Probing Galaxy Dark Matter at Cosmic Noon
Poster Number
22A
Format
Poster Presentation
Faculty Mentor Name
Guillermo Barro
Faculty Mentor Department
Physics
Abstract/Artist Statement
Dark matter is a form of matter that makes up the majority of the mass in a galaxy, yet is not directly detectable through any form of radiation. Although not directly observable, we can indirectly measure dark matter by measuring the rotation curves of galaxies.
Understanding and quantifying the presence of dark matter in galaxies is essential to understanding how galaxies form and evolve. Ultimately, the dark matter content of galaxies will be measured at half the universe's current age as well as later epochs in the universe.
The change in galaxy dark matter content over time will provide insight into how dark matter, and in turn how galaxies evolve over time.
Working under Dr. Guillermo Barro, I researched the dark evolution of dark matter in distant quiescent galaxies with a redshift z ~ 1. I started with several hundreds of galaxies taken from the HALO7D survey.
I then filtered this down to the quiescent galaxies that have a redshift z~1. I analyzed the spectroscopic properties of these galaxies using the technique of full-spectral fitting using the data from the HALO7D survey.
After this, I used the program index to measure line-strength indices in fully calibrated FITS spectra. I am currently sorting through the different properties found ( flux, SNR) of about 50 galaxies.
From here, I will be able to characterize some fundamental properties of these galaxies such as the age of their stars, their chemical compositions, and dark matter content.
Location
Information Commons, William Knox Holt Memorial Library and Learning Center
Start Date
29-4-2023 10:00 AM
End Date
29-4-2023 1:00 PM
Probing Galaxy Dark Matter at Cosmic Noon
Information Commons, William Knox Holt Memorial Library and Learning Center
Dark matter is a form of matter that makes up the majority of the mass in a galaxy, yet is not directly detectable through any form of radiation. Although not directly observable, we can indirectly measure dark matter by measuring the rotation curves of galaxies.
Understanding and quantifying the presence of dark matter in galaxies is essential to understanding how galaxies form and evolve. Ultimately, the dark matter content of galaxies will be measured at half the universe's current age as well as later epochs in the universe.
The change in galaxy dark matter content over time will provide insight into how dark matter, and in turn how galaxies evolve over time.
Working under Dr. Guillermo Barro, I researched the dark evolution of dark matter in distant quiescent galaxies with a redshift z ~ 1. I started with several hundreds of galaxies taken from the HALO7D survey.
I then filtered this down to the quiescent galaxies that have a redshift z~1. I analyzed the spectroscopic properties of these galaxies using the technique of full-spectral fitting using the data from the HALO7D survey.
After this, I used the program index to measure line-strength indices in fully calibrated FITS spectra. I am currently sorting through the different properties found ( flux, SNR) of about 50 galaxies.
From here, I will be able to characterize some fundamental properties of these galaxies such as the age of their stars, their chemical compositions, and dark matter content.