3. Cosmology and the Origin and Evolution of Galaxies
... The unique capabilities of the LMT and its suite of instrumentation provide an exciting solution to the problem of measuring the redshifts of the mm population of optically obscured galaxies. It has been demonstrated that dusty mm galaxies at high-redshift also contain enormous reservoirs of molecul ...
... The unique capabilities of the LMT and its suite of instrumentation provide an exciting solution to the problem of measuring the redshifts of the mm population of optically obscured galaxies. It has been demonstrated that dusty mm galaxies at high-redshift also contain enormous reservoirs of molecul ...
The first photometric analysis of the overcontact binary MQ UMa with
... 2006, 2011). It has been widely accepted that the eruption of V1309 Sco was the result of a cool short-period binary merging. In this paper, we focus on the high fill-out, low mass ratio overcontact binaries which are at the late evolutionary stages of the contact configuration. Photometric analysis ...
... 2006, 2011). It has been widely accepted that the eruption of V1309 Sco was the result of a cool short-period binary merging. In this paper, we focus on the high fill-out, low mass ratio overcontact binaries which are at the late evolutionary stages of the contact configuration. Photometric analysis ...
IAC_L2_thindisk
... • the thick disk stars are all old (> 10 Gyr) and have abundances between about -0.3 to -1.2, with a metal-weak tail extending down to about -2.0. • the thick disk stars form an -enhanced sequence in the [ /Fe] vs [Fe/H]. Because of operational difficulties in assigning individual stars kinematica ...
... • the thick disk stars are all old (> 10 Gyr) and have abundances between about -0.3 to -1.2, with a metal-weak tail extending down to about -2.0. • the thick disk stars form an -enhanced sequence in the [ /Fe] vs [Fe/H]. Because of operational difficulties in assigning individual stars kinematica ...
– 1 – 1. Galaxy Observations 1.1.
... The impact of the SDSS in this field has been profound. The combination of huge samples observed and processed in a uniform manner, an easily searchable database with intermittant public releases of hundreds of thousands of spectra, and precision 5 color photometry, has been revolutionary. The SDSS ...
... The impact of the SDSS in this field has been profound. The combination of huge samples observed and processed in a uniform manner, an easily searchable database with intermittant public releases of hundreds of thousands of spectra, and precision 5 color photometry, has been revolutionary. The SDSS ...
Hipparcos distance estimates of the Ophiuchus and the Lupus cloud
... Note that the reliability of the maximum-likelihood technique presented here was also checked with numerical simulations. It is well known that the maximum-likelihood method is, under certain circumstances (verified in our case), asymptotically unbiased; however, we decided to test its behaviour in ...
... Note that the reliability of the maximum-likelihood technique presented here was also checked with numerical simulations. It is well known that the maximum-likelihood method is, under certain circumstances (verified in our case), asymptotically unbiased; however, we decided to test its behaviour in ...
Observational studies of stellar rotation
... spectro-interferometry, to measure the position angle of the rotational axis of stars whose surface is not fully spatially resolved. The method consists in measuring the position of the star’s photocenter across a spectral line. Each velocity channel within the line profile corresponds to one isorot ...
... spectro-interferometry, to measure the position angle of the rotational axis of stars whose surface is not fully spatially resolved. The method consists in measuring the position of the star’s photocenter across a spectral line. Each velocity channel within the line profile corresponds to one isorot ...
Chemical composition of 90 F and G disk dwarfs
... kinematics of disk stars, but substantial dispersions imposed on weak statistical trends. (2) There exists a real scatter in the run of [α/Fe] vs. [Fe/H] possibly due to the mixture of stars with different origins. The scatter seems to increase with decreasing metallicity starting at [Fe/H] ' −0.4. ...
... kinematics of disk stars, but substantial dispersions imposed on weak statistical trends. (2) There exists a real scatter in the run of [α/Fe] vs. [Fe/H] possibly due to the mixture of stars with different origins. The scatter seems to increase with decreasing metallicity starting at [Fe/H] ' −0.4. ...
structure and evolution of white dwarfs and their
... Dreizler & Werner 1996) implies that He-rich white dwarfs must temporarily be seen as DA stars due to some physical process. ...
... Dreizler & Werner 1996) implies that He-rich white dwarfs must temporarily be seen as DA stars due to some physical process. ...
Heliacal Rising of Canopus in Indian Astronomy
... body’s entry into the Sun’s range of effulgence is called ‘heliacal setting’ [Heliacal: related to the Sun]. Similarly the body’s coming out of the Sun’s range of brightness is called heliacal rising. Since the concerned star is close to the Sun in this interval of its heliacal setting and heliacal ...
... body’s entry into the Sun’s range of effulgence is called ‘heliacal setting’ [Heliacal: related to the Sun]. Similarly the body’s coming out of the Sun’s range of brightness is called heliacal rising. Since the concerned star is close to the Sun in this interval of its heliacal setting and heliacal ...
thick disk - asteroSTEP
... • a gas-rich merger (Brook et al 2004, 2005). The thick disk stars are born in-situ • accretion (Abadi 2003). The thick disk stars come in from outside • heating of the early thin disk by accretion of a massive satellite • radial migration (stars on more energetic orbits migrate out from the inner g ...
... • a gas-rich merger (Brook et al 2004, 2005). The thick disk stars are born in-situ • accretion (Abadi 2003). The thick disk stars come in from outside • heating of the early thin disk by accretion of a massive satellite • radial migration (stars on more energetic orbits migrate out from the inner g ...
1 The Hubble Story (10:56)
... dust disks, dubbed proplyds, around the newly born stars in the Orion Nebula. The proplyds may very well be young planetary systems in the early stages of creation. The details revealed by Hubble are superior to anything seen to date with groundbased instruments and, thanks to Hubble, we have visual ...
... dust disks, dubbed proplyds, around the newly born stars in the Orion Nebula. The proplyds may very well be young planetary systems in the early stages of creation. The details revealed by Hubble are superior to anything seen to date with groundbased instruments and, thanks to Hubble, we have visual ...
Constraints on Long-Period Planets from an L
... – raising concerns about the standard procedure of assuming high completeness at 5σ, and demonstrating that blind sensitivity tests to establish the significance-completeness relation are an important analysis step for all planet-imaging surveys. We discovered a previously unknown ∼ 0.15M⊙ stellar c ...
... – raising concerns about the standard procedure of assuming high completeness at 5σ, and demonstrating that blind sensitivity tests to establish the significance-completeness relation are an important analysis step for all planet-imaging surveys. We discovered a previously unknown ∼ 0.15M⊙ stellar c ...
Stellar evolution - Statistical Physics Group
... hydrogen to helium supplies the star’s energy loss, is well understood and postmain-sequence evolution has been followed to the phase of helium burning or carbon burning at the centre of the star. I t is clear that it will only be a matter of time before these calculations are carried to a later sta ...
... hydrogen to helium supplies the star’s energy loss, is well understood and postmain-sequence evolution has been followed to the phase of helium burning or carbon burning at the centre of the star. I t is clear that it will only be a matter of time before these calculations are carried to a later sta ...
Red supergiants around the obscured open cluster Stephenson 2
... other RSG clusters is unclear. Though all the clusters are located at a similar distance and have similar ages, they span ∼500 pc in projection. There have been suggestions that this Scutum Complex represents a giant star formation region triggered by the dynamical excitation of the Galactic Bar, wh ...
... other RSG clusters is unclear. Though all the clusters are located at a similar distance and have similar ages, they span ∼500 pc in projection. There have been suggestions that this Scutum Complex represents a giant star formation region triggered by the dynamical excitation of the Galactic Bar, wh ...
FIELD ASTRONOMY
... equinox and is known as the sidereal day. Therefore, the lengths of the sidereal day and the solar day differ. The solar day is longer by 3 minutes and 56 seconds. The FA surveyor does not have to understand this differential in the lengths of the solar and sidereal days to compute azimuth data deri ...
... equinox and is known as the sidereal day. Therefore, the lengths of the sidereal day and the solar day differ. The solar day is longer by 3 minutes and 56 seconds. The FA surveyor does not have to understand this differential in the lengths of the solar and sidereal days to compute azimuth data deri ...
Course Materials - Weber State University
... 4. Choose a location for the Sun. The Sun remains stationary for the entire lesson after that! (It's often easiest to say that the 'Sun' is located at one end of the hallway.) 5. The Earth stands in one spot for the entire lesson (but can turn around to see the Moon). The Moon stands relative to the ...
... 4. Choose a location for the Sun. The Sun remains stationary for the entire lesson after that! (It's often easiest to say that the 'Sun' is located at one end of the hallway.) 5. The Earth stands in one spot for the entire lesson (but can turn around to see the Moon). The Moon stands relative to the ...
Magnificent Cosmos - Academic Program Pages at Evergreen
... Coronae Borealis. A ninth large object, which orbits the star known by its catalogue number HD114762, has also been observed—an object first detected in 1989 by astronomer David W. Latham of the Harvard-Smithsonian Center for Astrophysics and his collaborators. But this bulky companion has a mass mo ...
... Coronae Borealis. A ninth large object, which orbits the star known by its catalogue number HD114762, has also been observed—an object first detected in 1989 by astronomer David W. Latham of the Harvard-Smithsonian Center for Astrophysics and his collaborators. But this bulky companion has a mass mo ...
– 1 – 1. Emission Lines in Nearby Galaxies 1.1.
... Complex scenarios arise. For example, in a starburst there are so many SN that they bubbles they each blow in the ISM merge together and remain relatively clear of gas. However, in normal star-forming galaxies, the star formation is less vigorous, it takes place in individual HII regions, not huge g ...
... Complex scenarios arise. For example, in a starburst there are so many SN that they bubbles they each blow in the ISM merge together and remain relatively clear of gas. However, in normal star-forming galaxies, the star formation is less vigorous, it takes place in individual HII regions, not huge g ...
1 A Re-appraisal of the Habitability of Planets Around M Dwarf Stars
... characteristic features found in relatively low resolution spectra, initially obtained at optical wavelengths nearly a century ago. It was later understood that the observable spectral features were actually providing information about stellar surface temperatures and mass, but by then the classific ...
... characteristic features found in relatively low resolution spectra, initially obtained at optical wavelengths nearly a century ago. It was later understood that the observable spectral features were actually providing information about stellar surface temperatures and mass, but by then the classific ...
Ursa Major
Ursa Major /ˈɜrsə ˈmeɪdʒər/ (also known as the Great Bear and Charles' Wain) is a constellation in the northern celestial hemisphere. One of the 48 constellations listed by Ptolemy (second century AD), it remains one of the 88 modern constellations. It can be visible throughout the year in most of the northern hemisphere. Its name, Latin for ""the greater (or larger) she-bear"", stands as a reference to and in direct contrast with Ursa Minor, ""the smaller she-bear"", with which it is frequently associated in mythology and amateur astronomy. The constellation's most recognizable asterism, a group of seven relatively bright stars commonly known as the ""Big Dipper"", ""the Wagon"" or ""the Plough"" (among others), both mimicks the shape of the lesser bear (the ""Little Dipper"") and is commonly used as a navigational pointer towards the current northern pole star, Polaris in Ursa Minor. The Big Dipper and the constellation as a whole have mythological significance in numerous world cultures, usually as a symbol of the north.The third largest constellation in the sky, Ursa Major is home to many deep-sky objects including seven Messier objects, four other NGC objects and I Zwicky 18, the youngest known galaxy in the visible universe.