Updated Visit 56 exposure times to avoid visibility overruns. Visit 56 is the replacement for the failed Visit 06
----- Attempting Submission 7 (Tue Sep 14 18:32:29 GMT 2010) -----
Visit 56 is the replacement to Visit 06, the failed visit. This replacement has caused the number
of orbits in the proposal to no longer match its allocation.
The Cosmological Impact of AGN Outflows: Measuring Absolute Abundances and Kinetic Luminosities
AGN outflows are increasingly invoked as a major contributor to the formation and evolution of supermassive black holes, their host galaxies, the surrounding IGM, and cluster cooling flows. Our HST/COS proposal will determine reliable absolute chemical abundances in six AGN outflows, which influences several of the processes mentioned above. To date there is only one such determination, done by our team on Mrk 279 using 16 HST/STIS orbits and 100 ksec of FUSE time. The advent of COS and its high sensitivity allows us to choose among fainter objects at redshifts high enough to preclude the need for FUSE. This will allow us to determine the absolute abundances for six AGN (all fainter than Mrk 279) using only 40 HST COS orbits. This will put abundances studies in AGN on a firm footing, an elusive goal for the past four decades. In addition, prior FUSE observations of four of these targets indicate that it is probable that the COS observations will detect troughs from excited levels of C III. These will allow us to measure the distances of the outflows and thereby determine their kinetic luminosity, a major goal in AGN feedback research. We will use our state of the art column density extraction methods and velocity-dependent photoionization models to determine the abundances and kinetic luminosity. Previous AGN outflow projects suffered from the constraints of deciding what science we could do using ONE of the handful of bright targets that were observable. With COS we can choose the best sample for our experiment. As an added bonus, most of the spectral range of our targets has not been observed previously, greatly increasing the discovery phase space.
G130M and G160M observations of AGN. Primary science goals are maximum S/N at intrinsic Ly-a, Ly-b, and CIV.
MRK876 is a GTO target. Our science goals do not overlap (we are looking at intrinsic absorption, GTO is intervening systems). We do not overlap in grating/setting with the GTO observations, and we have arranged to share our data with the GTO team. At the request of the PC, Visit 3 (CVZ, F04250-5718) was split into two visits to enhance scheduling opportunities (now Visit 3 and Visit 33),
AGN/QUASARS
12
false
0.0
0.0
false
false
false
false
false
false
SUPPORTED
GALAXY
LYMAN ALPHA CLOUD
QSO
SEYFERT
F(1180) = 1.8E-14 (FUSE, Z9073902)
F(1600) = 1.9E-14 (IUE, SWP46321), F(2000)=1.4E-14, F(3000)=0.7E-14
Goals were; G130M: 9445s G160M: 8875s
In eight orbits we get:
G130M: 2393+3*3192=11969
G160M: 2238+3*3912=11814
3.0e-14 @ 1110 Angstroms
J224841.2-510954
REJ2248-511
J2000
22 48 41.2000
-51 09 54.00
J2000
GALAXY
LYMAN ALPHA CLOUD
QSO
SEYFERT
F(1180)=5E-14 (FUSE, f0260101)
F(1600)=2E-14 (IUE, swp52673), F(2000)=2E-14
Target is too bright for PSA+MIRRORB, so going spectroscopic.
We get safety and the BT from 2.5xflux, and the ET from 0.5xflux
COS71222 -> safe, BT = 546 *2/3 = 364
COS71223 -> ET=2.2 s
Goals were: G130M: 9445s G160M: 8875
Actual was :
G130M: 3805*4=15220
G160M; 3774*4=15096
F(1180)=5E-14
J042600.8-571201
1H0419-577
J2000
04 26 0.8000
-57 12 0.00
J2000
GALAXY
QSO
Nominal flux = 1.8E-14 at 1850 (IUE), F(1600)=2E-14 (swp40289, 1990)
FUSE(1180)=9E-14, F(1110)=8E-14 (p1073101, 1999)
FUSE(1180)=6E-14 (d0280203, 2004)
FUSE(1180)=2.5E-14 (d0280201, 2003)
FUSE(1180)=2.5E-14 (u1036601, 2006)
PI has also indicated 3.9e-14 @ 1110 Angstroms
F(1180)=2.5E-14, F(1600) = 2E-14
MRK0876
MRK-0876
J2000
16 13 57.2000
+65 43 10.00
J2000
GALAXY
LYMAN ALPHA CLOUD
QSO
SEYFERT
F(1180) = 2E-14 (d1310106,d1310101)
F(1180) = 1.5E-14 (z0020401)
GALEX J004818.9+394111 gives
NUV=16.56 +/- 0.03
FUV=16.77 +/- 0.04
F(1180)=2E-14, F(1110)=1.5E-14
RXJ0048.3+3941
J004819.0+394111
J2000
00 48 18.9000
+39 41 11.00
J2000
GALAXY
LYMAN ALPHA CLOUD
QSO
SEYFERT
F(1180)=7E-14 (FUSE, s6011001, Feb. 2008)
F(1180)=1E-13 (FUSE, p1011901, March 2008)
F(1180)=1.25E-13 (FUSE, p1011903, Apr. 2008)
F(1600)=6E-14, F(2000)=3E-14 (IUE, swp08882), But this target was fading from 1979-1986.
F(1180)=1.25E-14
0804+761
J081058.5+760243
J2000
08 10 58.6000
+76 02 42.00
J2000
GALAXY
LYMAN ALPHA CLOUD
QSO
SEYFERT
F(1180)=5E-14 (FUSE, p1019001)
GALEX J123050.1+011522
NUV=14.84 +/- 0.01
FUV=15.15 +/- 0.02
F(1180)=5e-14
SDSSJ123050.03+011522.6
J123050.0+011521
J2000
12 30 50.0000
+01 15 22.00
J2000
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/FUV
Spectroscopic
No
No
G130M
1291
COS/FUV
Spectroscopic
No
No
G160M
1600
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
IRAS-F22456-5125 G130M Four orbits, shortest possible 1291 wavelength settings
Goals were; G130M: 9445s G160M: 8875s
In eight orbits we get:
G130M: 2393+3*3192=11969
G160M: 2238+3*3912=11814
We deviate from our normal strategy to get maximum flux at the lowest wavelengths
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true
5
0
F(1180) = 1.8E-14 (FUSE, Z9073902)
F(1600) = 1.9E-14 (IUE, SWP46321), F(2000)=1.4E-14, F(3000)=0.7E-14
z=0.1
Simulating 2.5x the flux F(1600)=2.5x1.9E-14=4.75E-14 ->
COS71204 -> too bright for PSA+MIRRORA
COS71205 -> too bright for PSA+MIRRORB
COS71211 -> Good to go for G130M/1318 Spectroscopic TA, BT=566*2/3=377s
COS71212 -> Simulating 0.5x the flux (F1600)=0.95E-14 @1600 gives the TA time of 2.2s
see previous TA comments
see previous TA comments
COS71211 -> BT=566*2/3=377s
see previous G130M comment
see previous G130M comment
see previous G130M comment
see previous G130M comment
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
IRAS-F22456-5125 G160M (Four Orbits). G160M Spectroscopic TA
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true
4
0
F(1600)=1.9E-14
1/2 flux gives the ET, COS71215-> G160M/1589 ET = 3.5s
2.5x flux gives safety and BT, COS71216 -> G160M/1589 BT = 979 (2.5 x flux) *2/3 = 652s
see previous TA comment
see previous TA comment
F(1600)=1.9E-14
1/2 flux gives the ET, COS71215-> G160M/1589 ET = 3.5s
2.5x flux gives safety and BT, COS71216 -> G160M/1589 BT = 979 (2.5 x flux) *2/3 = 652s
see previous G160M comment
see previous G160M comment
see previous G160M comment
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
IRAS-F04250 G130M (Two CVZ Orbits): First 1/2 of G130M observations
Goals were: G130M: 9445s G160M: 8875
Actual was : G130M: 4*3750+4410s=19410s, G160M; 3774*4=15096
We deviate from our normal strategy to get maximum flux at the lowest wavelengths
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true
2
0
F(1180)=5E-14 (FUSE, f0260101)
F(1600)=2E-14 (IUE, swp52673), F(2000)=2E-14
Target is too bright for PSA+MIRRORB, so going spectroscopic.
We get safety and the BT from 2.5xflux, and the ET from 0.5xflux
COS71222 -> safe, BT = 546 *2/3 = 364
COS71223 -> ET=2.2 s
see previous TA comment
see previous TA comment
Bonus orbit at lowest wavelength setting, see previous G130M comments
COS71222 -> safe, BT = 546 *2/3 = 364s
Short wavelength coverage for LyB
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
IRAS-F04250 G130M (Two CVZ Orbits): Second 1/2 of G130M observations
Goals were: G130M: 9445s G160M: 8875
Actual was : G130M: 4*3750+4410s=19410s
G160M; 3774*4=15096
We deviate from our normal strategy to get maximum flux at the lowest wavelengths
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true
2
0
F(1180)=5E-14 (FUSE, f0260101)
F(1600)=2E-14 (IUE, swp52673), F(2000)=2E-14
Target is too bright for PSA+MIRRORB, so going spectroscopic.
We get safety and the BT from 2.5xflux, and the ET from 0.5xflux
COS71222 -> safe, BT = 546 *2/3 = 364
COS71223 -> ET=2.2 s
see previous TA comment
see previous TA comment
Bonus orbit at lowest wavelength setting, see previous G130M comments
see previous G130M comment
see previous G130M comment
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
IRAS-F04250 G160M (Three CVZ Orbits)
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true
3
0
F(1180)=5E-14 (FUSE, f0260101)
F(1600)=2E-14 (IUE, swp52673), F(2000)=2E-14
Target is too bright for PSA+MIRRORB, so going spectroscopic.
We get safety and the BT from 2.5xflux, and the ET from 0.5xflux
COS71234 -> safe, BT = 942 *2/3 = 628, COS71231 -> ET=3.5 s
see previous comment
see previous comment
see previous comment
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
MRK876 is also a GTO target. Here we observe only G160M and the lowest G130M setting (to get the intrinsic Ly-beta). We do not overlap in science, or grating/central wavelength combinations with the GTO proposal.
The G130M portions of this program have been modified to be the lowest FP-POS settings (the IHB provided incorrect information).
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true
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Using an uploaded IUE composite spectrum at 1/2 the nominal flux (COS69291) gives the ET=2.14s. Using 2.5x the flux for safety gives BT (1462/5 * 2/3 = 195s)
Nominal flux = 1.8E-14 at 1850 (IUE), F(1600)=2E-14
For comparison, a z=0.129 QSO with
F(1600)=1E-14 was also simulated (COS75572) gives G130M+1291 S/N=40 in 2.4 s with a BT=2094.
F(1600)=5E-14 was also simulated (COS75573) gives G130M+1291 S/N=40 in 0.5 s with a BT=583*2/3=388s.
see previous comment
see previous comment
ETC TEST SERVER ID: COS91664
Flux was 2.5x nominal = 4.5e-14 @ 1800,
this gives the BT=618*2/3 = ~412 using (1530-110)/3 =473
Here, BT=(1500-110)/4=463
see previous G130M comment
ETC TEST SERVER ID: COS91665
Nominal flux = 1.8E-14 at 1850 (IUE)
We use 2.5x the flux for safety and BT (1149*2/3=766) but 0.5*flux for exposure time.
Here, BT=(2960-110)/4=645
see previous G160M comment
see previous G160M comment
see previous G160M comment
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
Q0045 G130M (Four Orbits), Spectroscpic TA with ET=6.3 and BT=561s.
3x3 ACQ/SEARCH is probably overkill, a 2x2 would be sufficient.
Original goal was 9235 for G130M, and 11565 for G160M.
In eight orbits, we get
G130M; 2199+3*3049=11346.
G160M: 2168+3*3049=11315
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true
4
0
F(1180) = 2E-14 (d1310106,d1310101)
F(1180) = 1.5E-14 (z0020401)
GALEX J004818.9+394111 gives
NUV=16.56 +/- 0.03
FUV=16.77 +/- 0.04
As usual, we will get our BT from 2.5 times the brightest measurement, and the ET from 1/2 times the faintest. First the BT:
COS75710 usesG130M/1318+ F(1180)=2.5*2E-14=5E-14 for a z=0.134 FOS QSO template gives BT=2/3* 841= 561s (ET=0.7s)
COS75714 uses G130M/1318+ GALEX FUV -1 = 15.77 for a z=0.134 FOS QSO template gives BT=2/3* 1370= 914 (ET=1.26s)
Now at 1/2 the faintest to get ET:
COS75713 uses F(1180)=0.5*1.5E-14=0.75E-14 for a z=0.134 FOS QSO template gives ET=3.5s
COS75715 uses GALEX FUV +0.75 = 17.5 for a z=0.134 FOS QSO template gives ET=6.3
So, we are going with ET=6.3 and BT=561s
see previous comment
see previous comment
As usual, we will get our BT from 2.5 times the brightest measurement:
COS75710 usesG130M/1318+ F(1180)=2.5*2E-14=5E-14 for a z=0.134 FOS QSO template gives BT=2/3* 841= 561s (ET=0.7s)
COS75714 uses G130M/1318+ GALEX FUV -1 = 15.77 for a z=0.134 FOS QSO template gives BT=2/3* 1370= 914 (ET=1.26s)
So, we are going with BT=561s
see previous comment
see previous G130M comment
see previous G130M comment
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
Q0045 G160M (Four Orbits), Spectroscopic TA with BT=905 and ET=8.9s
3x3 ACQ/SEARCH is probably overkill, a 2x2 would be sufficient.
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G160M
COS75711 usesG160M/1577+ F(1180)=2.5*2E-14=5E-14 for a z=0.134 FOS QSO template gives BT=2/3* 1357= 905s (ET=1s)
COS75717 uses GALEX NUV -1.0 = 15.56 for a z=0.134 FOS QSO template gives ET=1.7s, BT=2398*2/3.=1599s
COS75712 uses G160M/1577 + F(1180)=0.5*1.5E-14=0.75E-14 for a z=0.134 FOS QSO template gives ET= 5s
COS75716 uses GALEX NUV +0.75 = 17.31 for a z=0.134 FOS QSO template gives ET=8.9s
So, we are being overly cautious and going with BT=905 and ET=8.9s
PEAKXD, see previous G160M TA comment
PEAKXD, see previous G160M TA comment
G160M
COS75711 usesG160M/1577+ F(1180)=2.5*2E-14=5E-14 for a z=0.134 FOS QSO template gives BT=2/3* 1357= 905s (ET=1s)
COS75717 uses GALEX NUV -1.0 = 15.56 for a z=0.134 FOS QSO template gives ET=1.7s, BT=2398*2/3.=1599s
COS75712 uses G160M/1577 + F(1180)=0.5*1.5E-14=0.75E-14 for a z=0.134 FOS QSO template gives ET= 5s
COS75716 uses GALEX NUV +0.75 = 17.31 for a z=0.134 FOS QSO template gives ET=8.9s
So, we are being overly cautious and going with BT=905 and ET=8.9s
see previous comment
see previous comment
see previous comment
bonus coverage at lowest G160M setting
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
PG0804+761, Four orbits split between G130M and G160M.
This target is highly variable, so we need to be conservative in the TA. Recent flux measurements are
F(1180)=7E-14 (FUSE, s6011001, Feb. 2008)
F(1180)=1E-13 (FUSE, p1011901, March 2008)
F(1180)=1.25E-13 (FUSE, p1011903, Apr. 2008)
F(1600)=6E-14, F(2000)=3E-14 (IUE, swp08882), But this target was fading from 1979-1986.
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true
4
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We will use the 2x the brightest recent FUSE flux for safety and BT determination, and 1/2 times the recent
faintest fuse for ET.
F(1180)=7E-14 (FUSE, s6011001, Feb. 2008)
F(1180)=1E-13 (FUSE, p1011901, March 2008)
F(1180)=1.25E-13 (FUSE, p1011903, Apr. 2008)
ET: COS75719 (z=0.1 QSO +FUV/G130M/1309 gives ET=1s) for F(1180)=3.5E-14
BT: COS75722 (z=0.1 QSO +FUV/G130M/1309 gives BT=161*2/3 ~111s) for F(1180)=2.5E-13
For G160M/1600
BT: COS75726 (z=0.1 QSO +FUV/G160M/1600 gives BT=306*2/3 ~204s) for F(1180)=2.5E-13
see previous TA comment
see previous TA comment
ET: COS75719 (z=0.1 QSO +FUV/G130M/1309 gives ET=1s) for F(1180)=3.5E-14
BT: COS75722 (z=0.1 QSO +FUV/G130M/1309 gives BT=161*2/3 ~111s) for F(1180)=2.5E-13
see previous comment
see previous G130M comments
see previous G130M comments
For G160M/1600
BT: COS75726 (z=0.1 QSO +FUV/G160M/1600 gives BT=306*2/3 ~204s) for F(1180)=2.5E-13
see previous G160M comment
see previous G160M comment
see previous G160M comment
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
RXJ1230- G130M (Four Orbits)
There are no BOT constraints (the reported violation is our target)
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F(1180)=5E-14 (FUSE, p1019001)
GALEX J123050.1+011522: NUV=14.84 +/- 0.01: FUV=15.15 +/- 0.02
As usual, we get our BT from the 2.5x the brightest observation, and ET from 0.5* the faintest observation.
G130M_1318: z=0.117
COS75737 gives BT = 316*2/3 = 211s (F1180=1.25E-13)
COS75741 gives BT = 366*2/3 = 244s (FUV=14.15)
COS75740 gives ET = 1.2s (F1180=0.25E-13)
COS75745 gives ET = 1.4s (FUV=15.9)
ET=1.4, BT=211
G160M_1589: z=0.0117
COS75738 gives BT = 526*2/3 = 351s (F1180=1.25E-13)
COS75742 gives BT = 614*2/3 = 409s (FUV=14.15)
COS75739 give ET=1.9s (F1180=0.25E-13)
COS75744 gives ET =2.24s (FUV=15.9)
ET=2.3s, BT=351
see previous G130M TA comment
see previous G130M comment
F(1180)=5E-14 (FUSE, p1019001)
GALEX J123050.1+011522: NUV=14.84 +/- 0.01: FUV=15.15 +/- 0.02
As usual, we get our BT from the 2.5x the brightest observation, and ET from 0.5* the faintest observation.
G130M_1318: z=0.117
COS75737 gives BT = 316*2/3 = 211s (F1180=1.25E-13)
COS75741 gives BT = 366*2/3 = 244s (FUV=14.15)
COS75740 gives ET = 1.2s (F1180=0.25E-13)
COS75745 gives ET = 1.4s (FUV=15.9)
ET=1.4, BT=211
see previous G130M comment
see previous G130M comment
see previous G130M comment
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
RXJ1230 G160M (Four Orbits)
There are no BOT constraints (the reported violation is our target)
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true
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F(1180)=5E-14 (FUSE, p1019001)
GALEX J123050.1+011522: NUV=14.84 +/- 0.01: FUV=15.15 +/- 0.02
As usual, we get our BT from the 2.5x the brightest observation, and ET from 0.5* the faintest observation.
G160M_1589: z=0.0117
COS75738 gives BT = 526*2/3 = 351s (F1180=1.25E-13)
COS75742 gives BT = 614*2/3 = 409s (FUV=14.15)
COS75739 give ET=1.9s (F1180=0.25E-13)
COS75744 gives ET =2.24s (FUV=15.9)
ET=2.3s, BT=351
see previous G160M TA comment
see previous G160M TA comment
F(1180)=5E-14 (FUSE, p1019001)
GALEX J123050.1+011522: NUV=14.84 +/- 0.01: FUV=15.15 +/- 0.02
As usual, we get our BT from the 2.5x the brightest observation, and ET from 0.5* the faintest observation.
G160M_1589: z=0.0117
COS75738 gives BT = 526*2/3 = 351s (F1180=1.25E-13)
COS75742 gives BT = 614*2/3 = 409s (FUV=14.15)
COS75739 give ET=1.9s (F1180=0.25E-13)
COS75744 gives ET =2.24s (FUV=15.9)
ET=2.3s, BT=351
see previous G160M comment
see previous G160M comment
see previous G160M comment
The scheduling data was generated by CASM 18.3.1.
CASM was run in Phase II mode.
/private/var/folders/43/43soeEaB2RW-oU+1Yxh+uU+++TI/-Tmp-/OPVisit6218942091912850606.xml
Q0045 G130M (Four Orbits), Spectroscpic TA with ET=6.3 and BT=561s.
3x3 ACQ/SEARCH is probably overkill, a 2x2 would be sufficient.
Original goal was 9235 for G130M, and 11565 for G160M.
In eight orbits, we get
G130M; 2199+3*3049=11346.
G160M: 2168+3*3049=11315
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true
4
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F(1180) = 2E-14 (d1310106,d1310101)
F(1180) = 1.5E-14 (z0020401)
GALEX J004818.9+394111 gives
NUV=16.56 +/- 0.03
FUV=16.77 +/- 0.04
As usual, we will get our BT from 2.5 times the brightest measurement, and the ET from 1/2 times the faintest. First the BT:
COS75710 usesG130M/1318+ F(1180)=2.5*2E-14=5E-14 for a z=0.134 FOS QSO template gives BT=2/3* 841= 561s (ET=0.7s)
COS75714 uses G130M/1318+ GALEX FUV -1 = 15.77 for a z=0.134 FOS QSO template gives BT=2/3* 1370= 914 (ET=1.26s)
Now at 1/2 the faintest to get ET:
COS75713 uses F(1180)=0.5*1.5E-14=0.75E-14 for a z=0.134 FOS QSO template gives ET=3.5s
COS75715 uses GALEX FUV +0.75 = 17.5 for a z=0.134 FOS QSO template gives ET=6.3
So, we are going with ET=6.3 and BT=561s
see previous comment
see previous comment
As usual, we will get our BT from 2.5 times the brightest measurement:
COS75710 usesG130M/1318+ F(1180)=2.5*2E-14=5E-14 for a z=0.134 FOS QSO template gives BT=2/3* 841= 561s (ET=0.7s)
COS75714 uses G130M/1318+ GALEX FUV -1 = 15.77 for a z=0.134 FOS QSO template gives BT=2/3* 1370= 914 (ET=1.26s)
So, we are going with BT=561s
see previous comment
see previous G130M comment
see previous G130M comment