Stellar populations in the nuclear regions of nearby radio galaxies
... respectively. This configuration provides the spectral resolution necessary to resolve the Mg b and CaT features and, at the same at 5.1-Å time, offers a wide spectral span: l3350–6000 A at 3.5-Å resolution in resolution in the blue and l7900–9400 A the red. In the 1997 run, in which we assess ...
... respectively. This configuration provides the spectral resolution necessary to resolve the Mg b and CaT features and, at the same at 5.1-Å time, offers a wide spectral span: l3350–6000 A at 3.5-Å resolution in resolution in the blue and l7900–9400 A the red. In the 1997 run, in which we assess ...
Summary of Talks at Growing Black Holes 2004 in Garching
... to estimates of quasar lifetimes. At z < 2.5, SDSS clustering scale is about 7 Mpc. There is now preliminary, tentative evidence for correlation length to increase with redshift. Spectra of emission lines in high z quasars & Continuum shape consistent with lower z objects -> implication : rapid ch ...
... to estimates of quasar lifetimes. At z < 2.5, SDSS clustering scale is about 7 Mpc. There is now preliminary, tentative evidence for correlation length to increase with redshift. Spectra of emission lines in high z quasars & Continuum shape consistent with lower z objects -> implication : rapid ch ...
Distance determination for RAVE stars using stellar models
... spirals, and finally dwarf galaxies. The power spectrum is used to measure the power of density perturbations on a certain scale. The current cosmological model predicts a HarrisonZel’dovich spectrum (P (k) ∝ k, where k is the wavenumber). This power spectrum predicts more power on small scale, so t ...
... spirals, and finally dwarf galaxies. The power spectrum is used to measure the power of density perturbations on a certain scale. The current cosmological model predicts a HarrisonZel’dovich spectrum (P (k) ∝ k, where k is the wavenumber). This power spectrum predicts more power on small scale, so t ...
The 2008 RBSE Journal - National Optical Astronomy Observatory
... A Double Radio Source Associated with a Galactic Nucleus (DRAGN) is a radio source that is produced by jets produced by active galactic nucleus that is not in the Milky Way. This happens when an accretion disk forms around a black hole and spins, converts gravitational and rotational energy into exc ...
... A Double Radio Source Associated with a Galactic Nucleus (DRAGN) is a radio source that is produced by jets produced by active galactic nucleus that is not in the Milky Way. This happens when an accretion disk forms around a black hole and spins, converts gravitational and rotational energy into exc ...
Measuring distances to the edge of the local group
... Scientific Justification Be sure to include overall significance to astronomy. For standard proposals limit text to one page with figures, captions and references on no more than two additional pages. We propose to measure the distance to the nearby dwarf irregular galaxies Sextans A, B, and NGC 310 ...
... Scientific Justification Be sure to include overall significance to astronomy. For standard proposals limit text to one page with figures, captions and references on no more than two additional pages. We propose to measure the distance to the nearby dwarf irregular galaxies Sextans A, B, and NGC 310 ...
When we look at a neighboring galaxy (such as M31, the
... The Andromeda Galaxy, also known as M31, is a spiral galaxy physically larger, but less massive, than our Milky Way Galaxy. The Andromeda is the largest member of the Local Group, a cluster of about 30 galaxies that are gravitationally attracted to one another. At a distance of 2.5 million light-yea ...
... The Andromeda Galaxy, also known as M31, is a spiral galaxy physically larger, but less massive, than our Milky Way Galaxy. The Andromeda is the largest member of the Local Group, a cluster of about 30 galaxies that are gravitationally attracted to one another. At a distance of 2.5 million light-yea ...
allowed planetary orbits
... Hence, we pass to theories of the origin of the solar system and demonstrations of the chaotic dynamics and planetary migration, which at present lead to new theories of the origin of the solar system and exoplanets. We provide a review of the quantization on a cosmic scale and its application to de ...
... Hence, we pass to theories of the origin of the solar system and demonstrations of the chaotic dynamics and planetary migration, which at present lead to new theories of the origin of the solar system and exoplanets. We provide a review of the quantization on a cosmic scale and its application to de ...
A new view of galaxy evolution
... These galaxies are very bright and thus traditional way to find distant galaxies easy to see because they are undergoing intense and is being used today to find the most distant star formation, a common process in the early galaxies in the universe. universe. However, there are also galaxies that We ...
... These galaxies are very bright and thus traditional way to find distant galaxies easy to see because they are undergoing intense and is being used today to find the most distant star formation, a common process in the early galaxies in the universe. universe. However, there are also galaxies that We ...
celt mthr spectrometer
... Fischer) made all these M dwarf-host planet detections using the HIRES high resolution optical spectrometer at Keck. We currently have over 120 other M dwarfs, as late as M5.5V under survey. Aside from the relatively large amounts of telescope time needed, these planet detections were not all that d ...
... Fischer) made all these M dwarf-host planet detections using the HIRES high resolution optical spectrometer at Keck. We currently have over 120 other M dwarfs, as late as M5.5V under survey. Aside from the relatively large amounts of telescope time needed, these planet detections were not all that d ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the mai ...
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the mai ...
Measurements of Neutron Star Masses
... develops (34), even if strange quark matter is densities, the nuclear lattice can turn insidenot the ultimate ground state of matter. Delinout and form a lattice of voids, which is eating the phase structure of dense cold quark eventually squeezed out at densities near n0 (32). If so, beginning at a ...
... develops (34), even if strange quark matter is densities, the nuclear lattice can turn insidenot the ultimate ground state of matter. Delinout and form a lattice of voids, which is eating the phase structure of dense cold quark eventually squeezed out at densities near n0 (32). If so, beginning at a ...
ROTATION CURVES OF HIGH-LUMINOSITY SPIRAL GALAXIES
... 4-m spectrographs plus Carnegie image tube, generally at a dispersion of 25A/mm. Errors in the rotational velocities (measuring errors plus projection uncertainties) are generally less than 8 km/s per point. Reproductions of 10 spectra are shown in Fig. 1. Rotation curves are drawn in Fig. 2; data f ...
... 4-m spectrographs plus Carnegie image tube, generally at a dispersion of 25A/mm. Errors in the rotational velocities (measuring errors plus projection uncertainties) are generally less than 8 km/s per point. Reproductions of 10 spectra are shown in Fig. 1. Rotation curves are drawn in Fig. 2; data f ...
The DBV stars: Progress and problems
... studied, some DB white dwarfs should be descendants of IBWD systems, based on circumstantial evidence. As the name implies, the IBWD stars are already white dwarfs, there is no evidence for hydrogen in either star, the mass gaining star has an effective temperature at or above the red edge of the “D ...
... studied, some DB white dwarfs should be descendants of IBWD systems, based on circumstantial evidence. As the name implies, the IBWD stars are already white dwarfs, there is no evidence for hydrogen in either star, the mass gaining star has an effective temperature at or above the red edge of the “D ...
Extrasolar Cosmochemistry
... be a strong relative depletion of those heavy elements that settle the fastest. Finally, even if a white dwarf has a circumstellar disk, the accretion need not be steady with time (Rafikov 2011b, www.annualreviews.org • Extrasolar Cosmochemistry ...
... be a strong relative depletion of those heavy elements that settle the fastest. Finally, even if a white dwarf has a circumstellar disk, the accretion need not be steady with time (Rafikov 2011b, www.annualreviews.org • Extrasolar Cosmochemistry ...
The Danish 1.5 m Telescope in Operation!
... The optical characteristics of the telescope make it especially suitable for direct observations with photographic as weil as more advanced detectors. For sufficiently accurate guiding of long exposures an automatic guiding system is essential, particularly because the asymmetric mounting of our tel ...
... The optical characteristics of the telescope make it especially suitable for direct observations with photographic as weil as more advanced detectors. For sufficiently accurate guiding of long exposures an automatic guiding system is essential, particularly because the asymmetric mounting of our tel ...
Eye in the sky - Academy of Science of South Africa
... see?’. The larger the telescope, the fainter the objects it can detect, since the more photons, or light particles, it can collect in a given time. In addition, with telescopes and their associated cameras you can keep collecting the light for long times, equivalent to leaving a bucket out in the ra ...
... see?’. The larger the telescope, the fainter the objects it can detect, since the more photons, or light particles, it can collect in a given time. In addition, with telescopes and their associated cameras you can keep collecting the light for long times, equivalent to leaving a bucket out in the ra ...
mg_colloq - University of Massachusetts Amherst
... Ellipticals: key testing grounds • Include the oldest, most massive galaxies • Formed the bulk of their stellar mass at high redshift, on short time scale: ≈90% at z>2 (Renzini 2006) • Probes of the physics of early star formation • Evolved passively since ...
... Ellipticals: key testing grounds • Include the oldest, most massive galaxies • Formed the bulk of their stellar mass at high redshift, on short time scale: ≈90% at z>2 (Renzini 2006) • Probes of the physics of early star formation • Evolved passively since ...
Essential physics of early galaxy formation
... medium (IGM) or to be brought in by mergers to re-ignite further star formation. As halos build-up mass with time, their DM potential well can sustain much larger star formation rates (SFR) without losing gas. This naturally implies that, at any given time, there is a limiting star formation efficie ...
... medium (IGM) or to be brought in by mergers to re-ignite further star formation. As halos build-up mass with time, their DM potential well can sustain much larger star formation rates (SFR) without losing gas. This naturally implies that, at any given time, there is a limiting star formation efficie ...
The formation of disc galaxies in high-resolution moving
... In this paper, we study the problem by applying a newly developed numerical methodology for cosmological galaxy formation to ‘zoom’ simulations of Milky Way-sized galaxies. The objects we study are taken from the Aquarius project (Springel et al. 2008), where they have been examined in great detail ...
... In this paper, we study the problem by applying a newly developed numerical methodology for cosmological galaxy formation to ‘zoom’ simulations of Milky Way-sized galaxies. The objects we study are taken from the Aquarius project (Springel et al. 2008), where they have been examined in great detail ...
Galaxies - Valhalla High School
... Some galaxies are spiral like the Milky Way while others are egg-shaped or completely irregular in appearance Besides shape, galaxies vary greatly in the star, gas, and dust content and some are more “active” than others Galaxies tend to cluster together and these clusters appear to be separating fr ...
... Some galaxies are spiral like the Milky Way while others are egg-shaped or completely irregular in appearance Besides shape, galaxies vary greatly in the star, gas, and dust content and some are more “active” than others Galaxies tend to cluster together and these clusters appear to be separating fr ...
Observing Stellar Evolution
... generations of stars generated the elements that make up our planet and the chemical elements required for life. It is not an understatement to say that we exist because stars exist. The Observing Stellar Evolution Observing Program will be of interest to beginning observers as well as more experien ...
... generations of stars generated the elements that make up our planet and the chemical elements required for life. It is not an understatement to say that we exist because stars exist. The Observing Stellar Evolution Observing Program will be of interest to beginning observers as well as more experien ...
Effect of the stellar spin history on the tidal evolution of close
... close-in gas giants orbiting highly dissipative stars. However, for very low-mass stars the effect of the initial rotation of the star on the planet’s evolution is apparent for less massive (1 M⊕ ) planets and typical dissipation values. We also find that planetary evolution can have significant effec ...
... close-in gas giants orbiting highly dissipative stars. However, for very low-mass stars the effect of the initial rotation of the star on the planet’s evolution is apparent for less massive (1 M⊕ ) planets and typical dissipation values. We also find that planetary evolution can have significant effec ...
Galaxy Spiral Arms
... tapering Spiral Arms of our Galaxy. That is, radially inward from where we are, there are very few nearby stars (for several thousand Light Years distance). In contrast with that, radially outward from where we are, there are many millions of stars within that same several thousand Light Years dista ...
... tapering Spiral Arms of our Galaxy. That is, radially inward from where we are, there are very few nearby stars (for several thousand Light Years distance). In contrast with that, radially outward from where we are, there are many millions of stars within that same several thousand Light Years dista ...
21_Testbank
... 2) Why are telescopes sometimes called "time machines"? A) because the author, H.G. Wells, used the term to describe telescopes in a book B) because some of the oldest telescopes are still in use today C) because observations of distant objects reveal them as they were in the past D) because astrono ...
... 2) Why are telescopes sometimes called "time machines"? A) because the author, H.G. Wells, used the term to describe telescopes in a book B) because some of the oldest telescopes are still in use today C) because observations of distant objects reveal them as they were in the past D) because astrono ...
The Astrophysics of Planetary Habitability
... 2.5. An age-period-activity relation for M dwarfs: implications for planetary habitability . . . . . . . . . . . . . . . . . . . . . . . . . . . 34 2.6. The effects of M dwarf magnetic fields and winds on potentially habitable planets . . . . . . . . . . . . . . . . . . . . . . . . . . . 35 2.7. Mag ...
... 2.5. An age-period-activity relation for M dwarfs: implications for planetary habitability . . . . . . . . . . . . . . . . . . . . . . . . . . . 34 2.6. The effects of M dwarf magnetic fields and winds on potentially habitable planets . . . . . . . . . . . . . . . . . . . . . . . . . . . 35 2.7. Mag ...
Space Interferometry Mission
The Space Interferometry Mission, or SIM, also known as SIM Lite (formerly known as SIM PlanetQuest), was a planned space telescope developed by the U.S. National Aeronautics and Space Administration (NASA), in conjunction with contractor Northrop Grumman. One of the main goals of the mission was the hunt for Earth-sized planets orbiting in the habitable zones of nearby stars other than the Sun. SIM was postponed several times and finally cancelled in 2010.In addition to hunting for extrasolar planets, SIM would have helped astronomers construct a map of the Milky Way galaxy. Other important tasks would have included collecting data to help pinpoint stellar masses for specific types of stars, assisting in the determination of the spatial distribution of dark matter in the Milky Way and in the Local Group of galaxies and using the gravitational microlensing effect to measure the mass of stars.The spacecraft would have used optical interferometry to accomplish these and other scientific goals. This technique collects light with multiple mirrors (in SIM's case, two) which is combined to make an interference pattern which can be very precisely measured.The initial contracts for SIM Lite were awarded in 1998, totaling US$200 million. Work on the SIM project required scientists and engineers to move through eight specific new technology milestones, and by November 2006, all eight had been completed.SIM Lite was originally scheduled for a 2005 launch, aboard an Evolved Expendable Launch Vehicle (EELV). As a result of continued budget cuts, the launch date has been pushed back at least five times. NASA has set a preliminary launch date for 2015 and U.S. federal budget documents confirm that a launch date is expected ""no earlier"" than 2015. The budget cuts to SIM Lite are expected to continue through FY 2010. As of February 2007, many of the engineers working on the SIM program had moved on to other areas and projects, and NASA directed the project to allocate its resources toward engineering risk reduction. However, the preliminary budget for NASA for 2008 included zero dollars for SIM.In December 2007, the Congress restored funding for fiscal year 2008 as part of an omnibus appropriations bill which the President later signed. At the same time the Congress directed NASA to move the mission forward to the development phase. In 2009 the project continued its risk reduction work while waiting for the findings and recommendations of the Astronomy and Astrophysics Decadal Survey, Astro2010, performed by the National Academy of Sciences, which would determine the project's future.On 13 August 2010, the Astro2010 Decadal Report was released and did not recommend that NASA continue the development of the SIM Lite Astrometric Observatory. This prompted NASA Astronomy and Physics Director, Jon Morse, to issue a letter on 24 September 2010 to the SIM Lite project manager, informing him that NASA was discontinuing its sponsorship of the SIM Lite mission and directing the project to discontinue Phase B activities immediately or as soon as practical. Accordingly, all SIM Lite activities were closed down by the end of calendar year 2010.