commit 20fe5a67818c2691db3c5bbfbc4bf519c744430e
Author: Thibaut Cuvelier <[email protected]>
Date: Sat Aug 1 04:09:45 2020 +0200
DocBook: slight improvement for AAS documents.
---
.../docbook/bibliography_precooked_aastex.xml | 34 ++++++++++----------
lib/layouts/aastex.layout | 3 +-
lib/layouts/aastex6.layout | 2 +-
3 files changed, 20 insertions(+), 19 deletions(-)
diff --git a/autotests/export/docbook/bibliography_precooked_aastex.xml
b/autotests/export/docbook/bibliography_precooked_aastex.xml
index cba8d88..d3381b3 100644
--- a/autotests/export/docbook/bibliography_precooked_aastex.xml
+++ b/autotests/export/docbook/bibliography_precooked_aastex.xml
@@ -6,11 +6,11 @@
</info>
<section>
<title>Introduction</title>
-<Standard>A focal problem today in the dynamics of globular clusters is core
collapse. It has been predicted by theory for decades <biblioref
endterm="hen61" />, <biblioref endterm="lyn68" />, <biblioref endterm="spi85"
/>, but observation has been less alert to the phenomenon. For many years the
central brightness peak in M15 <biblioref endterm="kin75" />, <biblioref
endterm="new78" /> seemed a unique anomaly. Then <biblioref endterm="aur82" />
suggested a central peak in NGC 6397, and a limited photographic survey of ours
<biblioref endterm="djo84" /> found three more cases, including NGC 6624, whose
sharp center had often been remarked on <biblioref endterm="can78" />.
</Standard>
+<para>A focal problem today in the dynamics of globular clusters is core
collapse. It has been predicted by theory for decades <biblioref
endterm="hen61" />, <biblioref endterm="lyn68" />, <biblioref endterm="spi85"
/>, but observation has been less alert to the phenomenon. For many years the
central brightness peak in M15 <biblioref endterm="kin75" />, <biblioref
endterm="new78" /> seemed a unique anomaly. Then <biblioref endterm="aur82" />
suggested a central peak in NGC 6397, and a limited photographic survey of ours
<biblioref endterm="djo84" /> found three more cases, including NGC 6624, whose
sharp center had often been remarked on <biblioref endterm="can78" />. </para>
</section>
<section>
<title>Observations</title>
-<Standard>All our observations were short direct exposures with CCD's. At Lick
Observatory we used a TI 500<inlineequation><alt role='tex'>\times</alt>
+<para>All our observations were short direct exposures with CCD's. At Lick
Observatory we used a TI 500<inlineequation><alt role='tex'>\times</alt>
<m:math>
<m:mrow><m:mo>×</m:mo>
@@ -64,17 +64,17 @@
<m:mrow><m:mi>B</m:mi>
</m:mrow>
- </m:math></inlineequation>. All four cameras had scales of the order of 0.4
arcsec/pixel, and our field sizes were around 3 arcmin.</Standard>
-<Standard>The CCD images are unfortunately not always suitable, for very poor
clusters or for clusters with large cores. Since the latter are easily studied
by other means, we augmented our own CCD profiles by collecting from the
literature a number of star-count profiles <biblioref endterm="kin68" />,
<biblioref endterm="pet76" />, <biblioref endterm="har84" />, <biblioref
endterm="ort85" />, as well as photoelectric profiles <biblioref
endterm="kin66" />, <biblioref endterm="kin75" /> and electronographic profiles
<biblioref endterm="kro84" />. In a few cases we judged normality by eye
estimates on one of the Sky Surveys.</Standard>
+ </m:math></inlineequation>. All four cameras had scales of the order of 0.4
arcsec/pixel, and our field sizes were around 3 arcmin.</para>
+<para>The CCD images are unfortunately not always suitable, for very poor
clusters or for clusters with large cores. Since the latter are easily studied
by other means, we augmented our own CCD profiles by collecting from the
literature a number of star-count profiles <biblioref endterm="kin68" />,
<biblioref endterm="pet76" />, <biblioref endterm="har84" />, <biblioref
endterm="ort85" />, as well as photoelectric profiles <biblioref
endterm="kin66" />, <biblioref endterm="kin75" /> and electronographic profiles
<biblioref endterm="kro84" />. In a few cases we judged normality by eye
estimates on one of the Sky Surveys.</para>
</section>
<section>
<title>Helicity Amplitudes</title>
-<Standard>It has been realized that helicity amplitudes provide a convenient
means for Feynman diagram<footnote><para>Footnotes can be inserted like
this.</para>
-</footnote> evaluations. These amplitude-level techniques are particularly
convenient for calculations involving many Feynman diagrams, where the usual
trace techniques for the amplitude squared becomes unwieldy. Our calculations
use the helicity techniques developed by other authors <biblioref
endterm="hag86" />; we briefly summarize below.</Standard>
+<para>It has been realized that helicity amplitudes provide a convenient means
for Feynman diagram<footnote><para>Footnotes can be inserted like this.</para>
+</footnote> evaluations. These amplitude-level techniques are particularly
convenient for calculations involving many Feynman diagrams, where the usual
trace techniques for the amplitude squared becomes unwieldy. Our calculations
use the helicity techniques developed by other authors <biblioref
endterm="hag86" />; we briefly summarize below.</para>
<section>
<title>Formalism</title>
-<Standard><anchor xml:id="bozomath" /></Standard>
-<Standard>A tree-level amplitude in <inlineequation><alt
role='tex'>e^{+}e^{-}</alt>
+<para><anchor xml:id="bozomath" /></para>
+<para>A tree-level amplitude in <inlineequation><alt
role='tex'>e^{+}e^{-}</alt>
<m:math>
<m:mrow>
@@ -293,9 +293,9 @@
</m:mrow>
</m:msubsup>
</m:mrow>
- </m:math></inlineequation> may be formed from particle four-momenta,
gauge-boson polarization vectors or fermion strings with an uncontracted
Lorentz index associated with final-state fermions.</Standard>
+ </m:math></inlineequation> may be formed from particle four-momenta,
gauge-boson polarization vectors or fermion strings with an uncontracted
Lorentz index associated with final-state fermions.</para>
<NoteToEditor>Figures 1 and 2 should appear side-by-side in
print</NoteToEditor>
-<Standard>In the chiral representation the <inlineequation><alt
role='tex'>\gamma</alt>
+<para>In the chiral representation the <inlineequation><alt
role='tex'>\gamma</alt>
<m:math>
<m:mrow><m:mi>γ</m:mi>
@@ -499,8 +499,8 @@
</m:math></informalequation> The spinors are expressed in terms of
two-component Weyl spinors as <informalequation><alt
role='tex'>u=\left(\begin{array}{c}
(u)_{-}\\
(u)_{+}
-\end{array}\right),v={\textbf{(}}\vdag_{+}{\textbf{,}}\vdag_{-}{\textbf{)}}.</alt>MathML
export failed. Please report this as a bug.</informalequation></Standard>
-<Standard>The Weyl spinors are given in terms of helicity eigenstates
<inlineequation><alt role='tex'>\chi_{\lambda}(p)</alt>
+\end{array}\right),v={\textbf{(}}\vdag_{+}{\textbf{,}}\vdag_{-}{\textbf{)}}.</alt>MathML
export failed. Please report this as a bug.</informalequation></para>
+<para>The Weyl spinors are given in terms of helicity eigenstates
<inlineequation><alt role='tex'>\chi_{\lambda}(p)</alt>
<m:math>
<m:mrow>
@@ -523,7 +523,7 @@
<m:mrow><m:mi>λ</m:mi><m:mo>=</m:mo><m:mo>±</m:mo><m:mn>1</m:mn>
</m:mrow>
</m:mrow>
- </m:math></inlineequation> by </Standard>
+ </m:math></inlineequation> by </para>
<MathLetters>
<informalequation><alt role='tex'>u(p,\lambda)_{\pm} & = &
(E\pm\lambda|{\textbf{p}}|)^{1/2}\chi_{\lambda}(p),\\
v(p,\lambda)_{\pm} & = &
\pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi_{-\lambda}(p)
@@ -618,7 +618,7 @@ v(p,\lambda)_{\pm} & = &
\pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi
</section>
<section>
<title>Floating material and so forth</title>
-<Standard>Consider a task that computes profile parameters for a modified
Lorentzian of the form <informalequation><alt
role='tex'>I=\frac{1}{1+d_{1}^{P(1+d_{2})}}</alt>
+<para>Consider a task that computes profile parameters for a modified
Lorentzian of the form <informalequation><alt
role='tex'>I=\frac{1}{1+d_{1}^{P(1+d_{2})}}</alt>
<m:math>
<m:mrow>
@@ -809,8 +809,8 @@ v(p,\lambda)_{\pm} & = &
\pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi
<m:mo>cos</m:mo><m:mo>Θ</m:mo>
</m:mrow>
</m:mrow>
- </m:math></informalequation></Standard>
-<Standard>In these expressions <inlineequation><alt role='tex'>x_{0}</alt>
+ </m:math></informalequation></para>
+<para>In these expressions <inlineequation><alt role='tex'>x_{0}</alt>
<m:math>
<m:mrow>
@@ -866,7 +866,7 @@ v(p,\lambda)_{\pm} & = &
\pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi
</m:mrow>
</m:mfrac>
</m:mrow>
- </m:math></inlineequation> of the electronically submitted abstracts for AAS
meetings are error-free. </Standard>
+ </m:math></inlineequation> of the electronically submitted abstracts for AAS
meetings are error-free. </para>
<Acknowledgements>We are grateful to V. Barger, T. Han, and R. J. N. Phillips
for doing the math in section <xref linkend="bozomath" />. More
information on the AASTeX macros package are available at <link
xlink:href="http://www.aas.org/publications/aastex";>http://www.aas.org/publications/aastex</link>
or the <link xlink:href="ftp://www.aas.org/pubs/AAS ftp site">AAS ftp
site</link>.</Acknowledgements>
<Software>IRAF, AIPS, Astropy, ...</Software>
<Appendix></Appendix>
diff --git a/lib/layouts/aastex.layout b/lib/layouts/aastex.layout
index 4da62d8..854b6b5 100644
--- a/lib/layouts/aastex.layout
+++ b/lib/layouts/aastex.layout
@@ -60,7 +60,7 @@ End
Style Standard
- Category MainText
+ Category MainText
Margin Static
LatexType Paragraph
LatexName dummy
@@ -69,6 +69,7 @@ Style Standard
Align Block
AlignPossible Block, Left, Right, Center
LabelType No_Label
+ DocBookTag para
End
diff --git a/lib/layouts/aastex6.layout b/lib/layouts/aastex6.layout
index 6153ea5..1c6054a 100644
--- a/lib/layouts/aastex6.layout
+++ b/lib/layouts/aastex6.layout
@@ -67,7 +67,7 @@ Style Software
LabelFont
Shape Italic
EndFont
-
+ DocBookTag application
End
# other new commands are mainly for the user preamble
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