SUMSS - 京都大学
... • Radio LF for star-forming galaxies implies that galaxies with SFR > 30 Msun/yr are far more common than Ha surveys suggest, and may account for up to 40% of the local star-formation density. • Dust obscuration in star-forming regions could lead to under-estimate of Ha line strength. • Deep VLA stu ...
... • Radio LF for star-forming galaxies implies that galaxies with SFR > 30 Msun/yr are far more common than Ha surveys suggest, and may account for up to 40% of the local star-formation density. • Dust obscuration in star-forming regions could lead to under-estimate of Ha line strength. • Deep VLA stu ...
chapter 24 instructor notes
... In 1837 Argelander, of the Bonn Observatory and orginator of the BD catalogue, was able to derive an apex for the solar motion from studying stellar proper motions. His result is very similar to that recognized today. Also in 1837, Frederick Struve found evidence for interstellar extinction in star ...
... In 1837 Argelander, of the Bonn Observatory and orginator of the BD catalogue, was able to derive an apex for the solar motion from studying stellar proper motions. His result is very similar to that recognized today. Also in 1837, Frederick Struve found evidence for interstellar extinction in star ...
11.3 MB PDF file
... the Fabry·Perot. Before proceeding further, it is useful to consider how we would use the photometer if we did not have the FP. First, we must calibrate the photometer-telescope combination, using observations of standard stars through continuum filters for which the transmission curves have been ac ...
... the Fabry·Perot. Before proceeding further, it is useful to consider how we would use the photometer if we did not have the FP. First, we must calibrate the photometer-telescope combination, using observations of standard stars through continuum filters for which the transmission curves have been ac ...
The APEX-CHAMP+ view of the Orion Molecular Cloud 1 core
... neighboring Orion Nebula Cluster and forms the archetypical photon-dominated region (PDR) with the prominent bar feature. Its nearness makes the OMC-1 core region a touchstone for research on the dense molecular interstellar medium and PDRs. Methods. Using the Atacama Pathfinder Experiment telescope ...
... neighboring Orion Nebula Cluster and forms the archetypical photon-dominated region (PDR) with the prominent bar feature. Its nearness makes the OMC-1 core region a touchstone for research on the dense molecular interstellar medium and PDRs. Methods. Using the Atacama Pathfinder Experiment telescope ...
Autumn Asterisms for binoculars 2013
... angles to your first line and have sweep round with your binoculars and you should find the Cascade. Cassiopeia: The Aeroplane The Aeroplane actually looks like its intended name, and appears to be dive-bombing M52! It’s alternative name is the Arrow, but I think the former is better. Images reveal ...
... angles to your first line and have sweep round with your binoculars and you should find the Cascade. Cassiopeia: The Aeroplane The Aeroplane actually looks like its intended name, and appears to be dive-bombing M52! It’s alternative name is the Arrow, but I think the former is better. Images reveal ...
Stellar Structure and Evolution II
... Life Stages of High-Mass Stars • Late life stages of high-mass stars are similar to those of low-mass stars: – Hydrogen core fusion (main sequence) – Hydrogen shell burning (supergiant) – Helium core fusion (supergiant) ...
... Life Stages of High-Mass Stars • Late life stages of high-mass stars are similar to those of low-mass stars: – Hydrogen core fusion (main sequence) – Hydrogen shell burning (supergiant) – Helium core fusion (supergiant) ...
Moitinho et al. - Wiley Online Library
... overdensity would be the remaining core of the disrupted galaxy and the ring would be the tidal debris left behind. However, unlike the Sagittarius dwarf, which is well below the Galactic plane and whose orbit, and thus tidal tail, is nearly perpendicular to the plane of the Milky Way, the putative ...
... overdensity would be the remaining core of the disrupted galaxy and the ring would be the tidal debris left behind. However, unlike the Sagittarius dwarf, which is well below the Galactic plane and whose orbit, and thus tidal tail, is nearly perpendicular to the plane of the Milky Way, the putative ...
mufon ufo symposium -1974
... Star types 0, B, A and down to F2 are massive hot stars. Gravity forces the atoms closer together so atomic reactions take place at a faster rate than on smaller stars. So, although they have more matter, they burn faster, and last for a shorter period on the main sequence, not long enough for life ...
... Star types 0, B, A and down to F2 are massive hot stars. Gravity forces the atoms closer together so atomic reactions take place at a faster rate than on smaller stars. So, although they have more matter, they burn faster, and last for a shorter period on the main sequence, not long enough for life ...
OUR COSMIC NEIGHBORS Story of the Stars
... A long winding stream of stars was placed by primitive man at the “top of the sky.” According to a Greek legend, Draco represents the Dragon that guarded the Golden Apples in the Garden of Hesperides. This dragon was finally killed by Hercules and was placed in the sky in a position where it would n ...
... A long winding stream of stars was placed by primitive man at the “top of the sky.” According to a Greek legend, Draco represents the Dragon that guarded the Golden Apples in the Garden of Hesperides. This dragon was finally killed by Hercules and was placed in the sky in a position where it would n ...
Apparent Motion of the Stars Worksheet
... Delimit the circumpolar region as seen from any location. [Rule: The circumpolar region where stars never set below the horizon is a circular area of the sky centered on the visible celestial pole and extending to the horizon. The declination of the circumpolar boundary is given by ±(90°-observer’ ...
... Delimit the circumpolar region as seen from any location. [Rule: The circumpolar region where stars never set below the horizon is a circular area of the sky centered on the visible celestial pole and extending to the horizon. The declination of the circumpolar boundary is given by ±(90°-observer’ ...
Magnetic fields in O-, B-and A-type stars on the main sequence
... Magnetic fields have first been discovered in the Sun [1] and in the chemically peculiar A-type star 78 Virginis [2]. These two stars are representative of two major groups of magnetic stars, which are directly related to the dominant mechanism of heat transport in the outer layers of the stars. For ...
... Magnetic fields have first been discovered in the Sun [1] and in the chemically peculiar A-type star 78 Virginis [2]. These two stars are representative of two major groups of magnetic stars, which are directly related to the dominant mechanism of heat transport in the outer layers of the stars. For ...
mg_colloq - University of Massachusetts Amherst
... – Dynamical properties being explored; certainly consistent with being massive, compact spheroids (Onodera et al. 2012; van Dokkum et al. 2011) – Some suggest that they include a significant (25-50%) fraction of compact disks (Bruce et al. 2012) or even that they are mostly compact disks (van der We ...
... – Dynamical properties being explored; certainly consistent with being massive, compact spheroids (Onodera et al. 2012; van Dokkum et al. 2011) – Some suggest that they include a significant (25-50%) fraction of compact disks (Bruce et al. 2012) or even that they are mostly compact disks (van der We ...
- newmanlib.ibri.org
... What is the universe? Is it "all that is, or ever was, or ever will be" (Carl Sagan)? We don't know. We could define it by Sagan's definition, but that might be misleading. We're inside, and don't know how big it is. The visible part apparently had a beginning at the big bang. What we do know: 1. Th ...
... What is the universe? Is it "all that is, or ever was, or ever will be" (Carl Sagan)? We don't know. We could define it by Sagan's definition, but that might be misleading. We're inside, and don't know how big it is. The visible part apparently had a beginning at the big bang. What we do know: 1. Th ...
The Essential Cosmic Perspective, 6e
... Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to travel from the object to us. 3) Starting from the Big Bang, briefly explain how our solar system came to contain the chemic ...
... Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to travel from the object to us. 3) Starting from the Big Bang, briefly explain how our solar system came to contain the chemic ...
H2CO and CO in S140
... infrared sources in the S140 core. Using CS and NH3 observations and IRAS data Tafalla et al. (1993) have suggested that the most dense cores (n(H2) > 105 cm-3) in the complex are associated with the very red IRAS sources. In this case follow the model in the Fig. 3 and Fig. 4 we would expect H2CO e ...
... infrared sources in the S140 core. Using CS and NH3 observations and IRAS data Tafalla et al. (1993) have suggested that the most dense cores (n(H2) > 105 cm-3) in the complex are associated with the very red IRAS sources. In this case follow the model in the Fig. 3 and Fig. 4 we would expect H2CO e ...
THE NEUTRAL GAS DYNAMICS OF THE NEARBY MAGELLANIC
... UGCA 105 has a low systemic velocity (Vsys = 90.8±2.0 km s−1 , derived from the tilted ring analysis discussed in § 3.2) for its distance well outside the Local Group, and hence HI emission from UGCA 105 is relatively close in velocity space to the foreground emission from the Milky Way. The selecti ...
... UGCA 105 has a low systemic velocity (Vsys = 90.8±2.0 km s−1 , derived from the tilted ring analysis discussed in § 3.2) for its distance well outside the Local Group, and hence HI emission from UGCA 105 is relatively close in velocity space to the foreground emission from the Milky Way. The selecti ...
Sternentstehung - Star Formation
... Jet launching from accretion disks “magnetic accretion-ejection structures” (Ferreira et al 1995-1997): 1) disk material diffuses across magnetic field lines, 2) is lifted upwards by MHD forces, then 3) couples to the field and 4) becomes accelerated magnetocentrifugally and 5) collimated ...
... Jet launching from accretion disks “magnetic accretion-ejection structures” (Ferreira et al 1995-1997): 1) disk material diffuses across magnetic field lines, 2) is lifted upwards by MHD forces, then 3) couples to the field and 4) becomes accelerated magnetocentrifugally and 5) collimated ...
Sky Maps Teacher`s Guide - Northern Stars Planetarium
... Circumpolar Constellations and Stars are the constellations and stars that never set. The number of circumpolar constellations you see depends on your latitude. The further north or south you travel from the equator, the more stars become circumpolar. At the equator, no stars are circumpolar. At the ...
... Circumpolar Constellations and Stars are the constellations and stars that never set. The number of circumpolar constellations you see depends on your latitude. The further north or south you travel from the equator, the more stars become circumpolar. At the equator, no stars are circumpolar. At the ...
powerpoint - High Energy Physics at Wayne State
... The interstellar gas is the fuel for the formation of stars. Yet, interstellar material is very sparse, space between stars is quite empty – much more so than an vacuum one can achieve in the laboratory on Earth. Possibility of dark matter. Star Clusters – contain up to hundreds of thousands of star ...
... The interstellar gas is the fuel for the formation of stars. Yet, interstellar material is very sparse, space between stars is quite empty – much more so than an vacuum one can achieve in the laboratory on Earth. Possibility of dark matter. Star Clusters – contain up to hundreds of thousands of star ...
Star formation and the interstellar medium in galaxy
... H2 clouds are heated mainly by the photoelectric ejection of electrons from dust grains by the interstellar radiation field (Wolfire et al. 1995). Star formation occurs in giant molecular clouds (GMCs). These typically have masses of a few 105 106 M , temperatures around 10 K and number densities i ...
... H2 clouds are heated mainly by the photoelectric ejection of electrons from dust grains by the interstellar radiation field (Wolfire et al. 1995). Star formation occurs in giant molecular clouds (GMCs). These typically have masses of a few 105 106 M , temperatures around 10 K and number densities i ...
Are WE CORRECTLY Measuring the Star formation in galaxies?
... UV and Hα can be significantly affected by extinction (and by differing amounts) Possible stochastic sampling of IMF impacting observables Integrated optical light does not scale linearly with SFR Comparisons of stellar light with reprocessed stellar light ...
... UV and Hα can be significantly affected by extinction (and by differing amounts) Possible stochastic sampling of IMF impacting observables Integrated optical light does not scale linearly with SFR Comparisons of stellar light with reprocessed stellar light ...
Observations of Infrared-identified Protost ars in Molecular Maser
... Many protostars were recently identified from the infrared data from the Spitzer space telescope. We present the results of a maser survey toward 99 protostars in the Orion molecular cloud complex. Observations were carried out in the water maser line at 22 GH z and three class I methanol maser line ...
... Many protostars were recently identified from the infrared data from the Spitzer space telescope. We present the results of a maser survey toward 99 protostars in the Orion molecular cloud complex. Observations were carried out in the water maser line at 22 GH z and three class I methanol maser line ...
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.