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<H2><A NAME="SECTION0004161000000000000000">SLA_RVLSRK - RV Corrn to Kinematical LSR</A>
<A NAME="xref_SLA_RVLSRK"> </A><A NAME="SLA_RVLSRK"> </A>
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<DL>
<DT><STRONG>ACTION:</STRONG>
<DD>Velocity component in a given direction due to the Sun's
motion with respect to a kinematical Local Standard of Rest.
<P> <DT><STRONG>CALL:</STRONG>
<DD><TT>R = sla_RVLSRK (R2000, D2000)</TT>
<P> </DL>
<P> <DL>
<DT><STRONG>GIVEN:</STRONG>
<DD>
<BR>
<TABLE CELLPADDING=3>
<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R2000,D2000</EM></TD>
<TH ALIGN="LEFT"><B>R</B></TH>
<TD ALIGN="LEFT" NOWRAP>J2000.0 mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
SRC="img3.gif"
ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
</TR>
</TABLE></DL>
<P> <DL>
<DT><STRONG>RETURNED:</STRONG>
<DD>
<BR>
<TABLE CELLPADDING=3>
<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RVLSRK</EM></TD>
<TH ALIGN="LEFT"><B>R</B></TH>
<TH ALIGN="LEFT" NOWRAP>Component of <I>standard</I> solar motion
in direction R2000,D2000 (km s<SUP>-1</SUP>)</TH>
</TR>
</TABLE></DL>
<P> <DL>
<DT><STRONG>NOTES:</STRONG>
<DD><DL COMPACT>
<DT>1.
<DD>Sign convention: the result is positive when
the Sun is receding from the given point on the sky.
<DT>2.
<DD>The Local Standard of Rest used here is one of several
<I>kinematical</I> LSRs in common use. A kinematical LSR is the
mean standard of rest of specified star catalogues or stellar
populations. The Sun's motion with respect to a kinematical
LSR is known as the <I>standard</I> solar motion.
<DT>3.
<DD>There is another sort of LSR, seldom used by observational
astronomers, called the <I>dynamical</I> LSR. This is a
point in the vicinity of the Sun which is in a circular orbit
around the Galactic centre. The Sun's motion with respect to
the dynamical LSR is called the <I>peculiar</I> solar motion. To
obtain a radial velocity correction with respect to the
dynamical LSR use the routine sla_RVLSRD.
<DT>4.
<DD>The adopted standard solar motion is 20 km s<SUP>-1</SUP>
towards <IMG WIDTH="132" HEIGHT="33" ALIGN="MIDDLE" BORDER="0"
SRC="img225.gif"
ALT="$\alpha=18^{\rm h},\delta=+30^{\circ}$"> (1900).
</DL></DL>
<P> <DL>
<DT><STRONG>REFERENCES:</STRONG>
<DD><DL COMPACT>
<DT>1.
<DD>Delhaye (1965), in <I>Stars and Stellar Systems</I>, vol 5, p73.
<DT>2.
<DD><I>Methods of Experimental Physics</I> (ed Meeks), vol 12,
part C, sec 6.1.5.2, p281.
</DL></DL>
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<ADDRESS>
<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
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