This target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.0Assigned ID: 678
----- Attempting Submission 1 (Fri Apr 05 19:48:49 GMT 2019) -----The three targets that are in the target list but not observed are the three targets that are to be included in our analysis but are already in the archive.This is a correction of a typo in the buffer time of visit 2 exposure 2-1186685045----- Attempting Submission 1 (Wed Jul 24 21:45:55 GMT 2019) -----
----- Attempting Submission 2 (Thu Oct 10 19:02:46 GMT 2019) -----COS-SAGA: The Circumgalactic Medium of Nearby Milky Way Analogs and their SatellitesWe propose COS FUV spectroscopy for 7 QSOs (complemented by 3 archival observations) around 7 nearby Milky Way-like galaxies to study the gaseous halos of these systems. The galaxies are selected from SAGA, an ongoing survey to characterize the low-luminosity dwarf galaxy satellites around Milky Way analogs. We have identified a set of QSO sightlines to study the gaseous halos of these Milky Way-like hosts and their satellites. The proposed FUV-bright QSOs are within the virial radius (~300 kpc) of each system. Armed with the combination of a complete satellite luminosity function for these hosts (M_V < -12) and the corresponding satellites' velocities, we will be in the unique position to directly compare CGM kinematics to that of the host halo. This is only possible because the satellite systems are fully characterized and matched simulations are available as a part of the SAGA project. This proposal's observations will be the first to compare halo gas kinematics with those of the dwarf satellite populations, which will allow assessments of how much of the absorption seen in more distant halos could arise in satellites. The relative kinematics of stars and gas will also constrain models of halo formation from numerical simulations. Hence, this proposal will open a new window on our understanding of the CGM by combining a large ground-based effort with the unique FUV capabilities of HST/COS.7 QSOs are to be observed for use as tracers of the CGM around several local MW-like galaxies. 3 of the QSOs have some extended redder galaxies they are embedded in, but all are brighter in the UV, so in COS they should be effectively point-sources. G130M with cenwave 1291 is used to hit most of the low-z CGM lines, with only FP-POS 3/4 being used because several of the critical CGM lines at low-z are on the B segment.Dr. Erik Tollerud is a SAGA team member, an expert in simulation/observation comparisons (particular for Local Group-like systems), spectroscopic observations, and HST data analysis software. Dr. Jason Tumlinson and Dr. Rongmon Bordoloi are experts on observations of the CGM with COS, the instrument used in this proposal, with tens of papers on the topic (e.g., the recent Tumlinson et al. 2017 review on the CGM). Profs. Marla Geha and Risa Wechsler are co-PIs of the SAGA Survey and have related expertise in survey design and analysis of the SAGA Survey, as well as spectroscopic analysis and interpretation of cosmological simulations. Dr. Benjamin Weiner is a SAGA team member with extensive spectroscopic observational experience and expertise in galaxy formation. Dr. Yao-Yuan Mao is a SAGA team member and expert on application of cosmological simulations and empirical models of the galaxy-halo connection. Prof Andrew Wetzel is an expert on hydrodynamic cosmological simulations and their connections to galaxy formation, as well as a member of the FIRE team. Dr. Cameron Hummels is an expert on and principal author of the Trident Synthetic Spectrum Generator, a tool specifically designed to use cosmological simulations to produce mock observations of the CGM like that this this proposal aims to generate.Galaxies and the IGM6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARNOJ2000J2000FUV=17.14GALAXYQSOQUASARNOJ2000J2000FUV=17.66GALAXYQSOQUASARNOJ2000J2000FUV=17.83GALAXYQSOQUASARNOJ2000J2000FUV=17.92GALAXYQSOQUASARNOJ2000J2000FUV=18.39GALAXYQSOQUASARNOJ2000J2000FUV=18.67GALAXYQSOQUASARNOJ2000J2000FUV=18.98COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode./private/var/folders/7_/0n3gbrls1sb2vn6xjprw8c280000gn/T/OPVisit13380508681375179736.xml(Tic-Visit
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