Submission failed communicating with the submission server: java.rmi.ConnectException: Connection refused to host: 130.167.201.116; nested exception is: java.net.ConnectException: Connection refused: connect Submission failed communicating with the submission server: java.rmi.ConnectException: Connection refused to host: 130.167.201.116; nested exception is: java.net.ConnectException: Connection refused: connect Submission failed communicating with the submission server: java.rmi.ConnectException: Connection refused to host: 130.167.201.116; nested exception is: java.net.ConnectException: Connection refused: connect Assigned ID: 133 ----- Attempting Submission 1 (Thu Feb 23 04:20:00 GMT 2012) ----- I think that I cleared out the exposure overruns (at least I don't see those problems now). There are still some warnings. The position is well-known, so I'm not concerned about that one but I don't know how to make the FP-POS sequencing more efficient. ----- Attempting Submission 1 (Fri Jul 20 17:32:26 GMT 2012) ----- HST Phase II Proposal 12904 (Prop12904_phII.apt) successfully submitted. ----- Attempting Submission 2 (Tue Aug 14 15:23:36 GMT 2012) ----- I checked all of these, so I don't see why I'm getting these warnings, but they are not errors. The Galactic Fountain Meets The Accreting Halo Galaxies grow by accretion of gas in addition to mergers, but the current accretion rate onto a typical spiral is uncertain by at least an order of magnitude. Gas can accrete hot and we observe X-ray emitting gas extending several kpc above the plane around spirals. This may be a hot accretion mode, a galactic fountain, or a combination. These phenomena are best studied around edge-on galaxies, where there is unambiguous height information. A unique set of conditions exist around the nearby edge-on galaxy NGC 891, which not only has an HI map and X-ray halo extending 10 kpc from the disk, it has a bright background AGN projected 5 kpc above the disk. Metal halo absorption lines of Fe II and Mg II are seen against the AGN continuum, offering the promise of using metallicities to differentiate between fountain gas, with near-solar metallicities, and accreted gas with 0.1-0.3 solar metallicities. We cannot achieve those goals with these low resolution NUV STIS spectra, but the proposed COS observation will permit us to determine metallicities as a function of velocity through the rotating halo. Depletions onto grains will be inferred from elemental column density ratios. These observations will determine the relative importance of fountain vs accretion and will provide the most complete picture for the properties of a gaseous halo around a normal spiral galaxy. This program is designed to obtain spectra of an AGN projected behind the halo of an edge-on galaxy, NGC 891 for the purpose of characterizing the metallicity distribution in multiple elements. ISM IN EXTERNAL GALAXIES 12 false 0.0 0.0 false false false false SUPPORTED GALAXY HALO QSO SPIRAL J2000 J2000 COS/FUV Spectroscopic No No G130M 1291 COS/NUV Spectroscopic No No G230L 3360 C:\Users\jbregman\AppData\Local\Temp\OPVisit1617089606502453669.xml The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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