![Binarity in carbon-enhanced metal-poor stars](http://s1.studyres.com/store/data/016473745_1-af325cfb29322a9fff97bbf5c534dd5e-300x300.png)
Binarity in carbon-enhanced metal-poor stars
... Pb absorption lines are very weak and the strongest line in the optical overlaps with the CH feature, this hypothesis is difficult to test, especially in C-rich stars. A robust upper limit could nonetheless be given for the brightest CEMP-no star, BD +44-493, which did not show the predicted overabu ...
... Pb absorption lines are very weak and the strongest line in the optical overlaps with the CH feature, this hypothesis is difficult to test, especially in C-rich stars. A robust upper limit could nonetheless be given for the brightest CEMP-no star, BD +44-493, which did not show the predicted overabu ...
Read Claudia`s PhD thesis
... The Galactic globular cluster NGC 2419, one of the brightest and most distant cluster in the MW halo, is a metal poor Oosterhoff type II system suspected to be the relic of an extragalactic system accreted by the MW (see e.g. Mackey & van den Bergh, 2005, and reference therein). We have obtained tim ...
... The Galactic globular cluster NGC 2419, one of the brightest and most distant cluster in the MW halo, is a metal poor Oosterhoff type II system suspected to be the relic of an extragalactic system accreted by the MW (see e.g. Mackey & van den Bergh, 2005, and reference therein). We have obtained tim ...
Infrared Photometry of Red Supergiants in Young Clusters in the
... discussion has relied upon these IR colours and the B−V colours of Robertson (1974). The observed properties of the RSG population has featured prominently in many of the subsequent discussions of the evolutionary implications of the populations of these clusters. Many of these discussions have to s ...
... discussion has relied upon these IR colours and the B−V colours of Robertson (1974). The observed properties of the RSG population has featured prominently in many of the subsequent discussions of the evolutionary implications of the populations of these clusters. Many of these discussions have to s ...
An improved classification of B[e]-type stars
... Geisel (1970), Wackerling (1970), Allen & Swings (1972, 1976) and Ciatti et al. (1974). The stars were sometimes indicated as ”BQ[ ] stars”, were the ”Q” indicates abnormal spectra with forbidden lines. Most authors noticed that the stars also show strong permitted lines, such as the Balmer lines, a ...
... Geisel (1970), Wackerling (1970), Allen & Swings (1972, 1976) and Ciatti et al. (1974). The stars were sometimes indicated as ”BQ[ ] stars”, were the ”Q” indicates abnormal spectra with forbidden lines. Most authors noticed that the stars also show strong permitted lines, such as the Balmer lines, a ...
Cosmic Evolution of Black Holes and Spheroids. I: The M_BH
... The third approach consists of measuring directly the evolution of scaling laws over cosmic time. The main obstacle to overcome to reach this goal is the determination of the BH mass at distances where the sphere of influence (with a radius ∼ GMBH σ −2 ) cannot be resolved. This approach is thus lim ...
... The third approach consists of measuring directly the evolution of scaling laws over cosmic time. The main obstacle to overcome to reach this goal is the determination of the BH mass at distances where the sphere of influence (with a radius ∼ GMBH σ −2 ) cannot be resolved. This approach is thus lim ...
Luminosity profiles and sizes of massive star clusters in NGC 7252
... remnant NGC 7252. In particular, we focus on the surface brightness profiles and effective radii Reff of 36 young massive clusters (YMCs) within the galaxy. All the clusters have masses exceeding 105 M and are, despite the 64 Mpc distance to the galaxy, (partly) resolved on the HST images. Effectiv ...
... remnant NGC 7252. In particular, we focus on the surface brightness profiles and effective radii Reff of 36 young massive clusters (YMCs) within the galaxy. All the clusters have masses exceeding 105 M and are, despite the 64 Mpc distance to the galaxy, (partly) resolved on the HST images. Effectiv ...
The Properties of Super Star Clusters in A Sample of
... “Super star clusters” are the most massive extreme in the continuum of young star clusters. In this thesis, I examine the properties of such super star clusters in a sample of starburst galaxies with space and ground-based observations and in the optical, mid-infrared, and radio regimes. Using optic ...
... “Super star clusters” are the most massive extreme in the continuum of young star clusters. In this thesis, I examine the properties of such super star clusters in a sample of starburst galaxies with space and ground-based observations and in the optical, mid-infrared, and radio regimes. Using optic ...
CO emissions from optically selected galaxies at z ∼0.1–0.2: Tight
... population gets older. Kauffmann et al. (2003) investigated the mean stellar age and star-formation history statistically using SDSS data combined with model calculations. They showed that Dn (4000) constrains the mean stellar age of galaxies as described above and that the Balmer absorptionline ind ...
... population gets older. Kauffmann et al. (2003) investigated the mean stellar age and star-formation history statistically using SDSS data combined with model calculations. They showed that Dn (4000) constrains the mean stellar age of galaxies as described above and that the Balmer absorptionline ind ...
Angular momentum and the formation of stars and
... momentum, and it may be especially so for black holes in galactic nuclei because they are smaller than stars in relation to the size of the system in which they form. The masses that massive stars and central black holes can attain may therefore be limited by the efficiency with which angular moment ...
... momentum, and it may be especially so for black holes in galactic nuclei because they are smaller than stars in relation to the size of the system in which they form. The masses that massive stars and central black holes can attain may therefore be limited by the efficiency with which angular moment ...
Stellar dust production and composition in the Magellanic Clouds F. Kemper
... first incarnation of the SAGE-LMC point source catalogue (Meixner et al., 2006) contained about 4 million sources, of which ∼820,000 point sources have a J and [3.6] magnitude measurement, mostly consisting of Red Giant Branch (RGB) stars (∼650,000), which are not considered significant contributors ...
... first incarnation of the SAGE-LMC point source catalogue (Meixner et al., 2006) contained about 4 million sources, of which ∼820,000 point sources have a J and [3.6] magnitude measurement, mostly consisting of Red Giant Branch (RGB) stars (∼650,000), which are not considered significant contributors ...
GoldCreation
... One of my favorite astronomy-themed t-shirts says “You are star dust”. It makes the point that we are all made from long dead stars. Of course, everything around us is also made of star stuff. This even includes rare elements such as gold. This paper discusses the processes of gold formation. Most m ...
... One of my favorite astronomy-themed t-shirts says “You are star dust”. It makes the point that we are all made from long dead stars. Of course, everything around us is also made of star stuff. This even includes rare elements such as gold. This paper discusses the processes of gold formation. Most m ...
Globular Cluster Bimodality in Isolated Elliptical Galaxies
... while Fornax dwarf spheroidal has 5 GCs (Kissler-Patig et al. 1997; Ashman & Zepf 1998). Fig. 1 shows the GC ω Centauri, the largest and brightest GC orbiting the MW. Most GCs probably formed at the same time as their host galaxies (Brodie & Strader 2006). Since they are the oldest objects that surv ...
... while Fornax dwarf spheroidal has 5 GCs (Kissler-Patig et al. 1997; Ashman & Zepf 1998). Fig. 1 shows the GC ω Centauri, the largest and brightest GC orbiting the MW. Most GCs probably formed at the same time as their host galaxies (Brodie & Strader 2006). Since they are the oldest objects that surv ...
Galaxy Pairs in the Sloan Digital Sky Survey
... redshifts. The final value of log Σ is the average of the spectroscopic redshift value and the value calculated with the inclusion of photometric redshifts (see Baldry et al 2006 for further discussion). We note that the distances to the 4th and 5th nearest neighbours are large (≫ 500 h−1 70 kpc) co ...
... redshifts. The final value of log Σ is the average of the spectroscopic redshift value and the value calculated with the inclusion of photometric redshifts (see Baldry et al 2006 for further discussion). We note that the distances to the 4th and 5th nearest neighbours are large (≫ 500 h−1 70 kpc) co ...
Asteroid Rotation Periods
... of a magnitude have been used. Even higher precision can be used, but this is not justified for measurements made by the eye alone, since the accuracy is about ½mag, and this is why the magnitude scale at first had only integer values. However today with the use of electronic sensors it is possible ...
... of a magnitude have been used. Even higher precision can be used, but this is not justified for measurements made by the eye alone, since the accuracy is about ½mag, and this is why the magnitude scale at first had only integer values. However today with the use of electronic sensors it is possible ...
Astrometric accuracy during the past 2000 years
... detailed comparisons, but it is difficult in many cases, if at all possible, to find sufficient information about this matter, and it cannot easily be presented in one line of a table. Internal errors are sometimes placed in brackets. The standard errors in the tables are sufficient for the original ...
... detailed comparisons, but it is difficult in many cases, if at all possible, to find sufficient information about this matter, and it cannot easily be presented in one line of a table. Internal errors are sometimes placed in brackets. The standard errors in the tables are sufficient for the original ...
WAS THE SUN BORN IN A MASSIVE CLUSTER?
... stars, on the basis that, in a larger cluster, close encounters between the Sun and other stars would have truncated the outer solar system or excited the outer planets into eccentric orbits. However, this dynamical limit is in tension with meteoritic evidence that the solar system was exposed to a ...
... stars, on the basis that, in a larger cluster, close encounters between the Sun and other stars would have truncated the outer solar system or excited the outer planets into eccentric orbits. However, this dynamical limit is in tension with meteoritic evidence that the solar system was exposed to a ...
The Secular and Rotational Brightness Variations of Neptune
... and Venus (Mallama et al. 2006) were observed with the Solar and Heliospheric Observatory satellite. The SOHO magnitudes augmented ground-based observations at illumination phases where the planets are too near the Sun to observe through the atmosphere. Mercury was found to have a very strong bright ...
... and Venus (Mallama et al. 2006) were observed with the Solar and Heliospheric Observatory satellite. The SOHO magnitudes augmented ground-based observations at illumination phases where the planets are too near the Sun to observe through the atmosphere. Mercury was found to have a very strong bright ...
Hot Horizontal Branch Stars in the Galactic Bulge. I
... photometry. Reddening proved highly variable, with E(B − V ) ranging from 0.0 to 0.55 around a mean of 0.28. The B − V colors of cool HB stars of solar metallicity reddenened by E(B − V ) ≥ 0.3 overlap those of foreground main-sequence stars, but the U − B vs. B − V diagram distinguishes these group ...
... photometry. Reddening proved highly variable, with E(B − V ) ranging from 0.0 to 0.55 around a mean of 0.28. The B − V colors of cool HB stars of solar metallicity reddenened by E(B − V ) ≥ 0.3 overlap those of foreground main-sequence stars, but the U − B vs. B − V diagram distinguishes these group ...
On the evolution and fate of supermassive stars
... Returning to the problem of IMBH formation, there are currently two models in favour. One involves the gradual accumulation of mass by accretion onto a seed black hole, which, while swallowing gas and stars in a stellar cluster, may grow to the intermediate mass range (see, e.g., Miller & Colbert 20 ...
... Returning to the problem of IMBH formation, there are currently two models in favour. One involves the gradual accumulation of mass by accretion onto a seed black hole, which, while swallowing gas and stars in a stellar cluster, may grow to the intermediate mass range (see, e.g., Miller & Colbert 20 ...
Chemical composition of 90 F and G disk dwarfs
... of 189 F and G dwarfs with −1.1 < [Fe/H] < 0.25 by Edvardsson et al. (1993a, hereafter EAGLNT). The main results from this work may be summarized as follows: (1) There are no tight relations between age, metallicity and kinematics of disk stars, but substantial dispersions imposed on weak statistica ...
... of 189 F and G dwarfs with −1.1 < [Fe/H] < 0.25 by Edvardsson et al. (1993a, hereafter EAGLNT). The main results from this work may be summarized as follows: (1) There are no tight relations between age, metallicity and kinematics of disk stars, but substantial dispersions imposed on weak statistica ...
PLANETS AND INFRARED EXCESSES: PRELIMINARY RESULTS
... might harbor both planets and extended dust emission has still not been verified. The aim of this paper is to use the MIPS on Spitzer (Rieke et al. 2004) to directly address this outstanding issue by searching for excess IR emission from known planetbearing stars. MIPS provides unprecedented sensiti ...
... might harbor both planets and extended dust emission has still not been verified. The aim of this paper is to use the MIPS on Spitzer (Rieke et al. 2004) to directly address this outstanding issue by searching for excess IR emission from known planetbearing stars. MIPS provides unprecedented sensiti ...
Question paper - Unit A141/01 - Modules B1, C1, P1
... Complete the sentences about chromosomes by choosing the correct words from this list. Each word may be used once, more than once or not at all. nucleus DNA genes protein Chromosomes are made from a chemical called ..................................... . Chromosomes in a pair always carry the same . ...
... Complete the sentences about chromosomes by choosing the correct words from this list. Each word may be used once, more than once or not at all. nucleus DNA genes protein Chromosomes are made from a chemical called ..................................... . Chromosomes in a pair always carry the same . ...
Progenitors and Hydrodynamics of Type II and lb Supernovae
... ilar to that accompanying iron core collapse in larger stars, but with some observational distinctions. First, the density gradient at the edge of the ONeMg core is very steep. Little 56 Ni will be produced. Mayle & Wilson (1988) calculate ~0.002 M 0 of 56 Ni for a model of this sort. Also the envel ...
... ilar to that accompanying iron core collapse in larger stars, but with some observational distinctions. First, the density gradient at the edge of the ONeMg core is very steep. Little 56 Ni will be produced. Mayle & Wilson (1988) calculate ~0.002 M 0 of 56 Ni for a model of this sort. Also the envel ...
The UV properties of E+ A galaxies: constraints on feedback
... nearby galaxies, we use simple energetic arguments to show that the bimodal behaviour of the quenching efficiency is consistent with AGN and supernovae (SN) being the principal sources of negative feedback above and below M ∼ 1010 M⊙ respectively. The arguments assume that quenching occurs through t ...
... nearby galaxies, we use simple energetic arguments to show that the bimodal behaviour of the quenching efficiency is consistent with AGN and supernovae (SN) being the principal sources of negative feedback above and below M ∼ 1010 M⊙ respectively. The arguments assume that quenching occurs through t ...
arXiv:astro-ph/9909369 v1 22 Sep 1999
... Without expanding on the nature of the dust giving rise to this family of bands, it is worthwhile to list a few properties that ISO has now firmly established. Even at the high resolution of the ISOSWS, the bands do not break up into a family of lines (as suggested e.g. by Léger et al., 1989). In f ...
... Without expanding on the nature of the dust giving rise to this family of bands, it is worthwhile to list a few properties that ISO has now firmly established. Even at the high resolution of the ISOSWS, the bands do not break up into a family of lines (as suggested e.g. by Léger et al., 1989). In f ...
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.