0Assigned ID: 666
----- Attempting Submission 1 (Fri Apr 05 19:39:42 GMT 2019) -----At LP4 SEGMENT=B is OFF by default for some G130M configurations. See "Errors and Warnings" for more details.Target Acq on Visit 02 was changed from imaging to spectroscopic mode.2071733210----- Attempting Submission 1 (Sun Jul 21 20:40:15 GMT 2019) -----
HST Phase II Proposal 15890 (subways_15890v1.apt) successfully submitted.
Receipt: # 15890-1
----- Attempting Submission 2 (Wed Nov 20 14:53:23 GMT 2019) -----
HST Phase II Proposal 15890 (subways_15890v1.apt) successfully submitted.
Receipt: # 15890-2
----- Attempting Submission 3 (Fri Feb 07 20:23:51 GMT 2020) -----While high-resolution observations at shorter wavelengths would be useful
(to include OVI and Ly beta) it is not possible to do these unless we use G130M/1222.
However, the long-wavelength end of 1222 does not cover Ly alpha and N V.
These are more important, so we will simply accept having Segment B off for 1327.Supermassive Black Hole Winds in X-rays (SUBWAYS): Building the HST Line with FUV SpectroscopyWinds powered by accretion onto the supermassive black holes at the centers of galaxies can have a profound impact on their hosts. These outflows may provide the feedback necessary to regulate star formation and the accretion of gas onto the host galaxy, thereby establishing a link for the co-evolution of the central black hole and its host. These winds are present on all scales, from the accretion disk around the black hole to the outskirts of the galaxy itself, and at multiple wavelengths, from the X-ray to the radio. As part of a multiwavelength program, this proposal will characterize the UV spectra and associated UV absorption of a well defined sample of moderate redshift AGN that are the hub of an approved XMM-Newton large program (1.5 Ms), designed to constrain the X-ray manifestations of AGN outflows. The proposed HST+COS spectra will cover the wavelength range from 1125 A to 2150 A, and include all strong UV resonance lines in the sample: OVI+Ly beta, Ly alpha, N V, Si IV, and C IV. These spectra form an essential ingredient to explore the UV counterparts of X-ray winds and to characterize the spectral energy distribution, line luminosities, and any outflows during the current epoch of the X-ray observations. The UV perspective on outflows is critical for understanding all phases of an outflow's components and of its energetics. This in turn will provide a more comprehensive view of the feeding and feedback cycle, and it will help to refine theoretical models for outflows from nuclear to galaxy-scales. Observations of the SUBWAYS sample will be a reference for AGN wind studies at intermediate redshift for years to come.Far-UV spectra of the SUBWAYS sample will be obtained using COS. Grating G140L/1105 covers the broadest possible wavelength range in a single exposure, allowing the continuum shape to be measured from 1125 A to 2000 A, as well as the primary spectral features associated with Ly beta, O VI, Ly alpha, N V, Si IV, and C IV. The R~3,000 resolving power of the G140L/1105 grating is well matched to detecting the 100 km/s widths of typical narrow UV absorption components, and fully resolving broad UV outflow components that have widths of 1000-3000 km/s. This resolution is adequate to resolve even complex assortments of narrow absorption lines, optical depths, and covering factors in all the observed troughs. For uniformity, all targets i nthe program will be observed with G140L/1105. For some objects, the redshift is high enough that NUV exposures are required to cover C IV, and in one case, we take advantage of the target's brightness and redshift to obtain higher resolution observations with G130M and G160M. The observations are summarize in the Table 1 below. The flux at 1516 A, obtained using GalexView or HST archival observations, is given in units of 1e-15 erg/s/cm2/A. (See the Phase 1 proposal for more details on each object in the program.)
Target z f1516 Gratings Orbits
PG0052+251 0.154 20.3 G140L/1105 1
2MASXJ0220-0728 0.213 2.2 G140L/1105 2
PG0947+396 0.205 16.9 G140L/1105,G130M/1222,G160M/1600,G185M/1953 2
PG0953+414 0.234 20.0 G140L/1105 1
PG1202+281 0.164 4.5 G140L/1105,G130M/1327 2
PG1216+069 0.331 17.2 G140L/1105,G185M/1953 2
PG1307+085 0.154 19.6 G140L/1105 1
LBQS1338-0038 0.237 2.2 G140L/1105 2
PG1352+183 0.151 10.3 G140L/1105 1
2MASXJ140251+2631 0.188 1.8 G140L/1105 2
PG1425+267 0.364 3.9 G140L/1105,G230L/3360 2
PG1427+480 0.221 6.5 G140L/1105,G185M/1864 3
PG1435-067 0.126 11.5 G140L/1105 1
SDSSJ144414+0633 0.207 3.0 G140L/1105 1
HB891529+050 0.218 0.44 G140L/1105 3
PG1626+554 0.133 16.6 G140L/1105 1
Table 2 below again gives the FUV fluxes. These observations pose no bright object concerns. All flux levels lie well below the bright object limits for COS, and checks of the surrounding fields using the GALEX and SDSS catalogs rule out nearby bright objects. Pointers to the ETC calculations for our targets are given here. For all estimates we used the FOS-based QSO spectrum, assumed E(B-V)=0.0, and used the tabulated redshift of the object. To calculate buffer times, we used the listed flux at 1516 A. All targets are sufficiently faint to use imaging target acquisitions with Mirror B. Only the faintest target, HB891529+050, uses Mirror A. For Target Acq calculations, to be conservative, we used a flux value that is half that given in the table, and then rounded the result up to the next whole integer.
Name RA Dec z f1516 COS_ETC_Pointer BufTime COS_TA ExpTime(s)
PG0052+251 00 54 52.10 +25 25 37.99 0.154 2.04E-14 COS.sp.1369753 2255 COS.ta.1369729 5.2
PG0953+414 09 56 52.40 +41 15 22.00 0.234 2.00E-14 COS.sp.1369752 4348 COS.ta.1369728 11.2
PG1626+554 16 27 56.10 +55 22 32.02 0.133 1.66E-14 COS.sp.1369754 2583 COS.ta.1369734 6.2
PG1202+281 12 04 42.12 +27 54 12.11 0.164 4.48E-15 COS.sp.1369399 6592 COS.ta.1369401 24.6
PG1435-067 14 38 16.10 -06 58 21.00 0.126 1.15E-14 COS.sp.1369756 3405 COS.ta.1369735 9
SDSSJ144414+0633 14 44 14.6 +06 33 06.77 0.207 3.04E-15 COS.sp.1369757 8812 COS.ta.1369717 36
PG1216+069 12 19 20.90 +06 38 39.01 0.331 1.72E-14 COS.sp.1369759 2831 COS.ta.1369736 5.5
PG0947+396 09 50 48.42 +39 26 50.64 0.205 1.69E-14 COS.sp.1369760 3317 COS.ta.1369737 8
HB891529+050 15 32 28.79 +04 53 58.46 0.219 8.86E-16 COS.sp.1369761 11975 COS.ta.1369408 7.2
PG1307+085 13 09 47.00 +08 19 48.22 0.154 1.96E-14 COS.sp.1369762 2322 COS.ta.1369738 5.4
PG1425+267 14 27 35.61 +26 32 14.63 0.364 3.94E-15 COS.sp.1369763 7326 COS.ta.1369739 24.2
PG1352+183 13 54 35.72 +18 05 18.05 0.151 1.03E-14 COS.sp.1369764 3762 COS.ta.1369740 10.3
2MASXJ0220-0728 02 20 14.58 -07 28 59.23 0.213 2.21E-15 COS.sp.1369765 9947 COS.ta.1369725 70
LBQS1338-0038 13 41 13.94 -00 53 14.97 0.237 2.18E-15 COS.sp.1369766 11078 COS.ta.1369741 115
2MASXJ140251+2631 14 02 51.19 +26 31 17.63 0.187 1.77E-15 COS.sp.1369767 9616 COS.ta.1369748 63.7
PG1427+480 14 29 43.10 +47 47 26.02 0.21 6.48E-15 COS.sp.1369768 6433 COS.ta.1369749 22.2
The proposed observations should be coordinated in a broad sense with the planned XMM-Newton observations. Ideally this would be within the 40-day XMM observing window for each target, but observations within 1 - 2 months can be considered acceptable.Our team (please see https://marcellabrusa.wixsite.com/subways2019/team) includes some of the foremost experts in multiwavelength observations of outflows from active galactic nuclei (AGN), and the theory of their impact on the evolution of their host galaxies. This proposal is only one piece of the study of a large, well defined sample anchored by an approved XMM-Newton large program led by Co-PI Brusa. Other components in addition to this proposal include proposals for high-energy X-ray observations with NuSTAR led by Co-I Bianchi, and ALMA+IRAM observations of associated galaxy-wide molecular outflows led by Co-PI Brusa. In the past 20 years our team has provided significant contributions to the field by characterizing the physical properties of outflows detected at various scales and in various gas phases in AGN and QSOs, both locally and at high redshift, as shown by the several papers coauthored by many of us (e.g. Piconcelli+05, Lanzuisi+12, Maiolino+12, Tombesi+10,13,15, Brusa+15, 18, Cresci+15, Nardini+15, Vignali+15, Cappi+16, Feruglio+17, Dadina+18). Collectively, our team has led or participated in nearly a dozen multiwavelength campaigns resulting in over one hundred publications. Co-PI Mathur was one of the first to make the observational link between X-ray warm absorbers and intrinsic UV absorption lines (NGC 5548: Mathur+95, Mathur+99). PI Kriss and Co-PI Kraemer led some of the earliest coordinated UV and X-ray observations of outflows from many of the nearest bright AGN (NGC 3516: Kriss+96a,b, Kraemer+02; NGC 3783: Gabel+03,05; Mrk 279: Scott+04, Costantini+07; NGC 7469: Kriss+03, Scott+05; NGC 4151: Kraemer+05,06). Various combinations of team members (Bianchi, Costantini, Kaastra, Kraemer, Kriss, Krongold, Petrucci) led or participated in large, successful multiwavelength monitoring campaigns over the past two decades, including NGC 3783, Mrk 279, Mrk 335, Mrk 509, NGC 5548, and NGC 7469. These campaigns have characterized the UV and X-ray variability of these AGN, leading to distance determinations for the warm absorber outflows and their impact on their host galaxies (NGC 3783: Gabel+05; Mrk 509: Kaastra+12, Petrucci+16, Kriss+19; NGC 5548: Arav+15, Kriss+19; NGC 7469: Arav+19). They have also established the new phenomenon of X-ray/UV obscurers, which are characterized by heavy, soft X-ray absorption and fast, broad, blue-shifted UV absorption with speeds intermediate between warm absorbers and ultra-fast outflows (UFOs). Although "obscurers" had been known before and studied by members of our team (NGC 3516: Mathur+97; NGC 4151: Kraemer+05,06), the discovery of unexpected obscuration in AGN with previously "clear" lines of sight was pioneered by many members of our team (NGC 5548: Kaastra+14, Kriss+19; Mrk 335: Longinotti+13,19; NGC 985: Ebrero+16; NGC 3783: Mehdipour+17, Kriss+19). Members of our team have also discovered links between X-ray UFOs and absorption in UV spectra (PG1211+143: Kriss+18a,b). To interpret these observations and place them in the context of the co-evolution of supermassive black holes and their host galaxies (e.g., Gaspari & Sadowski 2017, King 2005, King & Pounds 2015), Co-I Gaspari on this proposal and Co-I King on the XMM-Newton/SUBWAYS program will provide their theoretical expertise as part of our team, including the comparison with high-resolution hydrodynamical simulations leveraging adaptive mesh refinement.
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