The search for X-ray emission from an electron/ positron pair halo … · 2018. 11. 22. · Atchara Kueathan Srinakharinwirot university Siam Physics Congress, 2018 The search for

Atchara Kueathan Srinakharinwirot university Siam Physics Congress, 2018

The search for X-ray emission from an electron/positron pair halo using XMM-Newton observatory

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Atchara Kueathan Srinakharinwirot University

Siam Physics Congress, 21-23 May 2018

Wasutep Laungtip, Srinakharinwirot University

Wiraporn Maithong, Chiang Mai Rajabhat University

Anant Eungwanichayapant, Mae Fah Luang University

With

Introduction: An electron/positron pair halo

An electron/Positron pair halo

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• The high energy photons is produced by blazer from the extragalactic source

Toy model of blazarFrom: http://slideplayer.com/slide/1712095/


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Introduction: An electron/positron pair halo

An electron/Positron pair halo

• An electromagnetic cascade would happen due to the continuous processes of:• Pair production• Inverse Compton scattering

Electron/positron pair halo modelFrom: Anant Eungwanichayapant, 2003


Cosmic Microwave background (CMB)

Cosmic infrared background (CIB)

The high energy photons Electrons/Positrons

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Introduction: Synchrotron radiation from the halo

Synchrotron radiation from the halo

• Due to the presence of intergalactic magnetic field, the produced electron/positron pairs could gyrate before scattered with the CMB photons.

Synchrotron radiation produced by relativistic electrons gyrating in magnetic fields

From: https://bigkingken.files.wordpress.com/2010/12/synchrotron.jpg


Cosmic Microwave background (CMB)

Cosmic infrared background (CIB)

The high energy photons Electrons/Positrons

X-ray

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Introduction: Previous studies

Previous studies

1994

2001

2009

2010

2010

2011

Aharonian et.alThe Spectral Energy Distributions (SEDs) of gamma ray was calculated by the

Monte Carlo simulation method.

Aharonian et.alAttempt to detect the gamma rays from the halo using High-

Energy Gamma Ray Astronomy (HEGRA) telescope

Eungwanichayapant and Aharonian.

The angular distribution of the

gamma ray emission was calculated

Ando and Kusenko.Reported the detection of the electron/positron pair halo from the AGN

Neronor, Semikoz, Tinyakov and

Tkachav.Argued that the

detection is artifact

Eungwanichayapant, Maithong and Ruffolo.The SEDs and angular

distribution of the halo in the X-ray waveband was proposed.


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Objective

Objective

• To search for the observational evidence of the electron/positron pair halo in the X-ray waveband using XMM-Newton observatory.


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Introduction: XMM-Newton observatory

XMM-Newton observatory

• One of the best X-ray observatories in the current generation.• Consist of two main detectors:

• EPIC MOS (MOS1 and MOS2)• EPIC pn


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Methodology

• Select sample

• Simulate SED of the sample halo

• Simulate XMM-Newton spectra


The position of AGN H426+428From : https://xmm-tools.cosmos.esa.int/external/xmm_user_support/

documentation/uhb/epicmode.html

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Methodology: source selection

Source selection

• redshift z = 0.129 or 633 Mpc

• This is BL laceratea.

AGN H426+428

• The luminosity in the order of 1045 erg s-1


https://xmm-tools.cosmos.esa.int/external/xmm_user_support/documentation/uhb/epicmode.html

https://xmm-tools.cosmos.esa.int/external/xmm_user_support/documentation/uhb/epicmode.html

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Methodology: simulation of SEDs

Simulation of SEDs

• The monoenergetics, intrinsic gamma ray photon energy of 100 TeV

• The source luminosity of 1045 erg s-1

• The SEDs were calculated using Monte Carlo simulations following the model of Eungwanichayapant, Maithong and Ruffolo in 2011.

• The magnetics field of 1 Gµ


Defined regions to simulate SEDs

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Methodology: Selected regions for SED simulations

Selected regions for SED simulations

BRegion B : the outer regionThe angular distance covers from 0.133 - 0.200 degree.

A

Region A : the inner regionThe angular distance is from

0 - 0.133 degree.

C

Region C : the region out of XMM-Newton field of viewThe angular distance cover from 0.200 - infinite degree.


The pair halo X-ray SEDs simulated by assuming the monoenergetics, intrinsic gamma ray photon energy of 100 TeV, source luminosity of 10^45 erg s-1 and the magnetics field of 1 microG

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Methodology: Simulation of SEDs

Simulation of SEDs

Region ARegion BRegion C


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Methodology: Simulation of XMM-Newton spectra

Simulation of XMM-Newton spectra

• The SEDs were used as a model for simulating XMM-Newton spectra

• Add galactic absorption column (NH) of 1.11X1020 atoms cm2 into the model.

• Simulate the observed spectra of pn, MOS1 and MOS2 using RMF and ARF obtained from XMM-Newton official web.


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Methodology: Simulation of XMM-Newton spectra

Simulation of XMM-Newton spectra

The simulated pn spectra The simulated MOS spectra


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Conclusion

Conclusion

BThe outer region

The halo X-ray photons 580 counts (~17%).

A

The inner regionThe halo X-ray photons 2700

counts (~80%)

C

The region out of XMM-Newton field of view

The halo X-ray photons 70 counts (~3%)


• Up to ~97% of the halo photons would be detected in XMM-Newton detectors.

• In the region A, the halo photon could be much diluted by the AGN photons.

Atchara Kueathan Srinakharinwirot university Siam Physics Congress, 2018 !16

Conclusion

Conclusion

• The potential region to detect the halo X-ray emission is region B.

• XMM-Newton shows some possibility to detect the pair halo emission.

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Acknowledgement

Acknowledgement

• Science Achievement Scholarship of Thailand (SAST)

• National Astronomical Research Institute of Thailand (NARIT)

• National Science and Technology Development Agency (NSTDA)


Documents

The search for X-ray emission from an electron/ positron pair halo … · 2018. 11. 22. · Atchara Kueathan Srinakharinwirot university Siam Physics Congress, 2018 The search for