Analysis class of Astronomy & Astrophysics. Basic requirements

Analysis class of Astronomy & Astrophysics. Basic requirements

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RSAA runs its research telescopes when you look at the Mount Stromlo Observatory and Siding Spring Observatories.

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Wide-Field Spectrograph (WiFeS)

WiFeS can be an integral-field, or imaging, spectrograph, and thus a spectrum is recorded by it from each pixel for the region that is imaged. WiFeS had been created and built at RSAA and set up in the 2.3m telescope in might 2009. The style attracts upon the history of both the RSAA's Dual-Beam Spectrograph (DBS), in addition to concentric image-slicer concept for the Near-infrared Integral-Field Spectrograph (NIFS) which was produced by RSAA when it comes to Gemini Observatory.

WiFeS was created to deliver as numerous simultaneous spectra as feasible over a continuing area associated with sky, each covering since wide a spectral range as you possibly can. It runs over the full wavelength range that is optical. Two split digital digital cameras are acclimatized to record the spectra russianbrides, each optimised for the part that is particular of wavelength range. Additional information about spectroscopy and exactly how WiFeS works can be obtained within the article WiFeS additionally the art work of spectroscopy.

WiFeS will be employed for a wide array of systematic applications, including:

  • Findings of enigmatic, extremely remote Gamma-Ray Bursts
  • Studies of old movie stars within our Galaxy that may offer information on just just exactly how it absolutely was put together
  • Studies of mass being ejected from young movie movie stars being nevertheless being created and generally are much like our Sun, to know just just how planets form
  • Dimensions associated with the internal motions in galaxies to find black colored holes within their cores and matter that is dark their external components
  • Studies associated with the motions of gasoline around remote quasars and radio galaxies.

Fundamental specs

  • Field of view: 38 x 25 arcsec (25 slitlets which are 1 arcsec wide and 38 arcsec long)
  • Wavelength protection: 330 - 900 nm
  • Detectors: 4096 x 4096 pixel Fairchild Imaging CCD in each camera
  • Pixel size: 15 microns
  • Pixel scale: 1 arcsec (slitlet width) x 0.5 arcsec (spatial sampling along slitlets)

Information for observers

WiFeS is just a double-beam, image-slicing, integral-field spectrograph that records optical spectra over a contiguous 25 arcsec x 38 arcsec industry of view. This field that is spatial divided in to twenty-five 1 arcsec wide “slitlets” with 0.5 arcsec sampling across the 38 arcsec lengths.

Both regarding the digital digital cameras for the blue and red stations are loaded with a x that is 4k pixel CCD detector. The spectrum of the tool expands from 330 to 920nm. This range could be noticed in a solitary visibility of each of the red and blue digital cameras utilising the low-resolution grating setup (R=3000) plus in two exposures utilizing the group of four high-resolution gratings (R=7000).

Requirements

  • Nasmyth focus, tool de-rotator
  • Concentric image-slicing IFU
  • Field of view: 38 x 25 arcsec (25 slitlets which are 1 arcsec wide and 38 arcsec long)
  • Wavelength protection: 330 - 920 nm
  • Detectors: 4096x4096 pixel Fairchild Imaging CCDs (red and cameras that are blue
  • Pixel size: 15 microns
  • Pixel scale: 1 arcsec (slitlet width) x 0.5 arcsec (spatial sampling along slitlets)

To learn more in regards to the specifications and employ of this WiFeS tool, please download the documents displayed regarding the right hand part associated with web page and you also may additionally find useful the next website:

WiFeS gratings

Grating Ruling thickness (lines/mm) Blaze wavelength (micron) quality Simultaneous coverage (nm) Wavelength interval (nm) Wave. Offset (pix) Y offset
U7000 1948 0.385 7000 0.109 0.329 0.438 0 0
B7000 1530 0.49 7000 0.14 0.418 0.558 0 0
R7000 1210 0.62 7000 0.177 0.529 0.706 0 0
I7000 937 0.8 7000 0.229 0.683 0.91 0 0
B3000 708 0.468 3000 0.27 0.32 0.59 0 0
R3000 398 0.742 3000 0.45 0.53 0.98 0 0

Efficiency

Look at book Dopita et al. (2009) for detailed information regarding the performance regarding the tool.

Measured throughput

The calculated last throughput for the tool (and telescope) are plotted below for every grating (except that U7000).

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