poster
... Between June 2003 and May 2004, 65 candidates have been observed by VLT and 37 type Ia supernovae identified with a redshift comprised between 0.2 and ...
... Between June 2003 and May 2004, 65 candidates have been observed by VLT and 37 type Ia supernovae identified with a redshift comprised between 0.2 and ...
ppt
... Massive stars have small M/L. Low-mass stars have large M/L. Neutron stars and black holes hardly shine at all (they have very high M/L). ...
... Massive stars have small M/L. Low-mass stars have large M/L. Neutron stars and black holes hardly shine at all (they have very high M/L). ...
Ch 28 Class Notes
... Because Earth orbits the sun, astronomers experience parallax when they observe the stars. Astronomers can _____________ ______________________________________________________________________________, by knowing the angle between two observed positions and the distance between the observation point ...
... Because Earth orbits the sun, astronomers experience parallax when they observe the stars. Astronomers can _____________ ______________________________________________________________________________, by knowing the angle between two observed positions and the distance between the observation point ...
Stellar Clusters and Star Formation:
... In simple terms, star formation proceeds in the manner previously discussed – namely a ball of gas collapsed under its own self-gravity until it’s stabilized by sufficient internal pressure. At that point it is a hydrogen fusing main sequence star. However, over the last 25 years we have learned and ...
... In simple terms, star formation proceeds in the manner previously discussed – namely a ball of gas collapsed under its own self-gravity until it’s stabilized by sufficient internal pressure. At that point it is a hydrogen fusing main sequence star. However, over the last 25 years we have learned and ...
2P10.pdf
... The scientific goals of the Gaia mission require complementary astrometry, photometry and radial velocity data. After five years scanning the entire sky, Gaia will have performed measurements with broad (BBP), and medium (MBP) bands, and white light (G magnitude). The main goal of the photometry is ...
... The scientific goals of the Gaia mission require complementary astrometry, photometry and radial velocity data. After five years scanning the entire sky, Gaia will have performed measurements with broad (BBP), and medium (MBP) bands, and white light (G magnitude). The main goal of the photometry is ...
GAIA A Stereoscopic Census of our Galaxy
... distances to 1% for ~10 million stars to 2.5 kpc distances to 10% for ~100 million stars to 25 kpc rare stellar types and rapid evolutionary phases in large numbers parallax calibration of all distance indicators e.g. Cepheids and RR Lyrae to LMC/SMC ...
... distances to 1% for ~10 million stars to 2.5 kpc distances to 10% for ~100 million stars to 25 kpc rare stellar types and rapid evolutionary phases in large numbers parallax calibration of all distance indicators e.g. Cepheids and RR Lyrae to LMC/SMC ...
Here
... Hence the stellar populations characteristics of E galaxies must be derived from the integrated colors and spectra. As we saw before, the spectra of an E galaxy resembles that of a K giant star. E galaxies appear generally red: •very few stars made in the last 1-2 Gyr (recall that after 1 Gyr, only ...
... Hence the stellar populations characteristics of E galaxies must be derived from the integrated colors and spectra. As we saw before, the spectra of an E galaxy resembles that of a K giant star. E galaxies appear generally red: •very few stars made in the last 1-2 Gyr (recall that after 1 Gyr, only ...
Astrophysics - Part 2
... Parsec and light year. Definition of M, relation to m: m – M = 5 log (d / 10) Classification by temperature, black body radiation Stefan’s law and Wien’s displacement law.General shape of black body curves, experimental verification is not required. Use of Wien’s displacement law to estimate black-b ...
... Parsec and light year. Definition of M, relation to m: m – M = 5 log (d / 10) Classification by temperature, black body radiation Stefan’s law and Wien’s displacement law.General shape of black body curves, experimental verification is not required. Use of Wien’s displacement law to estimate black-b ...
HOLIDAYS HOME WORK
... Q7. A bus covered a distance of 182 km from Delhi to Roorkee in 5.5 hours. What is the average speed? Express it in appropriate number of significant figures. Q8. What is the difference in writing a length as 3.2 cm and 3.200 cm? Q9. In an experiment, Refractive Index of glass was observed to be 1.4 ...
... Q7. A bus covered a distance of 182 km from Delhi to Roorkee in 5.5 hours. What is the average speed? Express it in appropriate number of significant figures. Q8. What is the difference in writing a length as 3.2 cm and 3.200 cm? Q9. In an experiment, Refractive Index of glass was observed to be 1.4 ...
Measuring Distance Using Triangulation and Parallax Trigonometry
... the distance d, the angles will be almost 90 degrees. For example if S=5 ft and d=10 miles, the angle would be 89.9946 degrees. Measuring angles like this is very difficult. A different method may be a ...
... the distance d, the angles will be almost 90 degrees. For example if S=5 ft and d=10 miles, the angle would be 89.9946 degrees. Measuring angles like this is very difficult. A different method may be a ...
1 The Milky Way
... Galactic rotation. We can measure the rotation speed of the disc as a function of radial distance from the centre of the Galaxy - see Fig. 7. The very central parts rotate slowly. The speed picks up as you move outwards, and then flattens off, with rotation speed apparently constant as far out as we ...
... Galactic rotation. We can measure the rotation speed of the disc as a function of radial distance from the centre of the Galaxy - see Fig. 7. The very central parts rotate slowly. The speed picks up as you move outwards, and then flattens off, with rotation speed apparently constant as far out as we ...
File
... Earth Science 25.3 The Universe Galaxy Clusters: Once astronomers discovered that stars were found in groups, they wondered whether galaxies also were grouped or just randomly distributed among the universe. They found that, like stars, galaxies are grouped in clusters. Some clusters may cont ...
... Earth Science 25.3 The Universe Galaxy Clusters: Once astronomers discovered that stars were found in groups, they wondered whether galaxies also were grouped or just randomly distributed among the universe. They found that, like stars, galaxies are grouped in clusters. Some clusters may cont ...
Stars
... toward each other by gravity • Many stars orbit each other • More than 50% of stars occur in pairs or multiples. • Binary stars are used to determine the star property most difficult to calculate – It’s mass ...
... toward each other by gravity • Many stars orbit each other • More than 50% of stars occur in pairs or multiples. • Binary stars are used to determine the star property most difficult to calculate – It’s mass ...
PH607 – Galaxies 2
... Because of cool interstellar dust along the line of sight, the Galactic Centre cannot be studied at visible, ultraviolet or soft Xray wavelengths. The available information about the Galactic Center comes from observations at gamma ray, hard X-ray, infrared, sub-millimetre and radio wavelengths. ...
... Because of cool interstellar dust along the line of sight, the Galactic Centre cannot be studied at visible, ultraviolet or soft Xray wavelengths. The available information about the Galactic Center comes from observations at gamma ray, hard X-ray, infrared, sub-millimetre and radio wavelengths. ...
The Milky Way The Milky Way`s Neighbourhood
... Figuring out the shape of the Milky Way is, for us, somewhat like a fish trying to figure out the shape of the ocean. Based on careful observations and calculations, though, it appears that the Milky Way is a barred spiral galaxy, probably classified as a SBb or SBc on the Hubble tuning fork diagram ...
... Figuring out the shape of the Milky Way is, for us, somewhat like a fish trying to figure out the shape of the ocean. Based on careful observations and calculations, though, it appears that the Milky Way is a barred spiral galaxy, probably classified as a SBb or SBc on the Hubble tuning fork diagram ...
Summer Triangle (Winter in the south hemisphere) Lyra
... The Ring Nebula is often regarded as the prototype of all planetary nebulae. These objects are the remains of sunlike stars which have blown away their outer envelopes, leaving planet-sized white dwarfs at their centers. The distance to M 57 is not very well known; estimates range from 1400 to 4100 ...
... The Ring Nebula is often regarded as the prototype of all planetary nebulae. These objects are the remains of sunlike stars which have blown away their outer envelopes, leaving planet-sized white dwarfs at their centers. The distance to M 57 is not very well known; estimates range from 1400 to 4100 ...
Galaxies
... Dark Matter in the Universe Galaxy mass measurements show that galaxies need between 3 and 10 times more mass than can be observed to explain their rotation curves. The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the ...
... Dark Matter in the Universe Galaxy mass measurements show that galaxies need between 3 and 10 times more mass than can be observed to explain their rotation curves. The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the ...
A Stellar Astronomy Toolbox 9
... This is a very important equation in this class. Notice that brightness is something we can readily measure here on Earth using a telescope and a digital camera. So, 1. If we know how far away a star is (D) and we measure its brightness (B) then we can calculate how luminous (L) it is. 2. Or if we k ...
... This is a very important equation in this class. Notice that brightness is something we can readily measure here on Earth using a telescope and a digital camera. So, 1. If we know how far away a star is (D) and we measure its brightness (B) then we can calculate how luminous (L) it is. 2. Or if we k ...
IPHAS: Surveying the Northern Galactic Plane in Hα
... (red) stars in the (r'– i',r'–Hα) plane according to spectral type. The right-hand panel shows the observed sources in a field in the Cygnus region (black points), with some spectroscropically determined spectral types overplotted in colour; light blue points are early-type stars, red points are mos ...
... (red) stars in the (r'– i',r'–Hα) plane according to spectral type. The right-hand panel shows the observed sources in a field in the Cygnus region (black points), with some spectroscropically determined spectral types overplotted in colour; light blue points are early-type stars, red points are mos ...
Measuring the Properties of Stars - Sierra College Astronomy Home
... The sizes of a few very large stars have been measured directly by interferometry. Knowing the temperature of a star gives its energy emitted per square meter. Knowing the total energy emitted (from the absolute magnitude) one can then calculate the surface area of the star. From that the di ...
... The sizes of a few very large stars have been measured directly by interferometry. Knowing the temperature of a star gives its energy emitted per square meter. Knowing the total energy emitted (from the absolute magnitude) one can then calculate the surface area of the star. From that the di ...
GOFER Module: Google Sky Please open Google Earth, then
... Enter, or click the magnifying glass. Click on the star once you arrive at your destination. (It will separate from the crosshairs after your first click, then click on it again.) Which of the following is true about Polaris? A. It is one of the dimmest stars in its constellation. B. It is found in ...
... Enter, or click the magnifying glass. Click on the star once you arrive at your destination. (It will separate from the crosshairs after your first click, then click on it again.) Which of the following is true about Polaris? A. It is one of the dimmest stars in its constellation. B. It is found in ...
Astronomical units
... Color does not reflect temperature for objects with spectra very different from that of a blackbody. Still can be useful - e.g. basis of most successful method for finding very distant (high redshift) galaxies: Observed galaxy spectrum shifts to the right for source at higher redshift. Because spec ...
... Color does not reflect temperature for objects with spectra very different from that of a blackbody. Still can be useful - e.g. basis of most successful method for finding very distant (high redshift) galaxies: Observed galaxy spectrum shifts to the right for source at higher redshift. Because spec ...
Cosmology - RHIG - Wayne State University
... (99.9% of the speed of light) But we need a system (i.e. a chunk of matter and not just a single particle) so that the system can follow simple rules of thermodynamics and form a new state of matter in a particular phase. We use heavy ions (e.g. a Gold ion which is made of 197 protons and neutrons). ...
... (99.9% of the speed of light) But we need a system (i.e. a chunk of matter and not just a single particle) so that the system can follow simple rules of thermodynamics and form a new state of matter in a particular phase. We use heavy ions (e.g. a Gold ion which is made of 197 protons and neutrons). ...
ASTRONOMY 5
... shine in a different way by ejecting blobs of ionized, fast-moving gas mixed with magnetic fields. The electrons in the gas spiral around in the magnetic field, which causes them to emit bright synchrotron radio emission (and sometimes visible light). These appear as “jets” and “lobes” in radio imag ...
... shine in a different way by ejecting blobs of ionized, fast-moving gas mixed with magnetic fields. The electrons in the gas spiral around in the magnetic field, which causes them to emit bright synchrotron radio emission (and sometimes visible light). These appear as “jets” and “lobes” in radio imag ...
Planet Mass ~13 M E
... Note: amateurs discovered closest microlensed star (Casseopeia) November 2006; 8th magnitude at peak ...
... Note: amateurs discovered closest microlensed star (Casseopeia) November 2006; 8th magnitude at peak ...
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.