![The colour–magnitude relation of globular clusters in Centaurus and](http://s1.studyres.com/store/data/022547657_1-31e9328857ddc6b5a4ca9cf979a0d0e2-300x300.png)
The colour–magnitude relation of globular clusters in Centaurus and
... equivalent to a scaling with mass of Z ∝ M 0.3−0.7 , that depends on environment. Results have so far indicated that the trend sets in already at masses slightly below a million solar masses, at several 105 M . The most common interpretation of this colour-metallicity relation is self-enrichment. W ...
... equivalent to a scaling with mass of Z ∝ M 0.3−0.7 , that depends on environment. Results have so far indicated that the trend sets in already at masses slightly below a million solar masses, at several 105 M . The most common interpretation of this colour-metallicity relation is self-enrichment. W ...
The Ages of Stars
... systematic effects since we do not usually know what inherent physical relation to expect. The sensitivity of the indicator may be useful for only a limited age range or mass range. Inherent scatter in the quantity measured may mean that the age indicator is not very useful for single stars but can ...
... systematic effects since we do not usually know what inherent physical relation to expect. The sensitivity of the indicator may be useful for only a limited age range or mass range. Inherent scatter in the quantity measured may mean that the age indicator is not very useful for single stars but can ...
FIELD GALAXIES AND THEIR AGNs: NATURE VERSUS
... DMH density profiles have a universal shape, independent of the halo mass, the initial density fluctuation spectrum and the cosmological parameters. ...
... DMH density profiles have a universal shape, independent of the halo mass, the initial density fluctuation spectrum and the cosmological parameters. ...
Astronomy 1010L Lab Manual - The University of Tennessee at
... search. If the object exists in the program databank, it will be placed in the center of the screen. Search for Jupiter. On your data sheet, report (A) the rise and set times for today (B) the portion of the sky where it will be located at 6:00 PM and (C) the location of Jupiter in the sky so that ...
... search. If the object exists in the program databank, it will be placed in the center of the screen. Search for Jupiter. On your data sheet, report (A) the rise and set times for today (B) the portion of the sky where it will be located at 6:00 PM and (C) the location of Jupiter in the sky so that ...
Astronomy Astrophysics Spectral energy distributions of an AKARI-SDSS-GALEX sample of galaxies
... derives physical information about galaxies by fitting their UVto-far-IR SED (Noll et al. 2009b; Giovannoli et al. 2010). A Bayesian analysis is used to derive galaxy properties similar to that developed by Kauffmann et al. (2003a). CIGALE combines a UV-optical stellar SED and a dust, IR-emitting com ...
... derives physical information about galaxies by fitting their UVto-far-IR SED (Noll et al. 2009b; Giovannoli et al. 2010). A Bayesian analysis is used to derive galaxy properties similar to that developed by Kauffmann et al. (2003a). CIGALE combines a UV-optical stellar SED and a dust, IR-emitting com ...
The incidence of stellar mergers and mass gainers among massive
... few thermal timescales at most, which is short compared to the stellar lifetime. An exception are close systems that experience case A mass transfer (Nelson & Eggleton 2001), i.e. mass transfer from a main-sequence donor, which can last for up to about a third of the main sequence lifetime (e.g. Fig ...
... few thermal timescales at most, which is short compared to the stellar lifetime. An exception are close systems that experience case A mass transfer (Nelson & Eggleton 2001), i.e. mass transfer from a main-sequence donor, which can last for up to about a third of the main sequence lifetime (e.g. Fig ...
black holes can play a constructive role as well
... ionized gas velocities within the filamentary structure are similar to the cloud velocity (Schiminovich et al. 1994; Graham 1983, 1998). This scenario led a number of authors (e.g. Rejkuba et al. 2002; Gopal-Krishna & Wiita 2010) to suggest that the outer filament is a prime example of recent jet-in ...
... ionized gas velocities within the filamentary structure are similar to the cloud velocity (Schiminovich et al. 1994; Graham 1983, 1998). This scenario led a number of authors (e.g. Rejkuba et al. 2002; Gopal-Krishna & Wiita 2010) to suggest that the outer filament is a prime example of recent jet-in ...
The physics and modes of star cluster formation: observations
... spectroscopic surveys, especially those done with multi-object spectrographs, can be used to identify accreting objects in a cluster field. However, such observations can be time-consuming and even prohibitive for faint members, which can account for a significant portion of the cluster population. Ci ...
... spectroscopic surveys, especially those done with multi-object spectrographs, can be used to identify accreting objects in a cluster field. However, such observations can be time-consuming and even prohibitive for faint members, which can account for a significant portion of the cluster population. Ci ...
Jul y 9- 11,
... central supermassive black holes (SMBHs) will be more often present even in smaller galaxies when seeds are generated from the remnants of the first massive stars rather than via direct gas collapse. Consequently, measurement of the local occupation fraction provides an observational discriminator b ...
... central supermassive black holes (SMBHs) will be more often present even in smaller galaxies when seeds are generated from the remnants of the first massive stars rather than via direct gas collapse. Consequently, measurement of the local occupation fraction provides an observational discriminator b ...
Type Ia Supernovae
... after Tycho made his paradigm changing discovery using SN 1572, and some 60 years after supernovae had been identified as distant dying stars, two teams changed the view of the world again using supernovae. The found that the Universe was accelerating in its expansion, a conclusion that could most e ...
... after Tycho made his paradigm changing discovery using SN 1572, and some 60 years after supernovae had been identified as distant dying stars, two teams changed the view of the world again using supernovae. The found that the Universe was accelerating in its expansion, a conclusion that could most e ...
spatially resolved star formation history of milky way satellites
... galaxies and their own satellites form a self-gravitating association called the Local Group, and hence, the satellite galaxies that reside in it are called local dwarf galaxies. Local dwarf galaxies are crutial for understanding several key aspects of modern astrophysics (Mateo, 1998; Tolstoy et al ...
... galaxies and their own satellites form a self-gravitating association called the Local Group, and hence, the satellite galaxies that reside in it are called local dwarf galaxies. Local dwarf galaxies are crutial for understanding several key aspects of modern astrophysics (Mateo, 1998; Tolstoy et al ...
as a PDF - Research Database
... perature, for oxygen-rich dust-enshrouded Asymptotic Giant Branch stars and red supergiants. To this aim we obtained optical spectra of a sample of dust-enshrouded red giants in the Large Magellanic Cloud, which we complemented with spectroscopic and infrared photometric data from the literature. Tw ...
... perature, for oxygen-rich dust-enshrouded Asymptotic Giant Branch stars and red supergiants. To this aim we obtained optical spectra of a sample of dust-enshrouded red giants in the Large Magellanic Cloud, which we complemented with spectroscopic and infrared photometric data from the literature. Tw ...
PPT
... Additionally, a distance modulus of 13.46±0.1 has been recently derived for NGC 6791 using eclipsing binaries, a totally independent and reliable method that does not make use of theoretical models. Thus, a large error in the distance modulus is quite implausible. The only possibility left to ...
... Additionally, a distance modulus of 13.46±0.1 has been recently derived for NGC 6791 using eclipsing binaries, a totally independent and reliable method that does not make use of theoretical models. Thus, a large error in the distance modulus is quite implausible. The only possibility left to ...
Galactic spiral structure - Proceedings of the Royal Society A
... not unreasonable to calculate W0 as the mean motion of a population. However, in the absence of knowledge of the causes for streams, there is no way to relate the statistical properties of their motion to U0 and V0 . Francis & Anderson (2009) studied a population of 20 574 Hipparcos stars with compl ...
... not unreasonable to calculate W0 as the mean motion of a population. However, in the absence of knowledge of the causes for streams, there is no way to relate the statistical properties of their motion to U0 and V0 . Francis & Anderson (2009) studied a population of 20 574 Hipparcos stars with compl ...
Global structure and kinematics of stellar haloes in cosmological
... (Ferland et al. 1998) that contain cooling rates as a function of density, temperature, and redshift and that account for the presence of the cosmic microwave background and photoionisation from a Haardt & Madau (2001) ionising UV/X-Ray background (see Wiersma et al. 2009a). This background is switc ...
... (Ferland et al. 1998) that contain cooling rates as a function of density, temperature, and redshift and that account for the presence of the cosmic microwave background and photoionisation from a Haardt & Madau (2001) ionising UV/X-Ray background (see Wiersma et al. 2009a). This background is switc ...
The thin disk
... Later type galaxies mostly have near-exponential bulges, rather than r1/4 bulges - hint that their bulges are not merger products - more likely generated by disk instability (eg Balcells et al 2002) Boxy bulges, as in our Galaxy, are associated with bars eg Bureau & KF 1999 - believed to come from ...
... Later type galaxies mostly have near-exponential bulges, rather than r1/4 bulges - hint that their bulges are not merger products - more likely generated by disk instability (eg Balcells et al 2002) Boxy bulges, as in our Galaxy, are associated with bars eg Bureau & KF 1999 - believed to come from ...
Symbiotic Stars as Laboratories for the Study of
... stars, the details of the accretion process in symbiotic stars have been more difficult to ascertain than in CVs. Thus, many interesting and fundamental open questions remain. For example, symbiotic stars appear to be a new class of jet-producing astronomical objects, but how are these jets produced ...
... stars, the details of the accretion process in symbiotic stars have been more difficult to ascertain than in CVs. Thus, many interesting and fundamental open questions remain. For example, symbiotic stars appear to be a new class of jet-producing astronomical objects, but how are these jets produced ...
Clusters: age scales for stellar physics
... several well known clusters have been included. On the right-hand side estimates from the Lithium Depletion Boundary (LDB, see subsection 3.2.2), whereas the left-hand side includes values derived from isochrone fitting (both model dependent, but the modeling behind the LDB ages is simpler). As can ...
... several well known clusters have been included. On the right-hand side estimates from the Lithium Depletion Boundary (LDB, see subsection 3.2.2), whereas the left-hand side includes values derived from isochrone fitting (both model dependent, but the modeling behind the LDB ages is simpler). As can ...
SimulationDatabases
... Return the galaxy content at z=3 of the progenitors of a halo identified at z=0 Return the complete halo merger tree for a halo identified at z=0 Find all the z=3 progenitors of z=0 red ellipticals (i.e. B-V>0.8 B/T > 0.5) Find the descendents at z=1 of all LBG's (i.e. galaxies with SFR>10 Msun/yr) ...
... Return the galaxy content at z=3 of the progenitors of a halo identified at z=0 Return the complete halo merger tree for a halo identified at z=0 Find all the z=3 progenitors of z=0 red ellipticals (i.e. B-V>0.8 B/T > 0.5) Find the descendents at z=1 of all LBG's (i.e. galaxies with SFR>10 Msun/yr) ...
radioactive 26a1 in the galaxy: observations versus theory
... on Earth was estimated to ~10~~ cm-* s-l f rom the galactic centre direction, making 26A1 a prime target for the HEAO-3 detectors. Moreover it was pointed out that, because of its long mean life, 26A1 would have enough time to be thermalised in the interstellar medium; therefore, it would de-excite ...
... on Earth was estimated to ~10~~ cm-* s-l f rom the galactic centre direction, making 26A1 a prime target for the HEAO-3 detectors. Moreover it was pointed out that, because of its long mean life, 26A1 would have enough time to be thermalised in the interstellar medium; therefore, it would de-excite ...
Far-ultraviolet and far-infrared bivariate luminosity function of galaxies:
... related to the star formation in galaxies, but in a very complicated manner. In order to disentangle the relation between FUV and FIR emissions, we estimate the UV-IR bivariate LF (BLF) of galaxies with GALEX and AKARI All-Sky Survey datasets. Recently, we developed a new mathematical method to cons ...
... related to the star formation in galaxies, but in a very complicated manner. In order to disentangle the relation between FUV and FIR emissions, we estimate the UV-IR bivariate LF (BLF) of galaxies with GALEX and AKARI All-Sky Survey datasets. Recently, we developed a new mathematical method to cons ...
Limits on the Size and Orbit Distribution of Main Belt Comets
... recovery strength for simple additive and median stacking of the images assuming no systematic noise and perfect tail alignment among images. Figure 3 shows that our 18 segment scheme can detect tails at the 10−5 level if they have a strength of & 0.45 the background S/N . Increasing Nseg allows the ...
... recovery strength for simple additive and median stacking of the images assuming no systematic noise and perfect tail alignment among images. Figure 3 shows that our 18 segment scheme can detect tails at the 10−5 level if they have a strength of & 0.45 the background S/N . Increasing Nseg allows the ...
Colour-magnitude diagrams of the post
... (1985) also presents VHB = 18.2, but estimated a somewhat higher reddening of E(B − V ) = 0.88 which placed the cluster at d = 9.1 from the Sun. Webbink lists a rather low metallicity for the cluster, [M/H] = −1.56. The compilation by Harris (1996) indicates VHB = 18.20, E(B − V ) = 0.84, d = 8.9 ...
... (1985) also presents VHB = 18.2, but estimated a somewhat higher reddening of E(B − V ) = 0.88 which placed the cluster at d = 9.1 from the Sun. Webbink lists a rather low metallicity for the cluster, [M/H] = −1.56. The compilation by Harris (1996) indicates VHB = 18.20, E(B − V ) = 0.84, d = 8.9 ...
Giant Low Surface Brightness Galaxies
... in our Universe. Hα observations of the larger LSB disk galaxies and especially GLSB galaxies reveal that they have patches of localized star formation (e.g. Auld et al. 2006) associated with faint spiral arms or distributed sporadically over their disks. Surprisingly, in spite of their low Star For ...
... in our Universe. Hα observations of the larger LSB disk galaxies and especially GLSB galaxies reveal that they have patches of localized star formation (e.g. Auld et al. 2006) associated with faint spiral arms or distributed sporadically over their disks. Surprisingly, in spite of their low Star 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.