We propose to observe the bright active galactic nucleus NGC 4051 for 120 ks jointly with HST and Astro-H. This source hosts one of the most extraordinary multi-phase ionized outflows. For the first time, we will acquire a high-resolution spectrum of the low, medium and highly ionized outflow in a low-mass black hole. We will study the connection between the X-ray and UV absorber and the disk winds mapping the ionization structure, kinematic behavior and relative abundance. We will observe NGC 4051 simulataneously in the X-ray and the UV with a 120 ks observation using the RGS on XMM-Newton as the prime instrument combined with a an HST-COS observation of 4 orbits duration. We also ask to coordinate these observations with an expected Astro-H observation (with a net exposure of 100 ks) on a best effort basis. We will study the variability of the warm absorber in both the UV and the X-ray on short time scales, for the first time including HST, XMM-Newton and Astro-H. This source is one of the best cases for variability studies in the X-rays using both RGS and EPIC-pn. This will be done either through X-ray time resolved spectroscopy (Krongold et al. 2007) or the study of the continuum-lagging warm absorber using timing (Silva et al. 2015). * For the first time, we will have global, high-resolution, and simultaneous picture of the grand design of the ionized outflow and associated narrow emission lines: HST-COS will map the low ionization species (Si iii, Ciii, Si iv, Civ, Nv), possibly the long-distance tail of the disk wind. * XMM-Newton-RGS will bridge all the components: the low ionization ones (via the ions belonging to both the X-ray and UV band, Costantini 2010) and the intermediate ionization multi-layer gas, that is largely inaccessible to Astro-H. Finally, Astro-H-SXS, with 5 eV resolution, will provide an unprecedented coverage of the medium-hard energy band, opening an extraordinary discovery space. * The thorough census of the ionized gas will allow us to meaningfully test theoretical scenarios especially on the connection between high-velocity disk winds and the warm absorber: is the gas distributed in discrete components or a continuous flow? Would the initial energy be conserved throughout the flow? NGC 4051 has a history of significant changes in both the underlying continuum and ionization structure. Simultaneous UV-X-ray observations will be key for a true understanding of any unexpected event (e.g. obscuration, appearance or disappearance of new components). This has been the case in the past for e.g. NGC 5548 (Kaastra et al. 2014), in Mrk 335 (Longinotti et al. 2013), and in NGC 985 (Ebrero et al., submitted) We will observe NGC 4051 with HST-COS for 4 orbits using gratings G130M and G160M in order to observe the main absorption line transitions in C III* 1176, Ly alpha, N V, Si IV, and C IV. Our previous observational campaigns on Mrk 279, Mrk 509, NGC 5548, and NGC 985 all achieved good results with a signal-to-noise ratio of 20 per resolution element in the continuum for these objects. To achieve a 4-fold diversity of grating settings for each grating, we use multiple central wavelengths for G130M and G160M to make sure we span the gap between segments A and B, and we use different FPPOS positions for each of those. For Ly alpha and N V using grating G130M, assuming a historical median flux of 1.3e-14 erg/cm2/s/A at 1368 A (Dunn et al. 2006) this requires a minimum of t=2000 s, and for C IV in G160M, t=2000 s. Including overheads, these observations therefore require a total of 4 orbits. We note that the high resolution afforded by COS makes our proposed observations robust to flux variations to fainter levels. The ~100 km/s widths of the absorption troughs are spanned by 4 COS resolution elements. If NGC 4051 were half as bright, we could bin our spectrum up by a factor of two and still oversample the absorption troughs at the same S/N. These observations pose no bright object concerns. All historical flux levels for NGC 4051 lie below the bright object limits for COS. Since NGC 4051 has been observed successfully before (see HST PID 11834), there are also no surrounding field objects that are too bright. NGC 4051 is faint enough that we can safely use an imaging target acquisition. Our ETC calculations use the ETC FOS quasar spectrum redshifted to z=0.002336 with foreground extinction of E(B-V)=0.011 and normalized to the historical minimum and maximum flux at 1368 A (flam_min=0.57e-14, flam_max=2.2e-14, Dunn et al. 2006). In order to get our limiting cases and be absolutely sure that an imaging target acq is safe, we use a maximum flux that is twice the historical maximum: - ACQUISITION - Configuration Flux EXP time Max cts/s/pix Total rate Buffer Time COS ETC ID G130M/1291 4.40e-14 5.3 s 42 1387 ---- COS.im.768334 G130M/1291 0.57e-14 41 s 5.4 997 ---- COS.im.768333 - EXPOSURES - Configuration Flux EXP time Max cts/s/pix Total rate Buffer Time COS ETC ID G130M/1291 1.30e-14 1000 0.11 1013 2327 COS.sp.768323 G130M/1291 2.20e-14 1000 0.12 1429 1650 COS.sp.768330 G160M/1600 1.30e-14 1000 0.004 414 5695 COS.sp.768326 G160M/1600 2.20e-14 1000 0.007 606 3889 COS.sp.768331 AGN/QUASARS 12 false false false false false false SUPPORTED GALAXY ACCRETION DISK NUCLEUS SEYFERT WIND NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 F(1368)=1.3e-14 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G160M 1600 1454095378637 The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. Should be simultaneous with the coordinated XMM-Newton observation. To achieve a 4-fold diversity of grating settings for each grating, instead of using 4 FPPOS positions for each grating, we use multiple central wavelengths for G130M and G160M to make sure we span the gap between segments A and B, and we use different FPPOS positions for each of those. (Tic-Visit :proposal-id 14479 :visit-id "01" :proposal-version -1 :trans-version "20150609" :date "29-Jan-2016 14:22:57.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1426592 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14479 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14479 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2658 :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 2991 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14479 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2769 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2991 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14479 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2769 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2991 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14479 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2769 :al-overhead-at-end 0 :internal-dur-at-end 341 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2991 :pcs-gap 0 ) false 4 0 Exposure time is chosen for the faintest historical flux, 1.2e-14. We use BUFFER-TIMES much shorter than the 2/3*ETC value for brightest historical flux since this is even safer. They are optimized to be 110 s less than the exposure time to minimize the overhead between exposures. We use BUFFER-TIMES much shorter than the 2/3*ETC value for brightest historical flux since this is even safer. They are optimized to be 110 s less than the exposure time to minimize the overhead between exposures. We use BUFFER-TIMES much shorter than the 2/3*ETC value for brightest historical flux since this is even safer. They are optimized to be 110 s less than the exposure time to minimize the overhead between exposures. We use BUFFER-TIMES much shorter than the 2/3*ETC value for brightest historical flux since this is even safer. They are optimized to be 110 s less than the exposure time to minimize the overhead between exposures. We use BUFFER-TIMES much shorter than the 2/3*ETC value for brightest historical flux since this is even safer. They are optimized to be 110 s less than the exposure time to minimize the overhead between exposures. We use BUFFER-TIMES much shorter than the 2/3*ETC value for brightest historical flux since this is even safer. They are optimized to be 110 s less than the exposure time to minimize the overhead between exposures. We use BUFFER-TIMES much shorter than the 2/3*ETC value for brightest historical flux since this is even safer. They are optimized to be 110 s less than the exposure time to minimize the overhead between exposures. We use BUFFER-TIMES much shorter than the 2/3*ETC value for brightest historical flux since this is even safer. They are optimized to be 110 s less than the exposure time to minimize the overhead between exposures.