23 January 2014 The CLASH Multi-Cycle Treasury program (PI: Marc Postman) completed its Hubble Space Telescope (HST) multiwavelength obsrvations of 25 massive galaxy clusters in 2013 (Postman et al. 2011 describes the full survey). The full HST dataset and associated catalogs and gravitational lens models are available here, http://archive.stsci.edu/prepds/clash/ . A series or programs with Spitzer have covered all CLASH galaxy clusters with IRAC Channels 1 and 2. Several of the targets include Channels 3 and 4 data. All mosaics were created using MOPEX. The default recommended settings were used for the Channel 1 mosaicing. For the remaining Channels, the FIF.tlb table from Channel 1 was used as a reference, to ensure the same image dimensions and orientations. Catalogs were produced for all mosaics, using a best-effort optimization of detection parameters within Source Extractor (Bertin & Arnouts 1996). The following aperture diameters were used (unites=pixels) PHOT_APERTURES 2.,5.,10.0,16.67,20,40 with a pixel scale of PIXEL_SCALE 0.6 The gain was estimated through GAIN = [number of combined frames] x [individual gain] where the [number of combined frames] is taken from the mosaic coverage FITS file (mosaic_cov.fits) as output by the MOPEX procedure. The other essential parameters adopted for object detection are: SEEING_FWHM 1.66000 # FWHM from IRAC IH in units of arcsec WEIGHT_GAIN N FILTER Y FILTER_NAME mexhat_4.0_9x9.conv ANALYSIS_THRESH 1.5 BACKPHOTO_THICK 24 BACKPHOTO_TYPE LOCAL BACK_FILTERSIZE 3 BACK_SIZE 128 CATALOG_TYPE ASCII_HEAD CLEAN N CLEAN_PARAM 1.0 DEBLEND_MINCONT 0.001 DEBLEND_NTHRESH 32 DETECT_MINAREA 2 DETECT_THRESH 4.0 DETECT_TYPE CCD INTERP_TYPE ALL INTERP_MAXXLAG 16 INTERP_MAXYLAG 16 MAG_GAMMA 4.0 MASK_TYPE CORRECT MEMORY_BUFSIZE 4600 MEMORY_OBJSTACK 10000 MEMORY_PIXSTACK 2600000 PHOT_AUTOPARAMS 2.5,3.5 PHOT_FLUXFRAC 0.2,0.5,0.9 PIXEL_SCALE 0.6 # in units of arcsec SATUR_LEVEL 50000. STARNNW_NAME default.nnw The zeropoints follow the guidelines from http://irsa.ipac.caltech.edu/data/SPITZER/docs/irac/iracinstrumenthandbook/25/ and are MAG_ZEROPOINT 18.803 Channel 1 18.318 Channel 2 17.833 Channel 3 17.2122 Channel 4 Photometry was based on double-image mode, with Channel 1 as the reference image. The weights from the MOPEX process are used. Point Spread Functions We have generated empirical PSFs by identifying unresolved objects in the high-resolution HST data, and doing a median combination of those objects in each channel.