%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
% AGUtmpl.tex: this template file is for articles formatted with LaTeX2e,
% Modified November 2013
%
% This template includes commands and instructions
% given in the order necessary to produce a final output that will
% satisfy AGU requirements.
%
% PLEASE DO NOT USE YOUR OWN MACROS
% DO NOT USE \newcommand, \renewcommand, or \def.
%
% FOR FIGURES, DO NOT USE \psfrag
%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
% All questions should be e-mailed to latex@agu.org.
%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
% Step 1: Set the \documentclass
%
% There are two options for article format: two column (default)
% and draft.
%
% PLEASE USE THE DRAFT OPTION TO SUBMIT YOUR PAPERS.
% The draft option produces double spaced output.
%
% Choose the journal abbreviation for the journal you are
% submitting to:

% jgrga JOURNAL OF GEOPHYSICAL RESEARCH
% gbc   GLOBAL BIOCHEMICAL CYCLES
% grl   GEOPHYSICAL RESEARCH LETTERS
% pal   PALEOCEANOGRAPHY
% ras   RADIO SCIENCE
% rog   REVIEWS OF GEOPHYSICS
% tec   TECTONICS
% wrr   WATER RESOURCES RESEARCH
% gc    GEOCHEMISTRY, GEOPHYSICS, GEOSYSTEMS
% sw    SPACE WEATHER
% ms    JAMES
% ef    EARTH'S FUTURE
%
%
%
% (If you are submitting to a journal other than jgrga,
% substitute the initials of the journal for "jgrga" below.)

\documentclass[jgrga]{agutexSI}



%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
%  SUPPORTING INFORMATION TEMPLATE
%
%% ------------------------------------------------------------------------ %%
%
%
%Please use this template when formatting and submitting your Supporting Information.

%This template serves as both a “table of contents” for the supporting information for your article and as a summary of files.
%
%
%OVERVIEW
%
%Please note that all supporting information will be peer reviewed with your manuscript.
%In general, the purpose of the supporting information is to enable authors to provide and archive auxiliary information such as data %tables, method information, figures, video, or computer software, in digital formats so that other scientists can use it.
%The key criteria are that the data:
% 1. supplement the main scientific conclusions of the paper but are not essential to the conclusions (with the exception of
%    including %data so the experiment can be reproducible);
% 2. are likely to be usable or used by other scientists working in the field;
% 3. are described with sufficient precision that other scientists can understand them, and
% 4. are not exe files.
%
%USING THIS TEMPLATE
%
%All Supporting text and figures should be included in this document. Insert supporting information content into each appropriate section of the template. %Figures and tables should appear above each caption.  To add additional captions, simply copy and paste each sample caption as needed.

%Tables may be included, but can also be uploaded separately, especially if they are larger than 1 page, or if necessary for retaining table formatting. Data sets, large tables, movie files, and audio files should be uploaded separately, following AGU naming conventions. Include their captions in this document and list the file name with the caption. You will be prompted to upload these files on the Upload Files tab during the submission process, using file type “Supporting Information (SI)”

%IMPORTANT NOTE ON FIGURES AND TABLES
% Placeholders for figures and tables appear after the \end{article} command, after references.
% DO NOT USE \psfrag or \subfigure commands.
%
%  Uncomment the following command to include .eps files
 % \usepackage[dvips]{graphicx}
 \usepackage{graphicx}
%
%  Uncomment the following command to allow illustrations to print
%   when using Draft:
\setkeys{Gin}{draft=false}
%
% Substitute one of the following for [dvips] above
% if you are using a different driver program and want to
% proof your illustrations on your machine:
%
% [xdvi], [dvipdf], [dvipsone], [dviwindo], [emtex], [dviwin],
% [pctexps],  [pctexwin],  [pctexhp],  [pctex32], [truetex], [tcidvi],
% [oztex], [textures]
%
%
%% ------------------------------------------------------------------------ %%
%
%  ENTER PREAMBLE
%
%% ------------------------------------------------------------------------ %%

% Author names in capital letters:
%\authorrunninghead{BALES ET AL.}
\authorrunninghead{MARTENS ET AL.}

% Shorter version of title entered in capital letters:
%\titlerunninghead{SHORT TITLE}
\titlerunninghead{STRUCTURAL SENSITIVITY OF LOAD RESPONSE}

%Corresponding author mailing address and e-mail address:
%\authoraddr{Corresponding author: A. B. Smith,
%Department of Hydrology and Water Resources, University of
%Arizona, Harshbarger Building 11, Tucson, AZ 85721, USA.
%(a.b.smith@hwr.arizona.edu)}

\begin{document}

%% ------------------------------------------------------------------------ %%
%
%  TITLE
%
%% ------------------------------------------------------------------------ %%

%\includegraphics{agu_pubart-white_reduced.eps}


\title{Supporting Information for ``The Sensitivity of Surface Mass Loading Displacement Response to Perturbations in the Elastic Structure of the Crust and Mantle''}
%
% e.g., \title{Supporting Information for "Terrestrial ring current:
% Origin, formation, and decay $\alpha\beta\Gamma\Delta$"}
%
%DOI: 10.1002/%insert paper number here%

%% ------------------------------------------------------------------------ %%
%
%  AUTHORS AND AFFILIATIONS
%
%% ------------------------------------------------------------------------ %%


%Use \author{\altaffilmark{}} and \altaffiltext{}

% \altaffilmark will produce footnote;
% matching \altaffiltext will appear at bottom of page.

% \authors{A. B. Smith,\altaffilmark{1}
% Eric Brown,\altaffilmark{1,2} Rick Williams,\altaffilmark{3}
% John B. McDougall\altaffilmark{4}, and S. Visconti\altaffilmark{5}}

%\altaffiltext{1}{Department of Hydrology and Water Resources,
%University of Arizona, Tucson, Arizona, USA.}

%\altaffiltext{2}{Department of Geography, Ohio State University,
%Columbus, Ohio, USA.}

%\altaffiltext{3}{Department of Space Sciences, University of
%Michigan, Ann Arbor, Michigan, USA.}

%\altaffiltext{4}{Division of Hydrologic Sciences, Desert Research
%Institute, Reno, Nevada, USA.}

%\altaffiltext{5}{Dipartimento di Idraulica, Trasporti ed
%Infrastrutture Civili, Politecnico di Torino, Turin, Italy.}

\authors{Hilary R. Martens,\altaffilmark{1}
Luis Rivera,\altaffilmark{2}  Mark Simons,\altaffilmark{1}
 and Takeo Ito\altaffilmark{3}}

\altaffiltext{1}{Seismological Laboratory, Division of Geological and Planetary Sciences, California Institute of Technology,
Pasadena, California, USA.}

\altaffiltext{2}{Institut de Physique du Globe de Strasbourg  (UMR7516), Universit\'{e} de Strasbourg/CNRS,
Strasbourg, France.}

\altaffiltext{3}{Graduate School of Environmental Studies, Nagoya University, Nagoya, Japan.}



%% ------------------------------------------------------------------------ %%
%
%  BEGIN ARTICLE
%
%% ------------------------------------------------------------------------ %%

% The body of the article must start with a \begin{article} command
%
% \end{article} must follow the references section, before the figures
%  and tables.

\begin{article}

%% ------------------------------------------------------------------------ %%
%
%  TEXT
%
%% ------------------------------------------------------------------------ %%



\noindent\textbf{Contents of this file}
%%%Remove or add items as needed%%%
\begin{enumerate}
%\item Text S1 to Sx
\item Figures \ref{fig:llnpartial_homsph_n2} to \ref{fig:histograms}
%\item Tables S1 to Sx
%if Tables are larger than 1 page, upload as separate excel file
\end{enumerate}
\noindent\textbf{Additional Supporting Information (Files uploaded separately)}
\begin{enumerate}
\item Captions for Datasets S1 to S24
%\item Captions for large Tables S1 to S24 (if larger than 1 page, upload as separate excel file)
%\item Captions for Movies S1 to Sx
%\item Captions for Audio S1 to Sx
\end{enumerate}


\vspace{1cm}

\noindent\textbf{Introduction}

%In the interest of transparency and to help facilitate any efforts to reproduce our work, we provide 
This supporting information provides tables of the seismic velocity and density profiles for each of the six reference Earth models used in our study. We also provide tables of load Love numbers (LLNs) and load Green's functions (LGFs), in both the CE and CM reference frames, derived directly from each of the reference Earth models. Methods for computing the LLNs and LGFs are described in the main text and implemented using our internally developed software package, \texttt{LoadDef}. 

In the main text, we present partial derivatives of LLNs for spherical harmonic degrees 2, 100, and 10000, derived from the reference Earth model PREM (Figs. 1--3). Figure \ref{fig:llnpartial_homsph_n2} shows the partial derivatives of the LLNs for a homogeneous sphere. Figures \ref{fig:llnpartial_1066_n2p}--\ref{fig:llnpartial_1066_n2s} show partial derivatives for $n=2$ derived from Earth model 1066A, which may be compared directly with \citet{okubo1983partial}. In addition, we show partial derivatives of load, potential, shear, and stress Love numbers derived from PREM for a selection of other spherical harmonic degrees in Figs. \ref{fig:llnpartial_PREM_n1l}--\ref{fig:llnpartial_PREM_n1000}. 

Figure \ref{fig:lgfpartial_homsph} depicts displacement LGFs for a homogeneous sphere model. Figure \ref{fig:lgfpartial_layers_zoom} shows a zoomed-in version of Fig. 6 from the main text. Figure \ref{fig:lgfpartial_50kmlayers} depicts LGF sensitivity kernels for perturbations to layers of 50-km thickness through the crust and upper mantle (cf. Fig. 7 from the main text). Figures \ref{fig:IcelandProf1} and \ref{fig:IcelandProf2} are identical to Figs. 15 and 16 in the main text, respectively, albeit for the second profile line (B--B$^\prime$) from Fig. 11 in the main text. Figures \ref{fig:globalgridE}--\ref{fig:globalgridV} show the global spatial distributions of the east, north, and vertical components of the vector differences between pairs of predicted M$_2$ OTL-induced surface displacements derived from PREM and STW105. The vector differences for additional forward-model combinations are shown as histograms in Figure \ref{fig:histograms}.

Table \ref{table:PotLoveNum} provides a list of degree-2 potential Love numbers for six seismologically derived Earth models. 

%Type or paste your text here. The introduction gives a brief overview of the supporting information. You should include information %about as many of the following as possible (when appropriate):
% 1. a general overview of the kind of data files;
% 2. information about when and how the data were collected or created;
% 3. a general description of processing steps used;
% 4. any known imperfections or anomalies in the data.

%\clearpage

%Delete all unused file types below. Copy/paste for multiples of each file type as needed.
%\noindent\textbf{Text S1.}
%Type or paste text here. This should be additional explanatory text, such as: extended descriptions of results, full details of models, extended lists of acknowledgements etc.  It should not be additional discussion, analysis, interpretation or critique. It should not be an additional scientific experiment or paper.
%
%Repeat for any additional Supporting Text

%%Enter Data Set, Movie, and Audio captions here
%%EXAMPLE CAPTIONS

\noindent\textbf{Data Set S1.} %Type or paste caption here.
%upload your dataset(s) to AGU's journal submission site and select "Supporting Information (SI)" as the file type. Following naming %convention: ds01.
Radial profiles of density ($\rho$), P-wave velocity ($V_P$), and S-wave velocity ($V_S$) for the isotropic and oceanless version of the Preliminary Reference Earth Model (PREM) used in our study. We generated the model using the polynomial functions from Table 1 of \citet{dziewonski1981preliminary}, evaluated every 100 km within the core regions and every 100 m within the mantle and crust. We also assumed effective isotropic velocities between 220 and 24.4 km depth and replaced the water layer at the surface by the properties of the upper-most crust: $V_P$ = 5800 m s$^{-1}$, $V_S$ = 3200 m s$^{-1}$, and $\rho$ = 2600 kg m$^{-3}$. 

\noindent\textbf{Data Set S2.}
Radial profiles of $\rho$, $V_P$, and $V_S$ for STW105 \citep{kustowski2008anisotropic}. We acquired the model directly from the Incorporated Research Institutions for Seismology (IRIS) Data Management Center (DMC) \citep{trabant2012data} and replaced the water layer at the surface with typical values for the upper crust. 

\noindent\textbf{Data Set S3.}
Radial profiles of $\rho$, $V_P$, and $V_S$ for AK135f. AK135f was derived from seismic body waves \citep{kennett1995constraints}, with density and Q structure contributed by \citet{montagner1996reconcile}. We acquired the model directly from the IRIS DMC and replaced the water layer at the surface with typical values for the upper crust. 

\noindent\textbf{Data Set S4.}
Radial profiles of $\rho$, $V_P$, and $V_S$ for the Earth model 1066A, which we acquired from Table 5 of \citet{gilbert1975application}.

\noindent\textbf{Data Set S5.}
Radial profiles of $\rho$, $V_P$, and $V_S$ for the Earth model SNA, derived from an average of upper mantle shear-wave velocity structure in North America \citep{grand1984upper}. Below 1000 km depth, the model assumes the structural properties of AK135f.

\noindent\textbf{Data Set S6.}
Radial profiles of $\rho$, $V_P$, and $V_S$ for the Earth model CR, derived from an average of upper mantle P-wave velocity structure beneath stable North America \citep{chu2012upper}. The values for $V_S$ and $\rho$ were obtained from ratios of AK135 (Risheng Chu, personal communication). Below 1000 km depth, the model assumes the structural properties of AK135f.

\noindent\textbf{Data Set S7.}
Load Love numbers ($h_n'$, $l_n'$ and $k_n'$) derived from PREM (Data Set S1) up to spherical harmonic degree 10000. Asymptotic values for the Love numbers, computed using the second-order expressions derived by \citet{guo2004green}, are provided in the final three columns. 

\noindent\textbf{Data Set S8.}
Same as Data Set S7, but the load Love numbers are instead derived from STW105 (Data Set S2). 

\noindent\textbf{Data Set S9.}
Same as Data Set S7, but the load Love numbers are instead derived from AK135f (Data Set S3). 

\noindent\textbf{Data Set S10.}
Same as Data Set S7, but the load Love numbers are instead derived from 1066A (Data Set S4). 

\noindent\textbf{Data Set S11.}
Same as Data Set S7, but the load Love numbers are instead derived from SNA (Data Set S5). 

\noindent\textbf{Data Set S12.}
Same as Data Set S7, but the load Love numbers are instead derived from CR (Data Set S6). 

\noindent\textbf{Data Set S13.}
Load Green's functions in the CE reference frame derived from PREM (Data Set S1). The first column lists the angular distance between an observer and the load point in degrees, the second column provides the vertical-component of the elastic displacement response in meters per kilogram, and the third column provides the horizontal-component of the elastic displacement response in meters per kilogram. The fourth and fifth columns represent the second and third columns, respectively, multiplied by a factor of $10^{12} a \theta$, where $a$ is Earth's radius in meters and $\theta$ is the observer-to-load angular distance in radians. 

\noindent\textbf{Data Set S14.}
Same as Data Set 13, but for load Green's functions derived from STW105 (Data Set S2). 

\noindent\textbf{Data Set S15.}
Same as Data Set 13, but for load Green's functions derived from AK135f (Data Set S3). 

\noindent\textbf{Data Set S16.}
Same as Data Set 13, but for load Green's functions derived from 1066A (Data Set S4). 

\noindent\textbf{Data Set S17.}
Same as Data Set 13, but for load Green's functions derived from SNA (Data Set S5). 

\noindent\textbf{Data Set S18.}
Same as Data Set 13, but for load Green's functions derived from CR (Data Set S6). 

\noindent\textbf{Data Set S19.}
Same as Data Set 13, but for the CM reference frame.

\noindent\textbf{Data Set S20.}
Same as Data Set 14, but for the CM reference frame. 

\noindent\textbf{Data Set S21.}
Same as Data Set 15, but for the CM reference frame.

\noindent\textbf{Data Set S22.}
Same as Data Set 16, but for the CM reference frame.

\noindent\textbf{Data Set S23.}
Same as Data Set 17, but for the CM reference frame.

\noindent\textbf{Data Set S24.}
Same as Data Set 18, but for the CM reference frame. 

%Repeat for any additional Supporting data sets

%\noindent\textbf{Movie S1.} %Type or paste caption here.
%upload your movie(s) to AGU's journal submission site and select, "Supporting Information %(SI)" as the file type. Following naming convention: ms01.

%Repeat any additional Supporting movies

%\noindent\textbf{Audio S1.} %Type or paste caption here.
%upload your audio file(s) to AGU's journal submission site and select "Supporting Information %(SI)" as the file type. Following naming convention: auds01.

%Repeat for any additional Supporting audio files

%%% End of body of article:
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
% Optional Notation section goes here
%
% Notation -- End each entry with a period.
% \begin{notation}
% Term & definition.\\
% Second term & second definition.\\
% \end{notation}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


%% ------------------------------------------------------------------------ %%
%%  REFERENCE LIST AND TEXT CITATIONS
%
% Either type in your references using
% \begin{thebibliography}{}
% \bibitem{}
% Text
% \end{thebibliography}
%
% Or,
%
% If you use BiBTeX for your references, please use the agufull08.bst file (available at % ftp://ftp.agu.org/journals/latex/journals/Manuscript-Preparation/) to produce your .bbl
% file and copy the contents into your paper here.
%
% Follow these steps:
% 1. Run LaTeX on your LaTeX file.
%
% 2. Make sure the bibliography style appears as \bibliographystyle{agufull08}. Run BiBTeX on your LaTeX
% file.
%
% 3. Open the new .bbl file containing the reference list and
%   copy all the contents into your LaTeX file here.
%
% 4. Comment out the old \bibliographystyle and \bibliography commands.
%
% 5. Run LaTeX on your new file before submitting.
%
% AGU does not want a .bib or a .bbl file. Please copy in the contents of your .bbl file here.

%\bibliographystyle{agufull08}
%\bibliography{jabbrev,ReferenceDatabase}	

\begin{thebibliography}{11}
\providecommand{\natexlab}[1]{#1}
\expandafter\ifx\csname urlstyle\endcsname\relax
  \providecommand{\doi}[1]{doi:\discretionary{}{}{}#1}\else
  \providecommand{\doi}{doi:\discretionary{}{}{}\begingroup
  \urlstyle{rm}\Url}\fi

\bibitem[{\textit{Chu et~al.}(2012)\textit{Chu, Schmandt, and
  Helmberger}}]{chu2012upper}
Chu, R., B.~Schmandt, and D.~V. Helmberger (2012), Upper mantle {P} velocity
  structure beneath the {M}idwestern {U}nited {S}tates derived from triplicated
  waveforms, \textit{Geochemistry, Geophysics, Geosystems}, \textit{13}(2),
  \doi{10.1029/2011GC003818}.

\bibitem[{\textit{Dziewonski and Anderson}(1981)}]{dziewonski1981preliminary}
Dziewonski, A.~M., and D.~L. Anderson (1981), Preliminary reference {E}arth
  model, \textit{Physics of the earth and planetary interiors}, \textit{25}(4),
  297--356, \doi{10.1016/0031-9201(81)90046-7}.

\bibitem[{\textit{Gilbert and Dziewonski}(1975)}]{gilbert1975application}
Gilbert, F., and A.~Dziewonski (1975), An application of normal mode theory to
  the retrieval of structural parameters and source mechanisms from seismic
  spectra, \textit{Philosophical Transactions of the Royal Society of London.
  Series A, Mathematical and Physical Sciences}, \textit{278}(1280), 187--269.

\bibitem[{\textit{Grand and Helmberger}(1984)}]{grand1984upper}
Grand, S.~P., and D.~V. Helmberger (1984), Upper mantle shear structure of
  {N}orth {A}merica, \textit{Geophysical Journal International},
  \textit{76}(2), 399--438, \doi{10.1111/j.1365-246X.1984.tb05053.x}.

\bibitem[{\textit{Guo et~al.}(2004)\textit{Guo, Li, Huang, Deng, Xu, and
  Ning}}]{guo2004green}
Guo, J., Y.~Li, Y.~Huang, H.~Deng, S.~Xu, and J.~Ning (2004), Green's function
  of the deformation of the {E}arth as a result of atmospheric loading,
  \textit{Geophysical journal international}, \textit{159}(1), 53--68,
  \doi{10.1111/j.1365-246X.2004.02410.x}.

\bibitem[{\textit{Kennett et~al.}(1995)\textit{Kennett, Engdahl, and
  Buland}}]{kennett1995constraints}
Kennett, B., E.~Engdahl, and R.~Buland (1995), Constraints on seismic
  velocities in the {E}arth from traveltimes, \textit{Geophysical Journal
  International}, \textit{122}(1), 108--124,
  \doi{10.1111/j.1365-246X.1995.tb03540.x}.

\bibitem[{\textit{Kustowski et~al.}(2008)\textit{Kustowski, Ekstr{\"o}m, and
  Dziewo{\'n}ski}}]{kustowski2008anisotropic}
Kustowski, B., G.~Ekstr{\"o}m, and A.~Dziewo{\'n}ski (2008), Anisotropic
  shear-wave velocity structure of the {E}arth's mantle: {A} global model,
  \textit{Journal of Geophysical Research: Solid Earth}, \textit{113}(B06306),
  \doi{10.1029/2007JB005169}.

\bibitem[{\textit{Montagner and Kennett}(1996)}]{montagner1996reconcile}
Montagner, J.-P., and B.~Kennett (1996), How to reconcile body-wave and
  normal-mode reference {E}arth models, \textit{Geophysical Journal
  International}, \textit{125}(1), 229--248,
  \doi{10.1111/j.1365-246X.1996.tb06548.x}.

\bibitem[{\textit{Okubo and Endo}(1986)}]{okubo1986static}
Okubo, S., and T.~Endo (1986), Static spheroidal deformation of degree 1 -
  {C}onsistency relation, stress solution and partials, \textit{Geophysical
  Journal International}, \textit{86}(1), 91--102,
  \doi{10.1111/j.1365-246X.1986.tb01074.x}.

\bibitem[{\textit{Okubo and Saito}(1983)}]{okubo1983partial}
Okubo, S., and M.~Saito (1983), Partial derivative of {L}ove numbers,
  \textit{Bulletin g{\'e}od{\'e}sique}, \textit{57}(1), 167--179.

\bibitem[{\textit{Trabant et~al.}(2012)\textit{Trabant, Hutko, Bahavar,
  Karstens, Ahern, and Aster}}]{trabant2012data}
Trabant, C., A.~R. Hutko, M.~Bahavar, R.~Karstens, T.~Ahern, and R.~Aster
  (2012), Data products at the {IRIS} {DMC}: {S}tepping stones for research and
  other applications, \textit{Seismological Research Letters}, \textit{83}(5),
  846--854, \doi{10.1785/0220120032}.

\end{thebibliography}



%\begin{thebibliography}{}

%\providecommand{\natexlab}[1]{#1}
%\expandafter\ifx\csname urlstyle\endcsname\relax
%  \providecommand{\doi}[1]{doi:\discretionary{}{}{}#1}\else
%  \providecommand{\doi}{doi:\discretionary{}{}{}\begingroup
%  \urlstyle{rm}\Url}\fi
%
%\bibitem[{\textit{Atkinson and Sloan}(1991)}]{AtkinsonSloan}
%Atkinson, K., and I.~Sloan (1991), The numerical solution of first-kind
%  logarithmic-kernel integral equations on smooth open arcs, \textit{Math.
%  Comp.}, \textit{56}(193), 119--139.
%
%\bibitem[{\textit{Colton and Kress}(1983)}]{ColtonKress1}
%Colton, D., and R.~Kress (1983), \textit{Integral Equation Methods in
%  Scattering Theory}, John Wiley, New York.
%
%\bibitem[{\textit{Hsiao et~al.}(1991)\textit{Hsiao, Stephan, and
%  Wendland}}]{StephanHsiao}
%Hsiao, G.~C., E.~P. Stephan, and W.~L. Wendland (1991), On the {D}irichlet
%  problem in elasticity for a domain exterior to an arc, \textit{J. Comput.
%  Appl. Math.}, \textit{34}(1), 1--19.
%
%\bibitem[{\textit{Lu and Ando}(2012)}]{LuAndo}
%Lu, P., and M.~Ando (2012), Difference of scattering geometrical optics
%  components and line integrals of currents in modified edge representation,
%  \textit{Radio Sci.}, \textit{47},  RS3007, \doi{10.1029/2011RS004899}.

%\end{thebibliography}

%Reference citation examples:

%...as shown by \textit{Kilby} [2008].
%...as shown by {\textit  {Lewin}} [1976], {\textit  {Carson}} [1986], {\textit  {Bartholdy and Billi}} [2002], and {\textit  {Rinaldi}} [2003].
%...has been shown [\textit{Kilby et al.}, 2008].
%...has been shown [{\textit  {Lewin}}, 1976; {\textit  {Carson}}, 1986; {\textit  {Bartholdy and Billi}}, 2002; {\textit  {Rinaldi}}, 2003].
%...has been shown [e.g., {\textit  {Lewin}}, 1976; {\textit  {Carson}}, 1986; {\textit  {Bartholdy and Billi}}, 2002; {\textit  {Rinaldi}}, 2003].

%...as shown by \citet{jskilby}.
%...as shown by \citet{lewin76}, \citet{carson86}, \citet{bartoldy02}, and \citet{rinaldi03}.
%...has been shown \citep{jskilbye}.
%...has been shown \citep{lewin76,carson86,bartoldy02,rinaldi03}.
%...has been shown \citep [e.g.,][]{lewin76,carson86,bartoldy02,rinaldi03}.
%
% Please use ONLY \citet and \citep for reference citations.
% DO NOT use other cite commands (e.g., \cite, \citeyear, \nocite, \citealp, etc.).

%% ------------------------------------------------------------------------ %%
%
%  END ARTICLE
%
%% ------------------------------------------------------------------------ %%
\end{article}
\clearpage

% Delete all unused file types below. Copy/paste for multiples of each file type as needed.

% enter figures and tables here:
%
% EXAMPLE FIGURE
% ---------------
% \begin{figure}
%\setfigurenum{S1} %%Change number for each figure
% \noindent\includegraphics[width=20pc]{samplefigure.eps}
%\caption{Caption text here}
 %\label{figure_label}
 %\end{figure}
 
 \begin{figure}
 \setfigurenum{S1}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS1.pdf}
\caption{Partial derivatives of degree-2 load Love numbers with respect to the shear modulus, $\mu$, the bulk modulus, $\kappa$, and density, $\rho$, for a homogeneous sphere model of properties $V_P$ = 10000 m s$^{-1}$, $V_S$ = 5000 m s$^{-1}$, and $\rho$ = 5000 kg m$^{-3}$. The partial derivatives were computed using the techniques discussed by \citet{okubo1983partial}. Here, the profiles extend through the whole Earth, which is entirely solid. The partials have been multiplied by the depth profile of each elastic parameter, making them dimensionless. The horizontal axes are in units of $10^{-4}$ km$^{-1}$.}
\label{fig:llnpartial_homsph_n2}
\end{figure}
 
 \begin{figure}
\setfigurenum{S2}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS2.pdf}
\caption{Partial derivatives of degree-2 potential Love numbers with respect to the shear modulus, $\mu$, the bulk modulus, $\kappa$, and density, $\rho$, for Earth model 1066A \citep{gilbert1975application}, computed using the techniques discussed by \citet{okubo1983partial}. The partials have been multiplied by the depth profile of each elastic parameter, making them dimensionless. The horizontal axes are in units of $10^{-4}$ km$^{-1}$. The figure may be compared directly with fig. 1a in \citet{okubo1983partial} for Earth's crust and mantle.}
\label{fig:llnpartial_1066_n2p}
\end{figure}

\begin{figure}
\setfigurenum{S3}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS3.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_1066_n2p}, but for load, rather than potential, Love numbers (cf. \citet{okubo1983partial}, fig. 1b). The horizontal axes are in units of $10^{-4}$ km$^{-1}$. }
\label{fig:llnpartial_1066_n2l}
\end{figure}

\begin{figure}
\setfigurenum{S4}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS4.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_1066_n2p}, but for shear, rather than potential, Love numbers (cf. \citet{okubo1983partial}, fig. 1c). The horizontal axes are in units of $10^{-4}$ km$^{-1}$. }
\label{fig:llnpartial_1066_n2s}
\end{figure}
 
\begin{figure}
\setfigurenum{S5}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS5.pdf}
\caption{Partial derivatives of degree-1 load Love numbers with respect to the shear modulus, $\mu$, the bulk modulus, $\kappa$, and density, $\rho$, for Earth model PREM, computed using the techniques discussed by \citet{okubo1986static} and \citet{okubo1983partial}. The partials have been multiplied by the depth profile of each elastic parameter, making them dimensionless. The horizontal axes are in units of $10^{-4}$ km$^{-1}$.}
\label{fig:llnpartial_PREM_n1l}
\end{figure}

\begin{figure}
\setfigurenum{S6}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS6.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n1l}, but for stress Love numbers (see Table 1 in the main text for the relevant surface boundary conditions). The horizontal axes are in units of $10^{-4}$ km$^{-1}$. }
\label{fig:llnpartial_PREM_n1s}
\end{figure}

\begin{figure}
\setfigurenum{S7}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS7.pdf}
\caption{Partial derivatives of degree-2 potential Love numbers with respect to the shear modulus, $\mu$, the bulk modulus, $\kappa$, and density, $\rho$, for Earth model PREM. The partials have been multiplied by the depth profile of each elastic parameter, making them dimensionless. The horizontal axes are in units of $10^{-4}$ km$^{-1}$. Note that this figure is identical to Fig. \ref{fig:llnpartial_1066_n2p}, but here the partials are computed based on PREM rather than 1066A.}
\label{fig:llnpartial_PREM_n2p}
\end{figure}

\begin{figure}
\setfigurenum{S8}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS8.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2p}, but for load Love numbers. Note that this figure is identical to Fig. \ref{fig:llnpartial_1066_n2l}, but here the partials are computed based on PREM rather than 1066A. The horizontal axes are in units of $10^{-4}$ km$^{-1}$. }
\label{fig:llnpartial_PREM_n2l}
\end{figure}

\begin{figure}
\setfigurenum{S9}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS9.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2p}, but for shear Love numbers. Note that this figure is identical to Fig. \ref{fig:llnpartial_1066_n2s}, but here the partials are computed based on PREM rather than 1066A. The horizontal axes are in units of $10^{-4}$ km$^{-1}$. }
\label{fig:llnpartial_PREM_n2s}
\end{figure}

\begin{figure}
\setfigurenum{S10}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS10.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2p}, but for spherical harmonic degree $n=3$.}
\label{fig:llnpartial_PREM_n3p}
\end{figure}

\begin{figure}
\setfigurenum{S11}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS11.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2l}, but for spherical harmonic degree $n=3$.}
\label{fig:llnpartial_PREM_n3l}
\end{figure}

\begin{figure}
\setfigurenum{S12}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS12.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2s}, but for spherical harmonic degree $n=3$.}
\label{fig:llnpartial_PREM_n3s}
\end{figure}

\begin{figure}
\setfigurenum{S13}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS13.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2p}, but for spherical harmonic degree $n=4$.}
\label{fig:llnpartial_PREM_n4p}
\end{figure}

\begin{figure}
\setfigurenum{S14}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS14.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2l}, but for spherical harmonic degree $n=4$.}
\label{fig:llnpartial_PREM_n4l}
\end{figure}

\begin{figure}
\setfigurenum{S15}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS15.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2s}, but for spherical harmonic degree $n=4$.}
\label{fig:llnpartial_PREM_n4s}
\end{figure}

\begin{figure}
\setfigurenum{S16}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS16.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2l}, but for spherical harmonic degree $n=10$.}
\label{fig:llnpartial_PREM_n10}
\end{figure}

\begin{figure}
\setfigurenum{S17}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS17.pdf}
\caption{Same as Fig. \ref{fig:llnpartial_PREM_n2l}, but for spherical harmonic degree $n=1000$.}
\label{fig:llnpartial_PREM_n1000}
\end{figure}

\begin{figure}
\setfigurenum{S18}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS18.pdf}
\caption{Displacement-response sensitivity kernels for 1\% linear perturbations to the bulk modulus ($\kappa$), shear modulus ($\mu$), and density ($\rho$) of a homogeneous sphere with properties $V_P$ = 10000 m s$^{-1}$, $V_S$ = 5000 m s$^{-1}$, and $\rho$ = 5000 kg m$^{-3}$. Since the elastic properties ($\mu$, $\kappa$ and $\rho$) are Jeffrey's parameters, we define the model terms in common-log space. Explicitly, $\mathrm{\bf m}_\mu =$ log$_{10}\, \mu$, $\mathrm{\bf m}_\kappa =$ log$_{10}\, \kappa$ and $\mathrm{\bf m}_\rho =$ log$_{10}\, \rho$. For a 1\% linear perturbation to the elastic moduli and density, the model-parameter perturbation is $\Delta \mathrm{\bf m}_\beta^j = $ log$_{10}$(1.01). The horizontal components of the displacement LGFs and sensitivity kernels are shown in the left panels; the vertical components are shown in the right panels. The top panels (A \& B) depict the displacement LGFs in the CM reference frame derived from the original, unperturbed model. The lower panels depict the LGF sensitivities resulting from perturbations to the $\kappa$ (C \& D), $\mu$ (E \& F), and $\rho$ (G \& H) model parameters. Sensitivities are computed as the change in LGF per change in model parameter. The displacement LGFs, as well as the sensitivity kernels, were multiplied by the factor $10^{12} a \theta$ to remove the singularity at the load point and to normalize the magnitude of the response, where $a$ is Earth's radius in meters and $\theta$ is the angular distance from the load point in radians. Units of the unnormalized LGFs are meters of displacement per kilogram load.}
\label{fig:lgfpartial_homsph}
\end{figure}

\clearpage

\begin{figure}
\setfigurenum{S19}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS19.pdf}
\caption{The sensitivity of displacement LGFs to perturbations in elastic structure for a radially heterogeneous Earth model (same as Fig. 6 from the main text, but zoomed into the upper 200 km). We adopted an isotropic and oceanless version of PREM as the reference model. We examine the sensitivity of the displacement LGFs to linear perturbations of 1\% to the bulk modulus (panels C and D), shear modulus (panels E and F), and density (panels G and H) as a function of depth. We independently perturb each of the major regions of PREM down to 200 km depth as a distinct blocks, separated by dashed lines in the figure. Model parameters are defined in common-log space as $\mathrm{\bf m}_\mu =$ log$_{10}\, \mu$, $\mathrm{\bf m}_\kappa =$ log$_{10}\, \kappa$ and $\mathrm{\bf m}_\rho =$ log$_{10}\, \rho$. The applied model-parameter perturbation was $\Delta \mathrm{\bf m}_p^j = $ log$_{10}$(1.01). The horizontal components of the displacement LGFs and sensitivity kernels are shown in the left panels; the vertical components are shown in the right panels. The top panels (A \& B) depict the the displacement LGFs in the CM reference frame derived from the reference model. The displacement LGFs, as well as the sensitivity kernels, were multiplied by the factor $10^{12} a \theta$ to remove the singularity at the load point and to normalize the magnitude of the response, where $a$ is Earth's radius in meters and $\theta$ is the angular distance from the load point in radians. Units of the unnormalized LGFs are meters per kilogram.}
\label{fig:lgfpartial_layers_zoom}
\end{figure}

\begin{figure}
\setfigurenum{S20}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS20.pdf}
\caption{Same as Fig. \ref{fig:lgfpartial_layers_zoom}, except that we have perturbed layers of constant thickness instead of the major regions of PREM (cf. Fig. 7 from the main text). Specifically, we have partitioned the crust and mantle into a set of 50-km-thick spherical shells, which we perturb systematically down to 800 km depth. We adopted a model parameter perturbation of $\Delta \mathrm{\bf m}_p^j = $ log$_{10}$(1.01). Contour lines are included for clarity, with specific values denoted in the colorbar.}
\label{fig:lgfpartial_50kmlayers}
\end{figure}

\clearpage

\begin{figure}
\setfigurenum{S21}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS21.pdf}
\caption{Sensitivities of OTL-induced surface displacements to perturbations in elastic and density structure along a great-circle path through Iceland (profile B--B$^\prime$ from Fig. 11 in the main text). The profile maintains constant longitude along the 341$^{\circ}$E meridian and a node spacing of 0.01$^{\circ}$ ($\approx$1 km). The left column of panels shows the sensitivity of predicted surface displacements to perturbations in the bulk-modulus model parameter, $\Delta \log_{10}\kappa$. The center column of panels shows the sensitivity to perturbations in the shear-modulus model parameter, $\Delta \log_{10}\mu$. The right column of panels shows the sensitivity to perturbations in the density model parameter, $\Delta \log_{10}\rho$. In each case, we perturb the parameters by 1\% in linear space, or by $\Delta \mathrm{\bf m} = \log_{10}(1.01)$ in log space, where $\mathrm{\bf m} = \log_{10}\kappa$, $\log_{10}\mu$, or $\log_{10}\rho$. The top, middle, and bottom rows of panels show sensitivity kernels for OTL-induced surface displacements in the east, north, and vertical components, respectively. The colored lines denote perturbations to distinct layers of PREM down to a depth of 400 km and correspond to the same layer in every panel (see legend). The sensitivity kernels are computed, separately for each layer, as the magnitudes of vector differences between the predicted OTL-induced surface displacements (in millimeters) for the perturbed and reference (unperturbed PREM) models divided by the model-parameter perturbation, $\log_{10}(1.01)$.}
\label{fig:IcelandProf1}
\end{figure}

\begin{figure}
\setfigurenum{S22}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS22.pdf}
\caption{Same as Fig. \ref{fig:IcelandProf1}, but normalized by the layer thickness, $\mathrm{T}$ (in kilometers).}
\label{fig:IcelandProf2}
\end{figure}

\begin{figure}
\setfigurenum{S23}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS23.pdf}
\caption{Magnitudes of the vector differences between predicted OTL-induced surface displacements in the east component across a $2^{\circ} \times 2^{\circ}$ global grid for two forward models: one computed using LGFs derived from PREM and the other computed using LGFs derived from STW105. All other parameters, including the ocean-tide model and convolution procedure, remain consistent in each forward model computation. Histograms showing the magnitudes of the vector differences between predicted displacements for additional pairs of standard Earth models are shown in Fig. \ref{fig:histograms}.}
\label{fig:globalgridE}
\end{figure}

\begin{figure}
\setfigurenum{S24}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS24.pdf}
\caption{Same as Fig. \ref{fig:globalgridE}, but for the north component of the predicted displacements.}
\label{fig:globalgridN}
\end{figure}

\begin{figure}
\setfigurenum{S25}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS25.pdf}
\caption{Same as Fig. \ref{fig:globalgridE}, but for the vertical component of the predicted displacements.}
\label{fig:globalgridV}
\end{figure}

\begin{figure}
\setfigurenum{S26}
\noindent \includegraphics[width=43pc]{./Final-Figures-SOM/FigS26.pdf}
\caption{Histograms showing the magnitudes of the vector differences between predicted OTL-induced surface displacements for pairs of reference Earth models. Only the elastic Earth model changes between the forward model computations; all other parameters, including the ocean-tide model and convolution procedure, remain the same. We consider only the M$_2$ tidal harmonic and predict the response on a $2^{\circ} \times 2^{\circ}$ global grid of land-based locations. The left, center, and right panels depict the east, north, and vertical components of the vector differences, respectively. The top row of panels shows the vector differences on a linear scale; the bottom row of panels shows the vector differences on a log scale.}
\label{fig:histograms}
\end{figure}

% ---------------
% EXAMPLE TABLE
%
%\begin{table}
%\settablenum{S1} %%Change number for each table
%\caption{Time of the Transition Between Phase 1 and Phase 2\tablenotemark{a}}
%\centering
%\begin{tabular}{l c}
%\hline
% Run  & Time (min)  \\
%\hline
%  $l1$  & 260   \\
%  $l2$  & 300   \\
%  $l3$  & 340   \\
%  $h1$  & 270   \\
%  $h2$  & 250   \\
%  $h3$  & 380   \\
%  $r1$  & 370   \\
%  $r2$  & 390   \\
%\hline
%\end{tabular}
%\tablenotetext{a}{Footnote text here.}
%\end{table}
% ---------------
%
% EXAMPLE LARGE TABLE (UPLOADED SEPARATELY)
%\begin{table}
%\settablenum{S1} %%Change number for each table
%\caption{Time of the Transition Between Phase 1 and Phase 2\tablenotemark{a}}
%\end{table}

\clearpage

\begin{table}
\settablenum{S1}
\caption{Degree-2 potential Love numbers for the seismologically derived SNREI Earth models considered in our study (Data Sets S1--S6).}
\centering
\vspace{0.4cm}
\begin{tabular}{c|c|c} \hline
    Model & $h_2$ & $l_2$ 
    \\ \hline \hline
    PREM & 0.6067 & 0.0841
    \\ 
    STW105 & 0.6078 & 0.0839
    \\ 
    AK135f & 0.6074 & 0.0847
    \\ 
    SNA & 0.6069 & 0.0844
    \\ 
    CR & 0.6054 & 0.0837
    \\ 
    1066A & 0.6130 & 0.0851
    \\ \hline
\end{tabular}
\label{table:PotLoveNum}
\end{table}


\end{document}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

More Information and Advice:

%% ------------------------------------------------------------------------ %%
%
%  SECTION HEADS
%
%% ------------------------------------------------------------------------ %%

% Capitalize the first letter of each word (except for
% prepositions, conjunctions, and articles that are
% three or fewer letters).

% AGU follows standard outline style; therefore, there cannot be a section 1 without
% a section 2, or a section 2.3.1 without a section 2.3.2.
% Please make sure your section numbers are balanced.
% ---------------
% Level 1 head
%
% Use the \section{} command to identify level 1 heads;
% type the appropriate head wording between the curly
% brackets, as shown below.
%
%An example:
%\section{Level 1 Head: Introduction}
%
% ---------------
% Level 2 head
%
% Use the \subsection{} command to identify level 2 heads.
%An example:
%\subsection{Level 2 Head}
%
% ---------------
% Level 3 head
%
% Use the \subsubsection{} command to identify level 3 heads
%An example:
%\subsubsection{Level 3 Head}
%
%---------------
% Level 4 head
%
% Use the \subsubsubsection{} command to identify level 3 heads
% An example:
%\subsubsubsection{Level 4 Head} An example.
%
%% ------------------------------------------------------------------------ %%
%
%  IN-TEXT LISTS
%
%% ------------------------------------------------------------------------ %%
%
% Do not use bulleted lists; enumerated lists are okay.
% \begin{enumerate}
% \item
% \item
% \item
% \end{enumerate}
%
%% ------------------------------------------------------------------------ %%
%
%  EQUATIONS
%
%% ------------------------------------------------------------------------ %%

% Single-line equations are centered.
% Equation arrays will appear left-aligned.

Math coded inside display math mode \[ ...\]
 will not be numbered, e.g.,:
 \[ x^2=y^2 + z^2\]

 Math coded inside \begin{equation} and \end{equation} will
 be automatically numbered, e.g.,:
 \begin{equation}
 x^2=y^2 + z^2
 \end{equation}

% IF YOU HAVE MULTI-LINE EQUATIONS, PLEASE
% BREAK THE EQUATIONS INTO TWO OR MORE LINES
% OF SINGLE COLUMN WIDTH (20 pc, 8.3 cm)
% using double backslashes (\\).

% To create multiline equations, use the
% \begin{eqnarray} and \end{eqnarray} environment
% as demonstrated below.
\begin{eqnarray}
  x_{1} & = & (x - x_{0}) \cos \Theta \nonumber \\
        && + (y - y_{0}) \sin \Theta  \nonumber \\
  y_{1} & = & -(x - x_{0}) \sin \Theta \nonumber \\
        && + (y - y_{0}) \cos \Theta.
\end{eqnarray}

%If you don't want an equation number, use the star form:
%\begin{eqnarray*}...\end{eqnarray*}

% Break each line at a sign of operation
% (+, -, etc.) if possible, with the sign of operation
% on the new line.

% Indent second and subsequent lines to align with
% the first character following the equal sign on the
% first line.

% Use an \hspace{} command to insert horizontal space
% into your equation if necessary. Place an appropriate
% unit of measure between the curly braces, e.g.
% \hspace{1in}; you may have to experiment to achieve
% the correct amount of space.


%% ------------------------------------------------------------------------ %%
%
%  EQUATION NUMBERING: COUNTER
%
%% ------------------------------------------------------------------------ %%

% You may change equation numbering by resetting
% the equation counter or by explicitly numbering
% an equation.

% To explicitly number an equation, type \eqnum{}
% (with the desired number between the brackets)
% after the \begin{equation} or \begin{eqnarray}
% command.  The \eqnum{} command will affect only
% the equation it appears with; LaTeX will number
% any equations appearing later in the manuscript
% according to the equation counter.
%

% If you have a multiline equation that needs only
% one equation number, use a \nonumber command in
% front of the double backslashes (\\) as shown in
% the multiline equation above.

%% ------------------------------------------------------------------------ %%
%
%  SIDEWAYS FIGURE AND TABLE EXAMPLES
%
%% ------------------------------------------------------------------------ %%
%
% For tables and figures, add \usepackage{rotating} to the paper and add the rotating.sty file to the folder.
% AGU prefers the use of {sidewaystable} over {landscapetable} as it causes fewer problems.
%
% \begin{sidewaysfigure}
% \includegraphics[width=20pc]{samplefigure.eps}
% \caption{caption here}
% \label{label_here}
% \end{sidewaysfigure}
%
%
%
% \begin{sidewaystable}
% \caption{}
% \begin{tabular}
% Table layout here.
% \end{tabular}
% \end{sidewaystable}
%
%

