Site hosted by Angelfire.com: Build your free website today!

 

 

 

 

 

 

 

 

 

 

High Precision Photometry

My interest is in high precision differential photometry with the objective of being able to detect exoplanet transits.   I have set myself a target of being able to achieve 0.002 magnitude precision for stars of magnitude 11 with an integration time of 2 minutes. 

My technique is still developing, but the discussion below will touch on several important elements.  Bruce Gary has written a great book that describes how an amateur can observe exoplanet transits. 

 

The Camera - Linearity

The CCD camera used should have excellent linearity.  I currently use an SBIG ST-8XME without Anti-Blooming gates (NABG).  NABG gives the CCD higher sensitivity (QE), as well as greater well depth.  Both these factors help with collecting more photons and therefore reducing photon shot noise. 

I have also determined my CCD's limit of linearity.  Although the CCD will output > 60,000 ADU's (Analog Digital Units, or counts) there is a point beyond which the CCD response ceases to be linear.  Photometry will not be precise if stars being measured produce pixel values above this limit.  Bruce Gary estimates that his ST-8 is linear up to 62,000 ADU but I have found that mine is linear only up to 40,000 ADU.  He uses a number of tests (described on his website) to arrive at his conclusion, but I have found that for my CCD these tests were not conclusive.  Instead I noticed that when I plotted count Variance vs ADU (the same process as for calculating CCD gain - see http://www.mirametrics.com/tech_note_ccdgain.htm ) at 40,000 ADU the Variance started to deviate significantly from a linear trend (chart right).  Beyond 40,000 ADU, variance is less than expected, indicating onset of non-linearity.  The full calibration sheet of my CCD is here.

 

The Camera - Autoguiding

The ST-8XME has an additional chip built-in that enables autoguiding with the one camera.  I have found on the several occasions that the guide star has been lost (e.g. cloud), photometric precision suffers immensely.

 

Quantifying Errors

Given the importance of precision, it is very important to be able to model the expected error from a measurement as well as processing sequence.  Being able to do this enables the selection of acquisition parameters (exposure time, target star magnitude, filter), calibration frames (no. of flat frames and ADU level, dark frames, bias).  My approach is based on the paper by Newberry (1991), "Signal-to Noise Considerations for Sky-Subtracted CCD Data". 

I have made a spreadsheet that calculates the expected error given imaging and processing parameters.  I offer it here - but use with caution - the output seems to match actual results, but there may still be mistakes that have crept in.

 

Time series photometry software

Based on a discussion in AAVSO, I have selected Muniwin for this purpose.   Muniwin is excellent for time-series photometry.  It is fast, efficient, handles large datasets well, has automatic star detection as well as full frame photometry (i.e. it measures all detected stars on the CCD frames), permits use of multiple apertures - and runs on Windows XP.  The last point is important because all the important scientific photometry packages seem to run mainly on Linux (e.g. IRAF).

 

Ensemble photometry

Ensemble photometry is the use of multiple comparison stars rather than just one comp and one check star.  It results in improved precision is the comp stars are chosen such as to screen out those that are variable on the timescale of the observation.  The technique is described in Everett and Howell's paper "A Technique for Ultrahigh-Precision CCD Photometry", PASP 2001.  My implementation of this technique in a spreadsheet currently uses a maximum of 20 stars.

 

U Sco campaign photometry

The U Sco campaign was a good opportunity to test out these tools.  Below is a light curve for 19th Feb 2010, 23 days after eruption and when it had dimmed from 8th mag at peak to mag 14.5.  The light curve clearly show the eclipse of the dwarf star by its companion.  Note that the error bars are  +- 0.02 mag, far below the precision needed for exoplanet transits - but this is a mag 14 star, and I was using a V filter that significantly reduces the light.

 

Visitor  page counter  since 20th Sept 2008

 

Copyright 2003 to 2012, by TG Tan.  All rights reserved.  Copyright exists in all original material available on this website.  This material is for your personal individual, nonprofit use only.  Redistribution and/or public reproduction of this material is strictly prohibited without prior express written permission from the author.