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<!DOCTYPE html>
<!--[if lt IE 8 ]><html class="no-js ie ie7" lang="en"> <![endif]-->
<!--[if IE 8 ]><html class="no-js ie ie8" lang="en"> <![endif]-->
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<html class="no-js" lang="en">
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<head>
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<meta charset="utf-8">
<title>Ming-yi's astronomical website</title>
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<!-- <li><a class="smoothscroll" href="#about">About</a></li> -->
<!-- <li><a class="smoothscroll" href="#resume">Observations</a></li> -->
<!-- <li><a class="smoothscroll" href="#testimonials">Sciences</a></li> -->
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<!-- <h1 class="responsive-headline">Ming-Yi Lin</h1> -->
<h1>Ming-Yi Lin</h1>
<!-- style="font-size: 20px" -->
<h3>
I'm a postdoctral researcher in the Department of Physics and Astronomy at the University
of Toledo in Ohio, USA. My current scientific research interests include the supermassive
black hole (SMBH)-host galaxy co-evolution, feeding and feedback mechanism, and multi-wavelength observations.
I was a software testing engineer in the <a href="https://cartavis.org/" target="_blank">CARTA</a> project
in Academia Sinica Institute of Astronomy and Astrophysics (ASIAA) in Taipei, Taiwan.
I developed an automated framework for both the backend and frontend to ensure the accuracy and robustness of the software.
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and check <a class="smoothscroll" href="#about">my CV</a>.</h3> -->
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<img class="profile-pic" src="images/lin.jpg" alt="" />
</div>
<div class="nine columns main-col">
<h2>About Me</h2>
<p>
I was born in Taipei City, Taiwan. Since childhood, I have been fascinated by the beauty of the natural
sciences, which inspired me to pursue a B.S. degree in Earth Sciences. In my sophomore year, I was first
introduced to professional astronomy research, which led me to complete an M.S. degree in Astronomy at
National Taiwan Normal University and a Ph.D. in Astrophysics at Ludwig-Maximilians-Universität München.
I am now eager to further explore various aspects of astronomy, including both software and hardware
development. My personal interests include watching operas, musicals, and Japanese animation.
</p>
<div class="row">
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<h2>Contact Details</h2>
<p class="address">
<span>Ming-Yi LIN</span><br>
<span>University of Toledo<br>
2801 Bancroft St, Toledo, <br>
Ohio, 43606, USA
</span><br>
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<p>
<a href="./Website_Resume-2026-03-18.pdf" class="button"><i class="fa fa-download"></i>Download Curriculum
Vitae</a>
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<!-- Resume Section
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<section id="resume">
<!-- Education
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<div class="three columns header-col">
<h1><span>Observations </span></h1>
</div>
<div class="nine columns main-col">
<div class="row item">
<div class="twelve columns">
<h3>Near Infrared</h3>
<h5><p class="tight"> - Keck </p> </h5>
<p>
I am currently working on the NSF-funded AGN project (PI: <a href="https://www.utoledo.edu/nsm/physast/people/anne-medling.html" target="_blank">Prof. Anne Medling</a>).
My work focuses on analyzing OSIRIS data, including improving the mosaics and studying the gas and stellar kinematics.
I plan to build a dynamical mass model to test the modified Bondi SMBH accretion as well as accretion driven by
gravitational torques.
</p>
<h5><p class="tight"> - Very Large Telescope (VLT)</p> </h5>
<p>
The VLT Large Program (PI: <a href="http://www.mpe.mpg.de/ir/userpage.php?id=davies_ric" target="_blank">Dr. Richard Davies</a>) 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.
</p>
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<h3>Radio</h3>
<h5><p class="tight"> - Institut de Radioastronomie Millimétrique (IRAM)</p> </h5>
<p>
I studied HCN and HCO⁺ emission in the nuclear regions of nearby AGNs using data from the Plateau de Bure Interferometer (PdBI).
Recently, I have been using the new NOEMA-PolyFix instrument to observe CO gas kinematics and investigate AGN feedback mechanisms.
</p>
<h5><p class="tight"> - Yuan-Tseh Lee Array (YTLA) </p></h5>
<p>
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).
</p>
<h5><p class="tight"> - Submillimeter Array (SMA) </p></h5>
<p>
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.
</p>
</div>
</div> <!-- item end -->
<div class="row item">
<div class="twelve columns">
<h3>Optical</h3>
<h5><p class="tight"> - Binocular Telescope (LBT)</p> </h5>
<p>
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.
</p>
</div>
</div>
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</div> <!-- End Education -->
<!-- Portfolio Section
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<h1>Scientific Results & Daily Life Photos</h1>
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<h5>Obscured AGNs</h5>
<p>Scientific Results</p>
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<h5>Geometrically Thick Molecular Disk</h5>
<p>Scientific Results</p>
</div>
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</a>
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<h5>Nuclear Star Formation</h5>
<p>Scientific Results</p>
</div>
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<h5>Linderhof Palace</h5>
<p>Daily life photo</p>
</div>
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</a>
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<img alt="" src="images/alice.jpg">
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<h5>Ballet</h5>
<p>Daily life photo</p>
</div>
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</a>
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<img alt="" src="images/portfolio/small_flower.jpg">
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<div class="portfolio-item-meta">
<h5>Floristry</h5>
<p>Daily life photo</p>
</div>
</div>
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</a>
</div>
</div> <!-- item end -->
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</div> <!-- twelve columns end -->
<!-- Modal Popup
--------------------------------------------------------------- -->
<div id="modal-01" class="popup-modal mfp-hide">
<img class="scale-with-grid" src="images/kstest.jpg" alt="" />
<div class="description-box">
<h4>Kolmogorov-Smirnov test:</h4>
<p>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.</p>
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<a href="https://ui.adsabs.harvard.edu/abs/2016MNRAS.456.2735L/abstract" target="_blank">ADS</a>
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<img class="scale-with-grid" src="images/hcn_hco+.jpg" alt="" />
<div class="description-box">
<h4>Dense molecular gas in the nuclear regions of nearby AGNs</h4>
<p>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.</p>
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<div class="description-box">
<h4>Nuclear Star Formation</h4>
<p>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 pro le. 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 speci c radius. We attached the pPXF return mean stellar velocity
dispersion error (25km/s in average) in the bottom left
corner.</p>
<!-- <span class="categories"><i class="fa fa-tag"></i>Branding</span> -->
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<a href="https://ui.adsabs.harvard.edu/abs/2018MNRAS.473.4582L/abstract" target="_blank">ADS</a>
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<h4>Linderhof Palace</h4>
<p>2017.07.29</p>
<span class="categories"><i class="fa fa-tag"></i>Ettal, Germany</span>
</div>
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<h4>Alice in Wonderland Ballet</h4>
<p>2017.05.01</p>
<span class="categories"><i class="fa fa-tag"></i>München, Deutschland</span>
</div>
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<img class="scale-with-grid" src="images/flower.jpg" alt="" />
<div class="description-box">
<h4>Floristry</h4>
<p>2016.04.10</p>
<span class="categories"><i class="fa fa-tag"></i>München, Deutschland</span>
</div>
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<h4>Origami</h4>
<p>Proin gravida nibh vel velit auctor aliquet. Aenean sollicitudin, lorem quis bibendum auctor, nisi
elit consequat ipsum, nec sagittis sem nibh id elit.</p>
<span class="categories"><i class="fa fa-tag"></i>Branding, Illustration</span>
</div>
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<h4>Retrocam</h4>
<p>Proin gravida nibh vel velit auctor aliquet. Aenean sollicitudin, lorem quis bibendum auctor, nisi
elit consequat ipsum, nec sagittis sem nibh id elit.</p>
<span class="categories"><i class="fa fa-tag"></i>Webdesign, Photography</span>
</div>
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<li>© Copyright 2014 CeeVee</li>
<li>Design by <a href="http://www.styleshout.com/" title="Styleshout" target="_blank">Styleshout</a>
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<li>Modified by Ming-yi LIN</li>
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