https://tel.archives-ouvertes.fr/file/index/docid/1058049/filename/HOU_XIAN_2013.pdf
... This is a milestone in my life, even though there is still definitely a long way to go in the ultimate pursuit of science. I owe my deep acknowledgements to all who have made me who I am today. First of all, I’m extremely grateful to David Smith, my thesis supervisor, for having accepted me to be a ...
... This is a milestone in my life, even though there is still definitely a long way to go in the ultimate pursuit of science. I owe my deep acknowledgements to all who have made me who I am today. First of all, I’m extremely grateful to David Smith, my thesis supervisor, for having accepted me to be a ...
A Multi-wavelength study on gamma
... Distributions of tj and Δα for the XRT data and the optical data. . . . . 89 Comparisons of the distributions of EK,iso and p . . . . . . . . . . . . . . . . . . . 99 Comparison of the EK distribution . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 100 The EK,iso as a function of θj for bo ...
... Distributions of tj and Δα for the XRT data and the optical data. . . . . 89 Comparisons of the distributions of EK,iso and p . . . . . . . . . . . . . . . . . . . 99 Comparison of the EK distribution . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 100 The EK,iso as a function of θj for bo ...
The XMM-Newton Bright Serendipitous Survey
... s−1 , Brandt & Hasinger 2005; Worsley et al. 2005 and references therein) fluxes. At the energies (∼0.5-10 keV) covered by the instruments on board these two telescopes, Active Galactic Nuclei (AGN) can be efficiently selected and studied even when affected by large levels of absorption (up to NH ∼1 ...
... s−1 , Brandt & Hasinger 2005; Worsley et al. 2005 and references therein) fluxes. At the energies (∼0.5-10 keV) covered by the instruments on board these two telescopes, Active Galactic Nuclei (AGN) can be efficiently selected and studied even when affected by large levels of absorption (up to NH ∼1 ...
Discovery and Study of Exotic Radio Pulsars Jason William Thomas
... This draft paper presents searches for pulsars in 22 globular clusters with the Arecibo telescope. It is the deepest search of these clusters ever conducted. Our survey employed a higher observing frequency and higher resolution datarecording than the only previous major survey of these clusters wit ...
... This draft paper presents searches for pulsars in 22 globular clusters with the Arecibo telescope. It is the deepest search of these clusters ever conducted. Our survey employed a higher observing frequency and higher resolution datarecording than the only previous major survey of these clusters wit ...
Some Constraints on the Effects of Age and Metallicity - UvA-DARE
... consider only the X-ray sources that lie within the WFPC2 field of view. Thirty-six of the LMXB candidates in NGC 3115 and 44 in NGC 4365 meet this criterion (we eliminated the source corresponding to the nucleus of each galaxy, which may be associated with their central black holes). Nine of these ...
... consider only the X-ray sources that lie within the WFPC2 field of view. Thirty-six of the LMXB candidates in NGC 3115 and 44 in NGC 4365 meet this criterion (we eliminated the source corresponding to the nucleus of each galaxy, which may be associated with their central black holes). Nine of these ...
The Emission Line Spectrum of Active Galactic
... much smaller than L3 , where L is the typical size of the emitting region deduced from the variability time-scale and the ionization parameter. However, these requirements can also be fulfilled if the lines are emitted by a continuous medium whose thickness is much smaller than its lateral dimension ...
... much smaller than L3 , where L is the typical size of the emitting region deduced from the variability time-scale and the ionization parameter. However, these requirements can also be fulfilled if the lines are emitted by a continuous medium whose thickness is much smaller than its lateral dimension ...
Massive Disruptions in the Cool Core of MACS J1931.8-2634 Steven Ehlert
... Can AGN feedback supply enough energy to counteract the large radiative losses? ...
... Can AGN feedback supply enough energy to counteract the large radiative losses? ...
The redMaPPer Galaxy Cluster Catalog From DES Science
... object catalogs from the single-epoch and coadded images (Bertin & Arnouts 1996; Bertin 2011). After the initial production of these early data products, we detected several issues that were mitigated in post-processing, leading to the creation of the “SVA1 Gold” photometry catalog3 . First, we mask ...
... object catalogs from the single-epoch and coadded images (Bertin & Arnouts 1996; Bertin 2011). After the initial production of these early data products, we detected several issues that were mitigated in post-processing, leading to the creation of the “SVA1 Gold” photometry catalog3 . First, we mask ...
paper - Harvard-Smithsonian Center for Astrophysics
... allow us to estimate the systemic velocity of the star. The SiS spectrum shows the distinctive triple peak morphology as described by Ziurys et al. (2007) and Tenenbaum et al. (2010) that is interpreted as the signature of a slowly expanding shell and a pair of faster outflows nearly collimated with ...
... allow us to estimate the systemic velocity of the star. The SiS spectrum shows the distinctive triple peak morphology as described by Ziurys et al. (2007) and Tenenbaum et al. (2010) that is interpreted as the signature of a slowly expanding shell and a pair of faster outflows nearly collimated with ...
the Ëg infrared search for extraterrestrial civilizations with large
... As an essential step in our waste heat search, we have produced a clean catalog of the reddest sources resolved by WISE. The purpose of our focus, in this work, on resolved sources is twofold: resolved sources present their own challenges of interpretation and photometry, necessitating this separate ...
... As an essential step in our waste heat search, we have produced a clean catalog of the reddest sources resolved by WISE. The purpose of our focus, in this work, on resolved sources is twofold: resolved sources present their own challenges of interpretation and photometry, necessitating this separate ...
Fraction of the X-ray selected AGNs with optical emission lines in
... X-ray selected AGN sample, with well-defined flux limits and a reliable estimate of spectroscopic completeness. In this paper we will take the AGN sample obtained from the medium-depth (∼ 60 ks) XM M − COSM OS survey. Brusa et al. (2010) matched a multi-wavelength counterpart to 1,797/1,848 sources2 ...
... X-ray selected AGN sample, with well-defined flux limits and a reliable estimate of spectroscopic completeness. In this paper we will take the AGN sample obtained from the medium-depth (∼ 60 ks) XM M − COSM OS survey. Brusa et al. (2010) matched a multi-wavelength counterpart to 1,797/1,848 sources2 ...
R - Institut d`Astrophysique de Paris
... RGW+GRB = 6 10-3 RGW (8 sr + “standard values” of fg, qj) What will be the observed rate RGW in O2, O3? ...
... RGW+GRB = 6 10-3 RGW (8 sr + “standard values” of fg, qj) What will be the observed rate RGW in O2, O3? ...
Double relics in Abell 2345 and Abell 1240
... of Abell 2345 at 6 resolution is shown overlaid onto the optical emission (taken from the Digitalized Palomar Sky Survey II, red band). Two central radio-tail sources are associated with optical galaxies in the cluster center. The central cD is visible in the optical image. Relics are not visible ...
... of Abell 2345 at 6 resolution is shown overlaid onto the optical emission (taken from the Digitalized Palomar Sky Survey II, red band). Two central radio-tail sources are associated with optical galaxies in the cluster center. The central cD is visible in the optical image. Relics are not visible ...
Observation of the Crab pulsar wind nebula and microquasar Ph.D. Dissertation
... capable to increase the total number of known VHE emitting sources from a few to almost one hundred in just seven years of operation. This population comprises galactic and extragalactic objects. IACTs have proved to be very effective in both the discovery of new emitters, as well as in the fine ana ...
... capable to increase the total number of known VHE emitting sources from a few to almost one hundred in just seven years of operation. This population comprises galactic and extragalactic objects. IACTs have proved to be very effective in both the discovery of new emitters, as well as in the fine ana ...
Full text - UvA/FNWI - University of Amsterdam
... Quasi periodic oscillations (QPOs) between 300 and 1200 Hz in the X-ray emission from low mass X-ray binaries have been linked to Keplerian orbital motion at the inner edge of accretion disks. Lense-Thirring precession is precession of the line of nodes of inclined orbits with respect to the equator ...
... Quasi periodic oscillations (QPOs) between 300 and 1200 Hz in the X-ray emission from low mass X-ray binaries have been linked to Keplerian orbital motion at the inner edge of accretion disks. Lense-Thirring precession is precession of the line of nodes of inclined orbits with respect to the equator ...
Infrared identification of high-mass X
... us to update and discuss the Galactic HMXB population statistics. Methods. After previous photometric and spectroscopic observing campaigns in the optical and near-infrared, new photometry and spectroscopy was performed in the near-infrared with the SofI instrument on the ESO/NTT telescope in 2008 a ...
... us to update and discuss the Galactic HMXB population statistics. Methods. After previous photometric and spectroscopic observing campaigns in the optical and near-infrared, new photometry and spectroscopy was performed in the near-infrared with the SofI instrument on the ESO/NTT telescope in 2008 a ...
X-ray binaries in the Milky Way and other galaxies
... 6.1. Universal HMXB Luminosity Function ? . . . . . . . . . . . . . . . . . . . 6.2. High Luminosity cut-off . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.3. Total X-ray luminosity as SFR indicator . . . . . . . . . . . . . . . . . . . 6.4. Theoretical LX –SFR relation . . . . . . . . . ...
... 6.1. Universal HMXB Luminosity Function ? . . . . . . . . . . . . . . . . . . . 6.2. High Luminosity cut-off . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.3. Total X-ray luminosity as SFR indicator . . . . . . . . . . . . . . . . . . . 6.4. Theoretical LX –SFR relation . . . . . . . . . ...
THE COBE DIRBE POINT SOURCE CATALOG
... Table 1, this association is based solely on a positional offset of 10 . It is possible that in some cases the IRAS and 2MASS sources are two different objects; with the DIRBE data alone, it is impossible to discriminate between them. Also note that an IRAS counterpart to a 2MASS source is only inc ...
... Table 1, this association is based solely on a positional offset of 10 . It is possible that in some cases the IRAS and 2MASS sources are two different objects; with the DIRBE data alone, it is impossible to discriminate between them. Also note that an IRAS counterpart to a 2MASS source is only inc ...
the redshift evolution of the mean temperature
... profile at 0.04 R500 (Vikhlinin et al. 2007), making up the cool core (CC) subsample and the 50% least cuspy clusters defining the non-cool core (NCC) subsample. This yields the six subsamples summarized in Table 1. The choice of z = 0.6 as a dividing line was motivated by the desire to have an equa ...
... profile at 0.04 R500 (Vikhlinin et al. 2007), making up the cool core (CC) subsample and the 50% least cuspy clusters defining the non-cool core (NCC) subsample. This yields the six subsamples summarized in Table 1. The choice of z = 0.6 as a dividing line was motivated by the desire to have an equa ...
on the evolution of anomalous x-ray pulsars and soft gamma
... We show that the period clustering of anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs), their X-ray luminosities, ages, and statistics can be explained with fall back disks with large initial specific angular momentum. The disk evolution models are developed by comparison to self-s ...
... We show that the period clustering of anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs), their X-ray luminosities, ages, and statistics can be explained with fall back disks with large initial specific angular momentum. The disk evolution models are developed by comparison to self-s ...
SKA and VLBI synergies
... VLBI observations have remarkably strong impact in the Stellar physics studies. We can mention the study of Gamma Ray Bursts (GRBs), Radio Supernovae (RSNe) and Supernova Remnants (SNRs), Microquasars or Pulsars, among others. Moreover, VLBI astrometry is a unique tool providing stellar parallax mea ...
... VLBI observations have remarkably strong impact in the Stellar physics studies. We can mention the study of Gamma Ray Bursts (GRBs), Radio Supernovae (RSNe) and Supernova Remnants (SNRs), Microquasars or Pulsars, among others. Moreover, VLBI astrometry is a unique tool providing stellar parallax mea ...
Accreting millisecond X-ray pulsars, from accretion disk to magnetic
... Radio pulsars comprise the vast majority of known neutron stars: the present population exceeds ∼ 1700 objects and realistic estimates predict a galactic population of ∼ 105 active radio pulsars. The basic observational property of radio pulsars is their emission of broadband radio noise in the form ...
... Radio pulsars comprise the vast majority of known neutron stars: the present population exceeds ∼ 1700 objects and realistic estimates predict a galactic population of ∼ 105 active radio pulsars. The basic observational property of radio pulsars is their emission of broadband radio noise in the form ...
AVS03ML - Brigham Young University
... followed by slow oxidation. XPS shows no carbon peak. Concern: silicon doesn’t appear to oxidize, but mirror coatings such as U and Ni do. ...
... followed by slow oxidation. XPS shows no carbon peak. Concern: silicon doesn’t appear to oxidize, but mirror coatings such as U and Ni do. ...
Flare Observations
... by several orders of magnitude. At about the same time, S.E. Forbush noticed ground-level cosmic ray enhancements associated with major solar flares. These discoveries could only mean that the flare phenomena is not confined to thermal plasma, but includes high-energy particles and involves the coro ...
... by several orders of magnitude. At about the same time, S.E. Forbush noticed ground-level cosmic ray enhancements associated with major solar flares. These discoveries could only mean that the flare phenomena is not confined to thermal plasma, but includes high-energy particles and involves the coro ...
Particle kinematics in solar flares: observations - ETH E
... This thesis is devoted to the study of particle acceleration and propagation processes in solar flares. Solar flares are amongst the most powerful and energetic activity phenomena our Sun exhibits. They release energy of the order of 1032 erg in seconds to minutes. In the process, electrons and prot ...
... This thesis is devoted to the study of particle acceleration and propagation processes in solar flares. Solar flares are amongst the most powerful and energetic activity phenomena our Sun exhibits. They release energy of the order of 1032 erg in seconds to minutes. In the process, electrons and prot ...
History of X-ray astronomy
The history of X-ray astronomy begins in the 1920s, with interest in short wave communications for the U.S. Navy. This was soon followed by extensive study of the earth's ionosphere. By 1927, interest in the detection of X-ray and ultraviolet (UV) radiation at high altitudes inspired researchers to launch Goddard's rockets into the upper atmosphere to support theoretical studies and data gathering. The first successful rocket flight equipped with instrumentation able to detect solar ultraviolet radiation occurred in 1946. X-ray solar studies began in 1949. By 1973 a solar instrument package orbited on Skylab providing significant solar data.In 1965 the Goddard Space Flight Center program in X-ray astronomy was initiated with a series of balloon-borne experiments. In the 1970s this was followed by high altitude sounding rocket experiments, and that was followed by orbiting (satellite) observatories.The first rocket flight to successfully detect a cosmic source of X-ray emission was launched in 1962 by a group at American Science and Engineering (AS&E).X-ray wavelengths reveal information about the bodies (sources) that emit them.