Page   1
    PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS   ST ScI Use Only
                                                       ID 4341c
                                                       Report Date: 09-May-96:19:32
                                                       Version: **********
                                                       Check-in Date: **********

1.Proposal Title:
HIGH RESOLUTION OBSERVATIONS OF THE LOW REDSHIFT LY ALPHA  FOREST:CYCLE3 MEDIUM
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2. Scientific Category   3. Proposal For  4. Proposal Type        5. Continuation ID
QUASARS & AGN               GO                                       <none>
Sub Category
QUASAR ABSORPTION
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6. Principal Investigator   Institution                    Country    Telephone
 Vesa T Junkkarinen         CENTER FOR ASTROPHYSICS & SP   USA        619-534-0735

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7. Abstract
We propose high resolution UV spectroscopy of the bright low redshift QSO
KUV18217+64 to study selected absorption systems in the low redshift Lyman ALPHA
forest.  Observations with the G160M grating and GHRS will be used to resolve the
strong Lyman ALPHA and Lyman BETA absorption lines that have been detected in this
QSO at z = 0.214 and z = 0.225.   These observations will be used to determine the
amount of structure within these absorption systems. If the lines do not have
multiple components, then accurate values of the Doppler parameter will be
determined and used to set upper limits to the temperature in these Ly ALPHA clouds.
Ly ALPHA forest clouds are expected to evolve toward cooler temperatures at the
present epoch so these observations could reveal some low temperature clouds.  An
understanding of the physics of Lyman ALPHA clouds is necessary in order to use
observations of these clouds to probe physical conditions in the intergalactic
medium over a wide range of redshift.
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9. Est obs time (hours) pri: 17.13    par: 0       10. Num targs pri: 1      par: 0
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11. Instruments requested:  HRS
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                                                                  Page   2
I. GENERAL FORM    Proposal 4341c
PI:  Vesa T Junkkarinen
Proposal Title:
HIGH RESOLUTION OBSERVATIONS OF THE LOW REDSHIFT LY ALPHA  FOREST:CYCLE3 MEDIUM
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1. Proposers:
Proposers                        Institution                       Country       ESA
------------------------------------------------------------------------------------
Pi Vesa T Junkkarinen            CENTER FOR ASTROPHYSICS & SPACE   USA
                                 SCIENCES
 Ross D Cohen                    CENTER FOR ASTROPHYSICS & SPACE   USA
                                 SCIENCES
 Edward A Beaver                 CENTER FOR ASTROPHYSICS & SPACE   USA
                                 SCIENCES
 Margaret Burbidge               CENTER FOR ASTROPHYSICS & SPACE   USA
                                 SCIENCES
 Paul R Shapiro                  UNIVERSITY OF TEXAS               USA
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  3. Description of proposed observations.
  We will obtain two GHRS UV spectra of the QSO KUV18217+64 with the G160M
 (R=20000 nominal) grating and the Large Science Aperture. One spectrum will cover
 1469 -- 1504 Angstroms (Ly alpha) and the other spectrum will cover 1236 -- 1272
 Angstroms (Ly beta). The Ly alpha spectrum includes four known Ly alpha
 absorption lines (Bahcall et al. 1992). The integration times will be 5.3 hours
 and 6.6 hours, respectively, to provide S/N ratios of 12 at Ly alpha and 15 at Ly
 beta. The exposure times are predicted using the observed flux from the Bahcall
 et al. (1992) UV FOS spectrum of KUV18217+64. The exposures will be broken into
 approximately 5 minute segments to allow for shifting in wavelength to correct
 for geomagnetic and thermal drifts.  Additionally, the 5 minute observations will
 be grouped into exposure logsheet lines approximately 80 minutes long. Each of
 these segments will be preceded by a SPYBAL and a wavelength lamp observation.
 The SPYBALs will correct for drifts perpendicular to the diode array and the
 wavelength lamps will allow us to correct for errors in the thermal and magnetic
 drift models, as well as errors in resetting the carrousel after the SPYBALs.
 The SPYBALs should occur close in time to the observations, but should NOT be
 placed between the wavelength lamp and the observations of the object.
                                                                  Page   3
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  4. Justification of need for HST observations.
  The Lyman lines of the low redshift Ly alpha forest can only be studied from
 space because they occur in the far UV. Observations that spectrally resolve
 these lines take long integration times with HST on the brightest QSOs so these
 observations can only be carried out with HST and GHRS at the present time.
 Previous HST GHRS observations at high resolution on 3C 273 can be analyzed to
 obtain Doppler parameter and column density estimates on weaker lines. But the
 redshift of 3C 273 is too low to measure Ly beta at high resolution for the
 observed Ly alpha lines and the spectrum of 3C 273 does not have any really
 strong isolated Ly alpha absorption lines.   KUV18217+64 at V = 14.2 is the
 second brightest QSO after 3C 273 at z > 0.1.  The redshift of KUV18217+64 is
 0.297 so some Ly alpha clouds detected in absorption against KUV18217+64 can be
 studied in both Ly alpha and Ly beta. FOS observations by Bahcall et al. (1992)
 reveal strong absorption lines at z = 0.214 and 0.225 in both Ly alpha and Ly
 beta. Two observations are needed with the GHRS side 2 and the G160M grating to
 measure both lines.  One spectrum centered at 1486 Angstroms will cover the Ly
 alpha absorption lines at z = 0.214, 0.225, 0.226, 0.228, while the other,
 centered at 1254 Angstroms will cover the corresponding Ly beta lines. Monte
 Carlo simulations using the line spread function published in the GHRS handbook
 for the large science aperture (LSA) were used to estimate the signal to noise
 ratio needed. Repeated chi-squared fits were used to accumulate statistics. A
 Doppler parameter accurate to better than +/- 10% is desirable for comparison
 with high redshift results (for example Carswell et al. 1992). For temperature
 comparisons, an error of 10% in Doppler parameter translates to about a 20% error
 in temperature. Accurate temperature estimates are needed because the models
 predict modest temperature decreases (factors of 1.5 or 2.) from redshift 2.0 to
 0.2. The FOS observed equivalent width for the lambda 1489 line restricts the
 parameter space that must be searched if the lambda 1489 line consists of a
 single component Voigt profile. A S/N ratio of 12 per diode (6 per 1/4 step) is
 sufficient to   measure (at 80% confidence) b values from  the Ly alpha line at
 1489 of 20.0 -1.5/+1.4 km/s and 30.0 -2.7/+1.4 km/s (determined from Monte Carlo
 runs of 200 spectra). At larger b values and lower column densities, the Ly beta
 line provides the better constraint. A S/N ratio of 15 per diode allows the b
 value to be determined to about +/- 4 km/s at b = 60 km/s. For even larger b
 values, either line provides an accurate b value. The observed Ly beta equivalent
 width of 0.53 Angstroms, suggests that either b = 20 km/s or b = 50 km/s for the
 z = 0.225 system given the observed Ly alpha with W_lambda = 0.95 Angstroms, but
 the one sigma uncertainty in the ratio of observed equivalent widths allows a
 wide range of b values: 15 < b < 60 km/s. The integration time calculation
 includes the following assumptions: KUV18217+64 has a flux of 3.5E-14 at 1500 and
 1250 Angstroms (Bahcall et al. 1992), the GHRS side 2 G160M sensitivity is
 4.30E11 at 1500 Angstroms and and 5.03E11 at 1250 Angstroms (GHRS handbook LSA
 aperture), and that the background is an average of 0.011 counts/second/diode
 with the standard burst rejection. Using the above assumptions, the countrate
 predicted is 0.0129 and 0.0151 (counts/second/diode) at 1500 and 1250 Angstroms
 respectively. The required integration time to reach S/N of 12 and 15 per diode
 is then 5.3 hours and 6.6 hours at 1500 and 1250 Angstroms respectively.
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  6. Description of special calibration exposures.
  Because of the large wavelength drifts which will occur over the course of the
 entire observation, periodic measurements of the wavelength scale are required in
 order to reconstruct the spectrum of this faint object. They are also required
 both to check on the accuracy of the carrousel repositioning after the SPYBALs
 and to correct for any errors in the model of thermal and magnetic drift.
                                                                  Page   4
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  7. Data reduction and analysis plans.
  The data will be reduced and analyzed using existing software and computers at
 the PI's home institution. The data reduction will be done using existing
 software to remove background, correct detector sensitivity variations and flux
 the data. Computer programs have already been written for doing the chi-squared
 fitting using a numerical line spread function convolved with a Voigt profile. We
 will use the most accurate available lsf for the GHRS and can numerically
 investigate the additional uncertainty introduced by the approximate nature of
 the lsf. Monte Carlo simulations will be used to estimate the confidence level of
 the parameters determined from each fit. These programs have already been used to
 estimate the S/N required for accurate measurement of the Doppler parameter. The
 best estimate b values and temperature limits will be compared to the predictions
 of models for the Ly alpha forest at low redshift. Additional investigations
 using variations of the existing models or different sets of parameters, will be
 carried out as needed to analyze this data.
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  9. Description of previous HST work.
  Junkkarinen is a member of the FOS GTO team and has worked with GTO data, but he
 is not a Co-investigator. Some of the low resolution spectra obtained with the
 FOS are broadly pertinent to the nature of the low redshift Ly alpha forest.
 There is no direct relation to the goals of this project. Junkkarinen is a co-
 investigator on a program with Brian Espey as PI for archival studies of QSO
 emission lines.   "Far Ultraviolet Spectroscopy of the QSO UM675 with the Faint
 Object Spectrograph on the Hubble Space Telescope," Beaver, E. A., Burbidge, E.
 M., Cohen, R. D., Junkkarinen, V. T., Lyons, R. W., Rosenblatt, E. I., Hartig, G.
 F., Margon, B. H., Davidsen, A. F., ApJ, 377, L1, 1991. "The Ultraviolet
 Absorption Spectrum of 3C 273,", Bahcall, J. N., Januzzi, B. T., Schneider, D.
 P., Hartig, G. F., Bohlin, R., Junkkarinen, V., ApJ, 377, L5, 1991. "The Lyman
 alpha Forest at Low Redshift: FOS Observations of the QSO PG 1211+143,"
 Junkkarinen, V. T., Bartko, F., Beaver, E. A., Burbidge, E. M., Cohen, R. D.,
 Lyons, R. W., Rosenblatt, E. I., Burks, G. S., Harms, R. J., and Henriksen, M.,
 BAAS, 23, 1425, 1991. "Spectroscopy of QSOs with the Faint Object Spectrograph,"
 Beaver, E. A., Burbdige, M., Cohen, R. D., Junkkarinen, V., Lyons, R., and
 Rosenblatt, E., Paper presented by M. Burbidge at the "Science with the Hubble
 Space Telescope" Conference, June 29 -- July 7, 1992, Sardinia, Italy.   "HST-FOS
 and Ground--Based Observations of the Broad Absorption Line Quasar 0226-1024,"
 Korista, K. T., Weymann, R. J., Morris, S. L., Kopko, M., Turnshek, D. A.,
 Hartig, G. F., Foltz, C. B., Burbidge, E. M., and Junkkarinen, V. T., (to appear
 in December 20, 1992 ApJ).
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 10. Resources to be supplied by investigator's institution(s).
  We intend to use existing facilities at our home institutions. We hope to pay a
 graduate student from UCSD to do some of the data analysis and numerical
 simulations that are needed for this project. Computing at UCSD will be done by
 sharing resources with the FOS group and through a recharge-type arrangement with
 CASS.
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11. Address Information
Name:  VESA T JUNKKARINEN                                  Category: PI
Institution: Center for Astrophysics & Space S
Address:  CENTER FOR ASTROPHYSICS AND SPACE SCIENCES, 0111
          9500 GILMAN DRIVE
City: LA JOLLA                                  State: CA
Zip Code: 920930111                             Country: USA
Telephone: 619-534-0735
Telex (or e-mail):
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TARGET LIST    a) Fixed Targets                                                                    ID = 4341c            [  5]
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 1 |     2      |           3           |              4             |  5     |   6    |  7  |              8
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Tar|   Target   |         Target        |            Target          |Coord   | Radial |Acqui|FLX|     Flux data
No |    Name    |       Description     |           Position         |Eqnx    |  Vel.  |Prblm|REF|
   |            |                       |                            |        |        |     |   |
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1   KUV18217+64  E,313,H,515,519         RA = 18H 21M 57.106S +/-     2000     Z=0.297        1   V=14.1 +/- 0.5
                                         0.3",                                                2   F(1500)=3.5 +/- 0.5 E-14
                                         DEC = 64D 20' 36.69" +/-
                                         0.3",
                                         PLATE-ID = 00T0
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EXPOSURE LOGSHEET                                                                                  ID = 4341c            [  6]
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 1      |   2   |      3    |  4   |   5   |   6   |    7   |   8   |       9       |10 |   11  |   12    |13 |14|        15
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  Line  |  Seq  |   Target  |Instr | Oper. | Aper  |Spectral|Central|   Optional    |Num|  Time |   S/N   |Flx|Pr|     Special
 Number | Name  |    Name   |Config| Mode  |or FOV |Element |Waveln.|  Parameters   |Exp|       |Rel. Time|Ref|  |   Requirements
------------------------------------------------------------------------------------------------------------------------------------
1                KUV18217+64 HRS    ACQ     2.0     MIRROR-N2        BRIGHT=RETURN   1   1.8S              1   1  ONBOARD ACQ FOR
                                                                     MAP=DEF                                      1.1
                                                                     SEARCH-SIZE=3                                SEQ 1.0-3.45
                                                                     LOCATE=YES                                   CYCLE 3/1.0-3.45
     Comments: USED 0.2 SEC STEP-TIMES. IF
               THIS PROGRAM IS BROKEN INTO
               PARTS, REPEAT LINES 1.0 AND 1.1
               AS NECESSARY.
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1.1              KUV18217+64 HRS    ACQ/    2.0     MIRROR-N2                        1   20.4S             1   1  ONBOARD ACQ FOR
                                    PEAKUP                                                                        2.0-3.45
     Comments: USED 0.2 SEC STEP-TIMES. THIS
               ACQ REFINES THE CENTERING AFTER
               B-FIELD & THERMAL SHIFTS.
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2                WAVE        HRS    ACCUM   SC2     G160M    1486                    1   DEF                   1  CALIB FOR 2.05 NO
                                                                                                                  SLEW
                                                                                                                  SEQ 2.0-2.05 NO
                                                                                                                  GAP
     Comments: THE Y-BAL. FOR 2.05 SHOULD BE
               DONE PRIOR TO LINE 2.0. DO NOT
               INSERT A SPYBAL AND MOVE
               CAROUSEL BETWEEN LINES 2.0 AND
               2.05. SEQ IS TO OBTAIN A
               WAVELENGTH CAL; W/O DRIFT
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2.05             KUV18217+64 HRS    ACCUM   2.0     G160M    1486    STEP-PATT=3     15  317S    6.5       2   1
                                                                     CENSOR=YES
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2.1              WAVE        HRS    ACCUM   SC2     G160M    1486                    1   DEF                   1  CALIB FOR 2.15 NO
                                                                                                                  SLEW
                                                                                                                  SEQ 2.1-2.15 NO
                                                                                                                  GAP
     Comments: THE Y-BAL. FOR 2.15 SHOULD BE
               DONE PRIOR TO LINE 2.1. DO NOT
               INSERT A SPYBAL AND MOVE
               CAROUSEL BETWEEN LINES 2.1 AND
               2.15. SEQ IS TO OBTAIN A
               WAVELENGTH CAL W/O DRIFT
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2.15             KUV18217+64 HRS    ACCUM   2.0     G160M    1486    STEP-PATT=3     15  317S    6.5       2   1
                                                                     CENSOR=YES
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EXPOSURE LOGSHEET                                                                                  ID = 4341c            [  7]
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 1      |   2   |      3    |  4   |   5   |   6   |    7   |   8   |       9       |10 |   11  |   12    |13 |14|        15
------------------------------------------------------------------------------------------------------------------------------------
  Line  |  Seq  |   Target  |Instr | Oper. | Aper  |Spectral|Central|   Optional    |Num|  Time |   S/N   |Flx|Pr|     Special
 Number | Name  |    Name   |Config| Mode  |or FOV |Element |Waveln.|  Parameters   |Exp|       |Rel. Time|Ref|  |   Requirements
------------------------------------------------------------------------------------------------------------------------------------
2.2              WAVE        HRS    ACCUM   SC2     G160M    1486                    1   DEF                   1  CALIB FOR 2.25 NO
                                                                                                                  SLEW
                                                                                                                  SEQ 2.20-2.25 NO
                                                                                                                  GAP
     Comments: THE Y-BAL. FOR 2.25 SHOULD BE
               DONE PRIOR TO LINE 2.20. DO NOT
               INSERT A SPYBAL AND MOVE
               CAROUSEL BETWEEN LINES 2.2 AND
               2.25. SEQ IS TO OBTAIN A
               WAVELENGTH CAL W/O DRIFT.
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2.25             KUV18217+64 HRS    ACCUM   2.0     G160M    1486    STEP-PATT=3     15  317S    6.5       2   1
                                                                     CENSOR=YES
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2.3              WAVE        HRS    ACCUM   SC2     G160M    1486                    1   DEF                   1  CALIB FOR 2.35 NO
                                                                                                                  SLEW
                                                                                                                  SEQ 2.30-2.35 NO
                                                                                                                  GAP
     Comments: THE Y-BAL. FOR 2.35 SHOULD BE
               DONE PRIOR TO LINE 2.30. DO NOT
               INSERT A SPYBAL AND MOVE
               CAROUSEL BETWEEN LINES 2.30 AND
               2.35. SEQ IS TO OBTAIN A
               WAVELENGTH CAL W/O DRIFT
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2.35             KUV18217+64 HRS    ACCUM   2.0     G160M    1486    STEP-PATT=3     15  317S    6.5       2   1
                                                                     CENSOR=YES
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3                WAVE        HRS    ACCUM   SC2     G160M    1254                    1   DEF                   1  CALIB FOR 3.05 NO
                                                                                                                  SLEW
                                                                                                                  SEQ 3.0-3.05 NO
                                                                                                                  GAP
     Comments: SEQ 3.0-3.05 TO OBTAIN A
               WAVELENGTH CALIB. W/O DRIFT.
               THE Y-BAL FOR 3.05 SHOULD BE
               DONE FROM A WAVELENGTH LAMP
               BEFORE LINE 3.0. DO NOT INSERT
               A SPYBAL AND MOVE CAROUSEL
               BETWEEN LINES 3.0 AND 3.05.
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3.05             KUV18217+64 HRS    ACCUM   2.0     G160M    1254    STEP-PATT=3     15  318S    7         2   1
                                                                     CENSOR=YES
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EXPOSURE LOGSHEET                                                                                  ID = 4341c            [  8]
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 1      |   2   |      3    |  4   |   5   |   6   |    7   |   8   |       9       |10 |   11  |   12    |13 |14|        15
------------------------------------------------------------------------------------------------------------------------------------
  Line  |  Seq  |   Target  |Instr | Oper. | Aper  |Spectral|Central|   Optional    |Num|  Time |   S/N   |Flx|Pr|     Special
 Number | Name  |    Name   |Config| Mode  |or FOV |Element |Waveln.|  Parameters   |Exp|       |Rel. Time|Ref|  |   Requirements
------------------------------------------------------------------------------------------------------------------------------------
3.1              WAVE        HRS    ACCUM   SC2     G160M    1254                    1   DEF                   1  CALIB FOR 3.15 NO
                                                                                                                  SLEW
                                                                                                                  SEQ 3.1-3.15 NO
                                                                                                                  GAP
     Comments: SEQ 3.1-3.15 TO OBTAIN A
               WAVELENGTH CALIB. W/O DRIFT.
               THE Y-BAL FOR 3.15 SHOULD BE
               DONE FROM A WAVELENGTH LAMP
               BEFORE LINE 3.1. DO NOT INSERT
               A SPYBAL AND MOVE CAROUSEL
               BETWEEN LINES 3.1 AND 3.15.
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3.15             KUV18217+64 HRS    ACCUM   2.0     G160M    1254    STEP-PATT=3     15  318S    7         2   1
                                                                     CENSOR=YES
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3.2              WAVE        HRS    ACCUM   SC2     G160M    1254                    1   DEF                   1  CALIB FOR 3.25 NO
                                                                                                                  SLEW
                                                                                                                  SEQ 3.2-3.25 NO
                                                                                                                  GAP
     Comments: SEQ 3.2-3.25 TO OBTAIN A
               WAVELENGTH CALIB. W/O DRIFT.
               THE Y-BAL FOR 3.25 SHOULD BE
               DONE FROM A WAVELENGTH LAMP
               BEFORE LINE 3.2. DO NOT INSERT
               A SPYBAL AND MOVE CAROUSEL
               BETWEEN LINES 3.2 AND 3.25.
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3.25             KUV18217+64 HRS    ACCUM   2.0     G160M    1254    STEP-PATT=3     15  318S    7         2   1
                                                                     CENSOR=YES
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3.3              WAVE        HRS    ACCUM   SC2     G160M    1254                    1   DEF                   1  CALIB FOR 3.35 NO
                                                                                                                  SLEW
                                                                                                                  SEQ 3.3-3.35 NO
                                                                                                                  GAP
     Comments: SEQ 3.3-3.35 TO OBTAIN A
               WAVELENGTH CALIB. W/O DRIFT.
               THE Y-BAL FOR 3.35 SHOULD BE
               DONE FROM A WAVELENGTH LAMP
               BEFORE LINE 3.3. DO NOT INSERT
               A SPYBAL AND MOVE CAROUSEL
               BETWEEN LINES 3.3 AND 3.35.
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3.35             KUV18217+64 HRS    ACCUM   2.0     G160M    1254    STEP-PATT=3     15  318S    7         2   1
                                                                     CENSOR=YES
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EXPOSURE LOGSHEET                                                                                  ID = 4341c            [  9]
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 1      |   2   |      3    |  4   |   5   |   6   |    7   |   8   |       9       |10 |   11  |   12    |13 |14|        15
------------------------------------------------------------------------------------------------------------------------------------
  Line  |  Seq  |   Target  |Instr | Oper. | Aper  |Spectral|Central|   Optional    |Num|  Time |   S/N   |Flx|Pr|     Special
 Number | Name  |    Name   |Config| Mode  |or FOV |Element |Waveln.|  Parameters   |Exp|       |Rel. Time|Ref|  |   Requirements
------------------------------------------------------------------------------------------------------------------------------------
3.4              WAVE        HRS    ACCUM   SC2     G160M    1254                    1   DEF                   1  CALIB FOR 3.45 NO
                                                                                                                  SLEW
                                                                                                                  SEQ 3.4-3.45 NO
                                                                                                                  GAP
     Comments: SEQ 3.4-3.45 TO OBTAIN A
               WAVELENGTH CALIB. W/O DRIFT.
               THE Y-BAL FOR 3.45 SHOULD BE
               DONE FROM A WAVELENGTH LAMP
               BEFORE LINE 3.4. DO NOT INSERT
               A SPYBAL AND MOVE CAROUSEL
               BETWEEN LINES 3.4 AND 3.45.
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3.45             KUV18217+64 HRS    ACCUM   2.0     G160M    1254    STEP-PATT=3     15  318S    7         2   1
                                                                     CENSOR=YES
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            Summary Form for Proposal 4341c                                                                              [ 10]

  Item                          Used in this proposal
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  Configurations                HRS
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  Opmodes                       ACQ ACQ/PEAKUP ACCUM
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  Optional Parameters           BRIGHT MAP SEARCH-SIZE=3 LOCATE=YES STEP-PATT CENSOR
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  Proposal for                  GO
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  S/C Hours                     17.13
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  Scientific Category           QUASARS & AGN
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  Scientific Sub-category       QUASAR ABSORPTION
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  Special Requirements          ONBOARD ACQ FOR 1.1; SEQ 1.0-3.45; CYCLE 3/1.0-3.45; ONBOARD ACQ FOR 2.0-3.45 CALIB FOR 2.05 NO
                                SLEW; SEQ 2.0-2.05 NO GAP; CALIB FOR 2.15 NO SLEW; SEQ 2.1-2.15 NO GAP; CALIB FOR 2.25 NO SLEW; SEQ
                                2.20-2.25 NO GAP; CALIB FOR 2.35 NO SLEW; SEQ 2.30-2.35 NO GAP; CALIB FOR 3.05 NO SLEW; SEQ
                                3.0-3.05 NO GAP; CALIB FOR 3.15 NO SLEW; SEQ 3.1-3.15 NO GAP; CALIB FOR 3.25 NO SLEW; SEQ 3.2-3.25
                                NO GAP; CALIB FOR 3.35 NO SLEW; SEQ 3.3-3.35 NO GAP; CALIB FOR 3.45 NO SLEW; SEQ 3.4-3.45 NO GAP;
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  Spectral Elements             MIRROR-N2 G160M
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  Target Names                  KUV18217+64
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