The high energy instrument PDS on-board the BeppoSAX X–ray astronomy
satellite

Frontera, F.; Costa, E.; Fiume, D. Dal; Feroci, M.; Nicastro, L.; Orlandini, M.; Palazzi, E.; Zavattini, G.

doi:10.1051/aas:1997140

Cited by 360 publications

(207 citation statements)

References 14 publications

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“…As in Paper I, we used the data obtained with the Medium Energy Concentrator Spectrometer (MECS), operating in the 1.3-10 keV energy band (Boella et al 1997), and the Phoswich Detector System (PDS) operating in the 15-300 keV energy band (Frontera et al 1997). Furthermore, we considered the data obtained with the High Pressure Gas Scintillation Proportional Counter (HPGSPC; Manzo et al 1997), which worked in the nominal energy band 4-120 keV, and covers the gap between the two other instruments.…”

Section: Observation and Data Reductionmentioning

confidence: 99%

The complex behaviour of the microquasar GRS 1915+105 in theρclass observed withBeppoSAX

Mineo

Massaro

D’Aí

et al. 2011

A&A

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Context. BeppoSAX observed GRS 1915+105 on October 2000 with a long pointing lasting about ten days. During this observation, the source was mainly in the ρ class characterized by bursts with a recurrence time of between 40 and 100 s. Aims. We identify five segments in the burst structure and accumulate the average spectra of these segments during each satellite orbit. We present a detailed spectral analysis aimed at determining variations that occur during the burst and understanding the physical process that produces them. Methods. We compare MECS, HPGSPC, and PDS spectra with several models. Under the assumption that a single model is able to fit all spectra, we find that the combination of a multi-temperature black-body disk and a hybrid corona is able to give a consistent physical explanation of the source behaviour. Results. Our measured variations in KT el , τ, KT in , and R in appear to be either correlated or anti-correlated with the count rate in the energy range 1.6-10 keV. The strongest variations are detected along the burst segments: almost all parameters exhibit significant variations in the segments that have the highest fluxes (pulse) with the exception of R in , which varies continuously and reaches a maximum just before the peak. The flux of the multi-temperature disk strongly increases in the pulse and simultaneously the corona contribution is significantly reduced. Conclusions. The disk luminosity increases in the pulse and the R in − T in correlation can be most successfully interpreted in term of the slim disk model. In addition, the reduction in the corona luminosity during the bursts might represent the condensation of the corona onto the disk.

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Section: Observation and Data Reductionmentioning

confidence: 99%

The complex behaviour of the microquasar GRS 1915+105 in theρclass observed withBeppoSAX

Mineo

Massaro

D’Aí

et al. 2011

A&A

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“…The NFIs include a Low-Energy Concentrator Spectrometer (LECS, 0.1−10 keV; Parmar et al 1997), three Medium-Energy Concentrator Spectrometers (MECS, 1.5−10 keV; Boella et al 1997b), a High-Pressure Gas Scintillation Proportional Counter (HPGSPC, 4−120 keV; Manzo et al 1997), and a Phoswich Detection System (PDS, 15−300 keV; Frontera et al 1997). Both observations were performed with all three MECS units (MECS unit 1 failed on 1997 May 6).…”

Section: Observations and Data Analysismentioning

confidence: 99%

The transient hard X-ray tail of GX 17+2: New BeppoSAX results

Farinelli¹,

Frontera

Zdziarski

et al. 2005

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Abstract. We report on results of two BeppoSAX observations of the Z source GX 17+2. In both cases the source is in the horizontal branch of the colour-intensity diagram. The persistent continuum can be fit by two-component models consisting of a blackbody plus a Comptonization spectrum. With one of these models, two solutions for the blackbody temperature of both the observed and seed photons for Comptonization are equally accepted by the data. In the first observation, when the source is on the left part of the horizontal branch, we observe a hard tail extending up to 120 keV, while in the second observation, when the source moves towards right in the same branch, the tail is no longer detected. The hard ( > ∼ 30 keV) X-ray emission can be modeled either by a simple power-law with photon index Γ ∼ 2.8, or assuming Comptonization of ∼1 keV soft photons off a hybrid thermal plus non-thermal electron plasma. The spectral index of the non-thermal injected electrons is p ∼ 1.7. The observation of hard X-ray emission only in the left part of the horizontal branch could be indicative of the presence of a threshold in the accretion rate above which the hard tail disappears. An emission line at 6.7 keV with equivalent width ∼ 30 eV is also found in both observations. We discuss these results and their physical implications.

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“…GRB010214 was detected on February 14, 2001, at 08:48:11 UT with the BeppoSAX (Boella et al 1997) GammaRay Burst Monitor (GRBM, 40-700 keV, Frontera et al 1997), and the Wide Field Camera No. 2 (WFC, 2-28 keV, Jager et al 1997).…”

Section: Observations and Data Analysismentioning

confidence: 99%

The dark burst 010214 withBeppoSAX: Possible variable absorption and jet X–ray emission

Guidorzi

Frontera

Montanari

et al. 2003

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Abstract. We report on the prompt and afterglow emission observations of the dark burst GRB010214 with BeppoSAX. The prompt emission shows possible evidence of variable absorption from N H = 3.0 +5.1 −2.0 × 10 23 cm −2 in the first 6 s of the event to a value consistent with the Galactic column density (N G H = 2.66 × 10 20 cm −2 ) in the GRB direction. An X-ray afterglow emission in the 2-10 keV energy band was detected with BeppoSAX, but an analogue search at lower wavelengths (optical, IR and radio) was unsuccessful. The X-ray afterglow spectrum is consistent with a power-law with Galactic absorption. The light curve shows a complex decay, if the tail of the prompt emission is assumed as the onset of the afterglow: if the origin of the afterglow is coincident with the GRB onset, a bump before ∼3 × 10 4 s is inferred, while if the afterglow is assumed to start later, a steepening of the power-law light curve at t ∼ 3 × 10 4 s is deduced. We discuss these results in the light of the current models of afterglows and the possible origin of the GRB darkness. Finally, we tentatively derive an estimate of the burst redshift.

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The high energy instrument PDS on-board the BeppoSAX X–ray astronomy satellite

Cited by 360 publications

References 14 publications

The complex behaviour of the microquasar GRS 1915+105 in theρclass observed withBeppoSAX

The complex behaviour of the microquasar GRS 1915+105 in theρclass observed withBeppoSAX

The transient hard X-ray tail of GX 17+2: New BeppoSAX results

The dark burst 010214 withBeppoSAX: Possible variable absorption and jet X–ray emission

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