Presentation on theme: "Echelle Spectroscopy Dr Ray Stathakis, AAO. What is it? n Echelle spectroscopy is used to observe single objects at high spectral detail. n The spectrum."— Presentation transcript:
What is it? n Echelle spectroscopy is used to observe single objects at high spectral detail. n The spectrum is mapped as a 2-dimensional array onto the detector, providing large wavelength coverage.
How is it done ? 2 ) The Cross-Disperser Successive orders overlap with constant M. –M = order number, = wavelength –e.g. red light at 8000A in order 71 falls on top of blue light at 4000A in order 142. –the peak of the blaze function goes bluer for larger orders. n A prism or grating is used to disperse light in the perpendicular direction to the Echelle grating to separate the orders. n The result at the detector is a stack of spectra from successive orders, which goes from blue at the bottom left corner to red at the top right corner. n The FSR is the range of wavelengths most efficiently observed at each order.
How is it done ? 3) Spectrograph design n The main Echelle spectrograph at the AAT is UCLES. n It is floor-mounted at the Coude focus. n Two configurations: –31 g/mm gives wide wavelength range, full FSR coverage –79 g/mm gives 2.5 x sky coverage
Designing your Experiment 1) Pros and cons of Echelles n Advantages: –Efficient at high spectral resolution R where R= / = 30,000 -1,000,000 or resolving 10 - 0.3 km/sec at 6000A –Accurate removal of sky features –Large wavelength coverage. n Disadvantages –Limited magnitude range –Complex instrumental profile –Small sky coverage –Slow turnover time R=300 R=2500 R=40,000 R=1,000,000
Designing your Experiment 2) Getting it Right n Check whether you need larger sky coverage. n Check the location of important regions of the spectrum n Choose the optimum detector. n Check integration times using the S/N calculator.
Observing Technique n The detector is rotated and focused, and the grating is shifted to locate the wavelength region. n The beam is continuously rotated to align the slit with the direction of atmospheric dispersion. n A ThAr arc lamp exposure is taken to calibrate wavelengths. n An optional iodine cell provides even more accurate wavelengths.
Data Processing n Special packages exist to handle the format, e.g. DOECHELLE in IRAF & ECHEMOP in Starlink n Data reduction steps are: –standard detector correction –location and identification of orders –straightening of orders & forming “echellogram” –wavelength calibration –location of target and sky in each order and correction of sky –combination of orders into continuous spectra
Examples of Echelle Science n Searching for planets by finding stars which wobble. n Observing atmospheres of stars which pulsate. n Observing halo stars to determine the chemical history of our galaxy, and even the universe.
Other Echelle Techniques n UHRF - provides single order observations at up to R = 940,000. –UHRF is ideal for studying cool clouds in the ISM. –Other projects include atmospheric lines from Mercury and isotopes in stars. n The Semel polarimeter is used with UCLES. The main project is Zeeman Doppler Mapping of the magnetic structure of stars. n The Manchester Echelle provides single order observations over a large area, and is ideal for ISM emission line studies.
Useful sites and references Useful technical information can be obtained at the AAO web site: –http://www.aao.gov.au/astro/instrum.html under UCLES and UHRF. See the on-line manual, the S/N calculator and on-line ThAr arc atlas. Further reading includes: –“Astronomical Optics” by Daniel Schoeder, 1987, Academic Press Inc. (General) –Walker, D. D. & Diego, F. 1985, MNRAS, 217, 355-365 (UCLES) –Barlow, M. J. et al., 1995, MNRAS, 272, 333-345 (UHRF) –Diego, F., et al. 1995, MNRAS, 272, 323-332 (UHRF) –Diego, F. & Walker, D. D. 1985, MNRAS, 217, 347 (UCLES & UHRF)