For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.0Assigned ID: 4412
----- Attempting Submission 1 (Wed May 24 16:45:32 GMT 2023) -----
HST Phase I Proposal 4412 successfully submitted.
Receipt: # 4412-1
----- Attempting Submission 2 (Wed May 24 18:14:05 GMT 2023) -----We will use LP6 for COS G160M and 2 LP-POS positions becuase our S/N requirements are <20.Visit 02 failed and HOPR 93009 was approved to retake. Re-submitting to hopefully get the observations scheduled soon.1763442723----- Attempting Submission 1 (Mon Sep 11 15:13:25 GMT 2023) -----
HST Phase II Proposal 17503 successfully submitted.
Receipt: # 17503-1
----- Attempting Submission 2 (Wed Sep 13 08:32:35 GMT 2023) -----
----- Attempting Submission 3 (Fri Dec 01 15:18:43 GMT 2023) -----
----- Attempting Submission 4 (Mon Jan 08 10:46:47 GMT 2024) -----
HST Phase II Proposal 17503 successfully submitted.
Receipt: # 17503-4
----- Attempting Submission 5 (Tue Jan 09 08:33:45 GMT 2024) -----
----- Attempting Submission 6 (Mon Mar 04 09:37:39 GMT 2024) -----
HST Phase II Proposal 17503 successfully submitted.
Receipt: # 17503-6
----- Attempting Submission 7 (Mon Mar 04 15:14:22 GMT 2024) -----
----- Attempting Submission 8 (Tue Mar 12 08:51:49 GMT 2024) -----
HST Phase II Proposal 17503 successfully submitted.
Receipt: # 17503-8
----- Attempting Submission 9 (Tue Mar 12 09:38:37 GMT 2024) -----
----- Attempting Submission 10 (Wed Mar 20 08:38:30 GMT 2024) -----
----- Attempting Submission 11 (Sat Jun 15 09:45:23 GMT 2024) -----
----- Attempting Submission 12 (Thu Dec 05 15:08:02 GMT 2024) -----Visitibility overruns for Visits that are already completed or scheduled before July 7. FP-POS choices are to ensure coverage of the Mg II line, which not all positions cover.Hot Rock Stars: Capturing high-energy spectra of 5 M dwarfs hosting terrestrial exoplanets that JWST will test for atmospheresWith the launch of JWST we are finally in a position to determine if terrestrial exoplanets orbiting M dwarfs can develop and retain atmospheres in the presence of their hosts' harsh high-energy environments. Necessary to the interpretation of any planetary atmospheric data is the measured high-energy spectra, from the UV to the X-ray, of the M dwarf hosts. A JWST Cycle 2 Large program will survey nine rocky worlds orbiting nearby M dwarfs for the presence of atmospheres. If the rocky worlds in the JWST sample show evidence of having atmospheres, high-energy spectra of their host stars are needed to determine photochemical production rates of key molecular species, such as water, methane, carbon dioxide, and ozone. These constraints will alert us to disequilibrium chemistry, which can be a sign of surface processes such as volcanism and mantle outgassing. On the other hand, if the rocky worlds in the JWST sample are airless, high-energy spectra of their host stars are needed to calculate atmospheric mass-loss rates, which can explain how an atmosphere was lost, or could never form. Of the nine M dwarf planet hosts in the large JWST program, five are amenable to high-energy spectral observations, yet lack them. Only HST can capture the critical UV information, which we will supplement with X-ray observations, to provide a complete picture of the high-energy output of these M dwarf hosts. We request 47 HST orbits to capture the UV spectra of these five M dwarfs. Making these UV observations while HST is still operational is critical to the scientific output of JWST, and will further our understanding of the complexities of M dwarfs as long-lived exoplanet hosts.We will observe the complete UV spectra into the blue optical of five nearby M dwarfs hosting terrestrial exoplanets that are the subject of atmospheric investigations by JWST (the Hot Rocks Survey), as well as five sibling planets that are enhanced in volatiles. We will use HST/COS and STIS to measure the UV spectra of these five stars from 1050--5700 Angstroms. Where possible, data will be obtained in TIME-TAG mode so that we can monitor the stars' flaring activity during the exposures. Where possible, we will use the FLASH=YES setting to maximize exposure time on target.
For the purposes of estimating exposure times, we scale HST/COS and STIS data from M dwarfs in the (Mega-)MUSCLES programs (France et al., 2016; Froning et al., 2019) to each star in our sample. We choose the (Mega-)MUSCLES star to scale by their similarity in radius and effective temperature to each target star. For example, we take the M3 dwarf GJ 436 and scale it to the distance and stellar radius of HD 260655 to compute the exposure times we need to reach the target S/N in key transition region lines, Ly-alpha line wings, or NUV continuum. The stars in our sample can be considered inactive based on low activity indicators and long stellar rotation periods.
FUV: To measure prominent emission lines in the FUV we will use COS G130M (C iii, Si iii, N v, C ii) and COS G160M (Si iv, C iv, He ii). Exposure times for each target will provide S/N ~5 for N v, C ii, and C iv, the most prominent lines in the FUV. Remaining lines should also be detectable, but at a minimum S/N of 2 to 4. In alignment with the COS2025 policies, we choose a central wavelength of 1222 Angstrom for the G130M grating to place the Ly-alpha line in the gap between the A and B segments. We choose a central wavelength of 1533 Angstrom for the G160M observations so that they overlap the G130M observations without leaving a gap. Following the recommendation of the COS User Manual for G160M, we will use 2 FP-POS positions at LP6 to minimize overheads since our S/N requirements are <20.
NUV: For the NUV we will use short (< 1 orbit) exposures with COS G230L. COS G230L has a high sensitivity to the 1750--2100 Angstrom wavelength region, however, this grating misses a chunk of the NUV continuum, which is an important input to photochemical models. We make up for the missing NUV flux with the STIS G230L grating, where we also capture Fe ii and Mg ii lines. For COS/G230L observations we use two of the four FP-POS offsets to save overhead. Four FP-POS offset positions are available: a nominal position (0), two positions toward longer wavelengths (-2 and -1), and one position toward shorter wavelengths (+1). Positions -2, -1, 0, and +1 are designated respectively as FP-POS=1, 2, 3, and 4. The nominal position, FP-POS=3, is the setting used to define the wavelength range associated with the grating central wavelengths. We use FP-POS=3 and 4 becuase in these positions the Mg II line at ~2800 A is still observed. At FP-POS = 1 and 2 the Mg II line is cut off. We will take brief exposures with the STIS G430L grating which provides coverage from 2900|--5700 Angstroms. For all targets, we spend ~1 orbit each to capture NUV flux with the G230L and G430L gratings; we already expect plenty of S/N in these filters so separating out the wavelength calibration is not necessary.
Ly-alpha : For the brightest star in our sample, HD 260655, the Ly-alpha line profile can be reconstructed by measuring flux in the line wings (Youngblood et al., 2016). We set WAVECAL=NO and add a specific Wavecal observation after the orbit in order to increase exposure time. We do this becuase we want the highest S/N possible in the wings of the Ly-alpha line in order to perform a reconstruction.1) Professor Lars Buchhave is an expert in spectroscopic observations and interpretations of exoplanets, their host stars, and their atmospheres.
2) Dr. Hannah Diamond-Lowe is an observational astronomer specializing in investigations of exoplanet atmospheres and the high-energy environments provided by M dwarf host stars. She is the PI of two successful HST/COS and STIS programs (GO Programs 15704 and 16722) to capture UV spectra of planet-hosting M dwarfs similar to the targets in this program, and of a large JWST program (GO 3730) to observe the terrestrial exoplanets orbiting the targets in this proposal. HDL's UV-related work can be found in Diamond-Lowe+ (2021, 2022).
3) Dr. Maximilian N. Guenther is an expert in the analysis of space- and ground-based photometric and RV observations, in particular characterizing M dwarf exoplanets and flares using TESS data set. He is the lead author on the L 231-32 discovery paper (one of the targets in this proposal; Guenther+ 2019) and he coordinates the global TTV follow-up campaign from space and ground (e.g. Kaye+ 2022). MNG also supports several atmospheric characterization studies/proposals for L 231-32 using Spitzer, HST, JWST.
4) Dr. George King has substantial experience with analysing data of late-type stars taken with a slew of X-ray telescopes (XMM-Newton, ROSAT, Swift, and Chandra). He has used these measurements to characterize the XUV environments of numerous exoplanets, including current mass loss rates, and assessing the evolution of exoplanet atmospheres that results from XUV irradiation.
5) Dr. Laura Kreidberg is an expert in observational characterization of exoplanet atmospheres and has led numerous Hubble observing programs with both HST/WFC3 and COS.
6) Dr. Joao Mendonca is an expert in theoretical modeling of planet atmospheres, which includes using molecular cross-sections at UV wavelengths. These data can be passed as inputs to his atmospheric modelling platform, OASIS.
7) Dr. Thomas Mikal-Evans is an expert in exoplanet atmospheric characterization with both HST and Spitzer. He is the PI of GO Program 15814 to investigate the atmospheres of the two sub-Neptune worlds in the L 231-32 system, one of the targets in the proposed sample.
8) Dr. Allison Youngblood is an expert in UV spectroscopy of cool dwarf stars, specifically Ly-alpha reconstructions and stellar flare analysis with STIS and COS data. She is the PI of a recent large program to broadly capture the high-energy spectra of JWST Cycle 1 exoplanet targets (GO Program 16701), as well as many other COS and STIS programs (e.g., GO 15190 and 15463). She is a leading participant in the HST MUSCLES and Mega-MUSCLES Treasury Surveys (GO 13650 and 15071).Exoplanets and Exoplanet Formation6falsefalsetruefalsefalsefalsefalsetruePRIMARY45trueSUPPORTEDSTAREXTRA-SOLAR PLANETARY SYSTEMM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database. Updated by PI Diamond-Lowe from Gaia DR3 using astroquery. V-magnitude from Luque, et al. 2022.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database. Updated by PI Diamond-Lowe from Gaia DR3 using astroquery.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database. Updated by PI Diamond-Lowe from Gaia DR3 using astroquery. V-magnitude from Cloutier, et al. 2020.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database. Updated by PI Diamond-Lowe from Gaia DR3 using astroquery.J2000J2000STAREXTRA-SOLAR PLANETARY SYSTEMM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database. Updated by PI Diamond-Lowe from Gaia DR3 using astroquery.J2000J2000COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG230L2950STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG230L2950STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG230L2950STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG230L2950STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG230L2950STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/CCDSpectroscopicNoNoG430L4300The scheduling data was generated by CASM 32.1.CASM was run in Phase II mode.1725330706000270.7543523463559(Tic-Visit
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