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<H3><A NAME="SECTION00844100000000000000">
REGISTER/ROMAFOT</A>
</H3>
<TT>REGISTER/ROMAFOT</TT>
<FONT SIZE="-1"><TT>int_tab reg_tab [wnd_opt] [obj_opt]</TT></FONT>
<P>
This command creates a table with the results of the analysis.
However, all the photometric information obtained from the frame as
the absolute quantities (magnitudes, colour equations etc.) still
have to be derived. In this output table every object occupies one
row and the data are stored according the Table <A HREF="node104.html#romafot-output">5.2</A>.
<P>
<BR>
<DIV ALIGN="CENTER"><A NAME="4408"> </A>
<TABLE>
<CAPTION><STRONG>Table 5.2:</STRONG>
Romafot Registration Table</CAPTION>
<TR><TD>
<DIV ALIGN="CENTER">
<TABLE CELLPADDING=3 BORDER="1" ALIGN="CENTER">
<TR><TH ALIGN="RIGHT"><B>Column</B></TH>
<TH ALIGN="LEFT"><B>Name </B></TH>
<TH ALIGN="LEFT"><B>Description </B></TH>
</TR>
<TR><TD ALIGN="RIGHT">#1</TD>
<TD ALIGN="LEFT"><TT> :IDENT</TT></TD>
<TD ALIGN="LEFT">Identification</TD>
</TR>
<TR><TD ALIGN="RIGHT">#2</TD>
<TD ALIGN="LEFT"><TT> :X</TT></TD>
<TD ALIGN="LEFT">Physical X-coordinate</TD>
</TR>
<TR><TD ALIGN="RIGHT">#3</TD>
<TD ALIGN="LEFT"><TT> :Y</TT></TD>
<TD ALIGN="LEFT">Physical Y-coordinate</TD>
</TR>
<TR><TD ALIGN="RIGHT">#4</TD>
<TD ALIGN="LEFT"><TT> :INT</TT></TD>
<TD ALIGN="LEFT">central pixel intensity resulted from the fit</TD>
</TR>
<TR><TD ALIGN="RIGHT">#5</TD>
<TD ALIGN="LEFT"><TT> :LOC_BG</TT></TD>
<TD ALIGN="LEFT">Local sky background; see text</TD>
</TR>
<TR><TD ALIGN="RIGHT">#6</TD>
<TD ALIGN="LEFT"><TT> :MAG1</TT></TD>
<TD ALIGN="LEFT">Aperture magnitude no.1; see text</TD>
</TR>
<TR><TD ALIGN="RIGHT">#7</TD>
<TD ALIGN="LEFT"><TT> :MAG2</TT></TD>
<TD ALIGN="LEFT">Aperture magnitude no.2; see text</TD>
</TR>
<TR><TD ALIGN="RIGHT">#8</TD>
<TD ALIGN="LEFT"><TT> :MAG3</TT></TD>
<TD ALIGN="LEFT">Aperture magnitude no.3; see text</TD>
</TR>
<TR><TD ALIGN="RIGHT">#9</TD>
<TD ALIGN="LEFT"><TT> :MAG_CNV</TT></TD>
<TD ALIGN="LEFT">Instrumental magnitude; see text</TD>
</TR>
<TR><TD ALIGN="RIGHT">#10</TD>
<TD ALIGN="LEFT"><TT> :SIGMA</TT></TD>
<TD ALIGN="LEFT">Sigma of fit function (if not fixed by the user)</TD>
</TR>
<TR><TD ALIGN="RIGHT">#11</TD>
<TD ALIGN="LEFT"><TT> :BETA</TT></TD>
<TD ALIGN="LEFT">Parameter of the Moffat fit function</TD>
</TR>
<TR><TD ALIGN="RIGHT">#12</TD>
<TD ALIGN="LEFT"><TT> :SIQ</TT></TD>
<TD ALIGN="LEFT">Semi interquartle resulting from the fit</TD>
</TR>
<TR><TD ALIGN="RIGHT">#13</TD>
<TD ALIGN="LEFT"><TT> :CHI_SQ</TT></TD>
<TD ALIGN="LEFT"><IMG
WIDTH="54" HEIGHT="78" ALIGN="MIDDLE" BORDER="0"
SRC="img230.gif"
ALT="$\chi^{2}$">
resulting from the fit</TD>
</TR>
</TABLE></DIV>
<A NAME="romafot-output"> </A> </TD></TR>
</TABLE>
</DIV>
<BR>
<P>
The magnitudes MAG1, MAG2 and MAG3 (e.g. U, B and V) are accepted by
the commands <TT>FIND/ROMAFOT</TT> or <TT>SELECT/ROMAFOT</TT>
and are necessary for calibration. In case of program stars (search
made with <TT>SEARCH/ROMAFOT</TT>), these columns are filled with zeros.
<P>
The instrumental magnitude MAG_CNV is calculated as
<!-- MATH: $-2.5~ \log~VOL$ -->
<IMG
WIDTH="105" HEIGHT="40" ALIGN="MIDDLE" BORDER="0"
SRC="img231.gif"
ALT="$-2.5~ \log~VOL$">,
where <I>VOL</I> is the integral over the elementary surface to fit the
star, calculated from <IMG
WIDTH="1" HEIGHT="42" ALIGN="MIDDLE" BORDER="0"
SRC="img232.gif"
ALT="$-\infty$">
to <IMG
WIDTH="68" HEIGHT="70" ALIGN="MIDDLE" BORDER="0"
SRC="img233.gif"
ALT="$+\infty$">.
In case of linear data
this is expected to differ from the magnitude by a constant.
<P>
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<ADDRESS>
<I>Petra Nass</I>
<BR><I>1999-06-15</I>
</ADDRESS>
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