0 Assigned ID: 2535 ----- Attempting Submission 1 (Sun Sep 14 00:46:49 GMT 2014) ----- Submitting on behalf of the PI, Julia Lee, jclee@harvard.edu. -90733388 ----- Attempting Submission 1 (Mon Nov 03 20:50:35 GMT 2014) ----- I checked them, and there are no issues. Don't why this message is coming up. An X-ray, UV, and radio probe of the PG 1211+143 inflow-outflow dynamics We will study the QSO PG 1211+143 using a joint award of time from Chandra HETGS (450ks), HST COS (4 orbits), and JVLA (5 hrs JVLA-A). With Chandra, we will measure the kinematics of the ionized wind to establish energetics. Contemporaneous Chandra-HST observations will be necessary for determing thermodynamic stability conditions and wind-driving mechanisms. JVLA observations will enhance the outflow studies by identifying the radio emission (possibly from a jet) associated with PG1211, to tie in with HETGS studies of its ionized wind(s). Strong gravity signatures in PG 1211 using traditional methods and new probes will also be assessed. Existing Chandra LETGS, XMM RGS, Suzaku spectra lack the spectral resolution and S/N to enable a clear picture of the PG1211 inflow-outflow dynamics. To obtain the most accurate spectral energy distribution for PG1211+143, and to maximize our possibility of detecting simultaneous UV and X-ray absorption in any ultra-fast outflow, we will observe PG1211+143 in three separate visits coordinated with our Chandra X-ray observations. The Chandra observations are currently planned as three observations of 90 ks+180 ks+180 ks in February 2015. We will observe PG1211+143 once with HST in coordination with each visit. Our HST observations will use the COS G140L grating with a 1280 A central wavelength setting to cover the far-UV continuum from 1000 A to 2000 A in a single orbit on each visit. On the second visit we will also use grating G130M, so that we get complete velocity coverage across the detector segment gaps for the blue wing of the Lyman alpha profile in PG1211+143. The G140L exposures will also cover the brightest UV emission lines: O VI, Lya, NV and CIV, which are also tracers of the shape of the unobservable extreme UV continuum beyond the Lyman limit. Historically, the PG 1211 UV flux at 1465 A has ranged from (1.9-4.5)e-14 ergs cm-2 s-1 A-1 (Dunn et al., 2006). Using the mean HST FOS QSO spectrum normalized to the highest flux level (4.5e-14 ergs cm-2 s-1 A-1), the Exposure Time Calculator v22.2 predicts for each orbit a S/N per resolution element of > 10 between 1100-1800 A, with a peak continuum S/N~25 at 1400 A. This observation is also safe for COS. Given the G140L resolving power of 2000-3000, this is adequate to avoid intervening interstellar absorption features and bin the continuum measurements to a S/N>50 across most of the HST-COS spectral range. Presuming outflow velocities of 3000 kms-1 (i.e., as reported in the X-ray by Kaspi et al. 2006), this will allow us to detect weak UV absorption lines at the expected wavelengths for Lya, NV 1238,1242 and CIV 1548,1550 with 3-sigma EWs of <25mA in each HST orbit. This corresponds to optically thin column densities of < 2e13 cm-2. The HST-COS spectrum will also cover the higher ionization O VI doublet at 1032,1038 A, but at a lower S/N of 10, yielding a limiting equivalent width of 100 mA and a limiting column density of < 2e14 cm-2. These limits are much lower than the predictions for such ions in the low xi photoionization models for the X-ray transitions seen by Kaspi et al. (2006). AGN/QUASARS Default false false false false false SUPPORTED GALAXY ACCRETION DISK NUCLEUS QSO WIND This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 3.5e-14 at 1465 A COS/FUV Spectroscopic No No G140L 1280 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. To be coordinated with Chandra observation 1. (Tic-Visit :proposal-id 13947 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "03-Nov-2014 15:45:37.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 435008 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13947 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13947 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2614 :al-overhead-at-end 0 :internal-dur-at-end 385 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2997 :pcs-gap 0 ) false 1 0 Using the brightest flux ever observed, 4.5e-14 at 1465 A, this observation is still safe for COS. ETC run #638681. For observation planning, we used the *lowest* flux ever observed, 1.9e-14, in order to ensure the success of our target acquisition, ETC run #638682. Using the brightest flux ever observed, 4.5e-14 at 1465 A, this observation is still safe for COS. ETC run #638688. (We used the FOS-based QSO spectrum, z=0.0809, and E(B-V)=0.03.) The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. To be coordinated with Chandra observation 2. (Tic-Visit :proposal-id 13947 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "03-Nov-2014 15:45:47.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 852544 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13947 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13947 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2614 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2997 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13947 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2758 :al-overhead-at-end 0 :internal-dur-at-end 385 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2997 :pcs-gap 0 ) false 2 0 Using the brightest flux ever observed, 4.5e-14 at 1465 A, this observation is still safe for COS. ETC run #638681. For observation planning, we used the *lowest* flux ever observed, 1.9e-14, in order to ensure the success of our target acquisition, ETC run #638682. Using the brightest flux ever observed, 4.5e-14 at 1465 A, this observation is still safe for COS. ETC run #638688. (We used the FOS-based QSO spectrum, z=0.0809, and E(B-V)=0.03.) Using the brightest flux ever observed, 4.5e-14 at 1465 A, this observation is still safe for COS. ETC run #644855. (We used the FOS-based QSO spectrum, z=0.0809, and E(B-V)=0.03.) The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. To be coordinated with Chandra observation 3. (Tic-Visit :proposal-id 13947 :visit-id "04" :proposal-version -1 :trans-version "20140605" :date "03-Nov-2014 15:45:49.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 435008 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13947 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13947 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2614 :al-overhead-at-end 0 :internal-dur-at-end 385 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2997 :pcs-gap 0 ) false 1 0 Using the brightest flux ever observed, 4.5e-14 at 1465 A, this observation is still safe for COS. ETC run #638681. For observation planning, we used the *lowest* flux ever observed, 1.9e-14, in order to ensure the success of our target acquisition, ETC run #638682. Using the brightest flux ever observed, 4.5e-14 at 1465 A, this observation is still safe for COS. ETC run #638688. (We used the FOS-based QSO spectrum, z=0.0809, and E(B-V)=0.03.)