\documentstyle[twoside, epsf]{article}

\input ibvs2.sty

\begin{document}
\IBVShead{6076}{17 September 2013}

\IBVStitletl{Simultaneous multicolour photometry of late-type}{ giant stars}


\IBVSauth{KURATOV, K.~S.$^1$; MIROSHNICHENKO, A.~S.$^2$; ZAKHOZHAY, V.~A.$^3$; GORSHANOV, D.L.$^4$}

\IBVSinst{Fesenkov Astrophysical Institute, Kamenskoe plato, Almaty 050020, Kazakhstan, \newline 
e-mail: kenes$\_$kuratov@mail.ru}

\IBVSinst{Department of Physics and Astronomy, University of North Carolina at Greensboro, Greensboro, NC 27402, USA, 
e-mail: a$\_$mirosh@uncg.edu}

\IBVSinst{V.~N. Karazin Kharkiv National University, 4 Svobody Sq., 310022 Kharkov, Ukraine, \newline 
e-mail: zkhvladimir@mail.ru}

\IBVSinst{Central Astronomical Observatory of the Russian Academy of Sciences, Pulkovskoe chausse 65/1, Saint-Petersburg, 196140, Russia}

\SIMBADobj{EP Aqr}
\SIMBADobj{TW Peg}
\SIMBADobj{S Cep}
\SIMBADobj{S Per}
\SIMBADobj{R Cnc}
\SIMBADobj{R UMa}
\SIMBADobj{VY UMa}
\SIMBADobj{CS Dra}
\SIMBADobj{AZ UMa}
\SIMBADobj{RY Dra}
\SIMBADobj{Y CVn}
\SIMBADobj{V CVn}
\SIMBADobj{RZ UMa}
\SIMBADobj{RZ Peg}
\SIMBADobj{RV Peg}
\SIMBADobj{U Cyg}
\SIMBADobj{V CrB}

\IBVStyp{  } \IBVSkey{photometry}

\IBVSabs{A set of 64 simultaneous optical and near-infrared photometric observations} 
\IBVSabs{of 17 late-type giants in the Johnson $UBVRIJHK$ system obtained in 1995--1999} 
\IBVSabs{is presented for the first time.}

\begintext

Late-type giant stars are post-main-sequence objects undergoing a
relatively fast evolution of their interior structure (e.g.,
dredge-ups, thermal pulses) that causes multiwavelength variations
of their brightness. Simultaneous photometric observations in wide
wavelength ranges important to study the behaviour of the objects are
still rare. Here we report the results of an observing programme
that included 17 objects (7 carbon stars, 7 M--type giants, and 3
Mira variables) which have never been published, except for a short
presentation at a carbon star conference (Miroshnichenko et al.,
2000). The programme objects were selected from a list of IRAS
sources studied by Ivezi\'c \& Elitzur (1995).

The $UBVRIJHK$ observations in the Johnson photometric system were
obtained between August 1995 and March 1999 at a 1--meter telescope
of the Tien-Shan Observatory of the Fesenkov Astrophysical Institute
(Kazakhstan) with a two--channel photometer--polarimeter of the
Pulkovo Observatory (Bergner et al., 1988). The results are
presented in Table 1. The typical duration of an eight filter
observation was $\sim$20 minutes. Each object was observed with one
$UBVRI$ and one $JHK$ standard star. The photometric data of standard stars
shown in Table 2 was taken from Johnson et al. (1966) and Kornilov
et al. (1991). A few missing colour-indices (e.g., $R-I$ and $J-H$)
were derived by us. Observations of multiple standard stars every
night ensured accurate atmospheric extinction determination and
control of the detector's stability.

Transformations between the instrumental and standard photometric
systems were derived by observing groups of standard stars every
several months and found stable over long time (years). They depend
on the spectral sensitivity of the detectors, that changed
from time to time. The transformations for the detectors used in
1980's were published in Bergner et al. (1988). Those derived during
the time of reported observations are as follows: $\Delta(U-B) =
(0.958\pm0.008)\, \Delta(u-b)$, $\Delta(B-V) = (0.983\pm0.007)\,
\Delta(b-v)$, $\Delta V = \Delta v + (0.077\pm0.012)\,\Delta(b-v)$,
$\Delta R = \Delta r - (0.47\pm0.02)\,\Delta(r-i)$, $\Delta(R-I) =
(0.90\pm0.02)\, \Delta(r-i)$, $\Delta(J-H) = (0.82\pm0.02)\,
\Delta(j-h)$, $\Delta(H-K) = (0.99\pm0.02)\, \Delta(h-k)$, and
$\Delta K = \Delta k + (0.02\,\pm0.02)\,\Delta(h-k)$. Capital
letters refer to the standard system, and lower case letters refer
to the instrumental magnitudes and colour-indices free of atmospheric
extinction. The $\Delta$ notation refers to the magnitude and
colour-index differences between variables and comparison stars.

The photometer was designed to use two single-element detectors (a
GaAs photomultiplier for the optical range and a PbS photoresistor
for the near-IR range) simultaneously to collect the star light and
subtract the sky background. It was ideal for observing objects with
a very red continuum or strong IR excesses. Numerous results on a
wide variety of objects ranging from pre-main-sequence stars to
those at advanced evolutionary stages obtained with this device in
1984--2002 have been published in many papers. Some examples include
multicolour photometry of VV Cep stars (Miroshnichenko \& Ivanov,
1993), objects with the B[e] phenomenon (Bergner et al., 1995), the
newly discovered Mira V1137 Aql (Miroshnichenko, 2001), the LBV
candidate MWC\,930 (Miroshnichenko et al., 2005), and the Be binary
$\delta$ Scorpii (Carciofi et al., 2006).

The intent of this paper is to report the data which can be useful
for constructing more detailed light curves of the objects, analyzing
their spectral energy distributions, modeling their dusty envelopes,
etc. These data may be important because all the objects are very
bright in the near-IR region and therefore saturate most modern
detectors, including those of actively used all-sky surveys (2MASS,
DENIS, etc.). \vskip 5mm

\centerline{Table 1. Photometric data}
\begin{center}
\begin{tabular}{r@{\hskip2mm}c@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}rrrrr}
\hline \noalign{\smallskip}
Star  &JD$-$2400000  & $U-B$   & $B-V$ & $V$   & $V-R$ & $R-I$ & $J$     & $H$     & $K$     \\
\noalign{\smallskip} \hline \noalign{\smallskip}
EP Aqr& 49939.28 & 0.65    & 1.68  & 6.48  & 3.24  & 1.82  & $-$0.28 & $-$1.06 & $-$1.44 \\
EP Aqr& 49943.34 & 0.59    & 1.76  & 6.53  & 3.07  & 1.99  & $-$0.29 & $-$1.05 & $-$1.44 \\
R Cnc & 50093.35 & $-$0.29 & 1.80  & 7.93  & 3.56  & 2.33  &    0.37 & $-$0.49 & $-$0.94 \\
R Cnc & 50105.32 & $-$0.31 & 1.84  & 8.22  & 3.48  & 2.36  &    0.39 & $-$0.44 & $-$0.87 \\
R Cnc & 50415.48 & $-$0.03 & 1.78  & 7.98  & 3.39  & 2.25  &    0.69 & $-$0.04 & $-$0.51 \\
R Cnc & 50416.48 &    0.00 & 1.74  & 8.03  & 3.37  & 2.34  &    0.68 & $-$0.05 & $-$0.47 \\
R Cnc & 50417.47 &    0.00 & 1.75  & 7.99  & 3.32  & 2.29  &    0.58 & $-$0.15 & $-$0.52 \\
R Cnc & 50419.45 &    0.01 & 1.74  & 8.04  & 3.36  & 2.18  &    0.68 & $-$0.06 & $-$0.51 \\
R Cnc & 50422.43 &    0.00 & 1.77  & 8.07  & 3.29  & 2.12  &    0.66 & $-$0.10 & $-$0.52 \\
R Cnc & 50423.44 & $-$0.07 & 1.72  & 8.15  & 3.46  & 2.29  &    0.65 & $-$0.08 & $-$0.60 \\
R Cnc & 50424.44 & $-$0.04 & 1.79  & 8.09  & 3.37  & 2.27  &    0.65 & $-$0.15 & $-$0.53 \\
R Cnc & 50429.43 & $-$0.10 & 1.80  & 8.22  & 3.49  & 2.40  &    0.58 & $-$0.21 & $-$0.62 \\
R Cnc & 50433.40 & $-$0.11 & 1.75  & 8.32  & 3.41  & 2.29  &    0.67 & $-$0.01 & $-$0.53 \\
R Cnc & 50439.39 & $-$0.13 & 1.76  & 8.44  & 3.45  & 2.28  &    0.58 & $-$0.18 & $-$0.61 \\
R Cnc & 50538.16 & $-$0.08 & 1.74  &10.99  & 4.47  & 3.13  &    1.03 &    0.20 & $-$0.47 \\
R Cnc & 51153.41 & $-$0.11 & 1.64  & 7.74  & 3.56  & 2.24  & $-$     & $-$     & $-$     \\
Y CVn & 50101.51 &    5.32 & 3.28  & 5.50  & 2.04  & 1.35  &    1.17 &    0.14 & $-$0.61 \\
Y CVn & 50538.39 &    $-$  & 3.25  & 5.15  & 1.95  & 1.28  &    0.87 & $-$0.05 & $-$0.66 \\
Y CVn & 50540.34 &    $-$  & 3.20  & 5.30  & 1.95  & 1.27  &    0.90 & $-$0.02 & $-$0.70 \\
V CVn & 50540.38 &    1.13 & 1.81  & 7.97  & 2.64  & 1.86  &    2.21 &    1.41 &    1.10 \\
S Cep & 49940.44 & $-$     & 6.17$^{\rm a}$  & 9.44$^{\rm b}$  & 3.16$^{\rm b}$  & 1.75  &    2.54 & 1.23    & $-$0.01 \\
S Cep & 49944.36 & $-$     & 5.71  & 9.34  & 3.10  & 1.68  &    2.51 & 1.24    & $-$0.04 \\
S Cep & 50342.29 & $-$     & $-$   & $-$   & $-$   & $-$   &    2.99 & 1.83    &    0.64 \\
V CrB & 50540.41 &    $-$  & 3.77  & 7.85  & 1.89  & 1.25  &    3.29 &    2.32 &    1.47 \\
V CrB & 51246.45 &    $-$  & 4.64  & 8.76  & 2.22  & 1.29  &    3.67 &    2.64 &    1.69 \\
\noalign{\smallskip} \hline
\end{tabular}
\end{center}
\newpage

\centerline{Table 1. Photometric data (continued)} 
\begin{center}
\begin{tabular}{r@{\hskip2mm}c@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}rrrrr}
\hline \noalign{\smallskip}
Star  &JD$-$2400000& $U-B$   & $B-V$ & $V$   & $V-R$ & $V-I$ & $J$     & $H$     & $K$     \\
\noalign{\smallskip} \hline \noalign{\smallskip}
U Cyg & 50428.03 &    $-$  & 5.26  & 8.87  & 2.83  & 1.61  &    2.81 &    2.04 &    1.26 \\
U Cyg & 50433.03 &    $-$  & 5.29  & 8.58  & 2.66  & 1.69  &    2.75 &    1.94 &    1.20 \\
RY Dra& 50101.54 &    $-$  & 3.64  & 6.94  & 2.11  & 1.60  &    2.01 &    1.29 &    0.46 \\
RY Dra& 50107.46 &    4.42 & 3.72  & 6.92  & 2.17  & 1.43  &    2.00 &    1.28 &    0.44 \\
RY Dra& 50538.36 &    4.81 & 4.00  & 6.51  & 2.09  & 1.30  &    1.80 &    1.06 &    0.23 \\
CS Dra& 50093.49 &    0.49 & 2.02  &10.73  & 3.80  & 2.77  &    2.09 &    1.18 &    0.72 \\
CS Dra& 50538.27 &    0.70 & 1.99  &10.52  & 3.61  & 2.47  &    2.13 &    1.12 &    0.73 \\
CS Dra& 50540.31 &    0.28 & 1.75  &10.75  & 3.46  & 2.47  &    2.36 &    1.45 &    0.92 \\
RV Peg& 50673.36 &$-$0.03  & 1.97  &11.72  & 4.19  & 2.58  &    3.03 &    2.30 &    1.86 \\
RV Peg& 50674.37 &$-$0.09  & 1.92  &11.71  & 4.15  & 2.54  &    3.06 &    2.32 &    1.82 \\
RV Peg& 50677.35 &$-$      & 1.87  &11.74  & 4.28  & 2.58  &    3.05 &    2.22 &    1.83 \\
RZ Peg& 50424.03 &    $-$  & 4.29  & 9.78  & 2.27  & 1.40  &    4.36 &    3.45 &    2.88 \\
RZ Peg& 50427.03 &    $-$  & 4.52$^{\rm c}$  & 9.63  & 2.13  & 1.39  &    4.40 &    3.44 &    2.82 \\
RZ Peg& 50429.04 &    $-$  & $-$   & $-$   & $-$   & $-$   &    4.40 &    3.47 &    2.89 \\
RZ Peg& 50439.03 &    $-$  & 4.17  & 9.34  & 2.16  & 1.28  &    4.36 &    3.53 &    2.83 \\
TW Peg& 49940.39 & 1.24    & 1.68  & 7.24  & 2.89  & 2.29  &    0.61 & $-$0.13 & $-$0.51 \\
TW Peg& 49942.39 & 1.23    & 1.76  & 7.16  & 2.85  & 2.41  &    0.63 & $-$0.12 & $-$0.52 \\
TW Peg& 49944.32 & 1.24    & 1.48  & 7.35  & 2.94  & 2.17  &    0.58 & $-$0.12 & $-$     \\
S Per & 50093.14 & $-$     & 2.73  &11.11  & 4.07  & 2.58  &    2.87 & 1.87    &    1.24 \\
S Per & 50353.45 & $-$     & 2.68  &11.90  & 3.99  & 2.17  &    3.46 & 2.42    &    1.65 \\
R UMa & 50093.43 &    0.74 & 1.29  & 7.99  & 2.58  & 2.19  &    2.50 &    1.79 &    1.30 \\
R UMa & 50097.39 &    0.69 & 1.32  & 7.93  & 2.62  & 2.10  &    2.43 &    1.69 &    1.27 \\
R UMa & 50107.44 &    0.58 & 1.27  & 8.19  & 2.74  & 2.27  &    2.34 &    1.62 &    1.15 \\
R UMa & 50538.25 &    0.46 & 1.92  &11.97  & 4.13  & 2.71  &    2.70 &    1.89 &    1.44 \\
R UMa & 50540.27 &    0.26 & 2.08  &11.86  & 4.03  & 2.71  &    2.62 &    1.94 &    1.45 \\
R UMa & 51246.29 &    0.61 & 1.57  &10.74  & 3.74  & 2.52  &    3.06 &    2.34 &    1.76 \\
RZ UMa& 50419.48 &    0.76 & 1.80  & 9.46  & 3.36  & 2.16  &    2.09 &    1.42 &    1.09 \\
RZ UMa& 50422.48 &    0.68 & 1.98  & 9.38  & 3.08  & 1.98  &    2.07 &    1.35 &    1.03 \\
RZ UMa& 50423.48 &    0.76 & 1.78  & 9.54  & 3.45  & 2.24  &    2.11 &    1.32 &    1.00 \\
RZ UMa& 51160.43 &    0.88 & 1.82  & 8.89  & 3.15  & 2.12  & $-$     & $-$     & $-$     \\
VY UMa& 50093.46 &    4.63 & 2.59  & 6.06  & 1.62  & 1.34  &    2.15 &    1.18 &    0.64 \\
VY UMa& 50097.41 &    4.56 & 2.61  & 6.03  & 1.66  & 1.25  &    2.11 &    1.19 &    0.66 \\
VY UMa& 50101.46 &    4.65 & 2.56  & 6.08  & 1.64  & 1.30  &    2.13 &    1.15 &    0.62 \\
VY UMa& 50107.42 &    4.83 & 2.58  & 6.11  & 1.64  & 1.32  &    2.12 &    1.17 &    0.64 \\
VY UMa& 50538.22 &    4.79 & 2.60  & 6.14  & 1.65  & 1.24  &    1.98 &    1.12 &    0.64 \\
VY UMa& 50540.29 &    4.96 & 2.69  & 6.08  & 1.67  & 1.25  &    1.92 &    1.04 &    0.52 \\
VY UMa& 51246.29 &    4.81 & 2.63  & 6.15  & 1.68  & 1.32  &    2.12 &    1.14 &    0.65 \\
AZ UMa& 50097.48 &    0.93 & 1.72  & 8.72  & 3.12  & 2.00  &    2.09 &    1.23 &    0.84 \\
AZ UMa& 50538.30 &    0.90 & 1.52  & 8.64  & 3.04  & 2.02  &    2.01 &    1.20 &    0.82 \\
\noalign{\smallskip} \hline
\end{tabular}
\begin{list}{}
\item The typical uncertainties (including those of transformation from the
instrumental to the standard photometric system) are as follows:
$0\fmm02$ in $V$, $B-V$, $J$, $H$, and $K$; $0\fmm04$ in $V-R$ and
$R-I$; $0\fmm02$ in $U-B$ for $U \le$ 12\fmm5; $0\fmm04$ in $U-B$
for fainter $U$--magnitudes.\\
\item Larger uncertainties for specific cases are marked with letters:
$^{\rm a}$ $0\fmm08$, $^{\rm b}$ $0\fmm05$, $^{\rm c}$ $0\fmm04$.
\vskip 1cm
\end{list}
\end{center}

\vskip 1cm

\centerline{Table 2. Data on comparison stars} \vskip 3mm
\begin{center}
\begin{tabular}{r@{\hskip2mm}l@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}l@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}r@{\hskip2mm}}
\hline \noalign{\smallskip}
Var. & Vis. comp & $U-B$ & $B-V$ & $V$   & $V-R$ & $R-I$& IR comp & $J$  & $H$     & $K$    \\
\noalign{\smallskip} \hline \noalign{\smallskip}
EP Aqr& HD 207435& 0.83  & 1.01  & 6.67  & 0.75  & 0.32 & BS 8414 & 1.47  & 1.09   & 0.97     \\
R Cnc & HD 68425 & 1.75  & 1.55  & 7.65  & 1.02  & 0.90 & BS 3249 & 1.08  & 0.28   & 0.15     \\
V CVn & HD 116172& 0.47  & 0.93  & 6.98  & 0.71  & 0.47 & BS 4997 & 3.12  & 2.76   & 2.66     \\
Y CVn & HD 110835& 1.52  & 1.37  & 6.96  & 0.71  & 0.70 & BS 4785 & 3.23  & 2.88   & 2.84     \\
S Cep & HD 209111& 1.57  & 1.54  & 6.53  & 1.83  & 1.60 & BS 8347 & 2.62  & 1.90   & 1.70     \\
V CrB & HD 140086& 1.53  & 1.56  & 6.92  & 1.18  & 0.90 & BS 5901 & 3.09  & 2.58   & 2.49     \\
U Cyg & HD 194193& 1.98  & 1.65  & 5.94  & 1.28  & 0.85 & BS 7796 & 1.16  & 0.87   & 0.75     \\
RY Dra& HD 112640& 1.65  & 1.45  & 6.55  & 1.00  & 0.65 & BS 4928 & 3.08  & 2.47   & 2.35     \\
CS Dra& HD 97619 & 1.46  & 1.34  & 6.90  & 0.96  & 0.65 & BS 4301 & 0.05  & $-$0.55& $-$0.65  \\
TW Peg& HD 212750& 1.06  & 1.14  & 7.13  & 0.86  & 0.54 & BS 8430 & 2.98  & 2.78   & 2.67     \\
S Per & HD 13403 & 0.11  & 0.66  & 7.02  & 0.55  & 0.24 & BS 799  & 3.34  & 3.07   & 2.98     \\
RZ UMa& HD 66823 & 1.94  & 1.59  & 7.37  & 1.23  & 0.95 & BS 3323 & 1.98  & 1.49   & 1.44     \\
AZ UMa& HD 101853& 0.73  & 0.97  & 6.73  & 1.02  & 0.90 & BS 4518 & 1.72  & 1.08   & 0.95     \\
\noalign{\smallskip} \hline
\end{tabular}
\begin{list}{}
\item Comparison stars for R UMa and VY UMa were the same as for CS
Dra.\\
Comparison stars for RZ Peg and RV Peg were the same as for TW Peg .
\vskip 1cm
\end{list}
\end{center}

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\end{document}
