Final analysis of ELAIS 15-μm observations: method, reduction and catalogue     

M. Vaccari  C. Lari  L. Angeretti  D. Fadda  C. Gruppioni  F. Pozzi  O. Prouton  H. Aussel  T. Babbedge  P. Ciliegi  A. Franceschini  E. Gonzalez-Solares  F. La Franca  S. Oliver  I. Perez-Fournon  M. Rowan-Robinson  S. Serjeant  P. Väisänen 《Monthly notices of the Royal Astronomical Society》2005,358(2):397-418

We present the final analysis of the European Large Area Infrared Space Observatory ( ISO ) Survey (ELAIS) 15-μm observations, carried out with the ISO Camera (ISOCAM) instrument on board the ISO .
The data-reduction method, known as the Lari Method, is based on a mathematical model of the behaviour of the detector and was specifically designed for the detection of faint sources in ISOCAM/ISO Photopolarimeter (ISOPHOT) data. The method is fully interactive and leads to very reliable and complete source lists.
The resulting catalogue includes 1923 sources detected with signal-to-noise ratio of  > 5  in the 0.5–100 mJy flux range and over an area of 10.85 deg² split into four fields, making it the largest non-serendipitous extragalactic source catalogue obtained to date from the ISO data.
This paper presents the concepts underlying the data-reduction method together with its latest enhancements. The data-reduction process, the production and basic properties of the resulting catalogue are discussed. The catalogue quality is assessed by means of detailed simulations, optical identifications and comparison with previous analyses.  相似文献   

A Chandra observation of the X-ray environment and jet of 3C 31     

M. J. Hardcastle  D. M. Worrall  M. Birkinshaw  R. A. Laing  A. H. Bridle 《Monthly notices of the Royal Astronomical Society》2002,334(1):182-192

We have used a deep Chandra observation of the central regions of the twin-jet Fanaroff–Riley class I (FRI) radio galaxy 3C 31 to resolve the thermal X-ray emission in the central few kpc of the host galaxy, NGC 383, where the jets are thought to be decelerating rapidly. This allows us to make high-precision measurements of the density, temperature and pressure distributions in this region, and to show that the X-ray emitting gas in the centre of the galaxy has a cooling time of only  5×10⁷ yr  . In a companion paper, these measurements are used to place constraints on models of the jet dynamics.
A previously unknown one-sided X-ray jet in 3C 31, extending up to 8 arcsec from the nucleus, is detected and resolved. Its structure and steep X-ray spectrum are similar to those of X-ray jets known in other FRI sources, and we attribute the radiation to synchrotron emission from a high-energy population of electrons. In situ particle acceleration is required in the region of the jet where bulk deceleration is taking place.
We also present X-ray spectra and luminosities of the galaxies in the Arp 331 chain of which NGC 383 is a member. The spectrum and spatial properties of the nearby bright X-ray source 1E 0104+3153 are used to argue that the soft X-ray emission is mostly due to a foreground group of galaxies rather than to the background broad absorption-line quasar.  相似文献   

The flux-dependent amplitude of broadband noise variability in X-ray binaries and active galaxies     

Philip Uttley  Ian M. McHardy 《Monthly notices of the Royal Astronomical Society》2001,323(2):L26-L30

Standard shot-noise models, which seek to explain the broadband noise variability that characterizes the X-ray light curves of X-ray binaries and active galaxies, predict that the power spectrum of the X-ray light curve is stationary (i.e. constant amplitude and shape) on short time-scales. We show that the broadband noise power spectra of the black hole candidate Cyg X-1 and the accreting millisecond pulsar SAX J1808.4−3658 are intrinsically non-stationary, in that rms variability scales linearly with flux. Flux-selected power spectra confirm that this effect is due to changes in power-spectral amplitude and not shape. The light curves of three Seyfert galaxies are also consistent with a linear relationship between rms variability and flux, suggesting that it is an intrinsic feature of the broadband noise variability in compact accreting systems over more than six decades of central object mass. The rms variability responds to flux variations on all measured time-scales, raising fundamental difficulties for shot-noise models which seek to explain this result by invoking variations in the shot parameters. We suggest that models should be explored where the longest time-scale variations are fundamental and precede the variations on shorter time-scales. Possible models which can explain the linear rms-flux relation include the fractal break-up of large coronal flares, or the propagation of fluctuations in mass accretion rate through the accretion disc. The linear relationship between rms variability and flux in Cyg X-1 and SAX J1808.4−3658 is offset on the flux axis, suggesting the presence of a second, constant-flux component to the light curve which contributes ∼25 per cent of the total flux. The spectrum of this constant component is similar to the total spectrum, suggesting that it may correspond to quiet, non-varying regions in the X-ray emitting corona.  相似文献   

Relativistic large-scale jets and minimum power requirements     

G. Ghisellini  A. Celotti 《Monthly notices of the Royal Astronomical Society》2001,327(3):739-743

The recent discovery, by the Chandra satellite, that jets of blazars are strong X-ray emitters at large scales     , lends support to the hypothesis that emitting plasma is still moving at highly relativistic speeds on these scales. In this case in fact the emission via inverse Compton scattering off cosmic background photons is enhanced and the resulting predicted X-ray spectrum accounts well for the otherwise puzzling observations. Here we point out another reason to favour relativistic large-scale jets, based on a minimum power argument: by estimating the Poynting flux and bulk kinetic powers corresponding to, at least, the relativistic particles and magnetic field responsible for the emission, one can derive the value of the bulk Lorentz factor for which the total power is minimized. It is found that both the inner and extended parts of the jet of PKS     satisfy such a condition.  相似文献   

黄骅坳陷地区正断层位移模式     

王翔  王战 《地球科学与环境学报》1997,(4)

黄骅坳陷属新生代张性盆地。在第三纪的ＮＷ—ＳＥ向区域拉张作用下，本区形成大量走向ＮＥ—ＳＷ的正断层。通过对该区正断层位移分布的研究，划分出Ｃ、Ｅ、Ｄ、Ｍ和Ｚ型五种断层位移模式，并进一步探讨了诸如断裂生长机制、岩石力学性质、相邻断层的相互作用、次级断裂的相互衔接这样几种控制因素对断层位移分布的影响。  相似文献   

EVN observations of low-luminosity flat-spectrum active galactic nuclei     

A. Caccianiga  M.J.M. Marchã  A. Thean  J. Dennett-Thorpe 《Monthly notices of the Royal Astronomical Society》2001,328(3):867-872

We present and discuss the results of very-long baseline interferometry (VLBI, EVN) observations of three low-luminosity     broad emission line active galactic nuclei (AGNs) carefully selected from a sample of flat-spectrum radio sources (CLASS). Based on the total and the extended radio power at 5 and at 1.4 GHz respectively, these objects should be technically classified as radio-quiet AGN and thus the origin of their radio emission is not clearly understood. The VLBI observations presented in this paper have revealed compact radio cores which imply a lower limit on the brightness temperature of about     . This result rules out a thermal origin for the radio emission and strongly suggests an emission mechanism similar to that observed in more powerful radio-loud AGNs. Since, by definition, the three objects show a flat (or inverted) radio spectrum between 1.4 and 8.4 GHz, the observed radio emission could be relativistically beamed. Multi-epoch VLBI observations can confirm this possibility in two years' time.  相似文献   

On the interaction of FR II radio sources with the intracluster medium     

P. Alexander 《Monthly notices of the Royal Astronomical Society》2002,335(3):610-620

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地壳相对活动区的灰色划分     

李杰  杨沾吉 《大地测量与地球动力学》1993,(1)

本文根据灰色系统中的聚类原理,提出了有关复测网区内地壳活动区的灰色划分方法,即根据动态平差得到的观测值速率和关联度这两个灰类指标,对观测值按不同的灰类进行灰色聚类,从而划分地壳的相对活动区。文中给出了重力网重复观测值的灰色关联度、聚类权以及灰类白化函数的计算方法,并用一个复测重力网资料进行了计算,结果表明:用该方法所划出的相对活动区与实际情况比较符合。  相似文献   

常德1631年大震事件的多场点群发式构造模型     

甘家思  刘锁旺  申重阳 《大地测量与地球动力学》1993,(4)

根据对常德1631年地震事件的史料鉴别,尤其是江陵为典型七度震害这一事实,运用震声传播方向和地光物理场以及地震烈度衰减关系,拟合推断此地震事件的序列主要由安乡北6 3/4级地震、常德北太阳山7级地震、澧县6级地震、大庸6级地震和澧县—安乡6 1/2级地震组成,相应的地震地质背景是江汉—洞庭地区晚更新世以来的剩余形变呈四象限分布。若考虑地震-构造相关分布为“Z”字型,则该地震事件的主控构造——太阳山断裂带东断裂具左旋走滑的力学机制。根据区域地震—构造相关发展过程,常德大震事件可视为1668年郯城8 1/2级地震的前震序列组成部分。  相似文献   

The origin of [Fe ii] emission in NGC 4151     

James E. H.Turner  JeremyAllington-Smith †  ScottChapman ‡  RobertContent  ChristineDone  RogerHaynes §  DavidLee ¶  SimonMorris &#; 《Monthly notices of the Royal Astronomical Society》2002,331(2):284-292

The centre of NGC 4151 has been observed in the J band with the SMIRFS integral field unit (IFU) on the UK Infrared Telescope. A map of [Fe  ii ] emission is derived, and compared with the distributions of the optical narrow-line region and radio jet. We conclude that, because the [Fe  ii ] emission is associated more closely with the visible narrow-line region than with the radio jet, it arises mainly through photoionization of gas by collimated X-rays from the Seyfert nucleus. The velocity field and strength with respect to Pa β are found to be consistent with this argument. The performance of the IFU is considered briefly, and techniques for observation and data analysis are discussed.  相似文献