0Assigned ID: 895
----- Attempting Submission 1 (Fri Apr 07 21:12:18 GMT 2017) -----For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.Replaced Visit 56 with new Visit 57 due to lack of target acquisition.1589606554----- Attempting Submission 1 (Thu Jul 20 23:36:44 GMT 2017) -----
HST Phase II Proposal 15227 (ProdigiousPolluters_Phase2.apt) successfully submitted.
Receipt: # 15227-1
----- Attempting Submission 2 (Fri Aug 04 19:45:34 GMT 2017) -----
HST Phase II Proposal 15227 (ProdigiousPolluters_Phase2.apt) successfully submitted.
Receipt: # 15227-2
----- Attempting Submission 3 (Mon Aug 07 13:12:44 GMT 2017) -----
----- Attempting Submission 4 (Tue Aug 08 16:03:13 GMT 2017) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 5 (Thu Dec 06 20:33:29 GMT 2018) -----This submission adds the target acquisition that was missing from Visit 56, replacing Visit 56 with a new Visit 57.Finding the missing metals around the Universe's most prodigious pollutersAnalysis of the Hubble Deep Fields reveals that star-formation in the early universe is dominated by the faintest galaxies detected, and the formation and evolution of these dwarf galaxies drives the reionization, enrichment, and subsequent formation of more massive systems. In tandem, two decades of cosmological simulations have at least reached one consensus: reproducing realistic galaxy populations critically depends on the treatment of galactic feedback. Stellar and galactic winds regulate star formation but also distribute metal-enriched gas throughout the interstellar medium (ISM), into the circumgalactic medium (CGM), and beyond. Thus, a firm theoretical foundation to our understanding of galaxy evolution hinges on reproducing the enrichment and transport of heavy elements through the stars, ISM, CGM, and intergalactic medium. Current technology affords a detailed census of the metals currently in stars as well as those produced over the star formation history only in local analogs to the early dwarf polluters. Meanwhile, QSO absorption line spectroscopy can constrain the CGM component. We propose observations of UV-bright QSOs that probe the CGM of a sample of very-nearby low-mass dwarf galaxies for which the HST archive contains imaging suitable to constrain the metal production history, and the QSO spectra will enable us to 1) search for metal-enriched CGM material both at the velocities of the dwarfs and at high velocities characteristic of outflows, 2) estimate the mass of total carbon residing in these dwarf galaxy halos, and 3) compare these derived masses or limits with the amount of missing metal mass from the inner galactic regions.We have selected 12 UV-bright AGN targets, which probe the circumgalactic media of z~0 local dwarf galaxies, to observe with HST-COS. Our science goals depend critically on coverage of the C II 1334 Angstrom and C IV 1548,1550 Angstrom lines from which we will measure the covering fractions of these species and constrain the total carbon mass. Therefore, the calculated exposure times should provide S/N = 10 at the z=0.001 observed wavelengths of the C II and C IV 1548 lines. With standard configurations using the G130M and G160M gratings, we can also easily cover transitions of Si II, Si III, Si IV, and N V, and these lines will help corroborate detections of C II and C IV as well as provide further constraints on the mass modeling if detected.
All of our target galaxies have similar redshifts (z~0.001), so all of our AGN targets can employ the same grating/cenwave settings. Our Phase I proposal stated that we would employ the G130M/1291 and G130M/1308 cenwave settings to fill in the detector gap between Segments A and B; however, due to the COS 2025 restrictions, Segment B must be turned off for G130M/1308 observatons. To maintain maximum wavelength coverage, we have opted to use only G130M/1291, for which Segment B may still be used under COS2025. We understand that this will leave a segment gap in the data but have concluded that the location of the gap in wavelength will not impact our science goals. Our Contact Scientist is aware of this decision and has agreed that our modified observing plan is a simple and effective adjustment. Also due to COS2025, the G130M/1291 mode only permits FP-POS 3 & 4 settings, and we will employ both these FP-POS for each of our targets.
Our G160M observations will employ the 1600 and 1623 cenwave settings, and 8 of our targets will employ all 4 FP-POS for each cenwave. However, we have requested visit configurations that employ fewer than 4 FP-POS per cenwave for 4 of our targets; this request has been approved by the COS Support Lead. Although these configurations do not employ all FP-POS for each grating, at least 2 FP-POS are used at each of the two G160M cenwaves for each target. Per the advice of our Contact Scientist, this combination of cenwaves and FP-POS should spread out the gain sag-affected regions on the detector (especially Segment B) appropriately.
Per the recommendations for Cycle 25 to keep visits at 2-3 orbits maximum for scheduling purposes, we have kept all visits at 3 orbits or less except for one target, J0958+0655. We are requesting a 4-orbit visit for this single target to avoid the ~500 sec loss in overhead for a reacquisition at the start of a second visit.
All acquisition images will be obtained in the NUV, and we have calculated all exposure times for these images using the acquistion image ETC with the appropriate NUV magnitude from GALEX. The exposure times should yield S/N=45, exceeding the minimum S/N=40. For targets faint enough in the NUV, we acquire using Mirror A; however, we will use Mirror B for objects that exceed the count rate limit with Mirror A.Galaxies and the IGM6falsefalsetruefalsefalsefalsefalseSUPPORTEDEXT-MEDIUMABSORPTION LINE SYSTEMABSORPTION LINE SYSTEM - EXTRAGALACTICHALONOThe V magnitude above has been converted from SDSS DR12 g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.J2000J2000FUV mag: 17.81, NUV mag: 17.67EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICEJECTAHALOWINDNOCoordinates given here come from the PanSTARRS database. These coordinates agree with those given by 2MASS within 0.05 arcsec. We have adopted 0.1 arcsec as a conservative uncertainty.
The V magnitude above has been converted from PanSTARRS g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.J2000J2000FUV mag: 17.74, NUV mag: 17.22EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICHALOWINDNOCoordinates given here come from the PanSTARRS database. These coordinates agree with those given by 2MASS within 0.05 arcsec. We have adopted 0.1 arcsec as a conservative uncertainty.
The V magnitude above has been converted from PanSTARRS g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.J2000J2000FUV mag: 17.35, NUV mag:17.00EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICHALOYESThe V magnitude above has been converted from SDSS DR12 g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.
We have indicated this target as 'extended' based on the optical photometry (the AGN host galaxy is at relatively low redshift). However, we expect the central concentration of the AGN to dominate the signal and minimize issues arising from spatially extended flux.J2000J2000FUV mag: 17.98, NUV mag: 17.59EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICEJECTAHALOWINDNOThe V magnitude above has been converted from SDSS DR12 g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.Q1336.2+2531J2000J2000FUV mag: 17.00, NUV mag:17.42EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICEJECTAHALOWINDNOThe V magnitude above has been converted from SDSS DR12 g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.J2000J2000FUV mag: 17.80, NUV mag: 17.29EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICEJECTAHALOWINDNOThe V magnitude above has been converted from SDSS DR12 g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.J2000J2000FUV mag: 17.68, NUV mag: 17.53EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICEJECTAHALOWINDYESThe V magnitude above has been converted from SDSS DR12 g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.
We have indicated this target as 'extended' based on the optical photometry (the AGN host galaxy is at relatively low redshift). However, we expect the central concentration of the AGN to dominate the signal and minimize issues arising from spatially extended flux.MRK1447J2000J2000FUV mag: 17.73, NUV mag: 17.39EXT-MEDIUMABSORPTION LINE SYSTEM - GALACTICEJECTAHALOWINDNOThe V magnitude above has been converted from SDSS DR12 g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.J2000J2000FUV mag = 17.11, NUV mag: 17.31EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICEJECTAHALOWINDNOCoordinates given here come from the PanSTARRS database. These coordinates agree with those given by 2MASS within 0.05 arcsec. We have adopted 0.1 arcsec as a conservative uncertainty.
We are not aware of any variability in this target.
The V magnitude above has been converted from PanSTARRS g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.J2000J2000FUV mag: 18.2, NUV mag: 17.99EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICEJECTAHALOWINDYESThe V magnitude above has been converted from SDSS DR12 g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.
We have indicated this target as 'extended' based on the optical photometry (the AGN host galaxy is at relatively low redshift). However, we expect the central concentration of the AGN to dominate the signal and minimize issues arising from spatially extended flux.J2000J2000FUV mag = 17.24, NUV mag: 16.69EXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICEJECTAWINDYESThe V magnitude above has been converted from SDSS DR12 g- and r-band photometry using the Lupton (2005) filter transformations provided by SDSS at http://www.sdss.org/dr13/algorithms/sdssUBVRITransform/#Lupton2005.
We are not aware of any variability in this target.
We have indicated this target as 'extended' based on the optical photometry (the AGN host galaxy is at relatively low redshift). However, we expect the central concentration of the AGN to dominate the signal and minimize issues arising from spatially extended flux.J2000J2000FUV mag = 18.4, NUV mag = 18.21COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1623The scheduling data was generated by CASM 27.0.CASM was run in Phase II mode.In the interest of S/N in the spectral regions critical to our science goals, we have opted to use 3 FP-POS settings for our G160M/1623 observations and 2 FP-POS settings G160M/1600. The COS User Support Lead has approved our request for this observing plan.1555585328000102.3258122919924(Tic-Visit
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)true40/private/var/folders/46/4jpf0wpx40jbz16h87362w240001d2/T/OPVisit1642119252670342123.xmlIn the interest of S/N in the spectral regions critical to our science goals, we have opted to use 3 FP-POS settings for our G160M/1623 observations and 2 FP-POS settings G160M/1600. The COS User Support Lead has approved our request for this observing plan.(Tic-Visit
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)true30The scheduling data was generated by CASM 27.0.CASM was run in Phase II mode.In the interest of S/N in the spectral regions critical to our science goals, we are employing 3 FP-POS settings for our G160M/1623 observations of this target instead of all 4. The COS User Support Lead has approved our request for this observing plan.152464708200091.48181(Tic-Visit
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