0Assigned ID: 942
----- Attempting Submission 1 (Fri Apr 05 23:23:03 GMT 2019) -----
HST Phase I Proposal 942 (aumic.apt) successfully submitted.
Receipt: # 942-1
----- Attempting Submission 2 (Fri Apr 05 23:55:36 GMT 2019) -----
HST Phase I Proposal 942 (aumic.apt) successfully submitted.
Receipt: # 942-2
----- Attempting Submission 3 (Fri Apr 05 23:59:52 GMT 2019) -----ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
POS TARG OUTSIDE OF APERTURERemoved iterations from Orbits 15-22 to allow >6 min unused time at the end of each orbit.
Restructured visits for a single in-transit visit consisting of 5 orbits, and one after-transit orbit. Changed acquisition time from 0.2 to 0.1 seconds to avoid saturation.
Updated to change after-by to 0-12 hours.
Updated to remove the auto WAVECAL.
Increased one after-by per eclipse to 0-20 hour window.
Updated to remove ACQ from the 2/3rd orbits in a visit.
For my past Ly-alpha transit program, I know that scheduling was challenging, and I am happy to work with y'all to figure out how to make the observations schedulable.
The filters used for the WFC3 transits have been updated to use the narrowband filters at the red edge of each bandpass to minimize filter saturation.-1614242242----- Attempting Submission 1 (Thu Jul 25 14:34:55 GMT 2019) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 2 (Tue Sep 17 19:54:21 GMT 2019) -----
----- Attempting Submission 3 (Wed May 20 17:46:49 GMT 2020) -----
HST Phase II Proposal 15836 successfully submitted.
Receipt: # 15836-3
----- Attempting Submission 4 (Wed May 20 20:12:22 GMT 2020) -----
HST Phase II Proposal 15836 successfully submitted.
Receipt: # 15836-4
----- Attempting Submission 5 (Thu May 21 19:20:06 GMT 2020) -----
----- Attempting Submission 6 (Fri May 22 20:28:19 GMT 2020) -----
----- Attempting Submission 7 (Fri Mar 19 14:26:08 GMT 2021) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 8 (Tue Oct 12 21:29:09 GMT 2021) -----I believe all the errors are for visits that (thanks to y'all) have successfully been completed.
Can't get the target confirmation charts tool to run, but hoping it's fine since we've already got some observations. Most of the errors relate to the completed STIS visits, the last is one of the WFC3 visits and my understanding is that those are under control.
Hannah Wakeford worked with Kevin on the WFC3 orbits. We were told by Kevin to ignore this warning and that he will sort it out.A deep look into the atmosphere of an exoplanet around a pre-main sequence starTwo planets around the pre-main sequence M dwarf AU Mic have recently been detected, including the hot, 6 Earth radius AU Mic b. AU Mic thus joins the small number of known young planetary systems, and the even smaller number of planets that co-exist with debris disks. AU Mic b is the only planet in a young stellar association with both a mass and a radius, and AU Mic is a bright, nearby, and extremely well-observed host star. We propose to take advantage of the unique opportunities available with HST to conduct a multi-pronged investigation into the atmosphere of AU Mic b. First, we will constrain its atmospheric composition through WFC3 transmission spectroscopy. With transmission spectroscopy with both the G102 and G141 grisms, we can probe both H2O and CH4 features. We can then constrain the C/O ratio and thus where the planet formed. Second, we will probe atmospheric escape through STIS UV transit observations. Using the E140M grating, we will obtain high resolution UV spectra and can search for signatures of atmospheric outflows in Ly-alpha and C II. AU Mic b thus provides an exceptional opportunity to investigate planet formation and evolution.We propose a double-pronged investigation of the atmosphere of AU Mic b, obtaining transits with both WFC3/IR and STIS. We will use WFC3/IR to obtain multi-wavelength lightcurves, producing near-infrared exoplanet transmission spectra. We will use STIS to obtain transits at Ly-alpha, measuring the size of the planet at Ly-alpha wavelengths. Only HST has the ability to carry out these observations. The precision, wavelength coverage, and continuous observing capability are required for our WFC3 observations, while FUV transits cannot be observed from the ground.
We will observe AU Mic using WFC3/IR G102 and G141 grisms over two transit observations to measure the complete atmospheric transmission spectrum from 0.8 to 1.7 micron, which covers multiple H2O and CH4 spectral features (Figure 1). The precision of our proposed measurements would allow for strong constraints (0.5 dex) to be placed on the H2O abundance and the detection of CH4 and/or constraint of CH4 abundance to within an order of magnitude depending on atmospheric metallicity and the existence of clouds (Figure 2). Note that our simulations (e.g. Line et al., 2012) show that constraints obtained using 1 transit in each of G102 and G141 is tighter than those obtained from 2 transits in G102 or 2 transits in G141. CH4 is best constrained when the atmospheric metallicity is 30x solar and the cloud top is at or lower than 0.1 bar. In the event that the metallicity and/or cloud opacity is unfavorable to CH4 detection, H2O remains largely constrained to well within an order of magnitude. This would allow for constraints on the atmospheric metallicity, which is helpful in probing the diversity of exoplanet metallicities (e.g. Kreidberg et al., 2014; Wakeford et al., 2017a). Using STIS, we will search for an evaporating exosphere by detecting a deep and long transit at Ly-alpha, and potentially at C II.
The transit duration of AU Mic b is in excess of 4 hours; we use the ExoCTK HST Pandexo ETC (exoctk.stsci.edu) to determine the phase constraints and number of orbits required including the rst HST orbit which will be used to determine the instrument settling effeciency for this bright target. In total for each transit we will require 8 HST orbits, 4.2 in transit, to provide adequate stellar baseline to achieve the needed precision on the transit
depth. As AU Mic is a bright target (Jmag = 5.436) we will conduct both observations in spatial scan mode to spread the target across a column of pixels in the cross-dispersion direction, resulting in a 10-fold increase in the number of photons collected per exposure (McCullough et al., 2014). We simulate each grism observation using the online STScI ETC and ExoCTK (exoctk.stsci.edu) HST Pandexo simulator.
G102 set-up: We use the 256x256 subarray to reduce overhead times applied to each exposure. We will scan at a rate of 1.66 arcseconds/second over 6 seconds to produce a scan 10 arcseconds in length (80 pixels). The planetary transit extends over 3 HST orbits containing 95 exposures with a total of 200 exposures over the whole transit observation. This will result in precisions of 38 ppm in 20 channels between 0.8 to 1.15 micron. To force a buffer dump after each orbit of the 8 orbit transit each orbit is scheduled as a single visit where all 8 visits are requested to be conducted in sequence.
G141 set-up: We will again use the 256x256 subarray to reduce overheads. We will scan at a rate of 3.38 arcseconds/second over 5 seconds to produce a scan 17 arcseconds in length (130 pixels). This results in a total of 176 exposures over the whole observation. This will allow us to achieve precisions of 43 ppm in 27 channels between 1.1 and 1.7 micron. For both WFC3/IR measurements we will be limited to an NSAMP<3 due to the brightness of the target and the short exposure times, to minimize the impact on the observing effeciency we will use the SPARS5 sampling sequence. Each of our observation procedures will ensure that the maximum count stays in the sweet-spot between 28,000-36,000 e- shown by Wilkins et al. (2014) and Wakeford et al. (2017b). To force a buffer dump after each orbit of the 8 orbit transit each orbit is scheduled as a single visit where all 8 visits are requested to be conducted in sequence.
STIS set-up: We will use the E140M grating with STIS/MAMA, which delivers R =45800 spectra covering 1144 to 1710A. Both Ly-alpha and C II are simultaneously accessible. We have checked the bright object limits for AU Mic using the guidelines for active M1 dwarfs, finding that E140M is acceptable (see ETC STIS.sp.1330912). We will observe 2 transits (13 orbits total) using STIS, taking into considering crossings of the South Atlantic Anomaly. The C II transit is likely to be closer in size to the whitelight transit, while for the prototype system Gl 436b, the Ly transit begins 3 hours prior to the transit midpoint and lasts for 10 hours following. With transit 1, we will probe the time region corresponding to the white-light transit which we expect to more closely match the C II; we will obtain 2 orbits 10 hours before transit to set the baseline, and 5 orbits capturing egress and the transit midpoint. With transit 2, we will probe the full possible shape of the Ly transit by obtaining 2 orbits 10 hours prior to the transit to establish a baseline, 2 orbits centered on the transit midpoint, and 2 orbitsabout 5 hours after transit. With this observing strategy, we will have a full view of the exosphere transit, the opportunity to detect the transit in two different species, and the possibility to see time-dependent behavior in the Ly-alpha exosphere.
We estimate that the Ly-alpha transit depth is 38%. Modeling this decrement in flux in the Ly-alpha line of an observed spectrum of AU Mic (Texp = 2130s), we estimate S/N= 30 detection of a Ly-alpha exosphere in a single HST orbit. Our predictions for C II transits derive from a photo-evaporative atmospheric escape model. We use the radiative transfer code CLOUDY to calculate the ionization balance, and assume that the stellar wind can be described as a Parker wind. We estimate that we can detect the C II exosphere at 5-7 sigma in one transit.
2-GYRO IMPACT: As our observations are transit observations and required sequenced visits >3 orbits, scheduling would be challenging in 2-gyro mode. For our WFC3 observations, our fastest scan rate is 3.38 arcsec/sec and so would not be impacted by the limitations of the 2-gyro mode.Our team consists of experts in both the theory and observation of exoplanet atmospheres and atmospheric escape. Dr. Hannah Wakeford and Dr. Zachory Berta-Thompson are experts in atmospheric transmission spectroscopy with WFC3. Dr Wakeford has led 9 papers relating to transmission spectroscopy addressing topics ranging from starspot contamination to clouds. Dr Berta-Thompson is an expert in transmission spectroscopy and addressing systematics; he has also developed an analysis technique for assessing the impact of spots on WFC3 spectra. Dr. Natasha Batalha and Dr. Peter Gao are experts in the theory of planetary atmospheres. Dr. Batalha is a leading expert in predictions for transmission spectra observability with HST and JWST, as well as retrievals from HST and JWST spectra. Dr Gao brings diverse expertise in atmospheric modeling, having led publications on modeling hazes on Pluto, condensates in brown dwarf atmospheres, and the reflected light spectra of giant planets, among other topics. Their expertise will enable us to carry out the atmospheric transmission data analysis and modeling. Dr. Mark Marley and Dr. Roxana Lupu will play advisory roles on the specific atmospheric models that we will use to interpret our data, including supply the opacities of atmospheric molecules. Dr. Elisabeth Newton is an expert in M dwarf stellar physics, and has conducted prior observations of transits at Ly-alpha (a paper presenting the results, led by a graduate student supervised by Dr. Newton, is underway). Dr. Allison Youngblood is a leader in the study of the UV spectra of M dwarfs, and Dr. Eric Lopez is an expert in modeling atmospheric mass loss from exoplanets both considering individual systems and the overall demographics of exoplanets. Their expertise will enable us to carry out the UV transit data analysis and modeling. Additional team members include the discoverers of the planets around AU Mic (Plavchan, Lowrance, Gao), and experts in planetary atmospheres (Marley, Lupu). All team members will contribute to interpretation of results.Planets and Planet Formation6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETM III-ICoordinates were taken from SIMBAD (ICRS, Gaia coordinates traced back to epoch 2000.0). Proper motions and parallax taken from Gaia.J2000J2000WFC3/IRSpectroscopicNoNoG102WFC3/IRSpectroscopicNoNoG141STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425Timing link suitability includes constraints ([02 After 01 by at most 0.5 days])The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode./private/var/folders/w8/c_s9_s9d6dx1kb0j3994pjvw0000gq/T/OPVisit1027674723543032817.xmlThis is STIS Ly-alpha visit corresponds to Eclipse 1, and is the 1st of three visits associated with this eclipse event. Eclipse 1 captures the behavior surrounding the white-light transit. This visit should occur roughly 8 hours prior to the white-light transit event (specified by the period and phase entries for the "in transit" visit) in order provide a baseline Lyman-alpha flux level. The visit consists of 2 HST orbits.1593649248000265.0(Tic-Visit
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