I was born in Taipei City, Taiwan. I love the beauty of natural sciences since I was a child, thus I decide to study Earth Sciences for my B.S degree. I met the professional astronomy research in my sophomore year, after that, I finish the M.S degree in Astronomy in National Taiwan Normal University and the PhD degree in Astrophysics in Ludwig-Maximilians-Universität München. Now I would like to explore much knowledge related to astronomy, either from software or hardware development aspects. My personal interests include watching operas, musicals, and Japanese animations.
11F of Astronomy-Mathematics Building, AS/NTU
No.1, Sec. 4, Roosevelt Rd,
Taipei 10617, Taiwan
★ Binocular Telescope (LBT)
The science program belongs to Dr. Eva Wuyts. I was a volunteer student to work with instrument scientists and telescope operators. In the six-day observations, my works included assisting the observing program execution, assessing weather condition, communicating with LBTO staff.
★ Very Large Telescope (VLT)
The VLT Large Program (PI: Dr. Richard Davies) goes into individual ESO observation period (93P, 98P, and 99P). My works include preparing the observation blocks (OBs), doing the data reduction, and improving the calibration pipeline. In order to retrieve higher S/N ratio in absorption lines, I reduce the effects of differential atmospheric refraction by theoretical calculation in the both the image and spectroscopy. Such effect becomes significant for high-resolution observations (e.g. AO mode) at near-infrared wavelengths.
★ Submillimeter Array (SMA)
My first professional astronomy research is using SMA data to study the shell kinematics of post-AGB star. I used MIR and MIRID to flag out bad data and reconstruct the image. I also complete one night observation for the summer student group project – searching the methanol signal from high-z galaxy.
★ Institut de Radioastronomie Millimétrique (IRAM)
I studied the HCN and HCO+ in the nuclear regions for the nearby AGNs with Plateau de Bure Interferometer(PdBI) data. Recently I use new instrument – PolyFix to observe the CO gas kinematic to study the AGN feedback mechanism.
★ Yuan-Tseh Lee Array (YTLA)
It is a 7 small dishes interferometer project leaded by Taiwan (former name:AMiBA). I assist daytime and nighttime observing and work closely with engineers/project scientist to do the troubleshooting, for example: decompose the antennae amplitudes and looking for whether they correlate to the instrumental temperatures. I also measure the quasar continuum flux density, then compare to the System Equivalent Flux Density(SEFD) in order to check the instrument stability, it is a part of commissioning test and verification phases. (On site during Aug 2018, Oct-Dec 2018).
Distribution of XMM and Chandra indicate these samples are drawn from the same population. However, the distribution of 70μm/X-ray sample and X-ray selected samples seem not to be drawn from the same population. The distributions indicate an excess of HR ≥ -0.3, revealing that the cold dust from the host galaxy may be responsible for additional obscuration.
We use dense molecular gas HCN(1-0) and HCO+(1-0) at 1” resolution to trace the rotating molecular disk on scales of ~100 pc scale for nearby Seyferts. By modeling the observed kinematics, we find that the geometrically think molecular disk is quite common, indicating the supernovae could potentially being a source to provide the additional energy to maintain the vertical structure.
The best sample of simple toy model to explain the trend of radial stellar velocity dispersion. Top panel: The radial luminosity for observed data point (black pluses) and bulge component (red dashed line). Middle panel: The bulge fraction as a function of radius. Bottom panel: The radial stellar velocity dispersion with radius. The black solid line represents the intrinsic bulge velocity dispersion, which is calculated based on the bulge surface brightness prole. Considering the contributions come from both a dynamically hot bulge population (typical is several hundredkm/s) and a dynamically cold young star population (we assume 40-50 km/s), the luminosity-weighted velocity dispersion is presented in blue dashed line. Pink pluses are the observed data with the error bar representing the 1-σ error with respect to the velocity dispersion inside the 2-D elliptical rings at specic radius. We attached the pPXF return mean stellar velocity dispersion error (25km/s in average) in the bottom left corner.
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