Some of the galaxies/halos in the Caterpillar suite of simulations. We identify and investigate the ultra-faint dwarfs in each of these halos. Image from Griffen et al (2016).
Formation histories of ultra-faint dwarf galaxies in the Caterpillar simulations
Ultra-faint dwarf galaxies (UFDs) are the oldest and faintest galaxies in the cosmos. While some of them already merged with other galaxies to form bigger galaxies, we can still see many hanging around the Milky Way. Because they are incredibly old, they are like “cosmic fossils,” providing clues into what the early universe might have looked like.
But how do these ultra-faint dwarf galaxies form? This is the main question we seek to answer in this project. Are there differences in their formation depending on where they formed? That is, is there a difference between a UFD that is infalling (within the virial radius) with a large galaxy like the Milky Way versus one that is infalling with a smaller galaxy like the Large Magellanic Cloud (LMC)? Should we expect their formation histories to differ?
Within the Caterpillar simulations, we identify these two types of UFDs (those infalling with large Milky Way-like galaxies and those infalling with medium-sized LMC-like galaxies). After that, we look at their physical properties and see if there are any interesting differences.
For this project, I’m working with Professor Anna Frebel and Kaley Brauer at the MIT Kavli Institute for Astrophysics and Space Research. This project is under MIT’s Undergraduate Research Opportunities Program (UROP).
(Clockwise) Red elliptical, blue spiral, red spiral, blue elliptical. Image from Galaxy Zoo.
Investigating the origins of red spiral galaxies in the IllustrisTNG simulations
Galaxies are broadly classified by color and morphology. Color can be used as a crude indicator of the age of the galaxy’s stellar content. A blue galaxy is generally younger and more active at star formation because its emission is dominated by hot, blue stars which are relatively short-lived and therefore young. In contrast, a red galaxy is older and inactive because its stellar population is mostly composed of dim, red stars which have already burned through their fuel. On the other hand, a galaxy’s morphology–whether it is spiral or elliptical–contains information about its dynamical history.
Interestingly, most observed galaxies follow a color-morphology relation such that spiral galaxies are typically blue and elliptical galaxies are typically red. However, data from the Sloan Digital Sky Survey reveal hundreds of red spiral galaxies–a population which deviates from the classification scheme.
Now, how exactly did these red spirals form? Because of their anomalous nature, red spirals might reveal new insights about galaxy formation. For this project, I used data from IllustrisTNG, a state-of-the-art cosmological hydrodynamic simulation. From the galaxies in IllustrisTNG, we identified red spirals using color and morphological criteria. From there, we plotted their physical properties to see how they formed.
For this project, I worked with Professor Mark Vogelsberger and Hui Li at the MIT Kavli Institute for Astrophysics and Space Research. This project was under MIT’s Undergraduate Research Opportunities Program (UROP).
🎤 CONFERENCE PRESENTATION / INVITED TALK
Communicating science to the public through video: Experiences and techniques from a Breakthrough Junior Challenge winner
Andales, H.D. (2018)
Proceedings of the 36th Samahang Pisika ng Pilipinas (Physics Society of the Philippines) Physics Conference
More than ever, scientists are compelled to share relevant scientific knowledge to the public in order to address misinformation, inform decision-making, increase public support for scientific ventures, or promote widespread appreciation for science. Through accessible media production technology and social media, it is now much easier for scientists to be communicators and for the public to be receivers.
In this talk, I will elaborate my experiences, strategies, and lessons in video-based science communication as the sole researcher, writer, producer, and creator of two short Physics videos: (1) Feynman’s Path Integrals and (2) Relativity and the Equivalence of Reference Frames. The former was awarded the Special Prize during the 2016 Breakthrough Junior Challenge. Meanwhile, the latter video was declared the Winner of the 2017 edition of the same competition, where it bested 11,000 entries from 178 countries. This second video has accumulated over 5,000,000 views across all platforms.
The talk will also detail how I created the videos, how the public received and interpreted the videos’ information, as well as how scientists can use video for science communication.
H. D. Andales. Communicating science to the public through video: Experiences and techniques from a Breakthrough Junior Challenge winner, Proceedings of the Samahang Pisika ng Pilipinas 36, SPP-2018-INV-1C-02 (2018)
🎤 POSTER PRESENTATION
N-body simulation of celestial bodies with differentiable motions in 2D space
Andales, H.D. & Roque, P.J.C. (2017)
Proceedings of the 5th International Meeting of Complex Systems
My poster for the internship’s culminating poster presentation; received Best Poster Award
🔎 PROJECT 🎤 POSTER PRESENTATION
Fractal Visualization in Mathematica & Parallel Computing in C
Andales, H.D. (2015)
National Institute of Physics Interns’ Poster Presentations
In the summer after 9th grade, I interned at the National Institute of Physics in Diliman, Quezon City, Philippines. I worked with Professor Francis Paraan in the Structure and Dynamics (SanD) Lab. During the two-week program, I completed two projects: MandelZoom and Function Integration Through Rectangle Rule.
MandelZoom is a fractal visualization tool created using Mathematica while Function Integration computes integrals numerically using MPI (message passing interface) in C. At the end of the internship, I received the Best Poster Award out of the >20 interns in the program.