Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3....

31
XMM EPIC MOS Steve Sembay ([email protected]) Madrid 23/03/10 Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response “Calibration or just a mathematical exercise?” Ties together three themes.... 1) Computationally quick phenomenological RMF model 2) Derivation of RMF model parameters via optimisation algorithm 3) Use of “standard candle” spectra to constrain RMF solution Wednesday, 24 March 2010

Transcript of Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3....

Page 1: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response

“Calibration or just a mathematical exercise?”

Ties together three themes....

1) Computationally quick phenomenological RMF model2) Derivation of RMF model parameters via optimisation algorithm3) Use of “standard candle” spectra to constrain RMF solution

Wednesday, 24 March 2010

Page 2: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Di1 = N1 Σ Rij Aj1 Sj1

Di2 = N2 Σ Rij Aj2 Sj2

...

Din = Nn Σ Rij Ajn Sjn

Adjust parameters (using tnmin algorithm) which define rmf, R, and global normalisations, N, to minimise

Σ ((Oi - Di)/δOi)2 + Σ ((Oi - Di)/δOi)2 + ... + Σ ((Oi - Di)/δOi)2

Basic Scheme: For a given epoch and spatial region...

Wednesday, 24 March 2010

Page 3: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Previous Phenomenological Model: The VRMF Model

Blue Wing: Gaussian

Red Wing: Voigt Function

= Gaussian convolved with a Lorentian.

Dampening factor = 0 (Gaussian) > 0 (Lorentz-like)

Fit to Orsay Data

Wednesday, 24 March 2010

Page 4: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Frac in (red+orange) = 0.48Frac in orange = 0.52

Frac in (red+orange) = 0.53Frac in orange = 0.55

Frac in (red+orange) = 0.44Frac in orange = 0.23

Out of patch “wings (15”-40”)”

“core (0”-15”)”

New model adds a flat “shelf”

Evaluation time for 2400 x 2400array (5eV binning) ~ 3.5 seconds in IDL

Wednesday, 24 March 2010

Page 5: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Resolution = α1 + β1 x sqrt(e0)

Dampen= α2 exp( -(e0-β2) / γ2) for β2 > e0 = α2 β2 <= e0

i.e. tends to zero for large e0 (more Gaussian)

Parameters which define redistribution matrix, R

Wednesday, 24 March 2010

Page 6: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

FLoss = α3 exp( -(e0-β3) / γ3) for β3 > e0 = α3 β3 <= e0

FLoss = FLoss_peak + FLoss_shelf

FLoss_peak= α4 exp( -(e0-β4) / γ4) for β4 > e0 = α4 β4 <= e0

EEloss/e0 = α5 for e0 < 300 eV = α6 for e0 > 400 eV

Wednesday, 24 March 2010

Page 7: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Total parameters = 13

Not counting parameters giving intensityof silicon fluorescence and escape peaks(fixed to previous calibration)

Time to derive one solution for a given set of input spectra ~ 3 to 6 hours.

Wednesday, 24 March 2010

Page 8: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

“Standard Candle” Spectral Models

1) The white dwarf CAL83

2) The isolated neutron star RXJ 1856

3) The O star Zeta Puppis

4) The SNR 1ES0102

Wednesday, 24 March 2010

Page 9: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

“Standard Candle” Spectral Models

1) The white dwarf CAL83

See next slides

2) The isolated neutron star RXJ 1856

phabs * (bb + bb) (V. Burwtiz pn model)

3) The O star Zeta Puppis

Frank’s RGS model

4) The SNR 1ES0102

The IACHEC WG model (Plucinsky et al.)

Wednesday, 24 March 2010

Page 10: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Lantz, T, et al. (2005) ApJ, 619, 517

Non-LTE Model atmosphere derivedfrom LETG and RGS (Rev 0068)

Model file converted to atable model

nH = 6.5 x 1020 cm-2 (abund wilm)

0

5×10!18

10!17

norm

alize

d cou

nts s!

1 Hz!1

Black (RGS1) Red (RGS2)CAL83 RGS Rev 0068

20 30 40 50 60 700

1

2

3

ratio

Wavelength (Å)

0

5×10!18

10!17

norm

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d cou

nts s!

1 Hz!1

Black (old rmf) Red (new rmf)CAL 83 MOS1 rev 0068

20 30 40 50 60 700.5

1

1.5

ratio

Wavelength (Å)

Wednesday, 24 March 2010

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XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Lantz, T, et al. (2005) ApJ, 619, 517

Non-LTE Model atmosphere derivedfrom LETG and RGS (Rev 0068)

Model file converted to atable model

nH = 6.5 x 1020 cm-2 (abund wilm)

0

2×10−17

4×10−17

norm

alize

d cou

nts s−

1 Hz−1

Black (PN Thin) Red (PN Med)CAL 83 PN Rev 0068

20 30 40 50 60 700.5

1

1.5

ratio

Wavelength (Å)

Use instead best fit descriptive modelto PN = phabs * bb (abund wilm)

nH = 1.11 x 1021 cm-2

kT = 0.034 keV

Wednesday, 24 March 2010

Page 12: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Epoch 1: Revolution 0065 - 0156

“Pre-Patch”

Standards:

1E0102 (Rev 65)Cal 83 (Rev 68)Puppis (Rev 156)

Test Sources:

MS0737 (BL Lac) (Rev 63)3C 273 (Blazar) (Rev 94)

Wednesday, 24 March 2010

Page 13: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

1.2931.2931.2511.482

1.2501.2541.2261.354

1.2221.1981.2341.750

1.1901.1651.2211.510

0

1

2

3no

rmal

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coun

ts s

−1 k

eV−1

Black (thin) Red (med) Green (thick)CAL 83 MOS1 Rev 0068 (current rmf)

0.2 0.5

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Black (thin) Red (med) Green (thick)CAL 83 MOS1 Rev 0068 (new rmf)

0.2 0.5

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Black (thin) Red (med) Green (thick)CAL 83 MOS2 Rev 0068 (current rmf)

0.2 0.5

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Black (thin) Red (med) Green (thick)CAL 83 MOS2 Rev 0068 (new rmf)

0.2 0.5

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Black (thin) Red (med) Green (thick)

M1 M2

Wednesday, 24 March 2010

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XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

0.972 - 0.9731.993 - 1.422

0.944 - 0.9462.235 - 1.697

1.063 - 1.0612.253 - 2.441

1.106 - 1.1081.859 - 1.567

0

5

10

norm

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d co

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s−1

keV

−1

Black (current RMF) Red (new RMF)1E0102 MOS2 Rev 0065

10.2 0.5

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sign(

data−m

odel

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"2

Energy (keV)

0

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Black (current RMF) Red (new RMF)Puppis MOS2 Rev 0156

10.2 0.5

−20

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"2

Energy (keV)

0

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d co

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s−1

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−1Black (current RMF) Red (new RMF)

Puppis MOS1 Rev 0156

10.2 0.5

−20

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sign(

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Black (current RMF) Red (new RMF)1E0102 MOS1 Rev 0065

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sign(

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odel

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Wednesday, 24 March 2010

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XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

1.0531.129

1.1411.094

1.1471.093

1.0571.135

0.01

0.1

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norm

alize

d co

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s−1

keV

−1Black (PN) Red (MOS1 old RMF)

m0737 PN/MOS1 Rev 0063

10.2 0.5 2 5−20

−10

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sign(

data−m

odel

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Energy (keV)

0.01

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Black (PN) Red (MOS2 old RMF)m0737 PN/MOS2 Rev 0063

10.5 2 5−20

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0.01

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Black (PN) Red (MOS2 new RMF)m0737 PN/MOS2 Rev 0063

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data−m

odel

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"2

Energy (keV)

Wednesday, 24 March 2010

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XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

1.0531.033

1.0201.001

1.0251.037

1.0601.042

0.1

1

10no

rmal

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coun

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−1 k

eV−1

Black (PN) Red (MOS1 old RMF)3c273 PN/MOS1 Rev 0094

10.2 0.5 2 5−20

−10

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sign(

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0.1

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Black (PN) Red (MOS1 old RMF)3c273 PN/MOS1 Rev 0094

10.2 0.5 2 5−20

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data−m

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Energy (keV)

Black (PN) Red (MOS1 new RMF)

0.1

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−1

Black (PN) Red (MOS1 old RMF)3c273 PN/MOS2 Rev 0094

10.2 0.5 2 5−20

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odel

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0.1

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Black (PN) Red (MOS1 old RMF)3c273 PN/MOS2 Rev 0094

10.2 0.5 2 5−20

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data−m

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Energy (keV)

Black (PN) Red (MOS1 new RMF)

Wednesday, 24 March 2010

Page 17: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Epoch 2: Revolution 0795-0900

On-axis, “patch affected”

Standards:

RXJ1856 (Rev 878)Puppis (Rev 795)1E0102 (Rev 894-900)

Test Sources:

H1426 (BL Lac) (Rev 939)

Wednesday, 24 March 2010

Page 18: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Wednesday, 24 March 2010

Page 19: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

1.116 - 1.0891.425 - 1.287

1.089 - 1.0751.312 - 1.139

0.920 - 1.0408.152 - 1.506

0.990 - 0.98616.64 - 2.458

0

2

4

6

norm

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d co

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keV

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RXJ1856 MOS1 Rev 0878 Thin

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Black (current RMF) Red (new RMF)RXJ1856 MOS2 Rev 0878 Thin

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Energy (keV)

Black (current RMF) Red (new RMF)

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Black (current RMF) Red (new RMF)Puppis MOS1 Rev 0795

10.2 0.5

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Black (current RMF) Red (new RMF)Puppis MOS1 Rev 0795

10.2 0.5

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data−m

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Energy (keV)

“Core”

Wednesday, 24 March 2010

Page 20: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

1.073 - 1.0711.298 - 1.216

1.029 - 1.0351.298 - 1.214

0.817 - 0.9063.994 - 1.058

0.962 - 0.9852.846 - 1.344

0

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RXJ1856 MOS1 Rev 0878 Thin

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Black (current RMF) Red (new RMF)RXJ1856 MOS2 Rev 0878 Thin

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Black (current RMF) Red (new RMF)Puppis MOS1 Rev 0795

10.2 0.5

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0.4

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Black (current RMF) Red (new RMF)Puppis MOS1 Rev 0795

10.2 0.5

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“Wings”

Wednesday, 24 March 2010

Page 21: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

6.582 - 1.8364.728 - 1.713

1.325 - 1.173 2.060 - 2.121

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1E0102 MOS1 Rev 0894−0900

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Black (current RMF) Red (new RMF)1E0102 MOS2 Rev 0894−0900

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Energy (keV)

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Black (current RMF) Red (new RMF)1E0102 MOS1 Rev 0894−0900

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Energy (keV)

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Energy (keV)

“Core”

“Wings”

Wednesday, 24 March 2010

Page 22: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

1.0330.987

1.0001.059

0.9961.065

1.0361.010

0.01

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H1426 PN/MOS1 Rev 0939

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Black (PN) Red (MOS1 new RMF)H1426 PN/MOS1 Rev 0939

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Black (PN) Red (MOS2 old RMF)H1426 PN/MOS2 Rev 0939

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Black (PN) Red (MOS2 new RMF)H1426 PN/MOS2 Rev 0939

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Page 23: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Epoch 3: Revolution 1265-1335

Off axis (Still on CCD1)

Standards:

1E0102 (Rev 1265)RXJ1856 (Rev 1335)

Test Sources:

REJ 2248 (AGN) (Rev 1361)

Wednesday, 24 March 2010

Page 24: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

0.878 - 0.8833.624 - 1.590

0.908 - 0.9133.380 - 2.139

0.902 - 1.03634.74 - 1.324

0.874 - 0.95925.24 - 1.503

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Black (current RMF) Red (new RMF)1E0102 MOS1 Rev 1265

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RXJ1856 MOS1 Rev 1335

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Black (current RMF) Red (new RMF)RXJ1856 MOS2 Rev 1335

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Wednesday, 24 March 2010

Page 25: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

1.0341.254

1.0531.166

1.0791.225

1.0601.186

0.01

0.1

1

norm

alize

d co

unts

s−1

keV

−1Black (PN) Red (MOS1 old RMF)

REJ2248 PN/MOS1 Rev 1361

10.2 0.5 2 5−20

−10

0

10

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0.01

0.1

1

norm

alize

d co

unts

s−1

keV

−1

Black (PN) Red (MOS1 new RMF)REJ2248 PN/MOS1 Rev 1361

10.2 0.5 2 5−20

−10

0

10

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0.01

0.1

1

norm

alize

d co

unts

s−1

keV

−1

Black (PN) Red (MOS2 old RMF)REJ2248 PN/MOS2 Rev 1361

10.2 0.5 2 5−20

−10

0

10

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0.01

0.1

1

norm

alize

d co

unts

s−1

keV

−1

Black (PN) Red (MOS2 new RMF)REJ2248 PN/MOS2 Rev 1361

10.2 0.5 2 5−20

−10

0

10

20

sign(

data−m

odel

) × !

"2

Energy (keV)

Wednesday, 24 March 2010

Page 26: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Epoch 4: Revolution 1616-1636

On-axis, “patch affected”

Standards:

RXJ1856 (Rev 1616)1E0102 (Rev 1636)

Test Sources:

3C 273 (BL Lac) (Rev 1649)

Wednesday, 24 March 2010

Page 27: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

1.560 - 1.8741.955 - 1.770

0.821 - 0.97518.13 - 2.495

0.892 - 0.89428.09 - 7.000

0

1

2

3

norm

alize

d co

unts

s−1

keV

−1

Black (current RMF) Red (new RMF)1E0102 MOS1 Rev 1636

10.2 0.5

−20

0

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0

1

2

3

norm

alize

d co

unts

s−1

keV

−1

Black (current RMF) Red (new RMF)1E0102 MOS2 Rev 1636

10.2 0.5

−20

0

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0

2

4

6no

rmal

ized

coun

ts s

−1 k

eV−1

Black (current RMF) Red (new RMF)RXJ1856 MOS1 Rev 1616

0.1 0.2 0.5

−20

0

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0

2

4

6

norm

alize

d co

unts

s−1

keV

−1

Black (current RMF) Red (new RMF)RXJ1856 MOS2 Rev 1616

0.1 0.2 0.5

−20

0

20

sign(

data−m

odel

) × !

"2

Energy (keV)

“Core”

Wednesday, 24 March 2010

Page 28: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

3.647 - 1.5043.509 - 1.614

0.733 - 0.9355.390 - 0.992

0.907 - 0.9382.964 - 2.015

0

2

4

norm

alize

d co

unts

s−1

keV

−1

Black (current RMF) Red (new RMF)1E0102 MOS1 Rev 1636

10.2 0.5

−20

0

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0

2

4

6

norm

alize

d co

unts

s−1

keV

−1

Black (current RMF) Red (new RMF)1E0102 MOS2 Rev 1636

10.2 0.5

−20

0

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0

0.5

1

1.5

2no

rmal

ized

coun

ts s

−1 k

eV−1

Black (current RMF) Red (new RMF)RXJ1856 MOS1 Rev 1616

0.1 0.2 0.5

−20

0

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0

0.5

1

1.5

2

norm

alize

d co

unts

s−1

keV

−1

Black (current RMF) Red (new RMF)RXJ1856 MOS2 Rev 1616

0.1 0.2 0.5

−20

0

20

sign(

data−m

odel

) × !

"2

Energy (keV)

“Wings”

Wednesday, 24 March 2010

Page 29: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

1.0290.970

0.9590.953

0.9421.003

1.0271.024

0.1

1

10no

rmal

ized

coun

ts s

−1 k

eV−1

Black (PN) Red (MOS1 old RMF)3c273 PN/MOS1 Rev 1649

10.2 0.5 2 5−20

−10

0

10

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0.1

1

10

norm

alize

d co

unts

s−1

keV

−1

Black (PN) Red (MOS1 new RMF)3c273 PN/MOS2 Rev 1649

10.2 0.5 2 5−20

−10

0

10

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0.1

1

10

norm

alize

d co

unts

s−1

keV

−1

Black (PN) Red (MOS1 old RMF)3c273 PN/MOS2 Rev 1649

10.2 0.5 2 5−20

−10

0

10

20

sign(

data−m

odel

) × !

"2

Energy (keV)

0.1

1

10

norm

alize

d co

unts

s−1

keV

−1

Black (PN) Red (MOS1 new RMF)3c273 PN/MOS2 Rev 1649

10.2 0.5 2 5−20

−10

0

10

20

sign(

data−m

odel

) × !

"2

Energy (keV)

Wednesday, 24 March 2010

Page 30: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

Conclusions:

1) The MOS has a strongly variable on-axis response and needsto calibrated against “something” given that we have no physical model of the response which explains the changes we see.

2) The best we can do is probably pick models of astrophysical sources for which there is some consensus within the communityof what these models should be....i.e. so-called “standard candles”

3) We have a mathematical model of the response which looks togive a good fit to a chosen subset of these “standard candles”

4) If we adopt this route we need to make the ALL the “standard candle” models publically available to the community (i.e. XSPEC xcm files) with documentation as to how these models were derived.

Wednesday, 24 March 2010

Page 31: Using Standard Candle X-ray spectra to calibrate the strongly variable MOS response · 2010. 3. 26. · 1) The white dwarf CAL83 See next slides 2) The isolated neutron star RXJ 1856

XMMEPICMOS

Steve Sembay ([email protected])Madrid 23/03/10

End

Wednesday, 24 March 2010