Brightest Stars : Discovering the Universe Through the Sky`s Most
... six classes of star brightness. The brightest stars were said to be “first magnitude”—the first, brightest class. Slightly less brilliant were stars of “second magnitude,” then “third magnitude,” and so on with decreasing brightness. The faintest class of stars, those just barely visible to the nake ...
... six classes of star brightness. The brightest stars were said to be “first magnitude”—the first, brightest class. Slightly less brilliant were stars of “second magnitude,” then “third magnitude,” and so on with decreasing brightness. The faintest class of stars, those just barely visible to the nake ...
Clusters as laboratories for the study of galaxy evolution
... systems that are merging would not have been very much like the giant spiral galaxies we see today, which we believe formed over a much longer timescale. 2) The places where this happened were destined to be the cores of rich clusters, but they too were unlike the rich clusters we see today. A bette ...
... systems that are merging would not have been very much like the giant spiral galaxies we see today, which we believe formed over a much longer timescale. 2) The places where this happened were destined to be the cores of rich clusters, but they too were unlike the rich clusters we see today. A bette ...
On the nature of sn stars. I. A detailed abundance study
... belong to 12 open clusters and noted that the sn characteristics could occur simultaneously with a variety of chemical peculiarities, including He-weak, Bp(Si), and HgMn. These chemically peculiar (CP) stars present strong and/or weak intensities in the spectral lines of certain chemical species. Th ...
... belong to 12 open clusters and noted that the sn characteristics could occur simultaneously with a variety of chemical peculiarities, including He-weak, Bp(Si), and HgMn. These chemically peculiar (CP) stars present strong and/or weak intensities in the spectral lines of certain chemical species. Th ...
Hunting for Substructure in the Milky Way
... direction of the North Galactic Pole. In order to conserve angular momentum, over time this orbit remains approximately circular. Astronomers measure the velocity and distances of stars to analyse the angular momentum, and from this they can determine how circular the orbit of each star is. In previ ...
... direction of the North Galactic Pole. In order to conserve angular momentum, over time this orbit remains approximately circular. Astronomers measure the velocity and distances of stars to analyse the angular momentum, and from this they can determine how circular the orbit of each star is. In previ ...
Classification of Variable Stars
... White Yellow-white Yellowish Orange Reddish Red-infrared infrared infrared infrared ...
... White Yellow-white Yellowish Orange Reddish Red-infrared infrared infrared infrared ...
A Spectroscopically Confirmed Excess of 24 micron Sources in a
... Each redshift was then given a quality flag where Q = 3, 2, & 1 corresponded to definite, probable, and maybe (single emission line). The spectral range for most of the supergroup members covers [OII]λ3727 to [OIII]λ5007. The spectroscopic completeness in the HST/ACS footprint is shown in Fig. 2. Du ...
... Each redshift was then given a quality flag where Q = 3, 2, & 1 corresponded to definite, probable, and maybe (single emission line). The spectral range for most of the supergroup members covers [OII]λ3727 to [OIII]λ5007. The spectroscopic completeness in the HST/ACS footprint is shown in Fig. 2. Du ...
Spectral Matching for Elemental Abundances of Evolved Stars of Globular Clusters
... used to estimate the oxygen abundance of the stars, leading to a determination of whether a particular star was oxygen-rich or oxygen-poor. From this a catalogue of abundances of iron, carbon and barium of 848 giant branch stars were determined, of which 557 also had well-defined nitrogen abundances ...
... used to estimate the oxygen abundance of the stars, leading to a determination of whether a particular star was oxygen-rich or oxygen-poor. From this a catalogue of abundances of iron, carbon and barium of 848 giant branch stars were determined, of which 557 also had well-defined nitrogen abundances ...
THE MORPHOLOGICAL DEMOGRAPHICS OF GALAXIES IN THE
... We present a morphological analysis of distant field galaxies using the deep ACS images from the public parallel NICMOS observations of the Hubble Ultra Deep Field obtained in the F435W (B 435 ), F606W (V606 ), F775W (i775 ) and F850LP (z850 ) filters. We morphologically segregate galaxies using a c ...
... We present a morphological analysis of distant field galaxies using the deep ACS images from the public parallel NICMOS observations of the Hubble Ultra Deep Field obtained in the F435W (B 435 ), F606W (V606 ), F775W (i775 ) and F850LP (z850 ) filters. We morphologically segregate galaxies using a c ...
DUSTiNGS III: Distribution of Intermediate
... candidates from the larger DUSTiNGS sample. The variable AGB star candidates are a powerful tracer of stars at greater radii in the galaxies as the identification of the variable AGB stars is independent of photometric contamination. Thus, membership of an individual point source to the galaxy is mo ...
... candidates from the larger DUSTiNGS sample. The variable AGB star candidates are a powerful tracer of stars at greater radii in the galaxies as the identification of the variable AGB stars is independent of photometric contamination. Thus, membership of an individual point source to the galaxy is mo ...
Astronomy Astrophysics Detailed abundances of a large sample of giant stars in... and in the Sagittarius nucleus
... for 76 red giant stars in NGC 6715 (M 54), a massive globular cluster (GC) lying in the nucleus of the Sagittarius dwarf galaxy. We also derived detailed abundances for 27 red giants belonging to the Sgr nucleus. Our abundances measure the intrinsic metallicity dispersion (∼0.19 dex, rms scatter) of ...
... for 76 red giant stars in NGC 6715 (M 54), a massive globular cluster (GC) lying in the nucleus of the Sagittarius dwarf galaxy. We also derived detailed abundances for 27 red giants belonging to the Sgr nucleus. Our abundances measure the intrinsic metallicity dispersion (∼0.19 dex, rms scatter) of ...
Altas Farnese
... near the north pole (cf. Section A.2.2). (7) The ecliptic crosses the equator 5° west of the colure lines. This arrangement is wrong by definition, as precession moves the sky along the ecliptic, suggesting that the sculptor made the change because of his lack of astronomical knowledge. (8) The stri ...
... near the north pole (cf. Section A.2.2). (7) The ecliptic crosses the equator 5° west of the colure lines. This arrangement is wrong by definition, as precession moves the sky along the ecliptic, suggesting that the sculptor made the change because of his lack of astronomical knowledge. (8) The stri ...
Chapter 10 Formation and evolution of the Local Group
... Summary: The Local Group (LG) is the group of galaxies gravitationally associated with the Galaxy and M 31. Galaxies within the LG have overcome the general expansion of the universe. There are approximately 75 galaxies in the LG within a diameter of ∼3 Mpc having a total mass of 2-5 × 1012 M⊙ . A s ...
... Summary: The Local Group (LG) is the group of galaxies gravitationally associated with the Galaxy and M 31. Galaxies within the LG have overcome the general expansion of the universe. There are approximately 75 galaxies in the LG within a diameter of ∼3 Mpc having a total mass of 2-5 × 1012 M⊙ . A s ...
Binarity in carbon-enhanced metal-poor stars
... Pb absorption lines are very weak and the strongest line in the optical overlaps with the CH feature, this hypothesis is difficult to test, especially in C-rich stars. A robust upper limit could nonetheless be given for the brightest CEMP-no star, BD +44-493, which did not show the predicted overabu ...
... Pb absorption lines are very weak and the strongest line in the optical overlaps with the CH feature, this hypothesis is difficult to test, especially in C-rich stars. A robust upper limit could nonetheless be given for the brightest CEMP-no star, BD +44-493, which did not show the predicted overabu ...
bode elert johann
... maps were ideal for Herschel’s star reviews. For he was not interested in absolute positions, and so the (early) epoch of 1690 was no problem.36 Occasionally he encountered a star that was not plotted. This first happened on 18 February 1780, when he saw “a star not marked in my map tho’ visible to ...
... maps were ideal for Herschel’s star reviews. For he was not interested in absolute positions, and so the (early) epoch of 1690 was no problem.36 Occasionally he encountered a star that was not plotted. This first happened on 18 February 1780, when he saw “a star not marked in my map tho’ visible to ...
Stars, Galaxies, Superuniverses and the Urantia Book, by Frederick
... The Urantia Book is probably referring here to the Hale (Mt Palomar) telescope, which went into operation in 1948. The figure 375 million thus refers to the additional new galaxies observable when the Hale telescope was put into operation, not the number of galaxies in the master universe. Recently ...
... The Urantia Book is probably referring here to the Hale (Mt Palomar) telescope, which went into operation in 1948. The figure 375 million thus refers to the additional new galaxies observable when the Hale telescope was put into operation, not the number of galaxies in the master universe. Recently ...
ancient cultures 114 - Stellenbosch University
... astronomical texts, known as astrolabes, had already appeared – texts which made use of astronomical observations to serve calendar functions. During the Neo-Assyrian period (9th-7th centuries BCE), individual scholars were tasked to observing the heavens in order to make predictions of the future f ...
... astronomical texts, known as astrolabes, had already appeared – texts which made use of astronomical observations to serve calendar functions. During the Neo-Assyrian period (9th-7th centuries BCE), individual scholars were tasked to observing the heavens in order to make predictions of the future f ...
The Life Cycle of Stars: Supernovae in Starbursts by Jason Kezwer
... Figure 3.5 Sample Arp 220 nuclear light curve in the K-band from differential photometry relative to a single reference star. Photometry was performed using an aperture radius of 1.5 arcsec as described in the text. The red horizontal line denotes the baseline- the mean difference between Arp 220 an ...
... Figure 3.5 Sample Arp 220 nuclear light curve in the K-band from differential photometry relative to a single reference star. Photometry was performed using an aperture radius of 1.5 arcsec as described in the text. The red horizontal line denotes the baseline- the mean difference between Arp 220 an ...
A spectroscopic investigation of the O-type star - ORBi
... Results. We confirm the binarity for four objects: HD 193443, HD 228989, HD 229234 and HD 194649. We derive for the first time the orbital solutions of three systems, and we confirm the values of the fourth, showing that these four systems all have orbital periods shorter than 10 days. Besides these ...
... Results. We confirm the binarity for four objects: HD 193443, HD 228989, HD 229234 and HD 194649. We derive for the first time the orbital solutions of three systems, and we confirm the values of the fourth, showing that these four systems all have orbital periods shorter than 10 days. Besides these ...
365 days of SKYWATCHING
... night as the terminator - the line between sunset and shadow - progresses over the surface, revealing new details. Unlike a star chart, Moon feature instructions are based on lunar topography and not our Earthly cardinal directions. While these pages outline what features should be visible on any gi ...
... night as the terminator - the line between sunset and shadow - progresses over the surface, revealing new details. Unlike a star chart, Moon feature instructions are based on lunar topography and not our Earthly cardinal directions. While these pages outline what features should be visible on any gi ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... penetrate the haze of the Milky Way by detecting radiation that is unaffected by dust obscuration. These searches are almost certain to reveal several new Local Group members in coming years. Another complication in producing a complete census of the Local Group is the uncertainty involved with defi ...
... penetrate the haze of the Milky Way by detecting radiation that is unaffected by dust obscuration. These searches are almost certain to reveal several new Local Group members in coming years. Another complication in producing a complete census of the Local Group is the uncertainty involved with defi ...
Educator`s Guide
... The Orion Educator’s Guide is designed for Planetarians, Teachers, and parents. The information is researched, organized, and laid out so that the educator need not spend hours coming up with lesson plans or labs. This has already been accomplished by certified educators. The guide is written to all ...
... The Orion Educator’s Guide is designed for Planetarians, Teachers, and parents. The information is researched, organized, and laid out so that the educator need not spend hours coming up with lesson plans or labs. This has already been accomplished by certified educators. The guide is written to all ...
Legends Night Sky Orion
... The Orion Educator’s Guide is designed for Planetarians, Teachers, and parents. The information is researched, organized, and laid out so that the educator need not spend hours coming up with lesson plans or labs. This has already been accomplished by certified educators. The guide is written to all ...
... The Orion Educator’s Guide is designed for Planetarians, Teachers, and parents. The information is researched, organized, and laid out so that the educator need not spend hours coming up with lesson plans or labs. This has already been accomplished by certified educators. The guide is written to all ...
Star Clusters - Caltech Astronomy
... of the same origin) and which at the same time are sufficiently rich in stars for statistical investigation.’ Since virtually all clusters have been discovered either by visual examination of the sky with a telescope, or from inspection of photographic or electronic images in the visual or infrared, ...
... of the same origin) and which at the same time are sufficiently rich in stars for statistical investigation.’ Since virtually all clusters have been discovered either by visual examination of the sky with a telescope, or from inspection of photographic or electronic images in the visual or infrared, ...
Aries (constellation)
Aries is one of the constellations of the zodiac. It is located in the northern celestial hemisphere between Pisces to the west and Taurus to the east. The name Aries is Latin for ram, and its symbol is 20px (Unicode ♈), representing a ram's horns. It is one of the 48 constellations described by the 2nd century astronomer Ptolemy, and remains one of the 88 modern constellations. It is a mid-sized constellation, ranking 39th overall size, with an area of 441 square degrees (1.1% of the celestial sphere).Although Aries came to represent specifically the ram whose fleece became the Golden Fleece of Ancient Greek mythology, it has represented a ram since late Babylonian times. Before that, the stars of Aries formed a farmhand. Different cultures have incorporated the stars of Aries into different constellations including twin inspectors in China and a porpoise in the Marshall Islands. Aries is a relatively dim constellation, possessing only four bright stars: Hamal (Alpha Arietis, second magnitude), Sheratan (Beta Arietis, third magnitude), Mesarthim (Gamma Arietis, fourth magnitude), and 41 Arietis (also fourth magnitude). The few deep-sky objects within the constellation are quite faint and include several pairs of interacting galaxies. Several meteor showers appear to radiate from Aries, including the Daytime Arietids and the Epsilon Arietids.