# XMM-Newton large program on SN1006 - I. Methods and initial results of spatially resolved spectroscopy

Marco Miceli, Anne Decourchelle, Marco Miceli, Jacco Vink, Jiang-Tao Li, Fabrizio Bocchino

Risultato della ricerca: Article

12 Citazioni (Scopus)

Based on our newly developed methods and the XMM-Newton large program of SN1006, we extract and analyse the spectra from 3596 tessellated regions of this supernova remnant (SNR) each with 0.3-8 keV counts >10^4. For the first time, we map out multiple physical parameters, such as the temperature (kT), electron density (n_e), ionization parameter (n_et), ionization age (t$_ion), metal abundances, as well as the radio-to-X-ray slope ($\alpha$) and cutoff frequency ($\nu$$_cutoff) of the synchrotron emission. We construct probability distribution functions of kT and n_et, and model them with several Gaussians, in order to characterize the average thermal and ionization states of such an extended source. We construct equivalent width (EW) maps based on continuum interpolation with the spectral model of each region. We then compare the EW maps of O VII, O VIII, O VII K\delta - \zeta, Ne, Mg, Si XIII, Si XIV, and S lines constructed with this method to those constructed with linear interpolation. We further extract spectra from larger regions to confirm the features revealed by parameter and EW maps, which are often not directly detectable on X-ray intensity images. For example, O abundance is consistent with solar across the SNR, except for a low-abundance hole in the centre. This O hole' has enhanced O VII K\delta - \zeta and Fe emissions, indicating recently reverse shocked ejecta, but also has the highest n_et, indicating forward shocked interstellar medium (ISM). Therefore, a multitemperature model is needed to decompose these components. The asymmetric metal distributions suggest there is either an asymmetric explosion of the supernova or an asymmetric distribution of the ISM. Lingua originale English 3953-3974 22 Monthly Notices of the Royal Astronomical Society 453 Published - 2015 ### Fingerprint XMM-Newton telescope newton ionization spectroscopy supernova remnants interpolation cut-off probability distribution functions electron density explosions explosion metal ions x rays radio slopes ion metal programme method temperature ### All Science Journal Classification (ASJC) codes • Astronomy and Astrophysics • Space and Planetary Science ### Cita questo XMM-Newton large program on SN1006 - I. Methods and initial results of spatially resolved spectroscopy. / Miceli, Marco; Decourchelle, Anne; Miceli, Marco; Vink, Jacco; Li, Jiang-Tao; Bocchino, Fabrizio. In: Monthly Notices of the Royal Astronomical Society, Vol. 453, 2015, pag. 3953-3974. Risultato della ricerca: Article Miceli, Marco ; Decourchelle, Anne ; Miceli, Marco ; Vink, Jacco ; Li, Jiang-Tao ; Bocchino, Fabrizio. / XMM-Newton large program on SN1006 - I. Methods and initial results of spatially resolved spectroscopy. In: Monthly Notices of the Royal Astronomical Society. 2015 ; Vol. 453. pagg. 3953-3974. @article{2ad13a2fb8fc4f618307bda6ed314c92, title = "XMM-Newton large program on SN1006 - I. Methods and initial results of spatially resolved spectroscopy", abstract = "Based on our newly developed methods and the XMM-Newton large program of SN1006, we extract and analyse the spectra from 3596 tessellated regions of this supernova remnant (SNR) each with 0.3-8 keV counts >10^4. For the first time, we map out multiple physical parameters, such as the temperature (kT), electron density (n_e), ionization parameter (n_et), ionization age (t_ion), metal abundances, as well as the radio-to-X-ray slope (\alpha) and cutoff frequency (\nu$$_cutoff$) of the synchrotron emission. We construct probability distribution functions of kT and n$_e$t, and model them with several Gaussians, in order to characterize the average thermal and ionization states of such an extended source. We construct equivalent width (EW) maps based on continuum interpolation with the spectral model of each region. We then compare the EW maps of O VII, O VIII, O VII K$\delta$-$\zeta$, Ne, Mg, Si XIII, Si XIV, and S lines constructed with this method to those constructed with linear interpolation. We further extract spectra from larger regions to confirm the features revealed by parameter and EW maps, which are often not directly detectable on X-ray intensity images. For example, O abundance is consistent with solar across the SNR, except for a low-abundance hole in the centre. This O hole' has enhanced O VII K$\delta$-$\zeta$and Fe emissions, indicating recently reverse shocked ejecta, but also has the highest n$_e$t, indicating forward shocked interstellar medium (ISM). Therefore, a multitemperature model is needed to decompose these components. The asymmetric metal distributions suggest there is either an asymmetric explosion of the supernova or an asymmetric distribution of the ISM.", keywords = "acceleration of particles, shock waves, methods: data analysis, cosmic rays, ISM: supernova remnants, X-rays: ISM", author = "Marco Miceli and Anne Decourchelle and Marco Miceli and Jacco Vink and Jiang-Tao Li and Fabrizio Bocchino", year = "2015", language = "English", volume = "453", pages = "3953--3974", journal = "Monthly Notices of the Royal Astronomical Society", issn = "0035-8711", publisher = "Oxford University Press", } TY - JOUR T1 - XMM-Newton large program on SN1006 - I. Methods and initial results of spatially resolved spectroscopy AU - Miceli, Marco AU - Decourchelle, Anne AU - Miceli, Marco AU - Vink, Jacco AU - Li, Jiang-Tao AU - Bocchino, Fabrizio PY - 2015 Y1 - 2015 N2 - Based on our newly developed methods and the XMM-Newton large program of SN1006, we extract and analyse the spectra from 3596 tessellated regions of this supernova remnant (SNR) each with 0.3-8 keV counts >10^4. For the first time, we map out multiple physical parameters, such as the temperature (kT), electron density (n_e), ionization parameter (n_et), ionization age (t$_ion), metal abundances, as well as the radio-to-X-ray slope ($\alpha$) and cutoff frequency ($\nu$$_cutoff) of the synchrotron emission. We construct probability distribution functions of kT and n_et, and model them with several Gaussians, in order to characterize the average thermal and ionization states of such an extended source. We construct equivalent width (EW) maps based on continuum interpolation with the spectral model of each region. We then compare the EW maps of O VII, O VIII, O VII K\delta - \zeta, Ne, Mg, Si XIII, Si XIV, and S lines constructed with this method to those constructed with linear interpolation. We further extract spectra from larger regions to confirm the features revealed by parameter and EW maps, which are often not directly detectable on X-ray intensity images. For example, O abundance is consistent with solar across the SNR, except for a low-abundance hole in the centre. This O hole' has enhanced O VII K\delta - \zeta and Fe emissions, indicating recently reverse shocked ejecta, but also has the highest n_et, indicating forward shocked interstellar medium (ISM). Therefore, a multitemperature model is needed to decompose these components. The asymmetric metal distributions suggest there is either an asymmetric explosion of the supernova or an asymmetric distribution of the ISM. AB - Based on our newly developed methods and the XMM-Newton large program of SN1006, we extract and analyse the spectra from 3596 tessellated regions of this supernova remnant (SNR) each with 0.3-8 keV counts >10^4. For the first time, we map out multiple physical parameters, such as the temperature (kT), electron density (n_e), ionization parameter (n_et), ionization age (t_ion), metal abundances, as well as the radio-to-X-ray slope (\alpha) and cutoff frequency (\nu$$_cutoff$) of the synchrotron emission. We construct probability distribution functions of kT and n$_e$t, and model them with several Gaussians, in order to characterize the average thermal and ionization states of such an extended source. We construct equivalent width (EW) maps based on continuum interpolation with the spectral model of each region. We then compare the EW maps of O VII, O VIII, O VII K$\delta$ - $\zeta$, Ne, Mg, Si XIII, Si XIV, and S lines constructed with this method to those constructed with linear interpolation. We further extract spectra from larger regions to confirm the features revealed by parameter and EW maps, which are often not directly detectable on X-ray intensity images. For example, O abundance is consistent with solar across the SNR, except for a low-abundance hole in the centre. This O hole' has enhanced O VII K$\delta$ - $\zeta$ and Fe emissions, indicating recently reverse shocked ejecta, but also has the highest n$_e$t, indicating forward shocked interstellar medium (ISM). Therefore, a multitemperature model is needed to decompose these components. The asymmetric metal distributions suggest there is either an asymmetric explosion of the supernova or an asymmetric distribution of the ISM.

KW - acceleration of particles, shock waves, methods: data analysis, cosmic rays, ISM: supernova remnants, X-rays: ISM

UR - http://hdl.handle.net/10447/165819

M3 - Article

VL - 453

SP - 3953

EP - 3974

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

ER -