Discovery of Warm and Dense Molecular Gas Surrounding the Ring
... effect of their strong winds and spectacular mass ejections over the star surroundings ( Humphreys & Davidson 1994; Nota & Clampin 1997). The nested shells observed in several cases around LBV nebulae span masses from 0.1 to 20 M , most of which come from short-lived eruptions, such as the well-kno ...
... effect of their strong winds and spectacular mass ejections over the star surroundings ( Humphreys & Davidson 1994; Nota & Clampin 1997). The nested shells observed in several cases around LBV nebulae span masses from 0.1 to 20 M , most of which come from short-lived eruptions, such as the well-kno ...
Lecture 21 (pdf from the powerpoint)
... •Avg distance between galaxies ~ 1 million LY (10 to 30 big galaxy diameters) •If lake Mendota was the observable universe then each galaxy would be about 25 mm across and separated by about 1/2 meter away. •In contrast if the galaxy was the size of Mendota the solar system would be 25 microns in di ...
... •Avg distance between galaxies ~ 1 million LY (10 to 30 big galaxy diameters) •If lake Mendota was the observable universe then each galaxy would be about 25 mm across and separated by about 1/2 meter away. •In contrast if the galaxy was the size of Mendota the solar system would be 25 microns in di ...
Astrophysical false positives in direct imaging for exoplanets: a white
... bona-fide young star. The moderately large level of chromospheric activity and fast rotation, mimicking the properties of a young star, might be induced by the exchange of mass with the progenitor of the WD. This example demonstrates some of the challenges in determining accurate age estimates and i ...
... bona-fide young star. The moderately large level of chromospheric activity and fast rotation, mimicking the properties of a young star, might be induced by the exchange of mass with the progenitor of the WD. This example demonstrates some of the challenges in determining accurate age estimates and i ...
ASTROPHYSICAL PARAMETERS OF LS 2883 AND IMPLICATIONS FOR THE Y egueruela ,
... wind of the pulsar interacts with the massive star wind within the binary system. Relativistic electrons are accelerated in a shock region where the pressures of both winds balance. These electrons produce synchrotron radiation and upscatter UV–optical photons from the companion star via inverse Com ...
... wind of the pulsar interacts with the massive star wind within the binary system. Relativistic electrons are accelerated in a shock region where the pressures of both winds balance. These electrons produce synchrotron radiation and upscatter UV–optical photons from the companion star via inverse Com ...
Detecting Stars at the Galactic Centre via Synchrotron Emission
... ber of possible mechanisms have been proposed to account for the origin of the S-stars. Löckmann et al. (2008) argued that the dynamical interaction of two stellar disks in the central parsec could lead to the formation of the S-stars. Griv (2010) proposed that the S-stars were born in the disk and ...
... ber of possible mechanisms have been proposed to account for the origin of the S-stars. Löckmann et al. (2008) argued that the dynamical interaction of two stellar disks in the central parsec could lead to the formation of the S-stars. Griv (2010) proposed that the S-stars were born in the disk and ...
![Detection of [Ne ii] Emission from Young Circumstellar Disks](http://s1.studyres.com/store/data/014394769_1-fdf9c6283148d488005c87b005dab353-300x300.png)
Detection of [Ne ii] Emission from Young Circumstellar Disks
... To compute the X–ray luminosities we used the ROSAT PSPC All–Sky Survey count– rates and HR1 hardness ratios (Alcalá et al. 1997; Voges et al. 1999, 2000) following Fleming et al. (1995), and adopting the distances in Table 1. These X-ray luminosities are representative for the energy band 0.1–2.4 ...
... To compute the X–ray luminosities we used the ROSAT PSPC All–Sky Survey count– rates and HR1 hardness ratios (Alcalá et al. 1997; Voges et al. 1999, 2000) following Fleming et al. (1995), and adopting the distances in Table 1. These X-ray luminosities are representative for the energy band 0.1–2.4 ...
My talk on CO at z=0 from Santiago in June, 2011
... BIGIEL+ ’11, LEROY+ IN PREP. compiling many others ...
... BIGIEL+ ’11, LEROY+ IN PREP. compiling many others ...
find - UNAM
... (MeÂszaÂros & Rees 1992, 1993). This model requires the presence of a relatively baryon-free line of sight from the central engine to the observer, along which the fireball can expand at ultrarelativistic speeds. Additionally, the short-time-scale variations seen in many bursts (often in the millise ...
... (MeÂszaÂros & Rees 1992, 1993). This model requires the presence of a relatively baryon-free line of sight from the central engine to the observer, along which the fireball can expand at ultrarelativistic speeds. Additionally, the short-time-scale variations seen in many bursts (often in the millise ...
The Milky Way Laboratory
... Milky Way • Identify more Bones of the Milky Way. Combine with other tracers (e.g. CO, HI, dense gas) to develop a model of Galactic structure • Measure physical properties and kinematics of Bones – compare directly with simulations. Develop improved Galactic-scale simulations • Detect Bones in near ...
... Milky Way • Identify more Bones of the Milky Way. Combine with other tracers (e.g. CO, HI, dense gas) to develop a model of Galactic structure • Measure physical properties and kinematics of Bones – compare directly with simulations. Develop improved Galactic-scale simulations • Detect Bones in near ...
MEASURING THE STARS
... The magnitude system Stellar surface temperature The spectral classificaGon of stars Hertzprung-‐Russel Diagram Stellar Luminosity Classes Stellar Radii ...
... The magnitude system Stellar surface temperature The spectral classificaGon of stars Hertzprung-‐Russel Diagram Stellar Luminosity Classes Stellar Radii ...
and other gamma-ray telescopes
... LAT: 20 MeV – >300 GeV (LAT was originally called GLAST by itself) LAT field of view ~2.5 sr GLAST Burst Monitor GBM: 10 keV – 25 MeV GBM field of view ~9 sr Launch: This Winter Lifetime: 5 years minimum, 10 years goal ...
... LAT: 20 MeV – >300 GeV (LAT was originally called GLAST by itself) LAT field of view ~2.5 sr GLAST Burst Monitor GBM: 10 keV – 25 MeV GBM field of view ~9 sr Launch: This Winter Lifetime: 5 years minimum, 10 years goal ...
CHAPTER 4 THE SPATIAL DISTRIBUTION OF GALAXIES 4.13
... Having looked at the properties of individual galaxies – both normal and active – in some detail, it is now appropriate to consider how these galaxies are distributed in space. Surveys of the region outside our own Milky Way show that there are galaxies all around us. Deep field images such as those ...
... Having looked at the properties of individual galaxies – both normal and active – in some detail, it is now appropriate to consider how these galaxies are distributed in space. Surveys of the region outside our own Milky Way show that there are galaxies all around us. Deep field images such as those ...
Galaxies on Sub-Galactic Scales
... are HI-deficient stellar systems with upper limits for their neutral hydrogen masses at a few 104 M} (Grcevich & Putman 2009), orbiting the Milky Way within its virial radius of 250 kpc. They populate a mostly unexplored region of the galactic parameter space and seem to form a new galaxy class, the ...
... are HI-deficient stellar systems with upper limits for their neutral hydrogen masses at a few 104 M} (Grcevich & Putman 2009), orbiting the Milky Way within its virial radius of 250 kpc. They populate a mostly unexplored region of the galactic parameter space and seem to form a new galaxy class, the ...
The mid- and far-infrared range - International Space Science Institute
... and neutral molecules and dust attain temperatures in the range of about 5 K to 1000 K and therefore emit most of their energy at mid- and far-IR wavelengths. Generally, the near-IR range is defined as extending from 0.75 µm to 2.5 µm and the mid-IR range runs from 2.5 µm to about 25 µm. The far-IR ...
... and neutral molecules and dust attain temperatures in the range of about 5 K to 1000 K and therefore emit most of their energy at mid- and far-IR wavelengths. Generally, the near-IR range is defined as extending from 0.75 µm to 2.5 µm and the mid-IR range runs from 2.5 µm to about 25 µm. The far-IR ...
MS-SCI-PS-Unit 4 -- Chapter 15- Stars, Galaxies
... atmosphere. To detect these wavelengths, astronomers have placed telescopes in space. Some space telescopes are designed to detect visible light or infrared radiation, since Earth's atmosphere also interferes with the transmission of these forms of radiation. The Hubble Space Telescope is a reflecti ...
... atmosphere. To detect these wavelengths, astronomers have placed telescopes in space. Some space telescopes are designed to detect visible light or infrared radiation, since Earth's atmosphere also interferes with the transmission of these forms of radiation. The Hubble Space Telescope is a reflecti ...
hal.archives-ouvertes.fr - HAL-ENS
... bII = 48.5◦ ), but further to the North-West (∼ 2◦ ). These 2 sources seem aligned with a large arc-shaped structure that is above the galactic plane and stretches from lII ∼ 200◦ to lII ∼ 80 − 100◦ . However both clouds are compact (φ ∼ 1◦ ) and seem more likely related to the compact high-velocity ...
... bII = 48.5◦ ), but further to the North-West (∼ 2◦ ). These 2 sources seem aligned with a large arc-shaped structure that is above the galactic plane and stretches from lII ∼ 200◦ to lII ∼ 80 − 100◦ . However both clouds are compact (φ ∼ 1◦ ) and seem more likely related to the compact high-velocity ...
Background Information on Galaxy Classification
... Elliptical galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Inter ...
... Elliptical galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Inter ...
The Milky Way galaxy Contents Summary
... billions of stars. The smaller galaxies are much more numerous than the larger ones, but not by a sufficient factor to compensate for their lower luminosities. So most of the luminosity in the Universe is contributed by galaxies that lie just below the top of the scale. The Sun lies in just such a g ...
... billions of stars. The smaller galaxies are much more numerous than the larger ones, but not by a sufficient factor to compensate for their lower luminosities. So most of the luminosity in the Universe is contributed by galaxies that lie just below the top of the scale. The Sun lies in just such a g ...
Neutron Star and Superfluidity
... The idea of superfluidity exists inside neutron stars was first proposed by Migdal[1]. In analogy to electrons inside superconductor forming cooper pairs due to electron lattice interaction, it is expected that nucleons in neutron star at sufficiently high density and low temperature can also form coppe ...
... The idea of superfluidity exists inside neutron stars was first proposed by Migdal[1]. In analogy to electrons inside superconductor forming cooper pairs due to electron lattice interaction, it is expected that nucleons in neutron star at sufficiently high density and low temperature can also form coppe ...
sBzKs
... very similar, clustering amplitudes ～10 times higher than generic galaxies in the same magnitude range. This suggests an evolutionary link between sBzKs at z～2 and EROs at z～1, with star formation on sBzKs quenching by z～1 thus producing passively evolving EROs. The clustering amplitude of pBzKs is ...
... very similar, clustering amplitudes ～10 times higher than generic galaxies in the same magnitude range. This suggests an evolutionary link between sBzKs at z～2 and EROs at z～1, with star formation on sBzKs quenching by z～1 thus producing passively evolving EROs. The clustering amplitude of pBzKs is ...
The destruction and survival of polycyclic aromatic hydrocarbons in
... In Spitzer observations of Tauri stars and their disks, features of polycyclic aromatic hydrocarbons (PAHs) are detected in less than 10% of the objects, although the stellar photosphere is sufficiently hot to excite PAHs. To explain the deficiency, we discuss PAH destruction by photons, assuming that ...
... In Spitzer observations of Tauri stars and their disks, features of polycyclic aromatic hydrocarbons (PAHs) are detected in less than 10% of the objects, although the stellar photosphere is sufficiently hot to excite PAHs. To explain the deficiency, we discuss PAH destruction by photons, assuming that ...
part 2
... The X-ray study of rotation-powered or radio pulsars has had a close link with Xray astronomy from its very beginning. After the discovery of Sco X−1 as the first extra-solar X-ray source by rocket-borne Geiger counters (Giacconi et al. 1962), the next source of celestial X-rays identified was the C ...
... The X-ray study of rotation-powered or radio pulsars has had a close link with Xray astronomy from its very beginning. After the discovery of Sco X−1 as the first extra-solar X-ray source by rocket-borne Geiger counters (Giacconi et al. 1962), the next source of celestial X-rays identified was the C ...
black holes can play a constructive role as well
... The highest concentration of blue objects is found at the SWtip of the inner filament, which also harbours the brightest of the blue objects. It is also the only region that such blue objects are found in association with strong line-emission. The colours and magnitudes of these objects (discussed m ...
... The highest concentration of blue objects is found at the SWtip of the inner filament, which also harbours the brightest of the blue objects. It is also the only region that such blue objects are found in association with strong line-emission. The colours and magnitudes of these objects (discussed m ...
Swift and NuSTAR observations of XTE J1859+083
... The matter for the creation of the X-ray spectrum is supplied by the companion star and processed by the accretion of this matter onto the surface of the NS. Accretion is a very effective process to transform the energetic energy caused by the strong gravitational field into radiation energy. This m ...
... The matter for the creation of the X-ray spectrum is supplied by the companion star and processed by the accretion of this matter onto the surface of the NS. Accretion is a very effective process to transform the energetic energy caused by the strong gravitational field into radiation energy. This m ...
2. The X-ray-Radio correlation for bulgeless galaxies
... The study of integrated light measurements in both the X-ray and Radio bands in galaxies allows for the identification of populations of new stars – and therefore, star formation processes – as well as markers for the presence of Active Galactic Nuclei. Correlations between the X-ray and Radio emiss ...
... The study of integrated light measurements in both the X-ray and Radio bands in galaxies allows for the identification of populations of new stars – and therefore, star formation processes – as well as markers for the presence of Active Galactic Nuclei. Correlations between the X-ray and Radio emiss ...
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.