0 Assigned ID: 6731 ----- Attempting Submission 1 (Thu Apr 10 21:38:14 GMT 2025) ----- HST Phase I Proposal 6731 successfully submitted. Receipt: # 6731-1 ----- Attempting Submission 2 (Thu Apr 10 21:54:40 GMT 2025) ----- 0 ----- Attempting Submission 1 (Tue Aug 12 21:45:01 GMT 2025) ----- Growing in the Wind: OVI Spectroscopy of Cool Clouds mixing with a Hot CGM Models of the circumgalactic medium (CGM) show that it is fed by outflows from galaxies. These outflows expel cool clouds into a hot medium, where the clouds can grow by turbulent mixing and radiative cooling. Recent deep HST-UV images of the giant, luminous wind surrounding the massive, star-forming Makani galaxy show that T~10^5.5 K gas--as revealed by O VI 1032, 1038 Angstrom emission--has the same morphology as the cooler gas emitting [OII], implicating this mixing process. We propose deep COS spectroscopy to directly detect and spectrally resolve O VI in emission and absorption from the nebula center. This will complete the spatial+spectral picture of O VI in Makani and allow us to calculate the density and mass of the warm-hot phase of the wind-CGM interaction. We can then compare to galaxies of lower mass and star-formation rate. Makani is only the second galaxy imaged in O VI, and thus represents a key benchmark for future UV space missions like HWO. Fully characterizing its O VI nebula will best inform design requirements for such a mission. The primary goal is to achieve sufficient S/N to detect and characterize the O VI emission and absorption lines in Makani, an interacting system at z=0.459. These arise at an observed wavelength of 1510 A. Secondary goals include measuring the Lyalpha line at 1774 A and the Ly continuum (LyC) below 1331 A observed-frame. We select the G140L grating, which spectrally resolves the O VI lines which we expect to be quite broad (FWHM 1000 km/s) while maximizing S/N per resolution element. The 800 A wavelength position, covering wavelengths 800 to 1950 A, will probe OVI+Lyalpha and the stellar continuum while maximizing our sensitivity to any LyC leakage. The observing program is quite straightforward, and involves repeated exposures of one target with the same grating and central wavelength to maximize the signal-to-noise. We group the exposures into visits of 2 orbits each. The first orbit consists of an ACQ/IMAGE, followed by exposures at the first two FP-POS. The second orbit covers FP-POS 3 and 4. Acquisition: The target's coordinates are well-constrained by HST WFC3 imaging, registered to Gaia, to ~0.02" in either direction. (These are also consistent within <0.1" with the lower-precision SDSS and WISE catalog coordinates.) The target has a bright core, effectively a point source with FWHM~0.05", that contains about half of the total UV light. (The rest is distributed over a larger, ~1" area). Thus, the total GALEX NUV magnitude of 20.90 becomes 21.65 within the central point source. We use this to estimate the time needed to achieve S/N=20 for an ACQ/IMAGE of a spectrally flat point source and get 43 seconds. Using another method, we target a point source with observed flux 7e-17 erg/s/cm^-2/A at 1605 A based on ACS SBC F150LP imaging and a Kinney SB1 template redshifted to z=0.459 and extincted by E(B-V)=0.5. This yields 28 seconds to achieve S/N=20 in an ACQ/IMAGE. In the actual visit, we use a 60 second ACQ/IMAGE to be slightly conservative. The peak flux in ct/s/pix for a 43 s ACQ/IMAGE is 1.3. Science: We estimate an O VI flux (integrated over both 1032 and 1038 A lines) in the COS aperture of order 4e-16 erg/s/cm^2. Similarly, the central Lyalpha flux is approximately 4e-15 erg/s/cm^2. The continuum flux density is given above. We start with the Kinney SB1 starburst template spectrum; redshift it to z = 0.459 and extinct it by E(B-V) = 0.5; normalize to the Makani point source continuum emission; and add O VI and Lyalpha emission lines. These parameters go into the exposure time calculator for a 1100 s exposure. Splitting the FP-POS among two orbits results in exposures of duration 1000-1200 s. Dr. David Rupke is an expert on the target, Makani, including leading the Nature discovery paper and the ACS SBC detection of OVI, and has extensive experience with absorption- and emission-line spectroscopy of galaxies. Dr. Christy Tremonti originated the sample from which the data were drawn and is an expert in photoionized nebula and stellar populations. Dr. Alison Coil co-discovered the Makani nebula with PI Rupke and helped write the discovery paper; and has led other efforts to study the larger sample from which it is drawn. Dr. Sean Johnson is an expert on HST spectroscopy and imaging in the UV. Other Co-Is are active contributors to the analysis and interpretation of past and ongoing Makani observations. Intergalactic Medium and the Circumgalactic Medium Galaxies 6 false true false false false false SUPPORTED GALAXY INTERACTING GALAXY STARBURST NO SDSS-J211824.06+001729.4 WISEA-J211824.05+001729.4 J2000 J2000 GALEX NUV = 20.89 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G140L 1280 /Users/drupke/Documents/proposals/observing/hst/cycle33/phase-ii/OP-cache/makani-cos-phase-ii-v01.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. 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