0Assigned ID: 1743
----- Attempting Submission 1 (Thu Apr 08 22:54:02 GMT 2021) -----
HST Phase I Proposal 1743 successfully submitted.
Receipt: # 1743-1
----- Attempting Submission 2 (Fri Apr 09 19:45:57 GMT 2021) -----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.
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.updated ETC numbers and acq time for visit 06! Sorry about that.
Okay, I have revised the target acquisiton for the non-extended targets with no bright objects nearby to use the NUV acq/image strategy - I switched to this method of acquisition because it is so much more
efficient and buys me a bunch more science spectroscopic exposure time.
Also, on Target 2, the 10 orbit target, 2 visits of 5 orbits each is the only way to get our required S/N (as opposed to 3, 3, 2, 2 (or something else with more visits). Hopefully this is schedulable, there did not seem to be
issues. This should be the final version, barring any concerns at review. Thank you!51091603----- Attempting Submission 1 (Wed Jul 28 00:40:57 GMT 2021) -----
HST Phase II Proposal 16679 successfully submitted.
Receipt: # 16679-1
----- Attempting Submission 2 (Fri Jul 30 03:24:13 GMT 2021) -----
HST Phase II Proposal 16679 successfully submitted.
Receipt: # 16679-2
----- Attempting Submission 3 (Fri Nov 05 00:13:43 GMT 2021) -----The errors and warnings have to do with the extended sources, which I cautiously labeled as extended.
Most appear as unresolved in GALEX images, but a couple are low-z AGN that do appear extended.
I have modified the target acquisition process for these 4 extended targets, in particular to require S/N = 100,
and a slightly different centering procedure. I would very much appreciate a review to make sure what I'm doing is sensible.
I believe I address the extended target issue in the proposal description text and elsewhere here.Mainly on the Plane: Solving the Milky Way CGM Anomaly with Low-Galactic-Latitude QSOsEither the Milky Way's ionized CGM is an outlier compared to the CGM of other L* galaxies, or our primary method used to measure its content - hundreds of QSO sightlines that pierce its halo - is fundamentally biased. The latter possibility cannot yet be convincingly ruled out because 95% of existing UV-bright QSO sightlines with archival high-resolution UV spectra lie at Galactic latitudes |b| > 25 degrees. We now have a unique opportunity to address this huge low-latitude gap in UV-bright QSO lines of sight with our proposed sample of newly discovered, rare QSOs at |b| < 25 degrees. We argue that a key requirement to determining the structure, mass, and dynamics of the CGM is understanding its distribution along the disk axis. For the first time, we will be able to use these novel Milky Way sightlines to test the latest hydrodynamical, cosmological simulations that suggest extended, ionized disk-like structures in galaxies may persist out to ~100 kpc. Our study, which will combine high-resolution HST/COS G160M spectra of these new low-|b| QSOs with > 100 high-quality archival G160M QSO spectra, is designed to address two primary questions: (1) With an unbiased view of the halo, is the Milky Way truly an anomaly? (2) Does the MWCGM show evidence for an extended, outer, ionized disk morphology, and if so, what are its properties? Finally, if we find evidence for an extended disk, it would represent one of the largest structures on the sky ever discovered, covering nearly half of the sky.We will observe 18 UV-bright (16.2 < NUV < 18.5) newly-discovered, low-Galactic-latitude QSOs with HST/COS G160M to look for the observational signatures of an extended, ionized gas disk in the Milky Way. Each target requires between 2 and 10 orbits, amounting to 71 orbits in total for the program.
S/N Requirements:
----------------------
Our primary science goal requires the measurement of absorption features from the doublets SiIV (1393, 1402) and CIV (1548, 1550), the highest ionization state transitions available with COS at z = 0. Our experiment requires us to measure both gas kinematics (absorption-line profiles as a function of velocity, e.g. Doppler b widths, velocity centroids) and gas column densities for high-velocity features. Our models and previous extragalactic results (e.g. COS-Halos) suggest we must probe column density limits of log NSiIV ~ 12.8 cm^-2, and log NCIV ~13.2 cm^-2 . A column density limit of log NCIV ~13.2 cm^-2 (the most constraining requirement) corresponds to being able to detect a 40 mA feature at 2sigma. To achieve these values, we require a minimum S/N of ~ 12 at the wavelengths of the CIV (1548, 1550) doublet in our COS G160M spectra. The S/N at the wavelengths of the SiIV doublet (1393, 1402) is > 15 under this requirement for the same QSOs, which allows us to detect features down to log NSiIV of ~ 12.8, consistent with our requirements.
Instrument Set-up:
------------------
In order to adequately model the absorption features and detect their component structure, we choose the highest spectral resolution of COS (G160M) with a central wavelength of 1577 A. In addition to detecting CIV and SiIV, other transitions we probe will be SiII (1526), FeII (1608, 1611), AlII (1670), and CI (1656). Saturation of the higher ionization state transitions should not be a problem at these Galactic coordinates; we expect the absorption to span a range of velocities 80 < |vLSR| < 250 due to the rotation of the Milky Way and its possible extended outer disk.
Exposure times:
------------------------
Our QSOs have NUV magnitudes of 16.2 - 18.4 and redshifts ranging from 0.03 - 0.7. Using the COS Spectroscopic ETC, we model the QSOs as COS-based QSOs, adding in the appropriate extinction for each sightline, and normalizing the spectra to the QSO's GALEX NUV AB magnitude (e.g. COS.sp.1488159, COS.sp.1488162). To achieve a minimum S/N of ~12 at 1550 Angstroms and at 1400, our targets require between 2 and 10 orbits each in G160M with a central wavelength of 1577 A. None of these QSOs will pose a bright limit threat to COS and we have no timing or orientation constraints.
Phase II Strategy:
-------------------------
We are using the G160M grating centered at 1577 Angstroms. We require only one CENWAVE setting for this experiment since we are targeting specific absorption lines that will not fall near the gap between segments nor will they fall in the regions of siginficant gain sag with this set up in LP4. Because we have coordinates that are accurate to within 0.4", generally from GALEX (with one from SDSS), we skip the ACQ/SEARCH step. For our faint, non-extended targets, we use a NUV ACQ/IMAGE target acquisition strategy which maximizes the science exposure times for these faint sources. To calculate acquisition exposure times using the ETC, we require a S/N of 20 in these NUV acquisition images, and model the QSOs as FOS-based QSOs to be sure our input spectrum covers the full instrument throughput band. For extended sources and/or sources that trigger the BOT, we acquire the targets with a PEAKXD exposure followed by a PEAKD exposure. Most of our targets are QSOs at z ~> 0.1, and are effectively point sources in the FUV. The exposure times for our point-source target acquisitions are set by requiring a S/N of 40 for both segments and both types of acquistions, respectively using the target's GALEX FUV magnitude (when available) or the NUV magnitude.
Four of our low-z QSO targets have z < 0.07, and appear as moderately extended galaxies in the target confirmation charts (but are still unresolved in GALEX images). For these sources, we have selected the "EXTENDED" target keyword and have modified the acquisition process slightly, increasing the NUM-POS to 5, decreasing the STEP-SIZE to 0.9, and centering using FLUX-WT-FLR. Additionally, we have increased the acquisiton exposure times to achieve a S/N of 100 for these extended sources (which also happen to be some of our brightest targets in the program). Because all of these extended sources are spectroscopically-confirmed, low-z AGN we still expect their FUV flux to be centrally concentrated in the unresolved galaxy bulges and for their extended structure to impact the program science goals (e.g. required spectral resolution) minimally.
We generally split our observations of each target into visits each of 3 orbits or fewer. One exception is for target 2, our faintest target, which requires 10 orbits and is split into 2 visits of 5 orbits each. We have added an additional justification to the 5-orbit visits for this target, explaining that our total exposure time required can only be achieved with this schedule to reduce the overheads and help us achieve our sensitivity requirements for this faint but scientifically critical target -- being able to carry out two 5-orbit visits buys us an additional 2000 seconds of on-source exposure time compared to other visit arrangements.
None of these QSOs will pose a bright limit threat to COS and we have no timing or orientation constraints. In general, the buffer times are quite long, and we thus set the buffer time in the exposure manually to be approximately 100 seconds shorter than the exposure time. We proceed by attempting to maximize exposure times while keeping to a minimum of four FP-POS settings per visit.
In our final set-up, we achieve S/N of between 11 - 15 across 1400 - 1550 Angstroms for all of our targets, which is in generally line with the requirements we outlined in the science case of Phase 1. For our faintest target (Target 2), the ETC indicates that we will reach only S/N of ~10.5 at CIV (even with the 4 orbit visits), which is somewhat lower than anticipated, but will be >12 at SiIV -- this target, at the lowest Galactic latitude, is one of our most crucial targets for our science case.Principal Investigator Dr. Jessica Werk has been using COS, the instrument selected for these proposed observations, since cycle 17, when it first came online. She is the PI on 3 previous successful HST proposals (two with HST/COS), is a first author on 5 papers that focus on results from COS data, and a co-author on 25+ publications that present results based on HST/COS data. She is primarily an observer (spectroscopist) who seeks to understand the intricate relationship between galaxies and their extended gaseous envelopes. In addition, she works closely with theorists to interpret observational data. Her experience reducing and analyzing COS absorption line spectroscopy, from both QSO and stellar sources, is extensive.
Dr. Joshua Peek is an expert in the study of the Milky Way circumgalactic medium and the construction and testing of dynamical models of disk-halo interfaces and circumgalactic media. Dr. Peek also has a background in data driven machine learning techniques and the manipulation of large catalogs for precision analysis.
Dr. Kirill Tchernyshyov is an expert in inferring column densities and physical properties from absorption spectra and building sophisticated statistical models for datasets in general and large ensembles of absorption spectra in particular.
Ms. Hannah Bish, a graduate student at the University of Washington, is a Co-I on two previous HST/COS programs in cycles 25 and 26. She is quickly developing expertise reducing and analyzing HST/COS spectra, including detailed Voigt profile fitting of absorption lines.
Dr. Mary Putman is a world expert in the Milky Way gaseous halo, high-velocity clouds, circumgalactic material, and galaxy formation.
Dr. Yong Zheng is an expert in COS data reduction and is intimately familiar with the details of the archival COS quasar spectra. Dr. Zheng also is an expert in comparing simulation data of gaseous structures to observed data.
Dr. David Schiminovich is an expert in ultraviolet observations, including GALEX and HST observations, reduction and analysis. He is also an expert in the study of the Galactic and extragalactic interstellar medium and extended gaseous disks and halos.Intergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSONOOne of our faintest targets. GALEX CAUSE, no FUV mag. Looks spot on in Target conf. chart.
SFD ebv = 0.14
acq ETC: COS.sa.1528282 (92 seconds)
img acq: COS.ta.1530544 (39 seconds)
spec ETC: COS.sp.1528281 (24000 seconds)J2000J2000NUV =18.32GALAXYQSOQUASARNOdouble checked GALEX. bad FUV coverage. NUV may be as faint as 18.53; ebv = 0.10
acq ETC: COS.sa.1528293 (140 sec)
img acq: COS.ta.1530545 (51 seconds)
spec ETC: COS.sp.1528289J2000J2000NUV=18.50GALAXYQSOYESFUV = 17.64, SFD ebv = 0.03.
low-z QSO, looks very compact, but selected extended out of caution.
acq ETC: COS.sa.1528310 (24 seconds)
spec ETC: COS.sp.1528308J2000J2000NUV=16.65GALAXYQSOYESdefinitely an extended galaxy. UV should be fairly compact, however.
FUV = 16.72
SFD ebv = 0.03
acq ETC: COS.sa.1528311 (10 seconds) --> adjusting for total extent! COS.sa.1529136 to 30 seconds.
spec ETC: COS.sp.1528316J2000J2000NUV = 16.47GALAXYQSOYESextended-ish, compact in UV GALEX image.
FUV = 18.07, SFD ebv = 0.09
acq ETC: COS.sa.1528318 (38 seconds) --> modifying for extended source COS.sa.1529139 to 112 seconds S/N of 100.
spec ETC: COS.sp.1528317J2000J2000NUV = 17.23GALAXYQSONOFUV = 17.83, SFD ebv = 0.05
acq ETC: COS.sa.1528322 (33 sec)
acq image ETC: COS.ta.1530551 (17 seconds)
spec ETC: COS.sp.1528321 (7900 sec)J2000J2000NUV = 17.42GALAXYQSONOFUV = 17.89, SFD ebv = 0.05
acq ETC: COS.sa.1528325 (28 seconds)
spec ETC: COS.sp.1528324 (13000 sec)
acq image:COS.ta.1530552 (25 sec)J2000J2000NUV=17.92GALAXYQSONOFUV = 18.31, SFD ebv = 0.05
acq ETC: COS.sa.1528327 (47 seconds)
spec ETC: COS.sp.1528326 (13000 sec)
img acq:COS.ta.1530553 (23 seconds)J2000J2000NUV = 17.62GALAXYQSONOchecked SDSS updated to accurate coords; SFD ebv = 0.06 GALEX FUV = 17.73.
acq ETC: COS.sa.1528069 --> 25 seconds
spec ETC:COS.sp.1528075-- > 7500 seconds (S/N 15 at 1400).J2000J2000NUV = 17.25GALAXYQSONODespite low redshift, there is zero evidence this is a spatially extended source.
FUV = 17.75, SFD ebv = 0.05
acq ETC: COS.sa.1528094 (36 seconds)
spec ETC: COS.sp.1528091 (11,000 sec)J2000J2000NUV = 17.68GALAXYQSONOFUV = 17.71, verified coordinates in GALEX. since z > 0.1, saying not extended. looks point source like in every image.
spec etc: COS.sp.1528101 (12000 sec) and COS.sp.1528103 (11500).
acq ETC: COS.sa.1528105 (27 seconds)J2000J2000NUV = 17.55GALAXYQSONOGALEX coords, point-source like. FUV = 17.47, SFD ebv = 0.15
acq ETC: COS.sa.1528117 (24 seconds)
spec ETC: COS.sp.1528112 (6400 sec) and COS.sp.1528114 (5700) for NUV and FUV.J2000J2000NUV = 17.29GALAXYQSONOno FUV observation (GALEX CAUSE). Used GALEX coords, reasonable upon double checking.
SFD ebv = 0.16. There are two other sources nearby in target conf. chart from Aladin, but neither shows up in GALEX image so I think it's fine.
acq ETC: COS.sa.1528126 (20 seconds)
spec ETC: COS.sp.1528143 (9800 seconds)J2000J2000NUV =17.44GALAXYQSOYESlow-z QSO, looks a little extended in GALEX image, but FUV light is very centrally concentrated. beautiful S-shape galaxy in target conf. chart from Aladin.
FUV = 18.03, SFD ebv = 0.16
acq ETC: COS.sa.1528154 (31 seconds) --> modified for S/N =100 for extended source out of caution: COS.sa.1529622 (91 seconds)
spec ETC: COS.sp.1528149 (11,250), S/N of 12 or so at 1550 in 4 orbits: COS.sp.1528153J2000J2000NUV = 17.55GALAXYQSONOchecked GALEX coords.
FUV = 16.53
SFD ebv = 0.12
acq ETC: COS.sa.1528157 (9 seconds)
spec ETC: COS.sp.1528158 (3400 seconds)J2000J2000NUV = 16.24GALAXYQSONOFUV = 17.46, SFD ebv = 0.08
acq ETC: COS.sa.1528161 (18 seconds)
spec ETC: COS.sp.1528160 (7950 seconds)J2000J2000NUV = 17.23GALAXYQSONOFUV = 16.68, SFD ebv = 0.09
acq ETC: COS.sa.1528193 (10 sec)
spec ETC: COS.sp.1528190 (5100 sec)J2000J2000NUV = 16.69GALAXYQSONOFUV = 17.75, SFD ebv = 0.10
acq ETC: COS.sa.1528234 (28 seconds)
spec ETC: COS.sp.1528236 (11000 seconds)J2000J2000NUV = 17.42COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.(Tic-Visit
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)true30The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.This is our faintest target, but also one of our lowest latitude QSOs and is thus crucial for this experiment. Our original calculations included 10 orbits for this target. To maximize the amount of on-source time, we gain approximately 2000 seconds by configuring the exposures into two visits of 5 orbits each. This allows us to meet our science goals in 10 orbits.(Tic-Visit
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)true20target does not appear extended, but considering low-z, have selected extended out of caution.The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.this is our most extended target, which even appears mildly extended in GALEX images. Adjusting acquisition process accordingly.1639832864000355.06226323055307(Tic-Visit
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This is HOPR repeat of visit 08.164809454000085.89999999999998(Tic-Visit
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This is HOPR repeat of visit 58.(Tic-Visit
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