Is Draco II one of the faintest dwarf galaxies? First study from Keck
... of stars 2 and 10, which must have very similar stellar parameters as they are confirmed Dra II member stars with almost identical colours and magnitudes ((0.53,18.87) and (0.55,18.98)), implies that these two member stars have significantly different metallicities (a 4.5σ difference in the equivale ...
... of stars 2 and 10, which must have very similar stellar parameters as they are confirmed Dra II member stars with almost identical colours and magnitudes ((0.53,18.87) and (0.55,18.98)), implies that these two member stars have significantly different metallicities (a 4.5σ difference in the equivale ...
Galaxy Hunters Article, Cosmology Information, First Star Facts
... For faint galaxies, redshift can only be determined with a telescope as powerful as Keck. Now Steidel and his colleagues Mark Dickinson, Mauro Giavalisco, and graduate student Kurt Adelberger found themselves with two nights on the telescope. If they could demonstrate that their color method worked, ...
... For faint galaxies, redshift can only be determined with a telescope as powerful as Keck. Now Steidel and his colleagues Mark Dickinson, Mauro Giavalisco, and graduate student Kurt Adelberger found themselves with two nights on the telescope. If they could demonstrate that their color method worked, ...
Notes 6 - University of Northern Iowa
... winds we see when we see large scale mass loss from stars that produce very thick shells of material around them. The previously given relation for mass loss (equation 5-2) is valid but at these times the mass loss rate can be as much as 10-4 solar masses/year, which is considered a very large amoun ...
... winds we see when we see large scale mass loss from stars that produce very thick shells of material around them. The previously given relation for mass loss (equation 5-2) is valid but at these times the mass loss rate can be as much as 10-4 solar masses/year, which is considered a very large amoun ...
STELLAR FORMATION AND EVOLUTION
... region of young stars. As time goes on, stars change or evolve as the physics in their cores change. But for most of the lifetime of a star, it sits somewhere on the main sequence. We will begin by looking at what happens to most stars in the universe. These are the low mass stars. In space, there a ...
... region of young stars. As time goes on, stars change or evolve as the physics in their cores change. But for most of the lifetime of a star, it sits somewhere on the main sequence. We will begin by looking at what happens to most stars in the universe. These are the low mass stars. In space, there a ...
CHP 13
... d. they contain strong magnetic fields. e. they never use up their hydrogen. 2. A planetary nebula is a. the expelled outer envelope of a medium mass star. b. produced by a supernova explosion. c. produced by a nova explosion. d. a nebula within which planets are forming. e. a cloud of hot gas surro ...
... d. they contain strong magnetic fields. e. they never use up their hydrogen. 2. A planetary nebula is a. the expelled outer envelope of a medium mass star. b. produced by a supernova explosion. c. produced by a nova explosion. d. a nebula within which planets are forming. e. a cloud of hot gas surro ...
The Death of Stars
... d. they contain strong magnetic fields. e. they never use up their hydrogen. 2. A planetary nebula is a. the expelled outer envelope of a medium mass star. b. produced by a supernova explosion. c. produced by a nova explosion. d. a nebula within which planets are forming. e. a cloud of hot gas surro ...
... d. they contain strong magnetic fields. e. they never use up their hydrogen. 2. A planetary nebula is a. the expelled outer envelope of a medium mass star. b. produced by a supernova explosion. c. produced by a nova explosion. d. a nebula within which planets are forming. e. a cloud of hot gas surro ...
WORD - Astrophysics
... overcome crowding, and a 100m class telescope is required to study the brighter galaxies at their half-light radius - without it work is limited to the less representative outer regions where crowding is less of an issue. The more luminous elliptical ...
... overcome crowding, and a 100m class telescope is required to study the brighter galaxies at their half-light radius - without it work is limited to the less representative outer regions where crowding is less of an issue. The more luminous elliptical ...
1 Introduction - Wiley-VCH
... motion of stars within ellipticals is mainly random. These objects are often called early-type galaxies. The second family is characterized by a flat disk with a spiral morphology , with the possible presence of a bar, a bulge, and a nucleus (S). These systems are undergoing episodes of star formati ...
... motion of stars within ellipticals is mainly random. These objects are often called early-type galaxies. The second family is characterized by a flat disk with a spiral morphology , with the possible presence of a bar, a bulge, and a nucleus (S). These systems are undergoing episodes of star formati ...
LESSON 8: STARS
... The most apparent difference between high mass (10 to 30 solar masses) and low mass (0.5 to 10 solar masses) stars are the events leading up to the eventual death of the star. Low mass stars do not have the mass required to increase the core temperature enough to allow the carbon to fuse into heavie ...
... The most apparent difference between high mass (10 to 30 solar masses) and low mass (0.5 to 10 solar masses) stars are the events leading up to the eventual death of the star. Low mass stars do not have the mass required to increase the core temperature enough to allow the carbon to fuse into heavie ...
Our galaxy - School of Physics
... The disk of our Galaxy is shaped like a whirlpool with many spiral arms spanning out from the center of the Galaxy. ...
... The disk of our Galaxy is shaped like a whirlpool with many spiral arms spanning out from the center of the Galaxy. ...
Hertzsprung-Russell Diagrams
... converting hydrogen into helium. For these stars, the hotter they are, the brighter. These stars are in the most stable part of their existence; this stage generally lasts for about 5 billion years. As stars begin to die, they become giants and supergiants (above the main sequence). These stars have ...
... converting hydrogen into helium. For these stars, the hotter they are, the brighter. These stars are in the most stable part of their existence; this stage generally lasts for about 5 billion years. As stars begin to die, they become giants and supergiants (above the main sequence). These stars have ...
Sec 30.1 - Highland High School
... much as doubles from dimmest to brightest. By measuring a star’s period of pulsation, astronomers can determine the star’s absolute luminosity, and thus how far away the star is. ...
... much as doubles from dimmest to brightest. By measuring a star’s period of pulsation, astronomers can determine the star’s absolute luminosity, and thus how far away the star is. ...
Eclipsing Binary Stars as Astrophysical Laboratories
... hard to tell from this graph, but the diagonal lines represent the radius. So, for example, when we look at Sirius we can read off its luminosity, its temperature, and its radius right from that diagram. It is all right there in a compact two-dimensional form. The Hertzsprung-Russell diagram has bee ...
... hard to tell from this graph, but the diagonal lines represent the radius. So, for example, when we look at Sirius we can read off its luminosity, its temperature, and its radius right from that diagram. It is all right there in a compact two-dimensional form. The Hertzsprung-Russell diagram has bee ...
T Einstein’s Mirage Paul L. Schechter
... to be a close pair of virtually identical quasars was observed. Quasars are very bright distant sources, so light from them sometimes passes near galaxies on its way to us. The suspicion that they were the multiple images of a single quasar expected for a gravitational mirage was confirmed Perhaps t ...
... to be a close pair of virtually identical quasars was observed. Quasars are very bright distant sources, so light from them sometimes passes near galaxies on its way to us. The suspicion that they were the multiple images of a single quasar expected for a gravitational mirage was confirmed Perhaps t ...
Part 2 - Stellar Evolution
... Stars in a cluster form at nearly the same time “TOP” turnoff point can be used to determine the age of a cluster SGB: sub-giant branch RGB: red-giant branch ...
... Stars in a cluster form at nearly the same time “TOP” turnoff point can be used to determine the age of a cluster SGB: sub-giant branch RGB: red-giant branch ...
Betelgeuse
... and the narrow bandwidth avoids any spectral lines, and so we see the star relatively undistorted," said Townes. "We have also had the good fortune to have an instrument that has operated in a very similar manner for some 15 years, providing a long and consistent series of measurements that no one e ...
... and the narrow bandwidth avoids any spectral lines, and so we see the star relatively undistorted," said Townes. "We have also had the good fortune to have an instrument that has operated in a very similar manner for some 15 years, providing a long and consistent series of measurements that no one e ...
OBJXlab-JCU_Alt
... Most of the things in the sky look like dots or smudges of light. Even through the biggest telescopes only a few objects, like the large planets, a few galaxies and nebulae, show distinguishing details. It takes careful observation—with spectrometers, photometers, imaging cameras at a wide range of ...
... Most of the things in the sky look like dots or smudges of light. Even through the biggest telescopes only a few objects, like the large planets, a few galaxies and nebulae, show distinguishing details. It takes careful observation—with spectrometers, photometers, imaging cameras at a wide range of ...
Rotation Curves:
... • Does the TF make sense?? For a circular orbit, the rotational velocity is caused by the gravitational forces of the mass interior to the orbit. (This also follows from the Virial theorem.) – V2 = GM(r)/r (yes, we’ve been here before!), thus M(r) # rV2 – Assume that all galaxies have the same M/L ( ...
... • Does the TF make sense?? For a circular orbit, the rotational velocity is caused by the gravitational forces of the mass interior to the orbit. (This also follows from the Virial theorem.) – V2 = GM(r)/r (yes, we’ve been here before!), thus M(r) # rV2 – Assume that all galaxies have the same M/L ( ...
Spectra of Star Clusters
... • How are stars classified into spectral types? • Stars are classified according to their spectra, with different spectral types generally corresponding to different temperatures. In order from hottest to coolest, the major spectral types are O, B, A, F, G, K, and M. These are subdivided into num ...
... • How are stars classified into spectral types? • Stars are classified according to their spectra, with different spectral types generally corresponding to different temperatures. In order from hottest to coolest, the major spectral types are O, B, A, F, G, K, and M. These are subdivided into num ...
Chapter 17 Star Stuff
... • This double-shell burning stage never reaches equilibrium—fusion rate periodically spikes upward in a series of thermal pulses ...
... • This double-shell burning stage never reaches equilibrium—fusion rate periodically spikes upward in a series of thermal pulses ...
arXiv:1502.04693v1 [gr
... WISE candidates has only been capable with the Wide Field Camera 3 (WFC3) aboard the Hubble Space Telescope (HST). HST grism spectroscopy of the latest type brown dwarfs has been invaluable in the study and classification of these objects (Cushing et al. 2011, Kirkpatrick et al. 2012, Kirkpatrick et ...
... WISE candidates has only been capable with the Wide Field Camera 3 (WFC3) aboard the Hubble Space Telescope (HST). HST grism spectroscopy of the latest type brown dwarfs has been invaluable in the study and classification of these objects (Cushing et al. 2011, Kirkpatrick et al. 2012, Kirkpatrick et ...
Chapter 17 Star Stuff How does a star`s mass affect nuclear fusion
... Stellar Mass and Fusion • The mass of a main sequence star determines its core pressure and temperature • Stars of higher mass have higher core temperature and more rapid fusion, making those stars both more luminous and shorter-lived • Stars of lower mass have cooler cores and slower fusion rates, ...
... Stellar Mass and Fusion • The mass of a main sequence star determines its core pressure and temperature • Stars of higher mass have higher core temperature and more rapid fusion, making those stars both more luminous and shorter-lived • Stars of lower mass have cooler cores and slower fusion rates, ...
argo and other tidal structures around the milky way
... sample was limited to −25◦ < b < +25◦ , in order to avoid the Magellanic Clouds. The solar position is X = −8 kpc, Y = 0 kpc. A number of known structures can be seen in these plots: The Monoceros stream, Sagittarius, the TriAnd and Perseus systems (Rocha-Pinto et al. 2004). The large southern hemis ...
... sample was limited to −25◦ < b < +25◦ , in order to avoid the Magellanic Clouds. The solar position is X = −8 kpc, Y = 0 kpc. A number of known structures can be seen in these plots: The Monoceros stream, Sagittarius, the TriAnd and Perseus systems (Rocha-Pinto et al. 2004). The large southern hemis ...
PPT presentation
... Planetary nebulae in the intracluster regions of galaxy clusters Arnaboldi et al. (1996) measured velocities for 19 PNe in the outer regions of the giant elliptical galaxy NGC 4406, in the southern Virgo extension region. Although this galaxy has an RV of -227 km/s, three of the PNe had RV’s close ...
... Planetary nebulae in the intracluster regions of galaxy clusters Arnaboldi et al. (1996) measured velocities for 19 PNe in the outer regions of the giant elliptical galaxy NGC 4406, in the southern Virgo extension region. Although this galaxy has an RV of -227 km/s, three of the PNe had RV’s close ...
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.