LDAP: couldn't connect to LDAP server

Differences

This shows you the differences between two versions of the page.

Link to this comparison view

Both sides previous revision Previous revision
Next revision 		Previous revision
data_reduction [2013/09/05 08:04]
mjc [Flat-fielding] 		data_reduction [2013/09/06 03:06] (current)
mjc [Flux Calibration]
Line 77: Line 77:
 ---- ----
 ==== Data Cube Generation ==== ==== Data Cube Generation ====
-wire, ADR+Final WiFeS data cubes are generated by resampling the flux values at the observed (x,y,λ) positions onto a rectilinear grid grid of (α,δ,λ).  The true y value for each pixel in the WiFeS field of view is derived using a wire frame observation (see Figure below).
  
 {{ :wiki:wire_wifes.png?600 |}} {{ :wiki:wire_wifes.png?600 |}}
 +
 +Light from the same origin on the sky is dispersed to different positions due to the effect of Atmospheric Differential Refraction (ADR; [[http://adsabs.harvard.edu/abs/1982PASP...94..715F|Filippenko 1992]]), which is sometimes referred to as Differential Atmospheric Refraction (DAR).  For WiFeS the ADR deflections in x and y are calculated (see Figure below) using observation details in the FITS header.
  
 {{ :wiki:adr_wifes.png?600 |}} {{ :wiki:adr_wifes.png?600 |}}
  
-----+The true (α,δ) coordinates derived from the wire frame and ADR calculation, and the observed λ values from the wavelength solution, are used as input to the WiFeS cube generation routine.  The output of this routine is still in MEF format (to facilitate visual inspection of individual slitlets).
  
 +----
 ==== Flux Calibration ==== ==== Flux Calibration ====
-links to stdstar catalogs...+After WiFeS data have undergone standard image processing steps (e.g., bias subtraction, cosmic ray rejection, flat-fielding), the absolute flux scale of the data must still be assessed.  This is done by observing spectrophotometric standard stars and comparing their observed fluxes to reference spectra.  In PyWiFeS this is done with the procedure outlined schematically in the Figure below, using routines defined in the 'wifes_calib' sub-module.
  
 {{ :wiki:flux_cal_wifes.png?600 |}} {{ :wiki:flux_cal_wifes.png?600 |}}
 +
 +The flux calibration step corrects for the smooth instrument throughput curve, as well as atmospheric extinction.  However sharp absorption features caused by molecules in the atmosphere (primarily O<sub>2</sub> and H<sub>2</sub>O) remain, and must be corrected in object spectra (bottom panel below) by measuring their structure in the spectra of flux-calibrated smooth spectrum stars (top panel below).
  
 {{ :wiki:telluric_wifes.png?400 |}} {{ :wiki:telluric_wifes.png?400 |}}
 +
 +== Spectrophotometric Standard Star Catalogs ==
 +Flux calibration requires a set of reference spectra of spectrophotometric standard stars.  Included in PyWiFeS are two spectra catalogs:
 +  * [[http://adsabs.harvard.edu/abs/1999PASP..111.1426B|Bessell et al., 1999]]
 +  * [[http://adsabs.harvard.edu/abs/1990AJ.....99.1621O|Oke et al., 1990]]
 +Another excellent specphot standard star catalog we recommend downloading is:
 +  * [[http://adsabs.harvard.edu/abs/2005PASP..117..810S|Stritzinger et al., 2005]], Carnegie specphot standards, availaible [[http://www.das.uchile.cl/~mhamuy/SPECSTDS/|here]]
 +
 +Planned future catalogs of spectrophotometric standard stars which will soon be available are:
 +  * All-Sky HST spectrophotometric standards (Bessell et al., in prep.)
 +  * Gaia spectrophotometric standard star catalog ([[http://adsabs.harvard.edu/abs/2012MNRAS.426.1767P|Pancino et al., 2012]])
Back to top