Science Keywords: Select from 2 to 5 items. Science Keywords is a required field. Wavelength is a required field. Wavelength is a required field. 0 Assigned ID: 2558 ----- Attempting Submission 1 (Wed Sep 15 12:17:38 GMT 2021) ----- Joint Chandra/HST Justification for our choice of FP-POS settings are now included in the Proposal Description. 329134323 ----- Attempting Submission 1 (Wed Oct 06 19:33:34 GMT 2021) ----- HST Phase II Proposal 16842 successfully submitted. Receipt: # 16842-1 ----- Attempting Submission 2 (Tue Oct 19 21:45:11 GMT 2021) ----- HST Phase II Proposal 16842 successfully submitted. Receipt: # 16842-2 ----- Attempting Submission 3 (Thu Nov 18 01:18:41 GMT 2021) ----- Obscuring outflows are remarkably different from the warm-absorber outflows in AGN. They exhibit large columns of high-velocity gas close to the accretion disk. They shield the X-ray radiation, which has important implications for the launching of outflows. They were first discovered in NGC 5548 thanks to simultaneous X-ray and UV observations in 2013. Recent Swift monitoring of NGC 5548 points to remarkable long-term changes in the strength of X-ray obscuration in NGC 5548. In order to study this change, simultaneous X-ray and UV high-resolution spectroscopy is required. Therefore, we propose simultaneous Chandra/HETG (150 ks) and HST/COS (2 orbits) observations to help us address existing questions about the origin and physical structure of the long-lasting obscuration in NGC 5548. The goal of our proposal is to obtain joint X-ray (Chandra/HETG) and UV (HST/COS) spectra of NGC 5548 to determine the physical changes in the obscuring outflows in this AGN. To this end, as requested in our proposal we need the Chandra and HST observations to be taken contemporaneously since the source and the obscuring outflows vary over time. We have specified in our proposal that the Chandra and HST observations to be taken within +/- 2 days of each other, which has been approved. To help scheduling of the observations the 150 ks Chandra observation can be split. According to the 'Chandra Initial Parameter Signoff' that we recently checked and approved, the 150 ks Chandra observation is planned to be split into five 30 ks exposures. However, each exposure is still requested to be within +/- 2 days of the HST observation. We would greatly appreciate the coordination of Chandra and HST planners so that our observations are taken contemporaneously. Although reduced gyro operations for HST would be unfortunate, our program would still remain fully feasible. Reduced gyro operations would approximately halve the opportunities for coordination with Chandra. Also, any orientation limitation would not impact our program. Our HST/COS time and set-up is based on the prior observations of NGC 5548 (Kaastra et al. 2014, Science, 345, 64), which required 2 orbits per visit to observe broad absorption lines of Ly-alpha, N V, and C IV with gratings G130M and G160M. This yields a S/N of at least 15 in the continuum at C IV, adequate to measure the broad UV absorption in C IV and other lines, as well as the weak, low-ionization lines associated with the new ionization state of the warm absorber. The new HST/COS observation enables us to constrain the covering fraction of the broad UV absorber, and measure how much it has changed with the lower X-ray obscuration in NGC 5548. Following the Phase II Proposal instructions and the allowed COS settings for Cycle 29, the central wavelengths and FPPOS positions that we have selected provide the optimum full spectral coverage of the interested regions with the G130M and G160M gratings, and maximize the potential of the detection of the relevant broad and narrow absorption lines. This enables us to fully explore the UV spectral signatures of the obscuring outflow in NGC 5548. We obtained the required time for each exposure using the COS Exposure Time Calculator (ETC) tool and the NGC 5548 HST UV continuum (1367 A) fluxes published by Kriss et al. (2019, ApJ, 881, 153). For the target acquisition we used the minimum observed UV flux of NGC 5548 (1.8e-14 erg/cm^2/s/A, Kriss et al. 2019) and calculated the required exposure time to get a S/N of at least 30 using ACQ/IMAGE with BOA. Using the mean flux of the NGC 5548 campaign in 2014 (4.3e-14 erg/cm^2/s/A, Kriss et al. 2019), the exposure time is calculated to give a S/N of at least 10 for each exposure with G130M/1222, and for the total exposure with G130M/1291. Similarly, the exposure time is calculated to give a S/N of at least 10 for exposures with G160M/1600 and G160M/1623. The maximum flux ever observed with NGC 5548 (8.6e-14, Dunn et al. 2006, PASP, 118, 572. ETC run #1541128 for G130M/1291) does not pose a bright object risk for COS. For the BUFFER-TIME, we obtained the recommended buffer (2/3 of the buffer fill time) from the ETC for each exposure. NGC 5548 has been acquired and observed on many occasions at a variety of orientations, and there are no bright field objects that would prove an overlight risk to COS. Because we are using two different CENWAVES with each grating and two FP-POS positions in each, we already accomplish the actual objectives of switching between different FP-POS settings: (1) Better science return: the spectrum is placed at four different locations on the detector, enabling us to detect and reject detector anomalies like dead spots, hot spots, grid-wire shadows, etc. (2) Spread the flux across the detector in multiple locations, especially in bright emission lines, to decrease charge depletion and extend the lifetime of the detectors. We do not want to sacrifice S/N with unnecessary extra exposures and increased overhead during each visit by using all 4 FP-POS settings with each CENWAVE. When only one CENWAVE is used, then 4 FP-POS settings makes sense, but that's not the case for our observations. Our chosen FP-POS settings reflect our S/N requirements while still meeting the objectives of using different FP-POS settings in our program. The PI (Dr. Missagh Mehdipour) and Co-Is have extensive experience and expertise in study of AGN outflows and analysing and modelling data from Chandra, HST, XMM-Newton, Swift, and NuSTAR. Data from our previous X-ray and UV campaigns, and successful ToO programs, have been extensively published: Mrk 509 campaign with 16 refereed publication - NGC 5548 campaign with 9 refereed publication - NGC 7469 campaign with 6 refereed publication - NGC 3783 ToO programme with 5 refereed publication Some of our relevant publications directly related to the science case of the proposed Chandra/HETG and HST/COS project are: Mehdipour et al. 2015, A&A, 575, A22 Mehdipour et al. 2016, A&A, 588, A139 Mehdipour et al. 2017, A&A, 607, A28 Kaastra et al. 2014, Science, 345, 64 Kriss et al. 2019, A&A, 621, A12 Mao et al. 2019, A&A, 621, A99 Dr. Mehdipour has expertise in X-ray spectroscopy of ionised outflows in AGN, optical-UV-X-ray continuum modelling, and photoionisation modelling. He has previously led projects on the studies of ionised outflows in AGN with Chandra and XMM-Newton. He is the PI of successful Swift proposals targeting a sample of AGN that has included triggers for NGC 3783. Dr. Mehdipour will carry out the main analysis of the Chandra/HETG and HST/COS spectra to determine changes in the obscuration of NGC 5548. Dr. Kriss is a world expert in multi-wavelength observations of AGN. He has vast experience in HST analysis and modelling of UV absorption lines of different types of AGN outflows. Dr. Kriss will contribute to the analysis and modelling of the HST/COS observation. Prof. Kaastra is the lead developer of the SPEX code, which is used for X-ray spectroscopy and photoionisation modelling. Prof. Kaastra has experience and expertise in the X-ray studies of AGN outflows. He led the discovery of the obscuring wind in NGC 5548 with a multi-wavelength campaign using XMM-Newton, NuSTAR, Chandra, Swift, and HST in 2013-2014. Prof. Kaastra will contribute to photoionisation modelling of the new proposed observations. Dr. Mao is an expert in high-resolution X-ray spectroscopy of AGN using XMM-Newton and Chandra. He is the PI of an awarded Chandra Cycle 22 proposal targeting a possibly obscured AGN. Dr. Mao will contribute to the high-resolution spectroscopy of X-ray emission lines. Dr. Landt has great experience in study of NGC 5548 at long wavelengths. Her experience with NGC 5548 will be useful in the interpenetration of the new results. Dr. Gu is an expert on atomic data and modelling of hot plasmas. He will contribute towards modelling of the X-ray spectra. Supermassive Black Holes and Active Galaxies 6 false false false false false false false 150 true SUPPORTED GALAXY ACCRETION DISK BLR SEYFERT WIND NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1600 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1623 1634676301655 /home/missagh/Documents/Chandra_proposal_2021/APT/OP-cache/16842_MM_v6-v01.xml The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16842 :visit-id "01" :proposal-version -1 :trans-version "20210514" :date "19-Oct-2021 16:45:01.0" :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 104544 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16842 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16842 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 353 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2928 :pcs-gap 0 ) true 1 0 Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019), we took the lowest observed flux (1.8e-14 erg/cm^2/s/A), to calculate the required exposure time to obtain S/N ratio of 30 for ACQ/IMAGE with BOA. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated to give S/N ratio of about 7 with 1222. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated to give S/N ratio of about 7 with 1291. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated to give S/N ratio of about 7 with 1600. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated to give S/N ratio of about 7 with 1623. 1634676297428 /home/missagh/Documents/Chandra_proposal_2021/APT/OP-cache/16842_MM_v6-v02.xml The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16842 :visit-id "02" :proposal-version -1 :trans-version "20210514" :date "19-Oct-2021 16:44:57.0" :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 104544 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16842 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16842 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2535 :al-overhead-at-end 0 :internal-dur-at-end 353 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2928 :pcs-gap 0 ) true 1 0 Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019), we took the lowest observed flux (1.8e-14 erg/cm^2/s/A), to calculate the required exposure time to obtain S/N ratio of 30 for ACQ/IMAGE with BOA. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated to give S/N ratio of about 7 with 1222. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated to give S/N ratio of about 7 with 1291. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated to give S/N ratio of about 7 with 1600. Using the NGC 5548 HST UV continuum (1367 A) lightcurve published by Kriss et al. (2019) and the mean flux of the 2014 campaign (4.3e-14 erg/cm^2/s/A), the exposure time is calculated to give S/N ratio of about 7 with 1623.