1 / 13

Barred Magellanic Spirals: Understanding Global Properties

Explore the formation, evolution, and interactions of SBms; study dark matter distribution in Ursa Major and Canes Venatici galaxies. Use VLA to observe H.I. emissions for velocity determination. Compare with optical images and dark matter models.

bturnbow
Download Presentation

Barred Magellanic Spirals: Understanding Global Properties

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Kwayera Davis (College of Charleston) Advisor: Eric Wilcots (University of Wisconsin-Madison) University of Wisconsin-Madison REU 2003 Barred Magellanic Spirals in Ursa Major and Canes Venatici: Global Properties

  2. Motivation • Some galaxy types are not well studied • We want to better understand their • formation • evolution • interaction with neighbours • structure • dark matter distribution

  3. Barred Magellanic Spirals (SBms) • SBms are a transitional class • Some spiral structure • Some irregular structure • Barred • The LMC is a SBm

  4. H I emission • Neutral(atomic) hydrogen atom • 1 proton and 1 electron • Electron changes spin • Light emitted • 21 cm wavelength • 1.4 GHz frequency • This is in the radio part of the e.m. Spectrum

  5. Observing H I with the VLA • The Very Large Array is an interferometer • 30'' resolution • Observations in C configuration • Compact array gives increased sensitivity • H I line allows velocity determination • We know the radial velocity of the hydrogen gas we are seeing

  6. NGC 3264

  7. NGC 4288

  8. NGC 4861

  9. Conclusions • rotation curves are fairly typical • also have interesting differences • further analysis should be possible

  10. Further Work • Compare H I to optical image from WIYN • Calculate dark matter distribution • Compare with predictions of dark matter models

  11. Acknowledgments I would like to thank • University of Wisconsin-Madison REU Program • My advisor Dr. Eric Wilcots • My research partner Stephanie Bush • The scientists working in the department • My fellow students

  12. This Experience

  13. Some Optical Images

More Related