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8 results on '"Tamura, M [0000-0002-6510-0681]"'

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 JWST early release science program for the direct imaging and spectroscopy of exoplanetary systems

Author

Sasha Hinkley, Aarynn L. Carter, Shrishmoy Ray, Andrew Skemer, Beth Biller, Elodie Choquet, Maxwell A. Millar-Blanchaer, Stephanie Sallum, Brittany Miles, Niall Whiteford, Polychronis Patapis, Marshall Perrin, Laurent Pueyo, Glenn Schneider, Karl Stapelfeldt, Jason Wang, Kimberly Ward-Duong, Brendan P. Bowler, Anthony Boccaletti, Julien H. Girard, Dean Hines, Paul Kalas, Jens Kammerer, Pierre Kervella, Jarron Leisenring, Eric Pantin, Yifan Zhou, Michael Meyer, Michael C. Liu, Mickael Bonnefoy, Thayne Currie, Michael McElwain, Stanimir Metchev, Mark Wyatt, Olivier Absil, Jea Adams, Travis Barman, Isabelle Baraffe, Mariangela Bonavita, Mark Booth, Marta Bryan, Gael Chauvin, Christine Chen, Camilla Danielski, Matthew De Furio, Samuel M. Factor, Michael P. Fitzgerald, Jonathan J. Fortney, Carol Grady, Alexandra Greenbaum, Thomas Henning, Kielan K. W. Hoch, Markus Janson, Grant Kennedy, Matthew Kenworthy, Adam Kraus, Masayuki Kuzuhara, Pierre-Olivier Lagage, Anne-Marie Lagrange, Ralf Launhardt, Cecilia Lazzoni, James Lloyd, Sebastian Marino, Mark Marley, Raquel Martinez, Christian Marois, Brenda Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Mark Phillips, Simon Petrus, Sascha P. Quanz, Andreas Quirrenbach, Julien Rameau, Isabel Rebollido, Emily Rickman, Matthias Samland, B. Sargent, Joshua E. Schlieder, Anand Sivaramakrishnan, Jordan M. Stone, Motohide Tamura, Pascal Tremblin, Taichi Uyama, Malavika Vasist, Arthur Vigan, Kevin Wagner, Marie Ygouf, University of Exeter, University of California (UC), SUPA School of Physics and Astronomy [Edinburgh], University of Edinburgh, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Institute for Astronomy [Edinburgh] (IfA), Centre for Exoplanet Science, Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Space Telescope Science Institute (STSci), Steward Observatory, University of Arizona, University of Notre Dame [Indiana] (UND), McDonald Observatory, University of Texas at Austin [Austin], Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, University of Michigan [Ann Arbor], University of Michigan System, University of Hawaii, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, NASA, University of Western Ontario (UWO), University of Cambridge [UK] (CAM), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), The Open University [Milton Keynes] (OU), Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Université Paris-Saclay, Eureka Scientific, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Stockholm University, University of Warwick [Coventry], Leiden Observatory [Leiden], Universiteit Leiden, National Astronomical Observatory of Japan (NAOJ), Cornell University [New York], University of Victoria [Canada] (UVIC), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg] = Heidelberg University, GSFC Exoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center (GSFC), US Naval Research Laboratory, Maison de la Simulation (MDLS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut National de Recherche en Informatique et en Automatique (Inria)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), NASA ExoPlanet Science Institute (NExScI), Institute for Astronomy, Department of Physics, ETH Zürich, Ministerio de Ciencia e Innovación (España), European Commission, Hinkley, S [0000-0001-8074-2562], Carter, AL [0000-0001-5365-4815], Ray, S [0000-0003-2259-3911], Millar-Blanchaer, MA [0000-0001-6205-9233], Patapis, P [0000-0001-8718-3732], Perrin, M [0000-0002-3191-8151], Stapelfeldt, K [0000-0002-2805-7338], Wang, J [0000-0003-0774-6502], Ward-Duong, K [0000-0002-4479-8291], Boccaletti, A [0000-0001-9353-2724], Girard, JH [0000-0001-8627-0404], Kalas, P [0000-0002-6221-5360], Kammerer, J [0000-0003-2769-0438], Kervella, P [0000-0003-0626-1749], Leisenring, J [0000-0002-0834-6140], Zhou, Y [0000-0003-2969-6040], Meyer, M [0000-0003-2232-7664], Liu, MC [0000-0003-0241-8956], Absil, O [0000-0002-4006-6237], Bonavita, M [0000-0002-7520-8389], Booth, M [0000-0001-8568-6336], Chen, C [0000-0002-8382-0447], Danielski, C [0000-0002-3729-2663], De Furio, M [0000-0003-1863-4960], Factor, SM [0000-0002-8332-8516], Fortney, JJ [0000-0002-9843-4354], Greenbaum, A [0000-0002-7162-8036], Janson, M [0000-0001-8345-593X], Kenworthy, M [0000-0002-7064-8270], Kuzuhara, M [0000-0002-4677-9182], Martinez, R [0000-0001-6301-896X], Marois, C [0000-0002-4164-4182], Matthews, B [0000-0003-3017-9577], Matthews, EC [0000-0003-0593-1560], Quanz, SP [0000-0003-3829-7412], Rebollido, I [0000-0002-4388-6417], Rickman, E [0000-0003-4203-9715], Samland, M [0000-0001-9992-4067], Sargent, B [0000-0001-9855-8261], Sivaramakrishnan, A [0000-0003-1251-4124], Stone, JM [0000-0003-0454-3718], Tamura, M [0000-0002-6510-0681], Vigan, A [0000-0002-5902-7828], and Apollo - University of Cambridge Repository

Subjects
FOS: Physical sciences, 5109 Space Sciences, Space telescopes, detection-techniques, Exoplanet detection methods, Direct imaging, adaptive optics-instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), instrumentation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 5101 Astronomical Sciences, Astrophysics::Earth and Planetary Astrophysics, Coronagraphic imaging, Astrophysics - Instrumentation and Methods for Astrophysics, 51 Physical Sciences, interferometers-planets and satellites, high angular resolution, Exoplanet atmospheres, Astrophysics - Earth and Planetary Astrophysics
Abstract

Full list of authors: Hinkley, Sasha; Carter, Aarynn L.; Ray, Shrishmoy; Skemer, Andrew; Biller, Beth; Choquet, Elodie; Millar-Blanchaer, Maxwell A.; Sallum, Stephanie; Miles, Brittany; Whiteford, Niall; Patapis, Polychronis; Perrin, Marshall; Pueyo, Laurent; Schneider, Glenn; Stapelfeldt, Karl; Wang, Jason; Ward-Duong, Kimberly; Bowler, Brendan P.; Boccaletti, Anthony; Girard, Julien H.; Hines, Dean; Kalas, Paul; Kammerer, Jens; Kervella, Pierre; Leisenring, Jarron; Pantin, Eric; Zhou, Yifan; Meyer, Michael; Liu, Michael C.; Bonnefoy, Mickael; Currie, Thayne; McElwain, Michael; Metchev, Stanimir; Wyatt, Mark; Absil, Olivier; Adams, Jea; Barman, Travis; Baraffe, Isabelle; Bonavita, Mariangela; Booth, Mark; Bryan, Marta; Chauvin, Gael; Chen, Christine; Danielski, Camilla; De Furio, Matthew; Factor, Samuel M.; Fitzgerald, Michael P.; Fortney, Jonathan J.; Grady, Carol; Greenbaum, Alexandra; Henning, Thomas; Hoch, Kielan K. W.; Janson, Markus; Kennedy, Grant; Kenworthy, Matthew; Kraus, Adam; Kuzuhara, Masayuki; Lagage, Pierre-Olivier; Lagrange, Anne-Marie; Launhardt, Ralf; Lazzoni, Cecilia; Lloyd, James; Marino, Sebastian; Marley, Mark; Martinez, Raquel; Marois, Christian; Matthews, Brenda; Matthews, Elisabeth C.; Mawet, Dimitri; Mazoyer, Johan; Phillips, Mark; Petrus, Simon; Quanz, Sascha P.; Quirrenbach, Andreas; Rameau, Julien; Rebollido, Isabel; Rickman, Emily; Samland, Matthias; Sargent, B.; Schlieder, Joshua E.; Sivaramakrishnan, Anand; Stone, Jordan M.; Tamura, Motohide; Tremblin, Pascal; Uyama, Taichi; Vasist, Malavika; Vigan, Arthur; Wagner, Kevin; Ygouf, Marie.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/3.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., The direct characterization of exoplanetary systems with high-contrast imaging is among the highest priorities for the broader exoplanet community. As large space missions will be necessary for detecting and characterizing exo-Earth twins, developing the techniques and technology for direct imaging of exoplanets is a driving focus for the community. For the first time, JWST will directly observe extrasolar planets at mid-infrared wavelengths beyond 5 μm, deliver detailed spectroscopy revealing much more precise chemical abundances and atmospheric conditions, and provide sensitivity to analogs of our solar system ice-giant planets at wide orbital separations, an entirely new class of exoplanet. However, in order to maximize the scientific output over the lifetime of the mission, an exquisite understanding of the instrumental performance of JWST is needed as early in the mission as possible. In this paper, we describe our 55 hr Early Release Science Program that will utilize all four JWST instruments to extend the characterization of planetary-mass companions to ∼15 μm as well as image a circumstellar disk in the mid-infrared with unprecedented sensitivity. Our program will also assess the performance of the observatory in the key modes expected to be commonly used for exoplanet direct imaging and spectroscopy, optimize data calibration and processing, and generate representative data sets that will enable a broad user base to effectively plan for general observing programs in future Cycles. © 2022. The Author(s). Published by IOP Publishing Ltd on behalf of the Astronomical Society of the Pacific (ASP). All rights reserved., This project was supported by a grant from STScI (JWST-ERS-01386) under NASA contract NAS5-03127. M.T.is supported by JSPS KAKENHI Grant No.18H05442. M.B. acknowledges support from the Deutsche Forschungsgemeinschaft (DFG) through grant Kr 2164/13–2. K.W. acknowledges support from NASA through the NASA Hubble Fellowship grant HST-HF2-51472.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Published
2022

4. 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
Full Text
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5. TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

Author

Gilbert A. Esquerdo, Walter Boschin, Lars A. Buchhave, Allyson Bieryla, Karen A. Collins, Eric L. N. Jensen, Nobuhiko Kusakabe, David F. Phillips, Chelsea X. Huang, Jack J. Lissauer, Steve B. Howell, Norio Narita, E. Girardin, Christopher A. Watson, Enric Palle, Damien Ségransan, R. D. Haywood, P. Guerra, David W. Latham, S. Giacalone, Jonathan Irwin, Avi Shporer, Keivan G. Stassun, Giampaolo Piotto, E. Esparza-Borges, Gloria Andreuzzi, Felipe Murgas, Marco Pedani, Francesco Pepe, Mercedes Lopez-Morales, Scott McDermott, Courtney D. Dressing, Robert Massey, Motohide Tamura, George R. Ricker, Annelies Mortier, Giuseppina Micela, Jessie L. Christiansen, Emilio Molinari, Pau Bosch-Cabot, Jon M. Jenkins, Roland Vanderspek, Aldo F. M. Fiorenzano, Samuel N. Quinn, Hannu Parviainen, Ken Rice, Avet Harutyunyan, Akihiko Fukui, Sara Seager, Elisa V. Quintana, Massimo Cecconi, Mark E. Rose, R. Cloutier, Luca Di Fabrizio, Joshua N. Winn, Alessandro Sozzetti, Arjun B. Savel, Andrew Collier Cameron, David Charbonneau, Rachel A. Matson, Michel Mayor, Dimitar Sasselov, Christophe Lovis, Stéphane Udry, Gábor Fűrész, Xavier Dumusque, Cloutier, R [0000-0001-5383-9393], Charbonneau, D [0000-0002-9003-484X], Stassun, KG [0000-0002-3481-9052], Murgas, F [0000-0001-9087-1245], Mortier, A [0000-0001-7254-4363], Massey, R [0000-0001-8879-7138], Lissauer, JJ [0000-0001-6513-1659], Latham, DW [0000-0001-9911-7388], Haywood, RD [0000-0001-9140-3574], Guerra, P [0000-0002-4308-2339], Giacalone, SA [0000-0002-8965-3969], Bieryla, A [0000-0001-6637-5401], Winn, J [0000-0002-4265-047X], Watson, CA [0000-0002-9718-3266], Vanderspek, R [0000-0001-6763-6562], Udry, S [0000-0001-7576-6236], Tamura, M [0000-0002-6510-0681], Sozzetti, A [0000-0002-7504-365X], Shporer, A [0000-0002-1836-3120], Ségransan, D [0000-0003-2355-8034], Seager, S [0000-0002-6892-6948], Savel, AB [0000-0002-2454-768X], Sasselov, D [0000-0001-7014-1771], Rose, M [0000-0003-4724-745X], Ricker, G [0000-0003-2058-6662], Rice, K [0000-0002-6379-9185], Quintana, EV [0000-0003-1309-2904], Quinn, SN [0000-0002-8964-8377], Piotto, G [0000-0002-9937-6387], Phillips, D [0000-0001-5132-1339], Pedani, M [0000-0002-5752-6260], Parviainen, H [0000-0001-5519-1391], Palle, E [0000-0003-0987-1593], Narita, N [0000-0001-8511-2981], Molinari, E [0000-0002-1742-7735], Micela, G [0000-0002-9900-4751], Mayor, M [0000-0002-9352-5935], Matson, RA [0000-0001-7233-7508], López-Morales, M [0000-0003-3204-8183], Kusakabe, N [0000-0001-9194-1268], Jensen, ELN [0000-0002-4625-7333], Jenkins, JM [0000-0002-4715-9460], Huang, CX [0000-0003-0918-7484], Howell, SB [0000-0002-2532-2853], Fukui, A [0000-0002-4909-5763], Esquerdo, GA [0000-0002-9789-5474], Esparza-Borges, E [0000-0002-2341-3233], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Collins, KA [0000-0001-6588-9574], Cameron, AC [0000-0002-8863-7828], Christiansen, JL [0000-0002-8035-4778], Buchhave, LA [0000-0003-1605-5666], Boschin, W [0000-0001-9978-9109], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Physics, Earth and Planetary Astrophysics (astro-ph.EP), Radial velocity, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Radius, 3rd-DAS, Sitting, Exoplantet strcuture, QC Physics, Space and Planetary Science, Planet, astro-ph.EP, Period (geology), QB Astronomy, Planetary system formation, Low mass stars, Astrophysics::Earth and Planetary Astrophysics, Transit photometry, QC, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

Studies of close-in planets orbiting M dwarfs have suggested that the M dwarf radius valley may be well-explained by distinct formation timescales between enveloped terrestrials, and rocky planets that form at late times in a gas-depleted environment. This scenario is at odds with the picture that close-in rocky planets form with a primordial gaseous envelope that is subsequently stripped away by some thermally-driven mass loss process. These two physical scenarios make unique predictions of the rocky/enveloped transition's dependence on orbital separation such that studying the compositions of planets within the M dwarf radius valley may be able to establish the dominant physics. Here, we present the discovery of one such keystone planet: the ultra-short period planet TOI-1634 b ($P=0.989$ days, $F=121 F_{\oplus}$, $r_p = 1.790^{+0.080}_{-0.081} R_{\oplus}$) orbiting a nearby M2 dwarf ($K_s=8.7$, $R_s=0.45 R_{\odot}$, $M_s=0.50 M_{\odot}$) and whose size and orbital period sit within the M dwarf radius valley. We confirm the TESS-discovered planet candidate using extensive ground-based follow-up campaigns, including a set of 32 precise radial velocity measurements from HARPS-N. We measure a planetary mass of $4.91^{+0.68}_{-0.70} M_{\oplus}$, which makes TOI-1634 b inconsistent with an Earth-like composition at $5.9\sigma$ and thus requires either an extended gaseous envelope, a large volatile-rich layer, or a rocky portion that is not dominated by iron and silicates to explain its mass and radius. The discovery that the bulk composition of TOI-1634 b is inconsistent with that of the Earth favors the gas-depleted formation mechanism to explain the emergence of the radius valley around M dwarfs with $M_s\lesssim 0.5 M_{\odot}$., Comment: 27 pages, 13 figures, accepted to AAS journals. Our time series are included as a csv file in the arXiv source files

Published
2021

6. The JCMT BISTRO Survey: Revealing the Diverse Magnetic Field Morphologies in Taurus Dense Cores with Sensitive Submillimeter Polarimetry

Author

Eswaraiah, C, Li, D, Furuya, RS, Hasegawa, T, Ward-Thompson, D, Qiu, K, Ohashi, N, Pattle, K, Sadavoy, S, Hull, CLH, Berry, D, Doi, Y, Ching, TC, Lai, SP, Wang, JW, Koch, PM, Kwon, J, Kwon, W, Bastien, P, Arzoumanian, D, Coudé, S, Soam, A, Fanciullo, L, Yen, HW, Liu, J, Hoang, T, Ping Chen, W, Shimajiri, Y, Liu, T, Chen, Z, Li, HB, Lyo, AR, Hwang, J, Johnstone, D, Rao, R, Bich Ngoc, N, Ngoc Diep, P, Mairs, S, Parsons, H, Tamura, M, Tahani, M, Vivien Chen, HR, Nakamura, F, Shinnaga, H, Tang, YW, Cho, J, Won Lee, C, Inutsuka, SI, Inoue, T, Iwasaki, K, Qian, L, Xie, J, Liu, HL, Zhang, CP, Chen, M, Zhang, G, Zhu, L, Zhou, J, André, P, Liu, SY, Yuan, J, Lu, X, Peretto, N, Bourke, TL, Byun, DY, Dai, S, Duan, Y, Duan, HY, Eden, D, Matthews, B, Fiege, J, Fissel, LM, Kim, KT, Lee, CF, Kim, J, Pyo, TS, Choi, Y, Choi, M, Chrysostomou, A, Jung Chung, E, Ngoc Tram, L, 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, Kawabata, K, Jeong, IG, Kang, JH, Kang, SJ, Kang, M, Eswaraiah, C [0000-0003-4761-6139], Furuya, RS [0000-0003-0646-8782], Hasegawa, T [0000-0003-1853-0184], Ward-Thompson, D [0000-0003-1140-2761], Qiu, K [0000-0002-5093-5088], Ohashi, N [0000-0003-0998-5064], Pattle, K [0000-0002-8557-3582], Sadavoy, S [0000-0001-7474-6874], Hull, CLH [0000-0002-8975-7573], Berry, D [0000-0001-6524-2447], Doi, Y [0000-0001-8746-6548], Ching, TC [0000-0001-8516-2532], Lai, SP [0000-0001-5522-486X], Wang, JW [0000-0002-6668-974X], Koch, PM [0000-0003-2777-5861], Kwon, J [0000-0003-2815-7774], Kwon, W [0000-0003-4022-4132], Bastien, P [0000-0002-0794-3859], Arzoumanian, D [0000-0002-1959-7201], Coudé, S [0000-0002-0859-0805], Soam, A [0000-0002-6386-2906], Fanciullo, L [0000-0001-9930-9240], Yen, HW [0000-0003-1412-893X], Liu, J [0000-0002-4774-2998], Hoang, T [0000-0003-2017-0982], Ping Chen, W [0000-0003-0262-272X], Shimajiri, Y [0000-0001-9368-3143], Liu, T [0000-0002-5286-2564], Chen, Z [0000-0003-0849-0692], Li, HB [0000-0003-2641-9240], Lyo, AR [0000-0002-9907-8427], Hwang, J [0000-0001-7866-2686], Johnstone, D [0000-0002-6773-459X], Rao, R [0000-0002-1407-7944], Bich Ngoc, N [0000-0002-5913-5554], Ngoc Diep, P [0000-0002-2808-0888], Mairs, S [0000-0002-6956-0730], Parsons, H [0000-0002-6327-3423], Tamura, M [0000-0002-6510-0681], Tahani, M [0000-0001-8749-1436], Vivien Chen, HR [0000-0002-9774-1846], Nakamura, F [0000-0001-5431-2294], Shinnaga, H [0000-0001-9407-6775], Tang, YW [0000-0002-0675-276X], Cho, J [0000-0003-1725-4376], Won Lee, C [0000-0002-3179-6334], Inutsuka, SI [0000-0003-4366-6518], Iwasaki, K [0000-0002-2707-7548], Qian, L [0000-0003-0597-0957], Xie, J [0000-0002-2738-146X], Liu, HL [0000-0003-3343-9645], Zhang, CP [0000-0002-4428-3183], Zhou, J [0000-0003-0356-818X], André, P [0000-0002-3413-2293], Liu, SY [0000-0003-4603-7119], Lu, X [0000-0003-2619-9305], Bourke, TL [0000-0001-7491-0048], Byun, DY [0000-0003-1157-4109], Eden, D [0000-0002-5881-3229], Matthews, B [0000-0003-3017-9577], Fissel, LM [0000-0002-4666-609X], Kim, KT [0000-0003-2412-7092], Lee, CF [0000-0002-3024-5864], Kim, J [0000-0002-1229-0426], Pyo, TS [0000-0002-3273-0804], Chrysostomou, A [0000-0002-9583-8644], Jung Chung, E [0000-0003-0014-1527], Ngoc Tram, L [0000-0002-6488-8227], 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], Griffin, M [0000-0002-0033-177X], Gu, Q [0000-0002-2826-1902], Hatchell, J [0000-0002-4870-2760], Houde, M [0000-0003-4420-8674], Kawabata, K [0000-0001-6099-9539], Jeong, IG [0000-0002-5492-6832], Kang, JH [0000-0001-7379-6263], Kang, SJ [0000-0002-5004-7216], Kang, M [0000-0002-5016-050X], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 51 Physical Sciences
Abstract

We have obtained sensitive dust continuum polarization observations at 850 μm in the B213 region of Taurus using POL-2 on SCUBA-2 at the James Clerk Maxwell Telescope as part of the B-fields in STar-forming Region Observations (BISTRO) survey. These observations allow us to probe magnetic field (B-field) at high spatial resolution (∼2000 au or ∼0.01 pc at 140 pc) in two protostellar cores (K04166 and K04169) and one prestellar core (Miz-8b) that lie within the B213 filament. Using the Davis–Chandrasekhar–Fermi method, we estimate the B-field strengths in K04166, K04169, and Miz-8b to be 38 ± 14, 44 ± 16, and 12 ± 5 μG, respectively. These cores show distinct mean B-field orientations. The B-field in K04166 is well ordered and aligned parallel to the orientations of the core minor axis, outflows, core rotation axis, and large-scale uniform B-field, in accordance with magnetically regulated star formation via ambipolar diffusion taking place in K04166. The B-field in K04169 is found to be ordered but oriented nearly perpendicular to the core minor axis and large-scale B-field and not well correlated with other axes. In contrast, Miz-8b exhibits a disordered B-field that shows no preferred alignment with the core minor axis or large-scale field. We found that only one core, K04166, retains a memory of the large-scale uniform B-field. The other two cores, K04169 and Miz-8b, are decoupled from the large-scale field. Such a complex B-field configuration could be caused by gas inflow onto the filament, even in the presence of a substantial magnetic flux.

Published
2021

7. An Ultra-Hot Neptune in the Neptune desert

Author

Todd C. Klaus, Jose I. Vines, Ruth Titz-Weider, Motohide Tamura, Jessie L. Christiansen, Samuel N. Quinn, M. G. Soto, J. Villasenor, Pablo Rojas, George R. Ricker, Simon R. Walker, Maximiliano Moyano, Nicolás T. Kurtovic, Sara Seager, Sean McCauliff, Maximilian N. Günther, Andrés Jordán, Juan Cabrera, Pascal Torres, Michael R. Goad, Jerome de Leon, Giovanni Isopi, David R. Ciardi, Daniel Bayliss, K. I. Collins, Peter J. Wheatley, Jack J. Lissauer, Norio Narita, David W. Latham, François Bouchy, Sarah L. Casewell, Oliver Turner, Mayuko Mori, Andrea Ercolino, Cristobal Petrovich, Richard G. West, E. Foxell, Claudia Belardi, Philipp Eigmüller, James McCormac, Tom Louden, Eric D. Lopez, Liam Raynard, Benjamin F. Cooke, Edward Gillen, George W. King, Allyson Bieryla, Karen A. Collins, Matias Diaz, Heike Rauer, David J. Armstrong, Jack S. Acton, James A. G. Jackman, Don Pollacco, Anders Erikson, Néstor Espinoza, Michael Vezie, Samuel Gill, Nicholas M. Law, Carl Ziegler, Jon M. Jenkins, Edward M. Bryant, Rafael Brahm, Alexis M. S. Smith, Charles Beichman, Boris T. Gänsicke, Roland Vanderspek, Andrew W. Mann, Taku Nishiumi, Pía Cortés-Zuleta, Didier Queloz, Rosanna H. Tilbrook, Matthew J. Hooton, Louise D. Nielsen, Joshua N. Winn, Christopher J. Burke, Alexander Chaushev, Matthew R. Burleigh, Enric Palle, James S. Jenkins, Christopher E. Henze, Stéphane Udry, F. Mallia, Christopher A. Watson, Jenkins, JS [0000-0003-2733-8725], Espinoza, N [0000-0001-9513-1449], Brahm, R [0000-0002-9158-7315], Cortés-Zuleta, P [0000-0002-6174-4666], Wheatley, PJ [0000-0003-1452-2240], Winn, JN [0000-0002-4265-047X], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Bieryla, A [0000-0001-6637-5401], Christiansen, JL [0000-0002-8035-4778], Mori, M [0000-0003-1368-6593], Narita, N [0000-0001-8511-2981], Nishiumi, T [0000-0003-1510-8981], Tamura, M [0000-0002-6510-0681], Lissauer, JJ [0000-0001-6513-1659], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Armstrong, DJ [0000-0002-5080-4117], Bayliss, D [0000-0001-6023-1335], Cabrera, J [0000-0001-6653-5487], Casewell, SL [0000-0003-2478-0120], Eigmüller, P [0000-0003-4096-0594], Günther, MN [0000-0002-3164-9086], Hooton, MJ [0000-0003-0030-332X], Queloz, D [0000-0002-3012-0316], Smith, AMS [0000-0002-2386-4341], Udry, S [0000-0001-7576-6236], Watson, CA [0000-0002-9718-3266], West, RG [0000-0001-6604-5533], and Apollo - University of Cambridge Repository

Subjects
Extrasolare Planeten und Atmosphären, Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, 010504 meteorology & atmospheric sciences, Leitungsbereich PF, Library science, FOS: Physical sciences, Astronomy and Astrophysics, Northern ireland, 01 natural sciences, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Political science, 0103 physical sciences, astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Research center, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, QB, Astrophysics - Earth and Planetary Astrophysics
Abstract

About one out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultra-short-period planet (Sanchis-ojeda et al. 2014; Winn et al. 2018). All of the previously known ultra-short-period planets are either hot Jupiters, with sizes above 10 Earth radii (Re), or apparently rocky planets smaller than 2 Re. Such lack of planets of intermediate size (the "hot Neptune desert") has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here, we report the discovery of an ultra-short-period planet with a radius of 4.6 Re and a mass of 29 Me, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite (Ricker et al. 2015) revealed transits of the bright Sun-like star \starname\, every 0.79 days. The planet's mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0^(+2.7)_(-2.9)% of the total mass. With an equilibrium temperature around 2000 K, it is unclear how this "ultra-hot Neptune" managed to retain such an envelope. Follow-up observations of the planet's atmosphere to better understand its origin and physical nature will be facilitated by the star's brightness (Vmag=9.8)., Comment: 26 pages, 10 figures, 3 tables. Published in Nature Astronomy (21/09/2020)

Published
2020
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8. High-contrast Polarimetry Observation of T Tau Circumstellar Environment

Author

Eugene Serabyn, Wolfgang Brandner, Edwin L. Turner, Toru Yamada, Gillian R. Knapp, Thomas Henning, Satoshi Mayama, Shoken Miyama, Hideki Takami, Yi Yang, Jungmi Kwon, Eiji Akiyama, Michihiro Takami, Hiroshi Terada, Miwa Goto, Ryuji Suzuki, Takuya Suenaga, Naruhisa Takato, Lyu Abe, Yutaka Hayano, Tomoyuki Kudo, Michael W. McElwain, T. Currie, Tomonori Usuda, Ryo Kandori, Markus Janson, Takao Nakagawa, Nobuhiko Kusakabe, Klaus W. Hodapp, Yasuhiro H. Takahashi, Jun-Ichi Morino, Jun Hashimoto, Masayuki Kuzuhara, Tetsuo Nishimura, Roman R. Rafikov, Makoto Watanabe, Masanori Iye, Daehyeon Oh, Joseph C. Carson, Hiroshi Suto, Taro Matsuo, Munetake Momose, Timothy D. Brandt, Motohide Tamura, Tae-Soo Pyo, Christian Thalmann, Olivier Guyon, Amaya Moro-Martin, Miki Ishii, Carol A. Grady, Masahiko Hayashi, Sebastian Egner, Saeko S. Hayashi, Markus Feldt, John P. Wisniewski, Yang, Y [0000-0002-9024-4150], Mayama, S [0000-0002-3424-6266], Akiyama, E [0000-0002-5082-8880], Currie, T [0000-0002-7405-3119], Janson, M [0000-0001-8345-593X], Momose, M [0000-0002-3001-0897], Nakagawa, T [0000-0002-6660-9375], Oh, D [0000-0003-2691-804X], Kudo, T [0000-0002-9294-1793], Brandt, TD [0000-0003-2630-8073], Guyon, O [0000-0002-1097-9908], Hayano, Y [0000-0003-4937-4233], Hodapp, KW [0000-0003-0786-2140], Kandori, R [0000-0003-2610-6367], Knapp, GR [0000-0002-9259-1164], Kwon, J [0000-0003-2815-7774], Miyama, S [0000-0001-5017-180X], Moro-Martin, A [0000-0001-9504-8426], Pyo, TS [0000-0002-3273-0804], Takami, M [0000-0001-9248-7546], Terada, H [0000-0002-7914-6779], Thalmann, C [0000-0002-1664-2177], Watanabe, M [0000-0002-3656-4081], Wisniewski, J [0000-0001-9209-1808], Usuda, T [0000-0001-9855-0163], Tamura, M [0000-0002-6510-0681], and Apollo - University of Cambridge Repository

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Astrophysics, stars: pre-main sequence, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010309 optics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Adaptive optics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, binaries: general (T Tau), protoplanetary disks, Astronomy and Astrophysics, Polarization (waves), Position angle, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, stars: variables: T Tauri, Herbig Ae/Be, Outflow, Astrophysics::Earth and Planetary Astrophysics, Circumbinary planet, Subaru Telescope, Astrophysics - Earth and Planetary Astrophysics
Abstract

著者人数: 55名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 中川, 貴雄; 權, 靜美), Accepted: 2018-05-18, 資料番号: SA1180099000

Published
2018

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