Search

Your search keyword '"Arzoumanian, Doris"' showing total 41 results
Start Over Author "Arzoumanian, Doris" Publication Year Range Last 3 years
41 results on '"Arzoumanian, Doris"'

1. The JCMT BISTRO Survey: The Magnetic Fields of the IC 348 Star-forming Region

Author

Choi, Youngwoo, Kwon, Woojin, Pattle, Kate, Arzoumanian, Doris, Bourke, Tyler L., Hoang, Thiem, Hwang, Jihye, Koch, Patrick M., Sadavoy, Sarah, Bastien, Pierre, Furuya, Ray, Lai, Shih-Ping, Qiu, Keping, Ward-Thompson, Derek, Berry, David, Byun, Do-Young, Chen, Huei-Ru Vivien, Chen, Wen Ping, Chen, Mike, Chen, Zhiwei, Ching, Tao-Chung, Cho, Jungyeon, Choi, Minho, Choi, Yunhee, Coudé, Simon, Chrysostomou, Antonio, Chung, Eun Jung, Dai, Sophia, Debattista, Victor, Di Francesco, James, Diep, Pham Ngoc, Doi, Yasuo, Duan, Hao-Yuan, Duan, Yan, Eswaraiah, Chakali, Fanciullo, Lapo, Fiege, Jason, Fissel, Laura M., Franzmann, Erica, Friberg, Per, Friesen, Rachel, Fuller, Gary, Gledhill, Tim, Graves, Sarah, Greaves, Jane, Griffin, Matt, Gu, Qilao, Han, Ilseung, Hasegawa, Tetsuo, Houde, Martin, Hull, Charles L. H., Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Johnstone, Doug, Karoly, Janik, Könyves, Vera, Kang, Ji-hyun, Lacaille, Kevin, Law, Chi-Yan, Lee, Chang Won, Lee, Hyeseung, Lee, Chin-Fei, Lee, Jeong-Eun, Lee, Sang-Sung, Li, Dalei, Li, Di, Li, Guangxing, Li, Hua-bai, Lin, Sheng-Jun, Liu, Hong-Li, Liu, Tie, Liu, Sheng-Yuan, Liu, Junhao, Longmore, Steven, Lu, Xing, Lyo, A-Ran, Mairs, Steve, Matsumura, Masafumi, Matthews, Brenda, Moriarty-Schieven, Gerald, Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ngoc, Nguyen Bich, Ohashi, Nagayoshi, Onaka, Takashi, Park, Geumsook, Parsons, Harriet, Peretto, Nicolas, Priestley, Felix, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Jonathan, Rawlings, Mark, Retter, Brendan, Richer, John, Rigby, Andrew, Saito, Hiro, Savini, Giorgio, Seta, Masumichi, Sharma, Ekta, Shimajiri, Yoshito, Shinnaga, Hiroko, Soam, Archana, Kang, Miju, Kataoka, Akimasa, Kawabata, Koji, Kemper, Francisca, Kim, Jongsoo, Kim, Shinyoung, Kim, Gwanjeong, Kim, Kyoung Hee, Kim, Mi-Ryang, Kim, Kee-Tae, Kim, Hyosung, Kirchschlager, Florian, Kirk, Jason, Kobayashi, Masato I. N., Kusune, Takayoshi, Kwon, Jungmi, Tamura, Motohide, Tang, Ya-Wen, Tang, Xindi, Tomisaka, Kohji, Tsukamoto, Yusuke, Viti, Serena, Wang, Hongchi, Wang, Jia-Wei, Wu, Jintai, Xie, Jinjin, Yang, Meng-Zhe, Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Guoyin, Zhang, Yapeng, Zhang, Chuan-Peng, Zhou, Jianjun, Zhu, Lei, de Looze, Ilse, André, Philippe, Dowell, C. Darren, Eden, David, Eyres, Stewart, Falle, Sam, Gouellec, Valentin J. M. Le, Poidevin, Frédérick, and van Loo, Sven

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present 850 $\mu$m polarization observations of the IC 348 star-forming region in the Perseus molecular cloud as part of the B-fields In STar-forming Region Observation (BISTRO) survey. We study the magnetic properties of two cores (HH 211 MMS and IC 348 MMS) and a filamentary structure of IC 348. We find that the overall field tends to be more perpendicular than parallel to the filamentary structure of the region. The polarization fraction decreases with intensity, and we estimate the trend by power-law and the mean of the Rice distribution fittings. The power indices for the cores are much smaller than 1, indicative of possible grain growth to micron size in the cores. We also measure the magnetic field strengths of the two cores and the filamentary area separately by applying the Davis-Chandrasekhar-Fermi method and its alternative version for compressed medium. The estimated mass-to-flux ratios are 0.45-2.20 and 0.63-2.76 for HH 211 MMS and IC 348 MMS, respectively, while the ratios for the filament is 0.33-1.50. This result may suggest that the transition from subcritical to supercritical conditions occurs at the core scale ($\sim$ 0.05 pc) in the region. In addition, we study the energy balance of the cores and find that the relative strength of turbulence to the magnetic field tends to be stronger for IC 348 MMS than HH 211 MMS. The result could potentially explain the different configurations inside the two cores: a single protostellar system in HH 211 MMS and multiple protostars in IC 348 MMS., Comment: Accepted for publication in ApJ. 21 pages, 12 figures

Published
2024

2. Growth of Massive Molecular Cloud Filament by Accretion Flows. II. New Mechanism to Support a Supercritical Filament against Radial Collapse

Author

Abe, Daisei, Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, and Arzoumanian, Doris

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Observations indicate that dense molecular filamentary clouds are sites of star formation. The filament width determines the fragmentation scale and influences the stellar mass. Therefore, understanding the evolution of filaments and the origin of their properties is important for understanding star formation. Although observations show a universal width of 0.1 pc, theoretical studies predict the contraction of thermally supercritical filaments (> 17 Msun pc-1) due to radial collapse. Through non-ideal magnetohydrodynamics simulations with ambipolar diffusion, we explore the formation and evolution of filaments via slow-shock instability at the front of accretion flows. We reveal that ambipolar diffusion allows the gas in the filament to flow across the magnetic fields around the shock, forming dense blobs behind the concave points of the shock. The blobs transfer momentum that drives internal turbulence. We name this mechanism the "STORM" (Slow-shock-mediated Turbulent flOw Reinforced by Magnetic diffusion). The persistence and efficiency of the turbulence inside the filament are driven by the magnetic field and the ambipolar diffusion effect, respectively. The STORM sustains the width even when the filament reaches very large line masses (~ 100 Msun pc-1)., Comment: 26 pages, 20 figures

Published
2024

3. Relative Alignments Between Magnetic Fields, Velocity Gradients, and Dust Emission Gradients in NGC 1333

Author

Chen, Michael Chun-Yuan, Fissel, Laura M., Sadavoy, Sarah I., Rosolowsky, Erik, Doi, Yasuo, Arzoumanian, Doris, Bastien, Pierre, Coudé, Simon, Di Francesco, James, Friesen, Rachel, Furuya, Ray S., Hwang, Jihye, Inutsuka, Shu-ichiro, Johnstone, Doug, Karoly, Janik, Kwon, Jungmi, Kwon, Woojin, Gouellec, Valentin J. M. Le, Liu, Hong-Li, Mairs, Steve, Onaka, Takashi, Pattle, Kate, Rawlings, Mark G., Tahani, Mehrnoosh, Tamura, Motohide, and Wang, Jia-Wei

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Magnetic fields play an important role in shaping and regulating star formation in molecular clouds. Here, we present one of the first studies examining the relative orientations between magnetic ($B$) fields and the dust emission, gas column density, and velocity centroid gradients on the 0.02 pc (core) scales, using the BISTRO and VLA+GBT observations of the NGC 1333 star-forming clump. We quantified these relative orientations using the Project Rayleigh Statistic (PRS) and found preferential global parallel alignment between the $B$ field and dust emission gradients, consistent with large-scale studies with Planck. No preferential global alignments, however, are found between the $B$ field and velocity gradients. Local PRS calculated for subregions defined by either dust emission or velocity coherence further revealed that the $B$ field does not preferentially align with dust emission gradients in most emission-defined subregions, except in the warmest ones. The velocity-coherent structures, on the other hand, also showed no preferred $B$ field alignments with velocity gradients, except for one potentially bubble-compressed region. Interestingly, the velocity gradient magnitude in NGC 1333 ubiquitously features prominent ripple-like structures that are indicative of magnetohydrodynamic (MHD) waves. Finally, we found $B$ field alignments with the emission gradients to correlate with dust temperature and anticorrelate with column density, velocity dispersion, and velocity gradient magnitude. The latter two anticorrelations suggest that alignments between gas structures and $B$ fields can be perturbed by physical processes that elevate velocity dispersion and velocity gradients, such as infall, accretions, and MHD waves., Comment: Accepted to the Monthly Notices of the Royal Astronomical Society Main Journal

Published
2024

4. Herschel Gould Belt Survey in Taurus. II: A census of dense cores and filaments in the TMC1 region

Author

Kirk, Jason, Ward-Thompson, Derek, Di Francesco, James, André, Philippe, Bresnahan, David, Könyves, Vera, Marsh, Kenneth, Griffin, Matt, Schneider, Nicola, Men'shchikov, A., Palmeirim, Pedro, Bontemps, Sylvain, Arzoumanian, Doris, Benedettini, Milena, and Pezzuto, Stefania

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

We present a catalogue of dense cores and filaments in a $3.8^{\circ}\times2.4^{\circ}$ field around the TMC1 region of the Taurus Molecular Cloud. The catalogue was created using photometric data from the Herschel SPIRE and PACS instruments in the 70 $\mu$m, 160 $\mu$m, 250 $\mu$m, 350 $\mu$m, and 500 $\mu$m continuum bands. Extended structure in the region was reconstructed from a Herschel column density map. Power spectra and PDFs of this structure are presented. The PDF splits into log-normal and power-law forms, with the high-density power-law component associated primarily with the central part of TMC1. The total mass in the mapped region is 2000 M$_\odot$, of which 34% is above an extinction of AV $\sim$ 3 mag -- a level that appears as a break in the PDF and as the minimum column density at which dense cores are found. A total of 35 dense filaments were extracted from the column density map. These have a characteristic FWHM width of 0.07 pc, but the TMC1 filament itself has a mean FWHM of $\sim$ 0.13 pc. The thermally supercritical filaments in the region are aligned orthogonal to the prevailing magnetic field direction. Derived properties for the supercritical TMC1 filament support the scenario of it being relatively young. A catalogue of 44 robust and candidate prestellar cores is created and is assessed to be complete down to 0.1 M$_\odot$. The combined prestellar CMF for the TMC1 and L1495 regions is well fit by a single log-normal distribution and is comparable to the standard IMF., Comment: 21 pages, 23 figures, accepted for publication in MNRAS. For data products see http://gouldbelt-herschel.cea.fr/archives

Published
2024

5. AtLAST Science Overview Report

Author

Booth, Mark, Klaassen, Pamela, Cicone, Claudia, Mroczkowski, Tony, Cordiner, Martin A., Di Mascolo, Luca, Johnstone, Doug, van Kampen, Eelco, Lee, Minju M., Liu, Daizhong, Orlowski-Scherer, John, Saintonge, Amélie, Smith, Matthew W. L., Thelen, Alexander, Wedemeyer, Sven, Akiyama, Kazunori, Andreon, Stefano, Arzoumanian, Doris, Bakx, Tom J. L. C., Bot, Caroline, Bower, Geoffrey, Brajša, Roman, Chen, Chian-Chou, da Cunha, Elisabete, Eden, David, Ettori, Stefano, Gaches, Brandt, Hatziminaoglou, Evanthia, Luppe, Patricia, Magnelli, Benjamin, Marshall, Jonathan P., Montenegro-Montes, Francisco Miguel, Niemack, Michael, Nixon, Conor, de Pater, Imke, Perrott, Yvette, Raimundo, Sandra I., Redaelli, Elena, Richards, Anita, Rybak, Matus, Šarčević, Nikolina, Semenov, Dmitry, Spezzano, Silvia, Srinivasan, Sundar, Stanke, Thomas, Andreani, Paola, Beltrán, Maria T., Butler, Bryan J., Cantalupo, Sebastiano, Dagostino, Miguel Chavez, Duarte-Cabral, Ana, Emonts, Bjorn, Fletcher, Leigh, Gary, Dale E., Gunar, Stanislav, Hacar, Alvaro, Hagedorn, Bendix, Kaminski, Tomek, Kirton, Fiona, de Kleer, Katherine, Kontar, Eduard, Kuan, Yi-Jehng, Lightfoot, John, Lopez-Rodriguez, Enrique, Lundgren, Andreas, Milam, Stefanie N., Mohan, Atul, Moreno, Raphael, Motorina, Galina G., Moullet, Arielle, Pattle, Kate, Pellizzoni, Alberto, Peretto, Nicolas, Ramasawmy, Joanna, Ricci, Claudio, Rigby, Andrew J., Sánchez-Monge, Álvaro, Saberi, Maryam, Shimojo, Masumi, Simionescu, Aurora, Thompson, Mark, Traficante, Alessio, Vignali, Cristian, and White, Stephen M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Submillimeter and millimeter wavelengths provide a unique view of the Universe, from the gas and dust that fills and surrounds galaxies to the chromosphere of our own Sun. Current single-dish facilities have presented a tantalising view of the brightest (sub-)mm sources, and interferometers have provided the exquisite resolution necessary to analyse the details in small fields, but there are still many open questions that cannot be answered with current facilities. In this report we summarise the science that is guiding the design of the Atacama Large Aperture Submillimeter Telescope (AtLAST). We demonstrate how tranformational advances in topics including star formation in high redshift galaxies, the diffuse circumgalactic medium, Galactic ecology, cometary compositions and solar flares motivate the need for a 50m, single-dish telescope with a 1-2 degree field of view and a new generation of highly multiplexed continuum and spectral cameras. AtLAST will have the resolution to drastically lower the confusion limit compared to current single-dish facilities, whilst also being able to rapidly map large areas of the sky and detect extended, diffuse structures. Its high sensitivity and large field of view will open up the field of submillimeter transient science by increasing the probability of serendipitous detections. Finally, the science cases listed here motivate the need for a highly flexible operations model capable of short observations of individual targets, large surveys, monitoring programmes, target of opportunity observations and coordinated observations with other observatories. AtLAST aims to be a sustainable, upgradeable, multipurpose facility that will deliver orders of magnitude increases in sensitivity and mapping speeds over current and planned submillimeter observatories., Comment: 47 pages, 12 figures. For further details on AtLAST see https://atlast.uio.no

Published
2024

6. Atacama Large Aperture Submillimeter Telescope (AtLAST) Science: Our Galaxy

Author

Klaassen, Pamela, Traficante, Alessio, Beltrán, Maria T., Pattle, Kate, Booth, Mark, Lovell, Joshua B., Marshall, Jonathan P., Hacar, Alvaro, Gaches, Brandt A. L., Bot, Caroline, Peretto, Nicolas, Stanke, Thomas, Arzoumanian, Doris, Cabral, Ana Duarte, Duchêne, Gaspard, Eden, David J., Hales, Antonio, Kauffmann, Jens, Luppe, Patricia, Marino, Sebastian, Redaelli, Elena, Rigby, Andrew J., Sánchez-Monge, Álvaro, Schisano, Eugenio, Semenov, Dmitry A., Spezzano, Silvia, Thompson, Mark A., Wyrowski, Friedrich, Cicone, Claudia, Mroczkowski, Tony, Cordiner, Martin A., Di Mascolo, Luca, Johnstone, Doug, van Kampen, Eelco, Lee, Minju M., Liu, Daizhong, Maccarone, Thomas J., Saintonge, Amélie, Smith, Matthew, Thelen, Alexander E., and Wedemeyer, Sven

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

As we learn more about the multi-scale interstellar medium (ISM) of our Galaxy, we develop a greater understanding for the complex relationships between the large-scale diffuse gas and dust in Giant Molecular Clouds (GMCs), how it moves, how it is affected by the nearby massive stars, and which portions of those GMCs eventually collapse into star forming regions. The complex interactions of those gas, dust and stellar populations form what has come to be known as the ecology of our Galaxy. Because we are deeply embedded in the plane of our Galaxy, it takes up a significant fraction of the sky, with complex dust lanes scattered throughout the optically recognisable bands of the Milky Way. These bands become bright at (sub-)millimetre wavelengths, where we can study dust thermal emission and the chemical and kinematic signatures of the gas. To properly study such large-scale environments, requires deep, large area surveys that are not possible with current facilities. Moreover, where stars form, so too do planetary systems, growing from the dust and gas in circumstellar discs, to planets and planetesimal belts. Understanding the evolution of these belts requires deep imaging capable of studying belts around young stellar objects to Kuiper belt analogues around the nearest stars. Here we present a plan for observing the Galactic Plane and circumstellar environments to quantify the physical structure, the magnetic fields, the dynamics, chemistry, star formation, and planetary system evolution of the galaxy in which we live with AtLAST; a concept for a new, 50m single-dish sub-mm telescope with a large field of view which is the only type of facility that will allow us to observe our Galaxy deeply and widely enough to make a leap forward in our understanding of our local ecology., Comment: 27 pages, submitted to Open Research Europe as part of the AtLAST collection: https://open-research-europe.ec.europa.eu/collections/atlast/about

Published
2024
Full Text
View/download PDF

7. Filamentary Network and Magnetic Field Structures Revealed with BISTRO in the High-Mass Star-Forming Region NGC2264 : Global Properties and Local Magnetogravitational Configurations

Author

Wang, Jia-Wei, Koch, Patrick M., Clarke, Seamus D., Fuller, Gary, Peretto, Nicolas, Tang, Ya-Wen, Yen, Hsi-Wei, Lai, Shih-Ping, Ohashi, Nagayoshi, Arzoumanian, Doris, Johnstone, Doug, Furuya, Ray, Inutsuka, Shu-ichiro, Lee, Chang Won, Ward-Thompson, Derek, Gouellec, Valentin J. M. Le, Liu, Hong-Li, Fanciullo, Lapo, Hwang, Jihye, Pattle, Kate, Poidevin, Frédérick, Tahani, Mehrnoosh, Onaka, Takashi, Rawlings, Mark G., Chung, Eun Jung, Liu, Junhao, Lyo, A-Ran, Priestley, Felix, Hoang, Thiem, Tamura, Motohide, Berry, David, Bastien, Pierre, Ching, Tao-Chung, Coudé, Simon, Kwon, Woojin, Chen, Mike, Eswaraiah, Chakali, Soam, Archana, Hasegawa, Tetsuo, Qiu, Keping, Bourke, Tyler L., Byun, Do-Young, Chen, Zhiwei, Chen, Huei-Ru Vivien, Chen, Wen Ping, Cho, Jungyeon, Choi, Minho, Choi, Yunhee, Choi, Youngwoo, Chrysostomou, Antonio, Dai, Sophia, Di Francesco, James, Diep, Pham Ngoc, Doi, Yasuo, Duan, Yan, Duan, Hao-Yuan, Eden, David, Fiege, Jason, Fissel, Laura M., Franzmann, Erica, Friberg, Per, Friesen, Rachel, Gledhill, Tim, Graves, Sarah, Greaves, Jane, Griffin, Matt, Gu, Qilao, Han, Ilseung, Hayashi, Saeko, Houde, Martin, Inoue, Tsuyoshi, Iwasaki, Kazunari, Jeong, Il-Gyo, Könyves, Vera, Kang, Ji-hyun, Kang, Miju, Karoly, Janik, Kataoka, Akimasa, Kawabata, Koji, Khan, Zacariyya, Kim, Mi-Ryang, Kim, Kee-Tae, Kim, Kyoung Hee, Kim, Shinyoung, Kim, Jongsoo, Kim, Hyosung, Kim, Gwanjeong, Kirchschlager, Florian, Kirk, Jason, Kobayashi, Masato I. N., Kusune, Takayoshi, Kwon, Jungmi, Lacaille, Kevin, Law, Chi-Yan, Lee, Sang-Sung, Lee, Hyeseung, Lee, Jeong-Eun, Lee, Chin-Fei, Li, Dalei, Li, Hua-bai, Li, Guangxing, Li, Di, Lin, Sheng-Jun, Liu, Tie, Liu, Sheng-Yuan, Lu, Xing, Mairs, Steve, Matsumura, Masafumi, Matthews, Brenda, Moriarty-Schieven, Gerald, Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ngoc, Nguyen Bich, Park, Geumsook, Parsons, Harriet, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Jonathan, Retter, Brendan, Richer, John, Rigby, Andrew, Sadavoy, Sarah, Saito, Hiro, Savini, Giorgio, Seta, Masumichi, Sharma, Ekta, Shimajiri, Yoshito, Shinnaga, Hiroko, Tang, Xindi, Thuong, Hoang Duc, Tomisaka, Kohji, Tram, Le Ngoc, Tsukamoto, Yusuke, Viti, Serena, Wang, Hongchi, Whitworth, Anthony, Wu, Jintai, Xie, Jinjin, Yang, Meng-Zhe, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Chuan-Peng, Zhang, Yapeng, Zhang, Guoyin, Zhou, Jianjun, Zhu, Lei, de Looze, Ilse, André, Philippe, Dowell, C. Darren, Eyres, Stewart, Falle, Sam, Robitaille, Jean-François, and van Loo, Sven

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

We report 850 $\mu$m continuum polarization observations toward the filamentary high-mass star-forming region NGC 2264, taken as part of the B-fields In STar forming Regions Observations (BISTRO) large program on the James Clerk Maxwell Telescope (JCMT). These data reveal a well-structured non-uniform magnetic field in the NGC 2264C and 2264D regions with a prevailing orientation around 30 deg from north to east. Field strengths estimates and a virial analysis for the major clumps indicate that NGC 2264C is globally dominated by gravity while in 2264D magnetic, gravitational, and kinetic energies are roughly balanced. We present an analysis scheme that utilizes the locally resolved magnetic field structures, together with the locally measured gravitational vector field and the extracted filamentary network. From this, we infer statistical trends showing that this network consists of two main groups of filaments oriented approximately perpendicular to one another. Additionally, gravity shows one dominating converging direction that is roughly perpendicular to one of the filament orientations, which is suggestive of mass accretion along this direction. Beyond these statistical trends, we identify two types of filaments. The type-I filament is perpendicular to the magnetic field with local gravity transitioning from parallel to perpendicular to the magnetic field from the outside to the filament ridge. The type-II filament is parallel to the magnetic field and local gravity. We interpret these two types of filaments as originating from the competition between radial collapsing, driven by filament self-gravity, and the longitudinal collapsing, driven by the region's global gravity., Comment: Accepted for publication in the Astrophysical Journal. 43 pages, 32 figures, and 4 tables (including Appendix)

Published
2024

8. Evolution of the Angular Momentum of Molecular Cloud Cores in Magnetized Molecular Filaments

Author

Misugi, Yoshiaki, Inutsuka, Shu-ichiro, Arzoumanian, Doris, and Tsukamoto, Yusuke

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The angular momentum of molecular cloud cores plays a key role in the star formation process. However, the evolution of the angular momentum of molecular cloud cores formed in magnetized molecular filaments is still unclear. In this paper, we perform three-dimensional magnetohydrodynamics simulations to reveal the effect of the magnetic field on the evolution of the angular momentum of molecular cloud cores formed through filament fragmentation. As a result, we find that the angular momentum decreases by 30% and 50% at the mass scale of 1Msun in the case of weak and strong magnetic field, respectively. By analyzing the torques exerted on fluid elements, we identify the magnetic tension as the dominant process for angular momentum transfer for mass scales < 3Msun for the strong magnetic field case. This critical mass scale can be understood semi-analytically as the timescale of magnetic braking. We show that the anisotropy of the angular momentum transfer due to the presence of strong magnetic field changes the resultant angular momentum of the core only by a factor of two. We also find that the distribution of the angle between the rotation axis and the magnetic field does not show strong alignment even just before the first core formation. Our results also indicate that the variety of the angular momentum of the cores are inherited from the difference of the phase of the initial turbulent velocity field. The variety could contribute to the diversity in size and other properties of protoplanetary disks recently reported by observations., Comment: 25 pages, 17 figures, accepted for publication in The Astrophysical Journal

Published
2023

9. Tomographic Imaging of the Sagittarius Spiral Arm's Magnetic Field Structure

Author

Doi, Yasuo, Nakamura, Kengo, Kawabata, Koji S., Matsumura, Masafumi, Akitaya, Hiroshi, Coudé, Simon, Rodrigues, Claudia V., Kwon, Jungmi, Tamura, Motohide, Tahani, Mehrnoosh, Magalhães, Antonio Mario, Santos-Lima, Reinaldo, Angarita, Yenifer, Versteeg, José, Haverkorn, Marijke, Hasegawa, Tetsuo, Sadavoy, Sarah, Arzoumanian, Doris, and Bastien, Pierre

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The Galactic global magnetic field is thought to play a vital role in shaping Galactic structures such as spiral arms and giant molecular clouds. However, our knowledge of magnetic field structures in the Galactic plane at different distances is limited, as measurements used to map the magnetic field are the integrated effect along the line of sight. In this study, we present the first-ever tomographic imaging of magnetic field structures in a Galactic spiral arm. Using optical stellar polarimetry over a $17' \times 10'$ field of view, we probe the Sagittarius spiral arm. Combining these data with stellar distances from the $Gaia$ mission, we can isolate the contributions of five individual clouds along the line of sight by analyzing the polarimetry data as a function of distance. The observed clouds include a foreground cloud ($d < 200$ pc) and four clouds in the Sagittarius arm at 1.23 kpc, 1.47 kpc, 1.63 kpc, and 2.23 kpc. The column densities of these clouds range from 0.5 to $2.8 \times 10^{21}~\mathrm{cm}^{-2}$. The magnetic fields associated with each cloud show smooth spatial distributions within their observed regions on scales smaller than 10 pc and display distinct orientations. The position angles projected on the plane-of-sky, measured from the Galactic north to east, for the clouds in increasing order of distance are $135^\circ$, $46^\circ$, $58^\circ$, $150^\circ$, and $40^\circ$, with uncertainties of a few degrees. Notably, these position angles deviate significantly from the direction parallel to the Galactic plane., Comment: Accepted for publication in ApJ

Published
2023

10. Predicting reliable H$_2$ column density maps from molecular line data using machine learning

Author

Shimajiri, Yoshito, Kawanishi, Yasutomo, Fujita, Shinji, Miyamoto, Yusuke, Ito, Atsushi M., Arzoumanian, Doris, André, Philippe, Nishimura, Atsushi, Tokuda, Kazuki, Kaneko, Hiroyuki, Takekawa, Shunya, Ueda, Shota, Onishi, Toshikazu, Inoue, Tsuyoshi, Nishimoto, Shimpei, and Yoneda, Ryuki

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The total mass estimate of molecular clouds suffers from the uncertainty in the H$_2$-CO conversion factor, the so-called $X_{\rm CO}$ factor, which is used to convert the $^{12}$CO (1--0) integrated intensity to the H$_2$ column density. We demonstrate the machine learning's ability to predict the H$_2$ column density from the $^{12}$CO, $^{13}$CO, and C$^{18}$O (1--0) data set of four star-forming molecular clouds; Orion A, Orion B, Aquila, and M17. When the training is performed on a subset of each cloud, the overall distribution of the predicted column density is consistent with that of the Herschel column density. The total column density predicted and observed is consistent within 10\%, suggesting that the machine learning prediction provides a reasonable total mass estimate of each cloud. However, the distribution of the column density for values $> \sim 2 \times 10^{22}$ cm$^{-2}$, which corresponds to the dense gas, could not be predicted well. This indicates that molecular line observations tracing the dense gas are required for the training. We also found a significant difference between the predicted and observed column density when we created the model after training the data on different clouds. This highlights the presence of different $X_{\rm CO}$ factors between the clouds, and further training in various clouds is required to correct for these variations. We also demonstrated that this method could predict the column density toward the area not observed by Herschel if the molecular line and column density maps are available for the small portion, and the molecular line data are available for the larger areas., Comment: Accepted for publication in MNRAS

Published
2023

11. The JCMT BISTRO Survey: Studying the Complex Magnetic Field of L43

Author

Karoly, Janik, Ward-Thompson, Derek, Pattle, Kate, Berry, David, Whitworth, Anthony, Kirk, Jason, Bastien, Pierre, Ching, Tao-Chung, Coude, Simon, Hwang, Jihye, Kwon, Woojin, Soam, Archana, Wang, Jia-Wei, Hasegawa, Tetsuo, Lai, Shih-Ping, Qiu, Keping, Arzoumanian, Doris, Bourke, Tyler L., Byun, Do-Young, Chen, Huei-Ru Vivien, Chen, Wen Ping, Chen, Mike, Chen, Zhiwei, Cho, Jungyeon, Choi, Minho, Choi, Youngwoo, Choi, Yunhee, Chrysostomou, Antonio, Chung, Eun Jung, Dai, Sophia, Debattista, Victor, Di Francesco, James, Diep, Pham Ngoc, Doi, Yasuo, Duan, Hao-Yuan, Duan, Yan, Eswaraiah, Chakali, Fanciullo, Lapo, Fiege, Jason, Fissel, Laura M., Franzmann, Erica, Friberg, Per, Friesen, Rachel, Fuller, Gary, Furuya, Ray, Gledhill, Tim, Graves, Sarah, Greaves, Jane, Griffin, Matt, Gu, Qilao, Han, Ilseung, Hoang, Thiem, Houde, Martin, Hull, Charles L. H., Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Johnstone, Doug, Konyves, Vera, Kang, Ji-hyun, Kang, Miju, Kataoka, Akimasa, Kawabata, Koji, Kemper, Francisca, Kim, Jongsoo, Kim, Shinyoung, Kim, Gwanjeong, Kim, Kyoung Hee, Kim, Mi-Ryang, Kim, Kee-Tae, Kim, Hyosung, Kirchschlager, Florian, Kobayashi, Masato I. N., Koch, Patrick M., Kusune, Takayoshi, Kwon, Jungmi, Lacaille, Kevin, Law, Chi-Yan, Lee, Chang Won, Lee, Hyeseung, Lee, Yong-Hee, Lee, Chin-Fei, Lee, Jeong-Eun, Lee, Sang-Sung, Li, Dalei, Li, Di, Li, Guangxing, Li, Hua-bai, Lin, Sheng-Jun, Liu, Hong-Li, Liu, Tie, Liu, Sheng-Yuan, Liu, Junhao, Longmore, Steven, Lu, Xing, Lyo, A-Ran, Mairs, Steve, Matsumura, Masafumi, Matthews, Brenda, Moriarty-Schieven, Gerald, Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ngoc, Nguyen Bich, Ohashi, Nagayoshi, Onaka, Takashi, Park, Geumsook, Parsons, Harriet, Peretto, Nicolas, Priestley, Felix, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Jonathan, Rawlings, Mark, Retter, Brendan, Richer, John, Rigby, Andrew, Sadavoy, Sarah, Saito, Hiro, Savini, Giorgio, Seta, Masumichi, Sharma, Ekta, Shimajiri, Yoshito, Shinnaga, Hiroko, Tahani, Mehrnoosh, Tamura, Motohide, Tang, Ya-Wen, Tang, Xindi, Tomisaka, Kohji, Tram, Le Ngoc, Tsukamoto, Yusuke, Viti, Serena, Wang, Hongchi, Wu, Jintai, Xie, Jinjin, Yang, Meng-Zhe, Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Guoyin, Zhang, Yapeng, Zhang, Chuan-Peng, Zhou, Jianjun, Zhu, Lei, de Looze, Ilse, Andre, Philippe, Dowell, C. Darren, Eden, David, Eyres, Stewart, Falle, Sam, Gouellec, Valentin J. M. Le, Poidevin, Frederick, Robitaille, Jean-Francois, and van Loo, Sven

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present observations of polarized dust emission at 850 $\mu$m from the L43 molecular cloud which sits in the Ophiuchus cloud complex. The data were taken using SCUBA-2/POL-2 on the James Clerk Maxwell Telescope as a part of the BISTRO large program. L43 is a dense ($N_{\rm H_2}\sim 10^{22}$-10$^{23}$ cm$^{-2}$) complex molecular cloud with a submillimetre-bright starless core and two protostellar sources. There appears to be an evolutionary gradient along the isolated filament that L43 is embedded within, with the most evolved source closest to the Sco OB2 association. One of the protostars drives a CO outflow that has created a cavity to the southeast. We see a magnetic field that appears to be aligned with the cavity walls of the outflow, suggesting interaction with the outflow. We also find a magnetic field strength of up to $\sim$160$\pm$30 $\mu$G in the main starless core and up to $\sim$90$\pm$40 $\mu$G in the more diffuse, extended region. These field strengths give magnetically super- and sub-critical values respectively and both are found to be roughly trans-Alfv\'enic. We also present a new method of data reduction for these denser but fainter objects like starless cores., Comment: Accepted for publication in ApJ. 23 pages, 9 figures (7 main text, 2 appendix)

Published
2023
Full Text
View/download PDF

12. Insights on the Sun birth environment in the context of star-cluster formation in hub-filament systems

Author

Arzoumanian, Doris, Arakawa, Sota, Kobayashi, Masato I. N., Iwasaki, Kazunari, Fukada, Kohei, Mori, Shoji, Hirai, Yutaka, Kunitomo, Masanobu, Kumar, M. S. Nanda, and Kokubo, Eiichiro

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

Cylindrical molecular filaments are observed to be the main sites of Sun-like star formation, while massive stars form in dense hubs, at the junction of multiple filaments. The role of hub-filament configurations has not been discussed yet in relation to the birth environment of the solar system and to infer the origin of isotopic ratios of Short-Lived Radionuclides (SLR, such as $^{26}$Al) of Calcium-Aluminum-rich Inclusions (CAIs) observed in meteorites. In this work, we present simple analytical estimates of the impact of stellar feedback on the young solar system forming along a filament of a hub-filament system. We find that the host filament can shield the young solar system from the stellar feedback, both during the formation and evolution of stars (stellar outflow, wind, and radiation) and at the end of their life (supernovae). We show that the young solar system formed along a dense filament can be enriched with supernova ejecta (e.g., $^{26}$Al) during the formation timescale of CAIs. We also propose that the streamers recently observed around protostars may be channeling the SLR-rich material onto the young solar system. We conclude that considering hub-filament configurations as the birth environment of the Sun is important when deriving theoretical models explaining the observed properties of the solar system., Comment: Accepted for publication in The Astrophysical Journal Letters

Published
2023
Full Text
View/download PDF

13. On the 3D Curvature and Dynamics of the Musca filament

Author

Kaminsky, Aidan, Bonne, Lars, Arzoumanian, Doris, and Coudé, Simon

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Filaments are ubiquitous in the interstellar medium (ISM), yet their formation and evolution remains the topic of intense debate. In order to obtain a more comprehensive view of the 3D morphology and evolution of the Musca filament, we model the C$^{18}$O(2-1) emission along the filament crest with several large-scale velocity field structures. This indicates that Musca is well described by a 3D curved cylindrical filament with longitudinal mass inflow to the center of the filament unless the filament is a transient structure with a lifetime $\lesssim$~0.1 Myr. Gravitational longitudinal collapse models of filaments appear unable to explain the observed velocity field. To better understand these kinematics, we further analyze a map of the C$^{18}$O(2-1) velocity field at the location of SOFIA HAWC+ dust polarization observations that trace the magnetic field in the filament. This unveils an organized magnetic field that is oriented roughly perpendicular to the filament crest. Although the velocity field is also organized, it progressively changes its orientation by more than 90$^{o}$ when laterally crossing the filament crest and thus appears disconnected from the magnetic field in the filament. This strong lateral change of the velocity field over the filament remains unexplained and might be associated with important longitudinal motion in the filament that can be associated to the large-scale kinematics along the filament., Comment: 16 pages, 11 figures, 1 table, accepted in ApJ

Published
2023
Full Text
View/download PDF

14. First BISTRO observations of the dark cloud Taurus L1495A-B10: the role of the magnetic field in the earliest stages of low-mass star formation

Author

Ward-Thompson, Derek, Karoly, Janik, Pattle, Kate, Whitworth, Anthony, Kirk, Jason, Berry, David, Bastien, Pierre, Ching, Tao-Chung, Coude, Simon, Hwang, Jihye, Kwon, Woojin, Soam, Archana, Wang, Jia-Wei, Hasegawa, Tetsuo, Lai, Shih-Ping, Qiu, Keping, Arzoumanian, Doris, Bourke, Tyler L., Byun, Do-Young, Chen, Huei-Ru Vivien, Chen, Wen Ping, Chen, Mike, Chen, Zhiwei, Cho, Jungyeon, Choi, Minho, Choi, Youngwoo, Choi, Yunhee, Chrysostomou, Antonio, Chung, Eun Jung, Dai, Sophia, Debattista, Victor, Di Francesco, James, Diep, Pham Ngoc, Doi, Yasuo, Duan, Hao-Yuan, Duan, Yan, Eswaraiah, Chakali, Fanciullo, Lapo, Fiege, Jason, Fissel, Laura M., Franzmann, Erica, Friberg, Per, Friesen, Rachel, Fuller, Gary, Furuya, Ray, Gledhill, Tim, Graves, Sarah, Greaves, Jane, Griffin, Matt, Gu, Qilao, Han, Ilseung, Hayashi, Saeko, Hoang, Thiem, Houde, Martin, Hull, Charles L. H., Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Johnstone, Doug, Konyves, Vera, Kang, Ji-hyun, Kang, Miju, Kataoka, Akimasa, Kawabata, Koji, Kemper, Francisca, Kim, Jongsoo, Kim, Shinyoung, Kim, Gwanjeong, Kim, Kyoung Hee, Kim, Mi-Ryang, Kim, Kee-Tae, Kim, Hyosung, Kirchschlager, Florian, Kobayashi, Masato I. N., Koch, Patrick M., Kusune, Takayoshi, Kwon, Jungmi, Lacaille, Kevin, Law, Chi-Yan, Lee, Chang Won, Lee, Hyeseung, Lee, Yong-Hee, Lee, Chin-Fei, Lee, Jeong-Eun, Lee, Sang-Sung, Li, Dalei, Li, Di, Li, Guangxing, Li, Hua-bai, Lin, Sheng-Jun, Liu, Hong-Li, Liu, Tie, Liu, Sheng-Yuan, Liu, Junhao, Longmore, Steven, Lu, Xing, Lyo, A-Ran, Mairs, Steve, Matsumura, Masafumi, Matthews, Brenda, Moriarty-Schieven, Gerald, Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ngoc, Nguyen Bich, Ohashi, Nagayoshi, Onaka, Takashi, Park, Geumsook, Parsons, Harriet, Peretto, Nicolas, Priestley, Felix, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Jonathan, Rawlings, Mark, Retter, Brendan, Richer, John, Rigby, Andrew, Sadavoy, Sarah, Saito, Hiro, Savini, Giorgio, Seta, Masumichi, Shimajiri, Yoshito, Shinnaga, Hiroko, Tahani, Mehrnoosh, Tamura, Motohide, Tang, Ya-Wen, Tang, Xindi, Tomisaka, Kohji, Tram, Le Ngoc, Tsukamoto, Yusuke, Viti, Serena, Wang, Hongchi, Wu, Jintai, Xie, Jinjin, Yang, Meng-Zhe, Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Guoyin, Zhang, Yapeng, Zhang, Chuan-Peng, Zhou, Jianjun, Zhu, Lei, de Looze, Ilse, Andre, Philippe, Dowell, C. Darren, Eden, David, Eyres, Stewart, Falle, Sam, Gouellec, Valentin J. M. Le, Poidevin, Frederick, Robitaille, Jean-Francois, and van Loo, Sven

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

We present BISTRO Survey 850 {\mu}m dust emission polarisation observations of the L1495A-B10 region of the Taurus molecular cloud, taken at the JCMT. We observe a roughly triangular network of dense filaments. We detect 9 of the dense starless cores embedded within these filaments in polarisation, finding that the plane-of-sky orientation of the core-scale magnetic field lies roughly perpendicular to the filaments in almost all cases. We also find that the large-scale magnetic field orientation measured by Planck is not correlated with any of the core or filament structures, except in the case of the lowest-density core. We propose a scenario for early prestellar evolution that is both an extension to, and consistent with, previous models, introducing an additional evolutionary transitional stage between field-dominated and matter-dominated evolution, observed here for the first time. In this scenario, the cloud collapses first to a sheet-like structure. Uniquely, we appear to be seeing this sheet almost face-on. The sheet fragments into filaments, which in turn form cores. However, the material must reach a certain critical density before the evolution changes from being field-dominated to being matter-dominated. We measure the sheet surface density and the magnetic field strength at that transition for the first time and show consistency with an analytical prediction that had previously gone untested for over 50 years (Mestel 1965)., Comment: 14 pages, 5 figures. ApJ accepted

Published
2023
Full Text
View/download PDF

15. JCMT BISTRO Observations: Magnetic Field Morphology of Bubbles Associated with NGC 6334

Author

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

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We study the HII regions associated with the NGC 6334 molecular cloud observed in the sub-millimeter and taken as part of the B-fields In STar-forming Region Observations (BISTRO) Survey. In particular, we investigate the polarization patterns and magnetic field morphologies associated with these HII regions. Through polarization pattern and pressure calculation analyses, several of these bubbles indicate that the gas and magnetic field lines have been pushed away from the bubble, toward an almost tangential (to the bubble) magnetic field morphology. In the densest part of NGC 6334, where the magnetic field morphology is similar to an hourglass, the polarization observations do not exhibit observable impact from HII regions. We detect two nested radial polarization patterns in a bubble to the south of NGC 6334 that correspond to the previously observed bipolar structure in this bubble. Finally, using the results of this study, we present steps (incorporating computer vision; circular Hough Transform) that can be used in future studies to identify bubbles that have physically impacted magnetic field lines., Comment: Accepted for publication in Astrophysical Journal (ApJ)

Published
2022
Full Text
View/download PDF

16. Evolution of the Angular Momentum of Molecular Cloud Cores Formed from Filament Fragmentation

Author

Misugi, Yoshiaki, Inutsuka, Shu-ichiro, and Arzoumanian, Doris

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

The angular momentum of molecular cloud cores plays an essential role in the star formation process. However, the time evolution of the angular momentum of molecular cloud cores is still unclear. In this paper, we perform three-dimensional simulations to investigate the time evolution of the angular momentum of molecular cloud cores formed through filament fragmentation. As a result, we find that most of the cores rotate perpendicular to the filament axis. The mean angular momentum of the cores changes by only around 30% during the initial stage of their formation process and then remains almost constant. In addition, we analyze the internal angular momentum structure of the cores. Although the cores gain angular momentum with various directions from the initial turbulent velocity fluctuations of their parent filaments, the angular momentum profile in each core converges to the self-similar solution. We also show that the degree of complexity of the angular momentum structure in a core slightly decreases with time. Moreover, we perform synthetic observations and show that the angular momentum profile measured from the synthetic mean velocity map is compatible with the observations when the filament inclination is taken into account. The present study suggests a theory of core formation from filament fragmentation where the angular momentum structures of the cores are determined by the velocity fluctuation along the filaments and both are compatible with the observations. This theory also provides new insights on the core properties that could be observationally tested., Comment: 42 pages, 35 figures, accepted for publication in ApJ

Published
2022
Full Text
View/download PDF

17. The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament

Author

Ching, Tao-Chung, Qiu, Keping, Li, Di, Ren, Zhiyuan, Lai, Shih-Ping, Berry, David, Pattle, Kate, Furuya, Ray, Ward-Thompson, Derek, Johnstone, Doug, Koch, Patrick M., Lee, Chang Won, Hoang, Thiem, Hasegawa, Tetsuo, Kwon, Woojin, Bastien, Pierre, Eswaraiah, Chakali, Wang, Jia-Wei, Kim, Kyoung Hee, Hwang, Jihye, Soam, Archana, Lyo, A-Ran, Liu, Junhao, Gouellec, Valentin J. M. Le, Arzoumanian, Doris, Whitworth, Anthony, Di Francesco, James, Poidevin, Frederick, Liu, Tie, Coude, Simon, Tahani, Mehrnoosh, Liu, Hong-Li, Onaka, Takashi, Li, Dalei, Tamura, Motohide, Chen, Zhiwei, Tang, Xindi, Kirchschlager, Florian, Bourke, Tyler L., Byun, Do-Young, Chen, Mike, Chen, Huei-Ru Vivien, Chen, Wen Ping, Cho, Jungyeon, Choi, Yunhee, Choi, Youngwoo, Choi, Minho, Chrysostomou, Antonio, Chung, Eun Jung, Dai, Y. Sophia, Diep, Pham Ngoc, Doi, Yasuo, Duan, Yan, Duan, Hao-Yuan, Eden, David, Fanciullo, Lapo, Fiege, Jason, Fissel, Laura M., Franzmann, Erica, Friberg, Per, Friesen, Rachel, Fuller, Gary, Gledhill, Tim, Graves, Sarah, Greaves, Jane, Griffin, Matt, Gu, Qilao, Han, Ilseung, Hayashi, Saeko, Houde, Martin, Hull, Charles L. H., Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Konyves, Vera, Kang, Ji-hyun, Kang, Miju, Karoly, Janik, Kataoka, Akimasa, Kawabata, Koji, Kemper, Francisca, Kim, Jongsoo, Kim, Mi-Ryang, Kim, Shinyoung, Kim, Hyosung, Kim, Kee-Tae, Kim, Gwanjeong, Kirk, Jason, Kobayashi, Masato I. N., Kusune, Takayoshi, Kwon, Jungmi, Lacaille, Kevin, Law, Chi-Yan, Lee, Sang-Sung, Lee, Hyeseung, Lee, Jeong-Eun, Lee, Chin-Fei, Lee, Yong-Hee, Li, Guangxing, Li, Hua-bai, Lin, Sheng-Jun, Liu, Sheng-Yuan, Lu, Xing, Mairs, Steve, Matsumura, Masafumi, Matthews, Brenda, Moriarty-Schieven, Gerald, Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ngoc, Nguyen Bich, Ohashi, Nagayoshi, Park, Geumsook, Parsons, Harriet, Peretto, Nicolas, Priestley, Felix, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Mark, Rawlings, Jonathan, Retter, Brendan, Richer, John, Rigby, Andrew, Sadavoy, Sarah, Saito, Hiro, Savini, Giorgio, Seta, Masumichi, Shimajiri, Yoshito, Shinnaga, Hiroko, Tang, Ya-Wen, Tomisaka, Kohji, Tram, Le Ngoc, Tsukamoto, Yusuke, Viti, Serena, Wang, Hongchi, Wu, Jintai, Xie, Jinjin, Yang, Meng-Zhe, Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Chuan-Peng, Zhang, Yapeng, Zhang, Guoyin, Zhou, Jianjun, Zhu, Lei, de Looze, Ilse, Andre, Philippe, Dowell, C. Darren, Eyres, Stewart, Falle, Sam, Robitaille, Jean-Francois, and van Loo, Sven

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

We present 850 $\mu$m dust polarization observations of the massive DR21 filament from the B-fields In STar-forming Region Observations (BISTRO) survey, using the POL-2 polarimeter and the SCUBA-2 camera on the James Clerk Maxwell Telescope. We detect ordered magnetic fields perpendicular to the parsec-scale ridge of the DR21 main filament. In the sub-filaments, the magnetic fields are mainly parallel to the filamentary structures and smoothly connect to the magnetic fields of the main filament. We compare the POL-2 and Planck dust polarization observations to study the magnetic field structures of the DR21 filament on 0.1--10 pc scales. The magnetic fields revealed in the Planck data are well aligned with those of the POL-2 data, indicating a smooth variation of magnetic fields from large to small scales. The plane-of-sky magnetic field strengths derived from angular dispersion functions of dust polarization are 0.6--1.0 mG in the DR21 filament and $\sim$ 0.1 mG in the surrounding ambient gas. The mass-to-flux ratios are found to be magnetically supercritical in the filament and slightly subcritical to nearly critical in the ambient gas. The alignment between column density structures and magnetic fields changes from random alignment in the low-density ambient gas probed by Planck to mostly perpendicular in the high-density main filament probed by JCMT. The magnetic field structures of the DR21 filament are in agreement with MHD simulations of a strongly magnetized medium, suggesting that magnetic fields play an important role in shaping the DR21 main filament and sub-filaments., Comment: 26 pages, 13 figures, ApJ accepted

Published
2022
Full Text
View/download PDF

18. The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2

Author

Hwang, Jihye, Kim, Jongsoo, Pattle, Kate, Lee, Chang Won, Koch, Patrick M., Johnstone, Doug, Tomisaka, Kohji, Whitworth, Anthony, Furuya, Ray S., Kang, Ji-hyun, Lyo, A-Ran, Chung, Eun Jung, Arzoumanian, Doris, Park, Geumsook, Kwon, Woojin, Kim, Shinyoung, Tamura, Motohide, Kwon, Jungmi, Soam, Archana, Han, Ilseung, Hoang, Thiem, Kim, Kyoung Hee, Onaka, Takashi, Chakali, Eswaraiah, Ward-Thompson, Derek, Liu, Hong-Li, Tang, Xindi, Chen, Wen Ping, Matsumura, Masafumi, Hoang, Thuong Duc, Chen, Zhiwei, Gouellec, Valentin J. M. Le, Kirchschlager, Florian, Poidevin, Fr ed erick, Bastien, Pierre, Qiu, Keping, Hasegawa, Tetsuo, Lai, Shih-Ping, Byun, Do-Young, Cho, Jungyeon, Choi, Minho, Choi, Youngwoo, Choi, Yunhee, Jeong, Il-Gyo, Kang, Miju, Kim, Hyosung, Kim, Kee-tae, Lee, Jeong-Eun, Lee, Sang-sung, Lee, Yong-Hee, Lee, Hyeseung, Kim, Mi-Ryang, Yoo, Hyunju, Yun, Hyeong-Sik, Chen, Mike, Di Francesco, James, Fiege, Jason, Fissel, Laura M., Franzmann, Erica, Houde, Martin, Lacaille, Kevin, Matthews, Brenda, Sadavoy, Sarah, Moriarty-Schieven, Gerald, Tahani, Mehrnoosh, Ching, Tao-Chung, Dai, Y. Sophia, Duan, Yan, Gu, Qilao, Law, Chi-Yan, Li, Dalei, Li, Di, Li, Guangxing, Li, Hua-bai, Liu, Tie, Lu, Xing, Qian, Lei, Wang, Hongchi, Wu, Jintai, Xie, Jinjin, Yuan, Jinghua, Zhang, Chuan-Peng, Zhang, Guoyin, Zhang, Yapeng, Zhou, Jianjun, Zhu, Lei, Berry, David, Friberg, Per, Graves, Sarah, Liu, Junhao, Mairs, Steve, Parsons, Harriet, Rawlings, Mark, Doi, Yasuo, Hayashi, Saeko, Hull, Charles L. H., Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Kataoka, Akimasa, Kawabata, Koji, Kim, Gwanjeong, Kobayashi, Masato I. N., Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Pyo, Tae-Soo, Saito, Hiro, Seta, Masumichi, Shimajiri, Yoshito, Shinnaga, Hiroko, Tsukamoto, Yusuke, Zenko, Tetsuya, Chen, Huei-Ru Vivien, Duan, Hao-Yuan, Fanciullo, Lapo, Kemper, Francisca, Lee, Chin-Fei, Lin, Sheng-Jun, Liu, Sheng-Yuan, Ohashi, Nagayoshi, Rao, Ramprasad, Tang, Ya-Wen, Wang, Jia-Wei, Yang, Meng-Zhe, Yen, Hsi-Wei, Bourke, Tyler L., Chrysostomou, Antonio, Debattista, Victor, Eden, David, Eyres, Stewart, Falle, Sam, Fuller, Gary, Gledhill, Tim, Greaves, Jane, Griffin, Matt, Hatchell, Jennifer, Karoly, Janik, Kirk, Jason, Konyves, Vera, Longmore, Steven, van Loo, Sven, de Looze, Ilse, Peretto, Nicolas, Priestley, Felix, Rawlings, Jonathan, Retter, Brendan, Richer, John, Rigby, Andrew, Savini, Giorgio, Scaife, Anna, Viti, Serena, Diep, Pham Ngoc, Ngoc, Nguyen Bich, Tram, Le Ngoc, Andre, Philippe, Coude, Simon, Dowell, C. Darren, Friesen, Rachel, and Robitaille, Jean-Franc ois

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present and analyze observations of polarized dust emission at 850 $\mu$m towards the central 1 pc $\times$ 1 pc hub-filament structure of Monoceros R2 (Mon R2). The data are obtained with SCUBA-2/POL-2 on the James Clerk Maxwell Telescope (JCMT) as part of the BISTRO (B-fields in Star-forming Region Observations) survey. The orientations of the magnetic field follow the spiral structure of Mon R2, which are well-described by an axisymmetric magnetic field model. We estimate the turbulent component of the magnetic field using the angle difference between our observations and the best-fit model of the underlying large-scale mean magnetic field. This estimate is used to calculate the magnetic field strength using the Davis-Chandrasekhar-Fermi method, for which we also obtain the distribution of volume density and velocity dispersion using a column density map derived from $Herschel$ data and the C$^{18}$O ($J$ = 3-2) data taken with HARP on the JCMT, respectively. We make maps of magnetic field strengths and mass-to-flux ratios, finding that magnetic field strengths vary from 0.02 to 3.64 mG with a mean value of 1.0 $\pm$ 0.06 mG, and the mean critical mass-to-flux ratio is 0.47 $\pm$ 0.02. Additionally, the mean Alfv\'en Mach number is 0.35 $\pm$ 0.01. This suggests that in Mon R2, magnetic fields provide resistance against large-scale gravitational collapse, and magnetic pressure exceeds turbulent pressure. We also investigate the properties of each filament in Mon R2. Most of the filaments are aligned along the magnetic field direction and are magnetically sub-critical., Comment: This paper is accepted to the ApJ

Published
2022
Full Text
View/download PDF

19. From Bubbles and Filaments to Cores and Disks: Gas Gathering and Growth of Structure Leading to the Formation of Stellar Systems

Author

Pineda, Jaime E., Arzoumanian, Doris, André, Philippe, Friesen, Rachel K., Zavagno, Annie, Clarke, Seamus D., Inoue, Tsuyoshi, Chen, Che-Yu, Lee, Yueh-Ning, Soler, Juan D., and Kuffmeier, Michael

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

The study of the development of structures on multiple scales in the cold interstellar medium has experienced rapid expansion in the past decade, on both the observational and the theoretical front. Spectral line studies at (sub-)millimeter wavelengths over a wide range of physical scales have provided unique probes of the kinematics of dense gas in star-forming regions, and have been complemented by extensive, high dynamic range dust continuum surveys of the column density structure of molecular cloud complexes, while dust polarization maps have highlighted the role of magnetic fields. This has been accompanied by increasingly sophisticated numerical simulations including new physics (e.g., supernova driving, cosmic rays, non-ideal magneto-hydrodynamics, radiation pressure) and new techniques such as zoom-in simulations allowing multi-scale studies. Taken together, these new data have emphasized the anisotropic growth of dense structures on all scales, from giant ISM bubbles driven by stellar feedback on $\sim$50-100 pc scales through parsec-scale molecular filaments down to $<$0.1 pc dense cores and $<$1000 au protostellar disks. Combining observations and theory, we present a coherent picture for the formation and evolution of these structures and synthesize a comprehensive physical scenario for the initial conditions and early stages of star and disk formation., Comment: 42 pages, 20 figures. To appear in Protostars and Planets VII, Editors: Shu-ichiro Inutsuka, Yuri Aikawa, Takayuki Muto, Kengo Tomida, and Motohide Tamura. Small changes to match proofs and the updated format

Published
2022

20. B-fields in Star-Forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main

Author

Kwon, Woojin, Pattle, Kate, Sadavoy, Sarah, Hull, Charles L. H., Johnstone, Doug, Ward-Thompson, Derek, Di Francesco, James, Koch, Patrick M., Furuya, Ray, Doi, Yasuo, Gouellec, Valentin J. M. Le, Hwang, Jihye, Lyo, A-Ran, Soam, Archana, Tang, Xindi, Hoang, Thiem, Kirchschlager, Florian, Eswaraiah, Chakali, Fanciullo, Lapo, Kim, Kyoung Hee, Onaka, Takashi, Könyves, Vera, Kang, Ji-hyun, Lee, Chang Won, Tamura, Motohide, Bastien, Pierre, Hasegawa, Tetsuo, Lai, Shih-Ping, Qiu, Keping, Berry, David, Arzoumanian, Doris, Bourke, Tyler L., Byun, Do-Young, Chen, Wen Ping, Chen, Huei-Ru Vivien, Chen, Mike, Chen, Zhiwei, Ching, Tao-Chung, Cho, Jungyeon, Choi, Yunhee, Choi, Minho, Chrysostomou, Antonio, Chung, Eun Jung, Coudé, Simon, Dai, Sophia, Diep, Pham Ngoc, Duan, Yan, Duan, Hao-Yuan, Eden, David, Fiege, Jason, Fissel, Laura M., Franzmann, Erica, Friberg, Per, Friesen, Rachel, Fuller, Gary, Gledhill, Tim, Graves, Sarah, Greaves, Jane, Griffin, Matt, Gu, Qilao, Han, Ilseung, Hatchell, Jennifer, Hayashi, Saeko, Houde, Martin, Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Kang, Miju, Karoly, Janik, Kataoka, Akimasa, Kawabata, Koji, Kemper, Francisca, Kim, Kee-Tae, Kim, Gwanjeong, Kim, Mi-Ryang, Kim, Shinyoung, Kim, Jongsoo, Kirk, Jason, Kobayashi, Masato I. N., Kusune, Takayoshi, Kwon, Jungmi, Lacaille, Kevin, Law, Chi-Yan, Lee, Chin-Fei, Lee, Yong-Hee, Lee, Hyeseung, Lee, Jeong-Eun, Lee, Sang-Sung, Li, Dalei, Li, Di, Li, Hua-bai, Lin, Sheng-Jun, Liu, Sheng-Yuan, Liu, Hong-Li, Liu, Junhao, Liu, Tie, Lu, Xing, Mairs, Steve, Matsumura, Masafumi, Matthews, Brenda, Moriarty-Schieven, Gerald, Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ngoc, Nguyen Bich, Ohashi, Nagayoshi, Park, Geumsook, Parsons, Harriet, Peretto, Nicolas, Priestley, Felix, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Jonathan, Rawlings, Mark G., Retter, Brendan, Richer, John, Rigby, Andrew, Saito, Hiro, Savini, Giorgio, Seta, Masumichi, Shimajiri, Yoshito, Shinnaga, Hiroko, Tahani, Mehrnoosh, Tang, Ya-Wen, Tomisaka, Kohji, Tram, Le Ngoc, Tsukamoto, Yusuke, Viti, Serena, Wang, Hongchi, Wang, Jia-Wei, Whitworth, Anthony, Wu, Jintai, Xie, Jinjin, Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Yapeng, Zhang, Chuan-Peng, Zhang, Guoyin, Zhou, Jianjun, Zhu, Lei, de Looze, Ilse, André, Philippe, Dowell, C. Darren, Eyres, Stewart, Falle, Sam, Robitaille, Jean-François, and van Loo, Sven

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

We present 850 $\mu$m polarimetric observations toward the Serpens Main molecular cloud obtained using the POL-2 polarimeter on the James Clerk Maxwell Telescope (JCMT) as part of the B-fields In STar-forming Region Observations (BISTRO) survey. These observations probe the magnetic field morphology of the Serpens Main molecular cloud on about 6000 au scales, which consists of cores and six filaments with different physical properties such as density and star formation activity. Using the histogram of relative orientation (HRO) technique, we find that magnetic fields are parallel to filaments in less dense filamentary structures where $N_{H_2} < 0.93\times 10^{22}$ cm$^{-2}$ (magnetic fields perpendicular to density gradients), while being perpendicular to filaments (magnetic fields parallel to density gradients) in dense filamentary structures with star formation activity. Moreover, applying the HRO technique to denser core regions, we find that magnetic field orientations change to become perpendicular to density gradients again at $N_{H_2} \approx 4.6 \times 10^{22}$ cm$^{-2}$. This can be interpreted as a signature of core formation. At $N_{H_2} \approx 16 \times 10^{22}$ cm$^{-2}$ magnetic fields change back to being parallel to density gradients once again, which can be understood to be due to magnetic fields being dragged in by infalling material. In addition, we estimate the magnetic field strengths of the filaments ($B_{POS} = 60-300~\mu$G)) using the Davis-Chandrasekhar-Fermi method and discuss whether the filaments are gravitationally unstable based on magnetic field and turbulence energy densities., Comment: 18 pages, accepted for publication in ApJ

Published
2022
Full Text
View/download PDF

21. Velocity structure of the 50 pc-long NGC 6334 filamentary cloud: Hints of multiple compressions and their impact on the cloud properties?

Author

Arzoumanian, Doris, Russeil, Delphine, Zavagno, Annie, Chen, Michael Chun-Yuan, André, Philippe, Inutsuka, Shu-ichiro, Misugi, Yoshiaki, Sánchez-Monge, Álvaro, Schilke, Peter, Men'shchikov, Alexander, and Kohno, Mikito

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

[Abridged] The interstellar medium is observed to be organised in filamentary structures, as well as neutral (HI) and ionized (HII) bubbles. The expanding nature of these bubbles makes them shape their surroundings and possibly play a role in the formation and evolution of interstellar filaments. We present APEX $^{13}$CO and C$^{18}$O(2-1) observations of the NGC 6334 molecular cloud. We investigate the gas velocity structure along and across the 50 pc-long cloud and towards 75 identified velocity-coherent-filaments (VCFs). We measure a wealth of velocity gradients along the VCFs. We derive the column density and velocity power spectra of the VCFs. These power spectra are well represented with power laws showing similar slopes for both quantities (with a mean of about -2), albeit some differ by up to a factor of two. The position velocity diagrams perpendicular to three VCFs show the V-shaped velocity pattern, corresponding to a bent structure in velocity space with the filament at the tip of the V surrounded by an extended structure connected to it with a velocity gradient. This velocity structure is qualitatively similar to that resulting from numerical simulations of filament formation from large-scale compression from propagating shock fronts. In addition, the radial profiles perpendicular to these VCFs hint to small-scale internal impacts from neighbouring HII bubbles. The observed opposite curvature in velocity space towards the VCFs points to various origins of large-scale external compressions from propagating HI bubbles. This suggests the plausible importance of multiple HI compressions, separated in space and time, in the formation and evolution of molecular clouds and their star formation history. These latter atomic compressions due to past and distant star formation events are complemented by the impact of HII bubbles from present time and local star formation activity., Comment: Accepted for publication in Astronomy & Astrophysics

Published
2022
Full Text
View/download PDF

22. Atacama Large Aperture Submillimeter Telescope (AtLAST) science: Our Galaxy

Author

Klaassen, Pamela, primary, Traficante, Alessio, additional, Beltrán, Maria, additional, Pattle, Kate, additional, Booth, Mark, additional, Lovell, Joshua, additional, Marshall, Jonathan, additional, Hacar, Alvaro, additional, Gaches, Brandt, additional, Bot, Caroline, additional, Peretto, Nicolas, additional, Stanke, Thomas, additional, Arzoumanian, Doris, additional, Duarte Cabral, Ana, additional, Duchêne, Gaspard, additional, Eden, David, additional, Hales, Antonio, additional, Kauffmann, Jens, additional, Luppe, Patricia, additional, Marino, Sebastian, additional, Redaelli, Elena, additional, Rigby, Andrew, additional, Sánchez-Monge, Álvaro, additional, Schisano, Eugenio, additional, Semenov, Dmitry, additional, Spezzano, Silvia, additional, Thompson, Mark, additional, Wyrowski, Friedrich, additional, Cicone, Claudia, additional, Mroczkowski, Tony, additional, Cordiner, Martin, additional, Di Mascolo, Luca, additional, Johnstone, Doug, additional, van Kampen, Eelco, additional, Lee, Minju, additional, Liu, Daizhong, additional, Maccarone, Thomas, additional, Saintonge, Amélie, additional, Smith, Matthew, additional, Thelen, Alexander, additional, and Wedemeyer, Sven, additional

Published
2024
Full Text
View/download PDF

24. Filamentary Network and Magnetic Field Structures Revealed with BISTRO in the High-mass Star-forming Region NGC 2264: Global Properties and Local Magnetogravitational Configurations

Author

Wang, Jia-Wei, primary, Koch, Patrick M., additional, Clarke, Seamus D., additional, Fuller, Gary, additional, Peretto, Nicolas, additional, Tang, Ya-Wen, additional, Yen, Hsi-Wei, additional, Lai, Shih-Ping, additional, Ohashi, Nagayoshi, additional, Arzoumanian, Doris, additional, Johnstone, Doug, additional, Furuya, Ray, additional, Inutsuka, Shu-ichiro, additional, Lee, Chang Won, additional, Ward-Thompson, Derek, additional, Le Gouellec, Valentin J. M., additional, Liu, Hong-Li, additional, Fanciullo, Lapo, additional, Hwang, Jihye, additional, Pattle, Kate, additional, Poidevin, Frédérick, additional, Tahani, Mehrnoosh, additional, Onaka, Takashi, additional, Rawlings, Mark G., additional, Chung, Eun Jung, additional, Liu, Junhao, additional, Lyo, A-Ran, additional, Priestley, Felix, additional, Hoang, Thiem, additional, Tamura, Motohide, additional, Berry, David, additional, Bastien, Pierre, additional, Ching, Tao-Chung, additional, Coudé, Simon, additional, Kwon, Woojin, additional, Chen, Mike, additional, Eswaraiah, Chakali, additional, Soam, Archana, additional, Hasegawa, Tetsuo, additional, Qiu, Keping, additional, Bourke, Tyler L., additional, Byun, Do-Young, additional, Chen, Zhiwei, additional, Chen, Huei-Ru Vivien, additional, Chen, Wen Ping, additional, Cho, Jungyeon, additional, Choi, Minho, additional, Choi, Yunhee, additional, Choi, Youngwoo, additional, Chrysostomou, Antonio, additional, Dai, Sophia, additional, Di Francesco, James, additional, Diep​, Pham Ngoc, additional, Doi, Yasuo, additional, Duan, Yan, additional, Duan, Hao-Yuan, additional, Eden, David, additional, Fiege, Jason, additional, Fissel, Laura M., additional, Franzmann, Erica, additional, Friberg, Per, additional, Friesen, Rachel, additional, Gledhill, Tim, additional, Graves, Sarah, additional, Greaves, Jane, additional, Griffin, Matt, additional, Gu, Qilao, additional, Han, Ilseung, additional, Hayashi, Saeko, additional, Houde, Martin, additional, Inoue, Tsuyoshi, additional, Iwasaki, Kazunari, additional, Jeong, Il-Gyo, additional, Könyves, Vera, additional, Kang, Ji-hyun, additional, Kang, Miju, additional, Karoly, Janik, additional, Kataoka, Akimasa, additional, Kawabata, Koji, additional, Khan, Zacariyya, additional, Kim, Mi-Ryang, additional, Kim, Kee-Tae, additional, Kim, Kyoung Hee, additional, Kim, Shinyoung, additional, Kim, Jongsoo, additional, Kim, Hyosung, additional, Kim, Gwanjeong, additional, Kirchschlager, Florian, additional, Kirk, Jason, additional, Kobayashi, Masato I. N., additional, Kusune, Takayoshi, additional, Kwon, Jungmi, additional, Lacaille, Kevin, additional, Law, Chi-Yan, additional, Lee, Sang-Sung, additional, Lee, Hyeseung, additional, Lee, Jeong-Eun, additional, Lee, Chin-Fei, additional, Li, Dalei, additional, Li, Hua-bai, additional, Li, Guangxing, additional, Li, Di, additional, Lin, Sheng-Jun, additional, Liu, Tie, additional, Liu, Sheng-Yuan, additional, Lu, Xing, additional, Mairs, Steve, additional, Matsumura, Masafumi, additional, Matthews, Brenda, additional, Moriarty-Schieven, Gerald, additional, Nagata, Tetsuya, additional, Nakamura, Fumitaka, additional, Nakanishi, Hiroyuki, additional, Ngoc, Nguyen Bich, additional, Park, Geumsook, additional, Parsons, Harriet, additional, Pyo, Tae-Soo, additional, Qian, Lei, additional, Rao, Ramprasad, additional, Rawlings, Jonathan, additional, Retter, Brendan, additional, Richer, John, additional, Rigby, Andrew, additional, Sadavoy, Sarah, additional, Saito, Hiro, additional, Savini, Giorgio, additional, Seta, Masumichi, additional, Sharma, Ekta, additional, Shimajiri, Yoshito, additional, Shinnaga, Hiroko, additional, Tang, Xindi, additional, Thuong, Hoang Duc, additional, Tomisaka, Kohji, additional, Tram, Le Ngoc, additional, Tsukamoto, Yusuke, additional, Viti, Serena, additional, Wang, Hongchi, additional, Whitworth, Anthony, additional, Wu, Jintai, additional, Xie, Jinjin, additional, Yang, Meng-Zhe, additional, Yoo, Hyunju, additional, Yuan, Jinghua, additional, Yun, Hyeong-Sik, additional, Zenko, Tetsuya, additional, Zhang, Chuan-Peng, additional, Zhang, Yapeng, additional, Zhang, Guoyin, additional, Zhou, Jianjun, additional, Zhu, Lei, additional, de Looze, Ilse, additional, André, Philippe, additional, Dowell, C. Darren, additional, Eyres, Stewart, additional, Falle, Sam, additional, Robitaille, Jean-François, additional, and van Loo, Sven, additional

Published
2024
Full Text
View/download PDF

25. The JCMT BISTRO Survey: Studying the Complex Magnetic Field of L43

Author

Karoly, Janik, primary, Ward-Thompson, Derek, additional, Pattle, Kate, additional, Berry, David, additional, Whitworth, Anthony, additional, Kirk, Jason, additional, Bastien, Pierre, additional, Ching, Tao-Chung, additional, Coudé, Simon, additional, Hwang, Jihye, additional, Kwon, Woojin, additional, Soam, Archana, additional, Wang, Jia-Wei, additional, Hasegawa, Tetsuo, additional, Lai, Shih-Ping, additional, Qiu, Keping, additional, Arzoumanian, Doris, additional, Bourke, Tyler L., additional, Byun, Do-Young, additional, Chen, Huei-Ru Vivien, additional, Chen, Wen Ping, additional, Chen, Mike, additional, Chen, Zhiwei, additional, Cho, Jungyeon, additional, Choi, Minho, additional, Choi, Youngwoo, additional, Choi, Yunhee, additional, Chrysostomou, Antonio, additional, Chung, Eun Jung, additional, Dai, Sophia, additional, Debattista, Victor, additional, Di Francesco, James, additional, Diep, Pham Ngoc, additional, Doi, Yasuo, additional, Duan, Hao-Yuan, additional, Duan, Yan, additional, Eswaraiah, Chakali, additional, Fanciullo, Lapo, additional, Fiege, Jason, additional, Fissel, Laura M., additional, Franzmann, Erica, additional, Friberg, Per, additional, Friesen, Rachel, additional, Fuller, Gary, additional, Furuya, Ray, additional, Gledhill, Tim, additional, Graves, Sarah, additional, Greaves, Jane, additional, Griffin, Matt, additional, Gu, Qilao, additional, Han, Ilseung, additional, Hoang, Thiem, additional, Houde, Martin, additional, Hull, Charles L. H., additional, Inoue, Tsuyoshi, additional, Inutsuka, Shu-ichiro, additional, Iwasaki, Kazunari, additional, Jeong, Il-Gyo, additional, Johnstone, Doug, additional, Könyves, Vera, additional, Kang, Ji-hyun, additional, Kang, Miju, additional, Kataoka, Akimasa, additional, Kawabata, Koji, additional, Kemper, Francisca, additional, Kim, Jongsoo, additional, Kim, Shinyoung, additional, Kim, Gwanjeong, additional, Kim, Kyoung Hee, additional, Kim, Mi-Ryang, additional, Kim, Kee-Tae, additional, Kim, Hyosung, additional, Kirchschlager, Florian, additional, Kobayashi, Masato I. N., additional, Koch, Patrick M., additional, Kusune, Takayoshi, additional, Kwon, Jungmi, additional, Lacaille, Kevin, additional, Law, Chi-Yan, additional, Lee, Chang Won, additional, Lee, Hyeseung, additional, Lee, Yong-Hee, additional, Lee, Chin-Fei, additional, Lee, Jeong-Eun, additional, Lee, Sang-Sung, additional, Li, Dalei, additional, Li, Di, additional, Li, Guangxing, additional, Li, Hua-bai, additional, Lin, Sheng-Jun, additional, Liu, Hong-Li, additional, Liu, Tie, additional, Liu, Sheng-Yuan, additional, Liu, Junhao, additional, Longmore, Steven, additional, Lu, Xing, additional, Lyo, A-Ran, additional, Mairs, Steve, additional, Matsumura, Masafumi, additional, Matthews, Brenda, additional, Moriarty-Schieven, Gerald, additional, Nagata, Tetsuya, additional, Nakamura, Fumitaka, additional, Nakanishi, Hiroyuki, additional, Ngoc, Nguyen Bich, additional, Ohashi, Nagayoshi, additional, Onaka, Takashi, additional, Park, Geumsook, additional, Parsons, Harriet, additional, Peretto, Nicolas, additional, Priestley, Felix, additional, Pyo, Tae-Soo, additional, Qian, Lei, additional, Rao, Ramprasad, additional, Rawlings, Jonathan, additional, Rawlings, Mark, additional, Retter, Brendan, additional, Richer, John, additional, Rigby, Andrew, additional, Sadavoy, Sarah, additional, Saito, Hiro, additional, Savini, Giorgio, additional, Seta, Masumichi, additional, Sharma, Ekta, additional, Shimajiri, Yoshito, additional, Shinnaga, Hiroko, additional, Tahani, Mehrnoosh, additional, Tamura, Motohide, additional, Tang, Ya-Wen, additional, Tang, Xindi, additional, Tomisaka, Kohji, additional, Tram, Le Ngoc, additional, Tsukamoto, Yusuke, additional, Viti, Serena, additional, Wang, Hongchi, additional, Wu, Jintai, additional, Xie, Jinjin, additional, Yang, Meng-Zhe, additional, Yen, Hsi-Wei, additional, Yoo, Hyunju, additional, Yuan, Jinghua, additional, Yun, Hyeong-Sik, additional, Zenko, Tetsuya, additional, Zhang, Guoyin, additional, Zhang, Yapeng, additional, Zhang, Chuan-Peng, additional, Zhou, Jianjun, additional, Zhu, Lei, additional, de Looze, Ilse, additional, André, Philippe, additional, Dowell, C. Darren, additional, Eden, David, additional, Eyres, Stewart, additional, Falle, Sam, additional, Le Gouellec, Valentin J. M., additional, Poidevin, Frédérick, additional, Robitaille, Jean-François, additional, and van Loo, Sven, additional

Published
2023
Full Text
View/download PDF

28. JCMT BISTRO Observations: Magnetic Field Morphology of Bubbles Associated with NGC 6334

Author

Tahani, Mehrnoosh, Bastien, Pierre, Furuva, Ray S., Pattle, Kate, Johnstone, Doug, Arzoumanian, Doris, Doi, Yasuo, Hasegawa, Tetsuo, Inutsuka, Shu-Ichiro, Coude, Simon, Fissel, Laura, Chen, Michael Chun-Yuan, Poidevin, Frederick, Sadavoy, Sarah, Friesen, Rachel, Koch, Patrick M., Di Francesco, James, Moriarty-Schieven, Gerald, Chen, Zhiwei, Chung, Eun Jung, Eswaraiah, Chakali, Fanciullo, Lapo, Gledhill, Tim, Le Gouellec, Valentin J. M., Hoang, Thiem, Hwang, Jihye, Kang, Ji-Hyun, Kim, Kyoung Hee, Kirchschlager, Florian, Kwon, Woojin, Lee, Chang Won, Liu, Hong-Li, Onaka, Takashi, Rawlings, Mark G., Soam, Archana, Tamura, Motohide, Tang, Xindi, Tomisaka, Kohji, Whitworth, Anthony P., Kwon, Jungmi, Hoang, Thuong D., Redman, Matt, Berry, David, Ching, Tao-Chung, Wang, Jia-Wei, Lai, Shih-Ping, Qiu, Keping, Ward-Thompson, Derek, Houde, Martin, Byun, Do-Young, Chen, Huei-Reu Vivien, Chen, Wen Ping, Cho, Jungyeon, Choi, Minho, Choi, Yunhee, Chrysostomou, Antonio, Diep, Pham Ngoc, Duan, Hao-Yuan, Fiege, Jason, Franzmann, Erica, Friberg, Per, Fuller, Gary, Graves, Sarah F., Greaves, Jane S., Griffin, Mary J., Gu, Qilao, Han, Ilseung, Hatchell, Jennifer, Hayashi, Saeko S., Hull, Charles L. H., Inoue, Tsuyoshi, Iwasaki, Kazunari, Jeong, Il-Gyo, Kanamori, Yoshihiro, Kang, Miju, Kang, Sung-Ju, Kataoka, Akimasa, Kawabata, Koji S., Kemper, Francesca, Kim, Gwanjeong, Kim, Jongsoo Hee, Kim, Kee-Tae, Kim, Mi-Ryang, Kim, Shinyoung, Kirk, Jason Matthew, Kobayashi, Masato I. N., Konyves, Vera, Kusune, Takayoshi, Lacaille, Kevin, Law, Chi-Yan, Lee, Chin-Fei, Lee, Hyeseung, Lee, Jeong-Eun, Lee, Sang-Sung, Lee, Yong-Hee, Li, Dalei, Li, Di, Li, Hua-Bai, Liu, Junhao, Liu, Sheng-Yuan, Liu, Tie, de Looze, Ilse, Lyo, A-Ran, Mairs, Steve, Matsumara, Masafumi, Matthews, Brenda C., Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ohashi, Nagayoshi, Park, Geumsook, Parsons, Harriet, Peretto, Nicolas, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Retter, Brendan, Richer, John, Rigby, Andrew, Saito, Hiro, Savini, Giorgio, Scaife, Anna M. M., Seta, Masumichi, Shimajiri, Yoshito, Shinnaga, Hiroko, Tang, Ya-Wen, Tsukamoto, Yusuke, Vitti, Serena, Wang, Hongchi, Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Chuan-Peng, Zhang, Guoyin, Zhang, Yapeng, Zhou, Jianjun, Zhu, Lei, Andre, Philippe, Dowell, C. Darren, Eyres, Stewart Paul shore, Falle, Sam, van Loo, Sven, Robitaille, Jean-Francois, Tahani, Mehrnoosh, Bastien, Pierre, Furuva, Ray S., Pattle, Kate, Johnstone, Doug, Arzoumanian, Doris, Doi, Yasuo, Hasegawa, Tetsuo, Inutsuka, Shu-Ichiro, Coude, Simon, Fissel, Laura, Chen, Michael Chun-Yuan, Poidevin, Frederick, Sadavoy, Sarah, Friesen, Rachel, Koch, Patrick M., Di Francesco, James, Moriarty-Schieven, Gerald, Chen, Zhiwei, Chung, Eun Jung, Eswaraiah, Chakali, Fanciullo, Lapo, Gledhill, Tim, Le Gouellec, Valentin J. M., Hoang, Thiem, Hwang, Jihye, Kang, Ji-Hyun, Kim, Kyoung Hee, Kirchschlager, Florian, Kwon, Woojin, Lee, Chang Won, Liu, Hong-Li, Onaka, Takashi, Rawlings, Mark G., Soam, Archana, Tamura, Motohide, Tang, Xindi, Tomisaka, Kohji, Whitworth, Anthony P., Kwon, Jungmi, Hoang, Thuong D., Redman, Matt, Berry, David, Ching, Tao-Chung, Wang, Jia-Wei, Lai, Shih-Ping, Qiu, Keping, Ward-Thompson, Derek, Houde, Martin, Byun, Do-Young, Chen, Huei-Reu Vivien, Chen, Wen Ping, Cho, Jungyeon, Choi, Minho, Choi, Yunhee, Chrysostomou, Antonio, Diep, Pham Ngoc, Duan, Hao-Yuan, Fiege, Jason, Franzmann, Erica, Friberg, Per, Fuller, Gary, Graves, Sarah F., Greaves, Jane S., Griffin, Mary J., Gu, Qilao, Han, Ilseung, Hatchell, Jennifer, Hayashi, Saeko S., Hull, Charles L. H., Inoue, Tsuyoshi, Iwasaki, Kazunari, Jeong, Il-Gyo, Kanamori, Yoshihiro, Kang, Miju, Kang, Sung-Ju, Kataoka, Akimasa, Kawabata, Koji S., Kemper, Francesca, Kim, Gwanjeong, Kim, Jongsoo Hee, Kim, Kee-Tae, Kim, Mi-Ryang, Kim, Shinyoung, Kirk, Jason Matthew, Kobayashi, Masato I. N., Konyves, Vera, Kusune, Takayoshi, Lacaille, Kevin, Law, Chi-Yan, Lee, Chin-Fei, Lee, Hyeseung, Lee, Jeong-Eun, Lee, Sang-Sung, Lee, Yong-Hee, Li, Dalei, Li, Di, Li, Hua-Bai, Liu, Junhao, Liu, Sheng-Yuan, Liu, Tie, de Looze, Ilse, Lyo, A-Ran, Mairs, Steve, Matsumara, Masafumi, Matthews, Brenda C., Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ohashi, Nagayoshi, Park, Geumsook, Parsons, Harriet, Peretto, Nicolas, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Retter, Brendan, Richer, John, Rigby, Andrew, Saito, Hiro, Savini, Giorgio, Scaife, Anna M. M., Seta, Masumichi, Shimajiri, Yoshito, Shinnaga, Hiroko, Tang, Ya-Wen, Tsukamoto, Yusuke, Vitti, Serena, Wang, Hongchi, Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Chuan-Peng, Zhang, Guoyin, Zhang, Yapeng, Zhou, Jianjun, Zhu, Lei, Andre, Philippe, Dowell, C. Darren, Eyres, Stewart Paul shore, Falle, Sam, van Loo, Sven, and Robitaille, Jean-Francois

Abstract

We study the HII regions associated with the NGC 6334 molecular cloud observed in the sub-millimeter and taken as part of the B-fields In STar-forming Region Observations (BISTRO) Survey. In particular, we investigate the polarization patterns and magnetic field morphologies associated with these HII regions. Through polarization pattern and pressure calculation analyses, several of these bubbles indicate that the gas and magnetic field lines have been pushed away from the bubble, toward an almost tangential (to the bubble) magnetic field morphology. In the densest part of NGC 6334, where the magnetic field morphology is similar to an hourglass, the polarization observations do not exhibit observable impact from HII regions. We detect two nested radial polarization patterns in a bubble to the south of NGC 6334 that correspond to the previously observed bipolar structure in this bubble. Finally, using the results of this study, we present steps (incorporating computer vision; circular Hough Transform) that can be used in future studies to identify bubbles that have physically impacted magnetic field lines.

Published
2023

29. Predicting reliable H2 column density maps from molecular line data using machine learning.

Author

Shimajiri, Yoshito, Kawanishi, Yasutomo, Fujita, Shinji, Miyamoto, Yusuke, Ito, Atsushi M, Arzoumanian, Doris, André, Philippe, Nishimura, Atsushi, Tokuda, Kazuki, Kaneko, Hiroyuki, Takekawa, Shunya, Ueda, Shota, Onishi, Toshikazu, Inoue, Tsuyoshi, Nishimoto, Shimpei, and Yoneda, Ryuki

Subjects
MOLECULAR clouds, DENSITY, MACHINE learning, LEARNING ability, TRACE gases, MOLECULAR weights
Abstract

The total mass estimate of molecular clouds suffers from the uncertainty in the H2-CO conversion factor, the so-called X CO factor, which is used to convert the 12CO (1–0) integrated intensity to the H2 column density. We demonstrate the machine learning's ability to predict the H2 column density from the 12CO, 13CO, and C18O (1–0) data set of four star-forming molecular clouds: Orion A, Orion B, Aquila, and M17. When the training is performed on a subset of each cloud, the overall distribution of the predicted column density is consistent with that of the Herschel column density. The total column density predicted and observed is consistent within 10 per cent, suggesting that the machine learning prediction provides a reasonable total mass estimate of each cloud. However, the distribution of the column density for values >∼2 × 1022 cm−2, which corresponds to the dense gas, could not be predicted well. This indicates that molecular line observations tracing the dense gas are required for the training. We also found a significant difference between the predicted and observed column density when we created the model after training the data on different clouds. This highlights the presence of different X CO factors between the clouds, and further training in various clouds is required to correct for these variations. We also demonstrated that this method could predict the column density towards the area not observed by Herschel if the molecular line and column density maps are available for the small portion, and the molecular line data are available for the larger areas. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

30. First BISTRO Observations of the Dark Cloud Taurus L1495A-B10: The Role of the Magnetic Field in the Earliest Stages of Low-mass Star Formation

Author

Ward-Thompson, Derek, primary, Karoly, Janik, additional, Pattle, Kate, additional, Whitworth, Anthony, additional, Kirk, Jason, additional, Berry, David, additional, Bastien, Pierre, additional, Ching, Tao-Chung, additional, Coudé, Simon, additional, Hwang, Jihye, additional, Kwon, Woojin, additional, Soam, Archana, additional, Wang, Jia-Wei, additional, Hasegawa, Tetsuo, additional, Lai, Shih-Ping, additional, Qiu, Keping, additional, Arzoumanian, Doris, additional, Bourke, Tyler L., additional, Byun, Do-Young, additional, Chen, Huei-Ru Vivien, additional, Chen, Wen Ping, additional, Chen, Mike, additional, Chen, Zhiwei, additional, Cho, Jungyeon, additional, Choi, Minho, additional, Choi, Youngwoo, additional, Choi, Yunhee, additional, Chrysostomou, Antonio, additional, Chung, Eun Jung, additional, Dai, Sophia, additional, Debattista, Victor, additional, Di Francesco, James, additional, Diep, Pham Ngoc, additional, Doi, Yasuo, additional, Duan, Hao-Yuan, additional, Duan, Yan, additional, Eswaraiah, Chakali, additional, Fanciullo, Lapo, additional, Fiege, Jason, additional, Fissel, Laura M., additional, Franzmann, Erica, additional, Friberg, Per, additional, Friesen, Rachel, additional, Fuller, Gary, additional, Furuya, Ray, additional, Gledhill, Tim, additional, Graves, Sarah, additional, Greaves, Jane, additional, Griffin, Matt, additional, Gu, Qilao, additional, Han, Ilseung, additional, Hayashi, Saeko, additional, Hoang, Thiem, additional, Houde, Martin, additional, Hull, Charles L. H., additional, Inoue, Tsuyoshi, additional, Inutsuka, Shu-ichiro, additional, Iwasaki, Kazunari, additional, Jeong, Il-Gyo, additional, Johnstone, Doug, additional, Könyves, Vera, additional, Kang, Ji-hyun, additional, Kang, Miju, additional, Kataoka, Akimasa, additional, Kawabata, Koji, additional, Kemper, Francisca, additional, Kim, Jongsoo, additional, Kim, Shinyoung, additional, Kim, Gwanjeong, additional, Kim, Kyoung Hee, additional, Kim, Mi-Ryang, additional, Kim, Kee-Tae, additional, Kim, Hyosung, additional, Kirchschlager, Florian, additional, Kobayashi, Masato I. N., additional, Koch, Patrick M., additional, Kusune, Takayoshi, additional, Kwon, Jungmi, additional, Lacaille, Kevin, additional, Law, Chi-Yan, additional, Lee, Chang Won, additional, Lee, Hyeseung, additional, Lee, Yong-Hee, additional, Lee, Chin-Fei, additional, Lee, Jeong-Eun, additional, Lee, Sang-Sung, additional, Li, Dalei, additional, Li, Di, additional, Li, Guangxing, additional, Li, Hua-bai, additional, Lin, Sheng-Jun, additional, Liu, Hong-Li, additional, Liu, Tie, additional, Liu, Sheng-Yuan, additional, Liu, Junhao, additional, Longmore, Steven, additional, Lu, Xing, additional, Lyo, A-Ran, additional, Mairs, Steve, additional, Matsumura, Masafumi, additional, Matthews, Brenda, additional, Moriarty-Schieven, Gerald, additional, Nagata, Tetsuya, additional, Nakamura, Fumitaka, additional, Nakanishi, Hiroyuki, additional, Ngoc, Nguyen Bich, additional, Ohashi, Nagayoshi, additional, Onaka, Takashi, additional, Park, Geumsook, additional, Parsons, Harriet, additional, Peretto, Nicolas, additional, Priestley, Felix, additional, Pyo, Tae-Soo, additional, Qian, Lei, additional, Rao, Ramprasad, additional, Rawlings, Jonathan, additional, Rawlings, Mark, additional, Retter, Brendan, additional, Richer, John, additional, Rigby, Andrew, additional, Sadavoy, Sarah, additional, Saito, Hiro, additional, Savini, Giorgio, additional, Seta, Masumichi, additional, Shimajiri, Yoshito, additional, Shinnaga, Hiroko, additional, Tahani, Mehrnoosh, additional, Tamura, Motohide, additional, Tang, Ya-Wen, additional, Tang, Xindi, additional, Tomisaka, Kohji, additional, Tram, Le Ngoc, additional, Tsukamoto, Yusuke, additional, Viti, Serena, additional, Wang, Hongchi, additional, Wu, Jintai, additional, Xie, Jinjin, additional, Yang, Meng-Zhe, additional, Yen, Hsi-Wei, additional, Yoo, Hyunju, additional, Yuan, Jinghua, additional, Yun, Hyeong-Sik, additional, Zenko, Tetsuya, additional, Zhang, Guoyin, additional, Zhang, Yapeng, additional, Zhang, Chuan-Peng, additional, Zhou, Jianjun, additional, Zhu, Lei, additional, de Looze, Ilse, additional, André, Philippe, additional, Dowell, C. Darren, additional, Eden, David, additional, Eyres, Stewart, additional, Falle, Sam, additional, Le Gouellec, Valentin J. M., additional, Poidevin, Frédérick, additional, Robitaille, Jean-François, additional, and van Loo, Sven, additional

Published
2023
Full Text
View/download PDF

31. JCMT BISTRO Observations: Magnetic Field Morphology of Bubbles Associated with NGC 6334

Author

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

Published
2023
Full Text
View/download PDF

33. The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament

Author

Ching, Tao-Chung, primary, Qiu, Keping, additional, Li, Di, additional, Ren, Zhiyuan, additional, Lai, Shih-Ping, additional, Berry, David, additional, Pattle, Kate, additional, Furuya, Ray, additional, Ward-Thompson, Derek, additional, Johnstone, Doug, additional, Koch, Patrick M., additional, Lee, Chang Won, additional, Hoang, Thiem, additional, Hasegawa, Tetsuo, additional, Kwon, Woojin, additional, Bastien, Pierre, additional, Eswaraiah, Chakali, additional, Wang, Jia-Wei, additional, Kim, Kyoung Hee, additional, Hwang, Jihye, additional, Soam, Archana, additional, Lyo, A-Ran, additional, Liu, Junhao, additional, Le Gouellec, Valentin J. M., additional, Arzoumanian, Doris, additional, Whitworth, Anthony, additional, Francesco, James Di, additional, Poidevin, Frédérick, additional, Liu, Tie, additional, Coudé, Simon, additional, Tahani, Mehrnoosh, additional, Liu, Hong-Li, additional, Onaka, Takashi, additional, Li, Dalei, additional, Tamura, Motohide, additional, Chen, Zhiwei, additional, Tang, Xindi, additional, Kirchschlager, Florian, additional, Bourke, Tyler L., additional, Byun, Do-Young, additional, Chen, Mike, additional, Chen, Huei-Ru Vivien, additional, Chen, Wen Ping, additional, Cho, Jungyeon, additional, Choi, Yunhee, additional, Choi, Youngwoo, additional, Choi, Minho, additional, Chrysostomou, Antonio, additional, Chung, Eun Jung, additional, Dai, Y. Sophia, additional, Diep, Pham Ngoc, additional, Doi, Yasuo, additional, Duan, Yan, additional, Duan, Hao-Yuan, additional, Eden, David, additional, Fanciullo, Lapo, additional, Fiege, Jason, additional, Fissel, Laura M., additional, Franzmann, Erica, additional, Friberg, Per, additional, Friesen, Rachel, additional, Fuller, Gary, additional, Gledhill, Tim, additional, Graves, Sarah, additional, Greaves, Jane, additional, Griffin, Matt, additional, Gu, Qilao, additional, Han, Ilseung, additional, Hayashi, Saeko, additional, Houde, Martin, additional, Hull, Charles L. H., additional, Inoue, Tsuyoshi, additional, Inutsuka, Shu-ichiro, additional, Iwasaki, Kazunari, additional, Jeong, Il-Gyo, additional, Könyves, Vera, additional, Kang, Ji-hyun, additional, Kang, Miju, additional, Karoly, Janik, additional, Kataoka, Akimasa, additional, Kawabata, Koji, additional, Kemper, Francisca, additional, Kim, Jongsoo, additional, Kim, Mi-Ryang, additional, Kim, Shinyoung, additional, Kim, Hyosung, additional, Kim, Kee-Tae, additional, Kim, Gwanjeong, additional, Kirk, Jason, additional, Kobayashi, Masato I. N., additional, Kusune, Takayoshi, additional, Kwon, Jungmi, additional, Lacaille, Kevin, additional, Law, Chi-Yan, additional, Lee, Sang-Sung, additional, Lee, Hyeseung, additional, Lee, Jeong-Eun, additional, Lee, Chin-Fei, additional, Lee, Yong-Hee, additional, Li, Guangxing, additional, Li, Hua-bai, additional, Lin, Sheng-Jun, additional, Liu, Sheng-Yuan, additional, Lu, Xing, additional, Mairs, Steve, additional, Matsumura, Masafumi, additional, Matthews, Brenda, additional, Moriarty-Schieven, Gerald, additional, Nagata, Tetsuya, additional, Nakamura, Fumitaka, additional, Nakanishi, Hiroyuki, additional, Ngoc, Nguyen Bich, additional, Ohashi, Nagayoshi, additional, Park, Geumsook, additional, Parsons, Harriet, additional, Peretto, Nicolas, additional, Priestley, Felix, additional, Pyo, Tae-Soo, additional, Qian, Lei, additional, Rao, Ramprasad, additional, Rawlings, Mark, additional, Rawlings, Jonathan, additional, Retter, Brendan, additional, Richer, John, additional, Rigby, Andrew, additional, Sadavoy, Sarah, additional, Saito, Hiro, additional, Savini, Giorgio, additional, Seta, Masumichi, additional, Shimajiri, Yoshito, additional, Shinnaga, Hiroko, additional, Tang, Ya-Wen, additional, Tomisaka, Kohji, additional, Tram, Le Ngoc, additional, Tsukamoto, Yusuke, additional, Viti, Serena, additional, Wang, Hongchi, additional, Wu, Jintai, additional, Xie, Jinjin, additional, Yang, Meng-Zhe, additional, Yen, Hsi-Wei, additional, Yoo, Hyunju, additional, Yuan, Jinghua, additional, Yun, Hyeong-Sik, additional, Zenko, Tetsuya, additional, Zhang, Chuan-Peng, additional, Zhang, Yapeng, additional, Zhang, Guoyin, additional, Zhou, Jianjun, additional, Zhu, Lei, additional, de Looze, Ilse, additional, André, Philippe, additional, Dowell, C. Darren, additional, Eyres, Stewart, additional, Falle, Sam, additional, Robitaille, Jean-François, additional, and van Loo, Sven, additional

Published
2022
Full Text
View/download PDF

34. The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2

Author

Hwang, Jihye, primary, Kim, Jongsoo, additional, Pattle, Kate, additional, Lee, Chang Won, additional, Koch, Patrick M., additional, Johnstone, Doug, additional, Tomisaka, Kohji, additional, Whitworth, Anthony, additional, Furuya, Ray S., additional, Kang, Ji-hyun, additional, Lyo, A-Ran, additional, Chung, Eun Jung, additional, Arzoumanian, Doris, additional, Park, Geumsook, additional, Kwon, Woojin, additional, Kim, Shinyoung, additional, Tamura, Motohide, additional, Kwon, Jungmi, additional, Soam, Archana, additional, Han, Ilseung, additional, Hoang, Thiem, additional, Kim, Kyoung Hee, additional, Onaka, Takashi, additional, Eswaraiah, Chakali, additional, Ward-Thompson, Derek, additional, Liu, Hong-Li, additional, Tang, Xindi, additional, Chen, Wen Ping, additional, Matsumura, Masafumi, additional, Hoang, Thuong Duc, additional, Chen, Zhiwei, additional, Le Gouellec, Valentin J. M., additional, Kirchschlager, Florian, additional, Poidevin, Frédérick, additional, Bastien, Pierre, additional, Qiu, Keping, additional, Hasegawa, Tetsuo, additional, Lai, Shih-Ping, additional, Byun, Do-Young, additional, Cho, Jungyeon, additional, Choi, Minho, additional, Choi, Youngwoo, additional, Choi, Yunhee, additional, Jeong, Il-Gyo, additional, Kang, Miju, additional, Kim, Hyosung, additional, Kim, Kee-Tae, additional, Lee, Jeong-Eun, additional, Lee, Sang-Sung, additional, Lee, Yong-Hee, additional, Lee, Hyeseung, additional, Kim, Mi-Ryang, additional, Yoo, Hyunju, additional, Yun, Hyeong-Sik, additional, Chen, Mike, additional, Francesco, James Di, additional, Fiege, Jason, additional, Fissel, Laura M., additional, Franzmann, Erica, additional, Houde, Martin, additional, Lacaille, Kevin, additional, Matthews, Brenda, additional, Sadavoy, Sarah, additional, Moriarty-Schieven, Gerald, additional, Tahani, Mehrnoosh, additional, Ching, Tao-Chung, additional, Dai, Y. Sophia, additional, Duan, Yan, additional, Gu, Qilao, additional, Law, Chi-Yan, additional, Li, Dalei, additional, Li, Di, additional, Li, Guangxing, additional, Li, Hua-bai, additional, Liu, Tie, additional, Lu, Xing, additional, Qian, Lei, additional, Wang, Hongchi, additional, Wu, Jintai, additional, Xie, Jinjin, additional, Yuan, Jinghua, additional, Zhang, Chuan-Peng, additional, Zhang, Guoyin, additional, Zhang, Yapeng, additional, Zhou, Jianjun, additional, Zhu, Lei, additional, Berry, David, additional, Friberg, Per, additional, Graves, Sarah, additional, Liu, Junhao, additional, Mairs, Steve, additional, Parsons, Harriet, additional, Rawlings, Mark, additional, Doi, Yasuo, additional, Hayashi, Saeko, additional, Hull, Charles L. H., additional, Inoue, Tsuyoshi, additional, Inutsuka, Shu-ichiro, additional, Iwasaki, Kazunari, additional, Kataoka, Akimasa, additional, Kawabata, Koji, additional, Kim, Gwanjeong, additional, Kobayashi, Masato I. N., additional, Nagata, Tetsuya, additional, Nakamura, Fumitaka, additional, Nakanishi, Hiroyuki, additional, Pyo, Tae-Soo, additional, Saito, Hiro, additional, Seta, Masumichi, additional, Shimajiri, Yoshito, additional, Shinnaga, Hiroko, additional, Tsukamoto, Yusuke, additional, Zenko, Tetsuya, additional, Chen, Huei-Ru Vivien, additional, Duan, Hao-Yuan, additional, Fanciullo, Lapo, additional, Kemper, Francisca, additional, Lee, Chin-Fei, additional, Lin, Sheng-Jun, additional, Liu, Sheng-Yuan, additional, Ohashi, Nagayoshi, additional, Rao, Ramprasad, additional, Tang, Ya-Wen, additional, Wang, Jia-Wei, additional, Yang, Meng-Zhe, additional, Yen, Hsi-Wei, additional, Bourke, Tyler L., additional, Chrysostomou, Antonio, additional, Debattista, Victor, additional, Eden, David, additional, Eyres, Stewart, additional, Falle, Sam, additional, Fuller, Gary, additional, Gledhill, Tim, additional, Greaves, Jane, additional, Griffin, Matt, additional, Hatchell, Jennifer, additional, Karoly, Janik, additional, Kirk, Jason, additional, Könyves, Vera, additional, Longmore, Steven, additional, van Loo, Sven, additional, Looze, Ilse de, additional, Peretto, Nicolas, additional, Priestley, Felix, additional, Rawlings, Jonathan, additional, Retter, Brendan, additional, Richer, John, additional, Rigby, Andrew, additional, Savini, Giorgio, additional, Scaife, Anna, additional, Viti, Serena, additional, Diep, Pham Ngoc, additional, Ngoc, Nguyen Bich, additional, Tram, Le Ngoc, additional, André, Philippe, additional, Coudé, Simon, additional, Dowell, C. Darren, additional, Friesen, Rachel, additional, and Robitaille, Jean-Franćois, additional

Published
2022
Full Text
View/download PDF

36. Velocity structure of the 50 pc long NGC 6334 filamentary cloud

Author

Arzoumanian, Doris, primary, Russeil, Delphine, additional, Zavagno, Annie, additional, Chun-Yuan Chen, Michael, additional, André, Philippe, additional, Inutsuka, Shu-ichiro, additional, Misugi, Yoshiaki, additional, Sánchez-Monge, Álvaro, additional, Schilke, Peter, additional, Men’shchikov, Alexander, additional, and Kohno, Mikito, additional

Published
2022
Full Text
View/download PDF

37. The JCMT BISTRO Survey: multiwavelength polarimetry of bright regions in NGC 2071 in the far-infrared/submillimetre range, with POL-2 and HAWC+

Author

Fanciullo, Lapo, primary, Kemper, Francisca, additional, Pattle, Kate, additional, Koch, Patrick M, additional, Sadavoy, Sarah, additional, Coudé, Simon, additional, Soam, Archana, additional, Hoang, Thiem, additional, Onaka, Takashi, additional, Le Gouellec, Valentin J M, additional, Arzoumanian, Doris, additional, Berry, David, additional, Eswaraiah, Chakali, additional, Chung, Eun Jung, additional, Furuya, Ray, additional, Hull, Charles L H, additional, Hwang, Jihye, additional, Johnstone, Douglas, additional, Kang, Ji-hyun, additional, Kim, Kyoung Hee, additional, Kirchschlager, Florian, additional, Könyves, Vera, additional, Kwon, Jungmi, additional, Kwon, Woojin, additional, Lai, Shih-Ping, additional, Lee, Chang Won, additional, Liu, Tie, additional, Lyo, A-Ran, additional, Stephens, Ian, additional, Tamura, Motohide, additional, Tang, Xindi, additional, Ward-Thompson, Derek, additional, Whitworth, Anthony, additional, and Shinnaga, Hiroko, additional

Published
2022
Full Text
View/download PDF

38. B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main

Author

Kwon, Woojin, primary, Pattle, Kate, additional, Sadavoy, Sarah, additional, Hull, Charles L. H., additional, Johnstone, Doug, additional, Ward-Thompson, Derek, additional, Francesco, James Di, additional, Koch, Patrick M., additional, Furuya, Ray, additional, Doi, Yasuo, additional, Le Gouellec, Valentin J. M., additional, Hwang, Jihye, additional, Lyo, A-Ran, additional, Soam, Archana, additional, Tang, Xindi, additional, Hoang, Thiem, additional, Kirchschlager, Florian, additional, Eswaraiah, Chakali, additional, Fanciullo, Lapo, additional, Kim, Kyoung Hee, additional, Onaka, Takashi, additional, Könyves, Vera, additional, Kang, Ji-hyun, additional, Lee 이, Chang Won 창원, additional, Tamura, Motohide, additional, Bastien, Pierre, additional, Hasegawa 長谷, Tetsuo 川哲夫, additional, Lai, Shih-Ping, additional, Qiu, Keping, additional, Berry, David, additional, Arzoumanian, Doris, additional, Bourke, Tyler L., additional, Byun, Do-Young, additional, Chen, Wen Ping, additional, Chen, Huei-Ru Vivien, additional, Chen, Mike, additional, Chen, Zhiwei, additional, Ching 慶, Tao-Chung 道沖, additional, Cho, Jungyeon, additional, Choi, Yunhee, additional, Choi, Minho, additional, Chrysostomou, Antonio, additional, Chung, Eun Jung, additional, Coudé, Simon, additional, Dai, Sophia, additional, Diep, Pham Ngoc, additional, Duan, Yan, additional, Duan, Hao-Yuan, additional, Eden, David, additional, Fiege, Jason, additional, Fissel, Laura M., additional, Franzmann, Erica, additional, Friberg, Per, additional, Friesen, Rachel, additional, Fuller, Gary, additional, Gledhill, Tim, additional, Graves, Sarah, additional, Greaves, Jane, additional, Griffin, Matt, additional, Gu, Qilao, additional, Han, Ilseung, additional, Hatchell, Jennifer, additional, Hayashi, Saeko, additional, Houde, Martin, additional, Inoue, Tsuyoshi, additional, Inutsuka, Shu-ichiro, additional, Iwasaki, Kazunari, additional, Jeong, Il-Gyo, additional, Kang, Miju, additional, Karoly, Janik, additional, Kataoka, Akimasa, additional, Kawabata, Koji, additional, Kemper, Francisca, additional, Kim, Kee-Tae, additional, Kim, Gwanjeong, additional, Kim, Mi-Ryang, additional, Kim, Shinyoung, additional, Kim, Jongsoo, additional, Kirk, Jason, additional, Kobayashi, Masato I. N., additional, Kusune, Takayoshi, additional, Kwon, Jungmi, additional, Lacaille, Kevin, additional, Law, Chi-Yan, additional, Lee, Chin-Fei, additional, Lee, Yong-Hee, additional, Lee, Hyeseung, additional, Lee, Jeong-Eun, additional, Lee, Sang-Sung, additional, Li, Dalei, additional, Li, Di, additional, Li, Hua-bai, additional, Lin 林, Sheng-Jun 聖鈞, additional, Liu, Sheng-Yuan, additional, Liu, Hong-Li, additional, Liu 刘, Junhao 峻豪, additional, Liu 刘, Tie 铁, additional, Lu, Xing, additional, Mairs, Steve, additional, Matsumura 松村, Masafumi 雅文, additional, Matthews, Brenda, additional, Moriarty-Schieven, Gerald, additional, Nagata, Tetsuya, additional, Nakamura, Fumitaka, additional, Nakanishi, Hiroyuki, additional, Ngoc, Nguyen Bich, additional, Ohashi, Nagayoshi, additional, Park, Geumsook, additional, Parsons, Harriet, additional, Peretto, Nicolas, additional, Priestley, Felix, additional, Pyo, Tae-Soo, additional, Qian, Lei, additional, Rao, Ramprasad, additional, Rawlings, Jonathan, additional, Rawlings, Mark G., additional, Retter, Brendan, additional, Richer, John, additional, Rigby, Andrew, additional, Saito, Hiro, additional, Savini, Giorgio, additional, Seta, Masumichi, additional, Shimajiri, Yoshito, additional, Shinnaga, Hiroko, additional, Tahani, Mehrnoosh, additional, Tang, Ya-Wen, additional, Tomisaka, Kohji, additional, Tram, Le Ngoc, additional, Tsukamoto, Yusuke, additional, Viti, Serena, additional, Wang, Hongchi, additional, Wang, Jia-Wei, additional, Whitworth, Anthony, additional, Wu, Jintai, additional, Xie 謝, Jinjin 津津, additional, Yen, Hsi-Wei, additional, Yoo, Hyunju, additional, Yuan, Jinghua, additional, Yun, Hyeong-Sik, additional, Zenko, Tetsuya, additional, Zhang, Yapeng, additional, Zhang, Chuan-Peng, additional, Zhang, Guoyin, additional, Zhou, Jianjun, additional, Zhu, Lei, additional, Looze, Ilse de, additional, André, Philippe, additional, Dowell, C. Darren, additional, Eyres, Stewart, additional, Falle, Sam, additional, Robitaille, Jean-François, additional, and Loo, Sven van, additional

Published
2022
Full Text
View/download PDF

39. The JCMT BISTRO Survey: Evidence for Pinched Magnetic Fields in Quiescent Filaments of NGC 1333

Author

Doi, Yasuo, primary, Tomisaka, Kohji, additional, Hasegawa, Tetsuo, additional, Coudé, Simon, additional, Arzoumanian, Doris, additional, Bastien, Pierre, additional, Matsumura, Masafumi, additional, Tahani, Mehrnoosh, additional, Sadavoy, Sarah, additional, Hull, Charles L. H., additional, Johnstone, Doug, additional, Di Francesco, James, additional, Shimajiri, Yoshito, additional, Furuya, Ray S., additional, Kwon, Jungmi, additional, Tamura, Motohide, additional, Ward-Thompson, Derek, additional, Le Gouellec, Valentin J. M., additional, Hoang, Thiem, additional, Kirchschlager, Florian, additional, Hwang, Jihye, additional, Eswaraiah, Chakali, additional, Koch, Patrick M., additional, Whitworth, Anthony P., additional, Pattle, Kate, additional, Kwon, Woojin, additional, Kang, Jihyun, additional, Inutsuka, Shu-ichiro, additional, Bourke, Tyler L., additional, Tang, Xindi, additional, Fanciullo, Lapo, additional, Lee, Chang Won, additional, Liu, Hong-Li, additional, Lyo, A-Ran, additional, Qiu, Keping, additional, and Lai, Shih-Ping, additional

Published
2021
Full Text
View/download PDF

40. JCMT BISTRO Survey: multiwavelength polarimetry of bright regions in NGC 2071 in the far-infrared/submillimetre range, with POL-2 and HAWC+.

Author

Fanciullo, Lapo, Kemper, Francisca, Pattle, Kate, Koch, Patrick M, Sadavoy, Sarah, Coudé, Simon, Soam, Archana, Hoang, Thiem, Onaka, Takashi, Le Gouellec, Valentin J M, Arzoumanian, Doris, Berry, David, Eswaraiah, Chakali, Chung, Eun Jung, Furuya, Ray, Hull, Charles L H, Hwang, Jihye, Johnstone, Douglas, Kang, Ji-hyun, and Kim, Kyoung Hee

Subjects
SUBMILLIMETER astronomy, DUST explosions, POLARIMETRY, STELLAR magnetic fields, MAGNETIC structure, MOLECULAR clouds, INTERSTELLAR medium, BREWSTER'S angle
Abstract

Polarized dust emission is a key tracer in the study of interstellar medium and of star formation. The observed polarization, however, is a product of magnetic field structure, dust grain properties, and grain alignment efficiency, as well as their variations in the line of sight, making it difficult to interpret polarization unambiguously. The comparison of polarimetry at multiple wavelengths is a possible way of mitigating this problem. We use data from HAWC+ /SOFIA and from SCUBA-2/POL-2 (from the BISTRO survey) to analyse the NGC 2071 molecular cloud at 154, 214, and 850  |$\mu$| m. The polarization angle changes significantly with wavelength over part of NGC 2071, suggesting a change in magnetic field morphology on the line of sight as each wavelength best traces different dust populations. Other possible explanations are the existence of more than one polarization mechanism in the cloud or scattering from very large grains. The observed change of polarization fraction with wavelength, and the 214-to-154 |$\mu$| m polarization ratio in particular, are difficult to reproduce with current dust models under the assumption of uniform alignment efficiency. We also show that the standard procedure of using monochromatic intensity as a proxy for column density may produce spurious results at HAWC+wavelengths. Using both long-wavelength (POL-2, 850  |$\mu$| m) and short-wavelength (HAWC+, |$\lesssim 200\, \mu$| m) polarimetry is key in obtaining these results. This study clearly shows the importance of multi-wavelength polarimetry at submillimetre bands to understand the dust properties of molecular clouds and the relationship between magnetic field and star formation. [ABSTRACT FROM AUTHOR]

Published
2022
Full Text
View/download PDF

41. The JCMT BISTRO-2 survey : magnetic fields of the massive DR21 filament

Author

Tao-Chung Ching, Keping Qiu, Di Li, Zhiyuan Ren, Shih-Ping Lai, David Berry, Kate Pattle, Ray Furuya, Derek Ward-Thompson, Doug Johnstone, Patrick M. Koch, Chang Won Lee, Thiem Hoang, Tetsuo Hasegawa, Woojin Kwon, Pierre Bastien, Chakali Eswaraiah, Jia-Wei Wang, Kyoung Hee Kim, Jihye Hwang, Archana Soam, A-Ran Lyo, Junhao Liu, Valentin J. M. Le Gouellec, Doris Arzoumanian, Anthony Whitworth, James Di Francesco, Frédérick Poidevin, Tie Liu, Simon Coudé, Mehrnoosh Tahani, Hong-Li Liu, Takashi Onaka, Dalei Li, Motohide Tamura, Zhiwei Chen, Xindi Tang, Florian Kirchschlager, Tyler L. Bourke, Do-Young Byun, Mike Chen, Huei-Ru Vivien Chen, Wen Ping Chen, Jungyeon Cho, Yunhee Choi, Youngwoo Choi, Minho Choi, Antonio Chrysostomou, Eun Jung Chung, Y. Sophia Dai, Pham Ngoc Diep, Yasuo Doi, Yan Duan, Hao-Yuan Duan, David Eden, Lapo Fanciullo, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Saeko Hayashi, Martin Houde, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Vera Könyves, Ji-hyun Kang, Miju Kang, Janik Karoly, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Jongsoo Kim, Mi-Ryang Kim, Shinyoung Kim, Hyosung Kim, Kee-Tae Kim, Gwanjeong Kim, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Sang-Sung Lee, Hyeseung Lee, Jeong-Eun Lee, Chin-Fei Lee, Yong-Hee Lee, Guangxing Li, Hua-bai Li, Sheng-Jun Lin, Sheng-Yuan Liu, Xing Lu, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Mark Rawlings, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Sarah Sadavoy, Hiro Saito, Giorgio Savini, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Ya-Wen Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jintai Wu, Jinjin Xie, Meng-Zhe Yang, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Chuan-Peng Zhang, Yapeng Zhang, Guoyin Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, Stewart Eyres, Sam Falle, Jean-François Robitaille, Sven van Loo, National Natural Science Foundation of China, Chinese Academy of Sciences, Natural Sciences and Engineering Research Council of Canada, Ministerio de Ciencia, Innovación y Universidades (España), National Research Foundation of Korea, National Research, Japan Society for the Promotion of Science, Agencia Estatal de Investigación (España), Ching, Tao-Chung [0000-0001-8516-2532], Qiu, Keping [0000-0002-5093-5088], Li, Di [0000-0003-3010-7661], Ren, Zhiyuan [0000-0003-4659-1742], Lai, Shih-Ping [0000-0001-5522-486X], Berry, David [0000-0001-6524-2447], Pattle, Kate [0000-0002-8557-3582], Furuya, Ray [0000-0003-0646-8782], Ward-Thompson, Derek [0000-0003-1140-2761], Johnstone, Doug [0000-0002-6773-459X], Koch, Patrick M [0000-0003-2777-5861], Lee, Chang Won [0000-0002-3179-6334], Hoang, Thiem [0000-0003-2017-0982], Hasegawa, Tetsuo [0000-0003-1853-0184], Kwon, Woojin [0000-0003-4022-4132], Bastien, Pierre [0000-0002-0794-3859], Eswaraiah, Chakali [0000-0003-4761-6139], Wang, Jia-Wei [0000-0002-6668-974X], Kim, Kyoung Hee [0000-0001-9597-7196], Hwang, Jihye [0000-0001-7866-2686], Soam, Archana [0000-0002-6386-2906], Lyo, A-Ran [0000-0002-9907-8427], Liu, Junhao [0000-0002-4774-2998], Le Gouellec, Valentin JM [0000-0002-5714-799X], Arzoumanian, Doris [0000-0002-1959-7201], Whitworth, Anthony [0000-0002-1178-5486], Francesco, James Di [0000-0002-9289-2450], Poidevin, Frédérick [0000-0002-5391-5568], Liu, Tie [0000-0002-5286-2564], Coudé, Simon [0000-0002-0859-0805], Tahani, Mehrnoosh [0000-0001-8749-1436], Liu, Hong-Li [0000-0003-3343-9645], Onaka, Takashi [0000-0002-8234-6747], Tamura, Motohide [0000-0002-6510-0681], Chen, Zhiwei [0000-0003-0849-0692], Tang, Xindi [0000-0002-4154-4309], Kirchschlager, Florian [0000-0002-3036-0184], Bourke, Tyler L [0000-0001-7491-0048], Byun, Do-Young [0000-0003-1157-4109], Chen, Huei-Ru Vivien [0000-0002-9774-1846], Chen, Wen Ping [0000-0003-0262-272X], Cho, Jungyeon [0000-0003-1725-4376], Chrysostomou, Antonio [0000-0002-9583-8644], Chung, Eun Jung [0000-0003-0014-1527], Dai, Y Sophia [0000-0002-7928-416X], Diep, Pham Ngoc [0000-0002-2808-0888], Doi, Yasuo [0000-0001-8746-6548], Duan, Hao-Yuan [0000-0002-7022-4742], Eden, David [0000-0002-5881-3229], Fanciullo, Lapo [0000-0001-9930-9240], Fissel, Laura M [0000-0002-4666-609X], Franzmann, Erica [0000-0003-2142-0357], Friberg, Per [0000-0002-8010-8454], Friesen, Rachel [0000-0001-7594-8128], Fuller, Gary [0000-0001-8509-1818], Gledhill, Tim [0000-0002-2859-4600], Graves, Sarah [0000-0001-9361-5781], Greaves, Jane [0000-0002-3133-413X], Gu, Qilao [0000-0002-2826-1902], Hayashi, Saeko [0000-0001-5026-490X], Houde, Martin [0000-0003-4420-8674], Hull, Charles LH [0000-0002-8975-7573], Inoue, Tsuyoshi [0000-0002-7935-8771], Inutsuka, Shu-ichiro [0000-0003-4366-6518], Jeong, Il-Gyo [0000-0002-5492-6832], Könyves, Vera [0000-0002-3746-1498], Kang, Ji-hyun [0000-0001-7379-6263], Kang, Miju [0000-0002-5016-050X], Karoly, Janik [0000-0001-5996-3600], Kataoka, Akimasa [0000-0003-4562-4119], Kawabata, Koji [0000-0001-6099-9539], Kemper, Francisca [0000-0003-2743-8240], Kim, Jongsoo [0000-0002-1229-0426], Kim, Shinyoung [0000-0001-9333-5608], Kim, Kee-Tae [0000-0003-2412-7092], Kim, Gwanjeong [0000-0003-2011-8172], Kirk, Jason [0000-0002-4552-7477], Kobayashi, Masato IN [0000-0003-3990-1204], Kusune, Takayoshi [0000-0002-9218-9319], Kwon, Jungmi [0000-0003-2815-7774], Lacaille, Kevin [0000-0001-9870-5663], Law, Chi-Yan [0000-0003-1964-970X], Lee, Sang-Sung [0000-0002-6269-594X], Lee, Hyeseung [0000-0003-3465-3213], Lee, Jeong-Eun [0000-0003-3119-2087], Lee, Chin-Fei [0000-0002-3024-5864], Lee, Yong-Hee [0000-0001-6047-701X], Li, Guangxing [0000-0003-3144-1952], Li, Hua-bai [0000-0003-2641-9240], Lin, Sheng-Jun [0000-0002-6868-4483], Liu, Sheng-Yuan [0000-0003-4603-7119], Lu, Xing [0000-0003-2619-9305], Mairs, Steve [0000-0002-6956-0730], Matsumura, Masafumi [0000-0002-6906-0103], Matthews, Brenda [0000-0003-3017-9577], Moriarty-Schieven, Gerald [0000-0002-0393-7822], Nagata, Tetsuya [0000-0001-9264-9015], Nakamura, Fumitaka [0000-0001-5431-2294], Ngoc, Nguyen Bich [0000-0002-5913-5554], Ohashi, Nagayoshi [0000-0003-0998-5064], Park, Geumsook [0000-0001-8467-3736], Parsons, Harriet [0000-0002-6327-3423], Pyo, Tae-Soo [0000-0002-3273-0804], Qian, Lei [0000-0003-0597-0957], Rao, Ramprasad [0000-0002-1407-7944], Rawlings, Mark [0000-0002-6529-202X], Rawlings, Jonathan [0000-0001-5560-1303], Richer, John [0000-0002-9693-6860], Rigby, Andrew [0000-0002-3351-2200], Savini, Giorgio [0000-0003-4449-9416], Shimajiri, Yoshito [0000-0001-9368-3143], Shinnaga, Hiroko [0000-0001-9407-6775], Tang, Ya-Wen [0000-0002-0675-276X], Tomisaka, Kohji [0000-0003-2726-0892], Tram, Le Ngoc [0000-0002-6488-8227], Viti, Serena [0000-0001-8504-8844], Wang, Hongchi [0000-0003-0746-7968], Wu, Jintai [0000-0001-7276-3590], Xie, Jinjin [0000-0002-2738-146X], Yen, Hsi-Wei [0000-0003-1412-893X], Yoo, Hyunju [0000-0002-8578-1728], Yun, Hyeong-Sik [0000-0001-6842-1555], Zhang, Chuan-Peng [0000-0002-4428-3183], Zhang, Yapeng [0000-0002-5102-2096], Zhou, Jianjun [0000-0003-0356-818X], André, Philippe [0000-0002-3413-2293], Falle, Sam [0000-0002-9829-0426], Robitaille, Jean-François [0000-0001-5079-8573], van Loo, Sven [0000-0003-4746-8500], and Apollo - University of Cambridge Repository

Subjects
STAR-FORMING REGIONS, SUBMILLIMETER POLARIZATION, HERSCHEL, FOS: Physical sciences, Astronomy and Astrophysics, MU-M POLARIZATION, MOLECULAR CLOUD, Astrophysics - Astrophysics of Galaxies, 1ST, Astrophysics - Solar and Stellar Astrophysics, Physics and Astronomy, 5101 Astronomical Sciences, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), SCUBA-2, GOULD BELT SURVEY, DUST EMISSION, 51 Physical Sciences, Solar and Stellar Astrophysics (astro-ph.SR), FAR-INFRARED POLARIMETRY
Abstract

Tao-Chung Ching et al., We present 850 μm dust polarization observations of the massive DR21 filament from the B-fields In STar-forming Region Observations (BISTRO) survey, using the POL-2 polarimeter and the SCUBA-2 camera on the James Clerk Maxwell Telescope. We detect ordered magnetic fields perpendicular to the parsec-scale ridge of the DR21 main filament. In the subfilaments, the magnetic fields are mainly parallel to the filamentary structures and smoothly connect to the magnetic fields of the main filament. We compare the POL-2 and Planck dust polarization observations to study the magnetic field structures of the DR21 filament on 0.1–10 pc scales. The magnetic fields revealed in the Planck data are well-aligned with those of the POL-2 data, indicating a smooth variation of magnetic fields from large to small scales. The plane-of-sky magnetic field strengths derived from angular dispersion functions of dust polarization are 0.6–1.0 mG in the DR21 filament and ∼0.1 mG in the surrounding ambient gas. The mass-to-flux ratios are found to be magnetically supercritical in the filament and slightly subcritical to nearly critical in the ambient gas. The alignment between column density structures and magnetic fields changes from random alignment in the low-density ambient gas probed by Planck to mostly perpendicular in the high-density main filament probed by James Clerk Maxwell Telescope. The magnetic field structures of the DR21 filament are in agreement with MHD simulations of a strongly magnetized medium, suggesting that magnetic fields play an important role in shaping the DR21 main filament and subfilaments., This work is supported by National Natural Science Foundation of China (NSFC) grant Nos. 11988101, U1931117, 11725313, and 12073061 and the CAS International Partnership Program of Chinese Academy of Sciences grant No. 114A11KYSB20160008. T.-C.C. is funded by Chinese Academy of Sciences Taiwan Young Talent Program grant No. 2018TW2JB0002. T.-C.C. and C.E. were supported by Special Funding for Advanced Users, budgeted and administrated by Center for Astronomical Mega-Science (CAMS), Chinese Academy of Sciences. K.P. is a Royal Society University Research Fellow, supported by grant No. URF\R1\211322. D.J. is supported by the National Research Council of Canada and by a Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant. P.M.K. is supported by the Ministry of Science and Technology (MoST) in Taiwan through grants 109-2112-M-001-022 and 110-2112-M-001-057. C.W.L. is supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (NRF-2019R1A2C1010851), and by the Korea Astronomy and Space Science Institute grant funded by the Korea government (MSIT; Project No. 2022-1-840-05). T.H. is supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT) through the Mid-career Research Program (2019R1A2C1087045). W.K. was supported by the NRF grant funded by the MSIT (2021R1F1A1061794). C.E. acknowledges the financial support from grant RJF/2020/000071 as a part of Ramanujan Fellowship awarded by the Science and Engineering Research Board (SERB), Department of Science and Technology (DST), Govt. of India. F.P. acknowledges support from the Spanish State Research Agency (AEI) under grant No. PID2019-105552RB-C43. M.T. is supported by JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005. J.K. is supported by JSPS KAKENHI grant No. 19K14775. L.F. and F.K. acknowledge the support by the MoST in Taiwan through grant 107-2119-M-001-031-MY3 and Academia Sinica through grant AS-IA-106-M03. L.F. acknowledges the support by the MoST in Taiwan through grants 111-2811-M-005-007 and 109-2112-M-005-003-MY3. C.L.H.H. acknowledges the support of the NAOJ Fellowship and JSPS KAKENHI grants 18K13586 and 20K14527. F.K. is supported by the Spanish program Unidad de Excelencia María de Maeztu CEX2020-001058-M, financed by MCIN/AEI/10.13039/501100011033. K.Q. is partially supported by National Key R&D Program of China No. 2022YFA1603100, and acknowledges the National Natural Science Foundation of China (NSFC) grant U1731237. S.P.L. acknowledges grants from the Ministry of Science and Technology of Taiwan 106-2119-M-007-021-MY3 and 109-2112-M-007-010-MY3. Y.D. acknowledges the support of JSPS KAKENHI grants 25247016 and 18H01250. Y.S.D. is supported by the National Key R&D Program of China for grant No. 2022YFA1605300, and NSFC grants Nos. 12273051, 11933003.

Published
2022

Catalog

Books, media, physical & digital resources
See catalog results