Sep 17, 2008 UT: Photometry of new dwarf nova in Andromeda = V466 And

Michael Richmond
Sep 17, 2008

On the night of September 16/17, 2008, I observed a new object which was recently discovered in the constellation Andromeda. The name of this variable has now been set to V466 And. It's still very early, but you can find a bit of information on the new object in these sources:

The setup was:

Notes from the night

This is a chart of the field taken from the DSS.

The chart has several of the brighter stars in thefield labelled with letters, just to keep me straight as I perform the reductions. The star labelled "bright!" saturates my detector. Stars A and B are in the Tycho-2 catalog,

label                         RA        Dec          Bt        Vt         
  A    TYC 2828 1694 1     29.97369  +44.10297       12.081  11.143
  B    TYC 2841  810 1     30.22008  +44.08782       13.369  11.679

                    These stars appear in AAVSO VSP chart      V
  P                                                           14.2
  Q                                                           14.1
  R                                                           13.0

On this night, star A was saturated as the field rose high above the horizon and I re-focused. Therefore, I don't include A as a reference in the ensemble, though I do show its measurements in the graphs below.

I measured the instrumental magnitude of each star with aperture photometry, using a radius of 3 pixels = 5.6 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. The many high points are due to trailed images.

Below is a graph of the scatter in differential magnitude versus magnitude in the ensemble solution. The only good bright reference star is the one marked "B" in the chart above, which appears at differential magnitude 0.7. The star with elevated scatter, "A" at differential mag 0.0, is not included in the solution as a reference star.

The floor of this diagram corresponds to a scatter of about 0.007 mag. V466 And appears at differential magnitude 4.3; its scatter of 0.060 mag is a bit higher than that of stars of similar brightness.

Light curves for selected stars (V466 And and stars A - D, P, Q) in the field are shown below. V466 And is shown by light green crosses.

Here's a closeup of the variation in Nova And 2008 and a few comparison stars.

Look at its behavior relative to other stars in the field over the period of our measurements:

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 "B" in my chart, TYC 2841-810-1, has value 11.679. Remember these are unfiltered measurements.

Here's the start of the table.

# Measurements of V466_And made at RIT Obs, Sep 17, 2008 UT. 
# by Michael Richmond under good conditions. 
# Each exposure 30 seconds long with 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 5.6 arcseconds. 
#    which has been shifted so TYC 2841-810-1 mag=11.679 
#    to match Vt value in Tycho-2 catalog. 
# UT day      JD-2,450,000  HJD-2,450,000   mag    uncert
Sep17.09664     2454726.59664  2454726.59163  15.170  0.047 
Sep17.09709     2454726.59709  2454726.59208  15.278  0.049 
Sep17.09858     2454726.59858  2454726.59357  15.249  0.048 
Sep17.09903     2454726.59903  2454726.59402  15.273  0.047 

Last modified 9/17/2008 by MWR.