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| ○ | Article | Filamentary Network and Magnetic Field Structures Revealed with BISTRO in the High-mass Star-forming Region NGC 2264: Global Properties and Local Magnetogravitational Configurations | We report 850 mu m continuum polarization observations toward the filamentary high-mass star-forming region NGC 2264, taken as part of the B-fields In STar forming Regions Observations large program on the James Clerk Maxwell Telescope. These data reveal a well-structured nonuniform magnetic field in the NGC 2264C and 2264D regions with a prevailing orientation around 30 degrees from north to east. Field strength estimates and a virial analysis of the major clumps indicate that NGC 2264C is globally dominated by gravity, while in 2264D, magnetic, gravitational, and kinetic energies are roughly balanced. We present an analysis scheme that utilizes the locally resolved magnetic field structures, together with the locally measured gravitational vector field and the extracted filamentary network. From this, we infer statistical trends showing that this network consists of two main groups of filaments oriented approximately perpendicular to one another. Additionally, gravity shows one dominating converging direction that is roughly perpendicular to one of the filament orientations, which is suggestive of mass accretion along this direction. Beyond these statistical trends, we identify two types of filaments. The type I filament is perpendicular to the magnetic field with local gravity transitioning from parallel to perpendicular to the magnetic field from the outside to the filament ridge. The type II filament is parallel to the magnetic field and local gravity. We interpret these two types of filaments as originating from the competition between radial collapsing, driven by filament self-gravity, and longitudinal collapsing, driven by the region's global gravity. | Wang, Jia-Wei; Koch, Patrick M.; Clarke, Seamus D.; Fuller, Gary; Peretto, Nicolas; Tang, Ya-Wen; Yen, Hsi-Wei; Lai, Shih-Ping; Ohashi, Nagayoshi; Arzoumanian, Doris; Johnstone, Doug; Furuya, Ray; Inutsuka, Shu-ichiro; Lee, Chang Won; Ward-Thompson, Derek; Le Gouellec, Valentin J. M.; Liu, Hong-Li; Fanciullo, Lapo; Hwang, Jihye; Pattle, Kate; Poidevin, Frederick; Tahani, Mehrnoosh; Onaka, Takashi; Rawlings, Mark G.; Chung, Eun Jung; Liu, Junhao; Lyo, A-Ran; Priestley, Felix; Hoang, Thiem; Tamura, Motohide; Berry, David; Bastien, Pierre; Ching, Tao-Chung; Coude, Simon; Kwon, Woojin; Chen, Mike; Eswaraiah, Chakali; Soam, Archana; Hasegawa, Tetsuo; Qiu, Keping; Bourke, Tyler L.; Byun, Do-Young; Chen, Zhiwei; Chen, Huei-Ru Vivien; Chen, Wen Ping; Cho, Jungyeon; Choi, Minho; Choi, Yunhee; Choi, Youngwoo; Chrysostomou, Antonio; Dai, Sophia; Di Francesco, James; Diep, Pham Ngoc; Doi, Yasuo; Duan, Yan; Duan, Hao-Yuan; Eden, David; Fiege, Jason; Fissel, Laura M.; Franzmann, Erica; Friberg, Per; Friesen, Rachel; Gledhill, Tim; Graves, Sarah; Greaves, Jane; Griffin, Matt; Gu, Qilao; Han, Ilseung; Hayashi, Saeko; Houde, Martin; Inoue, Tsuyoshi; Iwasaki, Kazunari; Jeong, Il-Gyo; Koenyves, Vera; Kang, Ji-hyun; Kang, Miju; Karoly, Janik; Kataoka, Akimasa; Kawabata, Koji; Khan, Zacariyya; Kim, Mi-Ryang; Kim, Kee-Tae; Kim, Kyoung Hee; Kim, Shinyoung; Kim, Jongsoo; Kim, Hyosung; Kim, Gwanjeong; Kirchschlager, Florian; 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; Li, Dalei; Li, Hua-bai; Li, Guangxing; Li, Di; Lin, Sheng-Jun; Liu, Tie; Liu, Sheng-Yuan; Lu, Xing; Mairs, Steve; Matsumura, Masafumi; Matthews, Brenda; Moriarty-Schieven, Gerald; Nagata, Tetsuya; Nakamura, Fumitaka; Nakanishi, Hiroyuki; Ngoc, Nguyen Bich; Park, Geumsook; Parsons, Harriet; Pyo, Tae-Soo; Qian, Lei; Rao, Ramprasad; Rawlings, Jonathan; Retter, Brendan; Richer, John; Rigby, Andrew; Sadavoy, Sarah; Saito, Hiro; Savini, Giorgio; Seta, Masumichi; Sharma, Ekta; Shimajiri, Yoshito; Shinnaga, Hiroko; Tang, Xindi; Thuong, Hoang Duc; Tomisaka, Kohji; Tram, Le Ngoc; Tsukamoto, Yusuke; Viti, Serena; Wang, Hongchi; Whitworth, Anthony; Wu, Jintai; Xie, Jinjin; Yang, Meng-Zhe; 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 | Acad Sinica, Inst Astron & Astrophys, 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan; Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Oxford Rd, Manchester M13 9PL, Lancs, England; Univ Cologne, Phys Inst, Zulpicher Str 77, D-50937 Cologne, Germany; Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales; Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan; Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan; Natl Astron Observ Japan, Div Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan; NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada; Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada; Tokushima Univ, Inst Liberal Arts & Sci, Minami Jousanajima Machi 1-1, Tokushima 7708502, Japan; Nagoya Univ, Grad Sch Sci, Dept Phys, Furo Cho,Chikusa Ku, Nagoya, Aichi 4648602, Japan; Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea; Univ Sci & Technol, 217 Gajeong Ro, Daejeon 34113, South Korea; Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England; NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-6, Moffett Field, CA 94035 USA; Yunnan Univ, Sch Phys & Astron, Kunming 650091, Yunnan, Peoples R China; Natl Chung Hsing Univ, 145 Xingda Rd, Taichung 402, Taiwan; UCL, Dept Phys & Astron, London WC1E 6BT, England; Inst Astrofis Canarias, E-38200 Tenerife, Canary Islands, Spain; Univ La Laguna ULL, Dept Astrofis, E-38206 Tenerife, Spain; Stanford Univ, Kavli Inst Particle Astrophys & Cosmol KIPAC, Stanford, CA 94305 USA; Univ Tokyo, Grad Sch Sci, Dept Astron, 7-3-1 Hongo,Bunkyo Ku, Tokyo 1130033, Japan; Gemini Observ, NSFs NOIRLab, 670 North Aohoku Pl, Hilo, HI 96720 USA; Chungnam Natl Univ, Dept Astron & Space Sci, 99 Daehak Ro, Daejeon 34134, South Korea; East Asian Observ, 660 North Aohoku Pl,Univ Pk, Hilo, HI 96720 USA; 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; 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; Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA; Worcester State Univ, Dept Earth Environm & Phys, Worcester, MA 01602 USA; Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA; 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; Queens Univ, Dept Phys Engn Phys & Astrophys, Kingston, ON K7L 3N6, Canada; Indian Inst Sci Educ & Res IISER Tirupati, Rami Reddy Nagar,Karakambadi Rd,Mangalam PO, Tirupati 517507, Andhra Pradesh, India; Indian Inst Astrophys, II Block, Bengaluru 560034, India; 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; SKA Observ, Jodrell Bank, Macclesfield SK11 9FT, Cheshire, England; Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Peoples R China; Natl Cent Univ, Inst Astron, Zhongli 32001, Taiwan; Seoul Natl Univ, Dept Phys & Astron, 1 Gwanak Ro, Seoul 08826, South Korea; Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China; Vietnam Acad Sci & Technol, Vietnam Natl Space Ctr, 18 Hoang Quoc Viet, Hanoi, Vietnam; Univ Tokyo, Grad Sch Arts & Sci, Dept Earth Sci & Astron, 3-8-1 Komaba,Meguro Ku, Tokyo 1538902, Japan; Armagh Observ & Planetarium, Armagh BT61 9DG, North Ireland; Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada; Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA; Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England; Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China; Natl Astron Observ Japan, Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA; Univ Western Ontario, Dept Phys & Astron, 1151 Richmond St, London, ON N6A 3K7, Canada; Konan Univ, Dept Phys, Okamoto 8-9-1,Higashinada Ku, Kobe, Hyogo 6588501, Japan; Natl Astron Observ Japan, Ctr Computat Astrophys, Mitaka, Tokyo 1818588, Japan; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, 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; Kyung Hee Univ, Sch Space Res, 1732 Deogyeong Daero, Yongin 17104, Gyeonggi Do, South Korea; Ulsan Natl Inst Sci & Technol UNIST, UNIST Gil 50, Ulsan 44919, South Korea; Natl Astron Observ Japan, Natl Inst Nat Sci, Nobeyama Radio Observ, Minamisaku, Minamimaki, Nagano 3841305, Japan; Univ Ghent, Sterrenkundig Observatorium, Krijgslaan 281-S9, B-9000 Ghent, Belgium; Tohoku Univ, Astron Inst, Grad Sch Sci, 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; Ulsan Natl Inst Sci & Technol UNIST, 50 UNIST Gil, Ulsan 44919, South Korea; Seoul Natl Univ, Dept Phys & Astron, Astron Program, 1 Gwanak Ro, Seoul 08826, South Korea; Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China; Yunnan Univ, Dept Astron, Kunming 650091, Yunnan, Peoples R China; Chinese Acad Sci, CAS Key Lab FAST, Natl Astron Observ, Beijing, Peoples R China; Univ Chinese Acad Sci, Beijing 100049, Peoples R China; Chinese Acad Sci, Key Lab Res Galaxies & Cosmol, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China; 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; Grad Univ Adv Studies, SOKENDAI, 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; 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; UCL, Dept Phys & Astron, OSL, London WC1E 6BT, England; Kwansei Gakuin Univ, Sch Sci & Technol, Dept Phys, 2-1 Gakuen, Sanda, Hyogo 6691337, Japan; Kyushu Kyoritsu Univ, 1-8 Kitakyushu Shi,Yahatanishi Ku, Fukuoka 8078585, Japan; Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China; Univ Tokyo, Kavli Inst Phys & Math Universe WPI, UTIAS, Kashiwa, Chiba 2778583, Japan; Univ Sci & Technol Hanoi, Vietnam Acad Sci & Technol, 18 Hoang Quoc Viet, Hanoi, Vietnam; UCL, Dept Phys & Astron, London WC1E 6BT, England; Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China; Univ Paris Diderot, Serv Astrophys, Lab AIM, CEA,DSM,CNRS,CEA Saclay,IRFU, 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, CNRS, IPAG, F-38000 Grenoble, France; Univ Leeds, Sch Phys & Astron, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England | Lee, Jeong-Eun/E-2387-2013; Arzoumanian, Doris/JQT-3284-2023; Savini, Gianluca/C-1188-2009; ONAKA, TAKASHI/G-5058-2014; Gu, Qilao/LTZ-1282-2024; Van Loo, Sven/JRX-9178-2023; Han, Ilseung/MBG-4273-2025; Li, Guang-Xing/AAC-9285-2022; Nanayakkara, Themiya/AAT-6271-2020; 顏士韋, Hsi-Wei/C-8307-2011; Lee, Chin-Fei/AAZ-3391-2020; Yuan, Jinghua/W-4699-2017; Hwang, Jihye/JXW-6363-2024; Soam, Archana/AAG-4250-2021; Tang湯雅雯, Ya-Wen/AAZ-7382-2020; Li, Dalei/ABF-2406-2021; Lee, Sang-Sung/AFS-2722-2022; Doi, Yasuo/A-3395-2013; Li, Hua-bai/AEU-0239-2022; , Le Ngoc Tram/AAH-2951-2019; Tomisaka, Kohji/E-6508-2013; WANG, Qiuhong/L-9577-2016; Kataoka, Akimasa/AAU-5038-2020; Poidevin, Frédérick/Z-3492-2019; Li, Di/HLH-4146-2023; Chen, Zhiwei/LHA-3373-2024; Liu, Junhao/AAQ-3071-2021; Chakali, Eswaraiah/L-5146-2018; Ohashi, Nagayoshi/ABA-9767-2020; Shimajiri, Yoshito/B-1445-2013; Yen, Hsi-Wei/C-8307-2011; Liu, SY/HSD-2860-2023; Rao, Ramprasad/L-2115-2017; Clarke, Seamus/ABC-7965-2020; Liu, Hong-Li/AAR-1998-2020; WANG, Jiawei/GMX-3167-2022; Savini, Giorgio/F-5753-2019; Tsukamoto, Yusuke/AAU-3453-2020; Koch, Patrick/AAV-3373-2021; Priestley, Felix/KYP-3257-2024 | jwwang@asiaa.sinica.edu.tw; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 962 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2024 | 5.4 | 19.6 | 8 | MOLECULAR CLOUD; CLUSTER-FORMATION; SPITZER VIEW; DUST; GRAVITY; CORE; VELOCITY; POLARIZATION; HERSCHEL; SIMULATIONS | English | 2024 | 2024-02-01 | 10.3847/1538-4357/ad165b | 바로가기 | 바로가기 | 바로가기 | ||||||||||
| ○ | ○ | Article | Identifying Changing-look AGNs Using Variability Characteristics | Changing-look (CL) active galactic nuclei (AGNs), characterized by the appearance/disappearance of broad emission lines in the span of a few years, present a challenge for the AGN unified model, whereby the Type 1 versus Type 2 dichotomy results from orientation effects alone. We present a systematic study of a large sample of spectroscopically classified AGNs, using optical variability data from the Zwicky Transient Facility (ZTF) as well as follow-up spectroscopy data. We demonstrate that Type 1 and Type 2 AGNs can be neatly separated on the basis of the variability metric sigma QSO, which quantifies the resemblance of a light curve to a damped random walk model. For a small subsample, however, the ZTF light curves are inconsistent with their previous classification, suggesting the occurrence of a CL event. Specifically, we identify 35 (12) turn-on (turn-off) CL AGN candidates at z < 0.35. Based on follow-up spectroscopy, we confirm 17 (4) turn-on (turn-off) CL AGNs out of 21 (5) candidates, representing a high success rate for our method. Our results suggest that the occurrence rate of CL AGNs is similar to 0.3% over timescales of 5-20 yr, and confirm that the CL transition typically occurs at an Eddington ratio of less than or similar to 0.01. | Wang, Shu; Woo, Jong-Hak; Gallo, Elena; Guo, Hengxiao; Son, Donghoon; Kong, Minzhi; Mandal, Amit Kumar; Cho, Hojin; Kim, Changseok; Shin, Jaejin | Seoul Natl Univ, Dept Phys & Astron, Seoul 08826, South Korea; Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA; Chinese Acad Sci, Key Lab Res Galaxies & Cosmol, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China; Hebei Normal Univ, Dept Phys, 20 East South 2nd Ring Rd, Shijiazhuang 050024, Peoples R China; Korea Astron & Space Sci Inst, Daejeon 34055, South Korea; Kyungpook Natl Univ, Major Astron & Atmospher Sci, Daegu 41566, South Korea | ; Woo, Jong-Hak/A-2790-2014; Mandal, Amit/KDN-2756-2024 | 57196155538; 7401751171; 7101964055; 56330144400; 35222498700; 35187185100; 57200416169; 55961062600; 57476223300; 55554622900 | wangshu100002@gmail.com;woo@astro.snu.ac.kr;hengxiaoguo@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 966 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2024 | 5.4 | 19.6 | 3.93 | 2025-05-07 | 12 | 13 | DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; REVERBERATION MAPPING PROJECT; SURVEY QUASAR PROPERTIES; BROAD-LINE REGION; OPTICAL VARIABILITY; BLACK-HOLES; EMISSION; SAMPLE; GALAXY | English | 2024 | 2024-05-01 | 10.3847/1538-4357/ad3049 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Impacts of Bar-driven Shear and Shocks on Star Formation | Bars drive gas inflow. As the gas flows inward, shocks and shear occur along the bar dust lanes. Such shocks and shear can affect the star formation (SF) and change the gas properties. For four barred galaxies, we present H alpha velocity gradient maps that highlight bar-driven shocks and shear using data from the PHANGS-MUSE and PHANGS-ALMA surveys, which allow us to study bar kinematics in unprecedented detail. Velocity gradients are enhanced along the bar dust lanes, where shocks and shear are shown to occur in numerical simulations. Velocity gradient maps also efficiently pick up H ii regions that are expanding or moving relative to the surroundings. We put pseudo-slits on the regions where velocity gradients are enhanced and find that H alpha and CO velocities jump up to similar to 170 km s-1, even after removing the effects of circular motions due to the galaxy rotation. Enhanced velocity gradients either coincide with the peak of CO intensity along the bar dust lanes or are slightly offset from CO intensity peaks, depending on the objects. Using the Baldwin-Philips-Terlevich BPT diagnostic, we identify the source of ionization on each spaxel and find that SF is inhibited in the high-velocity gradient regions of the bar, and the majority of those regions are classified as a low-ionization nuclear emission-line region (LINER) or composite. This implies that SF is inhibited where bar-driven shear and shocks are strong. Our results are consistent with the results from the numerical simulations that show SF is inhibited in the bar where the shear force is strong. | Kim, Taehyun; Gadotti, Dimitri A.; Querejeta, Miguel; Perez, Isabel; Zurita, Almudena; Neumann, Justus; van de Ven, Glenn; Mendez-Abreu, Jairo; de Lorenzo-Caceres, Adriana; Sanchez-Blazquez, Patricia; Fragkoudi, Francesca; Martins, Lucimara P.; Silva-Lima, Luiz A.; Kim, Woong-Tae; Park, Myeong-Gu | Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 702701, South Korea; Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England; Observ Astron Nacl, C Alfonso XII 3, Madrid 28014, Spain; Univ Granada, Dept Fis Teor & Cosmos, Campus Fuentenueva, Granada 18071, Spain; Inst Carlosde I Fis Teor & Computac, Fac Ciencias, Granada 18071, Spain; Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany; Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria; Inst Astrofis Canarias, Calle Via Lactea S-N, San Cristobal la Laguna 38205, Tenerife, Spain; Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38200, Tenerife, Spain; Univ Complutense Madrid, Dept Fis Tierra & Astrofis, E-28040 Madrid, Spain; Univ Complutense Madrid, Inst Fis Particulas & Cosmos IPARCOS, E-28040 Madrid, Spain; Univ Durham, Inst Computat Cosmol, Dept Phys, South Rd, Durham DH1 3LE, England; Univ Cruzeiro Sul, Univ Cidade Sao Paulo, Rua Galvao Bueno 868, BR-01506000 Sao Paulo, SP, Brazil; Seoul Natl Univ, Dept Phys & Astron, Seoul 08826, South Korea; Seoul Natl Univ, SNU Astron Res Ctr, Seoul 08826, South Korea | ; Mendez Abreu, Jairo/B-2736-2019; Sanchez-Blazquez, Patricia/IYS-6088-2023; Zurita Munoz, Almudena/A-2218-2015; de Lorenzo-Cáceres, Adriana/AAA-6412-2020; Lima, Luiz/HRA-3630-2023; Perez, Isabel/AAF-9177-2019; Querejeta, Miguel/KVY-3638-2024; Zurita, Almudena/A-2218-2015; van de Ven, Glenn/R-5189-2019 | 57050549000; 55887354100; 35424450700; 57211263715; 7004420710; 56514665700; 18038742400; 23051261000; 23088009300; 16319840900; 55062198600; 23088660100; 57554553900; 37070117300; 7404490321 | tkim.astro@gmail.com;mgp@knu.ac.kr; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 968 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2024 | 5.4 | 19.6 | 2.14 | 2025-05-07 | 7 | 7 | MOLECULAR GAS KINEMATICS; DIGITAL SKY SURVEY; SPIRAL GALAXIES; IONIZED-GAS; FORMATION EFFICIENCY; MILKY-WAY; SECULAR EVOLUTION; STELLAR STRUCTURE; ROTATION CURVES; NUCLEAR REGION | English | 2024 | 2024-06-01 | 10.3847/1538-4357/ad410e | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Label-free visualization of internal organs and assessment of anatomical differences among adult Anopheles, Aedes, and Culex mosquito specimens using bidirectional optical coherence tomography | Mosquitoes transmit several fatal human diseases and constitute a global threat to the fight against infectious diseases. Thus, it is crucial to identify the diseases transmitted by mosquitoes, analyze their internal organs, investigate the life cycles of the viruses and pathogens they carry, and elucidate the anatomical changes they cause inside the host without dissecting them. Here we have demonstrated a method for label-free visualization of the internal organs of adult Anopheles, Aedes, and Culex mosquitoes using swept-source optical coherence tomography (SS-OCT). To overcome the limitation of depth-dependent signal-to-noise ratio (SNR) reduction, imaging was conducted using a dynamic rotational OCT scanner to acquire images of the top and bottom surfaces of the specimens. The internal structure and organ images of all the mosquito specimens had constant resolvability and higher SNR than in those obtained via conventional OCT. Furthermore, a depth profiling algorithm was developed to obtain quantitative information about the internal organs. Several internal organs, such as the salivary glands, heart, midgut, dorsal and ventral crop, and abdominal ganglia, were precisely identified and analyzed noninvasively using OCT. The average thicknesses of the heart, midgut, dorsal and ventral crop, and abdominal ganglia of Anopheles, Aedes, and Culex mosquitoes were 72.1, 107.3, 87.3, and 63.4 & mu;m, respectively. This study demonstrates the applicability of OCT in entomology research for high-resolution microscopic analysis. The findings of this study can guide future studies requiring nondestructive assessment of internal organs to evaluate the morphological differences among various virus-transmitting mosquito specimens. | Luna, Jannat Amrin; Ravichandran, Naresh Kumar; Abu Saleah, Sm; Wijesinghe, Ruchire Eranga; Seong, Daewoon; Choi, Kwang Shik; Jung, Hee-Young; Jeon, Mansik; Kim, Jeehyun | Kyungpook Natl Univ, Coll IT Engn, Sch Elect & Elect Engn, 80 Daehak ro, Daegu 41566, South Korea; Korea Basic Sci Inst, Ctr Sci Instrumentat, 169-148 Gwahak ro, Daejeon 34133, South Korea; Kyungpook Natl Univ, ICT Convergence Res Ctr, Daegu 41566, South Korea; Sri Lanka Inst Informat Technol, Fac Engn, Dept Elect & Elect Engn, Malabe, Sri Lanka; Kyungpook Natl Univ, Sch Life Sci, 80 Daehak ro, Daegu 41566, South Korea; Kyungpook Natl Univ, Sch Appl Biosci, 80 Daehak ro, Daegu 41566, South Korea | RAVICHANDRAN, NARESH KUMAR/D-2190-2017; Wijesinghe, Ruchire/K-3797-2016 | 58079161200; 57125825900; 57218499446; 56018152300; 57212512353; 36602283400; 7403029383; 24171094000; 7601373350 | msjeon@knu.ac.kr; | OPTICS AND LASER TECHNOLOGY | OPT LASER TECHNOL | 0030-3992 | 1879-2545 | 168 | SCIE | OPTICS;PHYSICS, APPLIED | 2024 | 5 | 19.6 | 1.26 | 2025-04-16 | 2 | 3 | Aedes; Anopheles; Culex; Mosquito; Optical signal intensity; Swept-source optical coherence tomography | LIGHT-SHEET MICROSCOPY | Aedes; Anopheles; Culex; Mosquito; Optical signal intensity; Swept-source optical coherence tomography | Crops; Data visualization; Depth profiling; Optical tomography; Signal to noise ratio; Viruses; Aedes; Anophele; Culex; Internal organs; Label free; Mosquito; Optical signal intensity; Optical signals; Signal intensities; Swept source optical coherence tomographies; Visualization | English | 2024 | 2024-01 | 10.1016/j.optlastec.2023.109849 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||
| ○ | ○ | Article | Morphology of Galaxies in JWST Fields: Initial Distribution and Evolution of Galaxy Morphology | A recent study from the Horizon Run 5 (HR5) cosmological simulation has predicted that galaxies with log M * / M (circle dot) less than or similar to 10 in the cosmic morning (10 greater than or similar to z greater than or similar to 4) dominantly have disk-like morphology in the Lambda CDM universe, which is driven by the tidal torque in the initial fluctuations of matter. For a direct comparison with observation we identify a total of about 19,000 James Webb Space Telescope (JWST) galaxies with log M * / M (circle dot) > 9 at z = 0.6-8.0 utilizing deep JWST/NIRCam images of publicly released fields, including North Ecliptic Pole Time-Domain Fields, Next Generation Deep Extragalactic Exploratory Public survey, Cosmic Evolution Early Release Science Survey, Cosmic Evolution Survey, UltraDeep Survey, and SMACS J0723-7327. We estimate their stellar masses and photometric redshifts with the redshift dispersion of sigma NMAD = 0.009 and an outlier fraction of only about 6%. We classify galaxies into three morphological types, disks, spheroids, and irregulars, applying the same criteria used in the HR5 study. The morphological distribution of the JWST galaxies shows that disk galaxies account for 60%-70% at all redshift ranges. However, in the high-mass regime ( log M * / M (circle dot) greater than or similar to 11 ), spheroidal morphology becomes the dominant type. This implies that the mass growth of galaxies is accompanied by a morphological transition from disks to spheroids. The fraction of irregulars is about 20% or less at all masses and redshifts. All the trends in the morphology distribution are consistently found in the six JWST fields. These results are in close agreement with the results from the HR5 simulation, particularly confirming the prevalence of disk galaxies at small masses in the cosmic morning and noon. | Lee, Jeong Hwan; Park, Changbom; Hwang, Ho Seong; Kwon, Minseong | Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Kyungpook Natl Univ, Ctr High Energy Phys, Daegu 41566, South Korea; Korea Inst Adv Study, 85 Hoegi ro, Seoul 02455, South Korea; 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; Seoul Natl Univ, Res Inst Basic Sci, Seoul 08826, South Korea | ; HWANG, Ho/AAS-6010-2020 | 57195344163; 7408417049; 15131707100; 58773009100 | hhwang@astro.snu.ac.kr; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 966 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2024 | 5.4 | 19.6 | 2.86 | 2025-05-07 | 10 | 9 | HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; DISTANT GALAXIES; ANGULAR-MOMENTUM; HUBBLE SEQUENCE; MASS RELATION; LUMINOSITY; DEPENDENCE; ASTROPY; SIZE | English | 2024 | 2024-05-01 | 10.3847/1538-4357/ad3448 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | Red Type-1 Quasars after Cosmic Noon and Impact on L UV-related Quasar Statistics | Over the past decades, nearly a million quasars have been explored to shed light on the evolution of supermassive black holes and galaxies. The ultraviolet-to-optical spectra of type-1 quasars particularly offer insights into their black hole activities. Recent findings, however, raise questions about the prevalence of red type-1 quasars of which colors might be due to dust obscuration and their potential influence on luminosity-related properties of quasars. We examine the fraction of red type-1 quasars within the redshift range of 0.68 <= z < 2.20, applying a spectral energy distribution (SED) fitting using optical-to-mid-infrared (MIR) photometric data of Sloan Digital Sky Survey Data Release 14 quasars. Approximately 10% of the type-1 quasars exhibit red colors suggestive of dust obscuration. There is an association between the brightness of the MIR luminosity and a higher fraction of red type-1 quasars, albeit with negligible redshift evolution. By employing E(B - V) values from the SED fitting, we obtained dereddened luminosity of the red type-1 quasars and reassess the quasar luminosity function (QLF) and black hole mass (M (BH)) estimates. Result shows a modest increase in the number density of bright quasars, linking to more flatten bright-end slope of QLFs, while M BH adjustments are minimal. Current SDSS selections with optical colors could miss a significant population of heavily dust-obscured quasars. As future MIR surveys like Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer expand, they may reveal enough obscured quasars to prompt a more profound revision of fundamental quasar properties. | Kim, Yongjung; Kim, Dohyeong; Im, Myungshin; Kim, Minjin | Korea Astron & Space Sci Inst, Daejeon 34055, South Korea; Kyungpook Natl Univ, Coll Nat Sci, Dept Astron & Atmospher Sci, Daegu 41566, South Korea; Pusan Natl Univ, Dept Earth Sci, Busan 46241, South Korea; Seoul Natl Univ, SNU Astron Res Ctr, 1 Gwanak Ro, Seoul 08826, South Korea; Seoul Natl Univ, Dept Phys & Astron, Astron Program, 1 Gwanak Ro, Seoul 08826, South Korea | , Yong Jung Kim/JRW-0681-2023; Im, Myungshin/B-3436-2013; Kim, Minjin/AAU-9910-2020 | 59622148200; 55574223678; 7004267711; 56898213300 | yjkim.ast@gmail.com;dh.dr2kim@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 972 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2024 | 5.4 | 19.6 | 1.43 | 2025-05-07 | 5 | 4 | DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; OSCILLATION SPECTROSCOPIC SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; INFRARED-SURVEY-EXPLORER; DUST-OBSCURED QUASARS; QSO REDSHIFT SURVEY; X-RAY LUMINOSITY; TO 6 QUASARS | English | 2024 | 2024-09-01 | 10.3847/1538-4357/ad5d5d | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES). V. Confusion-limited Submillimeter Galaxy Number Counts at 450 μm and Data Release for the COSMOS Field | We present confusion-limited SCUBA-2 450 mu m observations in the COSMOS-CANDELS region as part of the James Clerk Maxwell Telescope Large Program SCUBA-2 Ultra Deep Imaging EAO Survey. Our maps at 450 and 850 mu m cover an area of 450 arcmin(2). We achieved instrumental noise levels of sigma(450) = 0.59 mJy beam(-1) and sigma(850) = 0.09 mJy beam(-1) in the deepest area of each map. The corresponding confusion noise levels are estimated to be 0.65 and 0.36 mJy beam(-1). Above the 4 sigma (3.5 sigma) threshold, we detected 360 (479) sources at 450 mu m and 237 (314) sources at 850 mu m. We derive the deepest blank-field number counts at 450 mu m, covering the flux-density range of 2-43 mJy. These are in agreement with other SCUBA-2 blank-field and lensing-cluster observations but are lower than various model counts. We compare the counts with those in other fields and find that the field-to-field variance observed at 450 mu m at the R = 6 ' scale is consistent with Poisson noise, so there is no evidence of strong 2D clustering at this scale. Additionally, we derive the integrated surface brightness at 450 mu m down to 2.1 mJy to be 57.3(-6.2)(+1.0) Jy deg(-2), contributing to 41% +/- 4% of the 450 mu m extragalactic background light (EBL) measured by Cosmic Background Explorer and Planck. Our results suggest that the 450 mu m EBL may be fully resolved at 0.08(-0.08)(+0.09) mJy, which extremely deep lensing-cluster observations and next-generation submillimeter instruments with large aperture sizes may be able to achieve. | Gao, Zhen-Kai; Lim, Chen-Fatt; Wang, Wei-Hao; Chen, Chian-Chou; Smail, Ian; Chapman, Scott C.; Zheng, Xian Zhong; Shim, Hyunjin; Kodama, Tadayuki; Ao, Yiping; Chang, Siou-Yu; Clements, David L.; Dunlop, James S.; Ho, Luis C.; Hsu, Yun-Hsin; Hwang, Chorng-Yuan; Hwang, Ho Seong; Koprowski, M. P.; Scott, Douglas; Serjeant, Stephen; Toba, Yoshiki; Urquhart, Sheona A. | Acad Sinica Inst Astron & Astrophys ASIAA, 1 Sect 4,Roosevelt Rd, Taipei 10617, Taiwan; Natl Cent Univ, Grad Inst Astron, 300 Zhongda Rd, Taoyuan 32001, Taiwan; Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England; Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada; Chinese Acad Sci, Purple Mt Observ, 10 Yuanhua Rd, Nanjing 210023, Peoples R China; Chinese Acad Sci, Key Lab Radio Astron, 10 Yuanhua Rd, Nanjing 210023, Peoples R China; Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Anhui, Peoples R China; Kyungpook Natl Univ, Dept Earth Sci Educ, 80 Daehak Ro, Daegu 41566, South Korea; Tohoku Univ, Astron Inst, 6-3 Aramaki, Sendai, Miyagi 9808578, Japan; Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan; Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan; Imperial Coll London, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England; Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Scotland; Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China; Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China; Natl Taiwan Univ, Dept Philosophy, 1 Sect 4,Roosevelt Rd, Taipei 10617, Taiwan; 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; Nicolaus Copernicus Univ, Inst Astron, Fac Phys Astron & Informat, Grudziadzka 5, PL-87100 Torun, Poland; Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada; Open Univ, Sch Phys Sci, Milton Keynes MK7 6AA, England; Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan; Ehime Univ, Res Ctr Space & Cosm Evolut, 2-5 Bunkyo Cho, Matsuyama, Ehime 7908577, Japan; Ludwig Maximilians Univ Munchen, Univ Observ, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany | Smail, Ian/AAL-9018-2020; Koprowski, Maciej/M-7525-2019; HWANG, Ho/AAS-6010-2020; Serjeant, Stephen/AAN-1908-2021; Shim, Hyunjin/LZI-7486-2025; CHEN, Chian-Chou (TC)/ABB-2819-2020; Dunlop, James/ADB-7947-2022; Wang, Wei-Hao/ABD-9942-2020 | 57222184106; 57195235890; 8294170500; 44561018400; 7005932657; 24447889300; 7404091318; 14061137700; 7403300423; 7003967931; 57226333142; 25924805300; 7202804202; 57225302746; 57221601580; 7403387605; 15131707100; 56038935500; 7404952697; 7003485288; 37068332400; 55749698200 | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 971 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2024 | 5.4 | 19.6 | 0.71 | 2025-05-07 | 2 | 2 | STAR-FORMING GALAXIES; ALMA SPECTROSCOPIC SURVEY; X-RAY LUMINOSITY; LEGACY SURVEY; REDSHIFT DISTRIBUTION; PHYSICAL-PROPERTIES; SOURCE CATALOG; MULTIWAVELENGTH PROPERTIES; FORMATION HISTORY; LENSING CLUSTERS | English | 2024 | 2024-08-01 | 10.3847/1538-4357/ad53c1 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||||
| ○ | ○ | Article | The Calibration of Polycyclic Aromatic Hydrocarbon Dust Emission as a Star Formation Rate Indicator in the AKARI NEP Survey | Polycyclic aromatic hydrocarbon (PAH) dust emission has been proposed as an effective extinction-independent star formation rate (SFR) indicator in the mid-infrared, but this may depend on conditions in the interstellar medium. The coverage of the AKARI/Infrared Camera (IRC) allows us to study the effects of metallicity, starburst intensity, and active galactic nuclei on PAH emission in galaxies with f(nu )(L18W) less than or similar to 19 AB mag. Observations include follow-up, rest-frame optical spectra of 443 galaxies within the AKARI North Ecliptic Pole survey that have IRC detections from 7 to 24 mu m. We use optical emission line diagnostics to infer SFR based on H alpha and [O ii]lambda lambda 3726, 3729 emission line luminosities. The PAH 6.2 mu m and PAH 7.7 mu m luminosities (L(PAH 6.2 mu m) and L(PAH 7.7 mu m), respectively) derived using multiwavelength model fits are consistent with those derived from slitless spectroscopy within 0.2 dex. L(PAH 6.2 mu m) and L(PAH 7.7 mu m) correlate linearly with the 24 mu m dust-corrected H alpha luminosity only for normal, star-forming "main-sequence" galaxies. Assuming multilinear correlations, we quantify the additional dependencies on metallicity and starburst intensity, which we use to correct our PAH SFR calibrations at 0 < z < 1.2 for the first time. We derive the cosmic star formation rate density (SFRD) per comoving volume from 0.15 less than or similar to z less than or similar to 1. The PAH SFRD is consistent with that of the far-infrared and reaches an order of magnitude higher than that of uncorrected UV observations at z similar to 1. Starburst galaxies contribute greater than or similar to 0.7 of the total SFRD at z similar to 1 compared to main-sequence galaxies. | Kim, Helen Kyung; Malkan, Matthew A.; Takagi, Toshinobu; Oi, Nagisa; Burgarella, Denis; Miyaji, Takamitsu; Shim, Hyunjin; Matsuhara, Hideo; Goto, Tomotsugu; Ohyama, Yoichi; Buat, Veronique; Kim, Seong Jin | Univ Calif Los Angeles, Dept Phys & Astron, 475 Portola Plaza, Los Angeles, CA 90095 USA; JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan; Tokyo Univ Sci, Fac Sci, Div 2, Shinju Ku, Tokyo 1628601, Japan; Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France; Univ Nacl Autonoma Mexico, Inst Astron Sede Ensenada, Km 107,Carret Tij Ens, Ensenada 22060, Baja California, Mexico; Kyungpook Natl Univ, Dept Earth Sci Educ, Daegu 41566, South Korea; Natl Tsing Hua Univ, Inst Astron, 101 Sect 2,Kuang Fu Rd, Hsinchu 30013, Taiwan; Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan | ; Ohyama, Youichi/ABA-5890-2020; 大山陽一, Youichi/ABA-5890-2020; Malkan, Matthew/IWM-5356-2023; Shim, Hyunjin/LZI-7486-2025 | 57203269860; 7006872661; 35405904800; 23968436800; 8852232400; 57203194972; 14061137700; 7003505733; 57151800100; 14825669800; 7003733332; 57070819300 | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 974 | 2 | SCIE | ASTRONOMY & ASTROPHYSICS | 2024 | 5.4 | 19.6 | 0 | 2025-05-07 | 1 | 1 | INFRARED LUMINOSITY FUNCTIONS; MASS-METALLICITY RELATION; ACTIVE GALACTIC NUCLEI; STARBURST GALAXIES; PAH EMISSION; SPECTROSCOPIC SURVEY; FORMING GALAXIES; HIGH-REDSHIFT; DEEP SURVEY; H-ALPHA | English | 2024 | 2024-10-01 | 10.3847/1538-4357/ad72e6 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||||
| ○ | ○ | Article | The JCMT BISTRO Survey: The Magnetic Fields of the IC 348 Star-forming Region | We present 850 mu m polarization observations of the IC 348 star-forming region in the Perseus molecular cloud as part of the B-fields In STar-forming Region Observation survey. We study the magnetic properties of two cores (HH 211 MMS and IC 348 MMS) and a filamentary structure of IC 348. We find that the overall field tends to be more perpendicular than parallel to the filamentary structure of the region. The polarization fraction decreases with intensity, and we estimate the trend by power law and the mean of the Rice distribution fittings. The power indices for the cores are much smaller than 1, indicative of possible grain growth to micron size in the cores. We also measure the magnetic field strengths of the two cores and the filamentary area separately by applying the Davis-Chandrasekhar-Fermi method and its alternative version for compressed medium. The estimated mass-to-flux ratios are 0.45-2.20 and 0.63-2.76 for HH 211 MMS and IC 348 MMS, respectively, while the ratios for the filament are 0.33-1.50. This result may suggest that the transition from subcritical to supercritical conditions occurs at the core scale (similar to 0.05 pc) in the region. In addition, we study the energy balance of the cores and find that the relative strength of turbulence to the magnetic field tends to be stronger for IC 348 MMS than for HH 211 MMS. The result could potentially explain the different configurations inside the two cores: a single protostellar system in HH 211 MMS and multiple protostars in IC 348 MMS. | Choi, Youngwoo; Kwon, Woojin; Pattle, Kate; Arzoumanian, Doris; Bourke, Tyler L.; Hoang, Thiem; Hwang, Jihye; Koch, Patrick M.; Sadavoy, Sarah; Bastien, Pierre; Furuya, Ray; Lai, Shih-Ping; Qiu, Keping; Ward-Thompson, Derek; Berry, David; Byun, Do-Young; Chen, Huei-Ru Vivien; Chen, Wen Ping; Chen, Mike; Chen, Zhiwei; Ching, Tao-Chung; Cho, Jungyeon; Choi, Minho; Choi, Yunhee; Coude, Simon; Chrysostomou, Antonio; Chung, Eun Jung; Dai, Sophia; Debattista, Victor; Di Francesco, James; Diep, Pham Ngoc; Doi, Yasuo; Duan, Hao-Yuan; Duan, Yan; Eswaraiah, Chakali; 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; Hasegawa, Tetsuo; Houde, Martin; Hull, Charles L. H.; Inoue, Tsuyoshi; Inutsuka, Shu-ichiro; Iwasaki, Kazunari; Jeong, Il-Gyo; Johnstone, Doug; Karoly, Janik; Konyves, Vera; Kang, Ji-hyun; Kang, Miju; Kataoka, Akimasa; Kawabata, Koji; Kemper, Francisca; Kim, Jongsoo; Kim, Shinyoung; Kim, Gwanjeong; Kim, Kyoung Hee; Kim, Mi-Ryang; Kim, Kee-Tae; Kim, Hyosung; Kirchschlager, Florian; Kirk, Jason; Kobayashi, Masato I. N.; Kusune, Takayoshi; Kwon, Jungmi; Lacaille, Kevin; Law, Chi-Yan; Lee, Chang Won; Lee, Hyeseung; Lee, Chin-Fei; Lee, Jeong-Eun; Lee, Sang-Sung; Li, Dalei; Li, Di; Li, Guangxing; Li, Hua-bai; Lin, Sheng-Jun; Liu, Hong-Li; Liu, Tie; Liu, Sheng-Yuan; Liu, Junhao; Longmore, Steven; Lu, Xing; Lyo, A-Ran; Mairs, Steve; Matsumura, Masafumi; Matthews, Brenda; Moriarty-Schieven, Gerald; Nagata, Tetsuya; Nakamura, Fumitaka; Nakanishi, Hiroyuki; Ngoc, Nguyen Bich; Ohashi, Nagayoshi; Onaka, Takashi; Park, Geumsook; Parsons, Harriet; Peretto, Nicolas; Priestley, Felix; Pyo, Tae-Soo; Qian, Lei; Rao, Ramprasad; Rawlings, Jonathan; Rawlings, Mark; Retter, Brendan; Richer, John; Rigby, Andrew; Saito, Hiro; Savini, Giorgio; Seta, Masumichi; Sharma, Ekta; Shimajiri, Yoshito; Shinnaga, Hiroko; Soam, Archana; Tahani, Mehrnoosh; Tamura, Motohide; Tang, Ya-Wen; Tang, Xindi; Tomisaka, Kohji; Tram, Le Ngoc; Tsukamoto, Yusuke; Viti, Serena; Wang, Hongchi; Wang, Jia-Wei; Whitworth, Anthony; Wu, Jintai; Xie, Jinjin; Yang, Meng-Zhe; Yen, Hsi-Wei; Yoo, Hyunju; Yuan, Jinghua; Yun, Hyeong-Sik; Zenko, Tetsuya; Zhang, Guoyin; Zhang, Yapeng; Zhang, Chuan-Peng; Zhou, Jianjun; Zhu, Lei; de Looze, Ilse; Andre, Philippe; Dowell, C. Darren; Eden, David; Eyres, Stewart; Falle, Sam; Le Gouellec, Valentin J. M.; Poidevin, Frederick; van Loo, Sven | Seoul Natl Univ, Dept Phys & Astron, Seoul 08826, South Korea; 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; Seoul Natl Univ, Ctr Educ Res, 1 Gwanak Ro, Seoul 08826, South Korea; UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England; Natl Astron Observ Japan, Div Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan; Jodrell Bank, SKA Observ, Macclesfield SK11 9FT, Cheshire, England; Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester, Lancs, England; Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea; Univ Sci & Technol, 217 Gajeong Ro, Daejeon 34113, South Korea; Acad Sinica, Inst Astron & Astrophys, 1,Sec 4,Roosevelt Rd, Taipei 106216, Taiwan; Queens Univ, Dept Phys Engn Phys & Astrophys, Kingston, ON K7L 3N6, Canada; 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; Tokushima Univ, Inst Liberal Arts & Sci, Minami Jousanajima Machi 1-1, Tokushima 7708502, Japan; Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan; Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan; Nanjing Univ, Sch Astron & Space Sci, 163 Xianlin Ave, Nanjing 210023, Peoples R China; Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing 210023, Peoples R China; Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England; East Asian Observ, 660 N Aohoku Pl,Univ Pk, Hilo, HI 96720 USA; Natl Cent Univ, Inst Astron, Zhongli 32001, Taiwan; Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada; Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Peoples R China; Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA; Chungnam Natl Univ, Dept Astron & Space Sci, Daejeon 34134, South Korea; Worcester State Univ, Dept Earth Environm & Phys, Worcester, MA 01602 USA; Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA; Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China; NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada; Vietnam Acad Sci & Technol, Vietnam Natl Space Ctr, Hanoi, Vietnam; Univ Tokyo, Grad Sch Arts & Sci, Dept Earth Sci & Astron, 3-8-1 Komaba, Tokyo 1538902, Japan; Indian Inst Sci Educ & Res IISER Tirupati, Dept Phys, Tirupati 517619, Andhra Pradesh, India; Natl Chung Hsing Univ, 145 Xingda Rd, Taichung 402, Taiwan; Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada; Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA; Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England; Cardiff Univ, Sch Phys & Astron, Parade, Cardiff CF24 3AA, Wales; Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China; Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan; Univ Western Ontario, Dept Phys & Astron, 1151 Richmond St, London, ON N6A 3K7, Canada; Natl Astron Observ Japan, Alonso Cordova 3788,Off 61B, Santiago, Chile; Joint ALMA Observ, Alonso Cordova 3107, Santiago, Chile; Konan Univ, Dept Phys, Okamoto 8-9-1,Higashinada Ku, Kobe, Hyogo 6588501, Japan; Nagoya Univ, Grad Sch Sci, Dept Phys, Furo Cho,Chikusa Ku, Nagoya, Aichi 4648602, Japan; Doshisha Univ, Dept Environm Syst Sci, Miyakodani 1-3, Kyotanabe, Kyoto 6100394, Japan; Kyungpook Natl Univ, Dept Astron & Atmospher Sci, Daegu, South Korea; Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, 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 Univ, Kagamiyama 1-3-1, Higashihiroshima, Hiroshima 7398526, Japan; CSIC, Inst Space Sci ICE, Barcelona 08193, Spain; Pg Lluis Co 23, ICREA, Barcelona, Spain; Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain; Natl Inst Nat Sci, Natl Astron Observ Japan, Nobeyama Radio Observ, Nobeyama, Minamimaki, Nagano 3841305, Japan; Kyung Hee Univ, Sch Space Res, 1732 Deogyeong Daero, Yongin 17104, Gyeonggi Do, South Korea; Univ Ghent, Sterrenkundig Observ, Krijgslaan 281-S9, B-9000 Ghent, Belgium; Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan; Univ Tokyo, Grad Sch Sci, Dept Astron, 7-3-1 Hongo,Bunkyo Ku, Tokyo 1130033, 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; Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Xinjiang, Peoples R China; Chinese Acad Sci, CAS Key Lab FAST, Natl Astron Observ, Beijing, Peoples R China; Yunnan Univ, Dept Astron, Kunming 650091, Yunnan, Peoples R China; Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, 80 Nandan Rd, Shanghai 200030, Peoples R China; Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England; 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; Grad Univ Adv Studies, SOKENDAI, Hayama, Kanagawa 2400193, Japan; Kagoshima Univ, Grad Sch Sci & Engn, Dept Phys & Astron, 1-21-35 Korimoto, Kagoshima 8900065, Japan; Grad Univ Sci & Technol, Vietnam Acad Sci & Technol, Hanoi, Vietnam; Univ Tokyo, Grad Sch Sci, Dept Astron, 7-3-1 Hongo,Bunkyo Ku, Tokyo 1130033, Japan; Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA; NSF NOIRLab, Gemini Observ, 670 N Aohoku Pl, 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; UCL, Phys & Astron Dept, OSL, London WC1E 6BT, England; Kwansei Gakuin Univ, Sch Sci & Technol, Dept Phys, 2-1 Gakuen, Sanda, Hyogo 6691337, Japan; Kyushu Kyoritsu Univ, 1-8 Jiyugaoka,Yahatanishi Ku, Kitakyushu, Fukuoka 8078585, Japan; Indian Inst Astrophys, II Block, Bengaluru 560034, India; Stanford Univ, Kavli Inst Particle Astrophys & Cosmol KIPAC, Stanford, CA 94305 USA; Natl Inst Nat Sci, Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan; Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China; Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands; UCL, Phys & Astron Dept, London WC1E 6BT, England; Korea Astron & Space Sci Inst, Daejeon 34055, South Korea; Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China; Univ Paris Cite, Univ Paris Saclay, CNRS, Lab Astrophys AIM,CEA,AIM, F-91191 Gif Sur Yvette, France; Jet Prop Lab, M-S 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA; Armagh Observ & Planetarium, Coll Hill, Armagh BT61 9DB, North Ireland; Univ South Wales, Pontypridd CF37 1DL, M Glam, Wales; Univ Leeds, Dept Appl Math, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England; NASA Ames Res Ctr, Space Sci & Astrobiol Div, M-S 245-6, Moffett Field, CA 94035 USA; Inst Astrofis Canarias, Tenerife 38200, Canary Islands, Spain; Univ La Laguna ULL, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain; Univ Leeds, Sch Phys & Astron, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England | ONAKA, TAKASHI/G-5058-2014; Savini, Gianluca/C-1188-2009; Shimajiri, Yoshito/B-1445-2013; Lee, Chin-Fei/AAZ-3391-2020; Nanayakkara, Themiya/AAT-6271-2020; Hwang, Jihye/JXW-6363-2024; Chen, Zhiwei/LHA-3373-2024; Liu, Junhao/AAQ-3071-2021; Kemper, Francisca/AAZ-8274-2020; 顏士韋, Hsi-Wei/C-8307-2011; Lee, Sang-Sung/AFS-2722-2022; Priestley, Felix/KYP-3257-2024; Tang湯雅雯, Ya-Wen/AAZ-7382-2020; Gu, Qilao/LTZ-1282-2024; Poidevin, Frédérick/Z-3492-2019; Tsukamoto, Yusuke/AAU-3453-2020; Soam, Archana/AAG-4250-2021; Kataoka, Akimasa/AAU-5038-2020; Lee, Jeong-Eun/E-2387-2013; Li, Guangxing/HZK-1030-2023; Han, Ilseung/MBG-4273-2025; Liu, Shengyuan/AAC-2359-2019; Li, Dalei/ABF-2406-2021; Koch, Patrick/AAV-3373-2021; Yuan, Jinghua/W-4699-2017; Liu, Hong-Li/AAR-1998-2020; Chakali, Eswaraiah/L-5146-2018; Arzoumanian, Doris/JQT-3284-2023; Ohashi, Nagayoshi/ABA-9767-2020 | 57944161700; 15822192800; 56512202800; 36237885400; 35499669400; 16549809400; 57202952564; 7202929125; 35238413800; 7005805931; 7005566228; 7402935899; 36976168000; 7004002583; 8355600600; 57203026080; 12790268500; 35242015200; 56566873100; 55705656800; 56342326600; 7403536449; 55231989000; 57218669464; 56568251300; 7005084542; 59127396000; 57218489062; 6602592863; 6603570734; 24170690100; 7401662157; 55210722100; 57217586664; 8318213100; 55874635700; 6602882601; 22834355900; 55673595500; 7005672565; 8547622700; 9234005200; 7003509373; 22834101100; 7101632548; 7403310385; 57194592820; 57194798843; 7404174499; 35237077900; 7103332462; 55226383000; 35377433200; 24074312000; 35330159300; 57215516631; 57219237963; 36238131700; 57201082771; 25627568300; 55750138400; 57730823500; 7005283695; 7601365384; 57194595458; 36571804600; 34770134800; 55671720700; 7409321582; 57944655500; 55633098300; 35773361100; 57189663358; 56455301400; 55370384000; 57194605392; 57209260420; 59684797600; 57190230987; 35330124000; 59661685000; 37056945900; 56252021400; 58981067700; 55910516500; 35185338100; 57216330092; 56436978700; 55727743600; 7409459358; 57194603379; 8693281200; 56179884700; 6508022172; 55750223500; 7402157762; 35569334500; 7003401658; 13310130800; 7201941871; 36714093500; 57216925030; 7202558313; 57203067199; 18936782900; 35096693300; 16070455300; 57194941451; 6602816367; 38862759600; 7403068909; 7101942174; 7004265198; 57194586988; 7006586973; 56800212700; 7407452361; 15844178300; 6604032293; 57218295132; 23061889500; 35482578500; 55757586800; 57202847250; 7403258846; 27868095600; 55320822200; 6701467496; 57201731842; 36971326200; 7003564783; 56084174100; 57194606597; 7006011851; 57352212300; 57219690533; 57945146700; 43361931100; 55441261000; 55170380200; 57209281402; 57199325064; 56493265600; 57207478624; 49865000200; 56183368700; 36955785700; 36238023800; 7202964254; 35308644100; 55170000100; 7004237751; 7004415016; 57211397912; 6506192691; 14042952700 | wkwon@snu.ac.kr; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 977 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2024 | 5.4 | 19.6 | 0 | 2025-05-07 | 1 | 1 | PERSEUS MOLECULAR CLOUD; HUB-FILAMENT STRUCTURE; GOULD BELT SURVEY; RADIATIVE TORQUES; GRAIN ALIGNMENT; MU-M; PRESTELLAR CORES; FORMATION RATES; DUST EMISSION; RADIO-SOURCES | English | 2024 | 2024-12-01 | 10.3847/1538-4357/ad88ed | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Article | The Seoul National University AGN Monitoring Project. III. Hβ Lag Measurements of 32 Luminous Active Galactic Nuclei and the High-luminosity End of the Size-Luminosity Relation | We present the main results from a long-term reverberation mapping campaign carried out for the Seoul National University AGN Monitoring Project (SAMP). High-quality data were obtained during 2015-2021 for 32 luminous active galactic nuclei (AGNs; i.e., continuum luminosity in the range of 10(44-46) erg s(-1)) at a regular cadence, of 20-30 days for spectroscopy and 3-5 days for photometry. We obtain time lag measurements between the variability in the H beta emission and the continuum for 32 AGNs; 25 of those have the best lag measurements based on our quality assessment, examining correlation strength and the posterior lag distribution. Our study significantly increases the current sample of reverberation-mapped AGNs, particularly at the moderate-to-high-luminosity end. Combining our results with literature measurements, we derive an H beta broadline region size-luminosity relation with a shallower slope than reported in the literature. For a given luminosity, most of our measured lags are shorter than the expectations, implying that single-epoch black hole mass estimators based on previous calibrations could suffer large systematic uncertainties. | Woo, Jong-hak; Wang, Shu; Rakshit, Suvendu; Cho, Hojin; Son, Donghoon; Bennert, Vardha N.; Gallo, Elena; Hodges-Kluck, Edmund; Treu, Tommaso; Barth, Aaron J.; Cho, Wanjin; Foord, Adi; Geum, Jaehyuk; Guo, Hengxiao; Jadhav, Yashashree; Jeon, Yiseul; Kabasares, Kyle M.; Kang, Won-Suk; Kim, Changseok; Kim, Minjin; Kim, Tae-Woo; Le, Huynh Anh N.; Malkan, Matthew A.; Mandal, Amit Kumar; Park, Daeseong; Spencer, Chance; Shin, Jaejin; Sung, Hyun-il; Vivian, U.; Williams, Peter R.; Yee, Nick | Seoul Natl Univ, Dept Phys & Astron, Seoul 08826, South Korea; Aryabhatta Res Inst Observat Sci, Naini Tal 263001, Uttarakhand, India; Calif Polytech State Univ San Luis Obispo, Phys Dept, San Luis Obispo, CA 93407 USA; Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA; NASA GSFC, Code 662, Greenbelt, MD 20771 USA; Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA; Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA; Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA; Kyungpook Natl Univ, Major Astron & Atmospher Sci, Daegu 41566, South Korea; Chinese Acad Sci, Key Lab Res Galaxies & Cosmol, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China; Natl Youth Space Ctr, Goheung 59567, South Korea; Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 28644, South Korea; Univ Sci & Technol China, Dept Astron, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Peoples R China; Korea Astron & Space Sci Inst, Daejeon 34055, South Korea | Malkan, Matthew/IWM-5356-2023; U, Vivian/J-5875-2019; Kim, Minjin/AAU-9910-2020; Mandal, Amit/KDN-2756-2024; Treu, Tommaso/KYP-7127-2024; Woo, Jong-Hak/A-2790-2014 | 7401751171; 57196155538; 55572266300; 55961062600; 35222498700; 35222917400; 7101964055; 18037283600; 7003853565; 36088948300; 57211396825; 57194341522; 57237852600; 56330144400; 57226852976; 36621209700; 57208693037; 58749635300; 57476223300; 56898213300; 57205660055; 55201854700; 7006872661; 57200416169; 15127668500; 57219785009; 55554622900; 24537938900; 45361575500; 57218765930; 58750089100 | jhwoo@snu.ac.kr;wangshu100002@gmail.com; | ASTROPHYSICAL JOURNAL | ASTROPHYS J | 0004-637X | 1538-4357 | 962 | 1 | SCIE | ASTRONOMY & ASTROPHYSICS | 2024 | 5.4 | 19.6 | 5.36 | 2025-05-07 | 18 | 18 | BROAD-LINE REGION; BLACK-HOLE MASS; REVERBERATION MAPPING PROJECT; HIGH ACCRETION RATES; TELESCOPE RESULTS. I.; SPECTROSCOPIC CAMPAIGN; DYNAMICAL MODELS; SEYFERT-GALAXIES; 3C 273; VARIABILITY | English | 2024 | 2024-02-01 | 10.3847/1538-4357/ad132f | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||||
| ○ | ○ | Review | A Review of Plasma-Synthesized and Plasma Surface-Modified Piezoelectric Polymer Films for Nanogenerators and Sensors | In this review, we introduce recently developed plasma-based approaches for depositing and treating piezoelectric nanoparticles (NPs) and piezoelectric polymer films for nanogenerator (NG) and sensor applications. We also present the properties and an overview of recently synthesized or modified piezoelectric materials on piezoelectric polymers to highlight the existing challenges and future directions of plasma methods under vacuum, low pressure, and ambient air conditions. The various plasma processes involved in piezoelectric NGs and sensors, including plasma-based vapor deposition, dielectric barrier discharge, and surface modification, are introduced and summarized for controlling various surface properties (etching, roughening, crosslinking, functionalization, and crystallinity). | Jung, Eun-Young; Suleiman, Habeeb Olaitan; Tae, Heung-Sik; Park, Choon-Sang | Kyungpook Natl Univ, Inst Elect Technol, Coll IT Engn, Daegu 41566, South Korea; Kyungpook Natl Univ, Coll IT Engn, Sch Elect & Elect Engn, Daegu 41566, South Korea; Milligan Univ, Elect Engn, Johnson City, TN 37682 USA | 57203199724; 57764914500; 7006298844; 16025295400 | eyjung@knu.ac.kr;suleiman.habeeb16@knu.ac.kr;hstae@ee.knu.ac.kr;cpark@milligan.edu; | POLYMERS | POLYMERS-BASEL | 2073-4360 | 16 | 11 | SCIE | POLYMER SCIENCE | 2024 | 4.9 | 19.7 | 0.12 | 2025-05-07 | 4 | 4 | flexible nanogenerators; piezoelectric polymer film; plasma polymerization; plasma surface modification | THIN-FILMS; NANOFIBERS; PVDF | flexible nanogenerators; piezoelectric polymer film; plasma polymerization; plasma surface modification | Crystallinity; Dielectric materials; Electric discharges; Etching; Nanogenerators; Piezoelectricity; Plasma applications; Plasma polymerization; Semiconducting films; Flexible nanogenerator; Nanogenerators; Piezoelectric; Piezoelectric polymer film; Plasma surface modifications; Plasma surfaces; Property; Sensor applications; Surface-modified; Synthesised; Polymer films | English | 2024 | 2024-06 | 10.3390/polym16111548 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||
| ○ | ○ | Article | Analysis of Paint Properties According to Expandable Graphite and Fire Simulation Research on Firewall Penetration Part | In this research, we attempted to develop paints that can be applied to various fields such as high-rise building structures and electric vehicle batteries. To minimize damage to life and property in the event of a fire, we attempted to manufacture a highly elastic paint material that can block flames and control smoke spread, and that has additional sound insulation and waterproofing functions. A high-elasticity paint was manufactured by mixing a flame-retardant polyurethane dispersion (PUD) with an acrylic emulsion binder and adding different mass fractions of expandable graphite (EG). The thermal, physical, and morphological properties of the prepared mixed paint were analyzed. The thermal properties of the mixed paint were analyzed and intended to be used as input data (heat transfer coefficient, specific heat capacity) for fire simulation. Output data were used to predict how much the temperature would change depending on the time of fire occurrence. The reason for conducting simulations on the fire stability of paint materials is that the fire stability of paints can be predicted without conducting fire tests. Two hours after the fire broke out, the thermal temperature distribution was analyzed. The temperature distribution was compared with and without mixed paint. Two hours after a fire broke out in a virtual space, it was found that when the mixed paint was applied, the surrounding temperature of the penetration area was lower than when the mixed paint was not applied. Development costs for developing excellent paints can be reduced. Since fire safety can be predicted without actually conducting tests, the time required for product development can be reduced. We are confident that this is a very groundbreaking technology because it allows fire safety simulations for developed products to be conducted in a virtual space by creating an environment similar to actual fire test standards. | Yu, Seonghun; Lee, Jonghyuk; Yeo, Donghyun; Lee, Junhee; Bae, Jinseok; Sim, Jeehyun | DYETEC Dyeing & Finishing Technol Inst, Comp Aided Engn CAE Ctr, Daegu 41706, South Korea; Kyungpook Natl Univ, Dept Text Syst Engn, Daegu 41566, South Korea | 57487349300; 58803604200; 57487015900; 58673108800; 8857273700; 57487015800 | enviro1234@dyetec.or.kr;trueleejh@dyetec.or.kr;yd@dyetec.or.kr;junhee@dyetec.or.kr;jbae@knu.ac.kr;euler0423@naver.com; | POLYMERS | POLYMERS-BASEL | 2073-4360 | 16 | 1 | SCIE | POLYMER SCIENCE | 2024 | 4.9 | 19.7 | 0.35 | 2025-04-16 | 0 | 1 | fire simulation; virtual engineering; expandable graphite; mixed paint; fire wall penetration part | RESISTANT; VARNISH | expandable graphite; fire simulation; fire wall penetration part; mixed paint; virtual engineering | Fire protection; Fires; Graphite; Heat transfer; Smoke; Specific heat; Tall buildings; Temperature distribution; Virtual reality; Expandable graphite; Fire safety; Fire simulation; Fire wall; Fire wall penetration part; Mixed paint; Property; Virtual engineering; Virtual spaces; Wall penetration; Emulsification | English | 2024 | 2024-01 | 10.3390/polym16010098 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | |||
| ○ | ○ | Article | Comparative Analysis of Physicochemical and Functional Properties of Pectin from Extracted Dragon Fruit Waste by Different Techniques | Dragon fruit peel, often discarded, is a valuable source of commercial pectin. This study investigates different extraction methods, including cold-water (CW), hot-water (HW), ultrasound (US), and novel enzyme extraction (xylanase: EZX), to extract pectins from dragon fruit peel and compare their characteristics. The pectin yield ranged from 10.93% to 20.22%, with significant variations in physicochemical properties across methods (p < 0.05). FTIR analysis revealed that extraction methods did not alter the primary structural configuration of the pectins. However, molecular weights (Mws) varied significantly, from 0.84 to 1.21 x 10(3) kDa, and the degree of esterification varied from 46.82% to 51.79% (p < 0.05). Monosaccharide analysis identified both homogalacturonan (HG) and rhamnogalacturonan-I (RG-I) pectic configurations in all pectins, predominantly comprising galacturonic acid (77.21-83.12 %mol) and rhamnose (8.11-9.51 %mol), alongside minor side-chain sugars. These properties significantly influenced pectin functionalities. In the aqueous state, a higher Mw impacted viscosity and emulsification performance, while a lower Mw enhanced antioxidant activities and promoted the prebiotic function of pectin (Lactis brevies growth). This study highlights the impact of extraction methods on dragon fruit peel pectin functionalities and their structure-function relationship, providing valuable insights into predicting dragon fruit peel's potential as a food-grade ingredient in various products. | Du, Huimin; Olawuyi, Ibukunoluwa Fola; Said, Nurul Saadah; Lee, Won-Young | Kyungpook Natl Univ, Sch Food Sci & Technol, Daegu 41566, South Korea; Kyungpook Natl Univ, Res Inst Tailored Food Technol, Daegu 41566, South Korea | Said, Nurul Saadah/LFV-3208-2024; Lee, Wonyoung/AAL-2780-2021; Olawuyi, Ibukunoluwa/H-1232-2018 | 59004196400; 57204471854; 57211398275; 57195940408 | du19981212@knu.ac.kr;ifolawuyi@knu.ac.kr;nurulsaadah.said@gmail.com;wonyoung@knu.ac.kr; | POLYMERS | POLYMERS-BASEL | 2073-4360 | 16 | 8 | SCIE | POLYMER SCIENCE | 2024 | 4.9 | 19.7 | 1.6 | 2025-05-07 | 5 | 6 | dragon fruit peel; waste utilization; pectin; extraction method; structure-function | MICROWAVE-ASSISTED EXTRACTION; STRUCTURAL CHARACTERISTICS; HYLOCEREUS-POLYRHIZUS; ULTRASOUND; PEEL; POLYSACCHARIDES; ESTERIFICATION; PARAMETERS; XYLANASE; ACID | dragon fruit peel; extraction method; pectin; structure–function; waste utilization | Extraction; Fruits; Physicochemical properties; Cold waters; Comparative analyzes; Dragon fruit peel; Extraction method; Fruit peel; Functional properties; Hot water; Pectin; Physicochemical property; Structure functions; Emulsification | English | 2024 | 2024-04 | 10.3390/polym16081097 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||
| ○ | ○ | Article | Computational Fluid Dynamics Analysis and Empirical Evaluation of Carboxymethylcellulose/Alginate 3D Bioprinting Inks for Screw-Based Microextrusion | Three-dimensional microextrusion bioprinting technology uses pneumatics, pistons, or screws to transfer and extrude bioinks containing biomaterials and cells to print biological tissues and organs. Computational fluid dynamics (CFD) analysis can simulate the flow characteristics of bioinks in a control volume, and the effect on cell viability can be predicted by calculating the physical quantities. In this study, we developed an analysis system to predict the effect of a screw-based dispenser system (SDS) on cell viability in bioinks through rheological and CFD analyses. Furthermore, carboxymethylcellulose/alginate-based bioinks were used for the empirical evaluation of high-viscous bioinks. The viscosity of bioinks was determined by rheological measurement, and the viscosity coefficient for the CFD analysis was derived from a correlation equation by non-linear regression analysis. The mass flow rate derived from the analysis was successfully validated by comparison with that from the empirical evaluation. Finally, the cell viability was confirmed after bioprinting with bioinks containing C2C12 cells, suggesting that the developed SDS may be suitable for application in the field of bioengineering. Consequently, the developed bioink analysis system is applicable to a wide range of systems and materials, contributing to time and cost savings in the bioengineering industry. | Lee, Sungmin; Son, Minjae; Lee, Juo; Byun, Iksong; Kim, Jin-Woo; Kim, Jungsil; Seonwoo, Hoon | Sunchon Natl Univ, Coll Engn, Dept Human Harmonized Robot, Sunchon, South Korea; Sunchon Natl Univ, Interdisciplinary Program IT Bio Convergence Syst, Sunchon 57922, South Korea; Sunchon Natl Univ, Coll Engn, Grad Sch, Dept Aerosp Engn, Sunchon 57922, South Korea; Sunchon Natl Univ, Dept Anim Sci & Technol, Coll Life Sci & Nat Resources, Sunchon 57922, South Korea; Sunchon Natl Univ, Coll Life Sci & Nat Resources, Dept Agr Machinery Engn, Sunchon 57922, South Korea; Univ Arkansas, Dept Biol & Agr Engn, Fayetteville, AR 72701 USA; Univ Arkansas, Mat Sci & Engn Program, Fayetteville, AR 72701 USA; Kyungpook Natl Univ, Coll Agr & Life Sci, Dept Appl Biosci, Daegu 41566, South Korea; Sunchon Natl Univ, Coll Life Sci & Nat Resources, Dept Convergent Biosyst Engn, Sunchon 57922, South Korea | ; Kim, Jin-Woo/H-5148-2011 | 58607436000; 58790136900; 56464669600; 58753737400; 55907824700; 56523661500; 35424539900 | uhun906@gmail.com; | POLYMERS | POLYMERS-BASEL | 2073-4360 | 16 | 8 | SCIE | POLYMER SCIENCE | 2024 | 4.9 | 19.7 | 0.64 | 2025-05-07 | 4 | 4 | screw-based dispenser system (SDS); computational fluid dynamics (CFD); non-linear regression analysis; wall shear stress; bioprinting; cell viability | BIOINKS | bioprinting; cell viability; computational fluid dynamics (CFD); non-linear regression analysis; screw-based dispenser system (SDS); wall shear stress | Biological organs; Cells; Dispensers; Regression analysis; Screws; Shear stress; Viscosity; Bioprinting; Cell viability; Computational fluid dynamic; Empirical evaluations; Fluid dynamic analysis; Fluid-dynamic analysis; Non-linear regression analysis; Screw-based dispenser system; Wall shear stress; Wall-shear stress; Computational fluid dynamics | English | 2024 | 2024-04 | 10.3390/polym16081137 | 바로가기 | 바로가기 | 바로가기 | 바로가기 | ||
| ○ | ○ | Article | Enhanced Mechanical Properties of Polylactic Acid/Poly(Butylene Adipate-co-Terephthalate) Modified with Maleic Anhydride | An increase in plastic waste pollution and the strengthening of global environmental policies have heightened the need for research on biodegradable plastics. In this regard, polylactic acid (PLA) and poly(butylene adipate-co-terephthalate) (PBAT) are notable examples, serving as alternatives to traditional plastics. In this study, the compatibility and mechanical properties of PLA/PBAT blends were improved by the chemical grafting of maleic anhydride (MAH). In addition, qualitative analyses were conducted, dynamic mechanical properties were investigated, and the structure and mechanical characteristics of the blends were analyzed. With an increase in the MAH concentration, the grafting yield of the blends increased, and significantly improved the compatibility of the PLA/PBAT blend, with an similar to 2 and 2.9 times increase in the tensile strength and elongation at break, respectively. These findings indicate that the modified PLA/PBAT blend demonstrates potential for applications that require sustainable plastic materials, thereby contributing to the development of environmentally friendly alternatives in the plastics industry. | Nam, Kibeom; Kim, Sang Gu; Kim, Do Young; Lee, Dong Yun | Kyungpook Natl Univ, Dept Polymer Sci & Engn, Daegu 41566, South Korea | ; , Do Young Kim/AAB-1459-2021 | 57210467782; 56803104600; 56802861000; 57211001605 | ska2918@naver.com;sgkim@wschemical.co.kr;ddyykk9655@gmail.com;dongyunlee@knu.ac.kr; | POLYMERS | POLYMERS-BASEL | 2073-4360 | 16 | 4 | SCIE | POLYMER SCIENCE | 2024 | 4.9 | 19.7 | 3.19 | 2025-05-07 | 10 | 10 | biodegradable plastics; polylactic acid; poly(butylene adipate-co-terephthalate); maleic anhydride; grafting; compounding | GRAFTED POLY(LACTIC ACID); POLY(BUTYLENE ADIPATE-CO-TEREPHTHALATE); GLYCIDYL METHACRYLATE; THERMAL-PROPERTIES; BLEND; PLA; FILMS; PERFORMANCE; EXTRUSION; FOOD | biodegradable plastics; compounding; grafting; maleic anhydride; poly(butylene adipate-co-terephthalate); polylactic acid | Biodegradable polymers; Blending; Butenes; Elastomers; Environmental protection; Maleic anhydride; Plastic products; Polyesters; Tensile strength; Biodegradable plastics; Chemical grafting; Compounding; Environmental policy; Plastics waste; Polies (butylene adipate co terephthalate); Poly lactic acid; Poly(butylene adipate-co-terephthalate); Polylactic acid; Waste pollution; Grafting (chemical) | English | 2024 | 2024-02 | 10.3390/polym16040518 | 바로가기 | 바로가기 | 바로가기 | 바로가기 |
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