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Raffaele Rani (NTHU)Poster
CHIMPS2 is the follow-up to the 13CO/C18O (3 → 2) Heterodyne Inner Milky Way Plane Survey (CHIMPS) and the CO Hi-Resolution Survey (COHRS) and is a Large Program on the JCMT. The CHIMPS2 Inner Galaxy observations cover longitudes between 16º and 47º with −0.5º ≤ b ≤ 0.5º.
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When combined with the complementary 13CO/C18O/12CO(1-0) survey at the Nobeyama 45m at matching 15 arcsec resolution and... -
Hsiang-Yu Chen (National Central University)Poster
The Chamaeleon cloud complex is active in star formation hosting hundreds of newly born stars. Yet the adjacent Musca cloud, filamentary in shape, seem to be barren, with only a few dense cores detected, signifying the cloud being prestellar. While a far-infrared source, IRAS 12322-7023, on the basis of its IRAS colors, was reported in the literature as a T Tauri candidate, i.e., a newly...
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Chung-Chen Chang (National Taiwan Normal University Department of Earth Sciences)Poster
Multi-tracer surveys have revealed the hierarchical nature of molecular clouds, showing how high-density, small-scale features are always nested within more rarefied, larger envelopes. This structural hierarchy is, however, a non-trivial one: over-densities can always be found when smaller scales are resolved. The highest density in the hierarchy of cloud structure correspond to the site of...
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Jo-Shui Kao (NTHU/ASIAA)Poster
When dense cores or molecular clouds collapse, both the gas density (ρ) and magnetic field strength (B) increase (Crutcher+2010). Theoretical models predict that the power-law index of the B–ρ relation depends on the magnetic field orientation and the geometry of the contracting clouds (Tritsis+2015). In this project, we plan to test the core collapsing process predicted by the Textbook model...
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Yu-Xuan Lin (National Yang Ming Chiao Tung University)Poster
The magnetic field structure within protoplanetary disks is thought to influence key processes in star and planet formation.
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In this study, we aim to infer the magnetic field structure within the protoplanetary disk surrounding HD 163296, a young Class II Herbig Ae star, by analyzing archival ALMA polarization data at a wavelength of 870 µm.
Traditionally, magnetic field morphology is... -
Tien-Hao Hsieh (Taiwan Astronomical Research Alliance (TARA))Poster
Multiple systems are common in field stars and the frequency is found to be higher in early evolutionary stages. Thus, it is crucial to study young multiple systems during the embedded stages. In particular, the way material accretes from the large-scale envelope into the inner region and how this flow interacts with the system physically and chemically has not been well characterized to date....
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CHUAN-YUNG LIN (arstin001@gmail.com)Poster
We present a SMA survey of 18 Class II sources in Ophiuchus Molecular Cloud, extending previous spectral index studies from the Taurus-Auriga region. Our observations made 8 independent samples of flux densities over the 200–300 GHz frequency range. By measuring flux densities across multiple frequency bands, we derive $\alpha_{200−300\mathrm{GHz}}$ to investigate dust optical depth and grain...
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YU-SYUAN TU (中研院天文及天文物理研究所(ASIAA))Poster
HH212 is a nearby protostellar jet driven by a Class 0 protostar (IRAS 05413–0104), exhibiting a symmetric structure with knots. The Atacama Large Millimeter/submillimeter Array (ALMA) has observed the SiO J = 16–15 line in Band 9 with a resolution of 0.088″ × 0.067″, and the J = 8–7 line in Band 7 with a higher resolution of 0.022″ × 0.020″. By comparing the intensities of the two lines—after...
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Szu-Ting Chen (NTHU)Poster
To understand the influence of magnetic fields on star formation processes, we estimated the magnetic field strength in IC348, L1448, L1455, NGC1333, and B1 of the Perseus molecular cloud using the Davis-Chandrasekhar-Fermi (DCF) method and its modified approaches. The angular dispersion was derived from 850~$\mu$m polarization data observed by the JCMT, while velocity dispersion was measured...
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Raffaele Rani (NTHU)Poster
Turbulence modes and molecular cloud evolution in M33
The nature of turbulence in molecular clouds is one of the driving factors that influence the efficiency by which the gas is converted to stars. In the Milky Way, it is speculated that the high star formation efficiency observed in spiral-arm clouds is linked to the prevalence of compressive curl-free) turbulent modes in the motion of...
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