Extragalactic Globular Cluster Systems
... the old satellite galaxies, some of which host old globular clusters such as Fornax, whose morphology and stellar populations are determined by ongoing gravitational and hydrodynamical interactions with the Milky Way (e.g. Mayer et al. 2005). Recent papers have attempted to address the origin of the ...
... the old satellite galaxies, some of which host old globular clusters such as Fornax, whose morphology and stellar populations are determined by ongoing gravitational and hydrodynamical interactions with the Milky Way (e.g. Mayer et al. 2005). Recent papers have attempted to address the origin of the ...
Galactic Evolution - Harvard-Smithsonian Center for Astrophysics
... but if Pop-III stars really did exist, they must have contained hundreds of solar masses. No such colossal stars are seen today, the most massive star ever definitively “weighed” being ~76 M. (Repeated claims of discoveries for stars >100 M have in all cases been shown, under higher angular resolu ...
... but if Pop-III stars really did exist, they must have contained hundreds of solar masses. No such colossal stars are seen today, the most massive star ever definitively “weighed” being ~76 M. (Repeated claims of discoveries for stars >100 M have in all cases been shown, under higher angular resolu ...
R - Institut d`Astrophysique de Paris
... to the transient sky. SVOM is a mission deployed on the ground and in space. The space segment of SVOM is planned to be launched early in the next decade (2021), for a 3 year nominal mission. SVOM is currently in phase C (budget accepted for phase D, E1 (post-launch) ...
... to the transient sky. SVOM is a mission deployed on the ground and in space. The space segment of SVOM is planned to be launched early in the next decade (2021), for a 3 year nominal mission. SVOM is currently in phase C (budget accepted for phase D, E1 (post-launch) ...
X-ray spectra of highly magnetized neutron stars in binary systems
... having a mass of at least 1.4 M is already awesome in itself, more and more mysteries were revealed with time. If such a neutron star is forming a binary system with a stellar companion, it can accrete material from its companion (see Section 2.3). Due to the depth of the gravitational well of the ...
... having a mass of at least 1.4 M is already awesome in itself, more and more mysteries were revealed with time. If such a neutron star is forming a binary system with a stellar companion, it can accrete material from its companion (see Section 2.3). Due to the depth of the gravitational well of the ...
High-mass X-ray Binaries: X-raying the winds Ángel Giménez García
... & Astrophysics con la siguiente referencia: • An XMM-Newton view of FeKα in HMXBs, Giménez-García, A., Torrejón, J.M., Eikmann, W., et al. 2015, A&A, 576, A108 A continuación exponemos los puntos fundamentales de este estudio. ...
... & Astrophysics con la siguiente referencia: • An XMM-Newton view of FeKα in HMXBs, Giménez-García, A., Torrejón, J.M., Eikmann, W., et al. 2015, A&A, 576, A108 A continuación exponemos los puntos fundamentales de este estudio. ...
Core-Halo Age Gradients and Star Formation in the Orion Nebula
... within 1 pc from the centers to the halos of both clusters: from ∼ 0.1 Myr to ∼ 1.8 Myr in NGC 2024, and from ∼ 1.4 Myr to ∼ 2 Myr in the ONC. The large observed age spreads of individual stars about the median with the typical interquartile ranges ∼ 1 Myr and ∼ 2 Myr in NGC 2024 and ONC, respective ...
... within 1 pc from the centers to the halos of both clusters: from ∼ 0.1 Myr to ∼ 1.8 Myr in NGC 2024, and from ∼ 1.4 Myr to ∼ 2 Myr in the ONC. The large observed age spreads of individual stars about the median with the typical interquartile ranges ∼ 1 Myr and ∼ 2 Myr in NGC 2024 and ONC, respective ...
Annual Report 2012 - Max Planck Institute for Astrophysics
... PCs are not personalized, hardware failures are quickly repaired by a complete exchange of the computer. In addition to the desktop systems, which, in large part are younger than 5 years and which (in 2012) amount to more than 170 fully equipped working places, users have access to central number cr ...
... PCs are not personalized, hardware failures are quickly repaired by a complete exchange of the computer. In addition to the desktop systems, which, in large part are younger than 5 years and which (in 2012) amount to more than 170 fully equipped working places, users have access to central number cr ...
Student Worksheet
... WEBSITE: http://cse.ssl.berkeley.edu/segwayed/lessons/classifying_galaxies/student1.htm Your answers to questions below will come from the online lesson: Classifying Galaxies. Start with the "Student Lesson" and the blinking message : "Start Galaxy exploration here" What is a galaxy? 1)_____________ ...
... WEBSITE: http://cse.ssl.berkeley.edu/segwayed/lessons/classifying_galaxies/student1.htm Your answers to questions below will come from the online lesson: Classifying Galaxies. Start with the "Student Lesson" and the blinking message : "Start Galaxy exploration here" What is a galaxy? 1)_____________ ...
The Milky Way and Andromeda galaxies in a constrained
... predict the formation of a galaxy with different gas fractions, morphologies, stellar masses and angular momentum content. Aquila clearly demonstrated that the primary uncertainty in these types of simulations is related to the processes of the unresolved baryonic physics that result in star formatio ...
... predict the formation of a galaxy with different gas fractions, morphologies, stellar masses and angular momentum content. Aquila clearly demonstrated that the primary uncertainty in these types of simulations is related to the processes of the unresolved baryonic physics that result in star formatio ...
The star formation history of galaxies in 3D: CALIFA perspective
... 2.1. Hubble sequence: stellar population properties of galaxies in the tuning-fork diagram One step to understand how galaxies form and evolve is classifying galaxies and studying their properties. Most of the massive galaxies in the near Universe are E, S0 and spirals (Blanton & Moustakas 2009), fo ...
... 2.1. Hubble sequence: stellar population properties of galaxies in the tuning-fork diagram One step to understand how galaxies form and evolve is classifying galaxies and studying their properties. Most of the massive galaxies in the near Universe are E, S0 and spirals (Blanton & Moustakas 2009), fo ...
Fundamental properties of Ana González Galán
... send X-ray space missions above the Earth’s atmosphere with more than half a million X-ray sources detected up to date. X-ray binaries (XRBs) are point-like X-ray sources. These systems consist of a compact object – a neutron star (NS) or a black hole (BH) – orbiting a companion, or donor, star from ...
... send X-ray space missions above the Earth’s atmosphere with more than half a million X-ray sources detected up to date. X-ray binaries (XRBs) are point-like X-ray sources. These systems consist of a compact object – a neutron star (NS) or a black hole (BH) – orbiting a companion, or donor, star from ...
Magnetic fields in Local Group dwarf irregulars⋆
... Small Magellanic Cloud (SMC), a weak total field of about 3 μG was found, partly on large-scales (Mao et al. 2008). Since all these galaxies are optically bright and nearby objects, the detection of magnetic fields in them may be influenced by strong selection effects. The question then arises of whe ...
... Small Magellanic Cloud (SMC), a weak total field of about 3 μG was found, partly on large-scales (Mao et al. 2008). Since all these galaxies are optically bright and nearby objects, the detection of magnetic fields in them may be influenced by strong selection effects. The question then arises of whe ...
GRB 021004: A Possible Shell Nebula around a Wolf
... As part of the analysis, we modeled the radiation environment in a wind bubble system following a GRB explosion using detailed photoionization models. The models are especially constructed to provide constraints on the physical conditions of blueshifted absorbers. For these particular simulations, w ...
... As part of the analysis, we modeled the radiation environment in a wind bubble system following a GRB explosion using detailed photoionization models. The models are especially constructed to provide constraints on the physical conditions of blueshifted absorbers. For these particular simulations, w ...
Global Properties of Solar Flares
... into the corona and becomes visible in soft X-rays because the gas pressure has risen dramatically. In major two-ribbon flares multiple X-ray loops appear in a roughly cylindrical “arcade” formation. The newly formed high-temperature coronal plasma then gradually cools through the EUV, UV, and optic ...
... into the corona and becomes visible in soft X-rays because the gas pressure has risen dramatically. In major two-ribbon flares multiple X-ray loops appear in a roughly cylindrical “arcade” formation. The newly formed high-temperature coronal plasma then gradually cools through the EUV, UV, and optic ...
Abstracts - Space Telescope Science Institute
... The face-on grand design spiral galaxy M83 (d=4.6 Mpc) is an actively star-forming galaxy, with spiral arms filled with giant H II regions and an intense nuclear starburst. The galaxy itself is a veritable supernova factory, having generated six known SNe in less than 100 years. Hence, one might exp ...
... The face-on grand design spiral galaxy M83 (d=4.6 Mpc) is an actively star-forming galaxy, with spiral arms filled with giant H II regions and an intense nuclear starburst. The galaxy itself is a veritable supernova factory, having generated six known SNe in less than 100 years. Hence, one might exp ...
black hole masses and host galaxy evolution of radio
... (Padovani & Giommi 1995); its true redshift is 0:3819 0:0001 from fitting many absorption lines around the G band. For 1133+161, z ¼ 0:46 was reported by Fichtel et al. (1994), while Rector et al. (2000) estimated a much larger redshift, although they reported it as tentative since absorption line ...
... (Padovani & Giommi 1995); its true redshift is 0:3819 0:0001 from fitting many absorption lines around the G band. For 1133+161, z ¼ 0:46 was reported by Fichtel et al. (1994), while Rector et al. (2000) estimated a much larger redshift, although they reported it as tentative since absorption line ...
Chapter 17 - Astronomy
... (iv) Cold dark matter; an exotic form of matter, moving at relatively slow speed, which can be detected only by its gravitational interactions; it appears to be quite abundant throughout the universe. 10. It seems that the universe is only about 4% normal matter and 20% dark matter, the remaining 76 ...
... (iv) Cold dark matter; an exotic form of matter, moving at relatively slow speed, which can be detected only by its gravitational interactions; it appears to be quite abundant throughout the universe. 10. It seems that the universe is only about 4% normal matter and 20% dark matter, the remaining 76 ...
Gamma-Ray Line Emission from Radioactive Isotopes in Stars and
... as well as on the destructions through 26Al(p, g), in addition the rapidly decaying 26Al state at 228 keV excitation energy becomes an important agent in oxygen burning. The genesis of the central compact remnant in core-collapse supernovae bears on several interesting physical problems, some of whi ...
... as well as on the destructions through 26Al(p, g), in addition the rapidly decaying 26Al state at 228 keV excitation energy becomes an important agent in oxygen burning. The genesis of the central compact remnant in core-collapse supernovae bears on several interesting physical problems, some of whi ...
ON THE POLAR CAPS OF THE THREE MUSKETEERS1
... Finley 1993). The timing analysis unveiled the source pulsation, with a pulsed fraction increasing from 11% for energies <0.5 keV to 63% above 0.5 keV. The spectrum was best described by a two-component model. A blackbody with temperature of 8 ; 105 K, coming from a large portion of the surface, ...
... Finley 1993). The timing analysis unveiled the source pulsation, with a pulsed fraction increasing from 11% for energies <0.5 keV to 63% above 0.5 keV. The spectrum was best described by a two-component model. A blackbody with temperature of 8 ; 105 K, coming from a large portion of the surface, ...
Chapter 27
... • Taking advantage of the constant speed of light, we can look back in time to see how galaxies have evolved. • The most distant galaxies we can see are the oldest. • Using the Hubble Telescope, astronomers can see back more than 10 billion years, to see galaxies soon after they’d formed. • The earl ...
... • Taking advantage of the constant speed of light, we can look back in time to see how galaxies have evolved. • The most distant galaxies we can see are the oldest. • Using the Hubble Telescope, astronomers can see back more than 10 billion years, to see galaxies soon after they’d formed. • The earl ...
Article PDF - IOPscience
... nature of their power source. Specifically, most galaxies which possess a radio-luminous active galactic nucleus (AGN) and rapidly advancing jets show little evidence for a central accreting disk. For example, in Centaurus A and Virgo A (M87) there is no blue continuum or broad emission lines, but a ...
... nature of their power source. Specifically, most galaxies which possess a radio-luminous active galactic nucleus (AGN) and rapidly advancing jets show little evidence for a central accreting disk. For example, in Centaurus A and Virgo A (M87) there is no blue continuum or broad emission lines, but a ...
High-resolution radio emission from RCW 49/Westerlund 2
... Results. The new 2-GHz bandwidth data result in the most detailed radio continuum images of RCW 49 to date. The radio emission closely mimics the near-IR emission observed by Spitzer, showing pillars and filaments. The brightest continuum emission comes from the region known as the bridge. The overa ...
... Results. The new 2-GHz bandwidth data result in the most detailed radio continuum images of RCW 49 to date. The radio emission closely mimics the near-IR emission observed by Spitzer, showing pillars and filaments. The brightest continuum emission comes from the region known as the bridge. The overa ...
PH607 – Galaxies
... It suggests that there might be an upper ceiling to how large a galaxy can grow. Perhaps when a galaxy gets to be very large, its gravity is so strong that it rips up smaller galaxies that pass nearby before they can join it. Another question is why, if all galaxies are mergers of smaller ones, many ...
... It suggests that there might be an upper ceiling to how large a galaxy can grow. Perhaps when a galaxy gets to be very large, its gravity is so strong that it rips up smaller galaxies that pass nearby before they can join it. Another question is why, if all galaxies are mergers of smaller ones, many ...
Nuclear astrophysics: the unfinished quest for the origin of the
... The determination of the chemical composition of a distant star is not a trivial task. It basically relies on the analysis of the electromagnetic radiation emitted at different wavelengths (so-called spectra). For the case of the Solar System abundances, several sources of information, that combine ...
... The determination of the chemical composition of a distant star is not a trivial task. It basically relies on the analysis of the electromagnetic radiation emitted at different wavelengths (so-called spectra). For the case of the Solar System abundances, several sources of information, that combine ...
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.