CHANDRA X-ray Center Ping Zhao
... relative position between the aimpoint and optical axis is the intrinsic property of the HRMA and ACA, independent of the detectors. One can therefore calculate the optical axis position on other detectors based on its relative position to the aimpoint. Figures 9 and 10 show the optical axis and aim ...
... relative position between the aimpoint and optical axis is the intrinsic property of the HRMA and ACA, independent of the detectors. One can therefore calculate the optical axis position on other detectors based on its relative position to the aimpoint. Figures 9 and 10 show the optical axis and aim ...
Stellar Populations of Dwarf Elliptical Galaxies: UBVRI Photometry
... scaled, aligned, and averaged together to make a final combined image. For the non-photometric observations (WIYN), the individual exposures were scaled to the image with the most counts; scale factors were determined based on the relative intensity of several stars in each frame. The VATT data were ...
... scaled, aligned, and averaged together to make a final combined image. For the non-photometric observations (WIYN), the individual exposures were scaled to the image with the most counts; scale factors were determined based on the relative intensity of several stars in each frame. The VATT data were ...
the stebbins galaxy: the origins of interstellar medium studies
... the inclination of many astronomers to understand the spiral nebulae as vast stellar structures (‗island universes‘ as they said) and perhaps even galaxies comparable to our own. Moreover, between about 1928 and 1930, the work of Bertil Lindblad (1895 –1965), Jan Oort (1900 –1992), and John Plaskett ...
... the inclination of many astronomers to understand the spiral nebulae as vast stellar structures (‗island universes‘ as they said) and perhaps even galaxies comparable to our own. Moreover, between about 1928 and 1930, the work of Bertil Lindblad (1895 –1965), Jan Oort (1900 –1992), and John Plaskett ...
The ALMA Universe - ALMA Observatory
... antennas from the assembly and testing site (the Operations Support Facility (OSF), located at an altitude of 2,900 meters) to their final destination on the plains of Chajnantor (at an altitude of 5,000 meters), and also later moving the antennas on the same plain when we require a change in the ar ...
... antennas from the assembly and testing site (the Operations Support Facility (OSF), located at an altitude of 2,900 meters) to their final destination on the plains of Chajnantor (at an altitude of 5,000 meters), and also later moving the antennas on the same plain when we require a change in the ar ...
Preliminary Talk Abstract Book - MoCA
... from dark matter halos to the Inter-Galactic Medium. I will first review the microphysics of this process, highlighting the various forms of feedback that emerge from star formation: radiation pressure, ionising light, stellar winds, SN explosions not to mention the production of metals and dust. Th ...
... from dark matter halos to the Inter-Galactic Medium. I will first review the microphysics of this process, highlighting the various forms of feedback that emerge from star formation: radiation pressure, ionising light, stellar winds, SN explosions not to mention the production of metals and dust. Th ...
Observational evidence for AGN feedback in early
... strength of the Balmer lines that is at least what expected by recombination theory. From the fit to the stellar continuum and absorption features, we measure the line-of-sight velocity dispersions. From subtraction of the emission-line spectrum from the observed one, we get the clean absorption lin ...
... strength of the Balmer lines that is at least what expected by recombination theory. From the fit to the stellar continuum and absorption features, we measure the line-of-sight velocity dispersions. From subtraction of the emission-line spectrum from the observed one, we get the clean absorption lin ...
Dynamical evolution of planetary systems
... There are two possible mechanisms by which we envision that giant planets can form. The first is nicknamed the “core-accretion mechanism”: the coagulation of solid particles forms a core typically of about 10 Earth masses (M⊕ ) while the gas is still present in the proto-planetary disk; the core the ...
... There are two possible mechanisms by which we envision that giant planets can form. The first is nicknamed the “core-accretion mechanism”: the coagulation of solid particles forms a core typically of about 10 Earth masses (M⊕ ) while the gas is still present in the proto-planetary disk; the core the ...
to - NexStar Resource Site
... Jupiter shines brightly at about mag. -2 +/- and along with its four largest moons Io, Europa, Ganymede and Callisto is a very easy target for binoculars and any sized telescope. Viewing Jupiter from one night to the next will always provide the observer with a different image as the gaseous clouds ...
... Jupiter shines brightly at about mag. -2 +/- and along with its four largest moons Io, Europa, Ganymede and Callisto is a very easy target for binoculars and any sized telescope. Viewing Jupiter from one night to the next will always provide the observer with a different image as the gaseous clouds ...
DUSTiNGS III: Distribution of Intermediate
... or not stellar populations extending to the outer extremities of galaxies are purely old populations (supporting in-situ star formation in a contracting gaseous disk) or a mix of intermediate-age and old stars (supporting a combination of in-situ star formation, internal drivers of extended structur ...
... or not stellar populations extending to the outer extremities of galaxies are purely old populations (supporting in-situ star formation in a contracting gaseous disk) or a mix of intermediate-age and old stars (supporting a combination of in-situ star formation, internal drivers of extended structur ...
JENAM-2011 Book of abstracts
... the Hipparcos mission. With a focal plane containing more than 100 CCD detectors, Gaia will survey the sky and repeatedly observe the brightest 1000 million objects during its 5-year lifetime. Gaia’s science data will comprise absolute astrometry, broad-band photometry, and low-resolution spectro-ph ...
... the Hipparcos mission. With a focal plane containing more than 100 CCD detectors, Gaia will survey the sky and repeatedly observe the brightest 1000 million objects during its 5-year lifetime. Gaia’s science data will comprise absolute astrometry, broad-band photometry, and low-resolution spectro-ph ...
Confirmation of Hostless Type Ia Supernovae Using Hubble Space
... The conclusion that at least some SN Ia require progenitors that are > 2 Gyr old relies on the SN Ia rate in rich cluster galaxies, where the majority of the stellar population is old (e.g. Sand et al. 2012). However, there is evidence that low levels of star formation are present in elliptical gala ...
... The conclusion that at least some SN Ia require progenitors that are > 2 Gyr old relies on the SN Ia rate in rich cluster galaxies, where the majority of the stellar population is old (e.g. Sand et al. 2012). However, there is evidence that low levels of star formation are present in elliptical gala ...
Chemical Evolution of Galactic Systems
... models, in order to gain insight into the protogalaxy’s age and star formation history. We continue investigating the high-redshift universe, turning our attention to the issue of space-time variations in the fine-structure constant, as suggested by quasar absorption-line constraints. An excess abun ...
... models, in order to gain insight into the protogalaxy’s age and star formation history. We continue investigating the high-redshift universe, turning our attention to the issue of space-time variations in the fine-structure constant, as suggested by quasar absorption-line constraints. An excess abun ...
The spectroscopic Hertzsprung
... Section 2). This makes it difficult to determine masses from the g−T eff diagram in Fig. 1 for masses larger than 30 M⊙ , but allows Fig. 2 to be used as a diagnostic tool for stellar masses. Furthermore, it is interesting to compare the tracks of the stars in the three diagrams in Figs.1 and 2 that ...
... Section 2). This makes it difficult to determine masses from the g−T eff diagram in Fig. 1 for masses larger than 30 M⊙ , but allows Fig. 2 to be used as a diagnostic tool for stellar masses. Furthermore, it is interesting to compare the tracks of the stars in the three diagrams in Figs.1 and 2 that ...
SST-GATE: An Innovative Telescope for the Very High
... the night sky background, the exposure must match the duration of the Cherenkov light pulse, of the order of a few nsec. Therefore, unlike in conventional optical astronomy, the image on the camera, corresponding to the indirect signal from a single gamma-ray, cannot be improved through increased ex ...
... the night sky background, the exposure must match the duration of the Cherenkov light pulse, of the order of a few nsec. Therefore, unlike in conventional optical astronomy, the image on the camera, corresponding to the indirect signal from a single gamma-ray, cannot be improved through increased ex ...
The spectroscopic Hertzsprung-Russell diagram
... Methods. Our spectroscopic Hertzsprung-Russell (sHR) diagram shows the inverse of the flux-mean gravity versus the effective temperature. Observed stars whose spectra have been quantitatively analyzed can be entered in this diagram without the knowledge of the stellar distance or absolute brightness ...
... Methods. Our spectroscopic Hertzsprung-Russell (sHR) diagram shows the inverse of the flux-mean gravity versus the effective temperature. Observed stars whose spectra have been quantitatively analyzed can be entered in this diagram without the knowledge of the stellar distance or absolute brightness ...
Chap2-RadialVelocity
... 2.2 Measurement principles and accuracies (1) Doppler shift An instantaneous measurement of the stellar radial velocity about the star-planet barycenter is given by the small, systematic Doppler shift in wavelength of the many (thousands) absorption lines that make the star’s spectrum. In the obser ...
... 2.2 Measurement principles and accuracies (1) Doppler shift An instantaneous measurement of the stellar radial velocity about the star-planet barycenter is given by the small, systematic Doppler shift in wavelength of the many (thousands) absorption lines that make the star’s spectrum. In the obser ...
06 SIG Page 81-96 Scopes
... are considered rich-field telescopes (RFT) because they provide lower magnifications and wider fields of view (that is, you can see more of the sky through an eyepiece). Most telescopes have f/numbers that range from f/4 to f/15. The f/number is also referred to as the focal ratio and it is the same ...
... are considered rich-field telescopes (RFT) because they provide lower magnifications and wider fields of view (that is, you can see more of the sky through an eyepiece). Most telescopes have f/numbers that range from f/4 to f/15. The f/number is also referred to as the focal ratio and it is the same ...
Teaching Tips Table of Contents - Hubble Deep Field
... The Mathematical World: C. Shapes By the end of 8th grade, students should know that ...
... The Mathematical World: C. Shapes By the end of 8th grade, students should know that ...
Super-Earth and Sub-Neptune Exoplanets: a First Look from the
... Kepler satellite indicate that main-sequence stars on average host, at a minimum, about one planet per star (Fressin et al. 2013; Dressing & Charbonneau 2013). For the first time in human history, we have incontrovertible evidence that planets are common around other stars in the Milky Way. With thi ...
... Kepler satellite indicate that main-sequence stars on average host, at a minimum, about one planet per star (Fressin et al. 2013; Dressing & Charbonneau 2013). For the first time in human history, we have incontrovertible evidence that planets are common around other stars in the Milky Way. With thi ...
SPICA Yellow Book
... A complete understanding of the formation and evolution of galaxies, stars and planets can only be reached through the investigation of the cold and obscured parts of the Universe, where the basic processes of formation and evolution occur. Deep exploration of the cold Universe using high spatial re ...
... A complete understanding of the formation and evolution of galaxies, stars and planets can only be reached through the investigation of the cold and obscured parts of the Universe, where the basic processes of formation and evolution occur. Deep exploration of the cold Universe using high spatial re ...
Science with the Constellation
... the microwave background. The Next Generation Space Telescope (NGST) will zoom in on the first galaxies as they appear at high redshift. At intermediate redshift, Constellation-X and NGST will study the evolution of AGN and starburst galaxies. In addition, Constellation-X will also address fundament ...
... the microwave background. The Next Generation Space Telescope (NGST) will zoom in on the first galaxies as they appear at high redshift. At intermediate redshift, Constellation-X and NGST will study the evolution of AGN and starburst galaxies. In addition, Constellation-X will also address fundament ...
G030515-00 - DCC
... First observed during the solar eclipse of 1919 by Sir Arthur Eddington, when the Sun was silhouetted against the Hyades star cluster This effect now used to map out the distribution of dark matter ...
... First observed during the solar eclipse of 1919 by Sir Arthur Eddington, when the Sun was silhouetted against the Hyades star cluster This effect now used to map out the distribution of dark matter ...
Digital Universe Guide - American Museum of Natural History
... support from NASA, incorporates data from dozens of organizations worldwide to create the most complete and accurate 3-D atlas of the Universe from the local solar neighborhood out to the edge of the observable Universe. In preparation for the reopening of the Hayden Planetarium in 2000, the America ...
... support from NASA, incorporates data from dozens of organizations worldwide to create the most complete and accurate 3-D atlas of the Universe from the local solar neighborhood out to the edge of the observable Universe. In preparation for the reopening of the Hayden Planetarium in 2000, the America ...
Evolution of low mass stars
... The HRD inspired an English astronomer, Sir Arthur Stanley Eddington (18821944), when Russell visited London and presented his diagram at a meeting of the Royal Astronomical Society in 1913 (Eisberg, 2002). At the time, Eddington was the chief assistant of the Royal Greenwich Observatory. In 1926 Ed ...
... The HRD inspired an English astronomer, Sir Arthur Stanley Eddington (18821944), when Russell visited London and presented his diagram at a meeting of the Royal Astronomical Society in 1913 (Eisberg, 2002). At the time, Eddington was the chief assistant of the Royal Greenwich Observatory. In 1926 Ed ...
New Horizons Mission Design - SwRI Boulder
... NASA AO (NASA, 2001). Pluto was discovered by Clyde Tombaugh in 1930 and is currently located more than 31 Astronomical Units (AU) from the Sun. Spacecraft have been sent to the other eight planets but not yet to Pluto, although planning for a mission to Pluto dates as far back as the 1960s (Long, 1 ...
... NASA AO (NASA, 2001). Pluto was discovered by Clyde Tombaugh in 1930 and is currently located more than 31 Astronomical Units (AU) from the Sun. Spacecraft have been sent to the other eight planets but not yet to Pluto, although planning for a mission to Pluto dates as far back as the 1960s (Long, 1 ...
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.