%%
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%% Modified 2018 January
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%% This is a sample manuscript marked up using the
%% AASTeX v6.2 LaTeX 2e macros.
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%% AASTeX is now based on Alexey Vikhlinin's emulateapj.cls
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%% other external packages (latexsym, graphicx, amssymb, longtable, and epsf).
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%% The first piece of markup in an AASTeX v6.x document is the \documentclass
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%% typeset, one-column, single-spaced document.  It is the default and thus
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%% using aastex version 6.2
\documentclass[twocolumn]{aastex62}
\pdfoutput=1

%% The default is a single spaced, 10 point font, single spaced article.
%% There are 5 other style options available via an optional argument. They
%% can be envoked like this:
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%% \documentclass[argument]{aastex62}
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%%  twocolumn   : two text columns, 10 point font, single spaced article.
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%%  preprint2   : two text columns, 12 point font, single spaced article.
%%  modern      : a stylish, single text column, 12 point font, article with
%% 		  wider left and right margins. This uses the Daniel
%% 		  Foreman-Mackey and David Hogg design.
%%  RNAAS       : Preferred style for Research Notes which are by design
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%%                 the twocolumn substyle.
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%%  linenumbers  : turn on lineno package.
%%  trackchanges : required to see the revision mark up and print its output
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%%                 affiliation information after each name. Creates a much
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%% \documentclass[twocolumn,linenumbers,trackchanges]{aastex62}
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%% AASTeX v6.* now includes \hyperref support. While we have built in specific
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\usepackage{graphicx}
\usepackage{journals}
\usepackage[symbol]{footmisc}
\usepackage{url}
\usepackage{color}
\usepackage{multirow}
\usepackage{xspace}
\usepackage{amsmath}
\usepackage{mathtools}

\newcommand{\vdag}{(v)^\dagger}
\newcommand\aastex{AAS\TeX}
\newcommand\latex{La\TeX}
\newcommand{\iz}[1]{\textcolor{blue}{#1}}
\newcommand{\ic}[1]{\textcolor{red}{#1}}
\newcommand{\ik}[1]{\textcolor{green}{#1}}
\newcommand{\kg}[1]{\textcolor{orange}{#1}}
\newcommand{\ergscm}{\ensuremath{{\rm erg\,s^{-1}\,cm^{-2}}}\xspace}


%% Tells LaTeX to search for image files in the
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\graphicspath{{./}{figures/}}

%% Reintroduced the \received and \accepted commands from AASTeX v5.2
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\accepted{--}
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%\AuthorCollaborationLimit=3
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%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%
%% The following section outlines numerous optional output that
%% can be displayed in the front matter or as running meta-data.
%%
%% If you wish, you may supply running head information, although
%% this information may be modified by the editorial offices.
\shorttitle{J1605 H$\alpha$ broad line variability}
\shortauthors{Katkov et al.}
%%
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% \watermark{text}
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%% This is the end of the preamble.  Indicate the beginning of the
%% manuscript itself with \begin{document}.

\begin{document}

\title{Rapid variability of the broad H$\alpha$ emission line in the intermediate-mass black hole active galactic nucleus \textit{J160531.84+174826.1}}

%% LaTeX will automatically break titles if they run longer than
%% one line. However, you may use \\ to force a line break if
%% you desire. In v6.2 you can include a footnote in the title.

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%% autoindexing of affilations which prior was a manual process that could
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%% arguement which is the 16 digit ORCID. The syntax is:
%% \author[xxxx-xxxx-xxxx-xxxx]{Author Name}
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%% the ID to make sure it is valid.
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%% will issue a specific error message and quit. Please use multiple
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\correspondingauthor{Igor Chilingarian}
\email{igor.chilingarian@cfa.harvard.edu, chil@sai.msu.ru}

\author[0000-0002-6425-6879]{Ivan Yu. Katkov}
%\altaffiliation{These authors contributed equally to this work}
\affiliation{Sternberg Astronomical Institute, M.V.Lomonosov Moscow State University, Universitetsky prospect 13, Moscow, 119992, Russia}
%\nocollaboration

\author[0000-0002-7924-3253]{Igor V. Chilingarian}
%\altaffiliation{These authors contributed equally to this work}
\affiliation{Smithsonian Astrophysical Observatory, 60 Garden St. MS09, Cambridge, MA 02138, USA}
\affiliation{Sternberg Astronomical Institute, M.V.Lomonosov Moscow State University, Universitetsky prospect 13, Moscow, 119992, Russia}
%\nocollaboration

\author[0000-0003-3255-7340]{Kirill A. Grishin}
\affiliation{Sternberg Astronomical Institute, M.V.Lomonosov Moscow State University, Universitetsky prospect 13, Moscow, 119992, Russia}
\affiliation{Department of Physics, M.V. Lomonosov Moscow State University, 1 Vorobyovy Gory, Moscow, 119991, Russia}
%\nocollaboration

\author{Franz E. Bauer}
\affiliation{Pontifica Universidad Catolica, Chile}
%\nocollaboration

\author[0000-0002-5544-9476]{Ivan Yu. Zolotukhin}
%\altaffiliation{These authors contributed equally to this work}
\affiliation{Sternberg Astronomical Institute, M.V.Lomonosov Moscow State University, Universitetsky prospect 13, Moscow, 119992, Russia}
\affiliation{Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhnij Arkhyz 369167, Russia}
\affiliation{Universit\'e de Toulouse; UPS-OMP, IRAP, 9 avenue du Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France}
%\nocollaboration

%% Note that the \and command from previous versions of AASTeX is now
%% depreciated in this version as it is no longer necessary. AASTeX
%% automatically takes care of all commas and "and"s between authors names.

%% AASTeX 6.2 has the new \collaboration and \nocollaboration commands to
%% provide the collaboration status of a group of authors. These commands
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%% Mark off the abstract in the ``abstract'' environment.
\begin{abstract}
TBW
\end{abstract}

%% Keywords should appear after the \end{abstract} command.
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\keywords{cosmology: observations --- early universe --- galaxies: active --- galaxies: nuclei --- galaxies: Seyfert --- quasars: supermassive black holes}

%% From the front matter, we move on to the body of the paper.
%% Sections are demarcated by \section and \subsection, respectively.
%% Observe the use of the LaTeX \label
%% command after the \subsection to give a symbolic KEY to the
%% subsection for cross-referencing in a \ref command.
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%% to the KEY in the \bibitem in the reference list below.


\section{Introduction and motivation}
\label{sec:intro}

\section{Observations, Data Reduction and Analysis}

\subsection{An automated IMBH search workflow}



\begin{figure*}
\includegraphics[width=\hsize]{fig_spec.pdf}
\caption{Spectral decomposition of MagE and SDSS data for J160531.84+1748 object studied in this work.
Top row panel: The observed optical SDSS spectrum is shown in blue, the orange line is the best-fitting stellar population template without emission lines.
Middle row: A close-up view of several emission lines in the SDSS spectrum.
The emission line profile (observed data are shown in black) is constructed first by subtracting the best-fitting stellar population template, then in allowed lines it is decomposed into narrow line (blue) and broad line (red) components.
The total emission line model is shown in magenta and its residuals are displayed in gray shifted downward for clarity; light gray lines indicate $\pm 1\sigma$ flux uncertainties of the original SDSS spectrum.
A non-parametric narrow line model (rightmost panel, blue histogram) is computed simultaneously for all forbidden emission lines in the spectrum that reduces fitting residuals and allows us to detect even a very faint broad line component (rightmost panel, red line), a proxy for the BH mass.
Bottom row: Same as the middle row but for MagE data.
\label{fig_spec}}
\end{figure*}

\begin{figure*}
\includegraphics[width=\textwidth]{fig_j1605_variations_flx_sigma_cont.pdf}
\caption{Variations of flux in BLR component, continuum around 5007\AA\ and $\sigma_{\rm BLR}$.
\label{fig_variations}}
\end{figure*}

\section{Results and Discussion}



\acknowledgments
We thank our anonymous referee for useful comments on the manuscript and a number of individuals (M.~Elvis, M.~Khlopov, H.-Y.~Liu, A.~Loar, M.~Mezcua, K.~Postnov) who provided valuable feedback on the original arXiv submission.
IC, IK, IZ, and KG acknowledge the support by the Russian
Scientific Foundation grant 17-72-20119 that supported the final stages of this work and the manuscript preparation.
IZ acknowledges the Russian Scientific Foundation grant 14-50-00043 for the development of the pipeline system used for input catalog assembly.
The authors acknowledge partial support from the M.V.Lomonosov
Moscow State University Program of Development, and a Russian--French PICS International Laboratory program (no.  6590) co-funded by the RFBR (project 15-52-15050), entitled ``Galaxy evolution mechanisms in the Local Universe and at intermediate redshifts''.
The authors are grateful to citizen scientist A.~Zolotov for his help with the figure 1 of the manuscript.
Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number 18708581 issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060.
The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory (observations 20114, 20115).
Based on observations obtained with {\it XMM-Newton}, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA (observations 0795711301, 0795711401).
This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile.
Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
These observations are associated with the {\it HST} program 11142.
This research has made use of TOPCAT, developed by Mark Taylor at the University of Bristol; Aladin developed by the Centre de Donn\'ees Astronomiques de Strasbourg (CDS); the VizieR catalogue access tool (CDS); Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration, 2013); Atlassian JIRA issue tracking system and Bitbucket source code hosting service.
Funding for the \emph{SDSS} and \emph{SDSS}-II has been provided by the Alfred P.  Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England.
The \emph{SDSS} Web Site is \url{http://www.sdss.org/}.
The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.


\bibliographystyle{aasjournal}
\bibliography{j1605_variability}

\end{document}

% End of file `sample62.tex'.
