The only difference between this late submission and my earlier, on-time submission is the left subplot of Figure 2. After the deadline passed, I discovered a plotting error that
overestimates the flux of the target by a factor of 5. This might mislead the TAC into thinking the target is more favorable than it actually is. This is purely a local issue--all other plots,
in addition to all the SNR calculations, are correct.
I apologize for this error, and hope that this late submission will be accepted.-2119909717Assigned ID: 872
----- Attempting Submission 1 (Fri Mar 06 22:40:41 GMT 2020) -----
HST Phase I Proposal 872 successfully submitted.
Receipt: # 872-3
----- Attempting Submission 4 (Sat Mar 07 00:46:44 GMT 2020) -----
HST Phase I Proposal 872 successfully submitted.
Receipt: # 872-4
----- Attempting Submission 5 (Sat Mar 07 00:56:40 GMT 2020) -----
HST Phase I Proposal 872 successfully submitted.
Receipt: # 872-5
----- Attempting Submission 6 (Sat Mar 07 02:50:00 GMT 2020) -----
HST Phase I Proposal 872 successfully submitted.
Receipt: # 872-6LONG STIS MAMA SU LIKELY TO INTERSECT THE SAAFor planet b, visit 2 (the observations on March 19), I added one orbit to the first segment of the visit and subtracted one orbit from the second segment.1116588466----- Attempting Submission 1 (Tue Jun 30 02:10:49 GMT 2020) -----
----- Attempting Submission 2 (Fri Dec 25 19:05:03 GMT 2020) -----
----- Attempting Submission 3 (Thu Feb 18 23:39:51 GMT 2021) -----The Target Confirmation tool throws an exception when I try to run it:
Exception caught generating confirmation chart for coordinate string 07:49:55.0488 +27:21:47.28
java.io.IOException: This is not a binary file.
[SEVERE] Confirmation Chart Generator: Failed to write confirmation chart for target: HD-63433
Exception in thread "AWT-EventQueue-0" java.lang.NullPointerException
at com.google.common.base.Preconditions.checkNotNull(Preconditions.java:877)
at com.google.common.collect.ImmutableList$Builder.add(ImmutableList.java:788)
at edu.stsci.aladin.ConfirmationChartGenerator.exportHstTargetConfirmationFiles(Unknown Source)
at edu.stsci.aladin.ConfirmationChartGenerator.exportToFiles(Unknown Source)
at edu.stsci.aladin.ConfirmationChartGenerator.exportTargetConfirmationFiles(Unknown Source)
at edu.stsci.aladin.AladinTool.exportTargetConfirmationFiles(Unknown Source)
at edu.stsci.apt.model.ProposalSpecification$ExportTargetConfirmation.actionPerformedAsTool(Unknown Source)
at edu.stsci.apt.model.ProposalSpecification.executeExporterAsTool(Unknown Source)
at edu.stsci.tina.tools.ExportTool.runExporter(Unknown Source)
at edu.stsci.tina.tools.ExportTool.activate(Unknown Source)
at edu.stsci.tina.controller.AbstractTinaController.lambda$setActiveTool$3(Unknown Source)
at java.desktop/java.awt.event.InvocationEvent.dispatch(Unknown Source)
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at java.desktop/java.awt.EventQueue$4.run(Unknown Source)
at java.base/java.security.AccessController.doPrivileged(Native Method)
at java.base/java.security.ProtectionDomain$JavaSecurityAccessImpl.doIntersectionPrivilege(Unknown Source)
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at java.desktop/java.awt.EventDispatchThread.pumpEventsForFilter(Unknown Source)
at java.desktop/java.awt.EventDispatchThread.pumpEventsForHierarchy(Unknown Source)
at java.desktop/java.awt.EventDispatchThread.pumpEvents(Unknown Source)
at java.desktop/java.awt.EventDispatchThread.pumpEvents(Unknown Source)
at java.desktop/java.awt.EventDispatchThread.run(Unknown Source)Probing mass loss from two mini-Neptunes orbiting a young solar analoguePhotoevaporative mass loss is key to sculpting the properties of short period transiting exoplanets, yet current models have large theoretical uncertainties and relatively few observational constraints. In particular, mass loss has never been conclusively observed around mini Neptunes (2-3 $R_E$), even though this regime is crucial for understanding the bimodal radius distribution observed by \textit{Kepler}. The recently discovered transiting mini Neptunes TOI 1726.01 and 1726.02 are far and away the most promising targets for probing present-day mass loss. This pair orbits a nearby (22 pc) and young (400 Myr) solar analogue which is 50 times brighter than the Sun in X-rays, driving a strong outflow which should be detectable in Lyman alpha absorption.
We request 36 HST orbits to observe two UV transits of each planet with STIS/G140M. These observations will allow us to measure the size, shape, and kinematic structure of the exosphere, constrain the mass loss rate, and evaluate the magnitude of any visit-to-visit variability in the outflow structure. In addition, we will be able to test hydrodynamical models by comparing their predictions for the relative mass loss rates and exosphere geometries for the two planets to observations: a comparative approach that has hitherto been impossible.Our program will observe 2 transits of HD 63433b and 2 transits of HD 63433c. Each transit observation will consist of 9 orbits: 5 consecutive orbits containing the pre-transit baseline, the transit itself, and the post-transit baseline; and 4 consecutive orbits approximately 1 day after the transit, containing a pristine baseline free from any long exospheric tail. The idea is that HST would observe during 5 consecutive SAA-free orbits, followed by 7-9 SAA orbits with no observations, followed by the 4 consecutive SAA-free orbits.
The transit durations of b and c are 3.2 hours and 4 hours, corresponding to 2 and 2.5 orbits respectively. Our 5-orbit sequence will therefore capture the entire transit. We require observations before the transit to establish a pre-transit baseline, and observations after the transit in case the exosphere has an extended egress (as is the case for many other exoplanets). Because we can accomodate ~1 h of timing uncertainty, we set the phase requirements to +- 0.5 hours. The ephemeris uncertainty will add (in quadrature) another +- 0.5 hours by the end of 2020, although we are hoping to have an ephemeris update by the end of 2020.
We planned our observations so that the first orbit of each visit has an ACQ and ACQ-PEAKUP exposure, followed by a science exposure and wavelength calibration. Subsequent orbits only have a science exposure and a wavelength calibration exposure, with no ACQ or ACQ-PEAKUP. Because the few minutes' difference in orbital visibility due to precession has minimal impact on our science, we change the schedulability parameter from 30 to 90 to make scheduling easier. If possible, we kindly ask the Program Coordinator to expand our science observations to fill up the entire orbital visibility for the orbits that are actually scheduled.
Reduced gyro mode impacts our program by limiting the number of scheduling opportunities, which is already severely limited by planet c's long period (20.5 days). Otherwise, we do not forsee major impacts from RGM.Michael Zhang studies exoplanet atmospheres and has experience in analyzing HST data, especially WFC3 transmission spectra. He has additionally studied mass loss using Keck/NIRSPEC.
Heather Knutson has extensive expertise in many areas of exoplanet atmosphere observations, especially with HST and Spitzer.
Fei Dai is an expert on numerical modelling of exoplanet mass loss, especially from small planets such as mini Neptunes.
Shreyas Vissapragada is an expert on exoplanet exosphere observations, having developed a Palomar P200 filter that allows photometric measurement of escaping helium.
Yayaati Chachan is an expert on exoplanet atmospheres, and has studied the role of outgassing in mitigating atmospheric escape from super Earths.Exoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMG V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoG140M1222Timing link suitability includes constraints ([02 After 01 by 0.7 to 1.2 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.1611851515000118.68065832882138(Tic-Visit
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