Globular Cluster Bimodality in Isolated Elliptical Galaxies
... The relative number of GCs per unit magnitude of a GCS gives the GCLF which can be described by either a Gaussian or a t-distribution (df = 5) (Secker 1992). The GCLF is characterised by the dispersion and the turnover magnitude (TOM). GCLFs have a universal shape in all GCS studied, with an asymmet ...
... The relative number of GCs per unit magnitude of a GCS gives the GCLF which can be described by either a Gaussian or a t-distribution (df = 5) (Secker 1992). The GCLF is characterised by the dispersion and the turnover magnitude (TOM). GCLFs have a universal shape in all GCS studied, with an asymmet ...
the stebbins galaxy: the origins of interstellar medium studies
... Shapley was well aware that his cosmic conclusions were only valid if his distances to globular clusters were trustworthy, and his methods assumed that any interstellar absorption of starlight was negligible. For that reason he included a chapter on ―The Transparency of Space‖ in Star Clusters summa ...
... Shapley was well aware that his cosmic conclusions were only valid if his distances to globular clusters were trustworthy, and his methods assumed that any interstellar absorption of starlight was negligible. For that reason he included a chapter on ―The Transparency of Space‖ in Star Clusters summa ...
Variations in Integrated Galactic Initial Mass Functions due to
... clusters. These clusters follow a power-law mass function (the cluster mass function, CMF), which means that most stars form in low-mass clusters. In low-mass clusters there is a deficiency of massive stars (as the most massive star cannot exceed the total cluster mass), resulting in an integrated g ...
... clusters. These clusters follow a power-law mass function (the cluster mass function, CMF), which means that most stars form in low-mass clusters. In low-mass clusters there is a deficiency of massive stars (as the most massive star cannot exceed the total cluster mass), resulting in an integrated g ...
Luminosities and mass-loss rates of SMC and LMC AGB stars and
... Results. We derive (dust) mass-loss rates and luminosities for the entire sample. Based on luminosities, periods and amplitudes and colours, the O-rich stars are classified as foreground objects, AGB stars and Red Super Giants. For the O-rich stars silicates based on laboratory optical constants are ...
... Results. We derive (dust) mass-loss rates and luminosities for the entire sample. Based on luminosities, periods and amplitudes and colours, the O-rich stars are classified as foreground objects, AGB stars and Red Super Giants. For the O-rich stars silicates based on laboratory optical constants are ...
EROs and submm galaxies: Expectations for FMOS in the
... Can observe targets for an entire night (or longer) ...
... Can observe targets for an entire night (or longer) ...
Some Constraints on the Effects of Age and Metallicity - UvA-DARE
... decreases monotonically after an initial peak (White & Ghosh 1998; Wu 2001). If this is the case, the properties of the field LMXBs may be used to probe the star formation history of the host galaxy. In this scenario, the vast majority of the bright LMXBs in the Milky Way must be associated with rec ...
... decreases monotonically after an initial peak (White & Ghosh 1998; Wu 2001). If this is the case, the properties of the field LMXBs may be used to probe the star formation history of the host galaxy. In this scenario, the vast majority of the bright LMXBs in the Milky Way must be associated with rec ...
The effects of galaxy interactions on star formation
... This dissertation explores the effects of galaxy interactions on star formation through three separate projects. In the first two projects, we examine enhanced star formation by studying the star cluster populations of the interacting galaxies Arp 284 (NGC 7714/5) and Arp 261, using data from the Hu ...
... This dissertation explores the effects of galaxy interactions on star formation through three separate projects. In the first two projects, we examine enhanced star formation by studying the star cluster populations of the interacting galaxies Arp 284 (NGC 7714/5) and Arp 261, using data from the Hu ...
The Ages of Stars
... arrive at an understanding of a process. Some examples include: • The formation and evolution of proto-planetary disks appear to occur in the first ∼ 100 Myr of a star’s life, with debris disks forming later. At present we can just barely limit this time-scale with the methods available, but clearly ...
... arrive at an understanding of a process. Some examples include: • The formation and evolution of proto-planetary disks appear to occur in the first ∼ 100 Myr of a star’s life, with debris disks forming later. At present we can just barely limit this time-scale with the methods available, but clearly ...
Astronomy Astrophysics - Niels Bohr Institutet
... The resulting data set should place a wide range of studies of the evolution of the Galactic disk on a new and considerably improved footing. We caution, however, that no such thing as a fully unbiased sample exists in Galactic astronomy, and the reader is strongly urged to carefully study Sect. 5, ...
... The resulting data set should place a wide range of studies of the evolution of the Galactic disk on a new and considerably improved footing. We caution, however, that no such thing as a fully unbiased sample exists in Galactic astronomy, and the reader is strongly urged to carefully study Sect. 5, ...
Astrophysics for Physicists.
... I had to teach the course Fundamentals of Astrophysics in our department, I found that there was no textbook which was suitable for use in the whole course. The present book has grown out of the material I have taught in this course. While writing this book, I have kept in mind that most of the stud ...
... I had to teach the course Fundamentals of Astrophysics in our department, I found that there was no textbook which was suitable for use in the whole course. The present book has grown out of the material I have taught in this course. While writing this book, I have kept in mind that most of the stud ...
The spectroscopic Hertzsprung
... & Weigert (1990) showed that main sequence stars are expected to obey the relation L ∼ M α µβ , where µ is the average mean molecular weight and β > 1. An overluminosity is thus related to a larger mean molecular weight in a star than expected for an ordinary star (Langer 1992). In the HR diagram, t ...
... & Weigert (1990) showed that main sequence stars are expected to obey the relation L ∼ M α µβ , where µ is the average mean molecular weight and β > 1. An overluminosity is thus related to a larger mean molecular weight in a star than expected for an ordinary star (Langer 1992). In the HR diagram, t ...
The Evolution of the Mass-Size relation to z = 3.5 in the GOODS
... have smaller half-light radii. Their “norm optical sizes are thus perhaps not strong galaxies between 10 < log(M ...
... have smaller half-light radii. Their “norm optical sizes are thus perhaps not strong galaxies between 10 < log(M ...
SPIRAL STRUCTURE IN THE OUTER GALACTIC
... enough to produce clear cluster sequences, thus allowing straightforward distance determinations. As a final remark, the bright (massive) stars often include fast rotators, Be-type stars, and binaries ( just to mention some effects) that widen the cluster sequence and lead to poorly constrained clus ...
... enough to produce clear cluster sequences, thus allowing straightforward distance determinations. As a final remark, the bright (massive) stars often include fast rotators, Be-type stars, and binaries ( just to mention some effects) that widen the cluster sequence and lead to poorly constrained clus ...
Dark Matter, Dark Energy, and the Fate of the Universe
... orbit. We can similarly use the orbital motion of any other star around the galaxy to measure the mass of the Milky Way within that star’s orbit. In principle, we could determine the complete distribution of mass in the Milky Way by doing the same thing with the orbits of stars at every different di ...
... orbit. We can similarly use the orbital motion of any other star around the galaxy to measure the mass of the Milky Way within that star’s orbit. In principle, we could determine the complete distribution of mass in the Milky Way by doing the same thing with the orbits of stars at every different di ...
The COMPLETE Survey of Outflows in Perseus
... only the most powerful outflows and that individual outflows were not resolved in high-density regions; compare, for example, the results of Yu et al. (2000) and Fukui et al. (1986). Most of the recent outflow studies are restricted to small fields, focusing on individual objects or small dense regi ...
... only the most powerful outflows and that individual outflows were not resolved in high-density regions; compare, for example, the results of Yu et al. (2000) and Fukui et al. (1986). Most of the recent outflow studies are restricted to small fields, focusing on individual objects or small dense regi ...
Astronomy and Astrophysics (ASTRO) Iowa State University – 2013-2014 1
... An entirely web-based course covering topics in observing the sky and navigation by the stars for students with little or no previous experience. The course combines material on common naked-eye phenomena, such as daily and seasonal variations in the sky, with information on how these helped navigat ...
... An entirely web-based course covering topics in observing the sky and navigation by the stars for students with little or no previous experience. The course combines material on common naked-eye phenomena, such as daily and seasonal variations in the sky, with information on how these helped navigat ...
JCMT HARP CO 3-2 Observations of Molecular Outflows in W5
... presented, totaling an area of ∼ 12000 arcmin2 with sensitivity better than 0.1 K per 0.4 km s−1 channel. We have discovered 55 CO outflow candidates, 40 of which are associated with W5. Most of the outflows are located on the periphery of the W5 HII region, but two clusters of outflows are > 5 pc f ...
... presented, totaling an area of ∼ 12000 arcmin2 with sensitivity better than 0.1 K per 0.4 km s−1 channel. We have discovered 55 CO outflow candidates, 40 of which are associated with W5. Most of the outflows are located on the periphery of the W5 HII region, but two clusters of outflows are > 5 pc f ...
OBSERVATIONS OF PHYSICAL PROCESSES IN
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
Thesis
... only did they collect and combine the astronomy from e.g. Greece, Egypt and India into one mathematical language, they also made contributions to the Ptolemaic system and created instruments such as celestial globes, astrolabs and large observatories. Their motivation was mostly a practical one of w ...
... only did they collect and combine the astronomy from e.g. Greece, Egypt and India into one mathematical language, they also made contributions to the Ptolemaic system and created instruments such as celestial globes, astrolabs and large observatories. Their motivation was mostly a practical one of w ...
On the elemental abundance and isotopic mixture of mercury in
... flow of excited particles in one direction while unexcited particles flow in the opposite direction. Since the collisional cross sections typically are larger for excited than unexcited atoms on account of their larger effective radius, the flow of excited particles is decelerated more efficiently by c ...
... flow of excited particles in one direction while unexcited particles flow in the opposite direction. Since the collisional cross sections typically are larger for excited than unexcited atoms on account of their larger effective radius, the flow of excited particles is decelerated more efficiently by c ...
Far-ultraviolet and far-infrared bivariate luminosity function of galaxies:
... Far-ultraviolet (FUV) and far-infrared (FIR) luminosity functions (LFs) of galaxies show a strong evolution from z = 0 to z = 1, but the FIR LF evolves much stronger than the FUV one. The FUV is dominantly radiated from newly-formed short-lived OB stars, while the FIR is emitted by dust grains heate ...
... Far-ultraviolet (FUV) and far-infrared (FIR) luminosity functions (LFs) of galaxies show a strong evolution from z = 0 to z = 1, but the FIR LF evolves much stronger than the FUV one. The FUV is dominantly radiated from newly-formed short-lived OB stars, while the FIR is emitted by dust grains heate ...
The KMOS Redshift One Spectroscopic Survey
... that are fainter than KAB = 22.5 and/or have a red colour (i.e. r−z > 1.5). Lower priority faint and red galaxies are still observed because it is not usually possible to fill all of the arms of a KMOS configuration with high priority galaxies, due to both target density and allowed arm positioning. ...
... that are fainter than KAB = 22.5 and/or have a red colour (i.e. r−z > 1.5). Lower priority faint and red galaxies are still observed because it is not usually possible to fill all of the arms of a KMOS configuration with high priority galaxies, due to both target density and allowed arm positioning. ...
A catalogue of the Chandra Deep Field South with multi
... MIDAS package. A WFI image processing pipeline was developed by Wolf et al. (2001) and makes intensive use of programmes developed by K. Meisenheimer, H.-J. Röser and H. Hippelein for the Calar Alto Deep Imaging Survey (CADIS). The pipeline performes basic image reduction and standard operations of ...
... MIDAS package. A WFI image processing pipeline was developed by Wolf et al. (2001) and makes intensive use of programmes developed by K. Meisenheimer, H.-J. Röser and H. Hippelein for the Calar Alto Deep Imaging Survey (CADIS). The pipeline performes basic image reduction and standard operations of ...
β Relation for Local Galaxies
... galaxies on the IRX show a considerable amount of scatter compared to the starburst IRX relation. Currently, no single relation for normal star-forming galaxies exists between βGLX the UV attenuation nor is there agreement as to the underlying physical reason that causes the spread. It is necessary ...
... galaxies on the IRX show a considerable amount of scatter compared to the starburst IRX relation. Currently, no single relation for normal star-forming galaxies exists between βGLX the UV attenuation nor is there agreement as to the underlying physical reason that causes the spread. It is necessary ...
Uncovering the nucleus candidate for NGC 253
... Davies et al. 2014). Theses speculations are due mostly to the fact that an increasing number of the neighboring galaxies, as revealed by new observations, contain starbursts and active galactic nuclei (AGNs) in close proximity (see Levenson et al. 2001 and references therein). It remains unclear wh ...
... Davies et al. 2014). Theses speculations are due mostly to the fact that an increasing number of the neighboring galaxies, as revealed by new observations, contain starbursts and active galactic nuclei (AGNs) in close proximity (see Levenson et al. 2001 and references therein). It remains unclear wh ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.