![DUSTiNGS III: Distribution of Intermediate](http://s1.studyres.com/store/data/017242268_1-8161f02d52b9fe188608acb9571f2303-300x300.png)
DUSTiNGS III: Distribution of Intermediate
... asymptotic giant branch (TP-AGB) stars) and compare their distributions with that of an older stellar population (traced by RGB stars). We separate the majority of the TP-AGB population from the RGB populations by uniquely identifying the tip of the red giant branch (TRGB) at 3.6 µm. We also identif ...
... asymptotic giant branch (TP-AGB) stars) and compare their distributions with that of an older stellar population (traced by RGB stars). We separate the majority of the TP-AGB population from the RGB populations by uniquely identifying the tip of the red giant branch (TRGB) at 3.6 µm. We also identif ...
Gravitational Lensing: An Unique Probe of Dark Matter and Dark...
... infinite magnification called critical lines. Transferred to the source plane these line become caustics. The location of these lines depends on the relative distances of the source and lens and, of course, the distribution of matter in the lens. The position of the background source with respect to ...
... infinite magnification called critical lines. Transferred to the source plane these line become caustics. The location of these lines depends on the relative distances of the source and lens and, of course, the distribution of matter in the lens. The position of the background source with respect to ...
Extended Infrared Emission from LIRGs
... … resemble those of local LIRGs rather than ULIRGs. Kinematical evidence from ionized (Hα) and molecular (CO) gas are consistent the presence of extended (~5kpc) star forming disks There is a “broad” connection between mid-IR emission and star formation rates (with some caveats…) We wish to quantify ...
... … resemble those of local LIRGs rather than ULIRGs. Kinematical evidence from ionized (Hα) and molecular (CO) gas are consistent the presence of extended (~5kpc) star forming disks There is a “broad” connection between mid-IR emission and star formation rates (with some caveats…) We wish to quantify ...
THE HOBBY-EBERLY TELESCOPE CHEMICAL ABUNDANCES OF
... chain reactions. These nucleosynthesis reactions make it indeed possible for a star to self-enrich its atmosphere with Li, but only for a very short period of time before the freshly produced Li burns again. The enrichment can be quite extreme, however, with Li abundances sometimes 1Y2 dex higher th ...
... chain reactions. These nucleosynthesis reactions make it indeed possible for a star to self-enrich its atmosphere with Li, but only for a very short period of time before the freshly produced Li burns again. The enrichment can be quite extreme, however, with Li abundances sometimes 1Y2 dex higher th ...
Classification of Variable Stars
... Nomenclature of Variable Stars The name of a variable star generally consists of one or two capital letters or a Greek letter, followed by a three letter constellation abbreviation. There are also variables with names such as V746 Oph and V1668 Cyg. These are stars in constellations for which all of ...
... Nomenclature of Variable Stars The name of a variable star generally consists of one or two capital letters or a Greek letter, followed by a three letter constellation abbreviation. There are also variables with names such as V746 Oph and V1668 Cyg. These are stars in constellations for which all of ...
Astronomy Astrophysics
... The photometric data of the six program stars were analysed using the Scargle-Press period search routine (Scargle 1982; Horne & Baliunas 1986) to look for the period of the photometric rotational modulation. The results are summarized in the Tables 2–7, where we list: time interval (HJD range) to w ...
... The photometric data of the six program stars were analysed using the Scargle-Press period search routine (Scargle 1982; Horne & Baliunas 1986) to look for the period of the photometric rotational modulation. The results are summarized in the Tables 2–7, where we list: time interval (HJD range) to w ...
observations and theory of star cluster formation
... Most young, embedded clusters resemble Orion and W3 in this respect. They have some level of current star formation activity, with an age possibly less than 105 years, and are also part of an older OB association or other extended star formation up to galactic scales, with other clusters forming in ...
... Most young, embedded clusters resemble Orion and W3 in this respect. They have some level of current star formation activity, with an age possibly less than 105 years, and are also part of an older OB association or other extended star formation up to galactic scales, with other clusters forming in ...
A Wide-Field Study of the z~ 0.8 Cluster RX J0152. 7
... We focus in this paper on a mass-limited sample for this important epoch of cluster mass growth. Luminosity-limited samples selected in the rest-frame UV include many bright, low mass, star forming galaxies as a result of the large scatter in their mass-to-light ratios at a fixed galaxy stellar mass ...
... We focus in this paper on a mass-limited sample for this important epoch of cluster mass growth. Luminosity-limited samples selected in the rest-frame UV include many bright, low mass, star forming galaxies as a result of the large scatter in their mass-to-light ratios at a fixed galaxy stellar mass ...
Pre-main sequence evolution
... - T Tauris are associated with young groups/clusters/clouds - classical T Tauri stars have circumstellar discs, which are believed to be the places of planet formation - weak-line T Tauri stars (discovered later) host residual discs, which are the best places to search for extrasolar planets ...
... - T Tauris are associated with young groups/clusters/clouds - classical T Tauri stars have circumstellar discs, which are believed to be the places of planet formation - weak-line T Tauri stars (discovered later) host residual discs, which are the best places to search for extrasolar planets ...
exploring anticorrelations and light element variations
... just because it has access to many northern GCs. Its highresolution near-IR spectra allow the simultaneous determination of many elemental abundances generally not available in optical spectroscopic work of GC stars. C and N, which are elements heavily affected by the pollution phenomenon in GCs, ar ...
... just because it has access to many northern GCs. Its highresolution near-IR spectra allow the simultaneous determination of many elemental abundances generally not available in optical spectroscopic work of GC stars. C and N, which are elements heavily affected by the pollution phenomenon in GCs, ar ...
Spring 2015 Mercury - Astronomical Society of the Pacific
... he most famous 11th-century comet was Halley’s Comet of 1066, which was linked to the Norman Conquest of England. But another comet of that century is linked to battles in both Scotland and Holland, and we are just three years away from its 1,000th anniversary. While the Battle of Hastings sealed th ...
... he most famous 11th-century comet was Halley’s Comet of 1066, which was linked to the Norman Conquest of England. But another comet of that century is linked to battles in both Scotland and Holland, and we are just three years away from its 1,000th anniversary. While the Battle of Hastings sealed th ...
OLIMPO
... • We have selected 40 nearby rich clusters to be measured in a single long duration flight. • For all these clusters high quality data are available from XMM/Chandra ...
... • We have selected 40 nearby rich clusters to be measured in a single long duration flight. • For all these clusters high quality data are available from XMM/Chandra ...
Type II SuperNova - University of Dayton
... astronomers) was observed in a nearby galaxy called the Large Magellanic Cloud. This was the first "nearby" supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neut ...
... astronomers) was observed in a nearby galaxy called the Large Magellanic Cloud. This was the first "nearby" supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neut ...
Astronomy Laboratory Manual
... Every new stargazer thinks the first thing they need to get started in astronomy is a telescope, only to discover that they don't know how to find anything with it in the sky. The problem, of course, is that they don't know the bright stars and major constellations. Unfortunately, many never find th ...
... Every new stargazer thinks the first thing they need to get started in astronomy is a telescope, only to discover that they don't know how to find anything with it in the sky. The problem, of course, is that they don't know the bright stars and major constellations. Unfortunately, many never find th ...
THE GREAT AGN DEBATE `AGN VS STARBURST
... 5. Radio-quiet quasars/ and QSO (Quasi Stellar Object) are more luminous versions of Seyfert Type 1 galaxy. They show strong optical continuum emission, Xray continuum emission, and broad and narrow optical emission lines. Some astronomers use the term QSO for this object reserving 'quasar' for radi ...
... 5. Radio-quiet quasars/ and QSO (Quasi Stellar Object) are more luminous versions of Seyfert Type 1 galaxy. They show strong optical continuum emission, Xray continuum emission, and broad and narrow optical emission lines. Some astronomers use the term QSO for this object reserving 'quasar' for radi ...
the red supergiant content of m31
... these spectra to measure effective temperatures and assign spectral types, deriving physical properties for 192 RSGs. Comparison with the solar metallicity Geneva evolutionary tracks indicates astonishingly good agreement. The most luminous RSGs in M31 are likely evolved from 25–30 Me stars, while t ...
... these spectra to measure effective temperatures and assign spectral types, deriving physical properties for 192 RSGs. Comparison with the solar metallicity Geneva evolutionary tracks indicates astonishingly good agreement. The most luminous RSGs in M31 are likely evolved from 25–30 Me stars, while t ...
Tracing the evolution of NGC 6397 through the chemical
... products. The remaining gas is dispersed by core-collapse supernovae of the second generation and star formation ceases. The present-day cluster is dominated by the second generation, with a smaller fraction, approximately 30%, being left of the primordial population. Critical factors determining th ...
... products. The remaining gas is dispersed by core-collapse supernovae of the second generation and star formation ceases. The present-day cluster is dominated by the second generation, with a smaller fraction, approximately 30%, being left of the primordial population. Critical factors determining th ...
galaxy formation with cold gas accretion and evolving stellar initial
... naive speculation although its exact form is far from clear. There is theoretical and observational evidence for the stellar IMF at high z to be top-heavy or bottom-light (e.g., Larson 2005; van Dokkum 2008). Constraints on the stellar IMF can also be obtained from comparisons between the evolution ...
... naive speculation although its exact form is far from clear. There is theoretical and observational evidence for the stellar IMF at high z to be top-heavy or bottom-light (e.g., Larson 2005; van Dokkum 2008). Constraints on the stellar IMF can also be obtained from comparisons between the evolution ...
a new vla–hipparcos distance to betelgeuse and its implications
... The distance to the M supergiant Betelgeuse is poorly known, with the Hipparcos parallax having a significant uncertainty. For detailed numerical studies of M supergiant atmospheres and winds, accurate distances are a prerequisite to obtaining reliable estimates for many stellar parameters. New high ...
... The distance to the M supergiant Betelgeuse is poorly known, with the Hipparcos parallax having a significant uncertainty. For detailed numerical studies of M supergiant atmospheres and winds, accurate distances are a prerequisite to obtaining reliable estimates for many stellar parameters. New high ...
Where is the angular momentum in elliptical galaxies?
... elliptical galaxy populations spatially and in color. • GC formation observed in all starbursts in local universe – trace major formation episodes. • Each individual GC is a simple stellar population, most basic determination of ages and abundances. GC systems reveal distribution in age and metallic ...
... elliptical galaxy populations spatially and in color. • GC formation observed in all starbursts in local universe – trace major formation episodes. • Each individual GC is a simple stellar population, most basic determination of ages and abundances. GC systems reveal distribution in age and metallic ...
The SCUBA-2 Cosmology Legacy Survey: blank
... observation, scaling the data to units of pW. The signal recorded by each bolometer is then assumed to be a linear combination of: (a) a common mode signal dominated by atmospheric water and ambient thermal emission; (b) the astronomical signal (attenuated by atmospheric extinction) and finally (c) ...
... observation, scaling the data to units of pW. The signal recorded by each bolometer is then assumed to be a linear combination of: (a) a common mode signal dominated by atmospheric water and ambient thermal emission; (b) the astronomical signal (attenuated by atmospheric extinction) and finally (c) ...
Farthest Neighbor: The Distant Milky Way Satellite Eridanus II
... We observed EriII with the IMACS spectrograph (Dressler et al. 2006) on the Magellan Baade telescope on the nights of 2015October16–17 and 2015November18–19. The observing conditions on both runs were clear, with seeing that varied from 0 6 to 0 9. The observing procedure and instrument setup a ...
... We observed EriII with the IMACS spectrograph (Dressler et al. 2006) on the Magellan Baade telescope on the nights of 2015October16–17 and 2015November18–19. The observing conditions on both runs were clear, with seeing that varied from 0 6 to 0 9. The observing procedure and instrument setup a ...
The Formation and Survival of Discs in a Lambda
... 1994). As a result, discs contain too small a fraction of the stellar mass in comparison to observed spirals. In a limited number of cases, simulations have been able to produce individual examples of realistic disc galaxies in Λ cold dark matter (ΛCDM) universes (e.g. Abadi et al. 2003; Governato e ...
... 1994). As a result, discs contain too small a fraction of the stellar mass in comparison to observed spirals. In a limited number of cases, simulations have been able to produce individual examples of realistic disc galaxies in Λ cold dark matter (ΛCDM) universes (e.g. Abadi et al. 2003; Governato e ...
The Be/X-ray transient 4U 0115+ 63/V635 Cassiopeiae
... counterpart to the transient X-ray pulsar 4U 0115+63, taken at a time when the circumstellar envelope had disappeared. V635 Cas is classified as a B0.2Ve star at a distance of 7−8 kpc. We use the physical parameters derived from these observations and the orbit derived from X-ray observations to ela ...
... counterpart to the transient X-ray pulsar 4U 0115+63, taken at a time when the circumstellar envelope had disappeared. V635 Cas is classified as a B0.2Ve star at a distance of 7−8 kpc. We use the physical parameters derived from these observations and the orbit derived from X-ray observations to ela ...
Five New Extrasolar Planets
... the duration of observations. The minimization requires that each velocity measurement be assigned a weight which we assemble from two contributions, the internal error and the stellar jitter (Cumming, Marcy, & Butler 1999). The internal error is derived from the weighted uncertainty in the mean vel ...
... the duration of observations. The minimization requires that each velocity measurement be assigned a weight which we assemble from two contributions, the internal error and the stellar jitter (Cumming, Marcy, & Butler 1999). The internal error is derived from the weighted uncertainty in the mean vel ...
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.