Science Keywords: Select from 2 to 5 items. Science Keywords is a required field. Wavelength is a required field. 0 Assigned ID: 1307 ----- Attempting Submission 1 (Wed Dec 07 16:35:57 GMT 2016) ----- Joint XMM/HST 0 ----- Attempting Submission 1 (Mon Feb 20 16:24:52 GMT 2017) ----- The remarkable discovery of a system of three Earth-sized potentially-habitable planets transiting the ultra-cool dwarf TRAPPIST-1 provides an unprecedented opportunity for detailed study of the atmospheres of terrestrial exoplanets. Our analysis of an archival XMM-Newton observation of the star revealed XUV radiation that was fifty times stronger than assumed in a theoretical study of the planetary atmospheres, with enough XUV irradiation to profoundly modify and perhaps entirely strip those atmospheres. Here we propose a longer XMM-Newton observation that will cover a full spin cycle of the star and more accurately define the XUV irradiation of the exoplanets. This is an essential step in assessing the habitability of these and similar exoplanets around ultra-cool dwarfs. Our goal is to detect high-excitation UV emission lines from the chromosphere and corona of the exoplanet host star TRAPPIST-1. This is a very late type M dwarf (M8) that is host to potentially-habitable Earth-sized exoplanets. A joint analysis with our coordinated XMM-Newton X-ray observation will allow us to reconstruct the complete extreme-ultraviolet spectrum of the star and hence the high-energy irradiation of the planets in this system. We are particularly interested in detecting the SiIV lines at 1394 and 1403A, and the CIV lines at 1550A. We can also hope to detect SiIII 1207A, OV 1218A and/or NV 1240A, although these are close to Lyman-alpha and may suffer contamination by airglow emission. In order to maximise our sensitivity away from airglow lines we select the relatively wide 0.5arcsec slit. Because we expect the lines to be weak and close to the detection limit, we also chose the D1 pseudo-aperture in order to minimise dark current in the detector. We request that our three orbits are scheduld as a single visit that is simultaneous with one of our XMM-Newton observations. This will avoid ambiguity in our analysis related to stellar variability. We have put the visit on hold awaiting the coordination of HST and XMM scheduling. The XMM program consists of a series of 3 visits, each lasting 12 hours, and separated by about 2 days. The XMM visits will be scheduled in coordination with HST in one of two visibility windows: either May/June 2017 (when we note the visibility for HST is poor) or in Nov/Dec 2017 (when the visibility for HST is good). Extrasolar Planets and Planet Formation 6 false false false false false false SUPPORTED STAR M V-IV NO This position was measured using 2015 TRAPPIST images, and was used for the successful STIS obervations of programs 14493 and 14900. Radial velocity comes from Barnes et al. 2014 2MASSJ23062928-0502285 J2000 J2000 R=16.47+-0.07, I=14.0+-0.1, J=11.35+-0.02, K=10.30+-0.02 COS/FUV Spectroscopic No No G130M 1487590597964 The scheduling data was generated by CASM 25.0. CASM was run in Phase II mode. /Users/pete/props/xmm/ao16/trappist/phase2/hst/OP-cache/14906_boris_pete-v01.xml (Tic-Visit :proposal-id 14906 :visit-id "01" :proposal-version -1 :trans-version "20170109" :date "20-Feb-2017 11:36:37.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1235472 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14906 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14906 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2880 :al-overhead-at-end 0 :internal-dur-at-end 178 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3213 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14906 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2991 :al-overhead-at-end 0 :internal-dur-at-end 363 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3213 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14906 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2991 :al-overhead-at-end 0 :internal-dur-at-end 625 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3213 :pcs-gap 0 ) true 3 0 The HST visit should be carried out simultaneously, or as close in time as possible, with one of the visits of our XMM program. The XMM program consists of a series of 3 visits, each lasting 12 hours, and separated by about 2 days. The XMM visits will be scheduled in coordination with HST in one of two visibility windows: either May/June 2017 (when we note the visibility for HST is poor) or in Nov/Dec 2017 (when the visibility for HST is good). The target has been acquired with STIS using the default setup before as part of HST program 14493, here we use the same parameters.