8346( 11) - 05/09/00 10:33  - [  1]

    PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS   ST ScI Use Only
                                                       ID:      8346
                                                       Version: 11
                                                       Check-in Date: 09-May-2000
                                                                      10:32:43

1.Proposal Title:
Cosmological Parameters from Type Ia Supernovae at High Redshift
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2. Proposal For  3. Cycle
GO               8
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4. Investigators
                                                                                     Contact?
    PI: Saul Perlmutter                   University of California - Berkeley
   CoI: Prof. Reynald Pain                IN2P3-CNRS, Paris                             N
   CoI: Dr. Nino Panagia                  Space Telescope Science Institute             N
   CoI: Dr. Greg Aldering                 Lawrence Berkeley Laboratory                  N
   CoI: Prof. Richard Ellis               Institute of Astronomy, Cambridge             N
   CoI: Dr. Andrew Fruchter               Space Telescope Science Institute             N
   CoI: Prof. Gerson Goldhaber            Lawrence Berkeley Laboratory                  N
   CoI: Prof. Ariel Goobar                University of Stockholm                       N
   CoI: Dr. Don Groom                     Lawrence Berkeley Laboratory                  N
   CoI: Dr. Isobel Hook                   European Southern Observatory                 N
   CoI: Dr. Robert Knop                   Lawrence Berkeley Laboratory                  N
   CoI: Dr. Richard McMahon               Institute of Astronomy, Cambridge             N
   CoI: Dr. Peter Nugent                  Lawrence Berkeley Laboratory                  Y

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5. Abstract

HST can directly measure the cosmological parameters, Omega, Lambda, and thus the
curvature, Omega_k, using Type Ia supernovae (SNe Ia) as calibrated standard
candles. Observations of SNe Ia spanning a large redshift range are key to
decoupling Omega and Lambda. For Cycle 7 and Cycle 7-NICMOS we proposed a
measurement of Omega and Lambda with uncertainty ~11\ at z~0.5 and six at z~0.8 with
WFPC and NICMOS; we have since embarked on this program and the results have more
than met our expectations. We now propose to extend this successful project to study
five additional SNe Ia between z~0.85 and z~1.2. Measurement of these additional
high redshift SNe will dramatically shrink the major-axis of our current error
ellipse in the Omega_M---Lambda plane, and unambiguously determine whether the
universe contains a significant vacuum energy density as our current results
strongly suggest. Results of these proposed observations will further give the first
real limits on whether the universe is spatially flat. These data will test for
evolution in the properties of SNe Ia since it should be difficult for evolution to
alter corrected peak magnitudes with 15\ the redshift range 0<z<1.2.
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  Observations Description
  ------------------------

     noindent The Need for HST: The most important sources of uncertainty in
     measuring high-redshift SN can be alleviated by HST. They are: noindent Host
     galaxy background. As Fig. 4 shows, HST images have exquisite angular
     resolution and a stable PSF which guarantees a reliable measurement of any
     small amount of host light that remains under the SN. This is a serious problem
     for ground-based observations because at high--z the PSF and host size are
     comparable, and PSF variations require the subtraction of different amounts of
     host light. A host subtraction error affects the SN photometry least at peak,
     distorting the lightcurve width and therefore the brightness calibration. HST
     data largely avoids this source of error. noindent Extinction. Less then 25
     exhibit significant host-galaxy extinction, and no SNe Ia in ellipticals show
     evidence of extinction. Indeed, our current results (Perlmutter Etal 1998b) are
     the same with or without extinction correction (or width-luminosity correction
     for that matter) since any mean extinction (which is small for our data) is
     simply absorbed by the normalization. Extinction correction does decrease the
     intrinsic dispersion and we consider it important to obtain color as a check on
     shifts in the mean amount of reddening between our current z~0.1 and z~0.5 SNe
     and those proposed here. This allows us to check for any systematic bias in the
     shape of the SNe Ia Hubble diagram due to extinction. Given the large values of
     total- to-selective extinction (5.1 for U-B, 4.1 for B-V), accurate colors are
     necessary to correct for extinction without producing large uncertainties in
     the final measurements. Based on our current HST data, in a fraction of cases
     the HST images will reveal an E/S0 host or a large galacto-centric distance for
     the SN, allowing a subset analysis of SNe Ia without extinction. Optimal
     Redshift Distribution for Measurement of Omega_M, Omega_Lambda, and Omega_k:
     Wide-area detectors on large telescopes at sites with excellent seeing now make
     possible the efficient discovery of SNe Ia out to z~1.4. We have therefore
     optimized the redshift distribution of these proposed HST observations to best
     separate Omega_M, Omega_Lambda using 1.4 as an upper redshift limit, and
     including extra weight for redshifts were cross-filter K- corrections are
     small. Our calculations, (see Figs. 3c & 3d) show that z~1.2 SNe Ia make the
     greatest improvement over our current results (Figs. 3a & 3b). Spectroscopic
     confirmation of such SNe is challenging, even with Keck, so only about ~10 good
     SNe Ia at z\gs0.85 (~4 at z~1.2) can be harvested per year. When adding this
     additional constraint we find that observing three z~0.85 and two z~1.2 SNe Ia
     offers the best approach to improving our measurement of Omega_M, Omega_Lambda
     in the timeframe of Cycle 8. Based on the success of these proposed
     observations we would place more emphasis on SNe Ia at 1.2<z<1.4 in the future.
     As in past cycles the actual SNe redshifts approximate our target redshift
     distribution, since we use extra information after the SNe are discovered
     (distance from host, how early the discovery, etc.) to optimize the final
     results. Optimal Sampling of the Lightcurves: We plan to observe the 5 SNe with
     WFPC2 at five epochs soon after discovery. Observations of the z~ 0.85 SNe will
     be separated by 15+/-1 days, and those of the z~1.2 SNe will increase to 18+/-1
     days to account for the increased time-dilation. After the SNe have faded,
     observations will be made of their host galaxies to obtain a baseline point.
     Our extensive Monte Carlo tests of this sampling strategy on sample light
     curves (randomized with respect to discovery date) show this timing to be close
     to optimal for a given amount of observing time. In particular if follow-up
     commences within seven (observer) days of discovery, observations evenly
     distributed over the ~ 60 day period (~30 days in the SN rest frame) are
     optimal to parameterize the light curve. Four epochs sampled over the peak of
     the light curve are the bare minimum because three data points determine the
     peak and four data points determine the width of the light curve. As we have
     found for our current HST data, it is necessary to have five data points over
     the light curve peak to provide the additional degree of freedom needed to
     measure the dispersion (also allowing a potential test for lightcurve
     evolution). noindent Host Galaxy Extinction Corrections: As discussed earlier
     we want accurate reddening values for these SNe. For z\gs0.75 SNe NICMOS had
     provided the rest-frame V photometry most often used for measuring SN host-
     galaxy extinction. Our continuing work developing template U-band lightcurves
     (including our upcoming campaign to find ~30 nearby SNe Ia and obtain detailed
     spectroscopic and photometric follow-up) indicates that U-band lightcurves are
     excellent surrogates for the more commonly used B-band, and that U-B can be
     used in place of B- V. Therefore, for SNe Ia at z~0.85 we will use WFPC2 R and
     I photometry to determine rest-frame B-band luminosities, corrected for host
     galaxy extinction using rest-frame U-B. WFPC2 I-band photometry will provide
     the rest-frame U-band luminosities for the z~1.2 SNe Ia. AO systems now under
     construction at both Keck and VLT1 will allow single-epoch measures of SN rest-
     frame B and V colors at maximum light during Cycle 8 (and in fact should be
     sensitive enough to provide fainter lightcurve points). Choice of Filters: Our
     filters are chosen to cover the rest-frame UBV spectral region --- where SNe Ia
     are brightest and for which there is extensive comparison data from nearby SNe
     Ia --- for redshifts such that cross-filter K-corrections are small. For SNe Ia
     at z~0.85 the WFPC2 F675W and F814W detector+filter combinations are good
     matches to redshifted U and B, respectively. For SNe Ia at z~1.2 the
     combination WFPC2+F814W is a good match to redshifted U. noindent Choice of
     Exposure: In Perlmutter Etal\ 1998b we find peak magnitudes of I~23.5 for SNe
     Ia at z~0.85, and for our best- fit flat universe we expect I~24.4 for SNe Ia
     at z~ 1.2. To achieve the requisite 0.11 mag accuracy after width- brightness
     correction and extinction correction requires 3 photometry at five epochs over
     the critical portion of the lightcurve spanning -7 to +25 rest-frame days
     around peak brightness. (Since most of the final uncertainty comes from the
     extinction correction determined from the colors, only uncertainties
     uncorrelated between the R and I observations enter into this error component).
     From our current HST data we know that total integration of one orbit per epoch
     for SNe Ia in both F675W and F814W at z~0.85 will achieve the required
     photometric accuracy. The z~1.2 SNe Ia will be observed in F814W and will
     require one orbit per epoch near maximum and two orbits for the last two
     epochs. For integration times of 1/2 orbit per image the SN photon noise will
     dominate the noise budget. Although at maximum the exposures are slightly
     longer than needed to obtain the desired photon signal-to-noise ratio, these
     slightly longer exposures will have the important benefit of reducing
     systematic uncertainties from CTE and ``long versus short'' effects at all
     epochs by raising the background. All SNe Ia will require one final reference
     image in each band. These observations are not time-critical so initial final
     reference images will require one orbit each --- if there is indication of
     possible host contamination one or two additional orbits will be necessary.
     Synopsis: In summary, 12 orbits each are requested for WFPC2 R-band and I-band
     observations of three high--z (z~0.85) SNe Ia, and 11 orbits each are requested
     for WFPC2 I-band observations of two even higher redshift (z~1.2) SNe Ia. This
     results in a total request of 58 orbits, including lightcurve and final
     reference images. Only HST can provide the deep imaging at high spatial
     resolution with a stable PSF needed to accurately measure intrinsic
     luminosities and colors for high--z SNe and determine the cosmological
     parameters.

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

     None. Our search strategy guarantees the date of SNe discovery, their
     lightcurve phase, their redshift range (0.85--- 1.2) and even the possible sets
     of coordinates. Thus we specify our observing plan well in advance of the
     actual discovery of the new SNe. Except for exact coordinates, we provide the
     detailed observing plan as soon as the proposal is approved. Based on past
     results, our search campaigns should discover >10 SNe with z\gs0.8 during Cycle
     8. The supernova searches will use the CFHT12K CCD mosaic on the CFHT.
     Supernova search observations of a few hours each night will be embedded in
     week-long observing runs, making them quite robust against inclement weather.
     Optical/NIR spectroscopic follow-up will be obtained at Keck and VLT1. J-band
     observations will also be obtained once AO systems are in place at these
     facilities (expected at Keck by mid-1999). However, only the HST can provide
     the low background (including the host) and stable PSF needed to accurately
     determine the lightcurve shape and SN extinction for such distant SNe. Our
     search technique works as follows: Just after new moon, we observe many high-
     galactic-latitude fields using a wide-field CCD array on a 4-meter class
     telescope. Just before the following new moon, we observe the same fields
     again. Examination of the tens of thousands of high redshift galaxies yields ~
     twenty SNe on the rising part of their lightcurves. Preliminary analysis of all
     the images is completed within hours of the observations, and follow-up
     photometry and spectroscopy begin immediately. All SNe with z > 0.35 discovered
     with this technique have been SNe Ia, and we have followed more than 60 SNe
     selected from a larger pool of SNe discovered to date, including 12 using HST.
     The scheduled nature of the SNe discoveries means that HST follow-up can be
     scheduled in advance, as required for efficient use of HST.

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


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

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  Data Distribution

  Paper Products:  YES
  Media:           8MM
  Blocking Factor: 10
  Ship To:         PI_Address
  Ship Via:
  Email:
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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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888 EARLY1       EXT-STAR, SUPERNOVA     RA=14H 01M 10.27S +/- 0.01S,     J2000    Z = 1.2  R = 26.0+/-2.0
                 TYPE IA                 DEC=5D 0' 0" +/- 0.5"                              R-I = 1.0+/-1.0

889 EARLY2       EXT-STAR, SUPERNOVA     RA=14H 01M 10.27S +/- 0.01S,     J2000    Z = 1.2  R = 26.0+/-2.0
                 TYPE IA                 DEC=5D 0' 0" +/- 0.5"                              R-I = 1.0+/-1.0

890 EARLY3       EXT-STAR, SUPERNOVA     RA=14H 01M 10.27S +/- 0.01S,     J2000    Z = 1.2  R = 26.0+/-2.0
                 TYPE IA                 DEC=5D 0' 0" +/- 0.5"                              R-I = 1.0+/-1.0

891 EARLY4       EXT-STAR, SUPERNOVA     RA=14H 01M 10.27S +/- 0.01S,     J2000    Z = 1.2  R = 26.0+/-2.0
                 TYPE IA                 DEC=5D 0' 0" +/- 0.5"                              R-I = 1.0+/-1.0

900 BIG1         EXT-STAR, SUPERNOVA     RA=14H 01M 10.27S +/- 0.01S,     J2000    Z = 1.2  R = 26.0+/-2.0
                 TYPE IA                 DEC=5D 0' 0" +/- 0.5"                              R-I = 1.0+/-1.0

901 BIG2         EXT-STAR, SUPERNOVA     RA=14H 01M 10.27S +/- 0.01S,     J2000    Z = 1.2  R = 26.0+/-2.0
                 TYPE IA                 DEC=5D 0' 0" +/- 0.5"                              R-I = 1.0+/-1.0

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1        EARLY4      WFPC2  IMAGE   PC1     F814W            ATD-GAIN=7,CR-SPLIT=DEF           1   2200.00 EXPAND MAX DUR 200%
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Exposure|   Target  |Instr | Oper. | Aper  |Spectral|Central|             Optional            |Num|  Time |       Special
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1        BIG2        WFPC2  IMAGE   PC1     F814W            ATD-GAIN=7,CR-SPLIT=DEF           1   2200.00 EXPAND MAX DUR 200%
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Exposure|   Target  |Instr | Oper. | Aper  |Spectral|Central|             Optional            |Num|  Time |       Special
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1        BIG1        WFPC2  IMAGE   PC1     F814W            ATD-GAIN=7,CR-SPLIT=DEF           1   600.00  EXPAND MAX DUR 200%
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2        BIG1        WFPC2  IMAGE   PC1     F675W            ATD-GAIN=7,CR-SPLIT=DEF           1   600.00  EXPAND MAX DUR 200%
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4        BIG1        WFPC2  IMAGE   PC1     F814W            ATD-GAIN=7,CR-SPLIT=DEF           1   600.00  EXPAND MAX DUR 200%
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5        BIG1        WFPC2  IMAGE   PC1     F675W            ATD-GAIN=7,CR-SPLIT=DEF           1   600.00  EXPAND MAX DUR 200%
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6        BIG1        WFPC2  IMAGE   PC1     F555W            ATD-GAIN=7,CR-SPLIT=DEF           1   400.00  EXPAND MAX DUR 200%
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3        BIG1        WFPC2  IMAGE   PC1     F555W            ATD-GAIN=7,CR-SPLIT=DEF           1   400.00  EXPAND MAX DUR 200%
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4        BIG1        WFPC2  IMAGE   PC1     F814W            ATD-GAIN=7,CR-SPLIT=DEF           1   600.00  EXPAND MAX DUR 200%
------------------------------------------------------------------------------------------------------------------------------------
5        BIG1        WFPC2  IMAGE   PC1     F675W            ATD-GAIN=7,CR-SPLIT=DEF           1   600.00  EXPAND MAX DUR 200%
------------------------------------------------------------------------------------------------------------------------------------
6        BIG1        WFPC2  IMAGE   PC1     F555W            ATD-GAIN=7,CR-SPLIT=DEF           1   400.00  EXPAND MAX DUR 200%
------------------------------------------------------------------------------------------------------------------------------------
                                                8346( 11) - 05/09/00 10:33  - [ 19]

Visit: 57
     Visit Priority:      <none>
     Visit Requirements:  SCHED 100% AFTER 55 BY 26D to 28D
     On Hold Comments:    <none>
     Additional Comments: <none>


Exposures
------------------------------------------------------------------------------------------------------------------------------------
Exposure|   Target  |Instr | Oper. | Aper  |Spectral|Central|             Optional            |Num|  Time |       Special
 Number |    Name   |Config| Mode  |or FOV |Element |Waveln.|            Parameters           |Exp|       |     Requirements
------------------------------------------------------------------------------------------------------------------------------------
1        BIG1        WFPC2  IMAGE   PC1     F814W            ATD-GAIN=7,CR-SPLIT=DEF           1   800.00  EXPAND MAX DUR 200%
------------------------------------------------------------------------------------------------------------------------------------
2        BIG1        WFPC2  IMAGE   PC1     F675W            ATD-GAIN=7,CR-SPLIT=DEF           1   1000.00 EXPAND MAX DUR 200%
------------------------------------------------------------------------------------------------------------------------------------
                                                8346( 11) - 05/09/00 10:33  - [ 20]

Visit: 58
     Visit Priority:      <none>
     Visit Requirements:  SCHED 100% AFTER 55 BY 38D to 40D
     On Hold Comments:    <none>
     Additional Comments: <none>


Exposures
------------------------------------------------------------------------------------------------------------------------------------
Exposure|   Target  |Instr | Oper. | Aper  |Spectral|Central|             Optional            |Num|  Time |       Special
 Number |    Name   |Config| Mode  |or FOV |Element |Waveln.|            Parameters           |Exp|       |     Requirements
------------------------------------------------------------------------------------------------------------------------------------
1        BIG1        WFPC2  IMAGE   PC1     F814W            ATD-GAIN=7,CR-SPLIT=DEF           1   2200.00 EXPAND MAX DUR 200%
------------------------------------------------------------------------------------------------------------------------------------
2        BIG1        WFPC2  IMAGE   PC1     F675W            ATD-GAIN=7,CR-SPLIT=DEF           1   2200.00 EXPAND MAX DUR 200%
------------------------------------------------------------------------------------------------------------------------------------
                                                8346( 11) - 05/09/00 10:33  - [ 21]

Visit: 59
     Visit Priority:      <none>
     Visit Requirements:  SCHED 100% AFTER 55 BY 52D to 54D
     On Hold Comments:    <none>
     Additional Comments: <none>


Exposures
------------------------------------------------------------------------------------------------------------------------------------
Exposure|   Target  |Instr | Oper. | Aper  |Spectral|Central|             Optional            |Num|  Time |       Special
 Number |    Name   |Config| Mode  |or FOV |Element |Waveln.|            Parameters           |Exp|       |     Requirements
------------------------------------------------------------------------------------------------------------------------------------
1        BIG1        WFPC2  IMAGE   PC1     F814W            ATD-GAIN=7,CR-SPLIT=DEF           1   2200.00 EXPAND MAX DUR 200%
------------------------------------------------------------------------------------------------------------------------------------
2        BIG1        WFPC2  IMAGE   PC1     F675W            ATD-GAIN=7,CR-SPLIT=DEF           1   2200.00 EXPAND MAX DUR 200%
------------------------------------------------------------------------------------------------------------------------------------
                                                8346( 11) - 05/09/00 10:33  - [ 22]

            Summary Form for Proposal  8346

  Item                         Used in this proposal
------------------------------------------------------------------------------------------------------------------------------------
  Apertures                    PC1
------------------------------------------------------------------------------------------------------------------------------------
  Configurations               WFPC2
------------------------------------------------------------------------------------------------------------------------------------
  Opmodes                      IMAGE
------------------------------------------------------------------------------------------------------------------------------------
  Optional Parameters          ATD-GAIN=7 CR-SPLIT=DEF
------------------------------------------------------------------------------------------------------------------------------------
  Proposal Category            GO
------------------------------------------------------------------------------------------------------------------------------------
  Special Requirements         SCHED 100% BETWEEN 8-May-2000 00 00 00 AND 8-May-2000 23 59 59 SCHED 100% BETWEEN 8-May-2000 00 00
                               00 AND 8-May-2000 23 59 59 EXPAND MAX DUR 200% SCHED 100% BETWEEN 8-May-2000 00 00 00 AND
                               8-May-2000 23 59 59 SCHED 100% BETWEEN 8-May-2000 00 00 00 AND 8-May-2000 23 59 59 SCHED 100%
                               BETWEEN 15-May-2000 00 00 00 AND 15-May-2000 23 59 59 SCHED 100% AFTER 5 BY 11D TO 13D SCHED 100%
                               AFTER 5 BY 23D to 25D SCHED 100% AFTER 5 BY 35D to 37D SCHED 100% BETWEEN 15-May-2000 00 00 00 AND
                               15-May-2000 23 59 59 SCHED 100% AFTER 9 BY 11D to 13D SCHED 100% AFTER 9 BY 23D to 25D SCHED 100%
                               AFTER 9 BY 35D to 37D SCHED 100% BETWEEN 15-May-2000 00 00 00 AND 15-May-2000 23 59 59 SCHED 100%
                               AFTER 55 BY 11D TO 13D SCHED 100% AFTER 55 BY 26D to 28D SCHED 100% AFTER 55 BY 38D to 40D SCHED
                               100% AFTER 55 BY 52D to 54D
------------------------------------------------------------------------------------------------------------------------------------
  Spectral Elements            F814W F675W F555W
------------------------------------------------------------------------------------------------------------------------------------
  Target Names                 EARLY1 EARLY2 EARLY3 EARLY4 BIG1 BIG2
------------------------------------------------------------------------------------------------------------------------------------