Spectral Imaging of O VI and Ly-alpha from a Giant Intragroup Filament

Oops...hid the tracking changes! -1702748912 Assigned ID: 2422 ----- Attempting Submission 1 (Fri Apr 09 23:09:54 GMT 2021) ----- HST Phase I Proposal 2422 successfully submitted. Receipt: # 2422-1 ----- Attempting Submission 2 (Fri Apr 09 23:13:09 GMT 2021) ----- HST Phase I Proposal 2422 successfully submitted. Receipt: # 2422-2 ----- Attempting Submission 3 (Fri Apr 09 23:21:55 GMT 2021) ----- HST Phase I Proposal 2422 successfully submitted. Receipt: # 2422-3 Could not connect to APT Status Server We have defined a fixed target QSO-J1619+3342-FILAMENT that is offset from the Phase I target by about 3 arcsec. We use this target as the pointing center so that any observatory orientation will encompass the entire filament we are observing no matter the orientation. We have placed no constraints on the orientation in order to provide maximum flexibility for scheduling our visits, necessitating this slight offset position. 1912324709 ----- Attempting Submission 1 (Tue Jul 27 14:58:42 GMT 2021) ----- Difficulty connecting Spectral Imaging of O VI and Ly-alpha from a Giant Intragroup Filament Streams of gas in cosmological halos are critical to galaxy evolution, as they bring matter into halos (accretion) and carry matter out (outflows). In addition, "intergalactic transfer" from satellites and group members can be important for building up the gas mass of galaxies. We have discovered a giant (>100 kpc) [O II]-emitting nebula in the group environment of a z~0.5 QSO. The filament is devoid of starlight, showing instead knots of nebular emission in HST/ACS imaging; it is coincident in redshift with a partial Lyman-limit system having 1/20 solar metallicity in HST/COS spectroscopy. The filament may be an example of intragroup gas commonly identified via HI-selected absorption studies, representing either material stripped or shed from group members or accreting with new infall. We propose an ACS/SBC imaging campaign to study the spatial distribution and intensity of O VI and Ly-alpha emission from this filament, constructing a synthetic narrow band filter through difference imaging in two ACS longpass filters. Our proposed observations will allow us for the first time to understand how the warm/hot and cool phases of circumgalactic gas are related, provide a robust measure of the cooling rate of hot material in a gaseous halo, and give unique density and mass estimates in a filament. This filament is one of the few opportunities we have to image intergalactic gas prior to the next generation of UV telescopes and will be the only case for which we have both absorption and emission line data for the same species. Instrumental configuration: pseudo-filters to isolate emission lines Following the technique pioneered by Hayes+ (2005, 2016) we aim to isolate diffuse emission in the O VI 1034 doublet and Ly-alpha 1215 from the z = 0.4708 filament associated with the QSO J1619+3342. The observed wavelengths of these lines will be 1520 Ang and 1797 Ang. We will observe the field in the F150LP and F165LP filters of the ACS/SBC, covering an area 210 x 185 kpc at z = 0.47, roughly the size of the panels in Fig. 1. We will isolate O VI using image subtraction in the two longpass filters to create a synthetic narrowband filter: F155NBsyn = F150LP - F165LP. This approach takes advantage of the shared red wings of the longpass filters (Fig. 2), which allow the accurate removal of continuum and redder line emission from the bluest filter used. This approach has successfully been demonstrated in several previous cycles through programs 13656, 14079, 15298, 15655, and 16231 in Cycles 22-28. Unlike many of these previous programs, we are imaging pure nebular emission with no continuum (based on ACS/ WFC and deep ground-based broadband imaging); we may be able to use the F165LP filter to isolate Ly-alpha emission, as well (at least outside of galaxies). Observing approach We request that the visits are scheduled so that SBC has been switched off for at least 24 hours prior to reduce the dark current. For the same reason, we also request that each 2-orbit visit be spaced from the next visit by at least 24 hours, with the SBC turned off in between. The typical visibility of the O-tube is 53 minutes. In a 2-orbit visit, overheads total ~10.5 min and ~8 min in orbits 1 and 2. This leaves ~2.5 ks in each orbit for exposure. In each visit we will execute a square 4-point box dither pattern (with half-pixel shifts) to subsample the PSF. To address potential large-scale gradients in the flatfielding, etc., each visit will be made on a 3x3 grid with points offset by 2.5 arcsec using the POS TARG functionality. The last three visits repeat the positions of the first three (although even these will not be exactly the same if the orientations are not identical). The pointing center of this pattern is offset from the QSO by (delta RA, delta Dec) = (+3.21, +1.83) arcsec [centered at (RA, Dec) = (16:19:16.8, 33:42:40.2)]. This ensures that different observatory orientations will all include the full extent of the filament within the SBC field of view. Each visit obtains 1 orbit of exposure time in the F150LP and F165LP filters. The total exposure time in the two filters is the same when combining all 12 visits. PI Howk and CoIs Lehner and O'Meara have over 2 decades of experience analyzing HST UV spectra and studying the circumgalactic medium. Howk has experience with imaging diffuse gas near galaxies and with continuum subtraction of narrowband imaging. CoI Berg, along with Howk and O'Meara, is responsible for the KCWI observations and analyses that led to the discovery of the diffuse filament that is the target of this proposal. The proposed research program will be principally overseen by PI Howk at the University of Notre Dame. The program will be led by both the PI, CoI Lehner, and a graduate student at Notre Dame. They will lead the basic data reduction as well as the bulk of the analysis and interpretation of the results. CoIs O'Meara and Berg will particularly support the acquisition and interpretation of ancillary ground-based data. PI Howk and CoI O'Meara have institutional access to the Keck telescopes. Each will devote a portion of their time with the new KCRM instrument (including during 2022A commisioning) to obtain IFU imaging at longer wavelengths than available with KCWI in order to study the distribution of [O III], Hbeta, and Halpha. This will help diagnose the conditions of the filament itself. Howk will also apply institutional time with the MODS spectrograph on the LBT to characterize the galaxies themselves, notably their metallicities for comparison with that of the filament. Intergalactic Medium and the Circumgalactic Medium Galaxies 6 false false true false false false false false SUPPORTED GALAXY EMISSION LINE NEBULA LYMAN ALPHA CLOUD QSO This object was generated by the target selector and retrieved from the SIMBAD database. J2000 J2000 ACS/SBC Imaging No No F150LP ACS/SBC Imaging No No F165LP POS-TARG DITHER 0.894773 LINE 0.587116 false false 64.478514 4 20.151333 BOX 3

false

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