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\input ibvs2.sty

\begin{document}
\IBVShead{5459}{9 October 2003}

\IBVStitletl{Revised [F\lowercase{e}/H] and Radial Velocities for 28 Distant}{ RR Lyrae Stars}

\IBVSauth{Pier, J. R.$^1$; Saha, A.$^2$; Kinman, T. D.$^2$}

\IBVSinst{U.S. Naval Observatory, Flagstaff Station, P.O. Box 1149, Flagstaff, Arizona 86002-1129, USA.}

\IBVSinst{NOAO\IBVSfm, P.O.Box 26732, Tucson, Arizona 
 85726, USA; email: kinman@noao.edu}

\SIMBADobjAlias{LV And}{[KMW82] 01}  
\SIMBADobjAlias{MP And}{[KMW82] 12}  
\SIMBADobjAlias{MR And}{[KMW82] 14}  
\SIMBADobjAlias{MU And}{[KMW82] 18}  
\SIMBADobjAlias{MV And}{[KMW82] 20}  
\SIMBADobjAlias{DU And}{[KMW82] 21}  
\SIMBADobjAlias{MX And}{[KMW82] 23}  
\SIMBADobjAlias{MY And}{[KMW82] 24}  
\SIMBADobjAlias{VX Lyn}{[KMW82] 34}
\SIMBADobjAlias{VY Lyn}{[KMW82] 35}  
\SIMBADobjAlias{VZ Lyn}{[KMW82] 36}  
\SIMBADobjAlias{WX Lyn}{[KMW82] 38}
\SIMBADobjAlias{YY Lyn}{[KMW82] 44}  
\SIMBADobjAlias{ZZ Lyn}{[KMW82] 46}
\SIMBADobjAlias{RW Lyn}{[KMW82] 48}  
\SIMBADobjAlias{AC Lyn}{[KMW82] 50}
\SIMBADobjAlias{AD Lyn}{[KMW82] 52}  
\SIMBADobjAlias{AF Lyn}{[KMW82] 55}
\SIMBADobjAlias{AK Lyn}{[KMW82] 60}
\SIMBADobjAlias{AL Lyn}{[KMW82] 61}
\SIMBADobjAlias{KO Peg}{[S84e] IV v103}   
\SIMBADobjAlias{KM Peg}{[S84e] IV v104}   
\SIMBADobjAlias{KL Peg}{[S84e] IV v106}   
\SIMBADobjAlias{KN Peg}{[S84e] IV v107}   
\SIMBADobjAlias{NO And}{[S84e] IV v108}   
\SIMBADobjAlias{NN And}{[S84e] IV v201}   
\SIMBADobjAlias{NQ And}{[S84e] IV v301}   
\SIMBADobjAlias{IQ Peg}{[S84e] IV v401}   
\SIMBADobj{T Sex}         
\IBVStyp{ RR }
\IBVSkey{photometry}
\IBVSabs{New abundances ([Fe/H] and radial velocities are given for 28 RR Lyrae}
\IBVSabs{stars discovered by Kinman, Mahaffey and Wirtanen (1982) and by Saha}
\IBVSabs{(1984). The stars were observed with the IIDS scanner on the KPNO   }
\IBVSabs{2.1-m telescope. The scans were calibrated by observing 18 nearby RR }
\IBVSabs{Lyrae stars whose [Fe/H] have been given by Suntzeff et al. (1991).  }

\IBVSfoot{The National Optical Astronomy Observatories are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation}

\begintext


We discuss 20 RR Lyrae stars found
in the Anticenter fields of the Lick Survey (Kinman, Mahaffey and Wirtanen 
(1982) (KMW) and 8 RR Lyrae variables discovered by Saha (1984). 
Butler, Kemper, Kraft and
Suntzeff (1982)(BKKS) have given abundances for the Lick Survey stars;
Saha and Oke (1984)(SO) gave both abundances and 
radial velocities for 7 of the 8 Saha stars discussed here. 
We give both abundances and radial velocities for all these stars 
with improved accuracy and on a common system.
Our spectra  were obtained in 1983 with the intensified image 
dissector 
scanner (IIDS) attached to the Gold spectrograph on the KPNO 2.1-m telescope. 
For calibration we observed 18 brighter RR Lyrae stars for which
Suntzeff, Kinman \& Kraft (1991) (SKK) have given 
the Preston $\Delta$S (Preston, 1959) and [Fe/H] on the Zinn-West system. The
phases ($\phi$) for the program stars were computed using the ephemerides of KMW
and Saha (1984). The ephemerides for the brighter RR Lyrae stars were taken from
 the GCVS ({\tt http://www.sai.msu.su/groups/cluster/gcvs}) and
supplemented by those given in the Hipparcos Catalogue (Vol. 11)
(1997) and by ephemerides derived from unpublished photometry by Kinman. 

The abundances were determined by measuring the equivalent widths of the 
Ca\,{\sc II} K-line, and the Balmer lines 
H$_{\gamma}$ and  H$_{\delta}$. The Preston index $\Delta$S was determined from
these equivalent widths on a plot of the K-line equivalent width against the
mean of the Balmer equivalent widths on which a grid of $\Delta$S curves was 
superposed (see SO, Fig. 3). The grid was calibrated by using the 18 RR Lyrae
stars whose $\Delta$S is known from SKK. The $\Delta$S for the program stars 
were then converted to [Fe/H] using the formula given by SKK (Eqn. 3).
This formalism strictly applies only to  the type {\it ab} RR Lyrae
stars. We also applied it to the type {\it c} variables
because our single calibrating star of type {\it c} (T Sex) showed no 
difference from those of type {\it ab} on the calibrating plot. The results are
given in Table 1. The mean $\Delta$S quoted from BKKS omits the spectra
which they took  on the rising branch; the number of their spectra (N) in col. (6)
are only those in the range 0.00$\leq$$\phi$$\leq$0.85. [Fe/H] was derived from their 
$\Delta$S using the conversion of SKK. In the case of our data, we only derived
$\Delta$S from spectra whose $\phi$ was in the range 0.40 to 0.85 (i.e. near
minimum) and (unlike BKKS) no phase correction was applied to our $\Delta$S. 
The quality of our spectra and those of BKKH is similar, so our adopted 
[Fe/H] is the mean of our
new [Fe/H] and those from BKKH data weighted by N the number of 
spectra.
We adopted the [Fe/H] from our new data alone for the remaining stars. 

\newpage
\begin{table}[!ht]
\normalsize\
\centerline{{\bf Table 1.} Abundances of the RR Lyrae Variables.}
\begin{center}
\begin{tabular}{cccccccccccc}
\hline
\multicolumn{3}{c}{Identification} && \multicolumn{3}{c}{Previous Data}&&\multicolumn{3}{c}{New Data}&   \\
\cline{1-3}  
\cline{5-7} 
\cline{9-11} 
GCVS$^{1}$&KMW$^{2}$&Saha$^{3}$&RR&$\Delta$S&N  &[Fe/H]&&$\Delta$S$^{4}$&N  &[Fe/H]&
Adopted\\
   &   &  &Type&Source& &Source&&   &   &   &[Fe/H]  \\   
 (1)&(2)&(3)&(4)&(5)&(6)&(7)&&(8)&(9)&(10)&(11)     \\
\hline

 LV And& 01&$\cdots$    &ab& 6.8(a) &3&$-$1.48(c)&& 7.7 &3&$-$1.62&$-$1.55 \\
 MP And& 12&$\cdots$    &ab& 6.8(a) &2&$-$1.48(c)&& 8.0 &2&$-$1.67&$-$1.57 \\
 MR And& 14&$\cdots$    & c& 5.6(a) &3&$-$1.29(c)&& 5.2 &2&$-$1.23&$-$1.26 \\
 MU And& 18&$\cdots$    &ab& 7.2(aA)&4&$-$1.55(c)&& 7.7 &2&$-$1.62&$-$1.57 \\
 MV And& 20&$\cdots$    &ab& 8.2(a) &3&$-$1.70(c)&& 9.3 &3&$-$1.88&$-$1.78 \\
 DU And& 21&$\cdots$    &ab&11.0(aA)&2&$-$2.15(c)&&10.6 &2&$-$2.08&$-$2.11 \\
 MX And& 23&$\cdots$    &ab& 7.6(aA)&2&$-$1.61(c)&& 6.4 &2&$-$1.42&$-$1.50 \\
 MY And& 24&$\cdots$    &ab& 5.2(a) &3&$-$1.23(c)&& 6.7 &2&$-$1.47&$-$1.32 \\
 VX Lyn& 34&II v104     &ab& 7.4(a) &2&$-$1.58(c)&&(8.0)&0&$\cdots$&$-$1.58\\
 VY Lyn& 35&$\cdots$    & c& 7.8(a) &3&$-$1.64(c)&& 6.0 &1&$-$1.36&$-$1.57 \\
 VZ Lyn& 36&$\cdots$    & c& 6.8(a) &1&$-$1.48(c)&& 6.9 &1&$-$1.50&$-$1.48 \\
 WX Lyn& 38&II v208     &ab&9.6:(a) &1&$-$1.92:(c)&& 7.0&1&$-$1.51&$-$1.72\\
 YY Lyn& 44&$\cdots$    & c& 9.6(a) &1&$-$1.92(c)&& 9.0 &1&$-$1.83&$-$1.87 \\
 ZZ Lyn& 46&III v201    &ab& 6.4(a) &2&$-$1.42(c)&&(5.8)&0&$\cdots$&$-$1.42\\
 RW Lyn& 48&$\cdots$    &ab& 7.1(a) &3&$-$1.53(c)&&(7.4)&0&$\cdots$&$-$1.53\\
 AC Lyn& 50&III v204    &ab& 6.2(aA)&2&$-$1.39(c)&& 7.8 &2&$-$1.64&$-$1.50 \\
 AD Lyn& 52&$\cdots$    & c& 6.6(a) &1&$-$1.45(c)&& 6.7 &1&$-$1.47&$-$1.46 \\
 AF Lyn& 55&$\cdots$    &ab& 7.0(a) &3&$-$1.51(c)&& 8.3 &1&$-$1.72&$-$1.56 \\
 AK Lyn& 60&$\cdots$    &ab& 7.8(aA)&1&$-$1.64(c)&& 6.9 &1&$-$1.50&$-$1.56 \\
 AL Lyn& 61&$\cdots$    &ab& 9.9(aA)&1&$-$1.97(c)&& 9.0 &1&$-$1.83&$-$1.90 \\
 KO Peg&$\cdots$&IV v103&ab& 9.4(b) &1&$-$1.7 (b)&&10.9 &1&$-$2.13&$-$2.13 \\
 KM Peg&$\cdots$&IV v104&ab& 7.7(b) &1&$-$1.5 (b)&& 6.0 &1&$-$1.36&$-$1.35 \\
 KL Peg&$\cdots$&IV v106&ab& 4.9(b) &1&$-$1.0 (b)&& 6.1 &1&$-$1.37&$-$1.36 \\
 KN Peg&$\cdots$&IV v107&ab& 7.7(b) &1&$-$1.5 (b)&& 7.5 &1&$-$1.59&$-$1.59 \\
 NO And&$\cdots$&IV v108& c&$\cdots$&$\cdots$&$\cdots$&&8.0&1&$-$1.67&$-$1.67\\
 NN And&$\cdots$&IV v201&ab& 8.8(b) &1&$-$1.6 (b)&& 6.0 &2&$-$1.36&$-$1.35 \\
 NQ And&$\cdots$&IV v301&ab& 8.6(b) &1&$-$1.6 (b)&& 6.2 &1&$-$1.39&$-$1.38 \\
 IQ Peg&$\cdots$&IV v401&ab& 6.9(b) &1&$-$1.3 (b)&& 7.0 &1&$-$1.51&$-$1.51 \\
\hline
\end{tabular}
\end{center}
$^{1}$~~GCVS ({http://www.sai.msu.su/groups/cluster/gcvs})  \\
$^{2}$~~Kinman, Mahaffey and Wirtanen (1982) (KMW)~~~~~~\\
$^{3}$~~Saha (1984) \\
$^{4}$~~Parentheses indicate $\Delta$S derived from observations not at minimum
light \\
Sources of Data: \\
(a)~~Butler, et al. (1982) (BKKS); (aA) adjusted from BKKS (see text) \\
(b)~~Saha and Oke (1984) \\
(c)~~Derived from $\Delta$S using equation (3) in  Suntzeff et al. (1991) (SKK) \\
\end{table}

The mean difference between the adjusted mean values of $\Delta$S from BKKS and 
our new values is +0.03$\pm$0.03. The corresponding difference between the estimates
of [Fe/H] is $-$0.00$\pm$0.05. 

Radial velocities were determined from the IIDS spectra by a Fourier method
(Pier, 1983) 
in which the program spectra are cross correlated with that of a star of 
known velocity; the velocity in this case is defined by both the Balmer and
weak metal lines. The velocity was also 
derived from the three strong lines (H$_{\gamma}$, H$_{\delta}$ 
and the Ca\,{\sc II} K-line) and weights of 2, 1 and 0 were given if the     
$\sigma_{rms}$ of a single line was $<$ 40 km s$^{-1}$, between 40 and 70 km
s$^{-1}$ or $>$70 km s$^{-1}$ respectively. 

\begin{table}[!ht]
\normalsize
\centerline{{\bf Table 2.} Radial Velocities of the RR Lyrae Variables.}
\begin{center}
\begin{tabular}{ccccccccccc}
\hline
        &     &\multicolumn{2}{c}{Saha \& Oke~(1984)}&&\multicolumn{4}{c}{IIDS Spectra}& & Adopted \\
\cline{3-4} 
\cline{6-9} 
Variable &RR  &Rad. Vel.& N$^{1}$ & & Rad. Vel.$^{2}$&Wt$^{3}$&Rad.Vel.$^{4}$&Wt$^{3}$& &Rad. Vel. \\
    &Type   & km s$^{-1}$& & & km s$^{-1}$ & &  km s$^{-1}$& & & km s$^{-1}$ \\
 (1)&(2)& (3)& (4)& &(5)&(6)&(7)& (8)& &(9)     \\
\hline
LV And &ab&$\cdots$&$\cdots$& &$-$028.1 &8&$-$038.4&4& &$-$031.5 \\
MP And &ab&$\cdots$&$\cdots$& &$-$102.6 &4&$-$104.1&4& &$-$103.4 \\
MR And &c &$\cdots$&$\cdots$& &$-$081.7 &4&$-$079.6&4& &$-$080.6 \\
MU And &ab&$\cdots$&$\cdots$& &$-$099.6 &4&$-$091.7&4& &$-$095.6 \\
MV And &ab&$\cdots$&$\cdots$& &$-$066.1 &8&$-$068.2&8& &$-$067.2 \\
DU And &ab&$\cdots$&$\cdots$& &$-$343.0 &4&$-$362.3&3& &$-$351.3 \\
MX And &ab&$\cdots$&$\cdots$& &$\cdots$&$\cdots$&$-$187.8&2& &$-$187.8 \\
MY And &ab&$\cdots$&$\cdots$& &$-$138.8 &4&$-$130.3&4& &$-$134.6 \\
VX Lyn &ab&$+$48$\pm$23& 1 & &$-$024.9 &4&$+$027.5&4& &$+$001.3 \\
VY Lyn &c&$\cdots$&$\cdots$& &$+$103.9 &2&$+$125.1&2 & &$+$114.5 \\
VZ Lyn &c&$\cdots$&$\cdots$& &$-$167.4 &2&$-$196.8&2 & &$-$182.1 \\
WX Lyn &ab&$+$2$\pm$20& 2 & &$+$020.2 &4&$+$034.4&3& &$+$026.3 \\
YY And &c&$\cdots$&$\cdots$& &$-$082.3 &4&$-$103.9&4 & &$-$093.1 \\
ZZ Lyn &ab&$+$255$\pm$54& 1 & &$+$157.0 &2&$+$137.5&2& &$+$147.2\\
RW Lyn &ab&$\cdots$&$\cdots$& &$-$140.7 &4&$-$158.9&4& &$-$149.8 \\
AC Lyn &ab&$\cdots$&$\cdots$& &$-$022.5 &4&$-$029.0&4& &$-$025.8 \\
AD Lyn &c&$\cdots$&$\cdots$& &$+$124.0 &2&$+$123.2& 2& &$+$123.6 \\
AF Lyn &ab&$\cdots$&$\cdots$& &$-$108.0 &2&$-$149.0&1& &$-$121.7\\
AK Lyn &ab&$\cdots$&$\cdots$& &$+$234.8 &2&$+$243.1&1& &$-$237.6 \\
AL Lyn &ab&$\cdots$&$\cdots$& &$-$058.0 &4&$-$073.6&4& &$-$065.8 \\
KO Peg &ab&$-$272$\pm$25& 1 & &$-$342.9 &2&$-$331.1&2& &$-$335.0 \\
KM Peg &ab&$-$164$\pm$25& 1 & &$-$230.1 &2&$-$235.7&2& &$-$233.8 \\
KL Peg &ab&$-$342$\pm$35& 1 & &$-$393.8 &2&$-$376.9&2& &$-$382.5 \\
KN Peg &ab&$-$74$\pm$36& 1 & &$-$194.9 &2&$-$199.4&1& &$-$196.4 \\
NO And &c&$\cdots$&$\cdots$& &$-$079.7 &2&$-$064.2&1& &$-$074.5 \\
NN And &ab&$-$276$\pm$24& 1 & &$-$293.5 &4&$-$305.0&3& &$-$298.4 \\
NQ And &ab&$-$235$\pm$29& 1 & &$-$247.7 &2&$-$240.5&2& &$-$242.9 \\
IQ Peg &ab&$-$207$\pm$34& 1 & &$-$203.5 &2&$-$203.9&2& &$-$20-3.7\\
\hline
\end{tabular}
\end{center}
Notes:  \\
$^{1}$~~No. of spectra  ~~ $^{3}$ Weight as described in text  \\
$^{2}$~~Derived by Fourier method. ~~
$^{4}$~~Derived from H$_{\gamma}$, H$_{\delta}$ and the Ca\,{\sc II} K-line. \\
\end{table}

The $\gamma$-velocity was derived 
for type {\it ab} stars using the recipe given by Liu (1991). For type {\it c}
stars, we scaled the velocity curve of T Sex by the 
relative V-amplitudes and got a correction from that.
For the type {\it ab} variable SU Dra, the
velocity amplitude of H$_{\gamma}$ is about 100 km s$^{-1}$ compared with 
60 km s$^{-1}$ for the weaker metal lines 
(Oke, Giver \& Searle, 1962).
The use of the Liu-correction could therefore 
produce systematic effects in the difference (D) between the velocity based on
the strong lines  and that based on the weaker lines: D 
should be positive just before phase zero and negative just after. We did not
observe this and conclude that the effect  is too small to affect our results.
 The mean difference $\langle$D$\rangle$ is $-$3.7$\pm$4.9 km s$^{-1}$ so there is no
systematic difference between the two methods. The rms value of D for each star
is 21 km s$^{-1}$; on average therefore, 
these adopted velocities have an error of about $\pm$15 km s$^{-1}$. 


In Table 3  we give the most recent coordinates for these variables. These
have been taken from the USNO-B1.0 Catalog (Monet et al., 2003) and  checked 
against the original finding charts using the Digital Sky Survey 
({\tt http://cadcwww.dao.nrc.ca/dss/}). 


\newpage
\begin{table}[!ht]
\normalsize
\centerline{{\bf Table 3.} Coordinates of the RR Lyrae Variables.}
\begin{center}
\begin{tabular}{ccccccccc}
\hline
      &   &\multicolumn{2}{c}{J2000} & &    &     &\multicolumn{2}{c}{J2000}\\
\cline{3-4} 
\cline{8-9} 
Variable&$\langle$V$\rangle$& R.A. & Dec. & &Variable &$\langle$V$\rangle$ & R.A. & Dec. \\
        &(mag.)&       &      & &         &(mag.)  &      &      \\
\hline
LV And &15.44&02 19 26.39&+41 45 57& &RW Lyn&12.91&07 50 39.18&+38 27 15 \\
MP And &16.13&02 24 13.74&+41 19 47& &AC Lyn&16.38&07 54 42.16&+38 54 21 \\
MR And &15.56&02 25 27.81&+40 57 26& &AD Lyn&15.85&07 56 22.99&+39 22 59 \\
MU And &16.00&02 29 26.44&+39 31 45& &AF Lyn&16.12&08 35 57.43&+41 01 11 \\
MV And &15.99&02 30 12.29&+40 53 15& &AK Lyn&16.00&08 45 55.10&+39 14 55 \\
DU And &13.59&02 30 31.33&+40 50 34& &AL Lyn&16.52&08 49 13.07&+38 49 31 \\
MX And &17.18&02 32 03.09&+42 08 31& &KO Peg&16.03&00 02 15.33&+30 04 37 \\
MY And &15.56&02 32 09.47&+43 04 47& &KM Peg&17.67&23 55 45.11&+29 09 52 \\
VX Lyn &17.01&07 31 51.83&+39 07 48& &KL Peg&16.85&23 46 57.08&+29 51 02 \\
VY Lyn$^{1}$ &15.75&07 32 26.04&+38 50 07& &KN Peg&17.44&23 56 46.56&+31 40 23 \\
VZ Lyn &16.20&07 32 40.75&+41 37 39& &NO And&16.54&00 06 58.32&+32 02 07 \\
WX Lyn &16.84&07 35 38.47&+39 15 27& &NN And&16.68&00 06 55.84&+31 28 13 \\
YY Lyn &14.98&07 45 30.07&+37 22 59& &NQ And&16.31&00 11 32.68&+30 51 41 \\
ZZ Lyn &15.80&07 50 21.77&+37 42 00& &IQ Peg&16.11&00 06 05.68&+29 19 13 \\
\hline
\end{tabular}
\end{center}
Notes:  \\
$^{1}$~~The catalog lists two stars of similar brightness close to this
        position. The DSS only shows one star. \\
\end{table}

\references

Butler, D., Kemper, E., Kraft, R. P., and Suntzeff, N. B., 1982, {\it AJ},
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ESA (1997), {\it The Hipparcos \& Tycho Catalogues} ({\bf Vol. 11}), (ESA SP-1200)
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Kinman, T. D., Mahaffey, C. T. and Wirtanen, C. A. 1982, {\it AJ}, {\bf 87}, 314                (KMW)  

Liu, T. 1991, {\it PASP}, {\bf 103}, 205  

Monet, D. G., Levine, S. E., Casian, B. et al. 2003, {\it AJ}, {\bf 125}, 984  

Oke, J. B., Giver, L. P., and Searle, L. 1962, {\it ApJ}, {\bf 136}, 393

Pier, J. R. 1983, {\it ApJS}, {\bf 53}, 791 

Preston, G. W., 1959, {\it ApJ}, {\bf 130}, 507  

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\endreferences

\end{document}

