observing the universe
... of dust and gas intermingled, all held together by gravity. The Sun and Earth are in the Milky Way Galaxy. Galaxies have many different characteristics, but the easiest way to classify them is by shape, referred to as morphology. In 1925 astronomer Edwin Hubble established a classification scheme fo ...
... of dust and gas intermingled, all held together by gravity. The Sun and Earth are in the Milky Way Galaxy. Galaxies have many different characteristics, but the easiest way to classify them is by shape, referred to as morphology. In 1925 astronomer Edwin Hubble established a classification scheme fo ...
Supermassive black holes
... younger, more metal rich and orbit in the same orientation, excepting some up and down motion ...
... younger, more metal rich and orbit in the same orientation, excepting some up and down motion ...
D109-08x
... but bluer than NGC 1569, is the extreme V-R color. It is virtually impossible for galaxy stellar populations to have V-R colors this blue unless there is almost a complete absence of a red giant branch. Thus, globally, this object appears to be very young. Further V and I CCD imaging obtained in 198 ...
... but bluer than NGC 1569, is the extreme V-R color. It is virtually impossible for galaxy stellar populations to have V-R colors this blue unless there is almost a complete absence of a red giant branch. Thus, globally, this object appears to be very young. Further V and I CCD imaging obtained in 198 ...
Starburst Galaxies Under the Microscope: High
... Since the supernova rate is dominated by stars with a mass of about 8 M (the most numerous stars still producing supernovae), which have a lifetime of about 3 10 7 years, the BrG and [Fe II] emission trace phases of the starbursts that are temporally separated by this amount of time. In principle, ...
... Since the supernova rate is dominated by stars with a mass of about 8 M (the most numerous stars still producing supernovae), which have a lifetime of about 3 10 7 years, the BrG and [Fe II] emission trace phases of the starbursts that are temporally separated by this amount of time. In principle, ...
The Milky Way Galaxy (ch. 23)
... formation and evolution of our galaxy (Fig.23.14)—halo forms first in nearly spherical shape, rest of gas collapsed to disk which has formed stars continuously since that time. (Think about how above properties suggest this.) More recently it was discovered that our Galaxy has a weak but detectable ...
... formation and evolution of our galaxy (Fig.23.14)—halo forms first in nearly spherical shape, rest of gas collapsed to disk which has formed stars continuously since that time. (Think about how above properties suggest this.) More recently it was discovered that our Galaxy has a weak but detectable ...
PPT
... Modeling such collisions on a computer shows that two spiral galaxies can merge to make an elliptical ...
... Modeling such collisions on a computer shows that two spiral galaxies can merge to make an elliptical ...
1. The "Q" word and its meaning
... a. Is quenching a good word to describe the end of star-formation in galaxies ? b. What are the timescale(s) for quenching? Pablo , Jarle c. Is quenching due to starvation or gas expulsion? Romeel 2. What do we learn from the MS on the "Q" word ? a. Is the apparent sSFR dichotomy real, and is it a f ...
... a. Is quenching a good word to describe the end of star-formation in galaxies ? b. What are the timescale(s) for quenching? Pablo , Jarle c. Is quenching due to starvation or gas expulsion? Romeel 2. What do we learn from the MS on the "Q" word ? a. Is the apparent sSFR dichotomy real, and is it a f ...
Document
... • Detected a large amplitude soft X-ray flare from 3 galaxies which were classified as non-active from ground based spectra. ...
... • Detected a large amplitude soft X-ray flare from 3 galaxies which were classified as non-active from ground based spectra. ...
Stellar population models in the Near-Infrared Meneses
... of a spectral absorption line, determined by comparing the spectral flux on both sides of the feature with the flux inside the absorption line), integrated colours and Spectral Energy Distributions (SEDs). By combining optical and NIR models and data, we find evidence that the contribution of the AG ...
... of a spectral absorption line, determined by comparing the spectral flux on both sides of the feature with the flux inside the absorption line), integrated colours and Spectral Energy Distributions (SEDs). By combining optical and NIR models and data, we find evidence that the contribution of the AG ...
Galaxies * Island universes
... A Galaxy’s color evolves from bluer, towards redder as stellar population ages, young blue stars die out Galaxy collisions common because they’re usually only 100 or fewer galaxy diameters apart Collisions between galaxies produce irregulars which settle into ellipticals More massive ellipticals hav ...
... A Galaxy’s color evolves from bluer, towards redder as stellar population ages, young blue stars die out Galaxy collisions common because they’re usually only 100 or fewer galaxy diameters apart Collisions between galaxies produce irregulars which settle into ellipticals More massive ellipticals hav ...
astronomy advisory panel strategy
... Understanding the birth of stars is fundamental to astrophysics. Any realistic explanation of the formation and evolution of galaxies requires us to know what determines the rate of star formation, what determines any variation in the mass distribution of stars formed, and what determines the charac ...
... Understanding the birth of stars is fundamental to astrophysics. Any realistic explanation of the formation and evolution of galaxies requires us to know what determines the rate of star formation, what determines any variation in the mass distribution of stars formed, and what determines the charac ...
T Einstein’s Mirage Paul L. Schechter
... being imaged—it is a mirror image, but distorted. At least one of the other images must have the correct handedness, but it will also be distorted. The French call such distorted images gravitational mirages. In the half century following the confirmation of general relativity, the idea that cosmic ...
... being imaged—it is a mirror image, but distorted. At least one of the other images must have the correct handedness, but it will also be distorted. The French call such distorted images gravitational mirages. In the half century following the confirmation of general relativity, the idea that cosmic ...
Searching for stars in high-velocity clouds
... at similar distances to that of M31. In Fig. 1 we show the colour– magnitude plot for the three HVC fields and offsets. For a similar distance to M31 we would expect a cluster of stars (tip of red giant branch) around m I = 21–22 with colours of (V − I ) = 1.2–1.8 (box in Fig. 1). None of the colour ...
... at similar distances to that of M31. In Fig. 1 we show the colour– magnitude plot for the three HVC fields and offsets. For a similar distance to M31 we would expect a cluster of stars (tip of red giant branch) around m I = 21–22 with colours of (V − I ) = 1.2–1.8 (box in Fig. 1). None of the colour ...
Chapter 17
... “smudges” that were thought to be nebulae in the Milky Way were recognized to be whole galaxies far outside our own. The discovery was made in the 1920s by Edwin Hubble, an American astronomer. When he focused a huge telescope on an object thought to be a nebula in the constellation Andromeda, Hubbl ...
... “smudges” that were thought to be nebulae in the Milky Way were recognized to be whole galaxies far outside our own. The discovery was made in the 1920s by Edwin Hubble, an American astronomer. When he focused a huge telescope on an object thought to be a nebula in the constellation Andromeda, Hubbl ...
Are Gamma-Ray Bursts good Star Formation Indicators?
... observations are required if we are to obtain redshifts for statistical samples. GRBs are rare, building up sufficient numbers is a slow process, consuming considerable telescope time. GRBs can only be used as global indicators and aren’t useful for studying the star formation rate in individual gal ...
... observations are required if we are to obtain redshifts for statistical samples. GRBs are rare, building up sufficient numbers is a slow process, consuming considerable telescope time. GRBs can only be used as global indicators and aren’t useful for studying the star formation rate in individual gal ...
presentation source
... near center of the galaxy •Hole grows as dust/gas within galaxy falls into it •If large enough, the Black Hole could swallow entire stars and grow very massive, maybe millions of MO •If galaxy massive enough, or through encounters with other galaxies, could grow even more massive •As galaxy ages, av ...
... near center of the galaxy •Hole grows as dust/gas within galaxy falls into it •If large enough, the Black Hole could swallow entire stars and grow very massive, maybe millions of MO •If galaxy massive enough, or through encounters with other galaxies, could grow even more massive •As galaxy ages, av ...
Part1
... o The infrared continuum is a key tracer of the distribution of dust and the dust-to-gas ratio is intimately related to heavy element enrichment (e.g., you need dust to see IR!). o Along similar lines, millimeter line tracers of the ISM are key to robustly measure the dust-to-gas ratio in large syst ...
... o The infrared continuum is a key tracer of the distribution of dust and the dust-to-gas ratio is intimately related to heavy element enrichment (e.g., you need dust to see IR!). o Along similar lines, millimeter line tracers of the ISM are key to robustly measure the dust-to-gas ratio in large syst ...
The resolved stellar populations of M32 Monachesi, Antonela
... because they contain a predominant fraction of the total stellar mass in the local Universe. Although they appear as simple objects on the sky, ellipticals are in fact very complex systems. They are found in a variety of different sizes, ranging from the largest to the smallest known galaxies, and p ...
... because they contain a predominant fraction of the total stellar mass in the local Universe. Although they appear as simple objects on the sky, ellipticals are in fact very complex systems. They are found in a variety of different sizes, ranging from the largest to the smallest known galaxies, and p ...
File - Mr. Catt`s Class
... 2. The spectra of 3C 273 and 3C 48 (the second unusual object discovered in 1960) showed emission lines, which could not be identified. Because of their star-like appearance and strong radio emission, the objects were named quasars. 3. A quasar (quasi-stellar radio source) is a small, intense celes ...
... 2. The spectra of 3C 273 and 3C 48 (the second unusual object discovered in 1960) showed emission lines, which could not be identified. Because of their star-like appearance and strong radio emission, the objects were named quasars. 3. A quasar (quasi-stellar radio source) is a small, intense celes ...
PH607 – Galaxies
... Components: Almost 90% of its mass cannot be accounted for (the "dark matter" problem). The Local Group: It then goes on to consider how the Milky Way fits in with what we see in other galaxies, and what the morphologies of these systems tell us about their life histories. Evolution: Galaxies are no ...
... Components: Almost 90% of its mass cannot be accounted for (the "dark matter" problem). The Local Group: It then goes on to consider how the Milky Way fits in with what we see in other galaxies, and what the morphologies of these systems tell us about their life histories. Evolution: Galaxies are no ...
Lecture 2: ppt, 5 MB
... A scrapbook of the early universe Hubble images reveal "toddler" galaxies 400 to 800 million years after the Big Bang Unlike the Milky Way, baby galaxies take many shapes toothpicks links on a bracelet ...
... A scrapbook of the early universe Hubble images reveal "toddler" galaxies 400 to 800 million years after the Big Bang Unlike the Milky Way, baby galaxies take many shapes toothpicks links on a bracelet ...
Galactic Evolution:
... • The H flux from HII regions, which are ionized by young and hot stars, under the assumption that such flux is proportional to the SFR • The integrated UBV colors and spectra of galaxies (one can estimate the relative proportions of young and old stars and derive the ratio between the present time ...
... • The H flux from HII regions, which are ionized by young and hot stars, under the assumption that such flux is proportional to the SFR • The integrated UBV colors and spectra of galaxies (one can estimate the relative proportions of young and old stars and derive the ratio between the present time ...
Pea galaxy
A Pea galaxy, also referred to as a Pea or Green Pea, might be a type of Luminous Blue Compact Galaxy which is undergoing very high rates of star formation. Pea galaxies are so-named because of their small size and greenish appearance in the images taken by the Sloan Digital Sky Survey (SDSS).Pea Galaxies were first discovered in 2007 by the volunteer users within the forum section of the online astronomy project Galaxy Zoo (GZ).