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For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
0
----- Attempting Submission 1 (Tue May 12 20:23:09 GMT 2026) -----
I have selected observations with all four FP-POS using G160M across two visits.
Rocky Worlds DDT: HST Observations of TOI 771
Rocky Worlds is a joint JWST and HST Director's Discretionary Program designed to implement the top recommendations from the Working Group on Strategic Exoplanet Initiatives with HST and JWST. The HST side of the Rocky Worlds DDT focuses on ultraviolet (UV) characterization of the nearby M-dwarf hosts of the rocky planets observed with JWST. We will use COS and STIS to measure the UV to blue-optical spectra of these stars, including UV flare monitoring and measuring the wings of the Ly-alpha profile where appropriate. With these observations we will constrain the high-energy output of these host M dwarfs in the UV, which can be applied to planetary models of atmospheric escape, as well as photochemistry if a planetary atmosphere is present. Complementary observations and analysis to fill in the rest of the M-dwarf panchromatic spectra, from the X-ray to the infrared, are encouraged.
Each M-dwarf planet host observed by HST in the Rocky Worlds DDT program has its own Program ID. The observations in this program will focus on TOI 771
HST observations of TOI-771. 16 orbits of flare monitoring using G130M/1222, with time to account for long acquisitions. 6 orbits of FUV line coverage with G160M/1533 which provides complete coverage with G130M/1222 of 1070-1710 Angstroms. We obtain NUV/Vis low resolution spectroscopy with STIS G230L, G430L, and G750L and the 52x0.2 slit in order to construct an accurate stellar SED in seven orbits. All UV observations are obtained in time-tag mode to allow for light curves to be generated in the case of a flare or serendipitous transit.
For all observation SNR calculations we used archival spectroscopy of GJ 3929 from GO 17904 (PI: Diamond-Lowe), with a radius and distance scaled SED. For STIS CCD calculations we assumed a Phoenix M3.5 T=3400 K SED scaled to the Gaia G=13.34.
TBD
6
false
false
false
false
false
false
false
SUPPORTED
STAR
EXTRA-SOLAR PLANETARY SYSTEM
M V-IV
NO
2MASS-J10562716-7259054
J2000
The scheduling data was generated by CASM 34.0.
CASM was run in Phase II mode.
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Lifetime check for G160M:
Initial look is ~4 counts total in the Brightest emission line per FP-POS. We should be ok.
The scheduling data was generated by CASM 34.0.
CASM was run in Phase II mode.
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Lifetime check for G160M:
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The scheduling data was generated by CASM 34.0.
CASM was run in Phase II mode.
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Lifetime check for G160M:
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The scheduling data was generated by CASM 34.0.
CASM was run in Phase II mode.
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Lifetime check for G160M:
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The scheduling data was generated by CASM 34.0.
CASM was run in Phase II mode.
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Lifetime check for G160M:
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CASM was run in Phase II mode.
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Lifetime check for G160M:
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