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Assigned ID: 373
----- Attempting Submission 1 (Fri Aug 17 19:28:25 GMT 2018) -----
Changed visit 02 to GJ 65 A
Changed ACQ/PEAK for visit 14 to reflect correct aperture.
Changed ACQ/PEAK exposure time for visit 03 to reflect correct value in ETC calculation.
This also required lowering the time in exposure 3 of the first orbit to 1740 sec.
-1728963210
----- Attempting Submission 1 (Thu Dec 06 21:11:47 GMT 2018) -----
----- Attempting Submission 2 (Mon Aug 05 17:03:44 GMT 2019) -----
----- Attempting Submission 3 (Tue Sep 24 20:21:05 GMT 2019) -----
I only changed visits 02 and 14 and ran both of these tools for these visits.
I have only changed visit 03 and I have run the tools on this.
Testing M Dwarf Mass Loss Across the Fully Convective Boundary
Studies of the rotational distribution of open clusters show that the efficiency of stellar spin down dramatically decreases once stars become fully convective. It is generally understood that this stellar spin down is the result of magnetized stellar winds torquing down the stars as they age. The magnetic field properties of fully convetive stars suggest they should still efficiently spin down, yet they do not. One potential explanation is that the mass loss rates from dwarfs dramatically decreases once stars become fully convective. We will test this hypothesis using HST+STIS to measure astrospheric absorption in a sample of nearby M dwarfs to see if the winds of fully convective stars are significantly weaker as group relative to the partially radiative M dwarfs.
We plan to observe 8 late M dwarfs stars with STIS. Our project is focused on
detecting and measuring astrospheric absorption in the H I Lyman-alpha line
at 1216 Angstroms, using the E140M grating, but confidence in this analysis
is significantly improved with information provided by observations of the
Mg II h & k lines near 2800 Angstroms, so we also be observe the Mg II lines
using the E230H grating. We acquire each of our stars with a short exposure
onto the STIS/CCD. An accurate wavelength scale for the Mg II observations
is important for our purposes so we perform a peakup before our E230H
observations. The brightness of our targets vary, so we choose different
apertures for acquitsition and peak up as needed.
After acquisition and peakup, we spend 1-2 orbits as needed obtaining the
E230H spectrum of the 2574-2851 Angstrom wavelength range, through the
0.2x0.09 aperture. The remaining 2-7 orbits (as needed) are spent observing
the 1150-1700 Angstrom range with the E140M grating, through the 0.2x0.2
aperture. The E140M grating does not have quite the resolution of E230H, but
its R= 45,800 resolution is good enough to study the H I Lyman-alpha line
profile in the detail that we require. Because M dwarfs are known to be
variable, we plan on obtaining our spectra in TIME-TAG mode.
Estimating expected S/N for our planned spectra requires first estimating
Lyman-alpha and Mg II fluxes, which can be done roughly by extrapolating
from previously observed M dwarfs, particularly EV Lac. Chromospheric line
fluxes (such as Mg II and Lyman-alpha) are related to X-ray fluxes through
known scaling laws (Wood et al. 2005a). Thus, Lyman-alpha or MgII fluxes
for our stars can be estimated from known X-ray luminosities of our target
stars. We expect our E230H spectra to attain a sufficient signal-to-noise
of S/N>15 per resolution element at line center for the strong Mg II lines,
and the E140M spectrum to achieve a peak S/N>10 within the H I Lyman-alpha
line.
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. However, there is concern with
regards to using COS or STIS to observe stars that flare, as M dwarfs in
particular are known to do. A particularly massive flare could in principle
violate Bright Object limits, even if the quiescent emission is orders of
magnitude below them. In order to be sure our observations comply with the
BOP rules, we utilized the Mdwarf_template_v5 Excel spreadsheet provided
by our STIS Contact Scientist Tala Monroe and filled out all the required
information for our different observing configurations. We then used the
STIS ETC following the steps in Section 5 of the "Bright Object Protection
Considerations for M Dwarf Flare Events" ISR 2017-02. With the exception
of one target plus science exposure setting, all of our targets produced
no bright object safety warnings in the ETC. The one exception is our
E230H observation of GJ-166C. The total count rate in the case of the
large flare predicted by the Excel spreadsheet generated a total count
rate that exceeds the limit for irregularly-variable sources of 40 percent
of the bright limit 200000 counts per second. However, our STIS Contact
Scientist said this was OK in an email on Dec. 5, 2018.
Stellar Physics
6
false
false
true
false
false
false
false
SUPPORTED
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
CN-LEO
GJ-406
J2000
J2000
U = 16.706
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
GJ-866
J2000
J2000
U = 15.762
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
DY-ERI
GJ-166-C
J2000
J2000
B = 12.85
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
HH-AND
GJ-905
J2000
J2000
B = 14.19
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
VB-8
J2000
J2000
B=18.7
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
GJ-412-A
GSC-03012-02528
J2000
J2000
U=11.44
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
GJ-412-B
J2000
J2000
B=16.45
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
GJ-65-A
J2000
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
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