J-NEP: 60-band photometry and photometric redshifts for the James Webb Space Telescope North Ecliptic Pole Time-Domain Field

Abstract

<p> <span>The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will observe approximately one-third of the northern sky with a set of 56 narrow-band filters using the dedicated 2.55 m Javalambre Survey Telescope (JST) at the Javalambre Astrophysical Observatory. Prior to the installation of the main camera, in order to demonstrate the scientific potential of J-PAS, two small surveys were performed with the single-CCD Pathfinder camera: miniJPAS (~1 deg</span>²<span> along the Extended Groth Strip), and J-NEP (~0.3 deg</span>²<span> around the JWST North Ecliptic Pole Time Domain Field), including all 56 J-PAS filters as well as </span><em>u</em><span>, </span><em>g</em><span>, </span><em>r</em><span>, and </span><em>i</em><span>. J-NEP is ~0.5–1.0 mag deeper than miniJPAS, providing photometry for 24,618 </span><em>r</em><span>-band-detected sources and photometric redshifts (photo-</span><em>z</em><span>) for the 6662 sources with </span><em>r</em><span> < 23. In this paper, we describe the photometry and photo-</span><em>z</em><span> of J-NEP and demonstrate a new method for the removal of systematic offsets in the photometry based on the median colours of galaxies, which we call ‘galaxy locus recalibration’. This method does not require spectroscopic observations except in a few reference pointings and, unlike previous methods, is directly applicable to the whole J-PAS survey. We use a spectroscopic sample of 787 galaxies to test the photo-</span><em>z</em><span> performance for J-NEP and in comparison to miniJPAS. We find that the deeper J-NEP observations result in a factor ~1.5–2 decrease in </span><em>σ</em>_NMAD<span> (a robust estimate of the standard deviation of the photo-</span><em>z</em><span> error) and </span><em>η</em><span> (the outlier rate) relative to miniJPAS for </span><em>r</em><span> > 21.5 sources, but no improvement in brighter ones, which is probably because of systematic uncertainties. We find the same relation between </span><em>σ</em>_NMAD<span> and </span><em>odds</em><span> in J-NEP and miniJPAS, which suggests that we will be able to predict the </span><em>σ</em>_NMAD<span> of any set of J-PAS sources from their </span><em>odds</em><span> distribution alone, with no need for additional spectroscopy to calibrate the relation. We explore the causes of photo-</span><em>z</em><span> outliers and find that colour-space degeneracy at low S/N, photometry artefacts, source blending, and exotic spectra are the most important factors.</span> <br></p>