Circumnuclear Dust in Luminous Early-Type Galaxies -- I. Sample Properties and Stellar Luminosity Models

<p>This dataset contains the HST mosaic images created and described in the paper "Circumnuclear Dust in Luminous Early-Type Galaxies -- I. Sample Properties and Stellar Luminosity Models" by J. Davidson, B. Boizelle, J. Walsh, A. Barth, E. Rasmussen, A. Baker, D. Buote, J. Darling, L. Ho, K. Kabasares, and J. Cohn.</p> <p>Each mosaic was created by drizzling the data to a pixel scale of 0.08 and a pixel fraction of 0.75. The data are mostly in the infrared and optical and only occasionally in the ultraviolet.</p> <h2>Data Structure</h2> <p>These data are organized by target and each target has its own .zip file. Each .zip file is organized by HST camera, then by filter. For example, for the target Hydra A, the data are sorted into the following folders:</p> <ul> <li><strong>acs_sbc</strong> <ul> <li><strong>f140lp</strong></li> <li><strong>f150lp</strong></li> </ul> </li> <li><strong>acs_wfc</strong> <ul> <li><strong>f814w</strong></li> </ul> </li> <li><strong>wfc3</strong><br> <ul> <li><strong>f110w</strong></li> <li><strong>f160w</strong></li> <li><strong>f475w</strong></li> </ul> </li> <li><strong>aligned</strong></li> </ul> <p>The <strong>aligned</strong> folder for each target contains all the aligned mosaic images. These were aligned to their respective&nbsp;<em>wfc3/f160w</em> image using TweakReg, then further corrected using interpolation to obtain sub-pixel accuracy.</p> <h2>File Naming</h2> <p>All mosaic image files for all filters follow the same naming convention:&nbsp;<strong>&lt;target name + filter + pixel fraction + pixel scale&gt;_ drz_sci.fits.</strong> For example, the Hydra A <em>f160w</em> mosaic is named <strong>hydraa_f160w_pxfr075_pxsc008_drz_sci.fits.</strong></p> <p>PSF files, both empirical and Tiny Tim (each drizzled to the same pixel scale and pixel fraction as the HST data), are included in each&nbsp;<strong>f110w</strong> and <strong>f160w</strong> folder and follow a similar naming convention. To these file names are added either *emp_psfdrz* for the empirical PSF or *psfdrz* for the Tiny Tim PSF. For example, the Hydra A <em>f160w</em> empirical PSF file is named <strong>hydraa_f160w_emp_psfdrz_pxfr075_pxsc008_drz_sci.fits,</strong>&nbsp;whereas the Tiny Tim PSF file is named <strong>hydraa_f160w_psfdrz_pxfr075_pxsc008_drz_sci.fits.</strong></p> <p>The <strong>f160w</strong> folders for all targets also contain a few extra files:</p> <ol> <li>Mask files, called <strong>f160w_mask.fits</strong> in all cases, which indicate the positions and extents of all extraneous sources of light (foreground stars, background galaxies, cosmic ray hits, etc.) in the respective <em>f160w</em> mosaics.</li> <li>A .txt file that contains the final GALFIT MGE solution and follows the naming convention&nbsp;<strong>&lt;target&gt;_f160w_galfitmge_dustmask_tinytim_sol.txt.</strong> Note that the Tiny Tim PSF was used to obtain the final MGE solution in every case.</li> <li>&nbsp;A .fits file that contains the model based on the final GALFIT MGE solution. These follow the naming convention <strong>&lt;target&gt;_f160w_pxfr075_pxs0080_drz_galfit_ttpsf_qbounds020.fits.</strong></li> <li><em>For NGC 3862 only</em>, we also obtained an MGE solution using the empirical PSF for comparison purposes. For this target, the .txt MGE solution that utilizes the empirical PSF is named <strong>ngc3862_f160w_galfitmge_dustmask_emp_sol.txt&nbsp;</strong>and the corresponding model .fits file is named <strong>ngc3862_f160w_pxfr075_pxs0080_drz_galfit_cenpsf_emppsf_qbounds020.fits.</strong></li> </ol> <p>For NGC 1387, NGC 3862, NGC 4261, and NGC 4435, a second round of observations were obtained using a subarray and shorter exposure times. The <strong>f110w</strong> and&nbsp;<strong>f160w</strong> folders for these galaxies therefore also have a few extra files that contain the drizzled images and empirical and Tiny Tim PSFs for these subarray exposures. These files follow the same naming conventions as previously described, with the addition of *subarr* to distinguish between the full array and subarray files. For example, the NGC 1387 drizzled subarray image is named&nbsp;<strong>ngc1387_f160w_subarr_pxfr075_pxsc008_drz_sci.fits,&nbsp;</strong>whereas the full-array, longer exposure time image is named <strong>ngc1387_f160w_pxfr075_pxsc008_drz_sci.fits. </strong>Please note that these subarray images were not used in any of the final MGEs or the analysis described in the paper, but are included here for sake of completeness.</p> <p>In the <strong>aligned&nbsp;</strong>folders, all aligned images follow the same naming convention: <strong>&lt;target&gt;_&lt;camera&gt;_&lt;filter&gt;_pxfr075_pxsc008_drz_align_sci.fits.</strong></p>