Extending the nearby galaxy heritage with wise: First results from the wise enhanced resolution galaxy atlas

• Autores: Jarrett, T. H.; Masci, F.; Tsai, C. W.; Petty, S.; Cluver, M. E.; Assef, Roberto J.; Benford, D.; Blain, A.; Bridge, C.; Donoso, Emilio; Eisenhardt, P.; Koribalski, Bärbel; Lake, S.; Neill, James D.; Seibert, M.; Sheth, K.; Stanford, S.; Wright, E.
• Año de publicación: 2013
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: galaxies: fundamental parameters; galaxies: statistics; infrared: galaxies – surveys; techniques: image processing
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

The Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at mid-infrared wavelengths 3.4 μm, 4.6 μm, 12 μm, and 22 μm. The mission was primarily designed to extract point sources, leaving resolved and extended sources, for the most part, unexplored. Accordingly, we have begun a dedicated WISE Enhanced Resolution Galaxy Atlas (WERGA) project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we demonstrate the first results of the WERGA project for a sample of 17 galaxies, chosen to be of large angular size, diverse morphology, and covering a range in color, stellar mass, and star formation. It includes many well-studied galaxies, such as M51, M81, M87, M83, M101, and IC342. Photometry and surface brightness decomposition is carried out after special super-resolution processing, achieving spatial resolutions similar to that of Spitzer Infrared Array Camera. The enhanced resolution method is summarized in the first paper of this two-part series. In this second work, we present WISE, Spitzer, and Galaxy Evolution Explorer (GALEX) photometric and characterization measurements for the sample galaxies, combining the measurements to study the global properties. We derive star formation rates using the polycyclic aromatic hydrocarbon sensitive 12 μm (W3) fluxes, warm-dust sensitive 22 μm (W4) fluxes, and young massive-star sensitive ultraviolet (UV) fluxes. Stellar masses are estimated using the 3.4 μm (W1) and 4.6 μm (W2) measurements that trace the dominant stellar mass content. We highlight and showcase the detailed results of M83, comparing the WISE/Spitzer results with the Australia Telescope Compact Array H I gas distribution and GALEX UV emission, tracing the evolution from gas to stars. In addition to the enhanced images, WISE's all-sky coverage provides a tremendous advantage over Spitzer for building a complete nearby galaxy catalog, tracing both stellar mass and star formation histories. We discuss the construction of a complete mid-infrared catalog of galaxies and its complementary role of studying the assembly and evolution of galaxies in the local universe.
Fil: Jarrett, T. H.. California Institute of Technology; Estados Unidos. University of Cape Town; Sudáfrica
Fil: Masci, F.. California Institute of Technology; Estados Unidos
Fil: Tsai, C. W.. California Institute of Technology; Estados Unidos
Fil: Petty, S.. University of California at Los Angeles; Estados Unidos
Fil: Cluver, M. E.. Australian Astronomical Observatory; Australia
Fil: Assef, Roberto J.. University of California at Los Angeles; Estados Unidos
Fil: Benford, D.. National Aeronautics and Space Administration; Estados Unidos
Fil: Blain, A.. University of Leicester; Reino Unido
Fil: Bridge, C.. University of California at Los Angeles; Estados Unidos
Fil: Donoso, Emilio. University of California at Los Angeles; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Eisenhardt, P.. University of California at Los Angeles; Estados Unidos
Fil: Koribalski, Bärbel. CSIRO Astronomy & Space Science; Australia
Fil: Lake, S.. University of California at Los Angeles; Estados Unidos
Fil: Neill, James D.. University of California at Los Angeles; Estados Unidos
Fil: Seibert, M.. Carnegie Institution for Science; Estados Unidos
Fil: Sheth, K.. National Radio Astronomy Observatory; Estados Unidos
Fil: Stanford, S.. University of California at Davis; Estados Unidos
Fil: Wright, E.. University of California at Los Angeles; Estados Unidos