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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.
Near-IR Photometric Properties of HB, MSTO, and SGB for metal poor Galactic globular clusters
김재우,강아람,손영종,신인구,천상현 한국우주과학회 2007 Journal of Astronomy and Space Sciences Vol.24 No.1
We report photometric features of the HB, MSTO, and SGB for a set of metal-poorGalactic globular clusters on the near-IR CMDs. The magnitude and color of theMSTO and SGB are measured on the ducial normal points of the CMDs by apply-ing a polynomial t. The near-IR luminosity functions of horizontal branch stars inthe classical second parameter pair M3 and M13 indicate that HB stars in M13 aredominated by hot stars that are relatively faint in the infrared,whereas HB stars in M3are brighter than those in M13. The luminosity functions of HB stars in the observedbulge clusters, except for NGC 6717, show a trend that the fainter hot HB stars aredominated in the relatively metal-poor clusters while the relatively metal-rich clusterscontain the brighter HB stars. It is suggestive that NGC 6717 would be an extremeexample of the second-parameter phenomenon for the bulge globular clusters.
NEAR-IR TRGB DISTANCE TO DWARF ELLIPTICAL GALAXY NGC 147
강아람,손영종,김호일,김재우,신인구,천상현 한국우주과학회 2007 Journal of Astronomy and Space Sciences Vol.24 No.3
We report the distance modulus of nearby dwarf elliptical galaxy NGC 147 estimated from the Tip of Red-giant Branch (TRGB) method applying to the color-magnitude diagrams and luminosity functions in the near-infrared $JHK$ bands. Apparent magnitudes of TRGBs in each band are obtained by applying Savitzky-Golay filter to the luminosity functions, and the theoretical absolute magnitudes are estimated from Yonsei-Yale isochrones. The derived values of distance modulus to NGC 147 are $(m-M)=23.69\pm0.12, 23.78\pm0.17,$ and $23.85\pm0.22$ for $J, H,$ and $K$ bands, respectively. Distance modulus in bolometric magnitude is also derived as $(m-M)=23.87\pm0.11$. We compare the derived values of the TRGB distance modulus to NGC 147 in the near-infrared bands with the previous results in other bands.
Near-IR TRGB Distance to Nearby Dwarf Irregular Galaxy NGC 6822
손영종,강아람,한원용,박장현,김호일,김재우,신인구,천상현 한국우주과학회 2008 Journal of Astronomy and Space Sciences Vol.25 No.3
We report the distance modulus of nearby dwarf irregular galaxy NGC 6822 estimated from the so-called Tip of Red-giant Branch (TRGB) method. To detect the apparent magnitudes of the TRGB we use the color-magnitude diagrams (CMDs) and luminosity functions (LFs) in the near-infrared $JHK$ bands. Foreground stars, main-sequence stars, and supergiant stars have been classified on the $(g-K,g)$ plane and removed on the near-infrared CMDs, from which only RGB and AGB stars are remained on the CMDs and LFs. By applying the Savitzky-Golay filter to the obtained LFs and detecting the peak in the second derivative of the observed LFs, we determined the apparent magnitudes of the TRGB. Theoretical absolute magnitudes of the TRGB are estimated from Yonsei-Yale isochrones with the age of 12 Gyr and the metallicity range of $-2.0<$[Fe/H]$<-0.5$. The derived values of distance modulus to NGC 6822 are $(m-M)=23.35\pm0.26, 23.20\pm0.42,$ and $23.27\pm0.50$ for $J, H,$ and $K$ bands, respectively. Distance modulus in bolometric magnitude is also derived as $(m-M)=23.41\pm0.17$. We compare the derived values of the TRGB distance modulus to NGC 6822 in the near-infrared bands with the previous results in other bands. We report the distance modulus of nearby dwarf irregular galaxy NGC 6822 estimated from the so-called Tip of Red-giant Branch (TRGB) method. To detect the apparent magnitudes of the TRGB we use the color-magnitude diagrams (CMDs) and luminosity functions (LFs) in the near-infrared $JHK$ bands. Foreground stars, main-sequence stars, and supergiant stars have been classified on the $(g-K,g)$ plane and removed on the near-infrared CMDs, from which only RGB and AGB stars are remained on the CMDs and LFs. By applying the Savitzky-Golay filter to the obtained LFs and detecting the peak in the second derivative of the observed LFs, we determined the apparent magnitudes of the TRGB. Theoretical absolute magnitudes of the TRGB are estimated from Yonsei-Yale isochrones with the age of 12 Gyr and the metallicity range of $-2.0<$[Fe/H]$<-0.5$. The derived values of distance modulus to NGC 6822 are $(m-M)=23.35\pm0.26, 23.20\pm0.42,$ and $23.27\pm0.50$ for $J, H,$ and $K$ bands, respectively. Distance modulus in bolometric magnitude is also derived as $(m-M)=23.41\pm0.17$. We compare the derived values of the TRGB distance modulus to NGC 6822 in the near-infrared bands with the previous results in other bands.
KMT-2018-BLG-0029LB: A VERY LOW MASS-RATIO Spitzer MICROLENS PLANET
Andrew Gould,류윤현,Sebastiano Calchi Novati,Weicheng Zang,Michael D. Albrow,정선주,CHEONGHOHAN,황규하,정연길,신인구,Yossi Shvartzvald,Jennifer C. Yee,차상목,Dong-Jin Kim,김현우,김승리,이정욱,Dong-Joo Lee,이용석,Byeong-Gon Park,Ri 한국천문학회 2020 Journal of The Korean Astronomical Society Vol.53 No.1
At q = 1.81+/-0.20*10^{-5}, KMT-2018-BLG-0029Lb has the lowest planet-host mass ratio q of any microlensing planet to date by more than a factor of two. Hence, it is the first planet that probes below the apparent "pile-up" at q = 5-10*10^{-5}. The event was observed by Spitzer, yielding a microlens-parallax pi_E measurement. Combined with a measurement of the Einstein radius theta_E from finite-source effects during the caustic crossings, these measurements imply masses of the host M_host = 1.14+0.10-0.12 M_sun and planet M_planet = 7.59+0.75-0.69 M_Earth, system distance D_L = 3.38+0.22-0.26 kpc and projected separation a_p = 4.27+0.21-0.23 au. The blended light, which is substantially brighter than the microlensed source, is plausibly due to the lens and could be observed at high resolution immediately.
OGLE-2019-BLG-0362Lb: A Super-Jovian-Mass Planet around A Low-Mass Star
정선주,Jennifer C. Yee,Andrej Udalski,Andrew Gould,Michael D. Albrow,정연길,황규하,CHEONGHOHAN,Yoon-Hyun Ryu,신인구,Yossi Shvartzvald,Weicheng Zang,차상목,Dong Jin Kim,김승리,이충욱,Dong-Joo Lee,이용석,Byeong-Gon Park,Richar 한국천문학회 2022 Journal of The Korean Astronomical Society Vol.55 No.4
We present the analysis of a planetary microlensing event OGLE-2019-BLG-0362 with a short-duration anomaly (~0.4 days) near the peak of the light curve, which is caused by the resonant caustic. The event has a severe degeneracy with $\delcs = 0.9$ between the close and the wide binary lens models both with planet-host mass ratio $q \simeq 0.007$. We measure the angular Einstein radius but not the microlens parallax, and thus we perform a Bayesian analysis to estimate the physical parameters of the lens. We find that the OGLE-2019-BLG-0362L system is a super-Jovian-mass planet $M_{\rm p}=3.26^{+0.83}_{-0.58}~M_{\rm J}$ orbiting an M dwarf $M_{\rm h}=0.42^{+0.34}_{-0.23}~M_{\odot}$ at a distance $D_{\rm L} =5.83^{+1.04}_{-1.55}$ kpc. The projected star-planet separation is $a_{\perp} = 2.18^{+0.58}_{-0.72}~{\rm AU}$, which indicates that the planet lies beyond the snow line of the host star.