0Assigned ID: 484
----- Attempting Submission 1 (Fri Apr 05 15:37:09 GMT 2019) -----Changed STIS-ACCUM to STIS-TIME-TAG and included BUFFER TIMEs accordingly-557197372----- Attempting Submission 1 (Thu Jul 25 14:09:54 GMT 2019) -----
----- Attempting Submission 2 (Thu Oct 03 19:14:38 GMT 2019) -----Exocometary gas inventories at the epoch of volatile deliveryThe presence of exocometary gas in young (10-100 Myr) debris disks presents a unique opportunity to probe the composition of exocomets during the late stages of terrestrial planet formation. This is the evolutionary stage when ice-rich impacts are proposed to change the volatile environment of terrestrial planets, setting the stage for prebiotic chemistry.
In these young exocometary belts, high concentrations of debris result in frequent collisions and release of molecular gas, which rapidly photodissociates to produce atomic gas. Atomic inventories can only be comprehensively probed at UV wavelengths with HST, in absorption against the stellar background, within systems that are viewed edge-on.
We propose a UV chemical survey of gas released in two newly discovered, 15-16 Myr old exocometary belts around A stars HD110058 and HD131488. These are ideal targets as they are edge-on, rich in molecular gas based on CO emission detected by ALMA, and present circumstellar gas absorption at optical wavelengths. Exploiting the ALMA-HST synergy will allow us to put better constraints on the composition of these belts than ALMA observations alone can provide.
We will use COS and STIS to measure abundance ratios such as C/O, C/N and C/Fe and further model the elemental composition of exocometary belts. These ratios will be compared to exoplanets, young disks and Solar System comets, providing a missing link in the study of planet formation and physical-chemical evolution.
Finally, splitting our observations into several visits will enable us to look for star-grazing exocomets, providing evidence that inward scattering, and potentially volatile delivery, is ongoing in these systems.Our goal is to carry out a UV spectroscopic line survey of the edge-on exocometary belts around A stars HD110058 and HD131488, detecting all species of interest (N I, O I, C I, C II, C IV, CO, Mg I, Mg II, Al I, Al II, Si I, Si II, S I, Fe I and Fe II) seen in absorption against the stellar continuum. The shortest wavelength region we will observe in the FUV covers strong resonantlines of N I(1200A), O I(1302A)and C II(1335A). So far, these have been found to be the most abundant species in exocometary gas belts (e.g. Roberge et al., 2006; Wilson et al., 2019). Being the species of interest with the shortest wavelength transitions (where the stars are faintest), N I (1200A) COS observations drive our sensitivity and hence orbit request. Our calculations show that, even if carbon is depleted by a factor of 10 compared to the famous exocometary gas host beta Pictoris, the strength of the N I line ensures that we can detect nitrogen in our targets even for C/N ratios as high as found for the bulk silicate Earth (C/N~49). We note that atomic hydrogen may be abundant if water is being released with the observed CO (and then rapidly dissociated) from the exocomets. However, Lyman series detection of H I is prevented by severe airglow contamination, so we deem hydrogen detection unfeasible.
Given the steeply decreasing stellar spectrum at shorter FUV wavelengths, meeting our sensitivity requirement to detect these transitions requires use of COS below ~1500A. Therefore,we request use of the COS G130M grating,centered at 1222A, covering resonant lines of C I, C II, O I, N I and Si II. Longward of 1500A, STIS is able to detect transitions of interest, and we prefer it to COS given its advantage in resolving power (R=114000 vs R=14000 for COS) which is crucial to extract information on the absorption profiles and enable accurate modelling of the lower resolution COS spectra. At the velocity resolutions of ~2.6 (STIS) and ~21 km/s (COS), we expect that lines will be unresolved, unless heavily saturated, in which case we will use weaker, optically thin lines of the same species to constrain the gas column densities. The fact that lines will be unresolved is acceptable since we are most interested in column density, rather than line broadening measurements; the gas excitation temperature will instead be retrieved from comparison of absorption lines originating from different low-lying energy levels (available e.g. for C I, C II, O I and CO, as shown in Roberge et al., 2000).
Note that the resolution of STIS is also sufficient to separate circumstellar absorption lines from any absorption lines originating from the local interstellar medium (ISM). Optical spectroscopy indicates that potential ISM lines lie ~11.5 and ~7.2 km/s away from the stellar velocities of HD110058 and HD131488 (Rebollido et al., 2018). While COS will not be able to resolve these from circumstellar absorption, for the affected species we will be able to establish the contribution of the circumstellar component using a combination of 1) absorption lines from energy states above ground covered by COS, which are not expected from ISM gas, 2) other absorption lines from the same species observed at higher resolution by STIS, and 3) lines from other species expected to have similar ISM abundances observed by STIS.
We request four STIS spectral settings, all observed with the narrow spectroscopic slit (0.2"x0.09") recommended for the highest spectral resolution gratings and for minimizing air- glow contamination. In the FUV, we will use the E140H grating (i1562) to cover the CO A-X 0-0 (1544A), 1-0(1510A) and 2-0(1478A) bands, as well as resonant lines of C I(1560A,1657A), C IV (1548A) and Al II (1671A). In the NUV, we will use the E230H grating in 3 settings (c1763, i2463, and i2912) to cover the region between 1600 and 3000 A containing resonant transitions of remaining species S I Al I, Si I, Fe I, Fe II, Mg I and Mg II.
To predict UV stellar fluxes, since the shortest wavelength measurement available for both stars is U band, we ran a fit to the UBV, JHK, and Gaia G, BP and RP photometry using MESA evolutionary tracks through the isochrones python code. We use the best fit parameters (including Teff and AV as reported here in APT) to derive a probability distribution for predicted GALEX FUV magnitudes. To double-check, we also ran a fit using the pysynphot package which employs the same Castelli and Kurucz models as the ETC. While the Castelli-Kurucz best-fit Teffs are cooler by a few hundred K, the fits are also less extincted compared to the MESA results, leading overall to a similar predicted distribution of GALEX FUV magnitudes. Note that the spectral types reported by SIMBAD (A0V and A1V) come from a very old spectral catalog from optical plates measurements, and likely less reliable than the photometric fits carried out here.
We will also search for variability on day/week timescales in the line wings, originating from star-grazing exocomets. We request 4 (3) separate COS visits for HD110058 (HD131488) and 2 separate STIS visits covering the 1763 A setting for HD110058; these visits will be separated by 3-14 days from one another.Dr. Luca Matra, Dr. Meredith Hughes and Dr. David Wilner are experts in debris disk observations and modelling, particularly at millimeter wavelengths. Dr. Matra and Dr. Hughes in particular are experts in observations of exocometary line emission and radiative transfer. Dr. Matra is also an expert in modelling of molecular and atomic excitation which will be highly relevant for the multi-species, multi-transition UV line survey proposed here.
Dr. Karin Oberg and Dr. Wilner have extensive expertise related to gas in younger protoplanetary disks, which will help draw the link with exocometary gas. Additionally, Dr. Oberg is also an expert in astrochemistry and astrophysical ices, which will aid us in interpreting the results from the perspective of the exocometary gas release; she also led significant efforts to link exoplanet elemental abundances to their formation, which we will complement here by measuring elemental abundances of exocomets.
Dr. Aki Roberge and Dr. Seth Redfield have extensive experience with HST UV spectroscopic observations, including in the context of exocometary gas absorption. Together, they have led most past efforts to obtain gas abundances from UV spectroscopy of edge-on disks, as proposed for this project. Dr. Redfield is also an expert in the local interstellar medium, and his experience will be an asset for separating ISM absorption lines from circumstellar absorption lines in the spectra.
Dr. Hales is an expert in observations of gas in disks (protoplanetary and debris) across the spectrum, but in particular optical spectroscopy where he led a major recent survey to look for atomic absorption in edge-on debris disks, which led to the discovery of circumstellar gas absorption in one of our two targets, HD110058. He is also leading an approved ALMA program to further characterize the gas and dust environment of this target at mm wavelengths.Planets and Planet Formation6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARA0-A3 V-IVCIRCUMSTELLAR MATTERDISKNOSee Proposal Description from how stellar parameters were derived.
For ETC calculations for wavelength settings below ~1800 A, we use the GALEX FUV AB mags predicted by models (reported under 'Other Fluxes' above) and a Castelli and Kurucz ETC spectrum with a Teff of 8750 K.
The ETC calculations attached to this APT proposal assume the median of the predicted GALEX FUV AB mag distribution.
We also ran calculations with the brightest GALEX FUV AB magnitude in the predicted distribution (~10.5), which cleared the ETC with no issues.
For ETC calculations for wavelength settings above ~1800 A, we use the measured U-band magnitude reported here and a Castelli and Kurucz Teff of 8750 K.J2000J2000Johnson U = 8.22+-0.02 mag. Model fits to UBV, Gaia G, BP, RP, 2MASS J,H,K yield: Teff = 8750(-160,+170) K, A_V=0.09(-0.05,+0.05), predicted GALEX FUV: 11.9(-0.3,+ 0.3) AB magSTARA0-A3 V-IVCIRCUMSTELLAR MATTERDISKNOSee Proposal Description from how stellar parameters were derived.
For ETC calculations for wavelength settings below ~1800 A, we use the GALEX FUV AB mags predicted by models (reported under 'Other Fluxes' above) and a Castelli and Kurucz ETC spectrum with a Teff of 8250 K.
The ETC calculations attached to this APT proposal assume the median of the predicted GALEX FUV AB mag distribution.
We also ran calculations with the brightest GALEX FUV AB magnitude in the predicted distribution (~10.5), which cleared the ETC with no issues.
For ETC calculations for wavelength settings above ~1800 A, we use the measured U-band magnitude reported here and a Castelli and Kurucz Teff of 8250 K.J2000J2000Johnson U = 8.18+-0.02 mag. Model fits to UBV, Gaia G, BP, RP, 2MASS J,H,K yield: Teff = 8330(-200,+510) K, A_V=0.13(-0.07,+0.16), predicted GALEX FUV: 12.8(-0.9,+ 0.4) AB magCOS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1327STIS/FUV-MAMASpectroscopicNoNoE140H1562STIS/NUV-MAMASpectroscopicNoNoE230H1763STIS/FUV-MAMASpectroscopicNoNoE140H1562STIS/NUV-MAMASpectroscopicNoNoE230H1763STIS/NUV-MAMASpectroscopicNoNoE230H2463STIS/NUV-MAMASpectroscopicNoNoE230H2912STIS/NUV-MAMASpectroscopicNoNoE230H2463STIS/NUV-MAMASpectroscopicNoNoE230H2912Timing link suitability includes constraints ([19 After 01 by 3.0 to 14.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.COS FUV Observation of Target HD110058(Tic-Visit
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