![A STRONGLY MAGNETIZED PULSAR WITHIN THE GRASP OF THE MILKY... SUPERMASSIVE BLACK HOLE Rea ,](http://s1.studyres.com/store/data/008087478_1-0f58814ff52985868cb62da3d897edc0-300x300.png)
A STRONGLY MAGNETIZED PULSAR WITHIN THE GRASP OF THE MILKY... SUPERMASSIVE BLACK HOLE Rea ,
... Because of the complex shape and variability of the three peaked pulse profile (Figure 2), we decided not to use a pulse template for the timing analysis (which might artificially affect the phase shift), instead using two parallel methods: fitting a sinusoid to the profile at the fundamental period ...
... Because of the complex shape and variability of the three peaked pulse profile (Figure 2), we decided not to use a pulse template for the timing analysis (which might artificially affect the phase shift), instead using two parallel methods: fitting a sinusoid to the profile at the fundamental period ...
A re-examination of galactic conformity and a comparison with semi
... of the effect and how it changes as a function of the mass of the central galaxy. Conformity extends over a central galaxy stellar mass range spanning two orders of magnitude. The scale dependence and the precise nature of the effect depend on the mass of the central. In central galaxies with masses ...
... of the effect and how it changes as a function of the mass of the central galaxy. Conformity extends over a central galaxy stellar mass range spanning two orders of magnitude. The scale dependence and the precise nature of the effect depend on the mass of the central. In central galaxies with masses ...
The (galaxy-wide) IMF in giant elliptical galaxies: from top to bottom
... detection limit. For the three spiral galaxies in the sample, the MW, M31 and M81, ∼5–10 per cent of GCs have LMXBs. Taking into account the uncertainties of the stellar mass determination, these numbers compare well with the hypothesis that all these galaxies have similar IMFs. Additionally, very l ...
... detection limit. For the three spiral galaxies in the sample, the MW, M31 and M81, ∼5–10 per cent of GCs have LMXBs. Taking into account the uncertainties of the stellar mass determination, these numbers compare well with the hypothesis that all these galaxies have similar IMFs. Additionally, very l ...
the optical colors of giant elliptical galaxies and their metal
... The shape of the stellar initial mass function (IMF) is a fundamental property for studies of star and galaxy formation. It constitutes a crucial assumption when deriving physical parameters from observations. However, its origin remains relatively poorly understood. A particularly important questio ...
... The shape of the stellar initial mass function (IMF) is a fundamental property for studies of star and galaxy formation. It constitutes a crucial assumption when deriving physical parameters from observations. However, its origin remains relatively poorly understood. A particularly important questio ...
WSokolov-PROTVINO
... Gamma-ray bursts and their afterglows also allow us seeing the most distant explosions of massive stars at the end of their evolution. This is confirmed by observations of the "long" bursts, but, most probably, the "short" GRBs are also related to some very old compact objects formed in the course o ...
... Gamma-ray bursts and their afterglows also allow us seeing the most distant explosions of massive stars at the end of their evolution. This is confirmed by observations of the "long" bursts, but, most probably, the "short" GRBs are also related to some very old compact objects formed in the course o ...
A PCA approach to stellar effective temperatures⋆
... high-quality spectroscopic temperatures in the Elodie library, we define a temperature scale for FG-type disk dwarfs with an internal consistency of about 50 K, in excellent agreement with temperatures from direct determinations and widely used scales based on the infrared flux method. Key words. st ...
... high-quality spectroscopic temperatures in the Elodie library, we define a temperature scale for FG-type disk dwarfs with an internal consistency of about 50 K, in excellent agreement with temperatures from direct determinations and widely used scales based on the infrared flux method. Key words. st ...
The environment of high-redshift AGN OLIMPIA JUDIT FOGASY
... In order to understand the formation and evolution of local massive galaxies and to reveal the processes that engineered the tight correlations found between their supermassive black hole (SMBH) mass and bulge mass or velocity dispersion, the study of powerful, high-redshift active galactic nuclei ( ...
... In order to understand the formation and evolution of local massive galaxies and to reveal the processes that engineered the tight correlations found between their supermassive black hole (SMBH) mass and bulge mass or velocity dispersion, the study of powerful, high-redshift active galactic nuclei ( ...
CONSTELLATION PERSEUS The constellation
... Located 92.8 light-years from Earth, it varies in apparent magnitude from a minimum of 3.5 to a maximum of 2.3 over a period of 2.867 days. The star system is the prototype of a group of eclipsing binary stars named Algol variables. • Alpha Persei known as Mirfak (Arabic for elbow) is the brightest ...
... Located 92.8 light-years from Earth, it varies in apparent magnitude from a minimum of 3.5 to a maximum of 2.3 over a period of 2.867 days. The star system is the prototype of a group of eclipsing binary stars named Algol variables. • Alpha Persei known as Mirfak (Arabic for elbow) is the brightest ...
EBL - UCSC Physics - University of California, Santa Cruz
... Figure 4. The predicted z = 0 EBL spectrum from our fiducial WMAP5 model (solid black) and WMAP5+fixed (dash–dotted violet) dust parameters, and C!CDM (dotted black) models, compared with experimental constraints at a number of wavelengths. D11 is shown for comparison in dashed–dotted red with the s ...
... Figure 4. The predicted z = 0 EBL spectrum from our fiducial WMAP5 model (solid black) and WMAP5+fixed (dash–dotted violet) dust parameters, and C!CDM (dotted black) models, compared with experimental constraints at a number of wavelengths. D11 is shown for comparison in dashed–dotted red with the s ...
PDF file
... 4) Slow vs. rapid disk evolution. Early studies of nearinfrared dust emission from low-mass young stars suggested that most stars lose their optically thick disks over periods of ∼ 10 Myr, (e.g., Strom et al., 1993), similar to the timescale suggested for planet formation (Podosek and Cassen, 1994). ...
... 4) Slow vs. rapid disk evolution. Early studies of nearinfrared dust emission from low-mass young stars suggested that most stars lose their optically thick disks over periods of ∼ 10 Myr, (e.g., Strom et al., 1993), similar to the timescale suggested for planet formation (Podosek and Cassen, 1994). ...
Draft paper (submitted to MNRAS)
... from sizeable uncertainties when data are affected by crowding (especially in fields near the centre of a dwarf), small spatial coverage (many dwarfs are larger than the field of view of HST), or limited depth (models do best when the faint main sequence turnoff of the oldest population is reached). ...
... from sizeable uncertainties when data are affected by crowding (especially in fields near the centre of a dwarf), small spatial coverage (many dwarfs are larger than the field of view of HST), or limited depth (models do best when the faint main sequence turnoff of the oldest population is reached). ...
Microlensing Events by Proxima Centauri in 2014 and 2016
... radii of nearby stars, coupled with their typically large proper motions, yield relatively large probabilities of such events occurring. Searches for upcoming close stellar passages of high-proper-motion stars near background sources have been carried out by Salim & Gould (2000) and Proft, Demleitne ...
... radii of nearby stars, coupled with their typically large proper motions, yield relatively large probabilities of such events occurring. Searches for upcoming close stellar passages of high-proper-motion stars near background sources have been carried out by Salim & Gould (2000) and Proft, Demleitne ...
The chemical composition of two supergiants in the dwarf
... histories and thus should show a variety of α/Fe ratios throughout their evolution, but they are too distant for detailed analysis of their red giant branch (=RGB, stars that can sample ages >1 Gyr). It is possible to observe and analyse the spectra of their bright, young massive stars though, since ...
... histories and thus should show a variety of α/Fe ratios throughout their evolution, but they are too distant for detailed analysis of their red giant branch (=RGB, stars that can sample ages >1 Gyr). It is possible to observe and analyse the spectra of their bright, young massive stars though, since ...
CNO and F abundances in the barium star HD 123396
... 2010). In this context, CNO elements, along with s-process elements, are key tracers of the nucleosynthesis in the previous AGB progenitor, so they provide crucial constraints on the formation mechanism. According to the mass-transfer hypothesis, the former AGB stars would now be optically invisible ...
... 2010). In this context, CNO elements, along with s-process elements, are key tracers of the nucleosynthesis in the previous AGB progenitor, so they provide crucial constraints on the formation mechanism. According to the mass-transfer hypothesis, the former AGB stars would now be optically invisible ...
Studying explosive phenomena in astrophysics by the example of
... GRB’s data – statistics of occurrence, spectrum, lightcurves. But there are still a lot of questions in the theory of GRBs. We know that a significant fraction of GRBs, the so called long-duration GRBs, are related to the death of stars and that they are connected with supernovae. So gammaray bursts ...
... GRB’s data – statistics of occurrence, spectrum, lightcurves. But there are still a lot of questions in the theory of GRBs. We know that a significant fraction of GRBs, the so called long-duration GRBs, are related to the death of stars and that they are connected with supernovae. So gammaray bursts ...
William Herschel`s Wonderful Decade, 1781-1790
... every fifteen years or so, and then it may be possible to see moons of Saturn that are normally lost in the glare of the ring. In the summer of 1787, Herschel examined the planet with his twenty-foot, but it was then in a region with many background stars, and although he suspected he had seen a six ...
... every fifteen years or so, and then it may be possible to see moons of Saturn that are normally lost in the glare of the ring. In the summer of 1787, Herschel examined the planet with his twenty-foot, but it was then in a region with many background stars, and although he suspected he had seen a six ...
Formation of Massive Stars
... • Physical parameters of compact regions of ionized gas are determined mostly from radio data • Radio continuum is modeled as free-free from an isothermal homogeneous region of ionized gas • Te and EM = Ú ne2 dl are determined from the optically thick and thin portions of the spectrum, respectively ...
... • Physical parameters of compact regions of ionized gas are determined mostly from radio data • Radio continuum is modeled as free-free from an isothermal homogeneous region of ionized gas • Te and EM = Ú ne2 dl are determined from the optically thick and thin portions of the spectrum, respectively ...
Carbon-enhanced metal-poor stars: the most pristine - HAL
... Context. Carbon-enhanced metal poor stars (CEMP) form a significant proportion of the metal-poor stars, their origin is not well understood, and this carbon-enhancement appears in stars that exhibit different abundance patterns. Aims. Three very metal-poor C-rich turnoff stars were selected from the ...
... Context. Carbon-enhanced metal poor stars (CEMP) form a significant proportion of the metal-poor stars, their origin is not well understood, and this carbon-enhancement appears in stars that exhibit different abundance patterns. Aims. Three very metal-poor C-rich turnoff stars were selected from the ...
Gaia 1 and 2. A pair of new satellites of the Galaxy
... information, we have to be particularly careful when selecting objects for the satellite search (we cannot use colourmagnitude masks based on stellar isochrones, as in i.e. Koposov et al. 2015). For the analysis in this paper we apply only two selection cuts. First cut concerns the Gaia G magnitude: ...
... information, we have to be particularly careful when selecting objects for the satellite search (we cannot use colourmagnitude masks based on stellar isochrones, as in i.e. Koposov et al. 2015). For the analysis in this paper we apply only two selection cuts. First cut concerns the Gaia G magnitude: ...
Galaxy morphology, luminosity, and environment in the SDSS DR7
... de Lapparent et al. 2003) or photometric profile (Bell et al. 2003; Driver et al. 2007a); some studies use artificial neural networks for morphological classification (Ball et al. 2006). The most accurate, but by far the most time consuming approach is to use visual classification (Marzke et al. 199 ...
... de Lapparent et al. 2003) or photometric profile (Bell et al. 2003; Driver et al. 2007a); some studies use artificial neural networks for morphological classification (Ball et al. 2006). The most accurate, but by far the most time consuming approach is to use visual classification (Marzke et al. 199 ...
Polaris B, an optical companion of the Polaris (αUMi) system
... are eye-witnesses of evolutional history of two stars with different masses in the same stellar system. (v) Absolute magnitude of +3.30 mag is equal to one from Fernie (1966). The spectroscopically determined effective temperature 6900 K combined with radius of 1.38 R gives the distance of nearly 1 ...
... are eye-witnesses of evolutional history of two stars with different masses in the same stellar system. (v) Absolute magnitude of +3.30 mag is equal to one from Fernie (1966). The spectroscopically determined effective temperature 6900 K combined with radius of 1.38 R gives the distance of nearly 1 ...
AN ULTRA-DEEP NEAR-INFRARED SPECTRUM OF
... Several recent studies have shown that about half of the massive galaxies at z ∼ 2 are in a quiescent phase. Moreover, these galaxies are commonly found to be ultra-compact with half-light radii of ∼ 1 kpc. We have obtained a ∼ 29 hr spectrum of a typical quiescent, ultra-dense galaxy at z = 2.1865 ...
... Several recent studies have shown that about half of the massive galaxies at z ∼ 2 are in a quiescent phase. Moreover, these galaxies are commonly found to be ultra-compact with half-light radii of ∼ 1 kpc. We have obtained a ∼ 29 hr spectrum of a typical quiescent, ultra-dense galaxy at z = 2.1865 ...
β Relation for Local Galaxies
... galaxies on the IRX show a considerable amount of scatter compared to the starburst IRX relation. Currently, no single relation for normal star-forming galaxies exists between βGLX the UV attenuation nor is there agreement as to the underlying physical reason that causes the spread. It is necessary ...
... galaxies on the IRX show a considerable amount of scatter compared to the starburst IRX relation. Currently, no single relation for normal star-forming galaxies exists between βGLX the UV attenuation nor is there agreement as to the underlying physical reason that causes the spread. It is necessary ...
Slide 1
... support for the presence of an IMBH - Mass range = 6000 - 92000 M • Sub-Eddington radiation-pressure dominated accretion disk with a high (~4x10-4 M yr-1) at the outburst peak. • ~1yr recurrence timescale in the outbursts seen in the X-rays could be interpreted as the result of modulated mass-transf ...
... support for the presence of an IMBH - Mass range = 6000 - 92000 M • Sub-Eddington radiation-pressure dominated accretion disk with a high (~4x10-4 M yr-1) at the outburst peak. • ~1yr recurrence timescale in the outbursts seen in the X-rays could be interpreted as the result of modulated mass-transf ...
Hypervelocity Stars and the Galactic Center
... velocities. An HVS ejected from the Milky Way travels on a nearly radial trajectory; the expected proper motion for a 50 kpc distant HVS is a few tenths of a milliarcsecond per year (Gnedin et al. 2005). Thus radial velocity directly measures most of an HVS’s space motion. Deciding whether an HVS is ...
... velocities. An HVS ejected from the Milky Way travels on a nearly radial trajectory; the expected proper motion for a 50 kpc distant HVS is a few tenths of a milliarcsecond per year (Gnedin et al. 2005). Thus radial velocity directly measures most of an HVS’s space motion. Deciding whether an HVS is ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.