Methanol Masers in the NGC6334F Star Forming Region
... • These models suggest the following physical parameters for the masing region : nH2 = 106 cm-3, Tgas = 30K, Tdust = 150K, beaming factor around 10. • These parameters are all very plausible for young highmass star formation regions. • The modeling assumes that the emission from the different transi ...
... • These models suggest the following physical parameters for the masing region : nH2 = 106 cm-3, Tgas = 30K, Tdust = 150K, beaming factor around 10. • These parameters are all very plausible for young highmass star formation regions. • The modeling assumes that the emission from the different transi ...
ON THE POLAR CAPS OF THE THREE MUSKETEERS1
... The definitely brighter PSR 0656+14 was first detected by the Einstein satellite (Cordova et al. 1989). A ROSAT PSPC observation allowed Finley et al. (1992) to detect the X-ray pulsation and to measure a pulsed fraction of 14% 2%. Further pointings were then carried out with the ROSAT PSPC detect ...
... The definitely brighter PSR 0656+14 was first detected by the Einstein satellite (Cordova et al. 1989). A ROSAT PSPC observation allowed Finley et al. (1992) to detect the X-ray pulsation and to measure a pulsed fraction of 14% 2%. Further pointings were then carried out with the ROSAT PSPC detect ...
Planetary Nebula
... and fainter, smooth, circular outer envelope. The Lemon slice nebula is one of the most simple nebulae known, with an almost perfectly spherical shape. It appears very similar to a lemon for which it is named. The central star is a very hot and bright Red Giant, and can be seen as a red-orange hue. ...
... and fainter, smooth, circular outer envelope. The Lemon slice nebula is one of the most simple nebulae known, with an almost perfectly spherical shape. It appears very similar to a lemon for which it is named. The central star is a very hot and bright Red Giant, and can be seen as a red-orange hue. ...
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 ( ...
Harikane
... • [OII]Blobs are galaxies with strong and spatially extended [OII] emission beyond their stellar components. • Extended metal emission → strong outflow • Yuma+13 find 12 [OII]Blobs at z~1.2 using a Subaru large-area narrowband survey. ...
... • [OII]Blobs are galaxies with strong and spatially extended [OII] emission beyond their stellar components. • Extended metal emission → strong outflow • Yuma+13 find 12 [OII]Blobs at z~1.2 using a Subaru large-area narrowband survey. ...
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 ...
HH 222: A Giant Herbig-Haro Flow from the
... young stars, hence its inclusion among the HH objects (Reipurth 1999). What makes it unique and makes it stand out from all other known HH objects is a couple of very large streamers, the longest of which stretches across 260 arcsec, corresponding to 0.6 pc at the often-assumed distance of 460 pc fo ...
... young stars, hence its inclusion among the HH objects (Reipurth 1999). What makes it unique and makes it stand out from all other known HH objects is a couple of very large streamers, the longest of which stretches across 260 arcsec, corresponding to 0.6 pc at the often-assumed distance of 460 pc fo ...
Star Formation in the Orion Nebula II: Gas, Dust, Proplyds and
... This means that the dust in the Veil has a different size distribution than that in the interstellar medium, probably having fewer small particles (O’Dell 2001a), whether this is due to grain growth or destruction of small grains is undetermined. The Background PDR. The PDR has a density of at least ...
... This means that the dust in the Veil has a different size distribution than that in the interstellar medium, probably having fewer small particles (O’Dell 2001a), whether this is due to grain growth or destruction of small grains is undetermined. The Background PDR. The PDR has a density of at least ...
Formation of low-mass helium white dwarfs
... and low magnetic fields. These neutron stars are believed to be the end-product of binary evolution, in which an old neutron star accretes matter and angular momentum from a close stellar companion for an extended period of time, while being observable as an X-ray binary. During this evolutionary ph ...
... and low magnetic fields. These neutron stars are believed to be the end-product of binary evolution, in which an old neutron star accretes matter and angular momentum from a close stellar companion for an extended period of time, while being observable as an X-ray binary. During this evolutionary ph ...
Research Report for 2015/2016
... Rochester, Imperial College, and AWE to study shock waves in collimated jets using highpowered lasers. Funded by the DOE, one project uses the Omega laser to launch jets and observe what happens when strong shock waves intersect. A separate project explores what happens to shock waves in a plasma wh ...
... Rochester, Imperial College, and AWE to study shock waves in collimated jets using highpowered lasers. Funded by the DOE, one project uses the Omega laser to launch jets and observe what happens when strong shock waves intersect. A separate project explores what happens to shock waves in a plasma wh ...
The Formation of Population III Stars in Gas Accretion Stage: Effects
... 2003; Yoshida et al. 2006; Yoshida et al. 2008). Cosmological simulations have shown that the first collapsed objects had a baryonic mass of ∼ 103 − 104 M⊙ and a temperature of ∼ 200 − 300 K (e.g., Bromm et al. 2002). Until several years ago, it was thought that only a single massive star with a mass ...
... 2003; Yoshida et al. 2006; Yoshida et al. 2008). Cosmological simulations have shown that the first collapsed objects had a baryonic mass of ∼ 103 − 104 M⊙ and a temperature of ∼ 200 − 300 K (e.g., Bromm et al. 2002). Until several years ago, it was thought that only a single massive star with a mass ...
Evolution of high-redshift quasars
... discussed above, quasars do not show strong spectral evolution, indicating that their emission line region structure is not a function of redshift, is not affect by cosmic environment. This implies that the measurement calibrated locally can be reliably applied to high-redshift. The black hole mass ...
... discussed above, quasars do not show strong spectral evolution, indicating that their emission line region structure is not a function of redshift, is not affect by cosmic environment. This implies that the measurement calibrated locally can be reliably applied to high-redshift. The black hole mass ...
Kinematics of H $\ mathsf {_2} $ O masers in high
... EVN at three epochs (June, September and November, 1997). A description of the most relevant properties (i.e. source name, coordinates, velocity of the ambient medium, distance and bolometric luminosity) of each source is given in Table 1. An extensive description of the observations and of the data ...
... EVN at three epochs (June, September and November, 1997). A description of the most relevant properties (i.e. source name, coordinates, velocity of the ambient medium, distance and bolometric luminosity) of each source is given in Table 1. An extensive description of the observations and of the data ...
BLANCO CARDENAS
... antigua casera Sharo. A aquellos que se fueron de Granada hace un tiempo, estoy feliz de que sean piezas de este rompecabezas con la Alhambra de fondo: gracias Juliane Serres, Ana Victoria Cuesta, Sebastian “Chingue” Meier, Lucı́a Piñeiro Freire, Lizette Duque, Ana Marı́a Salazar; sigo recordándol ...
... antigua casera Sharo. A aquellos que se fueron de Granada hace un tiempo, estoy feliz de que sean piezas de este rompecabezas con la Alhambra de fondo: gracias Juliane Serres, Ana Victoria Cuesta, Sebastian “Chingue” Meier, Lucı́a Piñeiro Freire, Lizette Duque, Ana Marı́a Salazar; sigo recordándol ...
The drop in the cosmic star formation rate below redshift 2 is caused
... reduced for haloes with Mhalo & 1012 M⊙ (Booth & Schaye, 2009). The AGN simulation reproduces the observed mass density in black holes at z = 0 and the black hole scaling relations (Booth & Schaye, 2009) and their evolution (Booth & Schaye, 2010) as well as the observed optical and X-ray properties, ...
... reduced for haloes with Mhalo & 1012 M⊙ (Booth & Schaye, 2009). The AGN simulation reproduces the observed mass density in black holes at z = 0 and the black hole scaling relations (Booth & Schaye, 2009) and their evolution (Booth & Schaye, 2010) as well as the observed optical and X-ray properties, ...
U P C NIVERSITAT
... dwarf in a binary system — with either another white dwarf, through the so-called double-degenerate channel, or a main-sequence or red giant companion through the single-degenerate channel — could give rise to a Type Ia supernova event. Yet, despite the recent breakthrough detections of relatively n ...
... dwarf in a binary system — with either another white dwarf, through the so-called double-degenerate channel, or a main-sequence or red giant companion through the single-degenerate channel — could give rise to a Type Ia supernova event. Yet, despite the recent breakthrough detections of relatively n ...
Impact of Protostellar Outflow on Star Formation: Effects of Initial
... With a simple analytical approach, they showed that a wide-opening-angle outflow sweeps up the gas in the infalling envelope and ejects it into the interstellar space. They concluded that the protostellar outflow can limit star formation efficiency to ϵ ∼ 30 − 50%. In addition, feedback from the protost ...
... With a simple analytical approach, they showed that a wide-opening-angle outflow sweeps up the gas in the infalling envelope and ejects it into the interstellar space. They concluded that the protostellar outflow can limit star formation efficiency to ϵ ∼ 30 − 50%. In addition, feedback from the protost ...
Multiwavelength analysis for interferometric (sub
... We developed a method for constraining the dust properties and the disk structure through the self-consistent modeling of submm and mm observations. The method is based on the simultaneous uv-plane fit of several interferometric observations at different wavelengths. The strength of the method lies ...
... We developed a method for constraining the dust properties and the disk structure through the self-consistent modeling of submm and mm observations. The method is based on the simultaneous uv-plane fit of several interferometric observations at different wavelengths. The strength of the method lies ...
Protoplanetary Disks and Their Evolution
... star but, as the surrounding molecular core is used up or otherwise disperses, the accretion rate decreases and a small amount of material persists. That these disks can be considered protoplanetary is apparent through not only the geometry of the Solar System but also the high detection rate of exo ...
... star but, as the surrounding molecular core is used up or otherwise disperses, the accretion rate decreases and a small amount of material persists. That these disks can be considered protoplanetary is apparent through not only the geometry of the Solar System but also the high detection rate of exo ...
FERMI GBM detections of four AXPs at soft gamma-rays
... (1979) observed another, much weaker, burst from the same source. After these first observations several other sources with repeated bursts in the X- and γ-rays were detected. Several years later, in 1994, SGRs were discovered to show persistent X-ray emission by Vasisht et al. (1994), Rothschild et ...
... (1979) observed another, much weaker, burst from the same source. After these first observations several other sources with repeated bursts in the X- and γ-rays were detected. Several years later, in 1994, SGRs were discovered to show persistent X-ray emission by Vasisht et al. (1994), Rothschild et ...
New brown dwarfs and giant planets
... Thick disk stars can have high velocities - Reid, Hawley & Gizis (1995): PMSU M dwarf survey 4% of the sample would be classed as dark halo by Oppenheimer et al => ~2 x 10^-4 white dwarfs / pc^3 • Most of the Oppenheimer et al. white dwarfs are remnants of the first stars which formed in the thick d ...
... Thick disk stars can have high velocities - Reid, Hawley & Gizis (1995): PMSU M dwarf survey 4% of the sample would be classed as dark halo by Oppenheimer et al => ~2 x 10^-4 white dwarfs / pc^3 • Most of the Oppenheimer et al. white dwarfs are remnants of the first stars which formed in the thick d ...
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.