Submission v2 updated J. Stern email.-1413742439Assigned ID: 764
----- Attempting Submission 1 (Fri Apr 05 21:06:39 GMT 2019) -----
HST Phase I Proposal 764 (UV_outflow_COS.apt) successfully submitted.
Receipt: # 764-1
----- Attempting Submission 2 (Fri Apr 05 23:13:59 GMT 2019) -----
HST Phase I Proposal 764 (UV_outflow_COS.apt) successfully submitted.
Receipt: # 764-2INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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.
ORBITAL VISIBILITY OVERRUN
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
ORBITAL VISIBILITY OVERRUN
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.
INEFFICIENT ORDERING OF FP-POS POSITIONS
ORBITAL VISIBILITY OVERRUN
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.
ORBITAL VISIBILITY OVERRUN
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.
ORBITAL VISIBILITY OVERRUN
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.
ORBITAL VISIBILITY OVERRUN
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.
ORBITAL VISIBILITY OVERRUN
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.
INEFFICIENT ORDERING OF FP-POS POSITIONS
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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.
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.New ORIENT requirement on visit 60 which is a repeat of a failed visit.-487167815----- Attempting Submission 1 (Wed Jul 24 00:12:22 GMT 2019) -----
HST Phase II Proposal 15935 (UV_outflow_COS.apt) successfully submitted.
Receipt: # 15935-1
----- Attempting Submission 2 (Thu Jul 25 16:10:29 GMT 2019) -----
----- Attempting Submission 3 (Fri Aug 16 16:13:16 GMT 2019) -----
----- Attempting Submission 4 (Fri Oct 18 18:20:57 GMT 2019) -----
----- Attempting Submission 5 (Fri Nov 01 18:42:30 GMT 2019) -----
----- Attempting Submission 6 (Tue Nov 19 01:34:38 GMT 2019) -----
HST Phase II Proposal 15935 (UV_outflow_COS_same_orient_noshadow_bufferfixed.apt) successfully submitted.
Receipt: # 15935-6
----- Attempting Submission 7 (Tue Nov 19 15:20:12 GMT 2019) -----
----- Attempting Submission 8 (Thu Jul 16 19:58:40 GMT 2020) -----The warnings for inefficient change of FP-POS are due to exposures that are due to either (1) end of a sequence taken in shadow or (2) switch of target during an orbit. These cannot be avoided due to requirement of observations in shadow for certain targets/lines and because the nuclear exposure times do not always fill an orbit as the expected fluxes are brighter than the off-nuclear pointings.
We recieved three bright object warnings, all of which are associated with objects that do not have significant NUV. :
N8WX004264 at 08:33:14.9, +10:00:58.98. This is a star with an effective temperature of 5300 K. The warning is due to the erroneus assumption that it is an O-star which is ruled out by GAIA data.
N8WX004266 at 08:33:15.3, +10:01:04.08. This is a quiescent galaxy with no AGN activity and u=20.92. The warning is due to an erroneus assumption that it is an O-star
S6D0005306 at 12:22:17.8, -00:07:43.42. This is an obscured quasar with fuv=20.4, nuv=19.8 in GALEX and is one of our science targets. The warning is due to an erroneus assumption that it is an O-star.UV diagnostics as barometers for galactic scale AGN outflowsGalaxy evolution models require feedback from AGN to suppress star-formation in massive galaxies. However, the mechanisms that enable central black holes to couple to galactic scale ISM are widely debated with proposed mechanisms ranging from radiation pressure on dust to ISM entrainment in hot, shocked winds. Observations that enable measurements of the presence and properties of the hot wind component therefore represent a critical test of AGN feedback physics. Sensitive and spatially resolved UV diagnostics from highly ionized emission lines not only differentiate between AGN photoionized gas and shocks, but can also serve as barometers that enable estimates of the pressure of any ambient hot wind. In particular, highly ionized emission line ratios depend strongly on the ratio of the ambient hot gas pressure to radiation pressure from the AGN, and hence can determine which of these processes dominates the outflow dynamics. GO-15280 performed a pilot study with the first spatially resolved UV spectroscopy of a prototypical galactic scale AGN-driven. The observed OVI, NV, and CIV ratios are consistent with predictions from AGN photoionized clouds compressed by radiation pressure and rule out the presence of a dynamically important hot wind component ~10 kpc from the nucleus, providing a strong constraint on feedback models. Building on this success, we propose to perform spatially resolved UV spectroscopy for a representative sample of 7 galactic scale AGN outflows. These observations will enable unique insights into the presence of an unseen hot wind; the physical conditions of the cool, galactic-scale outflows; and accurate estimates of mass/momentum outflow rates.We will acquire spatially resolved and sensitive UV diagnostics (OVI, NV, CIV, SiIV, and HeII) with HST+COS of known, low-z galactic-scale AGN-driven winds to distinguish AGN feedback mechanisms by searching for signatures of pressure from a hot confining wind. These observations will also allow us to distinguish gas ionized by AGN photoionization from shocks and go beyond order-of-magnitude estimates of the ionized outflow rate by constraining unresolved density structure through ionization modeling.
Choice of COS and gratings:
The OVI, NV, CIV, SiIV, and HeII emission lines can be observed at low redshift with a combination of the FUV and NUV channels on STIS or COS. While the significantly higher spatial resolution of STIS would be useful for the proposed analysis, the lower throughput and significantly higher dark current per arcsec^2 make observations with STIS prohibitively expensive. We will carry out the observations with the COS NUV and FUV channels. Because the gas kinematics have already been measured based on optical data and the emission lines from different ions are well separated by hundreds of Angstroms (we do not require measurements of doublet ratios), the low-resolution data are sufficient for our purposes. The COS/FUV+G140L and COS/NUV+G230L setups are therefore ideal because of their broad wavelength coverage. Coverage of the desired wavelength range is possible with just G140L for most of the targets, but the somewhat higher redshifts of J0833+1005 (z=0.2547) and J1010+1413 (z=0.1987) require observations with G230L for CIV and HeII.
Two objects (J1222-0007 and J1255-0339) are at z=0.17 which places the OVI emission line close to geocoronal HI lya emission though not close enough for the Milky Way ISM damping wing to significantly effect the emission levels. With the low resolution grating, the geocoronal HI lya will significantly contaminate the OVI emission. We will therefore also observe these two systems with the higher resolution G130M grating which will cleanly separate the OVI emission from geocoronal contamination.
Finally, we note that for J0833+1000, the OVI emission line falls close to the geocoronal O I emission line at approx 1300 Angstroms. To minimize contamination, we therefore request G140L observations of the target when the spacecraft is in shadow which reduces the O I emission to negligible levels. The remaining portions of the orbit outside of shadow will be used for the other emission lines.
In order to search for signatures of hot gas pressure in optically identified, spatially resolved outflows, we require both a COS pointing at the location of the outflow and also a nuclear pointing. In order to determine whether radiation pressure or hot gas pressure dominate the dynamics of the emitting clouds, we require sufficient S/N to measure line ratios to within 0.05-0.1 dex requiring a S/N of approx 20-30 in OVI and CIV and S/N of approx 15 in NV.
To estimate exposure times, we measured the [O III] surface brightness based on existing measurements from spatially resolved ground-based spectroscopy (Greene et al. 2011, Sun et al. 2017, Jarvis et al., 2019). We then converted these to expected surface brightness in OVI, NV, CIV, and HeII lambda 1637 based on the observed line ratios of J1356+1026 observed in a Cycle 25 pilot program. Finally, we computed estimated flux levels accounting for the effective area of the COS primary science aperture (PSA). The total flux levels in the aperture expected in these emission lines for outflow pointings range from 5e-16 to 5e-15 (cgs) for the weakest line (NV) and 1e-16 to 1e-14 (cgs) for the strongest lines. Based on [OIII] measurements in the nuclear SDSS spectra, the expected flux levels in the nuclear COS pointings will be 2-10x higher. Based on the ETC, we therefore require total exposure times of 2400-4500 sec in G140L and G230L for the off-nuclear outflow pointings. Because the observations are not dark limited, the observing time in G130M for objects that require the additional grating setup are similar. Integration times for the nuclear pointings are significantly shorter and range from 400-2400 sec. For each grating setup, we will acquire exposures in 4 FP-POS settings to mitigate the impact of the grid-wire pattern on emission line profiles.
The targets are unresolved and some exhibit complex morphologies in archival HST images. Whenever possible, we will therefore perform an acquisition using a nearby star with coordinates precisely measured by GAIA. Because the coordinates are known to better than 0.01", we will acquire with a ACQ/IMAGE sequence in the NUV and then offset the telescope to place the nuclear or off-nuclear pointings in the primary science aperture. For one target, J1222-0007, the morphology is sufficiently simple that a direct acquisition on the nucleus is possible.
Impact of 1 Gyro mode: This program will not be significantly impacted by 1 gyro mode which would result in slightly higher overhead for acquisition (+2 minutes) and offset from the reference star to the target (+1 minute).Our team consists of numerous leading observers, theorists, and simulators who are experts in multi-wavelength constraints and models for AGN feedback that incorporate HST data. Collectively, we have published over 100 articles on observations and theory of AGN outflows and have a strong record of combining HST data with models for new insights into galaxy and black hole evolution.
PI S. Johnson has extensive experience with HST+COS both in archival analysis and as PI of the pilot for the current proposal. While the pilot program (GO-15280) is only partially completed with the majority of orbits still in scheduling, the data already place strong constraints on the presence of any hot wind component as discussed in the proposal.
co-PI J. Stern is a theorist with extensive background AGN outflows and a strong history of close collaboration with observers to discriminate between proposed AGN feedback mechanisms. J. Stern's modelling demonstrated that UV line ratios provide unique constraints on the physics of galactic scale AGN outflows (see Stern et al., 2016).
co-I's K. Alatalo, H.-W. Chen, A. Goulding, J. Greene, J. Mulchaey, K. Nyland, K. Rowlands, G. Rudie, M. Strauss, G. Walth, D. Wylezalek, and N. Zakamska are leading observers with collective experience studying AGN and galaxy evolution from the X-ray to radio. Their expertise will enable us to maximize the use of the proposed HST observations by combining constraints with those from existing multi-wavelength datasets. Moreover, with specialization ranging from black holes to the diffuse circum-galactic gas their perspective will provide broad context for interpreting the proposed observations in light of other observations of galaxy evolution generally.
Through PI S. Johnson and co-I's G. Rudie and J. Mulchaey we have guaranteed access to the Magellan Telescopes which will be used to acquire deeper, spatially resolved optical spectroscopy to cover a wide range of diagnostic emission lines. These data will complement the proposed HST observations to enable measurements of dust content in the outflow as described in the proposal.
co-I's E. Choi, M. Gaspari, C.-A. Faucher-Giguere, A. Laor, and E. Schneider are experts in modeling and simulations of galactic scale outflows. Their input will enable us to draw invaluable conclusions from the proposed data by combining it with predictions from both analytic models and a wide variety of hydrodynamic simulations.Massive Black Holes And Their Host GalaxiesGalaxies and the IGM6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARG V-IVNOJ0833+1005 offset star. Coordinates and mags from GAIA. Teff=5300 K.J2000u=17.16GALAXYNLRQUASARWINDYESnucleus to observe in G140L and G230L for 1 orbit eachJ2000J2000GALAXYNLRQUASARWINDYESJ2000J2000STARF0-F2NOJ0841+0101 offset star. Coordinates and mags from GAIA. Teff=7100 K F2 star.J2000nuv=17.75GALAXYNLRQUASARWINDYESV-band magnitude is uncertain as this is a line-emitting sourceJ2000J2000GALAXYNLRWINDYESJ2000J2000STARF3-F9NOJ1000+1242 offset star with coordinates from GAIA. Teff=6300 K. F-star.J2000nuv=20.40GALAXYNLRQUASARSEYFERTYESJ2000J2000GALAXYNLRWINDYESJ2000J2000STARG V-IVNOJ1010+1413 offset star coordinates from GAIA. Teff=5500 G-star.J2000nuv=20.83GALAXYNLRQUASARWINDYESJ2000J2000GALAXYNLRWINDYESJ2000J2000GALAXYNLRQUASARWINDYESJ2000J2000GALAXYNLRWINDYESJ2000J2000STARG III-INOJ1255-0339 offset star with GAIA coordinates. Teff=5900. G-starJ2000nuv=19.18GALAXYNLRQUASARWINDYESJ2000J2000GALAXYNLRWINDYESJ2000J2000COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3000COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3000COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG130M1291COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3000The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode./Users/seanjohnson/Dropbox/documents/proposals/HST/Cycle27/UV_outflow/APT/OP-cache/UV_outflow_COS_HOPR-v01.xmlJ0833+1005 nuclear and off-nuclera pointings for G140L. Requires shadow to measure OVI which falls near the geocoronal OI line at the object redshift. Non-shadow portions of orbit are filled with G140L to increase S/N in other lines.1585610470000106.33999999999997(Tic-Visit
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