articleexamplesdir = $(pkgdatadir)/examples/Articles
dist_articleexamples_DATA = \
examples/Articles/Astronomy_%26_Astrophysics.lyx \
- examples/Articles/American_Astronomical_Society_%28AASTeX_v._631%29.lyx \
+ examples/Articles/American_Astronomical_Society_%28AASTeX_v._6.3.1%29.lyx \
examples/Articles/American_Chemical_Society_%28ACS%29.lyx \
examples/Articles/American_Mathematical_Society_%28AMS%29.lyx
articletemplatesdir = $(pkgdatadir)/templates/Articles
dist_articletemplates_DATA = \
- templates/Articles/American_Astronomical_Society_%28AASTeX_v._631%29.lyx \
+ templates/Articles/American_Astronomical_Society_%28AASTeX_v._6.3.1%29.lyx \
templates/Articles/American_Economic_Association_%28AEA%29.lyx \
templates/Articles/American_Psychological_Association_%28APA%29.lyx \
templates/Articles/American_Psychological_Association_%28APA%29,_v._7.lyx \
--- /dev/null
+#LyX 2.4 created this file. For more info see https://www.lyx.org/
+\lyxformat 620
+\begin_document
+\begin_header
+\save_transient_properties true
+\origin unavailable
+\textclass aastex63
+\begin_preamble
+\newcommand{\myemail}{skywalker@galaxy.far.far.away}
+%\slugcomment{Not to appear in Nonlearned J., 45.}
+\shorttitle{Djorgovski et al.}
+\shortauthors{Collapsed Cores in Globular Clusters}
+\end_preamble
+\use_default_options true
+\maintain_unincluded_children no
+\language english
+\language_package default
+\inputencoding utf8
+\fontencoding auto
+\font_roman "default" "default"
+\font_sans "default" "default"
+\font_typewriter "default" "default"
+\font_math "auto" "auto"
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+\font_sc false
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+\font_sans_osf false
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+\font_tt_scale 100 100
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+\bibtex_command default
+\index_command default
+\float_placement class
+\float_alignment class
+\paperfontsize default
+\spacing single
+\use_hyperref false
+\papersize default
+\use_geometry false
+\use_package amsmath 1
+\use_package amssymb 1
+\use_package cancel 1
+\use_package esint 1
+\use_package mathdots 1
+\use_package mathtools 1
+\use_package mhchem 1
+\use_package stackrel 1
+\use_package stmaryrd 1
+\use_package undertilde 1
+\cite_engine natbib
+\cite_engine_type authoryear
+\biblio_style plain
+\use_bibtopic false
+\use_indices false
+\paperorientation portrait
+\suppress_date false
+\justification true
+\use_refstyle 0
+\use_formatted_ref 0
+\use_minted 0
+\use_lineno 0
+\index Index
+\shortcut idx
+\color #008000
+\end_index
+\secnumdepth 3
+\tocdepth 0
+\paragraph_separation indent
+\paragraph_indentation default
+\is_math_indent 0
+\math_numbering_side default
+\quotes_style english
+\dynamic_quotes 0
+\papercolumns 1
+\papersides 1
+\paperpagestyle default
+\tablestyle default
+\tracking_changes false
+\output_changes false
+\change_bars false
+\postpone_fragile_content false
+\html_math_output 0
+\html_css_as_file 0
+\html_be_strict false
+\docbook_table_output 0
+\docbook_mathml_prefix 1
+\end_header
+
+\begin_body
+
+\begin_layout Standard
+\begin_inset Note Note
+status open
+
+\begin_layout Plain Layout
+\noindent
+\align left
+Sample document for contributions to journals of the American Astronomical Society (AAS).
+ Please consult the
+\begin_inset CommandInset href
+LatexCommand href
+name "AASTeX user guide"
+target "http://journals.aas.org/authors/aastex/aasguide.html"
+literal "false"
+
+\end_inset
+
+ for details on how to use AASTeX.
+
+\end_layout
+
+\begin_layout Plain Layout
+\noindent
+\align left
+An up-to-date sample LaTeX article using AASTeX is available under
+\begin_inset Flex URL
+status open
+
+\begin_layout Plain Layout
+
+http://journals.aas.org/authors/aastex/aastex.html#_download
+\end_layout
+
+\end_inset
+
+.
+\end_layout
+
+\end_inset
+
+
+\begin_inset Note Note
+status open
+
+\begin_layout Plain Layout
+\noindent
+\align left
+The AASTeX document class uses a different name since version 6.0 (2016/02/16).
+ Depending on the version installed on your system,
+ set the document class to American Astronomical Society (AASTeX v.
+ 6) or American Astronomical Society (AASTeX v.
+ 5).
+
+\end_layout
+
+\begin_layout Plain Layout
+\noindent
+\align left
+New features (cf.
+
+\begin_inset Flex URL
+status collapsed
+
+\begin_layout Plain Layout
+
+http://journals.aas.org/authors/aastex/revisionhistory.html
+\end_layout
+
+\end_inset
+
+) are only partially supported by LyX (see
+\begin_inset Flex URL
+status collapsed
+
+\begin_layout Plain Layout
+
+https://www.lyx.org/trac/ticket/10027
+\end_layout
+
+\end_inset
+
+).
+\end_layout
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Title
+Collapsed Cores in Globular Clusters,
+ Gauge-Boson Couplings,
+ and AAS\SpecialChar TeX
+ Examples
+\end_layout
+
+\begin_layout Author
+S.
+ Djorgovski and Ivan R.
+ King
+\end_layout
+
+\begin_layout Affiliation
+Astronomy Department,
+ University of California,
+ Berkeley,
+ CA 94720
+\end_layout
+
+\begin_layout Altaffilation
+Visiting Astronomer
+\begin_inset Newline newline
+\end_inset
+
+ Cerro Tololo Inter-American Observatory.
+\begin_inset Newline newline
+\end_inset
+
+CTIO is operated by AURA Inc.
+\begin_inset space \space{}
+\end_inset
+
+under contract to the National Science Foundation.
+\end_layout
+
+\begin_layout Altaffilation
+Society of Fellows,
+ Harvard University.
+\end_layout
+
+\begin_layout Altaffilation
+present address:
+ Center for Astrophysics
+\begin_inset Newline newline
+\end_inset
+
+60 Garden Street,
+ Cambridge,
+ MA 02138
+\end_layout
+
+\begin_layout Author
+C.
+ D.
+ Biemesderfer
+\end_layout
+
+\begin_layout Affiliation
+National Optical Astronomy Observatories,
+ Tucson,
+ AZ 85719
+\end_layout
+
+\begin_layout Altaffilation
+Visiting Programmer,
+ Space Telescope Science Institute
+\end_layout
+
+\begin_layout Altaffilation
+Patron,
+ Alonso's Bar and Grill
+\end_layout
+
+\begin_layout Email
+aastex-help@aas.org
+\end_layout
+
+\begin_layout Author
+R.
+ J.
+ Hanisch
+\end_layout
+
+\begin_layout Affiliation
+Space Telescope Science Institute,
+ Baltimore,
+ MD 21218
+\end_layout
+
+\begin_layout Altaffilation
+Patron,
+ Alonso's Bar and Grill
+\end_layout
+
+\begin_layout Abstract
+This is a preliminary report on surface photometry of the major fraction of known globular clusters,
+ to see which of them show the signs of a collapsed core.
+ We also explore some diversionary mathematics and recreational tables.
+
+\end_layout
+
+\begin_layout Keywords
+clusters:
+ globular,
+ peanut—
+bosons:
+ bozos
+\end_layout
+
+\begin_layout Section
+Introduction
+\end_layout
+
+\begin_layout Standard
+A focal problem today in the dynamics of globular clusters is core collapse.
+ It has been predicted by theory for decades
+\begin_inset CommandInset citation
+LatexCommand citep
+key "hen61,lyn68,spi85"
+literal "false"
+
+\end_inset
+
+,
+ but observation has been less alert to the phenomenon.
+ For many years the central brightness peak in M15
+\begin_inset CommandInset citation
+LatexCommand citep
+key "kin75,new78"
+literal "false"
+
+\end_inset
+
+ seemed a unique anomaly.
+ Then
+\begin_inset CommandInset citation
+LatexCommand citep
+key "aur82"
+literal "false"
+
+\end_inset
+
+ suggested a central peak in NGC 6397,
+ and a limited photographic survey of ours
+\begin_inset CommandInset citation
+LatexCommand citep
+after "Paper I"
+key "djo84"
+literal "false"
+
+\end_inset
+
+ found three more cases,
+ including NGC 6624,
+ whose sharp center had often been remarked on
+\begin_inset CommandInset citation
+LatexCommand citep
+key "can78"
+literal "false"
+
+\end_inset
+
+.
+
+\end_layout
+
+\begin_layout Section
+Observations
+\end_layout
+
+\begin_layout Standard
+All our observations were short direct exposures with CCD's.
+ At Lick Observatory we used a TI 500
+\begin_inset Formula $\times$
+\end_inset
+
+500 chip and a GEC 575
+\begin_inset Formula $\times$
+\end_inset
+
+385,
+ on the 1-m Nickel reflector.
+ The only filter available at Lick was red.
+ At CTIO we used a GEC 575
+\begin_inset Formula $\times$
+\end_inset
+
+385,
+ with
+\begin_inset Formula $B,V,$
+\end_inset
+
+ and
+\begin_inset Formula $R$
+\end_inset
+
+ filters,
+ and an RCA 512
+\begin_inset Formula $\times$
+\end_inset
+
+320,
+ with
+\begin_inset Formula $U,B,V,R,$
+\end_inset
+
+ and
+\begin_inset Formula $I$
+\end_inset
+
+ filters,
+ on the 1.5-m reflector.
+ In the CTIO observations we tried to concentrate on the shortest practicable wavelengths;
+ but faintness,
+ reddening,
+ and poor short-wavelength sensitivity often kept us from observing in
+\begin_inset Formula $U$
+\end_inset
+
+ or even in
+\begin_inset Formula $B$
+\end_inset
+
+.
+ All four cameras had scales of the order of 0.4 arcsec/pixel,
+ and our field sizes were around 3 arcmin.
+\end_layout
+
+\begin_layout 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
+\begin_inset CommandInset citation
+LatexCommand citep
+key "kin68,pet76,har84,ort85"
+literal "false"
+
+\end_inset
+
+,
+ as well as photoelectric profiles
+\begin_inset CommandInset citation
+LatexCommand citep
+key "kin66,kin75"
+literal "false"
+
+\end_inset
+
+ and electronographic profiles
+\begin_inset CommandInset citation
+LatexCommand citep
+key "kro84"
+literal "false"
+
+\end_inset
+
+.
+ In a few cases we judged normality by eye estimates on one of the Sky Surveys.
+\end_layout
+
+\begin_layout Section
+Helicity Amplitudes
+\end_layout
+
+\begin_layout Standard
+It has been realized that helicity amplitudes provide a convenient means for Feynman diagram
+\begin_inset Foot
+status collapsed
+
+\begin_layout Plain Layout
+Footnotes can be inserted like this.
+\end_layout
+
+\end_inset
+
+ 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
+\begin_inset CommandInset citation
+LatexCommand cite
+key "hag86"
+literal "true"
+
+\end_inset
+
+;
+ we briefly summarize below.
+\end_layout
+
+\begin_layout Subsection
+Formalism
+\end_layout
+
+\begin_layout Standard
+\begin_inset CommandInset label
+LatexCommand label
+name "bozomath"
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Standard
+A tree-level amplitude in
+\begin_inset Formula $e^{+}e^{-}$
+\end_inset
+
+ collisions can be expressed in terms of fermion strings of the form
+\begin_inset Formula
+\begin{equation}
+\bar{v}(p_{2},\sigma_{2})P_{-\tau}\hat{a}_{1}\hat{a}_{2}\cdots\hat{a}_{n}u(p_{1},\sigma_{1}),
+\end{equation}
+
+\end_inset
+
+ where
+\begin_inset Formula $p$
+\end_inset
+
+ and
+\begin_inset Formula $\sigma$
+\end_inset
+
+ label the initial
+\begin_inset Formula $e^{\pm}$
+\end_inset
+
+ four-momenta and helicities
+\begin_inset Formula $(\sigma=\pm1)$
+\end_inset
+
+,
+
+\begin_inset Formula $\hat{a}_{i}=a_{i}^{\mu}\gamma_{\nu}$
+\end_inset
+
+ and
+\begin_inset Formula $P_{\tau}=\frac{1}{2}(1+\tau\gamma_{5})$
+\end_inset
+
+ is a chirality projection operator
+\begin_inset Formula $(\tau=\pm1)$
+\end_inset
+
+.
+ The
+\begin_inset Formula $a_{i}^{\mu}$
+\end_inset
+
+ may be formed from particle four-momenta,
+ gauge-boson polarization vectors or fermion strings with an uncontracted Lorentz index associated with final-state fermions.
+\end_layout
+
+\begin_layout NoteToEditor
+Figures 1 and 2 should appear side-by-side in print
+\end_layout
+
+\begin_layout Standard
+In the chiral representation the
+\begin_inset Formula $\gamma$
+\end_inset
+
+ matrices are expressed in terms of
+\begin_inset Formula $2\times2$
+\end_inset
+
+ Pauli matrices
+\begin_inset Formula $\sigma$
+\end_inset
+
+ and the unit matrix 1 as
+\begin_inset Formula
+\begin{eqnarray*}
+\gamma^{\mu} & = & \left(\begin{array}{cc}
+0 & \sigma_{+}^{\mu}\\
+\sigma_{-}^{\mu} & 0
+\end{array}\right),\gamma^{5}=\left(\begin{array}{cc}
+-1 & 0\\
+0 & 1
+\end{array}\right),\\
+\sigma_{\pm}^{\mu} & = & (\textbf{1},\pm\sigma),
+\end{eqnarray*}
+
+\end_inset
+
+ giving
+\begin_inset Formula
+\begin{equation}
+\hat{a}=\left(\begin{array}{cc}
+0 & (\hat{a})_{+}\\
+(\hat{a})_{-} & 0
+\end{array}\right),(\hat{a})_{\pm}=a_{\mu}\sigma_{\pm}^{\mu},
+\end{equation}
+
+\end_inset
+
+ The spinors are expressed in terms of two-component Weyl spinors as
+\begin_inset Formula
+\begin{equation}
+u=\left(\begin{array}{c}
+(u)_{-}\\
+(u)_{+}
+\end{array}\right),v=\textbf{(}v_{+}^{\dagger}\textbf{,}v_{-}^{\dagger}\textbf{)}.
+\end{equation}
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Standard
+The Weyl spinors are given in terms of helicity eigenstates
+\begin_inset Formula $\chi_{\lambda}(p)$
+\end_inset
+
+ with
+\begin_inset Formula $\lambda=\pm1$
+\end_inset
+
+ by
+\end_layout
+
+\begin_layout MathLetters
+\begin_inset Formula
+\begin{eqnarray}
+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)
+\end{eqnarray}
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Section
+Floating material and so forth
+\end_layout
+
+\begin_layout Standard
+Consider a task that computes profile parameters for a modified Lorentzian of the form
+\begin_inset Formula
+\begin{equation}
+I=\frac{1}{1+d_{1}^{P(1+d_{2})}}
+\end{equation}
+
+\end_inset
+
+ where
+\begin_inset Formula
+\[
+d_{1}=\sqrt{\left(\begin{array}{c}
+\frac{x_{1}}{R_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c}
+\frac{y_{1}}{R_{min}}\end{array}\right)^{2}}
+\]
+
+\end_inset
+
+
+\begin_inset Formula
+\[
+d_{2}=\sqrt{\left(\begin{array}{c}
+\frac{x_{1}}{PR_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c}
+\case{y_{1}}{PR_{min}}\end{array}\right)^{2}}
+\]
+
+\end_inset
+
+
+\begin_inset Formula
+\[
+x_{1}=(x-x_{0})\cos\Theta+(y-y_{0})\sin\Theta
+\]
+
+\end_inset
+
+
+\begin_inset Formula
+\[
+y_{1}=-(x-x_{0})\sin\Theta+(y-y_{0})\cos\Theta
+\]
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Standard
+In these expressions
+\begin_inset Formula $x_{0}$
+\end_inset
+
+,
+\begin_inset Formula $y_{0}$
+\end_inset
+
+ is the star center,
+ and
+\begin_inset Formula $\Theta$
+\end_inset
+
+ is the angle with the
+\begin_inset Formula $x$
+\end_inset
+
+ axis.
+ Results of this task are shown in table
+\begin_inset space ~
+\end_inset
+
+
+\begin_inset CommandInset ref
+LatexCommand ref
+reference "tbl-2"
+nolink "false"
+
+\end_inset
+
+.
+ It is not clear how these sorts of analyses may affect determination of
+\begin_inset Formula $M_{\text{\sun}}$
+\end_inset
+
+,
+ but the assumption is that the alternate results should be less than 90° out of phase with previous values.
+ We have no observations of
+\begin_inset Preview
+
+\begin_layout Standard
+\begin_inset ERT
+status open
+
+\begin_layout Plain Layout
+
+
+\backslash
+ion{Ca}{2}
+\end_layout
+
+\end_inset
+
+
+\end_layout
+
+\end_inset
+
+.
+ Roughly
+\begin_inset Formula $\nicefrac{4}{5}$
+\end_inset
+
+ of the electronically submitted abstracts for AAS meetings are error-free.
+
+\end_layout
+
+\begin_layout Acknowledgments
+We are grateful to V.
+ Barger,
+ T.
+ Han,
+ and R.
+ J.
+ N.
+ Phillips for doing the math in section
+\begin_inset space ~
+\end_inset
+
+
+\begin_inset CommandInset ref
+LatexCommand ref
+reference "bozomath"
+nolink "false"
+
+\end_inset
+
+.
+ More information on the AAS\SpecialChar TeX
+ macros package are available at
+\begin_inset Flex URL
+status collapsed
+
+\begin_layout Plain Layout
+
+http://www.aas.org/publications/aastex
+\end_layout
+
+\end_inset
+
+ or the
+\begin_inset CommandInset href
+LatexCommand href
+name "AAS ftp site"
+target "ftp://www.aas.org/pubs/AAS ftp site"
+literal "false"
+
+\end_inset
+
+.
+\end_layout
+
+\begin_layout Software
+IRAF,
+ AIPS,
+ Astropy,
+ ...
+\end_layout
+
+\begin_layout Appendix
+
+\end_layout
+
+\begin_layout Section
+Appendicial material
+\end_layout
+
+\begin_layout Standard
+Consider once again a task that computes profile parameters for a modified Lorentzian of the form
+\begin_inset Formula
+\begin{equation}
+I=\frac{1}{1+d_{1}^{P(1+d_{2})}}
+\end{equation}
+
+\end_inset
+
+ where
+\end_layout
+
+\begin_layout MathLetters
+\begin_inset Formula
+\[
+d_{1}=\frac{3}{4}\sqrt{\left(\begin{array}{c}
+\frac{x_{1}}{R_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c}
+\frac{y_{1}}{R_{min}}\end{array}\right)^{2}}
+\]
+
+\end_inset
+
+
+\begin_inset Formula
+\begin{equation}
+d_{2}=\case{3}{4}\sqrt{\left(\begin{array}{c}
+\frac{x_{1}}{PR_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c}
+\case{y_{1}}{PR_{min}}\end{array}\right)^{2}}
+\end{equation}
+
+\end_inset
+
+
+\begin_inset Formula
+\begin{eqnarray}
+x_{1} & = & (x-x_{0})\cos\Theta+(y-y_{0})\sin\Theta\\
+y_{1} & = & -(x-x_{0})\sin\Theta+(y-y_{0})\cos\Theta
+\end{eqnarray}
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Standard
+For completeness,
+ here is one last equation.
+
+\begin_inset Formula
+\begin{equation}
+e=mc^{2}
+\end{equation}
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Bibliography
+\begin_inset CommandInset bibitem
+LatexCommand bibitem
+label "Auri\\`ere(1982)"
+key "aur82"
+literal "true"
+
+\end_inset
+
+Aurière,
+ M.
+ 1982,
+
+\begin_inset ERT
+status collapsed
+
+\begin_layout Plain Layout
+
+
+\backslash
+aap
+\end_layout
+
+\end_inset
+
+,
+ 109,
+ 301
+\end_layout
+
+\begin_layout Bibliography
+\begin_inset CommandInset bibitem
+LatexCommand bibitem
+label "Canizares et al.(1978)"
+key "can78"
+literal "true"
+
+\end_inset
+
+Canizares,
+ C.
+ R.,
+ Grindlay,
+ J.
+ E.,
+ Hiltner,
+ W.
+ A.,
+ Liller,
+ W.,
+ and McClintock,
+ J.
+ E.
+ 1978,
+
+\begin_inset ERT
+status collapsed
+
+\begin_layout Plain Layout
+
+
+\backslash
+apj
+\end_layout
+
+\end_inset
+
+,
+ 224,
+ 39
+\end_layout
+
+\begin_layout Bibliography
+\begin_inset CommandInset bibitem
+LatexCommand bibitem
+label "Djorgovski and King(1984)"
+key "djo84"
+literal "true"
+
+\end_inset
+
+Djorgovski,
+ S.,
+ and King,
+ I.
+ R.
+ 1984,
+
+\begin_inset Preview
+
+\begin_layout Standard
+\begin_inset ERT
+status open
+
+\begin_layout Plain Layout
+
+
+\backslash
+apjl
+\end_layout
+
+\end_inset
+
+
+\end_layout
+
+\end_inset
+
+,
+ 277,
+ L49
+\end_layout
+
+\begin_layout Bibliography
+\begin_inset CommandInset bibitem
+LatexCommand bibitem
+label "Hagiwara and Zeppenfeld(1986)"
+key "hag86"
+literal "true"
+
+\end_inset
+
+Hagiwara,
+ K.,
+ and Zeppenfeld,
+ D.
+ 1986,
+ Nucl.Phys.,
+ 274,
+ 1
+\end_layout
+
+\begin_layout Bibliography
+\begin_inset CommandInset bibitem
+LatexCommand bibitem
+label "Harris and van den Bergh(1984)"
+key "har84"
+literal "true"
+
+\end_inset
+
+Harris,
+ W.
+ E.,
+ and van den Bergh,
+ S.
+ 1984,
+
+\begin_inset ERT
+status collapsed
+
+\begin_layout Plain Layout
+
+
+\backslash
+aj
+\end_layout
+
+\end_inset
+
+,
+ 89,
+ 1816
+\end_layout
+
+\begin_layout Bibliography
+\begin_inset CommandInset bibitem
+LatexCommand bibitem
+label "H\\`enon(1961)"
+key "hen61"
+literal "true"
+
+\end_inset
+
+Hénon,
+ M.
+ 1961,
+ Ann.d'Ap.,
+ 24,
+ 369
+\end_layout
+
+\begin_layout Bibliography
+\begin_inset CommandInset bibitem
+LatexCommand bibitem
+label "King(1966)"
+key "kin66"
+literal "true"
+
+\end_inset
+
+King,
+ I.
+ R.
+ 1966,
+
+\begin_inset ERT
+status collapsed
+
+\begin_layout Plain Layout
+
+
+\backslash
+aj
+\end_layout
+
+\end_inset
+
+,
+ 71,
+ 276
+\end_layout
+
+\begin_layout Bibliography
+\begin_inset CommandInset bibitem
+LatexCommand bibitem
+label "King(1975)"
+key "kin75"
+literal "true"
+
+\end_inset
+
+King,
+ I.
+ R.
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+<cell alignment="right" valignment="top" usebox="none">
+\begin_inset Text
+
+\begin_layout Plain Layout
+315.2
+\end_layout
+
+\end_inset
+</cell>
+<cell alignment="right" valignment="top" usebox="none">
+\begin_inset Text
+
+\begin_layout Plain Layout
+ 3.433
+\end_layout
+
+\end_inset
+</cell>
+<cell alignment="right" valignment="top" usebox="none">
+\begin_inset Text
+
+\begin_layout Plain Layout
+3.075
+\end_layout
+
+\end_inset
+</cell>
+<cell alignment="right" valignment="top" usebox="none">
+\begin_inset Text
+
+\begin_layout Plain Layout
+7.488
+\end_layout
+
+\end_inset
+</cell>
+<cell alignment="right" valignment="top" usebox="none">
+\begin_inset Text
+
+\begin_layout Plain Layout
+92.1
+\end_layout
+
+\end_inset
+</cell>
+<cell alignment="right" valignment="top" usebox="none">
+\begin_inset Text
+
+\begin_layout Plain Layout
+25.3
+\end_layout
+
+\end_inset
+</cell>
+<cell alignment="right" valignment="top" usebox="none">
+\begin_inset Text
+
+\begin_layout Plain Layout
+-12.052
+\end_layout
+
+\end_inset
+</cell>
+<cell alignment="right" valignment="top" usebox="none">
+\begin_inset Text
+
+\begin_layout Plain Layout
+8
+\end_layout
+
+\end_inset
+</cell>
+</row>
+</lyxtabular>
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Table note
+a
+\begin_inset ERT
+status collapsed
+
+\begin_layout Plain Layout
+
+}{
+\end_layout
+
+\end_inset
+
+Sample footnote for table
+\begin_inset space ~
+\end_inset
+
+
+\begin_inset CommandInset ref
+LatexCommand ref
+reference "tbl-2"
+nolink "false"
+
+\end_inset
+
+ that was generated with the \SpecialChar LaTeX
+ table environment
+\end_layout
+
+\begin_layout Table note
+b
+\begin_inset ERT
+status collapsed
+
+\begin_layout Plain Layout
+
+}{
+\end_layout
+
+\end_inset
+
+Yet another sample footnote for table
+\begin_inset space ~
+\end_inset
+
+
+\begin_inset CommandInset ref
+LatexCommand ref
+reference "tbl-2"
+nolink "false"
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Table note
+c
+\begin_inset ERT
+status collapsed
+
+\begin_layout Plain Layout
+
+}{
+\end_layout
+
+\end_inset
+
+Another sample footnote for table
+\begin_inset space ~
+\end_inset
+
+
+\begin_inset CommandInset ref
+LatexCommand ref
+reference "tbl-2"
+nolink "false"
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout TableComments
+We can also attach a long-ish paragraph of explanatory material to a table.
+ Use
+\backslash
+tablerefs to append a list of references.
+ The following references were from a different table:
+ I've patched them in here to show how they look,
+ but don't take them too seriously—
+I certainly have not.
+\end_layout
+
+\begin_layout TableRefs
+(1) Barbuy,
+ Spite,
+ & Spite 1985;
+ (2) Bond 1980;
+ (3) Carbon et al.
+ 1987;
+ (4) Hobbs & Duncan 1987;
+ (5) Gilroy et al.
+ 1988:
+ (6) Gratton & Ortolani 1986;
+ (7) Gratton & Sneden 1987;
+ (8) Gratton & Sneden (1988);
+ (9) Gratton & Sneden 1991;
+ (10) Kraft et al.
+ 1982;
+ (11) LCL,
+ or Laird,
+ 1990;
+ (12) Leep & Wallerstein 1981;
+ (13) Luck & Bond 1981;
+ (14) Luck & Bond 1985;
+ (15) Magain 1987;
+ (16) Magain 1989;
+ (17) Peterson 1981;
+ (18) Peterson,
+ Kurucz,
+ & Carney 1990;
+ (19) RMB;
+ (20) Schuster & Nissen 1988;
+ (21) Schuster & Nissen 1989b;
+ (22) Spite et al.
+ 1984;
+ (23) Spite & Spite 1986;
+ (24) Hobbs & Thorburn 1991;
+ (25) Hobbs et al.
+ 1991;
+ (26) Olsen 1983.
+\end_layout
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Standard
+\begin_inset Note Note
+status open
+
+\begin_layout Plain Layout
+LyX can load deluxetable files verbatim.
+ To see this in action,
+ dissolve the following Note and copy the file table.tex from the AASTeX 5.0 distribution into the same directory as this file.
+\end_layout
+
+\end_inset
+
+
+\end_layout
+
+\begin_layout Standard
+\begin_inset Note Note
+status open
+
+\begin_layout Plain Layout
+\begin_inset CommandInset include
+LatexCommand input
+filename "table"
+literal "true"
+
+\end_inset
+
+
+\end_layout
+
+\end_inset
+
+
+\end_layout
+
+\end_body
+\end_document
+++ /dev/null
-#LyX 2.4 created this file. For more info see https://www.lyx.org/
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-\save_transient_properties true
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-\newcommand{\myemail}{skywalker@galaxy.far.far.away}
-%\slugcomment{Not to appear in Nonlearned J., 45.}
-\shorttitle{Djorgovski et al.}
-\shortauthors{Collapsed Cores in Globular Clusters}
-\end_preamble
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-The AASTeX document class uses a different name since version 6.0 (2016/02/16).
- Depending on the version installed on your system,
- set the document class to American Astronomical Society (AASTeX v.
- 6) or American Astronomical Society (AASTeX v.
- 5).
-
-\end_layout
-
-\begin_layout Plain Layout
-\noindent
-\align left
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-
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-
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-\end_layout
-
-\begin_layout Title
-Collapsed Cores in Globular Clusters,
- Gauge-Boson Couplings,
- and AAS\SpecialChar TeX
- Examples
-\end_layout
-
-\begin_layout Author
-S.
- Djorgovski and Ivan R.
- King
-\end_layout
-
-\begin_layout Affiliation
-Astronomy Department,
- University of California,
- Berkeley,
- CA 94720
-\end_layout
-
-\begin_layout Altaffilation
-Visiting Astronomer
-\begin_inset Newline newline
-\end_inset
-
- Cerro Tololo Inter-American Observatory.
-\begin_inset Newline newline
-\end_inset
-
-CTIO is operated by AURA Inc.
-\begin_inset space \space{}
-\end_inset
-
-under contract to the National Science Foundation.
-\end_layout
-
-\begin_layout Altaffilation
-Society of Fellows,
- Harvard University.
-\end_layout
-
-\begin_layout Altaffilation
-present address:
- Center for Astrophysics
-\begin_inset Newline newline
-\end_inset
-
-60 Garden Street,
- Cambridge,
- MA 02138
-\end_layout
-
-\begin_layout Author
-C.
- D.
- Biemesderfer
-\end_layout
-
-\begin_layout Affiliation
-National Optical Astronomy Observatories,
- Tucson,
- AZ 85719
-\end_layout
-
-\begin_layout Altaffilation
-Visiting Programmer,
- Space Telescope Science Institute
-\end_layout
-
-\begin_layout Altaffilation
-Patron,
- Alonso's Bar and Grill
-\end_layout
-
-\begin_layout Email
-aastex-help@aas.org
-\end_layout
-
-\begin_layout Author
-R.
- J.
- Hanisch
-\end_layout
-
-\begin_layout Affiliation
-Space Telescope Science Institute,
- Baltimore,
- MD 21218
-\end_layout
-
-\begin_layout Altaffilation
-Patron,
- Alonso's Bar and Grill
-\end_layout
-
-\begin_layout Abstract
-This is a preliminary report on surface photometry of the major fraction of known globular clusters,
- to see which of them show the signs of a collapsed core.
- We also explore some diversionary mathematics and recreational tables.
-
-\end_layout
-
-\begin_layout Keywords
-clusters:
- globular,
- peanut—
-bosons:
- bozos
-\end_layout
-
-\begin_layout Section
-Introduction
-\end_layout
-
-\begin_layout Standard
-A focal problem today in the dynamics of globular clusters is core collapse.
- It has been predicted by theory for decades
-\begin_inset CommandInset citation
-LatexCommand citep
-key "hen61,lyn68,spi85"
-literal "false"
-
-\end_inset
-
-,
- but observation has been less alert to the phenomenon.
- For many years the central brightness peak in M15
-\begin_inset CommandInset citation
-LatexCommand citep
-key "kin75,new78"
-literal "false"
-
-\end_inset
-
- seemed a unique anomaly.
- Then
-\begin_inset CommandInset citation
-LatexCommand citep
-key "aur82"
-literal "false"
-
-\end_inset
-
- suggested a central peak in NGC 6397,
- and a limited photographic survey of ours
-\begin_inset CommandInset citation
-LatexCommand citep
-after "Paper I"
-key "djo84"
-literal "false"
-
-\end_inset
-
- found three more cases,
- including NGC 6624,
- whose sharp center had often been remarked on
-\begin_inset CommandInset citation
-LatexCommand citep
-key "can78"
-literal "false"
-
-\end_inset
-
-.
-
-\end_layout
-
-\begin_layout Section
-Observations
-\end_layout
-
-\begin_layout Standard
-All our observations were short direct exposures with CCD's.
- At Lick Observatory we used a TI 500
-\begin_inset Formula $\times$
-\end_inset
-
-500 chip and a GEC 575
-\begin_inset Formula $\times$
-\end_inset
-
-385,
- on the 1-m Nickel reflector.
- The only filter available at Lick was red.
- At CTIO we used a GEC 575
-\begin_inset Formula $\times$
-\end_inset
-
-385,
- with
-\begin_inset Formula $B,V,$
-\end_inset
-
- and
-\begin_inset Formula $R$
-\end_inset
-
- filters,
- and an RCA 512
-\begin_inset Formula $\times$
-\end_inset
-
-320,
- with
-\begin_inset Formula $U,B,V,R,$
-\end_inset
-
- and
-\begin_inset Formula $I$
-\end_inset
-
- filters,
- on the 1.5-m reflector.
- In the CTIO observations we tried to concentrate on the shortest practicable wavelengths;
- but faintness,
- reddening,
- and poor short-wavelength sensitivity often kept us from observing in
-\begin_inset Formula $U$
-\end_inset
-
- or even in
-\begin_inset Formula $B$
-\end_inset
-
-.
- All four cameras had scales of the order of 0.4 arcsec/pixel,
- and our field sizes were around 3 arcmin.
-\end_layout
-
-\begin_layout 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
-\begin_inset CommandInset citation
-LatexCommand citep
-key "kin68,pet76,har84,ort85"
-literal "false"
-
-\end_inset
-
-,
- as well as photoelectric profiles
-\begin_inset CommandInset citation
-LatexCommand citep
-key "kin66,kin75"
-literal "false"
-
-\end_inset
-
- and electronographic profiles
-\begin_inset CommandInset citation
-LatexCommand citep
-key "kro84"
-literal "false"
-
-\end_inset
-
-.
- In a few cases we judged normality by eye estimates on one of the Sky Surveys.
-\end_layout
-
-\begin_layout Section
-Helicity Amplitudes
-\end_layout
-
-\begin_layout Standard
-It has been realized that helicity amplitudes provide a convenient means for Feynman diagram
-\begin_inset Foot
-status collapsed
-
-\begin_layout Plain Layout
-Footnotes can be inserted like this.
-\end_layout
-
-\end_inset
-
- 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
-\begin_inset CommandInset citation
-LatexCommand cite
-key "hag86"
-literal "true"
-
-\end_inset
-
-;
- we briefly summarize below.
-\end_layout
-
-\begin_layout Subsection
-Formalism
-\end_layout
-
-\begin_layout Standard
-\begin_inset CommandInset label
-LatexCommand label
-name "bozomath"
-
-\end_inset
-
-
-\end_layout
-
-\begin_layout Standard
-A tree-level amplitude in
-\begin_inset Formula $e^{+}e^{-}$
-\end_inset
-
- collisions can be expressed in terms of fermion strings of the form
-\begin_inset Formula
-\begin{equation}
-\bar{v}(p_{2},\sigma_{2})P_{-\tau}\hat{a}_{1}\hat{a}_{2}\cdots\hat{a}_{n}u(p_{1},\sigma_{1}),
-\end{equation}
-
-\end_inset
-
- where
-\begin_inset Formula $p$
-\end_inset
-
- and
-\begin_inset Formula $\sigma$
-\end_inset
-
- label the initial
-\begin_inset Formula $e^{\pm}$
-\end_inset
-
- four-momenta and helicities
-\begin_inset Formula $(\sigma=\pm1)$
-\end_inset
-
-,
-
-\begin_inset Formula $\hat{a}_{i}=a_{i}^{\mu}\gamma_{\nu}$
-\end_inset
-
- and
-\begin_inset Formula $P_{\tau}=\frac{1}{2}(1+\tau\gamma_{5})$
-\end_inset
-
- is a chirality projection operator
-\begin_inset Formula $(\tau=\pm1)$
-\end_inset
-
-.
- The
-\begin_inset Formula $a_{i}^{\mu}$
-\end_inset
-
- may be formed from particle four-momenta,
- gauge-boson polarization vectors or fermion strings with an uncontracted Lorentz index associated with final-state fermions.
-\end_layout
-
-\begin_layout NoteToEditor
-Figures 1 and 2 should appear side-by-side in print
-\end_layout
-
-\begin_layout Standard
-In the chiral representation the
-\begin_inset Formula $\gamma$
-\end_inset
-
- matrices are expressed in terms of
-\begin_inset Formula $2\times2$
-\end_inset
-
- Pauli matrices
-\begin_inset Formula $\sigma$
-\end_inset
-
- and the unit matrix 1 as
-\begin_inset Formula
-\begin{eqnarray*}
-\gamma^{\mu} & = & \left(\begin{array}{cc}
-0 & \sigma_{+}^{\mu}\\
-\sigma_{-}^{\mu} & 0
-\end{array}\right),\gamma^{5}=\left(\begin{array}{cc}
--1 & 0\\
-0 & 1
-\end{array}\right),\\
-\sigma_{\pm}^{\mu} & = & (\textbf{1},\pm\sigma),
-\end{eqnarray*}
-
-\end_inset
-
- giving
-\begin_inset Formula
-\begin{equation}
-\hat{a}=\left(\begin{array}{cc}
-0 & (\hat{a})_{+}\\
-(\hat{a})_{-} & 0
-\end{array}\right),(\hat{a})_{\pm}=a_{\mu}\sigma_{\pm}^{\mu},
-\end{equation}
-
-\end_inset
-
- The spinors are expressed in terms of two-component Weyl spinors as
-\begin_inset Formula
-\begin{equation}
-u=\left(\begin{array}{c}
-(u)_{-}\\
-(u)_{+}
-\end{array}\right),v=\textbf{(}v_{+}^{\dagger}\textbf{,}v_{-}^{\dagger}\textbf{)}.
-\end{equation}
-
-\end_inset
-
-
-\end_layout
-
-\begin_layout Standard
-The Weyl spinors are given in terms of helicity eigenstates
-\begin_inset Formula $\chi_{\lambda}(p)$
-\end_inset
-
- with
-\begin_inset Formula $\lambda=\pm1$
-\end_inset
-
- by
-\end_layout
-
-\begin_layout MathLetters
-\begin_inset Formula
-\begin{eqnarray}
-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)
-\end{eqnarray}
-
-\end_inset
-
-
-\end_layout
-
-\begin_layout Section
-Floating material and so forth
-\end_layout
-
-\begin_layout Standard
-Consider a task that computes profile parameters for a modified Lorentzian of the form
-\begin_inset Formula
-\begin{equation}
-I=\frac{1}{1+d_{1}^{P(1+d_{2})}}
-\end{equation}
-
-\end_inset
-
- where
-\begin_inset Formula
-\[
-d_{1}=\sqrt{\left(\begin{array}{c}
-\frac{x_{1}}{R_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c}
-\frac{y_{1}}{R_{min}}\end{array}\right)^{2}}
-\]
-
-\end_inset
-
-
-\begin_inset Formula
-\[
-d_{2}=\sqrt{\left(\begin{array}{c}
-\frac{x_{1}}{PR_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c}
-\case{y_{1}}{PR_{min}}\end{array}\right)^{2}}
-\]
-
-\end_inset
-
-
-\begin_inset Formula
-\[
-x_{1}=(x-x_{0})\cos\Theta+(y-y_{0})\sin\Theta
-\]
-
-\end_inset
-
-
-\begin_inset Formula
-\[
-y_{1}=-(x-x_{0})\sin\Theta+(y-y_{0})\cos\Theta
-\]
-
-\end_inset
-
-
-\end_layout
-
-\begin_layout Standard
-In these expressions
-\begin_inset Formula $x_{0}$
-\end_inset
-
-,
-\begin_inset Formula $y_{0}$
-\end_inset
-
- is the star center,
- and
-\begin_inset Formula $\Theta$
-\end_inset
-
- is the angle with the
-\begin_inset Formula $x$
-\end_inset
-
- axis.
- Results of this task are shown in table
-\begin_inset space ~
-\end_inset
-
-
-\begin_inset CommandInset ref
-LatexCommand ref
-reference "tbl-2"
-nolink "false"
-
-\end_inset
-
-.
- It is not clear how these sorts of analyses may affect determination of
-\begin_inset Formula $M_{\text{\sun}}$
-\end_inset
-
-,
- but the assumption is that the alternate results should be less than 90° out of phase with previous values.
- We have no observations of
-\begin_inset Preview
-
-\begin_layout Standard
-\begin_inset ERT
-status open
-
-\begin_layout Plain Layout
-
-
-\backslash
-ion{Ca}{2}
-\end_layout
-
-\end_inset
-
-
-\end_layout
-
-\end_inset
-
-.
- Roughly
-\begin_inset Formula $\nicefrac{4}{5}$
-\end_inset
-
- of the electronically submitted abstracts for AAS meetings are error-free.
-
-\end_layout
-
-\begin_layout Acknowledgments
-We are grateful to V.
- Barger,
- T.
- Han,
- and R.
- J.
- N.
- Phillips for doing the math in section
-\begin_inset space ~
-\end_inset
-
-
-\begin_inset CommandInset ref
-LatexCommand ref
-reference "bozomath"
-nolink "false"
-
-\end_inset
-
-.
- More information on the AAS\SpecialChar TeX
- macros package are available at
-\begin_inset Flex URL
-status collapsed
-
-\begin_layout Plain Layout
-
-http://www.aas.org/publications/aastex
-\end_layout
-
-\end_inset
-
- or the
-\begin_inset CommandInset href
-LatexCommand href
-name "AAS ftp site"
-target "ftp://www.aas.org/pubs/AAS ftp site"
-literal "false"
-
-\end_inset
-
-.
-\end_layout
-
-\begin_layout Software
-IRAF,
- AIPS,
- Astropy,
- ...
-\end_layout
-
-\begin_layout Appendix
-
-\end_layout
-
-\begin_layout Section
-Appendicial material
-\end_layout
-
-\begin_layout Standard
-Consider once again a task that computes profile parameters for a modified Lorentzian of the form
-\begin_inset Formula
-\begin{equation}
-I=\frac{1}{1+d_{1}^{P(1+d_{2})}}
-\end{equation}
-
-\end_inset
-
- where
-\end_layout
-
-\begin_layout MathLetters
-\begin_inset Formula
-\[
-d_{1}=\frac{3}{4}\sqrt{\left(\begin{array}{c}
-\frac{x_{1}}{R_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c}
-\frac{y_{1}}{R_{min}}\end{array}\right)^{2}}
-\]
-
-\end_inset
-
-
-\begin_inset Formula
-\begin{equation}
-d_{2}=\case{3}{4}\sqrt{\left(\begin{array}{c}
-\frac{x_{1}}{PR_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c}
-\case{y_{1}}{PR_{min}}\end{array}\right)^{2}}
-\end{equation}
-
-\end_inset
-
-
-\begin_inset Formula
-\begin{eqnarray}
-x_{1} & = & (x-x_{0})\cos\Theta+(y-y_{0})\sin\Theta\\
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projects / features.git / commitdiff