Each module includes a short (0.6–2.3 µm) and long (2.4–5.0 µm) wavelength channel. NIRCam uses a dichroic to observe at both wavelengths simultaneously in roughly the same field of view.

NewportKinematic Mount

In a ~10 ks image, NIRCam reaches S/N ~ 10 on point sources as faint as ~8 nJy (AB mag 29.1) in some wide filters. See NIRCam Imaging Sensitivity.

Total system throughput for each NIRCam filter, including contributions from the JWST Optical Telescope Element (OTE), NIRCam optical train, dichroics, filters, and detector quantum efficiency (QE). Throughput refers to photon-to-electron conversion efficiency. Averages across all detectors are plotted. The vertical gray bar marks the approximate dichroic cutoff between the short and long wavelength channels. Filters marked "P" are located in the pupil wheel, requiring transmission through a second filter in the filter wheel, either F150W2, F322W2, or F444W. In these cases, the combined transmissions are plotted. (Figure version 6.0: May 16, 2024)

Kinematic MountThorlabs

Please note: this raises the bed height approx 8mm, you may need a longer pin for your Z end stop (e.g. 35mm pin vs 30mm).

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Kinematic mountrepeatability

Information about calibration is available in the JWST Science Data Overview article. This article and its links point to content about absolute astrometric, flux, and wavelength calibration, as well as information on calibration reference files.

Kinematic mountwiki

NIRCam was built by a team at the University of Arizona (UofA) and Lockheed Martin's Advanced Technology Center, led by Prof. Marcia Rieke at UoA.

Please use the Exposure Time Calculator (ETC) for the most up-to-date sensitivity estimates for specific proposed observations. See the NIRCam Sensitivity article for more information.

Beichman, C. et al. 2012, SPIE, 8442, 2Science opportunities with the near-IR camera (NIRCam) on the James Webb Space Telescope (JWST)

Kinematic mountcomponents

Within each module, light may (optionally) be passed through a coronagraphic occulting mask in the focal plane before being divided by the dichroic beam splitter to the short and long wavelength channels.

Installation went without a hitch. Bed seems very sturdily mounted. I also used the 3d-printed spacers as suggested by the build instructions.

† Not including reference pixels insensitive to light that are 4 pixels along each outer edge.‡ PSF undersampled at lower wavelengths; slightly broader for coronagraphy.

Each observing mode offers distinct capabilities and uses a subset of the optical elements available in the pupil and filter wheels.

Does what it says. Also allows the bed to be removed quickly and easily. FYI this does fit the build plate from the MPX kit. Holes are already pre-drilled so it's a quick and easy install.

The JWST Near Infrared Camera (NIRCam) observes from 0.6 to 5.0 μm and offers imaging, coronagraphy, wide field slitless spectroscopy, and time-series monitoring both in imaging and spectroscopy. NIRCam has 2 nearly identical modules pointing to adjacent fields of view. Each module uses a dichroic to observe simultaneously in a short wavelength channel (0.6–2.3 μm) and a long wavelength channel (2.4–5.0 μm).

KinematicBase

Kinematic mountdesign

Amazing fit and finish spot on design. Excellent Customer service . You can hear the bed as it changes during heat soak.Well worth the $$$.5 star customer service and fast shipping.

The NASA James Webb Space Telescope, developed in partnership with ESA and CSA, is operated by AURA’s Space Telescope Science Institute.

NIRCam consists of 2 redundant modules—A and B—with identical optical elements and nearly identical throughput. The imaging and wide field slitless spectroscopy observing modes include options to use either a single module or both simultaneously with identical integration times, readout patterns, and filters. Currently, the coronagraphy and grism time-series modes are restricted to module A and time-series imaging is restricted to module B.

In standard imaging mode NIRCam bright source saturation limits range between ~9 and ~16 Vega magnitudes, depending on the filter. Subarrays allow for shorter readout times to reach brighter magnitudes. Brighter magnitudes can also be reached in the time-series observing modes, as weak lenses (at short wavelengths) and grisms (at long wavelengths) spread the bright light over more detector pixels. Stars observable without saturation (80% full well) include those visible to the unaided eye: ~5th magnitude or brighter, depending on the observing mode, wavelength, and configuration.

Each channel includes a pupil wheel and a filter wheel, each with 12 optical elements, which may be used in various combinations. These elements include:

NIRCam has 10 Teledyne HgCdTe H2RG detectors, or sensor chip assemblies (SCAs), each with 2040 × 2040 pixels sensitive to light. Eight short wavelength detectors cover roughly the same area on the sky as the 2 long-wavelength detectors. In full frame imaging mode, all 10 detectors are read out non-destructively every 10.74 s. The smallest supported science subarray (64 × 64 pixels) can be read out in 49 ms (the shortest exposure time).

Kinematiccoupling

The JWST Near Infrared Camera (NIRCam) offers imaging, coronagraphy, wide field slitless spectroscopy, and time-series monitoring both in imaging and spectroscopy, as well as wavefront sensing measurements for JWST mirror alignment.

The 29 NIRCam filters have names "Fnnnx" where "nnn" refers to the central wavelength (e.g., 220 for 2.20 µm) and "x" refers to the filter width: "W2" for extra-wide (R ~ 1), "W" for wide (R ~ 4), "M" for medium (R ~ 10) and "N" for narrowband (R ~ 100).

Details about the structure and format of the data can be found in the Understanding JWST Data Files article. The JWST calibration pipeline is described in both the JWST Science Calibration Pipeline article and the official software documentation. More information about post-pipeline processing can be found in the JWST Post-Pipeline Data Analysis article.

Comes with all the fasteners you need to get this up and going. Please note, it does not work with the FYSETC kits as they do not follow the spec 150mm spacing requires to use this.

These are the laser-cut V2.4 kinematic bed mounts, meant to limit the effects of heat on your aluminum build plates, otherwise known as the taco effect.