Determination of the distance to the Andromeda Galaxy using variable stars U
... A.1 The observed phenomenon Flares are observed on magnetically active stars and, much more closely, on the Sun. Electromagnetic radiation is emitted across the entire spectrum, from radio waves through the optical range to X-rays and γ-rays. The total energy released during a typical solar flare is ...
... A.1 The observed phenomenon Flares are observed on magnetically active stars and, much more closely, on the Sun. Electromagnetic radiation is emitted across the entire spectrum, from radio waves through the optical range to X-rays and γ-rays. The total energy released during a typical solar flare is ...
Non-thermal hard X-ray emission from stellar coronae
... Fast rotation ⇒ efficient dynamo ⇒ enhanced magnetic activity ...
... Fast rotation ⇒ efficient dynamo ⇒ enhanced magnetic activity ...
Exploring Neutral Hydrogen and Galaxy Evolution with the SKA
... Analysis of thousands of galaxies in the Sloan Digital Sky Survey (SDSS) has shown that they follow a bimodal distribution in colour as a function of stellar mass (Baldry et al. (2004)); most galaxies are either located in the so-called blue cloud or on the red sequence, indicating that star formati ...
... Analysis of thousands of galaxies in the Sloan Digital Sky Survey (SDSS) has shown that they follow a bimodal distribution in colour as a function of stellar mass (Baldry et al. (2004)); most galaxies are either located in the so-called blue cloud or on the red sequence, indicating that star formati ...
Neutron Stars
... with Prof. Antony Hewish at Cambridge. Pulsars derive their name from ”pulsating radio sources” because they were first observed at radio wave frequencies. Hewish won the 1974 Nobel Prize in Physics along with Sir Martin Ryle for their ”pioneering discoveries in radio astrophysics.” Hewish was cited ...
... with Prof. Antony Hewish at Cambridge. Pulsars derive their name from ”pulsating radio sources” because they were first observed at radio wave frequencies. Hewish won the 1974 Nobel Prize in Physics along with Sir Martin Ryle for their ”pioneering discoveries in radio astrophysics.” Hewish was cited ...
THE MORPHOLOGICAL DEMOGRAPHICS OF GALAXIES IN THE
... were f (R) = 2π 0R I(r)dr is the integrated flux within the radius R. The determination of the radius R up to where to integrate the light is of importance particularly for the asymmetry values. As we sample galaxies over ever larger cosmic ages, the surface brightness of galaxies at higher redshift ...
... were f (R) = 2π 0R I(r)dr is the integrated flux within the radius R. The determination of the radius R up to where to integrate the light is of importance particularly for the asymmetry values. As we sample galaxies over ever larger cosmic ages, the surface brightness of galaxies at higher redshift ...
Module 11.1.1: Galaxies: Morphology and the Hubble Sequence
... [slide 2] First, we'll talk about morphology and classification. You can think of galaxies as the basic constituents of the universe, obviously distinct units when you look at the sky. And the reason ...
... [slide 2] First, we'll talk about morphology and classification. You can think of galaxies as the basic constituents of the universe, obviously distinct units when you look at the sky. And the reason ...
Jul y 9- 11,
... central supermassive black holes (SMBHs) will be more often present even in smaller galaxies when seeds are generated from the remnants of the first massive stars rather than via direct gas collapse. Consequently, measurement of the local occupation fraction provides an observational discriminator b ...
... central supermassive black holes (SMBHs) will be more often present even in smaller galaxies when seeds are generated from the remnants of the first massive stars rather than via direct gas collapse. Consequently, measurement of the local occupation fraction provides an observational discriminator b ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... of our Galaxy. This INTERSTELLAR MATTER effectively blocks all optical light from distant objects, making it impossible to find galaxies lurking in the background. Ongoing and planned surveys in the infrared and radio wavelengths can penetrate the haze of the Milky Way by detecting radiation that is ...
... of our Galaxy. This INTERSTELLAR MATTER effectively blocks all optical light from distant objects, making it impossible to find galaxies lurking in the background. Ongoing and planned surveys in the infrared and radio wavelengths can penetrate the haze of the Milky Way by detecting radiation that is ...
Eye in the sky - Academy of Science of South Africa
... like 10 – 20 millisecond chunks actually). Because of its size, and the long-exposure ability, SALT can see objects that are billions of times fainter than our naked eye can detect. And there’s still more to it. In astronomy resolution is essential. It is important that things can be resolved, or di ...
... like 10 – 20 millisecond chunks actually). Because of its size, and the long-exposure ability, SALT can see objects that are billions of times fainter than our naked eye can detect. And there’s still more to it. In astronomy resolution is essential. It is important that things can be resolved, or di ...
A New Science Strategy for Space Astronomy and Astrophysics
... next decade,1 prepared by a committee under the leadership of John Bahcall. Like previous decadal studies in this field, the report identified in priority order the most important scientific programs and projects for both groundand space-based research. It recommended a single large initiative for s ...
... next decade,1 prepared by a committee under the leadership of John Bahcall. Like previous decadal studies in this field, the report identified in priority order the most important scientific programs and projects for both groundand space-based research. It recommended a single large initiative for s ...
Detection of the Stochastic Background of nHz Gravitational Radiation from Massive Black
... (left) to the USNO master clock ensemble in Wash., DC (below). ...
... (left) to the USNO master clock ensemble in Wash., DC (below). ...
Neutron Star and Superfluidity
... form cooper pairs, just as what happen to electrons in conventional s-wave superconductor. Typical temperature of neutron star is much smaller than the estimated critical temperature for superfluidity by many-body simulation except new-born neutron star [5]. Hence it is believed that s-wave neutron s ...
... form cooper pairs, just as what happen to electrons in conventional s-wave superconductor. Typical temperature of neutron star is much smaller than the estimated critical temperature for superfluidity by many-body simulation except new-born neutron star [5]. Hence it is believed that s-wave neutron s ...
Is there a Supermassive Black Hole at the Center of the Milky Way?
... Very strong sources of radio waves were discovered in the early years of radio astronomy. Accurate positions of these sources revealed that they were often centered on distant galaxies. In the 1950s, radio interferometers revealed a totally unexpected picture of these “radio galaxies.” The radio wav ...
... Very strong sources of radio waves were discovered in the early years of radio astronomy. Accurate positions of these sources revealed that they were often centered on distant galaxies. In the 1950s, radio interferometers revealed a totally unexpected picture of these “radio galaxies.” The radio wav ...
English version - Richard de Grijs
... Chandra’s images are giving the astronomers a closer-than-ever look at the distinctive geometry of the charged particle winds radiating in X-rays and other wavelengths from the objects, according to Posselt. Pulsar wind nebulae (PWN) are produced when the energetic particles streaming from pulsar ...
... Chandra’s images are giving the astronomers a closer-than-ever look at the distinctive geometry of the charged particle winds radiating in X-rays and other wavelengths from the objects, according to Posselt. Pulsar wind nebulae (PWN) are produced when the energetic particles streaming from pulsar ...
Chapter 24
... hundreds can be seen in just this one photograph. Over the years, astronomers have accumulated similar images of many millions of galaxies. We begin our study of these enormous accumulations of matter simply by considering their appearance on the sky. Seen through even a small telescope, images of g ...
... hundreds can be seen in just this one photograph. Over the years, astronomers have accumulated similar images of many millions of galaxies. We begin our study of these enormous accumulations of matter simply by considering their appearance on the sky. Seen through even a small telescope, images of g ...
EROs and submm galaxies: Expectations for FMOS in the
... been resolved into submillimetre galaxies (SMGs) which appear to be dusty vigorous star-forming galaxies. Half the total extragalactic background is in the submm, while SMGs make up more than half the extragalactic submm background >25% of all stars since the Big Bang have formed in SMGs. ...
... been resolved into submillimetre galaxies (SMGs) which appear to be dusty vigorous star-forming galaxies. Half the total extragalactic background is in the submm, while SMGs make up more than half the extragalactic submm background >25% of all stars since the Big Bang have formed in SMGs. ...
Chapter 1 Telescopes 1.1 Lenses
... This is why many more stars are seen using a telescope than using the unaided eye. The greater the diameter of the objective of a telescope, the greater the number of stars that can be seen. Planets and other astronomical objects in the solar system are magnified using a telescope (unlike stars whic ...
... This is why many more stars are seen using a telescope than using the unaided eye. The greater the diameter of the objective of a telescope, the greater the number of stars that can be seen. Planets and other astronomical objects in the solar system are magnified using a telescope (unlike stars whic ...
X-ray emission from supernova shock waves Tanja Kramer Nymark Department of Astronomy
... in fact galaxies like our own, but very far away. If the novae really occured in those galaxies, this implied that they must be extremely bright to be seen from Earth. Lundmark realized that if the computed distance to M31 (the Andromeda galaxy) was correct, the nova which appeared there in 1885 (S ...
... in fact galaxies like our own, but very far away. If the novae really occured in those galaxies, this implied that they must be extremely bright to be seen from Earth. Lundmark realized that if the computed distance to M31 (the Andromeda galaxy) was correct, the nova which appeared there in 1885 (S ...
P1 09 Red Shift - Animated Science
... Satellites fitted with various telescopes orbit the Earth. These telescopes detect different types of electromagnetic radiation. Why are telescopes that detect different types of electromagnetic waves used to observe the Universe? ...
... Satellites fitted with various telescopes orbit the Earth. These telescopes detect different types of electromagnetic radiation. Why are telescopes that detect different types of electromagnetic waves used to observe the Universe? ...
Rest-frame Optical Spectra: A Window into Galaxy Formation at z~2
... • We typically target a small number of Xray and/or IR-selected AGNs on each mask. • Use MOSFIRE spectra to identify additional AGNs. • We will study AGN demographics, distributions of BH accretion rates, methods of AGN detection. • With early sample of AGNs (red X-ray, burgunday IR), we are sta ...
... • We typically target a small number of Xray and/or IR-selected AGNs on each mask. • Use MOSFIRE spectra to identify additional AGNs. • We will study AGN demographics, distributions of BH accretion rates, methods of AGN detection. • With early sample of AGNs (red X-ray, burgunday IR), we are sta ...
Globular Clusters
... which make the existing GCs perhaps just the survivors of a much wider population, partially disrupted and spread out throughout the Galactic halo and far beyond. In this respect, it has been estimated that, within the next ten billion years or so, most of the present Galactic GCs could disappear. O ...
... which make the existing GCs perhaps just the survivors of a much wider population, partially disrupted and spread out throughout the Galactic halo and far beyond. In this respect, it has been estimated that, within the next ten billion years or so, most of the present Galactic GCs could disappear. O ...
Constraining the star formation histories of spiral bulges
... possibility is an initial mass function (IMF) biased towards highmass stars in the early stages of galaxy formation. In this scenario the first few generations of stars generate large quantities of metals (Gibson & Matteucci 1997; Vazdekis et al. 1997). Alternatively, a period of star formation (SF) ...
... possibility is an initial mass function (IMF) biased towards highmass stars in the early stages of galaxy formation. In this scenario the first few generations of stars generate large quantities of metals (Gibson & Matteucci 1997; Vazdekis et al. 1997). Alternatively, a period of star formation (SF) ...
Gamma-ray burst
Gamma-ray bursts (GRBs) are flashes of gamma rays associated with extremely energetic explosions that have been observed in distant galaxies. They are the brightest electromagnetic events known to occur in the universe. Bursts can last from ten milliseconds to several hours. The initial burst is usually followed by a longer-lived ""afterglow"" emitted at longer wavelengths (X-ray, ultraviolet, optical, infrared, microwave and radio).Most observed GRBs are believed to consist of a narrow beam of intense radiation released during a supernova or hypernova as a rapidly rotating, high-mass star collapses to form a neutron star, quark star, or black hole. A subclass of GRBs (the ""short"" bursts) appear to originate from a different process – this may be due to the merger of binary neutron stars. The cause of the precursor burst observed in some of these short events may be due to the development of a resonance between the crust and core of such stars as a result of the massive tidal forces experienced in the seconds leading up to their collision, causing the entire crust of the star to shatter.The sources of most GRBs are billions of light years away from Earth, implying that the explosions are both extremely energetic (a typical burst releases as much energy in a few seconds as the Sun will in its entire 10-billion-year lifetime) and extremely rare (a few per galaxy per million years). All observed GRBs have originated from outside the Milky Way galaxy, although a related class of phenomena, soft gamma repeater flares, are associated with magnetars within the Milky Way. It has been hypothesized that a gamma-ray burst in the Milky Way, pointing directly towards the Earth, could cause a mass extinction event.GRBs were first detected in 1967 by the Vela satellites, a series of satellites designed to detect covert nuclear weapons tests. Hundreds of theoretical models were proposed to explain these bursts in the years following their discovery, such as collisions between comets and neutron stars. Little information was available to verify these models until the 1997 detection of the first X-ray and optical afterglows and direct measurement of their redshifts using optical spectroscopy, and thus their distances and energy outputs. These discoveries, and subsequent studies of the galaxies and supernovae associated with the bursts, clarified the distance and luminosity of GRBs. These facts definitively placed them in distant galaxies and also connected long GRBs with the explosion of massive stars, the only possible source for the energy outputs observed.