% Begin file here
%
%   NOTE:  This template has only extremely minor changes from Cycle 3.
%      The style file it calls is gross overkill for what is now needed for GALEX proposals
%          (leftover from earlier cycles).
%       However, we provide it for those proposers who may wish to resubmit a Cycle 3 
%           proposal with only modest changes.  
%       To convert a Cycle 3 to a Cycle 4 proposal, comment out the line about Proposal 
%           Number,   (" nasapropno"  )  and % change the style file to galex4.sty.
%
%
% GALEX Phase 1 observing proposal LaTex template (version 1.0)
%   Closely adapted from FUSE Phase 1 LaTex template (version 5.0)
%
% Date -  7 November, 2003. (SGN)
% Revised - 14 February, 2004 (SGN)
%           23 March, 2004 (SGN) (text only, not function)
%           17-19 March, 2005 (SGN) (for Cycle 2)
%           25 April, 2006 (JEH) (for Cycle 3)
%           10 May, 2007 (SGN, for Cycle 4)
%
%
%
% WHAT, WHERE, AND WHEN TO SUBMIT YOUR PROPOSAL
%-------------------------------------------------------------------------
%
%See iinformation at:  
%     http://galexgi.gsfc.nasa.gov/propforms/ProposalChecklist.html
%
% First, perform various target checks as outlined in the checklist.
% Then, the complete Phase 1 proposal submission consists of the
% following steps.  
%
% 1) Fill out either this LaTeX proposal template,  the Word proposal
%     template, or make one of your own that follows guidelines and page
%     limits given in long NRA.    Use to produce a .pdf file. 
%
% 2) Fill out cover and observation (target) forms on RPS/AKBAR, verify, and Submit.
%       http://heasarc.gsfc.nasa.gov/akbar/
%       
% 
% 3) In AKBAR, go to "Recent Activity" Page, click on the "Files" button, and 
%       upload your GALEX proposal .pdf   file  
%
%
%
% Please see the GALEX GI website for the due date for submitting the 
% Cycle 4 Phase 1 PDF justification and the AKBAR forms. 
% 
%
% LATEX
%---------
% All of the information to be provided in the form below should
% be inserted within the curly braces "{}", or as text blocks
% after a template keyword (a keyword is preceded by a backslash 
% character; example, \justification).  Comment lines start with
% the "%" sign and can be added at will, but will NOT show up in the
% formatted proposal or be processed by GALEX Mission Planning software.  
% You may remove any explanatory comments in this file or leave them in,
% as you wish; they are here only for your convenience.
%
% PostScript figures may be included in the formatted output by using
% the \plotone command.  Insert the following into your LaTeX file -
%   \begin{figure}[h]
%   \plotone{foo.eps}
%   \caption{}
%   \end{figure}
% where "foo.eps" is an Encapsulated PostScript file you have created.
% The figure will be scaled to a width of 95% of the width of the text.
% If you have a tall, narrow figure, you can scale it to a smaller
% fraction of the text with with \epsscale{fraction}.  For example -
%   \epsscale{0.5}\plotone{foo.eps}
% scales the figure to half of the text width.  Use \plottwo to plot
% two figures side-by-side, as in
%   \plottwo{foo1.eps}{foo2.eps}
%
%	NOTE -  Please do not use colons in any text blocks in 
% the proposal (such as "Scientific Justification", "Feasibility 
% and Safety", etc.), as this causes problems when interpreted 
% by the parser software.  Colons are required inside the 
% coordinate key-words \ra{} and \dec{} .  If your text 
% requires the use of a colon, you can use the latex
%  $\colon$ 
% 
%
% Proposers who wish to incorporate graphics using other techniques
% (e.g., with the commands provided with the Latex 2e graphics package,
% with the PSFIG macros, etc.) are free to do so, but GALEXGI
% cannot provide any support or advice to those who choose these approaches..
%
%
% For more information on LaTeX, see the LaTeX manual by Leslie Lamport,
% "LaTeX - A Document Preparation System, User's Guide and Reference Manual",
% 1994, Addison-Wesley Publishing Company.
%
%----------------------------------------------------------------------
% LaTeX template begins here -  Numbered headings correspond to listing
% of detailed instructions in section 3 of the Phase 1 Proposal 
% Instructions document.
 
%   ( http://galexgi.gsfc.nasa.gov/propforms/index.html )
%----------------------------------------------------------------------
% DO NOT DELETE THE NEXT TWO LINES
\documentclass[12pt]{article}
\usepackage{galex4}

% If you want to add any personal LaTeX definitions, please add them 
% here before the \begin{document} command

\begin{document}

% 1. Proposal Title
% The program's title should be as short and descriptive as possible 
% and should be no more than about 100 characters. Enter between the
% curly braces.

\title{UV Astronomy and the Revolution }   % (Required)

% 2. Principal Investigator Contact Information. (All Fields Required)

% Please supply the requested contact information for the PI 
% All fields should be supplied for the PI, who is assumed to be 
% the primary point of contact for any questions about the program.

% Title (Dr., Mr., Ms., Prof., etc.)
\pititle{Dr.}		

% First name (John, or John G. to include initial)
\pifirstname{Leia}		

% Last name   
\pilastname{Organa}	

% 3.	NASA Proposal Number

%No longer used  
%Please see http://heasarc.gsfc.nasa.gov/akbar/ 
%for instructions on submitting coversheet information 

%\nasapropno{}
 
% NOTE:  Complete Cover Page information such as the abstract, CoI 
% information, etc. will be collected in the AKBAR form 
%
%
%
%
% 3. Scientific Justification.  (Required, text block) 
% Enter text after the \justification keyword.  Describe the scientific
% justification for the proposed program, stating clearly its goals and
% significance to astronomy. You should include a brief discussion of
% scientific background, previous work, and why GALEX data are needed to
% address your goals. The Scientific Justification is limited to three
% pages for standard and survey proposals and five pages for Legacy 
% proposals, including figures, tables, and/or references.  
% PLEASE DO NOT USE ANY COLONS IN ANY TEXT FIELD
% (use  $\colon$ ).
% PLEASE DO NOT ATTEMPT TO CHANGE THE FONT SIZES OR SPACINGS.
% <=3 pages of 11pt text, except for Legacy 
%  proposals, which may use up to 5 pages for text.

\justification    

{\smallskip \noindent \bf Significance to Astronomy}     Active resistance to warlords occur in a significant fraction
of  galaxies and are thought to be related to supermassive
bureaucratic holes (SMBH).  Most $-$ perhaps all $-$ galaxies with bulges contain SMBH; when the SMBH are fed (generally by lobbyists) they can become oppressive and cruel.  This leads to the spontaneous formation of rebellions and Active Galactic Notinmybackyards (AGN). These AGN can interact with their surroundings, particularly in long strings or filaments which may be coherent over many kpc.
Filaments smuggle all sorts of matter out of galactic centers, and can have a dramatic effect on the surrounding Intergalactic Market (IGM). Radio galaxies, which are now known to z $\sim5$, are often found
to be full of talk show hosts, who are full of hot air (gas-rich), lumpy, and to be embedded in giant idiological nebulae which are aligned with their beliefs.     The Fishy Cluster (NGC~6666) is the nearest case of a filament interacting with the IGM; (D = 3.4 kpc);  it therefore
offers an excellent opportunity to observe, in detail, such an interaction.

\paragraph
{\smallskip \noindent \bf Background}
Past interactions have left a complex of stellar and
gaseous shells around the Fishy Cluster, at distances up to 15 kpc from
the Ellipse.  The well-known ``inner filament" (TV and radio source) extends $\sim$6 kpc NE from the Redfish galaxy and expands into an overpressured cloud of hot air.  Further out the filament appears to become collimated,
curving southwestward  to $\sim$20pc (Organa et al.\ 2005); diffuse radio emission continues curving
sharply to the north beyond that for $\sim$1500pc.  In two locations, the filament loses its organized structure - these are on the East and West edges.    Near these locations, bright optical filaments, enhanced
soft X-ray emission and sparks often fly.     A wide variety of environments occur along the filament.  Not
much is known about the filament very close to the galaxy nuclei. The ``inner filament"  (See Figure 1a) is rigid, linear and
appears to be self-absorbed and obscured by excessive hot air; it is mostly associated with the high metallicity big redfish.  The ``outer filament" seems to be excessively diffuse, blue, and difficult to confine (Figure 1b).  The ``Bridge"  forms a large arc of tangled streamers;  it appears at the edge of an H~I cloud; star formation there
was probably triggered by a red-blue interaction.

   The inner filament, outer filament, and bridge thus represent three quite different examples of the filament-IGM interaction: one (inner) where the filament appears to encounter no restraint, one (outer) where the filament has been diverted by the major
appeal of a free lunch, and one (bridge) where it has
apparently managed to ignore the temptation and continued past the same diversion.

\paragraph
{\smallskip \noindent \bf New Observations } Models predict that a filament interacting with the IGM
should drive shocks into the surrounding populations both along
and transverse to the filament; the models also predict that
instabilities along the interaction edge can lead to cloud
shredding and runaway rioting by the resulting mobs (Hitchcock 1963).  UV spectra of the filament can differentiate between various types of shredding and mobbing.  The storm und drung models predict that
strong UV (1200-1800\ang) emission lines should be produced in the interaction.   We believe that the Fishy Cluster provides a marvelous opportunity to study
a filament-IGM interaction up-close, in a range of interaction environments.  We wish to obtain  sensitive,
wide-field, GALEX GRISM spectroscopy of the filament and the galaxies. We will use these with new, deep, GALEX images as well as with existing exploratory images of the cluster, to explore the complex nature of a filament-IGM
interaction associated with a superpower.

\paragraph
 {\smallskip \noindent \bf Need for GALEX} Although HST could obtain much higher resolution UV images and spectra,
the HST UV fields-of-view are so small ($\sim$30\arcsec) that
it would not be feasible to image the entire filament.  Also, it appears unlikely that HST will be able to obtain UV spectra in the foreseeable future.  {\it Imaging:}  High sensitivity, wide-field, UV imaging is required
to identify locations where the filament interacts with the
ISM.  Preliminary GALEX imaging data is already in hand and this
analysis is progressing (Organa et al. 2005).
Deep FUV and NUV images  will also be used to search for UV emission
SW of the galaxies, at the location of a possible weak gamma-ray source and X-ray shell.
{\it Spectroscopy:}  FUV spectroscopy  of the  filament will
allow us to explore the nature of the different
environments along the filament.  We will be able to tell if the UV
emission is  stellar or it comes from
emission lines in hot gas (or both), since the expected UV spectra are
very different.  GALEX is the only instrument that can provide both the UV observations and the large Field-of-View needed. 

\paragraph
 {\smallskip \noindent \bf Relevance to NASA goals} NASA is now chartered with Exploration; surely learning how material flows from the centers of civilizations along filaments into the IGM is a part of this exploration needed to better galaxykind.
 

\paragraph
{\smallskip\noindent\bf References:} 
\begin{flushleft}
Albertson et al.,1998, TrJ 493, 571 \\
Burymealive et al., 2004, occult-ph/0412282 \\
Hitchcock et al.,1957, Quarterly Journal of Horror Films, 35, 666 \\
Lucas 1989, Journal of American Filmwriters 23, 27 \\
Organa et al., 2005, ApJL, in prep.\\ 
Orwell, 1969, Liberty Press, 1984 \\
Skywalker et al., 2000a, PB\&J 379, 781 \\
Skywalker et al., 2000b, A\&P  564, 688 \\
Solo  1973, PhD Thesis, 110 \\
Vader et al., 1984, JXXXX, 1\\
\end{flushleft}

 
% 4. Description of Observations.  (text block, not for Archival proposals)
% Enter text after the \describeobservations keyword.  Up to one page of
% additional description is permitted here to address any "strategy
% issues" on how the observations should be performed, including 
% explanation of special scheduling issues or other non-standard 
% requirements.  Justify any observations of previously observed 
% targets (e.g. need to go deeper, need particular timing, etc.)
% See Phase 1 Instructions document at:
%  http://galexgi.gsfc.nasa.gov/propforms/index.html  for more information.
%   
% PLEASE DO NOT USE ANY COLONS IN ANY TEXT FIELD
%(use  $\colon$ ).
% PLEASE DO NOT ATTEMPT TO CHANGE THE FONT SIZES OR SPACINGS.

%  <=1 page

\describeobservations  

    We will use new GALEX GRISM spectroscopy, together with
archival GALEX images,  to determine the nature of the FUV emission
at different locations in the Fishy galaxy cluster.  GALEX has already observed the cluster for $\sim$1800 sec, and has clearly detected the inner and outer filaments as well as faint emission between and beyond the filaments (Figure 1b).

    Although the filament is extended in the transverse
direction along much of its length,  we should be able to
obtain reasonable spectra by observing with the dispersion
$\sim$ perpendicular to the filaments, because they are fairly
linear and fairly thin (usually $<$ 5 arcsec wide).
We wish to take GRISM exposures at a range of orientations
to reduce spectral overlap and order confusion.  However,
we wish to avoid taking GRISM exposures with the dispersion
along the filament.  Therefore, we would like to let the Mission
Planning Software assign random GRISM angles, but with a 90
degree zone excluded which would place dispersion $\sim$ along the filaments.
The filament has orientations of 20 - 40 degrees on the sky, so we request observations {\it avoiding} dispersion angles
between -15 and 75 degrees E of N.

 
% 5. Feasibility and Safety.  (Required for all but Archival, text block)
% Not to exceed 1 page single spaced (12 pt).
% Enter text after the \feasibility keyword.  Discuss the target 
% availability in terms of the spacecraft observing constraints.  
% Discuss in detail your signal-to-noise calculations, sensitivity 
% requirements, and resolution requirements for your proposed
% observations.   Describe the quality of your flux estimates
% and explain how you arrived at them.  Describe explicitly any 
% targets or situations that may create concerns for instrument 
% safety. Describe your method of estimating the necessary 
% exposure times for your targets with sufficient information for
% technical reviewers to reproduce your results. 
% If your targets are expected to be near the bright limits for
% a single object or for the field, or if you are requesting FUV-only
% observations, explain why these observations do not pose a safety 
% risk to the instrument. If you are proposing observations that
% exceed the brightness limits, you must make a convincing case
% for obtaining a waiver and explain why the proposed observations
% will not damage the instrument.  See the discussion of brightness
% limits on our website 
%
% PLEASE DO NOT USE ANY COLONS IN ANY TEXT FIELD
%(use  $\colon$ ).
% PLEASE DO NOT ATTEMPT TO CHANGE THE FONT SIZES OR SPACINGS.
%  <=1 page
\feasibility      

\parindent 25pt
    The redfish and bluefish galaxies are the dominant UV
sources in the field, with typical integrated fluxes in the GALEX bands of
1.9$\times10^{-13}$   and
5.1$\times10^{-13}$~ergs~cm$^{-2}$s$^{-1}$\AA$^{-1}$ (FUV and NUV,
respectively).
The brightest location in the galaxy has a surface brightness of
5.2$\times10^{-16}$  and
1.3$\times10^{-15}$~ergs~cm$^{-2}$s$^{-1}$\AA$^{-1}$asec$^{-2}$ (FUV, NUV).

   Since GALEX has already observed this field, it is known to
be detector-safe.  As indicated by the GALEX Brightness Checker,
there are no very bright stars in or outside the field but near enough to be dangerous to the detectors.   We have offset the pointing center from the galaxy slightly, to
minimize internal reflections from nearby stars and to align
with the existing images.

FUV emission from the filament in the 2 ksec image is detected down to a level of 8~$\times$10$^{-18}$~ergs~cm$^{-2}$~sec$^{-1}$~\AA$^{-1}$
(5 $\times$ rms; m$_{\rm AB}$ $\sim$ 24.5 arcsec$^{-2}$). A ``typical" UV knot in the filament has a flux
3-5$\times$10$^{-16}$~ergs~cm$^{-2}$~sec$^{-1}$~\AA$^{-1}$
(m$_{\rm AB}$ $\sim$20.5); brighter knots are more like
2$\times$10$^{-15}$ cgs.
For exposure estimates, we use a ``typical" knot and
assume the UV emission has approximately a B-star spectrum.

   We require only moderate spectral resolution together with
reasonable S/N ($\sim$ 10 or better) to
identify the emission lines and measure approximate EW's for them.
Using a flux of
5$\times$10$^{-16}$~ergs~cm$^{-2}$~sec$^{-1}$~\AA$^{-1}$
and a B star spectrum with the GALEX Exposure Simulator,
we find that 15 ksec of exposure time will yield direct
images with S/N $\sim$ 50 at $\sim$1500 \AA.
For a B type spectrum (flat in the GALEX FUV band) this would
provide a spectral S/N of $<$ 1; so stellar spectra would be
detectable only from the brightest knots.  However, if the UV
is line emission from C~IV, C~III, and He~II, then we would
expect a spectral S/N $\sim$ 10; if all the emission is from
C~IV the S/N would be even higher.  We conclude that we should
be able to differentiate between shock-ionized gas, and young stars along most of the filament, with an exposure time of 15 ksec.
During parts of the year, the background from zodiacal light will be sufficiently strong that we cannot achieve the desired S/N.  We therefore request that these observations be done during times of low Zodi, i.e. between June and August 2007. We require that the Zodi be below 1.2 $\times$10$^{-18}$
 

% 6. Additional Information.  (Data analysis plan required for Archival proposals
%                 or for mixed  observing + archival proposals, 
%                otherwise optional,  text block)
% Enter text after the \additionalinfo keyword.  Up to one
% page of text can be supplied here to describe anything
% else about your proposed program that is relevant or that
% the review panel should know (such as data analysis plans,
% existence of corrolary data, justification for any coordinated 
% observations, willingness to forgo proprietary time, etc.).
% PLEASE DO NOT USE ANY COLONS IN ANY TEXT FIELD
%(use  $\colon$ ).
% PLEASE DO NOT ATTEMPT TO CHANGE THE FONT SIZES OR SPACINGS.
%  <=1 page
\additionalinfo   

\begin{itemize}

\item \noindent{\it X-ray spectra:} We have been granted XMM time
(R2D2, Solo, Skywalker) to
observe the UV-brightest location in the outer filament
to look for line emission, particularly from
[O VI]$\lambda\lambda$1032,1038 (predicted to
be very strong in  shocks) and will include the XMM results
in our analysis. Investigators Solo and R2D2 are
experienced at reducing and analyzing UV spectral data, and at
comparison with shock models.

\item \noindent{\it Neutral hydrogen:}  We will also
combine the GALEX data (imaging and spectroscopy) with
existing and new H~I data (investigators R2D2, Organa), to look
for evidence of interactions with smaller, less dense clouds.
\item\ \noindent {\it Optical imaging:} We have some emission line images in hand, and are analyzing them together with the existing GALEX image. Sensitive new ground-based emission-line imaging observations are planned, using the ESO WI-FI camera.  (investigators Organa, Solo)
\end{itemize}

% 7. Investigator Information.  (Optional, text block)
% If desired, provide a short biographical sketch for the PI, including
% recent publications relevant to this proposal.  Relevant
% information about co-investigators may also be included
% here at the proposer's discretion, but the total length
% of this section must not exceed 1 page when formatted.
% PLEASE DO NOT USE ANY COLONS IN ANY TEXT FIELD
% (use  $\colon$ ).
% PLEASE DO NOT ATTEMPT TO CHANGE THE FONT SIZES OR SPACINGS.
% <= 1 page
\vita   

L. Organa is  currently a research professor at Rebellion University. Since August 1999 she has been a member of the FUSE science
team, working on analysis of FUSE spectra of
Emperors and hot stars. She is an intergalactically recognized expert on the motivation, formation, and spontaneous self-organization of SBH's and AGN's. C. R2D2 is a staff astronomer at the Institute for Advanced Artifical Intelligence (IAAI), where he is a system scientist
with primary responsibilitiies to provide support for users of
the new Super duper Radio Telescope (both H~I and continuum).
His research involves multiwavelength (mainly optical and radio)
observations of active galaxies and the study of their ISM.
H. Solo is a Postdoctoral Scholar at Rumrunner, Inc., and a member of the Strange Transportation Devices Science Working Group.  His
research interests are focused primarily toward unorthodox but fast methods of interstellar travel and transport.  He is an expert on evasive action and masked emission signatures.

%---------------------------------------------------------------------- 
% 8. Target List and Cover Page Information
%----------------------------------------------------------------------
% 
% Cover and Target forms now submitted through AKBAR.
% DO NOT submit a LATEX target file from an earlier cycle.  
% Instead, proposers are REQUIRED to submit their target lists and 
% Cover Page information through AKBAR.   Please see 
% http://galexgi.gsfc.nasa.gov/propforms/index.html 
% or
% http://heasarc.gsfc.nasa.gov/AKBAR
% information. 
%

\end{document}