LACEwING: A New Moving Group Analysis Code
... kinematic and spatial information. LACEwING works in right-handed Cartesian Galactic coordinates, with UVW space velocities and XYZ space positions, where the U/X axis is toward the Galactic center. The matrices of Johnson & Soderblom (1987) transform observational equatorial coordinates into UVW an ...
... kinematic and spatial information. LACEwING works in right-handed Cartesian Galactic coordinates, with UVW space velocities and XYZ space positions, where the U/X axis is toward the Galactic center. The matrices of Johnson & Soderblom (1987) transform observational equatorial coordinates into UVW an ...
The ALMA Universe - ALMA Observatory
... a radiometer that will continually measure the radiation being emitted by water vapor found in the antenna’s line of sight. This will enable additional corrections to be applied to the observed signal. The combined effect of these techniques will be to greatly reduce measurement errors caused by wat ...
... a radiometer that will continually measure the radiation being emitted by water vapor found in the antenna’s line of sight. This will enable additional corrections to be applied to the observed signal. The combined effect of these techniques will be to greatly reduce measurement errors caused by wat ...
Type II SuperNova - University of Dayton
... 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-neutrinos, to be more precise) produced by the collapse ...
... 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-neutrinos, to be more precise) produced by the collapse ...
Decoding Galaxy Evolution with Gas
... guidance that made this dissertation possible. His excellent grasp of the larger picture continually forced me to understand our results in a broader context. His questions cut straight to the heart of the matter and would evoke sheer terror if asked by anyone who does not possess David’s constantly ...
... guidance that made this dissertation possible. His excellent grasp of the larger picture continually forced me to understand our results in a broader context. His questions cut straight to the heart of the matter and would evoke sheer terror if asked by anyone who does not possess David’s constantly ...
Article PDF - IOPscience
... periodically variable light curves (periods ranging from 0.2 to 0.9 days; Smith 2004). They are bright stars (MV = 0.6 0.1 mag) with distinct light curves, which makes them easy to identify with time-domain imaging surveys, even to large distances (5–120 kpc for surveys with a 14 < V < 21 magnitud ...
... periodically variable light curves (periods ranging from 0.2 to 0.9 days; Smith 2004). They are bright stars (MV = 0.6 0.1 mag) with distinct light curves, which makes them easy to identify with time-domain imaging surveys, even to large distances (5–120 kpc for surveys with a 14 < V < 21 magnitud ...
The Formation of Population III Stars in Gas Accretion Stage: Effects
... Using a three dimensional simulation, Saigo et al. (2004) investigated the evolution of a collapsing primordial cloud with a simple initial setting and showed fragmentation before protostar formation (see also Machida et al. 2008, 2009a,b). Recently, starting from the cosmological setting, Turk et a ...
... Using a three dimensional simulation, Saigo et al. (2004) investigated the evolution of a collapsing primordial cloud with a simple initial setting and showed fragmentation before protostar formation (see also Machida et al. 2008, 2009a,b). Recently, starting from the cosmological setting, Turk et a ...
Turbulence-driven Polar Winds from T Tauri Stars Energized by
... What sets the Sun’s mass loss? • Coronal heating must be ultimately responsible for the solar wind. • A fraction of the “coronal heating” is channeled downward by conduction. • Hammer (1982) & Withbroe (1988) suggested a balance between conduction (downward), enthalpy (upward), and radiation losses ...
... What sets the Sun’s mass loss? • Coronal heating must be ultimately responsible for the solar wind. • A fraction of the “coronal heating” is channeled downward by conduction. • Hammer (1982) & Withbroe (1988) suggested a balance between conduction (downward), enthalpy (upward), and radiation losses ...
A Variability Study of the Typical Red Supergiant Antares A
... Unfortunately, due to the long timescales of these variations they are not well studied, with the exception of the bright M-class supergiant Betelgeuse (α Orionis, M2 Iab). Betelgeuse has been well studied both observationally and theoretically, and has many features that are well described by model ...
... Unfortunately, due to the long timescales of these variations they are not well studied, with the exception of the bright M-class supergiant Betelgeuse (α Orionis, M2 Iab). Betelgeuse has been well studied both observationally and theoretically, and has many features that are well described by model ...
Astronomy Astrophysics Gaia-ESO Survey: The analysis of high-resolution The
... available. Exactly the same analysis strategy that we applied to iDR2 is being applied to iDR3. For completeness, we also present the analysis of iDR1 in an Appendix. There, we discuss the main differences between the analysis implementation for these two iDRs. The first Gaia-ESO science verification ...
... available. Exactly the same analysis strategy that we applied to iDR2 is being applied to iDR3. For completeness, we also present the analysis of iDR1 in an Appendix. There, we discuss the main differences between the analysis implementation for these two iDRs. The first Gaia-ESO science verification ...
Observational Studies of Interacting Galaxies and the Development
... through five CFHTLS broad band photometry up to z ∼ 1. Meanwhile, by comparing the merger and elliptical galaxy mass density function, I discovered that the most massive mergers are not all formed via merging processes, unless the merging timescale is much longer than the expected value. Spectroscop ...
... through five CFHTLS broad band photometry up to z ∼ 1. Meanwhile, by comparing the merger and elliptical galaxy mass density function, I discovered that the most massive mergers are not all formed via merging processes, unless the merging timescale is much longer than the expected value. Spectroscop ...
Carbon, nitrogen and oxygen abundances in
... stars are selected according to their effective temperatures Teff and surface gravities log g, namely: Teff is between 15 300 and 24 100 K and log g is mostly greater than 3.75; therefore, stars with medium masses of 5–11 M are selected. Theory predicts for the stars with such parameters that the C ...
... stars are selected according to their effective temperatures Teff and surface gravities log g, namely: Teff is between 15 300 and 24 100 K and log g is mostly greater than 3.75; therefore, stars with medium masses of 5–11 M are selected. Theory predicts for the stars with such parameters that the C ...
Evolution of low mass stars
... physics of stars was still poorly understood until the modern physics shed light on it. In the early 19th century when astronomers started to measure the distances of stars with parallaxes, they found it impossible to investigate the composition and characteristics of stars with the foreseeable tech ...
... physics of stars was still poorly understood until the modern physics shed light on it. In the early 19th century when astronomers started to measure the distances of stars with parallaxes, they found it impossible to investigate the composition and characteristics of stars with the foreseeable tech ...
WILLIAM HERSCHEL AND THE `GARNET` STARS: μ CEPHEI AND
... this famous red star is not well documented. Prior to and after Herschel, the identification of this star was the subject of confusion in various catalogues and atlases. The case is complex and involves other stars in southern Cepheus, including double stars, found by Herschel in the course of his s ...
... this famous red star is not well documented. Prior to and after Herschel, the identification of this star was the subject of confusion in various catalogues and atlases. The case is complex and involves other stars in southern Cepheus, including double stars, found by Herschel in the course of his s ...
Multiplicity in Early Stellar Evolution - Astronomy Group
... a 100-M⊙ cloud with their AMR MHD code, and found that the magnetic field could reduce the degree of fragmentation, compared to a nonmagnetic cloud collapse, by as much as a factor of 2. Commerçon et al. (2011) extended their previous work on 1-M⊙ clouds to include 100-M⊙ clouds, but again found tha ...
... a 100-M⊙ cloud with their AMR MHD code, and found that the magnetic field could reduce the degree of fragmentation, compared to a nonmagnetic cloud collapse, by as much as a factor of 2. Commerçon et al. (2011) extended their previous work on 1-M⊙ clouds to include 100-M⊙ clouds, but again found tha ...
Sowing the Seeds of Asymmetry Jet-like Outflows in pPNe and AGB
... Collimated (episodic) fast winds/ jets (CFWs), operating during the very late-AGB phase, interacting with round AGB circumstellar envelopes, are the primary agent which initiate the formation of aspherical shapes and structures (Sahai & Trauger 1998) • highly collimated lobes, multipolar morphologie ...
... Collimated (episodic) fast winds/ jets (CFWs), operating during the very late-AGB phase, interacting with round AGB circumstellar envelopes, are the primary agent which initiate the formation of aspherical shapes and structures (Sahai & Trauger 1998) • highly collimated lobes, multipolar morphologie ...
6.7 GHz Methanol Masers and the GBT
... • The methodology is to combine the initial mass function with the star formation law in the Galaxy (as a function of position) to create a distribution of massive stars as a function of galactic longitude. • Then, assuming that every massive star excites a methanol maser during its birth, one can d ...
... • The methodology is to combine the initial mass function with the star formation law in the Galaxy (as a function of position) to create a distribution of massive stars as a function of galactic longitude. • Then, assuming that every massive star excites a methanol maser during its birth, one can d ...
The universe of the coming ALMA revolution
... The colors of light that our eyes can detect are but a thin sliver of the entire spectrum. The universe emits light in every invisible color, from radio waves to gamma rays, and studies conducted within each band of the spectrum contribute uniquely to our understanding. Only now has technology cau ...
... The colors of light that our eyes can detect are but a thin sliver of the entire spectrum. The universe emits light in every invisible color, from radio waves to gamma rays, and studies conducted within each band of the spectrum contribute uniquely to our understanding. Only now has technology cau ...
A spectroscopic investigation of the O-type star - ORBi
... evidence of binarity is found can never be definitely considered as single. Even if no RV shift is detected, the system could be seen under a particular orientation, have a very long period or perhaps a high eccentricity, thereby making the RV variations not significant over a long timescale. We per ...
... evidence of binarity is found can never be definitely considered as single. Even if no RV shift is detected, the system could be seen under a particular orientation, have a very long period or perhaps a high eccentricity, thereby making the RV variations not significant over a long timescale. We per ...
The drop in the cosmic star formation rate below redshift 2 is caused
... 0.1 cm is the threshold density for star formation and β = 2. Note, however, that our results are insensitive to the choice for β as long as it is chosen to be large (see Booth & Schaye 2009). A fraction of 1.5 per cent of the rest-mass energy of the accreted gas is injected into the surrounding med ...
... 0.1 cm is the threshold density for star formation and β = 2. Note, however, that our results are insensitive to the choice for β as long as it is chosen to be large (see Booth & Schaye 2009). A fraction of 1.5 per cent of the rest-mass energy of the accreted gas is injected into the surrounding med ...
abstracts book - Instituto de Astrofísica e Ciências do Espaço
... the conference which is expected to set a critical milestone for the astero- and helioseismology community to prepare the future. The meeting will also cover major synergies with related fields, which benefit from a deeper understanding of the structure and evolution of the sun and stars across the ...
... the conference which is expected to set a critical milestone for the astero- and helioseismology community to prepare the future. The meeting will also cover major synergies with related fields, which benefit from a deeper understanding of the structure and evolution of the sun and stars across the ...
HH 222: A Giant Herbig-Haro Flow from the
... HH 222 is a giant shocked region in the L1641 cloud, and is popularly known as the Orion Streamers or ”the waterfall” on account of its unusual structure. At the center of these streamers are two infrared sources coincident with a nonthermal radio jet aligned along the principal streamer. The unique ...
... HH 222 is a giant shocked region in the L1641 cloud, and is popularly known as the Orion Streamers or ”the waterfall” on account of its unusual structure. At the center of these streamers are two infrared sources coincident with a nonthermal radio jet aligned along the principal streamer. The unique ...
Galactic Winds Sylvain Veilleux
... and the boundary conditions near the event horizon, and can reach ǫ ≈ 0.4 (e.g., Krolik 1999; Agol & Krolik 2000). Much of the energy released during accretion may be tapped to drive a GW; this can occur through several processes. Radiative processes may be important in luminous AGN such as Seyfert ...
... and the boundary conditions near the event horizon, and can reach ǫ ≈ 0.4 (e.g., Krolik 1999; Agol & Krolik 2000). Much of the energy released during accretion may be tapped to drive a GW; this can occur through several processes. Radiative processes may be important in luminous AGN such as Seyfert ...
Untitled - NMSU Astronomy
... drawn through the data points. We can figure out the equation of this straight line and then predict the temperature at any altitude. In high school you learned that the equation of a line was y = mx + b, where “m” is the “slope” of the line, and “b” is the “y intercept”. The y intercept is simply w ...
... drawn through the data points. We can figure out the equation of this straight line and then predict the temperature at any altitude. In high school you learned that the equation of a line was y = mx + b, where “m” is the “slope” of the line, and “b” is the “y intercept”. The y intercept is simply w ...
Stars: Stellar Evol & “death” Galaxies Astronomy 1 — Elementary Astronomy
... IN WHICH OUR WORLD BECAME SMALLER ANOTHER TIME ...
... IN WHICH OUR WORLD BECAME SMALLER ANOTHER TIME ...
Modeling Spatially and Spectrally Resolved Observations to
... This thesis owes much to the support of my officemate, Zach Berta, for five years of advice on life, computers, and astronomy. I thank Diego Muñoz, Robert Harris, Ragnhild Lunnan, and Sarah Rugheimer for countless snack and coffee breaks; Wen-fai Fong and Nick Stone for leading camping trips and t ...
... This thesis owes much to the support of my officemate, Zach Berta, for five years of advice on life, computers, and astronomy. I thank Diego Muñoz, Robert Harris, Ragnhild Lunnan, and Sarah Rugheimer for countless snack and coffee breaks; Wen-fai Fong and Nick Stone for leading camping trips and t ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.