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1. Search for Exoplanets around Northern Circumpolar Stars V. Three likely planetary companions to the giant stars HD 19615, HD 150010, and HD 174205

Author

Jeong, G., Lee, B. C., Park, M. G., Bang, T. Y., and Han, I.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Aims. We report the detection of long-period radial velocity (RV) variations in three giant stars, HD 19615, HD 150010, and HD 174205, using precise RV measurements. Methods. These detections are part of the Search for Exoplanets around Northern Circumpolar Stars (SENS) survey being conducted at the Bohyunsan Optical Astronomy Observatory (BOAO). The nature of the RV variations was investigated by analyzing the photometric and line shape variations. We found no variability with the RV period in these quantities and conclude that the RV variations are most likely caused by planetary companions. Results. Orbital solutions for the three stars yield orbital periods of 402 d, 562 d, and 582 d and minimum masses of 8.5 MJ , 2.4 MJ , and 4.2 MJ , respectively. These masses and periods are typical for planets around intermediate-mass stars, although some unclear interpretations and recent studies may being calling some planet convictions into question. Nevertheless, the SENS program is contributing to our knowledge of giant planets around intermediate-mass stars., Comment: 6 pages, 4 figures

Published
2021
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2. Stellar Interferometry for Gravitational Waves

Author

Park, I. H., Choi, K. -Y., Hwang, J., Jung, S., Kim, D. H., Kim, M. H., Lee, C. -H., Lee, K. H., Oh, S. H., Park, M. -G., Park, S. C., Pozanenko, A., Rho, C. D., Vedenkin, N., and Won, E.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, General Relativity and Quantum Cosmology
Abstract

We propose a new method to detect gravitational waves, based on spatial coherence interferometry with stellar light, as opposed to the conventional temporal coherence interferometry with laser sources. The proposed method detects gravitational waves by using two coherent beams of light from a single distant star measured at separate space-based detectors with a long baseline. This method can be applied to either the amplitude or intensity interferometry. This experiment allows for the search of gravitational waves in the lower frequency range of $10^{-6}$ to $10^{-4}$ Hz. In this work, we present the detection sensitivity of the proposed stellar interferometer by taking the detector response and shot and acceleration noises into account. Furthermore, the proposed experimental setup is capable of searching for primordial black holes and studying the size of the target neutron star, which are also discussed in the paper., Comment: 12 pages, 7 figures

Published
2019
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4. Physics Potentials with the Second Hyper-Kamiokande Detector in Korea

Author

proto-collaboration, Hyper-Kamiokande, Abe, K., Abe, Ke., Ahn, S. H., Aihara, H., Aimi, A., Akutsu, R., Andreopoulos, C., Anghel, I., Anthony, L. H. V., Antonova, M., Ashida, Y., Aushev, V., Barbi, M., Barker, G. J., Barr, G., Beltrame, P., Berardi, V., Bergevin, M., Berkman, S., Berns, L., Berry, T., Bhadra, S., no, D. Bravo-Bergu, Blaszczyk, F. d. M., Blondel, A., Bolognesi, S., Boyd, S. B., Bravar, A., Bronner, C., Avanzini, M. Buizza, Cafagna, F. S., Cheon, B. G., Cheoun, M. K., Cho, K., Choi, K. Y., Chun, E. J., Cole, A., Calland, R., Cao, S., Cartwright, S. L., Catanesi, M. G., Checchia, C., Chen-Wishart, Z., Choi, J. H., Choi, K., Coleman, J., Collazuol, G., Cowan, G., Cremonesi, L., Dealtry, T., De Rosa, G., Densham, C., Dewhurst, D., Drakopoulou, E. L., Di Lodovico, F., Drapier, O., Dumarchez, J., Dunne, P., Dziewiecki, M., Emery, S., Esmaili, A., Evangelisti, A., Fernandez-Martinez, E., Feusels, T., Finch, A., Fiorentini, G. A., Fiorillo, G., Fitton, M., Frankiewicz, K., Friend, M., Fujii, Y., Fukuda, Y., Fukuda, D., Ganezer, K., Ghosh, M., Giganti, C., Gonin, M., Grant, N., Gumplinger, P., Hadley, D. R., Hartfiel, B., Hartz, M., Hayato, Y., Hayrapetyan, K., Hill, J., Hirota, S., Horiuchi, S., Ichikawa, A. K., Iijima, T., Ikeda, M., Imber, J., Inoue, K., Insler, J., Intonti, R. A., Ioannisian, A., Ishida, T., Ishino, H., Ishitsuka, M., Itow, Y., Iwamoto, K., Izmaylov, A., Jamieson, B., Jang, H. I., Jang, J. S., Jeon, S. H., Jeong, K. S., Jiang, M., Jonsson, P., Joo, K. K., Kaboth, A., Kachulis, C., Kajita, T., Kang, S. K., Kameda, J., Kataoka, Y., Katori, T., Kayrapetyan, K., Kearns, E., Khabibullin, M., Khotjantsev, A., Kim, C. S., Kim, H. B., Kim, H. J., Kim, J. H., Kim, J. -S., Kim, J. Y., Kim, S. B., Kim, S. C., Kim, S. -W., Kim, S. Y., King, S., Kim, T. J., Kim, W., Kishimoto, Y., Ko, P., Kobayashi, T., Koga, M., Konaka, A., Kormos, L. L., Koshio, Y., Korzenev, A., Kowalik, K. L., Kropp, W. R., Kudenko, Y., Kurjata, R., Kutter, T., Kuze, M., Kwak, K., Kwon, E. H., Labarga, L., Lagoda, J., Lasorak, P. J. J., Laveder, M., Lawe, M., Learned, J. G., Lee, C. H., Lee, S. J., Lee, W. J., Lim, I. T., Lindner, T., Litchfield, R. P., Longhin, A., Loverre, P., Lou, T., Ludovici, L., Ma, W., Magaletti, L., Mahn, K., Malek, M., Maret, L., Mariani, C., Martens, K., Marti, Ll., Martin, J. F., Marzec, J., Matsuno, S., Mazzucato, E., McCarthy, M., McCauley, N., McFarland, K. S., McGrew, C., Mefodiev, A., Mermod, P., Metelko, C., Mezzetto, M., Migenda, J., Mijakowski, P., Minakata, H., Minamino, A., Mine, S., Mineev, O., Mitra, A., Miura, M., Mochizuki, T., Monroe, J., Moon, C. S., Moon, D. H., Moriyama, S., Mueller, T., Muheim, F., Murase, K., Muto, F., Nakahata, M., Nakajima, Y., Nakamura, K., Nakaya, T., Nakayama, S., Nantais, C., Needham, M., Nicholls, T., Nishimura, Y., Noah, E., Nova, F., Nowak, J., Nunokawa, H., Obayashi, Y., Oh, Y. D., Oh, Y., O'Keeffe, H. M., Okajima, Y., Okumura, K., Onishchuk, Yu., O'Sullivan, E., O'Sullivan, L., Ovsiannikova, T., Owen, R. A., Oyama, Y., Pac, M. Y., Palladino, V., Palomino, J. L., Paolone, V., Park, H. S., Park, J. C., Park, M. G., Park, S. C., Parker, W., Parsa, S., Payne, D., Perkin, J. D., Pidcott, C., Guerra, E. Pinzon, Playfer, S., Popov, B., Posiadala-Zezula, M., Poutissou, J. -M., Pritchard, A., Prouse, N. W., Pronost, G., Przewlocki, P., Quilain, B., Quinto, M., Radicioni, E., Ratoff, P. N., Retiere, F., Riccio, C., Richards, B., Rondio, E., Rose, H. J., Rott, C., Rountree, S. D., Ruggeri, A. C., Rychter, A., Ryu, D., Sacco, R., Sakuda, M., Sanchez, M. C., Scantamburlo, E., Scott, M., Sedgwick, S. Molina, Seiya, Y., Sekiguchi, T., Sekiya, H., Seo, H., Seo, S. H., Sgalaberna, D., Shah, R., Shaikhiev, A., Shimizu, I., Shiozawa, M., Shitov, Y., Short, S., Simpson, C., Sinnis, G., Smy, M. B., Snow, S., Sobczyk, J., Sobel, H. W., Son, D. C., Sonoda, Y., Spina, R., Stewart, T., Stone, J. L., Suda, Y., Suwa, Y., Suzuki, Y., Suzuki, A. T., Svoboda, R., Taani, M., Tacik, R., Takeda, A., Takenaka, A., Taketa, A., Takeuchi, Y., Takhistov, V., Tanaka, H. A., Tanaka, H. K. M., Tanaka, H., Terri, R., Thiesse, M., Thompson, L. F., Thorpe, M., Tobayama, S., Touramanis, C., Towstego, T., Tsukamoto, T., Tsui, K. M., Tzanov, M., Uchida, Y., Vagins, M. R., Vasseur, G., Vilela, C., Vogelaar, R. B., Walding, J., Walker, J., Ward, M., Wark, D., Wascko, M. O., Weber, A., Wendell, R., Wilkes, R. J., Wilking, M. J., Wilson, J. R., Won, E., Xin, T., Yamamoto, K., Yanagisawa, C., Yano, T., Yasuda, O., Yen, S., Yershov, N., Yeum, D. N., Yokoyama, M., Yoo, H. D., Yoo, J., Yoon, S. C., Yoon, T. S., Yoshida, T., Yu, I., Yu, M., Zalipska, J., Zaremba, K., Ziembicki, M., Zito, M., and Zsoldos, S.

Subjects
High Energy Physics - Experiment, High Energy Physics - Phenomenology, Physics - Instrumentation and Detectors
Abstract

Hyper-Kamiokande consists of two identical water-Cherenkov detectors of total 520~kt with the first one in Japan at 295~km from the J-PARC neutrino beam with 2.5$^{\textrm{o}}$ Off-Axis Angles (OAAs), and the second one possibly in Korea in a later stage. Having the second detector in Korea would benefit almost all areas of neutrino oscillation physics mainly due to longer baselines. There are several candidate sites in Korea with baselines of 1,000$\sim$1,300~km and OAAs of 1$^{\textrm{o}}$$\sim$3$^{\textrm{o}}$. We conducted sensitivity studies on neutrino oscillation physics for a second detector, either in Japan (JD $\times$ 2) or Korea (JD + KD) and compared the results with a single detector in Japan. Leptonic CP violation sensitivity is improved especially when the CP is non-maximally violated. The larger matter effect at Korean candidate sites significantly enhances sensitivities to non-standard interactions of neutrinos and mass ordering determination. Current studies indicate the best sensitivity is obtained at Mt. Bisul (1,088~km baseline, $1.3^\circ$ OAA). Thanks to a larger (1,000~m) overburden than the first detector site, clear improvements to sensitivities for solar and supernova relic neutrino searches are expected., Comment: 102 pages, 49 figures. Accepted by PTEP

Published
2016
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5. Search for exoplanet around northern circumpolar stars - Four planets around HD 11755, HD 12648, HD 24064, and 8 Ursae Minoris

Author

Lee, B. -C., Park, M. -G., Lee, S. -M., Jeong, G., Oh, H. -I., Han, I., Lee, J. W., Lee, C. -U., Kim, S. -L., and Kim, K. -M.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Aims. This program originated as the north pole region extension of the established exoplanet survey using 1.8 m telescope at Bohyunsan Optical Astronomy Observatory (BOAO). The aim of our paper is to find exoplanets in northern circumpolar stars with a precise radial velocity (RV) survey. Methods. We have selected about 200 northern circumpolar stars with the following criteria: Dec. > 70 degree, 0.6 < B-V < 1.6, HIPPARCOS_scat < 0.05 magnitude, and 5.0 < mv < 7.0. The high-resolution, fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) was used for the RV survey. Chromospheric activities, the HIPPARCOS photometry, and line bisectors were analyzed to exclude other causes for the RV variations. Results. In 2010, we started to monitor the candidates and have completed initial screening for all stars for the last five years. We present the detection of four new exoplanets. Stars HD 11755, HD 12648, HD 24064, and 8 UMi all show evidence for giant planets in Keplerian motion. The companion to HD 11755 has a minimum mass of 6.5 M_Jup in a 433-day orbit with an eccentricity of 0.19. HD 12648 is orbited by a companion of minimum mass of 2.9 M_Jup having a period of 133 days and an eccentricity of 0.04. Weak surface activity was suspected in HD 24064. However, no evidence was found to be associated with the RV variations. Its companion has a minimum mass of 9.4 M_Jup, a period of 535 days, and an eccentricity of 0.35. Finally, 8 UMi has a minimum mass of 1.5 M_Jup, a period of 93 days with an eccentricity of 0.06., Comment: 9 pages, 14 figures, 6 tables, accepted for publisation in Astronomy & Astrophysics

Published
2015
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6. Low-amplitude and long-period radial velocity variations in giants HD 3574, 63 Cygni, and HD 216946 (Research Note)

Author

Lee, B. -C., Han, I., Park, M. -G., Hatzes, A. P., and Kim, K. -M.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Aims. We study the low-amplitude and long-period variations in evolved stars using precise radial velocity measurements. Methods. The high-resolution, fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) was used from September 2004 to May 2014 as part of the exoplanet search program at the Bohyunsan Optical Astronomy Observatory (BOAO). Results. We report the detection of low-amplitude and long-period orbital radial velocity variations in three evolved stars, HD 3574, 63 Cyg, and HD 216946. They have periods of 1061, 982, and 1382 days and semi-amplitudes of 376, 742, and 699 m/s, respectively., Comment: 6 pages, 7 figures, 4 tables, accepted for publisation in Astronomy & Astrophysics

Published
2014
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7. Planetary companions in K giants beta Cancri, mu Leonis, and beta Ursae Minoris

Author

Lee, B. -C., Han, I., Park, M. -G., Mkrtichian, D. E., Hatzes, A. P., and Kim, K. -M.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Auns. The aim of our paper is to investigate the low-amplitude and long-period variations in evolved stars with a precise radial velocity (RV) survey. Methods. The high-resolution, the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) was used from 2003 to 2013 for a radial velocity survey of giant stars as part of the exoplanet search program at Bohyunsan Optical Astronomy Observatory (BOAO). Results. We report the detection of three new planetary companions orbiting the K giants beta Cnc, mu Leo, and beta UMi. The planetary nature of the radial velocity variations is supported by analyzes of ancillary data. The HIPPARCOS photometry shows no variations with periods close to those in RV variations and there is no strong correlation between the bisector velocity span (BVS) and the radial velocities for each star. Furthermore, the stars show weak or no core reversal in Ca II H lines indicating that they are inactive stars. The companion to beta Cnc has a minimum mass of 7.8 M_Jup in a 605-day orbit with an eccentricity of 0.08. The giant mu Leo is orbited by a companion of minimum mass of 2.4 M_Jup having a period of 357 days and an eccentricity of 0.09. The giant beta UMi is a known barium star and is suspected of harboring a white dwarf or substellar mass companion. Its companion has a minimum mass of 6.1 M_Jup, a period of 522 days, and an eccentricity e = 0.19., Comment: 9 pages (with 2 online), 11 figures, 6 tables, accepted for publisation in Astronomy & Astrophysics

Published
2014
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8. Detection of an exoplanet around the evolved K giant HD 66141

Author

Lee, B. -C., Mkrtichian, D. E., Han, I., Park, M. -G., and Kim, K. -M.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Aims. We have been carrying out a precise radial velocity (RV) survey for K giants to search for and study the origin of the lowamplitude and long-periodic RV variations. Methods. We present high-resolution RV measurements of the K2 giant HD 66141 from December 2003 to January 2011 using the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory (BOAO). Results. We find that the RV measurements for HD 66141 exhibit a periodic variation of 480.5 +/- 0.5 days with a semi-amplitude of 146.2 +/- 2.7 m/s. The Hipparcos photometry and bisector velocity span (BVS) do not show any obvious correlations with RV variations. We find indeed 706.4 +/- 35.0 day variations in equivalent width (EW) measurements of H_alpha line and 703.0 +/- 39.4 day variations in a space-born measurements 1.25{\mu} flux of HD 66141 measured during COBE/DIRBE experiment. We reveal that a mean value of long-period variations is about 705 +/- 53 days and the origin is a rotation period of the star and variability that is caused by surface inhomogeneities. For the 480 day periods of RV variations an orbital motion is the most likely explanation. Assuming a stellar mass of 1.1 +/- 0.1 M_Sun? for HD 66141, we obtain a minimum mass for the planetary companion of 6.0 +/- 0.3 M_Jup with an orbital semi-major axis of 1.2 +/- 0.1 AU and an eccentricity of 0.07 +/- 0.03., Comment: 7 pages, 10 figures, 3 tables, accepted for publisation in Astronomy & Astrophysics

Published
2012
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9. Planetary companions orbiting M giants HD 208527 and HD 220074

Author

Lee, B. -C., Han, I., and Park, M. -G.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Aims. The purpose of the present study is to research the origin of planetary companions by using a precise radial velocity (RV) survey. Methods. The high-resolution spectroscopy of the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory (BOAO) is used from September 2008 to June 2012. Results. We report the detection of two exoplanets in orbit around HD 208527 and HD 220074 exhibiting periodic variations in RV of 875.5 +/- 5.8 and 672.1 +/- 3.7 days. The RV variations are not apparently related to the surface inhomogeneities and a Keplerian motion of the planetary companion is the most likely explanation. Assuming possible stellar masses of 1.6 +/- 0.4 and 1.2 +/- 0.3 M_Sun, we obtain the minimum masses for the exoplanets of 9.9 +/- 1.7 and 11.1 +/- 1.8 M_Jup around HD 208527 and HD 220074 with an orbital semi-major axis of 2.1 +/- 0.2 and 1.6 +/- 0.1 AU and an eccentricity of 0.08 and 0.14, respectively. We also find that the previously known spectral classification of HD 208527 and HD 220074 was in error: Our new estimation of stellar parameters suggest that both HD 208527 and HD 220074 are M giants. Therefore, HD 208527 and HD 220074 are so far the first candidate M giants to harbor a planetary companion., Comment: 7 pages, 9 figures, 4 tables, accepted for publisation in Astronomy & Astrophysics

Published
2012
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10. A likely exoplanet orbiting the oscillating K-giant {\alpha} Arietis

Author

Lee, B. -C., Mkrtichian, D. E., Han, I., Kim, K. -M., and Park, M. -G.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Aims. To search for extrasolar planets around intermediate-mass stars, we are conducting a precise RV survey around K-giants. Methods. We present high-accuracy RV measurements of {\alpha} Ari made from November 2003 to February 2010. This star belongs to our sample of 55 K-giants studied for extrasolar planet and pulsation searches using the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) attached to the 1.8-m telescope at Bohyunsan Optical Astronomy Observatory (BOAO) in Korea. Results. We find a planetary companion with long-period and low-amplitude radial velocity (RV) variations in oscillating K2 III star {\alpha} Ari (HD 12929). We do not find the correlation between RV variations and chromospheric activity indicators (Ca II H & K region, H{\alpha} line). The bisector analysis also shows that the bisector velocity span (BVS) does not show any obvious correlation with RV variation but has periodic component that may be attributed to the rotation of the star. If the RV variation is indeed caused by a planetary companion, an orbital solution with a period of P = 381 days, a semi-amplitude of K = 41 m/s, and an eccentricity of e = 0.25 fits the data best. Assuming a possible stellar mass of M_star = 1.5 M_sun, we estimate the minimum mass for the planetary companion of m2 sin i = 1.8 M_Jupiter with an orbital semi-major axis of 1.2 AU. Conclusions. Our finding of a likely exoplanet in {\alpha} Ari supports searching for extrasolar planets around giant stars with multiperiodic oscillations., Comment: 6 pages, 9 figures, 2 tables

Published
2011
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13. Stellar interferometry for gravitational waves

Author

Park, I.H., primary, Choi, K.-Y., additional, Hwang, J., additional, Jung, S., additional, Kim, D.H., additional, Kim, M.H., additional, Lee, C.-H., additional, Lee, K.H., additional, Oh, S.H., additional, Park, M.-G., additional, Park, S.C., additional, Pozanenko, A., additional, Rho, C.D., additional, Vedenkin, N., additional, and Won, E., additional

Published
2021
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16. Ethyl formate as a methyl bromide alternative for phytosanitary disinfestation of imported banana in Korea with logistical considerations

Author

Park, M-G, Park, C-G, Yang, J-O, Kim, G-H, Ren, Y., Lee, B-H, Cha, D.H., Neven, L., Park, M-G, Park, C-G, Yang, J-O, Kim, G-H, Ren, Y., Lee, B-H, Cha, D.H., and Neven, L.

Abstract

Methyl bromide (MB) use for quarantine and phytosanitary purposes is being phased out. Several effective MB alternatives have been identified depending on the target system. Industry commitment for the shift to new technologies will depend not only on the efficacy of alternatives but also on their compatibility and integrability into existing operations. We compared the efficacy of MB and ethyl formate (EF) for disinfestation of Planococcus citri (Risso) (Hemiptera: Pseudococcidae) as a representative surface pest on banana and evaluated whether EF fumigation is compatible with the current packaging materials and loading ratio used by the South Korean banana import industry. Fumigation trials with P. citri adults and eggs showed that EF was at least as effective as MB at the EF and MB concentrations recommended under the current phytosanitary disinfestation guidelines. From a logistical standpoint, EF gas could not effectively penetrate plastic bagging typically used in banana cartons during commercial shipping. Also, EF sorption to bananas and packing materials (used as cushioning inside bagging) further lowered realized EF concentrations around bananas. These reductions in EF concentration translated into reduced mortality of P. citri eggs, indicating that despite similar efficacy of MB and EF for controlling P. citri, further consideration and optimization of other industry logistics such as packaging and loading ratio is necessary to enhance the adoption of this MB alternative.

Published
2020

17. Postharvest treatment of mandarin fruit using a combination of methyl bromide and phosphine against Bactrocera dorsalis (Diptera: Tephritidae)

Author

Li, L., Zhang, G., Li, B., Yang, J.O., Park, M‐G, Liu, T., Li, L., Zhang, G., Li, B., Yang, J.O., Park, M‐G, and Liu, T.

Abstract

BACKGROUND Chinese Nanfeng mandarin (Citrus reticulate Blanco ‘2–6’) fruit is host to the oriental fruit fly Bactrocera dorsalis Hendel, and therefore requires phytosanitary treatment before exporting abroad. The use of methyl bromide (MB) should be reduced because it has phytotoxic and ozone depleting properties. In the present study, fumigations with mixtures of gaseous phosphine (PH3) and MB were conducted to disinfest B. dorsalis. The effect of combined fumigation on postharvest quality of Nanfeng mandarin fruit was then evaluated. RESULTS There was a clear synergistic effect between MB and PH3 against B. dorsalis at 20 °C. The third‐instar larvae of B. dorsalis were the most tolerant to treatment with both MB alone and combined with PH3. Toxicity assay of third instars indicated that higher PH3 concentrations increased MB toxicity, and 1.42–2.84 g m−3 of PH3 was optimal when combined with MB. Probit analysis showed that, combined with 2.13 g m−3 PH3, similar mortality was achieved with 50% of the MB required when applied alone. Furthermore, the fruit quality test showed that MB fumigation resulted in a higher respiration rate and >40% fruit rot after storage. The combined treatment reduced these effects and did not have adverse effects on fruit firmness, soluble solid content, titratable acidity, or vitamin C content. CONCLUSION Our findings demonstrate the synergistic effect between PH3 and MB and indicate that this treatment has potential as a novel strategy for postharvest control of B. dorsalis, especially in MB‐sensitive fruit.

Published
2020

20. Physics potentials with the second Hyper-Kamiokande detector in Korea Proceedings of the KOSEF-JSPS Joint Seminar on New Developments in Neutrino Physics, Seoul, Korea, 2000 'Highlights in the T2KK Workshops in 2005 and 2006', 'T2K neutrino oscillation results with data up to 2017 summer' 'Conceptual Design Report' 'Hyper-Kamiokande Design Report' 'Near Detectors based on gas TPCs for neutrino long baseline experiments' Scientific Reports 5, Article number: 15225

Author

Abe, K, Abe, Ke, Ahn, S H, Aihara, H, Aimi, A, Akutsu, R, Andreopoulos, C, Anghel, I, Anthony, L H V, Antonova, M, Ashida, Y, Aushev, V, Barbi, M, Barker, G J, Barr, G, Beltrame, P, Berardi, V, Bergevin, M, Berkman, S, Berns, L, Berry, T, Bhadra, S, Blaszczyk, F d M, Blondel, A, Bolognesi, S, Boyd, S B, Bravar, A, Bronner, C, Buizza Avanzini, M, Cafagna, F S, Calland, R, Cao, S, Cartwright, S L, Catanesi, M G, Checchia, C, Chen-Wishart, Z, Cheon, B G, Cheoun, M K, Cho, K, Choi, J H, Choi, K, Choi, K Y, Chun, E J, Cole, A, Coleman, J, Collazuol, G, Cowan, G, Cremonesi, L, Dealtry, T, De Rosa, G, Densham, C, Dewhurst, D, Drakopoulou, E, Di Lodovico, F, Drapier, O, Dumarchez, J, Dunne, P, Dziewiecki, M, Emery, S, Esmaili, A, Evangelisti, A, Fernández-Martinez, E, Feusels, T, Finch, A, Fiorentini, G A, Fiorillo, G, Fitton, M, Frankiewicz, K, Friend, M, Fujii, Y, Fukuda, Y, Fukuda, D, Ganezer, K, Ghosh, M, Giganti, C, Gonin, M, Grant, N, Gumplinger, P, Hadley, D R, Hartfiel, B, Hartz, M, Hayato, Y, Hayrapetyan, K, Hill, J, Hirota, S, Horiuchi, S, Ichikawa, A K, Iijima, T, Ikeda, M, Imber, J, Inoue, K, Insler, J, Intonti, R A, Ioannisian, A, Ishida, T, Ishino, H, Ishitsuka, M, Itow, Y, Iwamoto, K, Izmaylov, A, Jamieson, B, Jang, H I, Jang, J S, Jeon, S H, Jeong, K S, Jiang, M, Jonsson, P, Joo, K K, Kaboth, A, Kachulis, C, Kajita, T, Kang, S K, Kameda, J, Kataoka, Y, Katori, T, Kayrapetyan, K, Kearns, E, Khabibullin, M, Khotjantsev, A, Kim, C S, Kim, H B, Kim, H J, Kim, J H, Kim, J-S, Kim, J Y, Kim, S B, Kim, S C, Kim, S-W, Kim, S Y, Kim, T J, Kim, W, King, S, Kishimoto, Y, Ko, P, Kobayashi, T, Koga, M, Konaka, A, Kormos, L L, Koshio, Y, Korzenev, A, Kowalik, K L, Kropp, W R, Kudenko, Y, Kurjata, R, Kutter, T, Kuze, M, Kwak, K, Kwon, E H, Labarga, L, Lagoda, J, Lasorak, P J J, Laveder, M, Lawe, M, Learned, J G, Lee, C H, Lee, S J, Lee, W J, Lim, I T, Lindner, T, Litchfield, R P, Longhin, A, Loverre, P, Lou, T, Ludovici, L, Ma, W, Magaletti, L, Mahn, K, Malek, M, Maret, L, Mariani, C, Martens, K, Marti, Ll, Martin, J F, Marzec, J, Matsuno, S, Mazzucato, E, McCarthy, M, McCauley, N, McFarland, K S, McGrew, C, Mefodiev, A, Mermod, P, Metelko, C, Mezzetto, M, Migenda, J, Mijakowski, P, Minakata, H, Minamino, A, Mine, S, Mineev, O, Mitra, A, Miura, M, Mochizuki, T, Monroe, J, Moon, C S, Moon, D H, Moriyama, S, Mueller, T, Muheim, F, Murase, K, Muto, F, Nakahata, M, Nakajima, Y, Nakamura, K, Nakaya, T, Nakayama, S, Nantais, C, Needham, M, Nicholls, T, Nishimura, Y, Noah, E, Nova, F, Nowak, J, Nunokawa, H, Obayashi, Y, Oh, Y D, Oh, Y, O’Keeffe, H M, Okajima, Y, Okumura, K, Onishchuk, Yu, O’Sullivan, E, O’Sullivan, L, Ovsiannikova, T, Owen, R A, Oyama, Y, Pérez, J, Pac, M Y, Palladino, V, Palomino, J L, Paolone, V, Park, H S, Park, J C, Park, M G, Park, S C, Parker, W, Parsa, S, Payne, D, Perkin, J D, Pidcott, C, Pinzon Guerra, E, Playfer, S, Popov, B, Posiadala-Zezula, M, Poutissou, J-M, Pritchard, A, Prouse, N W, Pronost, G, Przewlocki, P, Quilain, B, Quinto, M, Radicioni, E, Ratoff, P N, Retiere, F, Riccio, C, Richards, B, Rondio, E, Rose, H J, Rott, C, Rountree, S D, Ruggeri, A C, Rychter, A, Ryu, D, Sacco, R, Sakuda, M, Sanchez, M C, Scantamburlo, E, Scott, M, Molina Sedgwick, S, Seiya, Y, Sekiguchi, T, Sekiya, H, Seo, H, Seo, S H, Sgalaberna, D, Shah, R, Shaikhiev, A, Shimizu, I, Shiozawa, M, Shitov, Y, Short, S, Simpson, C, Sinnis, G, Smy, M B, Snow, S, Sobczyk, J, Sobel, H W, Son, D C, Sonoda, Y, Spina, R, Stewart, T, Stone, J L, Suda, Y, Suwa, Y, Suzuki, Y, Suzuki, A T, Svoboda, R, Taani, M, Tacik, R, Takeda, A, Takenaka, A, Taketa, A, Takeuchi, Y, Takhistov, V, Tanaka, H A, Tanaka, H K M, Tanaka, H, Terri, R, Thiesse, M, Thompson, L F, Thorpe, M, Tobayama, S, Touramanis, C, Towstego, T, Tsukamoto, T, Tsui, K M, Tzanov, M, Uchida, Y, Vagins, M R, Vasseur, G, Vilela, C, Vogelaar, R B, Walding, J, Walker, J, Ward, M, Wark, D, Wascko, M O, Weber, A, Wendell, R, Wilkes, R J, Wilking, M J, Wilson, J R, Won, E, Xin, T, Yamamoto, K, Yanagisawa, C, Yano, T, Yasuda, O, Yen, S, Yershov, N, Yeum, D N, Yokoyama, M, Yoo, H D, Yoo, J, Yoon, S C, Yoon, T S, Yoshida, T, Yu, I, Yu, M, Zalipska, J, Zaremba, K, Ziembicki, M, Zito, M, and Zsoldos, S

Subjects
Physics::Instrumentation and Detectors, High Energy Physics::Experiment
Abstract

Hyper-Kamiokande consists of two identical water-Cherenkov detectors of total 520 kt, with the first one in Japan at 295 km from the J-PARC neutrino beam with 2.5 off-axis angles (OAAs), and the second one possibly in Korea at a later stage. Having the second detector in Korea would benefit almost all areas of neutrino oscillation physics, mainly due to longer baselines. There are several candidate sites in Korea with baselines of 1000–1300 km and OAAs of 1–3. We conducted sensitivity studies on neutrino oscillation physics for a second detector, either in Japan (JD 2) or Korea (JD + KD), and compared the results with a single detector in Japan. Leptonic charge–parity (CP) symmetry violation sensitivity is improved, especially when the CP is non-maximally violated. The larger matter effect at Korean candidate sites significantly enhances sensitivities to non-standard interactions of neutrinos and mass ordering determination. Current studies indicate the best sensitivity is obtained at Mt. Bisul (1088 km baseline, OAA). Thanks to a larger (1000 m) overburden than the first detector site, clear improvements to sensitivities for solar and supernova relic neutrino searches are expected.

Published
2018

21. Physics potentials with the second Hyper-Kamiokande detector in Korea

Author

Abe, K, Abe, Ke, Ahn, S H, Aihara, H, Aimi, A, Akutsu, R, Andreopoulos, C, Anghel, I, Anthony, L H V, Antonova, M, Ashida, Y, Aushev, V, Barbi, M, Barker, G J, Barr, G, Beltrame, P, Berardi, V, Bergevin, M, Berkman, S, Berns, L, Berry, T, Bhadra, S, Blaszczyk, F d M, Blondel, A, Bolognesi, S, Boyd, S B, Bravar, A, Bronner, C, Buizza Avanzini, M, Cafagna, F S, Calland, R, Cao, S, Cartwright, S L, Catanesi, M G, Checchia, C, Chen-Wishart, Z, Cheon, B G, Cheoun, M K, Cho, K, Choi, J H, Choi, K, Choi, K Y, Chun, E J, Cole, A, Coleman, J, Collazuol, G, Cowan, G, Cremonesi, L, Dealtry, T, De Rosa, G, Densham, C, Dewhurst, D, Drakopoulou, E, Di Lodovico, F, Drapier, O, Dumarchez, J, Dunne, P, Dziewiecki, M, Emery, S, Esmaili, A, Evangelisti, A, Fernández-Martinez, E, Feusels, T, Finch, A, Fiorentini, G A, Fiorillo, G, Fitton, M, Frankiewicz, K, Friend, M, Fujii, Y, Fukuda, Y, Fukuda, D, Ganezer, K, Ghosh, M, Giganti, C, Gonin, M, Grant, N, Gumplinger, P, Hadley, D R, Hartfiel, B, Hartz, M, Hayato, Y, Hayrapetyan, K, Hill, J, Hirota, S, Horiuchi, S, Ichikawa, A K, Iijima, T, Ikeda, M, Imber, J, Inoue, K, Insler, J, Intonti, R A, Ioannisian, A, Ishida, T, Ishino, H, Ishitsuka, M, Itow, Y, Iwamoto, K, Izmaylov, A, Jamieson, B, Jang, H I, Jang, J S, Jeon, S H, Jeong, K S, Jiang, M, Jonsson, P, Joo, K K, Kaboth, A, Kachulis, C, Kajita, T, Kang, S K, Kameda, J, Kataoka, Y, Katori, T, Kayrapetyan, K, Kearns, E, Khabibullin, M, Khotjantsev, A, Kim, C S, Kim, H B, Kim, H J, Kim, J H, Kim, J-S, Kim, J Y, Kim, S B, Kim, S C, Kim, S-W, Kim, S Y, Kim, T J, Kim, W, King, S, Kishimoto, Y, Ko, P, Kobayashi, T, Koga, M, Konaka, A, Kormos, L L, Koshio, Y, Korzenev, A, Kowalik, K L, Kropp, W R, Kudenko, Y, Kurjata, R, Kutter, T, Kuze, M, Kwak, K, Kwon, E H, Labarga, L, Lagoda, J, Lasorak, P J J, Laveder, M, Lawe, M, Learned, J G, Lee, C H, Lee, S J, Lee, W J, Lim, I T, Lindner, T, Litchfield, R P, Longhin, A, Loverre, P, Lou, T, Ludovici, L, Ma, W, Magaletti, L, Mahn, K, Malek, M, Maret, L, Mariani, C, Martens, K, Marti, Ll, Martin, J F, Marzec, J, Matsuno, S, Mazzucato, E, McCarthy, M, McCauley, N, McFarland, K S, McGrew, C, Mefodiev, A, Mermod, P, Metelko, C, Mezzetto, M, Migenda, J, Mijakowski, P, Minakata, H, Minamino, A, Mine, S, Mineev, O, Mitra, A, Miura, M, Mochizuki, T, Monroe, J, Moon, C S, Moon, D H, Moriyama, S, Mueller, T, Muheim, F, Murase, K, Muto, F, Nakahata, M, Nakajima, Y, Nakamura, K, Nakaya, T, Nakayama, S, Nantais, C, Needham, M, Nicholls, T, Nishimura, Y, Noah, E, Nova, F, Nowak, J, Nunokawa, H, Obayashi, Y, Oh, Y D, Oh, Y, O’Keeffe, H M, Okajima, Y, Okumura, K, Onishchuk, Yu, O’Sullivan, E, O’Sullivan, L, Ovsiannikova, T, Owen, R A, Oyama, Y, Pérez, J, Pac, M Y, Palladino, V, Palomino, J L, Paolone, V, Park, H S, Park, J C, Park, M G, Park, S C, Parker, W, Parsa, S, Payne, D, Perkin, J D, Pidcott, C, Pinzon Guerra, E, Playfer, S, Popov, B, Posiadala-Zezula, M, Poutissou, J-M, Pritchard, A, Prouse, N W, Pronost, G, Przewlocki, P, Quilain, B, Quinto, M, Radicioni, E, Ratoff, P N, Retiere, F, Riccio, C, Richards, B, Rondio, E, Rose, H J, Rott, C, Rountree, S D, Ruggeri, A C, Rychter, A, Ryu, D, Sacco, R, Sakuda, M, Sanchez, M C, Scantamburlo, E, Scott, M, Molina Sedgwick, S, Seiya, Y, Sekiguchi, T, Sekiya, H, Seo, H, Seo, S H, Sgalaberna, D, Shah, R, Shaikhiev, A, Shimizu, I, Shiozawa, M, Shitov, Y, Short, S, Simpson, C, Sinnis, G, Smy, M B, Snow, S, Sobczyk, J, Sobel, H W, Son, D C, Sonoda, Y, Spina, R, Stewart, T, Stone, J L, Suda, Y, Suwa, Y, Suzuki, Y, Suzuki, A T, Svoboda, R, Taani, M, Tacik, R, Takeda, A, Takenaka, A, Taketa, A, Takeuchi, Y, Takhistov, V, Tanaka, H A, Tanaka, H K M, Tanaka, H, Terri, R, Thiesse, M, Thompson, L F, Thorpe, M, Tobayama, S, Touramanis, C, Towstego, T, Tsukamoto, T, Tsui, K M, Tzanov, M, Uchida, Y, Vagins, M R, Vasseur, G, Vilela, C, Vogelaar, R B, Walding, J, Walker, J, Ward, M, Wark, D, Wascko, M O, Weber, A, Wendell, R, Wilkes, R J, Wilking, M J, Wilson, J R, Won, E, Xin, T, Yamamoto, K, Yanagisawa, C, Yano, T, Yasuda, O, Yen, S, Yershov, N, Yeum, D N, Yokoyama, M, Yoo, H D, Yoo, J, Yoon, S C, Yoon, T S, Yoshida, T, Yu, I, Yu, M, Zalipska, J, Zaremba, K, Ziembicki, M, Zito, M, Zsoldos, S, Abe, K, Abe, Ke, Ahn, S H, Aihara, H, Aimi, A, Akutsu, R, Andreopoulos, C, Anghel, I, Anthony, L H V, Antonova, M, Ashida, Y, Aushev, V, Barbi, M, Barker, G J, Barr, G, Beltrame, P, Berardi, V, Bergevin, M, Berkman, S, Berns, L, Berry, T, Bhadra, S, Blaszczyk, F d M, Blondel, A, Bolognesi, S, Boyd, S B, Bravar, A, Bronner, C, Buizza Avanzini, M, Cafagna, F S, Calland, R, Cao, S, Cartwright, S L, Catanesi, M G, Checchia, C, Chen-Wishart, Z, Cheon, B G, Cheoun, M K, Cho, K, Choi, J H, Choi, K, Choi, K Y, Chun, E J, Cole, A, Coleman, J, Collazuol, G, Cowan, G, Cremonesi, L, Dealtry, T, De Rosa, G, Densham, C, Dewhurst, D, Drakopoulou, E, Di Lodovico, F, Drapier, O, Dumarchez, J, Dunne, P, Dziewiecki, M, Emery, S, Esmaili, A, Evangelisti, A, Fernández-Martinez, E, Feusels, T, Finch, A, Fiorentini, G A, Fiorillo, G, Fitton, M, Frankiewicz, K, Friend, M, Fujii, Y, Fukuda, Y, Fukuda, D, Ganezer, K, Ghosh, M, Giganti, C, Gonin, M, Grant, N, Gumplinger, P, Hadley, D R, Hartfiel, B, Hartz, M, Hayato, Y, Hayrapetyan, K, Hill, J, Hirota, S, Horiuchi, S, Ichikawa, A K, Iijima, T, Ikeda, M, Imber, J, Inoue, K, Insler, J, Intonti, R A, Ioannisian, A, Ishida, T, Ishino, H, Ishitsuka, M, Itow, Y, Iwamoto, K, Izmaylov, A, Jamieson, B, Jang, H I, Jang, J S, Jeon, S H, Jeong, K S, Jiang, M, Jonsson, P, Joo, K K, Kaboth, A, Kachulis, C, Kajita, T, Kang, S K, Kameda, J, Kataoka, Y, Katori, T, Kayrapetyan, K, Kearns, E, Khabibullin, M, Khotjantsev, A, Kim, C S, Kim, H B, Kim, H J, Kim, J H, Kim, J-S, Kim, J Y, Kim, S B, Kim, S C, Kim, S-W, Kim, S Y, Kim, T J, Kim, W, King, S, Kishimoto, Y, Ko, P, Kobayashi, T, Koga, M, Konaka, A, Kormos, L L, Koshio, Y, Korzenev, A, Kowalik, K L, Kropp, W R, Kudenko, Y, Kurjata, R, Kutter, T, Kuze, M, Kwak, K, Kwon, E H, Labarga, L, Lagoda, J, Lasorak, P J J, Laveder, M, Lawe, M, Learned, J G, Lee, C H, Lee, S J, Lee, W J, Lim, I T, Lindner, T, Litchfield, R P, Longhin, A, Loverre, P, Lou, T, Ludovici, L, Ma, W, Magaletti, L, Mahn, K, Malek, M, Maret, L, Mariani, C, Martens, K, Marti, Ll, Martin, J F, Marzec, J, Matsuno, S, Mazzucato, E, McCarthy, M, McCauley, N, McFarland, K S, McGrew, C, Mefodiev, A, Mermod, P, Metelko, C, Mezzetto, M, Migenda, J, Mijakowski, P, Minakata, H, Minamino, A, Mine, S, Mineev, O, Mitra, A, Miura, M, Mochizuki, T, Monroe, J, Moon, C S, Moon, D H, Moriyama, S, Mueller, T, Muheim, F, Murase, K, Muto, F, Nakahata, M, Nakajima, Y, Nakamura, K, Nakaya, T, Nakayama, S, Nantais, C, Needham, M, Nicholls, T, Nishimura, Y, Noah, E, Nova, F, Nowak, J, Nunokawa, H, Obayashi, Y, Oh, Y D, Oh, Y, O’Keeffe, H M, Okajima, Y, Okumura, K, Onishchuk, Yu, O’Sullivan, E, O’Sullivan, L, Ovsiannikova, T, Owen, R A, Oyama, Y, Pérez, J, Pac, M Y, Palladino, V, Palomino, J L, Paolone, V, Park, H S, Park, J C, Park, M G, Park, S C, Parker, W, Parsa, S, Payne, D, Perkin, J D, Pidcott, C, Pinzon Guerra, E, Playfer, S, Popov, B, Posiadala-Zezula, M, Poutissou, J-M, Pritchard, A, Prouse, N W, Pronost, G, Przewlocki, P, Quilain, B, Quinto, M, Radicioni, E, Ratoff, P N, Retiere, F, Riccio, C, Richards, B, Rondio, E, Rose, H J, Rott, C, Rountree, S D, Ruggeri, A C, Rychter, A, Ryu, D, Sacco, R, Sakuda, M, Sanchez, M C, Scantamburlo, E, Scott, M, Molina Sedgwick, S, Seiya, Y, Sekiguchi, T, Sekiya, H, Seo, H, Seo, S H, Sgalaberna, D, Shah, R, Shaikhiev, A, Shimizu, I, Shiozawa, M, Shitov, Y, Short, S, Simpson, C, Sinnis, G, Smy, M B, Snow, S, Sobczyk, J, Sobel, H W, Son, D C, Sonoda, Y, Spina, R, Stewart, T, Stone, J L, Suda, Y, Suwa, Y, Suzuki, Y, Suzuki, A T, Svoboda, R, Taani, M, Tacik, R, Takeda, A, Takenaka, A, Taketa, A, Takeuchi, Y, Takhistov, V, Tanaka, H A, Tanaka, H K M, Tanaka, H, Terri, R, Thiesse, M, Thompson, L F, Thorpe, M, Tobayama, S, Touramanis, C, Towstego, T, Tsukamoto, T, Tsui, K M, Tzanov, M, Uchida, Y, Vagins, M R, Vasseur, G, Vilela, C, Vogelaar, R B, Walding, J, Walker, J, Ward, M, Wark, D, Wascko, M O, Weber, A, Wendell, R, Wilkes, R J, Wilking, M J, Wilson, J R, Won, E, Xin, T, Yamamoto, K, Yanagisawa, C, Yano, T, Yasuda, O, Yen, S, Yershov, N, Yeum, D N, Yokoyama, M, Yoo, H D, Yoo, J, Yoon, S C, Yoon, T S, Yoshida, T, Yu, I, Yu, M, Zalipska, J, Zaremba, K, Ziembicki, M, Zito, M, and Zsoldos, S

Abstract

Hyper-Kamiokande consists of two identical water-Cherenkov detectors of total 520 kt, with the first one in Japan at 295 km from the J-PARC neutrino beam with 2.5∘ off-axis angles (OAAs), and the second one possibly in Korea at a later stage. Having the second detector in Korea would benefit almost all areas of neutrino oscillation physics, mainly due to longer baselines. There are several candidate sites in Korea with baselines of 1000–1300 km and OAAs of 1∘–3∘⁠. We conducted sensitivity studies on neutrino oscillation physics for a second detector, either in Japan (JD × 2) or Korea (JD + KD), and compared the results with a single detector in Japan. Leptonic charge–parity (CP) symmetry violation sensitivity is improved, especially when the CP is non-maximally violated. The larger matter effect at Korean candidate sites significantly enhances sensitivities to non-standard interactions of neutrinos and mass ordering determination. Current studies indicate the best sensitivity is obtained at Mt. Bisul (1088 km baseline, 1.3∘ OAA). Thanks to a larger (1000 m) overburden than the first detector site, clear improvements to sensitivities for solar and supernova relic neutrino searches are expected.

Published
2018

22. A likely exoplanet orbiting the oscillating K-giant �� Arietis

Author

Lee, B. -C., Mkrtichian, D. E., Han, I., Kim, K. -M., and Park, M. -G.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Aims. To search for extrasolar planets around intermediate-mass stars, we are conducting a precise RV survey around K-giants. Methods. We present high-accuracy RV measurements of �� Ari made from November 2003 to February 2010. This star belongs to our sample of 55 K-giants studied for extrasolar planet and pulsation searches using the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) attached to the 1.8-m telescope at Bohyunsan Optical Astronomy Observatory (BOAO) in Korea. Results. We find a planetary companion with long-period and low-amplitude radial velocity (RV) variations in oscillating K2 III star �� Ari (HD 12929). We do not find the correlation between RV variations and chromospheric activity indicators (Ca II H & K region, H�� line). The bisector analysis also shows that the bisector velocity span (BVS) does not show any obvious correlation with RV variation but has periodic component that may be attributed to the rotation of the star. If the RV variation is indeed caused by a planetary companion, an orbital solution with a period of P = 381 days, a semi-amplitude of K = 41 m/s, and an eccentricity of e = 0.25 fits the data best. Assuming a possible stellar mass of M_star = 1.5 M_sun, we estimate the minimum mass for the planetary companion of m2 sin i = 1.8 M_Jupiter with an orbital semi-major axis of 1.2 AU. Conclusions. Our finding of a likely exoplanet in �� Ari supports searching for extrasolar planets around giant stars with multiperiodic oscillations., 6 pages, 9 figures, 2 tables

Published
2011
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41. Structure and stellar population of ringed barred galaxy NGC 2336*

Author

Gusev, A. S., Park, M.–G., Gusev, A. S., and Park, M.–G.

Abstract

Results are presented for surface UBVRIphotometry of the giant spiral galaxy NGC 2336. The data were obtained with the 1.8-m telescope of the Bohyunsan Optical Astronomy Observatory in Korea, using a CCD camera. The structure and radial light distribution of the galaxy were studied. The compositions of the stellar populations in various regions of the galaxy were estimated using two-color diagrams, and regions of star formation were identified. The properties of the 34 largest such regions were determined. The ages of these star formation regions were estimated using stellar evolutionary synthesis models. It is shown that active, constant, non-burst star formation has been recently proceeding in the disk of NGC 2336.

Published
2003
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42. Planetary companions in K giants β Cancri, μ Leonis, and β Ursae Minoris.

Author

Lee, B.-C., Han, I., Park, M.-G., Mkrtichian, D. E., Hatzes, A. P., and Kim, K.-M.

Subjects
K stars, STELLAR evolution, GIANT stars, RADIAL velocity of stars, ASTRONOMICAL photometry
Abstract

Aims. The aim of our paper is to investigate the low-amplitude and long-period variations in evolved stars with a precise radial velocity survey. Methods. The high-resolution, the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) was used from 2003 to 2013 for a radial velocity survey of giant stars as part of the exoplanet search program at Bohyunsan Optical Astronomy Observatory (BOAO). Results. We report the detection of three new planetary companions orbiting the K giants β Cnc, μ Leo, and β UMi. The planetary nature of the radial velocity variations is supported by analyzes of ancillary data. The Hipparcos photometry shows no variations with periods close to those in radial velocity variations and there is no strong correlation between the bisector velocity span (BVS) and the radial velocities for each star. Furthermore, the stars show weak or no core reversal in Ca II H lines indicating that they are inactive stars. The companion to β Cnc has a minimum mass of 7.8 MJup in a 605-day orbit with an eccentricity of 0.08. The giant μ Leo is orbited by a companion of minimum mass of 2.4 MJup having a period of 357 days and an eccentricity of 0.09. The giant β UMi is a known barium star and is suspected of harboring a white dwarf or substellar mass companion. Its companion has a minimum mass of 6.1 MJup, a period of 522 days, and an eccentricity e = 0.19. [ABSTRACT FROM AUTHOR]

Published
2014
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45. Planetary companions orbiting M giants HD 208527 and HD 220074.

Author

Lee, B.-C., Han, I., and Park, M.-G.

Subjects
M stars, RADIAL velocity of stars, KEPLER'S laws, PLANETARY theory, EXTRASOLAR planets, ASTRONOMICAL observatories, ASTRONOMICAL photography
Abstract

Aims. The purpose of the present study is to research the origin of planetary companions by using a precise radial velocity (RV) survey. Methods. The high-resolution spectroscopy of the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory (BOAO) was used from September 2008 to June 2012. Results. We report the detection of two exoplanets in orbit around HD 208527 and HD 220074 exhibiting periodic variations in RV of 875.5 ± 5.8 and 672.1 ± 3.7 days. The RV variations are not apparently related to the surface inhomogeneities, and a Keplerian motion of the planetary companion is the most likely explanation. Assuming possible stellar masses of 1.6 ± 0.4 and 1.2 ± 0.3 M⊙, we obtain the minimum masses for the exoplanets at 9.9 ± 1.7 and 11.1 ± 1.8 MJup around HD 208527 and HD 220074 with orbital semi-major axes of 2.1 ± 0.2 and 1.6 ± 0.1 AU and eccentricities of 0.08 and 0.14, respectively. We also find that the previously known spectral classification of HD 208527 and HD 220074 was in error. Our new estimation of stellar parameters suggests that both HD 208527 and HD 220074 are M giants. Therefore, HD 208527 and HD 220074 are so far the first candidate M giants found to harbor a planetary companion. [ABSTRACT FROM AUTHOR]

Published
2013
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