Common-Resolution Convolution Kernels for Space- and Ground-Based Telescopes

By G. Aniano, B. Draine, K. Gordon, K. Sandstrom. 2011

349 citations recorded by the source corpus.

Multiwavelength study of extended astronomical objects requires combining images from instruments with differing point-spread functions (PSFs). We describe the construction of convolution kernels that allow one to generate (multiwavelength) images with a common PSF, thus preserving the colors of the astronomical sources. We generate convolution kernels for the cameras of Spitzer, Herschel Space Observatory, Galaxy Evolution Explorer (GALEX), Wide-field Infrared Survey Explorer (WISE), ground-based optical telescopes (Moffat functions and sum of Gaussians), and Gaussian PSFs. Kernels for other telescopes including IRAS, AKARI, and Planck, are currently being constructed. These kernels allow the study of the spectral energy distribution (SED) of extended objects, preserving the characteristic SED in each pixel. The convolution kernels and the IDL packages used to construct and use them are made publicly available.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f25342cd8be936b0b7bdb6d299218155afe829c0

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Citations in the corpus

ANDROMEDA'S DUST (2013, methodology): “Image convolutions were carried out using kernels obtained as described by Aniano et al. (2011).”
STELLAR MASSES AND STAR FORMATION RATES FOR 1 M GALAXIES FROM SDSS+WISE (2015, methodology): “…the missing light fraction for W1, W2, and W3 by generating with galfit (Peng et al. 2010) a series of simulated light distributions with 2-dimensional Sérsic profiles convolved with the W1 PSF models provided by Aniano et al. (2011), and inserted into empty sections of real W1 images5.”
RECONSTRUCTING THE STELLAR MASS DISTRIBUTIONS OF GALAXIES USING S4G IRAC 3.6 AND 4.5 μm IMAGES. I. CORRECTING FOR CONTAMINATION BY POLYCYCLIC AROMATIC HYDROCARBONS, HOT DUST, AND INTERMEDIATE-AGE STARS (2011, methodology): “This is to be expected given that the PSFs for the 3.6 and 4.5 µm bands are comparably sized (although highly structured in the wings; Reach et al. 2005 and Aniano et al. 2011).”
A z = 0 Multiwavelength Galaxy Synthesis. I. A WISE and GALEX Atlas of Local Galaxies (2019, methodology): “The 22µm WISE4 band represents the limiting factor and we use a somewhat “aggressive” kernel (see Aniano et al. 2011) to reach this resolution for WISE4.”
The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types (2014, positive): “All maps of the resolved subsample have been convolved from their native resolution ([O]88: 9.5′′, [O]63: 9.5′′; GALEX FUV: 6′′; MIPS 24 µm: 6′′) to the 12′′ resolution of PACS at 160 µm using the kernels presented in Aniano et al. (2011).”
THE CO-TO-H2 CONVERSION FACTOR AND DUST-TO-GAS RATIO ON KILOPARSEC SCALES IN NEARBY GALAXIES (2012, methodology): “We convolve the maps with kernels constructed using the techniques described by Aniano et al. (2011) to match the resolution of the SPIRE 350 maps.”
CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD (2013, methodology): “In the case of the UDS visible and near-infrared ground-based data, we adopt a slightly simpler method based on analysis in the Fourier space, similar to the convolution kernel derivation technique presented in Aniano et al. (2011).”