20.500.12556/RUL-178333 CANUCS/Technicolor data release 1: imaging, photometry, slit spectroscopy, and stellar population parameters We present the first data release of the Canadian NIRISS Unbiased Cluster Survey (CANUCS), a JWST Cycle 1 GTO program targeting five lensing clusters and flanking fields in parallel (A370, MACS0416, MACS0417, MACS1149, and MACS1423; survey area ∼100 arcmin$^2$), with NIRCam imaging, NIRISS slitless spectroscopy, and NIRSpec prism multiobject spectroscopy. Fields centered on cluster cores include imaging in eight bands from 0.9–4.4 μm, alongside continuous NIRISS coverage from 1.15–2 μm, while the NIRCam flanking fields provide five wide-band and nine medium-band filters for exceptional spectral sampling, all to ∼29 mag$_{AB}$. We also present JWST in Technicolor, a Cycle 2 follow-up GO program targeting three CANUCS clusters (A370, MACS0416, and MACS1149). The Technicolor program adds NIRISS slitless spectroscopy in F090W to the cluster fields while adding eight wide-, medium-, and narrowband filters to the flanking fields. This provides NIRCam imaging in all wide- and medium-band filters over ∼30 arcmin$^2$. This paper describes our data reduction and photometry methodology. We release NIRCam, NIRISS, and Hubble Space Telescope imaging, point-spread functions (PSFs), PSF-matched imaging, photometric catalogs, and photometric and spectroscopic redshifts. We provide lens models and stellar population parameters in up to 19 filters for ∼53,000 galaxies in the cluster fields, and ∼44,000 galaxies in up to 29 filters in the flanking fields. We further present 733 NIRSpec spectra and redshift measurements up to z = 10.8. Comparing against our photometric redshifts, we find catastrophic outlier rates of only 4%–7% and scatter of $\sigma_{\mathrm{NMAD}}$ of 0.01–0.03. galaxy evolution sky surveys photometry spectroscopy galaxy clusters razvoj galaksij pregledi neba fotometrija spektroskopija jate galaksij true false true Angleški jezik Slovenski jezik Članek v reviji 2026-01-23 10:08:47 2026-01-23 10:08:48 2026-01-24 04:32:39 0000-00-00 00:00:00 2026 0 0 45 str. no. 1, art. no. 3 Vol. 282 Jan. 2026 0000-00-00 Zaloznikova Objavljeno NiDoloceno 0000-00-00 0000-00-00 0000-00-00 524.8 1538-4365 10.3847/1538-4365/ae1611 265852419 Sarrouh_2026_ApJS_282_3.pdf Sarrouh_2026_ApJS_282_3.pdf 1 2A12E3318F69FC78B6588A6E157F95F3 64b78bbae5bde6012f200f86934a5611591c7224f155cbd7efc0c0ccb5cba2c8 d8ee39bb-f83b-11f0-a1ba-0050569b8976 https://repozitorij.uni-lj.si/Dokument.php?lang=slv&id=226084 https://iopscience.iop.org/article/10.3847/1538-4365/ae1611 0 e04bb6f5-f83b-11f0-a1ba-0050569b8976 https://repozitorij.uni-lj.si/Dokument.php?lang=slv&id=226085 Fakulteta za matematiko in fiziko 0 0 0