A physical model for the hard X-ray background     

R. J. Wilman  A. C. Fabian  P. E. J. Nulsen 《Monthly notices of the Royal Astronomical Society》2000,319(2):583-590

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X-ray absorption and rapid variability of the dwarf Seyfert nucleus of NGC 4395     

K. Iwasawa  A. C. Fabian  O. Almaini  P. Lira  A. Lawrence  K. Hayashida  H. Inoue 《Monthly notices of the Royal Astronomical Society》2000,318(3):879-888

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Hard X-ray emission from elliptical galaxies     

S. W. Allen  T. Di Matteo  A. C. Fabian 《Monthly notices of the Royal Astronomical Society》2000,311(3):493-506

We report the detection of hard X-ray emission components in the spectra of six nearby, giant elliptical galaxies observed with the ASCA satellite. The systems studied, which exhibit strong dynamical evidence for supermassive black holes in their nuclei, are M87, NGC 1399 and NGC 4696 (the dominant galaxies of the Virgo, Fornax and Centaurus clusters, respectively) and NGC 4472, 4636 and 4649 (three further giant ellipticals in the Virgo cluster). The ASCA data for all six sources provide clear evidence for hard emission components, which can be parametrized by power-law models with photon indices in the range Γ=0.6–1.5 (mean value 1.2) and intrinsic 1–10 keV luminosities of 2×10⁴⁰–2×10⁴² erg s⁻¹. Our results imply the identification of a new class of accreting X-ray source, with X-ray spectra significantly harder than those of binary X-ray sources, Seyfert nuclei or low-luminosity active galactic nuclei, and bolometric luminosities relatively dominated by their X-ray emission. We discuss various possible origins for the hard X-ray emission and argue that it is most likely to be due to accretion on to the central supermassive black holes, via low radiative efficiency accretion flows coupled with strong outflows. In the case of M87, our detected power-law flux is in good agreement with a previously reported measurement from ROSAT High Resolution Imager observations, which were able to resolve the jet from the nuclear X-ray emission components. We confirm previous results showing that the use of multiphase models in the analysis of the ASCA data leads to determinations of approximately solar emission-weighted metallicities for the X-ray gas in the galaxies. We also present results on the individual element abundances in NGC 4636.  相似文献   

An ionized disc reflection component for the X‐ray spectrum of NGC 4051 and IRAS13224–3809?     

G. Ponti  G. Miniutti  A. C. Fabian  M. Cappi  G. G. C. Palumbo 《Astronomische Nachrichten》2006,327(10):1055-1058

A spectral variability study of the two Narrow Line Seyfert 1 galaxies NGC 4051 and IRAS13224–3809 is presented. Both sources show a high degree of flux and spectral variability. The nuclear emission, lightly absorbed by warm material, has been decomposed into a direct power law emission and an ionized disc reflection plus constant emission from distant material. The ionized disc reflection component does not follow the variations of the primary component. Its flux is linearly correlated with the one of the power law component only at low fluxes, while it is almost constant at medium high‐flux. This behavior is expected when the light bending effect is important. If so, most of the primary emission comes from only a few gravitational radii from the black hole. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Quantitative high-resolution warm season rainfall recorded in varved sediments of Lake Oeschinen,northern Swiss Alps: calibration and validation AD 1901–2008     

Benjamin Amann  Fabian Mauchle  Martin Grosjean 《Journal of Paleolimnology》2014,51(3):375-391

High-resolution, well-calibrated records of lake sediments are critically important for quantitative climate reconstructions, but they remain a methodological and analytical challenge. While several comprehensive paleotemperature reconstructions have been developed across Europe, only a few quantitative high-resolution studies exist for precipitation. Here we present a calibration and verification study of lithoclastic sediment proxies from proglacial Lake Oeschinen (46°30′N, 7°44′E, 1,580 m a.s.l., north–west Swiss Alps) that are sensitive to rainfall for the period AD 1901–2008. We collected two sediment cores, one in 2007 and another in 2011. The sediments are characterized by two facies: (A) mm-laminated clastic varves and (B) turbidites. The annual character of the laminae couplets was confirmed by radiometric dating (²¹⁰Pb, ¹³⁷Cs) and independent flood-layer chronomarkers. Individual varves consist of a dark sand-size spring-summer layer enriched in siliciclastic minerals and a lighter clay-size calcite-rich winter layer. Three subtypes of varves are distinguished: Type I with a 1–1.5 mm fining upward sequence; Type II with a distinct fine-sand base up to 3 mm thick; and Type III containing multiple internal microlaminae caused by individual summer rainstorm deposits. Delta-fan surface samples and sediment trap data fingerprint different sediment source areas and transport processes from the watershed and confirm the instant response of sediment flux to rainfall and erosion. Based on a highly accurate, precise and reproducible chronology, we demonstrate that sediment accumulation (varve thickness) is a quantitative predictor for cumulative boreal alpine spring (May–June) and spring/summer (May–August) rainfall (r_MJ = 0.71, r_MJJA = 0.60, p < 0.01). Bootstrap-based verification of the calibration model reveals a root mean squared error of prediction (RMSEP_MJ = 32.7 mm, RMSEP_MJJA = 57.8 mm) which is on the order of 10–13 % of mean MJ and MJJA cumulative precipitation, respectively. These results highlight the potential of the Lake Oeschinen sediments for high-resolution reconstructions of past rainfall conditions in the northern Swiss Alps, central and eastern France and south-west Germany.  相似文献   

A Chandra X-ray survey of nearby dwarf starburst galaxies – I. Data reduction and results     

Jürgen Ott †  Fabian Walter †  Elias Brinks † 《Monthly notices of the Royal Astronomical Society》2005,358(4):1423-1452

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X-ray Spectroscopy of the Scattered Emission in NGC 1068     

K. Iwasawa  A.C. Fabian  G. Matt 《Astrophysics and Space Science》1997,248(1-2):199-206

We discuss the iron K line complex in NGC 1068. The line complex basically consists of three components, as previously reported. A new analysis of the ASCA data shows that cold reflection appears to dominate the observed X-ray emission above 4 keV based on the detection of ‘Compton shoulder’, a weak red wing of the 6.4 keV fluorescence iron K line, and a very flat continuum. The other two weaker lines at higher energies can be identified with FeXXV and FeXXVI and suggest an highly ionized X-ray mirror as well, although the line energies are systematically lower than those expected from the resonant lines, consistent with a redshift by 1.5%. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

A survey of molecular hydrogen in the central galaxies of cooling flows     

A. C. Edge  R. J. Wilman  R. M. Johnstone  C. S. Crawford  A. C. Fabian  S. W. Allen 《Monthly notices of the Royal Astronomical Society》2002,337(1):49-62

We present a large sample of H - and K -band spectra of 32 optically line-luminous central cluster galaxies. We find significant rovibrational H₂ emission in 23 of these galaxies as well as H recombination and/or [Fe  ii ] emission in another five. This represents a fourfold increase in the number of molecular line detections known. A number of the detections are of extended emission (5–20 kpc). In several objects we find significant [Si  vi ] emission that appears to correlate with the strength of high ionization lines in the optical (e.g. [O  iii ]). This comprehensive sample builds on previous work and confirms that warm (1000–2500 K) molecular hydrogen is present wherever there is ionized material in the cores of cooling flows and in most cases it also coincides with CO molecular line emission.  相似文献   

Accretion disc coronae as magnetic reservoirs     

A. Merloni  A. C. Fabian 《Monthly notices of the Royal Astronomical Society》2001,321(3):549-552

Most astrophysical sources powered by accretion on to a black hole, either of stellar mass or supermassive, when observed with hard X-rays show signs of a hot Comptonizing component in the flow, the so-called corona , with observed temperatures and optical depths lying in a narrow range (0.1≲ τ ≲1 and 1×10⁹ K≲ T ≲3×10⁹ K). Here we argue that these facts constitute strong supporting evidence for a magnetically dominated corona. We show that the inferred thermal energy content of the corona, in all black hole systems, is far too low to explain their observed hard X-ray luminosities, unless either the size of the corona is at least of the order of 10³ Schwarzschild radii, or the corona itself is in fact a reservoir , where the energy is mainly stored in the form of a magnetic field generated by a sheared rotator (probably the accretion disc). We briefly outline the main reasons why the former possibility is to be discarded, and the latter preferred.  相似文献   

Enrichment in the Centaurus cluster of galaxies     

J. S. Sanders  A. C. Fabian 《Monthly notices of the Royal Astronomical Society》2006,371(3):1483-1496

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