The Research in Astronomy and Astrophysics (RAA) macro package is required for preparing LaTeX manuscripts. A template from https://www.raa-journal.org/sub/macro/
\begin
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\documentclass[referee]{raa} % referee version: for submission
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\usepackage{graphicx,times} %for PS/EPS graphics inclusion, new
\usepackage{natbib}
\usepackage{amssymb,amsmath}
\bibpunct{(}{)}{;}{a}{}{,}
%\usepackage[UTF8]{ctex} % Open if you want also use your Chinese name
\usepackage[pagebackref=true]{hyperref}
\begin{document}
\title{Photometry of $\delta$ Sct and Related Stars: the Results of AD Arietis
}
% \subtitle{I. Place Your Subtitle Here}
\volnopage{Vol.0 (20xx) No.0, 000--000} %%preserved for Editor. DOn't remove!
\setcounter{page}{1} %%starting page, preserved for Editor. DOn't remove!
\author{Ai-Ying Zhou %(周爱英) %% Put your Chinese name in "( )" if you like. Note to open line 11 "\usepackage[UTF8]{ctex}"
\inst{1,2}
\and E. Rodr\'{\i}guez
\inst{2}
\and B. J. Smith
\inst{3}
}
%% Here is an example of three authors come from different institutes.
%% For single author or all the authors from an institute, use "\inst{}" only
\institute{National Astronomical Observatories, Chinese Academy of Sciences,
Beijing 100012, China; {\it aiying@bao.ac.cn}\\
%% Please give the E-mail address of the author, to whom future correspondence and
%% offprint requests will be sent.
\and
Full institute address for the second author\\
\and
Full institute address for the third author\\
\vs\no
{\small Received 20xx month day; accepted 20xx month day}}
\abstract{ This paper reports on the preliminary photometric results of
$\cdots\cdots$
\keywords{techniques: photometric --- stars:
variables: $\delta$ Scuti --- stars: individual: IP Vir, YZ Boo}
}
\authorrunning{A.-Y. Zhou, E. Rodriguez \& B. J. Smith } %author_head in even pages
\titlerunning{Photometry of $\delta$ Sct and Related Stars (I) } % title_head in odd pages
\maketitle
%% The author head (on even pages) and the title head (on odd pages) will be
%% automatically extracted from \author{} and \title{}. Whenever the title is too long,
%% you will be asked to supply a shorter one by inserting either \authorrunning{} or
%% \titlerunning{} before \maketitle. Anyway, you can specify your own heads.
%%
%%
%% Note: In the following text body of your manuscript, please note several differences from
%% other major journals:
%% (1) \subsection{Please Capitalize the First Letter of Each Notional Word in Subsection Title}
%% (2) Please Capitalize the First Letter of Each Notional Word in all tables' captions
%
%________________________________________________ sections below
%
\section{Introduction} %% first-level sections will be auto-capitalized
\label{sect:intro}
In 1996, we started a project to obtain Johnson $V$ and Str\"{o}mgren
$uvby\beta$ photometry for the poorly studied variables of
``pulsational interest''~$\cdots\cdots$.
We used the three-channel high-speed photoelectric photometer designed for
the Whole Earth Telescope campaign
(\citealt{Nather+etal+1990, Jiang+Hu+1998}),
and the four-channel Chevreton photoelectric photometer
(\citealt{Michel+etal+1990, Michel+etal+1992}) dedicated to
the STEPHI (STEllar Photometry International, \citealt{Michel+etal+1992}).
%% Authors can give a citation as 'Michel et al. 1992'.
%% You may also use \cite, \citep and \citet for citation, and use Table~1 or Figure~1
%% and so forth. Using \ref and \label for cross-references of Tables/Figures
%% is a good way in adjusting/adding/removing text, tables or figures.
\section{Observations}
\label{sect:Obs}
The photometry of three $\delta$ Sct stars AD Arietis, IP Virginis and
YZ Bootis was performed from 2000 February 26 to
2001 January 31\footnote{Please note the order: year, month, day}
with the three photometers mounted on the 85-cm telescope at
the Xinglong Station of BAO\footnote{Now NAOC}.
The typical accuracy yielded from magnitude differences between
reference stars is about 0.005\,mag.
The observing log is given in $\cdots\cdots$
\section{Data reduction}
\label{sect:data}
The time-series, i.e. pairs of Heliocentric Julian Day (HJD) versus magnitude,
used for pulsation analysis can be quickly established by using
an external IRAF task (\citealt{Zhou+etal+2001}) $\cdots\cdots$
\subsection{Please Capitalize the First Letter of Each Notional Word in Subsection Title}
\subsubsection{This is a third-level section --- subsubsection}
Some applications of the routines are given in Table~\ref{Tab1}.
\subsection{De-noise in the Lower Frequency Domain}
To reduce the red-noise in the frequency region, we $\cdots\cdots$
%
% one-column-spanning table
%________________________________________ Table 1: Use_of_the routines
\begin{table}
\begin{center}
\caption[]{ Please Capitalize the First Letter of Each Notional Word
in Table's Caption.}\label{Tab1}
%%Please Capitalize the First Letter of Each Notional Word in table's caption
\begin{tabular}{clcl}
\hline\noalign{\smallskip}
No & Star & Photometer & References \\
\hline\noalign{\smallskip}
1 & GSC 2683-3076 & CCD & \cite{Zhou+etal+2001} \\ % new variable
2 & IP Vir & 4-CH & present work \\
3 & YZ Boo & 3-CH & present work \\
\noalign{\smallskip}\hline
\end{tabular}
\end{center}
\end{table}
\section{Data analysis}
\label{sect:analysis}
In this part, we analyze the pulsation contents for the three stars
with the period-search program {\sc period98}
(\citealt{Breger+1990, Sperl+1998}).
\subsection{AD Arietis}
AD Ari (=HD~14147=SAO~92873=HIP~10701, $V$=7.43\,mag,
$\Delta$$V$=0.06\,mag, P$_0$=0$\fd$2699, F0) (\citealt{Kasarovets+etal+1999, Rodriguez+etal+2000})
is suspected to be a candidate of $\gamma$ Doradus-type
pulsating variables exhibiting both $p$- and $g$-modes
in terms of its long period and late spectral type. You can cite a figure like "as shown in Figure~\ref{Fig1}" or like (Fig.~\ref{Fig2}).
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%% Examples for figures using graphicx for LaTeX 2e
%% -- our recommended way for embodying graphics
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
% A figure as large as the width of the column
%-------------------------------------------------------------
\begin{figure}
\centering
\includegraphics[width=\textwidth, angle=0]{f1.eps}
\caption{Demo1: A figure as large as the width of the column using package `graphicx'. }
\label{Fig1}
\end{figure}
%
% One column rotated figure
%-------------------------------------------------------------
\begin{figure}
\centering
\includegraphics[width=8cm, angle=-180]{f2.eps}
\caption{Demo2: One column rotated figure using package `graphicx'. }
\label{Fig2}
\end{figure}
%----------------------------------------------------- Figs 3 & 4:
\begin{figure}[h]
\begin{minipage}[t]{0.495\linewidth}
\centering
\includegraphics[width=60mm]{f1.eps}
\caption{\label{Fig3}{\small Amplitudes evolution of . . .} }
\end{minipage}%
\begin{minipage}[t]{0.495\textwidth}
\centering
\includegraphics[width=60mm]{f2.eps}
\caption{\label{Fig4}{\small Amplitude variation of AN Lyn.}}
\end{minipage}%
\end{figure}
\subsection{IP Virginis}
IP Vir ($\alpha=14^{\rm h}40^{\rm m}08^{\rm s}.0$, $\delta=00\dg
01'45''$.0,
%% $00\degr01\arcmin45\arcsec$.0,
equinox=2000.0) was reported by \cite{Landolt+1990} to be
a $\delta$ Sct-type variable $\cdots\cdots$
\subsubsection{Wavelet Analysis}
%%This part intends to show the presentation of equations for LaTeX beginners
Universally, Lebseque integration
\begin{equation}\label{eq1}
\int_{\infty}^{\infty}|h(t)|^{p} dt < \infty, ~~~~~~1\leq p < \infty
\end{equation}
presents a measurable function of $L^{p}(\Re)$. Use Equation~\eqref{eq1} to cite an equation, and you can also cite an equation like (Eq.~\eqref{eq2}).
A function $\psi \in L^{2}(\Re)$ is called an orthogonal wavelet if
\begin{equation}\label{eq2}
\langle\psi_{j,k},~\psi_{l,m}\rangle = \delta_{j,l}\cdot\delta_{k,m}, ~~~~~~j,k,l,m\in{\cal Z}
\end{equation}
$\delta_{j,k}$ is Kronecker sign and for any $f(x) \in L^{2}(\Re)$
\begin{equation}\label{eq3}
f(x)= \sum_{j,k=-\infty}^{\infty} C_{j,k} \psi_{j,k}(x)
\end{equation}
This is wavelet series representation of $f(x)$. The most simplest
example of an orthogonal wavelet is Haar function:
\begin{equation}\label{eq4}
\psi_{\rm H}(x) \equiv \left\lbrace \begin{array}{ll}~1 ~~~~~~0\leq x <0.5\\
-1 ~~~~~~0.5\leq x < 1 \\
~0 ~~~~~~x<0,~x\geq 1.
\end{array} \right.
\end{equation}
Additionally, a Mexcian hat is also a wavelet.
Similar to Fourier series, wavelet coefficients $C_{j,k}$ is given as
\begin{equation}\label{eq5}
C_{j,k}=\langle f,~\psi_{j,k} \rangle
=\int_{-\infty}^{\infty} f(x) \overline{\psi_{j,k}(x)} ~{\rm d}x
\end{equation}
and we have
\begin{equation}\label{eq6}
(W_{\psi}f)(b,a) \equiv |a|^{-\frac{1}{2}} \int_{-\infty}^{\infty} f(t)
\overline{\psi(\frac{t-b}{a})}, ~~~~~~a,~b,~f\in L^{2}(\Re),~a\neq 0
\end{equation}
If $\psi,~\hat{\psi}$ satisfy the
window function condition, then $\hat{\psi}(0)=0$ or follows $ \int_{-\infty}^{\infty}
\psi(t) dt =0 $. Mother wavelet $\psi(x)$ oscillates and decays,
preferably rapidly. The oscillation property is expressed
mathematically by insisting that wavelets integrate to zero. Wavelet
functions are constrained, by definition, to be zero outside of a
small interval. This is what makes the WT able to operate on a
finite set of data, a property which formally called ``compact
support''. Compact support means that a basic wavelet like Harr
wavelet vanishes outside of a finite interval. If a mother wavelet
is zero outside of some interval---compactly supported, then it is
the ``fastest'' decay of all. This is the reason why we name $\psi$
``wavelet''.
\section{Discussion}
\label{sect:discussion}
I would like to give my discussion on the results elsewhere.
\section{Conclusions}
\label{sect:conclusion}
The preliminary photometric results on the $\cdots\cdots$
are reported along with an introduction to
the user-compiled IRAF task $\cdots\cdots$
\begin{acknowledgements}
This work was funded by the National Natural Science Foundation of China (NSFC)
under No.11080922.
\end{acknowledgements}
\appendix %%appendicial material is supported
\section{This shows the use of appendix}
A postscript file is actually an ASCII text file (you may even edit it).
However, you need to transfer a PDF file or any compressed or packaged
file in binary mode when using FTP.
\section{What is SCI?}
SCI is the abbreviation of Science Citation Index system powered by
the Institute for Scientific Information (ISI). For details please
visit {\it http://apps.isiknowledge.com}.
\begin{thebibliography}{99}
%% you can type \apj for ApJ, \aap for A&A, \apss for Ap&SS, etc. Please consult
%% the macro chjaa.cls. You can also find them in aasguide.tex (AASTeX for ApJ, AJ, PASP)
%% Please follow the format of ChJAA's reference list
\bibitem[Breger(1990)]{Breger+1990} Breger M., 1990,
Comm. in Asteroseismology, 20, 1 (Univ. of Vienna)
\bibitem[Kasarovets et al.(1999)]{Kasarovets+etal+1999} Kasarovets A. V., Samus N. N., Durlevich O. V. et al.,
1999, \ibvs, No. 4659
\bibitem[Jiang \& Hu(1998)]{Jiang+Hu+1998} Jiang X.-J., Hu J.-Y., 1998, Acta Astron. Sin., 39, 438
\bibitem[Landolt(1990)]{Landolt+1990} Landolt A. U., 1990, \pasp, 102, 1382
\bibitem[Michel et al.(1990)]{Michel+etal+1990} Michel E., Chevreton M., Belmonte J. A., Alvarez M.,
Jiang S.-Y., 1990, In: C. Cacciari and G. Clementini, eds.,
ASP Conf. Ser., Vol.11, Confrontation between stellar pulsation and evolution,
San Francisco: ASP, p.~332
\bibitem[Michel et al.(1992)]{Michel+etal+1992} Michel E., Belmonte J. A., Alvarez M., Jiang S.-Y., Chevreton M.,
Auvergne M., Goupil M. J., Baglin A. et al., 1992, A\&A, 255,139
\bibitem[Nather et al.(1990)]{Nather+etal+1990} Nather R. E., Winget D. E., Clemens J. C. et al.,
1990, \apj, 361,309
\bibitem[Rodr\'{\i}guez et al.(2000)]{Rodriguez+etal+2000} Rodr\'{\i}guez, E., L\'{o}pez-Gonz\'{a}lez, M. J.,
L\'{o}pez de Coca P., 2000, \aaps, 144, 469
\bibitem[Sperl(1998)]{Sperl+1998} Sperl M., 1998, Comm. in Asteroseismology,
111, 1 (Univ. of Vienna)
\bibitem[Zhou et al.(2001)]{Zhou+etal+2001} Zhou A.-Y., Rodr\'{\i}guez E., Rolland A.,
Costa V., 2001, MNRAS, 323, 923
\end{thebibliography}
\label{lastpage}
\end{document}
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