initial submission. expect to resubmit with more HST past usage material.
resubmission with fewer typos....Assigned ID: 284
----- Attempting Submission 1 (Fri Feb 24 02:56:50 GMT 2012) -----
HST Phase I Proposal 284 (HST20_uvlongslit.pdf.apt) successfully submitted.
----- Attempting Submission 2 (Fri Feb 24 13:20:49 GMT 2012) -----initial submission.
added orientation constraint for visit 5 exposure 1, but BOT is now complaining about our
F6IIIe target being an O5V. Can't figure out how to clear that.----- Attempting Submission 1 (Mon Jul 09 14:00:04 GMT 2012) -----
HST Phase II Proposal 13032 (hst13032_wcos.apt) successfully submitted.
----- Attempting Submission 2 (Tue Sep 18 18:35:33 GMT 2012) -----We are using 2 out of 4 FP-POS settings for each of the 3 COS wavelength settings for our 2
targets being observed with COS. Our COS team expert, Dr. Alexander Brown indicates that this
strategy will give us the requisite S/N and fill gaps in the COS spectral coverage.
Our target coordinates are all good to at least 0.4".
The BOT is complaining about HD 142527 being an O5V star. Spectral type is F6IIIe. Don't know how I can clear thisCrossing the Snow Line: Mapping Ice Photodesorption products in the Disks of Herbig Ae-Fe starsWater is a key constitutent of protoplanetary disks. In our Solar System, small, icy grains are thought to have boosted the disk solid surface density, setting the stage for icy planetesimal formation and ultimately the growth of gas giant planets, while water vapor warms the disk, facilitating chemistry. Survival of water, in either phase, is sensitive to the UV radiation field. Intermediate-mass PMS stars, the Herbig Ae stars, straddle the temperature range where icy grains can survive within 10 AU of the star to systems where ice is photodesorbed at the disk surface to beyond 100 AU. Far-IR studies with Herschel have shown that, while water vapor is rarely detected for Herbig Ae stars, its dissociation products such as OH and O I are common. Such data lack the spatial resolution to directly constrain where water in any phase is located. An alternate approach exploits HST's superb angular resolution and disk-to-star contrast in the FUV using HST STIS long-slit spectroscopy. Such observations can map the spatial distribution of water's other dissociation product, H I at Lyman alpha, with 7 AU resolution. The same spectra also simultaneously trace molecular hydrogen and dust, enabling an additional test of whether the HI traces the dust or the molecular gas in these stratified disks. We propose obtaining STIS G140M spectra at Lyman alpha for 4 otherwise well-studied Herbig Ae-Fe stars to test the hypothesis that spatially extended H I in these systems provides a fossil record of where ice was located in the disk which can be compared with where giant planets are found in these disks.Targets: Our targets are Herbig Ae stars with Hershel PACS [O I] data, NIR and mid-IR imagery of the dust disk, known system inclinations, and known locations of the disk major and minor axes. Three stars (AB Aur: STIS O57Z04010; HD 169142: IUE SWP 55483/LWP 31285; SAO 206462: COS LB9901060, LB9901070, LB9901080) have archival FUV spectra, one (HD 142527) does not, but should resemble SAO 206462 at shorter wavelengths. The available spectral data, while useful for estimating count rates in our proposed observations have no spatial resolution and cannot be used to address our science goals. We propose obtaining STIS G140M long-slit data using the 52x0.2′′ slit used in prior observations of HD 100546.
Star Sp.T. Teff Ref. Disk Inclination Phot. Range at V
AB Aur A0Ve 9280 Roberge et al. 01 12-20 D 7.06-7.12
HD 169142 A5Ve 8400 Dunkin et al. 97 11+/-2 8.05-8.28
SAO 206462 F4Ve 6810+/-80 Dunkin et al. 97 13+/-2 8.7+/-0.1*
Mueller et al. 11
HD 142527 F6IIIe 6600K Verhoeff et al. 2011 21+/-2 8.34-8.51
* Hipparcos data for this star refer to HD 135344, 21" from SAO 206462 along PA=17D
-----------------------------------------------------------------------------------------------------
Exposure Durations:
Target 1 -- AB Aur: This A0Ve star is a rapid rotator, with Teff more typical of A2V stars. The
star is incorrectly identified as B9neqIV-V by Shenavrin et al. (2011), but is more commonly,
and historically, classified as A0Ve. The FUSE spectrum lacks the conspicuous C I absorption and FUV flux levels expected for a B9 star - instead the FUSE spectrum is a featureless continuum consistent with the accretion luminosity and emission lines. For source detection, the FUSE data restrict E(B-V)<0.1 with R=3.1. From the optical data, and adopting A0V, E(B-V)=0.12, which would normally obliterate Lyman alpha emission, yet STIS E140M data (Roberge et al. 2001) demonstrate that Lyα is detected. For the STIS feasibility analysis, we used IUE SWP 50106, a low dispersion, large aperture spectrum with reasonable S/N (for IUE) at the shortest wavelengths as input data for the STIS exposure time calculations (ETC). Over 1145-1250 ̊A, the accretion luminosity rather than the photosphere dominates. The STIS ETC (STIS.sp.360465) predicts that the the brightest pixel count rate is 0.116 c/s, with a global count rate from the source of 222 c/s and a background contribution of 234 c/s. Analysis of IUE archival data
indicates that the continuum shortward of 2000 A varies by a factor of 2 (Wassell PhD thesis
2009). These count rates are a factor of 42 below the limits for irregularly varying sources.
A 2 ks integration produces S/N∼33 for the continuum at 1230 ̊A. The slit should be placed along the disk major axis (PA=45 degrees or orient=90 degrees).
STIS Target Acquisition: AB Aur has been successfully acquired by STIS using the F28x50OII
filter previously. Our proposed integration will yield S/N~60, as well as a photometric point
at 3741 A for SED modeling purposes. STIS.ta.415626 gives S/N=40 in 0.04s, we are requesting
0.1s integration time.
Target 2 -- HD 169142: This star has an optical spectral type of A5Ve (Dunkin et al. 1997) not the B9Ve listed on SIMBAD, with a slightly later type, A8Ve, in the UV (IUE SWP 55483), reflecting gravity darkening due to rapid rotation. Adopting (B-V)_0=0.17 for A5V, E(B-V)=0.09, which would normally affect Lyα detection for R=3.1. However, inspection of the IUE SI browse file for SWP 55483 indicates the presence of a point source superposed on geocoronal Lyα emission. The source was detected as the only source in the ACS SBC F122M field of view with a peak count rate well below the BOP limit (observation ids=J9JD02010, ..20, ..30, ..40), even given the red leak of this filter.
STIS target acquisition will use the F28x50OIII filter and will reach S/N=60 in 0.4s ( for
V=8.05, optical maximum light, STIS.ta.415634), as well as providing a photometric point at 5007 A for SED modeling.
The accretion luminosity for this star is 10× higher than for SAO 206462, but the emission lines appear comparable in strength. We have used several approaches to estimating the observed
fluxes. 1) Use IUE data longward of 1700 A, but splice to SAO 206462 at shorter wavelengths,
or use various scaled versions of the SAO 206462. Adopting SAO 206462 as a template spectrum, but scaling to the higher (continuum) accretion luminosity, we expect a peak count rate of 0.92 c/s at Lyα, and a global count rate of 249.5 from the target, with 234.8 c/s from background sources, assuming average airglow. These count rates are more than an order of magnitude below the irregularly variable object bright object limits. In 4 ks, if the spectrum is at this level, we will achieve S/N=15 at 1230 ̊A. S/N estimates using a simple splice of the SAO 206462 COS data shortward of 1700 A onto the IUE data result in S/N estimates a factor of 3 lower, again with no BOP issues and with S/N adequate for our scientific purposes.
We plan 2 STIS orbits for this STIS G140M spectra of this star, but with a precursor COS orbit (see below) to check our estimates. The slit should be placed to cross the bright arc at PA=115±10 degrees, orient=160 degrees. At this PA, the 9.2′′ separation T Tauri companions to HD 169142 will not be in the slit.
COS Precursor Spectra for HD 169142:
A single orbit is allocated for the COS observations. We propose obtaining COS G130M spectra, with segments centered at 1291, 1309, and 1327 (two FP-POS settings) using 380 - 400 second individual exposures, to confirm the IUE detection of Lyα. It is impossible to acquire spectra at all four FP-POS psoitions for each setting --- such a scenario results in catastrophic overheads and minimal exposure time. Our proposed observing sequence results in three independent spectra contributing at all wavelengths and minimizes the influence of the detector gap. Using the same source assumptions as for STIS, each of the exposures will provide spectra with S/N ~40 at the peaks of the C II 1334/5 A doublet, O I 1302/4/6 triplet, and H Lyman alpha (ETC COS.sp.412308). The brightest pixel in COS G130M segment B is at OI and is expected to produce a count rate of 0.17 c/s. For segment A, the peak count rate is at C II, and is 0.13 c/s. All spectra are well under the local and global bright limits. The total on-source exposure time will be 1560 seconds. The COS target acquisition will use MIRRORB and the BOA --- a 90 second exposure is required to achieve a peak S/N of 60 with the brightest pixel count rate being 5.4 c/s (COS.ta.412253).
Target 3 -- SAO 206462 (HD 135344B): This object has spectral types of F4-F8Ve in the literature, which may be due to its critical rotation (Mueller et al. 2011). Foreground extinction, measured from the V=7.05, A0V star HD 135344, 21′′ to the north, is E(B-V)=0.07 and is expected to apply to SAO 206462. The COS spectrum has a faint continuum (∼2x10−15 erg cm−2 s−1 ̊A) and a rich emission-line spectrum with Lyα the brightest line (peak flux of 2.5x10−13 erg/cm−2/ s−1 ̊A). This spectrum, binned to 0.1 ̊A and with geocoronal Lyα removed was used for STIS exposure estimation (STIS.sp.378175). The peak count rate for this source is 0.092 c/s at 1217.45 ̊A and the total source count rate is 0.151 c/s (STIS.sp.360012), well below bright object limits. In 4ks the S/N per spectral resolution element at 1230 ̊A is ~5 , at N V 1238 ̊A it is22 and at SiIII1206 ̊A it is∼17. Neither the N V nor SiIII are expected to be spatially extended, so we will concentrate the reflection nebulosity studies at those wavelengths and bin the H2 emission to improve the S/N. We are requesting two orbits for the STIS observation. We will place the slit aligned along the disk major axis (PA=55 degrees, orient=100 degrees). HD 135344 (A0V, V=7.05) will be out of the slit with this orient.
STIS Target Acquisition: We will achieve S/N=60 using F28x50OIII at optical maximum light for
this system, as well as a photometric data point at 5007 A for SED modeling with 0.6s integration time (STIS.ta.415638).
Target 4 -- HD 142527: The spectral type on SIMBAD is F6IIIe, with AV =0.6, corresponding to E(B-V)=0.19 if R=3.1 (unlikely) to 0.12 (R=5, typical of molecular clouds and similar to AB Aur). There are no UV spectra for this star. We request precursor COS G130M spectra to confirm that Lyα is detectable, and that our flux estimate based on SAO 206462 is valid. We assume that the spectrum is similar to HR 6077 (F 6 III, IUE SWP 36874), but with a spectrum at short wavelengths like SAO 206462, but scaled up by 5 times. We conservatively assume no additional extinction for exposure estimates. For STIS, we expect a peak local count rate at 1217 ̊A of 0.45 c/s, and a global count rate of 0.755 c/s again, both well under the bright object limit. We propose an integration of 4 ks, yielding S/N=42 at Lyα, and S/N ≥28 at 1230 ̊Aat the star. Our preferred PA of 90 degrees is unschedulable. We therefore propose placing the STIS long-slit along PA=255-265/75-85 degrees, Orient=300-310 degrees where it will cross structure seen in NICMOS F110W coronagraphic imagery.
STIS Target Acquisition: We are requesting 0.4s integrations using F28x50OIII for STIS acquisition which will yield S/N=60 if HD 142527 is at optical maximum light, and still be above S/N=40 if the star is closer to V=8.51 (Hipparcos minimum light). As for our other targets observed at this wavelength, the signal in this band will also provide a photometric point for SED modeling. For details see STIS.ta.411085.
COS spectra for HD 142527:
We are also requesting that the STIS spectrum be preceded by a single orbit with COS G130M spectra with the same central wavelengths settings as for HD 169142. We expect that the source count rates will be half of those for HD 169142 unless the extinction and N(H I) are higher. Using the same source assumptions as for STIS and individual exposure times of 425 - 450 seconds, each of the exposures will provide spectra with S/N ~35 at the peaks of the C II 1334/5 A doublet and O I 1302/4/6 triplet, and ~30 for the peak of H Lyman alpha (ETC COS.sp.412311). The brightest pixel in COS G130M segment B is at Lyman alpha and is expected to produce a count rate of 0.10 c/s. For segment A, the peak count rate is at C II, and is 0.07 c/s. All spectra are again well under the local and global bright limits. The total on-source exposure time will be 1775 seconds. The target acquisition will use MIRRORA and the BOA --- a ~10 second exposure is required to achieve a peak S/N of 40 with the brightest pixel count rate being 31 c/s (COS.ta.412261).N/ACalibration Needs: We require no special calibrations, if the cycle 20 calibration plan includes observation of at least one UV standard star at or near Lyα with STIS G140M.We require coordinated photometry and spectrophotometry for our STIS FUV observations, and prefer that our STIS observations be scheduled during plan windows where ground-based photometry is feasible. Coordination with the COS windows is not critical: getting the COS data at least 60 days prior to the STIS windows is critical.ISM AND CIRCUMSTELLAR MATTER12false0.00.0falsefalsefalsefalseSUPPORTEDSTARA0-A3 V-IVSpectral type for AB Aur is A0V (Simbad has recently updated to B9 which is inconsistent with IUE, HST STIS, and FUSE data). A0V covers a large range in T_eff (Gerbaldi et al. 1999), and
AB Aur is cool for the spectral type, and in the UV resembles objects with spectral types of A2V. The STIS E140M data in the wavelength range near Lyman alpha are shown in Roberge et al. (2001).
Radial velocity 8+/-5 km/s
Proper motion data are from van Leeuwen (2007), errors are 1+/-1.08, 0.6 mas/yr and
in general agreement with UCAC3 (Zacharias et al. 2010). Target has previously been successfully observed in optical and FUV by STIS.
Photometric range seen by Hipparcos is V =7.06-7.12
Target data taken from Simbad. UV Flux measures from STIS (Ly alpha0 and GHRS (N V).HD-31293HIP-22910J2000J2000B=7.18+/-0.03. Star is typically near V=7.06-7.08 but can irregularly drop to 7.12 FSTARA4-A9 V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.
Spectral type is A5Ve, as discussed in Dunkin et al. (1997) MNRAS 286, 604 NOT the B9V listed
on SIMBAD.
Proper motion data come from Hog et al. (2000) and are listed on SIMBAD. They give
a mean epoch of 1991.25 for proper motion. PM data are in full agrement with UCAC3
(Zacharias et al. 2010).
Hipparcos search facility gives a range in V of 8.05 to 8.28 (0.13 mag about the Johnson
magnitude of 8.15).
There are no tabulated parallax data on Simbad. Assumption in literature is d=145 pc.SAO-186777J2000J2000B=8.41.STARF3-F9This object was generated by the targetselector and retrieved from the SIMBAD database.
Proper motion data are from Hog et al. (2000) with a mean epoch of 1991.25
No parallax is given for this object by SIMBAD, but distance in literature is 145 pc.
Target has previously been successfully observed by HST STIS, NICMOS and ACS SBC.
Star has HD 135344 (A0V, V=7.76) 21" to the NNE; Hipparcos links to this star rather
than to SAO 206462.
The Hipparcos Search Facility gives a photometric range for this object of 8.45-HD-135344BJ2000J2000B=9.206+/-0.022, R=8.7STARA4-A9 III-IThis object was generated by the targetselector and retrieved from the SIMBAD database.
Distance estimate from parallax is 233 pc.
Proper motion data are from van Leeuwen (2007), and are +/-0.93, and 0.79 mas/year . Epoch is assumed to be 1991.25. general agrement with proper motion data from UCAC3 (Zacharias et al. 2010).
Hipparcos search facility has a photometric annex for this star and found gradual excursions between 8.41 and 8.51. Star is not listed in ASAS (not variable enough?).
Radial velocity -3.5 +/-0.8 km/s
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