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Galactic Detection. Deciphering Energy Sources in Galactic Nuclei. Heather Stewart, CUA SESI Presentation August 18, 2010 Dr. S Kraemer & Dr H. Schmitt. To do:. Goal Key Players Strategy Results Conclusions. Goal(s). To gain insight about the structure and size of galactic nuclei
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Galactic Detection Deciphering Energy Sources in Galactic Nuclei Heather Stewart, CUA SESI Presentation August 18, 2010 Dr. S Kraemer & Dr H. Schmitt
To do: Goal Key Players Strategy Results Conclusions
Goal(s) • To gain insight about the structure and size of galactic nuclei • To better understand the relationship between active galaxies and star forming (HII) galaxies • To better understand galactic • evolution and characteristics • of our universe! To determine what causes Hydrogen emission in the centers of LINER galaxies (BH or SF)
Key Players HST WFPC2 AGNs, LINERs, H II/SF Hα, [OIII], [NII], Stellar continuum radiation
Key Players Hubble Space Telescope archival images from Wide Field Planetary Camera 2
Key Players Active Galactic Nuclei Seyferts, Quasars, Blazars, Radio Galaxies Star formation Hydrogen II Region galaxies Low-Ionization Nuclear Emission Regions
Key Players Hydrogen alpha (656 nm) recombination Doubly Ionized Oxygen (501/496 nm) Singly Ionized Nitrogen (655/658 nm) de-excitation after collisional excitation Stellar continuum radiation
Strategy Shopping Hubble archive Cleaning Cosmic rays, background Processing Combining, subtracting Comparing Hα vs Continuum vs [OIII] emission Morphology and size
Results Surely an AGN NGC 4151 Surely star formation NGC 4826 Still a mystery NGC 4569 NLR size
Results – NGC 5194 AGN or SF
Conclusion / Future research Need more images and spectra Need more studies on interaction between AGN and SF How do AGN outflows (winds/jets) enrich/encourage star formation? How does star formation affect accretion rates of AGN?
Thank You! Special thanks to Dr. S Kraemer Dr. H Schmitt Dr. A Kinney Cori Quirk and the SESI Program at GSFC Questions or Insights?