Dust input from AGB stars in the Large Magellanic Cloud
... dust-to-gas ratio in the outflows of O-rich stars with metallicities Z = 0.001 and 0.004 are below 10−5 and are not shown here. These values are probably too low, because these models may underestimate the efficiency of dust condensation in stellar outflows from M-stars with low mass-loss rates, as ...
... dust-to-gas ratio in the outflows of O-rich stars with metallicities Z = 0.001 and 0.004 are below 10−5 and are not shown here. These values are probably too low, because these models may underestimate the efficiency of dust condensation in stellar outflows from M-stars with low mass-loss rates, as ...
A tale of two galaxies: light and mass in NGC 891 and NGC 7814
... not known inside 1 arcmin (3−4 kpc) because H I emission was not detected there. The conclusion was that “if the distribution of luminous matter were in any way related to the total mass distribution it would not be possible for the disk-dominated and the bulge-dominated galaxies to have such simila ...
... not known inside 1 arcmin (3−4 kpc) because H I emission was not detected there. The conclusion was that “if the distribution of luminous matter were in any way related to the total mass distribution it would not be possible for the disk-dominated and the bulge-dominated galaxies to have such simila ...
Galaxy Zoo: Are bars responsible for the feeding
... Section 6. Throughout this paper, we assume a flat cosmological model with H0 = 70 km s−1 Mpc−1 , m = 0.30, and = 0.70, and all magnitudes are given in the AB magnitude system. 2 DATA In this section, we briefly describe the three surveys and their respective data products that are used in this ...
... Section 6. Throughout this paper, we assume a flat cosmological model with H0 = 70 km s−1 Mpc−1 , m = 0.30, and = 0.70, and all magnitudes are given in the AB magnitude system. 2 DATA In this section, we briefly describe the three surveys and their respective data products that are used in this ...
Fraction of the X-ray selected AGNs with optical emission lines in
... based on precise photometric redshifts (Ilbert et al. 2009; Allevato et al. 2012). These galaxies satisfy zph < 1.2 and I(F814W) < 24.2 mag, and require a 3σ detection in the Ks band for the stellar mass estimation, which is complete to a typical depth of Ks = 24. With LX − M scaling relation calibr ...
... based on precise photometric redshifts (Ilbert et al. 2009; Allevato et al. 2012). These galaxies satisfy zph < 1.2 and I(F814W) < 24.2 mag, and require a 3σ detection in the Ks band for the stellar mass estimation, which is complete to a typical depth of Ks = 24. With LX − M scaling relation calibr ...
Analysis of cool DO-type white dwarfs from the Sloan Digital Sky
... absorption lines. Our non-LTE model atmosphere analyses of these objects and two not previously analyzed hot-wind DO WDs, revealed effective temperatures and gravities in the ranges T eff = 45−80 kK and log g = 7.50−8.75. In eight of the spectra we found traces of C (0.001−0.01, by mass). Two of these ...
... absorption lines. Our non-LTE model atmosphere analyses of these objects and two not previously analyzed hot-wind DO WDs, revealed effective temperatures and gravities in the ranges T eff = 45−80 kK and log g = 7.50−8.75. In eight of the spectra we found traces of C (0.001−0.01, by mass). Two of these ...
09-03-08_Meixner
... – Dominated by imaging and photometry – What are these newly discovered sources? Need spectroscopy…. ...
... – Dominated by imaging and photometry – What are these newly discovered sources? Need spectroscopy…. ...
Harikane
... high significance levels. • Systemic redshift is z=1.1800±0.0002 • These lines appear to have two Harikane+14 components. ...
... high significance levels. • Systemic redshift is z=1.1800±0.0002 • These lines appear to have two Harikane+14 components. ...
Annual Report 2012
... Chapter 1. Review of major events spectra they discovered the imprint of sugar molecules, showing that essential building blocks of life can be formed around young stars. Much progress has also been made in studying the distant Universe. Rychard Bouwens, Ivo Labbé and Marijn Franx have led several ...
... Chapter 1. Review of major events spectra they discovered the imprint of sugar molecules, showing that essential building blocks of life can be formed around young stars. Much progress has also been made in studying the distant Universe. Rychard Bouwens, Ivo Labbé and Marijn Franx have led several ...
The Emission Line Spectrum of Active Galactic
... (H I, He I λλ5876,6678,7065, He II λ4686 and Fe II in the visible domain). The narrow-line spectra of Seyfert 1s are very similar to those of Seyfert 2s; there are however significant differences, most notably much stronger high- ionization lines ([Fe VII]λ6087, [Fe X]λ6375, [Fe XI]λ7892) in some Se ...
... (H I, He I λλ5876,6678,7065, He II λ4686 and Fe II in the visible domain). The narrow-line spectra of Seyfert 1s are very similar to those of Seyfert 2s; there are however significant differences, most notably much stronger high- ionization lines ([Fe VII]λ6087, [Fe X]λ6375, [Fe XI]λ7892) in some Se ...
Neutron Stars and the Determination of the Dense Matter Equation
... A physical understanding of the behaviour of cold ultra-dense matter – at and above nuclear density – can only be achieved by the study of neutron stars. The surface thermal emission from neutron stars in quiescent low-mass X-ray binaries (qLMXBs) inside globular clusters has proven useful for that ...
... A physical understanding of the behaviour of cold ultra-dense matter – at and above nuclear density – can only be achieved by the study of neutron stars. The surface thermal emission from neutron stars in quiescent low-mass X-ray binaries (qLMXBs) inside globular clusters has proven useful for that ...
review - hrsbstaff.ednet.ns.ca
... c) Another formula for the Richter scale is based upon the energy, E, in kilowatt hours, released by the earthquake, R 0.67 log( 0.37 E ) 1.46 where R is the Richter magnitude. A 1906 earthquake in San Francisco measured 7.90 on the Richter scale. How much energy was released by this earthquake? ...
... c) Another formula for the Richter scale is based upon the energy, E, in kilowatt hours, released by the earthquake, R 0.67 log( 0.37 E ) 1.46 where R is the Richter magnitude. A 1906 earthquake in San Francisco measured 7.90 on the Richter scale. How much energy was released by this earthquake? ...
The Spatial Distribution of Satellite Galaxies Ing´olfur ´ Ag´ ustsson
... ∼ 30% of the MRS host galaxies are classified as ellipticals, while the rest are classified as disk galaxies (either spiral or lenticular). See AB10 and De Lucia et al. (2006) for details of the classification scheme. In addition, we divide our sample of theoretical host galaxies according to their ...
... ∼ 30% of the MRS host galaxies are classified as ellipticals, while the rest are classified as disk galaxies (either spiral or lenticular). See AB10 and De Lucia et al. (2006) for details of the classification scheme. In addition, we divide our sample of theoretical host galaxies according to their ...
Understanding Variable Stars - Central Florida Astronomical Society
... 2.2 The globular cluster M14, showing a Population II Cepheid variable star at maximum (left) and minimum (right) brightness 18 2.3 Cepheid variable stars discovered by E.P. Hubble (the numbered stars) in the nearby spiral galaxy M33 20 2.4 The proper motion is the annual angular (apparent) motion o ...
... 2.2 The globular cluster M14, showing a Population II Cepheid variable star at maximum (left) and minimum (right) brightness 18 2.3 Cepheid variable stars discovered by E.P. Hubble (the numbered stars) in the nearby spiral galaxy M33 20 2.4 The proper motion is the annual angular (apparent) motion o ...
Galaxy Evolution Over the Past Eleven Billion Years: Mergers and
... for being so helpful and accommodating. I thank Stefan for giving me an opportunity to observe on La Palma and in Chile, and Martin for commenting on parts of this thesis. I would like to thank Dave and Josh for hosting my six-month visit at IfA Hawaii. During my stay, I have learnt a lot about far- ...
... for being so helpful and accommodating. I thank Stefan for giving me an opportunity to observe on La Palma and in Chile, and Martin for commenting on parts of this thesis. I would like to thank Dave and Josh for hosting my six-month visit at IfA Hawaii. During my stay, I have learnt a lot about far- ...
Classical Be Stars: Rapidly Rotating B Stars with Viscous Keplerian
... forming a decretion disk2 , which more precisely is an outwardly diffusing gaseous Keplerian disk. This disk if fed by mass ejected from the central star, and its further fate, after formation, is governed by viscosity. That said, our knowledge of processes is far from complete, and very important p ...
... forming a decretion disk2 , which more precisely is an outwardly diffusing gaseous Keplerian disk. This disk if fed by mass ejected from the central star, and its further fate, after formation, is governed by viscosity. That said, our knowledge of processes is far from complete, and very important p ...
THE FUTURE IS NOW: THE FORMATION OF SINGLE LOW
... cooling curve age bins and divided the observed number in each mass bin by the lifetime in each bin. This provides an observational test of incompleteness, in the sense that if cooler WDs are missed in the survey, artificially low formation rates would be derived from older and cooler WDs. This is c ...
... cooling curve age bins and divided the observed number in each mass bin by the lifetime in each bin. This provides an observational test of incompleteness, in the sense that if cooler WDs are missed in the survey, artificially low formation rates would be derived from older and cooler WDs. This is c ...
Direct Evidence for Termination of Obscured Star Formation by
... Xu et al. 2002; Peterson & Fabian 2006), (2) the difficulties that early semi-analytic models faced in reproducing the large number of IR-luminous galaxies observed at high redshift (e.g. Baugh et al. 2005), and (3) the expectation that the mass return rate from stars would cause central SMBHs to be ...
... Xu et al. 2002; Peterson & Fabian 2006), (2) the difficulties that early semi-analytic models faced in reproducing the large number of IR-luminous galaxies observed at high redshift (e.g. Baugh et al. 2005), and (3) the expectation that the mass return rate from stars would cause central SMBHs to be ...
constellations - Richmond and Glen Allen Weather
... were derived from mankind's attempt to bring order to the chaos of stars above them. They also realized the celestial objects of the night sky were beyond the control of mankind and associated the heavens with religion. Observational astronomy and familiarity with the night sky today is limited for ...
... were derived from mankind's attempt to bring order to the chaos of stars above them. They also realized the celestial objects of the night sky were beyond the control of mankind and associated the heavens with religion. Observational astronomy and familiarity with the night sky today is limited for ...
The effects of galaxy interactions on star formation
... older, though the data in this part of the system are too limited to draw firm conclusions. The ages of the giant H ii regions in NGC 7714 are generally older than those of their constituent clusters, possibly indicating that the young clusters we detect are surrounded by their dispersed predecessor ...
... older, though the data in this part of the system are too limited to draw firm conclusions. The ages of the giant H ii regions in NGC 7714 are generally older than those of their constituent clusters, possibly indicating that the young clusters we detect are surrounded by their dispersed predecessor ...
Galaxy And Mass Assembly (GAMA): Gas Fuelling of Spiral Galaxies
... While a small minority of the group satellites are strongly quenched, the group centrals, and the large majority of satellites, exhibit levels of ψ∗ statistically indistinguishable from their field counterparts, for all M∗ , albeit with a higher scatter of 0.44 dex about the field reference relation ...
... While a small minority of the group satellites are strongly quenched, the group centrals, and the large majority of satellites, exhibit levels of ψ∗ statistically indistinguishable from their field counterparts, for all M∗ , albeit with a higher scatter of 0.44 dex about the field reference relation ...
Star formation in quasar hosts and the origin of radio emission in
... Our goal is to assemble a large sample of quasars (whether optically obscured or unobscured) for which the host star formation rates can be usefully constrained with existing archival data. Furthermore, because of the sensitivity of the existing radio surveys, in order to probe the radio-quiet popul ...
... Our goal is to assemble a large sample of quasars (whether optically obscured or unobscured) for which the host star formation rates can be usefully constrained with existing archival data. Furthermore, because of the sensitivity of the existing radio surveys, in order to probe the radio-quiet popul ...
H-alpha Imaging of Early-type (Sa
... massive star formation rates increase along the Hubble sequence from Sa to Sc(Kennicutt 1983; Kennicutt et al. 1994). Part of the problem is that the sample of early-type spirals selected by Kennicutt (1983) and Kennicutt (1994) is small in number and is biased towards galaxies with low values of L( ...
... massive star formation rates increase along the Hubble sequence from Sa to Sc(Kennicutt 1983; Kennicutt et al. 1994). Part of the problem is that the sample of early-type spirals selected by Kennicutt (1983) and Kennicutt (1994) is small in number and is biased towards galaxies with low values of L( ...
Fundamentals of Stellar Evolution Theory: Understanding the HRD
... stars lighter than MHeF quiescently burn helium in a convective core. Their position on the HB depends on several factors, among which the metallicity and the mass of the H-rich envelope dominate, the latter reduced by mass loss from the red giant precursor. For metal-rich stars, the core He-burning ...
... stars lighter than MHeF quiescently burn helium in a convective core. Their position on the HB depends on several factors, among which the metallicity and the mass of the H-rich envelope dominate, the latter reduced by mass loss from the red giant precursor. For metal-rich stars, the core He-burning ...
THE DEMOGRAPHICS OF LONG-PERIOD COMETS ABSTRACT
... were most likely either not real to begin with or fastmoving objects only visible for a short window of time. Secondly, some comets might have been inactive at these large heliocentric distances, and hence classified as minor planets. The minor planet centre database was checked for non-cometary obje ...
... were most likely either not real to begin with or fastmoving objects only visible for a short window of time. Secondly, some comets might have been inactive at these large heliocentric distances, and hence classified as minor planets. The minor planet centre database was checked for non-cometary obje ...
Some Constraints on the Effects of Age and Metallicity - UvA-DARE
... 4472 (Kundu, Maccarone, & Zepf 2002, hereafter KMZ; Maccarone, Kundu, & Zepf 2003, hereafter MKZ). LMXBs are formed especially efficiently in globular clusters (GCs), most likely because of dynamical interactions in the core (Clark 1975; Fabian, Pringle, & Rees 1975). In the Galaxy, GCs account for ...
... 4472 (Kundu, Maccarone, & Zepf 2002, hereafter KMZ; Maccarone, Kundu, & Zepf 2003, hereafter MKZ). LMXBs are formed especially efficiently in globular clusters (GCs), most likely because of dynamical interactions in the core (Clark 1975; Fabian, Pringle, & Rees 1975). In the Galaxy, GCs account for ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.