Photometry.

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Presentation transcript:

Photometry

Aperture Photometry

Aperture Photometry Image of open cluster NGC 957

Aperture Photometry Crowded Field Source Confusion

PSF Photometry : Point Spread Function(PSF)

PSF Photometry:

Photometry using IRAF Imexamine

Photometry using IRAF Sky FWHM = Annulus=2.5 FWHM (At least)

Photometry using IRAF

Photometry using IRAF

Photometry using IRAF

Photometry using IRAF

Photometry using IRAF Threshold between 4 and 6 Threshold too high Threshold too low

Photometry using IRAF

Photometry using IRAF annulus dannulus

Photometry using IRAF Aperture

PSF photometry with IRAF Select the PSF candidates Relative isolated stars Unsaturated stars Stars spread through the CCD 25 to 30 candidates!

PSF photometry with IRAF

PSF photometry with IRAF

PSF photometry with IRAF Estrela saturada

PSF photometry with IRAF Unsaturated star

PSF photometry with IRAF

PSF photometry with IRAF

PSF photometry with IRAF fitrad= circular area in which the pixels will be used to calculate the PSF fitting. Usually the FWHM can be used, unless there are too much crowding. Psfrad= radio in which the PSF is defined. Must be larger than the radius of the brightest star you want to measure.

PSF photometry with IRAF Function gaussian (black) lorentzia(red) Moffat b=1.5 (blue) Moffat b=3.5 (green) r is the distance to the center of the object. a and b are the fitting parameters

PSF photometry with IRAF Some commands of PSF task a= add star to the psf candidates list f= fits PSF d= delete star from the PSF list l = list the PSF candidates w= write the PSF to file

PSF photometry with IRAF task = seepsf

PSF photometry with IRAF

PSF photometry with IRAF Output from ALLSTAR Photometry list Rejected list Subtracted image

PSF photometry with IRAF Find stars in the subtracted image Concatenate files from FIND from original and subtracted (PCONCAT) Rename the resulting file (PRENUMBER) Re-do the aperture photometry with this new list Re-do the PSF photometry with the new list

PSF photometry with IRAF 1st subtraction Nth subtraction Original Image

PSF photometry with IRAF B V

Sharpness Isolated Star Sharpness próximo à zero Semi-resolved Galaxies Double or mixed sources Sharpness >> zero Cosmic rays and Image defects Sharpness << zero

Sharpness

Diagrama cor magnitude IRAF cl>pdump id,xcenter,ycenter,mag,merr,sharp terminal >sort 1,1b arquivo1 >sort 1,1b arquivo2 >join arquivo1 arquivo2

Color-magnitude Diagram