Spectroscopic Data
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Transcript Spectroscopic Data
Spectroscopic Data
ASTR 3010
Lecture 15
Textbook Ch.11
Spectroscopic Measurement
Schematic Diagram of a Typical Spectroscopic Data
Only Readout the relevant portion of CCD array
• Spectroscopic data are typically long and slender.
to save the readout time and storage space…
Actual Spectroscopic Data
• Similar to Imaging Data, a similar set of calibration images is obtained for
spectroscopic observation same pre-processing!!
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over-scan correction
trimming
bad-pixel correction
cosmic ray hits removal
zero correction
dark correction
flat-fielding
Unique spectroscopic calibration data
• Unlike imaging observations, two additional kinds of calibration data are
obtained for spectroscopic observations.
o arc images (wavelength correction)
o smooth spectrum standards (telluric feature correction)
o (and possibly flux standard stars = standard stars in imaging)
Steps of spectroscopic data reduction
Array pre-processing
bad pixel, bias, over-scan, trim, zero, flat-fielding
Spectrum Extraction
find trace extract normalize
Wavelength Calibration
Telluric Correction
Interpretation of Spectra
using arc images (e.g., gas emission lines)
using stars with known smooth spectra
line width measurement, Teff, [Z/H], vsini, etc.
Extraction of Spectra
words in green
denote corresponding
IRAF commands for the
task
finding the aperture and defining the sky regions apfind & apedit
spectral aperture is not always a horizontal line!
need to trace the aperture along the dispersion axis aptrace
Wavelength calibration using Arc images
• Excited lines from a combination of noble gases (He, Ne, Ar, Xe, Th, etc.)
using arc images, you can convert pixel
numbers to wavelength!
identify
How do we extract (find and trace) arc spectra?
• or very faint objects?
• Use well exposed bright star spectrum as a reference!
Normalization or Flux Calibration
continuum
sensfunc and calibrate
continuum or splot
Telluric Correction
Telluric standard stars : stars with no (or very little) spectral line feature.
low metallicity stars, white dwarfs, fast rotating stars
telluric
Plotting the extracted spectra and …
splot display the extracted spectrum and do simple operations on the
spectrum such as continuum normalization and equivalent width
measurements.
‘h’ + ‘k’
EW fit with
A Gaussian to
continuum=1
Equivalent Width
• Quantitative indicator of the strength of a spectral feature
• EW = area of the spectral feature
area = area
1.0
0.0
EW unit is the wavelength unit of the spectrum
One caveat in spectroscopic pre-processing…
Flat images…
flat images sometime taken w/wo the dispersing element.
Which one is better? Is only one kind useful?
Flats in spectroscopic data
this spectrum is a combination of the above detector flat + spectral response
of the system.
Flat-fielding is to remove the pixel-to-pixel sensitivity variation!
Other gradual, global variation can be taken out later.
In summary…
Important Concepts
Important Terms
• Structure of the spectroscopic data
• Steps of spectroscopic reduction
• aperture tracing
• telluric correction
• equivalent width
good manual http://iraf.noao.edu/iraf/ftp/iraf/docs/spect.ps.Z
Chapter/sections covered in this lecture : 11.6