Science Keywords is a required field. Science Keywords: Select from 3 to 5 items. Wavelength is a required field. Wavelength is a required field. Wavelength is a required field. 0 Assigned ID: 2508 ----- Attempting Submission 1 (Fri Jun 20 15:27:55 GMT 2014) ----- Joint XMM For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. INEFFICIENT ORDERING OF FP-POS POSITIONS 0 ----- Attempting Submission 1 (Thu Jul 17 17:07:24 GMT 2014) ----- For each grating we use at least 4 separate detector positions using multiple central wavelengths and FP-POS locations. These are carefully chosen to place the segment gap in innocuous portions fo the spectrum. Four FP-POS settings per central wavelength are unnecessary. We propose to obtain contemporaneous high resolution spectroscopy of the Narrow Line Seyfert 1 Galaxy Mrk 335 with triggered XMM-Newton/RGS (130 ks) and HST/COS (7 orbits) observations with the aim of studying the properties of the ionized outflow that has recently been discovered in archival data. XMM/RGS spectra obtained during an intermediate flux state (June 2009) revelead the presence of multi-component ionized gas outflowing at ~5000 km/s. In HST/COS data taken a few months later (Oct 2009-Feb 2010) we found evidence for smooth, broad and weak CIV absorption. The global behavior of the gas in both bands can be explained by variation of the covering factor and/or column density, possibly due to transverse motion of absorbing clouds at Broad Line Region scale. For HST, we request a non-disruptive ToO that we will trigger at the same time as XMM. This will ensure that within 2.5 weeks from the trigger we will observe the source both in X-ray and UV. This time scale works very well with our prior results (Longinotti et al. 2013, ApJ, 766, 104) that suggest that the absorber in the UV is persistent on a time scale of weeks/months. During XMM-A013, Mrk 335 has two XMM visibility windows of about 6 weeks in the period June-July and December-January, fully compatible with visibility for HST, which runs from May 18 through February 10. To obtain HST/COS spectra of Mrk 335 using gratings G130M and G160M, comparable to those in Longinotti et al. 2013, requires 2 orbits. For gratings G130M and G160M, we use three central wavelength settings and multiple FP-POS positions to bridge the gap between detector segments, and to avoid detector and flat-field artifacts. In addition, we will use grating G140L/1280 with four FP-POS positions to measure absorption in OVI 1034 and Lybeta. At the historical mean flux level of 5.6e-14 erg cm^{-2} s^{-1} A^{-1} at 1390 A (Dunn et al. 2006, PASP, 118, 572), using the on-line COS ETC shows that in the additional 4 orbits from our allocation (9320 s exposure time) we obtain a S/N of 17.5 in the continuum, comparable to the M-grating exposures described in Longinotti et al. 2013. We will organize our observation as two visits: The first will use 2 orbits for G130M and G160M, and one additional orbit for G140L; the second visit will use 3 more orbits of just G140L. Both visits should be spaced as closely in time as possible. To allow for the range of variability observed in Mrk 335, we have chosen BUFFER TIMES significantly shorter than the 2/3 factor recommended in the ETC. We have also chosen the BUFFER TIMES to be integer multiples of (exposure time - 110 s) to minimze the overheads due to buffer readouts between successive exspoures. These observations pose no bright object concerns. All historical flux levels for Mrk 335 lie below the bright object limits for COS. Since Mrk 335 has been observed successfully before, there are also no surrounding field objects that are too bright. This is confirmed by the BOT tool for GALEX in APT. AGN/QUASARS Default false false false false false SUPPORTED GALAXY ACCRETION DISK NUCLEUS SEYFERT Coordinates are copied from the prior successful GTO observation of this object in proposal 11524. J2000 J2000 5.6e-14 at 1390 A COS/FUV Spectroscopic No No G130M COS/FUV Spectroscopic No No G160M COS/FUV Spectroscopic No No G140L 1405615997700 /Users/gak/proposals/cycle22/Mrk335/PhaseII/OP-cache/13814_070814-v01.xml Timing link suitability includes constraints ([02 After 01 by at most 3.0 days]) The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. Coordinate this first visit as close in time as possible after the ToO observation with XMM is triggered. For HST this should be a non-disruptive ToO, scheduled within ~2.5 weeks of the trigger. The second visit should follow the first as close in time as possible, but not more than 2-3 days later. (Tic-Visit :proposal-id 13814 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "17-Jul-2014 12:53:17.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1400576 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13814 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13814 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2663 :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 2999 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13814 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2754 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2999 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13814 :visit-id "01" :orbit-number 3 :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 2999 :pcs-gap 0 ) true 3 0 Triggered by Swift; coordinated with XMM-Newton Exposure time increased by about 4x from ETC to allow for source variability. Exposure time increased by about 4x from ETC to allow for source variability. FP-POS=4 gives shortest wavelengths for G130M/1289. But, B->A segment gap falls in red wing of redshifted N V, so only want one exposure here. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. FP-POS=1 puts the B->A segment gap as far as possible to the red of redshifted N V, so only want one exposure here. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. FP-POS=3 and 4 for 1327 avoids the gap from 1318/FP-POS=1. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. FP-POS=3 and 4 for 1327 avoids the gap from 1318/FP-POS=1. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. FP-POS=4 gives shortest wavelengths for G160M/1577. But, B->A segment gap falls in blue wing of redshifted C IV, so only want one exposure here. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. FP-POS=3 and 4 for 1611 puts the gap in the far red wing of redshifted C IV. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. FP-POS=3 and 4 for 1611 puts the gap in the far red wing of redshifted C IV. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. FP-POS=1 and 2 for 1623 covers the gap from 1611. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. FP-POS=1 and 2 for 1623 covers the gap from 1611. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. 1405616009189 /Users/gak/proposals/cycle22/Mrk335/PhaseII/OP-cache/13814_070814-v02.xml Timing link suitability includes constraints ([02 After 01 by at most 3.0 days]) The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. This second visit should follow the first as close in time as possible, but not more than 2-3 days later. (Tic-Visit :proposal-id 13814 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "17-Jul-2014 12:53:28.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1496128 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13814 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13814 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2663 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2999 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13814 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2768 :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 2999 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13814 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2768 :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 2999 :pcs-gap 0 ) true 3 0 Triggered by Swift; coordinated with XMM-Newton Exposure time increased by 4x from ETC to allow for source variability. Exposure time increased by 4x from ETC to allow for source variability. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures. Buffer time reduced by more than 2/3 of the ETC value to allow for source variability. Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.