The new VLA HI-line data were taken during the transition from the VLA to the EVLA, so the array was a mixture of the two types of antennas. The aliasing problem led to complications in calibrating the data. Our calibration recipe is given here. For mapping, we used the multi-scale CLEAN algorithm implemented in AIPS. Since this is not yet in common use, we give our mapping recipe here. Our HI data are described by Hunter et al., in preparation.
We provide our Hanning-smoothed natural-weighted HI-line cube ([galaxyname]_NA_ICL001.FITS), and our robust=0.5-weighted cube ([galaxyname]_R_ICL001.FITS). We also provide the primary beam-corrected moment 0 (integrated flux; [galaxyname]_NA_X0_P_R.FITS, [galaxyname]_R_X0_P_R.FITS), intensity-weighted moment 1 (velocity field; [galaxyname]_NA_XMOM1.FITS, [galaxyname]_R_XMOM1.FITS), and intensity-weighted moment 2 (velocity dispersion; [galaxyname]_NA_XMOM2.FITS, [galaxyname]_R_XMOM2.FITS) maps derived from both of these cubes.
This web site contains our optical UBV, near-IR JHK, and Halpha images and their calibration parameters, and GALEX NUV and FUV ultraviolet images. Some of the GALEX data were obtained from the archives, including the LGS survey. The GALEX data were processed using the GR4/5 pipeline (see Zhang et al. (2011). Spitzer data were obtained from the archives, including the LVL and SINGS surveys.
The color images in the upper right corner of the galaxy pages are a combination of the NA-weighted integrated HI map (red), V-band (green), and FUV (blue). Most of the images were constructed by Ms. Lauren Hill.Optical and near-IR images for the full optical survey (136 galaxies), from which the LITTLE THINGS sample is drawn, are also available: UBVJHK images. Halpha images are available via NED.