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star2map

star2map. Shannon Guiles Cornell University July 16, 2004. Goal of star2map. To put together Starburst99 and Mappings to calculate mid-infrared photo-ionization lines for starburst galaxies. Starburst99. Models star-forming galaxies, outputting the integrated light of a stellar population

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star2map

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  1. star2map Shannon Guiles Cornell University July 16, 2004

  2. Goal of star2map To put together Starburst99 and Mappings to calculate mid-infrared photo-ionization lines for starburst galaxies.

  3. Starburst99 • Models star-forming galaxies, outputting the integrated light of a stellar population • Some important input parameters: • Continuous star formation or fixed mass (instantaneous burst) • Star formation rate if using continuous star formation • Total stellar mass if using fixed mass • Initial Mass Function (IMF) exponent • The output used for Mappings is the stellar population spectral energy distribution at each time

  4. Mappings • Photo-ionization code that includes the effects of dust photoelectric heating and gas-phase depletion of heavy elements • Mappings outputs the emission-line spectrum, giving each line’s wavelength and corresponding energy, the intensity of each line relative to Hb=1, and the species responsible for the emission line

  5. star2map: Overview • Get a composite stellar spectrum from Starburst99 for a given model • Input the Starburst99 spectrum with appropriate units and binning into Mappings as the ionizing radiation field source • Finally get the mid-infrared photo-ionization lines of choice from the Mappings output at each time step

  6. star2map: Details • Before running star2map run ‘setupstar2map’ to set up the input files for both Starburst99 and Mappings • Star2map first reads in the Starburst99 input file and then runs Starburst99 • Once Starburst99 finishes, its output spectrum and quanta files are read (the quanta file contains the total luminosity needed as an input Mappings parameter) • Loop over all times in SB99 output, creating a Mappings input file for each time

  7. star2map … • Use ‘convertnew.f’ to change SB99 output spectrum units (Log(luminosity) vs. wavelength) to Mappings input units (flux vs. energy), and to re-bin the spectrum into binning acceptable to Mappings • Create a batch file with the Mappings input files and output file names for each time • Run Mappings in batch mode • Move all relevant files to a folder given the same name as the model • After star2map finishes, use ‘lineratios’ to extract the lines wanted at each time from the Mappings output and graph the results

  8. First results

  9. Comparison with previous models • Rigby & Rieke, ApJ (2004) 606, 237 figures 3, 4, 11, 12 (Starburst99 with CLOUDY) • Thornley et al., ApJ (2000) 539, 641 figures 6, 10 (STARS with CLOUDY)

  10. Rigby & Rieke ApJ 606, 237 fig. 3cStarburst99 SEDs with CLOUDY photo-ionization codesolar metallicity, instantaneous burst, Salpeter IMF, 1 Msolar to Mup

  11. Thornley et al. ApJ (2000) 539, 641 fig. 10STARS SEDs with CLOUDY photo-ionization codevarying different parameters

  12. Limitations of star2map • It takes a long time to run • Currently it can only run on Unix, although hopefully it will be running on Linux soon

  13. Conclusions • Star2map calls Starburst99 and Mappings in order to calculate mid-infrared photo-ionization lines as a function of time for various models of starburst galaxies • We have just begun to get results for the [NeIII]/[NeII] ratio that traces massive stars

  14. Acknowledgments I would like to thank Daniel Devost for suggesting this project and for his guidance, Jim Houck for his support, Vassilis Charmandaris for his help and advice, Don Barry for his perl script and computer help, and all the people who wrote Starburst99 and Mappings.

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