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| WoS | SCOPUS | Document Type | Document Title | Abstract | Authors | Affiliation | ResearcherID (WoS) | AuthorsID (SCOPUS) | Author Email(s) | Journal Name | JCR Abbreviation | ISSN | eISSN | Volume | Issue | WoS Edition | WoS Category | JCR Year | IF | JCR (%) | FWCI | FWCI Update Date | WoS Citation | SCOPUS Citation | Keywords (WoS) | KeywordsPlus (WoS) | Keywords (SCOPUS) | KeywordsPlus (SCOPUS) | Language | Publication Stage | Publication Year | Publication Date | DOI | JCR Link | DOI Link | WOS Link | SCOPUS Link |
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| ○ | ○ | Article | High-resolution Spectroscopic Monitoring Observations of FU Orionis-type Object, V960 Mon | We present the results of high-resolution (R >= 30,000) optical and near-infrared (NIR) spectroscopic monitoring observations of an FU Orionis-type object (FUor), V960 Mon, which underwent an outburst in 2014 November. We have monitored this object with the Bohyunsan Optical Echelle Spectrograph and the Immersion GRating INfrared Spectrograph since 2014 December. Various features produced by a wind, disk, and outflow/jet were detected. The wind features varied over time and continually weakened after the outburst. We detected double-peaked line profiles in the optical and NIR, and the line widths tend to decrease with increasing wavelength, indicative of Keplerian disk rotation. The disk features in the optical and NIR spectra fit well with G-type and K-type stellar spectra convolved with a kernel to account for the maximum projected disk rotation velocities of about 40.3 3.8 km s(-1)and 36.3 3.9 km s(-1), respectively. We also report the detection of [Sii] and H-2 emission lines, which are jet/outflow tracers and rarely found in FUors. | Park, Sunkyung; Lee, Jeong-Eun; Pyo, Tae-Soo; Jaffe, Daniel T.; Mace, Gregory N.; Sung, Hyun-Il; Lee, Sang-Gak; Kang, Wonseok; Oh, Hyung-Il; Yoon, Tae Seog; Yoon, Sung-Yong; Green, Joel D. | Kyung Hee Univ, Sch Space Res, 1732 Deogyeong Daero, Yongin 17104, Gyeonggi Do, South Korea; Natl Astron Observ Japan, Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA; Univ Texas Austin, Dept Astron, 2515 Speedway, Austin, TX USA; Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea; Seoul Natl Univ, 1 Gwanak Ro, Seoul 08826, South Korea; Natl Youth Space Ctr, 200 Deokheungyangjjok Gil, Goheung Gun 59567, Jeollanam Do, South Korea; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Space Telescope Sci Inst, Baltimore, MD 21218 USA | ; Kang, Wonseok/KQV-2130-2024; Lee, Jeong-Eun/E-2387-2013 | 55862120900; 35748985900; 6602816367; 7102346782; 16304062400; 24537938900; 27169222800; 55861763100; 55608072300; 7201604397; 57208178458; 7404571675 | sunkyung@khu.ac.kr;jeongeun.lee@khu.ac.kr; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 900 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 0.88 | 2025-06-25 | 18 | 19 | FU Orionis stars; High resolution spectroscopy | EFFECTIVE TEMPERATURES; DATA RELEASE; EMISSION; ACCRETION; PROTOSTARS; EVOLUTION; SPECTRUM; TAURUS; TRACKS; WIND | English | 2020 | 2020-09 | 10.3847/1538-4357/aba532 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||
| ○ | ○ | Article | KMTNet Nearby Galaxy Survey II. Searching for Dwarf Galaxies in Deep and Wide-field Images of the NGC 1291 System | We present newly discovered dwarf galaxy candidates in deep and wide-field images of NGC 1291 obtained with the Korea Microlensing Telescope Network. We identify 15 dwarf galaxy candidates by visual inspection. Using imaging simulations, we demonstrate that the completeness rate of our detection is greater than 70% for the central surface-brightness value of mu(0,R) less than or similar to 26 mag arcsec(-2) and for magnitudes M-R less than or similar to -10 mag. The structural and photometric properties of the dwarf galaxy candidates appear to be broadly consistent with those of ordinary dwarf galaxies in nearby groups and clusters, with mu(0,R) similar to 22.5 to 26.5 mag arcsec(-2) and effective radii of 200 pc to 1 kpc. The dwarf galaxy candidates show a concentration toward NGC 1291 and tend to be redder the closer they are to the center, possibly indicating that they are associated with NGC 1291. The dwarf candidates presented in this paper appear to be bluer than those in denser environments, revealing that the quenching of star formation in dwarf galaxies is susceptible to the environment, while the morphology shaping is not. | Byun, Woowon; Sheen, Yun-Kyeong; Park, Hong Soo; Ho, Luis C.; Lee, Joon Hyeop; Kim, Sang Chul; Jeong, Hyunjin; Park, Byeong-Gon; Seon, Kwang-Il; Lee, Youngdae; Lee, Yongseok; Cha, Sang-Mok; Ko, Jongwan; Kim, Minjin | Korea Astron & Space Sci Inst, Daejeon 34055, South Korea; Univ Sci & Technol, Daejeon 34113, South Korea; Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China; Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China; Chungnam Natl Univ, Dept Astron & Space Sci, Daejeon 34134, South Korea; Kyung Hee Univ, Sch Space Res, Yongin 17104, Kyeonggi, South Korea; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea | ; LEE, YONGSEOK/AAF-3965-2020; Kim, Minjin/AAU-9910-2020 | 57216758314; 23568407100; 57203771728; 35229428100; 57214829257; 26659735200; 16202920600; 7402834628; 6603554666; 56433837000; 36068040300; 13610036800; 18434193800; 56898213300 | mkim@knu.ac.kr; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 891 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 0.81 | 2025-06-25 | 16 | 14 | Dwarf galaxies | SURFACE-BRIGHTNESS GALAXIES; DIGITAL SKY SURVEY; VIRGO CLUSTER; MILKY-WAY; ELLIPTIC GALAXIES; POPULATION; LIGHT; SATELLITES | English | 2020 | 2020-03-01 | 10.3847/1538-4357/ab6f6e | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||
| ○ | ○ | Article | Magnetohydrodynamics with Post-Newtonian Corrections | Using the fully nonlinear and exact perturbation formulation with magnetohydrodynamics (MHD) in the Minkowski background, we derive first-order, post-Newtonian (1PN) equations without imposing the slicing (temporal gauge) condition. The 1PN-MHD formulation is complementary to our recently presented fully relativistic MHD combined with 0PN gravity available only in the maximal slicing. We present the 1PN-MHD equations in two gauge conditions previously used in the literature and provide gauge transformation relations between different gauges. We derive the PN effects on MHD waves in a static homogeneous medium. | Hwang, Jai-chan; Noh, Hyerim | Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu, South Korea; Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Cambridge CB3 0WA, England; Korea Astron & Space Sci Inst, Ctr Large Telescope, Daejon, South Korea | Hwang, James/GOP-3586-2022 | 7403896548; 7103103544 | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 899 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 0.07 | 2025-06-25 | 2 | 2 | Plasma astrophysics; Relativity; Magnetohydrodynamics; Astrophysical fluid dynamics | EQUATIONS; HYDRODYNAMICS; GENERATION | English | 2020 | 2020-08 | 10.3847/1538-4357/ab9ff9 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | SCUBA-2 Ultra Deep Imaging EAO Survey (Studies). III. Multiwavelength Properties, Luminosity Functions, and Preliminary Source Catalog of 450 μm Selected Galaxies | We construct a SCUBA-2 450 mu m map in the COSMOS field that covers an area of 300 arcmin(2) and reaches a 1 sigma noise level of 0.65 mJy in the deepest region. We extract 256 sources detected at 450 mu m with signal-to-noise ratios >4.0 and analyze the physical properties of their multiwavelength counterparts. We find that most of the sources are at z less than or similar to 3, with a median of . About of our sources are classified as starburst galaxies based on their total star formation rates (SFRs) and stellar masses (M-*). By fitting the far-infrared spectral energy distributions, we find that our 450 mu m selected sample has a wide range of dust temperatures (20 K less than or similar to T-d less than or similar to 60 K), with a median of z < 3. However, we find a moderate correlation where the dust temperature increases with the deviation from the SFR-M-* relation. The increase in dust temperature also correlates with optical morphology, which is consistent with merger-triggered starbursts in submillimeter galaxies. Our galaxies do not show the tight IRX-beta(UV) correlation that has been observed in the local universe. We construct the infrared luminosity functions of our 450 mu m sources and measure their comoving SFR densities (SFRDs). The contribution of the z = 0 to 2 (proportional to(1 + z)(3.91.1)) and dominates the total SFRD at z greater than or similar to 2. | Lim, Chen-Fatt; Wang, Wei-Hao; Smail, Ian; Scott, Douglas; Chen, Chian-Chou; Chang, Yu-Yen; Simpson, James M.; Toba, Yoshiki; Shu, Xinwen; Clements, Dave; Greenslade, Josh; Ao, YiPing; Babul, Arif; Birkin, Jack; Chapman, Scott C.; Cheng, Tai-An; Cho, Brian S.; Dannerbauer, Helmut; Dudzeviciute, Ugne; Dunlop, James; Gao, Yu; Goto, Tomotsugu; Ho, Luis C.; Hsu, Li-Ting; Hwang, Ho Seong; Jeong, Woong-Seob; Koprowski, Maciej; Lee, Chien-Hsiu; Lin, Ming-Yi; Lin, Wei-Ching; Michalowski, Michal J.; Parsons, Harriet; Sawicki, Marcin; Shirley, Raphael; Shim, Hyunjin; Urquhart, Sheona; Wang, Jianfa; Wang, Tao | Natl Taiwan Univ, Grad Inst Astrophys, Taipei 10617, Taiwan; Acad Sinica, Inst Astron & Astrophys ASIAA, 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan; Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England; Univ British Columbia, Dept Phys & Astron, 6225 Agr Rd, Vancouver, BC V6T 1Z1, Canada; European Southern Observ, Karl Schwarzschild Str 2, Garching, Germany; Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan; Ehime Univ, Res Ctr Space & Cosm Evolut, 2-5 Bunkyo Cho, Matsuyama, Ehime 7908577, Japan; Anhui Normal Univ, Dept Phys, Wuhu 241000, Anhui, Peoples R China; Imperial Coll London, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England; Univ Groningen, Kapteyn Astron Inst, Postbus 800, NL-9700 AV Groningen, Netherlands; Chinese Acad Sci, Purple Mt Observ, Nanjing 210033, Peoples R China; Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada; Natl Res Council Canada, Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada; Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada; Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea; IAC, E-38205 Tenerife, Spain; Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain; Univ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland; Xiamen Univ, Dept Astron, Key Lab Radio Astron, Purple Mt Observ PMO, Xiamen 361005, Fujian, Peoples R China; Natl Tsing Hua Univ, 101,Sect 2,Kuang Fu Rd, Hsinchu 30013, Taiwan; Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China; Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China; Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea; Korea Univ Sci & Technol, 217 Gajeong Ro, Daejeon 34113, South Korea; Nicolaus Copernicus Univ, Fac Phys Astron & Informat, Inst Astron, Grudziadzka 5, PL-87100 Torun, Poland; NSF, Natl Opt Infrared Astron Res Lab, 950 North Cherry Ave, Tucson, AZ 85719 USA; Natl Taiwan Univ, Grad Inst Phys, Taipei 10617, Taiwan; Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, PL-60286 Poznan, Poland; Joint Astron Ctr, 660 North Aohoku Pl,Univ Pk, Hilo, HI 96720 USA; St Marys Univ, Dept Astron & Phys, Halifax, NS B3H 3C3, Canada; St Marys Univ, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada; Univ Sussex, Astron Ctr, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England; Kyungpook Natl Univ, Dept Earth Sci Educ, Deagu 41566, South Korea; Open Univ, Sch Phys Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England; Univ Tokyo, Grad Sch Sci, Inst Astron, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan; Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan | ; Shim, Hyunjin/LZI-7486-2025; Shirley, Raphael/AAE-2964-2019; HWANG, Ho/AAS-6010-2020; Michałowski, Michał/AAQ-4789-2021; Babul, Arif/E-2730-2010; Smail, Ian/AAL-9018-2020; Shu, Xinwen/ABG-3953-2020; Dannerbauer, Helmut/F-9382-2019; Dunlop, James/ADB-7947-2022; Wang, Wei-Hao/ABD-9942-2020; 高, 煜/AGW-4046-2022; Sawicki, Marcin/JZT-9160-2024; Koprowski, Maciej/M-7525-2019; Chang, Yu-Yen/GLR-5642-2022; CHEN, Chian-Chou (TC)/ABB-2819-2020 | 57195235890; 8294170500; 7005932657; 7404952697; 44561018400; 55505186100; 55430490600; 37068332400; 16065042200; 25924805300; 57190681415; 7003967931; 7003750215; 57207207864; 24447889300; 57203642039; 57215605904; 8680454200; 57210119070; 7202804202; 55547120397; 57151800100; 35229428100; 55611731400; 15131707100; 7102145940; 56038935500; 35196197200; 56342764900; 57199194846; 15822545300; 35096693300; 57203088473; 57204707479; 14061137700; 55749698200; 57215604756; 55709800200 | chenfatt.lim@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 889 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 1.22 | 2025-06-25 | 29 | 29 | High-redshift galaxies; Galaxy evolution; Luminosity function; Submillimeter astronomy | COSMOLOGY LEGACY SURVEY; STAR-FORMING GALAXIES; SIMILAR-TO 2; DEGREE EXTRAGALACTIC SURVEY; ACTIVE GALACTIC NUCLEI; FORMATION RATE DENSITY; SPECTRAL ENERGY-DISTRIBUTIONS; AZTEC MILLIMETER SURVEY; SUBMILLIMETER GALAXIES; HIGH-REDSHIFT | Machine-readable tables | English | 2020 | 2020-02-01 | 10.3847/1538-4357/ab607f | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||
| ○ | ○ | Article | SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES). IV. Spatial Clustering and Halo Masses of Submillimeter Galaxies | We analyze an extremely deep 450 mu m image (1 sigma = 0.56 mJy beam(-1)) of a similar or equal to 300 arcmin(2) area in the CANDELS/COSMOS field as part of the Sub-millimeter Common User Bolometric Array-2 Ultra Deep Imaging EAO Survey. We select a robust (signal-to-noise ratio >= 4) and flux-limited (>= 4 mJy) sample of 164 submillimeter galaxies (SMGs) at 450 mu m that have K-band counterparts in the COSMOS2015 catalog identified from radio or mid-infrared imaging. Utilizing this SMG sample and the 4705 K-band-selected non-SMGs that reside within the noise level <= 1 mJy beam(-1) region of the 450 mu m image as a training set, we develop a machine-learning classifier using K-band magnitude and color-color pairs based on the 13-band photometry available in this field. We apply the trained machine-learning classifier to the wider COSMOS field (1.6 deg(2)) using the same COSMOS2015 catalog and identify a sample of 6182 SMG candidates with similar colors. The number density, radio and/or mid-infrared detection rates, redshift and stellar-mass distributions, and the stacked 450 mu m fluxes of these SMG candidates, from the S2COSMOS observations of the wide field, agree with the measurements made in the much smaller CANDELS field, supporting the effectiveness of the classifier. Using this SMG candidate sample, we measure the two-point autocorrelation functions from z = 3 down to z = 0.5. We find that the SMG candidates reside in halos with masses of similar or equal to (2.0 +/- 0.5) x 10(13) h(-1) M-circle dot across this redshift range. We do not find evidence of downsizing that has been suggested by other recent observational studies. | Lim, Chen-Fatt; Chen, Chian-Chou; Smail, Ian; Wang, Wei-Hao; Tee, Wei-Leong; Lin, Yen-Ting; Scott, Douglas; Toba, Yoshiki; Chang, Yu-Yen; Ao, YiPing; Babul, Arif; Bunker, Andy; Chapman, Scott C.; Clements, David L.; Conselice, Christopher J.; Gao, Yu; Greve, Thomas R.; Ho, Luis C.; Hong, Sungwook E.; Hwang, Ho Seong; Koprowski, Maciej; Michalowski, Michal J.; Shim, Hyunjin; Shu, Xinwen; Simpson, James M. | Acad Sinica, Inst Astron & Astrophys ASIAA, 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan; Natl Taiwan Univ, Grad Inst Astrophys, Taipei 10617, Taiwan; European Southern Observ, Karl Schwarzschild Str 2, Garching, Germany; Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England; Univ Arizona, Dept Phys, Tucson, AZ 85721 USA; Univ British Columbia, Dept Phys & Astron, 6225 Agr Rd, Vancouver, BC V6T 1Z1, Canada; Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan; Ehime Univ, Res Ctr Space & Cosm Evolut, 2-5 Bunkyo Cho, Matsuyama, Ehime 7908577, Japan; Chinese Acad Sci, Purple Mt Observ, Nanjing 210033, Peoples R China; Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210033, Peoples R China; Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada; Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England; Natl Res Council Canada, Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada; Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada; Imperial Coll, Dept Phys, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England; Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England; Xiamen Univ, Dept Astron, Xiamen 361005, Fujian, Peoples R China; UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England; Cosm Dawn Ctr, Copenhagen, Denmark; Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China; Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China; Univ Seoul, Nat Sci Res Inst, 163 Seoulsiripdaero, Seoul 02504, South Korea; Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea; Nicolaus Copernicus Univ, Fac Phys Astron & Informat, Inst Astron, Grudziadzka 5, PL-87100 Torun, Poland; Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, PL-60286 Poznan, Poland; Kyungpook Natl Univ, Dept Earth Sci Educ, Deagu 41566, South Korea; Anhui Normal Univ, Dept Phys, Wuhu 241000, Anhui, Peoples R China; Univ Tokyo, Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Tokyo, Japan | TEE, WEI LEONG/IQS-0420-2023; Hong, Sungwook/J-1533-2019; Shim, Hyunjin/LZI-7486-2025; Smail, Ian/M-5161-2013; Conselice, Christopher/B-4348-2013; Babul, Arif/E-2730-2010; Michałowski, Michał/AAQ-4789-2021; Shu, Xinwen/ABG-3953-2020; Wang, Wei-Hao/ABD-9942-2020; 高, 煜/AGW-4046-2022; Koprowski, Maciej/M-7525-2019; Smail, Ian/AAL-9018-2020; CHEN, Chian-Chou (TC)/ABB-2819-2020; Chang, Yu-Yen/GLR-5642-2022; HWANG, Ho/AAS-6010-2020; Lin, Yen-Ting/ABC-4256-2020 | 57195235890; 44561018400; 7005932657; 8294170500; 57195238551; 35329761400; 7404952697; 37068332400; 55505186100; 7003967931; 7003750215; 7006104330; 24447889300; 25924805300; 7003910265; 55547120397; 10339159000; 35229428100; 56108601200; 15131707100; 56038935500; 15822545300; 14061137700; 16065042200; 55430490600 | chenfatt.lim@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 895 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 0.39 | 2025-06-25 | 13 | 15 | Clustering; Submillimeter astronomy; High-redshift galaxies; Galaxy evolution; Large-scale structure of the universe; Galaxy formation | COSMOLOGY LEGACY SURVEY; STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; REDSHIFT SURVEY; MU-M; ALMA SURVEY; LARGE-SCALE; LUMINOSITY DEPENDENCE; BOLOMETER CAMERA; PASSIVE GALAXIES | English | 2020 | 2020-06 | 10.3847/1538-4357/ab8eaf | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||
| ○ | ○ | Article | Search for Optically Dark Infrared Galaxies without Counterparts of Subaru Hyper Suprime-Cam in the AKARI North Ecliptic Pole Wide Survey Field | We present the physical properties of AKARI sources without optical counterparts in optical images from the Hyper Suprime-Cam (HSC) on the Subaru telescope. Using the AKARI infrared (IR) source catalog and HSC optical catalog, we select 583 objects that do not have HSC counterparts in the AKARI North Ecliptic Pole wide survey field (similar to 5 deg(2)). Because the HSC limiting magnitude is deep (g(AB) similar to 28.6), these are good candidates for extremely red star-forming galaxies (SFGs) and/or active galactic nuclei (AGNs), possibly at high redshifts. We compile multiwavelength data out to 500 mu m and use them for fitting the spectral energy distribution withCIGALEto investigate the physical properties of AKARI galaxies without optical counterparts. We also compare their physical quantities with AKARI mid-IR selected galaxies with HSC counterparts. The estimated redshifts of AKARI objects without HSC counterparts range up toz similar to 4, significantly higher than for AKARI objects with HSC counterparts. We find that (i) 3.6 - 4.5 mu m color, (ii) AGN luminosity, (iii) stellar mass, (iv) star formation rate, and (v)V-band dust attenuation in the interstellar medium of AKARI objects without HSC counterparts are systematically larger than those of AKARI objects with counterparts. These results suggest that our sample includes luminous, heavily dust-obscured SFGs/AGNs atz similar to 1-4 that are missed by previous optical surveys, providing very interesting targets for the coming era of the James Webb Space Telescope. | Toba, Yoshiki; Goto, Tomotsugu; Oi, Nagisa; Wang, Ting-Wen; Kim, Seong Jin; Ho, Simon C. -C.; Burgarella, Denis; Hashimoto, Tetsuya; Hsieh, Bau-Ching; Huang, Ting-Chi; Hwang, Ho Seong; Ikeda, Hiroyuki; Kim, Helen K.; Kim, Seongjae; Lee, Dongseob; Malkan, Matthew A.; Matsuhara, Hideo; Miyaji, Takamitsu; Momose, Rieko; Ohyama, Youichi; Oyabu, Shinki; Pearson, Chris; Santos, Daryl Joe D.; Shim, Hyunjin; Takagi, Toshinobu; Ueda, Yoshihiro; Utsumi, Yousuke; Wada, Takehiko | Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan; Acad Sinica, Inst Astron & Astrophys, AS NTU, 11F Astron Math Bldg,1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan; Ehime Univ, Res Ctr Space & Cosm Evolut, 2-5 Bunkyo Cho, Matsuyama, Ehime 7908577, Japan; Natl Tsing Hua Univ, Inst Astron, 101,Sect 2,Kuang Fu Rd, Hsinchu 30013, Taiwan; Tokyo Univ Sci, Shinjuku Ku, 1-3,Kagurazaka, Tokyo 1628601, Japan; Aix Marseille Univ, CNRS, CNES, LAM Marseille, Marseille, France; Natl Tsing Hua Univ, Ctr Informat & Computat Astron CICA, 101,Sect 2,Kuang Fu Rd, Hsinchu 30013, Taiwan; Grad Univ Adv Studies, SOKENDAI, Dept Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan; Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan; Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea; Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan; Wakayama Coll, Natl Inst Technol, Wakayama 6440023, Japan; UCLA, Dept Phys & Astron, 475 Portola Plaza, Los Angeles, CA 90095 USA; Univ Sci & Technol, Daejeon 34113, South Korea; Korea Astron & Space Sci Inst, Daejeon 34055, South Korea; Kyungpook Natl Univ, Dept Earth Sci Educ, Daegu 41566, South Korea; Univ Nacl Autonoma Mexico, Inst Astronoma Sede Ensenada, Km 107, Ensenada 22060, BC, Mexico; Leibniz Inst Astrophys Potsdam, Sternwarte 16, D-14482 Potsdam, Germany; Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan; Tokushima Univ, Inst Liberal Arts & Sci, Minami Jousanjima Machi 1-1, Tokushima, Tokushima 7708502, Japan; STFC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England; Univ Oxford, Oxford Astrophys, Keble Rd, Oxford OX1 3RH, England; Open Univ, Milton Keynes MK7 6AA, Bucks, England; Japan Space Forum, Chiyoda Ku, 3-2-1,Kandasurugadai, Tokyo 1010062, Japan; SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA; Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94035 USA | Hashimoto, Tetsuya/ABG-3643-2021; Ohyama, Youichi/ABA-5890-2020; Huang, Teddy/ABB-7532-2020; 大山陽一, Youichi/ABA-5890-2020; Malkan, Matthew/IWM-5356-2023; WADA, Takehiko/A-5247-2011; Huang, Ted/ABB-7532-2020; Shim, Hyunjin/LZI-7486-2025; HWANG, Ho/AAS-6010-2020; Wada, Takehiko/ACR-9959-2022 | 37068332400; 57151800100; 23968436800; 57211574957; 57070819300; 57216812477; 8852232400; 24518043000; 37053806800; 57203623570; 15131707100; 44561165200; 57203269860; 57194798031; 57218674853; 7006872661; 7003505733; 57203194972; 36615692700; 14825669800; 14825704200; 55531949600; 57218278835; 14061137700; 35405904800; 7403977828; 57203300466; 56431900300 | toba@kusastro.kyoto-u.ac.jp; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 899 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 1.83 | 2025-06-25 | 35 | 34 | DUST-OBSCURED GALAXIES; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATE; LUMINOSITY FUNCTIONS; SOURCE CATALOG; AGN SELECTION; POPULATION; MERGERS; SOFTWARE | English | 2020 | 2020-08 | 10.3847/1538-4357/ab9cb7 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Space Telescope and Optical Reverberation Mapping Project. XII. Broad-line Region Modeling of NGC 5548 | We present geometric and dynamical modeling of the broad line region (BLR) for the multi-wavelength reverberation mapping campaign focused on NGC 5548 in 2014. The data set includes photometric and spectroscopic monitoring in the optical and ultraviolet, covering the H beta, Civ, and Ly alpha broad emission lines. We find an extended disk-like H beta BLR with a mixture of near-circular and outflowing gas trajectories, while the Civand Ly alpha BLRs are much less extended and resemble shell-like structures. There is clear radial structure in the BLR, with Civand Ly alpha emission arising at smaller radii than the H beta emission. Using the three lines, we make three independent black hole mass measurements, all of which are consistent. Combining these results gives a joint inference of log(10) (M-BH/M-circle dot) = 7.64(-0.18)(+0.21). We examine the effect of using the V band instead of the UV continuum light curve on the results and find a size difference that is consistent with the measured UV-optical time lag, but the other structural and kinematic parameters remain unchanged, suggesting that theVband is a suitable proxy for the ionizing continuum when exploring the BLR structure and kinematics. Finally, we compare the H beta results to similar models of data obtained in 2008 when the active galactic nucleus was at a lower luminosity state. We find that the size of the emitting region increased during this time period, but the geometry and black hole mass remained unchanged, which confirms that the BLR kinematics suitably gauge the gravitational field of the central black hole. | Williams, P. R.; Pancoast, A.; Treu, T.; Brewer, B. J.; Peterson, B. M.; Barth, A. J.; Malkan, M. A.; De Rosa, G.; Horne, Keith; Kriss, G. A.; Arav, N.; Bentz, M. C.; Cackett, E. M.; Dalla Bonta, E.; Dehghanian, M.; Done, C.; Ferland, G. J.; Grier, C. J.; Kaastra, J.; Kara, E.; Kochanek, C. S.; Mathur, S.; Mehdipour, M.; Pogge, R. W.; Proga, D.; Vestergaard, M.; Waters, T.; Adams, S. M.; Anderson, M. D.; Arevalo, P.; Beatty, T. G.; Bennert, V. N.; Bigley, A.; Bisogni, S.; Borman, G. A.; Boroson, T. A.; Bottorff, M. C.; Brandt, W. N.; Breeveld, A. A.; Brotherton, M.; Brown, J. E.; Brown, J. S.; Canalizo, G.; Carini, M. T.; Clubb, K. I.; Comerford, J. M.; Corsini, E. M.; Crenshaw, D. M.; Croft, S.; Croxall, K. V.; Deason, A. J.; De Lorenzo-Caceres, A.; Denney, K. D.; Dietrich, M.; Edelson, R.; Efimova, N. V.; Ely, J.; Evans, P. A.; Fausnaugh, M. M.; Filippenko, A. V.; Flatland, K.; Fox, O. D.; Gardner, E.; Gates, E. L.; Gehrels, N.; Geier, S.; Gelbord, J. M.; Gonzalez, L.; Gorjian, V.; Greene, J. E.; Grupe, D.; Gupta, A.; Hall, P. B.; Henderson, C. B.; Hicks, S.; Holmbeck, E.; Holoien, T. W. -S.; Hutchison, T.; Im, M.; Jensen, J. J.; Johnson, C. A.; Joner, M. D.; Jones, J.; Kaspi, S.; Kelly, P. L.; Kennea, J. A.; Kim, M.; Kim, S.; Kim, S. C.; King, A.; Klimanov, S. A.; Knigge, C.; Krongold, Y.; Lau, M. W.; Lee, J. C.; Leonard, D. C.; Li, Miao; Lira, P.; Lochhaas, C.; Ma, Zhiyuan; MacInnis, F.; Manne-Nicholas, E. R.; Mauerhan, J. C.; McGurk, R.; McHardy, I. M.; Montuori, C.; Morelli, L.; Mosquera, A.; Mudd, D.; Muller-Sanchez, F.; Nazarov, S. V.; Norris, R. P.; Nousek, J. A.; Nguyen, M. L.; Ochner, P.; Okhmat, D. N.; Papadakis, I.; Parks, J. R.; Pei, L.; Penny, M. T.; Pizzella, A.; Poleski, R.; Pott, J. -U.; Rafter, S. E.; Rix, H. -W.; Runnoe, J.; Saylor, D. A.; Schimoia, J. S.; Scott, B.; Sergeev, S. G.; Shappee, B. J.; Shivvers, I.; Siegel, M.; Simonian, G. V.; Siviero, A.; Skielboe, A.; Somers, G.; Spencer, M.; Starkey, D.; Stevens, D. J.; Sung, H. -I.; Tayar, J.; Tejos, N.; Turner, C. S.; Uttley, P.; Van Saders, J.; Vaughan, S. A.; Vican, L.; Villanueva, S., Jr.; Villforth, C.; Weiss, Y.; Woo, J. -H.; Yan, H.; Young, S.; Yuk, H.; Zheng, W.; Zhu, W.; Zu, Y. | Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA; Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA; Univ Auckland, Dept Stat, Private Bag 92019, Auckland 1142, New Zealand; Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA; Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA; Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA; Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA; Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland; Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA; Georgia State Univ, Dept Phys & Astron, 25 Pk Pl,Suite 605, Atlanta, GA 30303 USA; Wayne State Univ, Dept Phys & Astron, 666 W Hancock St, Detroit, MI 48201 USA; Univ Padua, Dipartimento Fis & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy; INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy; Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA; Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England; Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA; SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands; Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands; MIT, Kavli Inst Space & Astrophys Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA; Univ Nevada, Dept Phys & Astron, 4505 South Maryland Pkwy,Box 454002, Las Vegas, NV 89154 USA; Univ Copenhagen, Niels Bohr Inst, DARK, Jagtvej 128, DK-2200 Copenhagen, Denmark; CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA; Univ Valparaiso, Inst Fis & Astron, Fac Ciencias, Gran Bretana N 1111, Valparaiso, Chile; Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA; Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA; INAF IASF Milano, Via Alfonso Corti 12, I-20133 Milan, Italy; Crimean Astrophys Observ, UA-298409 Nauchnyi, Crimea, Ukraine; Las Cumbres Observ, Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA; Southwestern Univ, Dept Phys FJS 149, Fountainwood Observ, 1011 E Univ Ave, Georgetown, TX 78626 USA; Penn State Univ, Dept Astron & Astrophys, Eberly Coll Sci, 525 Davey Lab, University Pk, PA 16802 USA; Penn State Univ, Dept Phys, Davey Lab, 104 Davey Lab, University Pk, PA 16802 USA; Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA; Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England; Univ Wyoming, Dept Phys & Astron, 1000 E Univ Ave, Laramie, WY 82071 USA; Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA; Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA; Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA; Western Kentucky Univ, Dept Phys & Astron, 1906 Coll Hts Blvd 11077, Bowling Green, KY 42101 USA; Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA; Univ Durham, Inst Computat Cosmol, Dept Phys, South Rd, Durham DH1 3LE, England; Inst Astrofis Canarias, Calle Via Lactea S-N, E-38205 Tenerife, Spain; Worcester State Univ, Dept Earth Environm & Phys, Worcester, MA 01602 USA; Univ Maryland, Dept Astron, College Pk, MD 20742 USA; Pulkovo Observ, St Petersburg 196140, Russia; Univ Leicester, Sch Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England; Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA; San Diego State Univ, Dept Astron, San Diego, CA 92182 USA; Oakwood Sch, 105 John Wilson Way, Morgan Hill, CA 95037 USA; Univ Reading, Sch Biol Sci, Reading RG6 6AS, Berks, England; Lick Observ, POB 85, Mt Hamilton, CA 95140 USA; NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA; Inst Astrofis Canarias, E-38200 Tenerife, Spain; Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain; Gran Telescopio Canarias GRANTECAN, E-38205 Tenerife, Spain; Spectral Sci Inc, 4 Fourth Ave, Burlington, MA 01803 USA; Eureka Sci Inc, 2452 Delmer St Suite 100, Oakland, CA 94602 USA; CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA; Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA; Morehead State Univ, Ctr Space Sci, 235 Martindale Dr, Morehead, KY 40351 USA; York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada; CALTECH, IPAC, Mail Code 100-22,1200 East Calif Blvd, Pasadena, CA 91109 USA; Observ Teh Carnegie Inst, 813 Santa Barbara St, Pasadena, CA 91101 USA; Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA; Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA; Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea; Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA; Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA; Brigham Young Univ, Dept Phys & Astron, N283 ESC, Provo, UT 84602 USA; Tel Aviv Univ, Sch Phys & Astron, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel; Technion, Phys Dept, IL-32000 Haifa, Israel; Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, 116 Church St SE, Minneapolis, MN 55455 USA; Korea Astron & Space Sci Inst, Daejeon, South Korea; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England; Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea; Korea Univ Sci & Technol UST, 217 Gajeong Ro, Daejeon 34113, South Korea; Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia; Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England; Univ Nacl Autonoma Mexico, Inst Astron, Mexico City, DF, Mexico; Columbia Univ, Dept Astron, 550 W120th St, New York, NY 10027 USA; Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile; Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA; Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA; Univ Insubria, DiSAT, Via Valleggio 11, Como, Italy; Univ Atacama, Inst Astron & Ciencias Planetarias, Copiapo, Chile; US Naval Acad, Dept Phys, Annapolis, MD 21403 USA; Univ Memphis, Dept Phys & Mat Sci, 3720 Alumni Ave, Memphis, TN 38152 USA; Univ Crete, Dept Phys, GR-71003 Iraklion, Greece; Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece; Fdn Res & Technol, IESL, GR-71110 Iraklion, Greece; Louisiana State Univ, Dept Phys & Astron, Nicholson Hall,Tower Dr, Baton Rouge, LA 70803 USA; Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland; Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany; Univ Haifa, Dept Phys, Fac Nat Sci, IL-31905 Haifa, Israel; Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA; Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Circle, Nashville, TN 37235 USA; Lab Interinst eAstron, Rua Gen Jose Cristino,77 Vasco Gama, Rio De Janeiro, RJ, Brazil; Univ Fed Santa Maria, CCNE, Dept Fis, BR-9710590 Santa Maria, RS, Brazil; Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA; Concord Univ, Dept Phys Sci, Vermillion St,POB 1000, Athens, WV 24712 USA; Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA; Pontificia Univ Catolica Valparaiso, Inst Fis, Casilla 4059, Valparaiso, Chile; Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands; Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England; Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA; Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada; Shanghai Jiao Tong Univ, 800 Dongchuan Rd, Shanghai 200240, Peoples R China | Lecoanet, Daniel/Y-4061-2019; Ma, ZhiYuan/GWN-1061-2022; Kim, Stacy/HKF-3776-2023; Morelli, Lorenzo/AAX-2452-2021; Ferland, Gary/AFO-6311-2022; Poleski, Radoslaw/AAM-7565-2021; Treu, Tommaso/KYP-7127-2024; Corsini, Enrico/AAE-1229-2021; Zu, Ying/ABE-1449-2022; Bonta', Elena/A-6432-2019; Efimova, Natalia/I-2196-2013; Im, Myungshin/B-3436-2013; Sergeyev, Sergey/LWH-7849-2024; Malkan, Matthew/IWM-5356-2023; Kim, Minjin/AAU-9910-2020; Papadakis, Iossif/C-3235-2011; Kennea, Jamie/AAF-2090-2019; de Lorenzo-Cáceres, Adriana/AAA-6412-2020; Penny, Matthew/AGE-0251-2022; Woo, Jong-Hak/A-2790-2014; Li, Miao/AAL-6344-2021; Vestergaard, Marianne/M-5247-2014; Skielboe, Andreas/E-6243-2015; Krongold, Yair/AAF-2844-2021; Lira, Paulina/G-8536-2016; done, chris/D-4605-2016; King, Andrew/AAS-4216-2021; Klimanov, Sergei/O-7827-2017; Norris, Ray/JQI-5303-2023; Peterson, Bradley/G-8226-2012; Adams, Scott/KIC-4492-2024; Norris, Ray/A-1316-2008; Hicks, Stephen/I-7155-2012; Grupe, Dirk/JVT-4185-2024; Brandt, William/N-2844-2015; Gupta, Anjali/HCH-5986-2022; Evans, Philip/JJC-1668-2023 | 57218765930; 36624101000; 7003853565; 12241991700; 16219777200; 36088948300; 7006872661; 56708167000; 55172662700; 7006072785; 7004138440; 7007172911; 8302847800; 57206712686; 57209887790; 35595494700; 35503330500; 23488608100; 7006511205; 55580882000; 35242747200; 7402610198; 36089155500; 35243272000; 6701789863; 43361722900; 55958923500; 23491705100; 57203331731; 14818934200; 25521379400; 35222917400; 57193699379; 57190802646; 55936419600; 57202954730; 7006617490; 35247682800; 6603460192; 56312481000; 57193701812; 55933048000; 6601959161; 7103191551; 24536972800; 7005041163; 7005674273; 55665128500; 14522085200; 8283329500; 25927011900; 23088009300; 15749792200; 24758008000; 57213232100; 7005798085; 55542009800; 57202328232; 55767439500; 34568722000; 56942413300; 57226394283; 55875326400; 35476049700; 57217578289; 13409026300; 6506351764; 59572965100; 6701360960; 7402743629; 57204299797; 55491981200; 35356071700; 41461135600; 57000000200; 57193691310; 56010513200; 57188864446; 7004267711; 56970247900; 57223328232; 6603675694; 46161347700; 7004725504; 25641134600; 10240135000; 56898213300; 57193702961; 26659735200; 56226004000; 6506581878; 6701924611; 6603127332; 55892840900; 44561285600; 7201953982; 57218259851; 7004380328; 57191281517; 56271785800; 57188862518; 35748755100; 8567321700; 35503513100; 7004698784; 35732309200; 15830351600; 35185478700; 56152100500; 14825359600; 16033756000; 57203761212; 55943988000; 8895449400; 16242110900; 54783071500; 22935453600; 20436555600; 55340311200; 36926032900; 6603938087; 16507612700; 7003480487; 16025343300; 35350466600; 51665761600; 56414526400; 55123116000; 56707598000; 7101928440; 38362184400; 44561605900; 7402331052; 55660997900; 55880601100; 55078382500; 55893172100; 56200618500; 57168772200; 55835005200; 58709627600; 55603167100; 24449720000; 56413968600; 57206439738; 36714576300; 7005383041; 37003120400; 36638690700; 24073775000; 57188862618; 7401751171; 55730037700; 56956181600; 57191892016; 7403566199; 57171299700; 37032950700 | pwilliams@astro.ucla.edu; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 902 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 1.42 | 2025-06-25 | 29 | 30 | Active galaxies; Active galactic nuclei; Reverberation mapping; Seyfert galaxies | AGN MONITORING PROJECT; ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; EMISSION; CONTINUUM; MASSES; VARIABILITY; STEPS; SIZE | English | 2020 | 2020-10 | 10.3847/1538-4357/abbad7 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||
| ○ | ○ | Article | The Infrared Medium-deep Survey. VII. Faint Quasars at z ∼ 5 in the ELAIS-N1 Field | The intergalactic medium ( IGM) at z.. 5 to 6 is largely ionized, and yet the main source for the IGM ionization in the early universe is uncertain. Of the possible contributors are faint quasars with -26. M1450. -23, but their number density is poorly constrained at z..5. In this paper, we present our survey of faint quasars at z..5 in the European Large-Area Infrared Space Observatory Survey-North 1 (ELAIS-N1) field over a survey area of 6.51 deg2 and examine if such quasars can be the dominant source of the IGM ionization. We use the deep optical/nearinfrared data of the ELAIS-N1 field as well as the additional medium-band observations to find z..5 quasars through a two-step approach using the broadband color selection, and spectral energy distribution fitting with the medium-band information included. Adopting Bayesian information criterion, we identify 10 promising quasar candidates. Spectra of three of the candidates are obtained, confirming all of them to be quasars at z..5 and supporting the reliability of the quasar selection. Using the promising candidates, we derive the z..5 quasar luminosity function at.-26...M1450...-23. The number density of faint z..5 quasars in the ELAIS-N1 field is consistent with several previous results that quasars are not the main contributors to the IGM-ionizing photons at z..5. | Shin, Suhyun; Im, Myungshin; Kim, Yongjung; Hyun, Minhee; Pak, Soojong; Jeon, Yiseul; Ahn, Hojae; Byeon, Seoyeon; Han, Jimin; Hwang, Sungyong; Kim, Sophia; Lim, Gu; Paek, Insu; Paek, Gregory S. H.; Taak, Yoon Chan; Choi, Changsu; Hong, Jueun; Jun, Hyunsung David; Kim, Dohyeong; Kim, Duho; Kim, Minjin; Kim, Jae-Woo; Kim, Ji Hoon; Lee, Hye-In; Lee, Seong-Kook; Park, Won-Kee; Park, Woojin; Yoon, Yongmin | Seoul Natl Univ, Ctr Explorat Origin Universe CEOU, Bldg 45,1 Gwanak Ro, Seoul 08826, South Korea; Seoul Natl Univ, Dept Phys & Astron, Astron PrograT, FPRD, 1 Gwanak Ro, Seoul 08826, South Korea; Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China; Kyung Hee Univ, Sch Space Res, 1732 Deogyeong Daero, Yongin 17104, Gyeonggi Do, South Korea; FEROKA Inc, 401 Open Innovat Bldg,117-3 Hoegi Ro, Seoul 02455, South Korea; Korea Inst Adv Study, 85 Hoegiro, Seoul 02455, South Korea; Arizona State Univ, Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA; Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea; Kyungpook Natl Univ, Coll Nat Sci, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Natl Astron Observ Japan, Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA; METASPACE Inc, Seoul 40136, South Korea | Lim, Gu/MHP-9254-2025; Kim, Ji Hoon/A-8989-2009; Kim, Ji/A-8989-2009; Im, Myungshin/B-3436-2013; , Yong Jung Kim/JRW-0681-2023; Kim, Minjin/AAU-9910-2020; Jun, Hyunsung/AAH-3501-2019; Pak, Soojong/E-2360-2013 | 57205483501; 7004267711; 59622148200; 56435655500; 56212344500; 36621209700; 56714980300; 57209206939; 57205490243; 57209217497; 57216527136; 57200876753; 57196357970; 57205495959; 57209205426; 56436682000; 18433745100; 56434911500; 27067602700; 55574223678; 55632221500; 56898213300; 55983723600; 57191685580; 56072657000; 59314270500; 35285730800; 56799632300; 56435175600 | myungshin.im@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 893 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 1.08 | 2025-06-25 | 18 | 18 | ACTIVE GALACTIC NUCLEI; Z-SIMILAR-TO-6 QUASARS; LUMINOSITY FUNCTION; LYMAN CONTINUUM; ESCAPE FRACTION; REDSHIFT; GALAXIES; UNIVERSE; CAMERA; AGN | English | 2020 | 2020-04 | 10.3847/1538-4357/ab7bde | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | The Infrared Medium-deep Survey. VIII. Quasar Luminosity Function at z ∼ 5 | Faint z similar to 5 quasars with M-1450 similar to -23 mag are known to be potentially important contributors to the ultraviolet ionizing background in the postreionization era. However, their number density has not been well determined, making it difficult to assess their role in the early ionization of the intergalactic medium (IGM). In this work, we present the updated results of our z similar to 5 quasar survey using the Infrared Medium-deep Survey (IMS), a near-infrared imaging survey covering an area of 85 deg(2). From our spectroscopic observations with the Gemini Multi-Object Spectrograph on the Gemini-South 8 m telescope, we discovered eight new quasars at z similar to 5 with -26.1 -27 mag) with the brighter Sloan Digital Sky Survey quasars (M-1450 < -27 mag), we derive the z similar to 5 quasar luminosity function (QLF) without any fixed parameters down to the magnitude limit of M-1450* = -23 mag. We find that the faint-end slope of the QLF is very flat (alpha = -1.2+(1.4)(-0.6)),), with a characteristic luminosity of M-1450* = -25.8(-1.1)(+1.4) mag. The number denisty of z similar to 5 quasars from the QLF gives an ionizing emissivity at 912 angstrom of epsilon(912) = (3.7-7.1) x 10(23) erg s(-1) Hz(-1) Mpc(-3) and an ionizing photon density o (n)over dot(ion) = (3.0 - 5.7) x 10(49) Mpc(-3) s(-1). These results imply that quasars are responsible for only 10%-20% (up to 50% even in the extreme case) of the photons required to completely ionize the IGM at z similar to 5, disfavoring the idea that quasars alone could have ionized the IGM at z similar to 5. | Kim, Yongjung; Im, Myungshin; Jeon, Yiseul; Kim, Minjin; Pak, Soojong; Hyun, Minhee; Taak, Yoon Chan; Shin, Suhyun; Lim, Gu; Paek, Gregory S. H.; Paek, Insu; Jiang, Linhua; Choi, Changsu; Hong, Jueun; Ji, Tae-Geun; Jun, Hyunsung D.; Karouzos, Marios; Kim, Dohyeong; Kim, Duho; Kim, Jae-Woo; Kim, Ji Hoon; Lee, Hye-In; Lee, Seong-Kook; Park, Won-Kee; Yoon, Yongmin; Byeon, Seoyeon; Hwang, Sungyong; Kim, Joonho; Kim, Sophia; Park, Woojin | Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China; Seoul Natl Univ, Ctr Explorat Origin Universe CEOU, Bldg 45,1 Gwanak Ro, Seoul 08826, South Korea; Seoul Natl Univ, Dept Phys & Astron, FPRD, Astron Program, 1 Gwanak Ro, Seoul 08826, South Korea; FEROKA Inc, 401 Open Innovat Bldg,117-3 Hoegi Ro, Seoul 02455, South Korea; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Coll Nat Sci, Daegu 41566, South Korea; Kyung Hee Univ, Sch Space Res, 1732 Deogyeong Daero, Yongin 17104, Gyeonggi Do, South Korea; Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China; Korea Inst Adv Study, 85 Hoegi Ro, Seoul 02455, South Korea; Springer Nat, Nat Astron, 4 Crinan St, London N1 9XW, England; Pusan Natl Univ, Dept Earth Sci, Busan 46241, South Korea; Korea Astron & Space Sci Inst, Daejeon 34055, South Korea; Metaspace Inc, 36 Nonhyeon Ro, Seoul 06312, South Korea | ; Pak, Soojong/E-2360-2013; Lim, Gu/MHP-9254-2025; Kim, Minjin/AAU-9910-2020; Jun, Hyunsung/AAH-3501-2019; Im, Myungshin/B-3436-2013; Kim, Ji/A-8989-2009; , Yong Jung Kim/JRW-0681-2023; Kim, Ji Hoon/A-8989-2009; Jiang, Linhua/H-5485-2016 | 59622148200; 7004267711; 36621209700; 56898213300; 56212344500; 56435655500; 56436682000; 57205483501; 57196357970; 57209205426; 57205495959; 14058258000; 18433745100; 56434911500; 56714980300; 27067602700; 57220339327; 55574223678; 55632221500; 55983723600; 57191685580; 56072657000; 59314270500; 35285730800; 56435175600; 57205490243; 57216527136; 57219528062; 57200876753; 56799632300 | yongjungkim@pku.edu.cn;mim@astro.snu.ac.kr; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 904 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 1.76 | 2025-06-25 | 32 | 31 | DIGITAL SKY SURVEY; IONIZING EMISSIVITY; BLACK-HOLE; REDSHIFT; EVOLUTION; SELECTION; SAMPLES; AGN; SPECTROGRAPH; CONSTRAINTS | Active galactic nuclei (16); Early universe (435); Observational astronomy (1145); Quasars (1319); Reionization (1383); Sky surveys (1464) | English | 2020 | 2020-12 | 10.3847/1538-4357/abc0ea | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||
| ○ | ○ | Article | Variability and the Size-Luminosity Relation of the Intermediate-mass AGN in NGC 4395 | We present a variability study of the lowest-luminosity Seyfert 1 nucleus of the galaxy NGC 4395 based on photometric monitoring campaigns in 2017 and 2018. Using 22 ground-based and space telescopes, we monitored NGC 4395 with a similar to 5-minute cadence during a period of 10 days and obtained light curves in the ultraviolet (UV), V, J, H, and K/K-s bands, as well as narrowband H alpha. The rms variability is similar to 0.13 mag in the Swift UVM2 and V filter light curves, decreasing down to similar to 0.01 mag in the K filter. After correcting for the continuum contribution to the H alpha narrow band, we measured the time lag of the H alpha emission line with respect to the V-band continuum as minutes in 2018, depending on assumptions about the continuum variability amplitude in the H alpha narrow band. We obtained no reliable measurements for the continuum-to-continuum lag between UV and V bands and among near-IR bands, owing to the large flux uncertainty of UV observations and the limited time baseline. We determined the active galactic nucleus (AGN) monochromatic luminosity at 5100 A, after subtracting the contribution of the nuclear star cluster. While the optical luminosity of NGC 4395 is two orders of magnitude lower than that of other reverberation-mapped AGNs, NGC 4395 follows the size-luminosity relation, albeit with an offset of 0.48 dex (>= 2.5 sigma) from the previous best-fit relation of Bentz et al. | Cho, Hojin; Woo, Jong-Hak; Hodges-Kluck, Edmund; Son, Donghoon; Shin, Jaejin; Gallo, Elena; Bae, Hyun-Jin; Brink, Thomas G.; Cho, Wanjin; Filippenko, Alexei, V; Horst, John C.; Ilic, Dragana; Joner, Michael D.; Kang, Daeun; Kang, Wonseok; Kaspi, Shai; Kim, Taewoo; Kovacevic, Andjelka B.; Kumar, Sahana; Le, Huynh Anh N.; Nadzhip, A. E.; Nunez, Francisco Pozo; Metlov, V. G.; Oknyansky, V. L.; Park, Songyoun; Popovic, Luka C.; Rakshit, Suvendu; Schramm, Malte; Shatsky, N., I; Spencer, Michelle; Sung, Eon-Chang; Sung, Hyun-il; Tatarnikov, A. M.; Vince, Oliver | Seoul Natl Univ, Dept Phys & Astron, Seoul 08826, South Korea; Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA; Univ Maryland, Dept Astron, College Pk, MD 20742 USA; NASA GSFC, Code 662, Greenbelt, MD 20771 USA; Kyungpook Natl Univ, Major Astron & Atmospher Sci, Daegu 41566, South Korea; Yonsei Univ, Dept Astron, Seoul 03722, South Korea; Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA; San Diego State Univ, San Diego, CA 92182 USA; Univ Belgrade, Dept Astron, Fac Math, Studentski Trg 16, Belgrade 11000, Serbia; Brigham Young Univ, Dept Phys & Astron, N283 ESC, Provo, UT 84602 USA; Natl Youth Space Ctr, Goheung 59567, South Korea; Tel Aviv Univ, Sch Phys & Astron, IL-6997801 Tel Aviv, Israel; Tel Aviv Univ, Wise Observ, IL-6997801 Tel Aviv, Israel; Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 28644, South Korea; Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA; Univ Sci & Technol China, Dept Astron, Hefei 230026, Peoples R China; Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Ski Pr 13, Moscow 119234, Russia; Univ Haifa, Haifa Res Ctr Theoret Phys & Astrophys, Haifa, Israel; Astron Observ Belgrade, Volgina 7, Belgrade 11000, Serbia; Indian Inst Astrophys, Block 2, Bangalore 560034, Karnataka, India; Univ Turku, Quantum, Finnish Ctr Astron ESO FINCA, Vesilinnantie 5, FI-20014 Turku, Finland; Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan; Korea Astron & Space Sci Inst, Daejeon 34055, South Korea; Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA | ; Ilic, Dragana/B-3152-2017; Oknyanskij, Victor/I-9267-2012; Woo, Jong-Hak/A-2790-2014; Pozo Nunez, Francisco/AAA-2812-2022; Tatarnikov, Andrey/ABH-7130-2020; Micheli, Marco/H-7598-2015; Kumar, Sahana/GRO-5526-2022; Bae, Hyun-Jin/J-8037-2015; Shatsky, Nicolai/R-9707-2016; Popovic, Luka/JPK-1417-2023; Kang, Wonseok/KQV-2130-2024 | 55961062600; 7401751171; 18037283600; 35222498700; 55554622900; 7101964055; 51563162500; 35736928000; 57211396825; 34568722000; 55958121600; 7005535773; 6603675694; 57195546528; 55861763100; 7004725504; 57205660055; 57193345334; 57211412703; 57216800982; 57213893777; 54407345500; 6602772514; 56392912500; 59081802400; 55958163000; 55572266300; 14833238000; 6507937021; 56200618500; 7006254254; 24537938900; 6701362594; 9238445200 | woo@astro.snu.ac.kr; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 892 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2020 | 5.877 | 14.0 | 0.68 | 2025-06-25 | 16 | 15 | SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEUS; BROAD-LINE REGIONS; OPTICAL VARIABILITY; SEYFERT-1 NUCLEUS; LIGHT CURVES; NGC-4395 | English | 2020 | 2020-04-01 | 10.3847/1538-4357/ab7a98 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Production of pyruvate from Ulva reticulata using the alkaliphilic, halophilic bacterium Halomonas sp. BL6 | Green macroalgae have gained attention as promising renewable sources for biorefining. Despite the wide potential availability of green macroalgae, their utilization has been limited to ethanol production, hindering their further application. In this study, we report that a bacterium, Halomonas sp. strain BL6 (isolated from a mangrove forest in Bach Long, Nam Dinh Province, Vietnam), produces pyruvate from a saccharified solution of the green seaweed Ulva reticulata and secretes it into the medium. Pyruvate, an important alpha-oxocarboxylic acid, plays a central role in energy and carbon metabolism in living organisms and is used mainly for the synthesis of various chemicals and polymers or as an ingredient or additive in food, cosmetics, and pharmaceuticals. To investigate the possibility of using U. reticulata from the seashore of Vietnam as biomass feedstock, the chemical composition and saccharification yield of this seaweed were studied. Dry biomass of U. reticulata was found to contain 65.5% carbohydrate, 10.3% protein, 1.8% lipid, and 10.6% ash. Reducing sugar content reached 608.79 mg g(-1) of biomass after pretreatment with diluted acid and 24 h of incubation with 50 IU g(-1) Viscozyme L. The resulting sugars were fermented by Halomonas sp. strain BL6 to produce pyruvate, and the maximal pyruvate concentration reached 55.23 g L-1 after 72 h of cultivation. This study is the first to report the production of valuable compounds other than bioethanol products, such as pyruvate, from U. reticulata hydrolysate by a Halomonas strain. | Hoang Thi Lan Anh; Kawata, Yoshikazu; Luu Thi Tam; Le Thi Thom; Nguyen Cam Ha; Hoang Thi Minh Hien; Ngo Thi Hoai Thu; Pham Quang Huy; Dang Diem Hong | Vietnam Acad Sci & Technol VAST, Inst Biotechnol IBT, 18 Hoang Quoc Viet, Hanoi, Vietnam; Natl Inst Adv Ind Sci & Technol, Biomed Res Inst, Osaka, Japan; Kyungpook Natl Univ, Sch Appl Biosci, Daegu, South Korea; Thuyloi Univ, Hanoi, Vietnam; Vietnam Acad Sci & Technol, Grad Univ Sci & Technol, Hanoi, Vietnam | Pham, Quang/AAB-3064-2022; Kawata, Yoshikazu/L-7714-2018 | 55256013700; 57197423043; 56052972000; 56649218600; 56053061300; 42161245300; 46661474100; 57214084374; 7201840679 | y-kawata@aist.go.jp;ddhong60vn@yahoo.com; | JOURNAL OF APPLIED PHYCOLOGY | J APPL PHYCOL | 0921-8971 | 1573-5176 | 32 | 4 | SCIE | BIOTECHNOLOGY & APPLIED MICROBIOLOGY;MARINE & FRESHWATER BIOLOGY | 2020 | 3.215 | 14.1 | 1.22 | 2025-06-25 | 14 | 17 | Halomonas; Green seaweed; Halophilic bacteria; Pyruvate; Ulva reticulata | BIOETHANOL PRODUCTION; ENZYMATIC-HYDROLYSIS; CHEMICAL-COMPOSITION; ESCHERICHIA-COLI; SP KM-1; BIOTECHNOLOGICAL PRODUCTION; (R)-3-HYDROXYBUTYRIC ACID; FERMENTABLE SUGARS; IN-SITU; SEAWEED | Green seaweed; Halomonas; Halophilic bacteria; Pyruvate; Ulva reticulata | English | 2020 | 2020-08 | 10.1007/s10811-020-02035-1 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||
| ○ | ○ | Article | Reliable organic memristors for neuromorphic computing by predefining a localized ion-migration path in crosslinkable polymer | In flexible neuromorphic systems for realizing artificial intelligence, organic memristors are essential building blocks as artificial synapses to perform information processing and memory. Despite much effort to implement artificial neural networks (ANNs) using organic memristors, the reliability of these devices is inherently hampered by global ion transportation and arbitrary growth of conductive filaments (CFs). As a result, the performance of ANNs is restricted. Herein, a novel concept for confining CF growth in organic memristors is demonstrated by exploiting the unique functionality of crosslinkable polymers. This can be achieved by predefining the localized ion-migration path (LIP) in crosslinkable polymers. In the proposed organic memristor, metal cations are locally transported along the LIP. Thus, CF growth is achieved only in a confined region. A flexible memristor with an LIP exhibits a vastly improved reliability and uniformity, and it is capable of operating with high mechanical and electrical endurance. Moreover, neuromorphic arrays based on the proposed memristor exhibit 96.3% learning accuracy, which is comparable to the ideal software baseline. The proposed concept of predefining the LIP in organic memristors is expected to provide novel platforms for the advance of flexible electronics and to realize a variety of practical neural networks for artificial intelligence applications. | Park, Hea-Lim; Kim, Min-Hwi; Kim, Min-Hoi; Lee, Sin-Hyung | Seoul Natl Univ, Dept Mat Sci & Engn, Gwanak Ku, Seoul 151600, South Korea; Seoul Natl Univ, Sch Elect & Comp Engn, Gwanak Ku, Seoul 151600, South Korea; Hanbat Natl Univ, Dept Creat Convergence Engn, Yuseong Ku, Daejeon 305719, South Korea; Kyungpook Natl Univ, Sch Elect Engn, Daegu 702701, South Korea; Kyungpook Natl Univ, Sch Elect & Elect Engn, Daegu 702701, South Korea | ; Lee, Sin-Hyung/ABD-6425-2022 | 55735654600; 56647038300; 38260922200; 57226880204 | haelim1017@snu.ac.kr;goldmand@snu.ac.kr;mhkim8@hanbat.ac.kr;sinhlee@knu.ac.kr; | NANOSCALE | NANOSCALE | 2040-3364 | 2040-3372 | 12 | 44 | SCIE | CHEMISTRY, MULTIDISCIPLINARY;MATERIALS SCIENCE, MULTIDISCIPLINARY;NANOSCIENCE & NANOTECHNOLOGY;PHYSICS, APPLIED | 2020 | 7.79 | 14.1 | 1.48 | 2025-06-25 | 48 | 45 | RESISTIVE SWITCHING CHARACTERISTICS; SYNAPTIC PLASTICITY; LINKING; GROWTH | Flexible electronics; Ions; Memristors; Organic polymers; Conductive filaments; Crosslinkable polymers; Ion migration paths; Ion transportation; Mechanical and electrical; Neuromorphic computing; Neuromorphic systems; Practical neural networks; Neural networks | English | 2020 | 2020-11-28 | 10.1039/d0nr06964g | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||
| ○ | ○ | Article; Proceedings Paper | Brand name and ethnicity of endorser in luxury goods: does a glocalization strategy work in China? | This study focuses on the effectiveness of a glocalization strategy in China to investigate the ways in which language and ethnicity affect the consumer's perceptions of a brand's luxuriousness and consequently their intention to purchase. The findings of the study suggest that although a foreign brand name (i.e., one that is written in the Roman alphabet) is more effective than a Chinese brand name, the effects of bilingual brand naming (both foreign and Chinese brand names) are somewhat complicated. The findings show that in terms of the perception of a brand's luxuriousness, bilingual brand naming is as ineffective as a Chinese brand name is. Regarding purchase intention, however, the effect of bilingual brand naming is as effective as a foreign brand name is. The findings further demonstrate the interaction effect of brand naming strategy and the ethnicity of the endorser. The results reveal that bilingual brand naming generates a weaker perception of a brand's luxuriousness than a foreign brand name does when the endorser is a Western celebrity rather than a Chinese celebrity. Finally, the findings also indicate the moderated mediation of the perceptions of a brand's luxuriousness. | Kim, Sojung; Yi Luk, Ka; Xia, Binfang; Xu, Nan; Yin, Xinzhu | Kyungpook Natl Univ, Dept Journalism & Commun, 80 Daehak Ro, Daegu, South Korea; Chinese Univ Hong Kong, Sch Journalism & Commun, Shatin, Hong Kong, Peoples R China; Carmel Secondary Sch, Kowloon, Hong Kong, Peoples R China; Sina Weibo, Shanghai, Peoples R China; Pinduoduo, Shanghai, Peoples R China; COFCO, Beijing, Peoples R China | 37057544300; 57205455347; 57205453398; 57205458965; 57205453005 | sojungkim@mail.knu.ac.kr; | INTERNATIONAL JOURNAL OF ADVERTISING | INT J ADVERT | 0265-0487 | 1759-3948 | 39 | 6 | SSCI | BUSINESS;COMMUNICATION | 2020 | 4.62 | 14.2 | 1.4 | 2025-06-25 | 17 | 22 | Global advertising; glocalization; brand name; celebrity endorser; luxury brand; China | CELEBRITY ENDORSER; CONSUMER MEMORY; MODERATING ROLE; PERCEPTIONS; LANGUAGE; SIGNALS | brand name; celebrity endorser; China; Global advertising; glocalization; luxury brand | English | 2020 | 2020-08-17 | 10.1080/02650487.2018.1548197 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||
| ○ | ○ | Article | Chromosomal features revealed by comparison of genetic maps of Glycine max and Glycine soja | Recombination is a crucial component of evolution and breeding. New combinations of variation on chromosomes are shaped by recombination. Recombination is also involved in chromosomal rearrangements. However, recombination rates vary tremendously among chromosome segments. Genome-wide genetic maps are one of the best tools to study variation of recombination. Here, we describe high density genetic maps of Glycine max and Glycine sofa constructed from four segregating populations. The maps were used to identify chromosomal rearrangements and find the highly predictable pattern of cross-overs on the broad scale in soybean. Markers on these genetic maps were used to evaluate assembly quality of the current soybean reference genome sequence. We find a strong inversion candidate larger than 3 Mb based on patterns of cross-overs. We also identify quantitative trait loci (QTL) that control number of cross-overs. This study provides fundamental insights relevant to practical strategy for breeding programs and for pan-genome researches. | Lee, Kwanghee; Kim, Myung-Shin; Lee, Ju Seok; Bae, Dong Nyuk; Jeong, Namhee; Yang, Kiwoung; Lee, Jeong-Dong; Park, Jung-Ho; Moon, Jung-Kyung; Jeong, Soon-Chun | Korea Res Inst Biosci & Biotechnol, Bioevaluat Ctr, Cheongju 28116, Chungbuk, South Korea; Rural Dev Adm, Natl Inst Crop Sci, Wonju 55365, Jeonbuk, South Korea; Kyungpook Natl Univ, Sch Appl Biosci, Daegu 41566, South Korea; Rural Dev Adm, Agr Genome Ctr, Natl Acad Agr Sci, Jeonju 55365, Jeonbuk, South Korea; Geolim Pharmaceut Co Ltd, QB E Centum 2307,Centumjunggang Ro 90, Busan, South Korea | 55930350000; 56949188400; 56604318000; 56996793100; 24177279200; 7404291604; 40462075100; 36546514200; 7403231454; 55646368100 | scjeong@kribb.re.kr; | GENOMICS | GENOMICS | 0888-7543 | 1089-8646 | 112 | 2 | SCIE | BIOTECHNOLOGY & APPLIED MICROBIOLOGY;GENETICS & HEREDITY | 2020 | 5.736 | 14.2 | 0.34 | 2025-06-25 | 5 | 6 | Genetic map; Inversion; Recombination; Soybean | RECOMBINANT INBRED LINES; REPLICATION PROTEIN-A; MEIOTIC RECOMBINATION; LINKAGE MAP; GENOME EVOLUTION; MAIZE; SEQUENCE; POLYMORPHISMS; DIVERSITY; POTATO | Genetic map; Inversion; Recombination; Soybean | Chromosomes, Plant; Crossing Over, Genetic; Gene Rearrangement; Genetic Linkage; Plant Breeding; Quantitative Trait Loci; Sequence Alignment; Soybeans; Article; chromosome inversion; chromosome rearrangement; comparative study; controlled study; crossing over; gene mapping; gene segregation; gene sequence; genetic marker; Glycine (plant); Glycine soja; nonhuman; plant breeding; plant chromosome; plant genetics; plant genome; prediction; priority journal; quantitative trait locus; soybean; classification; gene rearrangement; genetic linkage; genetics; plant chromosome; sequence alignment; soybean | English | 2020 | 2020-03 | 10.1016/j.ygeno.2019.08.019 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||
| ○ | ○ | Article | Incidence of oral anticoagulant interruption among stroke patients with atrial fibrillation and subsequent stroke | Background and purpose We analyzed the incidence and causes of oral anticoagulant (OAC) cessation and subsequent stroke after OAC withdrawal in a cohort of Korean stroke patients with atrial fibrillation. Methods The Korean Atrial Fibrillation Evaluation Registry in Ischemic Stroke patients (K-ATTENTION) is a multicenter cohort study, merging stroke registries from 11 tertiary centers in Korea. The number of OAC interruption episodes and the reasons were reviewed from hospital records. Stroke after OAC withdrawal was defined when a patient experienced ischaemic stroke within 31 days after OAC withdrawal. Clinical variables were compared between patients who experienced stroke recurrence during OAC interruption and those who did not experience recurrence. Results Among 3213 stroke patients with atrial fibrillation, a total of 329 episodes of OAC interruption were detected in 229 patients after index stroke (mean age 72.9 +/- 8.3 years, 113 female patients). The most frequent reason for OAC withdrawal was poor compliance [103 episodes (31.3%)] followed by extracranial bleeding [96 episodes (29.2%)]. Stroke after OAC withdrawal was noted in 13 patients. Mean age, vascular risk factor profile and mean CHA(2)DS(2)-VASc score were not significantly different between patients with and without recurrent stroke. Conclusions A considerable number of stroke patients with atrial fibrillation experienced temporary interruption of OAC after index stroke, which was associated with stroke recurrence of 4.0 cases per 100 interruption episodes. | Kim, J. -M.; Park, K. -Y.; Yu, I. -W.; Song, T. -J.; Kim, Y. -J.; Kim, B. J.; Heo, S. H.; Jung, J. -M.; Oh, K. -M.; Kim, C. K.; Yu, S.; Park, J. -H.; Choi, J. C.; Park, M. -S.; Kim, J. -T.; Choi, K. -H.; Hwang, Y. -H.; Chung, J. -W.; Bang, O. Y.; Kim, G. -M.; Seo, W. -K. | Chung Ang Univ, Dept Neurol, Coll Med, Seoul, South Korea; Sungkyunkwan Univ, Dept Neurol, Samsung Med Ctr, Sch Med, Seoul, South Korea; Ewha Womans Univ, Coll Med, Dept Neurol, Seoul Hosp, Seoul, South Korea; Catholic Univ Korea, Dept Neurol, Eunpyeong St Marys Hosp, Seoul, South Korea; Univ Ulsan, Coll Med, Dept Neurol, Asan Med Ctr, Seoul, South Korea; Kyung Hee Univ, Dept Neurol, Coll Med, Seoul, South Korea; Korea Univ, Coll Med, Dept Neurol, Ansan Hosp, Seoul, Kyungki Do, South Korea; Korea Univ, Dept Neurol, Guro Hosp, Coll Med, Seoul, South Korea; Korea Univ, Dept Neurol, Anam Hosp, Coll Med, Seoul, South Korea; Hanyang Univ, Myongji Hosp, Dept Neurol, Coll Med, Goyang, South Korea; Jeju Natl Univ, Dept Neurol, Jeju, South Korea; Chonnam Natl Univ Hosp, Dept Neurol, Gwangju, South Korea; Kyungpook Natl Univ, Dept Neurol, Sch Med & Hosp, Daegu, South Korea | choi, jo/O-5940-2014; Jung, Jin-Man/LJL-8037-2024; Kim, Bum Joon/S-2156-2017; Choi, Kangho/HKV-1503-2023; Kim, Yong-Jae/JQW-5758-2023; HWANG, Yang-Ha/F-3068-2013; Kim, Chi/AAR-9819-2020; kim, jong-eun/B-3550-2017; Heo, Sung/P-3529-2019; Chung, Jin/J-5649-2012 | 7601375827; 36060099300; 57209299636; 55507164200; 55865497600; 57214661365; 18835720200; 15755814800; 16048029600; 56701057800; 56144716300; 55716977200; 7501392645; 7404490852; 23667663000; 36491173100; 7402311308; 55553751200; 7006620221; 35237139600; 22981667600 | kwangyeol.park@gmail.com;mcastenosis@gmail.com; | EUROPEAN JOURNAL OF NEUROLOGY | EUR J NEUROL | 1351-5101 | 1468-1331 | 27 | 5 | SCIE | CLINICAL NEUROLOGY;NEUROSCIENCES | 2020 | 6.089 | 14.2 | 0.24 | 2025-06-25 | 3 | 4 | atrial fibrillation; ischaemic stroke; oral anticoagulant | atrial fibrillation; ischaemic stroke; oral anticoagulant | anticoagulant agent; apixaban; dabigatran; rivaroxaban; warfarin; aged; anticoagulant therapy; Article; atrial fibrillation; brain hemorrhage; brain ischemia; CHA2DS2-VASc score; cohort analysis; controlled study; drug withdrawal; female; human; Korea; major clinical study; male; medical record review; medication compliance; patient compliance; priority journal; recurrent disease; risk factor; stroke patient; treatment interruption | English | 2020 | 2020-05 | 10.1111/ene.14175 | 바로가기 | 바로가기 | 바로가기 | 바로가기 |
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