RHESSI Spectroscopy - OSPEX User Guide

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Revision as of 13:44, 19 August 2009 (view source) Agopie (Talk | contribs) ← Older edit		Revision as of 16:27, 19 August 2009 (view source) Agopie (Talk | contribs) Newer edit →
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	==Links to documentation for fitting RHESSI Data==		==Links to documentation for fitting RHESSI Data==
-	===Create a spectrum file using the HESSI GUI===	+	===[[Using the HESSI GUI to create spectrum files|Creating a spectrum file with the HESSI GUI]]===
-	Starting with the level zero RHESSI data this document goes through the steps necessary to create a spectrum file using the HESSI GUI:	+
-	[[Using the HESSI GUI to create spectrum files|Creating a spectrum file with the HESSI GUI]]	+	Starting with the level zero RHESSI data this document goes through the steps necessary to create a spectrum file using the HESSI GUI.
		+	Command Line instructions are also included. The documentation is for creating a spectrum and spectrum response matrix (SRM) file
		+	for a single detector, but is easily expandable  to creating files for multiple detectors.
-	This includes the details of creating a file for a single detector using the GUI as well as simple command line instructions for accomplishing the same. The end result is a spectrum and spectrum response matrix (SRM) file in the .fits format which can be read by OSPEX.	+	===[[OSPEX Documentation| Users Guide for the OSPEX GUI]]===
		+
		+	Using a spectrum file and SRM file this document goes through the steps necessary for using the OSPEX GUI to fit a RHESSI spectrum,
		+	including defining background, time intervals, a fit model and doing a fit.
-	===Fitting a time interval using the OSPEX GUI===	+	====[[Vth - Variable Thermal| Vth - Variable Thermal]]====
-	The following document gives a step by step example of using the OSPEX GUI to fit a time interval:	+
-	[[OSPEX Documentation|Users Guide for the OSPEX GUI]]	+	The variable thermal fit model component uses a single emission measure and temperature along with a measure of the relative abundance
		+	of the Fe-Ni line complex to fit the thermal emission of the RHESSI spectrum for a user defined time interval.
-	This includes defining background, setting up time intervals, choosing a fit model and doing a fit for a single interval.	+	====[[Bpow - Broken Power Law|Bpow - Broken Power law]]====
-	====Vth====	+	The broken power law fit model component uses a break energy, the spectral index above and below the break energy, and a normalization
-	This document contains a brief explanation and example of how to use the variable thermal model component:	+	dependent on the count rate to fit the non-thermal component of the RHESSI spectrum for a user defined time interval. This is the
		+	simplest model available for the non-thermal emission during a flare.
-	[[Vth - Variable Thermal| How to use Vth]]	+	====[[Thick2 - Thick Target Bremsstrahlung Version 2| Thick Target]]====
-		+
-	The variable thermal component uses a single emission measure and temperature along with the relative abundance of the Fe-Ni complex to model the thermal portion of the RHESSI spectrum as a function of energy for a user defined time interval.	+	The thick target fit model component uses a double broken power law in electron space to model to non-thermal portion of the RHESSI
-		+	spectrum. The measured photon distribution is calculated from the electron distribution using
-	====Bpow====	+
-	This document contains a brief description of how to use the broken power law component:	+
-		+
-	[[Bpow - Broken Power Law| How to use Bpow]]	+
-		+
-	The broken power law component is a single power law which uses a break energy, the power law index above the break energy and below, and a count rate dependent normalization to model the non-thermal component of the RHESSI spectrum as a function of energy for a user defined time interval.	+
-	====Thick Target====	+
-	[[Thick2 - Thick Target Bremsstrahlung Version 2| Thick Target]]	+
	====drm_mod====		====drm_mod====
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	===Fitting Multiple Intervals===		===Fitting Multiple Intervals===
	[[Fitting multiple intervals]]		[[Fitting multiple intervals]]
		+
		+	===View Fit Results===
		+	[[View fit results]]
	===Fitting a new detector===		===Fitting a new detector===

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Revision as of 16:27, 19 August 2009

Contents 1 Introduction 2 Links to documentation for fitting RHESSI Data 2.1 Creating a spectrum file with the HESSI GUI 2.2 Users Guide for the OSPEX GUI 2.2.1 Vth - Variable Thermal 2.2.2 Bpow - Broken Power law 2.2.3 Thick Target 2.2.4 drm_mod 2.2.5 pileup_mod 2.3 Fitting Multiple Intervals 2.4 View Fit Results 2.5 Fitting a new detector

Introduction

A general outline that covers the steps necessary to fit a RHESSI Spectra, starting with the creation of the RHESSI Spectrum file and going through the process of defining background, time intervals, and fitting models to the data using OSPEX.

Links to documentation for fitting RHESSI Data

Creating a spectrum file with the HESSI GUI

Starting with the level zero RHESSI data this document goes through the steps necessary to create a spectrum file using the HESSI GUI.
Command Line instructions are also included. The documentation is for creating a spectrum and spectrum response matrix (SRM) file 
for a single detector, but is easily expandable  to creating files for multiple detectors. 

Users Guide for the OSPEX GUI

Using a spectrum file and SRM file this document goes through the steps necessary for using the OSPEX GUI to fit a RHESSI spectrum,
including defining background, time intervals, a fit model and doing a fit. 

Vth - Variable Thermal

The variable thermal fit model component uses a single emission measure and temperature along with a measure of the relative abundance
of the Fe-Ni line complex to fit the thermal emission of the RHESSI spectrum for a user defined time interval.

Bpow - Broken Power law

The broken power law fit model component uses a break energy, the spectral index above and below the break energy, and a normalization
dependent on the count rate to fit the non-thermal component of the RHESSI spectrum for a user defined time interval. This is the 
simplest model available for the non-thermal emission during a flare.  

Thick Target

The thick target fit model component uses a double broken power law in electron space to model to non-thermal portion of the RHESSI
spectrum. The measured photon distribution is calculated from the electron distribution using 

drm_mod

 drm_mod

pileup_mod

 pileup_mod

Fitting Multiple Intervals

Fitting multiple intervals

View Fit Results

View fit results

Fitting a new detector

Fitting a new detector

'UNDER CONSTRUCTION'