0Assigned ID: 592
----- Attempting Submission 1 (Fri Mar 06 17:49:16 GMT 2020) -----
HST Phase I Proposal 592 successfully submitted.
Receipt: # 592-1
----- Attempting Submission 2 (Fri Mar 06 20:28:13 GMT 2020) -----0----- Attempting Submission 1 (Mon Jun 29 22:46:19 GMT 2020) -----The Circumgalactic Medium at the Lowest Mass EndCOS has created a legacy with the detection of large quantities of baryons in dark matter halos; however, there remains a crucial unprobed mass scale. Dwarf galaxies, or dark matter halo masses < 10^10.5 Msun, appear to have lost the vast majority of their baryons, but beyond the central few kpc the baryon distribution is unknown. The circumgalactic medium (CGM) may now harbor the baryons. CGM observations of dwarf galaxies provide crucial insight into the missing baryon problem and feedback efficiency at the low mass end.
We propose to study the distribution, kinematics, metal content, and ionization properties of the CGM of some of the smallest galaxies in the universe through UV-bright background QSOs within the virial radius of dwarf galaxies in the Local Volume. This sample is unique as the low mass range of the dwarf galaxies is unexplored and their proximity means comparisons can be made to their resolved stellar populations and gas distributions. The dwarf galaxy observations will allow for: (1) the ionization, mass and distribution of their CGM to be compared to larger galaxies, (2) constraints on the feedback prescriptions of state-of-the-art dwarf galaxy simulations, (3) a comparison of the metals in the CGM to what remains in the stars and gas in the main body of the dwarf galaxies.This survey of the circumgalactic medium of dwarf galaxies in the Local Volume uses the Cosmic Origins Spectrograph in medium resolution mode with the G130M and G160M gratings. We will observe 5 QSOs distributed within the virial radii of the dwarf galaxies. With the G130M and G160M gratings, we will cover 1150 - 1775 AA, and this will allow us to achieve our goal of observing a variety of metal absorption lines to constrain the ionization properties and mass of metals in the halos. For our science goals, carbon and silicon are key elements as their various ionization states are covered by both G130M and G160M gratings and these lines are frequently detected in the CGM. The observations are designed to yield S/N ~ 15, high resolution (~20 km/s) spectra at Si II (1260) and C IV (1550).
The GALEX data were examined for all sources to estimate the UV flux level and check if the sources are extended in the UV. The FUV fluxes are noted for each target and one of our original sources (MCG-03-01-002) was found to be extended on close inspection of the GALEX imaging. We have replaced this source with PG 1415+451 which provides an additional sightline for the dwarf galaxy DDO190 to map its CGM. The SDSS and NED images were checked to ensure there are no obvious stars or galaxies interfering with the GALEX flux. All our targets are selected to be brighter than 18.5 AB mag in FUV.
All exposure times were calculated with the COS ETC. We will acquire our sources with the NUV imaging mode and use Mirror B for all of our sources given their brightness. For the G130M grating, we have decided to stick with a central wavelength of 1291 and alternate between FP-POS 3 and 4 given Segment A is not available with the other central wavelengths. For G160M, we alternate between a central wavelength of 1589 and 1611 and use the majority of the FP-POS positions for each source to optimize the S/N across the spectrum.Mary Putman is a Professor of Astronomy at Columbia University and the PI of this proposal. Putman is an expert on observations of the gas surrounding galaxies in the local universe, in particular gas detected in HI. She has published numerous papers with collaborators and graduate students using COS data and will ensure the project is successfully brought to completion.
Yong Zheng is a Miller Postdoctoral Fellow at Berkeley and specializes in the analysis of UV spectra and HI data. She has conducted several research projects on the circumgalactic medium of galaxies using HST/COS that are now published. Yong has the full set of skills required to analyze the COS spectra we obtain.
Jessica Werk has been using COS, the instrument selected for these proposed observations, since Cycle 17, when it first came online. She has published over 30 papers that present results based on HST/COS data, with a focus on the intricate relationship between galaxies and their extended gaseous envelopes. Her experience reducing and analyzing COS absorption line spectroscopy is extensive, and her experience using CLOUDY, a full radiative-transfer code, to determine the physical properties of the absorption features will be highly useful in the analysis.
Andrew Emerick is a postdoctoral fellow at Caltech with significant experience in developing and running computational simulations of the type that will be used for direct comparison to the proposed observations. Mr. Emerick additionally has prior published experience in generating mock absorption spectra of these same types of simulations.
Benjamin Oppenheimer is an expert in computational hydrodynamic simulations of galaxies and their gaseous environments. He specializes in understanding how the physical and evolutionary parameters of the IGM/CGM can be quantified through observational campaigns. He is most expert at interpreting COS UV data and has published numerous papers in this area.
Evan Kirby is an expert in stellar spectroscopy. He has institutional access to the Keck telescopes and 14 years of experience observing and analyzing stellar spectra. Kirby is an expert on the resolved stellar spectroscopy of dwarf galaxies and will aid in the interpretation of the metals in the disks compared to what we find in the halos.
Joseph Burchett is an experienced analyst of COS spectra, having led 4 published papers based on COS data. He is leading the HST GO program 15227, which aims to constrain the mass in metals residing in dwarf galaxy halos relative to the metals produced over their star formation history. This program, which is obtaining data for galaxies at lower S/N, is complimentary to our current proposed program. Dr. Burchett will facilitate the synthesis of results from these two programs.
Kristen McQuinn is an expert on low-mass galaxy evolution. She has extensive experience in star formation histories and the age-metallicity relation derived from stellar populations in nearby dwarfs. McQuinn will provide perspective on the star formation that produced the metals and the stellar feedback that launched the metals into the CGM.Galaxies6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYQSONOJ2000J2000FUV=18.48GALAXYQSONOThis object was generated by the targetselector and retrieved from the SIMBAD database. Slight tweak of the coords to be the ICRS SIMBAD.J2000J2000FUV=17.43GALAXYQSONOExact coords on MAST slightly different?RXSJ00537+2232J2000J2000FUV = 16.53GALAXYQSONOJ2000J2000FUV=18.25GALAXYQSONOJ2000FUV=17.25COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611/System/Volumes/Data/solaris/user1/csoto/OP-cache/16301-v01.xmlThe scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.6 orbits G130M1621108781000237.63748009706075(Tic-Visit
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