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3 results on '"Lee, SS [0000-0002-6269-594X]"'

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

Author

Hwang, J, Kim, J, Pattle, K, Lee, CW, Koch, PM, Johnstone, D, Tomisaka, K, Whitworth, A, Furuya, RS, Kang, JH, Lyo, AR, Chung, EJ, Arzoumanian, D, Park, G, Kwon, W, Kim, S, Tamura, M, Kwon, J, Soam, A, Han, I, Hoang, T, Kim, KH, Onaka, T, Eswaraiah, C, Ward-Thompson, D, Liu, HL, Tang, X, Chen, WP, Matsumura, M, Hoang, TD, Chen, Z, Le Gouellec, VJM, Kirchschlager, F, Poidevin, F, Bastien, P, Qiu, K, Hasegawa, T, Lai, SP, Byun, DY, Cho, J, Choi, M, Choi, Y, Jeong, IG, Kang, M, Kim, H, Kim, KT, Lee, JE, Lee, SS, Lee, YH, Lee, H, Kim, MR, Yoo, H, Yun, HS, Chen, M, Di Francesco, J, Fiege, J, Fissel, LM, Franzmann, E, Houde, M, Lacaille, K, Matthews, B, Sadavoy, S, Moriarty-Schieven, G, Tahani, M, Ching, TC, Dai, YS, Duan, Y, Gu, Q, Law, CY, Li, D, Li, G, Li, HB, Liu, T, Lu, X, Qian, L, Wang, H, Wu, J, Xie, J, Yuan, J, Zhang, CP, Zhang, G, Zhang, Y, Zhou, J, Zhu, L, Berry, D, Friberg, P, Graves, S, Liu, J, Mairs, S, Parsons, H, Rawlings, M, Doi, Y, Hayashi, S, Hull, CLH, Inoue, T, Inutsuka, SI, Iwasaki, K, Kataoka, A, Hwang, J [0000-0001-7866-2686], Kim, J [0000-0002-1229-0426], Pattle, K [0000-0002-8557-3582], Lee, CW [0000-0002-3179-6334], Koch, PM [0000-0003-2777-5861], Johnstone, D [0000-0002-6773-459X], Tomisaka, K [0000-0003-2726-0892], Whitworth, A [0000-0002-1178-5486], Furuya, RS [0000-0003-0646-8782], Kang, JH [0000-0001-7379-6263], Lyo, AR [0000-0002-9907-8427], Chung, EJ [0000-0003-0014-1527], Arzoumanian, D [0000-0002-1959-7201], Park, G [0000-0001-8467-3736], Kwon, W [0000-0003-4022-4132], Kim, S [0000-0001-9333-5608], Tamura, M [0000-0002-6510-0681], Kwon, J [0000-0003-2815-7774], Soam, A [0000-0002-6386-2906], Han, I [0000-0002-9143-1433], Hoang, T [0000-0003-2017-0982], Kim, KH [0000-0001-9597-7196], Onaka, T [0000-0002-8234-6747], Eswaraiah, C [0000-0003-4761-6139], Ward-Thompson, D [0000-0003-1140-2761], Liu, HL [0000-0003-3343-9645], Tang, X [0000-0002-4154-4309], Chen, WP [0000-0003-0262-272X], Matsumura, M [0000-0002-6906-0103], Hoang, TD [0000-0002-3437-5228], Chen, Z [0000-0003-0849-0692], Le Gouellec, VJM [0000-0002-5714-799X], Kirchschlager, F [0000-0002-3036-0184], Poidevin, F [0000-0002-5391-5568], Bastien, P [0000-0002-0794-3859], Qiu, K [0000-0002-5093-5088], Hasegawa, T [0000-0003-1853-0184], Lai, SP [0000-0001-5522-486X], Byun, DY [0000-0003-1157-4109], Cho, J [0000-0003-1725-4376], Jeong, IG [0000-0002-5492-6832], Kang, M [0000-0002-5016-050X], Kim, KT [0000-0003-2412-7092], Lee, JE [0000-0003-3119-2087], Lee, SS [0000-0002-6269-594X], Lee, YH [0000-0001-6047-701X], Lee, H [0000-0003-3465-3213], Kim, MR [0000-0002-1408-7747], Yoo, H [0000-0002-8578-1728], Yun, HS [0000-0001-6842-1555], Di Francesco, J [0000-0002-9289-2450], Fissel, LM [0000-0002-4666-609X], Franzmann, E [0000-0003-2142-0357], Houde, M [0000-0003-4420-8674], Lacaille, K [0000-0001-9870-5663], Matthews, B [0000-0003-3017-9577], Moriarty-Schieven, G [0000-0002-0393-7822], Tahani, M [0000-0001-8749-1436], Ching, TC [0000-0001-8516-2532], Dai, YS [0000-0002-7928-416X], Gu, Q [0000-0002-2826-1902], Li, HB [0000-0003-2641-9240], Liu, T [0000-0002-5286-2564], Lu, X [0000-0003-2619-9305], Qian, L [0000-0003-0597-0957], Wu, J [0000-0001-7276-3590], Xie, J [0000-0002-2738-146X], Zhang, CP [0000-0002-4428-3183], Zhang, Y [0000-0002-5102-2096], Zhou, J [0000-0003-0356-818X], Berry, D [0000-0001-6524-2447], Friberg, P [0000-0002-8010-8454], Graves, S [0000-0001-9361-5781], Liu, J [0000-0002-4774-2998], Mairs, S [0000-0002-6956-0730], Parsons, H [0000-0002-6327-3423], Rawlings, M [0000-0002-6529-202X], Doi, Y [0000-0001-8746-6548], Hayashi, S [0000-0001-5026-490X], Hull, CLH [0000-0002-8975-7573], Inoue, T [0000-0002-7935-8771], Inutsuka, SI [0000-0003-4366-6518], Kataoka, A [0000-0003-4562-4119], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 51 Physical Sciences
Abstract

We present and analyze observations of polarized dust emission at 850 μm toward the central 1 × 1 pc hub-filament structure of Monoceros R2 (Mon R2). The data are obtained with SCUBA-2/POL-2 on the James Clerk Maxwell Telescope (JCMT) as part of the B-fields in Star-forming Region Observations survey. The orientations of the magnetic field follow the spiral structure of Mon R2, which are well described by an axisymmetric magnetic field model. We estimate the turbulent component of the magnetic field using the angle difference between our observations and the best-fit model of the underlying large-scale mean magnetic field. This estimate is used to calculate the magnetic field strength using the Davis–Chandrasekhar–Fermi method, for which we also obtain the distribution of volume density and velocity dispersion using a column density map derived from Herschel data and the C18O (J = 3 − 2) data taken with HARP on the JCMT, respectively. We make maps of magnetic field strengths and mass-to-flux ratios, finding that magnetic field strengths vary from 0.02 to 3.64 mG with a mean value of 1.0 ± 0.06 mG, and the mean critical mass-to-flux ratio is 0.47 ± 0.02. Additionally, the mean Alfvén Mach number is 0.35 ± 0.01. This suggests that, in Mon R2, the magnetic fields provide resistance against large-scale gravitational collapse, and the magnetic pressure exceeds the turbulent pressure. We also investigate the properties of each filament in Mon R2. Most of the filaments are aligned along the magnetic field direction and are magnetically subcritical.

Published
2022
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2. 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
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3. The JCMT BISTRO survey: An 850/450μm polarization study of NGC 2071IR in Orion B

Author

Lyo, AR, Kim, J, Sadavoy, S, Johnstone, D, Berry, D, Pattle, K, Kwon, W, Bastien, P, Onaka, T, Di Francesco, J, Kang, JH, Furuya, R, Hull, CLH, Tamura, M, Koch, PM, Ward-Thompson, D, Hasegawa, T, Hoang, T, Arzoumanian, D, Lee, CW, Lee, CF, Byun, DY, Kirchschlager, F, Doi, Y, Kim, KT, Hwang, J, Diep, PN, Fanciullo, L, Lee, SS, Park, G, Yoo, H, Chung, EJ, Whitworth, A, Mairs, S, Soam, A, Liu, T, Tang, X, Coudé, S, André, P, Bourke, TL, Chen, HRV, Chen, Z, Chen, WP, Chen, M, Ching, TC, Choi, M, Choi, Y, Chrysostomou, A, Dai, S, Zhang, CP, Duan, HY, Duan, Y, Cho, J, Eden, D, Eswaraiah, C, Eyres, S, 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, Kataoka, A, Kawabata, K, Kim, G, Kim, MR, Kim, S, Kim, KH, Kirk, J, Kobayashi, MIN, Kemper, F, Könyves, V, Kusune, T, Kwon, J, Lacaille, K, Lai, SP, Lee, JE, Lee, YH, Lee, H, Li, D, Li, HB, Liu, HL, Law, CY, Liu, J, Liu, SY, Lyo, AR [0000-0002-9907-8427], Kim, J [0000-0002-1229-0426], Johnstone, D [0000-0002-6773-459X], Pattle, K [0000-0002-8557-3582], Kwon, W [0000-0003-4022-4132], Bastien, P [0000-0002-0794-3859], Onaka, T [0000-0002-8234-6747], Kang, JH [0000-0001-7379-6263], Furuya, R [0000-0003-0646-8782], Hull, CLH [0000-0002-8975-7573], Tamura, M [0000-0002-6510-0681], Koch, PM [0000-0003-2777-5861], Ward-Thompson, D [0000-0003-1140-2761], Hoang, T [0000-0003-2017-0982], Arzoumanian, D [0000-0002-1959-7201], Lee, CF [0000-0002-3024-5864], Byun, DY [0000-0003-1157-4109], Kirchschlager, F [0000-0002-3036-0184], Doi, Y [0000-0001-8746-6548], Kim, KT [0000-0003-2412-7092], Hwang, J [0000-0001-7866-2686], Lee, SS [0000-0002-6269-594X], Park, G [0000-0001-8467-3736], Yoo, H [0000-0002-8578-1728], Chung, EJ [0000-0003-0014-1527], Mairs, S [0000-0002-6956-0730], Soam, A [0000-0002-6386-2906], Liu, T [0000-0002-5286-2564], Tang, X [0000-0002-4154-4309], Coudé, S [0000-0002-0859-0805], André, P [0000-0002-3413-2293], Bourke, TL [0000-0001-7491-0048], Chen, Z [0000-0003-0849-0692], Chen, WP [0000-0002-5519-0628], Ching, TC [0000-0001-8516-2532], Chrysostomou, A [0000-0002-9583-8644], Zhang, CP [0000-0002-4428-3183], Cho, J [0000-0003-1725-4376], Eden, D [0000-0002-5881-3229], 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], 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], Kim, G [0000-0003-2011-8172], Kim, MR [0000-0002-1408-7747], Kim, S [0000-0001-9333-5608], Kirk, J [0000-0002-4552-7477], Kobayashi, MIN [0000-0003-3990-1204], Kemper, F [0000-0003-2743-8240], Könyves, V [0000-0002-3746-1498], Kusune, T [0000-0002-9218-9319], Kwon, J [0000-0003-2815-7774], Lacaille, K [0000-0001-9870-5663], Lai, SP [0000-0001-5522-486X], Lee, JE [0000-0003-3119-2087], Lee, YH [0000-0001-6047-701X], Lee, H [0000-0003-3465-3213], Li, D [0000-0003-3010-7661], Li, HB [0000-0003-2641-9240], Law, CY [0000-0003-1964-970X], Liu, J [0000-0002-4774-2998], Liu, SY [0000-0003-4603-7119], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 51 Physical Sciences
Abstract

We present the results of simultaneous 450 μm and 850 μm polarization observations toward the massive star-forming region NGC 2071IR, a target of the BISTRO (B-fields in STar-forming Region Observations) Survey, using the POL-2 polarimeter and SCUBA-2 camera mounted on the James Clerk Maxwell Telescope. We find a pinched magnetic field morphology in the central dense core region, which could be due to a rotating toroidal disklike structure and a bipolar outflow originating from the central young stellar object IRS 3. Using the modified Davis–Chandrasekhar–Fermi method, we obtain a plane-of-sky magnetic field strength of 563 ± 421 μG in the central ∼0.12 pc region from 850 μm polarization data. The corresponding magnetic energy density of 2.04 × 10−8 erg cm−3 is comparable to the turbulent and gravitational energy densities in the region. We find that the magnetic field direction is very well aligned with the whole of the IRS 3 bipolar outflow structure. We find that the median value of polarization fractions is 3.0% at 450 μm in the central 3′ region, which is larger than the median value of 1.2% at 850 μm. The trend could be due to the better alignment of warmer dust in the strong radiation environment. We also find that polarization fractions decrease with intensity at both wavelengths, with slopes, determined by fitting a Rician noise model of 0.59 ± 0.03 at 450 μm and 0.36 ± 0.04 at 850 μm, respectively. We think that the shallow slope at 850 μm is due to grain alignment at the center being assisted by strong radiation from the central young stellar objects.

Published
2021
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