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STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
Visit 33 has been updated to include a new PSF reference star (PSF_DEL_CYG). The target and exposure times have been changed.
1165586362
----- Attempting Submission 3 (Mon Mar 07 13:23:58 GMT 2022) -----
----- Attempting Submission 4 (Tue Jul 19 18:19:33 GMT 2022) -----
All errors/warnings are for exposure times that were rounded to the nearest 0.1 seconds after applying CR-SPLITS
A deep and complete characterization of the Vega debris and planetary system in scattered light
The discovery that exoplanetary systems are common has posed the overarching question of how closely they resemble the Solar System. Although we have learned of many cases with dramatic differences, this perspective may be more a product of selection effects than of the general population. Systems where we can achieve au (or even sub-au) resolution hold the keys to understanding exoplanetary system structure at the necessary scale. At 7.7 parsecs, Vega enables one of the highest spatial resolution imaging opportunities of all exoplanetary systems. For example, its Kuiper-belt analog ring located at ~ 120 au is at an angular separation of 16.9'', while its Asteroid-belt analog is at ~ 12 au (corresponding to 1.6''). Giant and ice-giant planets will also likely be outward of 30 au (~ 4'') from the central star. At these angular distances, the STIS coronagraph has excellent imaging contrast. Furthermore, the luminous host star provides ample flux at optical wavelengths for the dust and planetary bodies in the system to scatter. Despite these attributes, the Vega disk has never been imaged with HST, and attempts to image its planets in scattered light integrated only deep enough to detect planets with radii above 3.6 R_Jupiter (at which sizes gas giants are not expected to exist). We propose a single heritage HST program that will provide a deep and complete characterization of the Vega debris and planetary system. Our program is designed to image the disk components and any Jupiter analogs outward of 30 au, assuming conservative albedo values. Our HST observations will complement JWST GTO Cycle 1 observations of the system with NIRCam and MIRI and existing ALMA observations.
We will obtain ultra-deep STIS PSF-template subtracted coronagraphic images of the Vega system. Ironically, the very properties that make the Vega disk uniquely important also make it uniquely challenging to observe: the disk is large, face-on (so scattering will be inefficient, and (from the ALMA image; Matra et al. 2020) likely to be very extended and of low surface brightness. Our ultra-deep observations will use the widest wedge position available, the WB2.8 location of the 50CORON coronagraphic mask of the 50CCD detector, with minimal but intentional saturation of the inner core. Luckily, the extensive STIS observations of the Fomalhaut system allow characterizing the various noise properties of the detector and its coronagraphic performance on a similar star. STIS GO programs 11818, 12576, 13037, and 13726 observed Fomalhaut for a total integration time of 27402 seconds. We reduced and combined all of the images taken within these programs, which were carried out identically at WedgeB2.5. This combined dataset pushes the STIS coronagraphic system close to its theoretical contrast limits (a 5-sigma contrast of 2e-11 near the debris ring). The combined data have yielded a spectacular image of the Fomalhaut ring, nearly artifact-free at the radii of interest for our Vega imaging (i.e., beyond half way to the ansae of the Fomalhaut ring: https://hubblesite.org/image/4625). From this analysis, plus the necessity of multiple roll angles, we have determined that we need to observe Vega and its PSF calibrator, alpha Cyg (or alpha Lac), using a total of 32 single orbit visits, separated into seven orbit sets (3x4 orbits and then 4x5 orbits), allowing for FULL roll coverage and providing optimal input to our PCA analysis. Within each set, the third orbit is used to observe the PSF star, and the rest for Vega. The orbits within each set must be executed in sequential, contiguous orbits (i.e., back to back with no interruptions except Earth occultation), to ensure PSF stability. The multi-roll technique has been proven in multiple HST programs (e.g. GO12228) to be superior to all other tried methods (Schneideret al. 2014), as the high number of roll dithers reduce systematic errors and image artifacts apart from also providing a full 360 degree imaging coverage of the target region. The target visits in each set are at relative orientations from nominal roll, with 10 degree steps (e.g.: -20 degrees,-10 degrees,0 degrees,10 degrees). The PSF template star is relatively close in the sky (23 degree) to Vega, minimizing variations in the PSF due to thermal instability of the OTA. As a result, we anticipate that with scheduling of the science orbits in each set at nominal roll, the PSF calibration star will also be at or close to its nominal roll and usually these two orbits will naturally without constraints have nearly the same celestial orientation angle. Subsequent visit sets should be are identical to the first, but at different relative nominal orientation for each set. Nominally, each set should be scheduled at an increasing orientation angle relative orientation from the first set. We require no special orientations. The individual visits will consist of the following sequence:
1. On-board autonomous target acquisition using the F25ND5 filter (S/N of 100).
2. Placing the target to its desired coronagraphic locations
3. Taking science exposures at the desired locations.
Note to our PC: initially we had planned for four sets of visits of 8 orbits each, but we understand that this would be challenging to schedule so we have increased this to seven sets of visits. Untimately, we want to maximize the integration time on our science target, Vega, but also require a continguous PSF reference. We belive our plan of seven sets including three sets of four orbit visits (3 science, 1 PSF) and four sets of five orbits (4 science, 1 PSF) is the best compromise. We would like to conduct the four orbit sets first, to inform any changes in observing strategy.
Exposure Times:
The STIS ETC does not inform on exposure times in coronagraphic mode, therefore we estimate exposure times based on various previous STIS programs (e.g. GO 13726). Our WEDGEB2.8 exposures will intentionally saturate. We base our program on the GO 13726 program observations, where Vega was used as a PSF source. For observations taken at a slightly smaller WEDGEB2.5 location, 10 second exposures did saturate, but resulted in a useful inner working angle of 4 arcseconds, which is adequate for our science goals of spatially resolving the disk morphology for Vega's Kuiper Belt analog.
Note to our PC: For each visit with a relative orient range we PREFER whenever possible to have the visit scheduled at the mid-range (but allow +/-5 deg relative offset tolerance if not possible). Sequential visits should not be scheduled to overlap in orientation angles at their extrema.
Dr. Andras Gaspar has experience with coronagraphic imaging with HST and is a member of the JWST GTO
program that will observer Vega. He is also an expert in modeling the collisional processing and orbital
dynamics of debris disks.
Dr. Schuyler Wolff is an expert in scattered light image modeling and precision high contrast image reduction.
Dr. Glenn Schneider is an expert in circumstellar disk imaging with HST. He pioneered the 6R/PSFTSC
technique for HST coronagraphic observations (Schneider et al. 2014, 2016, 2018).
Dr. Kate Su has much experience analyzing IR (Spitzer and Herschel) images of debris disks and has conducted
multiple studies of the structure of the Vega disk in particular (Su et al. 2005, 2013).
Dr. George Rieke is an expert in the field of debris disk studies. He was PI of the Spitzer/MIPS instrument and
is the US Science Team lead for JWST/MIRI.
Dr. Marie Ygouf and Dr. Charles Beichman are members of the JWST GTO program that will observer Vega.
Dr. Nicholas Ballering has much experience modeling debris disk SEDs and images (including from HST) with
an emphasis on grain properties (e.g., Ballering et al. 2016).
Dr. Jarron Leisenring is an expert on JWST image modeling and data reduction.
Dr. Wilner and Dr. Matra are the ALMA Vega disk experts on our team.
Exoplanets and Exoplanet Formation
Exoplanets and Exoplanet Formation
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A0-A3 V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
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A0-A3 III-I
This object was generated by the targetselector and retrieved from the SIMBAD database.
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STAR
A0-A3 V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
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A0-A3 V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
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