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\IBVShead{4813}{29 November 1999}

\IBVStitle{Revised Astrometry of 33 Variable Stars}

\IBVSauth{Yoshida, S.$^1$; Kadota, K.$^2$; Kato, T.$^3$}

\IBVSinst{MISAO Project, 1065-16 Miyawada Fujishiro-machi Kitasoma-gun Ibaraki 300-1514, Japan,\\ \indent e-mail: seiichi@muraoka.info.waseda.ac.jp}
\IBVSinst{MISAO Project, 77-1-3-12-204 Koshikiya Ageo City Saitama 362-0064, Japan,\\ \indent e-mail: kenic-k@astroarts.co.jp}
\IBVSinst{Dept.\ of Astronomy, Kyoto University, Kyoto 606-8502, Japan, e-mail: tkato@kusastro.kyoto-u.ac.jp}

\IBVSabs{This report describes the revised astrometry and identifications of 33}
\IBVSabs{variable stars discovered in the course of variable star survey based on}
\IBVSabs{the MISAO Project observations.}

\begintext

This report describes the revised astrometry and identifications of 33 variable stars discovered in the course of variable star survey based on the MISAO Project observations.

These objects are detected automatically by the PIXY system as candidates of new variable stars from unfiltered CCD images taken by Kadota between 1999 April and August. Further details are the same as described in Yoshida and Kadota (1999). The system searched the GCVS catalog, NSV catalog, etc., and no identified object were found within 5 arcsecs. But within a larger search area, the following known variable stars are found in the catalogs. We could not find any other variable objects on our images to be identified with the known variable stars at and around the positions. Therefore we judged the positions in the catalogs are inaccurate and our objects must be identified with them.

Table 1 shows the astrometry, photometry and identifications. The positions and magnitudes are measured using USNO-A1.0 catalog. The magnitude is based on a preliminary $V$ magnitude calculated from $R$ and $B$ magnitude in the catalog based on Kato's (1998) equation:
\[
V = R + 0.375 (B - R).
\]

In the revision of the GCVS, AF Aql is identified with USNO-A1.0 0750.16045701. However, USNO-A1.0 0750.16045701 is not detected from our images. In addition, the variable object we found is closer to the position given in the original GCVS\@. Therefore, we determined our object is true AF Aql.

VX Aql is identified with HS 1466, one of the variable stars discovered by FASTT, Flagstaff Astrometric Scanning Transit Telescope (cf.\ Henden et al.\ 1998). V886 Aql is also identified with HS 1463, one of the variable stars discovered by FASTT.

We identified USNO-A1.0 0750.16136750 with HS Aql. But this star is closer to HT Aql. HS Aql is Mira type and HT Aql is probably RR Lyrae type. USNO-A1.0 0750.16136750 is identified with IRAS 18577-0844, therefore, we determined it is proper for Mira-type object.

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\normalsize
Table 1: Revised Astrometry and Identifications
\vskip2mm
\begin{tabular}{cllrrl} \hline
& & & \multicolumn{2}{c}{Unfiltered} \\
Star & \multicolumn{2}{c}{R.A. (J2000.0) Decl.} & \multicolumn{2}{c}{CCD Mag.} & Identified with \\
& & & Max & Min \\
\hline
AF Aql & 18\hr59\mm32\fsec17  & $-$09\deg06\arcm58\farcs5  & 11.2 & 12.6 & \\
AG Aql & 18 59 32.748 & $-$06 08 51.14 & 10.7 & 11.9 & USNO-A1.0 0825.13965291 \\
AN Aql & 19 02 37.897 & $-$09 32 21.03 & 10.8 & 12.7 & GSC 5711.0895 \\
\multicolumn{5}{c}{} & USNO-A1.0 0750.16330736 \\
AO Aql & 19 02 44.043 & $-$06 11 11.51 &  9.9 & 12.0 & GSC 5140.1058 \\
\multicolumn{5}{c}{} & USNO-A1.0 0825.14217142 \\
EU Aql & 18 58 23.761 & +16 46 54.84 &  9.1 & 10.0 & GSC 1585.0882 \\
\multicolumn{5}{c}{} & USNO-A1.0 1050.12635261 \\
HS Aql & 19 00 27.795 & $-$08 40 26.07 & 10.8 & 12.5 & USNO-A1.0 0750.16136750 \\
QQ Aql & 19 02 08.451 & $-$09 04 11.18 & 10.9 & 11.8 & USNO-A1.0 0750.16289091 \\
UX Aql & 19 00 25.162 & $-$11 29 22.69 & 11.7 & 12.9 & USNO-A1.0 0750.16132360 \\
V431 Aql & 20 00 28.283 & +10 47 21.43 & 10.7 & 12.1 & GSC 1075.1268 \\
\multicolumn{5}{c}{} & USNO-A1.0 0975.17767279 \\
V757 Aql & 20 00 19.649 & +09 54 25.11 & 11.5 & 12.5 & GSC 1075.1971 \\
\multicolumn{5}{c}{} & USNO-A1.0 0975.17756839 \\
V759 Aql & 20 00 14.785 & +13 54 58.13 & 10.3 & 12.4 & USNO-A1.0 0975.17750986 \\
V886 Aql & 18 59 11.277 & $-$01 19 09.83 & 10.0 & 11.7 & USNO-A1.0 0825.13934521 \\
V938 Aql & 19 00 32.257 & $-$07 27 54.23 & 10.0 & 12.3 & USNO-A1.0 0825.14049433 \\
VX Aql & 19 00 09.508 & $-$01 34 56.99 &  8.3 &  9.2 & GSC 5128.0947 \\
\multicolumn{5}{c}{} & USNO-A1.0 0825.14018550 \\
DI Cyg & 21 02 26.024 & +30 55 23.05 &  9.2 & 10.8 & GSC 2701.1892 \\
\multicolumn{5}{c}{} & USNO-A1.0 1200.17132208 \\
DN Cyg & 21 58 15.41  & +52 02 12.5  & 11.6 & 12.4 & \\
KM Cyg & 20 00 13.42  & +36 08 45.8  & 10.3 & 11.5 & \\
V419 Cyg & 20 02 29.75  & +38 35 18.6  & 11.8 & 14.1 & \\
V739 Cyg & 19 58 23.811 & +37 15 52.19 & 13.5 & 14.9 & USNO-A2.0 1200.14007663 \\
V1463 Cyg & 19 57 43.163 & +36 05 44.16 & 12.7 & 13.8 & USNO-A1.0 1200.14176810 \\
V1511 Cyg & 20 00 29.538 & +36 46 10.72 & 10.3 & 11.3 & USNO-A2.0 1200.14138751 \\
V1893 Cyg & 20 59 47.910 & +34 20 06.91 & 12.4 & 13.3 & USNO-A1.0 1200.16985829 \\
V1897 Cyg & 21 02 27.084 & +35 09 59.29 & 12.7 & 13.5 & USNO-A1.0 1200.17133164 \\
DM Lac & 22 04 35.703 & +52 53 59.36 &  9.1 & 10.1 & USNO-A1.0 1425.12892254 \\
YY Lyr & 19 02 11.799 & +29 35 49.91 & 10.8 & 12.3 & USNO-A1.0 1125.11278836 \\
DQ Oph & 16 57 46.743 & $-$30 04 39.33 & 11.5 & 12.6 & USNO-A2.0 0525.25122865 \\
DX Oph & 16 58 18.348 & $-$25 34 09.66 & 10.6 & 12.1 & GSC 6814.1391 \\
\multicolumn{5}{c}{} & USNO-A2.0 0600.22660252 \\
EG Oph & 16 59 00.39  & $-$26 01 52.0  &  9.3 & 10.2 & \\
ES Oph & 17 01 16.57  & $-$29 54 51.4  & 11.6 & 12.9 & \\
MO Oph & 16 57 36.651 & $-$29 52 28.31 & 11.3 & 13.2 & USNO-A2.0 0600.22571075 \\
NT Oph & 16 59 06.979 & $-$25 44 22.27 & 11.8 & 13.9 & USNO-A2.0 0600.22770013 \\
NV Oph & 16 59 30.735 & $-$27 57 43.75 &  9.7 & 12.5 & USNO-A2.0 0600.22826044 \\
OW Oph & 17 00 35.835 & $-$30 09 24.08 & 10.8 & 13.3 & USNO-A2.0 0525.25560998 \\
\hline
\end{tabular}
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\references

Henden, A. A., Stone, R. C., 1998, {\it AJ}, {\bf 115}, 296

Kato, T., 1998, \\ {\tt http://www.kusastro.kyoto-u.ac.jp/vsnet/Mail/vsnet-chat/msg00700.html}

Yoshida, S., Kadota, K., 1999, {\it IBVS}, No.\ 4746

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