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Two New Triple Star Systems with Detectable Inner Orbital Motions
... We considered whether the combined and overlaid movement sequences (the three proven components) are visible and predictable. For the inner pair CHR4 Aa,Ab measurements exist from 1984 to 1994. These cover an arc of about 60 degrees and show a well-defined orbital arc. After 1994, the inner system u ...
... We considered whether the combined and overlaid movement sequences (the three proven components) are visible and predictable. For the inner pair CHR4 Aa,Ab measurements exist from 1984 to 1994. These cover an arc of about 60 degrees and show a well-defined orbital arc. After 1994, the inner system u ...
Effects of interaction on the properties of spiral galaxies. II. Isolated
... 1990; Combes & Elmegreen 1993). But the selection criteria we have adopted to define the sample of isolated spirals was designed to select objects that wouldn’t have experienced gravitational interaction in the last 109 years at least. The presence of those components in all of them should imply lon ...
... 1990; Combes & Elmegreen 1993). But the selection criteria we have adopted to define the sample of isolated spirals was designed to select objects that wouldn’t have experienced gravitational interaction in the last 109 years at least. The presence of those components in all of them should imply lon ...
Annual Report 2014 - Max Planck Institute for Astrophysics
... particles, and the calculation of transition probThe Max-Planck-Institut für Astrophysik, usually abilities and cross–sections for astrophysical procalled MPA for short, was founded in 1958 under cesses in rarefied media. From its inception the the directorship of Ludwig Biermann. It was estab- MPA h ...
... particles, and the calculation of transition probThe Max-Planck-Institut für Astrophysik, usually abilities and cross–sections for astrophysical procalled MPA for short, was founded in 1958 under cesses in rarefied media. From its inception the the directorship of Ludwig Biermann. It was estab- MPA h ...
The Balloon-borne Large Aperture Submillimeter Telescope
... The BLAST gondola incorporates a 2 m carbon-fiber primary mirror. The spherical mirror has a mass of 32 kg and a surface rms of 2.4 microns. The mirror was designed and built by Composite Optics Incorporated∗ . A 50 cm diameter correcting secondary mirror gives diffraction limited performance over a 1 ...
... The BLAST gondola incorporates a 2 m carbon-fiber primary mirror. The spherical mirror has a mass of 32 kg and a surface rms of 2.4 microns. The mirror was designed and built by Composite Optics Incorporated∗ . A 50 cm diameter correcting secondary mirror gives diffraction limited performance over a 1 ...
PDF file of document - University of Iowa Astrophysics
... commonly used in all sciences to express mass (kilograms, kg), size (meters, m), and time (seconds, s). It Stars, Galaxies and the Universe ...
... commonly used in all sciences to express mass (kilograms, kg), size (meters, m), and time (seconds, s). It Stars, Galaxies and the Universe ...
... Therefore, any probe of star formation which is insensitive to the obscuring effects of dust will have a tremendous advantage. Such a transparent view of the high z Universe is provided by sub-mm and mm observations, which now have the instrumental sensitivity (e.g., SCUBA, MAMBO) to detect the form ...
MUSE three-dimensional spectroscopy and kinematics of the
... indicate (e.g. O’Dea, Baum & Stanghellini 1991) that they have become confined (trapped) within the host galaxy nucleus by a very dense (clumpy and dusty) interstellar medium, or simply that they are observed very soon after the radio outburst is triggered (e.g. Morganti et al. 1997). It is now cons ...
... indicate (e.g. O’Dea, Baum & Stanghellini 1991) that they have become confined (trapped) within the host galaxy nucleus by a very dense (clumpy and dusty) interstellar medium, or simply that they are observed very soon after the radio outburst is triggered (e.g. Morganti et al. 1997). It is now cons ...
3 science case - Giant Magellan Telescope Organization
... Astronomy is a science driven by discovery. Bereft of physical contact with the celestial objects we study, astronomers can rarely carry out the controlled experiments that are the hallmark of the scientific method. Progress in our understanding of the cosmos often proceeds from the discovery of new ...
... Astronomy is a science driven by discovery. Bereft of physical contact with the celestial objects we study, astronomers can rarely carry out the controlled experiments that are the hallmark of the scientific method. Progress in our understanding of the cosmos often proceeds from the discovery of new ...
Visible neutral helium lines in main sequence B-type stars
... ≤ log g ≤ 4.5, but are well reproduced for Teff < 20000 K. 5. Effects of the microturbulence There is a considerable spread in the observed EW’s especially for Teff > 20000 K and, in certain cases, this is larger than accountable by the range of log g assumed in our calculations. We suggest that thi ...
... ≤ log g ≤ 4.5, but are well reproduced for Teff < 20000 K. 5. Effects of the microturbulence There is a considerable spread in the observed EW’s especially for Teff > 20000 K and, in certain cases, this is larger than accountable by the range of log g assumed in our calculations. We suggest that thi ...
... the hottest [WC] stars (Keller et al. 2014), showing a wide range in the C/He ratio, high Ne abundances, and N abundances much higher than those found in previous determinations. Six new emission line stars were discovered by Górny (2014), including two [WC] stars and one VL (or [WC11]) star, makin ...
Rearrangement of gas in disc galaxies
... maintenance of these two phenomena. We focus on the study of the physical conditions of the interstellar gas in the central kiloparsec region of the barred active galaxy NGC 1097 (Paper I). In Paper I we present different CO transitions and the consequent analysis realized in order to derive the mol ...
... maintenance of these two phenomena. We focus on the study of the physical conditions of the interstellar gas in the central kiloparsec region of the barred active galaxy NGC 1097 (Paper I). In Paper I we present different CO transitions and the consequent analysis realized in order to derive the mol ...
Max Planck Institute for Gravitational Physics
... star/body of distant stars/bodies is important: often more important than influence of close stars/bodies Let us consider a IDEALIZED galaxy of N identical stars with mass m, size R and uniform density Let us focus on a single star that crosses the system How long does it take for this star to chang ...
... star/body of distant stars/bodies is important: often more important than influence of close stars/bodies Let us consider a IDEALIZED galaxy of N identical stars with mass m, size R and uniform density Let us focus on a single star that crosses the system How long does it take for this star to chang ...
Stars, Galaxies, and Beyond
... Ivezić for allowing me this opportunity to explore these many important topics in astrophysics. Sources: The materials in this summary derive from the lecture notes, the assigned textbook, and many Web and published scientific articles and other sources as noted. I do not consider Wikipedia to be a ...
... Ivezić for allowing me this opportunity to explore these many important topics in astrophysics. Sources: The materials in this summary derive from the lecture notes, the assigned textbook, and many Web and published scientific articles and other sources as noted. I do not consider Wikipedia to be a ...
Galaxies
... evolution. We do not know for certain that all galaxies form at peaks in the dark matter density distribution. There is considerable debate about cold versus hot accretion of gas onto dark matter halos, and even more debate about which feedback mechanisms regulate star formation (photoionization, su ...
... evolution. We do not know for certain that all galaxies form at peaks in the dark matter density distribution. There is considerable debate about cold versus hot accretion of gas onto dark matter halos, and even more debate about which feedback mechanisms regulate star formation (photoionization, su ...
Zhu Qualifier Solutions - University of Toronto Astronomy
... 3.1.3. Why are the lower and upper limits of the IMF poorly understood compared to that of the middle (several M stars)? What constraints are there? 3.1.4. What’s the difference between a field and stellar cluster IMF? 3.1.5. How do you determine an a present-day mass function (PDMF) from an IMF? 3 ...
... 3.1.3. Why are the lower and upper limits of the IMF poorly understood compared to that of the middle (several M stars)? What constraints are there? 3.1.4. What’s the difference between a field and stellar cluster IMF? 3.1.5. How do you determine an a present-day mass function (PDMF) from an IMF? 3 ...
Str\" omgren uvby photometry of the peculiar globular cluster NGC
... photometric metallicity estimation and systematic effects. The lack of correlation between spectroscopic and photometric [Fe/H] of individual stars is further evidence against a [Fe/H] spread on the 0.1 dex level. Finally, the CN-sensitive δ4 , among other colour indices, anti-correlates strongly wi ...
... photometric metallicity estimation and systematic effects. The lack of correlation between spectroscopic and photometric [Fe/H] of individual stars is further evidence against a [Fe/H] spread on the 0.1 dex level. Finally, the CN-sensitive δ4 , among other colour indices, anti-correlates strongly wi ...
Understanding Mass-Loss and the Late Evolution of Intermediate
... New Mexico, first light in 2010), with resolutions ranging from 0.1 to 100, can be used to probe the launch regions of CFWs in late AGB stars and PPNs, in particular the disk temperature, geometry and density structure. Direct imaging, with space-based telescopes such as HST and JWST will remain uns ...
... New Mexico, first light in 2010), with resolutions ranging from 0.1 to 100, can be used to probe the launch regions of CFWs in late AGB stars and PPNs, in particular the disk temperature, geometry and density structure. Direct imaging, with space-based telescopes such as HST and JWST will remain uns ...
PDF - ASSA
... telescope and is one of the most sensitive detectors of very high-energy gamma rays. These are absorbed in the atmosphere, where they create a short-lived shower of particles. The HESS telescopes detect the faint, short flashes of bluish light which these particles emit (named Cherenkov light, lastin ...
... telescope and is one of the most sensitive detectors of very high-energy gamma rays. These are absorbed in the atmosphere, where they create a short-lived shower of particles. The HESS telescopes detect the faint, short flashes of bluish light which these particles emit (named Cherenkov light, lastin ...
- Max-Planck-Institut für Astronomie
... We have used the 28 ; 28 Hubble Space Telescope image mosaic from the GEMS (Galaxy Evolution from Morphology and SEDs) survey in conjunction with the COMBO-17 photometric redshift survey to constrain the incidence of major mergers between spheroid-dominated galaxies with little cold gas (dry mergers ...
... We have used the 28 ; 28 Hubble Space Telescope image mosaic from the GEMS (Galaxy Evolution from Morphology and SEDs) survey in conjunction with the COMBO-17 photometric redshift survey to constrain the incidence of major mergers between spheroid-dominated galaxies with little cold gas (dry mergers ...
Discovery of a Dwarf Poststarburst Galaxy near a High Column
... deep pencil beam galaxy survey around sight lines where very nearby (cz 10; 000 km s1) Ly absorbers have been found in the Penton et al. survey. This sample is ideal for studying the galaxies surrounding low column density Ly-only absorbers and the weak metal-line absorbers because even very fa ...
... deep pencil beam galaxy survey around sight lines where very nearby (cz 10; 000 km s1) Ly absorbers have been found in the Penton et al. survey. This sample is ideal for studying the galaxies surrounding low column density Ly-only absorbers and the weak metal-line absorbers because even very fa ...
$^{13} $ CO/C $^{18} $ O Gradients Across the Disks of Nearby
... line-integrated intensities on the Tmb scale. For each target, we quote the average ratio over the whole galaxy (from EMPIRE) and the mean ratio within the inner 3000 radius from ALMA and EMPIRE combined (except for NGC 3351, see Section 2). In cases without clear detections, we report 3σ upper limi ...
... line-integrated intensities on the Tmb scale. For each target, we quote the average ratio over the whole galaxy (from EMPIRE) and the mean ratio within the inner 3000 radius from ALMA and EMPIRE combined (except for NGC 3351, see Section 2). In cases without clear detections, we report 3σ upper limi ...
Modeling the chemical evolution of the Galaxy halo
... crucial information on the formation and evolution of a stellar system can be obtained from the kinematics and chemical composition of its stars. In particular, low-mass stars (m < 1 M ) live for a time comparable to or much longer than the present age of the Universe, retaining in their atmosphere ...
... crucial information on the formation and evolution of a stellar system can be obtained from the kinematics and chemical composition of its stars. In particular, low-mass stars (m < 1 M ) live for a time comparable to or much longer than the present age of the Universe, retaining in their atmosphere ...
Unlocking the secrets of stellar haloes using combined star counts
... In recent years, most attempts to trace the surface brightness profiles of stellar haloes have been based on direct star counts, i.e. by counting the number of bright halo stars (red giant branch stars, asymptotic giant branch stars and upper main sequence stars) within a certain area. The bright st ...
... In recent years, most attempts to trace the surface brightness profiles of stellar haloes have been based on direct star counts, i.e. by counting the number of bright halo stars (red giant branch stars, asymptotic giant branch stars and upper main sequence stars) within a certain area. The bright st ...
Cosmological Constraints from Baryonic Acoustic Oscillations
... Baryon acoustic oscillations z=0 ...
... Baryon acoustic oscillations z=0 ...
What Gaia can reveal about the matter distribution in the Milky Way
... Gaia’s mirrors are bigger (about 1.46 × 0.51 m compared to Hipparcos circular mirror with diameter of 30 cm), which allow more light to enter the telescope. Secondly, the detectors of Gaia are more sensitive as the used technique is CCDs and not photomultiplier tubes as on Hipparcos. Apart from the ...
... Gaia’s mirrors are bigger (about 1.46 × 0.51 m compared to Hipparcos circular mirror with diameter of 30 cm), which allow more light to enter the telescope. Secondly, the detectors of Gaia are more sensitive as the used technique is CCDs and not photomultiplier tubes as on Hipparcos. Apart from the ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.