0
Assigned ID: 3194
----- Attempting Submission 1 (Fri Mar 25 11:59:36 GMT 2022) -----
HST Phase I Proposal 3194 successfully submitted.
Receipt: # 3194-1
----- Attempting Submission 2 (Fri Mar 25 18:05:31 GMT 2022) -----
HST Phase I Proposal 3194 successfully submitted.
Receipt: # 3194-2
----- Attempting Submission 3 (Fri Mar 25 23:31:57 GMT 2022) -----
HST Phase I Proposal 3194 successfully submitted.
Receipt: # 3194-3
----- Attempting Submission 4 (Fri Mar 25 23:55:42 GMT 2022) -----
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
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 generally required to use all four FP-POS positions when observing at a given COS cenwave.
We have added visit 29 which is a duplicate of the failed visit 24. Please note that this is the second time this visit failed.
We have examined the warnings given by APT, but most of them are either already addressed
(since we have already used the FP-POS recommendations from the COS 2025 policy), are not
relevant (since we wish to use specific FP-POS orderings), or that they are not directly
relevant for the planning of the observations (for extended targets).
On running the orbit planner, we get the message "Timeout waiting for orbit planner server." This problem was mentioned to STScI staff earlier (for another visit), and cannot be fixed by us.
We request the STScI staff to fix it.
Please let me (Varsha Kulkarni) know if I need to do anything else. Thank you for all your help.
1711959658
----- Attempting Submission 1 (Fri Jul 15 01:40:44 GMT 2022) -----
----- Attempting Submission 2 (Wed Aug 16 22:21:10 GMT 2023) -----
----- Attempting Submission 3 (Tue Mar 05 15:43:57 GMT 2024) -----
----- Attempting Submission 4 (Tue May 21 20:00:14 GMT 2024) -----
----- Attempting Submission 5 (Thu Dec 12 06:37:19 GMT 2024) -----
----- Attempting Submission 6 (Wed Dec 18 17:47:08 GMT 2024) -----
----- Attempting Submission 7 (Wed Jan 08 14:55:48 GMT 2025) -----
We have examined the warnings given by APT, but most of them are either already addressed
(since we have already used the FP-POS recommendations from the COS 2025 policy), are not
relevant (since we wish to use specific FP-POS orderings), or that they are not directly
relevant for the planning of the observations (for extended targets). We had previously checked
with the PC about these warnings.
On running the orbit planner, we get the message "Timeout waiting for orbit planner server." This problem was mentioned to STScI staff earlier (for another visit), and cannot be fixed by us.
We request the STScI staff to fix it.
The only change being made now is the addition of visit 29 to duplicate the failed visit 24.
Probing the Gas in and around Local Galaxies Mapped with Integral Field Spectroscopy
An important question in understanding galaxy evolution is how the gas in the galactic disk, bulge and halo couples with the circumgalactic medium (CGM). Here we propose to study the multi-phase gas in and around 18 local galaxies (z<0.1) whose inner regions have been mapped in exquisite detail with integral field spectroscopy (IFS). To probe the warm and cool gas, we propose COS UV spectroscopy of background AGNs whose sight lines pass through the halos of the targeted galaxies. Our observations will allow us to combine the wealth of detailed maps already available for these galaxies from MaNGA with the physical diagnostics (e.g., metallicity, ionization, kinematics) of the multiphase gas that can be inferred robustly only from UV absorption-line spectroscopy. Our goals are to (1) measure element abundances in the cool gas from absorption lines and compare to ionized gas metallicity from MaNGA; (2) measure the composition of the warm, ionized gas and examine whether its velocity is sufficient to escape the galaxy; (3) determine whether gas metallicity and galaxy-absorber azimuthal angle are correlated (e.g. whether lower metallicity is seen along the major axis); (4) compare the cool gas kinematics with ionized gas kinematics, e.g. does the cool gas lag behind the galaxy's mid plane as the ionized gas does. Our study will shed light on how the inner and outer regions of galaxies interact; e.g., how gas, metals, and angular momentum are exchanged between different regions. Our program will greatly enhance the power of the MaNGA data for studies of galaxy formation and evolution. HST is essential because of the need for UV spectroscopy.
We will use the COS G130M 1222 and/or 1291 settings to cover the absorption lines of interest. All of the targets are background quasars or AGNs probing foreground galaxies. Thus the targets of interest are point sources in most cases. (In one case, the galaxy whose AGN is to be observed is listed as an extended source, but even in this case, we are only interested in the AGN point source which is the brightest part of the galaxy, and this AGN needs to be centered in the aperture.)
The ICRS coordinate uncertainties (adopted from Simbad) are < 0.1". Therefore target acquisitions are requested using the ACQ/IMAGE mode. The NUV/MIRRORB is assumed, to be safe, for all targets. Target acquisition calculations are performed assuming point source targets for s/n=20 to 40 (generally 25 or 30).
As per COS 2025 policies, FP-POS=1,2,3,4 are used for G130M/1222 and FP-POS=3,4 are used for G130M/1291.
PI Varsha Kulkarni: Dr. Kulkarni is an expert in the fields of the circumgalactic medium (CGM) and quasar absorption-line spectroscopy. She received her PhD at the Univ. of Chicago, and was a postdoc with the NICMOS science team at the Univ. of Arizona. She is now a Professor at the Univ. of South Carolina. She has successfully led and completed several HST programs related to the CGM and quasar absorption systems. She and her collaborators have published several papers making use of these HST programs that used STIS, COS, NICMOS, WFC3 (6 papers in the past 3 years). Dr. Kulkarni will lead the overall project, including the analysis and interpretation of the proposed COS data.
Co-I David Wake: Dr. Wake is an expert in galaxy structure and evolution studies. He is a member of the MaNGA team and has played a key role in MaNGA as the Sample Design Lead. He will assist in comparing the proposed HST data with the MaNGA data and the implications for galaxy evolution studies.
Co-I Arjun Karki: Mr. Karki is a graduate student working with Dr. Kulkarni at the Univ. of South Carolina. He is experienced in analyzing quasar spectra. He played a key role in constructing our proposed HST sample. He will assist with the phase 2 planning and with analysis of the proposed data.
Co-I Britt Lundgren: Dr. Lundgren is an expert in studies of the CGM and quasar absorption-line spectroscopy. She will assist in interpretation of the proposed CGM observations and comparisons of the results with other CGM studies.
Co-I Celine Peroux: Dr. Peroux is an expert in studies of the CGM and integral field spectroscopy. She has led several projects to detect the CGM around distant galaxies using integral field spectrographs on the VLT. She will assist in the interpretation of the proposed observations and in connecting the CGM data to the integral field spectroscopy data already available from MaNGA.
Co-I Matthew Bershady: Dr. Bershady is an expert in galaxy structure and evolution as well as spectroscopic instrumentation. He is a member of the MaNGA team and the SDSS IV Project Scientist. He will assist in comparing the proposed HST data with the MaNGA data and the implications for galaxy evolution studies.
Galaxies
Intergalactic Medium and the Circumgalactic Medium
6
false
false
true
false
false
false
false
false
SUPPORTED
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QSO
NO
J2000
J2000
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GALAXY
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2MASSJ09570217+1737129
J2000
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GALAXY
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GALAXY
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GALAXY
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SEYFERT
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GALAXY
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J2000
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GALAXY
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No
G130M
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COS/FUV
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No
G130M
1222
COS/FUV
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No
No
G130M
1222
COS/FUV
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No
No
G130M
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