0
Assigned ID: 893
----- Attempting Submission 1 (Fri Apr 05 22:50:03 GMT 2019) -----
HST Phase I Proposal 893 (toi270.apt) successfully submitted.
Receipt: # 893-1
----- Attempting Submission 2 (Fri Apr 05 23:57:27 GMT 2019) -----
HST Phase I Proposal 893 (toi270.apt) successfully submitted.
Receipt: # 893-2
The number of orbits used exceeds the number allocated
Unschedulable Visit
Unschedulable Visit
2022-Sep-26
Corrected timing requirements (date ranges). Otherwise the same as last submission.
2022-Sep-23
(I did not get a confirmation that the previous submission succeeded, so this is a re-attempt)
Trying to schedule the final 5 orbits of this program to observe a transit of TOI-270d.
Once this observation has been made, the program will be complete. In this submission,
the following visit opportunities are retained from the last submission:
4E, 4F, 4G, 4H, 4J
and the following visit opportunities have been added:
4K, 4L, 4M, 4N, 4O
Note that visits 4E-4J previously had 4 HST orbits, but they have been
edited to 5 HST orbits in this submission (which is also the number of
HST orbits that visit opportunities 4K-4O have).
Aug 13th 2022.
- Note that visit 4C has previously been submitted and
has been flagged as schedulable.
- In addition to 4C, we need one more transit visit to be
scheduled to complete this program.
- To this end, we've added new transit visit opportunties
4E, 4F, 4G, 4H, 4I, 4J.
i.e. one of these need to be scheduled in addition to 4C
if possible.
Jul 14th 2022.
- Added new visit opportunities 4C and 4D for September.
- Loosened phase constraints on all visits to 0.99693-0.00056,
corresponding to a 60 minute window (up from a 50 minute
window in the last submission).
- Added POST TARG Y -20.
Jul 6th 2022. Submission #2
Identical to previous submission except that most visits opportunities have been
removed, to just focus on those opportunities in the next 2 months.
Jul 6th 2022. Submission #1
Loosened the phase constraints applied on the following visits:
3U, 3V, 4A, 4B, 4C, 4D, 4E, 4F, 4G, 4H, 4I, 4J, 4K, 4L, 4M, 4N
from 0.99785-0.99965 (i.e. 30 minutes)
to 0.99724-0.00026 (i.e. 50 minutes).
Note the new 'Phase end' of 0.00026 is assumed to be the same
as 1.00026, but APT only allows values between 0-1 to be entered.
Jun 16th 2022.
Converted the visits listed below from 3-orbit to 4-orbit visits.
Deleted the old 3-orbit visits (lefthand column below).
3-orbit --> 4-orbit
3A --> 3W
3B --> 3X
3C --> 3Y
3D --> 3Z
3E --> 4A
3G --> 4B
3I --> 4C
3J --> 4D
3K --> 4E
3L --> 4F
3M --> 4G
3N --> 4H
3O --> 4I
3P --> 4J
3Q --> 4K
3R --> 4L
3S --> 4M
3T --> 4N
May 22nd 2022.
Had PCR approved to convert 3x 3-orbit visits converted to 2x 4-orbit visits.
This submission adds 4-orbit visits 3U and 3V, which are intended to replace
the currently scheduled 3-orbit visits 3F and 3H.
Mar 16th 2022.
1. Fixed an error in the "Zero Phase (HJD)" timing constraints for the TOI-270d visits of the last submission.
2. Updated the "Zero Phase (HJD)" values for a subset of the TOI-270c visit opportunities out to June 2022
and deleted visit opportunities from July 2022 onward, i.e. what used to be visits 1K-2T. The latter was
done due to the limited time I have available right now - these visit opportunities can be added in later as
new visits with updated "Zero Phase (HJD)" values.
3. For the updated TOI-270c visit opportunities that are still included (i.e. 0T-1J), set "Observability = 100".
Mar 15th 2022.
MAJOR UPDATE: Have now set "Observability = 100" and adjusted the exposures in each orbit accordingly
(was previously set to the default "Observability = 30"). So far this has only been done for TOI-270d
visits and involved deleting old TOI-270d visits (with the exception of visits 89 and 91 which were
kept and edited - for some reason when I edited the other old visits APT would give errors and Orbit
Planner returned nonsensical results) and adding new visits 2V-3T. The phase constrain for all of
these TOI-270d visits is now applied to the 1st exposure of the 2nd orbit of each visit (previously
it was applied to the last exposure of the 2nd orbit).
Mar 4th: Removed visits labelled as 'Withdrawn'.
Feb 14th 2022: Added new visit opportunities OQ through to 2T.
For the program to be completed, we require:
(1) 3x transits from visit opportunities 89 to OP, i.e. planet TOI-270d.
(2) 1x transit from visit opportunties OQ to 2T, i.e. planet TOI-270c.
Note that the planet names (TOI-270c and TOI-270d) are included in the visit labels.
Feb 10th 2022: Revised visits 89 and 90. Also submitted new visit opportunities (91 through to OP), all for TOI-270d transits.
May 27th 2021: Added visits 86, 87, 88, 89, 90. Aim is to schedule the remaining 3x transit observations for TOI-270d.
May 12th 2021: Updated timing "Epochs" for Visits 76, 77, 78, 84, 85.
Added new transit opportunities covering the period Jan-Jul 2021.
TOI-270c:
- Still require 1x transit observation.
- New visit opportunities are 67-78.
TOI-270d:
- Still require 3x transit observations.
- New visit opportunities are 79-85.
In each orbit there are 8x "Round-Trip" science exposures with NSAMP=7.
Note that final "Forward" exposure of 2nd orbits are phase-constrained and shorter (NSAMP=3) than the science exposures.
239460295
----- Attempting Submission 1 (Thu Jul 25 22:15:15 GMT 2019) -----
----- Attempting Submission 2 (Fri Sep 27 20:21:32 GMT 2019) -----
----- Attempting Submission 3 (Wed Oct 16 12:51:17 GMT 2019) -----
----- Attempting Submission 4 (Fri Dec 13 21:40:06 GMT 2019) -----
----- Attempting Submission 5 (Fri Dec 20 06:06:31 GMT 2019) -----
----- Attempting Submission 6 (Tue Mar 31 14:22:18 GMT 2020) -----
----- Attempting Submission 7 (Thu Jun 25 23:41:47 GMT 2020) -----
----- Attempting Submission 8 (Fri Dec 18 11:57:45 GMT 2020) -----
----- Attempting Submission 9 (Wed May 12 12:55:46 GMT 2021) -----
----- Attempting Submission 10 (Thu May 27 21:50:21 GMT 2021) -----
----- Attempting Submission 11 (Thu Feb 10 12:15:00 GMT 2022) -----
HST Phase II Proposal 15814 successfully submitted.
Receipt: # 15814-11
----- Attempting Submission 12 (Mon Feb 14 14:35:02 GMT 2022) -----
----- Attempting Submission 13 (Fri Mar 04 16:02:08 GMT 2022) -----
----- Attempting Submission 14 (Tue Mar 15 09:15:42 GMT 2022) -----
----- Attempting Submission 15 (Wed Mar 16 12:44:39 GMT 2022) -----
----- Attempting Submission 16 (Sun May 22 16:55:07 GMT 2022) -----
----- Attempting Submission 17 (Thu Jun 16 11:03:42 GMT 2022) -----
----- Attempting Submission 18 (Wed Jul 06 16:02:55 GMT 2022) -----
HST Phase II Proposal 15814 successfully submitted.
Receipt: # 15814-18
----- Attempting Submission 19 (Wed Jul 06 16:12:53 GMT 2022) -----
----- Attempting Submission 20 (Thu Jul 14 06:59:31 GMT 2022) -----
----- Attempting Submission 21 (Sat Aug 13 16:25:15 GMT 2022) -----
----- Attempting Submission 22 (Fri Sep 23 17:08:36 GMT 2022) -----
----- Attempting Submission 23 (Fri Sep 23 17:15:56 GMT 2022) -----
----- Attempting Submission 24 (Mon Sep 26 20:04:06 GMT 2022) -----
Visit opportunities flagged as 'unschedulable' have not been removed, in case there's any chance they
actually can be scheduled in practice.
Atmospheric characterization of two temperate mini-Neptunes formed in the same protoplanetary nebula
The TESS mission recently uncovered a remarkable multi-planet system consisting of a super-Earth and two temperate mini-Neptunes around the bright M3 dwarf star TOI-270. Here we propose to acquire near-infrared transmission spectra for the two mini-Neptunes (TOI-270 c&d) across the 1.1-1.6 micron wavelength range using WFC3. Both TOI-270 c&d are exceptionally favorable targets for transmission spectroscopy, despite having low equilibrium temperatures of 340K and 420K. This provides an unprecedented opportunity to compare the atmospheres of two planets belonging to this enigmatic class that formed from the same protoplanetary nebula. Chemical equilibrium models predict methane will be the dominant infrared absorber for both atmospheres, representing an uncharted chemistry regime for exoplanets. Our observations will have the sensitivity to measure methane abundances to within 1dex for metallicities up to 1000x solar, placing the first direct constraints on mini-Neptune chemical composition. Given the temperatures of TOI-270 c&d, condensed H2O or KCl clouds are not expected at the pressures probed by the transmission spectrum. However, photochemical haze may be present in one or both atmospheres. If so, our observations will provide a unique test of how photochemical haze production correlates with incident UV flux and planet temperature, given that both planets orbit the same star. As part of our program, we will also make use of HST's unparalleled UV capabilities to measure the stellar Lyman-alpha emission using STIS, providing an essential input to photochemical models.
There is a single target star for our program (TOI-270) and we will observe transits for two different planets orbiting this star. However, since the planets in this system exhibit significant transit timing variations (TTVs), the phasing must be carefully specified for each transit event. In other words, we cannot use a single ephemeris (i.e. the time corresponding to mid-transit) and orbital period for each planet. Instead, we need to specify an ephemeris for each transit event individually. To achieve this in APT, we have defined multiple "Targets", one for each *transit event* occurring between 2019 October 1st and 2020 October 1st for both of the planets. In all cases, the same star (TOI-270) is the actual target being observed.
Thomas Evans, Ian Crossfield, and Laura Kreidberg are experts in designing WFC3 observations of exoplanet transits and analyzing the data.
Maximilian Guenther led the discovery of the TOI-270 planets and has expertise in the Big Picture interpretation of this system. He is also coordinating much of the ground-based follow-up campaign, which will provide important support for the HST observations.
Nikku Madhusudhan is an expert in exoplanet atmosphere modeling and will conduct the retrieval analysis for this program, along with PhD student Luis Welbanks.
Ben Drummond is an expert at modeling exoplanet atmospheres and will lead the modeling of non-equilibrium effects (photochemistry and 3D circulation) for this program.
Tansu Daylan and Jason Dittmann are experts at analyzing transit timing variations, which must be accounted for in scheduling the HST observations.
Jason Dittmann is also an expert at using HST to characterize Lyman-alpha emission of M dwarfs, which is a major goal of our program.
Laetitia Delrez and Amaury Triaud are experts at analyzing transit data for multi-planet systems, providing valuable experience for our program.
Vincent Van Eylen is leading the ESPRESSO radial velocity program to measure masses for the TOI-270 planets, which will be crucial for our interpretation of the transmission spectra.
Planets and Planet Formation
0
false
false
false
false
false
false
false
SUPPORTED
STAR
EXTRA-SOLAR PLANETARY SYSTEM
Copied ICRS J2000 coordinates and proper motions from SIMBAD by hand.
J2000
J2000
J=9.099, H=8.531
WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Spectroscopic
No
No
G141
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
The scheduling data was generated by CASM 29.2.
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In this UV observation, we will measure the Lyman-alpha flux from the host star.
These observations must be scheduled far from times of transit by the three known planets in the TOI-270 system. The transit ephemerides for these planets are:
1. Planet b
Transit mid-time (JD) = 2458461.01464
Orbital period (day) = 3.360080
2. Planet c
Transit mid-time (JD) = 2458463.08481
Orbital period (day) = 5.660172
3. Planet d
Transit mid-time (JD) = 2458469.33834
Orbital period (day) = 11.38014
In practice it might make sense for this UV observation to be scheduled and then a check performed that it does not coincide with transits by any of the three known planets.
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The scheduling data was generated by CASM 29.2.
CASM was run in Phase II mode.
In this UV observation, we will measure the Lyman-alpha flux from the host star.
These observations must be scheduled far from times of transit by the three known planets in the TOI-270 system. The transit ephemerides for these planets are:
1. Planet b
Transit mid-time (JD) = 2458461.01464
Orbital period (day) = 3.360080
2. Planet c
Transit mid-time (JD) = 2458463.08481
Orbital period (day) = 5.660172
3. Planet d
Transit mid-time (JD) = 2458469.33834
Orbital period (day) = 11.38014
In practice it might make sense for this UV observation to be scheduled and then a check performed that it does not coincide with transits by any of the three known planets.
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