Lyman-alpha imaging of nearby galaxies

All files are calibrated in units of flux density (f_λ), in cgs, "observed" through the respective bandpass. I.e. erg/s/cm²/Å.
Adopting this convention, the line and continuum images have the same units, so if you want to get to the line fluxes themselves, you need to multiply the on-line image by the width of the bandpass.
- Hα was captured by FR656N, which is a 2% ramp filter. Thus the width of the bandpass should be taken as 0.02×6563×(1.+z).
- Lyα was captured by F122M, which is an unusually shaped medium band filter with a sharp blue cut-on but an extended red wing. Thus knowing which bandwidth to adopt is not straightforward. The IHB quotes Δλ of 60Å, which doesn't seem particularly applicable. Synphot quotes the rectangular width as 128.44Å and a bandwidth of 90.878Å. We have always adopted the rectangular width but you can take whatever bandpass you want; just be sure to quote it your paper. The most important thing is to be consistent.
Further images, e.g. E(B-V), CTN, etc. may be made available on request.
File naming convention. All files are named ttt_ooo.fits.
- ttt refers to the target ( haro - Haro 11; sbs - SBS 0335 052; iras - IRAS 08339+65; tol - Tololo 65; ngc - NGC 6090: eso - ESO 338-IG04 ) .
- ooo refers to the observation ( lya - Lyα; lyac - continuum at Lyα; ha - Hα; hac - continuum at Hα ) .

If you make use of these data, and decide to publish the results, please cite both the methodology paper (Hayes et al., 2009, AJ, 138, 911) and the data release paper (Östlin et al., 2009, AJ, 138, 923).