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101. The effects of ionization feedback on star formation: A case study of the M16 H II region

Author

Xu, Jin-Long, Zavagno, Annie, Yu, Naiping, Liu, Xiao-Lan, Xu, Ye, Yuan, Jinghua, Zhang, Chuan-Peng, Zhang, Si-Ju, Zhang, Guo-Yin, Ning, Chang-Chun, and Ju, Bing-Gang

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We aim to investigate the impact of the ionized radiation from the M16 HII region on the surrounding molecular cloud and on its hosted star formation. To present comprehensive multi-wavelength observations towards the M16 HII region, we used new CO data and existing infrared, optical, and submillimeter data. The 12CO J=1-0, 13CO J=1-0, and C18O J=1-0 data were obtained with the Purple Mountain Observatory (PMO) 13.7m radio telescope. To trace massive clumps and extract young stellar objects (YSOs) associated with the M16 HII region, we used the ATLASGAL and GLIMPSE I catalogs, respectively. From CO data, we discern a large-scale filament with three velocity components. Because these three components overlap with each other in both velocity and space, the filament may be made of three layers. The M16 ionized gas interacts with the large-scale filament and has reshaped its structure. In the large-scale filament, we find 51 compact cores from the ATLASGAL catalog, 20 of them being quiescent. The mean excitation temperature of these cores is 22.5 K, while this is 22.2 K for the quiescent cores. This high temperature observed for the quiescent cores suggests that the cores may be heated by M16 and do not experience internal heating from sources in the cores. Through the relationship between the mass and radius of these cores, we obtain that 45% of all the cores are massive enough to potentially form massive stars. Compared with the thermal motion, the turbulence created by the nonthermal motion is responsible for the core formation. For the pillars observed towards M16, the H II region may give rise to the strong turbulence., Comment: 18 pages, 12 figures, accepted for publication in A&A

Published
2019
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102. The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-Forming Region

Author

Coudé, Simon, Bastien, Pierre, Houde, Martin, Sadavoy, Sarah, Friesen, Rachel, Di Francesco, James, Johnstone, Doug, Mairs, Steve, Hasegawa, Tetsuo, Kwon, Woojin, Lai, Shih-Ping, Qiu, Keping, Ward-Thompson, Derek, Berry, David, Chen, Michael Chun-Yuan, Fiege, Jason, Franzmann, Erica, Hatchell, Jennifer, Lacaille, Kevin, Matthews, Brenda C., Moriarty-Schieven, Gerald H., Pon, Andy, André, Philippe, Arzoumanian, Doris, Aso, Yusuke, Byun, Do-Young, Chakali, Eswaraiah, Chen, Huei-Ru, Chen, Wen Ping, Ching, Tao-Chung, Cho, Jungyeon, Choi, Minho, Chrysostomou, Antonio, Chung, Eun Jung, Doi, Yasuo, Drabek-Maunder, Emily, Dowell, C. Darren, Eyres, Stewart P. S., Falle, Sam, Friberg, Per, Fuller, Gary, Furuya, Ray S., Gledhill, Tim, Graves, Sarah F., Greaves, Jane S., Griffin, Matt J., Gu, Qilao, Hayashi, Saeko S., Hoang, Thiem, Holland, Wayne, Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Kanamori, Yoshihiro, Kataoka, Akimasa, Kang, Ji-hyun, Kang, Miju, Kang, Sung-ju, Kawabata, Koji S., Kemper, Francisca, Kim, Gwanjeong, Kim, Jongsoo, Kim, Kee-Tae, Kim, Kyoung Hee, Kim, Mi-Ryang, Kim, Shinyoung, Kirk, Jason M., Kobayashi, Masato I. N., Koch, Patrick M., Kwon, Jungmi, Lee, Jeong-Eun, Lee, Chang Won, Lee, Sang-Sung, Li, Dalei, Li, Di, Li, Hua-bai, Liu, Hong-Li, Liu, Junhao, Liu, Sheng-Yuan, Liu, Tie, van Loo, Sven, Lyo, A-Ran, Matsumura, Masafumi, Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ohashi, Nagayoshi, Onaka, Takashi, Parsons, Harriet, Pattle, Kate, Peretto, Nicolas, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Mark G., Retter, Brendan, Richer, John, Rigby, Andrew, Robitaille, Jean-François, Saito, Hiro, Savini, Giorgio, Scaife, Anna M. M., Seta, Masumichi, Shinnaga, Hiroko, Soam, Archana, Tamura, Motohide, Tang, Ya-Wen, Tomisaka, Kohji, Tsukamoto, Yusuke, Wang, Hongchi, Wang, Jia-Wei, Whitworth, Anthony P., Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Zenko, Tetsuya, Zhang, Chuan-Peng, Zhang, Guoyin, Zhou, Jianjun, and Zhu, Lei

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the POL-2 850 $\mu$m linear polarization map of the Barnard 1 clump in the Perseus molecular cloud complex from the B-fields In STar-forming Region Observations (BISTRO) survey at the James Clerk Maxwell Telescope. We find a trend of decreasing polarization fraction as a function of total intensity, which we link to depolarization effects towards higher density regions of the cloud. We then use the polarization data at 850 $\mu$m to infer the plane-of-sky orientation of the large-scale magnetic field in Barnard 1. This magnetic field runs North-South across most of the cloud, with the exception of B1-c where it turns more East-West. From the dispersion of polarization angles, we calculate a turbulence correlation length of $5.0 \pm 2.5$ arcsec ($1500$ au), and a turbulent-to-total magnetic energy ratio of $0.5 \pm 0.3$ inside the cloud. We combine this turbulent-to-total magnetic energy ratio with observations of NH$_3$ molecular lines from the Green Bank Ammonia Survey (GAS) to estimate the strength of the plane-of-sky component of the magnetic field through the Davis-Chandrasekhar-Fermi method. With a plane-of-sky amplitude of $120 \pm 60$ $\mu$G and a criticality criterion $\lambda_c = 3.0 \pm 1.5$, we find that Barnard 1 is a supercritical molecular cloud with a magnetic field nearly dominated by its turbulent component., Comment: 22 pages, 7 figures, accepted in the Astrophysical Journal

Published
2019
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103. Variability in the analysis of a single neuroimaging dataset by many teams

Author

Botvinik-Nezer, Rotem, Holzmeister, Felix, Camerer, Colin F, Dreber, Anna, Huber, Juergen, Johannesson, Magnus, Kirchler, Michael, Iwanir, Roni, Mumford, Jeanette A, Adcock, R Alison, Avesani, Paolo, Baczkowski, Blazej M, Bajracharya, Aahana, Bakst, Leah, Ball, Sheryl, Barilari, Marco, Bault, Nadège, Beaton, Derek, Beitner, Julia, Benoit, Roland G, Berkers, Ruud MWJ, Bhanji, Jamil P, Biswal, Bharat B, Bobadilla-Suarez, Sebastian, Bortolini, Tiago, Bottenhorn, Katherine L, Bowring, Alexander, Braem, Senne, Brooks, Hayley R, Brudner, Emily G, Calderon, Cristian B, Camilleri, Julia A, Castrellon, Jaime J, Cecchetti, Luca, Cieslik, Edna C, Cole, Zachary J, Collignon, Olivier, Cox, Robert W, Cunningham, William A, Czoschke, Stefan, Dadi, Kamalaker, Davis, Charles P, Luca, Alberto De, Delgado, Mauricio R, Demetriou, Lysia, Dennison, Jeffrey B, Di, Xin, Dickie, Erin W, Dobryakova, Ekaterina, Donnat, Claire L, Dukart, Juergen, Duncan, Niall W, Durnez, Joke, Eed, Amr, Eickhoff, Simon B, Erhart, Andrew, Fontanesi, Laura, Fricke, G Matthew, Fu, Shiguang, Galván, Adriana, Gau, Remi, Genon, Sarah, Glatard, Tristan, Glerean, Enrico, Goeman, Jelle J, Golowin, Sergej AE, González-García, Carlos, Gorgolewski, Krzysztof J, Grady, Cheryl L, Green, Mikella A, Guassi Moreira, João F, Guest, Olivia, Hakimi, Shabnam, Hamilton, J Paul, Hancock, Roeland, Handjaras, Giacomo, Harry, Bronson B, Hawco, Colin, Herholz, Peer, Herman, Gabrielle, Heunis, Stephan, Hoffstaedter, Felix, Hogeveen, Jeremy, Holmes, Susan, Hu, Chuan-Peng, Huettel, Scott A, Hughes, Matthew E, Iacovella, Vittorio, Iordan, Alexandru D, Isager, Peder M, Isik, Ayse I, Jahn, Andrew, Johnson, Matthew R, Johnstone, Tom, Joseph, Michael JE, Juliano, Anthony C, Kable, Joseph W, Kassinopoulos, Michalis, Koba, Cemal, and Kong, Xiang-Zhen

Subjects
Generic health relevance, Brain, Data Analysis, Data Science, Datasets as Topic, Female, Functional Neuroimaging, Humans, Logistic Models, Magnetic Resonance Imaging, Male, Meta-Analysis as Topic, Models, Neurological, Reproducibility of Results, Research Personnel, Software, General Science & Technology
Abstract

Data analysis workflows in many scientific domains have become increasingly complex and flexible. Here we assess the effect of this flexibility on the results of functional magnetic resonance imaging by asking 70 independent teams to analyse the same dataset, testing the same 9 ex-ante hypotheses1. The flexibility of analytical approaches is exemplified by the fact that no two teams chose identical workflows to analyse the data. This flexibility resulted in sizeable variation in the results of hypothesis tests, even for teams whose statistical maps were highly correlated at intermediate stages of the analysis pipeline. Variation in reported results was related to several aspects of analysis methodology. Notably, a meta-analytical approach that aggregated information across teams yielded a significant consensus in activated regions. Furthermore, prediction markets of researchers in the field revealed an overestimation of the likelihood of significant findings, even by researchers with direct knowledge of the dataset2-5. Our findings show that analytical flexibility can have substantial effects on scientific conclusions, and identify factors that may be related to variability in the analysis of functional magnetic resonance imaging. The results emphasize the importance of validating and sharing complex analysis workflows, and demonstrate the need for performing and reporting multiple analyses of the same data. Potential approaches that could be used to mitigate issues related to analytical variability are discussed.

Published
2020

104. Building Sustainable Global Collaborative Networks: Recommendations from Music Studies and the Social Sciences

Author

Savage, Patrick E., primary, Jacoby, Nori, additional, Margulis, Elizabeth H., additional, Daikoku, Hideo, additional, Anglada-Tort, Manuel, additional, Castelo-Branco, Salwa El-Sawan, additional, Nweke, Florence Ewomazino, additional, Fujii, Shinya, additional, Hegde, Shantala, additional, Chuan-Peng, Hu, additional, Jabbour, Jason, additional, Lew-Williams, Casey, additional, Mangalagiu, Diana, additional, McNamara, Rita, additional, Müllensiefen, Daniel, additional, Opondo, Patricia, additional, Patel, Aniruddh D., additional, and Schippers, Huib, additional

Published
2023
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105. The JCMT BISTRO Survey: The Magnetic Field In The Starless Core $\rho$ Ophiuchus C

Author

Liu, Junhao, Qiu, Keping, Berry, David, Di Francesco, James, Bastien, Pierre, Koch, Patrick M., Furuya, Ray S., Kim, Kee-Tae, Coudé, Simon, Lee, Chang Won, Soam, Archana, Eswaraiah, Chakali, Li, Di, Hwang, Jihye, Lyo, A-Ran, Pattle, Kate, Hasegawa, Tetsuo, Kwon, Woojin, Lai, Shih-Ping, Ward-Thompson, Derek, Ching, Tao-Chung, Chen, Zhiwei, Gu, Qilao, Li, Dalei, Li, Hua-bai, Liu, Hong-Li, Qian, Lei, Wang, Hongchi, Yuan, Jinghua, Zhang, Chuan-Peng, Zhang, Guoyin, Zhang, Ya-Peng, Zhou, Jianjun, Zhu, Lei, André, Philippe, Arzoumanian, Doris, Aso, Yusuke, Byun, Do-Young, Chen, Michael Chun-Yuan, Chen, Huei-Ru Vivien, Chen, Wen Ping, Cho, Jungyeon, Choi, Minho, Chrysostomou, Antonio, Chung, Eun Jung, Doi, Yasuo, Drabek-Maunder, Emily, Dowell, C. Darren, Eyres, Stewart P. S., Falle, Sam, Fanciullo, Lapo, Fiege, Jason, Franzmann, Erica, Friberg, Per, Friesen, Rachel K., Fuller, Gary, Gledhill, Tim, Graves, Sarah F., Greaves, Jane S., Griffin, Matt J., Han, Ilseung, Hatchell, Jennifer, Hayashi, Saeko S., Hoang, Thiem, Holland, Wayne, Houde, Martin, Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Johnstone, Doug, Kanamori, Yoshihiro, Kang, Ji-hyun, Kang, Miju, Kang, Sung-ju, Kataoka, Akimasa, Kawabata, Koji S., Kemper, Francisca, Kim, Gwanjeong, Kim, Jongsoo, Kim, Kyoung Hee, Kim, Mi-Ryang, Kim, Shinyoung, Kirk, Jason M., Kobayashi, Masato I. N., Kusune, Takayoshi, Kwon, Jungmi, Lacaille, Kevin M., Lee, Chin-Fei, Lee, Jeong-Eun, Lee, Hyeseung, Lee, Sang-Sung, Liu, Sheng-Yuan, Liu, Tie, van Loo, Sven, Mairs, Steve, Matsumura, Masafumi, Matthews, Brenda C., Moriarty-Schieven, Gerald H., Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ohashi, Nagayoshi, Onaka, Takashi, Parker, Josh, Parsons, Harriet, Pascale, Enzo, Peretto, Nicolas, Pon, Andy, Pyo, Tae-Soo, Rao, Ramprasad, Rawlings, Mark G., Retter, Brendan, Richer, John, Rigby, Andrew, Robitaille, Jean-François, Sadavoy, Sarah, Saito, Hiro, Savini, Giorgio, Scaife, Anna M. M., Seta, Masumichi, Shinnaga, Hiroko, Tamura, Motohide, Tang, Ya-Wen, Tomisaka, Kohji, Tsukamoto, Yusuke, Wang, Jia-Wei, Whitworth, Anthony P., Yen, Hsi-Wei, Yoo, Hyunju, and Zenko, Tetsuya

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We report 850~$\mu$m dust polarization observations of a low-mass ($\sim$12 $M_{\odot}$) starless core in the $\rho$ Ophiuchus cloud, Ophiuchus C, made with the POL-2 instrument on the James Clerk Maxwell Telescope (JCMT) as part of the JCMT B-fields In STar-forming Region Observations (BISTRO) survey. We detect an ordered magnetic field projected on the plane of sky in the starless core. The magnetic field across the $\sim$0.1~pc core shows a predominant northeast-southwest orientation centering between $\sim$40$^\circ$ to $\sim$100$^\circ$, indicating that the field in the core is well aligned with the magnetic field in lower-density regions of the cloud probed by near-infrared observations and also the cloud-scale magnetic field traced by Planck observations. The polarization percentage ($P$) decreases with an increasing total intensity ($I$) with a power-law index of $-$1.03 $\pm$ 0.05. We estimate the plane-of-sky field strength ($B_{\mathrm{pos}}$) using modified Davis-Chandrasekhar-Fermi (DCF) methods based on structure function (SF), auto-correlation (ACF), and unsharp masking (UM) analyses. We find that the estimates from the SF, ACF, and UM methods yield strengths of 103 $\pm$ 46 $\mu$G, 136 $\pm$ 69 $\mu$G, and 213 $\pm$ 115 $\mu$G, respectively. Our calculations suggest that the Ophiuchus C core is near magnetically critical or slightly magnetically supercritical (i.e. unstable to collapse). The total magnetic energy calculated from the SF method is comparable to the turbulent energy in Ophiuchus C, while the ACF method and the UM method only set upper limits for the total magnetic energy because of large uncertainties., Comment: 22 pages, 12 figures

Published
2019
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109. In COVID-19 Health Messaging, Loss Framing Increases Anxiety with Little-to-No Concomitant Benefits: Experimental Evidence from 84 Countries

Author

Dorison, Charles A., Lerner, Jennifer S., Heller, Blake H., Rothman, Alexander J., Kawachi, Ichiro I., Wang, Ke, Rees, Vaughan W., Gill, Brian P., Gibbs, Nancy, Ebersole, Charles R., Vally, Zahir, Tajchman, Zuzanna, Zsido, Andras N., Zrimsek, Mija, Chen, Zhang, Ziano, Ignazio, Gialitaki, Zoi, Ceary, Chris D., Lin, Yijun, Kunisato, Yoshihiko, Yamada, Yuki, Xiao, Qinyu, Jiang, Xiaoming, Du, Xinkai, Yao, Elvin, Wilson, John Paul, Cyrus-Lai, Wilson, Jimenez-Leal, William, Law, Wilbert, Collins, W. Matthew, Richard, Karley L., Vranka, Marek, Ankushev, Vladislav, Schei, Vidar, Križanić, Valerija, Kadreva, Veselina Hristova, Adoric, Vera Cubela, Tran, Ulrich S., Yeung, Siu Kit, Hassan, Widad, Houston, Ralph, Lima, Tiago J. S., Ostermann, Thomas, Frizzo, Thomas, Sverdrup, Therese E., House, Thea, Gill, Tripat, Fedotov, Maksim, Paltrow, Tamar, Jernsäther, Teodor, Koptjevskaja-Tamm, Maria, Hostler, Thomas J., Ishii, Tatsunori, Szaszi, Barnabas, Adamus, Sylwia, Suter, Lilian, Habib, Sumaiya, Studzinska, Anna, Stojanovska, Dragana, Janssen, Steve M. J., Stieger, Stefan, Schulenberg, Stefan E., Tatachari, Srinivasan, Azouaghe, Soufian, Sorokowski, Piotr, Sorokowska, Agnieszka, Song, Xin, Lewis, Savannah C., Sinkolova, Sladjana, Grigoryev, Dmitry, Drexler, Shira Meir, Daches, Shimrit, Geniole, Shawn N., Vračar, Selena, Massoni, Sébastien, Zorjan, Saša, Sarıoğuz, Eylül, Izquierdo, Sara Morales, Alves, Sara G., Pöntinen, Sara, Solas, Sara Álvarez, Ordoñez-Riaño, Santiago, Očovaj, Sanja Batić, Onie, Sandersan, Lins, Samuel, Çoksan, Sami, Sacakli, Asli, Ruiz-Fernández, Susana, Geiger, Sandra J., FatahModares, Saeideh, Walczak, Radoslaw B., Betlehem, Ruben, Vilar, Roosevelt, Cárcamo, Rodrigo, Ross, Robert M., McCarthy, Randy, Ballantyne, Tonia, Westgate, Erin C., Afhami, Reza, Ren, Dongning, Monteiro, Renan P., Reips, Ulf-Dietrich, Reggev, Niv, Calin-Jageman, Robert J., Pourafshari, Razieh, Oliveira, Raquel, Nedelcheva-Datsova, Mina, Rahal, Rima-Maria, Ribeiro, Rafael R., Radtke, Theda, Searston, Rachel, Habte, Redeate, Zdybek, Przemysław, Chen, Sau-Chin, Maturan, Princess Lovella G., Perillo, Jennifer T., Isager, Peder Mortvedt, Kačmár, Pavol, Macapagal, Paulo Manuel, Szwed, Paulina, Hanel, Paul H. P., Forbes, Paul A. G., Arriaga, Patrícia, Paris, Bastien, Papachristopoulos, Konstantinos, Correa, Pablo Sebastián, Kácha, Ondřej, Bernardo, Márcia, Campos, Olatz, Bravo, Olalla Niño, Galindo-Caballero, Oscar J., Ogbonnaya, Chisom Esther, Bialobrzeska, Olga, Kiselnikova, Natalia, Simonovic, Nicolle, Cohen, Noga, Nock, Nora L., Johannes, Niklas, Albayrak-Aydemir, Nihan, Say, Nicolas, Torunsky, Nathan, Van Doren, Natalia, Sunami, Naoyuki, Rachev, Nikolay R., Majeed, Nadyanna M., Schmidt, Nadya-Daniela, Nadif, Khaoula, Corral-Frías, Nadia S., Ouherrou, Nihal, Pantazi, Myrto, Lucas, Marc Y., Vasilev, Martin R., Ortiz, María Victoria, Butt, Muhammad Mussaffa, Kabir, Muhib, Muda, Rafał, Tejada Rivera, Maria del Carmen MC, Sirota, Miroslav, Seehuus, Martin, Parzuchowski, Michal, Toro, Mónica, Hricova, Monika, Maldonado, Mónica Alarcón, Marszalek, Magdalena, Karekla, Maria, Mioni, Giovanna, Bosma, Minke Jasmijn, Westerlund, Minja, Vdovic, Milica, Bialek, Michal, Silan, Miguel A., Anne, Michele, Misiak, Michal, Grinberg, Maurice, Capizzi, Mariagrazia, Espinoza Barría, Mauricio F., Kurfali, Merve A., Mensink, Michael C., Harutyunyan, Mikayel, Khosla, Meetu, Korbmacher, Max, Adamkovič, Matúš, Ribeiro, Matheus Fernando Felix, Terskova, Maria, Hruška, Matej, Martončik, Marcel, Voracek, Martin, Čadek, Martin, Frías-Armenta, Martha, Kowal, Marta, Topor, Marta, Roczniewska, Marta, Oosterlinck, Marlies, Kohlová, Markéta Braun, Paruzel-Czachura, Mariola, Romanova, Marina, Papadatou-Pastou, Marietta, Lund, Maria Louise, Antoniadi, Maria, Jones, Marc V., Ortiz, Manuel S., Manavalan, Mathi, Muminov, Abdumalik, Kossowska, Małgorzata, Friedemann, Maja, Wielgus, Magdalena, Varella, Marco A. C., Colloff, Melissa F., Bradford, Maria, Vaughn, Leigh Ann, Eudave, Luis, Vieira, Luc, Pineda, Lina Maria Sanabria, Pérez, Laura Calderón, Lazarevic, Ljiljana B., Jaremka, Lisa M., Kushnir, Elizaveta, Anton-Boicuk, Lisa, de Holanda Coelho, Gabriel Lins, Ahlgren, Lina, Levitan, Carmel A., Micheli, Leticia, Volz, Leonhard, Stojanovska, Marija, Boucher, Leanne, Samojlenko, Lara, Delgado, Lady Grey Javela, Kaliska, Lada, Warmelink, Lara, Rojas-Berscia, Luis Miguel, Yu, Karen, Wachowicz, Jakub, Desai, Kermeka, Barzykowski, Krystian, Kozma, Luca, Evans, Kortnee, Kirgizova, Komila, Agesin, Bamikole Emmanuel, Koehn, Monica A, Wolfe, Kelly, Korobova, Tatiana, Klevjer, Kristoffer, van Schie, Kevin, Vezirian, Kevin, Damnjanović, Kaja, Thommesen, Katrine Krabbe, Schmidt, Kathleen, Filip, Katarzyna, Grzech, Karolina, Hoyer, Karlijn, Moon, Karis, Rana, Kafeel, Janjić, Kristina, Suchow, Jordan W., Kielińska, Julita, Cruz Vásquez, Julio E, Beitner, Julia, Vargas-Nieto, Juan Camilo, Roxas, Jose Carlos T., Taber, Jennifer, Urriago-Rayo, Joan, Pavlacic, Jeffrey M., Bavolar, Jozef, Soto, José A., Olofsson, Jonas K., Vilsmeier, Johannes K., Messerschmidt, Johanna, Czamanski-Cohen, Johanna, Boudesseul, Jordane, Lee, Jeong Min, Kamburidis, Julia, Zickfeld, Janis, Miranda, Jacob F., Verharen, Jeroen P. H., Hristova, Evgeniya, Beshears, Julie E., Đorđević, Jasna Milošević, Bosch, Jasmijn, Valentova, Jaroslava Varella, Antfolk, Jan, Berkessel, Jana B., Schrötter, Jana, Urban, Jan, Röer, Jan Philipp, Norton, James O, Silva, Jaime R., Pickering, Jade S., Vintr, Jáchym, Uttley, Jim, Kunst, Jonas R., Ndukaihe, Izuchukwu L. G., Iyer, Aishwarya, Vilares, Iris, Ivanov, Aleksandr, Ropovik, Ivan, Sula, Isabela, Sarieva, Irena, Metin-Orta, Irem, Prusova, Irina, Pinto, Isabel, Bozdoc, Andreea Ioana, Almeida, Inês A. T., Pit, Ilse L., Dalgar, Ilker, Zakharov, Ilya, Arinze, Azuka Ikechukwu, Ihaya, Keiko, Stephen, Ian D., Gjoneska, Biljana, Brohmer, Hilmar, Flowe, Heather, Godbersen, Hendrik, Kocalar, Halil Emre, Hedgebeth, Mattie V., Chuan-Peng, Hu, Sharifian, MohammadHasan, Manley, Harry, Akkas, Handan, Hajdu, Nandor, Azab, Habiba, Kaminski, Gwenael, Nilsonne, Gustav, Anjum, Gulnaz, Travaglino, Giovanni A., Feldman, Gilad, Pfuhl, Gerit, Czarnek, Gabriela, Marcu, Gabriela Mariana, Hofer, Gabriela, Banik, Gabriel, Adetula, Gabriel Agboola, Bijlstra, Gijsbert, Verbruggen, Frederick, Kung, Franki Y. H., Foroni, Francesco, Singer, Gage, Muchembled, Fany, Azevedo, Flavio, Mosannenzadeh, Farnaz, Marinov, Evelina, Štrukelj, Eva, Etebari, Zahra, Baskin, Ernest, Garcia, Elkin Oswaldo Luis, Musser, Erica, van Steenkiste, I.M.M., Ahn, El Rim, Pronizius, Ekaterina, Jackson, Emily A, Manunta, Efisio, Agadullina, Elena, Šakan, Dušana, Dursun, Pinar, Dujols, Olivier, Dubrov, Dmitrii, Willis, Megan, Tümer, Murat, Beaudry, Jennifer L., Popović, Dora, Dunleavy, Daniel, Djamai, Ikhlas, Krupić, Dino, Vega, Diego, Du, Hongfei, Mola, Débora, Davis, William E., Holford, Dawn Liu, Lewis, David M. G., Vaidis, David C., Ozery, Daphna Hausman, Ricaurte, Danilo Zambrano, Storage, Daniel, Sousa, Daniela, Alvarez, Daniela Serrato, Rosa, Anna Dalla, Krupić, Dajana, Marko, Dafne, Moreau, David, Reeck, Crystal, Correia, Rita C., Whitt, Cassie M., Lamm, Claus, Solorzano, Claudio Singh, von Bastian, Claudia C., Sutherland, Clare AM, Overkott, Clara, Aberson, Christopher L., Wang, Chunhui, Karashiali, Christiana, Noone, Chris, Chiu, Faith, Picciocchi, Chiara, Karaarslan, Cemre, Cellini, Nicola, Esteban-Serna, Celia, Reyna, Cecilia, Batres, Carlota, Li, Ranran, Grano, Caterina, Carpentier, Joelle, Tamnes, Christian K., Fu, Cynthia H.Y., Ishkhanyan, Byurakn, Bylinina, Lisa, Jaeger, Bastian, Bundt, Carsten, Allred, Tara Bulut, Bokkour, Ahmed, Bogatyreva, Natalia, Chopik, William J., Antazo, Benedict, Behzadnia, Behzad, Becker, Maja, Cocco, Beatrice, Chou, Wei-Lun, Hubena, Barbora, Žuro, Barbara, Aczel, Balazs, Baklanova, Ekaterina, Bai, Hui, Balci, Busra Bahar, Babinčák, Peter, Dixson, Barnaby James Wyld, Mokady, Aviv, Kappes, Heather Barry, Atari, Mohammad, Szala, Anna, Szabelska, Anna, Aruta, John Jamir Benzon, Domurat, Artur, Arinze, Nwadiogo Chisom, Modena, Arianna, Adiguzel, Arca, Monajem, Arash, ARABI, Kanza AIT EL, Özdoğru, Asil Ali, Olaya Torres, Adriana Julieth, Theodoropoulou, Andriana, Jurković, Anita Penić, Kassianos, Angelos P., Findor, Andrej, Hartanto, Andree, Thibault Landry, Anais, Ferreira, Ana, Santos, Anabela Caetano, De la Rosa-Gomez, Anabel, Gourdon-Kanhukamwe, Amélie, Todsen, Anna Louise, Karababa, Alper, Janak, Allison, Bran, Alexandre, Tullett, Alexa M., Kuzminska, Anna O., Krafnick, Anthony J, Urooj, Anum, Khaoudi, Ahmed, Ahmed, Afroja, Groyecka-Bernard, Agata, Askelund, Adrian Dahl, Adetula, Adeyemi, Belaus, Anabel, Charyate, Abdelilah Ca, Wichman, Aaron L., Stoyanova, Alina, Greenburgh, Anna, Thomas, Andrew G., Arvanitis, Alexios, Forscher, Patrick S., Mallik, Peter R, Primbs, Maximilian A., Miller, Jeremy K., Moshontz, Hannah, Urry, Heather L., IJzerman, Hans, Basnight-Brown, Dana M., Chartier, Christopher R., Buchanan, Erin M., and Coles, Nicholas A.

Published
2022
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110. JCMT BISTRO survey: Magnetic Fields within the Hub-Filament Structure in IC 5146

Author

Wang, Jia-Wei, Lai, Shih-Ping, Eswaraiah, Chakali, Pattle, Kate, Di Francesco, James, Johnstone, Doug, Koch, Patrick M., Liu, Tie, Tamura, Motohide, Furuya, Ray S., Onaka, Takashi, Ward-Thompson, Derek, Soam, Archana, Kim, Kee-Tae, Lee, Chang Won, Lee, Chin-Fei, Mairs, Steve, Arzoumanian, Doris, Kim, Gwanjeong, Hoang, Thiem, Hwang, Jihye, Liu, Sheng-Yuan, Berry, David, Bastien, Pierre, Hasegawa, Tetsuo, Kwon, Woojin, Qiu, Keping, André, Philippe, Aso, Yusuke, Byun, Do-Young, Chen, Huei-Ru, Chen, Michael C., Chen, Wen Ping, Ching, Tao-Chung, Cho, Jungyeon, Choi, Minho, Chrysostomou, Antonio, Chung, Eun Jung, Coudé, Simon, Doi, Yasuo, Dowell, C. Darren, Drabek-Maunder, Emily, Duan, Hao-Yuan, Eyres, Stewart P. S., Falle, Sam, Fanciullo, Lapo, Fiege, Jason, Franzmann, Erica, Friberg, Per, Friesen, Rachel K., Fuller, Gary, Gledhill, Tim, Graves, Sarah F., Greaves, Jane S., Griffin, Matt J., Gu, Qilao, Han, Ilseung, Hatchell, Jennifer, Hayashi, Saeko S., Holland, Wayne, Houde, Martin, Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Kanamori, Yoshihiro, Kang, Ji-hyun, Kang, Miju, Kang, Sung-ju, Kataoka, Akimasa, Kawabata, Koji S., Kemper, Francisca, Kim, Jongsoo, Kim, Kyoung Hee, Kim, Mi-Ryang, Kim, Shinyoung, Kirk, Jason M., Kobayashi, Masato I. N., Konyves, Vera, Kwon, Jungmi, Lacaille, Kevin M., Lee, Hyeseung, Lee, Jeong-Eun, Lee, Sang-Sung, Lee, Yong-Hee, Li, Dalei, Li, Di, Li, Hua-bai, Liu, Hong-Li, Liu, Junhao, Lyo, A-Ran, Matsumura, Masafumi, Matthews, Brenda C., Moriarty-Schieven, Gerald H., Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ohashi, Nagayoshi, Park, Geumsook, Parsons, Harriet, Pascale, Enzo, Peretto, Nicolas, Pon, Andy, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Mark G., Retter, Brendan, Richer, John, Rigby, Andrew, Robitaille, Jean-François, Sadavoy, Sarah, Saito, Hiro, Savini, Giorgio, Scaife, Anna M. M., Seta, Masumichi, Shinnaga, Hiroko, Tang, Ya-Wen, Tomisaka, Kohji, Tsukamoto, Yusuke, van Loo, Sven, Wang, Hongchi, Whitworth, Anthony P., Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Chuan-Peng, Zhang, Guoyin, Zhang, Ya-Peng, Zhou, Jianjun, and Zhu

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the 850 $\mu$m polarization observations toward the IC5146 filamentary cloud taken using the Submillimetre Common-User Bolometer Array 2 (SCUBA-2) and its associated polarimeter (POL-2), mounted on the James Clerk Maxwell Telescope (JCMT), as part of the B-fields In STar forming Regions Observations (BISTRO). This work is aimed at revealing the magnetic field morphology within a core-scale ($\lesssim 1.0$ pc) hub-filament structure (HFS) located at the end of a parsec-scale filament. To investigate whether or not the observed polarization traces the magnetic field in the HFS, we analyze the dependence between the observed polarization fraction and total intensity using a Bayesian approach with the polarization fraction described by the Rice likelihood function, which can correctly describe the probability density function (PDF) of the observed polarization fraction for low signal-to-noise ratio (SNR) data. We find a power-law dependence between the polarization fraction and total intensity with an index of 0.56 in $A_V\sim$ 20--300 mag regions, suggesting that the dust grains in these dense regions can still be aligned with magnetic fields in the IC5146 regions. Our polarization maps reveal a curved magnetic field, possibly dragged by the contraction along the parsec-scale filament. We further obtain a magnetic field strength of 0.5$\pm$0.2 mG toward the central hub using the Davis-Chandrasekhar-Fermi method, corresponding to a mass-to-flux criticality of $\sim$ $1.3\pm0.4$ and an Alfv\'{e}nic Mach number of $<$0.6. These results suggest that gravity and magnetic field is currently of comparable importance in the HFS, and turbulence is less important., Comment: 24 pages, 15 figures, accepted for publication in ApJ

Published
2018
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111. Physical properties and chemical composition of the cores in the California molecular cloud

Author

Zhang, Guo-Yin, Xu, Jin-Long, Vasyunin, A. I., Semenov, D. A., Wang, Jun-Jie, Dib, Sami, Liu, Tie, Liu, Sheng-Yuan, Zhang, Chuan-Peng, Liu, Xiao-Lan, Wang, Ke, Li, Di, Wu, Zhong-Zu, Yuan, Jing-Hua, Li, Da-Lei, and Gao, Yang

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We aim to reveal the physical properties and chemical composition of the cores in the California molecular cloud (CMC), so as to better understand the initial conditions of star formation. We made a high-resolution column density map (18.2") with Herschel data, and extracted a complete sample of the cores in the CMC with the \textsl{fellwalker} algorithm. We performed new single-pointing observations of molecular lines near 90 GHz with the IRAM 30m telescope along the main filament of the CMC. In addition, we also performed a numerical modeling of chemical evolution for the cores under the physical conditions. We extracted 300 cores, of which 33 are protostellar and 267 are starless cores. About 51\% (137 of 267) of the starless cores are prestellar cores. Three cores have the potential to evolve into high-mass stars. The prestellar core mass function (CMF) can be well fit by a log-normal form. The high-mass end of the prestellar CMF shows a power-law form with an index $\alpha=-0.9\pm 0.1$ that is shallower than that of the Galactic field stellar mass function. Combining the mass transformation efficiency ($\varepsilon$) from the prestellar core to the star of $15\pm 1\%$ and the core formation efficiency (CFE) of 5.5\%, we suggest an overall star formation efficiency of about 1\% in the CMC. In the single-pointing observations with the IRAM 30m telescope, we find that 6 cores show blue-skewed profile, while 4 cores show red-skewed profile. [$\rm {HCO}^{+}$]/[HNC] and [$\rm {HCO}^{+}$]/$\rm [N_{2}H^{+}]$ in protostellar cores are higher than those in prestellar cores; this can be used as chemical clocks. The best-fit chemical age of the cores with line observations is $\sim 5\times 10^4$~years., Comment: Accepted by Astronomy & Astrophysics (A&A)

Published
2018
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112. Dust spectrum and polarisation at 850 um in the massive IRDC G035.39-00.33

Author

Juvela, Mika, Guillet, Vincent, Liu, Tie, Ristorcelli, Isabelle, Pelkonen, Veli-Matti, Alina, Dana, Bronfman, Leonardo, Eden, David J., Kim, Kee Tae, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Malinen, Johanna, Micelotta, Elisabetta, Montillaud, Julien, Rawlings, Mark G., Sanhueza, Patricio, Soam, Archana, Traficante, Alessio, Ysard, Nathalie, and Zhang, Chuan-Peng

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The dust sub-millimetre polarisation of star-forming clouds carries information on dust and the role of magnetic fields in cloud evolution. With observations of a dense filamentary cloud G035.39-00.33, we aim to characterise the dust emission properties and the variations of the polarisation fraction. JCMT SCUBA-2/POL-2 data at 850um are combined with Planck 850um (353GHz) data to map polarisation fractions. With previous SCUBA-2 observations (450um and 850um) and Herschel data, the column densities are determined via modified blackbody fits and via radiative transfer modelling. Models are constructed to examine how the polarisation angles and fractions depend on potential magnetic field geometries and grain alignment. POL-2 data show clear changes in the magnetic field orientation. The filament has a peak column density of N(H2)~7 10^22 cm-2, a minimum dust temperature of T~12 K, and a mass of some 4300Msun for the area N(H2)> 5 10^21 cm-2. The estimated average value of the dust opacity spectral index is beta ~ 1.9. The ratio of sub-millimetre and J band optical depths is tau(250 um)/tau(J) ~ 2.5 10^-3, more than four times the typical values for diffuse medium. The polarisation fraction decreases as a function of column density to p ~ 1% in the central filament. Because of noise, the observed decrease of p(N) is significant only at N(H2)>2 10^22 cm-2. The observations suggest that the grain alignment is not constant. Although the data can be explained with a complete loss of alignment at densities above ~ 10^4 cm-3 or using the predictions of radiative torques alignment, the uncertainty of the field geometry and the spatial filtering of the SCUBA-2 data prevent strong conclusions. G035.39-00.33 shows strong signs of dust evolution and the low polarisation fraction is suggestive of a loss of polarised emission from its densest parts., Comment: accepted for publication in Astronomy and Astrophysics

Published
2018
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113. Magnetic fields towards Ophiuchus-B derived from SCUBA-2 polarization measurements

Author

Soam, Archana, Pattle, Kate, Ward-Thompson, Derek, Lee, Chang Won, Sadavoy, Sarah, Koch, Patrick M., Kim, Gwanjeong, Kwon, Jungmi, Kwon, Woojin, Arzoumanian, Doris, Berry, David, Hoang, Thiem, Tamura, Motohide, Lee, Sang-Sung, Liu, Tie, Kim, Kee-Tae, Johnstone, Doug, Nakamura, Fumitaka, Lyo, A-Ran, Onaka, Takashi, Kim, Jongsoo, Furuya, Ray S., Hasegawa, Tetsuo, Lai, Shih-Ping, Bastien, Pierre, Chung, Eun Jung, Kim, Shinyoung, Parsons, Harriet, Rawlings, Mark, Mairs, Steve, Graves, Sarah F., Robitaille, J. -F., Liu, Hong-Li, Whitworth, Anthony P., Eswaraiah, Chakali, Rao, Ramprasad, Yoo, Hyunju, Houde, Martin, Kang, Ji-hyun, Doi, Yasuo, Choi, Minho, Kang, Miju, Coude, Simon, Li, Hua-bai, Matsumura, Masafumi, Matthews, Brenda C., Pon, Andy, Di Francesco, James, Hayashi, Saeko S., Kawabata, Koji S., Inutsuka, Shu-ichiro, Qiu, Keping, Franzmann, Erica, Friberg, Per, Greaves, Jane S., Kirk, Jason M., Li, Di, Shinnaga, Hiroko, van Loo, Sven, Aso, Yusuke, Byun, Do-Young, Chen, Huei-Ru, Chen, Mike C. -Y., Chen, Wen Ping, Ching, Tao-Chung, Cho, Jungyeon, Chrysostomou, Antonio, Drabek-Maunder, Emily, Eyres, Stewart P. S., Fiege, Jason, Friesen, Rachel K., Fuller, Gary, Gledhill, Tim, Griffin, Matt J., Gu, Qilao, Hatchell, Jennifer, Holland, Wayne, Inoue, Tsuyoshi, Iwasaki, Kazunari, Jeong, Il-Gyo, Kang, Sung-ju, Kemper, Francisca, Kim, Kyoung Hee, Kim, Mi-Ryang, Lacaille, Kevin M., Lee, Jeong-Eun, Li, Dalei, Liu, Junhao, Liu, Sheng-Yuan, Moriarty-Schieven, Gerald H., Nakanishi, Hiroyuki, Ohashi, Nagayoshi, Peretto, Nicolas, Pyo, Tae-Soo, Qian, Lei, Retter, Brendan, Richer, John, Rigby, Andrew, Savini, Giorgio, Scaife, Anna M. M., Tang, Ya-Wen, Tomisaka, Kohji, Wang, Hongchi, Wang, Jia-Wei, Yen, Hsi-Wei, Yuan, Jinghua, Zhang, Chuan-Peng, Zhang, Guoyin, Zhou, Jianjun, Zhu, Lei, Andre, Philippe, Dowell, C. Darren, Falle, Sam, Tsukamoto, Yusuke, Kanamori, Yoshihiro, Kataoka, Akimasa, Kobayashi, Masato I. N., Nagata, Tetsuya, Saito, Hiro, Seta, Masumichi, Hwang, Jihye, Han, Ilseung, Lee, Hyeseung, and Zenko, Tetsuya

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the results of dust emission polarization measurements of Ophiuchus-B (Oph-B) carried out using the Submillimetre Common-User Bolometer Array 2 (SCUBA-2) camera with its associated polarimeter (POL-2) on the James Clerk Maxwell Telescope (JCMT) in Hawaii. This work is part of the B-fields In Star-forming Region Observations (BISTRO) survey initiated to understand the role of magnetic fields in star formation for nearby star-forming molecular clouds. We present a first look at the geometry and strength of magnetic fields in Oph-B. The field geometry is traced over $\sim$0.2 pc, with clear detection of both of the sub-clumps of Oph-B. The field pattern appears significantly disordered in sub-clump Oph-B1. The field geometry in Oph-B2 is more ordered, with a tendency to be along the major axis of the clump, parallel to the filamentary structure within which it lies. The degree of polarization decreases systematically towards the dense core material in the two sub-clumps. The field lines in the lower density material along the periphery are smoothly joined to the large scale magnetic fields probed by NIR polarization observations. We estimated a magnetic field strength of 630$\pm$410 $\mu$G in the Oph-B2 sub-clump using a Davis-Chandeasekhar-Fermi analysis. With this magnetic field strength, we find a mass-to-flux ratio $\lambda$= 1.6$\pm$1.1, which suggests that the Oph-B2 clump is slightly magnetically supercritical., Comment: 17 pages, 10 figures, Accepted for publication in ApJ

Published
2018
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114. The TOP-SCOPE survey of PGCCs: PMO and SCUBA-2 observations of 64 PGCCs in the 2nd Galactic Quadrant

Author

Zhang, Chuan-Peng, Liu, Tie, Yuan, Jinghua, Sanhueza, Patricio, Traficante, Alessio, Li, Guang-Xing, Li, Di, Tatematsu, Ken'ichi, Wang, Ke, Lee, Chang Won, Samal, Manash R., Eden, David, Marston, Anthony, Liu, Xiao-Lan, Zhou, Jian-Jun, Li, Pak Shing, Koch, Patrick M., Xu, Jin-Long, Wu, Yuefang, Juvela, Mika, Zhang, Tianwei, Alina, Dana, Goldsmith, Paul F., Tóth, L. V., Wang, Jun-Jie, and Kim, Kee-Tae

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

In order to understand the initial conditions and early evolution of star formation in a wide range of Galactic environments, we carried out an investigation of 64 \textit{Planck} Galactic Cold Clumps (PGCCs) in the second quadrant of the Milky Way. Using the $^{13}$CO and C$^{18}$O $J = 1 - 0$ lines, and 850\,$\mu$m continuum observations, we investigated cloud fragmentation and evolution associated with star formation. We extracted 468 clumps and 117 cores from the $^{13}$CO line and 850\,$\mu$m continuum maps, respectively. We make use of the Bayesian Distance Calculator and derived the distances of all 64 PGCCs. We found that in general, the mass-size plane follows a relation of $m\sim r^{1.67}$. At a given scale, the masses of our objects are around 1/10 of that of typical Galactic massive star-forming regions. Analysis of the clump and core masses, virial parameters, densities, and mass-size relation suggests that the PGCCs in our sample have a low core formation efficiency ($\sim$3.0\%), and most PGCCs are likely low-mass star-forming candidates. Statistical study indicates that the 850\,$\mu$m cores are more turbulent, more optically thick, and denser than the $^{13}$CO clumps for star formation candidates, suggesting that the 850\,$\mu$m cores are likely more appropriate future star-formation candidates than the $^{13}$CO clumps., Comment: 51 pages, 13 figures, 5 tables; Accepted for publication in ApJS; Supplementary figures can be downloaded in https://zcp521.github.io/pub/Figs.zip

Published
2018
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115. A First Look at BISTRO Observations of The $\rho$ Oph-A core

Author

Kwon, Jungmi, Doi, Yasuo, Tamura, Motohide, Matsumura, Masafumi, Pattle, Kate, Berry, David, Sadavoy, Sarah, Matthews, Brenda C., Ward-Thompson, Derek, Hasegawa, Tetsuo, Furuya, Ray S., Pon, Andy, Di Francesco, James, Arzoumanian, Doris, Hayashi, Saeko S., Kawabata, Koji S., Onaka, Takashi, Choi, Minho, Kang, Miju, Hoang, Thiem, Lee, Chang Won, Lee, Sang-Sung, Liu, Hong-Li, Liu, Tie, Inutsuka, Shu-Ichiro, Eswaraiah, Chakali, Bastien, Pierre, Kwon, Woojin, Lai, Shih-Ping, Qiu, Keping, Coude, Simon, Franzmann, Erica, Friberg, Per, Graves, Sarah F., Greaves, Jane S., Houde, Martin, Johnstone, Doug, Kirk, Jason M., Koch, Patrick M., Li, Di, Parsons, Harriet, Rao, Ramprasad, Rawlings, Mark, Shinnaga, Hiroko, Van Loo, Sven, Aso, Yusuke, Byun, Do-Young, Chen, Huei-Ru, Chen, Mike C. -Y., Chen, Wen Ping, Ching, Tao-Chung, Cho, Jungyeon, Chrysostomou, Antonio, Chung, Eun Jung, Drabek-Maunder, Emily, Eyres, Stewart P. S., Fiege, Jason, Friesen, Rachel K., Fuller, Gary, Gledhill, Tim, Griffin, Matt J., Gu, Qilao, Hatchell, Jennifer, Holland, Wayne, Inoue, Tsuyoshi, Iwasaki, Kazunari, Jeong, Il-Gyo, Kang, Ji-Hyun, Kang, Sung-Ju, Kemper, Francisca, Kim, Gwanjeong, Kim, Jongsoo, Kim, Kee-Tae, Kim, Kyoung Hee, Kim, Mi-Ryang, Kim, Shinyoung, Lacaille, Kevin M., Lee, Jeong-Eun, Li, Dalei, Li, Hua-Bai, Liu, Junhao, Liu, Sheng-Yuan, Lyo, A-Ran, Mairs, Steve, Moriarty-Schieven, Gerald H., Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ohashi, Nagayoshi, Peretto, Nicolas, Pyo, Tae-Soo, Qian, Lei, Retter, Brendan, Richer, John, Rigby, Andrew, Robitaille, Jean-Franois, Savini, Giorgio, Scaife, Anna M. M., Soam, Archana, Tang, Ya-Wen, Tomisaka, Kohji, Wang, Hongchi, Wang, Jia-Wei, Whitworth, Anthony P., Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Zhang, Chuan-Peng, Zhang, Guoyin, Zhou, Jianjun, Zhu, Lei, Andre, Philippe, Dowell, C. Darren, Falle, Sam, Tsukamoto, Yusuke, Nakagawa, Takao, Kanamori, Yoshihiro, Kataoka, Akimasa, Kobayashi, Masato I. N., Nagata, Tetsuya, Saito, Hiro, Seta, Masumichi, and Zenko, Tetsuya

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present 850 $\mu$m imaging polarimetry data of the $\rho$ Oph-A core taken with the Submillimeter Common-User Bolometer Array-2 (SCUBA-2) and its polarimeter (POL-2), as part of our ongoing survey project, BISTRO (B-fields In STar forming RegiOns). The polarization vectors are used to identify the orientation of the magnetic field projected on the plane of the sky at a resolution of 0.01 pc. We identify 10 subregions with distinct polarization fractions and angles in the 0.2 pc $\rho$ Oph A core; some of them can be part of a coherent magnetic field structure in the $\rho$ Oph region. The results are consistent with previous observations of the brightest regions of $\rho$ Oph-A, where the degrees of polarization are at a level of a few percents, but our data reveal for the first time the magnetic field structures in the fainter regions surrounding the core where the degree of polarization is much higher ($> 5 \%$). A comparison with previous near-infrared polarimetric data shows that there are several magnetic field components which are consistent at near-infrared and submillimeter wavelengths. Using the Davis-Chandrasekhar-Fermi method, we also derive magnetic field strengths in several sub-core regions, which range from approximately 0.2 to 5 mG. We also find a correlation between the magnetic field orientations projected on the sky with the core centroid velocity components., Comment: 22 pages, 11 figures, accepted for publication in ApJ

Published
2018
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116. A holistic perspective on the dynamics of G035.39-00.33: the interplay between gas and magnetic fields

Author

Liu, Tie, Li, Pak Shing, Juvela, Mika, Kim, Kee-Tae, Evans II, Neal J., Di Francesco, James, Liu, Sheng-Yuan, Yuan, Jinghua, Tatematsu, Ken'ichi, Zhang, Qizhou, Ward-Thompson, Derek, Fuller, Gary, Goldsmith, Paul F., Koch, P. M., Sanhueza, Patricio, Ristorcelli, I., Kang, Sung-ju, Chen, Huei-Ru, Hirano, N., Wu, Yuefang, Sokolov, Vlas, Lee, Chang Won, White, Glenn J., Wang, Ke, Eden, David, Li, Di, Thompson, Mark, Pattle, Kate M, Soam, Archana, Nasedkin, Evert, Kim, Jongsoo, Kim, Gwanjeong, Lai, Shih-Ping, Park, Geumsook, Qiu, Keping, Zhang, Chuan-Peng, Alina, Dana, Eswaraiah, Chakali, Falgarone, Edith, Fich, Michel, Greaves, Jane, Gu, Q. -L., Kwon, Woojin, Li, Hua-bai, Malinen, Johanna, Montier, Ludovic, Parsons, Harriet, Qin, Sheng-Li, Rawlings, Mark G., Ren, Zhi-Yuan, Tang, Mengyao, Tang, Y. -W., Toth, L. V., Wang, Jiawei, Wouterloot, Jan, Yi, H. -W., and Zhang, H. -W.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Magnetic field is one of the key agents that play a crucial role in shaping molecular clouds and regulating star formation, yet the complete information on the magnetic field is not well constrained due to the limitations in observations. We study the magnetic field in the massive infrared dark cloud G035.39-00.33 from dust continuum polarization observations at 850 $\micron$ with SCUBA-2/POL-2 at JCMT. The magnetic field tends to be perpendicular to the densest part of the main filament (F$_{M}$), whereas it has a less defined relative orientation in the rest of the structure, where it tends to be parallel to some diffuse regions. A mean plane-of-the-sky magnetic field strength of $\sim$50 $\mu$G for F$_{M}$ is obtained using Davis-Chandrasekhar-Fermi method. Based on $^{13}$CO (1-0) line observations, we suggest a formation scenario of F$_{M}$ due to large-scale ($\sim$10 pc) cloud-cloud collision. Using additional NH$_3$ line data, we estimate that F$_{M}$ will be gravitationally unstable if it is only supported by thermal pressure and turbulence. The northern part of F$_{M}$, however, can be stabilized by a modest additional support from the local magnetic field. The middle and southern parts of F$_{M}$ are likely unstable even if the magnetic field support is taken into account. We claim that the clumps in F$_{M}$ may be supported by turbulence and magnetic fields against gravitational collapse. Finally, we identified for the first time a massive ($\sim$200 M$_{\sun}$), collapsing starless clump candidate, "c8", in G035.39-00.33. The magnetic field surrounding "c8" is likely pinched, hinting at an accretion flow along the filament., Comment: Published on ApJ, 27 pages

Published
2018
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118. Data from the Human Penguin Project, a cross-national dataset testing social thermoregulation principles.

Author

Hu, Chuan-Peng, Yin, Ji-Xing, Lindenberg, Siegwart, Dalğar, İlker, Weissgerber, Sophia C, Vergara, Rodrigo C, Cairo, Athena H, Čolić, Marija V, Dursun, Pinar, Frankowska, Natalia, Hadi, Rhonda, Hall, Calvin J, Hong, Youngki, Joy-Gaba, Jennifer, Lazarević, Dušanka, Lazarević, Ljiljana B, Parzuchowski, Michal, Ratner, Kyle G, Rothman, David, Sim, Samantha, Simão, Cláudia, Song, Mengdi, Stojilović, Darko, Blomster, Johanna K, Brito, Rodrigo, Hennecke, Marie, Jaume-Guazzini, Francisco, Schubert, Thomas W, Schütz, Astrid, Seibt, Beate, Zickfeld, Janis H, and IJzerman, Hans

Subjects
Humans, Body Temperature, Climate, Demography, Body Temperature Regulation, Social Environment, Surveys and Questionnaires
Abstract

In the Human Penguin Project (N = 1755), 15 research groups from 12 countries collected body temperature, demographic variables, social network indices, seven widely-used psychological scales and two newly developed questionnaires (the Social Thermoregulation and Risk Avoidance Questionnaire (STRAQ-1) and the Kama Muta Frequency Scale (KAMF)). They were collected to investigate the relationship between environmental factors (e.g., geographical, climate etc.) and human behaviors, which is a long-standing inquiry in the scientific community. More specifically, the present project was designed to test principles surrounding the idea of social thermoregulation, which posits that social networks help people to regulate their core body temperature. The results showed that all scales in the current project have sufficient to good psychometrical properties. Unlike previous crowdsourced projects, this dataset includes not only the cleaned raw data but also all the validation of questionnaires in 9 different languages, thus providing a valuable resource for psychological scientists who are interested in cross-national, environment-human interaction studies.

Published
2019

119. Kama Muta: Conceptualizing and Measuring the Experience Often Labelled Being Moved Across 19 Nations and 15 Languages

Author

Zickfeld, Janis H, Schubert, Thomas W, Seibt, Beate, Blomster, Johanna K, Arriaga, Patrícia, Basabe, Nekane, Blaut, Agata, Caballero, Amparo, Carrera, Pilar, Dalgar, Ilker, Ding, Yi, Dumont, Kitty, Gaulhofer, Valerie, Gračanin, Asmir, Gyenis, Réka, Hu, Chuan-Peng, Kardum, Igor, Lazarević, Ljiljana B, Mathew, Leemamol, Mentser, Sari, Nussinson, Ravit, Onuki, Mayuko, Páez, Darío, Pásztor, Anna, Peng, Kaiping, Petrović, Boban, Pizarro, José J, Schönefeld, Victoria, Śmieja, Magdalena, Tokaji, Akihiko, Vingerhoets, Ad, Vorster, Anja, Vuoskoski, Jonna, Zhu, Lei, and Fiske, Alan Page

Subjects
Psychology, Concept Formation, Cross-Cultural Comparison, Emotions, Female, Humans, Language, Male, Metaphor, being moved, kama muta, cross-cultural, communal sharing, empathy, Cognitive Sciences, Experimental Psychology
Abstract

English-speakers sometimes say that they feel "moved to tears," "emotionally touched," "stirred," or that something "warmed their heart;" other languages use similar passive contact metaphors to refer to an affective state. The authors propose and measure the concept of kama muta to understand experiences often given these and other labels. Do the same experiences evoke the same kama muta emotion across nations and languages? They conducted studies in 19 different countries, 5 continents, 15 languages, with a total of 3,542 participants. They tested the construct while validating a comprehensive scale to measure the appraisals, valence, bodily sensations, motivation, and lexical labels posited to characterize kama muta. The results are congruent with theory and previous findings showing that kama muta is a distinct positive social relational emotion that is evoked by experiencing or observing a sudden intensification of communal sharing. It is commonly accompanied by a warm feeling in the chest, moist eyes or tears, chills or piloerection, feeling choked up or having a lump in the throat, buoyancy, and exhilaration. It motivates affective devotion and moral commitment to communal sharing. Although the authors observed some variations across cultures, these 5 facets of kama muta are highly correlated in every sample, supporting the validity of the construct and the measure. (PsycINFO Database Record (c) 2019 APA, all rights reserved).

Published
2019

120. Situational factors shape moral judgements in the trolley dilemma in Eastern, Southern and Western countries in a culturally diverse sample

Author

Bago, Bence, Kovacs, Marton, Protzko, John, Nagy, Tamas, Kekecs, Zoltan, Palfi, Bence, Adamkovic, Matus, Adamus, Sylwia, Albalooshi, Sumaya, Albayrak-Aydemir, Nihan, Alfian, Ilham N., Alper, Sinan, Alvarez-Solas, Sara, Alves, Sara G., Amaya, Santiago, Andresen, Pia K., Anjum, Gulnaz, Ansari, Daniel, Arriaga, Patrícia, Aruta, John Jamir Benzon R., Arvanitis, Alexios, Babincak, Peter, Barzykowski, Krystian, Bashour, Bana, Baskin, Ernest, Batalha, Luisa, Batres, Carlota, Bavolar, Jozef, Bayrak, Fatih, Becker, Benjamin, Becker, Maja, Belaus, Anabel, Białek, Michał, Bilancini, Ennio, Boller, Daniel, Boncinelli, Leonardo, Boudesseul, Jordane, Brown, Benjamin T., Buchanan, Erin M., Butt, Muhammad M., Calvillo, Dustin P., Carnes, Nate C., Celniker, Jared B., Chartier, Christopher R., Chopik, William J., Chotikavan, Poom, Chuan-Peng, Hu, Clancy, Rockwell F., Çoker, Ogeday, Correia, Rita C., Adoric, Vera Cubela, Cubillas, Carmelo P., Czoschke, Stefan, Daryani, Yalda, de Grefte, Job A. M., de Vries, Wieteke C., Burak, Elif G. Demirag, Dias, Carina, Dixson, Barnaby J. W., Du, Xinkai, Dumančić, Francesca, Dumbravă, Andrei, Dutra, Natalia B., Enachescu, Janina, Esteban-Serna, Celia, Eudave, Luis, Evans, Thomas R., Feldman, Gilad, Felisberti, Fatima M., Fiedler, Susann, Findor, Andrej, Fleischmann, Alexandra, Foroni, Francesco, Francová, Radka, Frank, Darius-Aurel, Fu, Cynthia H. Y., Gao, Shan, Ghasemi, Omid, Ghazi-Noori, Ali-Reza, Ghossainy, Maliki E., Giammusso, Isabella, Gill, Tripat, Gjoneska, Biljana, Gollwitzer, Mario, Graton, Aurélien, Grinberg, Maurice, Groyecka-Bernard, Agata, Harris, Elizabeth A., Hartanto, Andree, Hassan, Widad A. N. M., Hatami, Javad, Heimark, Katrina R., Hidding, Jasper J. J., Hristova, Evgeniya, Hruška, Matej, Hudson, Charlotte A., Huskey, Richard, Ikeda, Ayumi, Inbar, Yoel, Ingram, Gordon P. D., Isler, Ozan, Isloi, Chris, Iyer, Aishwarya, Jaeger, Bastian, Janssen, Steve M. J., Jiménez-Leal, William, Jokić, Biljana, Kačmár, Pavol, Kadreva, Veselina, Kaminski, Gwenaël, Karimi-Malekabadi, Farzan, Kasper, Arno T. A., Kendrick, Keith M., Kennedy, Bradley J., Kocalar, Halil E., Kodapanakkal, Rabia I., Kowal, Marta, Kruse, Elliott, Kučerová, Lenka, Kühberger, Anton, Kuzminska, Anna O., Lalot, Fanny, Lamm, Claus, Lammers, Joris, Lange, Elke B., Lantian, Anthony, Lau, Ivy Y.-M., Lazarevic, Ljiljana B., Leliveld, Marijke C., Lenz, Jennifer N., Levitan, Carmel A., Lewis, Savannah C., Li, Manyu, Li, Yansong, Li, Haozheng, Lima, Tiago J. S., Lins, Samuel, Liuzza, Marco Tullio, Lopes, Paula, Lu, Jackson G., Lynds, Trent, Máčel, Martin, Mackinnon, Sean P., Maganti, Madhavilatha, Magraw-Mickelson, Zoe, Magson, Leon F., Manley, Harry, Marcu, Gabriela M., Seršić, Darja Masli, Matibag, Celine-Justine, Mattiassi, Alan D. A., Mazidi, Mahdi, McFall, Joseph P., McLatchie, Neil, Mensink, Michael C., Miketta, Lena, Milfont, Taciano L., Mirisola, Alberto, Misiak, Michal, Mitkidis, Panagiotis, Moeini-Jazani, Mehrad, Monajem, Arash, Moreau, David, Musser, Erica D., Narhetali, Erita, Ochoa, Danielle P., Olsen, Jerome, Owsley, Nicholas C., Özdoğru, Asil A., Panning, Miriam, Papadatou-Pastou, Marietta, Parashar, Neha, Pärnamets, Philip, Paruzel-Czachura, Mariola, Parzuchowski, Michal, Paterlini, Julia V., Pavlacic, Jeffrey M., Peker, Mehmet, Peters, Kim, Piatnitckaia, Liudmila, Pinto, Isabel, Policarpio, Monica Renee, Pop-Jordanova, Nada, Pratama, Annas J., Primbs, Maximilian A., Pronizius, Ekaterina, Purić, Danka, Puvia, Elisa, Qamari, Vahid, Qian, Kun, Quiamzade, Alain, Ráczová, Beáta, Reinero, Diego A., Reips, Ulf-Dietrich, Reyna, Cecilia, Reynolds, Kimberly, Ribeiro, Matheus F. F., Röer, Jan P., Ross, Robert M., Roussos, Petros, Ruiz-Dodobara, Fernando, Ruiz-Fernandez, Susana, Rutjens, Bastiaan T., Rybus, Katarzyna, Samekin, Adil, Santos, Anabela C., Say, Nicolas, Schild, Christoph, Schmidt, Kathleen, Ścigała, Karolina A., Sharifian, MohammadHasan, Shi, Jiaxin, Shi, Yaoxi, Sievers, Erin, Sirota, Miroslav, Slipenkyj, Michael, Solak, Çağlar, Sorokowska, Agnieszka, Sorokowski, Piotr, Söylemez, Sinem, Steffens, Niklas K., Stephen, Ian D., Sternisko, Anni, Stevens-Wilson, Laura, Stewart, Suzanne L. K., Stieger, Stefan, Storage, Daniel, Strube, Justine, Susa, Kyle J., Szekely-Copîndean, Raluca D., Szostak, Natalia M., Takwin, Bagus, Tatachari, Srinivasan, Thomas, Andrew G., Tiede, Kevin E., Tiong, Lucas E., Tonković, Mirjana, Trémolière, Bastien, Tunstead, Lauren V., Türkan, Belgüzar N., Twardawski, Mathias, Vadillo, Miguel A., Vally, Zahir, Vaughn, Leigh Ann, Verschuere, Bruno, Vlašiček, Denis, Voracek, Martin, Vranka, Marek A., Wang, Shuzhen, West, Skye-Loren, Whyte, Stephen, Wilton, Leigh S., Wlodarczyk, Anna, Wu, Xue, Xin, Fei, Yadanar, Su, Yama, Hiroshi, Yamada, Yuki, Yilmaz, Onurcan, Yoon, Sangsuk, Young, Danielle M., Zakharov, Ilya, Zein, Rizqy A., Zettler, Ingo, Žeželj, Iris L., Zhang, Don C., Zhang, Jin, Zheng, Xiaoxiao, Hoekstra, Rink, and Aczel, Balazs

Published
2022
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121. The properties of Planck Galactic cold clumps in the L1495 dark cloud

Author

Tang, Mengyao, Liu, Tie, Qin, Sheng-Li, Kim, Kee-Tae, Wu, Yuefang, Tatematsu, Ken'ichi, Yuan, Jinghua, Wang, Ke, Parsons, Harriet, Koch, Patrick M., Sanhueza, Patricio, Ward-Thompson, D., Tóth, L. Viktor, Soam, Archana, Lee, Chang Won, Eden, David, Di Francesco, James, Rawlings, Jonathan, Rawlings, Mark G., Montillaud, Julien, Zhang, Chuan-Peng, and Cunningham, M. R.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Planck Galactic Cold Clumps (PGCCs) possibly represent the early stages of star formation. To understand better the properties of PGCCs, we studied 16 PGCCs in the L1495 cloud with molecular lines and continuum data from Herschel, JCMT/SCUBA-2 and the PMO 13.7 m telescope. Thirty dense cores were identified in 16 PGCCs from 2-D Gaussian fitting. The dense cores have dust temperatures of $T_{\rm d}$ = 11-14 K, and H$_{2}$ column densities of $N_{\rm H_{2}}$ = 0.36-2.5$\times10^{22}$ cm$^{-2}$. We found that not all PGCCs contain prestellar objects. In general, the dense cores in PGCCs are usually at their earliest evolutionary stages. All the dense cores have non-thermal velocity dispersions larger than the thermal velocity dispersions from molecular line data, suggesting that the dense cores may be turbulence-dominated. We have calculated the virial parameter $\alpha$ and found that 14 of the dense cores have $\alpha$ $<$ 2, while 16 of the dense cores have $\alpha$ $>$ 2. This suggests that some of the dense cores are not bound in the absence of external pressure and magnetic fields. The column density profiles of dense cores were fitted. The sizes of the flat regions and core radii decrease with the evolution of dense cores. CO depletion was found to occur in all the dense cores, but is more significant in prestellar core candidates than in protostellar or starless cores. The protostellar cores inside the PGCCs are still at a very early evolutionary stage, sharing similar physical and chemical properties with the prestellar core candidates.

Published
2018
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122. Hyssopus cuspidatus volatile oil: a potential treatment for steroid-resistant asthma via inhibition of neutrophil extracellular traps.

Author

Wang, Xu, Peng, Hui-Ming, Zhang, Meng-Ru, Li, Jing-Jing, Zhao, Chuan-Peng, Zhang, Ya-Li, Wang, Si-Yu, Zhu, Si-Ying, Lu, Jian-Kang, Yin, Hai-Long, Yin, Qiang, and Fang, Jin-Bo

Abstract

Background: Steroid-resistant asthma (SRA) is a form of asthma resistant to corticosteroid therapy, which is characterized by the presence of neutrophil-predominant inflammatory response and neutrophil extracellular traps (NETs) formation. Hyssopus cuspidatus Boriss., a traditional Uyghur medicine, is known for its efficacy in treating inflammatory lung conditions such as asthma. However, the therapeutic impact and underlying mechanisms of Hyssopus cuspidatus Boriss.'s volatile oil (HVO) in SRA have not been fully elucidated. Methods: This study established an ovalbumin/lipopolysaccharide (OVA/LPS)-induced SRA mice model to evaluate the therapeutic effect of HVO on SRA. UPLC-QE-Orbitrap-MS was applied to analyze the serum compositions of HVO. Network pharmacology and molecular docking were employed to uncover the complex mechanisms of HVO in treating SRA and predict potential effective compounds in HVO. Furthermore, in vivo studies in SRA mice and in vitro studies using HL-60 cells and bone marrow neutrophils were conducted to validate the mechanism. Results: HVO could significantly ameliorate OVA/LPS-induced SRA symptoms, including airway hyperresponsiveness, airway inflammation, mucus overproduction and airway remodeling. 41 prototype compounds, 65 Phase I metabolites and 50 Phase II metabolites were identified in serum-containing HVO. The integration of network pharmacology with experimental validation revealed that HVO can inhibit the formation of NETs by targeting neutrophil elastase, thereby exerting a therapeutic influence on SRA. Meanwhile, molecular docking results showed that 3-methoxy-4-hydroxy mandelonitrile, 1,2,3,4-tetrahydro-1,5,7-trimethyl-naphthalene, cis-calamenene and aristol-1(10)-en-9-yl isovalerate may be the therapeutic compounds of HVO in treating SRA. Conclusion: These findings suggest that HVO is a promising therapeutic candidate for neutrophil-dominant SRA by targeting NETs formation. [ABSTRACT FROM AUTHOR]

Published
2025
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123. The Effectiveness of Unimodal and Multimodal Warnings on Drivers' Response Time: A Meta-Analysis.

Author

Zhu, Ao, Ma, Ko-Hsuan, Choi, Annebella Tsz Ho, Hu, Duoduo, Hu, Chuan-Peng, Peng, Peng, and He, Jibo

Subjects
ACCIDENT prevention, STIMULUS & response (Psychology), WARNINGS, QUANTITATIVE research, REACTION time
Abstract

Driving warning systems are of great help in notifying emergencies. Based on the results of former studies as well as the multisensory integration effect (MIE), the current meta-analysis investigated the effectiveness of utilizing unimodal (i.e., auditory, visual, and tactile) and multimodal (i.e., bimodal and trimodal) driving warning systems in drivers' response time. Sixty eligible articles representing 308 individual studies were included in this meta-analysis. The results showed: First, both auditory warnings (pooled Hedges' g = 0.98, 95% CI: 0.34 to 1.61, p < 0.01) and tactile warnings (pooled Hedges' g = 0.77, 95% CI: 0.22 to 1.32, p < 0.01) were found to reduce the response time significantly compared to no warning, but visual warnings did not produce significant benefit; Second, tactile warnings outperformed the visual warnings (pooled Hedges' g = 0.74, 95% CI: 0.11 to 1.37, p < 0.05); Third, auditory-tactile bimodal warnings surpassed unimodal warnings (p < 0.05); Fourth, drivers' response time under trimodal warning conditions were shorter than that under bimodal warning conditions but not in a significant level. Overall, the results support multisensory redundant signal effect hypothesis in multimodal conditions. Current study provides a quantitative understanding of the effectiveness of driving warnings and could contribute to the design of related technologies. [ABSTRACT FROM AUTHOR]

Published
2025
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124. Two-Dimensional Molecular Gas and ongoing star formation around H II region Sh2-104

Author

Xu, Jin-Long, Xu, Ye, Yu, Naiping, Zhang, Chuan-peng, Liu, Xiao-Lan, Wang, Jun-Jie, Ning, Chang-Chun, Ju, Bing-Gang, and Zhang, Guo-Yin

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We performed a multiwavelength study towards HII region Sh2-104. New maps of 12CO J=1-0 and 13CO J=1-0 were obtained from the Purple Mountain Observatory (PMO) 13.7 m radio telescope. Sh2-104 displays a double-ring structure. The outer ring with a radius of 4.4 pc is dominated by 12 um, 500 um, 12CO J=1-0, and 13CO J=1-0 emission, while the inner ring with a radius of 2.9 pc is dominated by 22 um and 21 cm emission. We did not detect CO emission inside the outer ring. The north-east portion of the outer ring is blueshifted, while the south-west portion is redshifted. The present observations have provided evidence that the collected outer ring around Sh2-104 is a two-dimensional structure. From the column density map constructed by the Hi-GAL survey data, we extract 21 clumps. About 90\% of all the clumps will form low-mass stars. A power-law fit to the clumps yields M=281Msun(r/pc)^1.31. The selected YSOs are associated with the collected material on the edge of Sh2-104. The derived dynamical age of Sh2-104 is 1.6*10^6 yr. Compared the Sh2-104 dynamical age with the YSOs timescale and the fragmentation time of the molecular ring, we further confirm that collect-and-collapse process operates in this region, indicating a positive feedback from a massive star for surrounding gas., Comment: 19 pages, 14 figures, Accepted for publication in ApJ

Published
2017
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125. A statistical study towards the high-mass BGPS clumps with the MALT90 survey

Author

Liu, Xiao-Lan, Xu, Jin-Long, Ning, Chang-Chun, Zhang, Chuan-Peng, and Liu, Xiao-Tao

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

In this work, we perform a statistical investigation towards 50 high-mass clumps using the data from the Bolocam Galactic Plane Survey (BGPS) and the Millimetre Astronomy Legacy Team 90-GHz survey (MALT90). Eleven dense molecular lines (N$_2$H$^+$(1-0), HNC(1-0), HCO$^+$(1-0), HCN(1-0), HN$^{13}$C(1-0), H$^{13}$CO$^+$(1-0), C$_2$H(1-0), HC$_3$N(10-9), SiO(2-1), $^{13}$CS(2-1) and HNCO$(4_{4,0}-3_{0,3}))$ are detected. N$_2$H$^+$ and HNC are shown to be good tracers for clumps in virous evolutionary stages since they are detected in all the fields. And the detection rates of N-bearing molecules decrease as the clumps evolve, but those of O-bearing species increase with evolution. Furthermore, the abundance ratios [N$_2$H$^+$]/[HCO$^+$] and Log([HC$_3$N]/[HCO$^+$]) decline with Log([HCO$^+$]) as two linear functions, respectively. This suggests the transformation of N$_2$H$^+$ and HC$_3$N to HCO$^+$ as the clumps evolve. We also find that C$_2$H is the most abundant molecule with an order of $10^{-8}$. Besides, three new infall candidates G010.214-00.324, G011.121-00.128, and G012.215-00.118(a) are discovered to have large-scaled infall motions and infall rates in the magnitude of $10^{-3}$ M$_\odot$ yr$^{-1}$., Comment: 40 pages, 14 figures, 6 tables

Published
2017
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126. Gas structure and dynamics towards bipolar infrared bubble

Author

Xu, Jin-Long, Yu, Naiping, Zhan, Chuan-Peng, and Liu, Xiao-Lan

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present multi-wavelength analysis for four bipolar bubbles (G045.386-0.726, G049.998-0.125, G050.489+0.993, and G051.610-0.357) to probe the structure and dynamics of their surrounding gas. The 12CO J=1-0, 13CO J=1-0 and C18O J=1-0 observations are made with the Purple Mountain Observation (PMO) 13.7 m radio telescope. For the four bipolar bubbles, the bright 8.0 um emission shows the bipolar structure. Each bipolar bubble is associated with an HII region. From CO observations we find that G045.386-0.726 is composed of two bubbles with different distances, not a bipolar bubble. Each of G049.998-0.125 and G051.610-0.357 is associated with a filament. The filaments in CO emission divide G049.998-0.125 and G051.610-0.357 into two lobes. We suggest that the exciting stars of both G049.998-0.125 and G051.610-0.357 form in a sheet-like structure clouds. Furthermore, G050.489+0.993 is associated with a clump, which shows a triangle-like shape with a steep integrated intensity gradient towards the two lobes of G050.489+0.993. We suggest that the two lobes of G050.489+0.993 have simultaneously expanded into the clump., Comment: 13 pages, 11 figures, accepted for publication in ApSS

Published
2017
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127. Gas kinematics and star formation in the filamentary molecular cloud G47.06+0.26

Author

Xu, Jin-Long, Xu, Ye, Zhang, Chuan-Peng, Liu, Xiao-Lan, Yu, Naiping, Ning, Chang-Chun, and Ju, Bing-Gang

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We performed a multi-wavelength study toward the filamentary cloud G47.06+0.26 to investigate the gas kinematics and star formation. We present the 12CO (J=1-0), 13CO (J=1-0) and C18O (J=1-0) observations of G47.06+0.26 obtained with the Purple Mountain Observation (PMO) 13.7 m radio telescope to investigate the detailed kinematics of the filament. The 12CO (J=1-0) and 13CO (J=1-0) emission of G47.06+0.26 appear to show a filamentary structure. The filament extends about 45 arcmin (58.1 pc) along the east-west direction. The mean width is about 6.8 pc, as traced by the 13CO (J=1-0) emission. G47.06+0.26 has a linear mass density of about 361.5 Msun/pc. The external pressure (due to neighboring bubbles and H II regions) may help preventing the filament from dispersing under the effects of turbulence. From the velocity-field map, we discern a velocity gradient perpendicular to G47.06+0.26. From the Bolocam Galactic Plane Survey (BGPS) catalog, we found nine BGPS sources in G47.06+0.26, that appear to these sources have sufficient mass to form massive stars. We obtained that the clump formation efficiency (CFE) is about 18% in the filament. Four infrared bubbles were found to be located in, and adjacent to, G47.06+0.26. Particularly, infrared bubble N98 shows a cometary structure. CO molecular gas adjacent to N98 also shows a very intense emission. H II regions associated with infrared bubbles can inject the energy to surrounding gas. We calculated the kinetic energy, ionization energy, and thermal energy of two H II regions in G47.06+0.26. From the GLIMPSE I catalog, we selected some Class I sources with an age of about 100000 yr, which are clustered along the filament. The feedback from the H II regions may cause the formation of a new generation of stars in filament G47.06+0.26., Comment: 10 pages, 11 figures, accepted for publication in A&A

Published
2017
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128. First results from BISTRO -- a SCUBA-2 polarimeter survey of the Gould Belt

Author

Ward-Thompson, Derek, Pattle, Kate, Bastien, Pierre, Furuya, Ray S., Kwon, Woojin, Lai, Shih-Ping, Qiu, Keping, Berry, David, Choi, Minho, Coudé, Simon, Di Francesco, James, Hoang, Thiem, Franzmann, Erica, Friberg, Per, Graves, Sarah F., Greaves, Jane S., Houde, Martin, Johnstone, Doug, Kirk, Jason M., Koch, Patrick M., Kwon, Jungmi, Lee, Chang Won, Li, Di, Matthews, Brenda C., Mottram, Joseph C., Parsons, Harriet, Pon, Andy, Rao, Ramprasad, Rawlings, Mark, Shinnaga, Hiroko, Sadavoy, Sarah, van Loo, Sven, Aso, Yusuke, Byun, Do-Young, Chakali, Eswariah, Chen, Huei-Ru, Chen, Mike C. -Y., Chen, Wen Ping, Ching, Tao-Chung, Cho, Jungyeon, Chrysostomou, Antonio, Chung, Eun Jung, Doi, Yasuo, Drabek-Maunder, Emily, Eyres, Stewart P. S., Fiege, Jason, Friesen, Rachel K., Fuller, Gary, Gledhill, Tim, Griffin, Matt J., Gu, Qilao, Hasegawa, Tetsuo, Hatchell, Jennifer, Hayashi, Saeko S., Holland, Wayne, Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Kang, Ji-hyun, Kang, Miju, Kang, Sung-ju, Kawabata, Koji S., Kemper, Francisca, Kim, Gwanjeong, Kim, Jongsoo, Kim, Kee-Tae, Kim, Kyoung Hee, Kim, Mi-Ryang, Kim, Shinyoung, Lacaille, Kevin M., Lee, Jeong-Eun, Lee, Sang-Sung, Li, Dalei, Li, Hua-bai, Liu, Hong-Li, Liu, Junhao, Liu, Sheng-Yuan, Liu, Tie, Lyo, A-Ran, Mairs, Steve, Matsumura, Masafumi, Moriarty-Schieven, Gerald H., Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ohashi, Nagayoshi, Onaka, Takashi, Peretto, Nicolas, Pyo, Tae-Soo, Qian, Lei, Retter, Brendan, Richer, John, Rigby, Andrew, Robitaille, Jean-François, Savini, Giorgio, Scaife, Anna M. M., Soam, Archana, Tamura, Motohide, Tang, Ya-Wen, Tomisaka, Kohji, Wang, Hongchi, Wang, Jia-Wei, Whitworth, Anthony P., Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Zhang, Chuan-Peng, Zhang, Guoyin, Zhou, Jianjun, Zhu, Lei, André, Philippe, Dowell, C. Darren, Falle, Sam, and Tsukamoto, Yusuke

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the first results from the B-fields In STar-forming Region Observations (BISTRO) survey, using the Sub-millimetre Common-User Bolometer Array 2 (SCUBA-2) camera, with its associated polarimeter (POL-2), on the James Clerk Maxwell Telescope (JCMT) in Hawaii. We discuss the survey's aims and objectives. We describe the rationale behind the survey, and the questions which the survey will aim to answer. The most important of these is the role of magnetic fields in the star formation process on the scale of individual filaments and cores in dense regions. We describe the data acquisition and reduction processes for POL-2, demonstrating both repeatability and consistency with previous data. We present a first-look analysis of the first results from the BISTRO survey in the OMC 1 region. We see that the magnetic field lies approximately perpendicular to the famous 'integral filament' in the densest regions of that filament. Furthermore, we see an 'hour-glass' magnetic field morphology extending beyond the densest region of the integral filament into the less-dense surrounding material, and discuss possible causes for this. We also discuss the more complex morphology seen along the Orion Bar region. We examine the morphology of the field along the lower-density north-eastern filament. We find consistency with previous theoretical models that predict magnetic fields lying parallel to low-density, non-self-gravitating filaments, and perpendicular to higher-density, self-gravitating filaments., Comment: 12 pages, 8 figures, accepted for publication in ApJ

Published
2017
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129. Mass-size scaling M~ r^1.67 of massive star-forming clumps -- evidences of turbulence-regulated gravitational collapse

Author

Zhang, Chuan-Peng and Li, Guang-Xing

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We study the fragmentation of eight massive clumps using data from ATLASGAL 870 $\mu$m, SCUBA 850 and 450 $\mu$m, PdBI 1.3 and 3.5 mm, and probe the fragmentation from 1 pc to 0.01 pc scale. We find that the masses and the sizes of our objects follow $M \sim r^{1.68\pm0.05}$. The results are in agreements with the predictions of Li (2017) where $M \sim r^{5/3}$. Inside each object, the densest structures seem to be centrally condensed, with $\rho(r)\sim r^{-2}$. Our observational results support a scenario where molecular gas in the Milky Way is supported by a turbulence characterized by a constant energy dissipation rate, and gas fragments like clumps and cores are structures which are massive enough to be dynamically detached from the ambient medium., Comment: Accepted for publication in MNRAS

Published
2017
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130. Searching for initial stage of massive star formation around the H II region G18.2-0.3

Author

Zhang, Chuan-Peng, Yuan, Jing-Hua, Xu, Jin-Long, Liu, Xiao-Lan, Yu, Nai-Ping, Li, Nan, He, Li-Ping, Zhang, Guo-Yin, and Wang, Jun-Jie

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Sometimes the early star formation can be found in cold and dense molecular clouds, such as infrared dark cloud (IRDC). Considering star formation often occurs in clustered condition, HII regions may be triggering a new generation of star formation, so we can search for initial stage of massive star formation around HII regions. Based on that above, this work is to introduce one method of how to search for initial stage of massive star formation around HII regions. Towards one sample of the HII region G18.2-0.3, multiwavelength observations are carried out to investigate its physical condition. In contrast and analysis, we find three potential initial stages of massive star formation, suggesting that it is feasible to search for initial stage of massive star formation around HII regions., Comment: 15 pages, 8 figures, 5 tables. Accepted by Research in Astron. Astrophys

Published
2017
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133. A multi-wavelength observation and investigation of six infrared dark clouds

Author

Zhang, Chuan-Peng, Yuan, Jing-Hua, Li, Guang-Xing, Zhou, Jian-Jun, and Wang, Jun-Jie

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Context. Infrared dark clouds (IRDCs) are ubiquitous in the Milky Way, yet they play a crucial role in breeding newly-formed stars. Aims. With the aim of further understanding the dynamics, chemistry, and evolution of IRDCs, we carried out multi-wavelength observations on a small sample. Methods. We performed new observations with the IRAM 30 m and CSO 10.4 m telescopes, with tracers ${\rm HCO^+}$, HCN, ${\rm N_2H^+}$, ${\rm C^{18}O}$, DCO$^+$, SiO, and DCN toward six IRDCs G031.97+00.07, G033.69-00.01, G034.43+00.24, G035.39-00.33, G038.95-00.47, and G053.11+00.05. Results. We investigated 44 cores including 37 cores reported in previous work and seven newly-identified cores. Toward the dense cores, we detected 6 DCO$^+$, and 5 DCN lines. Using pixel-by-pixel spectral energy distribution (SED) fits of the $\textit{Herschel}$ 70 to 500 $\mu$m, we obtained dust temperature and column density distributions of the IRDCs. We found that ${\rm N_2H^+}$ emission has a strong correlation with the dust temperature and column density distributions, while ${\rm C^{18}O}$ showed the weakest correlation. It is suggested that ${\rm N_2H^+}$ is indeed a good tracer in very dense conditions, but ${\rm C^{18}O}$ is an unreliable one, as it has a relatively low critical density and is vulnerable to freezing-out onto the surface of cold dust grains. The dynamics within IRDCs are active, with infall, outflow, and collapse; the spectra are abundant especially in deuterium species. Conclusions. We observe many blueshifted and redshifted profiles, respectively, with ${\rm HCO^+}$ and ${\rm C^{18}O}$ toward the same core. This case can be well explained by model "envelope expansion with core collapse (EECC)"., Comment: 24 pages, 11 figures, 4 tables. To be published in A&A. The resolutions of the pictures are cut down

Published
2016
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134. An investigation of a magnetic cataclysmic variable with a period of 14.1 ks

Author

Wang, Song, Bai, Yu, Zhang, Chuan-peng, and Liu, Ji-feng

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Magnetic cataclysmic variables (CVs) contain a white dwarf with magnetic field strong enough to control the accretion flow from a late type secondary. In this paper, we discover a magnetic CV (CXOGSG J215544.4+380116) from the $Chandra$ archive data. The X-ray light curves show a significant period of 14.1 ks, and the X-ray spectra can be described by a multi-temperature hot thermal plasma, suggesting the source as a magnetic CV. The broad dip in the X-ray light curve is due to the eclipse of the primary magnetic pole, and the additional dip in the bright phase of the soft and medium bands may be caused by the accretion stream crossing our line of sight to the primary pole. Follow-up optical spectra show features of an M2--M4 dwarf dominating the red band and a WD which is responsible for the weak upturn in the blue band. The mass ($\sim$ 0.4 $M_{\odot}$) and radius ($\sim$ 0.4 $R_{\odot}$) for the M dwarf are obtained using CV evolution models and empirical relations between the orbital period and the mass/radius. The estimated low X-ray luminosity and accretion rate may suggest the source as a low-accretion-rate polar. In addition, Very Large Array observations reveal a possible radio counterpart to the X-ray source, but with a low significance. Further radio observations with high quality are needed to confirm the radio counterpart and explore the properties of this binary system., Comment: 15 pages, 8 figures, 3 tables. Accepted for publication in RAA

Published
2016
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137. Gas Kinematics and Star Formation in the Filamentary IRDC G34.43+0.24

Author

Xu, Jin-Long, Li, Di, Zhang, Chuan-Peng, Liu, Xiao-Lan, Wang, Jun-Jie, Ning, Chang-Chun, and Ju, Bing-Gang

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We performed a multiwavelength study toward infrared dark cloud (IRDC) G34.43+0.24. New maps of 13CO $J$=1-0 and C18}O J=1-0 were obtained from the Purple Mountain Observatory (PMO) 13.7 m radio telescope. At 8 um (Spitzer - IRAC), IRDC G34.43+0.24 appears to be a dark filament extended by 18 arcmin along the north-south direction. Based on the association with the 870 um and C18O J=1-0 emission, we suggest that IRDC G34.43+0.24 should not be 18 arcmin in length, but extend by 34 arcmin. IRDC G34.43+0.24 contains some massive protostars, UC H II regions, and infrared bubbles. The spatial extend of IRDC G34.43+0.24 is about 37 pc assuming a distance of 3.7 kpc. IRDC G34.43+0.24 has a linear mass density of 1.6*10^{3} M_{sun} pc^{-1}, which is roughly consistent with its critical mass to length ratio. The turbulent motion may help stabilizing the filament against the radial collapse. Both infrared bubbles N61 and N62 show a ringlike structure at 8 um. Particularly, N61 has a double-shell structure, which has expanded into IRDC G34.43+0.24. The outer shell is traced by 8 um and 13}CO J=1-0 emission, while the inner shell is traced by 24 um and 20 cm emission. We suggest that the outer shell (9.9*10^{5} yr) is created by the expansion of H II region G34.172+0.175, while the inner shell (4.1-6.3*10^{5} yr) may be produced by the energetic stellar wind of its central massive star. From GLIMPSE I catalog, we selected some Class I sources with an age of 10^{5} yr. These Class I sources are clustered along the filamentary molecular cloud., Comment: 44 pages, 13 figures, accepted for publication in ApJ

Published
2016
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138. N131: A dust bubble born from the disruption of a gas filament

Author

Zhang, Chuan-Peng, Li, Guang-Xing, Wyrowski, Friedrich, Wang, Jun-Jie, Yuan, Jing-Hua, Xu, Jin-Long, Gong, Yan, Yeh, Cosmos C., and Menten, Karl M.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

OB type stars have strong ionizing radiation, and drive energetic winds. The ultraviolet (UV) radiation from ionizing stars may heat dust and ionize gas to sweep up an expanding bubble shell. This shell may be the result of feedback leading to a new generation of stars. N131 is an infrared dust bubble residing in a molecular filament. We study the formation and fragmentation of this bubble with multi-wavelength dust and gas observations. Towards the bubble N131, we analyzed archival multi-wavelength observations including 3.6, 4.5, 5.8, 8.0, 24, 70, 160, 250, 350, 500 $\mu$m, 1.1 mm, and 21 cm. In addition, we performed new observations of CO (2-1), CO (1-0), and $^{13}$CO (1-0) with the IRAM 30-m telescope. Multi-wavelength dust and gas observations reveal a ringlike shell with compact fragments, two filamentary structures, and a secondary bubble N131-A. The bubble N131 is a rare object with a large hole at 24 $\mu$m and 21 cm in the direction of its center. The dust and gas clumps are compact and might have been compressed at the inner edge of the ringlike shell, while they are extended and might be pre-existing at the outer edge. The column density, excitation temperature, and velocity show a potentially hierarchical distribution from the inner to outer edge of the ringlike shell. We also detected the front and back sides of the secondary bubble N131-A in the direction of its center. The derived Lyman-continuum ionizing photon flux within N131-A is equivalent to an O9.5 star. Based on the above, we suggest that the bubble N131 might be triggered by the strong stellar winds from a group of massive stars inside the bubble. We propose a scenario in which the bubble N131 forms from the disruption of a gas filament by expansion of HII region, strong stellar winds, and fragments under self-gravity., Comment: Comments are welcome. 13 pages, 11 figures

Published
2015
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141. A multi-country test of brief reappraisal interventions on emotions during the COVID-19 pandemic

Author

Wang, Ke, Goldenberg, Amit, Dorison, Charles A., Miller, Jeremy K., Uusberg, Andero, Lerner, Jennifer S., Gross, James J., Agesin, Bamikole Bamikole, Bernardo, Márcia, Campos, Olatz, Eudave, Luis, Grzech, Karolina, Ozery, Daphna Hausman, Jackson, Emily A., Garcia, Elkin Oswaldo Luis, Drexler, Shira Meir, Jurković, Anita Penić, Rana, Kafeel, Wilson, John Paul, Antoniadi, Maria, Desai, Kermeka, Gialitaki, Zoi, Kushnir, Elizaveta, Nadif, Khaoula, Bravo, Olalla Niño, Nauman, Rafia, Oosterlinck, Marlies, Pantazi, Myrto, Pilecka, Natalia, Szabelska, Anna, van Steenkiste, I. M. M., Filip, Katarzyna, Bozdoc, Andreea Ioana, Marcu, Gabriela Mariana, Agadullina, Elena, Adamkovič, Matúš, Roczniewska, Marta, Reyna, Cecilia, Kassianos, Angelos P., Westerlund, Minja, Ahlgren, Lina, Pöntinen, Sara, Adetula, Gabriel Agboola, Dursun, Pinar, Arinze, Azuka Ikechukwu, Arinze, Nwadiogo Chisom, Ogbonnaya, Chisom Esther, Ndukaihe, Izuchukwu L. G., Dalgar, Ilker, Akkas, Handan, Macapagal, Paulo Manuel, Lewis, Savannah, Metin-Orta, Irem, Foroni, Francesco, Willis, Megan, Santos, Anabela Caetano, Mokady, Aviv, Reggev, Niv, Kurfali, Merve A., Vasilev, Martin R., Nock, Nora L., Parzuchowski, Michal, Espinoza Barría, Mauricio F., Vranka, Marek, Kohlová, Markéta Braun, Ropovik, Ivan, Harutyunyan, Mikayel, Wang, Chunhui, Yao, Elvin, Becker, Maja, Manunta, Efisio, Kaminski, Gwenael, Boudesseu, Jordane, Marko, Dafne, Evans, Kortnee, Lewis, David M. G., Findor, Andrej, Landry, Anais Thibault, Aruta, John Jamir Benzon, Ortiz, Manuel S., Vally, Zahir, Pronizius, Ekaterina, Voracek, Martin, Lamm, Claus, Grinberg, Maurice, Li, Ranran, Valentova, Jaroslava Varella, Mioni, Giovanna, Cellini, Nicola, Chen, Sau-Chin, Zickfeld, Janis, Moon, Karis, Azab, Habiba, Levy, Neil, Karababa, Alper, Beaudry, Jennifer L., Boucher, Leanne, Collins, W. Matthew, Todsen, Anna Louise, van Schie, Kevin, Vintr, Jáchym, Bavolar, Jozef, Kaliska, Lada, Križanić, Valerija, Samojlenko, Lara, Pourafshari, Razieh, Geiger, Sandra J., Beitner, Julia, Warmelink, Lara, Ross, Robert M., Stephen, Ian D., Hostler, Thomas J., Azouaghe, Soufian, McCarthy, Randy, Szala, Anna, Grano, Caterina, Solorzano, Claudio Singh, Anjum, Gulnaz, Jimenez-Leal, William, Bradford, Maria, Pérez, Laura Calderón, Cruz Vásquez, Julio E., Galindo-Caballero, Oscar J., Vargas-Nieto, Juan Camilo, Kácha, Ondřej, Arvanitis, Alexios, Xiao, Qinyu, Cárcamo, Rodrigo, Zorjan, Saša, Tajchman, Zuzanna, Vilares, Iris, Pavlacic, Jeffrey M., Kunst, Jonas R., Tamnes, Christian K., von Bastian, Claudia C., Atari, Mohammad, Sharifian, MohammadHasan, Hricova, Monika, Kačmár, Pavol, Schrötter, Jana, Rahal, Rima-Maria, Cohen, Noga, FatahModares, Saeideh, Zrimsek, Miha, Zakharov, Ilya, Koehn, Monica A., Esteban-Serna, Celia, Calin-Jageman, Robert J., Krafnick, Anthony J., Štrukelj, Eva, Isager, Peder Mortvedt, Urban, Jan, Silva, Jaime R., Martončik, Marcel, Očovaj, Sanja Batić, Šakan, Dušana, Kuzminska, Anna O., Djordjevic, Jasna Milosevic, Almeida, Inês A. T., Ferreira, Ana, Lazarevic, Ljiljana B., Manley, Harry, Ricaurte, Danilo Zambrano, Monteiro, Renan P., Etabari, Zahra, Musser, Erica, Dunleavy, Daniel, Chou, Weilun, Godbersen, Hendrik, Ruiz-Fernández, Susana, Reeck, Crystal, Batres, Carlota, Kirgizova, Komila, Muminov, Abdumalik, Azevedo, Flavio, Alvarez, Daniela Serrato, Butt, Muhammad Mussaffa, Lee, Jeong Min, Chen, Zhang, Verbruggen, Frederick, Ziano, Ignazio, Tümer, Murat, Charyate, Abdelilah C. A., Dubrov, Dmitrii, Tejada Rivera, María del Carmen M. C., Aberson, Christopher, Pálfi, Bence, Maldonado, Mónica Alarcón, Hubena, Barbora, Sacakli, Asli, Ceary, Chris D., Richard, Karley L., Singer, Gage, Perillo, Jennifer T., Ballantyne, Tonia, Cyrus-Lai, Wilson, Fedotov, Maksim, Du, Hongfei, Wielgus, Magdalena, Pit, Ilse L., Hruška, Matej, Sousa, Daniela, Aczel, Balazs, Hajdu, Nandor, Szaszi, Barnabas, Adamus, Sylwia, Barzykowski, Krystian, Micheli, Leticia, Schmidt, Nadya-Daniela, Zsido, Andras N., Paruzel-Czachura, Mariola, Muda, Rafał, Bialek, Michal, Kowal, Marta, Sorokowska, Agnieszka, Misiak, Michal, Mola, Débora, Ortiz, María Victoria, Correa, Pablo Sebastián, Belaus, Anabel, Muchembled, Fany, Ribeiro, Rafael R., Arriaga, Patricia, Oliveira, Raquel, Vaughn, Leigh Ann, Szwed, Paulina, Kossowska, Małgorzata, Czarnek, Gabriela, Kielińska, Julita, Antazo, Benedict, Betlehem, Ruben, Stieger, Stefan, Nilsonne, Gustav, Simonovic, Nicolle, Taber, Jennifer, Gourdon-Kanhukamwe, Amélie, Domurat, Artur, Ihaya, Keiko, Yamada, Yuki, Urooj, Anum, Gill, Tripat, Čadek, Martin, Bylinina, Lisa, Messerschmidt, Johanna, Kurfalı, Murathan, Adetula, Adeyemi, Baklanova, Ekaterina, Albayrak-Aydemir, Nihan, Kappes, Heather B., Gjoneska, Biljana, House, Thea, Jones, Marc V., Berkessel, Jana B., Chopik, William J., Çoksan, Sami, Seehuus, Martin, Khaoudi, Ahmed, Bokkour, Ahmed, El Arabi, Kanza Ait, Djamai, Ikhlas, Iyer, Aishwarya, Parashar, Neha, Adiguzel, Arca, Kocalar, Halil Emre, Bundt, Carsten, Norton, James O., Papadatou-Pastou, Marietta, De la Rosa-Gomez, Anabel, Ankushev, Vladislav, Bogatyreva, Natalia, Grigoryev, Dmitry, Ivanov, Aleksandr, Prusova, Irina, Romanova, Marina, Sarieva, Irena, Terskova, Maria, Hristova, Evgeniya, Kadreva, Veselina Hristova, Janak, Allison, Schei, Vidar, Sverdrup, Therese E., Askelund, Adrian Dahl, Pineda, Lina Maria Sanabria, Krupić, Dajana, Levitan, Carmel A., Johannes, Niklas, Ouherrou, Nihal, Say, Nicolas, Sinkolova, Sladjana, Janjić, Kristina, Stojanovska, Marija, Stojanovska, Dragana, Khosla, Meetu, Thomas, Andrew G., Kung, Franki Y. H., Bijlstra, Gijsbert, Mosannenzadeh, Farnaz, Balci, Busra Bahar, Reips, Ulf-Dietrich, Baskin, Ernest, Ishkhanyan, Byurakn, Czamanski-Cohen, Johanna, Dixson, Barnaby James Wyld, Moreau, David, Sutherland, Clare A. M., Chuan-Peng, Hu, Noone, Chris, Flowe, Heather, Anne, Michele, Janssen, Steve M. J., Topor, Marta, Majeed, Nadyanna M., Kunisato, Yoshihiko, Yu, Karen, Daches, Shimrit, Hartanto, Andree, Vdovic, Milica, Anton-Boicuk, Lisa, Forbes, Paul A. G., Kamburidis, Julia, Marinova, Evelina, Nedelcheva-Datsova, Mina, Rachev, Nikolay R., Stoyanova, Alina, Schmidt, Kathleen, Suchow, Jordan W., Koptjevskaja-Tamm, Maria, Jernsäther, Teodor, Olofsson, Jonas K., Bialobrzeska, Olga, Marszalek, Magdalena, Tatachari, Srinivasan, Afhami, Reza, Law, Wilbert, Antfolk, Jan, Žuro, Barbara, Van Doren, Natalia, Soto, Jose A., Searston, Rachel, Miranda, Jacob, Damnjanović, Kaja, Yeung, Siu Kit, Krupić, Dino, Hoyer, Karlijn, Jaeger, Bastian, Ren, Dongning, Pfuhl, Gerit, Klevjer, Kristoffer, Corral-Frías, Nadia S., Frias-Armenta, Martha, Lucas, Marc Y., Torres, Adriana Olaya, Toro, Mónica, Delgado, Lady Grey Javela, Vega, Diego, Solas, Sara Álvarez, Vilar, Roosevelt, Massoni, Sébastien, Frizzo, Thomas, Bran, Alexandre, Vaidis, David C., Vieira, Luc, Paris, Bastien, Capizzi, Mariagrazia, Coelho, Gabriel Lins de Holanda, Greenburgh, Anna, Whitt, Cassie M., Tullett, Alexa M., Du, Xinkai, Volz, Leonhard, Bosma, Minke Jasmijn, Karaarslan, Cemre, Sarıoğuz, Eylül, Allred, Tara Bulut, Korbmacher, Max, Colloff, Melissa F., Lima, Tiago J. S., Ribeiro, Matheus Fernando Felix, Verharen, Jeroen P. H., Karekla, Maria, Karashiali, Christiana, Sunami, Naoyuki, Jaremka, Lisa M., Storage, Daniel, Habib, Sumaiya, Studzinska, Anna, Hanel, Paul H. P., Holford, Dawn Liu, Sirota, Miroslav, Wolfe, Kelly, Chiu, Faith, Theodoropoulou, Andriana, Ahn, El Rim, Lin, Yijun, Westgate, Erin C., Brohmer, Hilmar, Hofer, Gabriela, Dujols, Olivier, Vezirian, Kevin, Feldman, Gilad, Travaglino, Giovanni A., Ahmed, Afroja, Li, Manyu, Bosch, Jasmijn, Torunsky, Nathan, Bai, Hui, Manavalan, Mathi, Song, Xin, Walczak, Radoslaw B., Zdybek, Przemysław, Friedemann, Maja, Rosa, Anna Dalla, Kozma, Luca, Alves, Sara G., Lins, Samuel, Pinto, Isabel R., Correia, Rita C., Babinčák, Peter, Banik, Gabriel, Rojas-Berscia, Luis Miguel, Varella, Marco A. C., Uttley, Jim, Beshears, Julie E., Thommesen, Katrine Krabbe, Behzadnia, Behzad, Geniole, Shawn N., Silan, Miguel A., Maturan, Princess Lovella G., Vilsmeier, Johannes K., Tran, Ulrich S., Izquierdo, Sara Morales, Mensink, Michael C., Sorokowski, Piotr, Groyecka-Bernard, Agata, Radtke, Theda, Adoric, Vera Cubela, Carpentier, Joelle, Özdoğru, Asil Ali, Joy-Gaba, Jennifer A., Hedgebeth, Mattie V., Ishii, Tatsunori, Wichman, Aaron L., Röer, Jan Philipp, Ostermann, Thomas, Davis, William E., Suter, Lilian, Papachristopoulos, Konstantinos, Zabel, Chelsea, Onie, Sandersan, Ebersole, Charles R., Chartier, Christopher R., Mallik, Peter R., Urry, Heather L., Buchanan, Erin M., Coles, Nicholas A., Primbs, Maximilian A., Basnight-Brown, Dana M., IJzerman, Hans, Forscher, Patrick S., and Moshontz, Hannah

Published
2021
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145. Effective substances and molecular mechanisms guided by network pharmacology: An example study of Scrophulariae Radix treatment of hyperthyroidism and thyroid hormone-induced liver and kidney injuries

Author

Sheng, Meng-Yuan, primary, Peng, De-Wei, additional, Peng, Hui-Ming, additional, Zhang, Ya-Li, additional, Xiao, Ling, additional, Zhang, Meng-Ru, additional, Wang, Si-Yu, additional, Zhao, Chuan-Peng, additional, Zhu, Si-Ying, additional, Lu, Jian-Kang, additional, Lin, Li, additional, Huang, Rong, additional, Nie, Jing, additional, and Fang, Jin-Bo, additional

Published
2024
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148. Author Correction: A multi-country test of brief reappraisal interventions on emotions during the COVID-19 pandemic

Author

Wang, Ke, Goldenberg, Amit, Dorison, Charles A., Miller, Jeremy K., Uusberg, Andero, Lerner, Jennifer S., Gross, James J., Agesin, Bamikole Bamikole, Bernardo, Márcia, Campos, Olatz, Eudave, Luis, Grzech, Karolina, Ozery, Daphna Hausman, Jackson, Emily A., Garcia, Elkin Oswaldo Luis, Drexler, Shira Meir, Jurković, Anita Penić, Rana, Kafeel, Wilson, John Paul, Antoniadi, Maria, Desai, Kermeka, Gialitaki, Zoi, Kushnir, Elizaveta, Nadif, Khaoula, Bravo, Olalla Niño, Nauman, Rafia, Oosterlinck, Marlies, Pantazi, Myrto, Pilecka, Natalia, Szabelska, Anna, van Steenkiste, I. M. M., Filip, Katarzyna, Bozdoc, Andreea Ioana, Marcu, Gabriela Mariana, Agadullina, Elena, Adamkovič, Matúš, Roczniewska, Marta, Reyna, Cecilia, Kassianos, Angelos P., Westerlund, Minja, Ahlgren, Lina, Pöntinen, Sara, Adetula, Gabriel Agboola, Dursun, Pinar, Arinze, Azuka Ikechukwu, Arinze, Nwadiogo Chisom, Ogbonnaya, Chisom Esther, Ndukaihe, Izuchukwu L. G., Dalgar, Ilker, Akkas, Handan, Macapagal, Paulo Manuel, Lewis, Savannah, Metin-Orta, Irem, Foroni, Francesco, Willis, Megan, Santos, Anabela Caetano, Mokady, Aviv, Reggev, Niv, Kurfali, Merve A., Vasilev, Martin R., Nock, Nora L., Parzuchowski, Michal, Espinoza Barría, Mauricio F., Vranka, Marek, Kohlová, Markéta Braun, Ropovik, Ivan, Harutyunyan, Mikayel, Wang, Chunhui, Yao, Elvin, Becker, Maja, Manunta, Efisio, Kaminski, Gwenael, Boudesseul, Jordane, Marko, Dafne, Evans, Kortnee, Lewis, David M. G., Findor, Andrej, Landry, Anais Thibault, Aruta, John Jamir Benzon, Ortiz, Manuel S., Vally, Zahir, Pronizius, Ekaterina, Voracek, Martin, Lamm, Claus, Grinberg, Maurice, Li, Ranran, Valentova, Jaroslava Varella, Mioni, Giovanna, Cellini, Nicola, Chen, Sau-Chin, Zickfeld, Janis, Moon, Karis, Azab, Habiba, Levy, Neil, Karababa, Alper, Beaudry, Jennifer L., Boucher, Leanne, Collins, W. Matthew, Todsen, Anna Louise, van Schie, Kevin, Vintr, Jáchym, Bavolar, Jozef, Kaliska, Lada, Križanić, Valerija, Samojlenko, Lara, Pourafshari, Razieh, Geiger, Sandra J., Beitner, Julia, Warmelink, Lara, Ross, Robert M., Stephen, Ian D., Hostler, Thomas J., Azouaghe, Soufian, McCarthy, Randy, Szala, Anna, Grano, Caterina, Solorzano, Claudio Singh, Anjum, Gulnaz, Jimenez-Leal, William, Bradford, Maria, Pérez, Laura Calderón, Cruz Vásquez, Julio E., Galindo-Caballero, Oscar J., Vargas-Nieto, Juan Camilo, Kácha, Ondřej, Arvanitis, Alexios, Xiao, Qinyu, Cárcamo, Rodrigo, Zorjan, Saša, Tajchman, Zuzanna, Vilares, Iris, Pavlacic, Jeffrey M., Kunst, Jonas R., Tamnes, Christian K., von Bastian, Claudia C., Atari, Mohammad, Sharifian, MohammadHasan, Hricova, Monika, Kačmár, Pavol, Schrötter, Jana, Rahal, Rima-Maria, Cohen, Noga, FatahModares, Saeideh, Zrimsek, Miha, Zakharov, Ilya, Koehn, Monica A., Esteban-Serna, Celia, Calin-Jageman, Robert J., Krafnick, Anthony J., Štrukelj, Eva, Isager, Peder Mortvedt, Urban, Jan, Silva, Jaime R., Martončik, Marcel, Očovaj, Sanja Batić, Šakan, Dušana, Kuzminska, Anna O., Djordjevic, Jasna Milosevic, Almeida, Inês A. T., Ferreira, Ana, Lazarevic, Ljiljana B., Manley, Harry, Ricaurte, Danilo Zambrano, Monteiro, Renan P., Etabari, Zahra, Musser, Erica, Dunleavy, Daniel, Chou, Weilun, Godbersen, Hendrik, Ruiz-Fernández, Susana, Reeck, Crystal, Batres, Carlota, Kirgizova, Komila, Muminov, Abdumalik, Azevedo, Flavio, Alvarez, Daniela Serrato, Butt, Muhammad Mussaffa, Lee, Jeong Min, Chen, Zhang, Verbruggen, Frederick, Ziano, Ignazio, Tümer, Murat, Charyate, Abdelilah C. A., Dubrov, Dmitrii, Tejada Rivera, María del Carmen M. C., Aberson, Christopher, Pálfi, Bence, Maldonado, Mónica Alarcón, Hubena, Barbora, Sacakli, Asli, Ceary, Chris D., Richard, Karley L., Singer, Gage, Perillo, Jennifer T., Ballantyne, Tonia, Cyrus-Lai, Wilson, Fedotov, Maksim, Du, Hongfei, Wielgus, Magdalena, Pit, Ilse L., Hruška, Matej, Sousa, Daniela, Aczel, Balazs, Hajdu, Nandor, Szaszi, Barnabas, Adamus, Sylwia, Barzykowski, Krystian, Micheli, Leticia, Schmidt, Nadya-Daniela, Zsido, Andras N., Paruzel-Czachura, Mariola, Muda, Rafał, Bialek, Michal, Kowal, Marta, Sorokowska, Agnieszka, Misiak, Michal, Mola, Débora, Ortiz, María Victoria, Correa, Pablo Sebastián, Belaus, Anabel, Muchembled, Fany, Ribeiro, Rafael R., Arriaga, Patricia, Oliveira, Raquel, Vaughn, Leigh Ann, Szwed, Paulina, Kossowska, Małgorzata, Czarnek, Gabriela, Kielińska, Julita, Antazo, Benedict, Betlehem, Ruben, Stieger, Stefan, Nilsonne, Gustav, Simonovic, Nicolle, Taber, Jennifer, Gourdon-Kanhukamwe, Amélie, Domurat, Artur, Ihaya, Keiko, Yamada, Yuki, Urooj, Anum, Gill, Tripat, Čadek, Martin, Bylinina, Lisa, Messerschmidt, Johanna, Kurfalı, Murathan, Adetula, Adeyemi, Baklanova, Ekaterina, Albayrak-Aydemir, Nihan, Kappes, Heather B., Gjoneska, Biljana, House, Thea, Jones, Marc V., Berkessel, Jana B., Chopik, William J., Çoksan, Sami, Seehuus, Martin, Khaoudi, Ahmed, Bokkour, Ahmed, El Arabi, Kanza Ait, Djamai, Ikhlas, Iyer, Aishwarya, Parashar, Neha, Adiguzel, Arca, Kocalar, Halil Emre, Bundt, Carsten, Norton, James O., Papadatou-Pastou, Marietta, De la Rosa-Gomez, Anabel, Ankushev, Vladislav, Bogatyreva, Natalia, Grigoryev, Dmitry, Ivanov, Aleksandr, Prusova, Irina, Romanova, Marina, Sarieva, Irena, Terskova, Maria, Hristova, Evgeniya, Kadreva, Veselina Hristova, Janak, Allison, Schei, Vidar, Sverdrup, Therese E., Askelund, Adrian Dahl, Pineda, Lina Maria Sanabria, Krupić, Dajana, Levitan, Carmel A., Johannes, Niklas, Ouherrou, Nihal, Say, Nicolas, Sinkolova, Sladjana, Janjić, Kristina, Stojanovska, Marija, Stojanovska, Dragana, Khosla, Meetu, Thomas, Andrew G., Kung, Franki Y. H., Bijlstra, Gijsbert, Mosannenzadeh, Farnaz, Balci, Busra Bahar, Reips, Ulf-Dietrich, Baskin, Ernest, Ishkhanyan, Byurakn, Czamanski-Cohen, Johanna, Dixson, Barnaby James Wyld, Moreau, David, Sutherland, Clare A. M., Chuan-Peng, Hu, Noone, Chris, Flowe, Heather, Anne, Michele, Janssen, Steve M. J., Topor, Marta, Majeed, Nadyanna M., Kunisato, Yoshihiko, Yu, Karen, Daches, Shimrit, Hartanto, Andree, Vdovic, Milica, Anton-Boicuk, Lisa, Forbes, Paul A. G., Kamburidis, Julia, Marinova, Evelina, Nedelcheva-Datsova, Mina, Rachev, Nikolay R., Stoyanova, Alina, Schmidt, Kathleen, Suchow, Jordan W., Koptjevskaja-Tamm, Maria, Jernsäther, Teodor, Olofsson, Jonas K., Bialobrzeska, Olga, Marszalek, Magdalena, Tatachari, Srinivasan, Afhami, Reza, Law, Wilbert, Antfolk, Jan, Žuro, Barbara, Van Doren, Natalia, Soto, Jose A., Searston, Rachel, Miranda, Jacob, Damnjanović, Kaja, Yeung, Siu Kit, Krupić, Dino, Hoyer, Karlijn, Jaeger, Bastian, Ren, Dongning, Pfuhl, Gerit, Klevjer, Kristoffer, Corral-Frías, Nadia S., Frias-Armenta, Martha, Lucas, Marc Y., Torres, Adriana Olaya, Toro, Mónica, Delgado, Lady Grey Javela, Vega, Diego, Solas, Sara Álvarez, Vilar, Roosevelt, Massoni, Sébastien, Frizzo, Thomas, Bran, Alexandre, Vaidis, David C., Vieira, Luc, Paris, Bastien, Capizzi, Mariagrazia, Coelho, Gabriel Lins de Holanda, Greenburgh, Anna, Whitt, Cassie M., Tullett, Alexa M., Du, Xinkai, Volz, Leonhard, Bosma, Minke Jasmijn, Karaarslan, Cemre, Sarıoğuz, Eylül, Allred, Tara Bulut, Korbmacher, Max, Colloff, Melissa F., Lima, Tiago J. S., Ribeiro, Matheus Fernando Felix, Verharen, Jeroen P. H., Karekla, Maria, Karashiali, Christiana, Sunami, Naoyuki, Jaremka, Lisa M., Storage, Daniel, Habib, Sumaiya, Studzinska, Anna, Hanel, Paul H. P., Holford, Dawn Liu, Sirota, Miroslav, Wolfe, Kelly, Chiu, Faith, Theodoropoulou, Andriana, Ahn, El Rim, Lin, Yijun, Westgate, Erin C., Brohmer, Hilmar, Hofer, Gabriela, Dujols, Olivier, Vezirian, Kevin, Feldman, Gilad, Travaglino, Giovanni A., Ahmed, Afroja, Li, Manyu, Bosch, Jasmijn, Torunsky, Nathan, Bai, Hui, Manavalan, Mathi, Song, Xin, Walczak, Radoslaw B., Zdybek, Przemysław, Friedemann, Maja, Rosa, Anna Dalla, Kozma, Luca, Alves, Sara G., Lins, Samuel, Pinto, Isabel R., Correia, Rita C., Babinčák, Peter, Banik, Gabriel, Rojas-Berscia, Luis Miguel, Varella, Marco A. C., Uttley, Jim, Beshears, Julie E., Thommesen, Katrine Krabbe, Behzadnia, Behzad, Geniole, Shawn N., Silan, Miguel A., Maturan, Princess Lovella G., Vilsmeier, Johannes K., Tran, Ulrich S., Izquierdo, Sara Morales, Mensink, Michael C., Sorokowski, Piotr, Groyecka-Bernard, Agata, Radtke, Theda, Adoric, Vera Cubela, Carpentier, Joelle, Özdoğru, Asil Ali, Joy-Gaba, Jennifer A., Hedgebeth, Mattie V., Ishii, Tatsunori, Wichman, Aaron L., Röer, Jan Philipp, Ostermann, Thomas, Davis, William E., Suter, Lilian, Papachristopoulos, Konstantinos, Zabel, Chelsea, Onie, Sandersan, Ebersole, Charles R., Chartier, Christopher R., Mallik, Peter R., Urry, Heather L., Buchanan, Erin M., Coles, Nicholas A., Primbs, Maximilian A., Basnight-Brown, Dana M., IJzerman, Hans, Forscher, Patrick S., and Moshontz, Hannah

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2022
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