xmm-newton tutorial - fudan universityblackhole2018.fudan.edu.cn/bh2018/s/2bc.pdf · xmm-newton...
TRANSCRIPT
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XMM-Newton tutorial
Mauro Dadina (largely based on Eleonora Torresi presentation)
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Image courtesy of Dornier Satellitensysteme GmbH and ESA
X-RAY TELESCOPES
EPIC MOS cameras
EPIC PN camera
RGS cameras
XMM-Newton payload
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Eccentric 48-hour orbit around the Earth Inclination 40 degrees to the Equator
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1. Download XMM-Newton data from the public archive 2. PN, MOS1 and MOS2 data reduction: - selection of Good Time Intervals (GTI) - generation of cleaned event files - source and background regions selection - check for the presence of pile-up - spectrum extraction (of both source and background) - creation of the Response Matrix Function (RMF) - creation of the Ancillary Response Function (ARF) - grouping of the spectra 3. Extraction of a light curve from a point-like source
OUTLINE
![Page 5: XMM-Newton tutorial - Fudan Universityblackhole2018.fudan.edu.cn/bh2018/S/2bc.pdf · XMM-Newton tutorial Mauro Dadina (largely based on Eleonora Torresi presentation) Image courtesy](https://reader034.vdocuments.net/reader034/viewer/2022052021/603622269198ea43eb2eb303/html5/thumbnails/5.jpg)
1. Download XMM-Newton data from the public archive 2. PN, MOS1 and MOS2 data reduction: - selection of Good Time Intervals (GTI) - generation of cleaned event fileS - source and background regions selection - check for the presence of pile-up - spectrum extraction (of both source and background) - creation of the Response Matrix Function (RMF) - creation of the Ancillary Response Function (ARF) - grouping of the spectra 3. Extraction of a light curve from a point-like source
OUTLINE
![Page 6: XMM-Newton tutorial - Fudan Universityblackhole2018.fudan.edu.cn/bh2018/S/2bc.pdf · XMM-Newton tutorial Mauro Dadina (largely based on Eleonora Torresi presentation) Image courtesy](https://reader034.vdocuments.net/reader034/viewer/2022052021/603622269198ea43eb2eb303/html5/thumbnails/6.jpg)
XMM-Newton Science Operations Centre (ESA-Vilspa, Spain) http://www.cosmos.esa.int/web/xmm-newton/xsa
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3C 111
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EPIC FILTERS
http://xmm-tools.cosmos.esa.int/external/xmm_user_support/documentation/uhb/XMM_UHB.pdf
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MOS
pn
full frame
large window
timing mode
small window
partial window
pn MOS
CCD 1
CCD 4
RAWX
EPIC SCIENCE MODES
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ODF (Observation Data Files): row data that need to be reprocessed PPS (Processing Pipeline Files): already reprocessed data using standard pipelines
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Loading of data reduction and analysis packages
XMM -> set the “heasoft” environment (heainit) -> set the SAS enironment -> re-set the “heasoft” envirnoment
XSPEC -> heainit
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Revolution number
Instrument (pn, MOS1, MOS2)
Content
FITS files
ODF files
ObsID
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Data produced by the satellite are stored in FITS (Flexible Image Transport System) format.
FITS files
All the information of your observation are contained in the header of the fits file. You can visualize it by using the FTOOL command fv: > fv nomefile.fits
But before you must have set the correct environment...
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ODF evt
pn.evt m1.evt m2.evt ccf.cif
Creation of event files
event files
CCF calibration index file (CIF)
SAS: epproc-emproc-cifbuild
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Extraction of a high energy light curve (>10 keV) to identify interval of flaring particle background
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EPIC background
For more information refer to the XMM-Newton User’s Handbook
Cosmic X-ray background (CXB)
Instrumental background
detector noise component (important below 300 eV)
second component due to the interaction of pa r t i c l e s w i th the detectors and the structures surrounding them (important at high energies, e.g. above a few keV)
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EPIC background
For more information refer to the XMM-Newton User’s Handbook
Cosmic X-ray background (CXB)
Instrumental background
detector noise component (important below 300 eV)
second component due to the interaction of pa r t i c l e s w i th the detectors and the structures surrounding them (important at high energies, e.g. above a few keV)
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EPIC particle induced background External ‘flaring’ component Internal ‘quiescent’ component strong and rapid var iabi l i ty; currently attributed to soft protons (Ep < a few 100 keV) l ikely organized in clouds populating the Earth’s magneto-sphere
high energy particles interacting with the structure surrounding the detectors and the detectors themselves
Al-Ka
Si-Ka MOS1
pn
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Extraction of a high energy light curve (>10 keV) to identify interval of flaring particle background
evselect table=pn.evt energycolumn=PI expression='#XMMEA_EP && (PI>10000) && (PATTERN==0)' withrateset=yes rateset="lcurve_sup10.lc" timebinsize=100 maketimecolumn=yes makeratecolumn=yes
lcurve
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L i gh t cu r ve above 10 keV
TIME
Coun
t/se
c
pn < 0.4 cts/s MOS < 0.35 cts/s
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1. Download XMM-Newton data from the public archive 2. PN, MOS1 and MOS2 data reduction: - selection of Good Time Intervals (GTI) - generation of cleaned event files - source and background regions selection - check for the presence of pile-up - spectrum extraction (of both source and background) - creation of the Response Matrix Function (RMF) - creation of the Ancillary Response Function (ARF) - grouping of the spectra 3. Extraction of a light curve from a point-like source
OUTLINE
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Selection of GOOD TIME INTERVALS (GTI)
tabgtigen table=lcurve_sup10.lc gtiset=good_bkg.gti expression=‘RATE<0.4'
Generation of the cleaned event file
evselect table=pn.evt expression='#XMMEA_EP (EM) && (PI > 150) && (GTI(good_bkg.gti,TIME))' withfilteredset=yes keepfilteroutput=yes filteredset=pn_new.evt(mos1_new.evt)updateexposure=yes cleandss=yes writedss=yes
27!
pn_new.evt mos1_new.evt mos2_new.evt
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1. Download XMM-Newton data from the public archive 2. PN, MOS1 and MOS2 data reduction: - selection of Good Time Intervals (GTI) - generation of cleaned event files - source and background regions selection - check for the presence of pile-up - spectrum extraction (of both source and background) - creation of the Response Matrix Function (RMF) - creation of the Ancillary Response Function (ARF) - grouping of the spectra 3. Extraction of a light curve from a point-like source
OUTLINE
![Page 26: XMM-Newton tutorial - Fudan Universityblackhole2018.fudan.edu.cn/bh2018/S/2bc.pdf · XMM-Newton tutorial Mauro Dadina (largely based on Eleonora Torresi presentation) Image courtesy](https://reader034.vdocuments.net/reader034/viewer/2022052021/603622269198ea43eb2eb303/html5/thumbnails/26.jpg)
Source and background regions selection
open event list file with ds9 > ds9 pn_new.evt &
source region http://ds9.si.edu/doc/ref/
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PN
Fractional encircled energy Fraction of photons contained within a certain radius (in arcsec).
This quantity is function of the angular radius (on-axis)
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MOS1
Fractional encircled energy Fraction of photons contained within a certain radius (in arcsec).
This quantity is function of the angular radius (on-axis)
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MOS2
Fractional encircled energy Fraction of photons contained within a certain radius (in arcsec).
This quantity is function of the angular radius (on-axis)
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Source and background regions selection
open event list file with ds9 > ds9 pn_new.evt &
source region http://ds9.si.edu/doc/ref/
> Region > save region > file format ‘ds9’ > coordinates ‘physical’ > source.reg
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background
Source and background regions selection
open event list file with ds9 > ds9 pn_new.evt &
> Region > save region > file format ‘ds9’ > coordinates ‘physical’ > back.reg
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out of time events
spider supporting the telescope’s mirrors
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1. Download XMM-Newton data from the public archive 2. PN, MOS1 and MOS2 data reduction: - selection of Good Time Intervals (GTI) - generation of cleaned event files - source and background regions selection - check for the presence of pile-up - spectrum extraction (of both source and background) - creation of the Response Matrix Function (RMF) - creation of the Ancillary Response Function (ARF) - grouping of the spectra 3. Extraction of a light curve from a point-like source
OUTLINE
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PILE-UP Arrival of two or more independent photons at nearby pixels that are erroneously read as one single event (whose energy is the sum of the energies of the individual photons) Jethwa et al. (2015)
Can affect the PSF (in its core many photons arrive at almost the same time) and the EPIC spectral response distorting the spectral shape:
EPIC MOS
2 cts/frame 5 cts/frame
12 cts/frame 16 cts/frame
-> by hardening the observed spectrum -> by suppressing flux due to the creation of invalid patterns -> by joining separate mono-pixel into a single multi-pixel event (pattern migration)
Jethwa et al. (2015)
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The term ‘pattern’ indicates the distribution of pixels over which a charge cloud spreads (= ‘grade’ in Chandra/ACIS)
An X-ray photon can generate a variety of patterns. The probability of each pattern is a function of the photon’s energy.
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Single- double- triple- quadruple- events are the four types of valid events which can be created by an X-ray photon
(GOOD patterns)
Double events can be produced only if the energy of both events is above the event threshold. Triple (quadruples) events start at 3 (4) times the event
threshold.
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> evselect table=pn_new.evt withfilteredset=yes filteredset=pnf.evt k e e p f i l t e r o u t p u t = y e s e x p r e s s i o n = " ( ( X , Y ) I N c i r c l e (27874.528,26645.58,699.99999))” > epatplot set=pnf.evt device="/CPS" plotfile="pnf_pat.ps" > gv pnf_pat.ps
spectral distributions as function of PI channels for single- double- triple- and quadruple- events fraction of the four valid event types
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1. Download XMM-Newton data from the public archive 2. PN, MOS1 and MOS2 data reduction: - selection of Good Time Intervals (GTI) - generation of cleaned event files - source and background regions selection - check for the presence of pile-up - spectrum extraction (of both source and background) - creation of the Response Matrix Function (RMF) - creation of the Ancillary Response Function (ARF) - grouping of the spectra 3. Extraction of a light curve from a point-like source
OUTLINE
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Spectrum extraction (source)
e v s e l e c t t a b l e = p n _ n e w . e v t w i t h s p e c t r u m s e t = y e s spectrumset=source_spectrum.fits energycolumn=PI spectralbinsize=5 withspecranges=yes specchannelmin=0 specchannelmax=20479 expression='(FLAG==0) && (PATTERN<=4) && ((X,Y) IN circle (27874.528,26645.58,699.99999))'
e v s e l e c t t a b l e = m o s 1 _ n e w . e v t w i t h s p e c t r u m s e t = y e s spectrumset=source_spectrum.fits energycolumn=PI spectralbinsize=15 withspecranges=yes specchannelmin=0 specchannelmax=11999 expression='(FLAG==0) && (PATTERN<=12) && ((X,Y) IN circle (28090.5,24221.5,775.48791))'
PN
MOS
PATTERN==0 (single events); PATTERN==[1-4] (double events); PATTERN==[5-12] (triple and quadruple events)
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e v s e l e c t t a b l e = p n _ n e w . e v t w i t h s p e c t r u m s e t = y e s spectrumset=back_spectrum.fits energycolumn=PI spectralbinsize=5 w i thspec ranges=yes specchanne lm in=0 specchanne lmax=20479 expression='(FLAG==0) && (PATTERN<=4) && (((X,Y) IN circle( )) || ((X,Y) IN circle( )))'
If you have more than one background region:
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PN
MOS
e v s e l e c t t a b l e = p n _ n e w . e v t w i t h s p e c t r u m s e t = y e s spectrumset=back_spectrum.fits energycolumn=PI spectralbinsize=5 withspecranges=yes specchannelmin=0 specchannelmax=20479 expression='(FLAG==0) && (PATTERN<=4) && ((X,Y) IN circle (27874.528,26645.58,699.99999))'
e v s e l e c t t a b l e = m o s 1 _ n e w . e v t w i t h s p e c t r u m s e t = y e s spectrumset=back_spectrum.fits energycolumn=PI spectralbinsize=15 withspecranges=yes specchannelmin=0 specchannelmax=11999 expression='(FLAG==0) && (PATTERN<=12) && ((X,Y) IN circle (28090.5,24221.5,775.48791))'
Spectrum extraction (background)
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Calculate the area of source and background regions used to make the spectral files
backscale spectrumset=source_spectrum.fits badpixlocation=pn_new.evt backscale spectrumset=back_spectrum.fits badpixlocation=pn_new.evt
This task takes into account any bad pixels or chip gaps and writes the result into the BACKSCAL keyword of the SPECTRUM table
The BACKSCALE task calculates the area of a source region used to make a spectral file.
The final value is: AREA= GEOMETRIC AREA-CCD GAPS-BAD PIXELS
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1. Download XMM-Newton data from the public archive 2. PN, MOS1 and MOS2 data reduction: - selection of Good Time Intervals (GTI) - generation of cleaned event files - source and background regions selection - check for the presence of pile-up - spectrum extraction (of both source and background) - creation of the Response Matrix Function (RMF) - creation of the Ancillary Response Function (ARF) - grouping of the spectra 3. Extraction of a light curve from a point-like source
OUTLINE
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Creation of the Redistribution Matrix File (RMF)
rmfgen spectrumset=source_spectrum.fits rmfset=pn.rmf
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The Redistribution Matrix File (RMF): associates to each instrument channel (I) the appropriate photon energy (E)
27!
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Creation of the Auxiliary Response File (ARF)
arfgen spectrumset=source_spectrum.f i ts arfset=pn.arf withrmfset=yes rmfset=pn.rmf badpixlocation=pn_new.evt detmaptype=psf
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27!
The Auxiliary Response File (ARF) includes information on the effective area, filter transmission and any additional energy-dependent
efficiencies, i.e. the efficiency of the instrument in revealing photons
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The combination of RMF and ARF produces the input spectrum weighted by telescope area and detector efficiencies versus
energy.
⊗ !
=!
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especget filestem=ngc7213_pn_r40 withfilestem=yes srcexp='((X,Y) IN circle(27655,26999,800))' backexp='((X,Y) IN circle(27737,23473,780))’ withbadpixcorr=yes useodfatt=no extendedsource=no table=pn_filt.fits withrmfset=no witharfset=yes
Or…..
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Grouping of the spectra
grppha source_spectrum.fits pn_25.grp comm= "chkey RESPFILE pn.rmf & chkey ANCRFILE pn.arf & chkey BACKFILE back_spectrum.fits & group min 25 & exit"
In order to apply the chi2 statistics (Gaussian distribution) you need to have at least 25 counts in each bin of your spectrum. Otherwise Cash statistics (Poisson distribution) is preferred (see also Statistics Tutorial).
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Grouping of the spectra
grppha source_spectrum.fits pn_25.grp comm= "chkey RESPFILE pn.rmf & chkey ANCRFILE pn.arf & chkey BACKFILE back_spectrum.fits & group min 25 & exit"
In order to apply the chi2 statistics (Gaussian distribution) you need to have at least 25 counts in each bin of your spectrum. Otherwise Cash statistics (Poisson distribution) is preferred (see also Statistics Tutorial).
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1. Download XMM-Newton data from the public archive 2. PN, MOS1 and MOS2 data reduction: - selection of Good Time Intervals (GTI) - generation of cleaned event files - source and background regions selection - check for the presence of pile-up - spectrum extraction (of both source and background) - creation of the Response Matrix Function (RMF) - creation of the Ancillary Response Function (ARF) - grouping of the spectra 3. Extraction of a light curve from a point-like source
OUTLINE
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EXTRACTION OF A LIGHT CURVE FROM A POINT-LIKE SOURCE
A light curve is the plot of the flux of a source vs time. It shows if and how the flux of the source varies during a certain time series. The variability of a source can manifest on different time scales.
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A light curve can be built in different temporal bins, e.g. if the observation is 1000 seconds long it is possible to extract light curves of 10 sec and 100 sec. The longer is the temporal bin the lower is the resolution but the higher is the S/N.
To establish if a source varied during the observation we can apply the chi2 test:
ci observed counts in every temporal bin i; σi Poissonian error; <c> average count during the observation; v=n-1 degrees of freedom;
A probability of chi2≤10-3 suggests that the source is varied. This test should be repeated for several temporal bins.
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EXTRACTION OF A LIGHT CURVE FROM A POINT-LIKE SOURCE (background corrected)
• Source+background light curve between 2-10 keV
evselect table=pn_new.evt energycolumn=PI expression=’#XMMEA_EP[M] && (PATTERN<=4[12]) && ((X,Y) IN circle(source.reg)) && (PI in [200:10000])’ withrateset=yes rateset=”PN_source_lc_raw.lc” timebinsize=100 maketimecolumn=yes makeratecolumn=yes
• Background light curve between 2-10 keV
evselect table=pn_new.evt energycolumn=PI expression=’#XMMEA_EP[M] && (PATTERN<=4 [12]) && ((X,Y) IN circle(back.reg)) && (PI in [200:10000])’ withrateset=yes rateset=”PN_back_lc_raw.lc” timebinsize=100 maketimecolumn=yes makeratecolumn=yes
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• Corrected light curve between 2-10 keV
epiclccorr srctslist=PN_source_lc_raw.lc eventlist=pn_new.evt outset=PN_lccorr.lc bkgtslist=PN_back_lc_raw.lc withbkgset=yes applyabsolutecorrections=yes
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Fitting group 2, from 5.47 to 5.62 Fitting 48 points in a band of 48. 1.0000000 ( -3) W-VAR= 62.47 ( -4) W-VAR= 62.47 16.526085
Example: > lcurve PN_source_lc_raw.lc > mo cons (fit di una costante) > fit
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http://www.fourmilab.ch/rpkp/experiments/analysis/chiCalc.html
62.47 48-1
0.0648
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> lcurve PN_source_lc_raw.lc > mo cons (fit di una costante) > fit
Fitting group 2, from 5.47 to 5.62 Fitting 48 points in a band of 48. 1.0000000 ( -3) W-VAR= 62.47 ( -4) W-VAR= 62.47 16.526085
The chance probability (Q) is 0.0648 (= the probability that this results is due to chance)
1-0.0648=0.9352 the source is variable at 93%.
Our acceptance threshold of variability is 99.9%
Example: