Final submission.1554274968Assigned ID: 2573
----- Attempting Submission 1 (Wed Sep 29 13:38:36 GMT 2021) -----
HST Phase I Proposal 2573 successfully submitted.
Receipt: # 2573-1
----- Attempting Submission 2 (Thu Sep 30 15:48:53 GMT 2021) -----
HST Phase I Proposal 2573 successfully submitted.
Receipt: # 2573-2
----- Attempting Submission 3 (Thu Sep 30 17:52:44 GMT 2021) -----
HST Phase I Proposal 2573 successfully submitted.
Receipt: # 2573-3
----- Attempting Submission 4 (Thu Sep 30 20:08:02 GMT 2021) -----
HST Phase I Proposal 2573 successfully submitted.
Receipt: # 2573-4
----- Attempting Submission 5 (Thu Sep 30 20:13:40 GMT 2021) -----
HST Phase I Proposal 2573 successfully submitted.
Receipt: # 2573-5
----- Attempting Submission 6 (Thu Sep 30 20:20:22 GMT 2021) -----
HST Phase I Proposal 2573 successfully submitted.
Receipt: # 2573-6We may relax the orientation requirements to alleviate the constraints on schedulability. We will notify our PC with the new values for the orientation range if need be.
We will double check the phase at the start of the first orbits when we have determined our observation windows.1148136130----- Attempting Submission 1 (Wed Dec 15 17:08:42 GMT 2021) -----Reconnaissance Transmission Spectroscopy of The BEST Temperate Mini-Neptune for Atmospheric CharacterisationroundWith no equivalent in our Solar system, sub-Neptunes and super-Earths are the most common categories of planet discovered so far. Formation models predict that they are one and the same: both composed of rocky cores, with sub-Neptunes retaining extended atmospheres, while super-Earths lose them early on. The puffy atmospheres of the smallest sub-Neptunes are outstanding candidates for atmospheric characterisation, as they represent an important step towards the study of Earth-analogs. Particularly, there is growing interest in exploring the atmospheres of temperate sub-Neptunes as these could be harbouring liquid water. In this context, TOI-4336 b is of the highest interest due to the parameters of the system putting it at the top of the list of temperate candidates for atmospheric exploration.
In anticipation of in-depth characterization with HST and the upcoming JWST, it is essential to perform atmospheric reconnaissance in order to discriminate between a clear H-dominated atmosphere (e.g. K2-18b) and a cloudy one (e.g. GJ 1214 b) which prevents the detection of absorbers. We propose the observation of TOI-4336 b with HST's WFC3 and the G141 grism in order to obtain a transmission spectrum covering the range between 1.1 and 1.7 microns. With this Mid-Cycle proposal we expect to probe the upper layers of the atmosphere and detect the presence of water vapour with only three transits at the 5 sigma level, confirming our hypothesis this sub-Neptune is ideal for a full atmospheric characterisation.TOI-4336 b is a temperate mini-Neptune (2.63 +/- 0.16Rp) with an orbital period of 16.33 days around a nearby (22pc) M4.5 star. The planet's equilibrium temperature of +/-300K, the exceptional brightness in J-band of the host (J=9.45) and its small radius (0.32 +/- 0.1Rs) give this planet an expected transmission spectroscopy metric TSM +/- 100-120, making it THE most favourable temperate mini-Neptune for transmission spectroscopy. The goal of our proposal is to probe the outer parts of the atmosphere of this sub-Neptune in the hopes of finding molecular signatures such as the one of water.
We request 12 orbits to observe three full transits of TOI-4336 b with the WFC3 G141 grism, with four orbits per transit. Owing to its high TSM, our calculation showed that with just three transits, we will be able to distinguish between the clear and cloudy atmosphere for TOI-4336 b, and in case of cloudless atmosphere detect the atmospheric water signal at greater than 5sigma level similar to K2-18 b. We ask for 3 transits to have some redundancy in our data, and build towards the detection of water feature at better than 16sigma level according to our simulations, or 5sigma level in the case of a dense mini-Neptune.We are the SPECULOOS team, and have confirmed TOI-4336b in transit from Cerro Paranal using our telescopes. We aim to continue using them, as well, as TRAPPIST-South to continue the photometric characterisation of this exciting new planetary system, and support our HST observations. We also have access to ASTEP in Antarctica. Teams members are all very experienced at detecting exoplanets, particularly those that orbit low-mass stars, using the transit and radial-velocity methods. Our team notably discovered the TRAPPIST-1 system. We also have a track record of rapidly transforming candidate planets into impactful discovery papers.
PI Georgina Dransfield: PhD student at the University of Birmingham, working on the confirmation and characterization of exoplanetary systems unlike the solar system. She is leading the ESO P109 109.2343 proposal to get precise mass measurement of TOI-4336 b. She has experience with HST WFC3 data analysis with her paper presenting how colour-magnitude diagrams and colour indexes can be used constrain the C/O ratio of exoplanets. She will participate in the reduction and analysis of the HST data with the purpose of publication in collaboration with Mathilde Timmermans.
Co-PI Mathilde Timmermans: PhD student at the University of Liege, works on the confirmation and characterization of super-Earths and sub-Neptunes from TESS. She is leading the validation paper of TOI-4336 b that Nature Astronomy has agreed to consider for publication. She is co-I in the ESO P109 109.2343 led by Georgina Dransfield for precise mass measurement of TOI-4336 b with ESPRESSO. She will participate in the reduction and analysis of the HST data under the supervision of Prof. Julien de Wit and Dr. Michael Gillon for future publication in collaboration with Georgina Dransfield.
Co-I Prof. Julien de Wit: has significant expertise in the detection and characterization of transiting planets and in the analysis of space-based infrared data. He was part of the team behind the discovery of the TRAPPIST-1 system, led the atmospheric reconnaissance of the planets with several HST programs (GO 14500, 2016Natur.537...69D; GO 14873, 2018NatAs...2..214D), and enabled new characterization techniques notably with the Spitzer Space Telescope (2016ApJ...820L..33D ). He will train the PIs accordingly.
Co-I Prajwal Niraula: has been focusing on the cross-section roles in transmission spectroscopy and uncertainty budgeting particularly in JWST. He is also a maintainer of tierra-transmission spectroscopy code developed at MIT and which will soon be released with the paper. He has been part of the effort for follow-up observation for GJ 9827 b system with HST (GO 15434, 2021AJ....161..136C). He ran the simulations for our HST data.
Co-I Prof Amaury Triaud: Is leading the confirmation of TESS planets orbiting M-Dwarfs as part of the SPECULOOS team. He has abundant experience in populations studies of the atmospheres of transiting exoplanets. He was part of the team behind the discovery of the TRAPPIST-1 system. Dr Triaud is also experienced in the analysis of transmission and emission spectroscopy data using Spitzer. He supervises Georging Dransfield and will guide her in the analysis of the HST data.
Co-I Dr Michael Gillon: is an expert in the detection and characterization of transiting planets. He led the discovery of the TRAPPIST-1 system. He was as PI and CoI of numerous Spitzer programs and was CoI of HST programs 13501, 11306, 14873, 14900, 14906, and 15304. He also initiated and chairs with V. Meadows the "TRAPPIST-1 JWST Community Initiative" which aims to maximize the scientific return of the upcoming study of TRAPPIST-1 planets with Webb.Exoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMM V-IVJ2000J2000WFC3/IRSpectroscopicNoNoG141Timing link suitability includes constraints ([02 After 01 by 0.1 to 0.1 days])The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode./System/Volumes/Data/solaris/user1/williamj/hst/work/cycle29/OP-cache/16875-v01.xml165510949000078.0(Tic-Visit
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