Young Galaxies Grow - Astronomical Society of the Pacific
... and with radio emission added to illustrate the distribution of its extended disk of low-density gas where the new young stars were found. Credits: R. Gendler/NASA/JPL-Caltech/NRAO/ ...
... and with radio emission added to illustrate the distribution of its extended disk of low-density gas where the new young stars were found. Credits: R. Gendler/NASA/JPL-Caltech/NRAO/ ...
Section IV High-Energy Astrophysics and Cosmology
... objects including X-rays and gamma-rays. The accreting supermassive black holes (SMBH) in active galactic nuclei (AGN) are found in the center of modern astrophysics. The main problem is connected with determining the masses of these objects. The virial theorem accepted to a flattened configuration ...
... objects including X-rays and gamma-rays. The accreting supermassive black holes (SMBH) in active galactic nuclei (AGN) are found in the center of modern astrophysics. The main problem is connected with determining the masses of these objects. The virial theorem accepted to a flattened configuration ...
Title The Correlation between Dispersion Measure and X
... including the atmosphere composition, surface magnetic field, and gravity. 4. For pulsars associated with bright PWNe, the nebular NH values are adopted if they are better constrained than those of the pulsars, because the simple PL spectra of PWNe can reduce systematic uncertainties in spectral mod ...
... including the atmosphere composition, surface magnetic field, and gravity. 4. For pulsars associated with bright PWNe, the nebular NH values are adopted if they are better constrained than those of the pulsars, because the simple PL spectra of PWNe can reduce systematic uncertainties in spectral mod ...
LANL Cosmology Summer School Lectures, July 2010
... ULIRGs: X = 0.8 MO/(K km/s pc^2) (CO rotation curves) Optically thin limit: X ~ 0.2 ...
... ULIRGs: X = 0.8 MO/(K km/s pc^2) (CO rotation curves) Optically thin limit: X ~ 0.2 ...
What caused the GeV flare of PSR B1259-63?
... responsible for the GeV emission could be localised in the pulsar wind, in the shocked pulsar wind, or in the shocked stellar wind. Here, we assume that the pairs are located at the apex of the cone, and come back to their origin later (Sect. 3.2). Localising the pairs at the apex is reasonable if t ...
... responsible for the GeV emission could be localised in the pulsar wind, in the shocked pulsar wind, or in the shocked stellar wind. Here, we assume that the pairs are located at the apex of the cone, and come back to their origin later (Sect. 3.2). Localising the pairs at the apex is reasonable if t ...
Cataclysmic Variables
... Hoard et al. (2003; an online updated list is at http://www.dwhoard.com/home/ biglist). A few of these SW Sex stars show low circular polarization, indicating a relatively high magnetic field for the white dwarf (for example, RodriguezGil et al. 2001). Some novalikes, including the SW Sex stars, occ ...
... Hoard et al. (2003; an online updated list is at http://www.dwhoard.com/home/ biglist). A few of these SW Sex stars show low circular polarization, indicating a relatively high magnetic field for the white dwarf (for example, RodriguezGil et al. 2001). Some novalikes, including the SW Sex stars, occ ...
Question 1
... the source of energy is very small. energy is coming from matter and antimatter. the energy source is rotating rapidly. a chain reaction of supernovas occurs. there are many separate sources of energy in the core. ...
... the source of energy is very small. energy is coming from matter and antimatter. the energy source is rotating rapidly. a chain reaction of supernovas occurs. there are many separate sources of energy in the core. ...
The Sun as an X-Ray Star. III. Flares
... high quality of the data collected with many instruments, and in particular with the Y ohkoh/SXT, optimized to observe Ñares. Apart from experimental limitations, intrinsic physical reasons make the diagnostics of the Ñare heating very difficult : the Ñare starts when a low density plasma is heated ...
... high quality of the data collected with many instruments, and in particular with the Y ohkoh/SXT, optimized to observe Ñares. Apart from experimental limitations, intrinsic physical reasons make the diagnostics of the Ñare heating very difficult : the Ñare starts when a low density plasma is heated ...
Why do some galaxies stop making new stars?
... have lifetimes of just 30 million years. spiral galaxies without star formation, utilising In cosmological terms, 30 million years is a blink of images from NASA's Wide-field Infrared Survey Explorer. the eye. Find a galaxy with these blue stars, and you are seeing a galaxy forming stars (or that We ...
... have lifetimes of just 30 million years. spiral galaxies without star formation, utilising In cosmological terms, 30 million years is a blink of images from NASA's Wide-field Infrared Survey Explorer. the eye. Find a galaxy with these blue stars, and you are seeing a galaxy forming stars (or that We ...
Dynamics
... as they accrete some of this abundant gas supply. In the final stage of the merger, when the nuclei of the two galaxies have spiralled very close together, the black holes can have a significant impact on the distribution of stars in their vicinity. Indeed, the merger leads to the formation of a bin ...
... as they accrete some of this abundant gas supply. In the final stage of the merger, when the nuclei of the two galaxies have spiralled very close together, the black holes can have a significant impact on the distribution of stars in their vicinity. Indeed, the merger leads to the formation of a bin ...
17.1 Introduction
... resulting in the observed radial expansion. As the star expands, it does work against gravity and the gas cools. As it does so, its temperature falls back to a point where the doubly ionized helium layer recombines and becomes transparent again, thereby allowing more radiation to pass. Without that ...
... resulting in the observed radial expansion. As the star expands, it does work against gravity and the gas cools. As it does so, its temperature falls back to a point where the doubly ionized helium layer recombines and becomes transparent again, thereby allowing more radiation to pass. Without that ...
Extraordinary Luminous Soft X-Ray Transient MAXI
... The Swift XRT spectra obtained after Ttrig + 0.44 days were reported to be similar to the SSS phase of novae (Li et al. 2012). Further follow-up observations by Swift and groundbased optical observations confirmed that this source is a binary system consisting of a WD and a Be star at the distance o ...
... The Swift XRT spectra obtained after Ttrig + 0.44 days were reported to be similar to the SSS phase of novae (Li et al. 2012). Further follow-up observations by Swift and groundbased optical observations confirmed that this source is a binary system consisting of a WD and a Be star at the distance o ...
Discovery of new bright quasars by the core
... (NVSS, Condon et al. 1998; FIRST, Becker et al. 1997) catalogs to distinguish X-ray and radio sources. We have surveyed 14 MAPS (POSS) fields so far and found 10-12 bright candidates in each, 50-60% being known AGN. Altogether, 145 objects have been found, 81 are known QSOs/Sys. Thus we are left wit ...
... (NVSS, Condon et al. 1998; FIRST, Becker et al. 1997) catalogs to distinguish X-ray and radio sources. We have surveyed 14 MAPS (POSS) fields so far and found 10-12 bright candidates in each, 50-60% being known AGN. Altogether, 145 objects have been found, 81 are known QSOs/Sys. Thus we are left wit ...
Observational Constraints on the Most Massive White Dwarf
... Here we plot the same initial-final mass relation from Slide 5, but we vary the assumed age of M35 within the current age uncertainty. The plotted error bars are the white dwarf observational uncertainties. For a younger assumed cluster age, the progenitor masses increase systematically for all of t ...
... Here we plot the same initial-final mass relation from Slide 5, but we vary the assumed age of M35 within the current age uncertainty. The plotted error bars are the white dwarf observational uncertainties. For a younger assumed cluster age, the progenitor masses increase systematically for all of t ...
The Strikingly Uniform, Highly Turbulent Interstellar Medium of the
... from optical lines (z = 4.593; Wu et al. 2012); the other three spectral windows probing the continuum blue-ward of the line. The on-source integration time was 956 s in array configuration C34-4. Flux, phase, and band-pass calibrators were also obtained, for a total time of 3330 s. We used the CASA ...
... from optical lines (z = 4.593; Wu et al. 2012); the other three spectral windows probing the continuum blue-ward of the line. The on-source integration time was 956 s in array configuration C34-4. Flux, phase, and band-pass calibrators were also obtained, for a total time of 3330 s. We used the CASA ...
A Modern Search for Wolf-Rayet Stars in the Magellanic Clouds. III
... Our most exciting discovery was identifying two new members of the class of WRs that we are calling WN3/O3s (Papers I and II). Other members of this class show the strong N v λλ4603,19 doublet, N v λ4945 and He ii λ4686 emission lines characteristic of a WN3 star, and a He ii and Balmer line absorpt ...
... Our most exciting discovery was identifying two new members of the class of WRs that we are calling WN3/O3s (Papers I and II). Other members of this class show the strong N v λλ4603,19 doublet, N v λ4945 and He ii λ4686 emission lines characteristic of a WN3 star, and a He ii and Balmer line absorpt ...
ppt - lenac
... Title Studying the low surface brightness galaxies from the SDSS With the advent of large aperture telescopes (VLT, Magellan, GEMINI, etc.) the detailed (high S/N spectroscopy, high spatial resolution, etc.) study of low surface brightness galaxies (LSBGs) become possible. These low stellar density ...
... Title Studying the low surface brightness galaxies from the SDSS With the advent of large aperture telescopes (VLT, Magellan, GEMINI, etc.) the detailed (high S/N spectroscopy, high spatial resolution, etc.) study of low surface brightness galaxies (LSBGs) become possible. These low stellar density ...
Indroduction
... more recent ones by Kau mann & Charlot (1996), and Kau mann & Charlot (1997) ellipticals are viewed as being formed by mergers of disk galaxies in a universe where structures are built through hierarchical clustering. In the local universe, ongoing merging is observed and it is generally assumed tha ...
... more recent ones by Kau mann & Charlot (1996), and Kau mann & Charlot (1997) ellipticals are viewed as being formed by mergers of disk galaxies in a universe where structures are built through hierarchical clustering. In the local universe, ongoing merging is observed and it is generally assumed tha ...
How the Stanford Linear Accelerator Center is transforming the
... A cadre of engineers, construction crews, physicists, and designers is preparing the linac for its completely new job—electron production for a powerful, innovative X-ray laser, the Linac Coherent Light Source (LCLS). In seizing this exciting opportunity, the linac repositions itself as a major play ...
... A cadre of engineers, construction crews, physicists, and designers is preparing the linac for its completely new job—electron production for a powerful, innovative X-ray laser, the Linac Coherent Light Source (LCLS). In seizing this exciting opportunity, the linac repositions itself as a major play ...
ABSTRACT XMM-Newton X-Ray Spectroscopy of the B2 Bright Giant
... For several decades there have been two major theories of X-ray production on 0 and B stars: coronal heating, and radiatively driven wind shocks (Cohen et al. 1996). The first theory is that the X-rays are produced in the corona, near the surface of the star. Coronal heating requires the presence of ...
... For several decades there have been two major theories of X-ray production on 0 and B stars: coronal heating, and radiatively driven wind shocks (Cohen et al. 1996). The first theory is that the X-rays are produced in the corona, near the surface of the star. Coronal heating requires the presence of ...
The relation among black holes, their host galaxies and AGN activity
... The local BH mass density is ρBH = 4.1±1.5 ×105 M Mpc-3. The local BH mass function and the BH mass function of AGN ...
... The local BH mass density is ρBH = 4.1±1.5 ×105 M Mpc-3. The local BH mass function and the BH mass function of AGN ...
3011800000810
... and imaged on-axis, we extracted source spectra from each detector using an extraction radius of r ¼ 18 00 ; we used r ¼ 30 00 in the third observation when IGR J163584726 was imaged offaxis. We then built instrument response files using the standard SAS tools arfgen and rmfgen. Background spectra ...
... and imaged on-axis, we extracted source spectra from each detector using an extraction radius of r ¼ 18 00 ; we used r ¼ 30 00 in the third observation when IGR J163584726 was imaged offaxis. We then built instrument response files using the standard SAS tools arfgen and rmfgen. Background spectra ...
The e-Science in the Transient Radio Sky Soon
... Accretion and High Energy Radiation Processes in Relativistic Compact Objects cosmic rays Shock : TeV Hot Spot ...
... Accretion and High Energy Radiation Processes in Relativistic Compact Objects cosmic rays Shock : TeV Hot Spot ...
The Universe
... Spiral galaxies consist of a rotating disk of stars and interstellar medium, along with a central bulge of generally older stars. Extending outward from the bulge are relatively bright arms. In the Hubble classification scheme, spiral galaxies are listed as type S, followed by a letter (a, b, or c) ...
... Spiral galaxies consist of a rotating disk of stars and interstellar medium, along with a central bulge of generally older stars. Extending outward from the bulge are relatively bright arms. In the Hubble classification scheme, spiral galaxies are listed as type S, followed by a letter (a, b, or c) ...
The Universe
... Spiral galaxies consist of a rotating disk of stars and interstellar medium, along with a central bulge of generally older stars. Extending outward from the bulge are relatively bright arms. In the Hubble classification scheme, spiral galaxies are listed as type S, followed by a letter (a, b, or c) ...
... Spiral galaxies consist of a rotating disk of stars and interstellar medium, along with a central bulge of generally older stars. Extending outward from the bulge are relatively bright arms. In the Hubble classification scheme, spiral galaxies are listed as type S, followed by a letter (a, b, or c) ...
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.