POSTERS SESSION I: Atmospheres of Massive Stars
... We demonstrate that it is possible to have clumping occur close to the star while still achieving an excellent fit to Hα by consistently treating the wind’s rotation in the spectral modeling. An excellent agreement to other important optical lines such as HeII 4686 Å and NIII 4634–4640 Å is also o ...
... We demonstrate that it is possible to have clumping occur close to the star while still achieving an excellent fit to Hα by consistently treating the wind’s rotation in the spectral modeling. An excellent agreement to other important optical lines such as HeII 4686 Å and NIII 4634–4640 Å is also o ...
Worlds Beyond: A Strategy for the Detection and Characterization of
... The calculations described on pages 85-92 of Chapter 9 (“Depth of search comparisons”) employed an incorrect mass-radius relation for iron-rock planets, due to the misapplication of the fitting formulas of Fortney et al. (2007) (specifically, loge was used instead of log10 ). Fig. 1 shows the origin ...
... The calculations described on pages 85-92 of Chapter 9 (“Depth of search comparisons”) employed an incorrect mass-radius relation for iron-rock planets, due to the misapplication of the fitting formulas of Fortney et al. (2007) (specifically, loge was used instead of log10 ). Fig. 1 shows the origin ...
A Zoo of Galaxies - Portsmouth Research Portal
... The variety of different galaxies observed in the sky naturally caused people to wonder what they were. The scientific arguments surrounding this question at the start of the 20th century, are best represented perhaps, by the public debate held in 1920 between Heber Curtis and Harlow Shapley. Many o ...
... The variety of different galaxies observed in the sky naturally caused people to wonder what they were. The scientific arguments surrounding this question at the start of the 20th century, are best represented perhaps, by the public debate held in 1920 between Heber Curtis and Harlow Shapley. Many o ...
A Zoo of Galaxies
... The variety of different galaxies observed in the sky naturally caused people to wonder what they were. The scientific arguments surrounding this question at the start of the 20th century, are best represented perhaps, by the public debate held in 1920 between Heber Curtis and Harlow Shapley. Many o ...
... The variety of different galaxies observed in the sky naturally caused people to wonder what they were. The scientific arguments surrounding this question at the start of the 20th century, are best represented perhaps, by the public debate held in 1920 between Heber Curtis and Harlow Shapley. Many o ...
Abstracts - Physics of Evolved Stars 2015
... solar masses per year. Evolutionary models suggest that this phase does not last much longer than 10^5 years, implying that these stars are not likely to have lost more than one solar mass before entering the high mass-loss phase. To evolve into a post-AGB star, with a white dwarf cooling at the cen ...
... solar masses per year. Evolutionary models suggest that this phase does not last much longer than 10^5 years, implying that these stars are not likely to have lost more than one solar mass before entering the high mass-loss phase. To evolve into a post-AGB star, with a white dwarf cooling at the cen ...
Properties of Wolf-Rayet Stars - Paul Crowther, University of Sheffield
... only lower velocity limits may be obtained. Observational evidence suggests lower wind velocities at later subtypes, by up to a factor of ten, with respect to early-types. Individual WO stars have been identified in a number of external galaxies. One observes a reduction in line width (and so wind v ...
... only lower velocity limits may be obtained. Observational evidence suggests lower wind velocities at later subtypes, by up to a factor of ten, with respect to early-types. Individual WO stars have been identified in a number of external galaxies. One observes a reduction in line width (and so wind v ...
the biggest game in the cosmos
... obsolescence. The two most important lie at opposite ends of the scales of size and time. Close to home, the Keck telescopes and others have observed more than 160 planets, most of them the size of Jupiter and orbiting stars other than our sun. But these enormous instruments can’t actually image ot ...
... obsolescence. The two most important lie at opposite ends of the scales of size and time. Close to home, the Keck telescopes and others have observed more than 160 planets, most of them the size of Jupiter and orbiting stars other than our sun. But these enormous instruments can’t actually image ot ...
Chemical abundances and winds of massive stars in M31: a B
... for OB 10–64. A non-LTE model atmosphere and abundance analysis for OB 10–64 is presented indicating that this star has similar photospheric CNO, Mg and Si abundances as solar neighbourhood massive stars. A wind analysis of this early B-type supergiant reveals a mass-loss rate of Ṁ = 1.6 × 10−6M⊙ y ...
... for OB 10–64. A non-LTE model atmosphere and abundance analysis for OB 10–64 is presented indicating that this star has similar photospheric CNO, Mg and Si abundances as solar neighbourhood massive stars. A wind analysis of this early B-type supergiant reveals a mass-loss rate of Ṁ = 1.6 × 10−6M⊙ y ...
Chapter 10 Formation and evolution of the Local Group
... Studies to determine the possible formation and evolution of the LG over a 13.7 Gyr timescale are of course subject to many uncertainties. It is usually assumed that the Galaxy and M 31 formed nearby to each other, and took part in the general expansion of the universe. Around 4 Gyr ago, their mutua ...
... Studies to determine the possible formation and evolution of the LG over a 13.7 Gyr timescale are of course subject to many uncertainties. It is usually assumed that the Galaxy and M 31 formed nearby to each other, and took part in the general expansion of the universe. Around 4 Gyr ago, their mutua ...
Towards the Intensity Interferometry Stellar Imaging System
... measurements of stellar surface features by SII can provide optimal contrast. In the last decade, several young, coeval stellar groups have been discovered in close proximity (∼50 pc) to the sun. Prominent examples of nearby coeval stellar groups include the TW Hydra and β Pic co-moving groups. The ...
... measurements of stellar surface features by SII can provide optimal contrast. In the last decade, several young, coeval stellar groups have been discovered in close proximity (∼50 pc) to the sun. Prominent examples of nearby coeval stellar groups include the TW Hydra and β Pic co-moving groups. The ...
PPT presentation
... able to obtain echelle spectra of them with 11.5 km/s resolution, using 1.0m and 2.3m telescopes. The nebulae were spatially unresolved from the ground but asymmetric velocity profiles indicate non-spherically symmetric nebulae. Vexp (OII) was found to exceed Vexp (OIII) on average. The radial veloc ...
... able to obtain echelle spectra of them with 11.5 km/s resolution, using 1.0m and 2.3m telescopes. The nebulae were spatially unresolved from the ground but asymmetric velocity profiles indicate non-spherically symmetric nebulae. Vexp (OII) was found to exceed Vexp (OIII) on average. The radial veloc ...
Science Case for the Chinese Participation of TMT
... the universe? Astonishingly, astronomers are now on the verge of answering these fundamental questions with the next generation extremely large class telescopes such as the Thirty Meter Telescope (TMT). The Chinese participation in the TMT will place China in the forefront of astronomy for many deca ...
... the universe? Astonishingly, astronomers are now on the verge of answering these fundamental questions with the next generation extremely large class telescopes such as the Thirty Meter Telescope (TMT). The Chinese participation in the TMT will place China in the forefront of astronomy for many deca ...
WHITE DWARFS AS A SOURCE OF CONSTRAINTS ON EXOTIC …
... theories in understanding stellar structure and evolution Stars serves as a source of constraints on non standard ideas Some of these constraints turn out to be more stringent than laboratory ones First idea: weakly interacting particles (axions, Kaluza-Klein gravitons, etc.) produced in hot and ...
... theories in understanding stellar structure and evolution Stars serves as a source of constraints on non standard ideas Some of these constraints turn out to be more stringent than laboratory ones First idea: weakly interacting particles (axions, Kaluza-Klein gravitons, etc.) produced in hot and ...
2 Justification and benefits in joining TMT
... the universe? Astonishingly, astronomers are now on the verge of answering these fundamental questions with the next generation extremely large class telescopes such as the Thirty Meter Telescope (TMT). The Chinese participation in the TMT will place China in the forefront of astronomy for many deca ...
... the universe? Astonishingly, astronomers are now on the verge of answering these fundamental questions with the next generation extremely large class telescopes such as the Thirty Meter Telescope (TMT). The Chinese participation in the TMT will place China in the forefront of astronomy for many deca ...
Chromospherically young, kinematically old stars
... The CYKOS can be identified by a diagram of spatial velocities (U × V or W × V ) showing only active stars, 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 veloci ...
... The CYKOS can be identified by a diagram of spatial velocities (U × V or W × V ) showing only active stars, 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 veloci ...
3. Cosmology and the Origin and Evolution of Galaxies
... some success in the measurement of optical and IR spectroscopic redshifts for a fraction of the bright mm galaxies (S850µm > 5 mJy) with reliable radio counterparts8. Radio interferometric data help refine the positions of the mm galaxies, which allows the optical and IR counterparts to be identified ...
... some success in the measurement of optical and IR spectroscopic redshifts for a fraction of the bright mm galaxies (S850µm > 5 mJy) with reliable radio counterparts8. Radio interferometric data help refine the positions of the mm galaxies, which allows the optical and IR counterparts to be identified ...
- CUNY Academic Works
... Figure 20. Infrared constellation ................................................................................................................. 55 Figure 21. Iconic images taken by the Hubble Space Telescope ................................................................ 64 ...
... Figure 20. Infrared constellation ................................................................................................................. 55 Figure 21. Iconic images taken by the Hubble Space Telescope ................................................................ 64 ...
Document
... The Polaris Telescope is temporarily polar mounted in one PARI’s observatory buildings, waiting for completion of the Polaris Observatory. The telescope was tested and used to begin the Polaris Monitoring Program from this site. ...
... The Polaris Telescope is temporarily polar mounted in one PARI’s observatory buildings, waiting for completion of the Polaris Observatory. The telescope was tested and used to begin the Polaris Monitoring Program from this site. ...
Spectral Line VLBI - Australia Telescope National Facility
... • VLBI Exploration of Radio Astrometry • Dedicated phase referencing VLBI network • Four 20-m antennas spread over Japan with dual-beam systems Up to 2 degree separation ...
... • VLBI Exploration of Radio Astrometry • Dedicated phase referencing VLBI network • Four 20-m antennas spread over Japan with dual-beam systems Up to 2 degree separation ...
Buying A Telescope - members.iinet.com.au
... It's true that you may, like most backyard astronomers, soon outgrow your first telescope. But here's a word of advice -long-time astronomers who end up owning many telescopes over the years often find that their first telescope, as basic as it was, was the one that provided them the most enjoyment. ...
... It's true that you may, like most backyard astronomers, soon outgrow your first telescope. But here's a word of advice -long-time astronomers who end up owning many telescopes over the years often find that their first telescope, as basic as it was, was the one that provided them the most enjoyment. ...
IRAS - the infrared - Imperial College London Astrophysics
... the IRAS all-sky survey of infrared point-sources: white: star-forming regions, blue: red giant stars, green: galaxies. IRAS detected 60,000 dusty, star-forming glaxies over the whole sky. Thessaloniki, Oct 3rd 2009 ...
... the IRAS all-sky survey of infrared point-sources: white: star-forming regions, blue: red giant stars, green: galaxies. IRAS detected 60,000 dusty, star-forming glaxies over the whole sky. Thessaloniki, Oct 3rd 2009 ...
JWST Project Report to the PMC
... New Frontiers of Astronomy 1.) Seek the first stars and galaxies that formed in the early Universe, and follow the ionization history 2.) Determine how galaxies evolve from the early Universe to the present day (stars, gas, metals, dark matter) 3.) Solve the mysteries of star formation and birth of ...
... New Frontiers of Astronomy 1.) Seek the first stars and galaxies that formed in the early Universe, and follow the ionization history 2.) Determine how galaxies evolve from the early Universe to the present day (stars, gas, metals, dark matter) 3.) Solve the mysteries of star formation and birth of ...
GALEX and Star Formation
... Extinction is a combination of scattering and absorption. Geometry, density, grain composition and UV radiation from hot stars are relevant parameters. Spectroscopic studies in the UV range show that in our Galaxy, an average extinction law can reproduce observed extinction curves (range 1250Å –3.5 ...
... Extinction is a combination of scattering and absorption. Geometry, density, grain composition and UV radiation from hot stars are relevant parameters. Spectroscopic studies in the UV range show that in our Galaxy, an average extinction law can reproduce observed extinction curves (range 1250Å –3.5 ...
from z=0 to z=1
... ratio (attenuation) for UV galaxies. For IR (24m) selected galaxies at z~0.6, no evidence is found for evolution of either the stellar mass or the IR/UV ratio for given LIR. 8. Both IR and UV evolve significantly from z=0 to z=1, and the ratio IR/UV increases by ~ 4. This is consistent with the ...
... ratio (attenuation) for UV galaxies. For IR (24m) selected galaxies at z~0.6, no evidence is found for evolution of either the stellar mass or the IR/UV ratio for given LIR. 8. Both IR and UV evolve significantly from z=0 to z=1, and the ratio IR/UV increases by ~ 4. This is consistent with the ...
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.