SPT 0538−50: PHYSICAL CONDITIONS IN THE ISM OF A STRONGLY... GALAXY AT Z=2.8
... The advent of millimeter/submillimeter (submm) instruments capable of surveying large areas of sky, including Herschel -SPIRE (Pilbratt et al. 2010; Griffin et al. 2010) and the South Pole Telescope (SPT; Carlstrom et al. 2011), has opened new vistas for the study of these submm bright systems (Viei ...
... The advent of millimeter/submillimeter (submm) instruments capable of surveying large areas of sky, including Herschel -SPIRE (Pilbratt et al. 2010; Griffin et al. 2010) and the South Pole Telescope (SPT; Carlstrom et al. 2011), has opened new vistas for the study of these submm bright systems (Viei ...
EXTREMELY EXTENDED DUST SHELLS AROUND EVOLVED
... 8.2 Basic observed parameters (distance, luminosity, pulsation period, mass loss rates and expansion velocities) for six target oxygen-rich intermediatemass stars found in literature that were used in calculations. . . . . . 177 8.3 Target evolved oxygen-rich intermediate-mass stars imaged by Infra ...
... 8.2 Basic observed parameters (distance, luminosity, pulsation period, mass loss rates and expansion velocities) for six target oxygen-rich intermediatemass stars found in literature that were used in calculations. . . . . . 177 8.3 Target evolved oxygen-rich intermediate-mass stars imaged by Infra ...
Submm Observations of Massive Star Formation in the Giant
... with these tools. Together with the optimization package MAGIX, the data are compared and reproduced with synthetic maps and spectra from these models. Results. 1. The main filament shows a velocity gradient from the end toward its center, where the most massive clumps accumulate at both ends, in ac ...
... with these tools. Together with the optimization package MAGIX, the data are compared and reproduced with synthetic maps and spectra from these models. Results. 1. The main filament shows a velocity gradient from the end toward its center, where the most massive clumps accumulate at both ends, in ac ...
Annual Report 2011 - Max Planck Institute for Astrophysics
... quickly repaired by a complete exchange of the computer. In addition to the desktop systems, which, are almost all younger than 5 years and which (in 2011) amount to more than 160 fully equipped working places, users have access to central number crunchers (about 20 machines, all 64-bit architecture ...
... quickly repaired by a complete exchange of the computer. In addition to the desktop systems, which, are almost all younger than 5 years and which (in 2011) amount to more than 160 fully equipped working places, users have access to central number crunchers (about 20 machines, all 64-bit architecture ...
OBSERVATIONS OF PHYSICAL PROCESSES IN
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
Circumstellar Material in Young Stellar Objects
... with the cloud. However, the study of molecular clouds did not reach its full growth until it became possible to observe mm and submm transitions of molecular species such as CO and NH (Cheung et al. 1968; Wilson et al. 1970; Kutner et al. 1977), allowing more detailed studies of the kinematics and ...
... with the cloud. However, the study of molecular clouds did not reach its full growth until it became possible to observe mm and submm transitions of molecular species such as CO and NH (Cheung et al. 1968; Wilson et al. 1970; Kutner et al. 1977), allowing more detailed studies of the kinematics and ...
Polaris B, an optical companion of Polaris (alpha UMi) system
... procedure see the paper of Diego (1985). In particular, at seeing β = 3 the weakening of the flux of a star located at distance ...
... procedure see the paper of Diego (1985). In particular, at seeing β = 3 the weakening of the flux of a star located at distance ...
the PDF program book
... either speak to the LOC representative at the registration desk or reserve a meeting room online. Online Instructions: To reserve a room using the spreadsheet, please leave a comment in the cell that corresponds to your desired room and start time. In the comment, please specify the length of your m ...
... either speak to the LOC representative at the registration desk or reserve a meeting room online. Online Instructions: To reserve a room using the spreadsheet, please leave a comment in the cell that corresponds to your desired room and start time. In the comment, please specify the length of your m ...
The old Nuclear Star Cluster in the Milky Way
... As a first step, the surface density distribution of stars in the central 100000 is fitted by a superposition of a spheroidal cluster with scale ∼ 10000 and a much larger nuclear disk component. The use of two flattened models is advantageous because it allows for a non-constant axial ratio. Having ...
... As a first step, the surface density distribution of stars in the central 100000 is fitted by a superposition of a spheroidal cluster with scale ∼ 10000 and a much larger nuclear disk component. The use of two flattened models is advantageous because it allows for a non-constant axial ratio. Having ...
Multiplicity in Early Stellar Evolution - Astronomy Group
... discussed in section 2. However, most protostars are still deeply embedded, so such observations are hampered by extinctions that can exceed AV ~ 100 mag. Hence infrared, submillimeter, or radio continuum observations are required. 4.1. Infrared Observations Class I protostars are often detectable ...
... discussed in section 2. However, most protostars are still deeply embedded, so such observations are hampered by extinctions that can exceed AV ~ 100 mag. Hence infrared, submillimeter, or radio continuum observations are required. 4.1. Infrared Observations Class I protostars are often detectable ...
ROSAT Ian R. Stevens* and David K. Strickland*
... which dominates at low energies, a hard power-law component and strong Fe K emission at around 6.6 keV. Iyomoto et al. (1997) interpreted the power-law emission as being due to a lowluminosity AGN. We have reanalysed both ROSAT PSPC observations, adjusted the pointing using the BL Lac object 1E0331. ...
... which dominates at low energies, a hard power-law component and strong Fe K emission at around 6.6 keV. Iyomoto et al. (1997) interpreted the power-law emission as being due to a lowluminosity AGN. We have reanalysed both ROSAT PSPC observations, adjusted the pointing using the BL Lac object 1E0331. ...
Evidence of suppression of star formation by quasar
... tribution of galaxy colors. If AGN feedback couples to the gas as efficiently as required by galaxy formation models, then massive, early-type galaxies will be gas-poor and passively aging, while younger galaxies, typically lower-mass, late-type galaxies will still have enough star formation materia ...
... tribution of galaxy colors. If AGN feedback couples to the gas as efficiently as required by galaxy formation models, then massive, early-type galaxies will be gas-poor and passively aging, while younger galaxies, typically lower-mass, late-type galaxies will still have enough star formation materia ...
A Herschel/HIFI study of Water in Two Intermediate
... Stars are large, luminous, gravitationally bound spheres of hot gas. Their luminosity lights up the galaxy, providing much of the energy that illuminates the less luminous features such as large molecular clouds of gas. Studying other galaxies in the universe is also possible because of stars. Galax ...
... Stars are large, luminous, gravitationally bound spheres of hot gas. Their luminosity lights up the galaxy, providing much of the energy that illuminates the less luminous features such as large molecular clouds of gas. Studying other galaxies in the universe is also possible because of stars. Galax ...
Type Ia Supernovae
... Ic have been attributed to these events. This thesis, however is dedicated to the second group of supernovae, the thermonuclear explosions of degenerate carbon and oxygen rich material and lacking hydrogen - called Type Ia supernovae (SNe Ia). White dwarf stars are formed at the end of a typical sta ...
... Ic have been attributed to these events. This thesis, however is dedicated to the second group of supernovae, the thermonuclear explosions of degenerate carbon and oxygen rich material and lacking hydrogen - called Type Ia supernovae (SNe Ia). White dwarf stars are formed at the end of a typical sta ...
part 2
... Disney, & Taylor 1969) and X-ray (Fritz et al. 1969; Bradt et al. 1969) pulsations, it became clear that a rapidly spinning neutron star is not only responsible for the pulsed emission, but is also powering the nebular emission as well. In general, X-ray observations of rotation-powered pulsars offe ...
... Disney, & Taylor 1969) and X-ray (Fritz et al. 1969; Bradt et al. 1969) pulsations, it became clear that a rapidly spinning neutron star is not only responsible for the pulsed emission, but is also powering the nebular emission as well. In general, X-ray observations of rotation-powered pulsars offe ...
STELLAR STRUCTURE AND EVOLUTION
... • Photometric measurements yield the apparent brightness of a star, i.e. the energy flux received on Earth, in different wavelength bands. These are usually expressed as magnitudes, e.g. B, V, I, etc. Flux ratios or colour indices (B − V, V − I, etc.) give a measure of the effective temperature, usi ...
... • Photometric measurements yield the apparent brightness of a star, i.e. the energy flux received on Earth, in different wavelength bands. These are usually expressed as magnitudes, e.g. B, V, I, etc. Flux ratios or colour indices (B − V, V − I, etc.) give a measure of the effective temperature, usi ...
View PDF
... For such long durations the two-component models yield significantly greater protostar mass than does the one-component core model. The increased mass accretion rate provided by the clump component in this model is needed to provide stars of sufficiently high mass, in the time periods associated wit ...
... For such long durations the two-component models yield significantly greater protostar mass than does the one-component core model. The increased mass accretion rate provided by the clump component in this model is needed to provide stars of sufficiently high mass, in the time periods associated wit ...
What Gaia can reveal about the matter distribution in the Milky Way
... In this master’s thesis, it is investigated to what extent the Galactic matter distribution can be determined using data coming from the astrometric satellite Gaia. This is done through a direct application of the Jeans equations on simulated data. The Galactic matter distribution Formation and evol ...
... In this master’s thesis, it is investigated to what extent the Galactic matter distribution can be determined using data coming from the astrometric satellite Gaia. This is done through a direct application of the Jeans equations on simulated data. The Galactic matter distribution Formation and evol ...
White dwarfs, black holes and neutron stars in close binaries
... hite dwarfs, neutron stars and black holes are remnants of stars that have ended their ‘active’ life. A star is born when an interstellar gas cloud contracts and forms a sphere which in its centre has a temperature and pressure high enough to start hydrogen fusion. The star remains in this phase for ...
... hite dwarfs, neutron stars and black holes are remnants of stars that have ended their ‘active’ life. A star is born when an interstellar gas cloud contracts and forms a sphere which in its centre has a temperature and pressure high enough to start hydrogen fusion. The star remains in this phase for ...
GRB prompt emission
... Allowed Astronomers To watch the bursts Fade, and then Study their Host Galaxy! ...
... Allowed Astronomers To watch the bursts Fade, and then Study their Host Galaxy! ...
GRB prompt emission
... Allowed Astronomers To watch the bursts Fade, and then Study their Host Galaxy! ...
... Allowed Astronomers To watch the bursts Fade, and then Study their Host Galaxy! ...
Cygnus X-1
Cygnus X-1 (abbreviated Cyg X-1) is a well-known galactic X-ray source, thought to be a black hole, in the constellation Cygnus. It was discovered in 1964 during a rocket flight and is one of the strongest X-ray sources seen from Earth, producing a peak X-ray flux density of 6977229999999999999♠2.3×10−23 Wm−2 Hz−1 (7003230000000000000♠2.3×103 Jansky). Cygnus X-1 was the first X-ray source widely accepted to be a black hole and it remains among the most studied astronomical objects in its class. The compact object is now estimated to have a mass about 14.8 times the mass of the Sun and has been shown to be too small to be any known kind of normal star, or other likely object besides a black hole. If so, the radius of its event horizon is about 7004440000000000000♠44 km.Cygnus X-1 belongs to a high-mass X-ray binary system about 7019574266339685654♠6070 ly from the Sun that includes a blue supergiant variable star designated HDE 226868 which it orbits at about 0.2 AU, or 20% of the distance from the Earth to the Sun. A stellar wind from the star provides material for an accretion disk around the X-ray source. Matter in the inner disk is heated to millions of degrees, generating the observed X-rays. A pair of jets, arranged perpendicular to the disk, are carrying part of the energy of the infalling material away into interstellar space.This system may belong to a stellar association called Cygnus OB3, which would mean that Cygnus X-1 is about five million years old and formed from a progenitor star that had more than 7001400000000000000♠40 solar masses. The majority of the star's mass was shed, most likely as a stellar wind. If this star had then exploded as a supernova, the resulting force would most likely have ejected the remnant from the system. Hence the star may have instead collapsed directly into a black hole.Cygnus X-1 was the subject of a friendly scientific wager between physicists Stephen Hawking and Kip Thorne in 1975, with Hawking betting that it was not a black hole. He conceded the bet in 1990 after observational data had strengthened the case that there was indeed a black hole in the system. This hypothesis has not been confirmed due to a lack of direct observation but has generally been accepted from indirect evidence.