0 Assigned ID: 92 ----- Attempting Submission 1 (Tue Apr 07 20:10:19 GMT 2015) ----- 0 ----- Attempting Submission 1 (Thu Jul 16 18:46:35 GMT 2015) ----- ----- Attempting Submission 2 (Fri Oct 09 20:12:12 GMT 2015) ----- HST Phase II Proposal 14162 (apt_koi314_cycle23_phase2_resubmit.apt) successfully submitted. Receipt: # 14162-2 ----- Attempting Submission 3 (Thu Oct 15 18:26:57 GMT 2015) ----- Magnetic activity is an ubiquitous phenomenon of cool stars and causes stellar high-energy emission, which is thought to be the driver of atmospheric evaporation of exoplanets in close orbits around their host stars. We have recently observed the super-earth hosting star KOI-314 in X-rays, in order to characterize the evaporation and evolution of its planets. However, we found the star to be very X-ray dim, indicating very low magnetic activity. This is in direct contrast with archival NUV observations with GALEX and optical high-resolution spectra, which show strong magnetic activity in the upper and lower chromosphere. We propose to obtain a new NUV spectrum with the WFC3/UVIS UV grism in one HST orbit in order to characterize the current activity level in the upper chromosphere, and compare this to current X-ray measurements of the coronal activity and optical spectra of the lower chromosphere activity. Investigating this stellar atmosphere that seems to deviate from the usual coronal and chromopsheric heating standard model is relevant for understanding the high-energy environment and evolution of exoplanetary atmospheres. We propose to observe the planetary system KOI-314 with WFC3/UVIS using the G280 UV grism to cover a wavelength region of 2000-4000 Angstrom, using one HST orbit split into four spectral exposures. We request 4 moderate duration spectra of 600 s each during one orbit, which we will later stack to reach higher S/N. This is within the data transmission constraints for WFC3. For the sequence of exposures during the orbit, we request first blind target acquisition; the proper motion of the target is small. Guide star acquisition will take 6 minutes according to the HST handbook. After that, we request several (identical) exposures of 600 s duration in UVIS-ACCUM mode. The readout overhead for the first exposure is 2.6 minutes, and 2.1 minutes for the subsequent exposures. The buffer can be dumped into the solid state recorder during each subsequent exposure, so that no additional overhead occurs for the buffer dump. We request to use the post-flash at the end of every exposure to mitigate effects of degrading charge transfer efficiency. This will add 0.1 minutes to each science exposure. This setup will require a total of 3318 s to perform, using 97% of the available visibility time of 3420 s in a single orbit. COOL STARS 12 false true false false SUPPORTED STAR CORONA EXTRA-SOLAR PLANETARY SYSTEM M V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. KOI-314 J2000 J2000 J=10.3, H=9.7, K=9.5 WFC3/UVIS Spectroscopic No No G280 /tmp/OPVisit6552025652934363122.xml 1444926080038 The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. I have dithered the exposures 1, 2, and 3 by hand, by setting different POS TARG arguments. This should be equivalent to a dither of 5 pixels between exposures. (Tic-Visit :proposal-id 14162 :visit-id "01" :proposal-version -1 :trans-version "20150609" :date "15-Oct-2015 12:21:19.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2021248 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14162 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14162 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2974 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) true 1 0