000195427 001__ 195427
000195427 005__ 20180913062315.0
000195427 0247_ $$2doi$$a10.1088/0004-6256/146/6/159
000195427 022__ $$a0004-6256
000195427 02470 $$2ISI$$a000327747700022
000195427 037__ $$aARTICLE
000195427 245__ $$aUvudf: Ultraviolet Imaging Of The Hubble Ultra Deep Field With Wide-Field Camera 3
000195427 260__ $$aBristol$$bInstitute of Physics$$c2013
000195427 269__ $$a2013
000195427 300__ $$a19
000195427 336__ $$aJournal Articles
000195427 520__ $$aWe present an overview of a 90 orbit Hubble Space Telescope treasury program to obtain near-ultraviolet imaging of the Hubble Ultra Deep Field using the Wide Field Camera 3 UVIS detector with the F225W, F275W, and F336W filters. This survey is designed to: (1) investigate the episode of peak star formation activity in galaxies at 1 < z < 2.5; (2) probe the evolution of massive galaxies by resolving sub-galactic units (clumps); (3) examine the escape fraction of ionizing radiation from galaxies at z similar to 2-3; (4) greatly improve the reliability of photometric redshift estimates; and (5) measure the star formation rate efficiency of neutral atomic-dominated hydrogen gas at z similar to 1-3. In this overview paper, we describe the survey details and data reduction challenges, including both the necessity of specialized calibrations and the effects of charge transfer inefficiency. We provide a stark demonstration of the effects of charge transfer inefficiency on resultant data products, which when uncorrected, result in uncertain photometry, elongation of morphology in the readout direction, and loss of faint sources far from the readout. We agree with the STScI recommendation that future UVIS observations that require very sensitive measurements use the instrument's capability to add background light through a "post-flash." Preliminary results on number counts of UV-selected galaxies and morphology of galaxies at z similar to 1 are presented. We find that the number density of UV dropouts at redshifts 1.7, 2.1, and 2.7 is largely consistent with the number predicted by published luminosity functions. We also confirm that the image mosaics have sufficient sensitivity and resolution to support the analysis of the evolution of star-forming clumps, reaching 28-29th magnitude depth at 5 sigma in a 0 ''.2 radius aperture depending on filter and observing epoch.
000195427 6531_ $$acosmology: observations
000195427 6531_ $$agalaxies: evolution
000195427 6531_ $$agalaxies: high-redshift
000195427 700__ $$aTeplitz, Harry I.$$uCALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA
000195427 700__ $$aRafelski, Marc$$uGoddard Space Flight Ctr, Lab Observat Cosmol, Astrophys Sci Div, Greenbelt, MD 20771 USA
000195427 700__ $$aKurczynski, Peter$$uUniv Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA
000195427 700__ $$aBond, Nicholas A.$$uGoddard Space Flight Ctr, Lab Observat Cosmol, Astrophys Sci Div, Greenbelt, MD 20771 USA
000195427 700__ $$aGrogin, Norman$$uSpace Telescope Sci Inst, Baltimore, MD 21218 USA
000195427 700__ $$aKoekemoer, Anton M.$$uSpace Telescope Sci Inst, Baltimore, MD 21218 USA
000195427 700__ $$0246906$$aAtek, Hakim$$g230964$$uEPFL, Astrophys Lab, CH-1290 Sauverny, Switzerland
000195427 700__ $$aBrown, Thomas M.$$uSpace Telescope Sci Inst, Baltimore, MD 21218 USA
000195427 700__ $$aCoe, Dan$$uSpace Telescope Sci Inst, Baltimore, MD 21218 USA
000195427 700__ $$aColbert, James W.$$uCALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA
000195427 700__ $$aFerguson, Henry C.$$uSpace Telescope Sci Inst, Baltimore, MD 21218 USA
000195427 700__ $$aFinkelstein, Steven L.$$uUniv Texas Austin, Dept Astron, Austin, TX 78712 USA
000195427 700__ $$aGardner, Jonathan P.$$uGoddard Space Flight Ctr, Lab Observat Cosmol, Astrophys Sci Div, Greenbelt, MD 20771 USA
000195427 700__ $$aGawiser, Eric$$uRutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA
000195427 700__ $$aGiavalisco, Mauro$$uUniv Massachusetts, Dept Astron, Amherst, MA 01003 USA
000195427 700__ $$aGronwall, Caryl$$uPenn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA
000195427 700__ $$aHanish, Daniel J.$$uCALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA
000195427 700__ $$aLee, Kyoung-Soo$$uPurdue Univ, Dept Phys, W Lafayette, IN 47907 USA
000195427 700__ $$aMello, De$$uGoddard Space Flight Ctr, Lab Observat Cosmol, Astrophys Sci Div, Greenbelt, MD 20771 USA
000195427 700__ $$aDuilia, F.$$uInterUniv Ctr Astron & Astrophys, Pune, Maharashtra, India
000195427 700__ $$aRavindranath, Swara$$uSpace Telescope Sci Inst, Baltimore, MD 21218 USA
000195427 700__ $$aRyan, Russell E.$$uUniv Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA
000195427 700__ $$aSiana, Brian D.$$uUniv Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA
000195427 700__ $$aScarlata, Claudia$$uCatholic Univ Amer, Dept Phys, Washington, DC 20064 USA
000195427 700__ $$aSoto, Emmaris$$uAix Marseille Univ, CNRS, LAM, F-13388 Marseille, France
000195427 700__ $$aVoyer, Elysse N.$$uUniv Calif San Diego, Dept Phys, La Jolla, CA 92093 USA
000195427 700__ $$aWolfe, Arthur M.
000195427 773__ $$j146$$k6$$tAstronomical Journal
000195427 909C0 $$0252365$$pLASTRO$$xU10933
000195427 909CO $$ooai:infoscience.tind.io:195427$$pSB$$particle
000195427 917Z8 $$x103317
000195427 937__ $$aEPFL-ARTICLE-195427
000195427 973__ $$aEPFL$$rREVIEWED$$sPUBLISHED
000195427 980__ $$aARTICLE