NIRCam and MIRI Coronagraphy of the Beta Pictoris Debris Disk
This Example Science Program presents an application of the JWST High Contrast Imaging Roadmap, demonstrating how to create a cross-instrument MIRI/NIRCam observing program to observe the Beta Pictoris Debris Disk.
Main article: JWST High Contrast Imaging Roadmap
See also: Step-by-step guides
The JWST High Contrast Imaging Roadmap guides readers through the process of designing a high-contrast imaging (HCI) observing program with JWST. Here we demonstrate this process, walking the user through the decisions made at each step, for an example science program that uses the NIRCam and MIRI coronagraphs to observe the Beta Pictoris debris disk.
The debris disk around Beta Pictoris (Beta Pic) is famous for being the first circumstellar disk to be spatially resolved. Since its discovery in 1984, generations of observations have delivered insights into its complex structure, composition of its constituent particles and physical processes that shape the disk. As one of the brightest and largest disks on the sky, it remains a compelling target for detailed investigations at unprecedented sensitivities with JWST.
The science case we describe here is based on the "Coronagraphy of the Debris Disk Archetype Beta Pictoris" GTO Program. Their goal is characterize the archetypical debris disk around Beta Pic with deep imaging in multiple filters across JWST’s entire wavelength range. Specific objectives include:
- Measure the disk structure, composition and interactions with planets.
- Test for the presence of water and CO2 ices and organic tholins (such as those on Titan).
- Measure color variations and asymmetries across the disk.
- Probe the thermal emission from both the warm inner belt and outer cooler main disk.
- Obtain a comprehensive legacy dataset on this target, for analysis alongside similar data and/or on other debris disks studied using JWST.
Main article: JWST High Contrast Imaging Roadmap
Below we follow the workflow outlined in the JWST High Contrast Imaging Roadmap to design an observing program for this example science case.
Becoming familiar with the HCI capabilities of JWST
JWST and its suite of instruments, modes and high contrast capabilities will open a dramatic new era in the study of debris disks. JWST offers an unprecedented raw sensitivity, orders of magnitude beyond what can be achieved from the ground, and a wavelength coverage that adds significantly to that covered by the Hubble Space Telescope (HST). JWST will provide resolved scattered light and thermal emission imaging of hundreds of debris disk systems.
Debris disks are circumstellar disks composed of dust created by the collisions of plants and/or minor bodies such as asteroids. They are very faint compared to their central star and so the ability to reject starlight at extreme levels is essential. The high performance coronagraphs on JWST will enable us to resolve many of these disks. There are 5 coronagraphs of different types in NIRCam and 4 in MIRI, collectively usable with various filters spanning 1.8 – 23 μm. This filter complement spans a wealth of spectral features that can be used to characterize the compositions of dust and ice particles present in debris disks.
Selecting a HCI observing mode
Achieving the science goals of this program requires multi-wavelength imaging of the Beta Pic debris disk with high-spatial resolution. Resolved images at multiple wavelengths are powerful when it comes to characterizing debris disks: images provide independent measurement of the spatial distribution of the dust, while the variation of its brightness with wavelength allows the size distribution and composition of the dust to be constrained (e.g. Debes et al 2008; Rodigas et al 2015). For this observing program, we will employ the NIRCam and MIRI coronagraphs, which cover nearly the full wavelength range of JWST.
NIRCam Coronagraphic Imaging will provide images of Beta Pic at HST-like resolution at near-IR wavelengths, with great sensitivity. We will use NIRCam’s F182M, F210M, F250M, F300M, F335M and F444W filters, which are sensitive to the presence of water and CO ices and organic tholins, to study the composition and spatial variation of the disk. We want to use the round coronagraphic masks (MASK210R and MASK445R) to obtain full azimuthal coverage of the disk, allowing us to study the vertical structure. With the F444W filter, we will also be able to search for unknown wide-separation (>10AU) planetary companions, reaching well below the mass of Saturn. We note, the known planet (Beta Pic b) will be at a small projected angular separation from the star at this time, after its near transit in front of the star in 2017—observing Beta Pic B is not a goal of this program.
With MIRI, Coronagraphic imaging at 15.5 and 23 μm will allow us to image faint disk structures close to the star that have been unresolvable until now. We will use the F1550C and F2300C coronagraphic filters to probe the warm inner asteroid belt and cooler outer main disk, respectively. For MIRI, the coronagraphic imaging filters are associated directly with each coronagraph and are not interchangeable—selecting the filter selects the coronagraph.
Selecting a PSF calibration strategy and suitable PSF calibrator
In order to draw out the best contrast and achieve the smallest inner working angles of each coronagraph, we will observe a nearby and color- and flux-matched PSF reference source, using contemporaneous and identically executed observation sequences. We will employ the standard coronagraphic sequence for every instrument, mask and filter combination: an initial observation orientated at a desired nominal aperture position angle (i.e. one that maximizes the spatial coverage of the disk); followed by a second observation with an aperture position angle ~10 degrees relative to the first observation; followed by an observation of the PSF reference star. Furthermore, all observations will be linked in a non-interruptible sequence to ensure the PSF calibrator is observed close in time to the science target. Lastly, because of the brightness of Beta Pic, we do not foresee the need to employ the small grid dithering technique.
Beta Pic, is a spectral type A6 star with a K magnitude of 3.48 and celestial co-ordinates of 05 47 -51 03. Following the guidelines provided in Selecting Suitable PSF Reference Stars for JWST High-Contrast Imaging, we are looking for a PSF reference calibrator that is:
- Relatively nearby (to ensure scheduability and minimal slew time – which in turn minimizes thermal changes to the telescope and thus changes to the PSF)
- Closely matched in spectral type (less critical at MIRI wavelengths, because the FQPM filters are relatively narrow, but has a stronger impact for NIRCam as the wavelengths shorten and as the spectral bandwidth widens)
- Close in magnitude (allowing shorter exposure time on PSF star – especially helpful given our choice to use SGDs)
- Is non-binary (and so will appear optically single at JWST resolution)
Successfully used as a PSF calibrator for Beta Pic in many HST observations and a known single star, Alpha Pictoris appears a good candidate as our PSF reference target. It is located ~19° from the target star (at 06 48 11.4516; -61 56 28.8060) and has an overlapping visibility window. The difference in K mag between Alpha Pic (K=2.57) and Beta Pic (K=3.48) is ~0.9. Furthermore, Alpha Pic (A8V) is fairly close in spectral type to Beta Pic (A6V), which provides a more than adequate color match (given previous estimates of the impact of color mismatch on NIRCam coronagraphy contrast) to minimize chromatic differences between the reference PSF and target PSF. For the MIRI observations, color match is even less important.
Assessing target visibilities and allowed position angles
In order to assess the target visibilities and their available position angles (PAs) versus time relative to the MIRI and NIRCam coronagraphic masks—in particular, relative to instrumental structures such as occulting bars in NIRCam or boundaries in the MIRI 4-quadrant phase mask (4QPM)—we will use the Coronagraphic Visibility Tool (CVT).
We first resolve Beta Pic using SIMBAD (see the CVT step-by-step guide). The disk's midplane is at a PA of 32° and has a separation and outer radius of around 0.4" and 13.4", respectively. Thus, we specify companions at a PA of 32° and separations of 0.4" and 13.3", to get an indication of the extent of the disk on the selected instrument and mask. We also define a another companion at a separation of 13.4" diametrically opposed to the first, to act as a proxy for the disk structure's position angle versus time.
For the NIRCam observations, because the disk is edge-on, we will chose an orientation that places the disk mid-plane near the diagonal of the NIRCam coronagraph subarray to maximize spatial coverage, but avoid the ND spots. We find that the ideal orientation would be at an aperture position angle (APA) of ~350°, and other orientations would sacrifice some of the science. Consequently, we determine that an APA range of 345°–360° will be suitable for our NIRCam observations.
For MIRI, we will orient the disk at an angle of ~45° from the 4QPM axes, which corresponds to an APA of ~345°. Note that this orientation also avoids the two supporting struts in the mounting bracket of the Lyot coronagraph, which themselves block light in the FOV. We will define a corresponding APA range of 340°–355°.
We note that while we plan to define these specific PA range requirements, they are not completely rigid. In the event of a TA issue or other scheduling problem, we could consider alternative orientations. For the MIRI observations in particular, we only require the disk mid-plane is oriented near ~45 deg from the 4QPM axes-- there are several orientations acceptable, but we can only program one into APT. For NIRCam, the orientation we request is ideal however alternative orientations could be considered if absolutely necessary.
Using the Exposure Time Calculator
Once target visibility is confirmed and a PSF calibration strategy adopted, we use the JWST Exposure Time Calculator (ETC) to determine the optimal exposure specifications for our program. Step-by-step ETC calculation instructions can be found in the ETC Step-by-Step Instructions for Beta Pictoris article.
Deciding on an observing strategy
Now that we have made a series of technical decisions for our program (such as our PSF calibration strategy, exposure specifications, etc.), we now need to identify an observing strategy that incorporates each of these components, whilst also minimizing observing overheads and performance degradation.
We find there are two strategies in which to schedule our set of observations. In the first approach, the observations made in each instrument are scheduled together in a non-interruptible sequence, at the orient in which the spatial coverage of the disk is maximized. Alternatively, by making a slight sacrifice in orientation and requiring that the NIRCam and MIRI observations be scheduled together in one long non-interruptible sequence (with the PSF reference observations placed between them) it is possible to save on overheads. However, this second approach puts very tight restrictions on the schedulability of the observations, resulting in a single two-day scheduling window. This is potentially problematic: if any observation failures were to occur that were not caused by the program itself (e.g., caused by an instrument or telescope operational problem, malfunction or safing event), there would not be another opportunity in which to repeat this sequence of observations within that observing cycle—the program would need to be deferred for at least another year. Thus, we will go with the first scheduling approach. This increases the schedulability of the observations from ~2 days per year to ~2 weeks and allows us slightly more ideal instrument orientations, at the expense of slightly longer overheads. We note that if there is a TA issue or something that prevents scheduling of the observations, there are other possible orientations that are available other than those provided.
The order in which the two sets of observations will be scheduled is as follows:
Table 1. Beta Pictoris observation techniques with NIRCam and MIRI coronagraphs
Observing Beta Pictoris with the NIRCam coronagraphs
Observing Beta Pictoris with the MIRI Coronagraphs:
This order was chosen in order to minimize overheads while also minimizing time between reference PSF observations and science target observations.
Using the Astronomers Proposal Tool
Once we have completed all other steps in the proposal planning process, we can write, validate and submit our proposal in the JWST Astronomers Proposal Tool Overview (APT). A step-by-step guide for entering this example science program into the APT is provided in the APT Step-by-Step Instructions for Beta Pictoris article.
Debes, J. H., Weinberger, A. J., & Schneider, G. 2008, ApJL, 673, L191
Rodigas, T. J., Stark, C. C., Weinberger, A., et al. 2015, ApJ, 798, 96