Minor formatting revisions and edits in preparation to identify volunteers to finish.

.gitignore

@@ -13,7 +13,6 @@
 # these rules might exclude image files for figures etc.
 # *.ps
 # *.eps
-# *.pdf
 
 ## Bibliography auxiliary files (bibtex/biblatex/biber):
 *.bbl

VersionDate.tex

@@ -1,4 +1,4 @@
 \begin{center}
-Version  
-March 24, 2015
+Version 1.0:  
+August 4, 2017
 \end{center} 

abstract.tex

@@ -1,9 +1,15 @@
-\begin{center}
-
-\vspace*{30mm}
 
-{\bf Abstract.} 
-
-TBD
 
+\vspace*{30mm}
+\begin{center}
+{\bf Abstract} 
 \end{center}
+\vspace*{5mm}
+
+{\justify
+The Large Synoptic Survey Telescope (LSST) will enable revolutionary studies of
+galaxies, dark matter, and black holes over cosmic time. The
+LSST Galaxies Science Collaboration (LSST GSC) has identified a host of preparatory research tasks required 
+to leverage fully the LSST dataset for extragalactic science beyond the study of dark energy.
+This {\it Galaxies Science Roadmap} provides a brief introduction to critical extragalactic science to be conducted ahead of LSST operations, and a detailed list of preparatory science tasks including the motivation, activities, and deliverables associated with each. The {\it Galaxies Science Roadmap} will serve as a guiding document for researchers interested in conducting extragalactic science in anticipation of the forthcoming LSST era.
+}

apj.bst

@@ -1,15 +1,18 @@
-
-%% 1998/08/12  J Baker
-%% Tweaked by hand to get correct results for ApJ.  Added functions from
-%% astrobib.
-
 %% $Log: apj.bst,v $
+%% Revision 1.4  2002/06/18 16:37:48  alberto
+%% Add comma after first author in two-author reference
+%% Fix courtesy of Tim Robishaw <[email protected]>
+%%
 %% Revision 1.3  2000/04/20 22:17:50  jbaker
 %% Fixed INBOOK bug, now works essentially like BOOK.
 %%
 %% Revision 1.2  1998/08/30 22:35:45  jbaker
 %% Added RCS keywords.
 %%
+%% 1998/08/12  J Baker
+%% Tweaked by hand to get correct results for ApJ.  Added functions from
+%% astrobib.
+
 
 %%
 %% This is file `apj.bst',
@@ -387,25 +390,35 @@ FUNCTION {format.names}
 { 's :=
   #1 'nameptr :=
   s num.names$ 'numnames :=
+
   numnames 'namesleft :=
     { namesleft #0 > }
-    { s nameptr
-      "{vv~}{ll}{, jj}{, f.}" format.name$
-    't :=
+    { 
+      s nameptr "{vv~}{ll}{, jj}{, f.}" format.name$ 't :=
       nameptr #1 >
         {
+          #8 numnames <
+	    { #0 'namesleft := }
+            'skip$
+          if$
           namesleft #1 >
             { ", " * t * }
             {
-              numnames #2 >
+                numnames #1 >
+%% AA 6/18/2002
+%% This fix courtesy of Tim Robishaw <[email protected]>:
+%% Original version left comma out after initials of first author
+%% for two-author papers!!
+%%              numnames #2 >
                 { "," * }
                 'skip$
               if$
               s nameptr "{ll}" format.name$ duplicate$ "others" =
                 { 't := }
                 { pop$ }
               if$
-              t "others" =
+              %t "others" =
+              #8 numnames <
                 {
                   " {et~al.}" *
                 }

arxiv/VersionDate.tex

@@ -0,0 +1,4 @@
+\begin{center}
+Version 1.0:  
+August 4, 2017
+\end{center} 

arxiv/abstract.tex

@@ -0,0 +1,15 @@
+
+
+\vspace*{30mm}
+\begin{center}
+{\bf Abstract} 
+\end{center}
+\vspace*{5mm}
+
+{\justify
+The Large Synoptic Survey Telescope (LSST) will enable revolutionary studies of
+galaxies, dark matter, and black holes over cosmic time. The
+LSST Galaxies Science Collaboration (LSST GSC) has identified a host of preparatory research tasks required 
+to leverage fully the LSST dataset for extragalactic science beyond the study of dark energy.
+This {\it Galaxies Science Roadmap} provides a brief introduction to critical extragalactic science to be conducted ahead of LSST operations, and a detailed list of preparatory science tasks including the motivation, activities, and deliverables associated with each. The {\it Galaxies Science Roadmap} will serve as a guiding document for researchers interested in conducting extragalactic science in anticipation of the forthcoming LSST era.
+}

arxiv/agn.tex

@@ -0,0 +1,219 @@
+\section{Active Galactic Nuclei}\label{sec:tasks:agn:intro} {\justify
+
+
+Active Galactic Nuclei (AGN) phenomena enable an understanding of
+the growth of supermassive black holes (BHs), aspects of galaxy evolution, the high-redshift universe, 
+and other physical activity including accretion physics, jets, and magnetic fields.  
+While AGN represent a distinct topic within the LSST Science Collaborations, the LSST
+dataset will reveal some aspects of AGN science via their role as an
+evolutionary stage of galaxies in addition to their ability to probe accretion physics around BHs.
+The tasks listed here present preparatory science efforts connected with AGN study as a special
+phase in galaxy evolution.
+
+
+\begin{tasklist}{AGN}
+\subsection{AGN Selection from LSST Data}
+\tasktitle{AGN Selection from LSST Data}
+\begin{task}
+\label{task:agn:selection}
+\motivation{
+LSST multiband photometry may select Active Galactic Nuclei using a variety of different methods.  At optical and near infrared wavelengths, the distinctive colors of AGN
+at particular redshifts enables their photometric selection \citep[e.g.,][]{richards2006a}.
+The LSST data will therefore augment methods that rely on X-ray or radio activity, or the
+identification of emission lines in spectroscopic data.
+LSST will also open up, in a more practical way, the identification of AGN based on their variability.   
+These LSST photometric, multiwavelength, and variability-selected samples may probe
+unique aspects of AGN phenomena.
+A better understanding of the AGN role in galaxy evolution requires 
+an understanding of how and why these selection methods include or exclude particular sources
+or phases of AGN-galaxy co-evolution.
+}
+~\\
+\activities{
+The use of LSST as a single way to identify AGN and characterize their diversity of AGN
+requires the development of selection criteria that can leverage the color, morphology,
+and variability information available from LSST imaging alone.
+A number of AGN surveys with input from multiple wavelength observations and spectra already
+exist, and precursor work must utilize these surveys to determine 
+whether AGN that prove difficult to identify via optical color selection will reveal
+themselves through the additional parameters of morphology, variability, and/or the 
+near-infrared data that LSST will provide.
+}
+~\\
+\deliverables{%Deliverables over the next several years from the activities described above include the following:
+~
+\begin{enumerate}
+\item Creation of a cross-matched catalog of known AGN selected and verified using different methods.
+\item Understanding of AGN variability sensitivity given the nominal LSST cadence. 
+\item Development of algorithms that probe how color selection accounts for AGN variability.
+\end{enumerate}
+}
+\end{task}
+%\end{tasklist}
+
+
+%\begin{tasklist}{T}
+\subsection{AGN Host Galaxy Properties from LSST Data}
+\tasktitle{AGN Host Galaxy Properties from LSST Data}
+\begin{task}
+\label{task:agn:host_galaxies}
+\motivation{
+Morphological characterizations from parameterized models, such as multiple-component 
+\cite{sersic1968a} profiles, or non-parametric measures like CAS and Gini-M20 
+\citep{abraham1994a,conselice2000a,lotz2004a} can help identify merging galaxies in the LSST data.
+The ability of these techniques to characterize efficiently and accurately the
+morphology of AGN host galaxies identified via their variability remains unproven.
+}
+~\\
+\activities{
+Simulated or model AGN host galaxies can characterize whether the
+LSST Level 2 data will enable the measurement of morphological features associated with
+AGN, as a function of host galaxy properties, AGN luminosity, and variability.
+For each model galaxy, varying the central AGN luminosity will reveal the impact of
+central source brightness on the recovery of morphological properties.
+Existing data sets, such as Pan-STARRS, may help inform LSST about the range of
+variability frequency and amplitude, and how these AGN properties may affect the
+recovery of morphological properties in AGN host galaxies. 
+}
+~\\
+\deliverables{%Deliverables over the next several years from the activities described above include the following:
+~
+\begin{enumerate}
+\item Characterization of the accuracy and precision afforded by the LSST dataset for the
+recovery of basic morphology properties as a function of AGN brightness and wavelength.
+\item Understanding of the effects of AGN brightness and variability on host-galaxy classification diagrams.
+\item Development of morphological parameters beyond star/galaxy separation and an understanding of the efficacy of LSST Level 2 data products for morphological selection of AGN.
+\item Development of color selection criteria that accounts for morphology.
+\end{enumerate}
+}
+\end{task}
+%\end{tasklist}
+
+\subsection{AGN Feedback in Clusters}
+\tasktitle{AGN Feedback in Clusters}
+\begin{task}
+\label{task:agn:feedback_in_clusters}
+\motivation{
+Brightest Cluster/Group Galaxies (hereafter BCGs) represent the most massive galaxies in the local 
+universe, residing at or near the centers of galaxy clusters and groups. 
+BCGs contain the largest known supermassive BHs that can influence the host galaxy properties,
+cluster gas, and other cluster members via the mechanical energy produced by their $>100$kpc 
+scale jets (``AGN feedback'').
+The relative proximity of low-redshift galaxy clusters enable detailed studies of 
+stars, gas, and AGN jets that may reveal the ramifications of AGN feedback. 
+LSST will provide a large sample of moderate- to high-redshift clusters 
+in which we can measure AGN feedback statistically. By combining X-ray, radio, and optical observations we can assess the average influence of BCG AGN on the hot intracluster medium (ICM) for different sub-populations \citep[e.g.,][]{stott2012a}.
+}
+~\\
+\activities{
+By assembling a multi-wavelength dataset (optical, X-ray, and radio), the BCG mass, cluster mass, ICM temperature, and mechanical power injected into the ICM by supermassive BHs can be constrained. 
+The interplay between the BCG, its black hole, and the cluster gas can then be studied, 
+providing an assessment of the balance of energies involved and a direct comparison with theoretical models of AGN feedback. 
+SDSS has enabled this multi-wavelength analysis for a few hundred clusters at $z<0.3$,
+but LSST cluster datasets will reach deeper to redshifts $z>1$.
+Such studies hold implications for cosmological studies by helping to distinguish between
+X-ray gas properties strongly influenced by AGN or that arise only in response
+to the 
+cluster gravitational potential.
+}
+~\\
+\deliverables{%Deliverables over the next several years from the activities described above include the following:
+~
+\begin{enumerate}
+\item Investigation and quantification of the ability of the LSST pipeline to select BCGs using precursor datasets such as the HSC survey.
+\item Compilation of existing and forthcoming radio and X-ray data available for AGN feedback studies (XCS, eROSITA, SKA-pathfinders, SUMSS, etc.).
+\item Assessment of theoretical predictions expected for the multi-wavelength properties of
+AGN host galaxies in clusters or groups (e.g., cosmological simulations such as EAGLE or more detailed single cluster studies).
+\end{enumerate}
+}
+\end{task}
+%\end{tasklist}
+
+%\begin{tasklist}{T}
+\subsection{AGN Variability Selection in LSST Data}
+\tasktitle{AGN Variability Selection in LSST Data}
+\begin{task}
+\label{task:agn:variability}
+\motivation{
+Most AGN exhibit broad-band aperiodic, stochastic variability across the entire electromagnetic
+spectrum on timescales ranging from minutes to years. Continuum variability arises in the accretion disk of the AGN, providing a powerful probe of accretion physics. 
+The main LSST Wide Fast Deep (WFD) survey will obtain $\sim10^8$ AGN light curves (i.e., flux as a function of time) with $\sim1000$ observations ($\sim200$ per filter band) over 10 years. 
+The Deep Drilling Fields will provide AGN lightcurves with much denser sampling for a small subset of the objects in the WFD survey. The science content of the lightcurves will critically depend on the exact sampling strategy used to obtain the light curves. For example, the observational uncertainty in determining the color variability of AGN will crucially depend on the interval between observations in individual filter bands. These concerns motivate a determination of guidelines for an optimal survey strategy (from an AGN variability perspective) and a discovery
+of possible biases and uncertainties introduced into AGN variability science as a result of the chosen survey strategy.}
+~\\
+\activities{
+Study existing AGN variability datasets (SDSS Stripe 82, OGLE, PanSTARRS, CRTS, PTF + iPTF, Kepler, \& K2) to constrain a comprehensive set of AGN variability models. Generate and study simulations using parameters selected from these models using observational constraints, and determine the appropriateness of simulations for carrying out various types of AGN variability science including power spectrum models, quasi-periodic oscillation searches, and binary AGN models.}
+~\\
+\deliverables{%Deliverables over the next several years from the activities described above include the following:
+~
+\begin{enumerate}
+\item Observational constraints on AGN variability models.
+\item Metrics for quantifying the efficacy of different survey strategies for AGN variability science.
+\end{enumerate}
+}
+\end{task}
+%\end{tasklist}
+
+%\begin{tasklist}{T}
+\subsection{AGN Photometric Redshifts from LSST Data}
+\tasktitle{AGN Photometric Redshifts from LSST Data}
+\begin{task}
+\label{task:agn:photoz}
+\motivation{
+Given the large number of AGN that LSST will discover, 
+many AGN will not receive follow-up with spectroscopic observations.
+Photometric redshifts can provide relatively accurate redshifts for large numbers of galaxies,
+but accurate photometric redshifts for AGN host galaxies remain challenging.
+}
+~\\
+\activities{
+Initial efforts include a comprehensive review of the state of the art in AGN host galaxy photo-$z$
+determinations and an analysis of AGN vs. non-AGN galaxy photo-$z$ performance.
+A comparison of model and/or observed AGN host SEDs with a matched set of
+non-host galaxies at a variety of redshifts will help engineer color selection criteria for identifying AGN hosts, and whether variability can break photo-$z$ degeneracies. 
+}
+~\\
+\deliverables{%Deliverables over the next several years from the activities described above include the following:
+~
+\begin{enumerate}
+\item Development of AGN host color selection criteria, and an identification of objects for which color selection might prove ambiguous or degenerate.
+\item Analysis of multiwavelength, morphological, or variability information that might break photo-$z$ degeneracies.  This task complements work described in Section \ref{task:photo_z:color_simulations}
+(Photometric Redshifts) and should be coordinated with those efforts.
+\end{enumerate}
+}
+\end{task}
+%\end{tasklist}
+
+%\begin{tasklist}{T}
+\subsection{AGN Merger Signatures from LSST Data}
+\tasktitle{AGN Merger Signatures from LSST Data}
+\begin{task}
+\label{task:agn:mergers}
+\motivation{
+Understanding the role AGN play in galaxy evolution requires identifying AGN phenomena at all stages and in all types of galaxies. 
+AGN host galaxies often show disturbed morphology, suggesting that the galaxy merger process may  trigger AGN activity. 
+While the ``trainwrecks'' may prove easy to identify in the high-quality LSST data, the
+identification of galaxies in other merger stages, such as ``pre-merger'' harassment, may be particularly hard to recognize.
+Preliminary work needs to be done to understand how to identify mergers from the LSST data products and whether galaxy deblending and segmentation methods and procedures are adequate.
+}
+~\\
+\activities{
+Create simulated or identify real images that contain known galaxy mergers, including
+systems with and without visible AGN.
+Run the LSST software stack on these images, and
+engineer metrics that quantify 
+the accurate detection of galaxy mergers with and without AGN.
+Activities for detecting some of these low surface brightness (LSB) features will parallel work described in Section \ref{task:gal:lsb}
+(Galaxy Evolution) and should be coordinated with those efforts.
+}
+~\\
+\deliverables{%Deliverables over the next several years from the activities described above include the following:
+~
+\begin{enumerate}
+\item Characterization and optimization of the ability of the LSST Level 2 data to enable the detection of galaxy mergers that host AGN.
+\item Identification of catalog parameters or merging galaxy images with properties that will prove challenging to recognize (semi-)automatically in the LSST dataset.
+\end{enumerate}
+}
+\end{task}
+\end{tasklist}
+}