Galaxy Spiral Arms
... Galaxy were a uniform distribution of stars and other mass, the usage of Kepler's Laws would not be too terribly wrong. But our Sun and Earth happen to be near the (inner) edge of one of the tapering Spiral Arms of our Galaxy. That is, radially inward from where we are, there are very few nearby sta ...
... Galaxy were a uniform distribution of stars and other mass, the usage of Kepler's Laws would not be too terribly wrong. But our Sun and Earth happen to be near the (inner) edge of one of the tapering Spiral Arms of our Galaxy. That is, radially inward from where we are, there are very few nearby sta ...
Stars and Galaxies - Red Hook Central Schools
... Images at http://hubblesite.org/newscenter/archive/releases/galaxy/elliptical/2007/08/image/a/format/large_web/results/50/ and http://hubblesite.org/newscenter/archive/releases/galaxy/elliptical/1995/07/results/50/ ...
... Images at http://hubblesite.org/newscenter/archive/releases/galaxy/elliptical/2007/08/image/a/format/large_web/results/50/ and http://hubblesite.org/newscenter/archive/releases/galaxy/elliptical/1995/07/results/50/ ...
Stellar Populations of Dwarf Elliptical Galaxies: UBVRI Photometry
... formation with subsequent blow-out of the ISM (e.g., Dekel & Silk 1986), or ram pressure stripping of the ISM as the galaxy plunges through the hot intra-cluster gas (e.g., Lin & Faber 1983). Both of these scenarios will result in an overabundance of dwarf elliptical galaxies in high density regions ...
... formation with subsequent blow-out of the ISM (e.g., Dekel & Silk 1986), or ram pressure stripping of the ISM as the galaxy plunges through the hot intra-cluster gas (e.g., Lin & Faber 1983). Both of these scenarios will result in an overabundance of dwarf elliptical galaxies in high density regions ...
Girardi
... NO. 6 Gyr old RC stars are ∼ 1.4 times more frequent than the 10-Gyr old, mainly because they leave the MS at a faster rate, and despite the IMF favouring old stars. Similar conclusions will apply to RGB stars. ...
... NO. 6 Gyr old RC stars are ∼ 1.4 times more frequent than the 10-Gyr old, mainly because they leave the MS at a faster rate, and despite the IMF favouring old stars. Similar conclusions will apply to RGB stars. ...
Recipes for ULX formation: necessary ingredients and garnishments
... Myr (Portegies Zwart & McMillan 2002). However, we have argued that there is no longer a compelling need to invoke intermediate-mass BHs in ULXs, and that the upper mass limit is likely to be somewhere between 50 and 200M . Correspondingly, if dynamical collapse and merger processes are still neede ...
... Myr (Portegies Zwart & McMillan 2002). However, we have argued that there is no longer a compelling need to invoke intermediate-mass BHs in ULXs, and that the upper mass limit is likely to be somewhere between 50 and 200M . Correspondingly, if dynamical collapse and merger processes are still neede ...
Investigate Planets, Stars, Galaxies, and the Universe
... To complete the jigsaw, have students return to their home groups to share their expert knowledge. Afterwards, you may wish to gather the class together and guide a class discussion, using questions such as: •W hat is a star? What are the characteristics of a star? (Answers may include: Stars, inc ...
... To complete the jigsaw, have students return to their home groups to share their expert knowledge. Afterwards, you may wish to gather the class together and guide a class discussion, using questions such as: •W hat is a star? What are the characteristics of a star? (Answers may include: Stars, inc ...
1. setting the scene 2. the cosmic dark ages and the first stars
... provide a backdrop against which the absorption lines produced by intervening gas, in galaxies and the intergalactic medium, can be studied in much more detail than would otherwise be possible. In Figure 3 different classes of absorption lines are indicated. Most of the ‘hydrogen absorption’ is prod ...
... provide a backdrop against which the absorption lines produced by intervening gas, in galaxies and the intergalactic medium, can be studied in much more detail than would otherwise be possible. In Figure 3 different classes of absorption lines are indicated. Most of the ‘hydrogen absorption’ is prod ...
Science with IMACS on Magellan
... The combination of large field and large aperture is achieved with some difficulty. The f/4.3 camera of IMACS produces an unvignetted 15-arcmin square field, comparable to DEIMOS on Keck, VIRMOS on VLT, and the planned Binospec on MMT, and an order-of-magnitude larger than LRIS or GMOS. The 27-arcmi ...
... The combination of large field and large aperture is achieved with some difficulty. The f/4.3 camera of IMACS produces an unvignetted 15-arcmin square field, comparable to DEIMOS on Keck, VIRMOS on VLT, and the planned Binospec on MMT, and an order-of-magnitude larger than LRIS or GMOS. The 27-arcmi ...
IR Universe
... IRAS discovered 6 new comets including comet IRAS-Araki-Alcock and collected infrared data on 25 previously known comets. Comets are balls of dust, rock and ice left over from the formation of the solar system. We can learn about the raw material from which the Sun and the planets formed. He ...
... IRAS discovered 6 new comets including comet IRAS-Araki-Alcock and collected infrared data on 25 previously known comets. Comets are balls of dust, rock and ice left over from the formation of the solar system. We can learn about the raw material from which the Sun and the planets formed. He ...
A GMOS dissection of the line-of
... Our observations show that there is no large cluster in front of the quasar, but rather several smaller groups at different redshifts. Hard to tell if there is strong magnification present from current data. Statistical properties of high-z radio quasars may be more useful in determining importance ...
... Our observations show that there is no large cluster in front of the quasar, but rather several smaller groups at different redshifts. Hard to tell if there is strong magnification present from current data. Statistical properties of high-z radio quasars may be more useful in determining importance ...
GAIA A Stereoscopic Census of our Galaxy
... Results: time-critical results available early (NEO, supernovae etc) ...
... Results: time-critical results available early (NEO, supernovae etc) ...
Deep Sky Catalogues, the New Uranometria and Other Stories
... Prior to the publication of the new Uranometria, Murray Cragin reported on the U.S. mailing list „amastro“ about the quality of the database (DSFG) and the involved experts. As some of my project colleagues are mentioned, I was first convinced that our work hab been taken into account. However, I wa ...
... Prior to the publication of the new Uranometria, Murray Cragin reported on the U.S. mailing list „amastro“ about the quality of the database (DSFG) and the involved experts. As some of my project colleagues are mentioned, I was first convinced that our work hab been taken into account. However, I wa ...
The Great Debate - The Story Behind The Science
... The significance of this rotational period requires understanding Shapley's size of the Milky Way. Shapley had been a supporter of the island universe idea until he determined the Milky Way to be 300,000 light-years in diameter (10x larger than the consensus estimate). He concluded this by measuring ...
... The significance of this rotational period requires understanding Shapley's size of the Milky Way. Shapley had been a supporter of the island universe idea until he determined the Milky Way to be 300,000 light-years in diameter (10x larger than the consensus estimate). He concluded this by measuring ...
Far-ultraviolet and far-infrared bivariate luminosity function of galaxies:
... star formation rate (hereafter SFR) has been of central importance to an understanding of the formation and evolution of galaxies. However, this has been a difficult task for a long time because of dust extinction. Active star formation (SF) is always accompanied by dust production through various d ...
... star formation rate (hereafter SFR) has been of central importance to an understanding of the formation and evolution of galaxies. However, this has been a difficult task for a long time because of dust extinction. Active star formation (SF) is always accompanied by dust production through various d ...
PPT presentation
... Monk et al. (1988) analysed 3.9m AAT spectra of 21 SMC and 50 LMC PNe. They found that the PN and HII region abundances of oxygen and neon agreed within the same galaxy but that the PN nitrogen was enhanced by 0.9 dex in the SMC and LMC. Interpreted as due to CN cycle processing of almost all of th ...
... Monk et al. (1988) analysed 3.9m AAT spectra of 21 SMC and 50 LMC PNe. They found that the PN and HII region abundances of oxygen and neon agreed within the same galaxy but that the PN nitrogen was enhanced by 0.9 dex in the SMC and LMC. Interpreted as due to CN cycle processing of almost all of th ...
On the Spiral Structure of the Milky Way Galaxy
... instability due to regular magnetic field directed along the arm. Observational indications for this assumption were recently found in the north-western fragment of the S4 spiral arm in the Andromeda galaxy, just the arm with regular wave-shaped magnetic field along it detected long ago [see 7, 8]. ...
... instability due to regular magnetic field directed along the arm. Observational indications for this assumption were recently found in the north-western fragment of the S4 spiral arm in the Andromeda galaxy, just the arm with regular wave-shaped magnetic field along it detected long ago [see 7, 8]. ...
San Pedro Mártir observations of microvariability in obscured quasars
... of α = 0.001 during three observing blocks. The positive detections were made for J0759+5050 (one observing block out of three) and Mrk 477 (microvariability detected in two out of two observing blocks). J0759+5050 was only variable during one of the observing blocks, we were unable to confirm the v ...
... of α = 0.001 during three observing blocks. The positive detections were made for J0759+5050 (one observing block out of three) and Mrk 477 (microvariability detected in two out of two observing blocks). J0759+5050 was only variable during one of the observing blocks, we were unable to confirm the v ...
ASTRO-114--Lecture 47-
... when the Sun is setting, you can sometimes look right at it because it’s not as bright as it is when it’s high in the sky. You can look at it and it doesn’t even hurt your eyes sometimes because it’s very red and it’s kind of faint. That’s because the dust and gas in the Earth’s atmosphere has scatt ...
... when the Sun is setting, you can sometimes look right at it because it’s not as bright as it is when it’s high in the sky. You can look at it and it doesn’t even hurt your eyes sometimes because it’s very red and it’s kind of faint. That’s because the dust and gas in the Earth’s atmosphere has scatt ...
Chapter 1 - Princeton University Press
... myriad of faint stars—faint because they are so distant. With the naked eye we can see only their combined faint glow; we cannot resolve that glow into individual stars. It took a telescope to do that. For a long time, this constituted the known universe. Our galaxy appeared to be sitting alone in s ...
... myriad of faint stars—faint because they are so distant. With the naked eye we can see only their combined faint glow; we cannot resolve that glow into individual stars. It took a telescope to do that. For a long time, this constituted the known universe. Our galaxy appeared to be sitting alone in s ...
BSA Astronomy Merit Badge
... Slurred speech or mumbling Stumbling Confusion or difficulty thinking Poor decision making, such as trying to remove warm clothes Drowsiness or very low energy Apathy, or lack of concern about one's condition Progressive loss of consciousness Weak pulse Shallow breathing ...
... Slurred speech or mumbling Stumbling Confusion or difficulty thinking Poor decision making, such as trying to remove warm clothes Drowsiness or very low energy Apathy, or lack of concern about one's condition Progressive loss of consciousness Weak pulse Shallow breathing ...
The Origin and Evolution of Dust in Galaxies
... Dust can be formed in AGB stars and SNe even at low metallicity AGE ...
... Dust can be formed in AGB stars and SNe even at low metallicity AGE ...
The Norma cluster (ACO3627) – II. The near-infrared Ks
... seem to have a steeper bright end than those without cD galaxies. Often the brightest galaxy is excluded to obtain a better fit, particularly in cD clusters. The Schechter parameters have also been found to vary depending on the region sampled within the cluster, the size of the area and the limitin ...
... seem to have a steeper bright end than those without cD galaxies. Often the brightest galaxy is excluded to obtain a better fit, particularly in cD clusters. The Schechter parameters have also been found to vary depending on the region sampled within the cluster, the size of the area and the limitin ...
Exploration of the Milky Way and Nearby galaxies
... Based on the apparent absence of the most metal-poor stars in present-day dwarf galaxies, recent studies (Helmi et al. 2006) claimed that the true Galactic building blocks must have been vastly different from the surviving dwarfs. The discovery of an extremely iron-poor star (S102054, [Fe/H] -3.8) ...
... Based on the apparent absence of the most metal-poor stars in present-day dwarf galaxies, recent studies (Helmi et al. 2006) claimed that the true Galactic building blocks must have been vastly different from the surviving dwarfs. The discovery of an extremely iron-poor star (S102054, [Fe/H] -3.8) ...
Galaxy Zoo
Galaxy Zoo is a crowdsourced astronomy project which invites people to assist in the morphological classification of large numbers of galaxies. (e.g.) It is an example of citizen science as it enlists the help of members of the public to help in scientific research. There have been seven versions up to July 2014, which are outlined in this article. Galaxy Zoo is part of the Zooniverse, a group of citizen science projects.