Extended Infrared Emission from LIRGs
... Kinematical evidence from ionized (Hα) and molecular (CO) gas are consistent the presence of extended (~5kpc) star forming disks There is a “broad” connection between mid-IR emission and star formation rates (with some caveats…) We wish to quantify the extended extranuclear emission in local LIRGs i ...
... Kinematical evidence from ionized (Hα) and molecular (CO) gas are consistent the presence of extended (~5kpc) star forming disks There is a “broad” connection between mid-IR emission and star formation rates (with some caveats…) We wish to quantify the extended extranuclear emission in local LIRGs i ...
The destruction and survival of polycyclic aromatic hydrocarbons in
... Our T Tauri model star has a total luminosity L∗ = 2 L . Its radiation consists of a photospheric, a FUV, an EUV and an X-ray component. Their parameters are listed in Table 1 and are very similar to those proposed by Gorti & Hollenbach (2008). The total spectrum is displayed in Fig. 1. We point ou ...
... Our T Tauri model star has a total luminosity L∗ = 2 L . Its radiation consists of a photospheric, a FUV, an EUV and an X-ray component. Their parameters are listed in Table 1 and are very similar to those proposed by Gorti & Hollenbach (2008). The total spectrum is displayed in Fig. 1. We point ou ...
Richard Congdon. pdf
... with the 1173 keV and 1332 keV lines. Each radionuclide has a characteristic fingerprint of one or more energy lines specific to that radionuclide. The gamma-rays are measured using a suitable detector outside the Earth’s atmosphere; because gamma-rays entering the atmosphere interact with the atmos ...
... with the 1173 keV and 1332 keV lines. Each radionuclide has a characteristic fingerprint of one or more energy lines specific to that radionuclide. The gamma-rays are measured using a suitable detector outside the Earth’s atmosphere; because gamma-rays entering the atmosphere interact with the atmos ...
Rich Clusters of Galaxies
... Module 8: Clusters of Galaxies. • General properties, masses and mass-to-light ratios, galaxy interactions, dynamic stability, the inter-galactic medium, magnetic fields, x-ray emission, • Virial temperature, gravitational lensing, dark matter content, mass derived from x-ray observations. • Rich Cl ...
... Module 8: Clusters of Galaxies. • General properties, masses and mass-to-light ratios, galaxy interactions, dynamic stability, the inter-galactic medium, magnetic fields, x-ray emission, • Virial temperature, gravitational lensing, dark matter content, mass derived from x-ray observations. • Rich Cl ...
Five Years of Swift Science: GRBs and More!
... automation to XRT temperature control and ACS slew behavior – Goal is to allow faster, easier science planning, with capability to increase GI monitoring campaigns and rapid ToO response to large numbers of targets ...
... automation to XRT temperature control and ACS slew behavior – Goal is to allow faster, easier science planning, with capability to increase GI monitoring campaigns and rapid ToO response to large numbers of targets ...
Resources: - Real Science
... mountains. ___ they weigh as much as our sun. This makes ____ incredibly dense. Magnetars are a type of neutron star. ___ they possess magnetic fields hundreds of trillions of times __ powerful as Earth's magnetic field which turns compass _______ north. The giant cosmic hiccup still has scientists ...
... mountains. ___ they weigh as much as our sun. This makes ____ incredibly dense. Magnetars are a type of neutron star. ___ they possess magnetic fields hundreds of trillions of times __ powerful as Earth's magnetic field which turns compass _______ north. The giant cosmic hiccup still has scientists ...
ON THE RADIAL ONSET OF CLUMPING IN THE WIND OF... J. M. Torrejón , N. S. Schulz , M. A. Nowak
... densities given by the smooth wind scenario. In other words, the Fe Kα fluorescence line is a tracer of the wind clumps. In this paper we aim to study the radial location of clumps of QV Nor , the B0 supergiant donor of the X-ray source 4U1538 −52 . We proposed to observe this unique system because o ...
... densities given by the smooth wind scenario. In other words, the Fe Kα fluorescence line is a tracer of the wind clumps. In this paper we aim to study the radial location of clumps of QV Nor , the B0 supergiant donor of the X-ray source 4U1538 −52 . We proposed to observe this unique system because o ...
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... Zickgraf et al. (1989), van Genderen & Sterken (2002) found S18 to be photometrically variable at optical wavelengths between 1987-1991. Modulation occured on timescales from days to years, with peak-to-peak amplitudes ranging from ∼ 0.1 − 1.0 mag (see Sect. 2.1.2. for a full description). At other ...
... Zickgraf et al. (1989), van Genderen & Sterken (2002) found S18 to be photometrically variable at optical wavelengths between 1987-1991. Modulation occured on timescales from days to years, with peak-to-peak amplitudes ranging from ∼ 0.1 − 1.0 mag (see Sect. 2.1.2. for a full description). At other ...
ASI 2017 Abstract Book - Astronomical Society of India
... One of the most outstanding challenges in extragalactic astronomy is to identify the astrophysical processes responsible for transforming simple dark matter haloes into the heterogenous population of galaxies inhabiting today's Universe. How did different morphological types form and evolve? Does th ...
... One of the most outstanding challenges in extragalactic astronomy is to identify the astrophysical processes responsible for transforming simple dark matter haloes into the heterogenous population of galaxies inhabiting today's Universe. How did different morphological types form and evolve? Does th ...
L31 ON THE DISAPPEARANCE OF KILOHERTZ QUASI
... One critical question is whether the neutron star magnetosphere can be disengaged from the Keplerian disk at the last stable orbit. Studies have shown that the evolution of the magnetic field configuration is very complicated as the disk approaches the last stable orbit (e.g., Lai 1998), but the exa ...
... One critical question is whether the neutron star magnetosphere can be disengaged from the Keplerian disk at the last stable orbit. Studies have shown that the evolution of the magnetic field configuration is very complicated as the disk approaches the last stable orbit (e.g., Lai 1998), but the exa ...
X-ray emission from supernova shock waves Tanja Kramer Nymark Department of Astronomy
... The field of supernova research is a quite new one, compared with astronomy in general – it is only about eighty years since astronomers first became aware that some of the “new stars” which occasionally appeared were far too energetic to be understood in the context of what was at the time known ab ...
... The field of supernova research is a quite new one, compared with astronomy in general – it is only about eighty years since astronomers first became aware that some of the “new stars” which occasionally appeared were far too energetic to be understood in the context of what was at the time known ab ...
The low-spin black hole in LMC X-3 Please share
... Middleton et al. 2006; Kolehmainen et al. 2011). In this method, the inner-disk radius is estimated using the thermal, multicolor blackbody continuum emission from the disk (e.g., Novikov & Thorne 1973; Shakura & Sunyaev 1973). The Fe-line method measures Rin using the redward extent of relativistic ...
... Middleton et al. 2006; Kolehmainen et al. 2011). In this method, the inner-disk radius is estimated using the thermal, multicolor blackbody continuum emission from the disk (e.g., Novikov & Thorne 1973; Shakura & Sunyaev 1973). The Fe-line method measures Rin using the redward extent of relativistic ...
An X-Ray, Optical and Infra-red study of High-Mass X
... BINARIES IN THE SMALL MAGELLANIC CLOUD by Lee John Townsend ...
... BINARIES IN THE SMALL MAGELLANIC CLOUD by Lee John Townsend ...
Towards Planetesimals in the Disk around TW Hya: 3.5 centimeter
... dust sufficient to form planetary systems like our own (Beckwith et al. 1990). Statistical studies indicate disk dissipation on timescales of ∼ 10 Myr (Strom et al. 1989), compatible with the standard paradigm of giant planet cores forming by dust coagulation followed by planetesimal accretion (Wuch ...
... dust sufficient to form planetary systems like our own (Beckwith et al. 1990). Statistical studies indicate disk dissipation on timescales of ∼ 10 Myr (Strom et al. 1989), compatible with the standard paradigm of giant planet cores forming by dust coagulation followed by planetesimal accretion (Wuch ...
Sample pages 1 PDF
... geometrically thick flow with the aspect ratio of H/R∼0.5–1. The soft (optically thick) and hard (optically thin) spectral components are formed in the accretion disk and the hot inner flow correspondingly. The value of the truncation radius can be inferred from the observations. Although their inte ...
... geometrically thick flow with the aspect ratio of H/R∼0.5–1. The soft (optically thick) and hard (optically thin) spectral components are formed in the accretion disk and the hot inner flow correspondingly. The value of the truncation radius can be inferred from the observations. Although their inte ...
Spectroscopic confirmation of a galaxy at redshift z=8.6
... Figure 1 | Two representations of the spectrum of UDFy-38135539 showing its significance. a, The spectrum shows a faint emission line detected at 6s significance at a wavelength of 11,615.6 Å, corresponding to a redshift of z 5 8.5549 6 0.0020 for Lya. The integrated spectrum was extracted from a s ...
... Figure 1 | Two representations of the spectrum of UDFy-38135539 showing its significance. a, The spectrum shows a faint emission line detected at 6s significance at a wavelength of 11,615.6 Å, corresponding to a redshift of z 5 8.5549 6 0.0020 for Lya. The integrated spectrum was extracted from a s ...
Identifying Young far from Giant Stars Molecular Clouds
... - 4tons (Walter et al. 1988). Additionally, the boundary layer of the disk contributes certain spectral features to the stellar spectra. When this boundary material heats up as it accretes onto the star, it radiates, contributing its own continuum to the stellar spectrum. When the material is heate ...
... - 4tons (Walter et al. 1988). Additionally, the boundary layer of the disk contributes certain spectral features to the stellar spectra. When this boundary material heats up as it accretes onto the star, it radiates, contributing its own continuum to the stellar spectrum. When the material is heate ...
Hidden57_rf
... Until 400 years ago when Galileo first turned his telescope towards the heavens, our perception of the Universe was limited by our eyes and the thoughts that sprung from considering what they could see. The huge leap in capability that even such a simple instrument could realise set us on the path o ...
... Until 400 years ago when Galileo first turned his telescope towards the heavens, our perception of the Universe was limited by our eyes and the thoughts that sprung from considering what they could see. The huge leap in capability that even such a simple instrument could realise set us on the path o ...
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 ...
Influence of extreme ultraviolet radiation on the Pv ionization fraction
... on the square of the density. Moreover, the ultraviolet P V resonance lines indicate a possible need for an even stronger reduction of hot star mass-loss rates, provided that P V is a dominant ionization stage of phosphorus, at least in some hot stars. The latter assumption is challenged by the poss ...
... on the square of the density. Moreover, the ultraviolet P V resonance lines indicate a possible need for an even stronger reduction of hot star mass-loss rates, provided that P V is a dominant ionization stage of phosphorus, at least in some hot stars. The latter assumption is challenged by the poss ...
Cooling neutron stars: Theory and observations
... Ordinary cooling isolates neutron stars of age 1 kyr—1 Myr • There is one basic phenomenological cooling concept (but many physical realizations) • Main cooling regulator: neutrino luminosity function • Warmest observed stars are low-massive; their neutrino luminosity seems to be <= 1/30 of modified ...
... Ordinary cooling isolates neutron stars of age 1 kyr—1 Myr • There is one basic phenomenological cooling concept (but many physical realizations) • Main cooling regulator: neutrino luminosity function • Warmest observed stars are low-massive; their neutrino luminosity seems to be <= 1/30 of modified ...
HWWS 2010 - Monash University
... • Latter two are both likely classes of magnetars, (possibly young) systems with extremely high magnetic fields 1014– 1015 G • Compact central objects (CCOs) about which very little is known, associated with supernova remnants Galloway, “Accreting Neutron Stars – tiny Galactic Powerhouses” ...
... • Latter two are both likely classes of magnetars, (possibly young) systems with extremely high magnetic fields 1014– 1015 G • Compact central objects (CCOs) about which very little is known, associated with supernova remnants Galloway, “Accreting Neutron Stars – tiny Galactic Powerhouses” ...
Understanding Mass-Loss and the Late Evolution of Intermediate
... AGB stars, with huge momentum-excesses which showed that these winds are not radiatively driven (e.g. Bujarrabal et al. 2001, Sahai et al. 2006). Using STIS/HST, a carbon star, V Hya, has been “caught in the act” of ejecting a very fast (250 km s−1 ), highly collimated blobby outflow (Sahai et al. 2 ...
... AGB stars, with huge momentum-excesses which showed that these winds are not radiatively driven (e.g. Bujarrabal et al. 2001, Sahai et al. 2006). Using STIS/HST, a carbon star, V Hya, has been “caught in the act” of ejecting a very fast (250 km s−1 ), highly collimated blobby outflow (Sahai et al. 2 ...
multiwavelength observations of the gamma-ray
... Blazars (BL Lac objects and gamma-ray loud flat spectrum radio quasars (FSRQs)) are the most extreme type of active galactic nuclei (AGNs). They were historically defined through extreme flux variability throughout the electromagnetic spectrum, and sometimes strong and variable linear polarization a ...
... Blazars (BL Lac objects and gamma-ray loud flat spectrum radio quasars (FSRQs)) are the most extreme type of active galactic nuclei (AGNs). They were historically defined through extreme flux variability throughout the electromagnetic spectrum, and sometimes strong and variable linear polarization a ...
Point Spread Function of real Wolter-I X-ray mirrors
... where α is the grazing incidence angle of X-rays, should be classified as roughness. Fourier components exceeding this limit should instead contribute to the geometric errors. Although reasonable, this criterion can apparently be applied only to a discrete power spectrum. In addition, it seems more l ...
... where α is the grazing incidence angle of X-rays, should be classified as roughness. Fourier components exceeding this limit should instead contribute to the geometric errors. Although reasonable, this criterion can apparently be applied only to a discrete power spectrum. In addition, it seems more l ...
X-ray astronomy
X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray observation and detection from astronomical objects. X-radiation is absorbed by the Earth's atmosphere, so instruments to detect X-rays must be taken to high altitude by balloons, sounding rockets, and satellites. X-ray astronomy is the space science related to a type of space telescope that can see farther than standard light-absorption telescopes, such as the Mauna Kea Observatories, via x-ray radiation.X-ray emission is expected from astronomical objects that contain extremely hot gasses at temperatures from about a million kelvin (K) to hundreds of millions of kelvin (MK). Although X-rays have been observed emanating from the Sun since the 1940s, the discovery in 1962 of the first cosmic X-ray source was a surprise. This source is called Scorpius X-1 (Sco X-1), the first X-ray source found in the constellation Scorpius. The X-ray emission of Scorpius X-1 is 10,000 times greater than its visual emission, whereas that of the Sun is about a million times less. In addition, the energy output in X-rays is 100,000 times greater than the total emission of the Sun in all wavelengths. Based on discoveries in this new field of X-ray astronomy, starting with Scorpius X-1, Riccardo Giacconi received the Nobel Prize in Physics in 2002. It is now known that such X-ray sources as Sco X-1 are compact stars, such as neutron stars or black holes. Material falling into a black hole may emit X-rays, but the black hole itself does not. The energy source for the X-ray emission is gravity. Infalling gas and dust is heated by the strong gravitational fields of these and other celestial objects.Many thousands of X-ray sources are known. In addition, the space between galaxies in galaxy clusters is filled with a very hot, but very dilute gas at a temperature between 10 and 100 megakelvins (MK). The total amount of hot gas is five to ten times the total mass in the visible galaxies.