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Date: Fri, 30 Jul 93 18:46:21 CDT
From: gav@astro.as.utexas.edu (Gerard de Vaucouleurs)
Subject: Revised list of comparison stars for SN93J
%new Final listing 7/12/93; rev.7.23.93; minor rev. HC 7.27.93
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\begin{center}
{\bf Revised magnitudes and colors of SN1993J comparison stars}\\
\vspace{5mm}
G.\ de Vaucouleurs (U.\ Texas), Harold\ G.\ Corwin, Jr.\ (IPAC, Caltech),
Brian A.\ Skiff (Lowell Obs.) \\
\end{center}
\vspace{1cm}
Tables 1 and 2 collect a number of old and new observations of the brighter
comparison stars of SN1993J, with cross-identifications in various maps and
catalogs. We would appreciate receiving any corrections that might have
escaped our attention. There are still some discrepant results which may
indicate incomplete corrections for color equation.\\ \par
We recommend to CCD observers\\ \par
(1) to use Richmond's star B = GSC 4383-0928, with H.\ Corwin's values (HC-4),
as the primary local standard, \\
(2) to re-measure Richmond's star C = GSC 4383-0340 which -- with V = 14.5 --
will soon be the most convenient comparison star, being only 25$''$ from the
supernova, but has still uncertain color indices.\\
(3) to measure as often as possible with accurate timing star AAVSO D =
GSC 4383-0384 which is a newly discovered W UMa variable (see table 2 note). \\
(4) to re-measure GSC 4383-1031, 4383-1037, and 4383-1123 which have
uncertain color indices, and GSC 4383-0094 which should be checked for
possible variability. \\
\\ \par
Table 1 shows the brighter BD stars newly measured at Lowell Observatory,
including the difficult DM 69.541 pair (separation 9$''$). Except for this
double star the corrected GSC magnitudes {\bf V$^{*}$} are in close agreement
with the Flagstaff measurements. We urge the visual observers to revise
the reduction of their early observations of the supernova with these
improved magnitudes and new color indices.\\
Table 2 collects photoelectric and CCD measurements of fainter stars,
many newly acquired at several observatories, to help a proper reduction,
including color terms, to the standard Johnson U,B,V and Cousins R$_{C}$,
I$_{C}$ systems. We urge the CCD/photoelectric observers to use this new
information to revise their provisional reductions and allow for the
varying color of the supernova.
\footnote{Also, please do not forget to correct for
the color dependence of atmospheric extinction in the B band, expressed by
the $-$0.033(B$-$V) term in the correction, meaning that even at the same
zenith distance blue stars are more strongly dimmed than red stars by
Rayleigh scattering. Do not apply such correction to the V band (where
the Chappuis band of ozone cancels locally the Rayleigh slope) or to the
U band (where it is = 0 by definition). A good reference to the
finer points of stellar photometry is the three chapters by A.\ T.\ Young
in "Methods of Experimental Physics", vol.\ 12, Part A: Astrophysics, Optical
and Infrared, (ed.\ N.\ Carleton), Academic Press, New York--London, 1974.} \\
\par
Table 3 gives the GSC photovisual magnitudes and their transformation to
the V system for all the comparison stars in the Thompson-Bryan M\,81 chart
which are brighter than 14.5 and have a value of B$-$V in Tables 1 and 2. \\
\par
Stars fainter than {\bf V} = 14.5 have not yet been re-measured (except
for the 17th mag star 25$''$ SSE of the SN, for which {\bf V = 17.8, B$-$V
$\simeq$ 1.3, V$-$R$_{C} \simeq$ 0.7}) and will be found in previous
compilations distributed by H.\ Corwin through the Nova network in
May-June 1993. \\
\newpage
\oddsidemargin 0.0in
\begin{center}
\begin{tabular}{cccccccccc}
\multicolumn{10}{c}{\bf Table 1. BD stars, 8.5 $<$ V $<$ 10.7}\\
\hline\hline
{\bf GSC} & {\em SAO} & {\em DM} & {\em HDC} & {AGK3} & {\em ADS} & {Source}
& {\em AAVSO} & {\em MAA} & {\em T-B} \\
{\em m$_{pv}$} & {\em m$_{v}$} & {\em m$_{v}$} & {\em m$_{v}$} & {\em m$_{v}$}
&{\em Gr.AC} & & {\em m$_{v}$} & {\em m$_{v}$} & {\em m$_{v}$}\\
{\em V$^{*}$} & & {\em V$^{*}$} & & & {\em GC} & {\bf V} & & & \\
& {\em \em m$_{p}$} & & {\em m$_{p}$} & {\em m$_{p}$} & Spectrum
& {\bf B$-$V} & & & \\
\hline
{\bf 4383-0848ab} & 15020 & 69.542 & 85548 & ----- & 7566AB & Sk 2n & ----- & ----- & -----\\
7.97 & 8.7 & 8.5 & 8.7 & ----- & 4007 & ----- & 8.9 & 8.9 & 8.9// \\
{\bf 8.44} & ----- & 8.8 & ----- & ----- & 13606 & {\bf 8.54} & ----- & ----- & ----- \\
----- & ----- & ----- & 9.1 & ----- & F5 & {\bf 0.49} & ----- & ----- & -----\\
\hline
{\bf 4383-0738} & 15026 & 69.544 & 85743 & 429 & ----- & Sk 2n & ----- & A & ----- \\
8.67 & 8.8 & 9.0 & 9.3 & 9.4 & 4008 & ----- & 9.4 & 9.4 & 9.4// \\
{\bf 9.23} & ----- & 9.4 & ----- & ----- & ----- & {\bf 9.20} & ----- & -----
& ----- \\
----- & 9.8 & ----- & 10.3 & 9.8 & 9.6;K0 & {\bf 1.04} & ----- & ----- & -----
\\
\hline
{\bf 4383-1127ab} & 15017,-8 & 69.541 & ----- & 426,-7 & 7565AB & Sk 2n & ----- & -----
& ----- \\
(8.53) & (9.75) & (9.4) & ----- & ----- & ----- & ----- & ----- & ----- &
----- \\
(9.04) & ----- & (9.8) & ----- & ----- & & {\bf 9.85} & ----- & ----- & ----- \\
----- & ----- & ----- & ----- & ----- & G: & {\bf 0.72} & ----- & ----- &
----- \\
\hline
{\bf 4383-1127 E} & 15018 & 69.541S & ----- & 427 & ----- & Sk 2n & B & ----- & ----- \\
----- & 10.5 & ----- & ----- & ----- & 4013 & ----- & 10.4 & ----- & 10.4// \\
----- & ----- & 10.5: & ----- & ----- & 13605 & {\bf 10.58:} & ----- & -----
& ----- \\
----- & ----- & ----- & ----- & 10.9 & G: & {\bf 0.72:} & ----- & ----- & ----- \\
\hline
{\bf 4383-1127 W} & 15017 & 69.541P & ----- & 426 & ----- & Sk 2n & C & ----- & ----- \\
----- & 10.5 & ----- & ----- & & 4012 & ----- & 10.5 & ----- & 10.5//\\
----- & ----- & 10.6: & ----- & ----- & 13603 & {\bf 10.63:} & ----- & -----
& ----- \\
----- & ----- & ----- & ----- & 10.9 & G: & {\bf 0.73:} & ----- & ----- &
----- \\
\hline
{\bf 4383-0150} & 15009 & 69.540 & ----- & 423 & ----- & Sk 2n & ----- & B & ----- \\
9.87 & 9.6 & 9.5 & ----- & 10.0 & ----- & ----- & 10.3 & 10.4 & 10.3// \\
{\bf 10.46} & ----- & 10.0 & ----- & ----- & ----- & {\bf 10.46} & ----- &
----- & ----- \\
----- & 11.1 & ----- & ----- & 11.1 & K0 & {\bf 1.25} & ----- & -----
& ----- \\
\hline\hline
\end{tabular}
\end{center}
\vspace {5mm}
{\bf V$^{*}$} magnitudes from GSC m$_{v}$ (see Appendix):
{\bf V$^{*}$} = m$_{v}$ + 0.40 + 0.15(B$-$V).\\
{\bf V$^{*}$} magnitudes from DM m$_{v}$ (ApJ 295, 287, 1985):
{\bf V$^{*}$} = 7.0 + 1.2(m$_{v} -$ 7.0).\\
\vspace{5mm}
{\bf Sources codes and references (Tables 1 and 2):}\\
BKR = McDonald Obs., Brandt, J.\ C., Kalinowski, J.\ K., and Roosen, R.\ G.
1972, ApJS 24, 421.\\
HC = McDonald Obs., Corwin, H.\ G., IAU Circ.\ 5742 (Apr 3, 1993).\\
JN = McDonald Obs., Neff, J.\ quoted in Table 3 of BKR. \\
KP = Kitt Peak N.\ Obs., Schulman, E.\ and Cox, C.\ communicated by
M.\ Richmond.\\
MR = M.\ Richmond's stars A, B, C (Nova network).\\
PP = Haute-Provence Obs., Prugniel, P.\ private communication.\\
Sa = Palomar Obs., Sandage, A.\ 1984, AJ 89, 621.\\
Sk = Lowell Obs., Skiff, B., to appear in Inf.\ Bull.\ Var.\ Stars.\\
SHV = van Vleck Obs., Salzer, J., Herbst, W.\ and Vinton, G.\ IAU Circ.\ 5741.\\
TK = Ouda Station, Kyoto U., Kato, T.\ private communication.\\
Sk = Lowell Obs., Skiff, B., to appear in Inf.\ Bull.\ Var.\ Stars.\\
SHV = van Vleck Obs., Salzer, J., Herbst, W.\ and Vinton, G.\ IAU Circ.\ 5741.\\
TK = Ouda Station, Kyoto U., Kato, T.\ private communication.\\
VBO = Vainu Bappu Obs., Pradhu, T.\ P.\ {\it et al.}, private communication.\\
WH = van Vleck Obs., Herbst, W.\ {\it et al.}, private communication.\\
\newpage
\begin{center}
\begin{tabular}{ccrccrcccll}
\multicolumn{11}{c}{\bf Table 2. Fainter comparison stars, 10.3 $<$ V $<$
14.6}\\
\hline\hline
{\bf GSC} & {\em AAVSO} & {\em MAA} & {\em T-B} & {\bf V} & {\bf U$-$B} &
{\bf B$-$V} & {\bf V$-$R$_{C}$} & {\bf V$-$I$_{C}$} & {\em Source} &
{\em Remarks}\\
\hline
{\bf 4383-0860} & 10.3 & B1 10.3 & 10.3/ & {\bf 10.32} & {\bf $-$0.06} &
{\bf 0.39} & ----- & ----- & Sa-19 1n & \\
{\bf 4383-0698} & 10.8 & C1 10.8 & ----- & {\bf 10.81} & ----- & {\bf 1.05} &
----- & ----- & Sk 5n & now C (MAA) \\
{\bf 4383-0384} & D 10.7v? & 10.8 & 10.7// & {\bf var.} & ----- & {\bf 0.48} &
----- & ----- & Sk 5n & see note\\
{\bf 4383-0565} & 11.4 & E 11.4 & ----- & {\bf 11.40} & ----- & {\bf 0.54} &
{\bf 0.30} & {\bf 0.61} & WH 20n & = MR-A\\
& & & & {\bf 11.41} & ----- & {\bf 0.56} & ----- & {\bf 0.63} & TK .. & \\
& & & & {\bf 11.42} & ----- & {\bf 0.57} & ----- & ----- & Sk 1n & \\
& & & & {\bf 11.41} & ----- & {\bf 0.54} & {\bf 0.31} & {\bf 0.60} & VBO ..
& \\
& & & & {\bf 11.40} & {\bf 0.06} & {\bf 0.56} & {\bf 0.29} & {\bf 0.60} &
KP 8n & \\
& & & & {\bf 11.38} & ----- & {\bf 0.58} & {\bf 0.30} & {\bf 0.57} & PP .. &
\\
{\bf 4383-1031} & 11.7 & D 11.7 & /11.6 & {\bf 11.62} & {\bf $-$0.04} &
{\bf 0.53} & {\bf 0.33} & {\bf 0.69} & HC-3 3n & \\
& & & & {\bf 11.73} & {\bf 0.05:} & {\bf 0.46:} & ----- & ----- & JN-B 1n
& \\
& & & & {\bf 11.73} & ----- & {\bf 0.51} & ----- & ----- & BKR-B 2n & \\
{\bf 4383-0224} & ----- & D1 11.8 & 11.8/ & {\bf 11.85} & {\bf 1.29} & {\bf 1.30}
& {\bf 0.68} & {\bf 1.29} & HC-6 3n & \\
& & & & {\bf 11.84} & {\bf 1.33} & {\bf 1.32} & ----- & ----- & Sa-8 5n
& \\
{\bf 4383-0928} & 11.9 & F 11.9 & /11.9 & {\bf 11.90} & {\bf $-$0.08} &
{\bf 0.50} & {\bf 0.30} & {\bf 0.60} & HC-4 2n & = MR-B \\
& & & & {\bf 11.93} & ----- & {\bf 0.48} & ----- & ----- & Sk 3n & HC Local\\
& & & & {\bf 11.89} & {\bf $-$0.08} & {\bf 0.52} & {\bf 0.28} & {\bf 0.59} &
KP 11n & standard \\
{\bf 4383-0308} & 11.8 & G 11.8 & /11.8 & {\bf 11.78} & {\bf 0.16} & {\bf 0.69} &
{\bf 0.40} & {\bf 0.80} & HC-2 3n & \\
{\bf 4383-0434} & 12.4 & H 12.4 & 12.4// & {\bf 12.45} & {\bf 0.11} & {\bf 0.63}
& {\bf 0.39} & {\bf 0.76} & HC-1 3n & \\
{\bf 4383-0863} & 12.9 & I 12.9 & 13.0// & {\bf 12.88} & ----- & {\bf 0.90} &
----- & ----- & Sk 1n & \\
{\bf 4383-0935} & 12.9 & I1 12.9 & 12.9/ & {\bf 12.89} & {\bf 0.17} & {\bf 0.73} &
----- & ----- & Sa-14 4n & \\
{\bf 4383-0244} & ----- & J 13.0 & 13.0/ & {\bf 12.99} & ----- & {\bf 1.20} &
----- & ----- & Sa-15 1n & \\
{\bf 4383-1123} & 13.6 & K 13.6 & /13.6 & {\bf 13.65} & {\bf $-$0.09:} &
{\bf 0.57} & {\bf 0.34} & {\bf 0.69} & HC-5 3n & \\
& & & & {\bf 13.64} & ----- & {\bf 0.70:} & ----- & ----- & Sk 1n & \\
{\bf 4383-1028} & 13.7 & L 13.7 & 13.7/ & {\bf 13.71} & ----- & {\bf 0.77} &
----- & ----- & Sa-1 1n & \\
{\bf 4383-0633} & 13.8 & M 13.8 & 13.8/ & {\bf 13.78} & {\bf 0.16:} & {\bf 0.58} &
----- & ----- & Sa-13 2n & \\
{\bf 4383-0094} & 13.9 & N 13.9 & 13.9/ & {\bf 13.92} & {\bf 0.42} & {\bf 0.80} &
----- & ----- & Sa-9 6n & \\
{\bf 4383-1005} & 14.0 & O 14.0 & 14.0/ & {\bf 14.03} & ----- & {\bf 0.95} &
----- & ----- & Sa-6 1n & \\
{\bf 4383-1037} & 14.1 & 14.1 & ----- & {\bf 14.08} & {\bf 0.36:} & {\bf 0.96} &
----- & ----- & JN-A 1n & \\
& & & & {\bf 14.08} & ----- & {\bf 0.98} & ----- & ----- & BH-A 2n & \\
{\bf 4383-0574} & G --- & ----- & 14.1// & {\bf 14.44} & ----- & {\bf 0.97} &
----- & ----- & Sk 5n & \\
{\bf 4383-0340} & var? & var? & 14.0// & {\bf 14.58} & {\bf $-$0.02} & {\bf 0.52}
& {\bf 0.37} & {\bf 0.75:} & KP 8n & = MR-C \\
& & & & {\bf 14.50} & ----- & {\bf 0.55} & {\bf 0.33} & {\bf 0.67} & WH 20n &
25$"$ SW of SN\\
& & & & {\bf 14.51} & ----- & {\bf 0.63} & {\bf 0.31} & {\bf 0.61} &
PP .. & NOT var.\\
& & & & {\bf 14.51} & ----- & ----- & ----- & ----- & TK 1n & NOT var.\\
\hline\hline
\end{tabular}
\end{center}
{\bf 4383-0384}: original label C on MAA chart was deleted after report of
variability in IAUC 5775. Label C is now applied to GSC 4383-0698, originally
marked C1 on MAA chart.\\
This is a newly-discovered W UMa eclipsing binary with a period
P = 0.53 d, mean V = 11.13, primary minimum at 11.38, secondary at 11.33,
maximum V = 10.99, according to Z.\ Mikulasek and D.\ Hanzl (N.\ Copernicus
Obs., Brno). Announced in IAUC 5775 and IBVS 3879, details and precise
elements will appear in IBVS and in N.\ Copernicus and Planetarium Contrib.\
No.\ 31 (D.\ Hanzl, private communication). The B$-$V is constant and
independent of phase. Radial velocities and additional photometry are needed.
\newpage
\vspace{0.7cm}
\begin{center}
{\bf APPENDIX : THE GSC MAGNITUDES}
\end{center}
Initially, some observers used for the comparison stars the photovisual
magnitudes, m$_{pv}$, listed in the ``Guide Star Catalog'' (GSC).
Unfortunately, these magnitudes have occasionally large errors and are
influenced by the background light of M\,81. Also, they are not in the
V system. According to Lasker {\it et al.} (AJ 99, 2019, 1990) the plates
taken
on Kodak IIa-D emulsion through Wratten 12 filters have an equivalent
wavelength of 0.576 $\mu$m and a bandwith (FWHM)
of 0.114 $\mu$m. The color coefficient of the transformation from V to m
(instrumental) is given as c = dm/d(B$-$V) = $-$0.15, meaning that red stars
appear brighter than in the V system.\\
This coefficient is in fair agreement with the value, c = $-$0.185, calculated
from the isophotal wavelengths of the B, V systems, respectively 0.437 and
0.544 $\mu$m (McFarlane, M., PASP, Feb 1967), and the quoted value for m$_{pv}$.
[The color coefficient is approximately equal to the ratio of
the wave numbers differences, here $(N_{pv} - N_{V})/(N_{B} - N_{V}) = (1.736
- 1.838)/(2.288 - 1.838) = - 0.185.$]\\ \par
It also agrees, within errors, with the color coefficients (of opposite
sign) that may be derived from a comparison of the GSC m$_{pv}$
with the V magnitudes listed in tables 1 and 2. After rejection of several
aberrant stars (GSC 4383-0094, 4383-0308, 4383-0340, 4383-0384, 4383-0565,
4383-0574, 4383-1127), the following transformation was calculated:\\
\hspace{5cm} {\bf V$^{*}$} = {m$_{pv} + (0.42 \pm 0.04) + (0.12 \pm 0.05)
(B-V)$} \hspace{1cm} (1)\\
with a s.d.\ = 0.05 (N = 17 stars).\\
A 2-parameter solution with arguments m$_{pv}$ and (B$-$V):\\
\hspace{6cm} {\bf V$^{*} - m_{pv} = + 0.51 - 0.01m_{pv} + 0.14(B-V)$}
\hspace{1cm} (2)\\
shows that the scale error is negligible and the color term is dominant. \\
The calculated coefficients confirm the GSC value (0.15) which will be adopted
here to reduce the GSC magnitudes to the V scale:\\
\hspace{6cm} {{\bf V$^{*}$} = m$_{pv}$ + 0.40 + 0.15(B$-$V)} \hspace{1cm} (3)\\
The GSC magnitudes of the comparison stars in tables 1 and 2, corrected
via equation (3), are listed in Table 3 where X$-$X$_{0}$, Y$-$Y$_{0}$ are the
differential coordinates from the nucleus of M\,81, and $r$\ the radial distance
(in arcmin).
A plot of the V$-$V$^{*}$ residuals versus $r$\ shows that all stars
(except 4383-0928) within 6$'$ from the center of M\,81
(GSC 4383-0308, 4383-0340, 4383-0565, 4383-0574) are
strongly affected by the galaxy background light and their transformed
magnitudes should be rejected. Beyond 6$'$ all stars (except 4383-0094) have
residuals within $\pm$ 0.1 mag and their corrected magnitudes could be
combined with those in Tables 1 and 2 (except for the best observed local
standards 4383-0340, 4383-0565, 4383-0928).
Because an independent determination of (B$-$V) is required to reduce
m$_{pv}$ to V, the photometric usefulness of the GSC magnitudes is rather
limited when good CCD or photolectric magnitudes and colors are available.
However, because most of the faint telescopic stars in the M\,81 field have
color indices in the range of 0.4 to 1.4 (median: 0.8), an average correction
of $<V^{*} - m_{pv}> = + 0.5 \pm 0.1$ may be used in the absence of color data
(but be aware of background effects and of occasional extreme colors). \\
\newpage
\begin{center}
\begin{tabular}{lrrrrrrl}
\multicolumn{8}{c}{\bf Table 3. GSC magnitudes transformed to V system}\\
\hline\hline
{\bf GSC} & m$_{pv}$ & {\bf V$^{*}$} & {\bf V$-$V$^{*}$} &
X$-$X$_{0}$ & Y$-$Y$_{0}$ & $r$($'$) & {\em Remarks} \\
\hline
4383-0094 & 13.63 & 14.15 & $-$0.23 & 6.37 & 5.13 & 8.18 & \\
4383-0150 & 9.87 & 10.46 & +0.01 & $-$12.00 & $-$1.21 & 12.06 & \\
4383-0224 & 11.17 & 11.77 & +0.08 & 6.40 & 6.14 & 8.87 & \\
4383-0244 & 12.48 & 13.06 & $-$0.07 & 11.18 & 6.90 & 13.18 & \\
4383-0308 & 11.86 & 12.36 & $-$0.58 & $-$4.54 & 1.92 & 4.93 & r$<6'$, rej. \\
4383-0340 & 14.59 & 15.06 & $-$0.57 & $-$0.83 & $-$3.11 & 3.22 & r$<6'$, rej.\\
4383-0384 & 10.85 & 11.32 & ----- & $-$5.81 & 9.40 & 11.05 & var. \\
4383-0434 & 12.00 & 12.49 & $-$0.04 & $-$5.45 & $-$2.52 & 6.00 & \\
4383-0565 & 12.33 & 12.81 & $-$1.41 & 1.09 & $-$2.16 & 2.42 & r$<6'$, rej.\\
4383-0574 & 14.50 & 15.04 & $-$0.60 & $-$3.55 & $-$0.15 & 3.55 & r$<6'$, rej.\\
4383-0633 & 13.30 & 13.79 & $-$0.01 & 5.45 & 3.97 & 6.74 & \\
4383-0698 & 10.37 & 10.93 & $-$0.12 & 2.67 & 14.58 & 14.82 & \\
4383-0738 & 8.67 & 9.23 & $-$0.03 & 7.88 & $-$9.77 & 12.55 & \\
4383-0848 & 7.97 & 8.44 & +0.08 & $-$2.51 & $-$9.86 & 10.17 & \\
4383-0860 & 9.85 & 10.31 & +0.01 & 13.31 & $-$6.43 & 14.78 & \\
4383-0863 & 12.34 & 12.87 & +0.01 & $-$6.62 & $-$1.34 & 6.76 & \\
4383-0928 & 11.42 & 11.89 & +0.02 & 0.77 & $-$3.42 & 3.50 & r$<6'$, OK \\
4383-0935 & 12.38 & 12.89 & 0.00 & 6.60 & 3.57 & 7.50 & \\
4383-1005 & 13.51 & 14.05 & $-$0.02 & 14.22 & 5.11 & 15.11 & \\
4383-1028 & 13.13 & 13.64 & +0.07 & 10.63 & $-$2.38 & 10.89 & \\
4383-1031 & 11.16 & 11.64 & +0.01 & $-$0.54 & $-$12.58 & 12.59 & \\
4383-1037 & 13.53 & 14.07 & +0.01 & $-$1.45 & $-$13.18 & 13.26 & \\
4383-1123 & 13.23 & 13.72 & $-$0.07 & 3.87 & $-$8.47 & 9.31 & \\
\hline\hline
\end{tabular}
\end{center}
\vspace{5mm}
{\em Remarks:}\\
{\bf 4383-0384}: if V$^{*}$ is correct the star was in eclipse, probably
near a primary minimum at the time the plate was taken, 1984 Feb 6, 09:17 UT
= JD 2445736.8868 (Lasker {\it et al.}, AJ 99, 2019, 1990).
\end{document}
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