Uploading stellar data

Global asteroseismic and classical surface parameters

  • Upload a whitespace-separated ASCII file of stellar parameters for your stars. The first line must be a header starting with #, and the first column should contain a unique string ID for each star (starid), should be utf-8 compliant, without spaces.

  • All succeeding column names must match the BASTA parameter list. For every measured quantity (at least those you want to fit against), provide an uncertainty column with the same name plus *_err (e.g. Teff, Teff_err).

  • If you want to predict distance or parallax, you should include either equatorial (RA, DEC) or galactic coordinates (l, b) and the photometric filters you want to use (see recognized filters).

  • If you also want to fit against individual frequencies, you need to include dnu and numax with your stellar parameters (although not used directly in the fitting).

  • Use a single, consistent placeholder for missing values (e.g. -999.99). Download an example stellar data file.

Distance Estimation

  • For fitting distance and/or parallax, you must specify which photometric filters to use. If you have included filters (and coordinates) in your stellar parameters file, checkboxes will show up automatically allowing you to choose which filters you want to include.

Individual frequencies

  • You can provide a separate ASCII file for each star if fitting individual mode frequencies or frequency ratios. The name of each file must exactly match the corresponding starid specified in the stellar data file, with extension *.fre; each header should again start with #.

  • At minimum, include the angular degree of each mode (labelled l, ell or degree), the mode frequency (freq or frequency) and their uncertainties.

  • Uncertainties should be a single column for symmetric (err or error), or two columns for asymmetric (error_plus and error_minus).

  • Optionally, you may also include the radial order (order or n) if available. Download an example frequency file. Otherwise BASTA estimates the radial order based on the radial modes, assuming they are continuous without any gaps in radial order!