For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.0Assigned ID: 5092
----- Attempting Submission 1 (Sat Mar 23 18:43:15 GMT 2024) -----
HST Phase I Proposal 5092 successfully submitted.
Receipt: # 5092-1
----- Attempting Submission 2 (Tue Mar 26 14:19:20 GMT 2024) -----
HST Phase I Proposal 5092 successfully submitted.
Receipt: # 5092-2
----- Attempting Submission 3 (Tue Mar 26 14:35:37 GMT 2024) -----Our requested exposure times and orbits have factored in the extra 4 minutes overheads per exposure for G160M at LP6.I updated G160M setup with 1589 CENWAVE and FP-POS=1,2,3,4, the following comments still apply (Sept 19, 2024). None of the QSOs have direct V band magnitudes. For the first target, 2MASS-J07380702+2127295, I was able to estimate the V mag based on SDSS ugriz measurements listed on Simbad, which is V=16.4 mag. Given the similarity of all the targets (QSOs) and their FUV magnitudes, my best guess is that their V band mag are around the same.1938234099----- Attempting Submission 1 (Tue Jul 30 18:05:40 GMT 2024) -----
HST Phase II Proposal 17733 successfully submitted.
Receipt: # 17733-1
----- Attempting Submission 2 (Tue Jul 30 18:11:19 GMT 2024) -----
----- Attempting Submission 3 (Thu Sep 19 20:22:10 GMT 2024) -----None of the QSOs have direct V band magnitudes. For the first target, 2MASS-J07380702+2127295, I was able to estimate the V mag based on SDSS ugriz measurements listed on Simbad, which is V=16.4 mag. Given the similarity of all the targets (QSOs) and their FUV magnitudes, my best guess is that their V band mag are around the same.When Clouds Collide: Observing Gas Accretion onto the Milky Way's DiskDespite it being the reference L* galaxy for extragalactic studies, our Milky Way (MW) seems to host a circumgalactic medium (CGM) with far less ionized gas content than their low-redshift counterparts. This program is designed to investigate the MW's CGM anomaly by examining whether there are large streams of ionized gas being accreted onto the MW's disk in a co-planner manner at low Galactic latitudes, which may elude previous studies that were limited to QSOs at high-latitude regions. We will observe 4 new QSO sightlines toward the anti-Galactic center direction, where a large population of infalling HI clouds are present. We will quantify the physical properties of the ionized gas associated with the infalling HI clouds, including ionization states, ion ratios, metallicity, neutral and ionized masses, and infalling time scales and mass rates. Detections of high ion column densities in our proposed observations will confirm that there are indeed large streams of ionized gas flowing from the MW's CGM to the disk, resolving the debate surrounding the MW's CGM anomaly. Null detection of ionized gas would also be extremely informative: it would indicate that the MW's CGM is truly different from those of other L* galaxies, with insufficient amounts of ionized gas in all directions.We will observe the QSOs using both G130M and G160M gratings to cover a wide range of UV ions, such as SiII, SII, AlII, CII, and CIV. The observations are split into 2-3 orbits per visit.
Observation setup strategy:
- Gratings and CENWAVE: we will use both G130M and G160M gratings for our observations. For G130M, we will use CENWAVE=1291 (SEGMENT=BOTH, FP-POS=3,4) to cover our targeted ion lines. For G160M, we will use CENWAVE=1589 and FP-POS=1,2,3,4.
- Target acquisition: our targets have coordiante uncertainties within 0.03-0.05 arcsec based on SIMBAD (except QSO 2: UVQS-J070919.25+254923.4 which has no reported uncertainties and we assume an uncertainty of 0.05 arcsec). All targets are at z>0.1 and appear to be point sources in 2MASS images, so we conduct target acquisition using ACQ/IMAGE in NUV, with sufficient exposure times to reach S/N=20 using an FOS-based template spectrum.
- Science exposure: for exposure time, we modeled the QSOs with COS-based QSO input spectra, adding in the appropriate extinction, and normalizing the spectra to each QSO's GALEX FUV AB magnitude. We aim to achieve a signal-to-noise ratio S/N=12 at 1300 A for G130M and 1550 A for G160M. The observations will be conducted in TIME-TAG mode. The Buffer Fill Time from COS ETC is generally long (a few thousands seccond), and we set the Buffer Time to equal to the exposure time following the flow chart in Figure 5.12 in COS instrument handbook.The PI, Dr. Yong Zheng, is an expert in the circumgalactic medium of the Milky Way and nearby galaxies. Dr. Zheng is experienced in COS data reduction and HI 21cm data reduction, and has worked closely with simulation data to conduct synthetic observations.
Dr. Jessica Werk is an expert in COS observations, data reduction, spectral analysis, and inferring column densities and physical properties from COS and other spectroscopic absorption line data. Dr. Werk is also experienced in conducting Cloudy modelings.
Dr. Hannah Bish is an expert in studying the Milky Way's CGM and has successfully led a recent HST large program -- QuaStar -- that investigated the distribution of CIV in the Milky Way's CGM through close pairs of QSO-star sightlines.Intergalactic Medium and the Circumgalactic Medium6falsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000FUV=17.38GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
No coordinate uncertainties in RA or DEC from SIMBAD. So we assumed an uncertaity of 0.05 arcsec in both RA and DEC, which is based on the coordinate uncertainties of other targets on our list.J2000J2000FUV=17.30GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000FUV=17.56GALAXYQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=17.42COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1611Observation for 2MASS-J07380702+21272951760808409000279.50384572033244(Tic-Visit
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:internal-dur-at-end 426
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3010
:pcs-gap 0
)true20/System/Volumes/Data/solaris/user1/williamj/hst/work/cycle32/OP-cache/17733-v15.xmlThe scheduling data was generated by CASM 33.1.CASM was run in Phase II mode.Observation for Q4: VV2000-J042630.1+070530
HOPR repeat of visit 12.(Tic-Visit
:proposal-id 17733
:visit-id "15"
:proposal-version -1
:trans-version "20250929"
:date "10-Dec-2025 06:32:03.0"
:trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 174016
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17733
:visit-id "15"
:obset-id "15"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17733
:visit-id "15"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2629
:al-overhead-at-end 0
:internal-dur-at-end 114
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2977
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 17733
:visit-id "15"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2630
:al-overhead-at-end 0
:internal-dur-at-end 424
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2977
:pcs-gap 0
)true22Observation for Q4: VV2000-J042630.1+0705301761476185000289.0100525741645(Tic-Visit
:proposal-id 17733
:visit-id "13"
:proposal-version -1
:trans-version "20240604"
:date "19-Sep-2024 16:06:24.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 304704
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17733
:visit-id "13"
:obset-id "13"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17733
:visit-id "13"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2630
:al-overhead-at-end 0
:internal-dur-at-end 2295
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3010
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 17733
:visit-id "13"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2630
:al-overhead-at-end 0
:internal-dur-at-end 2295
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3010
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 17733
:visit-id "13"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2630
:al-overhead-at-end 0
:internal-dur-at-end 546
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3010
:pcs-gap 0
)true30Observation for Q4: VV2000-J042630.1+0705301758472577000249.31884038697262(Tic-Visit
:proposal-id 17733
:visit-id "14"
:proposal-version -1
:trans-version "20240604"
:date "19-Sep-2024 16:06:46.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 208960
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17733
:visit-id "14"
:obset-id "14"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17733
:visit-id "14"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2630
:al-overhead-at-end 0
:internal-dur-at-end 2295
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3010
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 17733
:visit-id "14"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2630
:al-overhead-at-end 0
:internal-dur-at-end 546
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3010
:pcs-gap 0
)true20/System/Volumes/Data/solaris/user1/williamj/hst/work/cycle32/OP-cache/17733-v16.xmlThe scheduling data was generated by CASM 33.1.CASM was run in Phase II mode.Observation for Q4: VV2000-J042630.1+070530
HOPR repeat of visit 14.(Tic-Visit
:proposal-id 17733
:visit-id "16"
:proposal-version -1
:trans-version "20250929"
:date "10-Dec-2025 06:32:03.0"
:trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 208960
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17733
:visit-id "16"
:obset-id "16"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17733
:visit-id "16"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2629
:al-overhead-at-end 0
:internal-dur-at-end 2261
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2977
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 17733
:visit-id "16"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2630
:al-overhead-at-end 0
:internal-dur-at-end 544
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2977
:pcs-gap 0
)true22