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

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 &lt; z &lt; 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 &lt; M UV &lt; −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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>α</mml:mi> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.359</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.041</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.041</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> 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 &lt; −10 is derived as <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>ρ</mml:mi> </mml:mrow> <mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">U</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">V</mml:mi> </mml:mrow> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.339</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.030</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.027</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>26</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">e</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">r</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">g</mml:mi> </mml:mrow> </mml:mrow> <mml:mspace width="0.25em"/> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi mathvariant="normal">s</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:mrow> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">z</mml:mi> </mml:mrow> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">p</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">c</mml:mi> </mml:mrow> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> <mml:mo stretchy="false">)</mml:mo> </mml:math> 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.

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Journal
The Astrophysical Journal
Published
2024-08-21
DOI
https://doi.org/10.3847/1538-4357/ad5540
Citations
14
Primary Topic
Galaxies: Formation, Evolution, Phenomena
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article
Field-Weighted Citation Impact
4.64

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article

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

Matthew Hayes, Ray A. Lucas, Swara Ravindranath, Peter Kurczynski et al.
14 citations
The Astrophysical Journal
Galaxies: Formation, Evolution, Phenomena
4.64
article

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

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

Abstract

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 &lt; z &lt; 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 &lt; M UV &lt; −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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>α</mml:mi> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.359</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.041</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.041</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> 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 &lt; −10 is derived as <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>ρ</mml:mi> </mml:mrow> <mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">U</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">V</mml:mi> </mml:mrow> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.339</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.030</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.027</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>26</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">e</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">r</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">g</mml:mi> </mml:mrow> </mml:mrow> <mml:mspace width="0.25em"/> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi mathvariant="normal">s</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:mrow> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">z</mml:mi> </mml:mrow> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">p</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">c</mml:mi> </mml:mrow> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> <mml:mo stretchy="false">)</mml:mo> </mml:math> 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.

The Astrophysical JournalVol. 972(1)
Rutgers, The State University of New Jersey (US), University of California, Riverside (US), College of Wooster (US), University of the Pacific (US), California Institute of Technology (US), University of Copenhagen (DK), Space Telescope Science Institute (US), University of Minnesota (US), Goddard Space Flight Center (US), Pennsylvania State University (US), University of Arizona (US), University of Padua (IT), University of Hertfordshire (GB), University of Nottingham (GB), Johns Hopkins University (US), Minnesota State University, Mankato (US), Stockholm University (SE), University of America (US), University of California, Santa Cruz (US), University of Toronto (CA), Chinese Academy of Sciences (CN), University of Massachusetts Amherst (US), Beijing Normal University (CN), Korea Astronomy and Space Science Institute (KR), Max Planck Institute for Astronomy (DE), Canadian Institute for Theoretical Astrophysics (CA), National Space Science Center (CN), Carnegie Observatories (US), Community Science and Data Center (US), AlbaNova (SE), Computational Physics (United States) (US), NSF NOIRLab (US), Osservatorio Astronomico di Padova (IT), National Astronomical Observatories (CN), University of Chinese Academy of Sciences (CN), Infrared Processing and Analysis Center (US), Osservatorio di Astrofisica e Scienza dello Spazio, Deleted Institution, UK Astronomy Technology Centre (GB), University of Virginia (US), Arizona State University (US), Swinburne University of Technology (AU), University of Missouri (US), Catholic University of America (US), The University of Texas at Austin (US), University of Edinburgh (GB)
National Aeronautics and Space Administration, Space Telescope Science Institute, National Natural Science Foundation of China, Science and Technology Facilities Council, Fundamental Research Funds for the Central Universities
Openalex Percentile: Top 5%
Galaxies: Formation, Evolution, Phenomena
4.64
DOIOpen Access PDFOpenAlex
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