One of TMT’s three “Early Light” instruments, the Wide-Field Optical Spectrometer (WFOS), recently underwent an interim Conceptual Design Review via Zoom. The review’s purpose was to assess the instrument’s progress to date and to provide guidance on potential work needed to successfully complete the technical and scientific aspects to bring the overall design to a full Conceptual Design level. The review identified additional science cases, recommended additional functional requirements and provided an initial assessment of the new opto-mechanical concept.
The scope for the WFOS interim review included assessing the following:
Breadth of the proposed science cases
Flexibility, efficiency and risks within the operational concepts
Consideration given to trade-studies, manufacturability, performance and risks of the optical design
Consideration given to trade-studies, functionality, complexity, performance and risks of the mechanical design.
WFOS is envisioned as a workhorse instrument and is designed to provide highly flexible scientific capabilities while striving to maintain an overall low risk design. In 2018, WFOS underwent an extensive trade study between two fundamentally different architectures. These two concepts included exploring a bank of small, fiber fed, spectrographs and the current large ‘monolithic optic’ design. Since this down-select the WFOS team have diligently worked to produce an interim design concept that addresses and retires earlier identified risks for the chosen monolithic concept. The key design adaptations are summarized as follows:
Exploiting advances in manufacturing techniques for large optics has enabled the WFOS field of view to be centered on the telescope optical axis; as opposed to previous designs where the field was offset by 4.8 arcminutes. This enables the instrument to be physically smaller.
Flowing from the first bullet, the more compact on-axis design allowed the team to repackage the instrument so the incoming beam is now deflected downward within the instrument and hence is parallel to gravity. This allows WFOS to rotate around its vertical axis during operation, producing a gravity invariant design that greatly reduces concerns about instrument flexure and likely removes the need for a complicated flexure control system.
To maintain a simple and cost-effective design capable of achieving several spectral resolution modes as well as an imaging mode, the WFOS cameras articulate. The cameras’ articulation is also gravity invariant.
As described by one of the WFOS review panel members, the “WFOS technical team deserves a huge heartfelt congratulations for improving the design of WFOS on pretty much every axis. The descopes made from the WFOS-2013 design are smart, the instrument looks way more buildable, and the predicted performance is outstanding and realistic. I also want to commend the team for using a high-tech solution (the freeform collimator) to cleverly rebalance the risk! WFOS will be an instrument that will cause, what the young people call, FOMO (fear of missing out).”
More about the current design
WFOS will support three main modes of operation: direct imaging, long single slit spectroscopy, and multi-slit spectroscopy. The workhorse spectrograph will support several spectral resolutions including R = 1,500 and R = 3,500; with the R = 1,500 mode capturing the entire instrument bandpass in a single exposure. The current design also satisfies a goal of providing a spectral resolution mode of 5,000. The described modes use 0.75” slit widths; however, the instrument optics are designed to preserve image quality for narrower slits down to 0.25”, enabling higher spectral resolutions (up to 15,000) at the expense of throughput.
Science programs using narrow slits will benefit most from the implementation of ground layer adaptive optics correction as part of a potential future upgrade to the Observatory. WFOS is also capable of directly imaging its entire science field of view providing the Observatory with a wide-field imaging mode at early light.
WFOS will be the only TMT instrument capable of obtaining spectra at optical wavelengths (WFOS’s bandpass is 0.31−1.0 μm) for at least the first several years of TMT operations. For this reason, an important consideration for the design has been versatility, to ensure WFOS will be capable of addressing a very wide range of science.
WFOS core science themes include the study of:
Tomography of the high-redshift galaxies. How are proto-galaxies shaped by their gaseous environment and how do they affect that environment?
The origin and properties of stellar populations in nearby galaxies.
The key mechanisms that initiate the final stages of galaxy evolution.
The nature of transient sources.
WFOS will achieve the most sensitive optical spectroscopy ever attempted. It is expected that WFOS will often be used as the highest sensitivity spectroscopic capability, for the purpose of either initial identification or high-quality follow-up of new discoveries.
WFOS will promote advances in many different topics and will serve teams of researchers spanning a broad range of scientific interests. Its most exciting discoveries are likely impossible to predict, but among its many areas of investigations, WFOS will study the distribution and nature of dark matter in the universe, as well as the composition of high-redshift galaxies, the physics of supernovae and gamma-ray burst events.
The WFOS collaborating institutions are:
The California Institute of Technology (CIT);
The Indian Institute of Astrophysics (IIA) on behalf of the India TMT Co-ordination Center (ITCC);
The Nanjing Institute of Astronomical Optics and Technology (NIAOT) on behalf of the National Astronomical Observatory of China (NAOC);
The National Astronomical Observatory of Japan (NAOJ) on behalf of the National institute of Natural Science (NINS) and
The University of California Observatories (UCO).
