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\input ibvs2.sty

\begin{document}

\IBVShead{5165}{5 September 2001}

\IBVStitletl{Lost Harvard Variables in Sagittarius, Scutum, and}{ Scorpius Recovered on Nantucket and Moscow plates}

\IBVSauth{Samus, N.$^{1,2,3}$; Baranov, A.$^4$; Weirich, J.$^{5,3}$}

\IBVSinst{Institute of Astronomy, Russian Academy of Sciences,
48, Pyatnitskaya Str., Moscow 109017, Russia\\ \indent [samus@sai.msu.ru]} %email


\IBVSinst{Sternberg Astronomical Institute, Moscow University,
13, Universitetskii Ave., Moscow 119899, Russia}

\IBVSinst{Maria Mitchell Observatory, 3, Vestal Str., Nantucket, MA 02554, USA}

\IBVSinst{Moscow Astronomy Club (c/o Sternberg Astronomical Institute, Moscow
University, 13, Universitetskii\\ \indent Ave., Moscow 119899, Russia)}

\IBVSinst{University of Missouri-Rolla, 1870, Miner Circle, Rolla,
MO 65409-1060, USA [jweirich@umr.edu]} %email


\SIMBADobj{AB Sgr}
\SIMBADobj{BF Sgr}
\SIMBADobj{CN Sgr}
\SIMBADobj{AM Sco}
\SIMBADobj{AO Sco}
\SIMBADobj{AQ Sco}
\SIMBADobj{AS Sco}
\SIMBADobj{TU Sct}
\SIMBADobj{UV Sct}
\SIMBADobj{AM Sct}

\IBVSkey{coordinates}

\IBVSabs{For 10 ``lost'' Harvard variables recovered on Nantucket and Moscow}
\IBVSabs{plates, we present accurate coordinates, corrected types, light elements.}


\begintext

For the reasons discussed by Hazen \& Samus (1999), it is important to
recover variables lacking finding charts. This problem can be most
effectively solved using the Harvard plate collection, especially
because many stars with no finding charts ever published were first
discovered at Harvard Observatory. However, much can be done using
plate collections of other observatories. For several years, we
successfully use the plate collection of the Maria Mitchell Observatory
(MMO) to recover ``lost'' variables. The results of 1998 were presented
in Tam \&  Samus (2000); those of 1999, in Samus et al.\ (1999); those
of 2000, in Samus et al.\ (2001).  Plates of the Moscow collection are
also being used for this purpose for many years.

In 2001 we have successfully recovered 10 ``lost'' Harvard variable
stars on Nantucket and Moscow plates. The main results are presented in
Tables 1 and 2. The columns of Table 1 contain: GCVS name; preliminary
Harvard designation (HV -- Harvard Variable); GSC number (if
available); the star's right ascension and declination (equinox
2000.0); source of coordinates (A2.0 means the US Naval Observatory
A2.0 catalog, Monet et al.\ 1998; DSS means coordinates measured by us
on a DSS image, relative to several reference stars with coordinates
from the USNO A2.0 catalog).  For the two stars lacking GSC or USNO
A2.0 catalog identifications, we present finding charts based on DSS
images.  The columns of Table 2 contain: GCVS name; the star's type
found in our study; light elements (epoch and period) if they could be
derived from our data (epochs refer to minimum light for the probable
eclipsing variable and to maximum light for pulsating variables).
Remarks on individual stars follow the Tables.

Thanks are due to Vladimir Strelnitski for his help and attention
during the Nantucket part of this investigation. We are grateful to
Sergei Antipin for his assistance during the preparation of the
manuscript.  This study was supported, in part, by grants from the
NSF/REU (AST-0097694) and from Russian Foundation for Basic Research
(99-02-16333).

\begin{table}
\caption{Identifications and coordinates}
\begin{center}
\begin{tabular}{llllll}
\hline
Name & HV & GSC & $\alpha_{2000.0}$ & $\delta_{2000.0}$ & Source\\
\hline
AB Sgr & 3649 &            & 19\hr01\mm54\fsec75 & $-$12\deg56\arcm09\farcs7 & A2.0\\
BF Sgr & 3652 &            & 19 04 56.35 & $-$11 58 50.1 & A2.0\\
CN Sgr & 3758 &            & 19 02 53.30 & $-$13 11 46.3 & DSS \\
AM Sco & 1014 &            & 16 07 08.55 & $-$23 40 11.3 & A2.0\\
AO Sco & 1052 & 6213.0567  & 16 15 02.38 & $-$21 45 27.6 & GSC \\
AQ Sco & 1061 & 6794.0110  & 16 20 34.67 & $-$23 14 33.4 & GSC \\
AS Sco & 1065 &            & 16 22 36.12 & $-$20 58 32.3 & A2.0\\
TU Sct & 3645 &            & 18 57 44.92 & $-$12 55 26.5 & A2.0\\
UV Sct & 3642 & 5714.0420  & 18 55 23.80 & $-$12 46 56.6 & GSC \\
AM Sct & 3830 &            & 18 52 02.50 & $-$08 31 17.8 & DSS \\
\hline
\end{tabular}
\end{center}

\caption{Types and light elements}
\begin{center}
\begin{tabular}{llll}
\hline
\lower6pt\hbox{Name} & \lower6pt\hbox{Type \& epoch} & JD & \lower6pt\hbox{Period}\\[-3pt]
     &      & 24\dots\\
\hline
AB Sgr & SR  & 44491     & 260\day:\\
BF Sgr & SR: & 29430\\
CN Sgr & M   & 44817     & 276\fday4     \\
AM Sco & IS:\\
AO Sco & EB: & 40000.44  &         \\
AQ Sco & RRAB & 40706.48  & \phantom{00}0\fday482367\\
AS Sco &  ?                   \\
TU Sct & SRA & 43016     & 128\fday6    \\
UV Sct & SR  & 42979     & 102\day\\
AM Sct & M:  & 48082     & 435\fday3\\
\hline
\end{tabular}
\end{center}
\end{table}

\clearpage

\leftline{\bf Notes on individual stars}
\medskip

{\bf AB Sgr} Twelve maxima or brightenings (Table 3) were
observed on Nantucket plates. Their presentation with the period in Table 2
is not quite satisfactory, the star may belong to SRB variables.

\begin{table}[h]
\caption{Maxima and brightenings of AB Sgr}
\begin{center}
\begin{tabular}{lll}
\hline
Max JD 24\dots & Max JD 24\dots & Max JD 24\dots\\
\hline
25436::  &  29435:  &  42930: \\
26206::  &  29908   &  44491  \\
28020    &  33593:: &  48151: \\
28257::  &  35690:  &  48460::\\
\hline
\end{tabular}
\end{center}
\end{table}

{\bf BF Sgr} The star is double, the northern component of the pair varies. Its
position, measured using DSS images, confirms the identification with the
single A2.0 catalog object present in this region of the sky. The star is just
outside the error ellipse of IRAS PSC 19021--1203 but nevertheless the
IRAS object can be a correct identification. The maximum in Table 2 is based
on two Nantucket plates; the star was faint on JD 2428400.

{\bf CN Sgr} The period in Table 2 is from Harwood (1930). On Nantucket plates,
the star was found bright on JD 2444817 and faint on JD 2445231.

{\bf AM Sco} Leavitt (1904) considered the star a possible Mira-type
variable. It is in the error ellipse of IRAS PSC 16041--2332. Nevertheless,
the star is not red in the A2.0 catalog ($b-r=1.2$) and does not seem red
on DSS images. Moscow plates show strong brightness variations within
several days. No reliable period value could be found.

{\bf AO Sco} A period value of 9\fday42669 is possible from our limited
data, based on 45 Moscow plates.

{\bf AQ Sco} The star was initially thought to be a slow variable
(Leavitt, 1904), then a possible Orion variable (Himpel, 1944).
We now suggest to reclassify it again as an RRab star. The preliminary light elements of
Table 2 were found from 48 observations on Moscow plates (JD 2437074--2447347).

{\bf AS Sco} Our data (based on Moscow plates)
are not sufficient to classify this star, suspected
by Leavitt (1904) to be a short-period variable.

{\bf TU Sct} The new elements (Table 2) satisfactorily represent epochs
of 22 maxima (JD 2414210--2445231, many of them uncertain) found using
Nantucket plates (18 maxima or brightenings in Table 4) or available in the
literature (Harwood, 1962; 9 maxima, 5 of them also represented in our
observations).

\begin{table}[h]
\caption{Maxima and brightenings of TU Sct}
\begin{center}
\begin{tabular}{lll}
\hline
Max JD 24\dots & Max JD 24\dots & Max JD 24\dots\\
\hline
25143    &  27980:  &  32729: \\
25414:   &  28370:  &  33510: \\
26163:   &  29523:  &  33765: \\
26587:   &  29813   &  33900  \\
27361:   &  29930   &  43016  \\
27693    &  32082:  &  45231: \\
\hline
\end{tabular}
\end{center}
\end{table}

{\bf UV Sct} This is IRAS PSC 18525--1250. The period in Table 2 is from
Harwood (1962); the maximum was derived from 8 Nantucket plates. The star
was also bright on JD 2433186 and faint on JD 2433100.

{\bf AM Sct} The new light elements (Table 2) represent 7 epochs of
maxima found on Moscow plates (Table 5) and do not contradict
the two old approximate epochs available in the literature (Cannon, 1924).

\begin{table}[h]
\caption{Maxima of AM Sct}
\begin{center}
\begin{tabular}{lll}
\hline
Max JD 24\dots & Max JD 24\dots & Max JD 24\dots\\
\hline
32848    &  39342+  &  48096  \\
37198    &  41160$-$\\
38968    &  41566+\\
\hline
\end{tabular}
\end{center}
\end{table}

\IBVSfig{7cm}{5165-f1.ps}{The finding charts for CN Sgr (left) and AM Sct
(right), from red-light images of the second Digitized Sky Survey. The side
of each chart is $2'$}

\IBVSefigure{5165-f1a.ps}
\IBVSefigure{5165-f1b.ps}

\references

Cannon, A.J., 1924, {\it Harvard Obs.\ Circ.}, No.\ 265

Harwood, M., 1930, {\it Harvard Obs.\ Bull.}, No.\ 880, 10
% Original Harwood, M., 1931, {\it Harvard Obs.\ Bull.}, No.\ 880, 22
%Error corrected Mon Aug 16 16:02:44 MEST 2004
\IBVSecomment{Error corrected Aug 16 2004}

Harwood, M., 1962, {\it Leiden Obs.\ Ann.}, {\bf 21}, No.\ 8, 387

Hazen, M.L., \&  Samus, N., 1999, {\it IBVS}, No.\ 4665

Himpel, K., 1944, {\it Beobachtungs-Zirkular der AN}, No.\ 26, 25

Leavitt, H., 1904, {\it Harvard Obs.\ Circ.}, No.\ 90

Monet, D., Bird, A., Canzian, B., et al., 1998, USNO A V2.0. A Catalog of
Astrometric Standards, US Naval Observatory (11 CD-ROMs)

Samus, N.N., Haythe, L., Hornstein, S., Jisonna Jr., L.J., Lu, E., 1999,
{\it IBVS}, No.\ 4773

Samus, N., Peterson, C., Holmes, S., \&  Singer, K., 2001, {\it Journal of the
AAVSO}, {\bf 29}, 112

Tam, F., \&  Samus, N., 2000, {\it Journal of the AAVSO}, {\bf 28}, 94

\end{document}
