Search Publications
Global characteristics of the first IBIS/ISGRI catalogue sources: unveiling a murky episode of binary star evolution
Hill, A. B.; Walter, R.; Bird, A. J. +10 more
INTEGRAL is the first gamma-ray astronomy mission with a sufficient sensitivity and angular resolution combination appropriate to the detection and identification of considerable numbers of gamma-ray emitting sources. The large field of view (~30° zero response FWHM) enables INTEGRAL to survey the galactic plane on a regular (~weekly) basis as par…
Globular clusters in NGC 4365: new K-band imaging and a reassessment of the case for intermediate-age clusters
Larsen, S. S.; Strader, J.; Brodie, J. P.
We study the globular cluster (GC) system of the Virgo giant elliptical galaxy
Luminous X-Ray Flares from Low-Mass X-Ray Binary Candidates in the Early-Type Galaxy NGC 4697
Sarazin, Craig L.; Jordán, Andrés; Sivakoff, Gregory R.
We report results of the first search specifically targeting short-timescale X-ray flares from low-mass X-ray binaries in an early-type galaxy. A new method for flare detection is presented. In NGC 4697, the nearest, optically luminous, X-ray-faint elliptical galaxy, three out of 157 sources are found to display flares at >99.95% probability, a…
Variation in the Scattering Shroud Surrounding Markarian 231
Brandt, W. N.; Chartas, G.; Gallagher, S. C. +5 more
We present a detailed study of the nuclear structure of the highly polarized broad absorption line quasar, Mrk 231, through a multiwavelength campaign of Chandra observations, optical spectroscopy, optical spectropolarimetry, and imaging polarimetry. This campaign was designed to extend the 40 ks Chandra study of Gallagher and coworkers and the op…
The evolution of Ks-selected galaxies in the GOODS/CDFS deep ISAAC field
McLure, R. J.; Dunlop, J. S.; Caputi, K. I. +1 more
We present estimated redshifts and derived properties of a sample of 1663 galaxies with Ks<= 22 (Vega), selected from 50.4 arcmin2 of the Great Observatories Origins Deep Survey/Chandra Deep Field South (GOODS/CDFS) field with deep Infrared Spectrometer and Array Camera (ISAAC) imaging, and make an extensive comparison of …
XMM-Newton observations of SS 433 I. EPIC spectral analysis
Kawai, N.; Brinkmann, W.; Kotani, T.
SS433 was observed with XMM-Newton in four consecutive orbits at different binary phases at precessional phases near maximum blue-/red shift between April 2 and April 8, 2003. The light curves in the individual orbits are flat without statistically significant indications for short-term (⪆50 s) intrinsic variability. Orbit-to-orbit flux changes oc…
Projection of circumstellar disks on their environments
Pontoppidan, K. M.; Dullemond, C. P.
We use a 3D Monte Carlo radiative transfer code to study the projection of large shadows by circumstellar disks around young stellar objects on surrounding reflection nebulosity. It is shown that for a wide range of parameters a small (10-100 AU) circumstellar disk can project a large (1000-10 000 AU) dark band in the near-infrared that often rese…
Dynamic Harris current sheet thickness from Cluster current density and plasma measurements
Balogh, A.; Khurana, K. K.; Kistler, L. M. +5 more
We use the first accurate measurements of current densities in the plasma sheet to calculate the half-thickness and position of the current sheet as a function of time. Our technique assumes a Harris current sheet model, which is parameterized by lobe magnetic field B0, current sheet half-thickness h, and current sheet position z0<…
Secular light curve of Comet 28P/Neujmin 1 and of spacecraft target Comets 1P/Halley, 9P/Tempel 1, 19P/Borrelly, 21P/Giacobinni Zinner, 26P/Grigg Skjellerup, 67P/Churyumov Gerasimenko, and 81P/Wild 2
Ferrín, Ignacio
We present the secular light curves of eight comets listed in the title. Two plots per comet are needed to study these objects: a reduced magnitude (to Δ=1 AU = geocentric distance) vs time, and a reduced magnitude vs Log R ( R=heliocentric distance). A total of over 16 new parameters, are measured from both plots, and give an unprecedented amount…
How To Use Magnetic Field Information For Coronal Loop Identification
Solanki, S. K.; Inhester, B.; Lagg, A. +1 more
The structure of the solar corona is dominated by the magnetic field because the magnetic pressure is about four orders of magnitude higher than the plasma pressure. Due to the high conductivity the emitting coronal plasma (visible, e.g., in SOHO/EIT) outlines the magnetic field lines. The gradient of the emitting plasma structures is significantl…