The Ultraviolet Luminosity Function at 0.6 < z < 1 from UVCANDELS
Barro, Guillermo; Dickinson, Mark; Giavalisco, Mauro; Grazian, Andrea; Hathi, Nimish P.; Koekemoer, Anton M.; Lucas, Ray A.; Ravindranath, Swara; Yung, L. Y. Aaron; de Mello, Duilia; Gardner, Jonathan P.; Teplitz, Harry I.; Scarlata, Claudia; Hayes, Matthew; Mehta, Vihang; Cohen, Seth; Siana, Brian; Ji, Zhiyuan; Rafelski, Marc; Mobasher, Bahram; Brammer, Gabriel; Ferguson, Henry; Davé, Romeel; Ferreira, Leonardo; Gronwall, Caryl; Hemmati, Shoubaneh; Chartab, Nima; Windhorst, Rogier A.; Wang, Xin; Kaviraj, Sugata; Gawiser, Eric; Broussard, Adam; Darvish, Behnam; Sattari, Zahra; Guo, Yicheng; Grogin, Norman; Robertson, Brant; Mantha, Kameswara Bharadwaj; Nedkova, Kalina V.; Jansen, Rolf A.; Carleton, Timothy; Vanzella, Eros; Smith, Brent M.; MacKenty, John; Soto, Emmaris; Alavi, Anahita; Sunnquist, Ben; Prichard, Laura; Colbert, James; Baronchelli, Ivano; Dai, Y. Sophia; Martin, Alec; Sun, Lei; Kurczynski, Peter; Codoreanu, Alex; Cheng, Yingjie; Rutkowski, Michael; Iyer, Kartheik; Gburek, Timothy; Emami, Najmeh; Martin, Garreth; Howell, Justin; O'Connell, Robert; Bagley, Micaela; Lazar, Ilin; Finkelstein, Keely; Olsen, Charlotte; Conselice, Christopher; Degroot, Laura; Taamoli, Sina; The Uvcandels Team; Redshaw, Caleb; Finkelstein, Steven; Ashcraft, Teresa; Blanche, Alex; McCabe, Tyler; Otteson, Lillian; Zabelle, Bonnabelle
China, United States, Sweden, Denmark, United Kingdom, Italy, Australia, Canada, Germany, South Korea
Abstract
UVCANDELS is a Hubble Space Telescope Cycle-26 Treasury Program awarded 164 orbits of primary ultraviolet (UV) F275W imaging and coordinated parallel optical F435W imaging in four CANDELS fields—GOODS-N, GOODS-S, EGS, and COSMOS—covering a total area of ∼426 arcmin2. This is ∼2.7 times larger than the area covered by previous deep-field space UV data combined, reaching a depth of about 27 and 28 ABmag (5σ in 0."2 apertures) for F275W and F435W, respectively. Along with new photometric catalogs, we present an analysis of the rest-frame UV luminosity function (LF), relying on our UV-optimized aperture photometry method, yielding a factor of 1.5 increase over H-isophot aperture photometry in the signal-to-noise ratios of galaxies in our F275W imaging. Using well-tested photometric redshift measurements, we identify 5810 galaxies at redshifts 0.6 < z < 1, down to an absolute magnitude of M UV = ‑14.2. In order to minimize the effect of uncertainties in estimating the completeness function, especially at the faint end, we restrict our analysis to sources above 30% completeness, which provides a final sample of 4726 galaxies at ‑21.5 < M UV < ‑15.5. We performed a maximum likelihood estimate to derive the best-fit parameters of the UV LF. We report a best-fit faint-end slope of