Stellar Properties from Spectral Lines
Note: This exercise is for advanced students.

If you haven't read the Introduction, you should.

The form below will perform a model atmosphere/synthetic spectrum analysis of the equivalent widths (line strengths) of Fe I and Fe II lines, as well as those of many other elements, in the spectrum of M5 III-96. If you'd like to see the table of raw measurements, click here.

Remember, your goal is to select a temperature, surface gravity, and microturbulence that will result in consistent abundances of Fe for all lines, regardless of excitation potential, ionization state, and equivalent width.

Note: Only one person can be running this program at a time. If you get an error message that the program is in use, wait a few minutes and try again. This is a lot of math being done on an old computer!