Bio & Edu
Science and Technology have always had my interest, and I was a kid that rather play with lego and eletric trains than dolls.
When I returned to college I first studied at Santa Monica College, where I initially was a computer science major, but a visit to the Santa Monica College Astronomy Club changed that, and I switched major. In 2002 I transferred to University of California, Los Angeles (UCLA), from where I recieved a Bachelor of Science in Astrophysics Summer of 2004. At UCLA I did research on emission line ratios in the optical spectra of Seyfert Galaxies with Professor M. Malkan.In the fall of 2005 I began the Master's Program in Physics at California State University, Northridge (CSUN), and recieved the M.S. fall 2008. I did my Master's thesis on a temperature variation on the space telescope Wilkinsons Microwave Anisotropy Probe (WMAP) with Professor E. L. Wright at UCLA.
Science Education2004 Bachelor of Science - Astrophysics
University of California, Los Angeles.
2008 Master of Science - Physics
California State University, Northridge.
Research - Seyfert GalaxiesStudied the emission-line fluxes and luminosities of ~200 Seyfert Galaxies at low red shift Z = - 0.0001 to Z = 0.1848. Analyzed the spectroscopic properties in terms of the emission line fluxes at ten different wavelengths in the Optical and Ultraviolet bands, ranging from [NEON V] at 3425 Angstom to [SULFUR II] at 6724 Angstrom. New data involves correlating luminosities of these objects in optical spectra with X-ray data at 2-10 keV.
Research - Cosmology, WMAP InstrumetsInvestigating a spin-synchronous temperature variation (SST) of ~200 μK on WMAP caused by sun-rays scattering off the solar array. WMAP uses differential radiometers to process sky-signals from two back-to-back telescopes. The data is processed into full-sky pixelized maps of the CMB anisotopies.
A simulation of the SST gives a full-sky map symmetric about the ecliptic plane, with SST peaks at latitudes β ≈ ± (25° to 35°). The SST TT power spectrum has the maximum amplitude at ℓ=2. The quadrupole of the SST is close to orthogonal to the CMB's quadrupole, but detect no significant change in WMAP's CMB quadrupole.
Least Squares fit between a difference map of W-V bands (94 GHz - 61 GHz) and the SST shows that there's an emissivity difference of Δε = 0.01±0.01 between these two bands. I test the upper limit on the WMAP data from the SST by incresing Δε and constrain the Δε where Δχ^2=4. There's no significant contribution on WMAP's TT-power spectra at these limits.