We will explore ways to make astronomy, and STEM fields in general, a more inclusive and welcoming environment where EVERYONE can feel comfortable. This will make all people, including traditionally underrepresented groups, feel comfortable and welcomed working in our field.
Extinction mapping with LEGUS
The study of star formation and galaxy evolution in nearby galaxies depends on obtaining accurate stellar photometry in those galaxies. However, dust in the galaxies hinders our ability to obtain accurate stellar photometry, particularly in star-forming galaxies that have the highest concentrations of dust. This proposal presents a thesis project to develop a method for generating extragalactic extinction maps using photometry of massive stars from the Hubble Space Telescope. This photometry spans nearly 50 galaxies observed by the Legacy Extragalactic Ultraviolet Survey (LEGUS). The derived extinction maps can be used to correct other stars and Halpha maps (from the Halpha LEGUS) for extinction, and will be used to constrain changes in the dust-to-gas ratio across the galaxy sample and in different star formation rate, metallicity and morphological environments. Previous studies have found links between galaxy metallicty and the dust-to-gas mass ratio. The relationship between these two quantities can be used to constrain chemical evolution models.
Selected galaxies will also be compared to IR-derived dust maps for comparison to recent M31 results from Dalcanton et al. (2015) which found a minimum factor of 2 inconsistency between their extinction-derived maps and emission-derived maps from Draine et al. (2014).
The NMSU Department of Astronomy will hold an observatory open house at the NMSU campus observatory at 8 p.m.Friday, Sept. 9. Astronomy personnel on hand will be Chris Churchill and graduate assistants Xander Thelen, Trevor Picard and Jacob Vander Vliet.
Guests can view Mars and Saturn together in the evening sky in the constellation of Scorpio. Telescopes will also have the center of the Milky Way Galaxy in view, and in this region there are many beautiful star clusters and globular clusters (tight groups of millions of stars). High in the sky, viewers will see the constellation Vega with its double-double star system and the famous ring nebula, which is the remnants of a dying star much like our own sun. The moon will be in the phase called first quarter and will make a wonderful sight.
Contact the NMSU Astronomy Department at 575-646-4438 with questions. Everyone is welcome to come and spend an evening of stargazing. Admission is free and children are especially welcome to attend.
For information on what is up in September, go here: http://whatsouttonight.com/Resources/2016SepSkyWOT.pdf
Utilizing Planetary Oscillations to Constrain the Interior Structure of the Jovian Planets
Seismology has been the premier tool of study for understanding the
interior structure of the Earth, the Sun, and even other stars. Yet in this
thesis proposal, we wish to utilize these tools to understand the interior
structure of the Jovian planets, Saturn in particular. Recent observations
of spiral density structures in Saturn’s rings caused by its oscillations
have provided insight into which modes exist within Saturn and at what
frequencies. Utilizing these frequencies to compare to probable mode can-
didates calculated from Saturn models will also us to ascertain the interior
profiles of state variables such as density, sound speed, rotation, etc. Using
these profiles in a Saturn model, coupled with tweaking the interior struc-
ture of the model, i.e. the inclusion of stably stratified regions, should
allow us to explain which modes are responsible for the density structures
in the rings, as well as predict where to look to find more such structures.
In doing so, we will not only have a much greater understanding of Sat-
urn’s interior structure, but will have constructed a method that can also
be applied to Jupiter once observations of its mode frequencies become
available. In addition, we seek to explain if moist convection on Jupiter is
responsible for exciting its modes. We aim to do this by modeling Jupiter
as a 2D harmonic oscillator. By creating a resonance between moist con-
vective storms and Jovian modes, we hope to match the expected mode
energies and surface displacements of Jupiter’s oscillations.