Search

Your search keyword '"Fiege, J."' showing total 3 results
Start Over Author "Fiege, J." Topic astrophysics::galaxy astrophysics
3 results on '"Fiege, J."'

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

Author

Kwon, W, Pattle, K, Sadavoy, S, Hull, CLH, Johnstone, D, Ward-Thompson, D, Francesco, JD, Koch, PM, Furuya, R, Doi, Y, Le Gouellec, VJM, Hwang, J, Lyo, AR, Soam, A, Tang, X, Hoang, T, Kirchschlager, F, Eswaraiah, C, Fanciullo, L, Kim, KH, Onaka, T, Könyves, V, Kang, JH, Lee, CW, Tamura, M, Bastien, P, Hasegawa, T, Lai, SP, Qiu, K, Berry, D, Arzoumanian, D, Bourke, TL, Byun, DY, Chen, WP, Chen, HRV, Chen, M, Chen, Z, Ching, TC, Cho, J, Choi, Y, Choi, M, Chrysostomou, A, Chung, EJ, Coudé, S, Dai, S, Diep, PN, Duan, Y, Duan, HY, Eden, D, Fiege, J, Fissel, LM, Franzmann, E, Friberg, P, Friesen, R, Fuller, G, Gledhill, T, Graves, S, Greaves, J, Griffin, M, Gu, Q, Han, I, Hatchell, J, Hayashi, S, Houde, M, Inoue, T, Inutsuka, SI, Iwasaki, K, Jeong, IG, Kang, M, Karoly, J, Kataoka, A, Kawabata, K, Kemper, F, Kim, KT, Kim, G, Kim, MR, Kim, S, Kim, J, Kirk, J, Kobayashi, MIN, Kusune, T, Kwon, J, Lacaille, K, Law, CY, Lee, CF, Lee, YH, Lee, H, Lee, JE, Lee, SS, Li, D, Li, HB, Lin, SJ, Liu, SY, Liu, HL, Liu, J, Liu, T, Lu, X, Mairs, S, Matsumura, M, Kwon, W [0000-0003-4022-4132], Pattle, K [0000-0002-8557-3582], Sadavoy, S [0000-0001-7474-6874], Hull, CLH [0000-0002-8975-7573], Johnstone, D [0000-0002-6773-459X], Ward-Thompson, D [0000-0003-1140-2761], Francesco, JD [0000-0002-9289-2450], Koch, PM [0000-0003-2777-5861], Furuya, R [0000-0003-0646-8782], Doi, Y [0000-0001-8746-6548], Le Gouellec, VJM [0000-0002-5714-799X], Hwang, J [0000-0001-7866-2686], Lyo, AR [0000-0002-9907-8427], Soam, A [0000-0002-6386-2906], Tang, X [0000-0002-4154-4309], Hoang, T [0000-0003-2017-0982], Kirchschlager, F [0000-0002-3036-0184], Fanciullo, L [0000-0001-9930-9240], Kim, KH [0000-0001-9597-7196], Onaka, T [0000-0002-8234-6747], Könyves, V [0000-0002-3746-1498], Kang, JH [0000-0001-7379-6263], Tamura, M [0000-0002-6510-0681], Bastien, P [0000-0002-0794-3859], Lai, SP [0000-0001-5522-486X], Qiu, K [0000-0002-5093-5088], Arzoumanian, D [0000-0002-1959-7201], Bourke, TL [0000-0001-7491-0048], Byun, DY [0000-0003-1157-4109], Chen, WP [0000-0002-5519-0628], Chen, HRV [0000-0002-9774-1846], Chen, Z [0000-0003-0849-0692], Ching, TC [0000-0001-8516-2532], Cho, J [0000-0003-1725-4376], Chrysostomou, A [0000-0002-9583-8644], Chung, EJ [0000-0003-0014-1527], Coudé, S [0000-0002-0859-0805], Duan, HY [0000-0002-7022-4742], Eden, D [0000-0002-5881-3229], Fissel, LM [0000-0002-4666-609X], Franzmann, E [0000-0003-2142-0357], Friberg, P [0000-0002-8010-8454], Friesen, R [0000-0001-7594-8128], Fuller, G [0000-0001-8509-1818], Gledhill, T [0000-0002-2859-4600], Graves, S [0000-0001-9361-5781], Greaves, J [0000-0002-3133-413X], Gu, Q [0000-0002-2826-1902], Hatchell, J [0000-0002-4870-2760], Houde, M [0000-0003-4420-8674], Inoue, T [0000-0002-7935-8771], Inutsuka, SI [0000-0003-4366-6518], Iwasaki, K [0000-0002-2707-7548], Kang, M [0000-0002-5016-050X], Kataoka, A [0000-0003-4562-4119], Kawabata, K [0000-0001-6099-9539], Kemper, F [0000-0003-2743-8240], Kim, KT [0000-0003-2412-7092], Kim, G [0000-0003-2011-8172], Kim, MR [0000-0002-1408-7747], Kim, S [0000-0001-9333-5608], Kim, J [0000-0002-1229-0426], Kirk, J [0000-0002-4552-7477], Kobayashi, MIN [0000-0003-3990-1204], Kusune, T [0000-0002-9218-9319], Kwon, J [0000-0003-2815-7774], Lacaille, K [0000-0001-9870-5663], Law, CY [0000-0003-1964-970X], Lee, CF [0000-0002-3024-5864], Lee, YH [0000-0001-6047-701X], Lee, H [0000-0003-3465-3213], Lee, JE [0000-0003-3119-2087], Lee, SS [0000-0002-6269-594X], Li, D [0000-0003-3010-7661], Li, HB [0000-0003-2641-9240], Lin, SJ [0000-0002-6868-4483], Liu, SY [0000-0003-4603-7119], Liu, J [0000-0002-4774-2998], Lu, X [0000-0003-2619-9305], Mairs, S [0000-0002-6956-0730], Matsumura, M [0000-0002-6906-0103], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, Interstellar Matter and the Local Universe, 51 Physical Sciences, Astrophysics::Galaxy Astrophysics
Abstract

We present 850 μm polarimetric observations toward the Serpens Main molecular cloud obtained using the POL-2 polarimeter on the James Clerk Maxwell Telescope as part of the B-fields In STar-forming Region Observations 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 × 10 22 cm−2 (magnetic fields perpendicular to density gradients), while they are 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 ≈ 4.6 × 10 22 cm−2. This can be interpreted as a signature of core formation. At N H 2 ≈ 16 × 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 μG)) using the Davis–Chandrasekhar–Fermi method and discuss whether the filaments are gravitationally unstable based on magnetic field and turbulence energy densities.

Published
2022
Full Text
View/download PDF

2. Dust polarized emission observations of NGC 6334

Author

Arzoumanian, D, Furuya, RS, Hasegawa, T, Tahani, M, Sadavoy, S, Hull, CLH, Johnstone, D, Koch, PM, Inutsuka, S, Doi, Y, Hoang, T, Onaka, T, Iwasaki, K, Shimajiri, Y, Inoue, T, Peretto, N, André, P, Bastien, P, Berry, D, Chen, H-RV, Di Francesco, J, Eswaraiah, C, Fanciullo, L, Fissel, LM, Hwang, J, Kang, J-H, Kim, G, Kim, K-T, Kirchschlager, F, Kwon, W, Lee, CW, Liu, H-L, Lyo, A-R, Pattle, K, Soam, A, Tang, X, Whitworth, A, Ching, T-C, Coudé, S, Wang, J-W, Ward-Thompson, D, Lai, S-P, Qiu, K, Bourke, TL, Byun, D-Y, Chen, M, Chen, Z, Chen, WP, Cho, J, Choi, Y, Choi, M, Chrysostomou, A, Chung, EJ, Dai, S, Diep, PN, Duan, H-Y, Duan, Y, Eden, D, Fiege, J, Franzmann, E, Friberg, P, Fuller, G, Gledhill, T, Graves, S, Greaves, J, Griffin, M, Gu, Q, Han, I, Hatchell, J, Hayashi, S, Houde, M, Jeong, I-G, Kang, M, Kang, S-J, Kataoka, A, Kawabata, K, Kemper, F, Kim, M-R, Kim, KH, Kim, J, Kim, S, Kirk, J, Kobayashi, MIN, Könyves, V, Kusune, T, Kwon, J, Lacaille, K, Law, C-Y, Lee, C-F, Lee, Y-H, Lee, S-S, Lee, H, Lee, J-E, Li, H-B, Li, D, Li, DL, Liu, J, Liu, T, Liu, S-Y, Lu, X, Mairs, S, Matsumura, M, Matthews, B, Moriarty-Schieven, G, Nagata, T, Nakamura, F, Nakanishi, H, Ngoc, NB, Ohashi, N, Park, G, Parsons, H, Pyo, T-S, Qian, L, Rao, R, Rawlings, J, Rawlings, M, Retter, B, Richer, J, Rigby, A, Saito, H, Savini, G, Scaife, A, Seta, M, Shinnaga, H, Tamura, M, Tang, Y-W, Tomisaka, K, Tram, LN, Tsukamoto, Y, Viti, S, Wang, H, Xie, J, Yen, H-W, Yoo, H, Yuan, J, Yun, H-S, Zenko, T, Zhang, G, Zhang, C-P, Zhang, Y, Zhou, J, Zhu, L, de Looze, I, Dowell, CD, Eyres, S, Falle, S, Friesen, R, Robitaille, J-F, and van Loo, S

Subjects
Astrophysics::Galaxy Astrophysics
Abstract

Context. Molecular filaments and hubs have received special attention recently thanks to new studies showing their key role in star formation. While the (column) density and velocity structures of both filaments and hubs have been carefully studied, their magnetic field (B-field) properties have yet to be characterized. Consequently, the role of B-fields in the formation and evolution of hub-filament systems is not well constrained. Aims. We aim to understand the role of the B-field and its interplay with turbulence and gravity in the dynamical evolution of the NGC 6334 filament network that harbours cluster-forming hubs and high-mass star formation. Methods. We present new observations of the dust polarized emission at 850 μm toward the 2 pc × 10 pc map of NGC 6334 at a spatial resolution of 0.09 pc obtained with the James Clerk Maxwell Telescope (JCMT) as part of the B-field In STar-forming Region Observations (BISTRO) survey. We study the distribution and dispersion of the polarized intensity (PI), the polarization fraction (PF), and the plane-of-the-sky B-field angle (χB_POS) toward the whole region, along the 10 pc-long ridge and along the sub-filaments connected to the ridge and the hubs. We derived the power spectra of the intensity and χBPOS along the ridge crest and compared them with the results obtained from simulated filaments. Results. The observations span ~3 orders of magnitude in Stokes I and PI and ~2 orders of magnitude in PF (from ~0.2 to ~ 20%). A large scatter in PI and PF is observed for a given value of I. Our analyses show a complex B-field structure when observed over the whole region (~ 10 pc); however, at smaller scales (~1 pc), χBPOS varies coherently along the crests of the filament network. The observed power spectrum of χBPOS can be well represented with a power law function with a slope of − 1.33 ± 0.23, which is ~20% shallower than that of I. We find that this result is compatible with the properties of simulated filaments and may indicate the physical processes at play in the formation and evolution of star-forming filaments. Along the sub-filaments, χBPOS rotates frombeing mostly perpendicular or randomly oriented with respect to the crests to mostly parallel as the sub-filaments merge with the ridge and hubs. This variation of the B-field structure along the sub-filaments may be tracing local velocity flows of infalling matter in the ridge and hubs. Our analysis also suggests a variation in the energy balance along the crests of these sub-filaments, from magnetically critical or supercritical at their far ends to magnetically subcritical near the ridge and hubs. We also detect an increase in PF toward the high-column density (NH2 ≳ 1023 cm−2) star cluster-forming hubs. These latter large PF values may be explained by the increase in grain alignment efficiency due to stellar radiation from the newborn stars, combined with an ordered B-field structure. Conclusions. These observational results reveal for the first time the characteristics of the small-scale (down to ~ 0.1 pc) B-field structure of a 10 pc-long hub-filament system. Our analyses show variations in the polarization properties along the sub-filaments that may be tracing the evolution of their physical properties during their interaction with the ridge and hubs. We also detect an impact of feedback from young high-mass stars on the local B-field structure and the polarization properties, which could put constraints on possible models for dust grain alignment and provide important hints as to the interplay between the star formation activity and interstellar B-fields.

Published
2021

3. The JCMT BISTRO Survey:The Magnetic Field of the Barnard 1 Star-forming Region

Author

Coude, S, Bastien, P, Houde, M, Sadavoy, S, Friesen, R, Di Francesco, J, Johnstone, D, Mairs, S, Hasegawa, T, Kwon, W, Lai, S-P, Qiu, K, Ward-Thompson, D, Berry, D, Chen, MC-Y, Fiege, J, Franzmann, E, Hatchell, J, Lacaille, K, Matthews, BC, Moriarty-Schieven, GH, Pon, A, Andre, P, Arzoumanian, D, Aso, Y, Byun, D-Y, Eswaraiah, C, Chen, H-R, Chen, WP, Ching, T-C, Cho, J, Choi, M, Chrysostomou, A, Chung, EJ, Doi, Y, Drabek-Maunder, E, Dowell, CD, Eyres, SPS, Falle, S, Friberg, P, Fuller, G, Furuya, RS, Gledhill, T, Graves, SF, Greaves, JS, Griffin, MJ, Gu, Q, Hayashi, SS, Hoang, T, Holland, W, Inoue, T, Inutsuka, S-I, Iwasaki, K, Jeong, I-G, Kanamori, Y, Kataoka, A, Kang, J-H, Kang, M, Kang, S-J, Kawabata, KS, Kemper, F, Kim, G, Kim, J, Kim, K-T, Kim, KH, Kim, M-R, Kim, S, Kirk, JM, Kobayashi, MIN, Koch, PM, Kwon, J, Lee, J-E, Lee, CW, Lee, S-S, Li, D, Li, H-B, Liu, H-L, Liu, J, Liu, S-Y, Liu, T, van Loo, S, Lyo, A-R, Matsumura, M, Nagata, T, Nakamura, F, Nakanishi, H, Ohashi, N, Onaka, T, Parsons, H, Pattle, K, Peretto, N, Pyo, T-S, Qian, L, Rao, R, Rawlings, MG, Retter, B, Richer, J, Rigby, A, Robitaille, J-F, Saito, H, Savini, G, Scaife, AMM, Seta, M, Shinnaga, H, Soam, A, Tamura, M, Tang, Y-W, Tomisaka, K, Tsukamoto, Y, Wang, H, Wang, J-W, Whitworth, AP, Yen, H-W, Yoo, H, Yuan, J, Zenko, T, Zhang, C-P, Zhang, G, Zhou, J, Zhu, L, and The BISTRO Collaboration

Subjects
010504 meteorology & atmospheric sciences, INFRARED POLARIMETRY, RADIATIVE TORQUES, FOS: Physical sciences, Astrophysics, F500, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, 01 natural sciences, ISM: clouds, MOLECULAR, 0103 physical sciences, POLARIZATION MEASUREMENTS, SCUBA-2, GOULD BELT SURVEY, ISM: individual objects (Barnard 1), individual objects (Barnard 1) [ISM], ISM [submillimeter], 010303 astronomy & astrophysics, James Clerk Maxwell Telescope, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, LINEAR-POLARIZATION, polarization, stars: formation, formation [stars], Magnetic energy, Linear polarization, Molecular cloud, F510, CLOUDS, magnetic fields [ISM], Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, H2O MASERS, Magnetic field, ALIGNMENT, Amplitude, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, ISM: magnetic fields, INTERSTELLAR GRAINS, clouds [ISM]
Abstract

著者人数: The B-fields In STar-forming Regions Observations (BISTRO) Collaboration 121名 (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 權, 靜美), Number of authors: The B-fields In STar-forming Regions Observations (BISTRO) Collaboration 121 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Kwon, Jungmi), Accepted: 2019-04-18, 資料番号: SA1190042000

Published
2019

Catalog

Books, media, physical & digital resources
See catalog results