STELLAR AGE VERSUS MASS OF EARLY
... minor population of Virgo cluster early type galaxies with ongoing central star formation, a typical value for E(B − V ) of 0.1 was found for their centers (Lisker et al. 2006b), thus being much smaller for the galaxies as a whole, and certainly negligible for the vast majority of the sample. For ea ...
... minor population of Virgo cluster early type galaxies with ongoing central star formation, a typical value for E(B − V ) of 0.1 was found for their centers (Lisker et al. 2006b), thus being much smaller for the galaxies as a whole, and certainly negligible for the vast majority of the sample. For ea ...
Recent science results from VLTI commissioning
... but ~30 x 106 L at outburst (2nd brightest object in sky) • Super hot: 15-40 x 103 K • Super active: survivor of 1843 eruption that created the homunculus and expelled ~ 2-3M at up to 800 km/s • Current rate of mass loss 0.3-3 x 10-3 M/yr • Central object is not viewed directly but is obscured by ...
... but ~30 x 106 L at outburst (2nd brightest object in sky) • Super hot: 15-40 x 103 K • Super active: survivor of 1843 eruption that created the homunculus and expelled ~ 2-3M at up to 800 km/s • Current rate of mass loss 0.3-3 x 10-3 M/yr • Central object is not viewed directly but is obscured by ...
Mergers of massive main sequence binaries
... In this bachelor research project, we investigated mergers between close main-sequence binaries with the aim of determining whether they result in blue stragglers. We define blue stragglers to be hot and luminous stars that cannot be explained with canonical single star evolution models2 . Using a p ...
... In this bachelor research project, we investigated mergers between close main-sequence binaries with the aim of determining whether they result in blue stragglers. We define blue stragglers to be hot and luminous stars that cannot be explained with canonical single star evolution models2 . Using a p ...
Star Clusters - Caltech Astronomy
... mass of some of the younger clusters exceeds 104 M . Few if any open clusters have enough members to be characterized in terms of dynamically meaningful quantities, such as the core radius or tidal radius. Instead, open cluster sizes are based on the ‘angular diameter’ measurement where the diamete ...
... mass of some of the younger clusters exceeds 104 M . Few if any open clusters have enough members to be characterized in terms of dynamically meaningful quantities, such as the core radius or tidal radius. Instead, open cluster sizes are based on the ‘angular diameter’ measurement where the diamete ...
Wandering in the Redshift Desert
... relief may be offered by Ly-α, if the specSQNFQ@OG HR DEjBHDMS DMNTFG HM SGD 45 Indeed, even if not in emission, Ly-α is such a strong feature that it helps a lot in getting redshifts. However, in a spectrograph such as e.g., VIMOS, Ly-α does not enter before z ~ 1.8, hence the range 1.4 < z < 1.8 i ...
... relief may be offered by Ly-α, if the specSQNFQ@OG HR DEjBHDMS DMNTFG HM SGD 45 Indeed, even if not in emission, Ly-α is such a strong feature that it helps a lot in getting redshifts. However, in a spectrograph such as e.g., VIMOS, Ly-α does not enter before z ~ 1.8, hence the range 1.4 < z < 1.8 i ...
Star Trek ObservING List - Adirondack astronomy retreat
... about 2.3 times Jupiter’s mass. It takes approximately 1.614 Earth years to orbit its star. The man who discovered this planet is named A. Hatzes, and this planet was officially announced on June 16th, 2006. This star sits 33.6 light years away from Earth. The star Beta Geminorum is slightly cooler ...
... about 2.3 times Jupiter’s mass. It takes approximately 1.614 Earth years to orbit its star. The man who discovered this planet is named A. Hatzes, and this planet was officially announced on June 16th, 2006. This star sits 33.6 light years away from Earth. The star Beta Geminorum is slightly cooler ...
CW9_MOST_GSphot_RK_v1
... suitability asa photometric comparison star for HD209458 and found based on 2 nights (each a few hours) that this Object is of delta Scuti nature and hence of no use in the context of their HD209458 study ...
... suitability asa photometric comparison star for HD209458 and found based on 2 nights (each a few hours) that this Object is of delta Scuti nature and hence of no use in the context of their HD209458 study ...
Hubble Space Telescope Imaging of Post
... and/or supernova feedback. Observationally, post-starburst galaxies have been linked to mergers and AGN (e.g., Brown et al. 2009; Falkenberg et al. 2009; Wild et al. 2009, and references therein). The environments and morphologies of post-starburst galaxies are heterogeneous, which is suggestive of ...
... and/or supernova feedback. Observationally, post-starburst galaxies have been linked to mergers and AGN (e.g., Brown et al. 2009; Falkenberg et al. 2009; Wild et al. 2009, and references therein). The environments and morphologies of post-starburst galaxies are heterogeneous, which is suggestive of ...
Astronomy 112: The Physics of Stars Class 19 Notes: The Stellar
... older stellar population. Given a bunch of stars in an HR diagram this technique can get quite sophisticated. An example is a recent paper by Williams et al. that used this method to determine the star formation history in different parts of a nearby galaxy. They divided the galaxy into annuli, and ...
... older stellar population. Given a bunch of stars in an HR diagram this technique can get quite sophisticated. An example is a recent paper by Williams et al. that used this method to determine the star formation history in different parts of a nearby galaxy. They divided the galaxy into annuli, and ...
H-Band spectroscopic classification of OB stars
... Classification of hot stars at near infrared wavelengths is challenging because the photospheric absorption features used in the classification (primarily H, He I, and He II) are generally weaker than the molecular and atomic (metal) lines used for late–type stars. In addition, there can also be str ...
... Classification of hot stars at near infrared wavelengths is challenging because the photospheric absorption features used in the classification (primarily H, He I, and He II) are generally weaker than the molecular and atomic (metal) lines used for late–type stars. In addition, there can also be str ...
Слайд 1 - Tuorla Observatory
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
Distance
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
![Module 4.1 - The Scale of the Universe [slide 1] We now turn to](http://s1.studyres.com/store/data/002846843_1-9e0ec9d1a2abbbab3c0d406694bfc4e2-300x300.png)
Module 4.1 - The Scale of the Universe [slide 1] We now turn to
... them in galaxies up to maybe 25 mega parsecs or so. So we can calibrate distances to a number of nearby galaxies using Cepheids, which is not easy but it's possible. And then we can use distances to those galaxies to calibrate some other relations. It isn't all perfectly safe. The pulsation of stars ...
... them in galaxies up to maybe 25 mega parsecs or so. So we can calibrate distances to a number of nearby galaxies using Cepheids, which is not easy but it's possible. And then we can use distances to those galaxies to calibrate some other relations. It isn't all perfectly safe. The pulsation of stars ...
A Zoo of Galaxies - Cambridge University Press
... visual classification of the types galaxies impossible and in 2007 inspired the Galaxy Zoo project (www.galaxyzoo.org); starting the largest ever scientific collaboration by asking members of the public to help classify galaxies by type and shape. Galaxy Zoo has since shown itself, in a series of now ...
... visual classification of the types galaxies impossible and in 2007 inspired the Galaxy Zoo project (www.galaxyzoo.org); starting the largest ever scientific collaboration by asking members of the public to help classify galaxies by type and shape. Galaxy Zoo has since shown itself, in a series of now ...
Lives of the Stars Lecture 5: Star birth
... carried by the orbits of the planets: the spin of the Sun contains only about 1% of the total angular momentum of the Solar System. Remember that angular momentum = mass x velocity x distance so to have large angular momentum, you need to have either large mass, large velocity or large distance from ...
... carried by the orbits of the planets: the spin of the Sun contains only about 1% of the total angular momentum of the Solar System. Remember that angular momentum = mass x velocity x distance so to have large angular momentum, you need to have either large mass, large velocity or large distance from ...
Measuring the Stars Section 29.2
... The classes were originally based only on the pattern of spectral lines, but astronomers later discovered that the classes also correspond to stellar temperatures, with the O stars being the hottest and the M stars being the coolest. Thus, by examination of a star’s spectra, it is possible to estima ...
... The classes were originally based only on the pattern of spectral lines, but astronomers later discovered that the classes also correspond to stellar temperatures, with the O stars being the hottest and the M stars being the coolest. Thus, by examination of a star’s spectra, it is possible to estima ...
Document
... • The abundances depend on a variety of stellar parameters (effective temperature, gravity, etc) as well as oscillator strength f. In particular the the product of Af is obtained, the product of the abundance and the oscillator strength. • The uncertainties in the f value is what limits you in pract ...
... • The abundances depend on a variety of stellar parameters (effective temperature, gravity, etc) as well as oscillator strength f. In particular the the product of Af is obtained, the product of the abundance and the oscillator strength. • The uncertainties in the f value is what limits you in pract ...
Hipparcos distance estimates of the Ophiuchus and the Lupus cloud
... not included in the error estimate quoted above). For Ophiuchus, we find some evidence that the streamers are closer to us than the core. The method applied in this paper is currently limited to nearby molecular clouds, but it will find many natural applications in the GAIA-era, when it will be poss ...
... not included in the error estimate quoted above). For Ophiuchus, we find some evidence that the streamers are closer to us than the core. The method applied in this paper is currently limited to nearby molecular clouds, but it will find many natural applications in the GAIA-era, when it will be poss ...
The Submillimeter Frontier: A Space Science Imperative
... Cooling flows allow hot gas to fall to the centers of galaxy clusters and disappear from view, possibly forming stars (O’Connell and McNamara 1991). In many galaxies Active Galactic Nuclei (AGN) form in dense cores with accretion disks of infalling material and produce jets observable from radio to ...
... Cooling flows allow hot gas to fall to the centers of galaxy clusters and disappear from view, possibly forming stars (O’Connell and McNamara 1991). In many galaxies Active Galactic Nuclei (AGN) form in dense cores with accretion disks of infalling material and produce jets observable from radio to ...
Setting Instruction
... • The constellation display includes the positions of 452 fixed stars with a brightness of the 4.0th magnitude or brighter, 119 major nebulae and star clusters, delimitation of constellations, and the ecliptic and the celestial equator based on their positions for the year 2000.0. (Maximum magnitude ...
... • The constellation display includes the positions of 452 fixed stars with a brightness of the 4.0th magnitude or brighter, 119 major nebulae and star clusters, delimitation of constellations, and the ecliptic and the celestial equator based on their positions for the year 2000.0. (Maximum magnitude ...
ppt - SLAC
... Wolf-Rayet stars are hot (25-50,000+ degrees K), massive stars (20+ solar mass) with a high rate of mass loss. (This is WR124, at 19h11 +16 ) A few other spectral types don't fit the sequence but instead parallel it. Type W or Wolf-Rayet stars are as hot and blue as the hottest O stars but show stro ...
... Wolf-Rayet stars are hot (25-50,000+ degrees K), massive stars (20+ solar mass) with a high rate of mass loss. (This is WR124, at 19h11 +16 ) A few other spectral types don't fit the sequence but instead parallel it. Type W or Wolf-Rayet stars are as hot and blue as the hottest O stars but show stro ...
GAIA A Stereoscopic Census of our Galaxy
... rare stellar types and rapid evolutionary phases in large numbers parallax calibration of all distance indicators e.g. Cepheids and RR Lyrae to LMC/SMC ...
... rare stellar types and rapid evolutionary phases in large numbers parallax calibration of all distance indicators e.g. Cepheids and RR Lyrae to LMC/SMC ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.