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


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


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


Twisted magnetic field in star formation processes of L1521 F revealed by submillimeter dual-band polarimetry using the James Clerk Maxwell Telescope

Publications of the Astronomical Society of Japan


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


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


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

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.


Magnetic fields and outflows in the large Bok globule CB 54

Monthly Notices of the Royal Astronomical Society


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

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 μ 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 μ 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 μ m) and short-wavelength (HAWC+, ≲200μ 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.


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

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 ${N}_{{{m{H}}}_{2}}t 0.93imes {10}^{22}$ 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 ${N}_{{{m{H}}}_{2}}pprox 4.6imes {10}^{22}$ cm-2. This can be interpreted as a signature of core formation. At ${N}_{{{m{H}}}_{2}}pprox 16imes {10}^{22}$ 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 (BPOS = 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.


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

We investigate the internal 3D magnetic structure of dense interstellar filaments within NGC 1333 using polarization data at 850 μm from the B-fields In STar-forming Region Observations survey at the James Clerk Maxwell Telescope. Theoretical models predict that the magnetic field lines in a filament will tend to be dragged radially inward (i.e., pinched) toward the central axis due to the filament's self-gravity. We study the cross-sectional profiles of the total intensity (I) and polarized intensity (PI) of dust emission in four segments of filaments unaffected by local star formation that are expected to retain a pristine magnetic field structure. We find that the filaments' FWHMs in PI are not the same as those in I, with two segments being appreciably narrower in PI (FWHM ratio ≃0.7 0.8) and one segment being wider (FWHM ratio ≃1.3). The filament profiles of the polarization fraction (P) do not show a minimum at the spine of the filament, which is not in line with an anticorrelation between P and I normally seen in molecular clouds and protostellar cores. Dust grain alignment variation with density cannot reproduce the observed P distribution. We demonstrate numerically that the I and PI cross-sectional profiles of filaments in magnetohydrostatic equilibrium will have differing relative widths depending on the viewing angle. The observed variations of FWHM ratios in NGC 1333 are therefore consistent with models of pinched magnetic field structures inside filaments, especially if they are magnetically near-critical or supercritical.


The JCMT BISTRO Survey: An 850/450 μm Polarization Study of NGC 2071IR in Orion B

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.


The JCMT BISTRO Survey: The Distribution of Magnetic Field Strengths toward the OMC-1 Region


Two-component Magnetic Field along the Line of Sight to the Perseus Molecular Cloud: Contribution of the Foreground Taurus Molecular Cloud


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


The JCMT BISTRO-2 Survey: The Magnetic Field in the Center of the Rosette Molecular Cloud


OMC-1 dust polarization in ALMA Band 7: diagnosing grain alignment mechanisms in the vicinity of Orion Source I


Dust polarized emission observations of NGC 6334. BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network


JCMT POL-2 and BISTRO Survey Observations of Magnetic Fields in the L1689 Molecular Cloud


Observations of Magnetic Fields Surrounding LkHα 101 Taken by the BISTRO Survey with JCMT-POL-2


The JCMT BISTRO Survey: Alignment between Outflows and Magnetic Fields in Dense Cores/Clumps


The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333


Application of a helicity proxy to edge-on galaxies

Monthly Notices of the Royal Astronomical Society


Editorial: The Role of Magnetic Fields in the Formation of Stars

Frontiers in Astronomy and Space Sciences


JCMT BISTRO Survey Observations of the Ophiuchus Molecular Cloud: Dust Grain Alignment Properties Inferred Using a Ricean Noise Model


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


JCMT BISTRO Survey: Magnetic Fields within the Hub-filament Structure in IC 5146


The JCMT BISTRO Survey: The Magnetic Field in the Starless Core ρ Ophiuchus C


A 1000 au Scale Molecular Outflow Driven by a Protostar with an Age of <4000 yr


Magnetic fields towards Ophiuchus-B derived from SCUBA-2 polarization measurements

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


First Observations of the Magnetic Field inside the Pillars of Creation: Results from the BISTRO Survey

We present the first high-resolution, submillimeter-wavelength polarimetric observations of and thus direct observations of the magnetic field morphology within the dense gas of the Pillars of Creation in M16. These 850 m observations, taken as part of the B-Fields in Star-forming Region Observations Survey (BISTRO) using the POL-2 polarimeter on the Submillimeter Common-User Bolometer Array 2 (SCUBA-2) camera on the James Clerk Maxwell Telescope (JCMT), show that the magnetic field runs along the length of the Pillars, perpendicular to and decoupled from the field in the surrounding photoionized cloud. Using the Chandrasekhar Fermi method we estimate a plane-of-sky magnetic field strength of 170 320 G in the Pillars, consistent with their having been formed through the compression of gas with initially weak magnetization. The observed magnetic field strength and morphology suggests that the magnetic field may be slowing the Pillars' evolution into cometary globules. We thus hypothesize that the evolution and lifetime of the Pillars may be strongly influenced by the strength of the coupling of their magnetic field to that of their parent photoionized cloud i.e., that the Pillars' longevity results from magnetic support.


A First Look at BISTRO Observations of the ϱ Oph-A core

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


The JCMT BISTRO Survey: The Magnetic Field Strength in the Orion A Filament

We determine the magnetic field strength in the OMC 1 region of the Orion A filament via a new implementation of the Chandrasekhar Fermi method using observations performed as part of the James Clerk Maxwell Telescope (JCMT) B-Fields In Star-forming Region Observations (BISTRO) survey with the POL-2 instrument. We combine BISTRO data with archival SCUBA-2 and HARP observations to find a plane-of-sky magnetic field strength in OMC 1 of ${B}_{athrm{pos}}=6.6m 4.7$ mG, where $elta {B}_{athrm{pos}}=4.7$ mG represents a predominantly systematic uncertainty. We develop a new method for measuring angular dispersion, analogous to unsharp masking. We find a magnetic energy density of $im 1.7imes {10}^{-7}$ J m-3 in OMC 1, comparable both to the gravitational potential energy density of OMC 1 (~10-7 J m-3) and to the energy density in the Orion BN/KL outflow (~10-7 J m-3). We find that neither the Alfvén velocity in OMC 1 nor the velocity of the super-Alfvénic outflow ejecta is sufficiently large for the BN/KL outflow to have caused large-scale distortion of the local magnetic field in the ~500 yr lifetime of the outflow. Hence, we propose that the hourglass field morphology in OMC 1 is caused by the distortion of a primordial cylindrically symmetric magnetic field by the gravitational fragmentation of the filament and/or the gravitational interaction of the BN/KL and S clumps. We find that OMC 1 is currently in or near magnetically supported equilibrium, and that the current large-scale morphology of the BN/KL outflow is regulated by the geometry of the magnetic field in OMC 1, and not vice versa.


High-resolution Observations of the Massive Protostar in IRAS 18566+0408

We report 3 mm continuum, CH3CN(5 4) and 13CS(2 1) line observations with CARMA (Combined Array for Research in Millimeter-wave Astronomy), in conjunction with 6 and 1.3 cm continuum VLA data, and 12 and 25 m broadband data from the Subaru Telescope toward the massive proto-star IRAS 18566+0408. The VLA data resolve the ionized jet into four components aligned in the E W direction. Radio components A, C, and D have flat centimeter SEDs indicative of optically thin emission from ionized gas, and component B has a spectral index = 1.0, and a decreasing size with frequency $ropto {u }^{-0.5}$. Emission from the CARMA 3 mm continuum and from the 13CS(2 1) and CH3CN(5 4) spectral lines is compact (i.e., $t 6700athrm{au}$) and peaks near the position of the VLA centimeter source, component B. Analysis of these lines indicates hot and dense molecular gas, which is typical for HMCs. Our Subaru telescope observations detect a single compact source, coincident with radio component B, demonstrating that most of the energy in IRAS 18566+0408 originates from a region of size $t 2400athrm{au}$. We also present UKIRT near-infrared archival data for IRAS 18566+0408, which show extended K-band emission along the jet direction. We detect an E W velocity shift of about 10 km s-1 over the HMC in the CH3CN lines possibly tracing the interface of the ionized jet with the surrounding core gas. Our data demonstrate the presence of an ionized jet at the base of the molecular outflow and support the hypothesis that massive protostars with O-type luminosity form with a mechanism similar to lower mass stars.


First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt

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


A massive dense gas cloud close to the nucleus of the Seyfert galaxy NGC 1068

Using the ALMA archival data of both 12CO (6 5) line and 689-GHz continuum emission towards the archetypical Seyfert galaxy, NGC 1068, we identified a distinct continuum peak separated by 15 pc from the nuclear radio component S1 in projection. The continuum flux gives a gas mass of 2 × 105 M and bolometric luminosity of 108 L, leading to a star formation rate of 0.1 M yr-1. Subsequent analysis on the line data suggest that the gas cloud has a size of 10 pc, yielding to a mean H2 number density of 105 cm-3. We therefore refer to the gas as a ''massive dense gas cloud'': the gas density is high enough to form a ''protostar cluster'' with a stellar mass of 104 M. We found that the gas stands at a unique position between galactic and extraglactic clouds in the diagrams of start formation rate (SFR) vs. gas mass proposed by Lada et al. (2012, ApJ, 745, 190) and surface density of gas vs. SFR density by Krumholz and McKee (2005, ApJ, 630, 250). All the gaseous and star-formation properties may be understood in terms of the turbulence-regulated star formation scenario. Since there are two stellar populations with ages of 300 Myr and 30 Myr in the 100 pc scale circumnulear region, we discuss that NGC 1068 has experienced at least three episodic star-formation events with the likelihood that the inner star-forming region is the younger. Together with several lines of evidence that the dynamics of the nuclear region is decoupled from that of the entire galactic disk, we discuss that the gas inflow towards the nuclear region of NGC 1068 may be driven by a past minor merger.

Publications of the Astronomical Society of Japan


Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA


A Dynamically Collapsing Core and a Precursor of a Core in a Filament Supported by Turbulent and Magnetic Pressures


A study on subarcsecond scales of the ammonia and continuum emission toward the G16.59-0.05 high-mass star-forming region

Aims. We wish to investigate the structure, velocity field, and stellar content of the G16.590.05 high-mass star-forming region, where previous studies have established the presence of two almost perpendicular (NESW and SENW), massive outflows, and a rotating disk traced by methanol maser emission.Methods. We performed Very Large Array observations of the radio continuum and ammonia line emission, complemented by COMICS/Subaru and Hi-GAL/Herschel images in the mid- and far-infrared.Results. Our centimeter continuum maps reveal a collimated radio jet that is oriented EW and centered on the methanol maser disk, placed at the SE border of a compact molecular core. The spectral index of the jet is negative, indicating non-thermal emission over most of the jet, except the peak close to the maser disk, where thermal free-free emission is observed. We find that the ammonia emission presents a bipolar structure consistent (on a smaller scale) in direction and velocity with that of the NESW bipolar outflow detected in previous CO observations. After analyzing our previous N2H+(10) observations again, we conclude that two scenarios are possible. In one case both the radio jet and the ammonia emission would trace the root of the large-scale CO bipolar outflow. The different orientation of the jet and the ammonia flow could be explained by precession and/or a non-isotropic density distribution around the star. In the other case, the N2H+(10) and ammonia bipolarity is interpreted as two overlapping clumps moving with different velocities along the line of sight. The ammonia gas also seems to undergo rotation consistent with the maser disk. Our infrared images complemented by archival data allow us to derive a bolometric luminosity of ~104 L and to conclude that most of the luminosity is due to the young stellar object associated with the maser disk.Conclusions. The new data suggest a scenario where the luminosity and the outflow activity of the whole region could be dominated by two massive young stellar objects: 1) a B-type star of ~12 M at the center of the maser/ammonia disk; 2) a massive young stellar object (so far undetected), very likely in an earlier stage of evolution than the B-type star, which might be embedded inside the compact molecular core and power the massive, SENW outflow.


Massive star-formation toward G28.87+0.07 (IRAS 18411 0338) investigated by means of maser kinematics and radio to infrared, continuum observations


Infall, outflow, and rotation in the G19.61- 0.23 hot molecular core


Class I and Class II methanol masers in high-mass star forming regions


VLBI study of maser kinematics in high-mass SFRs. I. G16.59-0.05


VLBI study of maser kinematics in high-mass SFRs. II. G23.01-0.41


Looking for high-mass young stellar objects: and H2O masers in massive ammonia cores


Warm Extended Dense Gas Lurking At The Heart of A Cold Collapsing Dense Core


High Velocity Outflow in CO J=7 6 from the Orion Hot Core


Spectroscopic Evidence for Gas Infall in GF9-2


Submillimeter Observations of the Isolated Massive Dense Clump IRAS 20126+4104


Low-Mass Star-Forming Cores in the GF9 Filament


Candidate Rotating Toroids around High-Mass (Proto)Stars


Massive Star- Formation in G24.78+0.08 Explored through VLBI Maser Observations


The Initial Conditions for Gravitational Collapse of a Core: An Extremely Young Low-Mass Class 0 Protostar GF9-2


Infall of Gas as the Formation Mechanism of Stars with Mass up to 20 Times More Massive than the Sun

Theory predicts and observations confirm that low-mass stars (like the Sun) in their early life grow by accreting gas from the surrounding material. But for stars approximately 10 times more massive than the Sun (approximately 10M(o)), the powerful stellar radiation is expected to inhibit accretion and thus limit the growth of their mass. Clearly, stars with masses >10M(o) exist, so there must be a way for them to form. The problem may be solved by non-spherical accretion, which allows some of the stellar photons to escape along the symmetry axis where the density is lower. The recent detection of rotating disks and toroids around very young massive stars has lent support to the idea that high-mass ( > 8M(o)) stars could form in this way. Here we report observations of an ammonia line towards a high-mass star forming region. We conclude that the gas is falling inwards towards a very young star of approximately 20M(o), in line with theoretical predictions of non-spherical accretion.


First results from a VLBA Proper Motion Survey of H2O Masers in Low-Mass YSOs: the Serpens Core and RNO15-FIR


A Detailed Study of the Rotating toroids in G31.41+0.31 and G24.78+0.08


Relative Evolutionary Time Scale of Hot Molecular Cores with Respect to Ultra Compact HII Regions


Proper Motion of H2O Masers in IRAS 20050+2720 MMS1: An AU Scale Jet Associated with An Intermediate- Mass Class 0 Source


Rotating Disks in High-Mass Young Stellar Objects


A Giant Flare on a T Tauri Star Observed at Millimeter Wavelengths

Publications of the Astronomical Society of Japan


Interferometric Observations of FeO towards Sagittarius B2


Anatomy of a High-Mass Star Forming Cloud: The G24.78+0.08 (Proto)Stellar Cluster


Water Maser Survey towards Low-Mass Young Stellar Objects in the Northern Sky with the Nobeyama 45-m Telescope and the Very Large Array

The Astrophysical Journal. Supplement Series


Monthly Notices of the Royal Astronomical Society


G24.78 +0.08: A Cluster of High-Mass (Proto)Stars


Water Maser Survey toward Low-Mass Young Stellar Objects in the Northern Sky: Observational Constraints on Maser Excitation Conditions


VLA Observations of H2O Masers in the Class 0 Protostar S106 FIR: Evidence for a 10 AU Scale Accelerating Jetlike Flow


大型サブミリ波望遠鏡LST計画 科学白書2023

大型サブミリ波望遠鏡LST計画 科学白書2023

Large Submillimeter Telescope Document Series, DOI 10.15000/lstds118687, https://www.lstobservatory.org/post/lst-wp-2023j


Pinched Magnetic Field around the Massive Star Forming Region Monoceros R2: An Analysis of Planck Polarimetric Images

IAU Symposium No. 360, "Astronomical Polarimetry 2020: New Era of Multiwavelength Polarimetry"


Magnetic field of a dense core L1521 F in Taurus molecular cloud


Magnetic Fields Studies in the Next Decade: EAO Submillimetre Futures White Paper Series, 2019


Compact Molecular Outflow from a Protostar at the Earliest Evolutionary Phase

"The Labyrinth of Star Formation", Astrophysics and Space Science Proceedings, Volume 36. ISBN 978-3-319-03040-1, Springer International Publishing Switzerland


An Interview to Faculties and High Schools in Tokushima : Towards Seamless Connections from High Schools to University --- ―高校から大学への教育の接続をより良いものにするために―

徳島大学教員と徳島県内の高校関係者へのインタビュー調査 --- ―高校から大学への教育の接続をより良いものにするために―

これまで高等学校までの教育内容にゆとりを持たせていたことに加え,少子化による大学進学率 の上昇が相まって,大学初年度で学ぶべき水準についていけない学生の存在が徳島大学においても顕在 化している．一方で,大学卒業生の質は一定の水準を保つべきという社会的要請がある．この現状を鑑 み,本学の理念に基づく,教育目標と教育水準を堅持するため,高校と大学の接続教育に求められるも のは何かを明確にすることが求められている．このため,アンケート調査では拾い上げることが容易で ない,教職員の率直な意見を2012年夏から冬にかけて大学と高校双方における対面インタビュー調査に よって収集した．寄せられた意見と教育現場からの示唆の大部分は,中央教育審議会や日本学術会議等 の答申等と整合する．したがって,大局的な見地に立ちつつ,地域の特性も考慮した,より良い高等教 育システムを作り上げることが求められている．

Journal of University Education Research


Infall and the Formation of a Massive Star

"Massive Star Formation: Observations Confront Theory", ASP Conference Series, Astronomical Society of the Pacific


Probing Jet and Disk Winds toward Low-Mass Protostars

"Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA", ASP Conference Proceedings, Astronomical Society of the Pacific


"Galactic Star Formation Across the Stellar Mass Spectrum", ASP Conference Series, Astronomical Society of the Pacific


Imaging of 2-mm dust continuum emission towards S106 FIR and its spectral energy distribution

"Cosmic Masers: From Proto-Stars to Black Holes", IAU Symposium 206, Astronomical Society of the Pacific