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\begin{document}

\IBVShead{5457}{9 October 2003}

\IBVStitletl{Confirmation of Variability of Bidelman-MacConnell}{ Suspected Variables}

\IBVSauth{Wils, P.}
\IBVSinsto{Vereniging Voor Sterrenkunde, Belgium; e-mail: patrick.wils@cronos.be}

\IBVSkey{Variable stars - photometry}
\IBVSabs{Precise positions are given for the NSV stars originating from}
\IBVSabs{a paper by Bidelman and MacConnell (1973).}
\IBVSabs{Variability is confirmed and type and period are given for a number}
\IBVSabs{of these stars, base on ASAS3 and TASS survey data.}

\begintext

Bidelman and MacConnell (1973, hereafter BM) gave a number of lists of remarkable 
southern hemisphere stars, among which a list of 311 stars, selected on the 
presence of $H\gamma$ or $H\delta$ emission lines in their spectrum
on top of an M type continuum.  A large number
of these stars were known or have been found to be Mira or semi-regular variables.
The remaining 60 stars from the list (6 of which were suspected in variability by other sources
as well) were catalogued in the NSV, as suspected Mira variables.
Positions were given with an accuracy of $0\fmm1$ in RA and $1\arcm$ in declination.
Most of the known variable stars were found within 4\arcm\ radius, though three had large 
errors of up to $1\deg$ due to typographical errors.

This study will give more accurate positions for the NSV stars from the BM paper.  Identifications were
made based on either the presence of an IRAS source or a bright red star in the 2MASS
survey ($J < 9$, $J-K_s > 1$), and in addition, on the variability shown by the publicly available 
data of the 
ASAS3 (Pojmanski, 2002) and the TASS (Richmond et al., 2000; Droege, 2003) surveys.
The latter could only be used for stars near the equator.

In some cases, no obvious identification could be made in the close vicinity of
the given positions.  This may be due to a typographical error in the BM paper.

The positively identified variable stars are given in Table~1, while
proposed but less certain identifications, with no candidate within a distance of
$4\arcm$ from the BM position, are given in Table~2.  Probably the only way to
verify the latter will be by the original plates.
The first column of both tables gives the NSV number of the variable star.  
The following columns contain the IRAS identification if present, the position of the star as found from the 2MASS survey,
maximum and minimum $V$ magnitude (derived from the ASAS3 survey), 
the $J-K_s$ colour index (from the 2MASS survey), an epoch of maximum (JD -- 2400000),
the period (in days, found by use of the PDM method, Stellingwerf, 1978) 
and the type of variability as derived from the light curve 
(with ``SR:'' indicating that the star may be either a semi-regular or irregular
variable).  An asterisk in the first column indicates a comment below the table.
Light curves (ASAS3: filled circles, TASS MkIII: asterisks, TASS MkIV: open squares),
links to Simbad, and ASAS3 and TASS identifications are available in the tables of the
electronic version of the IBVS.

\IBVSetable{5457-t3.tex}

Note that the given periods may not be very accurate, as in some cases only (part of) two cycles have been 
observed, and that the minimum magnitude may be fainter, as the minimum itself could not always be observed by ASAS3.


\begin{table}[!ht]
\normalsize
\centerline{\normalsize {\bf Table 1.} Identifications for the BM variables}
\begin{center}
\begin{tabular}{r@{}lcccr@{}lrrr@{}lc}
\hline
\multicolumn{3}{c}{Star name} & \multicolumn{2}{c}{Coordinates (J2000)} & \multicolumn{2}{c}{$V$} & $J$$-$$K_s$ & Epoch & \multicolumn{2}{c}{Period} & Type \\
\multicolumn{2}{c}{NSV } & IRAS & RA & Dec & \multicolumn{2}{c}{[mag]} & [mag] & $-$2400000 & \multicolumn{2}{c}{[day]} &  \\
\hline
 1043 &   &  03038-5229 & 03 05 21.31 & $-$52 18 04.6 & 10.0 & $-$10.9 & 1.31 &       &     &   & SR   \\
 3033 &   &  06325-6333 & 06 32 49.58 & $-$63 35 49.8 & 11.7 & $-$15.7 & 1.26 & 52763 & 201 &   & M    \\
 3245 &   &  $-$          & 06 50 54.86 & $-$37 29 23.0 & 12.4 & $-$15.2 & 1.49 & 52566 & 148 & : & M    \\
 3286 &   &  06534-3603 & 06 55 12.44 & $-$36 07 09.9 & 11.5 & $-$14.2 & 1.24 & 52628 & 286 &   & M    \\
 3513 &   &  07152-3444 & 07 17 05.76 & $-$34 49 39.7 & 11.6 & $-$14.6 & 1.82 & 52745 & 302 &   & M    \\
 3539 &   &  07178-1925 & 07 20 04.06 & $-$19 30 45.3 &  9.5 & $-$10.0 & 1.24 & 52702 & 274 &   & SRA  \\
 3840 &   &  07569-2217 & 07 59 08.97 & $-$22 26 12.3 & 11.5 & $-$13.9 & 1.75 & 52400 & 420 &   & M    \\
 3873 &   &  08003-4838 & 08 01 49.42 & $-$48 46 55.7 & 11.0 & $-$14.5 & 1.41 & 52254 & 317 &   & M    \\
 3966 &   &  08133-0141 & 08 15 52.43 & $-$01 50 49.3 & 12.0 & $-$14.2 & 1.40 & 52390 &     &   & M    \\
 4052 &   &  08211-6047 & 08 22 03.68 & $-$60 57 12.7 & 10.6 & $-$15.0 & 1.34 & 51875 & 206 &   & M    \\
 4082 & * &  08239-0307 & 08 26 26.81 & $-$03 17 43.7 & 10.9 & $-$14.1 & 1.30 & 52776 & 313 &   & M    \\
 4116 &   &  08286-3110 & 08 30 39.15 & $-$31 20 26.3 & 13.3 & $-$14.4 & 1.86 & 52819 &     &   & SR:  \\
 4574 & * &  $-$          & 09 39 46.31 & $-$41 04 03.0 & 10.7 &       & 0.85 &       &     &   & BY:  \\
 4583 & * &  09396-7419 & 09 39 55.10 & $-$74 32 42.6 & 10.3 & $-$14.2 & 1.28 & 52192 & 185 &   & M    \\
 4775 &   &  10092-5733 & 10 11 02.95 & $-$57 48 13.9 &  9.6 & $-$ 9.9 & 1.24 & 51953 &     &   & SR:  \\
 5003 &   &  10508-4121 & 10 53 07.92 & $-$41 37 27.7 & 11.4 & $-$14.8 & 1.43 & 52717 & 188 &   & M    \\
 5271 &   & F11348-5013 & 11 37 17.62 & $-$50 30 23.2 & 10.7 & $-$11.9 & 1.11 & 52411 &  82 &   & SRA  \\
 5273 &   &  11352-4347 & 11 37 43.22 & $-$44 04 31.1 & 10.4 & $-$14.3 & 1.29 & 51906 & 240 &   & M    \\
 5295 &   &  11390-7213 & 11 41 19.52 & $-$72 30 38.5 & 11.0 & $-$14.4 & 1.67 & 52239 & 199 &   & M    \\
 5924 & * &  12428-4723 & 12 45 40.41 & $-$47 40 04.6 & 12.0 & $-$14.8 & 1.31 & 52878 & 270 &   & M    \\
 6040 & * &  12559-4214 & 12 58 44.70 & $-$42 30 42.5 & 10.4 & $-$11.7 & 1.44 & 52820 & 337 &   & M    \\
 6071 &   &  13005-1547 & 13 03 10.64 & $-$16 03 20.3 &  9.5 & $-$15.1 & 1.27 & 51995 & 253 &   & M    \\
 6160 & * &  13131-3644 & 13 16 01.38 & $-$37 00 10.7 & 10.4 & $-$10.9 & 1.23 & 51886 & 101 & : & SR:  \\
 6288 &   &  13285-7556 & 13 32 52.52 & $-$76 12 22.5 & 11.1 & $-$14.0 & 1.23 & 52731 & 166 &   & M    \\
 6400 &   & F13399-4821 & 13 43 01.28 & $-$48 36 21.9 & 11.7 & $-$13.8 & 1.38 & 52724 & 248 & : & M:   \\
 6404 &   &  13408-1734 & 13 43 33.97 & $-$17 49 37.6 &  9.3 & $-$11.1 & 1.38 & 52469 & 200 &   & SRA  \\
 6453 & * &  13464-4611 & 13 49 32.16 & $-$46 26 10.6 & 10.6 & $-$11.4 & 1.62 & 52662 & 347 & : & M:   \\
 6494 &   &  13531-3014 & 13 55 58.21 & $-$30 29 36.0 &  9.6 & $-$10.4 & 1.28 & 52893 &     &   & SRB  \\
 6700 &   &  14303-1042 & 14 32 59.89 & $-$10 56 03.6 & 11.8 & $-$14.9 & 1.54 & 52851 & 380 & : & M    \\
 6856 &   &  14530-2630 & 14 56 01.64 & $-$26 42 38.5 & 12.4 & $-$15.5 & 1.40 & 52393 & 266 &   & M    \\
 6929 &   &  15035-6953 & 15 08 19.97 & $-$70 04 34.8 & 10.9 & $-$14.0 & 1.34 & 52786 & 314 &   & M    \\
 7075 &   & F15236+0042 & 15 26 10.69 & +00 31 56.5 & 10.8 & $-$12.9 & 1.16 & 52765 & 170 &   & SRA  \\
 7190 & * &  15379-6529 & 15 42 25.72 & $-$65 39 08.8 & 10.4 & $-$11.2 & 0.90 & 52713 & 247 &   & SRA  \\
 7458 &   &  16046-2637 & 16 07 42.66 & $-$26 45 08.0 & 11.2 & $-$13.1 & 1.26 & 52761 & 185 &   & M    \\
 7884 &   &  16367-2046 & 16 39 41.39 & $-$20 52 38.8 & 10.3 & $-$11.3 & 1.50 & 52388 & 281 &   & SR   \\
 8761 &   &  $-$          & 17 29 25.10 & $-$51 10 22.8 & 11.2 & $-$14.7 & 1.34 & 52406 & 186 &   & M    \\
 8952 &   &  17273+0132 & 17 29 51.44 & +01 29 46.1 & 10.1 & $-$11.9 & 1.20 & 52473 & 109 &   & SRA  \\
10943 &   &  18285-4439 & 18 32 13.89 & $-$44 37 01.5 & 11.4 & $-$13.5 & 1.54 & 52546 & 320 &   & M    \\
10964 &   &  $-$          & 18 32 09.58 & $-$29 55 46.9 & 11.0 & $-$13.2 & 1.23 & 52025 & 162 &   & M    \\
11320 & * &  18435-4741 & 18 47 20.56 & $-$47 38 05.6 & 10.5 & $-$13.0 & 1.61 & 52122 & 380 &   & M    \\
11330 &   &  $-$          & 18 47 21.78 & $-$31 07 47.6 & 13.3 & $-$15.2 & 1.27 & 52088 & 191 &   & M    \\
11475 &   &  18508-2225 & 18 53 52.84 & $-$22 22 03.9 & 11.8 & $-$14.6 & 1.79 & 52757 & 123 &   & M    \\
12041 & * &  19249-2142 & 19 27 53.58 & $-$21 35 52.6 &      &       & 1.39 &       &     &   & ?    \\
12190 &   &  19335-2841 & 19 36 40.49 & $-$28 35 04.1 & 11.8 & $-$15.1 & 1.45 & 52775 & 377 &   & M    \\
12294 &   &  19390-2853 & 19 42 08.96 & $-$28 46 11.1 & 11.7 & $-$14.7 & 1.30 & 52812 & 216 &   & M    \\
12305 &   &  19395-2213 & 19 42 30.99 & $-$22 06 11.9 & 11.3 & $-$15.0 & 1.44 & 52510 & 278 &   & M    \\
12313 &   &  $-$          & 19 42 25.86 & $-$10 58 18.3 & 10.1 & $-$12.2 & 1.24 & 51996 & 157 &   & SR   \\
12652 &   &  19570-2306 & 19 59 58.04 & $-$22 58 14.7 & 11.3 & $-$15.4 & 1.45 & 52757 & 284 &   & M    \\
13090 &   &  $-$          & 20 27 29.17 & $-$30 48 37.3 & 12.6 & $-$15.0 & 1.34 & 52156 & 230 &   & M    \\
13131 &   &  20302-2350 & 20 33 10.51 & $-$23 40 11.3 & 10.8 & $-$12.6 & 1.40 & 52156 & 242 &   & SRA  \\
13344 &   &  20480-3505 & 20 51 09.04 & $-$34 53 53.3 & 11.1 & $-$15.3 & 1.27 & 52816 & 233 &   & M    \\
14283 & * &  22403-4147 & 22 43 11.54 & $-$41 31 58.3 &  9.9 & $-$14.4 & 1.30 & 52211 & 264 &   & M    \\
\hline
\end{tabular}
\end{center}
\end{table}

\begin{table}[!hb]
\normalsize
\centerline{\normalsize {\bf Table 2.} Suggested identification for some BM variables}
\begin{center}
\begin{tabular}{r@{}lcccr@{}lrrr@{}lc}
\hline
\multicolumn{3}{c}{Star name} & \multicolumn{2}{c}{Coordinates (J2000)} & \multicolumn{2}{c}{$V$} & $J$$-$$K_s$ & Epoch & \multicolumn{2}{c}{Period} & Type \\
\multicolumn{2}{c}{NSV } & IRAS & RA & Dec & \multicolumn{2}{c}{[mag]} & [mag] & $-$2400000 & \multicolumn{2}{c}{[day]} &  \\
\hline
 3357 & * &  $-$          & 07 03 11.05 & $-$24 51 05.7 & 11.8 & $-$12.1 & 1.32 &       &     &   & SR   \\
 3611 & * &  07229-8440 & 07 14 09.41 & $-$84 45 47.0 & 10.8 & $-$14.8 & 1.15 & 52226 & 199 &   & M    \\
 4314 & * &  08536-6239 & 08 54 35.43 & $-$62 50 37.3 & 13.1 & $-$13.8 & 1.45 &       &     &   & SR   \\
 7500 & * &  16077-6628 & 16 12 34.86 & $-$66 36 35.9 & 10.5 & $-$13.0 & 1.29 & 52491 & 259 &   & M    \\
 9654 & * &  17444-5843 & 17 48 53.48 & $-$58 44 43.1 &  8.4 & $-$14.7 & 1.26 & 52142 & 287 &   & M    \\
10851 & * &  18255-1547 & 18 28 26.77 & $-$15 45 17.5 & 10.0 & $-$10.3 & 1.45 & 52755 &  64 &   & SRA  \\
11632 & * &  $-$          & 19 00 35.66 & $-$16 25 22.9 & 11.8 &       & 1.15 &       &     &   & Cst? \\
13567 & * &  21070-4902 & 21 10 31.25 & $-$48 49 59.2 & 11.0 & $-$12.4 & 1.42 & 52761 & 202 &   & SRA  \\
\hline
\end{tabular}
\end{center}
\large
Notes on individual stars:  \\
NSV 3357: $5\arcm$ from BM position \\
NSV 3611: $6\arcm$ from BM position \\
NSV 4082: See also Wils (2003) \\
NSV 4314: $8\arcm$ from BM position \\
NSV 4574 = Gliese 358 = LHS2166 = 1RXS J093945.7-410405: Long wave of 0.1 mag amplitude. \\
NSV 4583 = NSV 4586 = BV 1054.  Large variation between cycles. \\
NSV 4775 = 2RXP J101103.0-574810 ? \\
NSV 5924: Position from Kato (1999) \\
NSV 6040: Component of close double, not separated by ASAS3.  Fairly large range of magnitude at maximum. \\
NSV 6160 = V1044 Cen (ZAnd type) \\
NSV 6453: Component of close double, not separated by ASAS3. \\
NSV 7190: Position from Morel (1994).  The flat bottomed minimum may be an indication for a close companion.  There is however no indication of duplicity on NOFS images, nor in the 2MASS survey. \\
NSV 7500 = TbrV0117 (Tabur, 2003), $6\arcm$ from BM position  \\
NSV 9654 = RZ Pav, $8\arcm$ from BM position  \\
NSV 10851: $8\arcm$ from BM position  \\
NSV 11320 = NSV11324 = BV1449 \\
NSV 11632: $9\arcm$ from BM position , no other obvious candidate present. \\
NSV 12041: Position from Yamaoka (2000).  No ASAS3 data available. \\
NSV 13567 = TbrV0117 (Tabur, 2003), $6\arcm$ from BM position  \\
NSV 14283: Position from Demartino et al. (1996) \\
\end{table}

\clearpage

\IBVSfig{7cm}{5457-f36.eps}{Light curve of NSV 7190 from ASAS3 data (Pojmanski, 2002).}
%%\IBVSfigKey{5457-f36.eps}{NSV 7190}{light curve}


{\bf Acknowledgements:} 
Brian Skiff and John Greaves are gratefully acknowledged for helpful comments and assistance 
with the research.  
The TASS \footnote{\tt http://www.tass-survey.org} and ASAS \footnote{\tt http://archive.princeton.edu/\~{}asas/} teams are acknowledged for providing public access to their archives.
This research has made use of the SIMBAD and VizieR 
databases operated at the {\it Centre de Donn\'ees Astronomiques (Strasbourg)} in France
and the USNOFS Image and Catalogue Archive operated by the United States Naval Observatory, 
Flagstaff Station ({\tt http://www.nofs.navy.mil/data/fchpix/}). 
This publication makes use of data products from the Two Micron All Sky Survey, 
which is a joint project of the University of Massachusetts and the Infrared Processing 
and Analysis Center/California Institute of Technology, funded by the National Aeronautics 
and Space Administration and the National Science Foundation.

\references

Bidelman, W. P., MacConnell, D. J., 1973, {\it AJ}, {\bf 78}, 687

Demartino, R., Kocyla, D., Predom, C., Wetherbee, E., 1996, {\it IBVS}, No.\,4322

Kato, T., 1999, {\it IBVS}, No.\,4799

Morel, M., 1994, {\it IBVS}, No.\,4037

Pojmanski, G., 2000, {\it Acta Astronomica}, {\bf 50}, 177

Pojmanski, G., 2002, {\it Acta Astronomica}, {\bf 52}, 397

Richmond, M. W., Droege, T. F., Gombert, G., Gutzwiller, M., Henden, A. A., Albertson, C., 
  Beser, N., Molhant, N., Johnson, H., 2000, {\it PASP}, {\bf 112}, 397 

Stellingwerf, R. F., 1978, {\it ApJ}, {\bf 224}, 953

Tabur, V., 2003, {\tt http://www.tip.net.au/\~{}vello/varstar2/index.htm}

Yamaoka, H., 2000, \\{\tt http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/Mail/vsnet-id/msg00288.html}

Wils, P., 2003, {\it IBVS}, No.\,5401

\endreferences



\end{document}

