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    RESOLVE's optical spectroscopy campaign makes use of UNC guaranteed time on the SOAR and SALT telescopes, supplemented with NOAO-awarded SOAR, Gemini, and AAT time as well as Rutgers/SAAO partner SALT time. Our 21cm campaign depends on the Arecibo and Green Bank telescopes to supplement the ALFALFA HI inventory. We have also used the GALEX and Swift space telescopes to ensure complete medium-depth NUV coverage and the WIRO 2.3m telescope to help with redshift completion. Details are given below. Along with reprocessed archival data, all RESOLVE survey data will be made fully public online for the benefit other scientists, educators, students, and amateur astronomers.

    click here (txt) or here (csv) for RESOLVE Tidal Feature data (one table, all galaxies, tidal feature IDs, SFRs, morphology metric mu_delta, and nearest neighbor distances) from Hood et al. 2018 and its erratum

    click here and here for ECO and RESOLVE-B group data based on luminosity selection (two tables, all galaxies with RESOLVE-A included in ECO) from Eckert et al. 2017 WARNING: The central flag from E17 was tabulated incorrectly. An erratum will be provided asap.

    click here and here for RESOLVE DR2 data (two tables, all galaxies, HI masses and environment metrics) from Stark et al. 2016 and its erratum

    click here for RESOLVE DR1 photometry (all galaxies, UV/optical/near-IR) from Eckert et al. 2015 and its erratum

    click here for ECO DR1 catalog (all galaxies) from Moffett et al. 2015

  • The RESOLVE Image Slicer: (a) design showing slicer as viewed from the spectrograph side; (b) photo of slicer as viewed from the telescope side; (c) velocity field derived from slicer data overlaid on a galaxy image.

  • Optical Spectroscopy: SOAR's Goodman Spectrograph is the workhorse instrument of RESOLVE, with a custom three-slit image slicer front end optimized for the angular size range of RESOLVE galaxies. We are actively observing in three setups: a low-resolution broad wavelength coverage setup ideal for stellar population and emission-line ratio analysis, a high-resolution blue setup ideal for stellar absorption line kinematics,and a high-resolution red setup ideal for ionized gas emission line kinematics. In poor weather we obtain redshifts for galaxies suspected to meet the RESOLVE selection criteria despite lacking SDSS redshifts (due to incompleteness in the original redshift survey). The goal is to obtain at least one broad and one kinematic-quality observation of all ~1600 galaxies in RESOLVE's volume-limited census, with selected faint galaxies reserved for the SALT RSS long slit mode, the smallest galaxies reserved for the Gemini GMOS IFU, and the most face-on galaxies divided between SALT/RSS Fabry-Perot, AAT KOALA/Gemini, and Gemini/GMOS depending on angular size.
  • HI Data: RESOLVE's unique fractional mass limited 21cm census is almost complete as of late 2015. To ensure detections or strong upper limits (MHI<0.05M*) for all galaxies in RESOLVE, we have obtained deep pointed observations of galaxies undetected by the flux-limited ALFALFA survey over several years of observing with both Arecibo and the GBT. We have also observed all RESOLVE galaxies in the southern half of Stripe 82 (the only part of RESOLVE not covered by the ALFALFA 21cm survey footprint).
  • UV Data: GALEX completed priority MIS-depth coverage of the RESOLVE-A footprint (encompassed within ECO) in the fall of 2011, complementing existing MIS-depth coverage of RESOLVE-B. Our dedicated program on Swift added UV data for a few galaxies not observed due to GALEX safety limits. The UV photometry is included in published RESOLVE and ECO data tables (Eckert et al. 2015 and Moffett et al. 2015).
  • Archival Data: RESOLVE's equatorial footprints lie conveniently at the intersection of several wide-area surveys in the optical (SDSS), near-IR (2MASS/UKIDSS/VISTA), and mid/far-IR (WISE/AKARI), with future accessibility for ALMA. The footprints overlap extensively with multiple redshift surveys, deep imaging programs (e.g., Stripe 82 DES/SpIES/VLA continuum plus the smaller COSMOS and GAMA fields), Herschel programs (ATLAS and HeLMS), and the blind 21cm ALFALFA survey, which covers all but the southern half of Stripe 82. The RESOLVE team has developed custom optical and near-IR pipelines as well as redshift compilations and environment metrics.