Science Keywords: Exo-Comets is not a valid selection.initial submission. One co-I's affiliation and email need to be updated.
resubmit with updated address for co-I, and typos fixed. Suggested fix
for omission of Exo-comets DOES NOT WORK
resubmit typo fix in .pdf file. Ready to add exo-comet to keyword list. Added Exo-Comet BSB-1851231542Assigned ID: 57
----- Attempting Submission 1 (Sat Apr 01 19:44:56 GMT 2017) -----
HST Phase I Proposal 57 (phileo_cy25.apt) successfully submitted.
Receipt: # 57-1
----- Attempting Submission 2 (Mon Apr 03 12:49:54 GMT 2017) -----
HST Phase I Proposal 57 (phileo_cy25.apt) successfully submitted.
Receipt: # 57-2
----- Attempting Submission 3 (Tue Apr 04 13:59:53 GMT 2017) -----
HST Phase I Proposal 57 (phileo_cy25.apt) successfully submitted.
Receipt: # 57-3
----- Attempting Submission 4 (Tue Apr 04 19:46:17 GMT 2017) -----
----- Attempting Submission 5 (Sat Apr 08 12:05:41 GMT 2017) -----Added KeywordUnschedulable Visit
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
Unschedulable Visit
Unschedulable Visit
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
Unschedulable Visit
Unschedulable Visit
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
Unschedulable Visit
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.Fixed timing issues between visits.
Shortened exposures to fix visibilities given longer gs reaquisition times.
Appear to be missing an orbit: No cos visit to go with visit 56....
change back to tiny aperture, not that I expect it to work...
fiddled with exposure times to fit everything within the visibility windows.
Most of the error apply to the visits that have already executed and failed.-100324354----- Attempting Submission 1 (Mon Jul 17 17:39:24 GMT 2017) -----
HST Phase II Proposal 15168 (GO15168_phaseII_vers2.apt) successfully submitted.
Receipt: # 15168-1
----- Attempting Submission 2 (Mon Jul 17 18:59:52 GMT 2017) -----
HST Phase II Proposal 15168 (GO15168_phaseII_vers2.apt) successfully submitted.
Receipt: # 15168-2
----- Attempting Submission 3 (Tue Jul 18 13:56:18 GMT 2017) -----
HST Phase II Proposal 15168 (GO15168_phaseII_vers2.apt) successfully submitted.
Receipt: # 15168-3
----- Attempting Submission 4 (Tue Jul 18 13:58:21 GMT 2017) -----
HST Phase II Proposal 15168 (GO15168_phaseII_vers2.apt) successfully submitted.
Receipt: # 15168-4
----- Attempting Submission 5 (Tue Jul 18 15:04:54 GMT 2017) -----
HST Phase II Proposal 15168 (GO15168_phaseII_vers2.apt) successfully submitted.
Receipt: # 15168-5
----- Attempting Submission 6 (Wed Jul 19 12:49:59 GMT 2017) -----
----- Attempting Submission 7 (Thu Aug 10 13:40:01 GMT 2017) -----
----- Attempting Submission 8 (Mon Aug 14 12:55:15 GMT 2017) -----
----- Attempting Submission 9 (Fri Feb 16 12:28:57 GMT 2018) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 10 (Wed Nov 28 18:51:35 GMT 2018) -----
----- Attempting Submission 11 (Sat Dec 08 17:31:38 GMT 2018) -----
HST Phase II Proposal 15168 (15168_4.apt) successfully submitted.
Receipt: # 15168-11
----- Attempting Submission 12 (Tue Dec 18 17:13:37 GMT 2018) -----There are only 2 warnings, just replicated since visits 3 and 5 are identical.
Warnings triggered by STScI changes in COS operation.
I am NOT using 4 FP positions, since these obtain spectra covering Lyman alpha,
which is being handled by STIS.
Unschedulable visits will be examined by PC.The Nature of the Star-Grazing Bodies in a System at the Age of the Late Heavy BombardmentStudies of bodies exhibiting redshifted gaseous absorption features associated with star-grazing planetesimals offer unique data on the composition of the bodies, as well as the presence of planetesimal belt analogs and giant planets in systems throughout the stellar lifecycle. Studies of young systems, such as the A stars in the beta Pictoris moving group, suggest that the star grazing bodies contain abundant carbon and water dissociation products, indicating a cometary origin. A recent analysis of another system, phi Leo (A7 IV, age=400-900 Myr) shows similar infall features in Ca II and Ti II, with what may be a 15-year cycle. This system is similar in age to the Late Heavy Bombardment in our system, a time when terrestrial planets in our system are thought to have been veneered in organics and water. The available data indicate frequent infall events interpreted as transiting exo-comets, but sample only lithophile to super-refractory elements. Archival IUE data lack the FUV S/N to establish high carbon abundance or the presence of water dissociation products. We therefore seek COS and STIS spectra to sample the volatile gas dat, and constrain the origin of the star-grazing bodies. The FUV data will be augmented with NUV data sampling siderophiles and lithophiles.The Target: Phi Leo has archival IUE high dispersion spectra consistent with an A7 V star with Teff=7500 K. Interstellar absorption (not seen in Ca II) is predicted to be at +1.75 km/s assuming that the star is at the centroid velocity for the Leo cloud (Redfield & Linsky 2008). At A7, (B-V)_0=0.191, so E(B-V)=0.007, and N(H) = 2.52E19. Given the uncertainty in spectral type, we scale integration times from our GO-13798 observations of HD 172555 by delta V and assuming no extinction.
STIS TA: We will use F25ND5 for ACQ, and G430M, center 5471 for ACQ/PEAKUP.
STIS Spectral Observations: We propose obtaining a STIS G140M long-slit spectrum with central wavelength 1222 A, to provide simultaneous measurement of airglow emission and circumstellar Lyman alpha. Scaling from HD 172555, this will require 4 ks or 2 orbits and will yield S/N=2.5 for the photosphere with chromospheric emission expected to be a factor of 2 above that. We will augment this observation with a STIS E140M observation providing coverage of Si II (2), C IV, Fe II 1608 A. The S/N will be ~5 at 1543 assuming an F0V type, and >20 assuming A5V (STIS.sp.905753, STIS.sp.905752). We will also obtain 3 E230H segments, centered at 2762, 2513, and 1763 A(STIS.sp.921476 for 2513 A) . Estimates were calculated using an A5V Kurucz model scaled to the peak continuum flux 3E-11 erg cm -2 s-1 / A seen in IUE LWP 27901 near 3000 A, and are expected to be conservative since the spectral type is A7V. The longer wavelength exposures have warnings due to irregular variable count rate compared to global limit, which does not apply for a continuum source such as phi Leo with variable absorption. The 1763 setting has no warning for count rates. There are short buffer time warnings for the E230H exposures. The E230H observations will fit in the same orbit as acquisition and peakup observations. The E140M data will require 1 orbit, while the G140M needs 2 orbits.
COS TA: We will use an ACQ/SEARCH, ACQ/PEAKXD and ACQ/PEAKD.
COS Observations: We propose obtaining a COS G130M spectrum with the gap between the A and B segments set at 1291 A, but plan to readout only the A segment, per operations at LP4. (COS.sp.92275). This will require at least 3.5 ks (2 orbits), but will provide coverage of O I, C I, C II and Si IV. The observation should be made during orbital night, ensuring minimal geocoronal contamination of O I and N I. If the star more closely resembles beta Pic, we anticipate S/N=26 (COS.sp.1007139), while if the star is closer to F0V, we expect S/N=6.2 in 2000 s, or 8.88 in 4000 s. Our COS observation will require 2 orbits each (COS.sp.92275) to yield photospheric S/N assuming A7V. We break the observations into 2 visits, STIS 4 orbtis, and COS
2 orbits with an after constraint to ensure that they are observed together. We request a second visit be scheduled 10 to 15 days after the first visit to permit us to assess variability in the transiting material.
Need for a spectral comparison object: We expect that, like Beta Pic and HD 172555, phi Leo will have chromospheric emission. For HD 172555, identification of emission in transitions of C II and O I required use of archival GHRS spectra as a photospheric model, and is particularly critical when the chromospheric emission distorts the blue wing of the line profile, but does not produce net emission in the observed spectrum. We currently lack suitable comparison object data at C IV, with alpha Cep as the comparison object, and O I. For coverage of the C IV region, we propose STIS G140M with a wavelength center of 1550 A. Assuming an F0V Kurucz model for alpha Cep, we will achieve 18<SNR<26 with no warnings in 900s (STIS.sp.905758). At O I, there is no moderate resolution GHRS data, and the archival GHRS G140L data are too coarsely sampled to provide a useful photospheric template. To cover O I, we propose obtaining a STIS G140M observation, centered at 1321
4 A, and covering 1294-1348 A. We obtain S/N=30.7 in 800s with no warnings and a peak count rate of 0.4c/s at 1345 A [STIS.sp.901509]. The alpha Cep observations will add 1 orbit to our total orbit request, bringing our total orbit request to 13 orbits. The comparison object spectra can be used to interpret data for HD 172555 and beta Pic, HD 169142, and HD 32297 in addition to phi Leo.
Total Time Request: We request a total of 13 orbits for this program.
Scheduling Constraints: The COS G130M phi Leo observations should be carried out within 2 months of opposition to eliminate airglow contamination of N I and O I transitions. phi Leo has one visibility window during this period, from 28 Mar-25 April 2018. alpha Cep has numerous visibility windows throughout cycle 25.
Planned Analysis: COS data: We will first verify that all observing segments have no airglow contamination in the x1d spectral files, or obvious spectral variability. Absent variability, we will merge data from the individual FP-SPLIT settings into 1 spectrum per visit, binning as necessary. Our analysis will include: identification of the photospheric continuum using the comparison star data, fitting chromospheric emission with Gaussian profiles, and then normalization of the observed profiles by the photosphere+chromosphere, following our treatment of HD 172555.
STIS G140M/E140M: STIS G140M data centered at 1222 A provides coverage of NI, Si III, and H I Lyman alpha, and using the 52x0.2" slit restricts airglow contamination to +/-40 km/s of the telluric value and offers sky data in the same observation. Our analysis will include a) search for emission in the pipeline processed but non-sky subtracted x2d spectrum, extract a sky spectrum and subtract the sky data from the source. Next we will follow studies of Lyman alpha profiles in nearby stars, model the line-of-sight N(H I) and corresponding extinction, search for asymmetric absorption wings (see Wilson et al. 2016), and place limits on the presence or absence of circumstellar H I absorption. An H I detection, in tandem with O I, would indicate that the star-grazing bodies in this system have water, and therefore resemble outer asteroid belt to cometary bodies. We will next search both the COS and STIS data for infalling N I features, if the S/N in the STIS data are sufficiently high. Their presence would indicate parent bodies with an origin in a putative Kuiper Belt analog, while the absence would be consistent with an origin in a warmer debris belt. The remainder of our analysis will follow studies of beta Pic and HD 172555. A byproduct of this analysis will be a more complete chromospheric to transition region line inventory for this system, and a study of the dependence of chromospheric emission on the stellar equatorial velocity.
Special Requirements: Wilson et al. (2016) demonstrated that observations made within 2 months of opposition result in no airglow contamination of COS G130M/PSA spectra at O I or N I, and minimize contamination of H I Lyman alpha. Opposition for phi Leo Is in early March, so observations from January through early May would meet this requirement. There is one month-long visibility window for phi Leo 28 March-25 April 2018. We will make use of the BETWEEN special requirement to ensure that observations are made near opposition. Apart from that we will require that the COS and STIS G140M observations of phi Leo take place on back to back orbits using the AFTER special requirement. COS data will be taken in Time-Tag mode and using FP-SPLIT=4, but only with the single central wavelength.
Coordinated Observations: We will seek coordinated observations of phi
Leo at Ca II, but these should not drive scheduling of the HST observations.
Justify Duplications: No duplications. phi Leo has no HST UV spectroscopy. alpha Cep has no moderate resolution data at O I or C IV.
BOT Concerns: Our science target, Phi Leo, is flagged as a health and safety concern under the assumption that its spectral type is 05V. IUE spectral data for the star clearly indicate that the spectral type is A7-8V with at most a small amount of extinction (<0.01 in E(B-V)). We expect a drop-off in flux similar to HD 172555 (5 orders of magnitude in flux shortward of 1800 A). The long wavelength portion of this drop off can be seen in SWP 15504. This star is the brightest object in the field of view, by a large margin. It is not flagged as photometrically variable, and should present as a continuum source with variable absorption features.Planets and Planet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARA4-A9 V-IVCIRCUMSTELLAR MATTERCORONADISKEXTRA-SOLAR PLANETARY SYSTEMNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
IUE data exist, for both the FUV and NUV, but large aperture data are available only in the NUV.HD-98058HIP-55084J2000J2000F(2655)=3E-11 erg/cm/cm/s/A (IUE LWP 27899)STARA4-A9 V-IVCORONANOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000F(2650.1)=2.1E-10, F(1298)=3.7E-13 erg/cm/cm/s/ACOS/FUVSpectroscopicNoNoG130M1291STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H2513STIS/NUV-MAMASpectroscopicNoNoE230H1763COS/FUVSpectroscopicNoNoG130M1291STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H2513STIS/NUV-MAMASpectroscopicNoNoE230H1763STIS/FUV-MAMASpectroscopicNoNoG140M1321STIS/FUV-MAMASpectroscopicNoNoG140M1550Timing link suitability includes constraints ([03 After 01 by at most 0.3 days] [04 After 01 by 14.0 to 20.0 days])The scheduling data was generated by CASM 26.2.CASM was run in Phase II mode.1523337312000115.0(Tic-Visit
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