0
Assigned ID: 1237
----- Attempting Submission 1 (Thu Feb 28 16:53:52 GMT 2013) -----
HST Phase I Proposal 1237 (atauprop.apt) successfully submitted.
0
----- Attempting Submission 1 (Wed Jun 05 16:49:39 GMT 2013) -----
Tracking the Winds of Red Giants from the Star to the ISM
We propose to study the stellar winds of nine red giants from their origins near the stellar surface all the way to their merger with the ambient ISM. We will do so by studying absorption features in UV emission lines observed with STIS. The STIS spectra will include many broad absorption lines from the stellar wind. We expect that at least some of the spectra will also show narrow astrospheric absorption from the wind-ISM interaction, like that which has been observed in the Mg II h & k lines of Alpha Tau (K5 III). The astrospheric absorption will be used to study the nature of the wind-ISM collision, and will also be used as an in situ probe of ISM properties in the Local Bubble.
We will observe nine red giants with STIS for 4 orbits each. We acquire each of our rather bright stars with a 0.1 second exposure onto the STIS/CCD with the F28X50OII filter. An accurate wavelength scale is important for our purposes so we will perform a peakup into the narrow 0.3X0.05ND aperture. This neutral density aperture is required to reduce the flux for our bright targets and we use a 0.1 s exposure for the peakups. After acquisition and peakup, the first orbit will consist of an E230H spectrum of the 2574--2851 A wavelength range through the 0.2X0.09 aperture. The remaining three orbits will be used for an E140M spectrum of the 1150--1700 A wavelength range through the 0.2X0.2 aperture. All of our targets are comfortably in compliance with STIS/MAMA bright object limits, as verified using both Table 13.44 in the STIS Instrument Handbook and the online STIS exposure time calculator.
The E230H observation will provide the highest resolution (R= \lambda / \Delta\lambda = 110,000) spectrum of the Mg II h & k lines at 2800 A. High resolution is required for studying the narrow astrospheric absorption. We can only crudely predict line fluxes for our
target stars, so accurately predicting signal-to-noise (S/N) is problematic. The best we can do is assume that intrinsic fluxes are similar to those seen for Alpha Tau, and then correct for target distance. After acquisition, peakup, and observational overhead are considered, we expect at least 28 minutes to be available in the first orbit for the E230H exposure. We expect this to be more than enough time to attain very high S/N of ~100 at line center for the strong Mg II lines. We also expect to see numerous Fe II lines in the spectrum at lower S/N, for which we can also study stellar wind and possibly astrospheric absorption.
After acquisition and overheads are considered, we expect our 3-orbit E140M exposure to amount to about 135 minutes of total exposure time. The O I 1300 triplet lines should all be observed at S/N>25 if fluxes are similar to Alpha Tau. This should be sufficient to study wind and astrospheric absorption in these lines. Other FUV lines, such as C II 1335, where we would also like to see wind and astrospheric absorption, will be observed at significantly lower S/N unless they are significantly stronger than they are for Alpha Tau. We also hope the exposure time will be sufficient to detect weak high-temperature lines such as the Si IV 1400 and
C IV 1550 doublets, which would indicate the coexistence of coronae and massive warm winds. Note that the E140M grating does not have quite the resolution of E230H, but its R= 45,800 resolution should be just good enough to mostly resolve any narrow astrospheric absorption.
COOL STARS
12
false
true
0.0
0.0
false
false
false
SUPPORTED
STAR
K III-I
SIGMA-PUP
J2000
J2000
TYPE=K5III, F-LINE(2796)=1.2E-11, W-LINE(2796)=0.4, F-LINE(1302)=2.7E-13, W-LINE(1302)=0.2
STAR
K III-I
ALPHA-TUC
J2000
J2000
TYPE=K3III, F-LINE(2796)=1.0E-11, W-LINE(2796)=0.4, F-LINE(1302)=2.2E-13, W-LINE(1302)=0.2
STAR
K III-I
THETA-CMA
J2000
J2000
TYPE=K4III, F-LINE(2796)=6.3E-12, W-LINE(2796)=0.4, F-LINE(1302)=1.4E-13, W-LINE(1302)=0.2
STAR
M III-I
HR5192
J2000
J2000
TYPE=M4.5III, F-LINE(2796)=1.3E-11, W-LINE(2796)=0.4, F-LINE(1302)=2.9E-13, W-LINE(1302)=0.2
STAR
M III-I
GAMMA-ERI
J2000
J2000
TYPE=M1III, F-LINE(2796)=8.1E-12, W-LINE(2796)=0.4, F-LINE(1302)=1.8E-13, W-LINE(1302)=0.2
STAR
M III-I
TAU4-ERI
J2000
J2000
TYPE=M3-4III, F-LINE(2796)=6.0E-12, W-LINE(2796)=0.4, F-LINE(1302)=1.3E-13, W-LINE(1302)=0.2
STAR
K III-I
HR3980
J2000
J2000
TYPE=K4III, F-LINE(2796)=5.3E-12, W-LINE(2796)=0.4, F-LINE(1302)=1.2E-13, W-LINE(1302)=0.2
STAR
K III-I
HR-3145
J2000
J2000
TYPE=K2III, F-LINE(2796)=5.8E-12, W-LINE(2796)=0.4, F-LINE(1302)=1.3E-13, W-LINE(1302)=0.2
STAR
M III-I
MU-GEM
J2000
J2000
TYPE=M3III, F-LINE(2796)=7.4E-12, W-LINE(2796)=0.4, F-LINE(1302)=1.6E-13, W-LINE(1302)=0.2
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
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No
E140M
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STIS/NUV-MAMA
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No
E230H
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STIS/FUV-MAMA
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No
No
E140M
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STIS/NUV-MAMA
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No
E230H
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STIS/FUV-MAMA
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No
E140M
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STIS/NUV-MAMA
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No
E230H
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STIS/FUV-MAMA
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E140M
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STIS/NUV-MAMA
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E230H
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STIS/FUV-MAMA
Spectroscopic
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E140M
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STIS/NUV-MAMA
Spectroscopic
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No
E230H
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STIS/FUV-MAMA
Spectroscopic
No
No
E140M
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STIS/NUV-MAMA
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No
E230H
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STIS/FUV-MAMA
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E140M
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STIS/NUV-MAMA
Spectroscopic
No
No
E230H
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STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3229
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)
(Tic-Orbit
:proposal-id 13462
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)
(Tic-Orbit
:proposal-id 13462
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)
(Tic-Orbit
:proposal-id 13462
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:dark-offset NIL
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)
true
4
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/home/wood/marmoset/props/hst13/OP-cache/atauprop-v09.xml
The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
(Tic-Visit
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 4
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 365968
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
(Tic-Orbit
:proposal-id 13462
:visit-id "09"
:orbit-number 4
:pcs-time 222
:si-vis-utilization 3022
:al-overhead-at-end 194
:internal-dur-at-end 319
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
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:pcs-gap 0
)
true
4
0