! Proposal 6808, submission 1
! PI: Andrea K. Dupree
! Received Fri Mar 8 16:31:33 EST 1996
! From: gillil@stsci.edu
! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template
! $Id: 6808,v 3.1 1996/03/08 22:02:57 pepsa Exp $
! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template
! $Id: 6808,v 3.1 1996/03/08 22:02:57 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: Lucas
! Phone: 410-338-4716 , E-mail: lucas@stsci.edu
!
! This partially completed template was generated from a Phase I proposal.
! Name of Phase I Proposal: archive-1075.dupree.prop
! Date generated: Fri Dec 22 16:42:13 EST 1995
!
Proposal_Information ! Section 4
Title: Capella: Separating the Giants
Proposal_Category: GO
Scientific_Category: COOL STARS
Cycle: 6
Investigators
PI_name: Andrea K. Dupree
PI_Institution: Smithsonian Astrophysical Observatory
CoI_Name: Nancy S. Brickhouse
CoI_Institution: Smithsonian Astrophysical Observatory
Contact: ! Y or N (designate at most one contact)
CoI_Name: Ronald L. Gilliland
CoI_Institution: Space Telescope Science Institute
Contact: Y ! Y or N (designate at most one contact)
Abstract: ! Free format text (please update)
The bright giants in the Capella system form a test of the
evolution of stellar magnetic activity: the primary star is a
clump giant in the helium burning phase; the secondary star is
a rapidly rotating star in the Hertzsprung Gap. Optical,
ultraviolet, and EUV studies give differing and puzzling
results as to the assignment of Capella's prodigious
radiative output. We propose a unique use of the objective
prism on the FOC in order to separate the two components,
firmly identify the sources of emission, and answer
fundamental questions about the presence and evolution of
stellar chromospheres and coronae.
Questions ! Free format text (please update)
Observing_Description:
The observations will be made at elongation when the stars
are separated by their maximum amount (56.5 mas; Hummel Etal\
1994). This occurs approximately every half-period or 52
days. We will select an appropriate time so that the major
axis of the apparent orbit is perpendicular to the dispersion
of the prisms. The first orbit will be an interactive Bright
Target acquisition followed by direct imaging in the near
ultraviolet continuum to define the stellar positions and
separations. Although we expect the atmospheres to be
extended, and hence appear larger in the ultraviolet, they
will still have an apparent size less than or comparable to a
pixel (14 mas) (If the ultraviolet continuum disk is twice
the size of the star in the visible, the disk of the primary
is 17.0 mas, and of the secondary 12.8 mas.) We plan to use
the Objective Prisms on the FOC in order to obtain spectra of
the regions \gl\gl1235--1425; \gl\gl1525-1675; and the
2800Angstrom\ region. The setup and exposures amount to one
orbit for each of the 3 bands. We will use various crossed
filter configurations to acquire our principal lines of
interest (see Table 2), and to exclude the red spectral
region. The major neutral density filters are located on the
same filter wheel as the prisms, and so a mix of crossed wide
and medium band filters will need to be set up. We are not
concerned about the absolute calibration of the emission line
flux since that has been well studied, but we wish to
estimate the relative flux in each line from the two stars. A
serious consideration is the dynamic range of the detectors,
and the unknown relative contribution of the two giants. We
will evaluate filter combinations and exposures at the top of
the dynamic range for the total flux from the system which is
well known; individual fluxes will be less. To isolate the
important He II \gl1640 transition, two filter configurations
will likely be needed, although it may be that two prism
configurations will also be necessary. The FOC team has
obtained prism spectra of standard stars, so those should
serve to define the point spread function ( cf. Jakobsen
Etal\ 1993; Paresce Etal\ 1995). We note that we detected a
bug in the prism simulator program for the FOC when applied
to line spectra in the far ultraviolet, so that detailed
computations of many crossed filter configurations were not
possible for this proposal. We have had discussions with the
FOC team at the STScI and the computer program could not be
modified in time to meet the Cycle 6 deadline for proposals.
We are confident however that the spectra can be obtained as
proposed in the requested time. =2pc centerline Table
2: Ultraviolet Fluxes from the Capella System def width
16.5 truecm # & # & # & # noalign 2pt noalign 4
pt Emission& Wavelength& multispan2 Observed Flux at Earth
noalign\kern -2pt Feature&(AA)&(10^-12 erg\ cm^-2 s^-
1)&(photon\ cm^-2 s^-1) noalign 2pt noalign\kern 2pt N
V& 1240. &8.8&0.55 O I& 1305. &31.4& 2.06 C II& 1335.
&23.7&1.59 Si IV& 1400.& 23.9&1.68 C IV& 1549.& 41.0&3.20
He II& 1640.&6.7&0.55 Mg II&2800.&1400.&197. noalign\kern
2pt noalign 2pt \medskip ^\dagger Fluxes from from Linsky
Etal\ 1995 and Ayres and Linsky 1980.
Real_Time_Justification:
Bright Target Acquisition Procedure for the FOC will be used.
A real-time acquisition will be necessary. The brightness of
Capella (V=0.08), and our desire to use the 128x128 IMAGE
mode force real-time contacts to: 1) verify filter positions
before a slew to the target can be made, and 2) perform an
interactive acquisition to center the target for the 1.8''
square 128x128 IMAGE field. This program is Time-Critical
because an observing date (~ +/- 3 days) must maximize the
separation of the stars.
We have time awarded on EUVE through 1995 to continue
monitoring Capella; we are proposing for additional
simultaneous time on ASCA and EUVE in order to better define
the emission measure at high temperatures, and to determine
the coronal abundances in the system.
Calibration_Justification: ! Move appropriate text from Real_Time_Justification
Additional_Comments:
Fixed_Targets ! Section 5.1
Target_Number: 1
Target_Name: HD34029
Alternate_Names: CAPELLA, GSC3358-03141
Description: STAR, G III-I
Position: RA = 05H 16M 41.35S +/- 0.01S,
DEC = 45D 59' 52.9" +/- 0.1"
! RA=0H 0M 0.00S +/- 0S,
! DEC=0D 0' 0.0" +/- 0",
! PLATE-ID=0000
Equinox: J2000
RV_or_Z:
RA_PM: +0.0073 ! Units are seconds of time per year
Dec_PM: -0.425 ! Units are seconds of arc per year
Epoch: 2000.0
Annual_Parallax: 0.075
Flux: V = 0.08 +/- 0.01,
B-V = 0.80 +/- 0.01,
F-LINE(1335) = 21 +/- 2 E-12,
F-LINE(1356) = 8 +/- 1 E-12,
F-LINE(1394) = 15 +/- 1 E-12,
F-LINE(1486) = 18 +/- 5 E-13,
F-LINE(1640) = 10 +/- 1 E-12
Comments: Coords, PM from Hipparcos INCA (as given in GO-5886)
! This is a template for a single visit containing a single exposure
! Repeat exposure and visit blocks as needed
Visits ! Section 6
Visit_Number: 1
Visit_Requirements: ! Section 7.1
PERIOD 52.011D AND ZERO-PHASE JD2447502.44
ORIENT 171D TO 177D
SCHED 90%
! ORIENT 342D to 348D
! Uncomment or copy visit level special requirements needed
! Most of these requirements (including ORIENT) will limit scheduling
! PCS MODE [Fine | Gyro]
! GUIDing TOLerance <angle>
! DROP TO GYRO IF NECESSARY [NO REACQuisition]
! ORIENTation <angle1> TO <angle2>
! ORIENTation <angle1> TO <angle2> FROM <visit>
! ORIENTation <angle1> TO <angle2> FROM NOMINAL
! SAME ORIENTation AS <visit>
! CVZ
! PARallel
! SCHEDulability <percentage>
! 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-list>]
On_Hold_Comments:
Visit_Comments: Must be scheduled within +/- 2 days of
phase 0.0 or 0.5 for maximum component separation.
Period is given as 0.5 of real period, and zero phase
is maximum elongation -0.25*period. Orient is
calculated to give maximum cross-dispersion
separation (max sep in X of FOC).
Exposure_Number: 10 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: ACQ
Aperture: 512X1024
Sp_Element: F278M,F140W,F6ND,F1ND
Wavelength:
Optional_Parameters: PIXEL=50X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 120s
Special_Requirements: ! Section 7.2
INT ACQ FOR 20-110;
PHASE 0.46 TO 0.54
! Uncomment or copy exposure level special requirements needed
! INTeractive ACQuisition FOR <exp-list>
! ONBOARD ACQuisition FOR <exp-list>
! SAVE OFFSET <id>
! USE OFFSET <id>
! 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
! REQuires EPHEMeris CORRection <id>
! END ORBIT
! EXPAND
! LOW-SKY
! MAXimum DURation [<time> | <%>]
! MINimum DURation [<time> | <%>]
! NO SPLIT
! PHASE <number1[0,1]> TO <number2[0,1]>
! SEQuence <exp-list> NON-INTerruptible
! SHADOW
Comments: Expect center px count rate of 0.8/s.
INT ACQ should place target at 48,86 of final 128X128
format, i.e., slightly off-center.
Exposure_Number: 20 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 128X128
Sp_Element: F278M,F140W,F6ND
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 340s
Special_Requirements: ! Section 7.2
NO SPLIT;
Comments: 2.1 cts/s central px.
for each star
Exposure_Number: 30 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 128X128
Sp_Element: F278M,F140W,F6ND
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 320s
Special_Requirements: ! Section 7.2
POS TARG +0.007,+0.000
Comments: Provides sub-pixel sampling cross dispersion.
Exposure_Number: 40 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 128X128
Sp_Element: F140M,F140W
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 300s
Special_Requirements: ! Section 7.2
POS TARG +0.007,0.000
Comments: Far UV image, 3.1 cts/s central px.
Exposure_Number: 50 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 128X128
Sp_Element: F140M,F140W
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 300s
Special_Requirements: ! Section 7.2
POS TARG +0.000,0.000
Comments: Far UV image, 3.1 cts/s central px.
Exposure_Number: 60 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 256X256
Sp_Element: F140W,F165W,PRISM2
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 660s
Special_Requirements: ! Section 7.2
NO SPLIT;
POS TARG +0.077,-5.900
Comments: to place 1640A 20 px from y-max, rate at 1640 = 0.15,
rate at 1800 = 0.9
Provides spectrum 1630-1830A.
Exposure_Number: 70 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 256X256
Sp_Element: F140W,F165W,PRISM2
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 720s
Special_Requirements: ! Section 7.2
POS TARG +0.070,-5.900
Comments: to place 1640A 20 px from y-max, rate at 1640 = 0.15,
rate at 1800 = 0.9
Provides spectrum 1630-1830A.
Exposure_Number: 80 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 256X256
Sp_Element: F140W,F165W,PRISM2
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 670s
Special_Requirements: ! Section 7.2
POS TARG +0.140,-0.860
Comments: count rate max of 1.6; at 2800A and below max of 0.8
provides spectrum 2000-3250A
Exposure_Number: 90 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 256X256
Sp_Element: F140W,F165W,PRISM2
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 670s
Special_Requirements: ! Section 7.2
NO SPLIT;
POS TARG +0.147,-0.860
Comments: count rate max of 1.6; at 2800A and below max of 0.8
provides spectrum 2000-3250A
Exposure_Number: 100 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 256X256
Sp_Element: F140W,F130M,PRISM1
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 1160s
Special_Requirements: ! Section 7.2
POS TARG +0.270,-5.180
Comments: max long wave counts about 1/s;
0.01 cts/s at 1640, 0.35 at 1335, 0.16 at 1216
Need 1400A at format center.
Exposure_Number: 110 ! Section 6.5
Target_Name: HD34029
Config: FOC/96
Opmode: IMAGE
Aperture: 256X256
Sp_Element: F140W,F130M,PRISM1
Wavelength:
Optional_Parameters: PIXEL=25X25,CHECK-FILTER=YES
Number_of_Iterations: 1
Time_Per_Exposure: 1150s
Special_Requirements: ! Section 7.2
NO SPLIT;
POS TARG +0.277,-5.180
Comments: max long wave counts about 1/s;
0.01 cts/s at 1640, 0.35 at 1335, 0.16 at 1216
Need 1400A at format center.
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:
!
! MS-15
! 60 Garden Street
! Cambridge
! 02138
!
!
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>
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