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A Spatially-Resolved Look at the Relationships between Star-Formation and AGN
Program ID 19098
Science Category Galaxies
Program Type Analysis
Category Medium
Principal Investigator Massimo Griggio
PI Institution Space Telescope Science Institute / STScI
Co-Investigators
  • Russell Ryan (Space Telescope Science Institute)
  • Preethi Nair (The University of Alabama)
  • Andreea Petric (Space Telescope Science Institute)
  • Pierluigi Rinaldi (Space Telescope Science Institute)
  • Nor Pirzkal (Space Telescope Science Institute)
  • Travis Fischer (Space Telescope Science Institute)
  • Justin Kader (University of California, Irvine)
  • Anton Koekemoer (Space Telescope Science Institute)
  • Norman Grogin (Space Telescope Science Institute)
  • Seth Cohen (Arizona State University)
  • Mitchell Revalski (Space Telescope Science Institute)
  • Barry Ryan (US Naval Observatory/George Mason University Institute)
  • Stacey Alberts (Space Telescope Science Institute)
  • Patrick Ogle (Space Telescope Science Institute)
  • Stephanie LaMassa (Space Telescope Science Institute)
  • Pallavi Patil (Johns Hopkins Univserity)
  • Swetha Sankar (Johns Hopkins Univesity)
  • Steven Finkelstein (University of Texas, Austin)
  • Annie Giman (Johns Hopkins University)
  • Kate Rowlands (Space Telescope Science Institute)
  • James DerKacy (Space Telescope Science Institute)
Abstract We propose to leverage the unprecedented wide-field, slitless spectroscopy provided by the Roman HLTDS and HLWAS-Deep for our comprehensive analysis of spatially-resolved star formation. Importantly, this spatial resolution will be incredibly informative in further constraining the interplay between the active-galactic nucleus (AGN) and its host galaxy, in particular any positive or negative feedback it may have in fueling or quenching star formation. We will employ advanced analysis techniques to derive three-dimensional, IFU-like flux-cubes and two-dimensional emission-line maps for >10,000 galaxies and AGN over the ~20 deg2. From this sample we will address five concrete concepts: 1. How does the mass-metallicity relation change with redshift and/or galaxy properties? Our sample will be sensitive to 1<z<2.5 on spatial scales of ~900 pc/pixel. 2. Is there evidence for Case B violation? Many IGM studies rely on the case B assumption, but we will have the data to make precise tests of the validity of this assumption on various spatial and redshift scales. 3. Where is the dust in the galaxies? From the resolved spectroscopy, we can pinpoint the dustiest regions and how they link to the above properties of mass-metallicity and/or case B violations. 4. What more can we learn of little-red dots? Uniquely deciphering the spectra of the core versus the outskirts of the little-red dots is crucial to understand the energetics powering these enigmatic objects. 5. What are the spatial signatures of the AGN-galaxy coevolution? At cosmic noon, AGN are known to play a symbiotic role in galaxy evolution, and here we can spatially deconstruct these relationships. Our program fulfills the promise of resolved spectroscopy to the study of galaxies and their AGN in ways never before possible.