Field of View: 25.5 (8.3x3) arcmin2
Wavelength range: 0.31 – 1.0 µm (full spectral range @R=1500 in a single exposure)
Spatial Resolution: Seeing limited
Spatial Sampling: 0.05 arcsec per pixel
Imaging mode - <0.45 arcsec FWHM (including contributions from the ADC at z = 60°
Spectroscopic modes - 0.25 arcsec >80% encircled energy at every wavelength
Total Slit Length: >500 arcseconds (8” slits and 0.5” gap provides for maximum 58 targets)
Spectral Resolution: R = 1500-3500 @0.75" slits
Throughput: >25% from 0.31 – 1.0µm, >30% from 0.35 - 0.9 µm, not including the telescope
Sensitivity: texp=5x900s, S/N=150 per element, R=3500 V=20.5
Status (October 2018): Architecture downselect complete. Conducting conceptual Design Phase including refreshment of Science Requirements
Chuck Steidel (Caltech)
Eric Peng (KIAA-PKU)
TMT Science Instrumentation Group Lead
WFOS will provide near-ultraviolet and optical (0.31 – 1.0 μm) imaging and spectroscopy over a 8.3x3 arcminute field-of-view. Using precision cut focal plane masks, WFOS will enable short-slit observations of ~50 to 80 objects simultaneously (depending on the chosen slit length and gap, limited by the total slit length which is required to be >500 arcsec). WFOS will be able to be used in natural seeing. The full wavelength range can be captured in a single exposure at R=1500 with a 0.75 arcsec slit. Between 1 and 4 separate observations using articulating cameras will be needed to cover the full wavelength range, depending on the desired resolution.
WFOS has a gravity invariant vertical rotation axis to minimize instrument flexure and will incorporate a robust structure to support the various components of the instrument. In addition, it will incorporate an enclosure to protect its components and provide a light tight environment for the optical elements. Possible upgrades and additional functionality include an integral field unit, image slicing spectroscopy and options for gratings if funding allows.
Multi-slitmasks are designed by the user(s), fabricated by the observatory, and then loaded into the instrument prior to observing. Users generate the list of fields and science, wavefront sensing and guiding objects to be observed, objects, calibration sources, filters, resolution modes, and exposure times according to observing plans for specific to atmospheric conditions and other variables. Observer/operator Graphical User Interfaces are developed according to TMT standards for all instruments and subsystems. Data reduction pipeline modules for quick look and quality control includes a full instrument simulator for support instrument design and development of the data processing, archiving and distribution system. Full system configuration, guide star and science target acquisition occurs in less than 5 minutes.
The science cases that motivate the need for WFOS and dictate its design range from solar system programs to the most distant objects in the universe. Some of the most challenging science areas include;
Tomography of the high-redshift intergalactic medium: A flagship science case for WFOS is the characterization of circumgalactic and intergalactic material. The spatial density of faint galaxies is much higher than that of quasars and faint galaxies can be used as background sources for high line-of-sight density Lyman alpha forest mapping of the comsic web and for probing the chemistry, temperature, density and kinematics of circumgalactic material.
Rest-frame UV properties of high-redshift galaxies: The internal processes affecting galaxy evolution, such as star formation and AGN activity and the interplay with the local environment are complex topics that require a highly sensitive instrument to advance observational studies into unexplored periods of cosmic history when the universe was very different to what it is today.
Gamma-ray bursts, supernovae, tidal flares and other transients: Rapid spectrophotometric followup of transient sources, especially those of low brightness, e.g. high redshift supernovae, will revolutionise many areas of astrophysics from Cosmology to Fundamental Physics.
Dark Energy: Deep multi-object spectroscopy of faint galaxies will secure accurate redshifts and spectral energy distributions, allowing accurate calibration of photometric redshifts obtained with 8-m class telescopes such as LSST, determination of how galaxy SEDs depend on environment. Weak lensing cosmology will be improved by spectroscopic studies of galaxies to determine their kinematic orientations. For more details, see https://arxiv.org/abs/1903.09325
California Institute of Technology:
Chuck Steidel - (Principal Investigator)
Reston Nash - (Lead Mechanical Engineer)
Jason Fucik - (Lead Optical Engineer)
Stephen Kaye - (Electrical/Detector Engineer)
Roger Smith - (Electrical/Detector Engineer)
Indian Institute of Astrophysics:
Govinda KV - (Senior Mechanical Engineer)
Viswanatha N - (Senior Mechanical Engineer)
Sudarsan K - (Mechanical Engineer)
Hari Mohan Varshney - (Mechanical Engineer)
Devika Divakar - (Optical design analysis & ZEMAX simulations)
Amirul Hasan (Optical Designer)
Ramya Sethuram - (TMT India WFOS Project Scientist)
Sivarani Thirupathi (Astronomer)
National Astronomical Observatory of Japan:
Yutaka Komiyama - (Mechanical Engineer)
Fumihiro Uraguchi - (Mechanical Engineer)
Satoshi Miyazaki - (Astronomer/Optical Engineer)
European Southern Observatory:
Bernard Delabre - (Optical Engineer)
Hangxin Ji - (Optical Engineer - NIAOT)
Eric Peng - (WFOS Project Scientist - KIAA-PKU)
Thirty Meter Telescope Organization:
Davide Lasi - (Project Manager)
John Miles - (Lead Systems Engineer)
Eric Chisholm - (Instrument Technical Manager)