)M(circle dot), (ii) a mini-Neptune with M-p = 7.9(-1.2)(+1.8)M(circle plus) orbiting a brown dwarf host with M-h = 0.068(-0.011)(+0.019)M(circle dot), and (iii) a super-Earth with M-p = 3.2(-0.3)(+0.5)M(circle plus) orbiting a low-mass brown dwarf host with M-h = 0.025(-0.004)(+0.005)M(circle dot), which is slightly favored. The 3D planet-host separations are 4.6(-1.2)(+4.7) au, 2.1(-0.2) (+1.0) au, and 0.94(-0.02)(+0.67) au, which are 8.9(-1.4)(+10.5), 12(-1)(+7), or 14(-1)(+11) times larger than a(snow) for these models, respectively. Keck adaptive optics observations confirm that the lens is faint. This discovery suggests that low-mass planets with Neptune-like orbits are common. Therefore processes similar to the one that formed Neptune in our own solar system or cold super-Earths may be common in other solar systems.</P>
신인구,Y.-H. Ryu,A. Udalski,M. Albrow,S.-M. Cha,J.-Y. Choi,S.-J. Chung,C. Han,K.-H. Hwang,Y. K. Jung,D.-J. Kim,S.-L. Kim,C.-U. Lee,Y. Lee,B.-G. Park,H. Park,R. W. Pogge,J. C. Yee,P. Pietrukowicz,P. Mroz 한국천문학회 2016 Journal of The Korean Astronomical Society Vol.49 No.3
We report the characterization of a massive $(m_p=3.9\pm 1.4 M_{\rm jup})$ microlensing planet (OGLE-2015-BLG-0954Lb) orbiting an M dwarf host ($M=0.33\,\pm 0.12 M_\odot$) at a distance toward the Galactic bulge of $0.6^{+0.4}_{-0.2}\,$kpc, which is extremely nearby by microlensing standards. The planet-host projected separation is $a_\perp \sim 1.2\,\au$. The characterization was made possible by the wide-field ($4\,\rm deg^2$) high cadence ($\Gamma = 6\,\rm hr^{-1}$) monitoring of the Korea Microlensing Telescope Network (KMTNet), which had two of its three telescopes in commissioning operations at the time of the planetary anomaly. The source crossing time $t_*=16\,$min is among the shortest ever published. The high-cadence, wide-field observations that are the hallmark of KMTNet are the only way to routinely capture such short crossings. High-cadence resolution of short caustic crossings will preferentially lead to mass and distance measurements for the lens. This is because the short crossing time typically implies a nearby lens, which enables the measurement of additional effects (bright lens and/or microlens parallax). When combined with the measured crossing time, these effects can yield planet/host masses and distance.
The KMTNet/K2-C9 (<i>Kepler</i>) Data Release
Kim, H.-W.,Hwang, K.-H.,Kim, D.-J.,Albrow, M. D.,Cha, S.-M.,Chung, S.-J.,Gould, A.,Han, C.,Jung, Y. K.,Kim, S.-L.,Lee, C.-U.,Lee, D.-J.,Lee, Y.,Park, B.-G.,Pogge, R. W.,Ryu, Y.-H.,Shin, I.-G.,Shvartzv American Astronomical Society 2018 The Astronomical journal Vol.155 No.5
<i>SPITZER</i>MICROLENS MEASUREMENT OF A MASSIVE REMNANT IN A WELL-SEPARATED BINARY
Shvartzvald, Y.,Udalski, A.,Gould, A.,Han, C.,Bozza, V.,Friedmann, M.,Hundertmark, M.,Beichman, C.,Bryden, G.,Novati, S. Calchi,Carey, S.,Fausnaugh, M.,Gaudi, B. S.,Henderson, C. B.,Kerr, T.,Pogge, R. IOP Publishing 2015 The Astrophysical journal Vol.814 No.2
<P>We report the detection and mass measurement of a binary lens OGLE-2015-BLG-1285La, b, with the more massive component having M-1 > 1.35M(circle dot) (80% probability). A main-sequence star in this mass range is ruled out by limits on blue light, meaning that a primary in this mass range must be a neutron star (NS) or black hole (BH). The system has a projected separation r(perpendicular to) = 6.1 +/- 0.4 AU and lies in the Galactic bulge. These measurements are based on the 'microlens parallax' effect, i.e., comparing the microlensing light curve as seen from Spitzer, which lay at 1.25 AU projected from Earth, to the light curves from four ground-based surveys, three in the optical and one in the near-infrared. Future adaptive optics imaging of the companion by 30 m class telescopes will yield a much more accurate measurement of the primary mass. This discovery both opens the path and defines the challenges to detecting and characterizing BHs and NSs in wide binaries, with either dark or luminous companions. In particular, we discuss lessons that can be applied to future Spitzer and Kepler K2 microlensing parallax observations.</P>