Battisti, A. J.Bagley, M. B.Rafelski, M.Baronchelli, I.Dai, Y. S.Henry, A. L.Atek, H.Colbert, J.Malkan, M. A.McCarthy, P. J.Scarlata, C.Siana, B.Teplitz, H. I.Alavi, A.Boyett, K.Bunker, A. J.Gardner, J. P.Hathi, N. P.Masters, D.Mehta, V.Rutkowski, M.Shahinyan, K.Sunnquist, B.Wang, X.2025-05-312025-05-310035-8711http://www.scopus.com/inward/record.url?scp=85190243648&partnerID=8YFLogxKhttps://hdl.handle.net/1885/733755693We present reduced images and catalogues of photometric and emission-line data ( ∼230 000 and ∼8000 sources, respectively) for the WFC3 (Wide Field Camera 3) Infrared Spectroscopic Parallel (WISP) survey. These data are made publicly available on the Mikulski Archive for Space Telescopes and include reduced images from various facilities: ground-based ugri , Hubble Space Telescope ( HST ) WFC3, and Spitzer IRAC (Infrared Array Camera). Co v erage in at least one additional filter beyond the WFC3/IR data are available for roughly half of the fields (227 out of 483), with ∼20 per cent (86) having co v erage in six or more filters from u band to IRAC 3.6 μm (0.35-3.6 μm). For the lower spatial resolution (and shallower) ground-based and IRAC data, we perform PSF (point spread function)-matched, prior-based, deconfusion photometry (i.e. forced-photometry) using the TPHOT software to optimally extract measurements or upper limits. We present the methodology and software used for the WISP emission-line detection and visual inspection. The former adopts a continuous wavelet transformation that significantly reduces the number of spurious sources as candidates before the visual inspection stage. We combine both WISP catalogues and perform spectral energy distribution fitting on galaxies with reliable spectroscopic redshifts and multiband photometry to measure their stellar masses. We stack WISP spectra as functions of stellar mass and redshift and measure average emission-line fluxes and ratios. We find that WISP emission-line sources are typically 'normal' star-forming galaxies based on the mass-excitation diagram ([O III ]/H βversus M⊙ ; 0.74 < z grism < 2.31), the galaxy main sequence (SFR versus M⊙ ; 0.30 < z grism < 1.45), S 32 ratio versus M⊙ (0.30 < z grism < 0.73), and O 32 and R 23 ratios versus M⊙ (1.27 < z grism < 1.45).The authors thank the anonymous referee, whose suggestions helped to clarify and improve the content of this work. AJB thanks the staff at the WIYN and Magellan facilities for their assistance with technical aspects of the observations. AJB is also thankful for attending ASTRO 3D writing retreats that provided a helpful environment to complete portions of this manuscript. Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project no. CE170100013. We acknowledge the invaluable labour of the maintenance and clerical staff at our institutions, whose contributions make our scientific discoveries a reality. This research was conducted on Ngunnawal Indigenous land, as well as within the traditional homelands of the Dakota people. This work is sponsored by the National Key R&D Program of China for grant no. 2022YFA1605300, the National Nature Science Foundation of China (NSFC) grants nos 12273051 and 11933003. HA is supported by CNES (Centre National d\u2019Etudes Spatiales). AJ Bunker acknowledges funding from the \u2018FirstGalaxies\u2019 Advanced Grant from the European Research Council (ERC) under the European Union\u2019s Horizon 2020 research and innovation programme (grant agreement no. 789056). Support for WISP (HST programs GO-11696, 12283, 12568, 12902, 13517, 13352, and 14178) was provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work uses data from WIYN. The WIYN Observatory is a joint facility of the NSF\u2019s National Optical-Infrared Astronomy Research Laboratory, Indiana University, the University of Wisconsin-Madison, Pennsylvania State University, the University of Missouri, the University of California-Irvine, and Purdue University. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. This work uses data from Palomar. The Palomar Observatory is a joint facility of the Caltech/Caltech Optical Observatories, Jet Propulsion Laboratory, Yale University, and National Astronomical Observatories of China. This work uses data from SDSS. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This work uses data from PAN-STARRS. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen\u2019s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant no.AST\u20131238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.35enPublisher Copyright: © 2024 The Author(s).cataloguesgalaxies: evolutiongalaxies: generalgalaxies: photometryISM: evolutionsurv e ys2024-05-0110.1093/mnras/stae91185190243648