Supplemental data for "Improving the Photometric Calibration of the
Enigmatic Star KIC 8462852" by Lahey, Dimick & Layden 2017.


JAAVSO_45_202.pdf = the final journal article

KIC_I_??.eps  =  finder charts showing KIC and comp stars (N is down
		  and E is to the left, 21 x 21 arcmin field of view)

Tave_ave?_kicFIN?.new2  \
ave?_kicFIN?.new2        = Photometric data as follows:
kic_fin?.dat            /

  Photometry from indivdividual images & nightly means, calibrated 
  using magntudes from a=Table1(APASS) or b=Table3(BGSU):

aveV_kicFINa.new2  &  Tave_aveV_kicFINa.new2  use APASS comp* mags
aveV_kicFINb.new2  &  Tave_aveV_kicFINb.new2  use BGSU comp* mags
     N=15 nights

aveI_kicFINa.new2  &  Tave_aveI_kicFINa.new2  use APASS comp* mags
aveI_kicFINb.new2  &  Tave_aveI_kicFINb.new2  use BGSU comp* mags
     N=29 nights

kic_finV.dat   (100 lines)
kic_finI.dat   (532 lines)
  format:   JD    V_apass  SD   SEM   V_bgsu   SD   SEM  Ncomp
     where SD=standard deviation, SEM=standard error of the mean


kic_lc_AAVSO.eps      Figure 1: AAVSO with our indiv data in blue Xs
kic_lc_AAVSOta.eps    Figure 1: AAVSO wtih our nightly means in blue Os.

comp_mags4.eps        Figure 2 from the journal article

comp_meds_kic.eps     The differntial photometry of KIC was calculated
		      using each of the comparison stars along the
		      horizontal axis in turn.  Each point represents
		      the median magnitude of the time-series data
		      using the respective comparison star, and the
		      error bars marks the SEM.  Open squres us the
		      APASS magnitudes from Table 1 and the dotten
		      line is their median.  Solid circles use the
		      BGSU magnitudes from Table 3 and the dashed line
		      is their median.  The goal of this figure is to
		      use more data (15 nights in V versus 3
		      photometric nights in Figure 2; 29 nights in I
		      vs. 3 photometric nights in Figure 2).  Outlier
		      points mark stars with questionalbe photometry.

comp_meds_116.eps     Analogous plot using comp star 116 rather
			than KIC as the "variable star".  Used 
			to check for consistency with KIC version.

kic_lc_Idip.eps	      The magnitude of KIC on our individual frames 
		      taken near the dipping event of 2017 May-June are
		      shown as a function of time (blue crosses).  The
		      nightly mean magnitudes are shown as red
		      circles.  The dashed line is the median of our
		      23 nights obtained before JD=7852 days, and the
		      dotted lines mark the +/- 1-sigma range of those
		      values.  The curve shows, for context, the
		      central portion of the D1500 dimming event from
		      Boyajian (2016) placed at an arbitrary time to
		      demonstrate the depth and duration of a known
		      event.

kic_lc_Idip_zooms.eps   The bottom panel is from kic_lc_Idip.eps and
			the top panels show details of nights 2, 3, and 4
			in the lower panel, with expanded time axes to
			show that most of the vertical scatter is
			random, not secular.  We believe that the
			vertical spread seen in some nights,
			particularly JD=7888, is more likely due to
			the star trailing across poorly-calibrated
			pixels on our CCD than actual variations in
			the brightness of KIC.  The green line in
			panel (3) shows the steep ingress to the
			deepest dip in the bottom panel -- even the
			steepest slope observed by Kepler appears
			shallow compared to the variations of the
			first six data points in this night,
			suggesting they are not real.



