The medium-energy concentrator spectrometer on board the 
BeppoSAX X-ray astronomy satellite

Boella, G.; Chiappetti, L.; Conti, G.; Cusumano, G.; Sordo, S. Del; Rosa, G. La; Maccarone, M. C.; Mineo, T.; Molendi, S.; Re, S.; Sacco, B.; Tripiciano, M.

doi:10.1051/aas:1997138

Cited by 315 publications

(256 citation statements)

References 5 publications

Supporting

Mentioning

254

Contrasting

Order By: Relevance

“…Mkn 841 was also observed between the 11th and 14th of February 2001 by the BeppoSAX satellite (Boella et al 1997 and references therein). The source was pointed for a total net time exposure of ∼90, 40 and 20 ks for the MECS, PDS and LECS instruments respectively.…”

Section: Observation and Data Analysismentioning

confidence: 82%

A rapidly variable narrow X-ray iron line in Mkn 841

Petrucci

Henri

Maraschi

et al. 2002

A&A

View full text Add to dashboard Cite

Abstract. We report on the detection of a rapidly variable narrow Fe Kα line in Mkn 841. The source has been observed two times by XMM-Newton and simultaneously with BeppoSAX. The two observations, of about 10 ks long each, were separated by ∼15 hours. The line flux reaches a maximum during the first observation and is significantly reduced in the second one. The continuum shape and flux, instead, keep roughly constant between the two pointings. Such rapid variability of a narrow (unresolved by the XMM-pn instrument) line has never been reported in the past. These results are not easily explained in the standard cold reflection model where the narrow line component is supposed to be produced far from the primary X-ray source (e.g. from the torus) and is thus not expected to vary rapidly. Different interpretations are discussed.

show abstract

Section: Observation and Data Analysismentioning

confidence: 82%

A rapidly variable narrow X-ray iron line in Mkn 841

Petrucci

Henri

Maraschi

et al. 2002

A&A

View full text Add to dashboard Cite

show abstract

“…The temperature for these perpendicular components is taken to be the same as that Ðtted to the thermal bremsstrahlung emitted at energies less than 10 keV. A Ðt to the BeppoSAX Medium Energy Concentrator (MECS ; Boella et al 1997) spectrum from 1997 November 26 determined this temperature at 3.3 keV. This Ðt is shown in Figure 1.…”

Section: The Electron Distribution Function From Lower Hybrid Wave Damentioning

confidence: 99%

Accelerated Electrons in Cassiopeia A: An Explanation for the Hard X‐Ray Tail

Laming

2001

ApJ

View full text Add to dashboard Cite

We propose a model for the hard X-ray ([10 keV) emission observed from the supernova remnant Cas A. Lower hybrid waves are generated in strong (mG) magnetic Ðelds, generally believed to reside in this remnant, by shocks reÑected from density inhomogeneities. These then accelerate electrons to energies of several tens of keV. Around 4% of the X-rayÈemitting plasma electrons need to be in this accelerated distribution, which extends up to electron velocities of order the electron speed and is Alfven directed along magnetic Ðeld lines. Bremsstrahlung from these electrons produces the observed hard X-ray emission. Such waves and accelerated electrons have been observed in situ at comet Halley, and we discuss the viability of the extrapolation from this case to the parameters relevant to Cas A.

show abstract

“…We analyze data taken with the Medium Energy Concentrator Spectrometer (MECS) on board BeppoSAX. The MECS (see Boella et al 1997 for details) is composed of two identical gas scintillation proportional counters (three detectors before 1997 May 9) that are sensitive in the 1.3È10.5 keV energy range. The event Ðles for all 12 clusters were subjected to the standard screening criteria of the BeppoSAX SDC.…”

Section: Sample and Data Reductionmentioning

confidence: 99%

“…At 9@ the telescope entrance-window support structure (the strongback) strongly absorbs X-rays, making spectroscopy difficult in this area of the detector. In addition, for o †-axis angles greater than 10@, the departure of the PSF from radial symmetry becomes noticeable (Boella et al 1997). With this in mind, we ended the radial proÐles at 9@.…”

Section: Sample and Data Reductionmentioning

confidence: 99%

Iron Abundance Profiles of 12 Clusters of Galaxies Observed withBeppoSAX

Irwin

Bregman

2001

ApJ

View full text Add to dashboard Cite

We have derived azimuthally averaged radial iron-abundance proÐles of the X-ray gas contained within 12 clusters of galaxies with redshift 0.03 ¹ z ¹ 0.2 observed with BeppoSAX. We Ðnd evidence for a negative metal-abundance gradient in most of the clusters, particularly signiÐcant in clusters that possess cooling Ñows. The composite proÐle from the 12 clusters resembles that of cluster simulations of Metzler & Evrard. This abundance gradient could be the result of the spatial distribution of gas-losing galaxies within the cluster being more centrally condensed than the primordial hot gas. Both inside and outside the core region we Ðnd a higher abundance in cooling-Ñow clusters than in nonÈcooling-Ñow clusters. Outside of the cooling region this di †erence cannot be the result of more efficient sputtering of metals into the gaseous phase in cooling-Ñow clusters but might be the result of the mixing of lowmetallicity gas from the outer regions of the cluster during a merger.

show abstract

The medium-energy concentrator spectrometer on board the BeppoSAX X-ray astronomy satellite

Cited by 315 publications

References 5 publications

A rapidly variable narrow X-ray iron line in Mkn 841

A rapidly variable narrow X-ray iron line in Mkn 841

Accelerated Electrons in Cassiopeia A: An Explanation for the Hard X‐Ray Tail

Iron Abundance Profiles of 12 Clusters of Galaxies Observed withBeppoSAX

Contact Info

Product

Resources

About