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Probing the proper motion of the central compact object in Puppis-A with the Chandra high resolution camera
Hui, C. Y.; Becker, W.
By making use of the sub-arcsecond angular resolution of the High Resolution Camera (HRC-I) aboard the Chandra X-ray satellite we have examined the central compact object RX J0822-4300 in the supernova remnant Puppis-A for a possible proper motion. Using data which span an epoch of 1952 days we found the position of RX J0822-4300 different by 0.57…
Subaru optical observations of the two middle-aged pulsars PSR B0656+14 and Geminga
Kawai, N.; Zharikov, S. V.; Urata, Y. +6 more
Aims.We carried out a deep subarcsecond BRI imaging of the two middle-aged pulsars to establish their properties in the optical range. Methods.Astrometry and photometry methods are applied to identify the pulsars and to measure their fluxes. We also reanalyze archival ESO/NTT and HST broadband data and find that some published fluxes for Geminga w…
Galaxies under the cosmic microscope: resolved spectroscopy and new constraints on the z = 1 Tully-Fisher relation
Kneib, J. -P.; Smith, Graham P.; Smail, Ian +5 more
We exploit the gravitational potential of massive cluster lenses to probe the emission-line properties of six z = 1 galaxies which appear as highly magnified luminous arcs. Using the Gemini Multi-Object Spectrograph (GMOS) integral field spectrograph together with detailed cluster lens models, we reconstruct the intrinsic morphologies and two-dime…
Where are the sources of the near-infrared background?
Ferrara, Andrea; Salvaterra, Ruben
The observed near-infrared background excess over light from known galaxies is commonly ascribed to redshifted radiation from early, very massive, Population III (Pop III) stars. We show here that this interpretation must be discarded as it largely overpredicts the number of J-dropouts and Lyα emitters in ultradeep field searches. Independently of…
Observations of magnetic anomaly signatures in Mars Express ASPERA-3 ELS data
Coates, A. J.; Kallio, E.; Fedorov, A. +40 more
Mars Express (MEX) Analyser of Space Plasmas and Energetic Atoms (ASPERA-3) data is providing insights into atmospheric loss on Mars via the solar wind interaction. This process is influenced by both the interplanetary magnetic field (IMF) in the solar wind and by the magnetic 'anomaly' regions of the martian crust. We analyse observations from th…
IGR J17252-3616: an accreting pulsar observed by INTEGRAL and XMM-Newton
Walter, R.; Stephen, J. B.; De Cesare, G. +5 more
The discovery of the X-ray source
On the nitrogen abundance of fast, low-ionization emission regions: the outer knots of the planetary nebula NGC 7009
Corradi, R. L. M.; Gonçalves, D. R.; Ercolano, B. +2 more
We have constructed a 3D photoionization model of a planetary nebula (PN) similar in structure to NGC 7009 with its outer pair of knots (also known as FLIERs - fast, low-ionization emission regions). The work is motivated by the fact that the strong [NII]λ6583 line emission from FLIERs in many PNe has been attributed to a significant local overabu…
X-Ray Absorption and an X-Ray Jet in the Radio-loud Broad Absorption-line Quasar PG 1004+130
Brandt, W. N.; Garmire, G. P.; Gallagher, S. C. +4 more
We investigate the X-ray properties of PG 1004+130, a radio-loud broad absorption-line (BAL) quasar with a hybrid FR I/II radio morphology. This optically bright, low-redshift quasar was undetected by Einstein, marking it as anomalously X-ray weak relative to other radio-loud quasars. The 22.2 ks XMM-Newton and 41.6 ks Chandra observations present…
On the CME velocity distribution
Chen, P. F.; Fang, C.; Chen, A. Q.
Context: .Coronal mass ejections (CMEs) are often categorized into flare-associated and filament-associated types, which logically is incomplete since there are many CMEs of the intermediate type.
Aims: .With this new classification, this paper aims to reexamine whether flare-associated CMEs and filament eruption-associated CMEs have distinct…
The Transparency of Solar Coronal Active Regions
Schmelz, J. T.; Brickhouse, N. S.
Resonance scattering has often been invoked to explain the disagreement between the observed and predicted line ratios of Fe XVII λ15.01 to Fe XVII λ15.26 (the ``3C/3D'' ratio). In this process photons of λ15.01, with its much higher oscillator strength, are preferentially scattered out of the line of sight, thus reducing the observed line ratio. …