Point Spread Function of real Wolter-I X-ray mirrors
... spatial wavelengths, whilst short spatial wavelengths are identified as microroughness. The former contribution is in general treated by means of geometrical optics, while the contribution of the latter – strongly dependent on the X-ray energy – is usually derived from the first order scattering theor ...
... spatial wavelengths, whilst short spatial wavelengths are identified as microroughness. The former contribution is in general treated by means of geometrical optics, while the contribution of the latter – strongly dependent on the X-ray energy – is usually derived from the first order scattering theor ...
Active Galactic Nuclei
... AGN + control sample: major merger do not trigger AGN at z~2 (but minor merger?) Difference between dry and wet (= gas-rich) merger? eLISA/NGO will tell us what the real AGN merger rate is QuickTime™ and a decompressor are needed to see this picture. ...
... AGN + control sample: major merger do not trigger AGN at z~2 (but minor merger?) Difference between dry and wet (= gas-rich) merger? eLISA/NGO will tell us what the real AGN merger rate is QuickTime™ and a decompressor are needed to see this picture. ...
Two extremely luminous WN stars in the Galactic center with
... 2001; Simpson et al. 2007) surveys of the GC reveal a complex structure of the ionized gas with many small-scale compact sources of thermal emission. In this paper we investigate the emission from such nebulae around our program stars. ...
... 2001; Simpson et al. 2007) surveys of the GC reveal a complex structure of the ionized gas with many small-scale compact sources of thermal emission. In this paper we investigate the emission from such nebulae around our program stars. ...
Annual Report 2014 - Max Planck Institute for Astrophysics
... 2.3 An observational and theoretical view of the atomic gas distribution in galaxies . . . . . 2.4 New analytical model for turbulence pressure in galaxy clusters . . . . . . . . . . . . . . 2.5 Resolving the radio sky . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.6 Stell ...
... 2.3 An observational and theoretical view of the atomic gas distribution in galaxies . . . . . 2.4 New analytical model for turbulence pressure in galaxy clusters . . . . . . . . . . . . . . 2.5 Resolving the radio sky . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.6 Stell ...
The mass, temperature and distance of the white dwarf in V 471 Tauri
... Survey X-ray and EUV observations. Consequently, Barstow et al. (1992) were able to confirm that the X-ray and optical light variations were indeed out of phase and the rotation/accretion model was the correct one. Most recently, this interpretation has been supported by detailed studies using a com ...
... Survey X-ray and EUV observations. Consequently, Barstow et al. (1992) were able to confirm that the X-ray and optical light variations were indeed out of phase and the rotation/accretion model was the correct one. Most recently, this interpretation has been supported by detailed studies using a com ...
Galaxies - gilbertmath.com
... with more dust than others tend to produce more __________. This is because stars form from ________ and __________ present in nebulae. Some ancient galaxies have almost no dust because it has all been used up in making __________. It is thought that each galaxy contains, at its centre, a ____ ...
... with more dust than others tend to produce more __________. This is because stars form from ________ and __________ present in nebulae. Some ancient galaxies have almost no dust because it has all been used up in making __________. It is thought that each galaxy contains, at its centre, a ____ ...
X-ray narrow emission lines from the nuclear region of NGC 1365
... 2007, 2009a) covering its X-ray emission (intrinsic L2–10 keV ∼ 1042 erg s−1 Risaliti et al. 2005b). Notably, especially for this work, there is a nuclear starburst with a diameter of 1000 , which is resolved in optical wavelengths into multiple compact star clusters (using the HST Faint Object Came ...
... 2007, 2009a) covering its X-ray emission (intrinsic L2–10 keV ∼ 1042 erg s−1 Risaliti et al. 2005b). Notably, especially for this work, there is a nuclear starburst with a diameter of 1000 , which is resolved in optical wavelengths into multiple compact star clusters (using the HST Faint Object Came ...
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... Results. In contrast to historical expectations for sgB[e] stars, S18 is both photometrically and spectroscopically highly variable. The lightcurve is characterised by rapid aperiodic ‘flaring’ throughout the 16 years of observations. Changes in the high excitation emission line component of the spe ...
... Results. In contrast to historical expectations for sgB[e] stars, S18 is both photometrically and spectroscopically highly variable. The lightcurve is characterised by rapid aperiodic ‘flaring’ throughout the 16 years of observations. Changes in the high excitation emission line component of the spe ...
SOME CONSTRAINTS ON GALAXY EVOLUTION IMPOSED BY
... frequency < S > = 9.3 in nine cD/E galaxies is higher than that in 34 E + S0 galaxies for which < S > = 5.1. Furthermore, the specific frequency < S > = 0.8 in eight late-type spirals (Sb - Scd) is significantly lower than the value < S > = 1.9 in three bulge-dominated Sa and Sab galaxies. In summar ...
... frequency < S > = 9.3 in nine cD/E galaxies is higher than that in 34 E + S0 galaxies for which < S > = 5.1. Furthermore, the specific frequency < S > = 0.8 in eight late-type spirals (Sb - Scd) is significantly lower than the value < S > = 1.9 in three bulge-dominated Sa and Sab galaxies. In summar ...
Wolfgang Voges
... visualisation of multi-wavelength cluster data deprojection algorithms to allow study of morphology in survey data conversion of simulation data to the space of observable parameters 3D-interface for visualisation (to schools) Wolfgang Voges ...
... visualisation of multi-wavelength cluster data deprojection algorithms to allow study of morphology in survey data conversion of simulation data to the space of observable parameters 3D-interface for visualisation (to schools) Wolfgang Voges ...
GoldCreation
... One of my favorite astronomy-themed t-shirts says “You are star dust”. It makes the point that we are all made from long dead stars. Of course, everything around us is also made of star stuff. This even includes rare elements such as gold. This paper discusses the processes of gold formation. Most m ...
... One of my favorite astronomy-themed t-shirts says “You are star dust”. It makes the point that we are all made from long dead stars. Of course, everything around us is also made of star stuff. This even includes rare elements such as gold. This paper discusses the processes of gold formation. Most m ...
Transparencies - Rencontres de Moriond
... Dark stellar cluster (BD, neutron star, stellar BH ) : would impose a central density = 1017-19 M pc-3 lifetime < 105 years rejected Ball of fermions (neutrinos, gravitinos, axinos, …) finite size of 7000 ...
... Dark stellar cluster (BD, neutron star, stellar BH ) : would impose a central density = 1017-19 M pc-3 lifetime < 105 years rejected Ball of fermions (neutrinos, gravitinos, axinos, …) finite size of 7000 ...
Matter under extreme conditions experiments at the Linac
... LCLS x-ray beam, with high-power lasers consisting of two nanosecond Nd:glass laser beams and one short-pulse Ti:sapphire laser. These lasers produce short-lived states of matter with high pressures, high temperatures or high densities with properties that are important for applications in nuclear f ...
... LCLS x-ray beam, with high-power lasers consisting of two nanosecond Nd:glass laser beams and one short-pulse Ti:sapphire laser. These lasers produce short-lived states of matter with high pressures, high temperatures or high densities with properties that are important for applications in nuclear f ...
The Nuclear Equation of State and Neutron Star Masses
... At the same time, ongoing laboratory measurements of nuclear properties and theoretical studies of pure neutron matter are limiting the properties of neutron star matter near the saturation density (usually expressed as baryon density, ns 0.16 baryons fm−3 ; mass density, ρs 2.7 × 1014 g cm−3 ; ...
... At the same time, ongoing laboratory measurements of nuclear properties and theoretical studies of pure neutron matter are limiting the properties of neutron star matter near the saturation density (usually expressed as baryon density, ns 0.16 baryons fm−3 ; mass density, ρs 2.7 × 1014 g cm−3 ; ...
The impact of surface temperature inhomogeneities on quiescent
... spectral fitting method. Previous works have checked the effects of variations between hydrogen atmosphere models (Heinke et al. 2006; Haakonsen et al. 2012), distance errors (Heinke et al. 2006; Guillot et al. 2011, 2013; Heinke et al. 2014; Bogdanov et al. 2016), detector systematics (Heinke et al ...
... spectral fitting method. Previous works have checked the effects of variations between hydrogen atmosphere models (Heinke et al. 2006; Haakonsen et al. 2012), distance errors (Heinke et al. 2006; Guillot et al. 2011, 2013; Heinke et al. 2014; Bogdanov et al. 2016), detector systematics (Heinke et al ...
11.3 MB PDF file
... astronomers at the Kitt Peak 4 m and the Canada-FranceHawaii 3.5 m telescopes were immediately successful in detecting P/Halley. At ESO, the first (unsuccessful) attempts were already made in 1980, with the ESO 3.6 m telescope on .Photographic plates and with the Oanish 1.5 m telescope by ,means of ...
... astronomers at the Kitt Peak 4 m and the Canada-FranceHawaii 3.5 m telescopes were immediately successful in detecting P/Halley. At ESO, the first (unsuccessful) attempts were already made in 1980, with the ESO 3.6 m telescope on .Photographic plates and with the Oanish 1.5 m telescope by ,means of ...
astro-ph/9505110 PDF
... same time, C/N also appears to increase with O/H in the irregular galaxies, but the trend appears to be broken between the irregulars and the solar neighborhood. This seems to indicate that most of the nitrogen production in our Galaxy is decoupled from that of carbon and oxygen. One possible interp ...
... same time, C/N also appears to increase with O/H in the irregular galaxies, but the trend appears to be broken between the irregulars and the solar neighborhood. This seems to indicate that most of the nitrogen production in our Galaxy is decoupled from that of carbon and oxygen. One possible interp ...
Massive Stars in the Arches Cluster 12
... high resolution mode, covering K-band wavelengths (1.98 µm to 2.28 µm). The long slit (2400 ) was positioned in a north-south orientation on the sky, and a slit scan covering a 2400 ×1400 rectangular region was made by offsetting the telescope by a fraction of a slit width to the west between succes ...
... high resolution mode, covering K-band wavelengths (1.98 µm to 2.28 µm). The long slit (2400 ) was positioned in a north-south orientation on the sky, and a slit scan covering a 2400 ×1400 rectangular region was made by offsetting the telescope by a fraction of a slit width to the west between succes ...
Hint of a transiting extended atmosphere on 55 Cancri b⋆
... complemented by contemporaneous measurements of the stellar X-ray flux. In fact, planet “e” has been detected in transit, suggesting the system is seen nearly edge-on. Yet, planet “b” has not been observed in transit so far. Here, we report on Hubble Space Telescope STIS Lyα and Chandra ACIS-S X-ray ...
... complemented by contemporaneous measurements of the stellar X-ray flux. In fact, planet “e” has been detected in transit, suggesting the system is seen nearly edge-on. Yet, planet “b” has not been observed in transit so far. Here, we report on Hubble Space Telescope STIS Lyα and Chandra ACIS-S X-ray ...
Preliminary results of the Be stars proportion in LMC open
... To properly compare the SMC study with the LMC, it is needed to constrain the freedom degrees and therefore to use the same age distribution (see Fig. 3), leading to the metallicity being the only variable parameter. The LMC sample is formed by 90 open clusters distributed along the LMC. A total of ...
... To properly compare the SMC study with the LMC, it is needed to constrain the freedom degrees and therefore to use the same age distribution (see Fig. 3), leading to the metallicity being the only variable parameter. The LMC sample is formed by 90 open clusters distributed along the LMC. A total of ...
1. INTRODUCTION 2. MASS AND LIGHT
... Although to date no stars have been detected in the Magellanic Stream, it could in principle have a stellar component which would likewise be extended. The debris could also be from an unrelated galaxy which, like the Sagittarius dwarf (D5¡ ] 20¡), might be substantially extended along its orbit. Su ...
... Although to date no stars have been detected in the Magellanic Stream, it could in principle have a stellar component which would likewise be extended. The debris could also be from an unrelated galaxy which, like the Sagittarius dwarf (D5¡ ] 20¡), might be substantially extended along its orbit. Su ...
A massive hypergiant star as the progenitor of the supernova SN
... substantially deeper than those obtained in 1997, show no trace of SN 2005gl, nor of NGC266_LBV 1, to a deep limit: V . 25.6 mag at the 3s confidence level (V . 25.9 mag at the 2s level; Supplementary Information section 2). These new data attend to both caveats noted above, and show that NGC266_LBV ...
... substantially deeper than those obtained in 1997, show no trace of SN 2005gl, nor of NGC266_LBV 1, to a deep limit: V . 25.6 mag at the 3s confidence level (V . 25.9 mag at the 2s level; Supplementary Information section 2). These new data attend to both caveats noted above, and show that NGC266_LBV ...
H.E.S.S. observations of the binary system PSR B1259
... currently in preparation. Observations of the binary system PSR B1259-63/LS 2883 at HEs were performed using the Large Area Telescope (LAT) on board of Fermi. The data taken around the periastron passage were analysed by two independent working groups (Abdo et al. 2011; Tam et al. 2011), yielding si ...
... currently in preparation. Observations of the binary system PSR B1259-63/LS 2883 at HEs were performed using the Large Area Telescope (LAT) on board of Fermi. The data taken around the periastron passage were analysed by two independent working groups (Abdo et al. 2011; Tam et al. 2011), yielding si ...
Chapter: The Evolution of Binary Systems
... One particularly important concept in studying the evolution of binary systems is the Roche lobe. Considering the so-called restricted three-body problem, where one follows the motion of a mass-less test particle in the gravitational field of two orbiting masses M1 and M2 , one can define an effecti ...
... One particularly important concept in studying the evolution of binary systems is the Roche lobe. Considering the so-called restricted three-body problem, where one follows the motion of a mass-less test particle in the gravitational field of two orbiting masses M1 and M2 , one can define an effecti ...
Symbiotic Stars as Laboratories for the Study of
... to occur every few years to decades. In some symbiotics, material that is transferred from the red giant to the WD forms a disk around the WD. Thus, symbiotic stars are a bit like overgrown cataclysmic variables (CVs), but with less violent eruptions. Symbiotic stars are not as well understood as CV ...
... to occur every few years to decades. In some symbiotics, material that is transferred from the red giant to the WD forms a disk around the WD. Thus, symbiotic stars are a bit like overgrown cataclysmic variables (CVs), but with less violent eruptions. Symbiotic stars are not as well understood as CV ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.