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\begin{document}
\IBVShead{4230}{16 August 1995}

\title{NEW SPECTRAL CLASSIFICATIONS FOR 49 RED VARIABLE STARS}

\begintext


  Over the years spectral classifications of a great many red variables have been
published from objective-prism plates taken with CWRU's Burrell Schmidt telescope
and its twin, the University of Michigan's Curtis Schmidt. These plates have variously
covered the photographic, visual, and infrared parts of the spectrum.
 
 In looking through our extensive cardfiles, we have found 49 further red
variables for which we have useful, apparently unpublished, spectral data. Most of
the relevant plates were taken and searched many years ago in the course of our
surveys for high-luminosity early-type stars. Table 1 lists the stars for which we
present new data.
 \vskip 1mm
\centerline{Table 1}
\vskip 1mm
\begin{center}
\begin{tabular}{lccl}
\hline
Name  &Catalogue Sp.&New Data&Remarks\\
      &   Type& & \\
\hline
\\
TZ Aps  &   ---  &           M9:e& \\
TU Aql  &   M4-9 &           M2e& \\ 
EM Aql  &   M7   &           M4e& \\
PX Aql  &   M5   &           M2e& \\
V434 Aql&   M6   &           M4e& \\[0.6ex]
V630 Ara&   Me   &           M6e& \\
V352 Car&   Me   &           M5e& \\
UV Cen  &   Me   &           M5e& \\
GR CrA  &   Me   &           M4e& \\
KM CrA  &   Me   &           M4e& \\[0.6ex]
RT Lup  & Me   &  M8e& \\
ST Mon  & M6.5 & MSe& \\
AZ Mon  & M9   &  M6e& \\
CH Mus  & Me   &  M5e& \\
CR Mus  & Me   &  M4e &identical with FP Mus\\[0.6ex]
EK Mus  & Me   &  M8:e& \\ 
BD Nor  & Me   &  $>$M5e& \\
FS Nor  & Me   &  M7e& \\
PP Nor  & Me   &  $>$M5e& \\
UX Oph  & M4e  &  M1e& \\[0.6ex]             
V585 Oph&  M5  & M6e& \\
BZ Pup  &  M5  & M4:e& \\
FO Pup  &  Me  & M7e& \\
UU Pyx  &  Me  & M4e& \\
GH Sgr  &  Me  & M4e& \\
\end{tabular}
\end{center}
\vfill \eject

\centerline{2}
\vskip 1mm
\centerline{Table 1 (cont.)}
\vskip 1mm
\begin{center}
\begin{tabular}{lccl}
\hline
Name  &Catalogue Sp.&New Data&Remarks\\
      &   Type& & \\
\hline
\\
IM Sgr  &  M9e & M2e& \\
V361 Sgr&  M3 III& M3e& \\
V930 Sgr & M5-6 &    &emission noted\\
V931 Sgr & M7-8 &    &emission noted\\
V1592 Sgr& ---  & Me& \\[0.6ex]
V1683 Sgr& M7   &    & emission noted\\
V1690 Sgr& M7   &    & emission noted\\
V2512 Sgr& --  &    M:e& \\
V2543 Sgr& M8e$\alpha$& &  error in GCVS; should be M3e\\
RX Sco   & Me  &  M7:e& \\[0.6ex]
V880 Sco & Me  &    M8e& \\
VW Sct   & M4-7&    M6e& \\
XY Ser   & M3  &    M3e& \\
BE Ser   & M5  &    M5e& \\
Y TrA    & S4,1&        &emission noted, called M6e\\[0.6ex]
RS TrA  &       Me  &      M8e& \\
ER TrA  &       Me  &      M8e& \\
GY TrA  &       --- &      Me& \\
HK TrA  &       Me  &      M4e& \\
TZ Vel  &       --  &      M7:e& \\[0.6ex]
NSV 4665&       --  &      M9e:& \\
NSV 6929&       Me  &      M5e& \\
NSV 8952&       Me  &      M2e& \\
NSV 13052&      --- &      M3e& \\
\hline
\end{tabular}
\end{center}
\vskip 2mm

 Two facts should be borne in mind concerning objective-prism studies of 
M-type variables: (1) blue-sensitive plates are the most efficient ones for the detection of
emission lines; thus red and infrared plates will generally not show such features even
if they are present elsewhere, and (2) objective-prism observations, made at random,
of course tend to favor the brighter parts of the variables' light curves, but can
occasionally refer to phases rather far from maximum light. Thus objective-prism
spectral types are usually somewhat later than the variables' types at maximum light,
which are those usually tabulated.

\vskip .8cm

\beginauthors
\authorsrightcol
N. SANDULEAK$^{\star}$
C.B. STEPHENSON
W.P. BIDELMAN
Warner \& Swasey Observatory
Case Western Reserve University
Cleveland, OH 44106-7215 USA
\endauthors

\vskip 3mm
$^{\star}$ Deceased 7 May 1990


\vfill \eject

\centerline{3}
\vskip 6mm
\centerline{\bf ERRATUM FROM IBVS 4266}
\vskip 1.5cm

In IBVS No.\,4230, the spectral type of ST Mon was incorrectly given due to an
unfortunate 

typographic error. The new spectral type of ST Mon is M5e.

\vskip 2cm
\hspace*{10cm}The editors

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