The Intricate Role of Cold Gas and Dust in Galaxy Evolution at Early
... - idea: z>4 galaxy dust spectral energy distributions peak beyond 500 µm! ! can use (sub)mm colors to determine reasonable photometric redshifts! ! “red” sources are strong candidates for starbursts at the earliest epochs Systematic approach, but…how well does it work?! ...
... - idea: z>4 galaxy dust spectral energy distributions peak beyond 500 µm! ! can use (sub)mm colors to determine reasonable photometric redshifts! ! “red” sources are strong candidates for starbursts at the earliest epochs Systematic approach, but…how well does it work?! ...
How Marius Was Right and Galileo Was Wrong Even Though
... these ideas will require further discussion and explanation. Lastly, he concedes to Galileo that the stars shine by their own light -- they are distinct in appearance from the planets (being notably more intense in brilliance).13 ...
... these ideas will require further discussion and explanation. Lastly, he concedes to Galileo that the stars shine by their own light -- they are distinct in appearance from the planets (being notably more intense in brilliance).13 ...
Perseid Watch at Weiser State Forest August 12
... chemical elements in stars in the Milky Way. The light chemical element lithium is one of the few elements that is predicted to have been created by the Big Bang, 13.8 billion years ago. But understanding the amounts of lithium observed in stars around us today in the Universe has given astronomers ...
... chemical elements in stars in the Milky Way. The light chemical element lithium is one of the few elements that is predicted to have been created by the Big Bang, 13.8 billion years ago. But understanding the amounts of lithium observed in stars around us today in the Universe has given astronomers ...
Using Parallax to Measure the Distance of Stars
... determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby (for example, the Moon), and the Hubble Law being useful at the farthest distances. In this exercise, we investigate the use of the ...
... determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby (for example, the Moon), and the Hubble Law being useful at the farthest distances. In this exercise, we investigate the use of the ...
Constellation
... harvest in the fall. But in some regions, there is not much difference between the seasons. Since different constellations are visible at different times of the year, you can use them to tell what month it is. For example, Scorpius is only visible in the northern hemisphere's evening sky in the summ ...
... harvest in the fall. But in some regions, there is not much difference between the seasons. Since different constellations are visible at different times of the year, you can use them to tell what month it is. For example, Scorpius is only visible in the northern hemisphere's evening sky in the summ ...
MAGNITUDE AND COLOR SYSTEMS
... where f is the mean spectral flux density (see Lec. 2) from a source at the top of the Earth’s atmosphere averaged over a defined band and Q is a normalizing constant for that band. Although this definition looks peculiar, it offers two important practical conveniences: (1) Cosmic sources have an en ...
... where f is the mean spectral flux density (see Lec. 2) from a source at the top of the Earth’s atmosphere averaged over a defined band and Q is a normalizing constant for that band. Although this definition looks peculiar, it offers two important practical conveniences: (1) Cosmic sources have an en ...
NUCLEOSYNTHESIS
... 1. Spectral analysis of the Sun • photospheric absorption lines −→ abundance ratios element:hydrogen – exceptions: He, Ne, Ar, rare heavy elements – no information on isotopic abundances, except from some molecules (e.g. CO, CN, MgH) • emission lines from chromosphere, corona (far-UV) −→ He, Ne, Ar, ...
... 1. Spectral analysis of the Sun • photospheric absorption lines −→ abundance ratios element:hydrogen – exceptions: He, Ne, Ar, rare heavy elements – no information on isotopic abundances, except from some molecules (e.g. CO, CN, MgH) • emission lines from chromosphere, corona (far-UV) −→ He, Ne, Ar, ...
Carbon, nitrogen, oxygen and lithium abundances of six
... whereas the Sc abundance has been determined from other lines (Paper I). The oxygen abundance was then derived by fitting the observed [OI] line with the line computed with different oxygen abundance values; let us note that the [OI] and the nearby ScII lines form roughly in the same atmospheric lay ...
... whereas the Sc abundance has been determined from other lines (Paper I). The oxygen abundance was then derived by fitting the observed [OI] line with the line computed with different oxygen abundance values; let us note that the [OI] and the nearby ScII lines form roughly in the same atmospheric lay ...
Name: Period:______ Date:______ Astronomy Vocabulary DUE
... To help you learn the up and coming vocabulary for the unit, students are to APPLY the vocabulary terms in different ways to assist in long term memory to be applied in labs in the future. In the box provided, provide eth application strategy that is necessary for each term. MUST be neat and COLORED ...
... To help you learn the up and coming vocabulary for the unit, students are to APPLY the vocabulary terms in different ways to assist in long term memory to be applied in labs in the future. In the box provided, provide eth application strategy that is necessary for each term. MUST be neat and COLORED ...
Spinar Paradigm
... The proposed scenario allows the observed variety of gamma-ray bursts, precursors, and flares to be reduced to just two parameters: magnetic field and initial angular momentum. In the case of weak magnetic field and large angular momentum (the bottom-right corner) the first burst is weak (because of ...
... The proposed scenario allows the observed variety of gamma-ray bursts, precursors, and flares to be reduced to just two parameters: magnetic field and initial angular momentum. In the case of weak magnetic field and large angular momentum (the bottom-right corner) the first burst is weak (because of ...
File
... The star is new and it doesn't understand it's solar system. What should they do? How can they solve their problem? They shouldn't be worried, it is all normal. Why should they do that? What facts can we give to them to reinforce our answer? The objects revolving around the star are probably planets ...
... The star is new and it doesn't understand it's solar system. What should they do? How can they solve their problem? They shouldn't be worried, it is all normal. Why should they do that? What facts can we give to them to reinforce our answer? The objects revolving around the star are probably planets ...
CO OBSERVATIONS OF SPIRAL STRUCTURE AND THE LIFETIME
... and on the other hand you show that they are gravitationally bound, what prevents these clouds from collapsing? Scoville: It is clear that there is some mechanism restraining the ob served clouds from free-fall collapse. It is also clear from observa tions of external galaxies that although dust c ...
... and on the other hand you show that they are gravitationally bound, what prevents these clouds from collapsing? Scoville: It is clear that there is some mechanism restraining the ob served clouds from free-fall collapse. It is also clear from observa tions of external galaxies that although dust c ...
PARALLAX – IT`S SIMPLE! Abstract
... needed to calculate the real energy output of the star (luminosity). Other physical properties (core temperature, radius, mass) are also connected to the star’s luminosity. How far can parallax measurements reach? The diameter of our Galaxy is about 30 thousands parsecs, so it is clear that the HIPP ...
... needed to calculate the real energy output of the star (luminosity). Other physical properties (core temperature, radius, mass) are also connected to the star’s luminosity. How far can parallax measurements reach? The diameter of our Galaxy is about 30 thousands parsecs, so it is clear that the HIPP ...
Constraints on the exosphere of CoRoT-7b*
... 4520 Å. There are two detectors for the red channel, which cover the wavelength regions from 4780 to 5740 Å, and from 5820 to 6760 Å. We used a slit-width of 0.6 arcsec, which provides a resolution of λ/Δλ = 65 000. Apart from the differences in exposure time, the second data-set has the disadvantage ...
... 4520 Å. There are two detectors for the red channel, which cover the wavelength regions from 4780 to 5740 Å, and from 5820 to 6760 Å. We used a slit-width of 0.6 arcsec, which provides a resolution of λ/Δλ = 65 000. Apart from the differences in exposure time, the second data-set has the disadvantage ...
New Suns in the Cosmos?
... upsurge along the past 15 years, with the discovery of many extra-solar planetary systems, demonstrating that the Sun is not unique as a planet host star. In this context, the main question now is the extent to which the properties of the Sun and its planetary system can be considered as representat ...
... upsurge along the past 15 years, with the discovery of many extra-solar planetary systems, demonstrating that the Sun is not unique as a planet host star. In this context, the main question now is the extent to which the properties of the Sun and its planetary system can be considered as representat ...
Starfarer
... steer towards whichever star rises or sets in the direction of the island destination. The bearing of the destination is the azimuth or bearing of its guiding star, at rise if the course is an easterly one and at set if it is westerly. Although stars rise 4 minutes earlier each night, so that after ...
... steer towards whichever star rises or sets in the direction of the island destination. The bearing of the destination is the azimuth or bearing of its guiding star, at rise if the course is an easterly one and at set if it is westerly. Although stars rise 4 minutes earlier each night, so that after ...
SW - Calculating Magnitudes
... how bright an object is relative to other objects in the Universe, we must account for the object’s distance from Earth. To do this, astronomers hypothetically place all objects at an equal distance from Earth and measure what their brightness would be from this point. This is a distance of 10 parse ...
... how bright an object is relative to other objects in the Universe, we must account for the object’s distance from Earth. To do this, astronomers hypothetically place all objects at an equal distance from Earth and measure what their brightness would be from this point. This is a distance of 10 parse ...
How to interpret LPV in roAp stars Hiromoto Shibahashi , Don Kurtz
... one pulsation cycle. This maximum speed is much higher than the radial velocity pulsation amplitudes so far detected from other spectral lines in other roAp stars -- of the order of 1 km s-1 or less. This is possible if the Nd III 6145 line is formed in a high layer where the density is very low. ...
... one pulsation cycle. This maximum speed is much higher than the radial velocity pulsation amplitudes so far detected from other spectral lines in other roAp stars -- of the order of 1 km s-1 or less. This is possible if the Nd III 6145 line is formed in a high layer where the density is very low. ...
Finnish Centre for Astronomy with ESO
... cosmology, active galaxies, and galaxy formation and evolution, through properties of nearby galaxies, to supernovae and their progenitor stars, stellar magnetic activity, star formation and exoplanets in our own Galaxy. In our research, we use radio to gamma-rays multi-wavelength observational data ...
... cosmology, active galaxies, and galaxy formation and evolution, through properties of nearby galaxies, to supernovae and their progenitor stars, stellar magnetic activity, star formation and exoplanets in our own Galaxy. In our research, we use radio to gamma-rays multi-wavelength observational data ...
R136a1
RMC 136a1 (usually abbreviated to R136a1) is a Wolf-Rayet star located at the center of R136, the central condensation of stars of the large NGC 2070 open cluster in the Tarantula Nebula. It lies at a distance of about 50 kiloparsecs (163,000 light-years) in the Large Magellanic Cloud. It has the highest mass and luminosity of any known star, at 265 M☉ and 8.7 million L☉, and also one of the hottest at over 50,000 K.