A Breakaway from Incremental Science: Full Characterization of the z<1 CGM and Testing Galaxy Evolution Theory
In the modern theory of galaxy evolution, the circumgalactic medium (CGM), the massive, metal-enriched, extended gaseous reservoir surrounding galaxies, is the environment through which the large-scale physics of galaxy formation and evolution is controlled and regulated. Testing/confronting galaxy evolution theory requires observations characterizing the CGM kinematics, geometric distribution, metallicities, and gas phases. Expensive resources have been dedicated for z~0.1 (look-back 0-2 Gyr) and for z~2.5 (10-11 Gyr), but the epoch 0.3<z<1.0 (2-8 Gyr) has been relegated to an incremental approach hampering breakaway progress in understanding and constraining galaxy evolution theory; this extended cosmic epoch ties together and therefore increases the value of the extensive z~0.1 and z~2.5 campaigns. To perform breakaway science, we must quantify the "meteorological character'' of the CGM, not simply chart the "atmospheric conditions'' surrounding a few galaxies, and obtain the data required to directly confront theoretical predictions.
We propose COS NUV+FUV high-resolution quasar spectra to uniformily measure OVI, CIV, and HI (and many other low and high ionization metals, including NeVII and OIV) in the CGM of 39 z=0.08-0.97 spectroscopically measured galaxies with HST images. We will augment these 39 galaxies with 12 additional galaxies from our previous programs, for a total of 51 galaxies. Our analysis directly addresses and tests the current theoretical paradigm of galaxy evolution. Our program promises a Legacy for HST, providing the essential data for ground-based follow up and for testing galaxy evolution as theory/simulations progress in coming decades.
We propose to obtain COS high-resolution spectra of 10 quasars to probe the CGM of 39 galaxies (0.08 < z < 0.97) [to which we add 12 existing COS galaxies/absorbers]. We used the online COS ETC to estimate the required exposure time to achieve signal-to-noise ratios S/N greater than 10 (as an absolute minimum) with a target minimum of 15 so prohibitively long exposure times are not required. We assume a point source with an established flux value at the observed wavelengths of the target transitions. UV fluxes for all targets were obtained from FOS G190H and G160L spectra, and/or GALEX NUV and FUV images. For all targets we have measured flux values, except for the targeted 1400-1600 A for Q0122-003. There are no potential Lyman breaks below 1600 A; we are confident that the flux in this region is equal to that above 1600 A. None of the targets exceed the bright object limits.
For the exposure time estimates, we employed average Galactic extinction, standard zodiacal light normalizations, standard earth shine light normalizations, and average air glow. The estimated visibility for our targets is 50 minutes.
Justifying Signal-to-Noise: Our analysis is predicated on detailed kinematic and ionization modeling. For COS resolution and pixelization, S/N = 15 per resolution element yields a 5-sigma detection limit of 15 mA.
Target acquisition: We have obtained coordinates by converting the GS1 coordinates to GS2 (ICRS system) using the tool provided by STScI. We then used the Target Confirmation chart from APT to adjust the positions in order to center as accurately as possible. We use these coordinates as a starting point for dispersed light acquisition using either of the FUV gratings. For 9 of the 10 quasars we choose to use ACQ/SEARCH with a 2x2 search pattern, followed by ACQ/PEAKXD and ACQ/PEAKD with 5 positions. The S/N needed for the SEARCH and PEAKD exposures is 40, and we use the APT to calculate the needed exposure time (using the measured flux in the grating. We use the grating setting corresponding to the first observations in the orbit unless the exposures are all in the near-UV. If they are in the near-UV, we use G130M if we have verified there is flux at those wavelengths, and G160M otherwise.
The choice to use a dispersed light acquisition was made because our analysis of archival HST data suggests that programs using dispersed light instead of imaging have a more accurate and consistent wavelength solution. This is important for our program. We also based this decision upon section 8.8 of the COS Instrument Handbook. Although we believe our coordinates are accurate enough that a ACQ/SEARCH should not be necessary, we are doing one as a precaution. The one exception to this is for Q0454-220 for which we have proposed only a one orbit exposure, and which has been observed before many times with COS.
Visits were set up with the following ideas in mind:
1) If there is only one orbit devoted to a particular grating tilt then we use two FP-POS positions, 3 and 4 because it is difficult to fit all four exposures in one orbit. FP-POS =3 is favored because of shorter overheads.
2) For 2-5 orbit observations we use all four FP-POS positions, splitting them roughly equally. For two orbit observations we do FP-POS=1 and 2 in one orbit and 3 and 4 in the other. For three orbit observations we split observations between orbits to equalize time. For four orbit observations we use one FP-POS per orbit. For five orbits observations we have a couple of strategies. Sometimes we favor FP-POS=3 since it is the central one coinciding with our specified wavelength ranges for the systems of interest. We also usually begin with FP-POS=3 in G160M and NUV exposures since this default position gains us 70s in exposure time in the first orbit of the visit. In a couple of cases we choose another tilt for the fifth orbit in order to cover a gap region at least with some S/N.
3) Some of our visits include both some FUV and some NUV observations in order to calibrate wavelength scales, since generally the wavelength solution is more consistent between observations in the same visit.
4) Buffer time is set to about 90% of the exposure time for exposures ending during an orbit, to minimize the impact of readout time on the total exposure time. For exposures ending with the orbit we set the buffer time at or a couple seconds higher than the exposure time.
QUASAR ABSORPTION LINES AND IGM
0
false
false
false
false
false
SUPPORTED
GALAXY
QSO
FOS G160M and G230M provided
J2000
J2000
f_lam=3-5E-15 from 1600-3300A; GALEX FUV=18.86 NUV=17.58
GALAXY
QSO
G160M and G230M provided
J2000
J2000
f_lam=2E-14 from 1600-2300A ; GALEX FUV=17.04 NUV=16.18
GALAXY
QSO
FOS G130M, G190M, G270M provided
J2000
J2000
f_lam=1-2E-14 from 1350-2300A; GALEX FUV=16.39 NUV=15.74
GALAXY
QSO
FOS G190H and G270H provided
J2000
J2000
f_lam=5E-15 from 1600-2300A; GALEX FUV=18.41 NUV=17.93
GALAXY
QSO
FOS G190H and G270H provided
J2000
J2000
f_lam=5E-15 at 1350-2300A; GALEX FUV=18.11 NUV 16.9
GALAXY
QSO
F)S G130H, G190H, G270H provided
J2000
J2000
f_lam=1-2E-14 at 1150-2300A; GALEX FUV=16.39 NUV=16.38
GALAXY
QSO
IUE 1200-2000A; FOS G190H G270H provided
J2000
J2000
f_lam=3-8E-15 at 1200-3300A; GALEX NUV=22.04
GALAXY
QSO
IUE 1200-2000A and FOS G190H and G270H provided
J2000
J2000
f_lam=1-2E-14 at 1350-2800A; GALEX FUV=16.51 NUV=15.74
GALAXY
QSO
FOS G130H and G190H provided
J2000
J2000
f_lam=3E-14 to 5E-15 at 1200-2300A; GALEX FUV=19.6 NUV=19.33
GALAXY
QSO
FOS G190H and G270H provided
J2000
J2000
f_lam=5-6E-15 at 1600-3200A; GALEX FUV=17.93 NUV=16.94
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G185M
1913
COS/NUV
Spectroscopic
No
No
G185M
1941
COS/NUV
Spectroscopic
No
No
G225M
2233
COS/NUV
Spectroscopic
No
No
G225M
2268
COS/FUV
Spectroscopic
No
No
G130M
1327
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G185M
1953
COS/NUV
Spectroscopic
No
No
G185M
2010
COS/NUV
Spectroscopic
No
No
G225M
2283
COS/FUV
Spectroscopic
No
No
G130M
1222
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G185M
1890
COS/NUV
Spectroscopic
No
No
G185M
1913
COS/NUV
Spectroscopic
No
No
G225M
2339
COS/FUV
Spectroscopic
No
No
G160M
1577
COS/NUV
Spectroscopic
No
No
G185M
1864
COS/NUV
Spectroscopic
No
No
G225M
2325
COS/NUV
Spectroscopic
No
No
G285M
2695
COS/FUV
Spectroscopic
No
No
G130M
1222
COS/FUV
Spectroscopic
No
No
G130M
1327
COS/FUV
Spectroscopic
No
No
G160M
1623
COS/NUV
Spectroscopic
No
No
G185M
1953
COS/FUV
Spectroscopic
No
No
G130M
1318
COS/FUV
Spectroscopic
No
No
G160M
1611
COS/NUV
Spectroscopic
No
No
G185M
1882
COS/NUV
Spectroscopic
No
No
G225M
2283
COS/NUV
Spectroscopic
No
No
G225M
2357
COS/FUV
Spectroscopic
No
No
G130M
1300
COS/FUV
Spectroscopic
No
No
G160M
1577
COS/NUV
Spectroscopic
No
No
G185M
1882
COS/NUV
Spectroscopic
No
No
G225M
2217
COS/FUV
Spectroscopic
No
No
G130M
1222
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G185M
1850
COS/FUV
Spectroscopic
No
No
G130M
1300
COS/NUV
Spectroscopic
No
No
G185M
1986
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true
4
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
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true
4
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
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false
5
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
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true
5
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
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false
3
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
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true
3
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
(Tic-Visit
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true
4
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
(Tic-Visit
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true
5
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
(Tic-Visit
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true
2
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
(Tic-Visit
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true
4
0
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
(Tic-Visit
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false
4
0