0 Assigned ID: 139 ----- Attempting Submission 1 (Wed Apr 05 13:36:07 GMT 2017) ----- remove last exposure per orbit to accomodate new gs reacq times -408522417 ----- Attempting Submission 1 (Tue Jul 04 14:39:01 GMT 2017) ----- ----- Attempting Submission 2 (Fri Dec 07 12:58:00 GMT 2018) ----- NUV Transit Spectroscopy of HD189733b: Measuring the Mass-loss and Ionization State of a Prototypical Escaping Atmosphere The benchmark hot Jupiters HD209458b and HD189733b have provided the foundations of comparative planetology for giant exoplanets, making them of paramount importance for atmospheric studies of short-period planets. HD189733b is the closest transiting hot Jupiter to Earth and transit observations have been obtained and studied across the electromagnetic spectrum, with the surprising exception of the near-ultraviolet: a unique window for atmospheric mass-loss studies owing to the strong resonance lines and large photospheric flux in this band. In order to make a quantitative assessment of the metallicity, ionization state, and outflow rate of this important system, and to complete the panchromatic archive of transit spectroscopy of this archetypal object, we request 15 HST orbits to obtain three STIS near-ultraviolet transit light curves of HD189733b. These observations will allow us to study the physical properties of the planet's upper atmosphere, constrain the composition of the haze layer characterising the optical transmission spectrum, and provide a reference spectrum for NASA's recently funded Colorado Ultraviolet Transit Experiment (CUTE) exoplanet mission, which will carry out a 1-year science mission to observe multiple near-ultraviolet transits of the brightest and most nearby short-period transiting planets to study the physics of atmospheric escape. We will observe HD189733 for 3 visits timed with the planet's primary transit. Each visit will be composed of 5 consecutive HST orbits. The transit happens every 2.219 days and lasts for about 1.8 hours. The observations aim at completely covering the planet transit with the first 3 science observations placed before the transit, the 4th in transit, and the 5th after the transit. The timing constrain is set on the beginning of the target acquisition and it gives a freedom of about 29 minutes on the starting time. The conditions driving the phase constrain are 1) the last science exposure sequence (5th orbit) falls integrally after the transit and 2) the 4th science exposure sequence (4th orbit) starts before the mid-transit. For the ETC runs, we used a G2V stellar type, although the target has a K2V spectral type. This was suggested by the STIS team in order to account for the chemospheric emission. In phase 1 we requested to use the TIME-TAG mode, but in phase 2 this reavealed to be too expensive for the buffer. For this reason, we modified our observing mode to ACCUM and therefore split the science exposure along each orbit in several consecutive short exposures. This part of the sky is not covered by GALEX, but observations of this target have already been done in the past with STIS and COS in the FUV without any problem. Planets and Planet Formation 6 false false true false false false false SUPPORTED STAR EXTRA-SOLAR PLANET K V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. No Galex or TD1 UV fluxes available. Towards the ultraviolet, we were able to find just a Johnson U-band magnitude, given above. J2000 J2000 Johnson U: 9.241 mag STIS/NUV-MAMA Spectroscopic No No E230M 2707 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. Observation of the third planet transit consisting of 5 consecutive orbits. 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