Jul 07, 2010 UT: Photometry of cataclysmic variable SDSS 162520.3+120309

Michael Richmond
Jul 7, 2010

On the night of July 6/7, 2010, I observed the cataclysmic variable star SDSS 162520.3+120309 which is currently in outburst.

The setup was:

Notes from the night

This is a chart of the field based on one of my images last night.

The chart has several of the brighter stars in the field labelled with letters, just to keep me straight as I perform the reductions. Star P is in the Tycho-2 catalog, but it's so bright that it is saturated in my measurements. The star labelled "C" is in the USNO B1.0 catalog:

         name                   RA             Dec           B         R
 USNOB1.0 1019-0299359      16:25:25.739    +11:59:21.18   14.27     13.24
                                                           14.46     13.30

Note the star labelled "X", which shows evidence for very short dips in its light (eclipses??).

         name                   RA             Dec           B         R
 USNOB1.0 1020-0302453      16:25:01.638    +12:02:32.57   15.05     14.02
                                                           15.56     14.14

I measured the instrumental magnitude of each star with aperture photometry, using a radius of 4 pixels = 4.2 arcseconds and sky defined by an annulus around each star. Following the procedures outlined by Kent Honeycutt's article on inhomogeneous ensemble photometry, I used all stars available in each image to define a reference frame, and measured each star against this frame.

One output of the ensemble solution is the value of the zero-point of each frame relative to the others. In the graph below, I plot this zero-point as a function of time. There's a gradual rise as the field sinks lower into the western sky.

Below is a graph of the scatter in differential magnitude versus magnitude in the ensemble solution.

The floor of this diagram corresponds to a scatter of about 0.010 mag, which is rather mediocre; this may be due in part to the haze, and in part due to the rotation of the field halfway through the observing run. The target is the second-brightest star, at differential magnitude 0.2. its scatter of 0.064 mag is due to the changes in its light. The star at differential magnitude 1.07, with scatter 0.037 mag, is the one labelled "X" in the chart above.

Light curves for selected stars (SDSS162520 and stars A - D, as well as X) in the field are shown below. The target is shown by light green crosses.

The star "X" is shown by red-orange circles near the bottom of the graph. Note the two brief dips in light -- I've verified by inspecting the images that these dips are not due to any image defects.

Here's a closeup of the variation in SDSS162520 and two comparison stars.

Bill Stein kindly sent a copy of his measurements from slightly later in the night to me. You can see the good agreement of our measurements in the overlap period, and a gradual brightening trend.

I've made a table of the measurements themselves, with three different flavors of time. The differential magnitudes from the ensemble solution have been shifted so that star "C" in my chart, USNOB1.0 1019-0299359, has value 13.8; that should be close to its V-band magnitude.

Here's the start of the table.

# Measurements of SDSS162520+120309 made at RIT Obs, Jul 7, 2010 UT, 
#    by Michael Richmond, using 14-inch Celestron and SBIG ST-9E CCD. 
# Exposures 30 seconds long, no filter. 
# Tabulated times are midexposure (FITS header time - half exposure length) 
#    and accurate only to +/- 1 second (??). 
# 'mag' is a differential magnitude based on ensemble photometry 
#    using a circular aperture of radius 4.2 arcseconds. 
#    which has been shifted so USNOB1.0 1019-0299359 has mag=13.8 
#    as a very rough estimate of its V-band value. 
# UT_day             JD            HJD        mag    uncert
Jul07.09156     2455384.59156  2455384.59517  14.081  0.011 
Jul07.09197     2455384.59197  2455384.59558  14.083  0.011 
Jul07.09236     2455384.59236  2455384.59597  14.074  0.011 

Last modified 7/07/2010 by MWR.