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Math and formulae

Formulae should be tagged using the formula element in DTD 4. Blackwell's currently requires the following:

1. Maths tagged as MathML or as LaTeX 2e
2. Graphics of individual equations
   • Graphics of individual equations should be supplied in GIF format
   • The GIF should be marked up as the main element in the formula. The MathML or Latex 2e versions tagged as alternativemath elements. (See example below)
   • The GIF should be cropped to the boundaries of the equation (i.e. not surrounded by white space)
   • The equation number (if there is one) should be captured in the XML as shown below, not in the GIF
   • The dimensions of the equation GIF should be equivalent to the print version. A sample GIF is shown below. The border is intended to show the boundaries of the GIF image and is not part of the GIF.
     

A sample equation and its corresponding markup is shown below. The following points should be noted in the 'Extract from XML':

1. Alternative versions - Alternative versions of the formula are available, and these are tagged using the alternativemath element. Each alternative is specified in the element's type attribute.
2. Markup characters in TeX - The contents of the tex element need to be enclosed in CDATA markers (<![CDATA[...]]>) markers so that any < or &, characters in the TeX code will be ignored during parsing. For an explanation of CDATA markers, see here.
3. Punctuation - The comma separating the equation from the equation number is tagged as x in formula, not as part of any one of the equations.
4. Formula numbers - The formula number is tagged using the number element in formula
5. Equation ID numbers - The ID number, used for linking to the equation, is contained in the ID attribute of formula.

1. Display formula

The markup for the above display formula is shown below. Note the following which are highlighted in the sample XML code:

• The format attribute on formula is "display".
• The id attribute on formula is given an appropriate id value ("m3" in the example below). See ID prefixes.
• The formula is delivered as a gif, details of which are in the file element.
• The formula is also available in LaTeX 2e (the only type of LaTeX which Blackwell Publishing currently accepts). The LaTeX code is given in an alternativemath element with a type attribute of "latex2e".
• The LaTeX code is contained within CDATA markers. For an explanation of why, see the tex element page.
• The formula is also available as MathML (supported by DTD 4). The MathML code is contained in another alternativemath element with a type attribute of "mathml".
• The punctuation between the formula and the formula number is contained in an x element.
• The equation number is contained in a number element.

...

<p><formula format="display" id="m3">

<file name="gji_195_m3.gif" type="gif"/>

<alternativemath type="latex2e">
<tex><![CDATA[\mu \left(s\right) = 
\frac{\mu s}{s+\displaystyle \frac{\mu}{\nu}}]]></tex>
</alternativemath>

<alternativemath type="mathml">
 <math>
    <mrow>
       <mi>&mu;</mi><mo>(</mo><mi>s</mi><mo>)</mo><mo>=</mo>
       <mfrac>
          <mrow><mi>&mu;</mi><mi>s</mi></mrow>
          <mrow><mi>s</mi><mo>+</mo>
             <mfrac>
                <mrow><mi>&mu;</mi></mrow>
                <mrow><mi>&nu;</mi></mrow>
             </mfrac>
          </mrow>
       </mfrac>
    </mrow>
 </math>
 </alternativemath>

<x>,</x><number>(3)</number>


</formula></p>

<p>with &nu; denoting the Maxwell viscosity. The linearized equation of motion 
for an incompressible Maxwell body with constant density in each layer is</p>

...

2. Inline formula

The markup for the above inline formulae is shown below. The inline formula highlighted above is highlighted in the XML markup below. Note the following:

• The format attribute is "inline".
• The inline formula is delivered as a GIF, details of which are contained in a file element.
• The inline equation is also available in LaTeX 2e format, contained in a alternativemath element.

<p>Three different classes of cosmological model are examined in this work, 
each with a simple cold dark matter (CDM) power spectrum. The models are specified 
in terms of the usual cosmological parameters: <formula format="inline"><simplemath>
&Omega;<sub>0</sub>&equals;<i>&rho;</i>&sol;<i>&rho;</i>
<sub>crit</sub></simplemath></formula> is the normalized matter density, <formula 
format="inline"><file name="mnr_5178_mu1.gif" type="gif"/><alternativemath type="latex2e">
<tex><![CDATA[\lambda _{0}=\Lambda _{0}\mathit{c}^{2}/(3\mathit{H}^{2}_{0})]]></tex>
</alternativemath></formula> is the normalized vacuum energy density, and Hubble's 
constant is <formula format="inline"><simplemath><i>H</i><sub>0</sub>
&equals;100&thinsp;<i>h</i>&thinsp;km&thinsp;s<sup>-1</sup>&thinsp;
Mpc<sup>-1</sup></simplemath></formula> with <formula format="inline"><simplemath>
0&lt;<i>h</i>&le;1</simplemath></formula>. The models are a standard CDM model 
(SCDM) with <formula format="inline"><simplemath>(&Omega;<sub>0</sub>,<i>&
lambda;</i><sub>0</sub>)&equals;(1.0,0.0)</simplemath></formula>, an open CDM 
model (OCDM) with <formula format="inline"><simplemath>(&Omega;<sub>0</sub>,<i>
&lambda;</i><sub>0</sub>)&equals;(0.3,0.0)</simplemath></formula> and a 
flat model with a cosmological constant (LCDM) where <formula format="inline"><simplemath>
(&Omega;<sub>0</sub>,<i>&lambda;</i><sub>0</sub>)&equals;(0.3,0.7)
</simplemath></formula>.</p>

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