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The Ultraviolet Luminosity Function at 0.6 < z < 1 from UVCANDELS

2024; IOP Publishing; Volume: 972; Issue: 1 Linguagem: Inglês

10.3847/1538-4357/ad5540

1538-4357

Lei Sun, Xin Wang, Harry I. Teplitz, Vihang Mehta, Anahita Alavi, Marc Rafelski, Rogier A. Windhorst, Claudia Scarlata, Jonathan P. Gardner, Brent M. Smith, Ben Sunnquist, Laura Prichard, Y. Cheng, Norman A. Grogin, Nimish P. Hathi, Matthew Hayes, Anton M. Koekemoer, Bahram Mobasher, K. Nedkova, R. W. O’Connell, Brant Robertson, Sina Taamoli, L. Y. Aaron Yung, Gabriel Brammer, James Colbert, Christopher J. Conselice, Eric Gawiser, Yicheng Guo, Rolf A. Jansen, Zhiyuan Ji, Ray A. Lucas, Michael Rutkowski, Brian Siana, E. Vanzella, Teresa Ashcraft, Micaela B. Bagley, Ivano Baronchelli, Guillermo Barro, Alex Blanche, Adam Broussard, Timothy Carleton, Nima Chartab, Alex Codoreanu, Seth H. Cohen, Y. Sophia Dai, Behnam Darvish, Romeel Davé, Laura DeGroot, D. F. de Mello, Mark Dickinson, Najmeh Emami, Henry C. Ferguson, Leonardo Ferreira, Keely Finkelstein, Steven L. Finkelstein, Timothy Gburek, Mauro Giavalisco, A. Grazian, C. Gronwall, Shoubaneh Hemmati, Justin Howell, Kartheik G. Iyer, Sugata Kaviraj, Peter Kurczynski, Ilin Lazar, John MacKenty, Kameswara Bharadwaj Mantha, Alec Martin, Garreth Martin, Tyler McCabe, Charlotte Olsen, Lillian Otteson, Swara Ravindranath, Caleb Redshaw, Zahra Sattari, Emmaris Soto, Bonnabelle Zabelle,

Astronomy and Astrophysical Research

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 arcmin 2 . 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 (5 σ 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 α = − 1.359 − 0.041 + 0.041 at z ∼ 0.8. Creating subsamples at z ∼ 0.7 and z ∼ 0.9, we observe a possible evolution of α with redshift. The unobscured UV luminosity density at M UV < −10 is derived as ρ U V = 1.339 − 0.030 + 0.027 ( × 10 26 e r g s − 1 H z − 1 M p c − 3 ) using our best-fit LF parameters. The new F275W and F435 photometric catalogs from UVCANDELS have been made publicly available on the Barbara A. Mikulski Archive for Space Telescopes.