Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of
... “A really correct and reliable edition, with reproductions of the drawings in the original shape, using some of the oldest extant manuscripts remains a desideratum,” (Kunitzsch, 1989). This was what Professor Paul Kunitzsch wrote when he was describing one of the most important books in the history ...
... “A really correct and reliable edition, with reproductions of the drawings in the original shape, using some of the oldest extant manuscripts remains a desideratum,” (Kunitzsch, 1989). This was what Professor Paul Kunitzsch wrote when he was describing one of the most important books in the history ...
SXDS Highlights : Subaru / FOCAS Spectroscopy
... HST/NICMOS H-band Observations are not sufficient ! H-band observation only covers up to 4000A in the rest-frame, and star-forming regions can dominate the morphology. HST/NICMOS sample is limited to a small number of objects in Hubble Deep Field and does not have bright (~Mv*) galaxies at z~3. The ...
... HST/NICMOS H-band Observations are not sufficient ! H-band observation only covers up to 4000A in the rest-frame, and star-forming regions can dominate the morphology. HST/NICMOS sample is limited to a small number of objects in Hubble Deep Field and does not have bright (~Mv*) galaxies at z~3. The ...
Understanding the Astrophysics of Galaxy Evolution: the role of
... correlated with dark matter halo mass and so the best link to the underlying cosmological model. A survey must be large (∼ few ×105 galaxies) in order to disentangle covariances in the physical properties of galaxies. One reason it is so difficult to understand how galaxies form is because almost al ...
... correlated with dark matter halo mass and so the best link to the underlying cosmological model. A survey must be large (∼ few ×105 galaxies) in order to disentangle covariances in the physical properties of galaxies. One reason it is so difficult to understand how galaxies form is because almost al ...
X. Nuclear star clusters in low-mass early-type galaxies
... At faint magnitudes, the dominant noise is a combination of the readnoise and the sky background noise with a small contribution of Poisson noise from the host galaxy (see also Section 4.3 and Fig. 6). For a host galaxy absolute magnitude MF814W = −13 mag, the difference between the host galaxy magn ...
... At faint magnitudes, the dominant noise is a combination of the readnoise and the sky background noise with a small contribution of Poisson noise from the host galaxy (see also Section 4.3 and Fig. 6). For a host galaxy absolute magnitude MF814W = −13 mag, the difference between the host galaxy magn ...
Galaxy Evolution
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
Galaxies - WordPress.com
... A galaxies occasionally collide with one another, particularly within cluster of galaxies B galaxies are so closely packed in the universe that they are always interacting with one another C galaxies are so widely separated that they never interact or collide D the universe is composed of one giant ...
... A galaxies occasionally collide with one another, particularly within cluster of galaxies B galaxies are so closely packed in the universe that they are always interacting with one another C galaxies are so widely separated that they never interact or collide D the universe is composed of one giant ...
here - NASA/IPAC Extragalactic Database
... be called spectroscopically an O4 V. This includes any star with a mass from ∼35M⊙ to ∼85M⊙. There are a few other caveats that need to be kept in mind when talking about the main-sequence evolution of massive stars. First, the luminosity class (“I” vs “V”, say) of O-type stars depends primarily on ...
... be called spectroscopically an O4 V. This includes any star with a mass from ∼35M⊙ to ∼85M⊙. There are a few other caveats that need to be kept in mind when talking about the main-sequence evolution of massive stars. First, the luminosity class (“I” vs “V”, say) of O-type stars depends primarily on ...
Document
... To this day, the objects in Messier’s list are commonly known by their Messier numbers (see figures). They are among the brightest and most beautiful objects in the sky visible from mid-northern latitudes. A set of photographs of all the Messier objects appears as an Appendix. ...
... To this day, the objects in Messier’s list are commonly known by their Messier numbers (see figures). They are among the brightest and most beautiful objects in the sky visible from mid-northern latitudes. A set of photographs of all the Messier objects appears as an Appendix. ...
Colloquial Jakartan Indonesian
... which are descended existing terms and meanings associated with the field of navigation. For the most part they are terms of the physical world, of the night sky and the ocean seascape. Also explored are terms such as the Polynesian kaveŋa (star or other object for which one steers) and the Micrones ...
... which are descended existing terms and meanings associated with the field of navigation. For the most part they are terms of the physical world, of the night sky and the ocean seascape. Also explored are terms such as the Polynesian kaveŋa (star or other object for which one steers) and the Micrones ...
Lecture-25 Notes - Georgia Southern University Astrophysics
... distances from us. 2) Telescopic surveys try to measure as many spectra as possible, and derive distances using “Hubble Law”. 3) Galaxies are found along vast “sheets” surrounding ~Mpc sized “voids” where few galaxies are found. Galaxy clusters appear as large (~2-5 Mpc) concentrations on ...
... distances from us. 2) Telescopic surveys try to measure as many spectra as possible, and derive distances using “Hubble Law”. 3) Galaxies are found along vast “sheets” surrounding ~Mpc sized “voids” where few galaxies are found. Galaxy clusters appear as large (~2-5 Mpc) concentrations on ...
20_Testbank
... B) two clumps, one blue with relatively low luminosity, one red with relatively high luminosity, and a valley in between with few galaxies C) a continuum from faint, blue galaxies to bright, red galaxies D) a continuum from faint, red galaxies to bright, blue galaxies E) A main sequence, just as for ...
... B) two clumps, one blue with relatively low luminosity, one red with relatively high luminosity, and a valley in between with few galaxies C) a continuum from faint, blue galaxies to bright, red galaxies D) a continuum from faint, red galaxies to bright, blue galaxies E) A main sequence, just as for ...
Discovery of White Dwarfs—1 Oct • Adams’ discovery
... Abs mag of a star is its apparent mag if the star is moved to a distance of 10 pc. If the abs mag changes by -2.5 mag, the luminosity is brighter by a factor of 10. ...
... Abs mag of a star is its apparent mag if the star is moved to a distance of 10 pc. If the abs mag changes by -2.5 mag, the luminosity is brighter by a factor of 10. ...
ASPEN WORKSHOP 2003
... ellipticals, larger in bluer galaxies, up to few tenths. AI(Red), or AI(Blue) >0.3 suggests interaction, as in half of ULIRGS [as long as they are identified as “single galaxy”!] Simulations show that AI stays above 0.35 for about 700 Myears, but NOT for face-on HDF application: rest frame B morphol ...
... ellipticals, larger in bluer galaxies, up to few tenths. AI(Red), or AI(Blue) >0.3 suggests interaction, as in half of ULIRGS [as long as they are identified as “single galaxy”!] Simulations show that AI stays above 0.35 for about 700 Myears, but NOT for face-on HDF application: rest frame B morphol ...
Activity III: Calibrating Images
... When you observe stars with your eyes, or with a telescope, you are receiving starlight that has traveled vast distances. Amazingly, the light remains virtually unaffected by the first 99.999999999999% or so of its journey. However, in the trip through the Earth’s atmosphere, and even through the op ...
... When you observe stars with your eyes, or with a telescope, you are receiving starlight that has traveled vast distances. Amazingly, the light remains virtually unaffected by the first 99.999999999999% or so of its journey. However, in the trip through the Earth’s atmosphere, and even through the op ...
The Stars - Springer
... Ionized calcium (CaII), weak hydrogen CaII prominent, very weak hydrogen Neutral metals, faint hydrogen, hydrocarbon bands Molecular bands, titanium oxide (TiO) ...
... Ionized calcium (CaII), weak hydrogen CaII prominent, very weak hydrogen Neutral metals, faint hydrogen, hydrocarbon bands Molecular bands, titanium oxide (TiO) ...
The Big Bang
... • Earth-Sun distance is 1.5x108 km, so at this very moment we see the sun as it looked 500 sec = 8.3 min ago • distance to the closest star is about 3 light years, so when we look at this star we see it as it looked 3 years ago • distance to our “sister galaxy” (M31) is about 2.6 million light years ...
... • Earth-Sun distance is 1.5x108 km, so at this very moment we see the sun as it looked 500 sec = 8.3 min ago • distance to the closest star is about 3 light years, so when we look at this star we see it as it looked 3 years ago • distance to our “sister galaxy” (M31) is about 2.6 million light years ...
Lab 14 Galaxy Morphology
... Figure 14.1: A fisheye lens view of the summertime sky showing the band of light called the Milky Way. This faint band of light is composed of the light from thousands and thousands of very faint stars. The Milky Way spans a complete circle across the celestial sphere because our solar system is loc ...
... Figure 14.1: A fisheye lens view of the summertime sky showing the band of light called the Milky Way. This faint band of light is composed of the light from thousands and thousands of very faint stars. The Milky Way spans a complete circle across the celestial sphere because our solar system is loc ...
Stellar populations in the nuclear regions of nearby radio galaxies
... galaxy (DA 240) was observed with this alternative setup. The dichroics 5700 and 6100 were used in 1997 November and 1998 February, and in both runs we used a filter to avoid second-order contamination in the spectra. We obtained flux standards (HZ 44 and G1912 B2B) for the four nights and gratings, ...
... galaxy (DA 240) was observed with this alternative setup. The dichroics 5700 and 6100 were used in 1997 November and 1998 February, and in both runs we used a filter to avoid second-order contamination in the spectra. We obtained flux standards (HZ 44 and G1912 B2B) for the four nights and gratings, ...
Chromospherically young, kinematically old stars
... analogy to their first discovery by Soderblom. Not all objects identified in a U × V diagram are also identified in a W × V diagram, and vice versa. We expect that CYKOS showing high velocities in more than one component are really peculiar objects, and not just stars having a component velocity in ...
... analogy to their first discovery by Soderblom. Not all objects identified in a U × V diagram are also identified in a W × V diagram, and vice versa. We expect that CYKOS showing high velocities in more than one component are really peculiar objects, and not just stars having a component velocity in ...
Stars & Galaxies - newmanlib.ibri.org
... that they differ in brightness. • As one looks at the stars more carefully, it becomes apparent that they are not all the same color. • Look at the constellation of Orion shown in the next panel. ...
... that they differ in brightness. • As one looks at the stars more carefully, it becomes apparent that they are not all the same color. • Look at the constellation of Orion shown in the next panel. ...
PDF - ASSA
... of other properties. At the same time, some pairs can be amazingly frustrating. The bright, third magnitude upsilon Carinae, at the southern edge of the rich southern ...
... of other properties. At the same time, some pairs can be amazingly frustrating. The bright, third magnitude upsilon Carinae, at the southern edge of the rich southern ...
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 ...
The evolution of spiral galaxies in clusters Kutdemir, Elif
... studied in different environmental conditions and at different lookback times to understand their formation, evolution and the origin of the variety in their morphological properties. Their diversity was studied for the first time in 1926 by Edwin Hubble, who expressed it in his well-known classific ...
... studied in different environmental conditions and at different lookback times to understand their formation, evolution and the origin of the variety in their morphological properties. Their diversity was studied for the first time in 1926 by Edwin Hubble, who expressed it in his well-known classific ...
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.