6484( 4) - 05/02/96 20:31 - [ 1] PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID: 6484 Version: 4 Check-in Date: 02-May-1996 20:28:09 1.Proposal Title: Absorbing Outflows in Quasars and AGN ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Cycle QSO ABSORPTION LINES GO 6 ------------------------------------------------------------------------------------ 5. Investigators Contact? PI: Dr. Smita Mathur Smithsonian Astrophysical Observatory CoI: Dr. Belinda Wilkes Smithsonian Astrophysical Observatory Y CoI: Dr. Martin Elvis Smithsonian Astrophysical Observatory N ------------------------------------------------------------------------------------ 6. Abstract Intrinsic ``associated'' absorption has been a well known but little understood phenomenon in ultraviolet (UV) studies of both low and high luminosity active galactic nuclei (AGN) and in X-ray observations of the former. Recently it has become evident that a form of X-ray absorption is also common in high luminosity quasars. The identity of the absorber was not established in either UV or X-rays. In a recent study of 3C351 we have demonstrated, using both UV and X-ray data, that the associated UV metal lines and the soft X-ray absorption are due to the same material. This is the first confirmed UV/X-ray absorber and the combination of constraints provided by both datasets is powerful in determining the physical conditions and ionization state of the absorber, which we determine to be low density, highly ionized, outflowing material situated outside the broad line region. This is a previously unknown component of nuclear material. Following the result in 3C351, we have shown that the UV and X-ray absorbers are one and the same in two more AGN: 3C212 and NGC5548. We propose to obtain HST (FOS) UV spectra for 2 AGN with known, ionized X-ray absorbers in search of other UV/X- ray absorbers. The resulting dataset will allow us to investigate the properties of the absorbing material with unprecedented accuracy. ------------------------------------------------------------------------------------ 6484( 4) - 05/02/96 20:31 - [ 2] Observations Description ------------------------ Table 1 details our proposed observations. Objects are listed in the order of priority. Note that MR2251-178 has a FOC/Prism spectrum with data not good enough to detect and measure absorption lines. Here we propose to obtain good quality, high resolution spectra with the FOS. High resolution (R ~ 1300) is needed to resolve the doublets and to put stronger equivalent width limits. The very high resolution of GHRS is not necessary at this first stage. The spectral range of interest is that containing the associated absorption lines of OVI Lambda Lambda 1031, 1037, LyAlpha, NV Lambda Lambda 1238, 1242, CIV Lambda Lambda 1548, 1550, and MgII Lambda Lambda 2796, 2803. These absorption lines are expected to lie within the profiles of the broad emission lines. For each object, those high resolution dispersers were chosen which would enable us to observe any/all of these lines (Table 1). The blue detector would be used for G130H and the red detector for G190H and G270H to take advantage of its higher quantum efficiency. Lower resolution G140L on side 1 of GHRS would be more efficient than G130H on FOS for Lambda < 1500 Angstrom but switching between the instruments would increase the number of `visits' and so, the total number of orbits. The exposure times were determined using the formulae given in the FOS instrument handbook. Known IUE flux values (Lanzetta et al 1993, Courvoisier and Paltani 1992) at the center of each grating were used to estimate the HST count rate per diode. Total exposure time was designed to yield signal to noise ratio 20 to 30 (optimizing the total number of orbits) per resolution element near the center of each grating. For example: for PG1114+445; the IUE flux is 0.8 * 10^-14 erg s^-1 cm^-2 AA^-1 near 1300 Angstrom. Using formula N_Lambda = (F_lambda/S_Lambda)T_Lambda gives N_Lambda = 0.049 per diode. For SNR=25 per resolution element, the estimated exposure time is 13020 sec. This would yield about 630 counts at 1300 Angstrom\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\ and about 804 counts at 1600 Angstrom\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\ per diode with G130H. Exposure times for the other gratings were calculated similarly. All the objects would be observed with the 1.0" aperture and read out in a standard ACCUM mode. A target acquisition sequence of A+B1+C1+F1 would be used to ensure pointing accuracy of 0.12" . The number of orbits required for the observations were calculated using the FOS worksheet. begincenter Table 1: List of ionized X-ray absorbers to be observed with HST. begintabularlrcccccrc &&&&&&&&, Name & RA (2000) & f_Lambda^a & z & Config. & Spec. El.& Line & Exp. & Orbits , & Dec (2000) & & & & & & (min)& , &&&&&&&, PG1114+445 & 11 17 06.79 & 0.8 & 0.144 & FOS/BL & G130H & LyAlpha, NV, OVI & 217 & 8 , & +44 13 37.62 & 0.2&&FOS/RD & G190H & CIV & 58 &, & & 0.7 && & G270H & MgII & 3&, MR2251-178 & 22 54 05.84 & 2.5 & 0.064&FOS/BL&G130H &LyAlpha, NV & 61 & 4 , & -17 34 54.64& 2.0 &&FOS/RD & G190H& CIV & 7 &, & & 1.0 && & G270H & MgII & 2 &, &&&&&&&Total=& 12 , endtabular endcenter a. f_Lambda is in the units of 10^-14 erg s^-1 cm^- 2 AA^-1. Real Time Justification ----------------------- Calibration Justification ------------------------- Additional Comments ------------------- ------------------------------------------------------------------------------------ 6484( 4) - 05/02/96 20:31 - [ 3] Data Distribution Media: 8MM Blocking Factor: 10 Ship To: PI_Address Ship Via: UPS Email: , ------------------------------------------------------------------------------------ 6484( 4) - 05/02/96 20:31 - [ 4] TARGET LIST a) Fixed Targets ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial | Flux data No | Name | Description | Position |Eqnx | Vel. | ------------------------------------------------------------------------------------------------------------------------------------ 996 PG1114+445 GALAXY,QSO,RADIO RA=11H 17M 06.41S +/- J2000 Z = F(1300)=8.0e-15 QUIET,QUASAR, 0.04S,DEC=44D 13' 34.23" +/- 0.144 F(2700)=7e-15 0.6",PLATE-ID=01RA F(1900)=2.2e-15 997 MR2251-178 GALAXY,QSO,QUASAR, RA=22H 54M 05.83S +/- 0.04S,DEC= J2000 Z = F(1300)=2.5e-14 -17D 34' 55.2" +/- 0.6",PLATE- 0.064 F(1900)=2e-14 ID=020O F(2700)=1e-14 Comments: The target is in a little crowded field, though it IS the brightest object in the field. While getting the GSS coordinates i found that the fit to the data points was not perfect in the centering algorithm. 6484( 4) - 05/02/96 20:31 - [ 5] Visit: 10 Visit Requirements: On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 11 PG1114+445 FOS/BL ACQ/PEA 4.3 MIRROR SEARCH-SIZE-X=1,SEARCH-SIZE-Y=3, 1 1S ONBOARD ACQ FOR 12 K SCAN-STEP-Y=1.23 ------------------------------------------------------------------------------------------------------------------------------------ 12 PG1114+445 FOS/BL ACQ/PEA 1.0 MIRROR SEARCH-SIZE-X=6,SEARCH-SIZE-Y=2, 1 1S ONBOARD ACQ FOR 13 K SCAN-STEP-X=0.61,SCAN-STEP-Y=0.61 ------------------------------------------------------------------------------------------------------------------------------------ 13 PG1114+445 FOS/BL ACQ/PEA 0.5 MIRROR SEARCH-SIZE-X=3,SEARCH-SIZE-Y=3, 1 1S ONBOARD ACQ FOR 14 K SCAN-STEP-X=0.29,SCAN-STEP-Y=0.29 ------------------------------------------------------------------------------------------------------------------------------------ 14 PG1114+445 FOS/BL ACQ/PEA 0.3 MIRROR SEARCH-SIZE-X=3,SEARCH-SIZE-Y=3, 1 5S ONBOARD ACQ FOR 20-40 K SCAN-STEP-X=0.17,SCAN-STEP-Y=0.17 ------------------------------------------------------------------------------------------------------------------------------------ 20 PG1114+445 FOS/BL ACCUM 1.0 G130H 1 217M Comments: I am interested in observing OVI lambda 1034, Ly alpha and NV lambda 1240 lines with this grating. The OVI is observable at 1183 angstroms, Ly alpha is observable at 1391 & NV is observable at 1419 angstroms. ------------------------------------------------------------------------------------------------------------------------------------ 30 PG1114+445 FOS/RD ACCUM 1.0 G190H 1 77M Comments: I am interested in observing line CIV lambda 1548 with this grating. It is observable at 1771 angstroms. The grating should be centered around this line. ------------------------------------------------------------------------------------------------------------------------------------ 40 PG1114+445 FOS/RD ACCUM 1.0 G270H 1 3M Comments: I am interested in observing MgII lambda 2798 line with this grating. It is observable at 3201 angst. This is towards the edge of the grating. Can the central wavelength be adjusted to observe the line properly? ------------------------------------------------------------------------------------------------------------------------------------ 6484( 4) - 05/02/96 20:31 - [ 6] Visit: 20 Visit Requirements: On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 51 MR2251-178 FOS/BL ACQ/PEA 4.3 MIRROR SEARCH-SIZE-X=1,SEARCH-SIZE-Y=3, 1 1.0S ONBOARD ACQ FOR 52 K SCAN-STEP-Y=1.23 ------------------------------------------------------------------------------------------------------------------------------------ 52 MR2251-178 FOS/BL ACQ/PEA 1.0 MIRROR SEARCH-SIZE-X=6,SEARCH-SIZE-Y=2, 1 1.0S ONBOARD ACQ FOR 53 K SCAN-STEP-X=0.61,SCAN-STEP-Y=0.61 ------------------------------------------------------------------------------------------------------------------------------------ 53 MR2251-178 FOS/BL ACQ/PEA 0.5 MIRROR SEARCH-SIZE-X=3,SEARCH-SIZE-Y=3, 1 1.0S ONBOARD ACQ FOR 54 K SCAN-STEP-X=0.29,SCAN-STEP-Y=0.29 ------------------------------------------------------------------------------------------------------------------------------------ 54 MR2251-178 FOS/BL ACQ/PEA 0.3 MIRROR SEARCH-SIZE-X=4,SEARCH-SIZE-Y=4, 1 5.0S ONBOARD ACQ FOR 60-80 K SCAN-STEP-X=0.11,SCAN-STEP-Y=0.11 ------------------------------------------------------------------------------------------------------------------------------------ 60 MR2251-178 FOS/BL ACCUM 1.0 G130H 1 79M Comments: I am interested in observing Ly alpha and NV lambda 1240 lines with this grating. The ly alpha is observable at 1294 angstroms and NV is observable at 1319 angstroms. ------------------------------------------------------------------------------------------------------------------------------------ 70 MR2251-178 FOS/RD ACCUM 1.0 G190H 1 27M EXPAND Comments: I am interested in observing the CIV lambda 1548 line with this grating. It is observable at 1647 angstroms. ------------------------------------------------------------------------------------------------------------------------------------ 80 MR2251-178 FOS/RD ACCUM 1.0 G270H 1 5M Comments: I am interested in observing the MgII lambda 2798 line with this grating. It is observable at 2977 angstroms. ------------------------------------------------------------------------------------------------------------------------------------ 6484( 4) - 05/02/96 20:31 - [ 7] Summary Form for Proposal 6484 Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOS/BL FOS/RD ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ/PEAK ACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters SEARCH-SIZE-X=1 SEARCH-SIZE-Y=3 SCAN-STEP-Y=1.23 SCAN-STEP-Y=0.61 SCAN-STEP-Y=0.29 SCAN-STEP-Y=0.17 SCAN-STEP-X=0.61 SCAN-STEP-X=0.29 SCAN-STEP-Y=0.11 ------------------------------------------------------------------------------------------------------------------------------------ Proposal Category GO ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category QSO ABSORPTION LINES ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements ONBOARD ACQ FOR 12 ONBOARD ACQ FOR 13 ONBOARD ACQ FOR 14 ONBOARD ACQ FOR 20-40 ONBOARD ACQ FOR 52 ONBOARD ACQ FOR 53 ONBOARD ACQ FOR 54 ONBOARD ACQ FOR 60-80 EXPAND ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR G130H G190H G270H ------------------------------------------------------------------------------------------------------------------------------------ Target Names PG1114+445 MR2251-178 ------------------------------------------------------------------------------------------------------------------------------------