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<!DOCTYPE HTML>
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<h2>Evolution of massive galaxies and galaxy clusters</h2>
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<p>Our Universe was most active 10-11 billion years ago. At this time, the bulk of the star formation was enshrouded in the most dust-obscured galaxies, and they form stars at a very high rate. My research focuses on unresolved issues about the nature of these dusty galaxies. What are the fundemental drivers of the extreme star formation in the early Universe: violent galaxy interactions/mergers or secularly evolving processes? What are the relative contributions of these processes to the cosmic star formation history? How do these dusty galaxies link to the first collapses of the Universe's largest structure - massive galaxy clusters?</p>
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<h3>A talk on "Galaxy Collisions!" at Astronomy on Tap in Austin</h3>
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<h3>Physical drivers of extreme star formation</h3>
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<p>I have been tackling this issue through the combination of multiwavelength observational data and hydrodynamical simulations. My early work on characterizing more than two thousands dusty galaxiess selected by Herschel observations show that galaxy interactions are responsible to trigger more than half of these galaxies at redshift of 1. This link between galaxy mergers and dusty galaxiess has important implications on the assembly of massive galaxy clusters. Several progenitors of massive galaxy clusters host overabundance of these dusty galaxiess. A possible explaination for this type of protoclusters is that the build-up of massive structure in the early Universe may be highly episodic rather than a steady process lasting several billion year. A few undergraduate researchers have been working with me on this topic through characterizing overall population of galaxy pairs and gas content in these large structures to better understand the formation of massive clusters. </p>
<ul class="actions">
<li><a href="http://adsabs.harvard.edu/abs/2013ApJ...778..129H" class="button" target="_blank">Hung et al. (2013)</a></li>
<li><a href="http://adsabs.harvard.edu/abs/2016ApJ...826..130H" class="button" target="_blank">Hung et al. (2016b)</a></li>
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<img src="images/PC2.png" alt="" width="400"></a>
<p>My recent work on a young galaxy cluster at redshift of 2. This structure sits in the center of the COSMOS/CANDELS field. The rich ancillary data allow us to study the details of dusty galaxies.</p>
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<h3>Calibrating observational tools</h3>
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<p>Our observational tools to study distant dusty galaxies can be limited and sometimes biased. For example, large-scale tidal features commonly seen in nearby galaxy mergers often fade away or become less prominent if they were more distant. I have compiled a set of nearby well-studied dusty galaxies (so called ultraluminous infrared galaxies) and simulate how their high-resolution imaging and integral field spectrosgraph (IFS) observations degrade at higher redshift. With this I show that when identifying merger signatures (e.g., tidal tails, bridges) visually, at least 20% of the distant mergers can be missed simply due to data differences like surface brightness dimming and band-shifting. Interaction-induced disturbances in galaxy dynamics (from 2D velocity and velocity dispersion maps) are often absent in late-stage galaxy mergers with resolutions (~1 kpc) comparable to high-redshift observations. My follow-up analysis using hydrodynamic simulations confirm these conclusions with various initial conditions of galaxy interactions. The goal is that we can eventually use these simulations and nearby well-studied galaxies to calibrate and correct for our measurements of high-redshift galaxies.</p>
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<li><a href="http://adsabs.harvard.edu/abs/2016ApJ...816...99H" class="button" target="_blank">Hung et al. (2016a)</a></li>
<li><a href="http://adsabs.harvard.edu/abs/2014ApJ...791...63H" class="button" target="_blank">Hung et al. (2014)</a></li>
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<img src="images/ulirg_ifu.png" alt="" width="400"></a>
<p>This figure demonstrates the breadth of galaxy velocity fields (in terms of the level of complexity) at a given galaxy interaction stage.</p>
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<li><a href="http://adsabs.harvard.edu/abs/2015ApJ...803...62H" class="button" target="_blank">Hung et al. (2015)</a></li>
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