The Simbol-X Mission

Ferrando, P.; Arnaud, M.; Briel, U. G.; Cavazzuti, E.; Clédassou, R.; Counil, J. L.; Fiore, F.; Giommi, P.; Goldwurm, A.; Lamarle, O.; Pueyo, Laurent; Lebrun, F.; Malaguti, G.; Mereghetti, S.; Micela, G.; Pareschi, G.; Piermaria, M.; Roques, J. P.; Santangelo, A.; Tagliaferri, G.; Rodríguez, J.; Ferrando, Phillippe

doi:10.1063/1.3149459

Cited by 17 publications

(14 citation statements)

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“…The study of a X-ray mission with a good resolution at high energy is a challenge since several years, beginning with the Simbol-X [1] and HEXIT-SAT [2] missions and evolving into New Hard X-ray Mission (NHXM) [3] composed by 4 identical telescopes: three of them are equipped with spectro-imaging cameras, while the fourth is equipped with a X-ray polarimeter hosting two alternating detectors covering the range 2-35 keV in the focus of one of the four identical telescopes. The optics will be accommodated on the service module platform at a 10 m focal length distance from the instrument platform accommodating the focal plane assembly.…”

Section: Introductionmentioning

confidence: 99%

The optics system of the New Hard X-ray Mission: status report

et al. 2011

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The New Hard X-ray Mission (NHXM) is a space X-ray telescope project focused on the 0.2 to 80 keV energy band, coupled to good imaging, spectroscopic and polarimetry detectors. The mission is currently undergoing the Phase B study and it has been proposed to ESA as a small-size mission to be further studied in the context of the M3 call; even if the mission was not downselected for this call, its study is being continued by ASI. The required performance is reached with a focal length of 10 m and with four mirror modules, each of them composed of 70 NiCo electroformed mirror shells. The reflecting coating is a broadband graded multilayer film, and the focal plane is mounted onto an extensible bench. Three of the four modules are equipped with a camera made of two detectors positioned in series, a Silicon low energy detector covering the range 0.2 to 15 keV and a high energy detector based on CdTe sensitive from 10 keV up to 120 keV. The fourth module is dedicated to the polarimetry to be performed with enhanced imaging capabilities. In this paper the latest development in the design and manufacturing of the optics is presented. The design has been optimized in order to increase as much as possible the effective area in the high-energy band. The manufacturing of the mirror shells benefits from the latest development in the mandrel production (figuring and polishing), in the multilayer deposition and in the integration improvements.

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Section: Introductionmentioning

confidence: 99%

The optics system of the New Hard X-ray Mission: status report

et al. 2011

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“…Unfortunately, the limited EPIC bandpass does not allow the strength of this spectral component in 3C 234 to be meaningfully constrained, and, in turn, test the validity of this hypothesis. Future spectroscopy in the 10-60 keV range, say with Simbol-X (Ferrando et al 2006), will therefore be crucial for distinguishing a transmission from a reflection origin for the Fe Kα line in this QSO2. Young et al (1998) inferred a dust extinction toward 3C 234 of A V = 60 mag, which corresponds to an absorbing column density of ≈1.1 × 10 23 cm −2 , if the standard Galactic gasto-dust ratio is assumed (i.e.…”

Section: The Hard X-ray Spectrum and The Fe Kα Emission Linementioning

confidence: 99%

Heavy absorption and soft X-ray emission lines in the XMM-Newton spectrum of the type 2 radio-loud quasar 3C 234

Piconcelli¹,

Bianchi²,

Miniutti

et al. 2008

A&A

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Aims. We report results on a 40 ks XMM-Newton observation of the type 2 quasar 3C 234. Optical spectropolarimetric data have demonstrated the presence of a hidden broad-line region in this powerful (M V ≤ −24.2 after reddening and starlight correction) narrow-line FRII radio galaxy. Our analysis is aimed at investigating the X-ray spectral properties of this peculiar source that have remained poorly known so far. Methods. We analyze the 0.5-10 keV spectroscopic data collected by the EPIC cameras in 2006.Results. The X-ray spectrum of this radio-loud quasar is typical of a local Compton-thin Seyfert 2 galaxy. It exhibits strong absorption (N H ∼ 3.5 × 10 23 cm −2 ) and a narrow, neutral Fe Kα emission line with an equivalent width of ≈140 ± 40 eV. Our observation also reveals that the soft portion of the spectrum is characterized by strong emission lines with a very low level of scattered primary continuum. A possible explanation of these features in terms of thermal emission from a two-temperature, collisionally ionized plasma emission seems to be unlikely due to the high luminosity estimated for this component (L 0.5−2 ∼ 6 × 10 42 erg s −1 ). It is likely that most of the soft X-ray emission originates from a photoionized plasma as commonly observed in obscured, radio-quiet Seyfertlike AGNs.Conclusions. This X-ray observation has definitively confirmed the presence of a hidden quasar in 3C 234. The line-rich spectrum and the steepness of the hard X-ray continuum (Γ ≈ 1.7) found in this source weaken the hypothesis that the bulk of the X-ray emission in radio-loud AGNs with high-excitation optical lines arises from jet non-thermal emission.

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“…13 the ICS emission spectrum of the secondary electrons is shown for the radio emitting clusters (A2199, Coma, Perseus, A2163, A2390, RX J1347.5-1145). These fluxes, referring to the evaluation strategy i), can be compared with the expected sensitivity in the HXR band of the next coming mission Simbol-X (Ferrando et al 2005), which is approximately ∼10 −8 photons cm −2 s −1 keV −1 in the energy band 10−50 keV. From this figure we can conclude that the clusters A2199, Coma and Perseus should be detectable by Simbol-X, if the magnetic fields in these clusters are those inferred by assuming that the radio emission is produced by secondary electrons.…”

Section: Diffuse Hard X-ray Emission In Cool Core Clustersmentioning

confidence: 99%

Warming rays in cluster cool cores

Colafrancesco¹,

Marchegiani²

2008

A&A

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Context. Cosmic rays are confined in the atmospheres of galaxy clusters and, therefore, they can play a crucial role in the heating of their cool cores. Aims. We discuss here the thermal and non-thermal features of a model of cosmic ray heating of cluster cores that can provide a solution to the cooling-flow problems. To this aim, we generalize a model originally proposed by Colafrancesco, Dar & DeRujula (2004) and we show that our model predicts specific correlations between the thermal and non-thermal properties of galaxy clusters and enables various observational tests. Methods. The model reproduces the observed temperature distribution in clusters by using an energy balance condition in which the X-ray energy emitted by clusters is supplied, in a quasi-steady state, by the hadronic cosmic rays, which act as "warming rays" (WRs). The temperature profile of the intracluster (IC) gas is strictly correlated with the pressure distribution of the WRs and, consequently, with the non-thermal emission (radio, hard X-ray and gamma-ray) induced by the interaction of the WRs with the IC gas and the IC magnetic field. Results. The temperature distribution of the IC gas in both cool-core and non cool-core clusters is successfully predicted from the measured IC plasma density distribution. Under this contraint, the WR model is also able to reproduce the thermal and non-thermal pressure distribution in clusters, as well as their radial entropy distribution, as shown by the analysis of three clusters studied in detail: Perseus, A2199 and Hydra. The WR model provides other observable features of galaxy clusters: a correlation of the pressure ratio (WRs to thermal IC gas) with the inner cluster temperature (P WR /P th ) ∼ (kT inner ) −2/3 , a correlation of the gamma-ray luminosity with the inner cluster temperature L γ ∼ (kT inner ) 4/3 , a substantial number of cool-core clusters observable with the GLAST-LAT experiment, a surface brightness of radio halos in cool-core clusters that recovers the observed one, a hard X-ray ICS emission from cool-core clusters that is systematically lower than the observed limits and yet observable with the next generation high-sensitivity and spatial resolution HXR experiments like Simbol-X. Conclusions. The specific theoretical properties and the multi-frequency distribution of the e.m. signals predicted in the WR model render it quite different from the other models so far proposed for the heating of clusters' cool-cores. Such differences make it possible to prove or disprove our model as an explanation for the cooling-flow problems on the basis of multi-frequency observations of galaxy clusters.

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The Simbol-X Mission

Cited by 17 publications

References 0 publications

The optics system of the New Hard X-ray Mission: status report

The optics system of the New Hard X-ray Mission: status report

Heavy absorption and soft X-ray emission lines in the XMM-Newton spectrum of the type 2 radio-loud quasar 3C 234

Warming rays in cluster cool cores

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