연구성과로 돌아가기
2022 연구성과 (92 / 280)
※ 컨트롤 + 클릭으로 열별 다중 정렬 가능합니다.
Excel 다운로드
| 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 |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| ○ | ○ | Article | Mid-infrared Variability of Low-redshift Active Galactic Nuclei: Constraints on a Hot Dust Component with a Variable Covering Factor | We utilize mid-infrared multiepoch data from the Wide-field Infrared Survey Explorer over a similar to 10 yr period in the W1 (3.4 mu m) and W2 (4.6 mu m) bands to investigate the structure of dusty torus in low-redshift (0.15 < z <= 0.4) active galactic nuclei (AGNs). We calculate a Spearman correlation coefficient (r (12)) between the W1 magnitude and W1 - W2 color based on the light curve in individual objects. Interestingly, r (12) spans a broad range from -1 to 1 and is detected to be correlated with mean W1 - W2 color and AGN bolometric luminosity, in the sense that objects with a blue W1 - W2 color and low AGN luminosity tend to become redder (bluer) with increasing (decreasing) W1 brightness in the light curve (i.e., r (12) < 0), although the correlation of r (12) with the bolometric luminosity is relatively weak. The fit for the spectral energy distribution reveals a significant contribution from the host galaxy in the W1 and W2 bands. However, the dependencies of r (12) on the W1 - W2 color and AGN luminosity still persist even after careful elimination of the host light contribution. We propose that this result can be explained if the covering factor of the hot dust component decreases as the AGN luminosity increases. | Son, Suyeon; Kim, Minjin; Ho, Luis C. | Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 702701, South Korea; Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China; Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China | ; Kim, Minjin/AAU-9910-2020 | 57226328130; 56898213300; 57225302746 | mkim.astro@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 927 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 0.92 | 2025-06-25 | 11 | 11 | SPECTRAL ENERGY-DISTRIBUTIONS; BLACK-HOLE MASSES; PHYSICAL-PROPERTIES; INFRARED-SPECTRA; STAR-FORMATION; GALAXIES; EMISSION; TORUS; QUASARS; MORPHOLOGY | English | 2022 | 2022-03-01 | 10.3847/1538-4357/ac4dfc | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Optimal β-galactosidases for producing high-titer 3,6-anhydro-L-galactose from red-algal agarobiose | 3,6-Anhydro-L-galactose (L-AHG) is a monomeric sugar in agarose derived from red macroalgae. Owing to its various physiological activities such as anti-inflammation, moisturizing, skin whitening, anti-colon cancer, and anti-cariogenicity, L-AHG is a potential functional ingredient. In our previous study, a simple and efficient two-step L-AHG production process was designed for high-titer L-AHG production, where a single enzyme was used after the liquefaction of agarose by acid prehydrolysis. However, the enzyme used did not completely hydrolyze agarobiose (AB). Therefore, in this study, for the efficient hydrolysis of AB and the high-titer production of L-AHG, various beta-galactosidases belonging to glycoside hydrolase families 1, 2, 35, and 42 were compared by testing their substrate specificities and kinetic parameters. Among the five beta-galactosidases, Bga42A, originating from Bifidobacterium longum ssp. infantis ATCC 15,697, showed the highest substrate specificity. Consequently, the two-step process utilizing Bga42A as a single enzyme resulted in a high-titer production of L-AHG at 85.9 g/L, demonstrating the feasibility of producing L-AHG from agarose. | Kim, Dong Hyun; Park, So Young; Kim, Kyoung Heon | Kyungpook Natl Univ, Sch Food Sci & Biotechnol, Daegu 41566, South Korea; Kyungpook Natl Univ, Dept Integrat Biotechnol, Daegu 41566, South Korea; Korea Univ, Grad Sch, Dept Biotechnol, Seoul 02841, South Korea; Korea Univ, Coll Life Sci & Biotechnol, Dept Food Biosci & Technol, Seoul 02841, South Korea | Kim, Dong Hyun/LDT-2672-2024 | 55574224522; 57209271964; 34770896300 | khekim@korea.ac.kr; | APPLIED MICROBIOLOGY AND BIOTECHNOLOGY | APPL MICROBIOL BIOT | 0175-7598 | 1432-0614 | 106 | 24 | SCIE | BIOTECHNOLOGY & APPLIED MICROBIOLOGY | 2022 | 5 | 22.5 | 0.2 | 2025-06-25 | 2 | 2 | 3,6-Anhydro-L-galactose; Agarose; Agarobiose; Agarobiose hydrolase; beta-galactosidase; Bga42A; Bifidobacterium longum ssp; infantis; Red macroalgae | AGAROSE; AGARASE; SACCHARIFICATION; HYDROLYSIS; FUSION | 3,6-Anhydro-L-galactose; Agarobiose; Agarobiose hydrolase; Agarose; β-galactosidase, Bga42A, Bifidobacterium longum ssp. infantis, Red macroalgae | beta-Galactosidase; Galactose; Humans; Hydrolysis; Physiology; Substrates; agarose; beta galactosidase; glycosidase; hydrolase; beta galactosidase; galactose; 3,6-anhydro-L-galactose; Agarobiose; Agarobiose hydrolase; Agarose; Bifidobacterium longum; Infanti, red macroalga; Macro-algae; Substrate specificity; β- Galactosidase; Β-galactosidase, bga42a, bifidobacteria longum ssp.; concentration (composition); enzyme activity; hydrolysis; liquefaction; red alga; substrate; sugar; Article; Bifidobacterium longum subsp. infantis; cell suspension; cost effectiveness analysis; enzyme activity; enzyme mechanism; enzyme specificity; Escherichia coli; feasibility study; flow rate; heat shock; high performance liquid chromatography; hydrolysis; industrial production; kinetic parameters; macroalga; molecular weight; negative feedback; nonhuman; polyacrylamide gel electrophoresis; polymerase chain reaction; quantitative analysis; recombinant plasmid; refraction index; size exclusion chromatography; thin layer chromatography; human; Hydrolases | English | 2022 | 2022-12 | 10.1007/s00253-022-12274-6 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |
| ○ | ○ | Article | Properties of Fast and Slow Bars Classified by Epicyclic Frequency Curves from Photometry of Barred Galaxies | We test the idea that bar pattern speeds decrease with time owing to angular momentum exchange with a dark matter halo. If this process actually occurs, then the radii of the corotation resonance and other resonances should generally increase with time. We therefore derive the angular velocity omega and epicyclic frequency kappa as functions of galactocentric radius for 85 barred galaxies using photometric data. Mass maps are constructed by assuming a dynamical mass-to-light ratio and then solving the Poisson equation for the gravitational potential. The locations of Lindblad resonances and the corotation resonance radius are then derived using the standard precession frequency curves in conjunction with bar pattern speeds recently estimated from the Tremaine-Weinberg method as applied to integral field spectroscopy data. Correlations between physical properties of bars and their host galaxies indicate that bar length and the corotation radius depend on the disk circular velocity while bar strength and pattern speed do not. As the bar pattern speed decreases, bar strength, length, and corotation radius increase, but when bars are subclassified into fast, medium, and slow domains, no significant change in bar length is found. Only a hint of an increase in bar strength from fast to slow bars is found. These results suggest that bar length in a galaxy undergoes little evolution, and is determined instead mainly by the size of the host galaxy. | Lee, Yun Hee; Park, Myeong-Gu; Hwang, Ho Seong; Ann, Hong Bae; Chung, Haeun; Kim, Taehyun | Korea Astron & Space Sci Inst KASI, 776 Daedeokdae Ro, Daejeon 34055, South Korea; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Seoul Natl Univ, Dept Phys & Astron, Astron Program, 1 Gwanak Ro, Seoul 08826, South Korea; Seoul Natl Univ, SNU Astron Res Ctr, 1 Gwanak Ro, Seoul 08826, South Korea; Pusan Natl Univ, Dept Earth Sci Educ, Busan 46241, South Korea; Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA | ; HWANG, Ho/AAS-6010-2020 | 57206855558; 7404490321; 15131707100; 55880768900; 56514444900; 57050549000 | hhwang@astro.snu.ac.kr; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 926 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 1.01 | 2025-06-25 | 12 | 12 | TREMAINE-WEINBERG METHOD; PATTERN SPEED; COROTATION RADII; GRAVITATIONAL TORQUES; DISK GALAXIES; STELLAR BARS; DARK-MATTER; EVOLUTION; MASS; HALO | English | 2022 | 2022-02-01 | 10.3847/1538-4357/ac3bc1 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Radio Spectra of Luminous, Heavily Obscured WISE-NVSS Selected Quasars | We present radio spectra spanning 0.1-10 GHz for the sample of heavily obscured luminous quasars with extremely red mid-infrared-optical colors and compact radio emission. The spectra are constructed from targeted 10 GHz observations and archival radio survey data that together yield 6-11 flux-density measurements for each object. Our primary result is that most (62%) of the sample have peaked or curved radio spectra and many (37%) could be classified as Gigahertz-Peaked Spectrum (GPS) sources. This indicates compact emission regions likely arising from recently triggered radio jets. Assuming synchrotron self-absorption (SSA) generates the peaks, we infer compact source sizes (3-100 pc) with strong magnetic fields (6-100 mG) and young ages (30-10(4) yr). Conversely, free-free absorption (FFA) could also create peaks due to the high column densities associated with the deeply embedded nature of the sample. However, we find no correlations between the existence or frequency of the peaks and any parameters of the MIR emission. The high-frequency spectral indices are steep (alpha approximate to -1) and correlate, weakly, with the ratio of MIR photon energy density to magnetic energy density, suggesting that the spectral steepening could arise from inverse Compton scattering off the intense MIR photon field. This study provides a foundation for combining multifrequency and mixed-resolution radio survey data for understanding the impact of young radio jets on the ISM and star-formation rates of their host galaxies. faGithub | Patil, Pallavi; Whittle, Mark; Nyland, Kristina; Lonsdale, Carol; Lacy, Mark; Kimball, Amy E.; Lonsdale, Colin; Peters, Wendy; Clarke, Tracy E.; Efstathiou, Andreas; Giacintucci, Simona; Kim, Minjin; Lanz, Lauranne; Mukherjee, Dipanjan; Polisensky, Emil | Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA; Univ Virginia, Dept Astron, 530 McCormick Rd, Charlottesville, VA 22903 USA; US Naval Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA; Natl Radio Astron Observ, 520 Edgemt Rd, Charlottesville, VA 22903 USA; MIT, Haystack Observ, Westford, MA 01886 USA; European Univ Cyprus, Sch Sci, CY-1516 Nicosia, Cyprus; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Coll New Jersey, Dept Phys, 2000 Pennington Rd, Ewing, NJ 08628 USA; Interuniv Ctr Astron & Astrophys, Post Bag 4, Pune 411007, Maharashtra, India | ; Kim, Minjin/AAU-9910-2020; Nyland, Kristina/AAT-5789-2021; Peters, Wendy/Z-1657-2019; Patil, Pallavi/AAU-1181-2021; Mukherjee, Dipanjan/ADX-8683-2022 | 57206841167; 56274963100; 37079464100; 35187480800; 7101765328; 35417434300; 35357992400; 36612316600; 7202915714; 7005273826; 6506851709; 56898213300; 22835067800; 57210240679; 36662849100 | ppatil@nrao.edu; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 934 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 1.17 | 2025-06-25 | 13 | 14 | COMPACT STEEP-SPECTRUM; SYNCHROTRON SELF-ABSORPTION; GIGAHERTZ-PEAKED-SPECTRUM; RELATIVISTIC JET FEEDBACK; DIGITAL SKY SURVEY; BLACK-HOLES; NONTHERMAL EMISSION; STAR-FORMATION; GALAXIES; FREQUENCY | English | 2022 | 2022-07-01 | 10.3847/1538-4357/ac71b0 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Reclassifying Swift Gamma-Ray Bursts with Diverse Duration Distributions | We select the largest sample of Swift gamma-ray bursts (GRBs) so far to reexamine the classification in terms of time duration, hardness ratio, and physical collapse model. To analyze the sample selection effect, we divide the observed Swift GRB sample into four subsamples according to signal-to-noise level, spectral quality, and extended emission. First, we find that only the sample of Swift GRBs with well-measured peak energy can be evidently divided into two types at a boundary of similar to 1 s, and other data sets are well described by three Gaussian functions. Using Swift GRBs with known redshift, a Kolmogorov-Smirnov test shows the intrinsic duration distributions of five data sets are equally distributed. Second, we ascertain in the plane of hardness ratio versus duration that the hardness ratio of short GRBs is significantly higher than those of middle classes and long GRBs, while the latter two components are the same in statistics, implying the so-called middle class to be artificial. Third, we apply a collapse model to discriminate the boundaries between collapse and noncollapse Swift bursts. It is interesting to find that a significant fraction, >= 30%, of Swift short GRBs could have originated from the collapsing progenitors, while all long GRBs are produced from the collapsars only. Finally, we point out that short GRBs with extended emission are the main contributors to the noncollapsar population with longer duration. | Deng, Q.; Zhang, Z. -B.; Li, X. -J.; Chang, H. -Y.; Zhang, X. -L.; Zhen, H. -Y.; Sun, H.; Pan, Q.; Dong, X. -F. | Qufu Normal Univ, Sch Phys & Phys Engn, Qufu 273165, Peoples R China; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, 1370 Sankyuk Dong, Daegu 702701, South Korea; Huantai No 1 Middle Sch Shandong Prov, Huantai 256499, Peoples R China | Zhang, Kai/ABA-7428-2020; DONG, Xufeng/AGT-9485-2022 | 57976770400; 57192634952; 57216877690; 7407524806; 58449541200; 57222135158; 55848814300; 57211411146; 57216888420 | z-b-zhang@163.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 940 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 0.5 | 2025-06-25 | 7 | 6 | EXTENDED EMISSION; GRAVITATIONAL-WAVES; TEMPORAL PROPERTIES; PEAK ENERGY; SHORT GRBS; LONG; FERMI; BATSE | English | 2022 | 2022-11-01 | 10.3847/1538-4357/ac9590 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2 | We present and analyze observations of polarized dust emission at 850 mu m toward the central 1 x 1 pc hub-filament structure of Monoceros R2 (Mon R2). The data are obtained with SCUBA-2/POL-2 on the James Clerk Maxwell Telescope (JCMT) as part of the B-fields in Star-forming Region Observations survey. The orientations of the magnetic field follow the spiral structure of Mon R2, which are well described by an axisymmetric magnetic field model. We estimate the turbulent component of the magnetic field using the angle difference between our observations and the best-fit model of the underlying large-scale mean magnetic field. This estimate is used to calculate the magnetic field strength using the Davis-Chandrasekhar-Fermi method, for which we also obtain the distribution of volume density and velocity dispersion using a column density map derived from Herschel data and the (CO)-O-18 (J = 3 - 2) data taken with HARP on the JCMT, respectively. We make maps of magnetic field strengths and mass-to-flux ratios, finding that magnetic field strengths vary from 0.02 to 3.64 mG with a mean value of 1.0 +/- 0.06 mG, and the mean critical mass-to-flux ratio is 0.47 +/- 0.02. Additionally, the mean Alfven Mach number is 0.35 +/- 0.01. This suggests that, in Mon R2, the magnetic fields provide resistance against large-scale gravitational collapse, and the magnetic pressure exceeds the turbulent pressure. We also investigate the properties of each filament in Mon R2. Most of the filaments are aligned along the magnetic field direction and are magnetically subcritical. | Hwang, Jihye; Kim, Jongsoo; Pattle, Kate; Lee, Chang Won; Koch, Patrick M.; Johnstone, Doug; Tomisaka, Kohji; Whitworth, Anthony; Furuya, Ray S.; Kang, Ji-hyun; Lyo, A-Ran; Chung, Eun Jung; Arzoumanian, Doris; Park, Geumsook; Kwon, Woojin; Kim, Shinyoung; Tamura, Motohide; Kwon, Jungmi; Soam, Archana; Han, Ilseung; Hoang, Thiem; Kim, Kyoung Hee; Onaka, Takashi; Eswaraiah, Chakali; Ward-Thompson, Derek; Liu, Hong-Li; Tang, Xindi; Chen, Wen Ping; Matsumura, Masafumi; Thuong Duc Hoang; Chen, Zhiwei; Le Gouellec, Valentin J. M.; Kirchschlager, Florian; Poidevin, Frederick; Bastien, Pierre; Qiu, Keping; Hasegawa, Tetsuo; Lai, Shih-Ping; Byun, Do-Young; Cho, Jungyeon; Choi, Minho; Choi, Youngwoo; Choi, Yunhee; Jeong, Il-Gyo; Kang, Miju; Kim, Hyosung; Kim, Kee-Tae; Lee, Jeong-Eun; Lee, Sang-Sung; Lee, Yong-Hee; Lee, Hyeseung; Kim, Mi-Ryang; Yoo, Hyunju; Yun, Hyeong-Sik; Chen, Mike; Di Francesco, James; Fiege, Jason; Fissel, Laura M.; Franzmann, Erica; Houde, Martin; Lacaille, Kevin; Matthews, Brenda; Sadavoy, Sarah; Moriarty-Schieven, Gerald; Tahani, Mehrnoosh; Ching, Tao-Chung; Dai, Y. Sophia; Duan, Yan; Gu, Qilao; Law, Chi-Yan; Li, Dalei; Li, Di; Li, Guangxing; Li, Hua-bai; Liu, Tie; Lu, Xing; Qian, Lei; Wang, Hongchi; Wu, Jintai; Xie, Jinjin; Yuan, Jinghua; Zhang, Chuan-Peng; Zhang, Guoyin; Zhang, Yapeng; Zhou, Jianjun; Zhu, Lei; Berry, David; Friberg, Per; Graves, Sarah; Liu, Junhao; Mairs, Steve; Parsons, Harriet; Rawlings, Mark; Doi, Yasuo; Hayashi, Saeko; Hull, Charles L. H.; Inoue, Tsuyoshi; Inutsuka, Shu-ichiro; Iwasaki, Kazunari; Kataoka, Akimasa; Kawabata, Koji; Kim, Gwanjeong; Kobayashi, Masato I. N.; Nagata, Tetsuya; Nakamura, Fumitaka; Nakanishi, Hiroyuki; Pyo, Tae-Soo; Saito, Hiro; Seta, Masumichi; Shimajiri, Yoshito; Shinnaga, Hiroko; Tsukamoto, Yusuke; Zenko, Tetsuya; Chen, Huei-Ru Vivien; Duan, Hao-Yuan; Fanciullo, Lapo; Kemper, Francisca; Lee, Chin-Fei; Lin, Sheng-Jun; Liu, Sheng-Yuan; Ohashi, Nagayoshi; Rao, Ramprasad; Tang, Ya-Wen; Wang, Jia-Wei; Yang, Meng-Zhe; Yen, Hsi-Wei; Bourke, Tyler L.; Chrysostomou, Antonio; Debattista, Victor; Eden, David; Eyres, Stewart; Falle, Sam; Fuller, Gary; Gledhill, Tim; Greaves, Jane; Griffin, Matt; Hatchell, Jennifer; Karoly, Janik; Kirk, Jason; Konyves, Vera; Longmore, Steven; van Loo, Sven; de Looze, Ilse; Peretto, Nicolas; Priestley, Felix; Rawlings, Jonathan; Retter, Brendan; Richer, John; Rigby, Andrew; Savini, Giorgio; Scaife, Anna; Viti, Serena; Pham Ngoc Diep; Nguyen Bich Ngoc; Le Ngoc Tram; Andre, Philippe; Coude, Simon; Dowell, C. Darren; Friesen, Rachel; Robitaille, Jean-Francois | Korea Astron & Space Sci Inst KASI, 776 Daedeokdae Ro, Daejeon 34055, South Korea; Univ Sci & Technol Korea UST, 217 Gajeong Ro, Daejeon 34113, South Korea; UCL, Dept Phys & Astron, London WC1E 6BT, England; Acad Sinica, Inst Astron & Astrophys, 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan; NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada; Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada; Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan; SOKENDAI Grad Univ Adv Studies, Hayama, Kanagawa 2400193, Japan; Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales; Tokushima Univ, Inst Liberal Arts & Sci, Minami Jousanajima Machi 1-1, Tokushima 7708502, Japan; Chungnam Natl Univ, Dept Astron & Space Sci, 99 Daehak Ro, Daejeon 34134, South Korea; Natl Astron Observ Japan, Div Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan; Seoul Natl Univ SNU, Dept Earth Sci Educ, 1 Gwanak Ro, Seoul 08826, South Korea; Seoul Natl Univ, SNU Astron Res Ctr, 1 Gwanak Ro, Seoul 08826, South Korea; Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan; Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan; Natl Inst Nat Sci, Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan; Indian Inst Astrophys, 2 Block, Koramangala 560034, Bengaluru, India; Basic Sci Bldg 108,50 UNIST Gil, Ulsan, South Korea; Meisei Univ, Fac Sci & Engn, Dept Phys, 2-1-1 Hodokubo, Hino, Tokyo 1918506, Japan; Indian Inst Sci Educ & Res IISER Tirupati, Karakambadi Rd,Mangalam PO, Tirupati 517507, Andhra Pradesh, India; Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England; Yunnan Univ, Dept Astron, Kunming 650091, Yunnan, Peoples R China; Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China; Natl Cent Univ, Inst Astron, Zhongli 32001, Taiwan; Kagawa Univ, Fac Educ, Saiwai Cho 1-1, Takamatsu, Kagawa 7608522, Japan; Kagawa Univ, Ctr Educ Dev & Support, Saiwai Cho 1-1, Takamatsu, Kagawa 7608522, Japan; Univ Tokyo, Kavli Inst Phys & Math Universe Kavli IPMU, UTIAS, WPI, Kashiwa, Chiba 2778583, Japan; Univ Sci & Technol Hanoi USTH, Vietnam Acad Sci & Technol VAST, 18 Hoang Quoc Viet, Hanoi, Vietnam; Chinese Acad Sci, Purple Mt Observ, 10 Yuanhua Rd, Nanjing 210023, Peoples R China; Univ Space Res Assoc, SOFIA Sci Ctr, NASA Ames Res Ctr, Moffett Field, CA 94035 USA; Univ Paris Saclay, Astrophys Instrumentat & ModA Lisat Paris Saclay, CEA, CNRS, F-91191 Gif Sur Yvette, France; Inst Astrofis Canarias, E-38200 Tenerife, Canary Islands, Spain; Univ La Laguna ULL, Dept Astrofis, E-38206 Tenerife, Spain; Univ Montreal, Ctr Rech Astrophys Quebec, 1375 Ave Therese Lavoi Roux, Montreal, PQ H2V OB3, Canada; Univ Montreal, Dept Phys, 1375 Ave Therese Lavoi Roux, Montreal, PQ H2V OB3, Canada; Nanjing Univ, Sch Astron & Space Sci, 163 Xianlin Ave, Nanjing 210023, Peoples R China; Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210023, Peoples R China; Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan; Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan; Seoul Natl Univ, Dept Phys & Astron, 1 Gwanak Ro, Seoul 08826, South Korea; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Kyung Hee Univ, Sch Space Res, 1732 Deogyeong Daero, Yongin 17104, Gyeonggi Do, South Korea; East Asian Observ, 660 N Aohoku Pl,Univ Pk, Hilo, HI 96720 USA; Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada; Queens Univ, Dept Phys Engn Phys & Astrophys, Kingston, ON K7L 3N6, Canada; Univ Western Ontario, Dept Phys & Astron, 1151 Richmond St, London, ON N6A 3K7, Canada; McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada; Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada; Natl Res Council Canada, Herzberg Astron & Astrophys Res Ctr, Dominion Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada; Stanford Univ, Kavli Inst Particle Astrophys & Cosmol KIPAC, Stanford, CA 94305 USA; Res Ctr Intelligent Comp Platforms, Zhejiang Lab, Hangzhou 311100, Peoples R China; Natl Astron Observ NAOC, Chinese Acad Sci South Amer Ctr Astron CASSACA, 20A Datun Rd, Beijing 100012, Peoples R China; Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China; Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China; Chinese Univ Hong Kong, Dept Phys, Shatin, Hong Kong, Peoples R China; Chalmers Univ Technol, Dept Space Earth & Environm, SE-41296 Gothenburg, Sweden; Res Ctr Intelligent Comp, Zhejiang Lab, Hangzhou 311100, Peoples R China; Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, 80 Nandan Rd, Shanghai 200030, Peoples R China; Chinese Acad Sci, Natl Astron Observ, CAS Key Lab FAST, Beijing, Peoples R China; Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Peoples R China; Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China; Gemini Observ NSFs NOIRLab, 670 N Aohoku Pl, Hilo, HI 96720 USA; Univ Tokyo, Grad Sch Arts & Sci, Dept Earth Sci & Astron, Meguro Ku, 3-8-1 Komaba, Tokyo 1538902, Japan; Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA; Natl Astron Observ Japan, Alonso de Cordova 3788,Off 61B, Santiago, Chile; Joint ALMA Observ, Alonso de Cordova 3107, Santiago, Chile; Konan Univ, Dept Phys, Higashinada Ku, Okamoto 8-9-1, Kobe, Hyogo 6588501, Japan; Nagoya Univ, Grad Sch Sci, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan; Doshisha Univ, Dept Environm Syst Sci, Miyakodani 1-3, Kyotanabe, Kyoto 6100394, Japan; Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Kagamiyama 1-3-1, Higashihiroshima, Hiroshima 7398526, Japan; Hiroshima Univ, Dept Phys, Kagamiyama 1-3-1, Higashihiroshima, Hiroshima 7398526, Japan; Hiroshima Univ, Core Res Energet Universe CORE U, Kagamiyama 1-3-1, Higashihiroshima, Hiroshima 7398526, Japan; Natl Inst Nat Sci, Nobeyama Radio Observ, Natl Astron Observ Japan, Minamisa Ku, Minamimaki, Nagano 3841305, Japan; Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan; Kagoshima Univ, Grad Sch Sci & Engn, Dept Phys & Astron, 1-21-35 Korimoto, Kagoshima, Kagoshima 8900065, Japan; Univ Tsukuba, Fac Pure & Appl Sci, 1-1-1 Tennodai, Tsukuba, Ibaraki 3058577, Japan; Kwansei Gakuin Univ, Sch Sci & Technol, Dept Phys, 2-1 Gakuen, Sanda, Hyogo 6691337, Japan; Natl Chung Hsing Univ, 145 Xingda Rd, Taichung 402, Taiwan; CSIC, Inst Ciencies Espai ICE, Can Magrans S-N, E-08193 Barcelona, Spain; ICREA, Pg Lluis Co 23, Barcelona, Spain; Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain; SKA Observ, Jodrell Bank, Macclesfield SK11 9FT, Cheshire, England; Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Oxford Rd, Manchester M13 9PL, Lancs, England; Armagh Observ & Planetarium, Coll Hill, Armagh BT61 9DG, North Ireland; Univ South Wales, Pontypridd CF37 1DL, M Glam, Wales; Univ Leeds, Dept Appl Math, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England; Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England; Univ Exeter, Phys & Astron, Stocker Rd, Exeter EX4 4QL, Devon, England; Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England; Univ Leeds, Sch Phys & Astron, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England; UCL, Phys & Astron Dept, London WC1E 6BT, England; Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England; Univ Cambridge, Kavli Inst Cosmol, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England; UCL, Phys & Astron Dept, OSL, London WC1E 6BT, England; Vietnam Acad Sci & Technol, Vietnam Natl Space Ctr, 18 Hoang Quoc Viet, Hanoi, Vietnam; Grad Univ Sci & Technol, Vietnam Acad Sci & Technol, 18 Hoang Quoc Viet, Hanoi, Vietnam; Univ Paris Diderot, CNRS, Lab AIM CEA DSM, IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France; Jet Prop Lab, M-S 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA; Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA; Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France | Lee, Chang/HME-1129-2023; Liu, Sheng-Yuan/AAZ-4303-2020; Chakali, Eswaraiah/L-5146-2018; Priestley, Felix/KYP-3257-2024; chen, zhiwei/AAP-5465-2020; Doi, Yasuo/A-3395-2013; Duc-Thuong, Hoang/U-1874-2017; Poidevin, Frédérick/Z-3492-2019; Han, Ilseung/MBG-4273-2025; Arzoumanian, Doris/JQT-3284-2023; Van Loo, Sven/JRX-9178-2023; Gu, Qilao/LTZ-1282-2024; WANG, Qiuhong/L-9577-2016; Hoang, Thuong/U-1874-2017; Hwang, Jihye/JXW-6363-2024; Lee, Sang-Sung/AFS-2722-2022; Shimajiri, Yoshito/B-1445-2013; 顏士韋, Hsi-Wei/C-8307-2011; Savini, Giorgio/F-5753-2019; Koch, Patrick/AAV-3373-2021; Ohashi, Nagayoshi/ABA-9767-2020; Rao, Ramprasad/L-2115-2017; Li, Guang-Xing/AAC-9285-2022; Li, Hua-bai/AEU-0239-2022; Li, Di/HLH-4146-2023; Kim, Shinyoung/JEO-8879-2023; Liu, Junhao/AAQ-3071-2021; Inutsuka, Shu-ichiro/I-7024-2014; LI, DI/HLH-4146-2023; NGOC, NGUYEN/JQJ-4239-2023; Soam, Archana/AAG-4250-2021; Savini, Gianluca/C-1188-2009; Kemper, Francisca/AAZ-8274-2020; Nanayakkara, Themiya/AAT-6271-2020; Kataoka, Akimasa/AAU-5038-2020; Liu, Hong-Li/AAR-1998-2020; Tsukamoto, Yusuke/AAU-3453-2020; Tang湯雅雯, Ya-Wen/AAZ-7382-2020; Lee, Chin-Fei/AAZ-3391-2020; Tomisaka, Kohji/E-6508-2013; Yuan, Jinghua/W-4699-2017; ONAKA, TAKASHI/G-5058-2014; , Le Ngoc Tram/AAH-2951-2019; Lee, Jeong-Eun/E-2387-2013 | 57202952564; 7601365384; 56512202800; 59684797600; 7202929125; 57215516631; 6701467496; 7006011851; 7005566228; 57201082771; 6508022172; 57206389610; 36237885400; 18936782900; 15822192800; 57194595458; 7403258846; 55370384000; 55757586800; 57194798843; 16549809400; 34770134800; 57203067199; 8318213100; 7004002583; 56436978700; 55320822200; 35242015200; 7402157762; 57200142325; 55705656800; 57211397912; 55633098300; 6506192691; 7005805931; 36976168000; 7404174499; 7402935899; 57203026080; 7403536449; 55231989000; 57944161700; 57218669464; 35330159300; 25627568300; 57944655500; 7409321582; 35748985900; 37056945900; 57209285153; 57190230987; 55671720700; 55441261000; 57209281402; 56566873100; 6603570734; 6602882601; 22834355900; 55673595500; 35237077900; 57194605392; 35569334500; 35238413800; 7003401658; 57202847250; 56342326600; 35321993600; 57217586664; 57194592820; 57209260420; 56252021400; 7405326474; 55910516500; 35185338100; 55727743600; 56179884700; 38862759600; 56084174100; 57352212300; 57219690533; 55170380200; 49865000200; 56493265600; 57207478624; 56183368700; 36955785700; 8355600600; 7005672565; 22834101100; 57194603379; 55750223500; 35096693300; 7004265198; 7401662157; 7404169517; 7103332462; 55226383000; 35377433200; 24074312000; 55750138400; 7201640315; 36571804600; 57189663358; 13310130800; 7201941871; 36714093500; 6602816367; 7407452361; 6604032293; 23061889500; 35482578500; 36971326200; 57199325064; 12790268500; 55210722100; 55874635700; 7005283695; 35330124000; 57216330092; 7409459358; 7202558313; 7403068909; 27868095600; 57194606597; 57945146700; 43361931100; 35499669400; 7005084542; 6602592863; 55170000100; 7004237751; 7004415016; 9234005200; 7003509373; 7101632548; 7403310385; 6603664735; 57219237963; 35773361100; 36238131700; 8693281200; 14042952700; 36238023800; 16070455300; 57194941451; 7101942174; 57194586988; 7006586973; 56800212700; 15844178300; 6603887796; 7003564783; 24170690100; 57216925030; 57201731842; 59821849300; 56568251300; 35308644100; 8547622700; 36908360800 | hjh3772@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 941 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 1.34 | 2025-06-25 | 16 | 16 | DENSE CORES; SCUBA-2; 1ST; POLARIZATION; GRAVITY; REGIONS; CLOUDS; POL-2; MODEL | English | 2022 | 2022-12-01 | 10.3847/1538-4357/ac99e0 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament | We present 850 mu m dust polarization observations of the massive DR21 filament from the B-fields In STar-forming Region Observations (BISTRO) survey, using the POL-2 polarimeter and the SCUBA-2 camera on the James Clerk Maxwell Telescope. We detect ordered magnetic fields perpendicular to the parsec-scale ridge of the DR21 main filament. In the subfilaments, the magnetic fields are mainly parallel to the filamentary structures and smoothly connect to the magnetic fields of the main filament. We compare the POL-2 and Planck dust polarization observations to study the magnetic field structures of the DR21 filament on 0.1-10 pc scales. The magnetic fields revealed in the Planck data are well-aligned with those of the POL-2 data, indicating a smooth variation of magnetic fields from large to small scales. The plane-of-sky magnetic field strengths derived from angular dispersion functions of dust polarization are 0.6-1.0 mG in the DR21 filament and similar to 0.1 mG in the surrounding ambient gas. The mass-to-flux ratios are found to be magnetically supercritical in the filament and slightly subcritical to nearly critical in the ambient gas. The alignment between column density structures and magnetic fields changes from random alignment in the low-density ambient gas probed by Planck to mostly perpendicular in the high-density main filament probed by James Clerk Maxwell Telescope. The magnetic field structures of the DR21 filament are in agreement with MHD simulations of a strongly magnetized medium, suggesting that magnetic fields play an important role in shaping the DR21 main filament and subfilaments. | Ching, Tao-Chung; Qiu, Keping; Li, Di; Ren, Zhiyuan; Lai, Shih-Ping; Berry, David; Pattle, Kate; Furuya, Ray; Ward-Thompson, Derek; Johnstone, Doug; Koch, Patrick M.; Lee, Chang Won; Hoang, Thiem; Hasegawa, Tetsuo; Kwon, Woojin; Bastien, Pierre; Eswaraiah, Chakali; Wang, Jia-Wei; Kim, Kyoung Hee; Hwang, Jihye; Soam, Archana; Lyo, A-Ran; Liu, Junhao; Le Gouellec, Valentin J. M.; Arzoumanian, Doris; Whitworth, Anthony; Di Francesco, James; Poidevin, Frederick; Liu, Tie; Coude, Simon; Tahani, Mehrnoosh; Liu, Hong-Li; Onaka, Takashi; Li, Dalei; Tamura, Motohide; Chen, Zhiwei; Tang, Xindi; Kirchschlager, Florian; Bourke, Tyler L.; Byun, Do-Young; Chen, Mike; Chen, Huei-Ru Vivien; Chen, Wen Ping; Cho, Jungyeon; Choi, Yunhee; Choi, Youngwoo; Choi, Minho; Chrysostomou, Antonio; Chung, Eun Jung; Dai, Y. Sophia; Diep, Pham Ngoc; Doi, Yasuo; Duan, Yan; Duan, Hao-Yuan; Eden, David; Fanciullo, Lapo; Fiege, Jason; Fissel, Laura M.; Franzmann, Erica; Friberg, Per; Friesen, Rachel; Fuller, Gary; Gledhill, Tim; Graves, Sarah; Greaves, Jane; Griffin, Matt; Gu, Qilao; Han, Ilseung; Hayashi, Saeko; Houde, Martin; Hull, Charles L. H.; Inoue, Tsuyoshi; Inutsuka, Shu-ichiro; Iwasaki, Kazunari; Jeong, Il-Gyo; Konyves, Vera; Kang, Ji-hyun; Kang, Miju; Karoly, Janik; Kataoka, Akimasa; Kawabata, Koji; Kemper, Francisca; Kim, Jongsoo; Kim, Mi-Ryang; Kim, Shinyoung; Kim, Hyosung; Kim, Kee-Tae; Kim, Gwanjeong; Kirk, Jason; Kobayashi, Masato I. N.; Kusune, Takayoshi; Kwon, Jungmi; Lacaille, Kevin; Law, Chi-Yan; Lee, Sang-Sung; Lee, Hyeseung; Lee, Jeong-Eun; Lee, Chin-Fei; Lee, Yong-Hee; Li, Guangxing; Li, Hua-bai; Lin, Sheng-Jun; Liu, Sheng-Yuan; Lu, Xing; Mairs, Steve; Matsumura, Masafumi; Matthews, Brenda; Moriarty-Schieven, Gerald; Nagata, Tetsuya; Nakamura, Fumitaka; Nakanishi, Hiroyuki; Ngoc, Nguyen Bich; Ohashi, Nagayoshi; Park, Geumsook; Parsons, Harriet; Peretto, Nicolas; Priestley, Felix; Pyo, Tae-Soo; Qian, Lei; Rao, Ramprasad; Rawlings, Mark; Rawlings, Jonathan; Retter, Brendan; Richer, John; Rigby, Andrew; Sadavoy, Sarah; Saito, Hiro; Savini, Giorgio; Seta, Masumichi; Shimajiri, Yoshito; Shinnaga, Hiroko; Tang, Ya-Wen; Tomisaka, Kohji; Tram, Le Ngoc; Tsukamoto, Yusuke; Viti, Serena; Wang, Hongchi; Wu, Jintai; Xie, Jinjin; Yang, Meng-Zhe; Yen, Hsi-Wei; Yoo, Hyunju; Yuan, Jinghua; Yun, Hyeong-Sik; Zenko, Tetsuya; Zhang, Chuan-Peng; Zhang, Yapeng; Zhang, Guoyin; Zhou, Jianjun; Zhu, Lei; de Looze, Ilse; Andre, Philippe; Dowell, C. Darren; Eyres, Stewart; Falle, Sam; Robitaille, Jean-Francois; van Loo, Sven | Zhejiang Lab, Res Ctr Intelligent Comp Platforms, Hangzhou 311100, Peoples R China; Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China; Nanjing Univ, Sch Astron & Space Sci, 163 Xianlin Ave, Nanjing 210023, Peoples R China; Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210023, Peoples R China; Univ Chinese Acad Sci, Dept Astron, Beijing 100049, Peoples R China; Univ KwaZulu Natal, NAOC UKZN Computat Astrophys Ctr, ZA-4000 Durban, South Africa; Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan; Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan; Acad Sinica, Inst Astron & Astrophys, 1,Sec 3,Roosevelt Rd, Taipei 10617, Taiwan; East Asian Observ, 660 N Aohoku Pl,Univ Pk, Hilo, HI 96720 USA; UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England; Tokushima Univ, Minami Jousanajima Machi 1-1, Tokushima 7708502, Japan; Tokushima Univ, Inst Liberal Arts & Sci, Minami Jousanajima Machi 1-1, Tokushima 7708502, Japan; Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England; NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada; Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada; Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea; Univ Sci & Technol, 217 Gajeong Ro, Daejeon 34113, South Korea; Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan; Seoul Natl Univ, Dept Earth Sci Educ, 1 Gwanak Ro, Seoul 08826, South Korea; Seoul Natl Univ, SNU Astron Res Ctr, 1 Gwanak Ro, Seoul 08826, South Korea; Univ Montreal, Ctr Rech Astrophys Quebec, 1375 Ave Therese Lavoie Roux, Montreal, PQ H2V 0B3, Canada; Univ Montreal, Dept Phys, 1375 Ave Therese Lavoie Roux, Montreal, PQ H2V 0B3, Canada; Indian Inst Sci Educ & Res IISER Tirupati, Karakambadi Rd,Mangalam PO, Tirupati 517507, Andhra Pradesh, India; Ulsan Natl Inst Sci & Technol UNIST, Coll Nat Sci, Dept Phys, 50 UNIST Gil, Ulsan 44919, South Korea; Indian Inst Astrophys IIA, Bangalore 560034, Karnataka, India; Univ Space Res Assoc, SOFIA Sci Ctr, NASA Ames Res Ctr, Moffett Field, CA 94035 USA; Univ Paris Saclay, CNRS, CEA, Astrophys Instrumentat & Modelisat Paris Saclay, F-91191 Gif Sur Yvette, France; Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales; Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Canary Islands, Spain; Univ La Laguna ULL, Dept Astrofis, E-38206 Tenerife, Spain; Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China; Worcester State Univ, Dept Earth Environm & Phys, Worcester, MA 01602 USA; Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA; Natl Res Council Canada, Herzberg Astron & Astrophys Res Ctr, Dominion Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada; Yunnan Univ, Kunming 650091, Yunnan, Peoples R China; Meisei Univ, Fac Sci & Engn, Dept Phys, 2-1-1 Hodokubo, Hino, Tokyo 1918506, Japan; Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan; Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China; Natl Inst Nat Sci, Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan; Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Peoples R China; SKA Observ, Jodrell Bank, Macclesfield SK11 9FT, Cheshire, England; Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Oxford Rd, Manchester M13 9PL, Lancs, England; Natl Cent Univ, Inst Astron, Zhongli 32001, Taiwan; Chungnam Natl Univ, Dept Astron & Space Sci, 99 Daehak Ro, Daejeon 34134, South Korea; Seoul Natl Univ, Dept Phys & Astron, 1 Gwanak Ro, Seoul 08826, South Korea; Vietnam Acad Sci & Technol, Vietnam Natl Space Ctr, 18 Hoang Quoc Viet, Hanoi, Vietnam; Univ Tokyo, Grad Sch Arts & Sci, Dept Earth Sci & Astron, Meguro Ku, 3-8-1 Komaba, Tokyo 1538902, Japan; Armagh Observ & Planetarium, Coll Hill, Armagh BT61 9DB, North Ireland; Natl Chung Hsing Univ, 145 Xingda Rd, Taichung 402, Taiwan; Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada; Queens Univ, Dept Phys Engn Phys & Astrophys, Kingston, ON K7L 3N6, Canada; Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA; Univ Hertfordshire, Dept Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England; Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA; Univ Western Ontario, Dept Phys & Astron, 1151 Richmond St, London, ON N6A 3K7, Canada; Natl Astron Observ Japan, Alonso de Cordova 3788,Off 61B, Santiago, Chile; Joint ALMA Observ, Alonso de Cordova 3107, Santiago, Chile; Nagoya Univ, Grad Sch Sci, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan; Doshisha Univ, Dept Environm Syst Sci, Miyakodani 1-3, Kyoto 6100394, Japan; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Kagamiyama 1-3-1, Higashihiroshima, Hiroshima 7398526, Japan; Hiroshima Univ, Dept Phys, Kagamiyama 1-3-1, Higashihiroshima, Hiroshima 7398526, Japan; Hiroshima Univ, Core Res Energet Universe CORE U, Kagamiyama 1-3-1, Higashihiroshima, Hiroshima 7398526, Japan; CSIC, Inst Ciencies Espai ICE, Can Magrans S-N, E-08193 Barcelona, Spain; ICREA, Pg Lluis Co 23, Barcelona, Spain; Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain; Natl Inst Nat Sci, Nobeyama Radio Observ, Natl Astron Observ Japan, Minamisa Ku, Minamimaki, Nagano 3841305, Japan; Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan; McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada; Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada; Chinese Univ Hong Kong, Dept Phys, Shatin, Hong Kong, Peoples R China; Chalmers Univ Technol, Dept Space Earth & Environm, SE-41296 Gothenburg, Sweden; Kyung Hee Univ, Sch Space Res, 1732 Deogyeong Daero, Yongin 17104, Gyeonggi Do, South Korea; Kagawa Univ, Fac Educ, Saiwai Cho 1-1, Takamatsu, Kagawa 7608522, Japan; Kagawa Univ, Ctr Educ Dev & Support, Saiwai Cho 1-1, Takamatsu, Kagawa 7608522, Japan; Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan; SOKENDAI Grad Univ Adv Studies, Hayama, Kanagawa 2400193, Japan; Kagoshima Univ, Grad Sch Sci & Engn, Dept Phys & Astron, 1-21-35 Korimoto, Kagoshima, Kagoshima 8900065, Japan; Grad Univ Sci & Technol, Vietnam Acad Sci & Technol, 18 Hoang Quoc Viet, Hanoi, Vietnam; Chinese Acad Sci, Natl Astron Observ, CAS Key Lab FAST, Beijing, Peoples R China; Gemini Observ NSFs NOIRLab, 670 N Aohoku Pl,Univ Pk, Hilo, HI 96720 USA; Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England; Univ Cambridge, Kavli Inst Cosmol, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England; Univ Tsukuba, Fac Pure & Appl Sci, 1-1-1 Tennodai, Tsukuba, Ibaraki 3058577, Japan; Kwansei Gakuin Univ, Sch Sci & Technol, Dept Phys, 2-1 Gakuen, Sanda, Hyogo 6691337, Japan; Univ Sci & Technol Hanoi, Vietnam Acad Sci & Technol, 18 Hoang Quoc Viet, Hanoi, Vietnam; Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China; Univ Paris Diderot, Lab AIM CEA DSM CNRS, CEA Saclay, IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France; Jet Prop Lab, M-S 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA; Univ South Wales, Pontypridd CF37 1DL, M Glam, Wales; Univ Leeds, Dept Appl Math, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England; Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France; Univ Leeds, Sch Phys & Astron, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England; Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA; Stanford Univ, Kavli Inst Particle Astrophys & Cosmol KIPAC, Stanford, CA 94305 USA | ; Liu, Sheng-Yuan/AAZ-4303-2020; Tang湯雅雯, Ya-Wen/AAZ-7382-2020; Li, Dalei/ABF-2406-2021; Li, Di/HLH-4146-2023; Priestley, Felix/KYP-3257-2024; Van Loo, Sven/JRX-9178-2023; Ohashi, Nagayoshi/ABA-9767-2020; Savini, Gianluca/C-1188-2009; Li, Hua-bai/AEU-0239-2022; Savini, Giorgio/F-5753-2019; Arzoumanian, Doris/JQT-3284-2023; Koch, Patrick/AAV-3373-2021; Lee, Chang/HME-1129-2023; Inutsuka, Shu-ichiro/I-7024-2014; Poidevin, Frédérick/Z-3492-2019; Rao, Ramprasad/L-2115-2017; Kemper, Francisca/AAZ-8274-2020; Shimajiri, Yoshito/B-1445-2013; Lee, Sang-Sung/AFS-2722-2022; Liu, Hong-Li/AAR-1998-2020; Kataoka, Akimasa/AAU-5038-2020; LI, DI/HLH-4146-2023; Hwang, Jihye/JXW-6363-2024; Li, Guang-Xing/AAC-9285-2022; Kim, Shinyoung/JEO-8879-2023; Han, Ilseung/MBG-4273-2025; Gu, Qilao/LTZ-1282-2024; WANG, Qiuhong/L-9577-2016; Tomisaka, Kohji/E-6508-2013; 顏士韋, Hsi-Wei/C-8307-2011; Doi, Yasuo/A-3395-2013; , Le Ngoc Tram/AAH-2951-2019; Nanayakkara, Themiya/AAT-6271-2020; NGOC, NGUYEN/JQJ-4239-2023; Lee, Chin-Fei/AAZ-3391-2020; Tsukamoto, Yusuke/AAU-3453-2020; Liu, Junhao/AAQ-3071-2021; ONAKA, TAKASHI/G-5058-2014; Chakali, Eswaraiah/L-5146-2018; Lee, Jeong-Eun/E-2387-2013; Yuan, Jinghua/W-4699-2017; Soam, Archana/AAG-4250-2021; chen, zhiwei/AAP-5465-2020 | 56342326600; 36976168000; 7405326474; 55472994100; 7402935899; 8355600600; 56512202800; 7005566228; 7004002583; 57215516631; 7202929125; 59684797600; 16549809400; 7404174499; 15822192800; 7005805931; 8318213100; 57194606597; 34770134800; 57202952564; 55757586800; 6508022172; 57194603379; 57211397912; 36237885400; 7006011851; 6603570734; 6506192691; 55727743600; 56568251300; 57202847250; 56436978700; 57203067199; 56252021400; 7403258846; 55705656800; 55320822200; 55633098300; 35499669400; 57203026080; 56566873100; 12790268500; 35242015200; 7403536449; 57218669464; 57944161700; 55231989000; 7005084542; 57206389610; 35321993600; 24170690100; 7401662157; 57217586664; 55210722100; 55170000100; 55874635700; 6602882601; 22834355900; 55673595500; 7005672565; 8547622700; 9234005200; 7003509373; 22834101100; 7101632548; 7403310385; 57194592820; 57194798843; 7404169517; 35237077900; 7103332462; 55226383000; 35377433200; 24074312000; 35330159300; 36238131700; 57201082771; 25627568300; 57219237963; 55750138400; 7201640315; 7005283695; 7601365384; 55671720700; 57194595458; 57944655500; 7409321582; 36571804600; 35773361100; 57189663358; 56455301400; 55370384000; 57194605392; 57209260420; 37056945900; 57190230987; 35748985900; 35330124000; 57209285153; 55910516500; 35185338100; 57216330092; 7409459358; 56179884700; 55750223500; 7402157762; 35569334500; 7003401658; 13310130800; 7201941871; 36714093500; 57216925030; 7202558313; 18936782900; 35096693300; 16070455300; 57194941451; 6602816367; 38862759600; 7403068909; 7004265198; 7101942174; 57194586988; 7006586973; 56800212700; 35238413800; 7407452361; 15844178300; 6604032293; 23061889500; 35482578500; 27868095600; 6701467496; 57201731842; 36971326200; 7003564783; 56084174100; 57352212300; 57219690533; 57945146700; 43361931100; 55441261000; 55170380200; 57209281402; 57199325064; 49865000200; 57207478624; 56493265600; 56183368700; 36955785700; 36238023800; 59821849300; 35308644100; 7004237751; 7004415016; 36908360800; 14042952700 | chingtaochung@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 941 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 1.09 | 2025-06-25 | 15 | 13 | FAR-INFRARED POLARIMETRY; STAR-FORMING REGIONS; GOULD BELT SURVEY; MU-M POLARIZATION; MOLECULAR CLOUD; SUBMILLIMETER POLARIZATION; DUST EMISSION; SCUBA-2; HERSCHEL; GAS | English | 2022 | 2022-12-20 | 10.3847/1538-4357/ac9dfb | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | The Lick AGN Monitoring Project 2016: Dynamical Modeling of Velocity-resolved Hβ Lags in Luminous Seyfert Galaxies | We have modeled the velocity-resolved reverberation response of the H beta broad emission line in nine Seyfert 1 galaxies from the Lick Active Galactic Nucleus (AGN) Monitoring Project 2016 sample, drawing inferences on the geometry and structure of the low-ionization broad-line region (BLR) and the mass of the central supermassive black hole. Overall, we find that the H beta BLR is generally a thick disk viewed at low to moderate inclination angles. We combine our sample with prior studies and investigate line-profile shape dependence, such as log(10) (FWHM/sigma), on BLR structure and kinematics and search for any BLR luminosity-dependent trends. We find marginal evidence for an anticorrelation between the profile shape of the broad H beta emission line and the Eddington ratio, when using the rms spectrum. However, we do not find any luminosity-dependent trends, and conclude that AGNs have diverse BLR structure and kinematics, consistent with the hypothesis of transient AGN/BLR conditions rather than systematic trends. | Villafana, Lizvette; Williams, Peter R.; Treu, Tommaso; Brewer, Brendon J.; Barth, Aaron J.; Vivian, U.; Bennert, Vardha N.; Vogler, H. Alexander; Guo, Hengxiao; Bentz, Misty C.; Canalizo, Gabriela; Filippenko, Alexei, V; Gates, Elinor; Hamann, Frederick; Joner, Michael D.; Malkan, Matthew A.; Woo, Jong-Hak; Abolfathi, Bela; Abramson, L. E.; Armen, Stephen F.; Bae, Hyun-Jin; Bohn, Thomas; Boizelle, Benjamin D.; Bostroem, K. Azalee; Brandel, Andrew; Brink, Thomas G.; Channa, Sanyum; Cooper, M. C.; Cosens, Maren; Donohue, Edward; Fillingham, Sean P.; Gonzalez-Buitrago, Diego; Halevi, Goni; Halle, Andrew; Hood, Carol E.; Horne, Keith; Horst, J. Chuck; de Kouchkovsky, Maxime; Kuhn, Benjamin; Kumar, Sahana; Leonard, Douglas C.; Loveland, Donald; Manzano-King, Christina; McHardy, Ian; Michel, Raul; Olaes, Melanie Kae B.; Park, Daeseong; Park, Songyoun; Pei, Liuyi; Ross, Timothy W.; Runco, Jordan N.; Sanchez, Javier; Scott, Bryan; Sexton, Remington O.; Shin, Jaejin; Shivvers, Isaac; Spencer, Chance L.; Stahl, Benjamin E.; Stegman, Samantha; Stomberg, Isak; Valenti, Stefano; Walsh, Jonelle L.; Yuk, Heechan; Zheng, WeiKang | Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA; Univ Auckland, Dept Stat, Private Bag 92019, Auckland 1142, New Zealand; Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA; Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA; Calif Polytech State Univ San Luis Obispo, Phys Dept, San Luis Obispo, CA 93407 USA; Univ Calif Davis, Dept Phys & Astron, 1 Shields Ave, Davis, CA 95616 USA; Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA; Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA; Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA; Lick Observ, POB 85, Mt Hamilton, CA 95140 USA; Brigham Young Univ, Dept Phys & Astron, N283 ESC, Provo, UT 84602 USA; Seoul Natl Univ, Dept Phys & Astron, 1 Gwanak Ro, Seoul 08826, South Korea; Seoul Natl Univ, SNU Astron Res Ctr, 1 Gwanak Ro, Seoul 08826, South Korea; Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA; San Diego State Univ, Dept Astron, San Diego, CA 92182 USA; Univ Washington, DiRAC Inst, Dept Astron, 3910 15th Ave, Seattle, WA 98195 USA; Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA; Stanford Univ, Dept Phys, Stanford, CA 94305 USA; Univ Calif San Diego, Phys Dept, 9500 Gilman Dr, La Jolla, CA 92093 USA; Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA; Booz Allen, 1615 Murray Canyon Rd,Suite 8000, San Diego, CA 92108 USA; Univ Nacl Autonoma Mexico, Inst Astron, AP 106, Ensenada 22860, Baja California, Mexico; Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA; Calif State Univ San Bernardino, Dept Phys, 5500 Univ Pkwy, San Bernardino, CA 92407 USA; Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland; Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA; Florida State Univ, Dept Phys, 77 Chieftan Way, Tallahassee, FL 32306 USA; Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA; Univ Southampton, Southampton SO17 1BJ, Hants, England; Univ Nacl Autonoma Mexico, Inst Astron, AP 877, Ensenada 22830, Baja California, Mexico; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Korea Astron & Space Sci Inst, Daejeon 34055, South Korea; Fermilab Natl Accelerator Lab, Kirk Rd & Pine St, Batavia, IL 60510 USA; Kavli Inst Cosmol Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA; US Naval Observ, 3450 Massachusetts Ave NW, Washington, DC 20392 USA; George Mason Univ, Dept Phys & Astron, 4400 Univ Dr, Fairfax, VA 22030 USA; Calif State Univ Fresno, Dept Phys, Fresno, CA 93740 USA; Univ Wisconsin, Dept Chem, Madison, WI 53706 USA; Deutsch Elektronen Synchrotron DESY, D-22607 Hamburg, Germany; Texas A&M Univ, Dept Phys & Astron, George P & Cynthia W Mitchell Inst Fundamental Ph, 4242 TAMU, College Stn, TX 77843 USA; Univ Oklahoma, Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA | Hall, Andrew/H-8691-2015; Woo, Jong-Hak/A-2790-2014; Treu, Tommaso/KYP-7127-2024; Malkan, Matthew/IWM-5356-2023; Micheli, Marco/H-7598-2015; Bae, Hyun-Jin/J-8037-2015; Kumar, Sahana/GRO-5526-2022; Sanchez, Javier/AAA-4861-2021; Halevi, Goni/AAZ-1254-2021; U, Vivian/J-5875-2019; Abramson, Louis/MFK-3176-2025; Zheng, Weikang/KXS-0844-2024 | 57214806376; 57218765930; 7003853565; 12241991700; 36088948300; 45361575500; 35222917400; 57610112600; 56330144400; 7007172911; 6601959161; 34568722000; 35476049700; 36477308800; 6603675694; 7006872661; 7401751171; 57194339171; 55370614700; 57172805700; 51563162500; 58440395400; 55370470600; 55542785100; 57194343654; 35736928000; 57200333385; 57210936254; 56925363000; 57204023575; 57189894863; 55535507600; 57194328633; 57217512479; 55976168000; 55172662700; 57610112700; 57205630514; 57365614700; 57211412703; 7201953982; 58830614400; 57194324078; 7004698784; 55993707500; 57694552100; 15127668500; 59081802400; 55340311200; 57201527090; 57188816803; 57204811576; 56707598000; 57206494431; 55554622900; 44561605900; 57219785009; 57194328745; 57205624999; 57222113678; 7005589908; 57210948381; 57191892016; 7403566199 | lvillafana@astro.ucla.edu; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 930 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 2.1 | 2025-06-25 | 29 | 25 | BROAD-LINE REGION; BLACK-HOLE MASSES; ACTIVE GALACTIC NUCLEI; SPACE TELESCOPE; SPECTROSCOPIC CAMPAIGN; ARP 151; REVERBERATION; ACCRETION | English | 2022 | 2022-05-01 | 10.3847/1538-4357/ac6171 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | The Lick AGN Monitoring Project 2016: Velocity-resolved Hβ Lags in Luminous Seyfert Galaxies | We carried out spectroscopic monitoring of 21 low-redshift Seyfert 1 galaxies using the Kast double spectrograph on the 3 m Shane telescope at Lick Observatory from 2016 April to 2017 May. Targeting active galactic nuclei (AGNs) with luminosities of lambda L ( lambda )(5100 angstrom) approximate to 10(44) erg s(-1) and predicted H beta lags of similar to 20-30 days or black hole masses of 10(7)-10(8.5) M (circle dot), our campaign probes luminosity-dependent trends in broad-line region (BLR) structure and dynamics as well as to improve calibrations for single-epoch estimates of quasar black hole masses. Here we present the first results from the campaign, including H beta emission-line light curves, integrated H beta lag times (8-30 days) measured against V-band continuum light curves, velocity-resolved reverberation lags, line widths of the broad H beta components, and virial black hole mass estimates (10(7.1)-10(8.1) M (circle dot)). Our results add significantly to the number of existing velocity-resolved lag measurements and reveal a diversity of BLR gas kinematics at moderately high AGN luminosities. AGN continuum luminosity appears not to be correlated with the type of kinematics that its BLR gas may exhibit. Follow-up direct modeling of this data set will elucidate the detailed kinematics and provide robust dynamical black hole masses for several objects in this sample. | Vivian, U.; Barth, Aaron J.; Vogler, H. Alexander; Guo, Hengxiao; Treu, Tommaso; Bennert, Vardha N.; Canalizo, Gabriela; Filippenko, Alexei, V; Gates, Elinor; Hamann, Frederick; Joner, Michael D.; Malkan, Matthew A.; Pancoast, Anna; Williams, Peter R.; Woo, Jong-Hak; Abolfathi, Bela; Abramson, L. E.; Armen, Stephen F.; Bae, Hyun-Jin; Bohn, Thomas; Boizelle, Benjamin D.; Bostroem, Azalee; Brandel, Andrew; Brink, Thomas G.; Channa, Sanyum; Cooper, M. C.; Cosens, Maren; Donohue, Edward; Fillingham, Sean P.; Gonzalez-Buitrago, Diego; Halevi, Goni; Halle, Andrew; Hood, Carol E.; Horne, Keith; Horst, J. Chuck; de Kouchkovsky, Maxime; Kuhn, Benjamin; Kumar, Sahana; Leonard, Douglas C.; Loveland, Donald; Manzano-King, Christina; McHardy, Ian; Michel, Raul; Olaes, Melanie Kae B.; Park, Daeseong; Park, Songyoun; Pei, Liuyi; Ross, Timothy W.; Runco, Jordan N.; Samuel, Jenna; Sanchez, Javier; Scott, Bryan; Sexton, Remington O.; Shin, Jaejin; Shivvers, Isaac; Spencer, Chance L.; Stahl, Benjamin E.; Stegman, Samantha; Stomberg, Isak; Valenti, Stefano; Villafana, L.; Walsh, Jonelle L.; Yuk, Heechan; Zheng, Weikang | Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA; Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA; Univ Calif Davis, Dept Phys & Astron, 1 Shields Ave, Davis, CA 95616 USA; Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA; Calif Polytech State Univ San Luis Obispo, Phys Dept, San Luis Obispo, CA 93407 USA; Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA; Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA; Lick Observ, POB 85, Mt Hamilton, CA 95140 USA; Brigham Young Univ, Dept Phys & Astron, N283 ESC, Provo, UT 84602 USA; Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA; Seoul Natl Univ, Dept Phys & Astron, Astron Rogram, 1 Gwanak Ro, Seoul 08826, South Korea; Seoul Natl Univ, SNU Astron Res Ctr, 1 Gwanak Ro, Seoul 08826, South Korea; Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA; San Diego State Univ, Dept Astron, San Diego, CA 92182 USA; Univ Washington, DiRAC Inst, Dept Astron, 3910 15th Ave NE, Seattle, WA 98195 USA; Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA; Stanford Univ, Dept Phys, Stanford, CA 94305 USA; Univ Calif San Diego, Phys Dept, 9500 Gilman Dr, La Jolla, CA 92093 USA; Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA; Booz Allen, 1615 Murray Canyon Rd,Suite 8000, San Diego, CA 92108 USA; Univ Nacl Autonoma Mexico, Inst Astron, AP 106, Ensenada 22860, Baja California, Mexico; Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA; Calif State Univ San Bernardino, Dept Phys, 5500 Univ Pkwy, San Bernardino, CA 92407 USA; Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland; Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA; Florida State Univ, Dept Phys, 77 Chieftan Way, Tallahassee, FL 32306 USA; Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA; Univ Southampton, Southampton SO17 1BJ, Hants, England; Univ Nacl Autonoma Mexico, Inst Astron, AP 877, Ensenada 22830, Baja California, Mexico; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Korea Astron & Space Sci Inst, Daejeon 34055, South Korea; Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA; Fermilab Natl Accelerator Lab, Kirk Rd & Pine St, Batavia, IL 60510 USA; Kavli Inst Cosmol Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA; US Naval Observ, 3450 Massachusetts Ave NW, Washington, DC 20392 USA; George Mason Univ, Dept Phys & Astron, 4400 Univ Dr, Fairfax, VA 22030 USA; Calif State Univ Fresno, Dept Phys, Fresno, CA 93740 USA; Univ Wisconsin, Dept Chem, Madison, WI 53706 USA; Deutsch Elektronen Synchrotron DESY, D-22607 Hamburg, Germany; Texas A&M Univ, Dept Phys & Astron, George P & Cynthia W Mitchell Inst Fundamental Ph, 4242 TAMU, College Stn, TX 77843 USA; Univ Oklahoma, Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA | Abramson, Louis/MFK-3176-2025; Halevi, Goni/AAZ-1254-2021; Sanchez, Javier/AAA-4861-2021; Bae, Hyun-Jin/J-8037-2015; Kumar, Sahana/GRO-5526-2022; Malkan, Matthew/IWM-5356-2023; Hall, Andrew/H-8691-2015; Zheng, Weikang/KXS-0844-2024; Micheli, Marco/H-7598-2015; U, Vivian/J-5875-2019; Treu, Tommaso/KYP-7127-2024; Woo, Jong-Hak/A-2790-2014 | 45361575500; 36088948300; 57194190175; 56330144400; 7003853565; 35222917400; 6601959161; 34568722000; 35476049700; 36477308800; 6603675694; 7006872661; 36624101000; 57218765930; 7401751171; 57194339171; 55370614700; 57172805700; 51563162500; 58440395400; 55370470600; 54388603500; 57194343654; 35736928000; 57200333385; 57210936254; 56925363000; 57204023575; 57189894863; 55535507600; 57194328633; 57217512479; 55976168000; 55172662700; 55958121600; 57219640485; 57365614700; 57211412703; 7201953982; 58830614400; 57194324078; 7004698784; 55993707500; 57191190050; 15127668500; 59081802400; 55340311200; 57201527090; 57188816803; 57211888976; 57204811576; 56707598000; 57206494431; 55554622900; 44561605900; 57219785009; 57194328745; 57205624999; 57222113678; 7005589908; 57214806376; 57210948381; 57191892016; 7403566199 | vivianu@uci.edu; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 925 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 2.77 | 2025-06-25 | 12 | 34 | ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; BROAD-LINE REGION; REVERBERATION MAPPING DATA; HIGH ACCRETION; VARIABILITY; EMISSION; QUASARS; TELESCOPE; SAMPLE | English | 2022 | 2022-01-01 | 10.3847/1538-4357/ac3d26 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | The Paschen Jump as a Diagnostic of the Diffuse Nebular Continuum Emission in Active Galactic Nuclei* | Photoionization modeling of active galactic nuclei (AGN) predicts that diffuse continuum (DC) emission from the broad-line region makes a substantial contribution to the total continuum emission from ultraviolet through near-infrared wavelengths. Evidence for this DC component is present in the strong Balmer jump feature in AGN spectra, and possibly from reverberation measurements that find longer lags than expected from disk emission alone. However, the Balmer jump region contains numerous blended emission features, making it difficult to isolate the DC emission strength. In contrast, the Paschen jump region near 8200 angstrom is relatively uncontaminated by other strong emission features. Here, we examine whether the Paschen jump can aid in constraining the DC contribution, using Hubble Space Telescope Space Telescope Imaging Spectrograph spectra of six nearby Seyfert 1 nuclei. The spectra appear smooth across the Paschen edge, and we find no evidence of a Paschen spectral break or jump in total flux. We fit multicomponent spectral models over the range 6800-9700 angstrom and find that the spectra can still be compatible with a significant DC contribution if the DC Paschen jump is offset by an opposite spectral break resulting from blended high-order Paschen emission lines. The fits imply DC contributions ranging from similar to 10% to 50% at 8000 angstrom, but the fitting results are highly dependent on assumptions made about other model components. These degeneracies can potentially be alleviated by carrying out fits over a broader wavelength range, provided that models can accurately represent the disk continuum shape, Fe ii emission, high-order Balmer line emission, and other components. | Guo, Hengxiao; Barth, Aaron J.; Korista, Kirk T.; Goad, Michael R.; Cackett, Edward M.; Bentz, Misty C.; Brandt, William N.; Gonzalez-Buitrago, D.; Ferland, Gary J.; Gelbord, Jonathan M.; Ho, Luis C.; Horne, Keith; Joner, Michael D.; Kriss, Gerard A.; McHardy, Ian; Mehdipour, Missagh; Park, Daeseong; Remigio, Raymond; Vivian, U.; Vestergaard, Marianne | Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA; Western Michigan Univ, Dept Phys, 1120 Everett Tower, Kalamazoo, MI 49008 USA; Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England; Wayne State Univ, Dept Phys & Astron, 666 W Hancock St, Detroit, MI 48201 USA; Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA; Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA; Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA; Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA; Univ Nacl Autonoma Mexico, Inst Astron, AP 106, Ensenada 22860, Baja California, Mexico; Univ Kentucky, Phys, Lexington, KY 40506 USA; Spectral Sci Inc, 4 Fourth Ave, Burlington, MA 01803 USA; Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China; Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China; Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland; Brigham Young Univ, Dept Phys & Astron, N283 ESC, Provo, UT 84602 USA; Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA; Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Univ Copenhagen, Niels Bohr Inst, DARK, Jagtvej 155, DK-2200 Copenhagen N, Denmark; Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA; Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA | Ferland, Gary/AFO-6311-2022; Micheli, Marco/H-7598-2015; Vestergaard, Marianne/M-5247-2014; U, Vivian/J-5875-2019; Brandt, William/N-2844-2015 | 56330144400; 36088948300; 57195693154; 10241897600; 8302847800; 7007172911; 35247682800; 55535507600; 35503330500; 6506351764; 57225302746; 55172662700; 6603675694; 7006072785; 7004698784; 36089155500; 15127668500; 57239077400; 45361575500; 43361722900 | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 927 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 0.92 | 2025-06-25 | 11 | 11 | LAG-LUMINOSITY RELATIONSHIP; ACCRETION-DISK; SPACE TELESCOPE; BROAD EMISSION; SEYFERT 1; FE-II; H-I; QUASARS; SPECTRA; GALAXY | English | 2022 | 2022-03-01 | 10.3847/1538-4357/ac4bc6 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||||
| ○ | ○ | Article | The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion | Understanding the faint end of quasar luminosity function (LF) at a high redshift is important since the number density of faint quasars is a critical element in constraining ultraviolet (UV) photon budgets for ionizing the intergalactic medium (IGM) in the early universe. Here, we present quasar LF reaching M-1450 similar to -22.0 AB mag at z similar to 5, about 1 mag deeper than previous UV LFs. We select quasars at z similar to 5 with a deep learning technique from deep data taken by the Hyper Suprime-Cam Subaru Strategic Program, covering a 15.5 deg(2) area. Beyond the traditional color selection method, we improved the quasar selection by training an artificial neural network to distinguish z similar to 5 quasars from nonquasar sources based on their colors and adopting the Bayesian information criterion that can further remove high-redshift galaxies from the quasar sample. When applied to a small sample of spectroscopically identified quasars and galaxies, our method is successful in selecting quasars at similar to 83% efficiency (5/6) while minimizing the contamination rate of high-redshift galaxies (1/8) by up to three times compared to the selection using color selection alone (3/8). The number of our final quasar candidates with M (1450) < -22.0 mag is 35. Our quasar UV LF down to M-1450 = -22 mag or even fainter (M-1450 = -21 mag) suggests a rather low number density of faint quasars and the faint-end slope of -1.6(-0.19)(+0.21) favoring a scenario where quasars play a minor role in ionizing the IGM at high redshift. | Shin, Suhyun; Im, Myungshin; Kim, Yongjung | Seoul Natl Univ, SNU Astron Res Ctr SNUARC, Dept Phys & Astron, Astron Program, 1 Gwanak Ro, Seoul 08826, South Korea; Kyungpook Natl Univ, Coll Nat Sci, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China | Im, Myungshin/B-3436-2013; , Yong Jung Kim/JRW-0681-2023 | 57205483501; 7004267711; 59622148200 | suhyun.shin.s2@gmail.com;myungshin.im@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 937 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 0.34 | 2025-06-25 | 3 | 4 | DIGITAL-SKY-SURVEY; PHOTOMETRIC SELECTION; AGN CONTRIBUTION; FAINT QUASARS; GALAXIES; REIONIZATION; DISCOVERY; EVOLUTION; MODEL; BAND | English | 2022 | 2022-09-01 | 10.3847/1538-4357/ac854b | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Unexpected Dancing Partners: Tracing the Coherence between the Spin and Motion of Dark Matter Halos | A recent study conducted using CALIFA survey data has found that the orbital motions of neighbor galaxies are coherent with the spin direction of a target galaxy on scales of many megaparsecs. We study this so-called "large-scale coherence" phenomenon using N-body cosmological simulations. We confirm a strong coherence signal within 1 Mpc h (-1) of a target galaxy, reaching out to 6 Mpc h (-1). We divide the simulation halos into subsamples based on mass, spin, merger history, and local halo number density for both target and neighbor halos. We find a clear dependency on the mass of the target halo only. Another key parameter is the local number density of both target and neighbor halos, with high-density regions such as clusters and groups providing the strongest coherence signals, rather than filaments or lower-density regions. However we do not find a clear dependency on halo spin or time since last major merger. The most striking result we find is that the signal can be detected up to 15 Mpc h (-1) from massive halos. These results provide valuable lessons on how observational studies could more clearly detect coherence, and we discuss the implications of our results for the origins of large-scale coherence. | Kim, Yigon; Smith, Rory; Shin, Jihye | Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu, South Korea; Univ Tecn Federico Santa Maria, Dept Fis, Ave Vicuna Mackenna 3939, Santiago, Chile; Korea Astron & Space Sci Inst KASI, 776 Daedeokdae Ro, Daejeon 34055, South Korea | Smith, Rory/AAU-8567-2021 | 57376307100; 56497254800; 55670670700 | yigon@outlook.com;rorysmith274@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 935 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 0.59 | 2025-06-25 | 7 | 7 | LARGE-SCALE STRUCTURE; SDSS-IV MANGA; ANGULAR-MOMENTUM; COSMIC WEB; ATLAS(3D) PROJECT; GALAXY ROTATION; SAURON PROJECT; STELLAR; ALIGNMENT; MASS | English | 2022 | 2022-08-01 | 10.3847/1538-4357/ac7e45 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Unraveling the Innermost Jet Structure of OJ 287 with the First GMVA plus ALMA Observations | We present the first very long baseline interferometric (VLBI) observations of the blazar OJ 287 carried out jointly with the Global Millimeter VLBI Array (GMVA) and the phased Atacama Large Millimeter/submillimeter Array (ALMA) at 3.5 mm on 2017 April 2. The participation of phased ALMA has not only improved the GMVA north-south resolution by a factor of similar to 3, but has also enabled fringe detections with signal-to-noise ratios up to 300 at baselines longer than 2 G lambda. The high sensitivity has motivated us to image the data with newly developed regularized maximum likelihood imaging methods, revealing the innermost jet structure with unprecedentedly high angular resolution. Our images reveal a compact and twisted jet extending along the northwest direction, with two bends within the inner 200 mu as, resembling a precessing jet in projection. The component at the southeastern end shows a compact morphology and high brightness temperature, and is identified as the VLBI core. An extended jet feature that lies at similar to 200 mu as northwest of the core shows a conical shape, in both total and linearly polarized intensity, and a bimodal distribution of the linear polarization electric vector position angle. We discuss the nature of this feature by comparing our observations with models and simulations of oblique and recollimation shocks with various magnetic field configurations. Our high-fidelity images also enabled us to search for possible jet features from the secondary supermassive black hole (SMBH) and test the SMBH binary hypothesis proposed for this source. | Zhao, Guang-Yao; Gomez, Jose L.; Fuentes, Antonio; Krichbaum, Thomas P.; Traianou, Efthalia; Lico, Rocco; Cho, Ilje; Ros, Eduardo; Komossa, S.; Akiyama, Kazunori; Asada, Keiichi; Blackburn, Lindy; Britzen, Silke; Bruni, Gabriele; Crew, Geoffrey B.; Dahale, Rohan; Dey, Lankeswar; Gold, Roman; Gopakumar, Achamveedu; Issaoun, Sara; Janssen, Michael; Jorstad, Svetlana; Kim, Jae-Young; Koay, Jun Yi; Kovalev, Yuri Y.; Koyama, Shoko; Lobanov, Andrei P.; Loinard, Laurent; Lu, Ru-Sen; Markoff, Sera; Marscher, Alan P.; Marti-Vidal, Ivan; Mizuno, Yosuke; Park, Jongho; Savolainen, Tuomas; Toscano, Teresa | CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain; Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany; INAF Ist Radioastron, Via P Gobetti 101, I-40129 Bologna, Italy; MIT, Haystack Observ, 99 Millstone Rd, Westford, MA 01886 USA; Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan; Harvard Univ, Black Hole Initiat, 20 Garden St, Cambridge, MA 02138 USA; Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan; Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA; INAF Ist Astrofis & Planetol Spaziali, Via Fosso del Cavaliere 100, I-00133 Rome, Italy; Indian Inst Sci Educ & Res Kolkata, Nadia 741246, W Bengal, India; Tata Inst Fundamental Res, Dept Astron & Astrophys, Mumbai 400005, Maharashtra, India; Univ Southern Denmark, CP3 Origins, Campusvej 55, DK-5230 Odense M, Denmark; Radboud Univ Nijmegen, Dept Astrophys, Inst Math Astrophys & Particle Phys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands; Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA; St Petersburg Univ, Astron Inst, Univ Skij Pr 28, St Petersburg 198504, Russia; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 702701, South Korea; Korea Astron & Space Sci Inst, Daedeok Daero 776, Daejeon 34055, South Korea; Russian Acad Sci, Lebedev Phys Inst, Leninsky Prospekt 53, Moscow 119991, Russia; Moscow Inst Phys & Technol, Inst Sky 9, Dolgoprudnyi 141700, Moscow Region, Russia; Niigata Univ, Nishi Ku, 8050 Ikarashi Nino Cho, Niigata 9502181, Japan; Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico; Univ Nacl Autonoma Mexico, Inst Astron, Cdmx 04510, Mexico; Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China; Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210008, Peoples R China; Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands; Univ Amsterdam, Gravitat & Astroparticle Phys Amsterdam GRAPPA In, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands; Univ Valencia, Dept Astron & Astrofis, C Dr Moliner 50, E-46100 Valencia, Spain; Univ Valencia, Observ Astron, C Catedrat Jose Beltran 2, E-46980 Valencia, Spain; Shanghai Jiao Tong Univ, Tsung Dao Lee Inst, Shengrong Rd 520, Shanghai 201210, Peoples R China; Shanghai Jiao Tong Univ, Sch Phys & Astron, 800 Dongchuan Rd, Shanghai 200240, Peoples R China; Goethe Univ Frankfurt, Inst Theoret Phys, Max von Laue Str 1, D-60438 Frankfurt, Germany; Aalto Univ, Dept Elect & Nanoengn, PL 15500, FI-00076 Aalto, Finland; Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, FI-02540 Kylmala, Finland | Loinard, Laurent/MCX-8116-2025; Koay, Jun/E-4952-2015; Fuentes, Antonio/R-3900-2019; Toscano Domingo, Teresa/ITV-2430-2023; Gómez, José/C-4195-2008; Gomez, Jose L./C-4195-2008; Bruni, Gabriele/ABB-2523-2021; Lico, Rocco/L-8308-2019; Kovalev, Yuri/J-5671-2013; Park, Jongho/JFB-2747-2023; Asada, Keiichi/ABC-2456-2020; Cho, Ilje/LSL-5339-2024; Ros, Eduardo/B-1014-2015; Kim, Jae-Young/IUO-6466-2023; Jorstad, Svetlana/AAM-3279-2021; Toscano, Teresa/ITV-2430-2023; 浅田圭一, Keiichi/ABC-2456-2020; Zhao, Guang-Yao/AAA-7324-2019; Gold, Roman/AAX-5851-2021; Lobanov, Andrei/G-5891-2014 | 55478882500; 7402094981; 56699569900; 7004015011; 57204824800; 55363924100; 57203071154; 7102531000; 7003307661; 55669706400; 7102181737; 35271380400; 6602806448; 56950092500; 6701566715; 57274820700; 57198515081; 55504461000; 6602906830; 57190760991; 57213908458; 59785012300; 57211836467; 16203179600; 7004589011; 55441260500; 7101957568; 6603796954; 55328189400; 6701324987; 7004154914; 12040474800; 15070911300; 56953647500; 7003371610; 57702184700 | gyzhao@iaa.es; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 932 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2022 | 4.9 | 22.5 | 1.84 | 2025-06-25 | 22 | 22 | SIMULTANEOUS MULTIFREQUENCY OBSERVATIONS; RADIO FLARE; LINEAR-POLARIZATION; MAGNETIC-FIELDS; BL-LACERTAE; LIGHT-CURVE; AGN JETS; MM-VLBI; X-RAY; BINARY | English | 2022 | 2022-06-01 | 10.3847/1538-4357/ac6b9c | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Editorial Material | Editorial for "Clinical Application of Non-Contrast-Enhanced Dixon Water-Fat Separation Compressed SENSE Whole-Heart Coronary MR Angiography at 3.0 T With and Without Nitroglycerin" | Kang, Eun-Ju; Lee, Jongmin | Dong A Univ, Med Ctr, Radiol, Busan, South Korea; Kyungpook Natl Univ, Sch Med, Dept Radiol, Dong Duk Ro 130, Daegu 41944, South Korea | Lee, Jongmin/AAR-6361-2020; Kang, Eun-Ju/N-7376-2015 | 8395421600; 55689919700 | jonglee@knu.ac.kr; | JOURNAL OF MAGNETIC RESONANCE IMAGING | J MAGN RESON IMAGING | 1053-1807 | 1522-2586 | 55 | 2 | SCIE | RADIOLOGY, NUCLEAR MEDICINE & MEDICAL IMAGING | 2022 | 4.4 | 22.6 | 0 | 2025-06-25 | 1 | 0 | Contrast Media; Coronary Angiography; Humans; Image Enhancement; Magnetic Resonance Angiography; Magnetic Resonance Imaging; Nitroglycerin; Water; glyceryl trinitrate; contrast medium; water; artery diameter; artery wall; clinical protocol; computed tomographic angiography; coronary angiography; coronary artery; coronary artery dilatation; coronary artery disease; coronary artery spasm; coronary computed tomography angiography; diagnostic accuracy; Editorial; human; image reconstruction; magnetic resonance angiography; non contrast enhanced Dixon water fat separation coronary MR angiography; coronary angiography; image enhancement; magnetic resonance angiography; nuclear magnetic resonance imaging | English | 2022 | 2022-02 | 10.1002/jmri.27869 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||||
| ○ | ○ | Article | Enantioselective Henry reaction catalysed by Chiral-copper(II) Complexes: Chirality effect derived from ligand backbone and Side-chain | Copper(II) complexes based on two diastereopure camphor-derived iminomethylpyridine ligands were resolved and structurally characterised by single-crystal X-ray diffraction. Each chiral Cu(II) complex was an efficient catalyst for theenantioselective Henry reaction of phenyl propionaldehyde and nitromethane, affording 1-nitro-4-phenylbutan-2-ol in high yields (up to 99%) and excellent enantioselectivities (up to 99%) that were governed by the combined chirality effect of the ligand backbone and side-chain. | Cho, Juhyun; Nayab, Saira; Lee, Jungkyu K.; Jeong, Jong Hwa; Lee, Hyosun | Kyungpook Natl Univ, Green Nano Mat Res Ctr, 80 Daehakro, Daegu 41566, South Korea; Kyungpook Natl Univ, Dept Chem, 80 Daehakro, Daegu 41566, South Korea; Shaheed Benazir Bhutto Univ, Dept Chem, Peshawar 18000, Khyber Pakhtunk, Pakistan | ; Nayab, Saira/JBS-3013-2023 | 57198450723; 36490286400; 8312040000; 57856481500; 15750846000 | jjh@knu.ac.kr;hyosunlee@knu.ac.kr; | INORGANIC CHEMISTRY COMMUNICATIONS | INORG CHEM COMMUN | 1387-7003 | 1879-0259 | 144 | SCIE | CHEMISTRY, INORGANIC & NUCLEAR | 2022 | 3.8 | 22.6 | 0 | 2025-06-25 | 0 | 0 | Enantioselective Henry reaction; Chiral-copper(II) complex; Diastereopure; Resolution; Camphor -derived iminomethylpyridines | COPPER(II) COMPLEXES; ASYMMETRIC-SYNTHESIS; CU(II); POLYMERIZATION; DERIVATIVES; ACTIVATION; ZN(II) | Camphor-derived iminomethylpyridines; Chiral-copper(II) complex; Diastereopure; Enantioselective Henry reaction; Resolution | English | 2022 | 2022-10 | 10.1016/j.inoche.2022.109880 | 바로가기 | 바로가기 | 바로가기 | 바로가기 |
페이지 이동: