removed between on visit 06 to allow earlier scheduling185513684----- Attempting Submission 1 (Thu Feb 21 20:53:52 GMT 2013) -----
----- Attempting Submission 2 (Mon Jun 03 20:06:20 GMT 2013) -----
HST Phase II Proposal 13184 (13184_060313.apt) successfully submitted.
----- Attempting Submission 3 (Tue Jun 25 20:01:32 GMT 2013) -----
----- Attempting Submission 4 (Thu Jul 25 15:37:21 GMT 2013) -----
----- Attempting Submission 5 (Tue Sep 03 14:06:48 GMT 2013) -----NGC 5548 has been observed before with HST/COS with no issues. The BOT tool did not show any field objects that were a problem. ETC calculations show that NGC 5548 itself is safe to observe.
This is a Cycle 21 proposal being submitted early to perform a coordinated observations with XMM-Newton early, while still in Cycle 20. The Visit Planner in APT appears not to be able to schedule Cycle 21 proposals before August 1, 2013, even though NGC 5548 is visible in our desired windows.
The warnings recommend 4 FP-POS positions for each grating setting. We have used an alternative that uses combinations of central wavelengths and FP-POS selections to avoid gaps in a combined spectrum. Each grating gets four exposures with different displacements for the spectrum on the detector that permit us to bridge the gaps and remove other detector defects and flat field features while at the same time avoiding intrinsic features in the obsject spectrum..Deciphering AGN outflows: multiwavelength monitoring of NGC 5548AGN outflows couple supermassive black holes to their environments. Using an ambitious multiwavelength campaign on NGC 5548, (XMM-Newton, HST, Swift, and optical) we propose to achieve a new level of physical understanding for these enigmatic winds by obtaining the deepest RGS spectrum of any AGN, allowing us to determine the ionisation structure of the gas. Using EPIC data we will measure the response of the outflow to continuum variations, which combined with HST/COS data determines unambiguously the location and tomography of the outflow components. Time-dependent UV and X-ray continuum variations will constrain the geometry and physics close to the black hole. Our team pioneered this approach, and recently applied it successfully (12 refereed papers) to Mrk 509.We will use COS/FUV with gratings G130M and G160M to observe the 1150-1800 A spectrum of the Seyfert 1 galaxy NGC 5548. These observations will be coordinated with XMM-Newton X-ray spectral observations, which are to be scheduled as 10 visits, each ~1 day long, at 4 day intervals in June/July 2013, followed by 2 visits in January 2014. We will schedule five 2-orbit HST visits in coordination with the core of the campaign in June/July 2013, and one additional 2-orbit visit in January 2014. The HST observations should be scheduled to within 1 day of the XMM observations, offering a 3-day window around each. Preliminary XMM-Newton observing times are as follows:
Tstart -> Tstop
2013-Jun-22 00:36:56 GMT -> 2013-Jun-22 22:21:03 GMT
2013-Jul-11 23:18:56 GMT -> 2013-Jul-12 21:03:04 GMT
2013-Jul-23 22:31:47 GMT -> 2013-Jul-24 20:33:33 GMT
2013-Jul-29 22:07:46 GMT -> 2013-Jul-30 20:09:32 GMT
2013-Jul-31 21:59:49 GMT -> 2013-Aug-01 20:01:34 GMT
2014-Jan-01 00:00:00 GMT -> 2014-Feb-01 00:00:00 GMT
The far-UV continuum of NGC 5548 shows 17 to 30% rms variability with peak-to-trough variations of 2-5 over 2-month time scales. Extremely low FUV flux episodes are very rare (Dunn et al. 2006). We expect a roughly linear response for the column density of Ly alpha, N V, and C IV in response to continuum changes. Therefore, to be sensitive to changes in the absorption lines at the 3-sigma level, a conservative estimate of the required S/N per resolution element is 3/0.17=17.6. For Ly and NV using grating G130M, assuming a historical median flux Fmed of
3.5x1e-14 erg cm^{-2} s^{-1} A^{-1}1 at 1376 A (Dunn et al. 2006), this requires t >1000 s and for C IV in G160M t > 2000 s. Since only 2000 s per orbit remain after overheads for science exposures, we need two HST orbits per visit to obtain sufficient S/N. With 2 orbits and all overheads accounted for, we have 1800 s for science in the first orbit with G130M, and 2280 s in the 2nd orbit with G160M. At the median flux, this gives per visit S/N>25 in the Lyalpha and N V
region in G130M, and S/N>20 for C IV in G160M.
COS observations of NGC 5548 have been carried out safely and successfully before (see HST PID 12212), and they do not pose a bright object risk. We verify this with the following ETC calculations for which we use the FOS quasar spectrum in the ETC at a redshift of z=0.017 normalized to flux levels at 1360 A as given below. For limiting cases we use the following maximum and minimum historical flux levels from Dunn et al. (2006) (263 observations spanning 35 years):
Max: 8.6e-14 at 1360 A
Min: 0.66e-14 at 1360 A
COS ETC ID Config Flux Max cts/s/pix Total rate Buffer Time
COS.sa.468856 G130M/1291 0.66e-14 0.1 689 3423
COS.sa.468862 G130M/1291 8.6e-14 0.2 4189 563
COS.sp.468865 G130M/1309 8.6e-14 0.13 4343 543
COS.sp.468872 G160M/1600 8.6e-14 0.13 1876 1257AGN/QUASARSDefaultfalsefalsefalsefalsefalseSUPPORTEDGALAXYACCRETION DISKNUCLEUSSEYFERTWINDThis object was generated by the targetselector and retrieved from the NED database.J20004.39e-14 at 1360 A (historical mean)COS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MCOS/FUVSpectroscopicNoNoG130MCOS/FUVSpectroscopicNoNoG160MThe scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.To be coordinated with XMM-Newton observations tentatively scheduled for
2013-Jun-22 00:36:56 GMT -> 2013-Jun-22 22:21:03 GMT1371907508000126.79656507613299(Tic-Visit
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)true20To be coordinated with XMM-Newton Observations.Our spectroscopic target acq calculation is based on the observed historical minimum flux for NGC 5548 of 0.66e-14 at 1360 A to ensure adequate S/N even if the target is in a faint state.Our spectroscopic target acq calculation is based on the observed historical minimum flux for NGC 5548 of 0.66e-14 at 1360 A to ensure adequate S/N even if the target is in a faint state.The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.To be coordinated with XMM-Newton observations tentatively scheduled for
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2013-Jul-23 22:31:47 GMT -> 2013-Jul-24 20:33:33 GMT1374684180000108.2251822426274(Tic-Visit
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