0Assigned ID: 633
----- Attempting Submission 1 (Fri Apr 10 18:12:01 GMT 2015) -----
HST Phase I Proposal 633 (BetaPic.apt) successfully submitted.
Receipt: # 633-1
----- Attempting Submission 2 (Fri Apr 10 20:27:05 GMT 2015) -----
HST Phase I Proposal 633 (BetaPic.apt) successfully submitted.
Receipt: # 633-2
----- Attempting Submission 3 (Fri Apr 10 23:40:37 GMT 2015) -----
HST Phase I Proposal 633 (BetaPic.apt) successfully submitted.
Receipt: # 633-3INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS2015-12-31: Updated buffer time for STIS observations-348219704----- Attempting Submission 1 (Tue Jul 21 08:11:53 GMT 2015) -----
----- Attempting Submission 2 (Fri Aug 28 14:17:44 GMT 2015) -----
----- Attempting Submission 3 (Thu Dec 10 13:26:28 GMT 2015) -----
HST Phase II Proposal 14089 (14089_in_progress.apt) successfully submitted.
Receipt: # 14089-3
----- Attempting Submission 4 (Fri Dec 11 17:43:52 GMT 2015) -----
----- Attempting Submission 5 (Sun Dec 13 11:07:22 GMT 2015) -----
----- Attempting Submission 6 (Mon Dec 14 15:07:50 GMT 2015) -----
HST Phase II Proposal 14089 (14089_Dec_14th.apt) successfully submitted.
Receipt: # 14089-6
----- Attempting Submission 7 (Thu Dec 31 17:11:30 GMT 2015) -----The APT warning is raised because we are doing FP=1, 2, 3, 4 several times with no cenwave change in between (just a POS-TARG). The issue was raised and a reply from Julia Duval informs us that this is not something which will cause any problems.Far-UV observations of H, C, N and O in exocomets of Beta PicThe Beta Pictoris system is a young planetary system embedded in a debris disk that is continually replenished by the collision and evaporation of planetesimals and exocomets. As a result of the edge-on inclination of the debris disk, the gas component of the disk and transiting exocomets can be observed in great detail using absorption spectroscopy. In February 2014, our COS observations yielded the first detection of exocomets in the far-UV. Several new exocometary species were detected for the first time including HI, CII, NI, OI and all the ionization states of Si. The measured radial velocities of these two exocomets are consistent with the two dynamically different exocomet populations known to exist in the Beta Pictoris system. We propose to determine the abundance of key species in a larger sample of exocomets and test the hypothesis that the two dynamically different exocomet populations have different compositions. This can be achieved by the acquisition of several spectra at different epochs. This will allow us to better distinguish the signatures of the interstellar medium, the gas disk and the transiting exocomets. Measuring the abundance of the key species H, C, N and O in a larger sample of evaporating exocomets will enable us to trace the condensation and evaporation processes present in the late stages of planetary formation. Notably, such abundance measurements are only possible via far-UV observations. These measurements will provide insight into the origins of the exocomets of the Beta Pictoris system.Airglow corrections for HI, OI and NI:
==========================================
The geocoronal line emission, known as airglow, inevitably affects the observations of the HI, OI and to a lesser extent the NI lines. The airglow from terrestrial hydrogen at high altitude produces a Lyman-Alpha emission line superimposed on the target spectrum. As a result off-target observations are required to be able to remove the airglow contamination.
With our most recent HST/COS observations of Beta Pictoris (using the same setup as proposed here) we demonstrated that the airglow contamination is very stable from one HST orbit to the other. Furthermore we found that the airglow produces variable but reproducible features as a function of HST orbital position and can be corrected. Using real data we measured an increase in the residual noise of no more than 5 to 8% above the photon noise. Provided an off-target sky exposure after the science exposure is obtained, we can successfully remove the contaminating airglow emission which is essential to accurately perform measurements in the Lyman-Alpha and the airglow contaminated lines (NI and OI).
Development of a new airglow contamination correction procedure
==========================================
We will use the second orbit of the first visit (out of three visits) to develop a new Lyman-Alpha airglow contamination correction procedure, which we think will allow for an even better airglow correction whilst increasing the on-target time. We aim to do this by dividing the second orbit of the first visit into three equal parts. The first part will measure the airglow by observing 1 arcmin away from the target as done in cycle 21. The second part will consist of Beta Pictoris being placed 0.8 arcseconds along the dispersion axis such that the airglow will only cover the blue wing of the lines. In this configuration the red part of the lines will be totally clear of airglow contamination. During the third part, Beta Pictoris will be offset 0.8 arcseconds in the opposite direction along the dispersion axis to clear the blue part of the lines of airglow contamination. This will allow us to accurately measure most of the Lyman-Alpha line except for the very central part (~40 km/s) which is in any case of negligible interest because of the HI ISM absorption. This new technique, aimed at shifting the airglow away from the spectral lines of Beta Pictoris, will remove the need for a dedicated orbit for observing the airglow and will effectively double the on-target time. If shown to be successful, this technique will positively impact all future Lyman-Alpha observations of exoplanet atmospheres. We will observe Beta Pictoris using the same set-up and exposure time as in our observation of
program #13406.
Visit schedule description
==========================================
Each visit of the program requires 2 HST orbits of observation. The first orbit will be fully dedicated to obtain the best G130M spectrum of Beta Pictoris. The second orbit will be dedicated to obtain the airglow spectrum that will be used to correct the first orbit spectrum. Two thirds of this second orbit of the first of the three visits will be used to experiment a new procedure to overcome the airglow contamination by observing the target off-center, away from the center of the aperture as described in the above paragraph. The subsequent two visits will be put on hold until this new technique has been verified as more efficient. If successful this new approach will be applied during the second orbit of the two next visits. Should it not prove to be a viable observation technique, the observations will resume without the offsets.DEBRIS DISKS12falsetruefalsefalseSUPPORTEDCALIBRATIONUNDESIGNATEDNOThe offset is designed to measure the geocoronal airglow in the direction of Beta Pic (thus an area 1 arcmin away is chosen).
The V-magnitude is arbitrarily set to 20 to be compatible with "Bright Object Sensitive Detectors".J2000~5e-13 erg /s/cm2/A at 1216A (Earth airglow at Lyman-alpha)STARA4-A9 V-IVAGB STARCIRCUMSTELLAR MATTERDISKNOThis object was generated by the targetselector and retrieved from the SIMBAD database.BETA-PICTORISJ2000J2000COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291Timing link suitability includes constraints ([02 After 01 by 14.0 to 30.0 days] [03 After 01 by 7.0 to 30.0 days])The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.First orbit: Beta Pic is observed directly.
Second orbit: Divided into three equal parts.
1/3: Beta Pic will be placed 0.8 arcseconds along the dispersion axis (red side masked).
2/3: Beta Pic will be placed 0.8 arcseconds along the dispersion axis (blue side masked).
3/3: Airglow observed 1 arcmin away from target.
NOTE: It is essential that the Earth's airglow contamination is minimised.Please conduct all visists within the period 1st of October 2015 to 1st of March 2016. Our preferred time of observations is during the months November 2015 to January 2016.1449741275000350.33329234725943(Tic-Visit
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