! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template
! $Id: 5813,v 1.1 1994/12/14 19:43:31 pepsa Exp $
!
! Refer to the HST Phase II Proposal Instructions to fill this out
!
! Anything after a "!" is ignored, and may be deleted
!
! All keywords with multiple entries are comma delimited except the
! Visit_Requirements and Special_Requirements keywords which can be
! delimited with carriage returns or semi-colons, but not commas
!
! For help call your Program Coordinator: n/a
! Phone: n/a , E-mail: n/a
!
! This partially completed template was generated from a Phase I proposal.
! Name of Phase I Proposal: szalay-568.prop
! Date generated: Wed Dec 14 14:43:24 EST 1994
!
Proposal_Information ! Section 4
Title: Revealing the Universe on Gigaparsec
Scales: The Power Spectrum of QSO
Absorption Line Systems
Proposal_Category: AR
Scientific_Category: Quasars
Cycle: 5
Investigators
PI_name: Alexander Szalay
PI_Institution: Johns Hopkins University
CoI_Name: Michael Vogeley
CoI_Institution: Johns Hopkins University
Contact: ! Y or N (designate at most one contact)
CoI_Name: Andrew Connolly
CoI_Institution: Johns Hopkins University
Contact: ! Y or N (designate at most one contact)
CoI_Name: Thomas Broadhurst
CoI_Institution: Johns Hopkins University
Contact: ! Y or N (designate at most one contact)
Abstract: ! Free format text (please update)
Between the wavelength scales corresponding to the anisotropy
detected by COBE and the scales probed by current galaxy
redshift surveys lies an order of magnitude gap in our
knowledge of large-scale clustering in the universe. To
measure power on the missing scales, we propose to analyze the
spatial distribution of QSO absorption line systems from
archival HST spectra. These absorption systems probe a much
larger volume than any of the galaxy surveys, with almost
isotropic coverage. The different species of absorbers (Ly-
alpha vs. metals) measure different aspects of the intervening
mass distribution and may exhibit different clustering
properties and cross-correlation with deep galaxy samples.
Applying innovative statistical tools, we will measure the
large-scale 3D power spectrum of the Ly-alpha absorbers,
taking advantage of the isotropy of the quasar sample, and the
cross-correlation power spectra (1D and 3D) between the Ly-
alpha, metal systems, and normal galaxies of our existing deep
redshift surveys, to elucidate the physical relationship of
these systems.
Questions ! Free format text (please update)
Observing_Description:
Real_Time_Justification:
Calibration_Justification: ! Move appropriate text from Real_Time_Justification
Additional_Comments:
Fixed_Targets ! Section 5.1
Target_Number:
Target_Name:
Alternate_Names:
Description:
Position: ! Most common specification format is
! RA=0H 0M 0.00S +/- 0S,
! DEC=0D 0' 0.0" +/- 0",
! PLATE-ID=0000
Equinox:
RV_or_Z:
RA_PM: ! Units are seconds of time per year
Dec_PM: ! Units are seconds of arc per year
Epoch:
Annual_Parallax:
Flux: ! Include at least V and B-V
Comments:
Solar_System_Targets ! Section 5.2
Target_Number:
Target_Name:
Description:
Level_1: ! Satellite of Sun
Level_2: ! Satellite of Level_1
Level_3: ! Satellite of Level_2
Window:
Flux: ! Include at least V and B-V
Comments:
Generic_Targets ! Section 5.3
Target_Number:
Target_Name:
Description:
Criteria:
Flux:
Comments:
Scan_Data ! Appendix B
Scan_Number:
FGS_Scan:
Cont_or_Dwell:
Dwell_Points:
Dwell_Secs:
Scan_Width:
Scan_Length:
Sides_Angle:
Number_Lines:
Scan_Rate:
First_Line_PA:
Scan_Frame:
Length_Offset:
Width_Offset:
! This is a template for a single visit containing a single exposure
! Repeat exposure and visit blocks as needed
Visits ! Section 6
Visit_Number:
Visit_Requirements: ! Section 7.1
! Uncomment or copy visit level special requirements needed
! Most of these requirements (including ORIENT) will limit scheduling
! PCS MODE [Fine | Gyro]
! GUIDing TOLerance <angle>
! ORIENTation <angle1> TO <angle2>
! ORIENTation <angle1> TO <angle2> FROM <visit>
! ORIENTation <angle1> TO <angle2> FROM NOMINAL
! SAME ORIENTation AS <visit>
! CVZ
! PARallel
! AFTER <visit> [BY <time1> [TO <time2>]]
! AFTER <date>
! BEFORE <date>
! BETWEEN <date1> AND <date2>
! GROUP <visit-list> WITHIN <time>
! PERIOD <time> AND ZERO-PHASE <date>
! SEQ <visit-list> WITHIN <time>
! ON HOLD [FOR <visit>]
On_Hold_Comments:
Visit_Comments:
Exposure_Number: ! Section 6.5
Target_Name:
Config:
Opmode:
Aperture:
Sp_Element:
Wavelength:
Optional_Parameters:
Number_of_Iterations:
Time_Per_Exposure:
Special_Requirements: ! Section 7.2
! Uncomment or copy exposure level special requirements needed
! INTeractive ACQuisition FOR <exp-list>
! ONBOARD ACQuisition FOR <exp-list>
! POSition TARGet <x-value>,<y-value>
! SAME POSition AS <exp>
! DO FOR TARGets <targ-list> ! FGS only
! PARallel WITH <exp>
! GROUP-FGS <exp-list> WITHIN <time>
! SPATIAL SCAN <#> [<exp-list> | SINGLE-EXP ]
! RT ANALYSIS [FOR <exp-list>]
! REQuires UPLINK
! DARK TIME
! END ORBIT
! EXPAND
! MAXimum DURation [<time> | <%>]
! MINimum DURation [<time> | <%>]
! NO SPLIT
! PHASE <number1[0,1]> TO <number2[0,1]>
! SEQuence <exp-list> NON-INTerruptible
Comments:
Data_Distribution ! Defaults indicated; change if desired
Medium: 8MM ! 8MM or 6250BPI or 1600BPI
Blocking_Factor: 10 ! 10 or 1
! Only astronomers with very old 9-
! track tape drives should consider
! a blocking factor of 1
Ship_To: PI_Address ! STSCI or PI_Address or <free-text>
! PI Address from Phase I is:
!
! Department of Physics and Astro
! nomy,3400 N. Charles Street ,
! Baltimore, MD 21218
!
!
Ship_Via: UPS ! UPS (2-day) or OVERNIGHT
! Overnight shipping done at PI expense
Recipient_Email: ! Needed if Ship_To: is not PI_Address
! <free-text>
! Let us know what you think of this template and software!
! Please send a list of your likes and dislikes to your Program Coordinator