0Assigned ID: 272
----- Attempting Submission 1 (Thu Apr 04 21:15:25 GMT 2019) -----
HST Phase I Proposal 272 (n4565.apt) successfully submitted.
Receipt: # 272-1If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONS
If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONS
If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
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.
If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONS
If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
INEFFICIENT ORDERING OF FP-POS POSITIONSNov 2019: for visit 7 ACQ, changed from MIRROR-A to MIRROR-B at request of COS contact scientist.
Target 3 is a bright Seyfert nucleus. Use of PSA+MIRROR-A for its ACQ/IMAGE
leads to "bright limit" warnings from the ETC and is flagged as a
Health&Saftey issue by the BOT. We've therefore changed the ACQ to use
MIRROR-B instead (is this the best solution?).276595580----- Attempting Submission 1 (Fri Jul 12 09:01:03 GMT 2019) -----
HST Phase II Proposal 15885 (n4565.apt) successfully submitted.
Receipt: # 15885-1
----- Attempting Submission 2 (Tue Nov 26 17:19:41 GMT 2019) -----Impossible to implement a full set of FP-POS as there are only 2 for the
1291 setting of the G130M.
For the two FP-POS settings, FP-POS=3 is always selected first before
FP-POS=4; this follows the "most effecient order" as stated in the IHB of
1, 2, 3 & 4 when 1 & 2 doesn't exist.
All targets are quoted as having position accuracies of 0.3 arcsec, so only
a simple ACQ-IMAGE is required.Skewered: A Census of the Circumgalactic Medium of NGC 4565 from 13 QSO Sightlines Within its Virial RadiusWe propose using COS to observe 6 new QSO sightlines within a virial radius Rv of 0.5 - 1.0 of NGC 4565 in order to probe its circumgalactic medium (CGM) at multiple positions. NGC 4565 (the Needle Galaxy) is a highly inclined (i=86 degrees) spiral galaxy, and its orientation makes it an ideal target for looking for kinematic and metallicity signatures from outflows along its minor axis, or inflows into the disk along its major axis. NGC4565 is currently part of a COS program to probe the inner CGM below 0.5 Rv with 7 QSO lines-of-sight (GO-15196), and this proposal is designed to extend the map of HI and metals into the outer CGM beyond 0.5 Rv. Our data will enable us to measure how HI and metal line column densities change with galactocentric radius. They will also allow us to investigate how the properties of the absorbing gas, including its column density, multi-component structure, and bulk velocity, change with position relative to the major and minor axes of the galaxy. For example, two of the new sightlines lie close (within +/- 20 degrees) to the major axis of the galaxy's disk, and absorption along their sightlines will test whether the decline in velocity relative to the systemic velocity seen at small distances from the center of NGC 4565 continues into the outer halo.These are G130M observations of mostly faint QSOs. The most important absorption lines from the intervening galaxy is Lyman-alpha and SiIII 1206. As the foreground galaxy is at low redshift, these lines remain near geocoronal Lyman-alpha. We therefore need to use the remaining G130M-1291 grating setting. We utilize the 2 remaining FP-POS positions to mitigate the effects of large-scale defects. There will be a gap left between 1274-1294A which can no longer be filled using a different grating setting, but few absorption lines from the intervening galaxies are expected at these wavelengths.
Target ACQs: exposure times set by assuming half the cataloged FUV GALEX flux (to account for variability), and assuming a flat spectrum.
Observations are not affected by RGM, except for access to the sightlines because of a reduced Field of Regard. Since the main science goal is to sample the halo of NGC4565 using as many background QSO sightlines as possible, it remains important to observe as many of the probes as possible, despite their concentration in one area of the sky.Dr. David Bowen is a Research Astronomer in the Astrophysical Sciences department of Princeton University. He has over 30 years experience designing programs to study the distribution of baryons in the universe. He has lead more than 22 programs using HST, the Far Ultraviolet Spectroscopic Explorer (FUSE) and the Galaxy Evolution Explorer (GALEX). Dr. Edward Jenkins is also a Research Astronomer at Peyton. He is a world leader in the analysis of the interstellar medium (ISM) and has pioneered numerous techniques in the analysis of satellite-based data. In several cases he has led or participated significantly in the development of space missions (e.g. Copernicus, IMPAS). Prof. Todd Tripp is a professor at the Univ. of Mass and is one of the preeminent experts in the study of the intergalactic medium and the circumgalactic medium (CGM), as well as the ISM of our own Milky Way. He too has extensive expertise in the analysis of HST data and has led several large COS programs. Prof. Doron Chelouche is an expert in the theory of astrophysical plasmas and in their relationship to the circumgalactic medium around the halos of galaxies.Galaxies and the IGM6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSONOJ2000J2000GALEX FUV = 34 micro-JyGALAXYQSONOJ2000J2000GALEX FUV = 29 micro-JyGALAXYSEYFERTYESJ2000J2000GALEX FUV = 269 micro-JyGALAXYQSONOJ2000J2000GALEX FUV = 118 micro-JyGALAXYQSONOJ2000J2000GALEX FUV = 72 micro-JyGALAXYQSONOJ2000J2000GALEX FUV = 36 micro-JyCOS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291/Users/dvb/Props/c27/n4565/P2/OP-cache/n4565-v01.xmlThe scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.First of 2 visits, 3 orbits of 6(Tic-Visit
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