Composition-Tunable Properties Of CdSxTe1
... the quantum yield of NC colloids was maximized. Characterization. UV-vis absorption and photoluminescence (PL) spectra were recorded using a CARY 50 scan spectrometer and a Jobin Yvon Flurolog FL3-11 fluorescence spectrophotometer. PL quantum yield of sufficiently dilute nanocrystal suspensions was ...
... the quantum yield of NC colloids was maximized. Characterization. UV-vis absorption and photoluminescence (PL) spectra were recorded using a CARY 50 scan spectrometer and a Jobin Yvon Flurolog FL3-11 fluorescence spectrophotometer. PL quantum yield of sufficiently dilute nanocrystal suspensions was ...
Equations of state and structure of neutron stars
... see by our eyes or telescopes. When the life of the stars is approaching end, i.e., when the pressure gradient can not balance the gravity any more, the interior of the stars starts to collapse and different products can be formed. The star can collapse to a white dwarf, neutron star or black hole∗ ...
... see by our eyes or telescopes. When the life of the stars is approaching end, i.e., when the pressure gradient can not balance the gravity any more, the interior of the stars starts to collapse and different products can be formed. The star can collapse to a white dwarf, neutron star or black hole∗ ...
Miguel Pereira Santaella
... HF dissociated by intense UV radiation and reformed rapidly χ > 107 and high density nH2 > 107 cm-3 Possible close to the AGN ...
... HF dissociated by intense UV radiation and reformed rapidly χ > 107 and high density nH2 > 107 cm-3 Possible close to the AGN ...
Star Formation and Young Clusters in Cygnus
... based on the star count data by Dobashi et al. (2005). The figure shows the Galactic plane between longitudes 67◦ and 100◦ . The Great Cygnus Rift is most prominent to the right, and the 10 degree large Cygnus X region provides the highest extinction in the whole field. The North America nebula is i ...
... based on the star count data by Dobashi et al. (2005). The figure shows the Galactic plane between longitudes 67◦ and 100◦ . The Great Cygnus Rift is most prominent to the right, and the 10 degree large Cygnus X region provides the highest extinction in the whole field. The North America nebula is i ...
Environment and self-regulation in galaxy formation
... The kinematics of gas and stars are determined for all 48,023 objects, using the code GANDALF developed by Sarzi et al. (2006). Stellar population and emission line templates are fitted simultaneously to the galaxy spectrum. The outcome are emission line fluxes and kinematics of the gas. On the stel ...
... The kinematics of gas and stars are determined for all 48,023 objects, using the code GANDALF developed by Sarzi et al. (2006). Stellar population and emission line templates are fitted simultaneously to the galaxy spectrum. The outcome are emission line fluxes and kinematics of the gas. On the stel ...
Early-type dwarf galaxies in clusters - ARI
... 3.2 Relations with luminosity A fundamental characteristic of early-type galaxies is the well-defined relation between colour and magnitude, with more luminous objects having redder colours (e.g. Caldwell, 1983; Sandage & Visvanathan, 1978). While this trend includes the dEs, there has been disagree ...
... 3.2 Relations with luminosity A fundamental characteristic of early-type galaxies is the well-defined relation between colour and magnitude, with more luminous objects having redder colours (e.g. Caldwell, 1983; Sandage & Visvanathan, 1978). While this trend includes the dEs, there has been disagree ...
Evidence of suppression of star formation by quasar
... lines, polycyclic aromatic hydrocarbon (PAH) features and mid- and far-infrared luminosities (Kennicutt 1998a). In AGN, however, all these diagnostics can be severely affected by ionizing radiation by the AGN which introduces a large scatter to these calibrations. We utilize the least biased techniq ...
... lines, polycyclic aromatic hydrocarbon (PAH) features and mid- and far-infrared luminosities (Kennicutt 1998a). In AGN, however, all these diagnostics can be severely affected by ionizing radiation by the AGN which introduces a large scatter to these calibrations. We utilize the least biased techniq ...
formation of z 6 quasars from hierarchical
... 6 Nagoya University, Dept. of Physics, Nagoya, Aichi 464-8602, Japan and 7 Spitzer Fellow Accepted to ApJ ...
... 6 Nagoya University, Dept. of Physics, Nagoya, Aichi 464-8602, Japan and 7 Spitzer Fellow Accepted to ApJ ...
A fundamental metallicity relation for galaxies at z = 0.84–1.47 from
... FMOS H-Long (R = 2600) filter, to measure Hα 6563 Å and [N II] 6583Å line fluxes, and the J-Long (R = 1900) filter, to obtain the [O III] 5007Å and Hβ 4861 Å fluxes. Those in the secondary, z = 0.84, subsample are observed using the J-Long filter again to obtain Hα and [N II]. In total we observed s ...
... FMOS H-Long (R = 2600) filter, to measure Hα 6563 Å and [N II] 6583Å line fluxes, and the J-Long (R = 1900) filter, to obtain the [O III] 5007Å and Hβ 4861 Å fluxes. Those in the secondary, z = 0.84, subsample are observed using the J-Long filter again to obtain Hα and [N II]. In total we observed s ...
Zhu Qualifier Solutions - University of Toronto Astronomy
... 3.1.1. What is the IMF useful for? 3.1.2. Is there a universal IMF? 3.1.3. Why are the lower and upper limits of the IMF poorly understood compared to that of the middle (several M stars)? What constraints are there? 3.1.4. What’s the difference between a field and stellar cluster IMF? 3.1.5. How d ...
... 3.1.1. What is the IMF useful for? 3.1.2. Is there a universal IMF? 3.1.3. Why are the lower and upper limits of the IMF poorly understood compared to that of the middle (several M stars)? What constraints are there? 3.1.4. What’s the difference between a field and stellar cluster IMF? 3.1.5. How d ...
SN 2006gy: DISCOVERY OF THE MOST LUMINOUS
... peak visual magnitude of about 22, it is the most luminous supernova ever recorded. Its very slow rise to maximum took 70 days, and it stayed brighter than 21 mag for about 100 days. It is not yet clear what powers the enormous luminosity and the total radiated energy of 1051 erg, but we argue t ...
... peak visual magnitude of about 22, it is the most luminous supernova ever recorded. Its very slow rise to maximum took 70 days, and it stayed brighter than 21 mag for about 100 days. It is not yet clear what powers the enormous luminosity and the total radiated energy of 1051 erg, but we argue t ...
EUV and X-ray Spectroscopy of the Active Sun
... path of propagating electrons towards the dense chromosphere (c). Heating of the chromosphere results in chromospheric evaporation (d) which fills the loops with hot, SXR emitting plasma (e). Direct heating of the looptop can result in large pressure gradients that drive conductive fronts (f ). . . ...
... path of propagating electrons towards the dense chromosphere (c). Heating of the chromosphere results in chromospheric evaporation (d) which fills the loops with hot, SXR emitting plasma (e). Direct heating of the looptop can result in large pressure gradients that drive conductive fronts (f ). . . ...
STRUCTURAL CHARACTERISTICS AND STELLAR
... Table 2 contains the colors of those galaxies observed through all four UBV I lters. Each color has three entries. The rst is the color of the inner regions as measured through a small (1000 ) aperture. In some cases, this color represents a true color of the bulge component while in others it re ...
... Table 2 contains the colors of those galaxies observed through all four UBV I lters. Each color has three entries. The rst is the color of the inner regions as measured through a small (1000 ) aperture. In some cases, this color represents a true color of the bulge component while in others it re ...
from z=0 to z=1
... • IR-quiet UV galaxies (low metallicity dwarfs) • UVLGs and ULIRGs • LBGs and SCUBA galaxies: UV and IR galaxies at z ~ 3 • UV and IR galaxies at intermediate redshifts (0.5 < z < 0.7) --- early results from a GALEX/SWIRE comparison study • evolution of attenuation in UV and IR selected galaxies • e ...
... • IR-quiet UV galaxies (low metallicity dwarfs) • UVLGs and ULIRGs • LBGs and SCUBA galaxies: UV and IR galaxies at z ~ 3 • UV and IR galaxies at intermediate redshifts (0.5 < z < 0.7) --- early results from a GALEX/SWIRE comparison study • evolution of attenuation in UV and IR selected galaxies • e ...
A UV study of nearby luminous infrared galaxies: star formation
... morphologies is reliable) indicates that a small fraction (∼ 4%) have spheroidal or near-spheroidal morphologies and could be progenitors of elliptical galaxies. The remaining galaxies are morphologically late-type or ongoing mergers. 61% of the LIRGs do not show signs of interactions (at the depth ...
... morphologies is reliable) indicates that a small fraction (∼ 4%) have spheroidal or near-spheroidal morphologies and could be progenitors of elliptical galaxies. The remaining galaxies are morphologically late-type or ongoing mergers. 61% of the LIRGs do not show signs of interactions (at the depth ...
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 ...
The nature of the faint galaxies in the Hubble Deep Field
... further confirmed using the FOCAS/IRAF source identification package. Aperture photometry was then carried out with PHOTOM on all the identified galaxies, using an aperture size of O.5-arcsec radius. For 0.5 < z < 3, this corresponds to a linear diameter of 4.0 ± 0.4 (Ho/50)-1 kpc. The photometry ze ...
... further confirmed using the FOCAS/IRAF source identification package. Aperture photometry was then carried out with PHOTOM on all the identified galaxies, using an aperture size of O.5-arcsec radius. For 0.5 < z < 3, this corresponds to a linear diameter of 4.0 ± 0.4 (Ho/50)-1 kpc. The photometry ze ...
Diapositiva 1
... Slow pulsars with low magnetic fields are not observable as radio sources any more ...
... Slow pulsars with low magnetic fields are not observable as radio sources any more ...
Merging white dwarfs and thermonuclear supernovae
... Our alternative is that SN Ia result generally from mergers of carbon–oxygen white dwarfs, including those with sub-Chandrasekhar total mass [3]. Both theoretical [3] and empirical [24] rates are a factor 3 or so higher than near-Chandrasekhar rates, making them consistent with the SN Ia rate. Furth ...
... Our alternative is that SN Ia result generally from mergers of carbon–oxygen white dwarfs, including those with sub-Chandrasekhar total mass [3]. Both theoretical [3] and empirical [24] rates are a factor 3 or so higher than near-Chandrasekhar rates, making them consistent with the SN Ia rate. Furth ...
Jets and Outflows From Star to Cloud: Observations Confront Theory
... radius is often considered to be its co-rotation radius with the star. In the case of CTTSs, this energy is mainly observed in the UV-band (Gullbring et al. 2000), but direct observation of this UV excess can be difficult as it may be highly extincted, particularly in more embedded sources. Fortunat ...
... radius is often considered to be its co-rotation radius with the star. In the case of CTTSs, this energy is mainly observed in the UV-band (Gullbring et al. 2000), but direct observation of this UV excess can be difficult as it may be highly extincted, particularly in more embedded sources. Fortunat ...
The optical afterglow and z = 0.92 early
... Astrometry relative to the USNO-B catalog provides an absolute position for the optical afterglow of α =00h 45m 04.660s, δ =−01◦ 35′ 41.89′′ (J2000), with an uncertainty of 0.26′′ in each coordinate. This position is 1.5′′ away from the center of the XRT error circle, which has an uncertainty of 2.4 ...
... Astrometry relative to the USNO-B catalog provides an absolute position for the optical afterglow of α =00h 45m 04.660s, δ =−01◦ 35′ 41.89′′ (J2000), with an uncertainty of 0.26′′ in each coordinate. This position is 1.5′′ away from the center of the XRT error circle, which has an uncertainty of 2.4 ...
Evolution of high-redshift quasars
... Surveys such as the SDSS only sample the brightest end of the quasar luminosity function. Does fainter quasars and AGNs evolve differently at high-redshift? We know from the 2dF quasar survey that at low-redshift, quasar luminosity function is well fit by a double power law with pure luminosity evol ...
... Surveys such as the SDSS only sample the brightest end of the quasar luminosity function. Does fainter quasars and AGNs evolve differently at high-redshift? We know from the 2dF quasar survey that at low-redshift, quasar luminosity function is well fit by a double power law with pure luminosity evol ...
Heating and Cooling of Neutron Star Crusts
... With the launch of Chandra and XMM, many new and exciting observations of neutron stars are being made. Some of these observations have detected transient neutron stars cooling into quiescence. Transient neutron stars are a class of objects which are observed to go through accretion outburst periods ...
... With the launch of Chandra and XMM, many new and exciting observations of neutron stars are being made. Some of these observations have detected transient neutron stars cooling into quiescence. Transient neutron stars are a class of objects which are observed to go through accretion outburst periods ...
Here
... balance between formation on dust and self-shielding of H2 from photodissociation (Solomon & Wickramasinghe 1969) by the interstellar radiation field. This transition from atomic to molecular hydrogen at a moderate interstellar density means that all dense clouds are molecular. Molecular clouds are ...
... balance between formation on dust and self-shielding of H2 from photodissociation (Solomon & Wickramasinghe 1969) by the interstellar radiation field. This transition from atomic to molecular hydrogen at a moderate interstellar density means that all dense clouds are molecular. Molecular clouds are ...
Star formation in luminous quasar host galaxies at z = 1–2 ⋆
... 1982). Seyfert galaxies are frequently found with circumnuclear starbursts (Heckman et al. 1997; González Delgado, Heckman & Leitherer 2001; Gu et al. 2001; Cid Fernandes et al. 2004; Davies et al. 2007; Riffel et al. 2009). The presence of intermediate-age stellar populations has also been extensi ...
... 1982). Seyfert galaxies are frequently found with circumnuclear starbursts (Heckman et al. 1997; González Delgado, Heckman & Leitherer 2001; Gu et al. 2001; Cid Fernandes et al. 2004; Davies et al. 2007; Riffel et al. 2009). The presence of intermediate-age stellar populations has also been extensi ...
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.