Remeis-Wiki - User contributions [en]

Presentations:felixgx301

2018-04-13T15:15:00Z

Castro:

[[Category:LaTeX]]
====== GX 301-2 talk ======

===== Header =====
<pre>
\documentclass{beamer}
\usetheme{Madrid}

\useinnertheme{circles}
\usecolortheme{dolphin}

\usepackage[utf8]{inputenc} % ggfs. anpassen -- Eingabekodierung
\usepackage[T1]{fontenc} % Zeichensatzkodierung
\usepackage[english]{babel} % Sprache einstellen
\usepackage{ragged2e} % besserer Flattersatz
\usepackage{xspace} % intelligenter Abstand

\usepackage{tikz} % Plotting and alignment tools
\usetikzlibrary{shadows}
\usetikzlibrary{fadings}

\usepackage{natbib}
\bibliographystyle{jwaabib}
\def\newblock{\hskip .11em plus .33em minus .07em}
</pre>
===== Example slide =====
<pre>
\begin{frame}
\frametitle{Time resolved spectroscopy}

\begin{tikzpicture}[x=\columnwidth, y=0.6\textheight]

\path<1-> [use as bounding box] (0,0) rectangle(1,1); % define the coordinate system

\node<1> at (0.5,0.5) {\includegraphics[width=0.78\columnwidth]{plots/all4speclc_2-10.pdf}}; %plot figure in the center
\node<2> at (0.5,0.5) {\includegraphics[width=0.78\columnwidth]{plots/all4speclc_zoom.pdf}};
\node<3> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_nogslines.pdf}};
\node<4-8> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_normnogslines.pdf}};

\draw<5-6> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Eqw. of \feka highest during part II} ;
% text in a nice box
\draw<6> (-0.02,0.65) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Spectra change strongly with time.} ;
\draw<7-8> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Energy shift could be due to change in ionization.} ;
\draw<8> (-0.02,0.55) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Mixture of different states necessary to explain \fekb/\feka ratio (Fe\,VI--XIV).} ;
\node<9-> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_felineeqw.pdf}};
\draw<10-> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Gainshift also explains shifts!} ;
\draw<11> (-0.02,0.65) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Gainshift can be due to change of CTI.} ;

\end{tikzpicture}
\end{frame}
</pre>

===== Source =====
The complete talk can be found here: ''/home/fuerst/Public/talks/gx301/''

Presentations:thomas feLines

2018-04-13T15:14:00Z

Castro:

[[Category:LaTeX]]

=== Fe Lines Talk ===

I made this presentation in only a few days. Hence, not everything is coded very well. Nevertheless you might find some interesting features you can use for your presentation. If you've got questions: Just ask me! :-)

===== Header =====

<pre>
\documentclass[usenatbib]{beamer}
% if you use the draft option (\documentclass[usenatbib,draft]{beamer}) the images
% are not included. You can safe a lot of time using this option, if you do not need
% to look at your figures.

\usepackage[latin1]{inputenc}
\usepackage{hyperref}
\usepackage{colortbl} % colored tables
\usepackage{natbib} % the bibliography is in natbib style
\usepackage{url} % est urls with \url{...} correctly
\usepackage{amssymb} % more symbols
\usepackage{amsmath} % standard math packag
\usepackage{amsfonts}
\usepackage{graphicx}
\usepackage{multicol} % allows you to create multiple columns
\usepackage{pstricks,pst-grad,pst-text} % pstricks ...

% set your graphics path
\graphicspath{{./figs/}}

% select your favourite theme
\usetheme{Frankfurt}
</pre>

===== Definitions/Functions =====
<pre>
% define your own colors:
% especially the standard green needs to be dark
\definecolor{tdgreen}{rgb}{0,0.6,0}
\definecolor{tdblue} {rgb}{.114, .157, .706 }
\definecolor{tdred} {rgb}{0.922, .086, .086 }

% for creating my title page, I define my font sizes
\newcommand\titleFontSize{\fontsize{0.65cm}{0.6cm}\selectfont}
\newcommand\authorFontSize{\fontsize{0.55cm}{0.5cm}\selectfont}

% simple commands for highlighting text in different colors
\newcommand{\greentext}[1]{{\color{tdgreen}#1}}
\newcommand{\redtext}[1]{{\color{tdred}#1}}
\newcommand{\bluetext}[1]{{\color{tdblue}#1}}

% define my own slides: style chosen here is plain
\newcommand{\tdframe}[1]{\frame[plain]{#1}}

% define a compact itemize-environment
\newenvironment{itemize*}%
{\begin{itemize}%
\setlength{\itemsep}{0pt}%
\setlength{\parskip}{0pt}}%
{\end{itemize}}

% define an outlined caption with ps-tricks: text in "Caption" is surrounded by a black line.
% this is useful if you use a background image, but the title/authors should still be readable
\definecolor{Caption}{rgb}{0.8,0.1,0.01}
\newcommand\outlineCaption[1]{\textbf{\pscharpath[linecolor=black,linewidth=.1pt,
gradangle=90,fillstyle=gradient,gradbegin=Caption,gradend=Caption,gradmidpoint=1]{#1}}}
</pre>

===== Title Page =====
<pre>
{
% this sets the background image. It is set only for this slide, as the whole section is enclosed
% in brackets
\usebackgroundtemplate{\includegraphics[width=\paperwidth,height=\paperheight]{agn_nasa}}

% start the slide
\tdframe{
\centering
\vspace{0.5cm}
\color{Authors}
\bf
{\titleFontSize \outlineCaption{Measuring the Spin of a Black Hole:}}
{\titleFontSize \outlineCaption{Broad Iron Emission Lines}}

\vspace{1cm}

{\authorFontSize\textbf{Thomas Dauser$^1$} }

\vspace{0.66cm}

{\tiny in collaboration with} \\
\vspace{0.1cm}

\small
J.~Wilms$^1$, R.~Duro$^1$, C.~S.~Reynolds~(UMd), L.~Brenneman~(CfA),
K.~Pottschmidt~(CRESST/UMBC/NASA-GSFC), M.~A.~Nowak(MIT),
N.~Schartel~(ESA-ESOC), and J.~Svoboda~(CAS)

\vspace{0.4cm}

{\footnotesize $^1$ Dr. Karl Remeis Observatory Bamberg \& ECAP}

% set the logos
\raisebox{-1.35cm}[0cm][0cm]{
% logs need a white box to look good
\colorbox{white}{
\includegraphics[width=0.25\textwidth]{uni-erlangen.eps} \hspace{5.1cm}
\includegraphics[width=0.2\textwidth]{ecap_logo_transparent.eps}
}
}
}
}
</pre>

====== Example Slide ======

<pre>
\tdframe{
\frametitle{Accretion Geometry: Source of hard X-rays}

\begin{columns}
\begin{column}{0.55\textwidth}
\includegraphics[width=\columnwidth]{diff_geo_corona}
\end{column}
\begin{column}{0.5\textwidth}
\begin{alertblock}{}\textbf{Sandwich/Sphere Corona}
{\footnotesize Comptonization from a \bluetext{hot electron
plasma} surrounding the disk {\tiny
\citep[][\ldots]{Haardt1993a,Dove1997a}}}
\greentext{canonical $\alpha$-disk: $r^{-3}$} {\footnotesize
{\tiny\citep[in AGN usually higher values observed, e.g.,
][]{wilms2001a}}}
\end{alertblock}
\end{column}
\end{columns}

\vspace{0.9cm}\hrule\vspace{0.6cm}

\begin{columns}
\begin{column}{0.55\textwidth}
\includegraphics[width=\columnwidth]{diff_geo_jet}
\end{column}
\begin{column}{0.5\textwidth}
\begin{alertblock}{}\textbf{Jet Base Geometry}
{\footnotesize Comptonization from the base of a jet {\tiny
\citep[][\ldots]{Matt1992a,Markoff2005a,Miniutti2007a}}}
\greentext{``lensing effect'': steep emissivity} towards
$r_\mathrm{ISCO}$
\end{alertblock}
\end{column}
\end{columns}

}
</pre>

Getting started with TIKZ

2018-04-13T12:41:04Z

Castro: Alex M.: basic TIKZ for positioning text/figures and drawing

==== Getting started with TIKZ ====

TIKZ can give you some measure of control when you want to position
text or figures, and is useful for drawing basic shapes (lines,
arrows, highlight boxes, polygons).

Most of what I learned from TIKZ comes from
1) Z. Walczak's manual at
http://www.tug.org/TUGboat/tb29-1/tb91walczak.pdf
and 2) other people's TIKZ slides.

See also http://www.cremeronline.com/LaTeX/minimaltikz.pdf

This page summarizes what I have been able to understand;
please see the tex file and pdf result for the code below at
/home/markowitz/talks/litclub/tikzprac.pdf and tikzprac.tex

=== Header and definitions (mostly taken from one of Tommy's talks) ===

\documentclass{beamer}
\usetheme{Frankfurt}

\useinnertheme{circles}
\usecolortheme{wolverine}

\usepackage[utf8]{inputenc} % ggfs. anpassen -- Eingabekodierung
\usepackage[T1]{fontenc} % Zeichensatzkodierung
\usepackage[english]{babel} % Sprache einstellen
\usepackage{ragged2e} % besserer Flattersatz
\usepackage{xspace} % intelligenter Abstand
\usepackage{graphicx}
\usepackage{multicol}
\usepackage{pdfpages}

\usepackage{tikz} % Plotting and alignment tools
\usetikzlibrary{shadows}
\usetikzlibrary{fadings}
\usepackage[outline]{contour}
\contourlength{0.2pt}
% set your graphics path
\graphicspath{{./figsXTE/}}
\newcommand{\Msun}{\hbox{$\rm\thinspace M_{\odot}$}}
\newcommand{\Lsun}{\hbox{$\rm\thinspace L_{\odot}$}}

\setbeamersize{text margin left=5mm}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
% define your own colors:
% especially the standard green needs to be dark
\definecolor{tdgreen}{rgb}{0,0.6,0}
\definecolor{tdblue}{rgb}{.114, .157, .706 }
\definecolor{tdred}{rgb}{0.922, .086, .086 }
\definecolor{agmcyan}{rgb}{0.401, .986, .986 }

% for creating my title page, I define my font sizes
\newcommand\titleFontSize{\fontsize{0.65cm}{0.6cm}\selectfont}
\newcommand\authorFontSize{\fontsize{0.55cm}{0.5cm}\selectfont}
% simple commands for highlighting text in different colors
\newcommand{\greentext}[1]{{\color{tdgreen}#1}}
\newcommand{\redtext}[1]{{\color{tdred}#1}}
\newcommand{\bluetext}[1]{{\color{tdblue}#1}}
\newcommand{\yellowtext}[1]{{\color{yellow}#1}}
\newcommand{\cyantext}[1]{{\color{agmcyan}\contour{black}{#1}}}

% define my own slides: style chosen here is plain
\newcommand{\tdframe}[1]{\frame[plain]{#1}}

\definecolor{Authors}{rgb}{0.8,0.1,0.01}
\newcommand\outlineCaption[1]{\textbf{\pscharpath[linecolor=orange,linewidth=.1pt, gradangle=90,fillstyle=gradient,gradbegin=Authors,gradend=Authors,gradmidpoint=1]{#1}}}

=== Code for setting up a TIKZ picture, positioning and drawing ===

\begin{document}
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\section{Intro.}
\begin{frame}
\frametitle{Anchors, Lines, Arrows}
\centering

%%% Do "y=\textheight" if there is no "\frametitle"
%%% Do "y=0.88\textheight" if there is a "\frametitle"
\begin{tikzpicture}[x=\columnwidth, y=0.88\textheight]
% define the coordinate system
\path [use as bounding box] (0,0) rectangle(1,1);

% % % % % % % % anchoring a picture:

\draw (0.06,0.85) node [anchor=west]
{\includegraphics[height=2.8\baselineskip]{f3a.jpg}} ;

% % % % % % % % anchoring text:

\draw[color=tdgreen] (0.50,0.90) node [anchor=west]
{\tiny \centering \textbf{0.50 0.90 anchor=west}} ;

\draw[color=red] (0.50,0.90) node [anchor=east]
{\tiny \centering \textbf{0.50 0.90 anchor=east}} ;

\draw[color=blue] (0.50,0.90) node [anchor=north]
{\tiny \centering \textbf{0.50 0.90 anchor=north}} ;

\draw[color=pink] (0.50,0.90) node [anchor=south]
{\tiny \centering \textbf{0.50 0.90 anchor=south}} ;

% % % % % % % % Highlight boxes:

\draw[color=yellow] (0.87,0.94) node [anchor=center,text width=2.4cm,fill=black!65, rounded corners]
{\centering \textbf{Highlight box}};

\draw[color=yellow] (0.87,+0.80)
node [anchor=center, text width=0.7cm, fill=tdgreen!85, drop shadow]
{ {\scriptsize \centering \textbf{Box2}} };

\draw[color=black] (0.87,+0.66)
node [anchor=center, text width=0.7cm, fill=black!05, drop shadow, rounded corners]
{ {\scriptsize \centering \textbf{Box3}} };

% % % % % % % % Lines and arrows (curved \& straight):

\draw [-, line width=0.1mm, color=purple] (0.00,0.00) -- (0.00,1.00);
\draw [-, line width=0.1mm, color=yellow] (1.00,0.00) -- (1.00,1.00);

\draw [->,line width=0.8mm, color=orange] (0.06,0.43) -- (0.18,0.43);
\draw [-, line width=0.6mm, color=red] (0.06,0.40) -- (0.18,0.38);

\draw [<->,line width=0.4mm, color=green] (0.06,0.35) to
[out=40,in=135] (0.18,0.33);

\draw [->,line width=0.2mm, color=cyan] (0.06,0.32) to
[out=+40,in=-70] (0.22,0.25);

\draw [->,line width=0.2mm, color=tdblue] (0.06,0.25) to
[out=-40,in=-70] (0.22,0.15);

% % % % % % % % drawing shapes and associated text:

\draw (0.50,0.25) node
[circle,draw,dashed]{1} -- (0.55,0.33) node [circle,draw,dashed]{2};

\draw
(0.50,0.11) node [anchor=north east,circle,draw,dashed]{3} --
(0.55,0.19) node [anchor=south west,circle,draw,dashed]{4};

% % % % % % % % drawing shapes and associated text: a rectangle with text:

\draw [color=red] (0.85,0.25) node
[rectangle,dashed,draw,color=green,label=above:On Top,label=below:{\textbf{under}}]{\textit{my rectangle}};

\end{tikzpicture}
\end{frame}

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
\section{more shapes}
\begin{frame}
%\frametitle{Slide 2}
\centering

%%% Do "y=\textheight" if there is no "\frametitle"
%%% Do "y=0.88\textheight" if there is a "\frametitle"
\begin{tikzpicture}[x=\columnwidth, y=\textheight]
% define the coordinate system
\path [use as bounding box] (0,0) rectangle(1,1);
\draw [-, line width=0.1mm, color=brown] (0.00,0.00) -- (0.00,1.00)
-- (1.00,1.00) -- (1.00,0.00) -- cycle;

% % % % % % % % % % % % Circles:
\draw (0.08,0.86) circle (6mm);
\draw [line width=0.8mm,color=green] (0.23,0.86) circle (4ex);

% % % % % % % % % % % % Filled circle:
\draw [line width=1.8mm,color=orange,fill=gray!30!white] (0.38,0.86) circle (4ex);

% % % % % % % % % % % % Ellipses:
\draw (0.56, 0.86) [line width=0.2mm,color=blue] ellipse (7pt and 24pt);
\draw (0.56, 0.86) [line width=0.2mm,color=gray] ellipse (24pt and 7pt);

% % % % % % % % % % % % A filled triangle:
\draw [color=green,fill=brown,line width=0.2mm] (0.82,0.90) -- (0.89,0.97) --
(0.94,0.93) -- cycle;

% % % % % % % % % % % % Arcs and filled arcs:
% % % % % % % % % % % % (notice that those are semicolons,
% % % % % % % % % % % % not commas, in the arguments for 'arc')
\draw (0.23,0.65) [line width=0.6mm,color=brown,dashed] arc (-65:+80:2ex);
\draw (0.33,0.65) [line width=0.2mm,color=red] arc (-45:+60:2ex);
\draw (0.43,0.65) [line width=0.4mm,color=blue,fill=yellow] arc (-45:+68:2ex);

% % % % % % % % % % % % A shape with an arc and lines:
\fill [yellow] (0.50,0.50) -- (0.56,0.57) arc(-135:+88:5ex) -- cycle;

% % % % % % % % % % % % Grids:
\draw [step=0.50cm,cyan,thin,dashed] (0.12,0.03) grid (0.9,0.45);
\draw [step=0.25cm,gray,thick,dotted] (0.9,0.03) grid (0.97,0.45);

% % % % % % % % % % % % Polygons featuring arcs:
% % % % % % % % % % % % Pac-man:
\draw [line width=0.1mm,fill=yellow] (0.39,0.24) --
(0.4766,0.29) arc (+25:+335:1.1cm) -- cycle;
% % % % % % % % % % % % Ghost:
\draw [color=cyan,fill=blue,line width=0.2mm] (0.60,0.17) -- (0.60,0.25)
arc (+180:0:0.05\textwidth) -- (0.70,0.17) --
(0.683,0.19) --
(0.667,0.17) --
(0.650,0.19) --
(0.633,0.17) --
(0.616,0.19) -- cycle;
\draw (0.6363,0.26) [color=pink,fill] circle (0.31ex);
\draw (0.6637,0.26) [color=pink,fill] circle (0.31ex);
\draw [-,color=pink,line width=0.2mm] (0.617,0.22) to
[out=+0,in=+180] (0.628,0.225) to
[out=+0,in=+180] (0.639,0.22) to
[out=+0,in=+180] (0.650,0.225) to
[out=+0,in=+180] (0.661,0.22) to
[out=+0,in=+180] (0.672,0.225) to
[out=+0,in=+180] (0.683,0.22) ;

\end{tikzpicture}
\end{frame}

Presentations:thomas feLines

2018-04-13T12:24:37Z

Castro:

[[Category:LaTeX]]

=== Fe Lines Talk ===

I made this presentation in only a few days. Hence, not everything is coded very well. Nevertheless you might find some interesting features you can use for your presentation. If you've got questions: Just ask me! :-)

===== Header =====

\documentclass[usenatbib]{beamer}
% if you use the draft option (\documentclass[usenatbib,draft]{beamer}) the images
% are not included. You can safe a lot of time using this option, if you do not need
% to look at your figures.

\usepackage[latin1]{inputenc}
\usepackage{hyperref}
\usepackage{colortbl} % colored tables
\usepackage{natbib} % the bibliography is in natbib style
\usepackage{url} % est urls with \url{...} correctly
\usepackage{amssymb} % more symbols
\usepackage{amsmath} % standard math packag
\usepackage{amsfonts}
\usepackage{graphicx}
\usepackage{multicol} % allows you to create multiple columns
\usepackage{pstricks,pst-grad,pst-text} % pstricks ...

% set your graphics path
\graphicspath{{./figs/}}

% select your favourite theme
\usetheme{Frankfurt}

===== Definitions/Functions =====

% define your own colors:
% especially the standard green needs to be dark
\definecolor{tdgreen}{rgb}{0,0.6,0}
\definecolor{tdblue} {rgb}{.114, .157, .706 }
\definecolor{tdred} {rgb}{0.922, .086, .086 }

% for creating my title page, I define my font sizes
\newcommand\titleFontSize{\fontsize{0.65cm}{0.6cm}\selectfont}
\newcommand\authorFontSize{\fontsize{0.55cm}{0.5cm}\selectfont}

% simple commands for highlighting text in different colors
\newcommand{\greentext}[1]{{\color{tdgreen}#1}}
\newcommand{\redtext}[1]{{\color{tdred}#1}}
\newcommand{\bluetext}[1]{{\color{tdblue}#1}}

% define my own slides: style chosen here is plain
\newcommand{\tdframe}[1]{\frame[plain]{#1}}

% define a compact itemize-environment
\newenvironment{itemize*}%
{\begin{itemize}%
\setlength{\itemsep}{0pt}%
\setlength{\parskip}{0pt}}%
{\end{itemize}}

% define an outlined caption with ps-tricks: text in "Caption" is surrounded by a black line.
% this is useful if you use a background image, but the title/authors should still be readable
\definecolor{Caption}{rgb}{0.8,0.1,0.01}
\newcommand\outlineCaption[1]{\textbf{\pscharpath[linecolor=black,linewidth=.1pt,
gradangle=90,fillstyle=gradient,gradbegin=Caption,gradend=Caption,gradmidpoint=1]{#1}}}

===== Title Page =====

{
% this sets the background image. It is set only for this slide, as the whole section is enclosed
% in brackets
\usebackgroundtemplate{\includegraphics[width=\paperwidth,height=\paperheight]{agn_nasa}}

% start the slide
\tdframe{
\centering
\vspace{0.5cm}
\color{Authors}
\bf
{\titleFontSize \outlineCaption{Measuring the Spin of a Black Hole:}}
{\titleFontSize \outlineCaption{Broad Iron Emission Lines}}

\vspace{1cm}

{\authorFontSize\textbf{Thomas Dauser$^1$} }

\vspace{0.66cm}

{\tiny in collaboration with} \\
\vspace{0.1cm}

\small
J.~Wilms$^1$, R.~Duro$^1$, C.~S.~Reynolds~(UMd), L.~Brenneman~(CfA),
K.~Pottschmidt~(CRESST/UMBC/NASA-GSFC), M.~A.~Nowak(MIT),
N.~Schartel~(ESA-ESOC), and J.~Svoboda~(CAS)

\vspace{0.4cm}

{\footnotesize $^1$ Dr. Karl Remeis Observatory Bamberg \& ECAP}

% set the logos
\raisebox{-1.35cm}[0cm][0cm]{
% logs need a white box to look good
\colorbox{white}{
\includegraphics[width=0.25\textwidth]{uni-erlangen.eps} \hspace{5.1cm}
\includegraphics[width=0.2\textwidth]{ecap_logo_transparent.eps}
}
}
}
}

====== Example Slide ======

\tdframe{
\frametitle{Accretion Geometry: Source of hard X-rays}

\begin{columns}
\begin{column}{0.55\textwidth}
\includegraphics[width=\columnwidth]{diff_geo_corona}
\end{column}
\begin{column}{0.5\textwidth}
\begin{alertblock}{}\textbf{Sandwich/Sphere Corona}
{\footnotesize Comptonization from a \bluetext{hot electron
plasma} surrounding the disk {\tiny
\citep[][\ldots]{Haardt1993a,Dove1997a}}}
\greentext{canonical $\alpha$-disk: $r^{-3}$} {\footnotesize
{\tiny\citep[in AGN usually higher values observed, e.g.,
][]{wilms2001a}}}
\end{alertblock}
\end{column}
\end{columns}

\vspace{0.9cm}\hrule\vspace{0.6cm}

\begin{columns}
\begin{column}{0.55\textwidth}
\includegraphics[width=\columnwidth]{diff_geo_jet}
\end{column}
\begin{column}{0.5\textwidth}
\begin{alertblock}{}\textbf{Jet Base Geometry}
{\footnotesize Comptonization from the base of a jet {\tiny
\citep[][\ldots]{Matt1992a,Markoff2005a,Miniutti2007a}}}
\greentext{``lensing effect'': steep emissivity} towards
$r_\mathrm{ISCO}$
\end{alertblock}
\end{column}
\end{columns}

}

Presentations:thomas feLines

2018-04-13T10:39:18Z

Castro:

[[Category:LaTeX]]

=== Fe Lines Talk ===

I made this presentation in only a few days. Hence, not everything is coded very well. Nevertheless you might find some interesting features you can use for your presentation. If you've got questions: Just ask me! :-)

===== Header =====

\documentclass[usenatbib]{beamer}
% if you use the draft option (\documentclass[usenatbib,draft]{beamer}) the images
% are not included. You can safe a lot of time using this option, if you do not need
% to look at your figures.

\usepackage[latin1]{inputenc}
\usepackage{hyperref}
\usepackage{colortbl} % colored tables
\usepackage{natbib} % the bibliography is in natbib style
\usepackage{url} % est urls with \url{...} correctly
\usepackage{amssymb} % more symbols
\usepackage{amsmath} % standard math packag
\usepackage{amsfonts}
\usepackage{graphicx}
\usepackage{multicol} % allows you to create multiple columns
\usepackage{pstricks,pst-grad,pst-text} % pstricks ...

% set your graphics path
\graphicspath{{./figs/}}

% select your favourite theme
\usetheme{Frankfurt}

===== Definitions/Functions =====

% define your own colors:
% especially the standard green needs to be dark
\definecolor{tdgreen}{rgb}{0,0.6,0}
\definecolor{tdblue} {rgb}{.114, .157, .706 }
\definecolor{tdred} {rgb}{0.922, .086, .086 }

% for creating my title page, I define my font sizes
\newcommand\titleFontSize{\fontsize{0.65cm}{0.6cm}\selectfont}
\newcommand\authorFontSize{\fontsize{0.55cm}{0.5cm}\selectfont}

% simple commands for highlighting text in different colors
\newcommand{\greentext}[1]{{\color{tdgreen}#1}}
\newcommand{\redtext}[1]{{\color{tdred}#1}}
\newcommand{\bluetext}[1]{{\color{tdblue}#1}}

% define my own slides: style chosen here is plain
\newcommand{\tdframe}[1]{\frame[plain]{#1}}

% define a compact itemize-environment
\newenvironment{itemize*}%
{\begin{itemize}%
\setlength{\itemsep}{0pt}%
\setlength{\parskip}{0pt}}%
{\end{itemize}}

% define an outlined caption with ps-tricks: text in "Caption" is surrounded by a black line.
% this is useful if you use a background image, but the title/authors should still be readable
\definecolor{Caption}{rgb}{0.8,0.1,0.01}
\newcommand\outlineCaption[1]{\textbf{\pscharpath[linecolor=black,linewidth=.1pt,
gradangle=90,fillstyle=gradient,gradbegin=Caption,gradend=Caption,gradmidpoint=1]{#1}}}
</file>

===== Title Page =====
<file>
{
% this sets the background image. It is set only for this slide, as the whole section is enclosed
% in brackets
\usebackgroundtemplate{\includegraphics[width=\paperwidth,height=\paperheight]{agn_nasa}}

% start the slide
\tdframe{
\centering
\vspace{0.5cm}
\color{Authors}
\bf
{\titleFontSize \outlineCaption{Measuring the Spin of a Black Hole:}}
{\titleFontSize \outlineCaption{Broad Iron Emission Lines}}

\vspace{1cm}

{\authorFontSize\textbf{Thomas Dauser$^1$} }

\vspace{0.66cm}

{\tiny in collaboration with} \\
\vspace{0.1cm}

\small
J.~Wilms$^1$, R.~Duro$^1$, C.~S.~Reynolds~(UMd), L.~Brenneman~(CfA),
K.~Pottschmidt~(CRESST/UMBC/NASA-GSFC), M.~A.~Nowak(MIT),
N.~Schartel~(ESA-ESOC), and J.~Svoboda~(CAS)

\vspace{0.4cm}

{\footnotesize $^1$ Dr. Karl Remeis Observatory Bamberg \& ECAP}

% set the logos
\raisebox{-1.35cm}[0cm][0cm]{
% logs need a white box to look good
\colorbox{white}{
\includegraphics[width=0.25\textwidth]{uni-erlangen.eps} \hspace{5.1cm}
\includegraphics[width=0.2\textwidth]{ecap_logo_transparent.eps}
}
}
}
}
</file>

===== Example Slide ======

<file>
\tdframe{
\frametitle{Accretion Geometry: Source of hard X-rays}

\begin{columns}
\begin{column}{0.55\textwidth}
\includegraphics[width=\columnwidth]{diff_geo_corona}
\end{column}
\begin{column}{0.5\textwidth}
\begin{alertblock}{}\textbf{Sandwich/Sphere Corona}
{\footnotesize Comptonization from a \bluetext{hot electron
plasma} surrounding the disk {\tiny
\citep[][\ldots]{Haardt1993a,Dove1997a}}}
\greentext{canonical $\alpha$-disk: $r^{-3}$} {\footnotesize
{\tiny\citep[in AGN usually higher values observed, e.g.,
][]{wilms2001a}}}
\end{alertblock}
\end{column}
\end{columns}

\vspace{0.9cm}\hrule\vspace{0.6cm}

\begin{columns}
\begin{column}{0.55\textwidth}
\includegraphics[width=\columnwidth]{diff_geo_jet}
\end{column}
\begin{column}{0.5\textwidth}
\begin{alertblock}{}\textbf{Jet Base Geometry}
{\footnotesize Comptonization from the base of a jet {\tiny
\citep[][\ldots]{Matt1992a,Markoff2005a,Miniutti2007a}}}
\greentext{``lensing effect'': steep emissivity} towards
$r_\mathrm{ISCO}$
\end{alertblock}
\end{column}
\end{columns}

}
</file>

Presentations:thomas feLines

2018-04-13T10:37:00Z

Castro: Thomas\' Fe Lines talk

=== Fe Lines Talk ======

I made this presentation in only a few days. Hence, not everything is coded very well. Nevertheless you might find some interesting features you can use for your presentation. If you've got questions: Just ask me! :-)

===== Header =====

<file>
\documentclass[usenatbib]{beamer}
% if you use the draft option (\documentclass[usenatbib,draft]{beamer}) the images
% are not included. You can safe a lot of time using this option, if you do not need
% to look at your figures.

\usepackage[latin1]{inputenc}
\usepackage{hyperref}
\usepackage{colortbl} % colored tables
\usepackage{natbib} % the bibliography is in natbib style
\usepackage{url} % est urls with \url{...} correctly
\usepackage{amssymb} % more symbols
\usepackage{amsmath} % standard math packag
\usepackage{amsfonts}
\usepackage{graphicx}
\usepackage{multicol} % allows you to create multiple columns
\usepackage{pstricks,pst-grad,pst-text} % pstricks ...

% set your graphics path
\graphicspath{{./figs/}}

% select your favourite theme
\usetheme{Frankfurt}

</file>

===== Definitions/Functions =====

<file>

% define your own colors:
% especially the standard green needs to be dark
\definecolor{tdgreen}{rgb}{0,0.6,0}
\definecolor{tdblue} {rgb}{.114, .157, .706 }
\definecolor{tdred} {rgb}{0.922, .086, .086 }

% for creating my title page, I define my font sizes
\newcommand\titleFontSize{\fontsize{0.65cm}{0.6cm}\selectfont}
\newcommand\authorFontSize{\fontsize{0.55cm}{0.5cm}\selectfont}

% simple commands for highlighting text in different colors
\newcommand{\greentext}[1]{{\color{tdgreen}#1}}
\newcommand{\redtext}[1]{{\color{tdred}#1}}
\newcommand{\bluetext}[1]{{\color{tdblue}#1}}

% define my own slides: style chosen here is plain
\newcommand{\tdframe}[1]{\frame[plain]{#1}}

% define a compact itemize-environment
\newenvironment{itemize*}%
{\begin{itemize}%
\setlength{\itemsep}{0pt}%
\setlength{\parskip}{0pt}}%
{\end{itemize}}

% define an outlined caption with ps-tricks: text in "Caption" is surrounded by a black line.
% this is useful if you use a background image, but the title/authors should still be readable
\definecolor{Caption}{rgb}{0.8,0.1,0.01}
\newcommand\outlineCaption[1]{\textbf{\pscharpath[linecolor=black,linewidth=.1pt,
gradangle=90,fillstyle=gradient,gradbegin=Caption,gradend=Caption,gradmidpoint=1]{#1}}}
</file>

===== Title Page =====
<file>
{
% this sets the background image. It is set only for this slide, as the whole section is enclosed
% in brackets
\usebackgroundtemplate{\includegraphics[width=\paperwidth,height=\paperheight]{agn_nasa}}

% start the slide
\tdframe{
\centering
\vspace{0.5cm}
\color{Authors}
\bf
{\titleFontSize \outlineCaption{Measuring the Spin of a Black Hole:}}
{\titleFontSize \outlineCaption{Broad Iron Emission Lines}}

\vspace{1cm}

{\authorFontSize\textbf{Thomas Dauser$^1$} }

\vspace{0.66cm}

{\tiny in collaboration with} \\
\vspace{0.1cm}

\small
J.~Wilms$^1$, R.~Duro$^1$, C.~S.~Reynolds~(UMd), L.~Brenneman~(CfA),
K.~Pottschmidt~(CRESST/UMBC/NASA-GSFC), M.~A.~Nowak(MIT),
N.~Schartel~(ESA-ESOC), and J.~Svoboda~(CAS)

\vspace{0.4cm}

{\footnotesize $^1$ Dr. Karl Remeis Observatory Bamberg \& ECAP}

% set the logos
\raisebox{-1.35cm}[0cm][0cm]{
% logs need a white box to look good
\colorbox{white}{
\includegraphics[width=0.25\textwidth]{uni-erlangen.eps} \hspace{5.1cm}
\includegraphics[width=0.2\textwidth]{ecap_logo_transparent.eps}
}
}
}
}
</file>

===== Example Slide ======

<file>
\tdframe{
\frametitle{Accretion Geometry: Source of hard X-rays}

\begin{columns}
\begin{column}{0.55\textwidth}
\includegraphics[width=\columnwidth]{diff_geo_corona}
\end{column}
\begin{column}{0.5\textwidth}
\begin{alertblock}{}\textbf{Sandwich/Sphere Corona}
{\footnotesize Comptonization from a \bluetext{hot electron
plasma} surrounding the disk {\tiny
\citep[][\ldots]{Haardt1993a,Dove1997a}}}
\greentext{canonical $\alpha$-disk: $r^{-3}$} {\footnotesize
{\tiny\citep[in AGN usually higher values observed, e.g.,
][]{wilms2001a}}}
\end{alertblock}
\end{column}
\end{columns}

\vspace{0.9cm}\hrule\vspace{0.6cm}

\begin{columns}
\begin{column}{0.55\textwidth}
\includegraphics[width=\columnwidth]{diff_geo_jet}
\end{column}
\begin{column}{0.5\textwidth}
\begin{alertblock}{}\textbf{Jet Base Geometry}
{\footnotesize Comptonization from the base of a jet {\tiny
\citep[][\ldots]{Matt1992a,Markoff2005a,Miniutti2007a}}}
\greentext{``lensing effect'': steep emissivity} towards
$r_\mathrm{ISCO}$
\end{alertblock}
\end{column}
\end{columns}

}
</file>

Presentations:felixgx301

2018-04-13T10:33:24Z

Castro:

[[Category:LaTeX]]
====== GX 301-2 talk ======

===== Header =====

\documentclass{beamer}
\usetheme{Madrid}

\useinnertheme{circles}
\usecolortheme{dolphin}

\usepackage[utf8]{inputenc} % ggfs. anpassen -- Eingabekodierung
\usepackage[T1]{fontenc} % Zeichensatzkodierung
\usepackage[english]{babel} % Sprache einstellen
\usepackage{ragged2e} % besserer Flattersatz
\usepackage{xspace} % intelligenter Abstand

\usepackage{tikz} % Plotting and alignment tools
\usetikzlibrary{shadows}
\usetikzlibrary{fadings}

\usepackage{natbib}
\bibliographystyle{jwaabib}
\def\newblock{\hskip .11em plus .33em minus .07em}

===== Example slide =====
\begin{frame}
\frametitle{Time resolved spectroscopy}

\begin{tikzpicture}[x=\columnwidth, y=0.6\textheight]

\path<1-> [use as bounding box] (0,0) rectangle(1,1); % define the coordinate system

\node<1> at (0.5,0.5) {\includegraphics[width=0.78\columnwidth]{plots/all4speclc_2-10.pdf}}; %plot figure in the center
\node<2> at (0.5,0.5) {\includegraphics[width=0.78\columnwidth]{plots/all4speclc_zoom.pdf}};
\node<3> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_nogslines.pdf}};
\node<4-8> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_normnogslines.pdf}};

\draw<5-6> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Eqw. of \feka highest during part II} ;
% text in a nice box
\draw<6> (-0.02,0.65) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Spectra change strongly with time.} ;
\draw<7-8> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Energy shift could be due to change in ionization.} ;
\draw<8> (-0.02,0.55) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Mixture of different states necessary to explain \fekb/\feka ratio (Fe\,VI--XIV).} ;
\node<9-> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_felineeqw.pdf}};
\draw<10-> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Gainshift also explains shifts!} ;
\draw<11> (-0.02,0.65) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Gainshift can be due to change of CTI.} ;

\end{tikzpicture}
\end{frame}

===== Source =====
The complete talk can be found here: ''/home/fuerst/Public/talks/gx301/''

How to start chatting with irssi

2018-04-13T10:10:45Z

Castro:

[[Category:Current Members]]
How to start chatting with '''irssi''':
screen -S chat # will open a screened terminal that you can detach and attach (called "chat")
irssi # open irssi, an awesome chat tool
/set nick <nick> # set your nickname
/set real_name <real name> # optional
/server add -auto -network Freenode irc.freenode.net 6667 # "Freenode" is just a name for the
network that includes the given IRC server attached to some local port (here 6667)
/network add -nick <nick> Freenode # add your nickname # add your nick to the network
/channel add -auto #remeis Freenode # automatically add the channel #remeis to known chat channels within the "Freenode" network
/j #remeis # join the chat
Cntr -a -d

Ok, how to use it best?
Now you told irssi everything about the network, the server, your name and the chat channel you want to join.
When logging in to your computer, you just need to open a terminal and type

screen -r chat # resume the screen called "chat" you detached from your terminal the last time

when logging out:
Cntr -a -d # detach screen

And now magic:
Create a file in your startup directory of your operating system, here KDE:
.kde/Autostart/IrssiRemeis.sh
containing the line
term -bg 'black' -fg 'white' -T 'Remeis Chat' -e 'screen -r -d'

this will automatically open a terminal every time you log in to your computer and attach the screen.
So all you got to do is to detach the screen before logging out with
Cntr -a -d

That's it. Sometimes you may encounter the problem that you opened screens from different computers and your nickname 'bla' will get '_bla', '__bla'....
Then you have to kill all screens except of one with
screen -S name_of_screen -X quit

How to start chatting with xchat:
open the terminal and start the program xchat
$ xchat

Fill out name + stuff and connect to the server called FreeNode
Then join the channel #remeis:

Three possibilites to do that:
- The first time you start xchat you should be asked which channel to join type remeis
- type /j #remeis in the chat
- click on the tab server and click Join a Channel... -> Type remeis as a channel name

Link to some useful stuff when using irc:
[[http://www.mirchelp.net/mirc_commands/]]

How to start chatting with irssi

2018-04-13T09:40:32Z

Castro: Created page with " Category:Current Members How to start chatting with **irssi**:\\ <file>screen -S chat # will open a screened terminal that you can detach and attach (called "chat")\\ ir..."

[[Category:Current Members]]

How to start chatting with **irssi**:\\
<file>screen -S chat # will open a screened terminal that you can detach and attach (called "chat")\\
irssi # open irssi, an awesome chat tool\\
/set nick <nick> # set your nickname\\
/set real_name <real name> # optional\\
/server add -auto -network Freenode irc.freenode.net 6667 # "Freenode" is just a name for the
network that includes the given IRC server attached to some local port (here 6667)\\
/network add -nick <nick> Freenode # add your nickname # add your nick to the network\\
/channel add -auto #remeis Freenode # automatically add the channel #remeis to known chat channels within the "Freenode" network\\
/j #remeis # join the chat\\
Cntr -a -d</file>\\

Ok, how to use it best?
Now you told irssi everything about the network, the server, your name and the chat channel you want to join.
When logging in to your computer, you just need to open a terminal and type

<file>screen -r chat # resume the screen called "chat" you detached from your terminal the last time</file>

when logging out:
<file>Cntr -a -d # detach screen</file>

And now magic:
Create a file in your startup directory of your operating system, here KDE:
.kde/Autostart/IrssiRemeis.sh
containing the line
<file>term -bg 'black' -fg 'white' -T 'Remeis Chat' -e 'screen -r -d'</file>

this will automatically open a terminal every time you log in to your computer and attach the screen.
So all you got to do is to detach the screen before logging out with
<file>Cntr -a -d</file>

That's it. Sometimes you may encounter the problem that you opened screens from different computers and your nickname 'bla' will get '_bla', '__bla'....
Then you have to kill all screens except of one with
<file>screen -S name_of_screen -X quit</file>\\

How to start chatting with xchat:\\
open the terminal and start the program xchat \\
$ xchat\\
\\
Fill out name + stuff and connect to the server called FreeNode\\
Then join the channel #remeis: \\

Three possibilites to do that:\\
- The first time you start xchat you should be asked which channel to join type remeis
- type /j #remeis in the chat
- click on the tab server and click Join a Channel... -> Type remeis as a channel name

Link to some useful stuff when using irc:\\
[[http://www.mirchelp.net/mirc_commands/]]

Time Series Analysis

2018-04-12T14:34:31Z

Castro: Blanked the page

Time Series Analysis

2018-04-12T14:27:58Z

Castro: Created page with " Category:Isis / Slang ====== Time Series Analysis ====== Note: This tutorial is based on the excellent time series tutorial produced by Tomaso Belloni for the 2010 summe..."

[[Category:Isis / Slang]]

====== Time Series Analysis ======
Note: This tutorial is based on the excellent time series tutorial
produced by Tomaso Belloni for the 2010 summer school on
multiwavelength data analysis available at
[[http://www.black-hole.eu/index.php/schools-workshops-and-conferences/2nd-school-on-multiwavelength-astronomy/program|that
school's www page]] (link at the bottom).

===== Introduction =====

In this part of the tutorial, we’ll approach some basic tasks in
timing analysis of x-ray time series, with particular emphasis on the
typical signals found in the data from Black-Hole Binaries. This
document is simply meant to provide rather general guidelines and is
not yet intended to be exhaustive.

Specifically, the techniques described below only apply if the time series does not have gaps and is evenly sampled.

===== Warm-up Exercise =====

Before jumping to the data, let us start with some simple simulations.
We will be using the routines from
[[http://space.mit.edu/cxc/analysis/SITAR/|SITAR]], which are part of
our standard ''isisscripts''.

We first look at some examples based on a fake data set consisting of
a sinusoidal and Gaussian noise.

To generate this example data set, a light curve with a time resolution of 1/1024 seconds and a total length of 16 seconds, use the following code:
<code>
variable ti, th, co, omega, period;

% 1024*16 time points from 0 to 16s
variable npt=1024*16;
(ti,th)=linear_grid(0,16,npt);

% our period is 1/100 s
period = 0.01;

variable pi=4.*atan(1.);

% trivial sinus plus a constant
omega=2.*pi/period;
co=10.+sin(omega*ti);

% plot the data
plot(ti,co);

% have a meaningful look
xrange(0,1); plot(ti,co);
</code>
In reality, normal data are noisy, so let's add some Gaussian noise with
zero average and unit variance:
<code>
co=co+grand(npt);
</code>
We now produce a power spectrum of our signal ''co'', using intervals
of 1024*16 length (i.e. only one interval) with a time resolution of
1/1024:
<code>
(f,pa,na,ctsa) = sitar_avg_psd(co,1024*16,1./1024,ti);
</code>
Outputs are arrays containing the frequency ''f'', the power ''pa''.
and a number containing the number of intervals in the lightcurve that
were averaged to reduce the noise, ''na'' (in this case 1),
and average intensity of the signal, ''ctsa''.

**Exercise 1**

Without looking, you should be able to guess the ﬁrst and last values
of ''f'' and its number of elements. In other words: what is the
minimum frequency, what the maximum frequency and how many frequencies
do you have? What is the frequency resolution of your power spectrum?

Verify your guesses by examining the array. Do not forget that in
slang arrays are zero based.

Plotting the power spectrum should show a peak at 100 Hz

<code>
xlabel("Frequency (Hz)");
ylabel("PSD");
% xrange resets the x range to automatic, PSDs are often plotted
% in log log
xrange; xlog; ylog;
plot(f,pa);
</code>
The rest is noise. We are not dealing with counting noise here (we
simply added some additional noisy signal), so we should not be
concerned with the normalization. If you go on a linear frequency axis
(''xlin'') and zoom on the peak at 100 Hz with ''xrange'', you can see
that the peak has a width: you should know how broad it is even
without looking.

Let us try to reduce the length of the time series by splitting it
into shorter intervals (16 intervals of 1 second each) and averaging
the resulting power spectra
<code>
(f,pa,na,ctsa) = sitar_avg_psd(co,1024,1./1024,ti);
</code>

**Exercise 2**

What are now the minimum and maximum frequency? How broad is the peak
now?

The signal we played with until now is too good. Try increasing the
amount of noise (for instance, its variance) and see whether you can
still detect the signal. It is instructive to have a visual look at
the light curves as well: Fourier analysis is a very powerful
technique and can pick up signals that are completely invisible by
eye.

**Exercise 3**

Before moving to the real data, play with signals for a bit and get a
feeling of what you can do with just a simple power spectrum command
such as ''sitar_avg_psd'':

* Try two sinusoids at different periods, harmonically related or not
* Add a phase shift to the sinusoid(s) and compare power spectra
* Try some weird combination of signal and noise

===== Time Series Analysis with Real Data ====

We have selected four RXTE data sets to cover typical examples.
These data can be downloaded at
[[http://www.black-hole.eu/index.php/schools-workshops-and-conferences/2nd-school-on-multiwavelength-astronomy/course-materials/144-hands-on-x-ray-timing|the
WWW pages of ITN 215212]]. In order to allow you to concentrate upon
the timing analysis aspect of the work, we have made available already
extracted binned light curves for the four cases:

* ''bln.lc'': An observation of Cygnus X-1 in its Low-Hard State. The short-term time variability is dominated by a number of strong band-limited noise components.
* ''typec.lc'': An observation of XTE J550-564 in its Hard Intermediate State. Here, a strong and narrow Quasi-Periodic Oscillation, with typical frequencies between 1 and 10 Hz is present, together with band-limited noise. The QPO has additional harmonic peaks.
* typeb.lc: An observation of GX 339-4 in its Soft Intermediate State. The power density spectrum is dominated by the presence of a strong 4-8 Hz QPO, accompanied by a power-law noise. The QPO has additional harmonic peaks and jitters on a time scale of about 10 seconds.
* hfqpo.lc: An observation of GRS 1915+105 where a high-frequency QPO is detected. These oscillations are weak and elusive. This is the best case ever, so that detection should not prove to be a problem.

==== Low-Hard State ====

Before moving to the frequency domain with a power spectrum, let us
have a look at the raw data and see what the light curve looks like.
The time resolution of this curve is 1.953125 ms, corresponding to 512
bins per second. The total length is 3634 seconds, just over one hour.
We can load the data and convert the number of counts to integer (to
speed up the FFT and save memory) with
<code>
(ta,ca) = fits_read_col("bln.lc","time","counts");
ca = typecast(ca,Integer_Type);
Time to plot your light curve
xlabel("Time (sec)");
ylabel("Counts");
plot_bin_integral;
xlin; ylin;
xrange; yrange;
plot(ta-ta[0],ca);
</code>

{{ :isis:tutorial:lc1.png?direct |}}

It is difﬁcult to see much at this high time resolution. Zooming on
the ﬁrst 10 seconds
<code>
xrange(0,10);
</code>
reveals some structure, but there are so few counts in each bin that
one can see the jumps between integers. At any rate, the data are
quite variable, as expected:

{{ :isis:tutorial:lc2.png?direct |}}

Let move to the frequency domain and produce a power spectrum. We’ll
calculate a PSD for each 16s interval and then average the PDS
together
<code>
(f,pa,na,ctsa) = sitar_avg_psd(ca,8192,1./2^9,ta);
</code>
here ca is the time series, 8192 is the number of points per data
interval (i.e. 16 seconds at 512 pps), 1./2^9 is the time resolution
and ta are the times for the bins, so that gaps can be taken care of.
There should not be any gap here. Plotting the PSD is not particularly
enlightening
<code>
xlabel("Frequency (Hz)");
ylabel("PSD");
% remember we limited the X axis between 0 and 10, so we need
% to reset the range
xrange;
plot(f,pa);
</code>

{{ :isis:tutorial:psd1.png?direct |}}

Plotting in loglog seems to be a much better idea
<code>
xlog; ylog;
plot(f,pa);
</code>

{{ :isis:tutorial:psd2.png?direct |}}

Some rebinning is in order. A logarithmic rebinning with a factor of 1%, meaning that each
frequency bin is 1% broader than the previous one, leads to a much
more satisfying result
<code>
(aflo,afhi,apsd,nf) = sitar_lbin_psd(f,pa,0.01);
hplot(aflo,afhi,apsd);
</code>

{{ :isis:tutorial:psd3.png?direct |}}

The flattening at high frequencies is due to the Poissonian noise,
which should be at an average level of 2 but is modiﬁed (lowered) by
the effects of detector dead time. The two possible courses to follow
in order to remove it from the data are to estimate it through the
available models or to ﬁt it with a constant value. Then subtract (see
below). Just to have a look, let us pretend it is exactly at 2 and
subtract it
<code>
dumpsd = apsd - 2.0;
hplot(aflo,afhi,dumpsd);
</code>
The full shape of the PDS is now clearly visible.

{{ :isis:tutorial:psd4.png?direct |}}

In order to extract useful information, we must fit this PSD with a
suitable model. First we must assign the PDS as a fittable data set,
with errors (power/sqrt(number of average):
<code>
variable id = sitar_define_psd(aflo,afhi,apsd,apsd/sqrt(na*nf));
</code>
This convinces isis that the PSD is really an (energy) spectrum, with
frequencies taking the place of energy. This means that all spectral models
available in isis can be used to fit the data.

If needed, we can restrict the fittable part of the PDS to a range of
frequencies, say 0.1 to 100 Hz (although 10 Hz would be a better limit!)
<code>
xnotice_en(id,0.1,100);
</code>
Now we deﬁne a suitable model for the fit as a constant (for the Poisson noise) and two zero-centered Lorentzians for the source
intrinsic noise
<code>
fit_fun("constant(1)+zfc(1)+zfc(2)");
set_par("constant(1).factor",1.99);
</code>
notice the value lower than 2!
<code>
set_par("zfc(1).norm",100);
set_par("zfc(1).f",8);
set_par("zfc(2).norm",50);
set_par("zfc(2).f",0.8);
</code>
Now we can renormalize to the integral, to help the fit, and try a fit
<code>
() = renorm_counts;
() = fit_counts;
</code>
Looking at the parameters gives you some feeling what is going on:
<code>
isis> list_par;
constant(1)+zfc(1)+zfc(2)
idx param tie-to freeze value min max
1 constant(1).factor 0 0 1.912599 0 1e+10
2 zfc(1).norm 0 0 7.5585 0 1e+08 rms
3 zfc(1).f 0 0 3.689417 1e-06 1000 Hz
4 zfc(2).norm 0 0 10.97784 0 1e+08 rms
5 zfc(2).f 0 0 0.2474409 1e-06 1000 Hz
</code>
We need to plot the fit to see how things are going. To make the plots
nice, let us define a plot structure for the plotting routines:
<code>
set_plot_widths(;d_width=3, r_width=3, m_width=3, de_width=1,re_width=1);
set_frame_line_width(3);
charsize(1.12);
fancy_plot_unit("psd","psd_leahy");
popt.dsym=0;
popt.dcol=4;
popt.decol=5;
popt.rsym=0;
popt.rcol=4;
popt.recol=5;
popt.xrange={0.05,256}; % X range: not necessary, but you can see how we do it
popt.res=1; % Plot also residuals
</code>
and then plot the resulting fit:
<code>
plot_counts(id,popt);
</code>

{{ :isis:tutorial:psd5.png?direct |}}

The fit could be better, but for the moment we will ignore this. For now,
let us be content with the result and estimate some error on the
parameters in the same way we would also do this for a spectrum:
<code>
(,) = conf_loop([1:5];save,prefix="first_bln.");
() = system("more first_bln.save");
</code>
In case you want to start from scratch, you can delete all data and restart
<code>
delete_data(all_data);
</code>

** Exercise 4**

Now you can try to do more. For instance:
* Add another zero-centered Lorentzian component to the fit and see if it gets any better.
* It is difficult to see how the model is doing even with the residuals. Try to restrict the fit to the high frequency part, say above 100 Hz, where Poissonian noise dominates. Fit this area with a constant and then subtract it from your data and go on without Poisson noise.
* Produce power spectra extending to lower frequencies to see how the noise ﬂattens. Can you also extend it to higher frequencies?
* Divide the data in more than one segment and see whether there are differences between the segments.
* Can you calculate the integrated fractional rms of the different components? What do you need to do that?

** Exercise 5 **

In order to get more of a feeling for what is going on in the data, try your hands on one of the following sections

==== Type-C Quasi-Periodic Oscillation ====
Here you encounter a low-frequency QPO in addition to band-limited
noise.

* Extract the light curve and have a look. Does it look any different from the previous one?
* Extract the power spectrum and see the QPO. How many noise components and how many QPO peaks do you think you will need? Always better to start with an underestimate and add as you go. The model to use for a QPO in isis is, not surprisingly, called ''qpo''. Its parameters are the ''norm'', ''Q'', and ''f''. They correspond to normalization, quality factor (centroid divided by FWHM of the peak) and centroid frequency.
* Do you see any differences in PDS taken at different times?
* Can you calculate the integrated fractional rms of the different components? What do you need to do that?

==== Type-B Quasi-Periodic Oscillation ====
Yet another low-frequency QPO on top of some power-law noise

* Extract the light curve, as usual. Do you see some section which is different from the others?
* Produce the power spectrum and have a look. Does the peak look like a Lorentzian? Try fitting. You can use a powerlaw (model powerlaw) for the continuum. See whether this is sufficient. Does a Lorentzian model work for the QPO? You might want to try a Gaussian (''gaussian'').
* Extract a power spectrum from the first 120 seconds of observation. What does the QPO look like here? Compare it with any other 120 s interval.
* Try to follow the QPO on higher time scales, a few seconds.
* Determine the fractional rms of the components.

==== High-frequency Quasi-Periodic Oscillation ====

Here we move to higher energies. The source, GRS 1915+105, is also pretty weird. A light curve will produce some interesting plots.

* Produce a power spectrum and concentrate on frequencies above 10 keV, away from the messy part. That’s where the important signal lies.
* Fit the HFQPO and get its parameters. Is it significant? At what confidence level?
* How strong (in fractional rms) is the oscillation?

Presentations:felixgx301

2018-04-12T14:14:30Z

Castro:

[[Category:LaTeX]]
====== GX 301-2 talk ======

===== Header =====

<file>
\documentclass{beamer}
\usetheme{Madrid}

\useinnertheme{circles}
\usecolortheme{dolphin}

\usepackage[utf8]{inputenc} % ggfs. anpassen -- Eingabekodierung
\usepackage[T1]{fontenc} % Zeichensatzkodierung
\usepackage[english]{babel} % Sprache einstellen
\usepackage{ragged2e} % besserer Flattersatz
\usepackage{xspace} % intelligenter Abstand

\usepackage{tikz} % Plotting and alignment tools
\usetikzlibrary{shadows}
\usetikzlibrary{fadings}

\usepackage{natbib}
\bibliographystyle{jwaabib}
\def\newblock{\hskip .11em plus .33em minus .07em}
</file>

===== Example slide =====
<file>
\begin{frame}
\frametitle{Time resolved spectroscopy}

\begin{tikzpicture}[x=\columnwidth, y=0.6\textheight]

\path<1-> [use as bounding box] (0,0) rectangle(1,1); % define the coordinate system

\node<1> at (0.5,0.5) {\includegraphics[width=0.78\columnwidth]{plots/all4speclc_2-10.pdf}}; %plot figure in the center
\node<2> at (0.5,0.5) {\includegraphics[width=0.78\columnwidth]{plots/all4speclc_zoom.pdf}};
\node<3> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_nogslines.pdf}};
\node<4-8> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_normnogslines.pdf}};

\draw<5-6> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Eqw. of \feka highest during part II} ;
% text in a nice box
\draw<6> (-0.02,0.65) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Spectra change strongly with time.} ;
\draw<7-8> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Energy shift could be due to change in ionization.} ;
\draw<8> (-0.02,0.55) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Mixture of different states necessary to explain \fekb/\feka ratio (Fe\,VI--XIV).} ;
\node<9-> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_felineeqw.pdf}};
\draw<10-> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Gainshift also explains shifts!} ;
\draw<11> (-0.02,0.65) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Gainshift can be due to change of CTI.} ;

\end{tikzpicture}
\end{frame}
</file>

===== Source =====
The complete talk can be found here: ''/home/fuerst/Public/talks/gx301/''

List of cyclotron line sources

2018-04-12T13:38:35Z

Castro: Created page with " Category:Accreting X-ray Pulsars ====== Cyclotron line sources ====== ===== Source list ===== This table attempts to summarize all known cyclotron line sources. It is s..."

[[Category:Accreting X-ray Pulsars]]

====== Cyclotron line sources ======

===== Source list =====
This table attempts to summarize all known cyclotron line sources. It is sortable by clicking
on column headers.

It is based on the presentation [[http://astrons.sabanciuniv.edu/astrons2010/wordpress/wp-content/uploads/2009/12/Spectral-continua-of-accreting-neutron-star-systems.pdf|"Spectral continua of accreting neutron star systems"]] by Jörn Wilms at the conference
[[http://astrons.sabanciuniv.edu/astrons2010/wordpress/|Astrophysics of Neutron Stars 2010]] with some information added later.

T/P = Transient/Persistent
<sortable>
^ Source ^ Ecyc [keV] ^Pspin [s] ^ Porbital [d] ^ Companion ^ T/P ^ Discovery ^
| [[Swift J1822.3-1606]] | 5-12 (varying with phase, proton line?) | 8.4 | - | Magnetar | T | XMM ([(:biblio:RodriguezCastillo16)]) |
| [[Swift J1626.6-5156]] | 10 | 15.4 | 132.9| Be | P | RXTE ([(:biblio:DeCesar09)]) |
| [[xrp:4U 0115+634]] | 14, 24, 36, 48, 62 | 3.6 | 24.3| Be | T | HEAO-1 ([(:biblio:Wheaton79)]) RXTE ([(:biblio:Heindl99)]), BeppoSAX ([(:biblio:Santangelo99)]) |
| [[xrp:1907|4U 1907+09]] | 18, 38 | 441 | 8.37| B2 III-IV | P | BeppoSAX ([(:biblio:Cusumano98b)]) |
| [[xrp:4u_1538-52|4U 1538-52]] | 22, 47 | 530 | 3.7| B0I | P | Ginga ([(:biblio:Clark90)]), RXTE ([(:biblio:RodesRoca09)]) |
| [[xrp:vela|Vela X-1]] | 24, 52 | 283 | 8.96| B0.5Ib | P | Mir-HEXE ([(:biblio:Kendziorra92)]), RXTE ([(:biblio:Kreykenbohm02)]) |
| [[xrp:v_0332_53|V 0332+53]] | 27, 51, 74 | 4.37 | 34.25| Be | T | Ginga ([(:biblio:Makishima90)]) |
| [[xrp:cep_x-4 |Cep X-4]] | 28 | 66.25 | >23| B1 | T | Ginga ([(:biblio:Mihara91)]) |
| [[Cen X-3]] | 29 | 4.8 | 2.09| O6.5II | P | BeppoSAX ([(:biblio:Santangelo98)]), RXTE ([(:biblio:HeindlChakrabarty99)])|
| [[xrp:X_per|X Per]] | 29? | 837 | 250.3| B0 III–Ve | P | RXTE ([(:biblio:Coburn01)]) |
| [[RX J0440.9+4431]] | 32 | 203 | 155 | B0.2 Ve | T | INTEGRAL, RXTE + Swift ([(:biblio:Tsygankov12)]) |
| [[xrp:mxb_0656-07|MXB 0656-072]] | 33 | 160 | 100?| O9.7Ve | T | RXTE ([(:biblio:Heindl03b)]) |
| [[xrp:xte_j1946_274|XTE J1946+274]] | 36 | 15.8 | 169.2| B0-1V-IVe | T | RXTE ([(:biblio:Heindl01)]) |
| [[xrp:4u_1626-67|4U 1626-67]] | 37 | 7.66 | 0.028| WD? | P | BeppoSAX ([(:biblio:Orlandini98b)]), RXTE ([(:biblio:HeindlChakrabarty99)]) |
| [[xrp:gx301|GX 301-2]] | 37 | 690 | 41.5| B1.2Ia | P | Ginga ([(:biblio:MiharaPhD)]) |
| [[Her X-1]] | 41 | 1.24 | 1.7| A9-B | P | Ballon-HEXE ([(:biblio:Truemper78)]) |
| [[A0535+26]] | 45, 100+ | 104 | 110.6| Be | T | HEXE ([(:biblio:Kendziorra92)], [(:biblio:Kendziorra94)]), CGRO ([(:biblio:Maisack97)]) |
| [[xrp:1a_1118-616|1A1118-616]] | 55, 110? | 408 | 400-800?| O9.5IV-Ve | T | RXTE ([(:biblio:Doroshenko10)]), Suzaku ([(:biblio:Suchy11)]) |
| [[xrp:gro_j1008-57|GRO J1008-57]] | 88? | 93.7 | 249.46| B1-B2 | T | CGRO ([(:biblio:Shrader99)]) |
| [[xrp:gx_304-1|GX 304-1]] | 54 | 272 | 132.2 | B2 Vne | P | RXTE ([(:biblio:Yamamoto11)]), INTEGRAL ([(:biblio:Klochkov12)]) |
| [[xrp:ks_1947_300|KS 1947+300]] | 12 | 18.8 | 40.4 | B0Ve | T | NuSTAR ([(:biblio:Fuerst14a)]) |

</sortable>

===== Location in the Galaxy =====

The figure below displays the position of the sources listed above in the Galaxy as far as known at this moment. Click on the figure for a larger version. Labels indicate the ordinal number in the first column of the table. Uncertainties in the distances are not indicated. Empty symbols represent sources for which there is no distance info in the literature; they have been artificially set to a distance
of 7.6 kpc. The spiral arms are from [(:biblio:Vallee08)]. Figure and data provided by Arash Bodaghee, SSL, UC Berkeley. {{:cyclo:overview:cyclotronlinesourcesinthegalaxy.ps|Original PostScript version}}

^ ^ # ^ Source ^ Dist. [kpc] ^ Reference ^
| {{:cyclo:overview:cyclotronlinesourcesinthegalaxy.png?464}} | 1 | [[Swift J1626.6-5156]] | 8±2.4 | [(:biblio:Reig11b)] |
| ::: | 2 | [[xrp:4U 0115+634]] | 8±1 | [(:biblio:Negueruela01)] |
| ::: | 3 | [[xrp:1907|4U 1907+09]] | 5 | [(:biblio:Cox05)] |
| ::: | 4 | [[4U 1538-52]] | 6.4±1 | [(:biblio:Reynolds92)] |
| ::: | 5 | [[xrp:vela|Vela X-1]] | 1.4±0.5 | [(:biblio:ChevalierIlovaisky98)] |
| ::: | 6 | [[V 0332+53]] | 7.5±1.5 | [(:biblio:Negueruela99)] |
| ::: | 7 | [[xrp:cep_x-4 |Cep X-4]] | 3.8±0.6 | [(:biblio:BonnetBidaudMouchet98)] |
| ::: | 8 | [[Cen X-3]] | 10±1 | [(:biblio:Hutchings79)] |
| ::: | 9 | [[X Per]] | 0.7±0.3 | [(:biblio:Lyubimkov97)] |
| ::: | 10 | [[MXB 0656-072]] | 3.9±0.1 | [(:biblio:McBride06)] |
| ::: | 11 | [[XTE J1946+274]] | 9.5±2.9 | [(:biblio:Wilson03)] |
| ::: | 12 | [[4U 1626-67]] | 9 | [(:biblio:GrimmGilfanovSunyaev02)] |
| ::: | 13 | [[GX 301-2]] | 4.1 | [(:biblio:Leahy02a)] |
| ::: | 14 | [[Her X-1]] | 6.6±0.4 | [(:biblio:Reynolds97)] |
| ::: | 15 | [[A0535+26]] | 2-0.7+0.4 | [(:biblio:Steele98)] |
| ::: | 16 | [[1A1118−61]] | 5±2 | [(:biblio:JanotPacheco81 )] |
| ::: | 17 | [[xrp:gro_j1008-57|GRO J1008−57]] | 5 | [(:biblio:GrimmGilfanovSunyaev02)] |

Pictures

2018-04-12T13:16:45Z

Castro: Created page with "Category:Observatory ===== Pictures ===== ==== Astronomical Pictures ==== All interesting astronomical pictures taken in the domes or with other equipment should be copie..."

[[Category:Observatory]]
===== Pictures =====
==== Astronomical Pictures ====

All interesting astronomical pictures taken in the domes or with other equipment should be copied to the following location:

<nowiki>/data/observations/</nowiki>

The subfolder ''canon'' is meant for pictures taken with the Canon DSLR, the subfolder ''CCD'' for pictures taken with the SBIG cameras. Both directories contain subdirectories for the objects observed, e.g. ''M42''. The directories should be globally writable, so put your new pictures in the corresponding subdirectories or create a new one.

See the [[remeis:obs|observation log]] which pictures are already available

==== Pictures of the Observatory ====

Photos of the observatory can be made available at:

''/data/media/photos/Sternwarte''

New subdirectories can be created for your own photos.

=== Pictures by T. Melnicky ===

The pictures taken by the professional photographer Thorsten Melnicky of the observatory are available at:

''/data/media/photos/Sternwarte/Melnicky''

**Important**: these pictures are copyright by [[http://www.specialmoments-media.de/|Thorsten Melnicky, Special Moments Verlag]]. The observatory acquired the right to use these pictures for our own purposes. This means that we can put these pictures on our webpage or use them for posters, and other publications. However, we are absolutely **not** allowed to further distribute these pictures, especially not to people who might use them commercially.

==== Other interesting Pictures ====

Various pictures of the instrumentation, the exhibition, scans, etc can be found at:

''/data/media/photos''

List of observations at the Remeis observatory

2018-04-12T13:13:13Z

Castro: Created page with "Category:Observatory ====== Observation log ====== This page should contain an overview which objects have been observed, when and by whom and show some of our best resul..."

[[Category:Observatory]]
====== Observation log ======

This page should contain an overview which objects have been observed, when and by whom and show some of our best results. Please refer to [[remeis:obsinfo| The Guide ]] to learn more about the cameras and how to use them.

For the pages of the indivudal objects please use this [[remeis:obs:sample|prototype]] by copy and pasting it.

===== Solar system objects =====

<sortable>
^ Name ^ Mag. ^ Distance (AU) ^ Mass (kg) ^ Eq. radius (km) ^ Size ^ Notes ^
| [[remeis:obs:Moon]] | (-2.5) -- (-12.9) | 0.0024 -- 0.0027 | 7.3477 * 1e+22 | 1738.14 | 29.3′ -- 34.1′ | |
| [[remeis:obs:Jupiter]] | (-1.6) -- (-2.94) | 3.934 -- 6.471 | 1.899 * 1e+27 | 142984 | 29.8″ -- 50.1″ | |
| [[remeis:obs:Saturn]] | (+1.47) -- (-0.24) | 8.048 -- 11.115 | 5.6846 * 1e+26 | 60268 | 14.5″ -- 20.1″ | |
| [[remeis:obs:Venus]] | max. -4.6 | 0.256 -- 1.744 | 4.869 * 1e+24 | 12103.6 | | |
| [[remeis:obs:Sun]] | (-24) -- (-24) | 1 | 1.989 * 1e+30 | 696350 | 31.5' -- 32.5' | |
</sortable>

===== Messier objects =====

<sortable 1>
^ Cat. No. ^ Other Name ^ Type ^ Mag. ^ Size ^ Coordinates (RA/DEC) ^ Notes ^
| [[remeis:obs:M1]] | Crab Nebula | Supernova Remnant | 8.4 | 6′00″ | 05h 34m 31.97s / +22° 00′ 52.1″ | |
| [[remeis:obs:M3]] | NGC 5272 | Globular Cluster | 6.2 | | 13h 42m 11.62s / +28° 22′ 38.2″ | |
| [[remeis:obs:M10]] | NGC 6254 | Globular Cluster | 6.4 | 20" | 16h 57m 8.92s / -04° 05′ 58.07" | |
| [[remeis:obs:M11]] | Wild Duck Cluster | Open Cluster | 5.8 | 14′00″ | 18h 51m 6.00s / -6° 16′ | |
| [[remeis:obs:M13]] | NGC 6205 | Globular Cluster | 5.9 | 16′36″ | 16h 41m 41.44s / +36° 27′ 36.9″ | Great Cluster in Hercules |
| [[remeis:obs:M15]] | NGC 7078 | Globular Cluster | 6.2 | 18′00″ | 21h 29m 58.38s / +12° 10′ 00.6″ | |
| [[remeis:obs:M16]] | NGC 6611 | Diffuse Nebula |6.0|7.0′|18h 18m 48s / -13° 49′ |Eagle Nebula |
| [[remeis:obs:M17]] | Omega Nebula, NGC 6618 | Emission Nebula | 6.0 | 11′00″ | 18h 20m 26.0s / -16° 10′ 36.0″ | also known as Swan Nebula, Checkmark Nebula, Lobster Nebula and Horseshoe Nebula |
| [[remeis:obs:M27]] | NGC 6853 | Planetary Nebula | 7.5 | 8.0′ x 5.6′ | 19h 59m 36.34s / +22° 43′ 16.09″ | |
| [[remeis:obs:M31]] | Andromeda Galaxy | Spiral Galaxy | 3.44 | 190′ x 60′ | 00h 42m 44.3s / +41° 16′ 9″ | two companion galaxies next to it |
| [[remeis:obs:M33]] | Triangulum Galaxy | Spiral Galaxy | 5.72 | 70.8′ × 41.7′ | 01h 33m 50.02s / +30° 39′ 36.7″ | |
| [[remeis:obs:M35]] | NGC 2168 | Open Cluster | 5.1 | | 06h 08m 54s / +24° 20′ | |
| [[remeis:obs:M39]] | NGC 7092 | Open Cluster | 4.6 | 32′ | 21h 32m 12.0s / +48° 25′ 60.0″ | relatively unspectacular |
| [[remeis:obs:M42]] | Orion Nebula | Diffuse Nebula | 4.0 | 65′ x 60′ | 05h 35m 17.3s / -05° 23′ 28″ | |
| [[remeis:obs:M51]] | Whirlpool Galaxy | Spiral/Irregular Galaxy | 8.4 | 11.2′ x 6.9′ | 13h 29m 52.7s / +47° 11′ 43″ | interacting with the galaxy NGC 5195 |
| [[remeis:obs:M52]] | NGC 7654 | Open Cluster | 7.3 | 13′ | 23h 24.8m / +61° 35′ | |
| [[remeis:obs:M53]] | NGC 5024 | Globular Cluster | 8.33 |12.6' | 13h 12m 55.25s / +18° 10′ 05.4″ | |
| [[remeis:obs:M57]] | Ring Nebula | Planetary Nebula|8.8|1,4' x 1'|18h 53m 35,079s/+33° 01′ 45,03''| |
| [[remeis:obs:M63]] | Sunflower Galaxy | Spiral Galaxy | 9.3 | 12′.6 x 7′.2 | 13h 15m 49.3s / +42° 01′ 45″ | big spiral |
| [[remeis:obs:M64]] | Black Eye Galaxy | Spiral Galaxy | 8.5 | 6′.8 x 3′.9 | 12h 56m 43.7s / +21° 40′ 58″ | Seyfert galaxy with dust torus |
| [[remeis:obs:M74]] | NGC 628 | Spiral Galaxy | 10.0 | 10′12″ | 01h 36m 41.8s / +15° 47′ 01″ | face-on spiral |
| [[remeis:obs:M81]] | Bode's Galaxy | Spiral Galaxy | 6.94 | 26′.9 × 14′.11 | 09h 55m 33.2s / +69° 3′ 55 | face-on spiral |
| [[remeis:obs:M82]] | NGC 3034| Spiral Galaxy| 8.6|11,2' x 4,3'|09h 55m 52,2s/+69° 40′ 48,8″ | |
| [[remeis:obs:M92]] | NGC 6341 | Globular Cluster | 6.3 | | 17h 17m 07.39s / +43° 08′ 09.4″ | |
| [[remeis:obs:M95]] | NGC 3351 | Spiral Galaxy | 9.73 | 4.8′ x 4.2′ | 10h 43m 57.733s / +11° 42′ 13.00″ | bar enclosed by ring shaped arm, faint |
| [[remeis:obs:M97]] | NGC 3587 | Planetary Nebula | 9.9 | 3.4′ x 3.3′ | 11h 14.8m / +55° 01′ | |
| [[remeis:obs:M104]] | Sombrero Galaxy | Spiral Galaxy | 8.0 | 5.9′ x 3.2′ | 12h 39m 59.43s / -11° 37′ 23.00″ | prominent dust lane, unusual large halo |
| [[remeis:obs:M106]] | - | Spiral Galaxy |8.3|17' × 6.5'|12h 18m 57.54s / +47° 18′ 14.3″|faint spiral arms |
</sortable>

Planning page for the [[remeis:obs:marathon|Photographic Messier Marathon]] 2011.

===== NGC and IC objects =====

<sortable>
^ Cat. No. ^ Other Name ^ Type ^ Mag. ^ Size ^ Coordinates (RA/DEC) ^ Notes ^
| [[remeis:obs:b33|Barnard 33]] | Horsehead Nebula | Dark Nebula / Emission Nebula | N/A | 8′ x 6′ | 05h 40m 59.0s / −02° 27′ 30.0″ | Beautiful dark nebula in Orion |
| [[remeis:obs:NGC891]] | Caldwell 23 |Spiral Galaxy| 10.1|13.5′ x 2.5′ | 02h 22m 33.41s / +42° 20′ 56.9″| Nice Edge-On Spiral Galaxy|
| [[remeis:obs:NGC2237]] | Rosette Nebula | Emission Nebula | 9.0 | 1.3° | 06h 33m 45s / +04° 59′ 54″ | Multipart nebula |
| [[remeis:obs:NGC2264]] | Christmas Tree Cluster / Cone Nebula | Open Cluster and Nebula | 3.9 | 1° | 06h 41m 06s / +09° 53′ | Nice nebula around many stars, values are for the Cone Nebula |
| [[remeis:obs:NGC2392]]| Eskimo Nebula|Planetary Nebula|9.1| 0.9′ x 0.9′ | 07h 29m 10.8s / +20° 54′ 42.5″ | Nice inner structure|
| [[remeis:obs:NGC2905]] | | barred spiral galaxy | 9.7 | 12′.6 × 6′.0 | 09h 32m 10.1s / +21° 30′ 03″ | |
| [[remeis:obs:NGC3193]] | part of Hickson 44 | Galaxy Cluster | 12.0 | 2′25″ | 10h18m24.80s/ +21°53′37.0″ | interacting Galaxies |
| [[remeis:obs:NGC6543]] | Cat's Eye Nebula | Planetary Nebula | 9.8 | 6′24″ | 17h 58m 33.4s / +66° 37′ 59.5″ | more deep sky objects in field of view |
| [[remeis:obs:NGC6826]] | Blinking Planetary | Planetary Nebula | 10.0 | 2′18″ | 19h 44m 48.0s / +50° 31′ 00.0″ | small but nice Pl. N. |
| [[remeis:obs:NGC6888]] | Crescent Nebula | Emission Nebula | 10.0 | 18' x 13' | 20h 12m 6.46s / +38° 21′ 17.9″ | |
| [[remeis:obs:NGC7000]] | North America Nebula | Emission Nebula | 4.0 | 2° × 1°40′ | 20h 59m 17.1s / +44° 31′ 44.0″ | Shape of the Nebula resembles North America |
| [[remeis:obs:NGC7023]] | Iris Nebula | Reflection Nebula | 6.8 | 18′ × 18′ | 21h 01m 35.6s / +68° 10′ 10.0″ | Nebula surrounded by faint absorption clouds |
| [[remeis:obs:steph_quint|NGC7320]] | Stephan's Quintett | Cluster of 5 Galaxies | ~13 | ~1′ | 22h 35m 57.5s / +33° 57′ 36″ | very nice interacting galaxies |
| [[remeis:obs:NGC7331]] | | Spiral Galaxy | 9.5 | 10.7' x 4.4' | 22h 37m 04.29s / +34° 24′ 58.5″ | smaller Galaxys close to it| |
| [[remeis:obs:NGC7635]] | Bubble Nebula | Emission Nebula | 11.0 | 15' x 8' | 23h 20m 45.6s / +61° 12′ 44″ | mainly h alpha|
| [[remeis:obs:IC405]] | Flaming Star Nebula | Emission/Reflection Nebula | 6.0 | 37′ × 10′ | 05h 16m 05s / +34° 27′ 49″ | Good visibility in Hα |
| [[remeis:obs:IC5146]] | Cocoon Nebula | Emission Nebula | 7.2 | 12′00″ | 21h 53m 28.7s / +47° 16′ 01″ | In the Milkyway with nice dark dust clouds next to it |
</sortable>

===== Comets =====

<sortable>
^ Name ^ Size ^ Aphelion ^ Perihelion ^ Eccentricity ^ Orbital Period ^ Inclination ^ Notes ^
| [[remeis:obs:C_2011_L4_PanSTARRS|C/2011 L4 PanSTARRS]] | ? | ? | 0.30161 AU | 1.000087 | ~106000 yr | 84.199° | was brightest in March 2013 (~1 mag) |
</sortable>

[[http://pulsar.sternwarte.uni-erlangen.de/hanke/science/talks/download.cgi?file=2009-10-24.HighlightsAmHimmel.pdf|"Highlights am Himmel" (slide show for the observatory's 120th anniversary on 2009-10-24)]]

Cuno Hoffmeister Telescope

2018-04-11T14:27:14Z

Castro: Created page with "Category:Observatory ====== The Remeis Observatory ====== Information on instruments, techniques and usage can also be found in the Lab Course manual. The domes are buil..."

[[Category:Observatory]]

====== The Remeis Observatory ======

Information on instruments, techniques and usage can also be found in the Lab Course manual.
The domes are built on an East-West axis with the 40cm telescope in the West dome and the new 50cm telescope in the East dome.
Inside the domes the parquet shows the North-South direction with a continous parquet-inlay in the middle.

===== Telescope quantities =====

Magnification <latex>V = f_{\text{telescope}}/f_{\text{ocular}}</latex>

Oeffnungsverhaeltnis: <latex>f/D</latex>

Austrittspupille: Okularbrennweite/Oeffnungsverhaeltnis

Minimal sinnvolle Vergroesserung: Austrittspupille < 6.5 mm

===== 40cm MEADE-Telescope =====

[[http://www.sternwarte.uni-erlangen.de/new/Institut/Geraete/40cmMeadeTeleskop.html]]

Before starting to observe, remove the caps of the fucuser and the tubus to allow the air to exchange with the surrounding.
This is important for a good seeing.
The tubus' cap must be removed gently and must not be fully pressed over the tubus when finished
as the mount can be damaged when pulling and pushing too hard.
The following pictures illustrate that.

{{:remeis:remove_lid_1.jpg?200|}}

This is Michael. Michael wants to see the stars, but he can't with a metal lid on top.
So he geeently

{{:remeis:remove_lid_2.jpg?200|}}

removes it, which looks like that:

{{:remeis:remove_lid_3.jpg?200|}}

The dome is rotated using a heavy, black device with two buttons - self-explanatory.

==== Using the AstroPhysics 1200 GTO mount in the West dome ====

First of all, a detailed manual is found in the drawer of the table next to the computer.

The mount is switched on using the blue power supply attached to the pilar of the mount.

{{:remeis:powersupply.jpg?200|}}

After switching on the device, the telescope will be found in parking position.

{{:remeis:parking_pos.jpg?200|}}

Objects can be found with a GOTO function. The mount is calibrated two-fold with small wheels measuring the distance driven when slewing the axes:
* first the dictance measured by the wheels translated into RA/DEC units of the equatorial coordinate system
* second the alignment of the telescope's coordinate system with the celestial one

Therefore the RA-axis is already adjusted to point to the celestial North-pole.
The telescope's coordinate system should also accord to the celestial one.

The usage of the keypad menu is more or less straightforward.
Press

{{:remeis:keypad_manu.jpg?200|}}

to access the main menu.
It is arranged as follows:
* **1-Objects**
* **2-Setup**
* **3-Tools**
* **4-Time/LST**
* **5-S**
* **6-B**
* **7-A**

{{:remeis:keypad_mainmenu.jpg?200|}}

Pressing the appropriate numbers will lead you to the sub-menus.
Pressing **6** several times will change the slew rate when steering the mount manually via the E-W-N-S buttons.
Option **5** allows to change the slew rate for an automatic driving process when pressing **GOTO** after selecting an object.

The sub-menu after pressing **1** for **Objects** includes amongst other points
* **1-M** - Messier catalog
* **2-NGC** - New Galactic Catalog
* **3-IC** - International Catalog
* **4-Sol** - objects of the solar system
* **5-Strs** - list of the brightest stars

{{:remeis:keypad_objectmenu.jpg?200|}}

You can directly select objects with well known catalog names using this menu.

{{:remeis:keypad_objectmenu_messier.jpg?200|}}

In the **Strs**-list you can scroll through the objects via the **PREV**- and **NEXT** buttons,
while it is enough to give the appropriate numbers in the other sub-menus.
In the **Sol** sub-menu a list is already given and can be chosen with numbers.

After choosing one object, make the mount drive to it by pressing the **GOTO** button down left.

{{:remeis:keypad_goto.jpg?200|}}

Make sure to be able to press the **STOP** button

{{:remeis:keypad_stop.jpg?200|}}

at each time while the telescope is slewing to interrupt the process
in case of tightening cables (also pay attention to the motor-cables of the mount), things or humans that could be hit by the driving telescope or whatever.

After the telescope has focused the chosen object, make sure that it is properly centered in the field of view.
Therefore use one of the oculars and the wheels at the focuser to focus the stars (see also [[syntax#focusing using the bahtinov mask|Bahtinov mask]] for focusing the telescope properly).
If not use the N-S-E-W buttons to correct for that. The chosen position is automatically tracked by the mount.
After centering the object manually, you can re-calibrate the internal coordinate-system to the celestial one
by choosing the option **Ra/Dec REV** and **Recalibrate** while beeing in the main menu.

When finished, return the mount in parking position choosing the menu **Setup** and **Park Mount**.
The best position is position **1**.
Here, the right ascension axis is oriented in E-W direction with the tubus in the West pointing North.

//tb//

==== Using the Telrad-finder ====

The Telrad finder projects three concentric circles (similar to a head up-display). So you have a good overview where the telescope points, and if with a little experience you can find a lot of objects just by using the Telrad.

* rotate the turn-switch on the right side of the Telrad to activate the power supply and to tune the luminosity.
* press the yellow button on the right side of the Telrad. The LED light will we activated for a short span of time (so the batteries won't become empty if you forget to switch it off).

==== Focusing ====
The 40cm telescope can be focused using the wheels next to the focuser. The big wheels for raw-focusing and the smaller
whell attached on only one side for vernier adjustment.

Furthermore it is often necessary to even move the mirror when switching between oculars and the CCD camera.
This can be done with a long silver screw after loosening the knob next to it to position "unlock".
When finished arrest the mirror again.
When moving the main mirror it is best to point the telescope to a position high in the sky, low declinations should be avoided because it would boost the risk of a stuck mirror.

==== Focusing using the Bahtinov mask ====
{{ :remeis:bahtinov_mask_setup.gif?direct&332|}}

Up in the west dome there is a so called [[http://en.wikipedia.org/wiki/Bahtinov_mask|Bahtinov mask]] available, which makes the focusing much easier. Normally, the focus is varried until one (or more) star is sharpest, i.e. smallest, on the picture (if using a CCD camera). This method, however, depends on the seeing conditions: a bad seeing causes the image of the star to "wobble", making focusing very difficult. In a worst case, the star isn't focused well, which would result in an unsharpen image after a long exposure.

The Bahtinov mask gets rid of the seeing problem by creating 3 diffraction pattern via a grid. Two pattern cross the image at the center, while the position of the third one depends on the focus: if the image is defocused, the diffraction spike is off the center. On the other hand, if the perfect focus is found, all 3 diffraction pattern cross at the same point in the center.

The Bahtinov mask has to be put on top of the Schmidt plate, before the telescope. The diameter of the mask is slightly smaller then the outer radius of the tube. In consequence, the mask is hold by the casing of the tube itself. Please **be careful** not to scratch the Schmidt plate while using the Bahtinov mask!

{{:remeis:bahtinov_mask.jpg?direct&332|}}

==== CCD camera SBIG STL-11000M ====

The CCD camera is located in the lockers of the Meridian building (black box).
It brings the CCD camera itself and a power cable that has to be connected to a power socket.
Make sure that the transformator box attached to the power cable is fixed to the pillar
as the cable might get too short if the box would lie on the floor.
Inside the board next to the computer

{{:remeis:pc_dome.jpg?200|}}

there is a quite long USB cable that also has to be connected to the CCD camera.
The camera itself is connected to the focuser of the telescope with the upper side of the chassis
pointing North indicated by the elongation of the RA-axis pointing to the North pole.

Now type:
setenv VBOX_USB sysfs
into the terminal!

Now you can log-in, open a shell and run the command **VirtualBox** which opens a Windows XP emulation within Linux.
Now the fan inside the camera will start to run.
Open the program **CCDops** which communicates with the camera.
Click on the menu point **Setup** and a connection between the CCD camera and your machine will be established.
Click again on Setup, set the \\cooling\\ to "active" and the desired temperature to -20 degrees.
This will attenuate thermal noise of the CCD chip.
The \\resolution mode\\ should be set to "auto" which will automatically use the high resolution mode for grabed pictures
and low resolution elsewhere. The \\binning\\ can be set to "1" for the most information inside the picture.
For larger binning more pixels will be averaged to one to save memory.
It is also possible to extract only parts of the CCD in the appropriate menu to save time to transfer the data.

First make sure that the detector is located in the focal plane. Therefore use the Bathinov mask and center the brightest star available.
In CCDops choose **Focus** from the manu bar. This mode allows to continously transfer low resolution images with short exposure times
(fractions of a second), which takes less time to transfer the accumulated data from the camera to the computer.
Now you can check changes in the diffraction pattern of the star using the Bathinov mask with changes in the focus nearly in real time.
When reached the desired diffraction pattern, pause the data traffic and quit the appropriate window.

Now you can start taking proper images using the **Grap** option in the main menu.
Choose a suitable exposure time that depends on the brightness of the source.
Right click on the image when downloaded and a cross-hair appears. It gives back the pixel values in ADU units that should not exceed 65,000
in order not to overexposure the image.
The exposure time should not exceed 150s as the tracking of the mount will get inaccurate at that point.

In the drop-down menu you can also choose **filters**. For black and white images simply use the "clear" filter.

The best way to go is to measure both a dark frame and a proper frame at each time depending on how many frames you want to measure.
Afterwards one can substract the dark frame (shutter closed) from the illuminated frame in order to get rid of detector internal bias.
This bias is thermal noise also called dark current.
Then one can add and average as many substracted frames as necessary to reduce statistical noise from the images.

You can also measure a fully illuminated frame and dark frame in one step. The software will automatically substract both and
show you the final image. It is, however, better to store both separately to be able to see and better control the effects of correction.

When finished with the observing session, a flat field should be measured. Therefore use the white flat field mask,
steer the tubus in an upright position and just put it on top.
A proper exposure time is 0.1s. A flat field is good to correct for non uniform distributed pixel responses.
It will at the end be multiplied with the dark-substracted images.

Frames can be stored to a shared directory within the Virtual Machine.
This shared directory is accessable from the Linux machine at
reticulum:/scratch1/VirtualBox/...

//tb//

===== 60cm Telescope =====

[[http://www.sternwarte.uni-erlangen.de/new/Institut/Geraete/60cmTeleskop.html]]

===== 2.1m Radio Telescope =====

[[http://www.sternwarte.uni-erlangen.de/new/Institut/Geraete/RadioTeleskop.html]]

[[remeis:srt|Description]] how to use the [[remeis:srt|Small Radio Telescope (SRT)]] and a presentation of possible research with it.

===== CGEM DX =====

* to assemble on one of the two east pillars in the garden
* mountable telescopes:
* [[MEADE 10 Inch]]
* [[Apochromatic refractor]]
* [[http://www.celestron-deutschland.de/product.php?CatID=9&ProdID=1017|more information]]

===== LXD75 =====

* to assemble on one of the two east pillars in the garden
* mountable telescopes:
* [[MEADE 10 Inch]]
* [[Apochromatic refractor]]
* [[Coronado PST]]
* [[http://www.luntsolarsystems-by-apmtelescopes.com/pro_info.php?ebene1=48&id=94473&catchoice1=|Solar telescope 60mm H-alpha]]
* for information about assembling the mounting see the [[intern:labmanuals|lab course manual]], section telescopes

===== Observations and Images =====
[[remeis:obsinfo|Information]] on how to make beautiful images of the sky and an [[remeis:obs|overview]] of what has already been achieved with our instruments.

There is also a compilation of tips and landscapes for [[remeis:stellarium|Stellarium]].

Presentations:felixgx301

2018-04-11T14:12:04Z

Castro: Blanked the page

Presentations:felixgx301

2018-04-11T14:06:32Z

Castro: Created page with "====== GX 301-2 talk ====== ===== Header ===== <file> \documentclass{beamer} \usetheme{Madrid} \useinnertheme{circles} \usecolortheme{dolphin} \usepackage[utf8]{inputenc}..."

====== GX 301-2 talk ======

===== Header =====

<file>
\documentclass{beamer}
\usetheme{Madrid}

\useinnertheme{circles}
\usecolortheme{dolphin}

\usepackage[utf8]{inputenc} % ggfs. anpassen -- Eingabekodierung
\usepackage[T1]{fontenc} % Zeichensatzkodierung
\usepackage[english]{babel} % Sprache einstellen
\usepackage{ragged2e} % besserer Flattersatz
\usepackage{xspace} % intelligenter Abstand

\usepackage{tikz} % Plotting and alignment tools
\usetikzlibrary{shadows}
\usetikzlibrary{fadings}

\usepackage{natbib}
\bibliographystyle{jwaabib}
\def\newblock{\hskip .11em plus .33em minus .07em}
</file>

===== Example slide =====
<file>
\begin{frame}
\frametitle{Time resolved spectroscopy}

\begin{tikzpicture}[x=\columnwidth, y=0.6\textheight]

\path<1-> [use as bounding box] (0,0) rectangle(1,1); % define the coordinate system

\node<1> at (0.5,0.5) {\includegraphics[width=0.78\columnwidth]{plots/all4speclc_2-10.pdf}}; %plot figure in the center
\node<2> at (0.5,0.5) {\includegraphics[width=0.78\columnwidth]{plots/all4speclc_zoom.pdf}};
\node<3> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_nogslines.pdf}};
\node<4-8> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_normnogslines.pdf}};

\draw<5-6> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Eqw. of \feka highest during part II} ;
% text in a nice box
\draw<6> (-0.02,0.65) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Spectra change strongly with time.} ;
\draw<7-8> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Energy shift could be due to change in ionization.} ;
\draw<8> (-0.02,0.55) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Mixture of different states necessary to explain \fekb/\feka ratio (Fe\,VI--XIV).} ;
\node<9-> at (0.5,0.5) {\includegraphics[width=0.80\columnwidth]{plots/all4speclc_felineeqw.pdf}};
\draw<10-> (-0.02,0.9) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Gainshift also explains shifts!} ;
\draw<11> (-0.02,0.65) node [anchor=west, fill=black!05, text width=4.0cm,drop shadow, rounded corners] {Gainshift can be due to change of CTI.} ;

\end{tikzpicture}
\end{frame}
</file>

===== Source =====
The complete talk can be found here: ''/home/fuerst/Public/talks/gx301/''

Presentation Tips for LaTeX Beamer

2018-04-11T13:58:38Z

Castro: Created page with " Category:LaTeX ====== Presentation Tips for LaTeX Beamer ====== A few random bits and pieces to improve your LaTeX-Beamer presentations. ===== ECAP corporate design l..."

[[Category:LaTeX]]

====== Presentation Tips for LaTeX Beamer ======

A few random bits and pieces to improve your LaTeX-Beamer presentations.

===== ECAP corporate design latex template =====

Nice corporate design template by Susanne Raab.
Possibility to choose between different "projects"; now also able to choose "XMM" project where the XMM satellite appears on front page in ECAP blue with the ECAP logo.

Latest version:
/userdata/data/beuchert/work/talks/template_ecap/fauecap/

Documentation:
/userdata/data/beuchert/work/talks/template_ecap/fauecap_docu.pdf

Example including tikz:
/userdata/data/beuchert/work/talks/Karlsbad_2017/fauecap/ngc4151_beuchert.tex

For being up to date, go to
http://pi1250.physik.uni-erlangen.de/sraab/Beamer
and open a standard account, then you are able to use that to clone the repository via

git clone http://pi1250.physik.uni-erlangen.de/sraab/Beamer.git

===== Examples =====
* [[presentations:felixgx301|Felix' GX 301-2 talk]]: using TikZ to put blocks above pictures
* [[presentations:thomas_feLines|Thomas' Fe Lines talk]]
* [[presentations:alexmbasictikz|Alex M.: basic TIKZ for positioning text/figures and drawing]]

===== The Remeis TikZ sketch gallery =====
* [[presentations:fancyremeistikz| The Remeis TikZ gallery]]: similar to our [[isis:slxfig:fancyremeisplots| Remeis X-fig plot gallery]], which additionally to "normal" plots also features nice sketches and drawings, here you can show your fancy TikZ creations that you used in presentations, posters, theses, publications, ...

===== Literature =====
* H. Voß, //Präsentationen mit LaTeX//, 2009, Lehmanns Media, Berlin, ISBN 978-3-86541-365-6\\ (In German only, Felix has a copy)