Cannot find file /Users/Sanch/Dropbox/Sanch/HST_Disk_halo/SJ_sanch_April10.pdf
Trial submission 1 ----
-1502119303
Assigned ID: 149
----- Attempting Submission 1 (Wed Apr 08 21:49:22 GMT 2015) -----
HST Phase I Proposal 149 (APT_ALFALFA.apt) successfully submitted.
Receipt: # 149-1
----- Attempting Submission 2 (Fri Apr 10 10:33:47 GMT 2015) -----
HST Phase I Proposal 149 (APT_ALFALFA.apt) successfully submitted.
Receipt: # 149-2
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
Phase II submitted July 23, 2015.
Added in the description that the exposure times would yield usable spectra (S?N=8.5) even if the QSO FUV flux drops to 19.3 mag i.e by 50%.Phase II submitted July 23, 2015.
Phase II submitted Sep 10, 2015.
Eleven 4-orbits visits have been shorten into Twenty-two 2-orbit visits. Each covers 2 FOP-pos setting so that all the four are covered within the 2 visits.
-194509153
----- Attempting Submission 1 (Tue Jul 21 20:32:52 GMT 2015) -----
HST Phase II Proposal 14071 (APT_Disk_Halo_Phase_II_16July.pdf.apt) successfully submitted.
Receipt: # 14071-1
----- Attempting Submission 2 (Thu Jul 23 08:07:20 GMT 2015) -----
HST Phase II Proposal 14071 (APT_Disk_Halo_Phase_II_16July.pdf.apt) successfully submitted.
Receipt: # 14071-2
----- Attempting Submission 3 (Thu Jul 23 20:02:15 GMT 2015) -----
----- Attempting Submission 4 (Thu Sep 10 23:35:40 GMT 2015) -----
Each covers 2 FOP-pos setting so that all the four are covered within the 2 visits.
This is done after consultation with John Biretta.
How are HI Disks Fed? Probing Condensation at the Disk-Halo Interface
Galaxy disks need a continuous supply of cold gas to fuel star formation. While accretion from the intergalactic medium brings in gas, this gas needs to condense down to a temperature <100K to form stars. In this proposal, we propose to investigate the process of accretion and condensation of inflowing warm ionized gas into neutral atomic gas (HI) in the disks of galaxies. Motivated by the need to learn more about the process of condensation, we propose to mount the first controlled absorption-line experiment to probe the interface between the disk and the circumgalactic medium (CGM). This study will complement the parameter space (in terms of impact parameter versus HI disk size) probed by the large HST program COS-GASS (PI:Heckman). Together these two programs will give us a continuous coverage of gas properties from disks to the virial radii of galaxies. Our sample provides QSO-sightlines through 35 gas-rich galaxies (z= 0.003-0.05) probing them at the disk-CGM interface. The proposed observations will probe a wide range of absorption-line transitions that will help us in identifying the underlying physics behind the process of condensation.
We will also use state-of-the art numerical simulations in a synergistic way that will both enable the observations to be interpreted in a physically-based context, and provide constraints that test (and then improve) the simulations. We will generate artifitial spectra that will enable us to analyze the simulations in the exact same way as the proposed observations. Therefore, we will also be able to interpret our results in the context of physics of gas accretion and connect it to the global properties of the galaxies.
Our strategic goal is to build a sample of QSO/galaxy pairs with impact parameter < 3.5 times the HI disk radii to study multi-phase gas in galactic halos and its dependence on galaxy properties. Our G130M COS data range over 1150 - 1450 A, which gives us access to a host of important ionization, density, and metallicity diagnostics. The galaxy redshifts range from z ~ 0.002-0.05, where these ions will be covered on at least one of the grating settings.
Exposure times: Most of our target QSOs are newly discovered by SDSS, and so have not been observed spectroscopically in the UV before. To ensure sufficient flux in the G130M bands we have cross-referenced our QSO catalog with the GALEX DR4 all-sky survey (AIS) and selected only QSOs with a significant detection in the GALEX FUV band (~ 1500 \AA). Measured GALEX FUV magnitudes for our sample range from 17.8 to 19.0. The redshifts range from z = 0.07 to 1.3. Note that if we assume the FOS composite QSO in the ETC, QSOs in this range of redshift and magnitude are always well below the bright limits of COS for both FUV spectroscopic exposures and NUV imaging target acquisitions with MIRRORB.
We use the COS online ETC to calculate that we will achieve S/N = 8-12 per resolution element over 1150 - 1450 A with 2-4 orbit exposures for our target objects. In each case we shift the central wavelength halfway through the full exposure for each grating to fill the ~ 15 A gap between detector segments. Use of the GALEX fluxes means that we do not need to correct for interstellar extinction, which in any case is E(B-V) <~ 0.1 for these high-latitude targets. Each visit has had the two central wavelengths packed for maximim efficiency, with the central wavelengths chosen to place the resulting low-S/N gap away from absorption lines of interest. Based on our experience with the ETC for QSOs in this range of redshift and magnitude and with similar objects observed by COS-GASS in Cycles 19, we know that these spectra always have their brightest pixel at the position of geocoronal Lyman alpha emission, not from the QSO source. These objects never get close to the bright limits, whatever the magnitude, redshift, or central wavelength setting.
Notes on Acquisitions:
Our coordinates are all from SDSS, with astrometry good to 100 mas, so we adopt NUV imaging (ACQ/IMAGE) for all targets. Our experience in Cycles 19 with COS-GASS is that IMAGE acquisitions are working well for these targets. We have set the exposure times for each "orbit bin" (2,3, or 4) using the faintest target at S/N = 40 in each bin as the limiting case, and then rounding up to provide a margin of safety against QSO fading. We use 219, 252 and 257 sec for the 2, 3, and 4 orbit targets, respectively. Adding 1 mag margin, more that 90% our targets are too bright for MIRRORA acquisitions, so we use MIRRORB in every case.
The Phase II ISR says use 1 mag brighter for bright-object check on ACQs. Brightest target here has GALEX NUV = 16.6, and this one is acquired in 33 sec at S/N = 40 for MIRRORB and PSA (ETC COS 732558). It has 5 ct/s in the brightest pixel, and 39 ct/s in the 9x9 selcted region. At one magnitude brighter (GALEX FUV = 15.6), this target is still safe to acquire with MIRRORB in the NUV, with 14 ct/s in the brightest pixel, 98 ct/s in the selected region, and 1038 ct/s on the entire detector (ETC COS 732559). In fact this target at one magnitude brighter is safe to observe with MIRRORB even for our longest exposure of 291 secs (COS.im.733006). The ETC run shows that the brightest will be at 7ct/s, 38 ct/s for the selected region and the count rate for the entire detector is 1010 ct/s.
MIRROR B:
NUV Mag Exposure Time ETC_COS_ID Safety_Check Safety_Check_ETC_ID_for_plus1mag Visits
16.6 ------ 33s ------ 732558 ---- Safe ---------- 732559 -------------- 9
17.6 ------ 84s ------ 732529 ---- Safe ---------- 732536 -------------- 11,
17.9 ------ 110s ------ 732530 ---- Safe ---------- 732537 -------------- 1,7,21,22,25
18.0 ------ 120s ------ 732531 ---- Safe ---------- 732539 -------------- 4,19
18.3 ------ 159s ------ 732540 ---- Safe ---------- 732555 -------------- 10,26
18.5 ------ 191s ------ 732541 ---- Safe ---------- 732556 -------------- 8,17,18,23,24,27
Similarly, we have checked for one-or-of magnitude brighter targets for those with MIRROR A exposures. All of them were found to be safe.
MIRROR A:
NUV Mag Exposure Time ETC_COS_ID Safety_Check Safety_Check_ETC_ID_for_plus1mag
18.7 ------ 12s ------ 732553 ---- Safe ---------- 732554 -------------- 3,13,14,15
18.8 ------ 13s ------ 732550 ---- Safe ---------- 732558 -------------- 2,5,6,20
19.0 ------ 15s ------ 732544 ---- Safe ---------- 732546 -------------- 12
20.1 ------ 42s ------ 732558 ---- Safe ---------- 732559 -------------- 16
For program targets with multi-epoch GALEX data, the true variability of these QSOs is of order ~< 0.2 mag, much less than this 1 mag assumption. For this reason, and because our brightest target is safe to acquire, all our targets are safe to acquire in NUV imaging with MIRRORB.
As anticipated for these targets selected from SDSS+GALEX, the BOT returns no health-and-safety issues for the targets or their fields.
To estimate the range of S/N ratios we will acquire for our science exposures, and to estimate their count rates for health-and safety checks, we ran a grid of representative ETC calculations for a range of QSO brightness and redshift. All these ETCs use the FOS QSO template spectrum normalized by the specified GALEX FUV flux at the specified redshift. There are two representative redshifts (0.02, 0.05) and three representative FUV magnitudes (17.8-18.0, 18.0-18.5, 18.5-19.0). The exposure times are the averages 9f the times drawn from the Phase II for those These ETCs are:
At FUV=18.0mag -> G130M=3158s- 3816s
z=0.02 wave=1240A COS.sp.732977
z=0.05 wave=1276A COS.sp.732980
Sightlines with FUVmag between 17.8- 18.0 (2 orbit bin: Targets 9,11; Visits 9,11 )
At FUV=18.5mag -> G130M=6113s- 6153 s
z=0.02 wave=1240A COS.sp.732998
z=0.05 wave=1276A COS.sp.733000
Sightlines with FUVmag between 18.0- 18.5 (3 orbit bin: Targets 7,21, 25, 26 ; Visits)
At FUV=19.0mag -> G130M= 9952s - 10018s
z=0.02 wave=1240A COS.sp.732994
z=0.05 wave=1276A COS.sp.732991
Sightlines with FUVmag between 18.5-19.0 (4 orbit bin; Targets 1,2,3,4,5,6,8,10,12,13,14,15,16,17,18,19,20,22,23,24,27; Visits 1,2,3,4,5,6,8,10,12,13,14,15,16,17,18,19,20,22,23,24,27 )
Targets-1,3,4,6,8,15,16,19,22,23,27 are scheduled as two 2-orbits visits. The visits are = Target# (for FP-pos =1,2 ) and Target#+50 (for FP-pos =3,4)
Just as a precaution we tested if 4 orbits are sufficient for a QSO at FUV 19.3mag . The ETC (COS.sp.734163/) yielded a S/N of more than 8.5 which will suffice for our study.
Note than in every case, the local and global count rates are far below the limits, and that in every case for G130M the brightest pixels correspond to geocoronal Lya, which is >1-2 orders of magnitude brighter than the source QSOs. In any case these count rates are well below the local and global limits.
The central wavelengths are set to optimally cover the interesting absorption lines from the galaxies of interest. The representative ETCs show that geocoronal Lya is always the brightest spot in G130M regardless of the cenwave, but is still well below the limits (0.1 cts at Lya vs. 0.67 cts limit), and the targets tend to be at least an order of magnitude fainter. Since the FOS template spectrum is relatively flat (see the representative cases) the global count rate is almost invariant with cenwave and never gets close to the limits
ISM IN EXTERNAL GALAXIES
12
false
true
false
false
SUPPORTED
GALAXY
QSO
NO
J2000
J2000
GALEX FUV = 18.8, GALEX NUV = 17.8
GALAXY
QSO
NO
J2000
J2000
GALEX FUV=19.0, GALEX NUV = 18.8
GALAXY
QSO
NO
J2000
J2000
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GALAXY
QSO
NO
J2000
J2000
GALEX FUV=18.8, GALEX NUV = 18.1
GALAXY
QSO
NO
J2000
J2000
GALEX FUV=18.9, GALEX NUV = 18.8
GALAXY
QSO
NO
J2000
J2000
GALEX FUV=18.7, GALEX NUV = 18.8
GALAXY
QSO
NO
J2000
J2000
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GALAXY
QSO
NO
J2000
J2000
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GALAXY
QSO
NO
J2000
J2000
GALEX FUV=17.8, GALEX NUV = 16.6
GALAXY
QSO
NO
J2000
J2000
GALEX FUV=18.9, GALEX NUV = 18.1
GALAXY
QSO
NO
J2000
J2000
GALEX FUV=17.9, GALEX NUV = 17.6
GALAXY
QSO
NO
J2000
J2000
GALEX FUV=19.0, GALEX NUV = 18.9
GALAXY
QSO
NO
J2000
J2000
GALEX FUV=18.9, GALEX NUV = 18.7
GALAXY
QSO
NO
J2000
J2000
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GALAXY
QSO
NO
J2000
J2000
GALEX FUV=18.7, GALEX NUV = 18.6
GALAXY
QSO
NO
J2000
J2000
GALEX FUV = 18.7, GALEX NUV = 20.1
GALAXY
QSO
NO
J2000
J2000
GALEX FUV =19.0, GALEX NUV = 18.5
GALAXY
QSO
NO
J2000
J2000
GALEX FUV = 19.0, GALEX NUV = 18.6
GALAXY
QSO
NO
J2000
J2000
GALEX FUV =18.8, GALEX NUV = 18.0
GALAXY
QSO
NO
J2000
J2000
GALEX FUV =18.9, GALEX NUV = 18.8
GALAXY
QSO
NO
J2000
J2000
GALEX FUV = 18.0, GALEX NUV = 17.9
GALAXY
QSO
NO
J2000
J2000
GALEX FUV = 18.8, GALEX NUV = 17.9
GALAXY
QSO
NO
J2000
J2000
GALEX FUV =18.6, GALEX NUV = 18.4
GALAXY
QSO
NO
J2000
J2000
GALEX FUV = 19.0, GALEX NUV = 18.4
GALAXY
QSO
NO
J2000
J2000
GALEX FUV =18.0, GALEX NUV = 17.7
GALAXY
QSO
NO
J2000
J2000
GALEX FUV = 18.2, GALEX NUV = 18.2
GALAXY
QSO
NO
J2000
J2000
GALEX FUV =18.7, GALEX NUV = 18.5
COS/FUV
Spectroscopic
No
No
G130M
1300
COS/FUV
Spectroscopic
No
No
G130M
1300
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1318
COS/FUV
Spectroscopic
No
No
G130M
1300
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G130M
1327
COS/FUV
Spectroscopic
No
No
G130M
1300
COS/FUV
Spectroscopic
No
No
G130M
1318
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G130M
1300
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1327
COS/FUV
Spectroscopic
No
No
G130M
1300
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G130M
1300
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G130M
1327
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true
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