0Assigned ID: 1985
----- Attempting Submission 1 (Fri Apr 09 15:53:33 GMT 2021) -----
HST Phase I Proposal 1985 successfully submitted.
Receipt: # 1985-1
----- Attempting Submission 2 (Fri Apr 09 19:34:46 GMT 2021) -----The number of orbits used exceeds the number allocated
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M.I added visit Z6 at the end, this is a repeat of visit 06, which failed due to a failure to reacquire guidestars. I filed a HOPR on 7/15 (HOPR 92274), and
received approval from the TTRB for a repeat. Please review and let me know if I need anything else! Thanks!-119727132----- Attempting Submission 1 (Sat Jul 24 20:31:50 GMT 2021) -----
HST Phase II Proposal 16650 successfully submitted.
Receipt: # 16650-1
----- Attempting Submission 2 (Thu Jul 29 23:19:32 GMT 2021) -----
----- Attempting Submission 3 (Tue Jul 19 18:13:06 GMT 2022) -----I did not think I needed to rerun all orbit and visit planners to submit this with the new Z6. Nothing changed except I have added visit Z6 which is a repeat of visit 06. I did run the orbit and visit planner on this one!Connecting Galaxy Black Hole Mass with the State of the Circumgalactic MediumThis proposal directly addresses a missing link in the story of galaxy formation: the physical connection between feedback from a galaxy's supermassive black hole and the kiloparsec-scale gas flows that comprise the circumgalactic medium (CGM). Now well-established, the relationship between the properties of the highly-ionized CGM and a galaxy's star formation history is one of the most surprising and informative results from the last decade of HST/COS observations. Similar to the black hole (BH) M-sigma relation, such a global relationship likely reflects multi-scale feedback processes. We have assembled a novel sample of eight nearby ~L* galaxies for which the SMBHs have dynamically resolved mass measurements, and which have nine FUV-bright background QSOs close on the sky ( Rproj < 130 kpc). The sample galaxies span a narrow range in stellar mass, but host SMBHs that vary in mass by nearly two orders of magnitude. COS spectroscopy of the background QSOs will establish the relationship between the cumulative feedback energy associated with long-term BH growth (as traced by the BH mass) and the content and kinematics of the gaseous halos around these systems. Specifically, we will measure CIV column densities and kinematics to test two predictions: (1) that galaxies with more massive BHs have more evacuated CGMs; and (2) that more massive BHs drive more extreme halo gas kinematics. The HST/COS/G160M observations we propose will be the first and only empirical test to constrain the existence of any such connection between long-term SMBH growth and the physical state of the surrounding halo gas.Description of Observations:
----------------------------------
We are targeting 9 FUV-bright QSOs (GALEX FUV < 19) within 130 kpc of 8 nearby, low-z (v < 700 km s^-1), isolated galaxies that have dynamically-resolved mass measurements for their central black holes. The sample galaxies span a narrow range in stellar mass, but host SMBHs that vary in mass by nearly two orders of magnitude. We checked the GALEX NUV magnitudes of our targets for large NUV - FUV colors, which would potentially indicate the presence of a strong Lyman Limit system (NHI > 10^17 cm^-2; LLS) along the line of sight that may contaminate our transitions of interest. One line of sight raised a potential red flag, but upon further examination of its SDSS spectrum and a very fortunate archival G140L spectrum, we determined this line of sight was free of such LLS contamination. All of the QSOs themselves have z < 1.
Our primary science goal is to examine a range of metal ion transitions out to 130 kpc in the CGM. CIV is the highest ionization state transition available at these low redshifts, and tracks the overall baryonic content of the gaseous halo well in the cosmological simulations. Based on predictions from the simulations, and previous observations we would ideally be able to detect CIV down to a column density limit of log NCIV = 13.3 cm^-2, which requires us to be able to detect a 40mA feature at 2 sigma. Thus, we require a S/N of 10 - 12 at the wavelengths of CIV in our COS spectra (1548, 1550).
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 Angstroms. In addition to detecting CIV (1548, 1550), other key transitions we probe will be SiII (1526), FeII (1608, 1611), AlII (1670), SiIV (1393, 1402), and CI (1656). The metal ion transitions will be separated from the MW features. The range of transitions and ionization potential energies (10 eV - 65 eV) probed by our observations will allow us to determine the ionization state of the gas using, e.g., CLOUDY.
Phase II Observing Strategy:
-----------------------
We are taking COS/FUV spectra of QSOs with GALEX FUV magnitudes that range from 18.2 - 19.0. 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 0.1", we skip the ACQ/SEARCH step, and acquire the targets with a NUV ACQ/IMAGE using MIRRORB to guard against QSO brightening. All of these objects are faint enough that this method of acquisition is safe. The Exposure times for these acquisitions are set by requiring a S/N of 20. For the acquisiton ETC, we modeled the QSOs as FOS-based QSOs which have broad spectral ranges that overlap entirely with the throughput of the detector.
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 FUV AB magnitude (e.g. COS.sp.1527029). Our targets each require between 4 and 8 orbits, and are generally split into 2-3 visits each of 3 orbits or fewer. One exception is for target 1, our faintest target, which requires 8 orbits and is split into 2 visits of 5 and 3 orbits. We have added an additional justification to visit 1 for this target, explaining that our total exposure time required can only be achieved in 2 visits rather than 3 separate visits, understanding that visits longer than 4 orbits can be challenging to schedule. 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 ~100 seconds shorter than the target's exposure time. We proceed by attempting to maximize exposure times and spread all four FP-POS over multiple visits when possible.
In our final set-up we achieve S/N of between 10-12 across our full wavelength range for all of our targets, which is in line with the requirements we outlined in the science case of Phase 1.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-GO proposals, 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.
Benjamin Oppenheimer is an expert in computational hydrodynamic simulations of galaxies and their gaseous environments, of the sort that will be instrumental in interpreting the proposed COS observations. He specializes in understanding how the physical and evolutionary parameters of the IGM/CGM can be quantified through observational campaigns. He is most expert at interpreting COS UV data, and at making testable predictions for observers to explore, such as those outlined in this proposal. He has been the principal investigator on 5 HST theory grants and a co-investigator on over a dozen HST general observing grants. He has published over ten papers as first author on the IGM/CGM, and has been a co-author on over 60 papers relating to his area of expertise.
Kate Rubin has expertise in galaxy slit and IFU spectroscopy at both UV and optical wavelengths with a focus on galaxy-scale winds and gas accretion. She specializes in gas kinematic measurements, which will be crucial for the science goals outlined in this proposal.
Misty Benz is an experienced HST observer, and an author on > 100 papers related to black-hole galaxy scaling relationships. Her expertise most relevant to this proposal is in direct galaxy black hole mass measurements.
J. Xavier Prochaska has used UV spectrographs since GHRS was active on HST. He has been a PI and Co-I on > 50 HST programs since cycle 13, and is an author on 383 peer-reviewed journal articles. Relevant to this proposal, he recently developed an MCMC-based python tool for analyzing CLOUDY models (to determine gas ionization state), and has a number of python tools he has developed and released publicly for QSO absorption analyses (e.g. the linetools package: www.github.com/linetools/linetools; the pyigm package: https://github.com/pyigm/pyigm ).
Joseph Burchett has expertise on nearby galaxies, and the environmental and halo mass-dependence of the CGM. In particular, his previous datasets tabulating CIV column densities in the halos of nearby galaxies will make up the bulk of our proposed control sample observations, instrumental for the proposed program.
Robert Crain and Jonathan Davies are experts in computational hydrodynamic simulations with a focus on the formation of galaxies and their dynamic co-evolution with their gaseous environments.They will be actively engaged in the theoretical interpretation of our proposed observations.Intergalactic Medium and the Circumgalactic MediumGalaxies6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALEX FUV = 18.99, z =0.635GALAXYQSONOThis object was generated by the targetselector and retrieved from the NED database.
NUV image/acq ETC: COS.ta.1530525 (44 seconds)J2000J2000GALEX FUV = 18.72, z = 0.295GALAXYQSONOThis object was generated by the targetselector and retrieved from the NED database.
acq/image ETC: COS.ta.1530528 (29 seconds)J2000J2000GALEX FUV = 18.82, z = 0.707GALAXYQSONOacq ETC: COS.ta.1530531 (28 seconds)J2000J2000GALEX FUV = 18.30, z = 0.111GALAXYQSONOThis object was generated by the targetselector and retrieved from the NED database.
acq ETC:COS.ta.1530532 (36 seconds)J2000J2000GALEX FUV = 18.62, z = 0.368GALAXYQSONOThis object was generated by the targetselector and retrieved from the SIMBAD database.
acq ETC: COS.ta.1530534 (21 seconds)J2000J2000GALEX FUV = 18.20, z =0.423GALAXYQSONOThis object was generated by the targetselector and retrieved from the NED database.
acq ETC: COS.ta.1530535 (45 seconds)J2000J2000GALEX FUV = 18.76, z = 0.315GALAXYQSONOacq ETC: COS.ta.1530536 (24 seconds)J2000J2000GALEX FUV = 18.46, z = 0.524GALAXYQSONOThis object was generated by the targetselector and retrieved from the NED database.
COS.ta.1530537 (32 seconds)J2000J2000GALEX FUV = 18.99, z = 0.945COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.trying NUV/ACQ/IMAGE instead of PEAKD and PEAKXD1652514418000115.2655395313543(Tic-Visit
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(Tic-Orbit
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:si-vis-utilization 2756
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
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)
(Tic-Orbit
:proposal-id 16650
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)
(Tic-Orbit
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)true30other FP-POS will be in subsequent 3 orbits.other FP-POS will be in subsequent 2 orbits.other FP-POS will be in subsequent 2 orbits.other FP-POS will be in subsequent 2 orbits.The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.1654686824000117.99379521871703(Tic-Visit
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:trans-version "20211222"
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:number-of-orbits 2
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:data-volume 400256
:tdrss-contact-duration 0
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)
(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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)true20other FP-POS will be in subsequent 3 orbits.other FP-POS will be in subsequent 2 orbits.other FP-POS will be in subsequent 2 orbits.other FP-POS will be in subsequent 2 orbits.This is a HOPR repeat for failed visit 22(Tic-Visit
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:trans-version "20211222"
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(Tic-Obset
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)
(Tic-Orbit
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(Tic-Orbit
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)false20other FP-POS will be in subsequent 3 orbits.other FP-POS will be in subsequent 2 orbits.other FP-POS will be in subsequent 2 orbits.other FP-POS will be in subsequent 2 orbits.The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode./private/var/folders/9y/97268rwx4k96s99djjzk9h2h0000gn/T/OPVisit17309249296623930993.xmlThis is a repeat of failed visit 6, as per HOPR 92274, approved for a repeat on 7/18/2022.(Tic-Visit
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:trans-version "20220516"
:date "19-Jul-2022 11:08:06.0"
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:si-bright-earth-limb-angle 20.0
:data-volume 382880
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
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:dark-offset NIL
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)
(Tic-Orbit
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:dark-offset NIL
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:low-sky "N"
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)true20other FP-POS will be in subsequent 3 orbits.other FP-POS will be in subsequent 2 orbits.other FP-POS will be in subsequent 2 orbits.other FP-POS will be in subsequent 2 orbits.