! Proposal 6428, submission 1
! PI: Paolo Battinelli
! Received Tue Feb 13 10:24:52 EST 1996
! From: marconi@susy.mporzio.astro.it
!  +====================+
!  | PED OUTPUT PRODUCT |
!  +====================+
!
!  /SUSY/u/marconi/p/p2/1515.prop
!  Generated by PREPROCESSOR, version 6.0e
!  Date: Mon Feb 12 11:26:15 MET 1996

Proposal_Information
              Title: The nature of the density cusp in the core of Ursa Minor
  Proposal_Category: GO
Scientific_Category: GALAXIES & CLUSTERS
              Cycle: 6


Investigators

            PI_Name: Paolo Battinelli
     PI_Institution: Osservatorio Astronomico di Roma


           CoI_Name: Serge Demers
    CoI_Institution: Departement de Physique, Universite de Montreal
            Contact: 

           CoI_Name: Michael Irwin
    CoI_Institution: Royal Greenwich Observatory
            Contact: 


Abstract:
The determination by Hargreaves et al. (1994, MNRAS 271, 639)
of a mass-to-light ratio of M/L = 59 for the core of Ursa
Minor and the recent finding by Demers et al. (1995, MNRAS
274,491) of a central cusp in the stellar surface density
profile strongly suggest the presence of a black hole in Ursa
Minor. Thus, we plan to use the WFPC2 to determine the stellar
surface density profile of the central part of the core of
Ursa Minor so to obtain a very precise definition of the cusp.
This is crutial for a reliable estimate of the central mass.
Ursa Minor observations will be compared to black hole models
of Quinlan et al. (1995, ApJ 440, 554) to obtain the
parameters of the black hole and also to set limits on the
properties of the core of Ursa Minor.


Questions


    Observing_Description:
We propose to image the innermost part of Ursa Minor using
the WFPC2 V (F606W) filter. Placing the target close to the
center of the  WF3 we could estimate the stellar surface
density (along two perpendicular directions) up to 100'' from
the Ursa Minor center, a distance  fully encompassing the
cusp found by Demers et al. (1995).  The small number of
foreground stars in the Ursa Minor direction (~ 5
stars/arcmin^2 at V_lim=29 from Ratnatunga & Bahcall 1985,
ApJS 59, 63) makes observations in a second filter not
needed.

  Real_Time_Justification:
None
None

Calibration_Justification:


      Additional_Comments:



Fixed_Targets

  Target_Number: 1
    Target_Name: DDO199
Alternate_Names: URSA-MINOR
    Description: GALAXY,DWARF SPHEROIDAL,
       Position: RA=15H 8M 41.15S +/- 10",DEC=67D 12' 36" +/- 10"
        Equinox: J2000
        RV_or_Z: 
          RA_PM: 
         Dec_PM: 
          Epoch: 
Annual_Parallax: 
           Flux: 
                V = 17+/-1
       Comments: 


Solar_System_Targets


Generic_Targets


Scan_Data


Visits

      Visit_Number: 01
Visit_Requirements: 
  On_Hold_Comments: 
    Visit_Comments: 

     Exposure_Number: 1
         Target_Name: DDO199
              Config: WFPC2
              Opmode: IMAGE
            Aperture: WF3-FIX
          Sp_Element: F606W
          Wavelength: 
 Optional_Parameters: ATD-GAIN=15
Number_of_Iterations: 1
   Time_Per_Exposure: 1300S
Special_Requirements: 
            Comments: 

     Exposure_Number: 5
         Target_Name: DDO199
              Config: WFPC2
              Opmode: IMAGE
            Aperture: WF3-FIX
          Sp_Element: F606W
          Wavelength: 
 Optional_Parameters: ATD-GAIN=15
Number_of_Iterations: 1
   Time_Per_Exposure: 1100S
Special_Requirements: 
            Comments: 

     Exposure_Number: 10
         Target_Name: DDO199
              Config: WFPC2
              Opmode: IMAGE
            Aperture: WF3-FIX
          Sp_Element: F606W
          Wavelength: 
 Optional_Parameters: ATD-GAIN=15
Number_of_Iterations: 2
   Time_Per_Exposure: 1200S
Special_Requirements: 
            Comments: 

Data_Distribution         ! Defaults indicated; change if desired

         Medium: 8MM
Blocking_Factor: 10
        Ship_To: PI_Address
       Ship_Via: UPS
Recipient_Email: 

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