10125(  5) - 11/07/05 09:00  - [  1]

                  HUBBLE SPACE TELESCOPE OBSERVING PROGRAM 10125

Version: 5    Check-in Time: 07-Nov-2005 14:00:07

Title
Where is the Wind in 1H0707-495?
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Type             Cycle     Parallel Pointing Tolerance
GO               13        <none>
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Investigators
                                                                                     Contact?
    PI: Dr. Karen M. Leighly              University of Oklahoma Norman Campus
   CoI: Mr. Darrin Casebeer               University of Oklahoma Norman Campus          N

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Abstract

We propose three observations using HST STIS of the narrow-line Seyfert 1 galaxy 1H
0707-495 to be coordinated with already-approved deep exposures using FUSE. A
previous HST observation of 1H 0707-495 revealed strongly blueshifted high-
ionization lines, suggesting an origin in an outflowing wind. Detailed
photoionization modeling reveals that the wind line fluxes and ratios are consistent
with two solutions: a high-density, high-column solution, originating close to the
central engine, and a low-density, low-column solution, located much further out.
These two locations, interestingly, correspond to those predicted by two different
physical models for winds in AGNs. We can differentiate between these models by
observing emission line variability on two time scales, and examining relative
variability of OVI obtained by FUSE and CIV and other lines obtained by HST. We will
also look for profile variability, constrain velocity ionization stratification
through a detailed study of the profiles, and investigate metallicity, which has
been suggested to be high in NLS1s. This program, requiring only a modest amount of
time, is expected to make significant contributions to our understanding of outflows
in AGN, and the structure, origin and metallicity of the broad-line region.
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                                                10125(  5) - 11/07/05 09:00  - [  2]

  Observations Description
  ------------------------

     Introduction----------------- We plan three observations of 1H0707-495 using
     HST ACS SBC in spectroscopic mode to be conducted simultaneously with three
     already-approved deep FUSE observations. The FUSE observations are highly time
     constrained by the observing constraints of the satellite (see below). The goal
     to look for variability in flux and profile in the OVI line observed with FUSE,
     and principally the flux in the FUV spectrum observed using the HST ACS. Our
     approach to the data analysis will be to compare the spectra from individual
     epochs of observation to the high SNR combined spectrum from all three
     observations. We will search for line flux and possibly profile variability,
     refine photoionization models presented in Leighly 2004 (ApJ 611, 125), and
     construct a radially-stratified photoionization model, if warranted by the
     emission-line profiles. Coordination with FUSE---------------------------------
     The HST observations should be coordinated with three already-approved FUSE
     monitoring observations. The FUSE observations are highly time constrained for
     the following reason. After the loss of two of the reaction wheels, FUSE is
     limited in the area of the sky that it can observe at any particular time.
     1H0707-495 is a good target for FUSE because its high latitude means that it is
     more accessible than other objects. 1H0707-495 will be available to FUSE for
     three periods each 11--18 days in length between December 2004 to April 2005
     (Table 1). Our science goals require that we observe the target on two
     different time scales. For the shorter time scale, we will observe the object
     at the beginning and the end of one of the longer periods; these two
     observations will be separated by more than three days. For the longer time
     scale, we will observe the object once during one of the other periods; thus it
     will be separated from the other two observations by 2--4 months. Our
     preference would be to do the two observations during the 2005 April window, as
     it is one of the longer periods of visibility, and do the third observation
     during the 2004 December window, to maximize the long interval. Each of the
     FUSE observations is 50 ks in length. FUSE observes with about 30% efficiency;
     this means that each observation will require almost two days of exposure. Each
     HST observation, comprised of one orbit, should be conducted any time within
     that two-day interval. Table 1 -- FUSE Observing Intervals---------------------
     -------------------------------------- Start End Duration (days)---------------
     -------------------------------------------- 2004:12:01:07:57:11
     2004:12:12:08:57:52 11 <== 2005:01:27:13:32:17 2005:02:15:06:00:00 18.7
     2005:03:24:12:00:00 2005:04:11:21:32:59 18.4 <==-------------------------------
     ---------------------------- (the <== mark the preferred windows). Details of
     Observations-------------------------------- The primary science goal of these
     observations is to see whether the CIV flux changes between the observations.
     Therefore, it is essential to have good wavelength calibration and an
     understanding of any potential systematic uncertainties. To obtain good
     wavelength calibration, it is essential that the position of the zeroth order
     image be known. Therefore, we choose to make a short direct imaging SBC
     observation at the beginning of each visit. Bright object limit constraints are
     a concern here. We use the ACS Imaging ETC, using the merged observed Cycle 7
     HST STIS FUV and NUV spectra as input. We find that we cannot use the clear
     filter (F115LP) because the bright object limits are violated by about a factor
     of two. F150LP gives an acceptable rate (30.5 c/s in the brightest pixel);
     however, we worry about variability of the object so deem that filter also
     unacceptable. We finally conclude that only the Lyalpha filter (F122M) predicts
                                                10125(  5) - 11/07/05 09:00  - [  3]

     an acceptably conservative rate of 5.2 counts/second in brightest pixel. This
     is a factor of 10 lower than the local bright object limit maximum. The source
     count rate is 48.8 counts/s and the background rate is 6.6 counts/s, so there
     will be no problem in identifying the position of the source. The predicted
     count rate in the entire detector is 9, 036 counts/s, much smaller than the
     acceptable global count rate of 80, 000 counts/s. A 180 second observation
     should give us a well exposed image. Note that there is no obviously UV-bright
     object in the 32x32 arcsec field of view around 1H0707-495 in the DSS. To
     ameliorate any systematic uncertainty, we use a AC-SBC-DITHER-BOX to sample the
     spectrum on four different places on the detector. We use box sides of 1 and
     1.5 arcseconds, box orientation of 20 degrees, and box side angle of 60
     degrees. The spectra obtained at each of the four points of the box are 623
     second in exposure time. Using the ACS SBC Spectroscopic ETC with the Cycle 7
     HST STIS spectrum as input we find that the count rate in the brightest pixel
     is 4.6 count/s, far below the bright object limit. In 623 seconds, we obtain
     2866 photons in the brightest pixel, so we are far from the full-well capacity
     of the detector (65, 523 counts). In each of these four spectra, the ACS
     spectroscopic ETC predicts a signal-to-noise of between 80 and 120 between 1250
     and 1700 Angstroms.

  Real Time Justification
  -----------------------


  Calibration Justification
  -------------------------


  Additional Comments
  -------------------

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TARGET LIST    Fixed Targets
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Tar|   Target   |         Target        |            Target              |Coord   | Radial |             Flux data
No |    Name    |       Description     |           Position             |Eqnx    |  Vel.  |
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1   1H0707-495   GALAXY, BLR, SEYFERT,   RA=07H08M41.4700S +/- 0.1",      J2000             V = 15.7
                 WIND                    DEC=-49D33'5.80" +/- 0.1",                         B-V=0.32
                                         PLATE-ID=019B                                      U-B=-0.71
                                                                                            F-CONT(2500)=7.4E-15
                                                                                            F-CONT(1400)=1.4E-14
                                                                                            F-LINE(1264)=2.4E-14
                                                                                            F-LINE(2914)=3.0E-15
    Coordinate Source: GSC_SURVEY_PLATE
    Comments: F-CONT(2500), F-CONT(1400) are the observed flux in
              the continuum from previous STIS observation in 1999
              in erg/cm^2/s/Angstrom. F-LINE(1264) is the difference
              in the peak flux of the Lyalpha line, which is the
              brightest line in the FUV, and the continuum under the
              line. F-LINE(2914) is the difference in the peak flux
              in the MgII line, which is the brightest line in the
              NUV, and the continuum under the line.

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Patterns
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Pattern_Number: 1

                    Primary_Pattern                   Secondary_Pattern
Pattern_Type        BOX
Pattern_Purpose     DITHER
Number_Of_Points    4
Point_Spacing       1.5
Line_Spacing        1.0
Coordinate_Frame    POS-TARG
Pattern_Orient      20.0
Angle_Between_Sides 60.0
Center_Pattern      YES

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                                                10125(  5) - 11/07/05 09:00  - [  6]

Visit: 01
     Visit Priority:      <none>
     Visit Requirements:  <none>
     On Hold Comments:    <none>
     Additional Comments: This observation should be coordinated with the first of the three FUSE
                          observations. The FUSE observation should span a time period of about 2
                          days. The HST observation should be done at some time during the FUSE
                          observation. Ideally, that first FUSE observation will be done sometime
                          during the first window that the target is available to FUSE:
                          2004:12:01:07:57:11 2004:12:12:08:57:52.


Exposures
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Exp |   Target  | Instr  | Oper. | Aper    |Spectral|Central|           Optional           |Num|   Time   |       Special
Num |    Name   | Config | Mode  | or FOV  |Element |Waveln.|          Parameters          |Exp|          |     Requirements
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1    1H0707-495  ACS/SBC  ACCUM   SBC       F122M                                           1   180 S
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2    1H0707-495  ACS/SBC  ACCUM   SBC       PR130L                                          1   593 S      PATTERN 1 2
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Sub Exposures
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Target             | Exp |Instr   | Oper. |  Aper  |Spectral|Cent.|Primary     |Secondary   |Iteration |CR-SPLIT  |Orbit  |Duration
Name               | Num |Config  | Mode  | or FOV |Element |Wave.|Pattern Pos |Pattern Pos |Num       |Num       |Number |
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1H0707-495          1     ACS/SBC  ACCUM   SBC      F122M          none         none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         1            none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         2            none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         3            none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         4            none         none       none       1       N/A
                                                10125(  5) - 11/07/05 09:00  - [  7]

Visit: 02
     Visit Priority:      <none>
     Visit Requirements:  <none>
     On Hold Comments:    <none>
     Additional Comments: This observation should be coordinated with the second of the three FUSE
                          observations. The FUSE observation should span a time period of about 2
                          days. The HST observation should be done at some time during the FUSE
                          observation. Ideally, that second FUSE observation will be done sometime
                          near the beginning of the third window that the target is available to FUSE:
                          2005:03:24:12:00:00 2005:04:11:21:32:59.


Exposures
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Exp |   Target  | Instr  | Oper. | Aper    |Spectral|Central|           Optional           |Num|   Time   |       Special
Num |    Name   | Config | Mode  | or FOV  |Element |Waveln.|          Parameters          |Exp|          |     Requirements
------------------------------------------------------------------------------------------------------------------------------------
1    1H0707-495  ACS/SBC  ACCUM   SBC       F122M                                           1   180 S
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2    1H0707-495  ACS/SBC  ACCUM   SBC       PR130L                                          1   623 S      PATTERN 1 2
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Sub Exposures
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Target             | Exp |Instr   | Oper. |  Aper  |Spectral|Cent.|Primary     |Secondary   |Iteration |CR-SPLIT  |Orbit  |Duration
Name               | Num |Config  | Mode  | or FOV |Element |Wave.|Pattern Pos |Pattern Pos |Num       |Num       |Number |
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1H0707-495          1     ACS/SBC  ACCUM   SBC      F122M          none         none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         1            none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         2            none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         3            none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         4            none         none       none       1       N/A
                                                10125(  5) - 11/07/05 09:00  - [  8]

Visit: 03
     Visit Priority:      <none>
     Visit Requirements:  AFTER 02 BY 3 D TO 11 D
     On Hold Comments:    <none>
     Additional Comments: This observation should be coordinated with the third of the three FUSE
                          observations. The FUSE observation should span a time period of about 2
                          days. The HST observation should be done at some time during the FUSE
                          observation. Ideally, that third FUSE observation will be done sometime
                          during the third window that the target is available to
                          FUSE:2005:03:24:12:00:00 2005:04:11:21:32:59.


Exposures
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Exp |   Target  | Instr  | Oper. | Aper    |Spectral|Central|           Optional           |Num|   Time   |       Special
Num |    Name   | Config | Mode  | or FOV  |Element |Waveln.|          Parameters          |Exp|          |     Requirements
------------------------------------------------------------------------------------------------------------------------------------
1    1H0707-495  ACS/SBC  ACCUM   SBC       F122M                                           1   180 S
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2    1H0707-495  ACS/SBC  ACCUM   SBC       PR130L                                          1   623 S      PATTERN 1 2
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Sub Exposures
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Target             | Exp |Instr   | Oper. |  Aper  |Spectral|Cent.|Primary     |Secondary   |Iteration |CR-SPLIT  |Orbit  |Duration
Name               | Num |Config  | Mode  | or FOV |Element |Wave.|Pattern Pos |Pattern Pos |Num       |Num       |Number |
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1H0707-495          1     ACS/SBC  ACCUM   SBC      F122M          none         none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         1            none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         2            none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         3            none         none       none       1       N/A
1H0707-495          2     ACS/SBC  ACCUM   SBC      PR130L         4            none         none       none       1       N/A
                                                10125(  5) - 11/07/05 09:00  - [  9]

            Summary Form for Proposal  10125

  Item                         Used in this proposal
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  Apertures                    SBC
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  Configurations               ACS/SBC
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  Opmodes                      ACCUM
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  Special Requirements         PATTERN 1 2; AFTER 02 BY 3 D TO 11 D;
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  Spectral Elements            F122M PR130L
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  Target Names                 1H0707-495
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