A5050268221- Astrophysical Phenomena and Observations
- Gamma-ray bursts and supernovae
- Pulsars and Gravitational Waves Research
- Astrophysics and Cosmic Phenomena
- Particle Detector Development and Performance
- High-pressure geophysics and materials
- Astronomical Observations and Instrumentation
- Nuclear Physics and Applications
- Astronomy and Astrophysical Research
- Astro and Planetary Science
- Dark Matter and Cosmic Phenomena
- Stellar, planetary, and galactic studies
- Geophysics and Gravity Measurements
- Mechanics and Biomechanics Studies
- Particle Accelerators and Free-Electron Lasers
- Galaxies: Formation, Evolution, Phenomena
- Solar and Space Plasma Dynamics
- Superconducting Materials and Applications
- Neutrino Physics Research
- Astrophysics and Star Formation Studies
- SAS software applications and methods
- Spacecraft Design and Technology
- CCD and CMOS Imaging Sensors
- Radiation Detection and Scintillator Technologies
- Geomagnetism and Paleomagnetism Studies
National Institute for Astrophysics
2012-2023
University of Turku
2023
Durham University
2023
Osservatorio di Astrofisica e Scienza dello Spazio
2018-2023
TU Dortmund University
2023
University of Łódź
2023
Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas
2023
Niels Brock
2023
University of Copenhagen
2023
Main Astronomical Observatory
2023
BeppoSAX/PDS experiment is one of four narrow field instruments the BeppoSAX payload, that also includes two wide cameras. The goal PDS to extend energy range hard X–rays. operative 15 300 keV, where can perform sensitive spectral and temporal studies celestial sources. detector composed 4 actively shielded NaI(Tl)/CsI(Na) phoswich scintillators with a total geometric area view 13 (FWHM). In this paper we describe design discuss its functional performance calibration data analysis system.
GRB 221009A is the brightest gamma-ray burst ever detected since discovery of this kind energetic explosions. However, an accurate measurement prompt emission properties very challenging due to its exceptional brightness. With joint observations \textit{Insight}-HXMT and GECAM-C, we made unprecedentedly during first $\sim$1800 s 221009A, including precursor, main (ME, which dominates in flux), flaring early afterglow, hard X-ray soft band from $\sim$ 10 keV 6 MeV. Based on GECAM-C...
We report the discovery of a transient equivalent hydrogen column density with an absorption edge at approximately 3.8 kiloelectron volts in spectrum prompt x-ray emission gamma-ray burst (GRB) 990705. This feature can be satisfactorily modeled photoelectric by medium located redshift 0.86 and iron abundance 75 times solar one. The behavior is attributed to strong ionization produced circumburst GRB photons. high points existence environment enriched supernova along line sight. explosion...
We investigated the spectral evolution in 2-700 keV energy band of gamma-ray bursts (GRBs) detected by Gamma-Ray Burst Monitor (GRBM) and localized with Wide Field Cameras (WFCs) aboard BeppoSAX satellite before 1998 May. Most them have been followed up Narrow Instruments same satellite. In light these results we discuss open issues on GRB phenomenon. find that optically thin synchrotron shock model (SSM) provides an acceptable representation most time-resolved spectra extending down to 2...
We present BeppoSAX follow-up observations of GRB 980425 obtained with the Narrow Field Instruments (NFI) in 1998 April, May, and November. The first NFI observation has detected within 8' radius error box gamma-ray burst (GRB) an X-ray source positionally consistent supernova 1998bw, which exploded a day 980425, fainter source, not position supernova. former is following pointings exhibits decline factor 2 six months. If it associated SN this detection emission from Type I above keV. latter...
We report the hard X-ray spectrum of Coma cluster obtained using PDS data two independent BeppoSAX observations performed with a time interval about three years. In both spectra non thermal excess respect to emission is present at confidence level ~ 3.4 sigma. The combined by adding up allows measurement 4.8 sigma energies above 20 keV. analysis full set provides revised non-thermal flux which slightly lower than that previously estimated (Fusco-Femiano et al. 1999) and in agreement measured...
The recurrent hard pulsating X-ray transient X0115+63 was observed with BeppoSAX on 1999 March 19, when the source at a 2-10 keV flux level of ~310 mcrab. We report high-energy spectrum source, concentrating cyclotron resonant scattering features. is strongly pulse phase dependent, and absorption features are detected virtually all phases. In particular, four absorption-like 12.74, 24.16, 35.74, 49.5 in descending edge main peak profile. ratios between centroid energies lines respect to...
We report on an accurate measurement of the CXB in 15-50 keV range performed with Phoswich Detection System (PDS) instrument aboard BeppoSAX satellite. establish that most likely intensity level at its emission peak (26-28 keV) is ~40 keV/cm2/s/sr, a value consistent derived from best available obtained over 25 years ago first High Energy Astronomical Observatory satellite mission (HEAO-1; Gruber et al. 1999), whose intensity, lying well below extrapolation some lower energy measurements...
We report on the 0.5-200 keV spectral properties of Cyg X-1 observed at different epochs with Narrow Field Instruments BeppoSAX satellite. The source was in its soft state during first observation 1996 June. In second September, had parameters characteristic to hard state. A X-ray excess, a broad Fe Kα line and Compton reflection are clearly detected both states. soft-state broadband continuum is well modeled by disk blackbody (accounting for excess) upscattering photons hybrid,...
We report on an observation of the low-mass X-ray binary 4U 1626-67 performed during BeppoSAX science verification phase. An absorption feature at ~37 keV, which is attributable to electron cyclotron resonance, has been discovered in its pulse-averaged spectrum. The inferred neutron star magnetic field strength 3.2(1+z)×1012 G, where z gravitational redshift. deep and narrow resolved both broadband fit ratio observed counts those seen from Crab pulsar. resonance energy good agreement with...
Observations of the prompt afterglow Gamma Ray Burst (GRB) events are unanimously considered paramount importance for GRB science and related cosmology. Such observations at NIR wavelengths even more promis-ing allowing one to monitor high-z Ly-α absorbed bursts as well occurring in dusty star-forming regions. In these pages we present REM (Rapid Eye Mount), a fully robotized fast slewing telescope equipped with high throughput (Z, J, H, K) camera dedicated detecting IR afterglow. can...
We report on the catalog of gamma-ray bursts (GRBs) detected with Gamma-Ray Burst Monitor aboard BeppoSAX satellite. It includes 1082 GRBs 40–700 keV fluences in range from 1.3 × 10−7 to 4.5 10−4 erg cm−2, and peak fluxes 3.7 10−8 7.0 10−5 cm−2 s−1. some relevant parameters each GRB discuss derived statistical properties.
No robust detection of prompt electromagnetic counterparts to fast radio bursts (FRBs) has yet been obtained, in spite several multi-wavelength searches carried out so far. Specifically, X/gamma-ray are predicted by some models. We planned on searching for gamma-ray the Insight-Hard X-ray Modulation Telescope (Insight-HXMT) data, taking advantage unique combination large effective area keV-MeV energy range and sub-ms time resolution. selected 39 FRBs that were promptly visible from...
Abstract Nuclear astrophysics, and particularly nuclear emission line diagnostics from a variety of cosmic sites, has remained one the least developed fields in experimental astronomy, despite its central role addressing number outstanding questions modern astrophysics. Radioactive isotopes are co-produced with stable fusion reactions nucleosynthesis supernova explosions other violent events, such as neutron star mergers. The origin 511 keV positron annihilation observed direction Galactic...
We report the results of a survey Galactic center region (∣ l ∣ < 2°, b 05) performed with BeppoSAX satellite. The flux from our Galaxy corresponds to luminosity ~3 × 1035 ergs s-1 in 2-10 keV range. Due limited angular resolution (≳1'), only part it is supposed come Sagittarius A*, nonthermal radio source that believed mark dynamical Galaxy. In addition diffuse emission, several bright (LX ≳ 1036 s-1) point sources have been observed, both persistent (A1742-294, SLX 1744-299, 1744-300, 1E...
We report on BeppoSAX and Chandra observations of three Hard X-Ray Transients in quiescence containing fast spinning (P<5 s) neutron stars: A 0538-66, 4U 0115+63 V 0332+53. These allowed us to study these transients at the faintest flux levels thus far. Spectra are remarkably different from ones obtained luminosities a factor >10 higher, testifying that quiescent emission mechanism is different. Pulsations were not detected any sources, indicating accretion matter down star surface has...
We report on results of a Target-of-Opportunity observation the X-ray transient XTE J1118+480 performed 2000 April 14-15 with Narrow Field Instruments (0.1-200 keV) BeppoSAX satellite. The measured spectrum is power law photon index ~1.7 modified by an ultrasoft excess and high-energy cutoff above ~100 keV. soft consistent blackbody temperature ~40 eV low flux, while well fitted thermal Comptonization in plasma electron ~102 keV optical depth order unity. Consistent weakness blackbody,...
We observed with Chandra two peculiar galactic X-ray sources, 4U 1700+24 and 1954+319, which are suspected to have a M-type giant star as optical counterpart, in order get high-precision astrometric position for both of them. The peculiarity these sources lies the fact that only cases among low-mass binaries (LMXBs), besides confirmed case GX 1+4, companion can possibly be giant. found field is indeed counterpart sources. also determined distance 1954+319 ~1.7 kpc. This result suggests...
The transient 500 s X-ray pulsar MAXI J1409−619 was discovered by the slit cameras aboard Monitor of All-sky Image (MAXI) on 2010 October 17, and soon after accurately localized Swift. We found that source position serendipitously observed in 2000 during BeppoSAX observations Galactic plane. Two sources are clearly detected Medium-Energy Concentrator Spectrometer (MECS): one is consistent with IGR J14043−6148 other J1409−619. report analysis this archival BeppoSAX/MECS observation integrated...
We report high-energy spectral data of the prompt emission GRB 970228 and its X-ray afterglow. establish that nature afterglow is nonthermal similar to later portion 970228. Our can be used discriminate different models afterglows. While cooling excited compact objects ruled out, fireball are constrained in physics radiation processes their evolution.
We report on a BeppoSAX observation of the transient X-ray pulsar 4U 0115+63 close to periastron. This led discovery dramatic luminosity variation from ~2x10^34 erg/s ~5x10^36 (factor ~250) in less than 15 hr. The was accompanied by only minor (if any) changes emitted spectrum and pulse fraction. On contrary an near apastron detected source nearly constant state at level ~2x10^33 erg/s. Direct accretion onto neutron star surface encounters major difficulties explaining variability...
We report the detection by Gamma-Ray Burst Monitor on board BeppoSAX of strongest and longest outburst ever detected from SGR 1900+14. Oscillations are detectable with a period ~5.16 s for entire duration event (~300 s). The temporal analysis reveals also remarkable periodic substructure: after about 35 onset, each 5.16 pulse shows pattern four subpulses dip, separated ~1 s. Significant spectral variation is during individual oscillation. first most intense part quite hard similar to what...
We report on ASCA and BeppoSAX X–ray broad band observations of the galactic low-luminosity source 4U 1700+24 performed 1995 1998, respectively, (quasi-)simultaneous ground its optical counterpart, V934 Her, from Loiano 1.5-meter telescope. In order to better understand nature we also analyze public archival ROSAT RXTE data as well ASM light curve 1700+24; re–analyze a 1985 EXOSAT pointing. The spectra are typical M2 III star; this allows us determine revised distance object ~400 pc. While...