High-resolution spectroscopy and Fe abundance analysis of very metal poor red-giant stars Public Deposited

http://ir.library.oregonstate.edu/concern/undergraduate_thesis_or_projects/rr171z81h

Descriptions

Attribute NameValues
Creator
Abstract or Summary
  • Studying the evolution of the Milky Way galaxy helps us understand our place in the Universe. Early evolution of the Galaxy can effectively be studied by observing stars with low metallicity values since they are the oldest stars still visible. Due to the formation of the Galaxy, the oldest stars can predominantly be found in the halo and thick disk regions. G2 0701+6247, G2 0934+3614, and G2 1540+3200 are the three stars selected from a survey of very metal-poor star candidates for high-resolution spectroscopy in order to determine the chemical composition and metallicity. Two standard very metal-poor stars, HD 88609 and HD 122563, were also chosen to compare to previous research to verify the methods used. Echelle spectra were collected by a spectrograph on the Mayall 4-m telescope at the Kitt Peak Nation Observatory for each star in March 2010. The charge coupled device images are reduced using Image Reduction and Analysis Facility. Background noise from the equipment is eliminated using bias frames. Pixel-to-pixel variations are corrected using flat frames. Then the sky background is removed and the images are extracted to one dimension. Wavelength calibration is then conducted using a Th-Ar lamp image as the reference. Equivalent widths for iron I & II are measured and used as parameters for MOOG in order to determine the iron abundances of each star. The metallicity values for HD 88609, HD 122563, G2 0701+6247, G2 0934+3614, and G2 1540+3200 are -3.09±0.017 -2.84±0.016, -3.00±0.029, -1.66±0.022, and -3.02±0.049 respectively.
Resource Type
Date Available
Date Issued
Degree Level
Degree Name
Degree Field
Degree Grantor
Commencement Year
Advisor
Non-Academic Affiliation
Rights Statement
Funding Statement (additional comments about funding)
Language
Replaces
Additional Information
  • description.provenance : Made available in DSpace on 2014-06-05T20:22:00Z (GMT). No. of bitstreams: 1FinalThesis.pdf: 2585771 bytes, checksum: ea5c1fd7936df93373e794190a0f1cb8 (MD5)
  • description.provenance : Approved for entry into archive by Patricia Black(patricia.black@oregonstate.edu) on 2014-06-05T20:22:00Z (GMT) No. of bitstreams: 1FinalThesis.pdf: 2585771 bytes, checksum: ea5c1fd7936df93373e794190a0f1cb8 (MD5)
  • description.provenance : Submitted by Daniel Gluck (gluckd@onid.orst.edu) on 2014-06-05T18:06:52ZNo. of bitstreams: 1FinalThesis.pdf: 2585771 bytes, checksum: ea5c1fd7936df93373e794190a0f1cb8 (MD5)

Relationships

Parents:

This work has no parents.

Last modified

Downloadable Content

Download PDF

Items