Low-Res Version - Chandra X
... known in our galaxy, radiating energy at a rate 5 million times that of our sun. Its mass has been estimated at 120 times the mass of our sun, making it a candidate for the most massive known star in our galaxy. The Chandra observation shows three distinct structures: an outer, horseshoe-shaped ring ...
... known in our galaxy, radiating energy at a rate 5 million times that of our sun. Its mass has been estimated at 120 times the mass of our sun, making it a candidate for the most massive known star in our galaxy. The Chandra observation shows three distinct structures: an outer, horseshoe-shaped ring ...
The presence of gamma rays in space was known before they were
... Gamma rays were first discovered in 1900 by Villiard, although they become known as gamma rays due to Rutherford. It was not until 1948 when Freeberg and Primakoff theorised that gamma rays are produced in space. The first actual gamma rays detected from space were detected by sensors mounted on a h ...
... Gamma rays were first discovered in 1900 by Villiard, although they become known as gamma rays due to Rutherford. It was not until 1948 when Freeberg and Primakoff theorised that gamma rays are produced in space. The first actual gamma rays detected from space were detected by sensors mounted on a h ...
Abstracts
... field) structure and Faraday rotation distributions of these objects, as well as their time variability. ...
... field) structure and Faraday rotation distributions of these objects, as well as their time variability. ...
Barger - Chandra X-Ray Observatory (CXC)
... • Deep MIR and radio images are an obvious avenue for searching for highly-obscured AGNs, since extinction in the MIR & radio is small • People have tried to use combined MIR & radio selections, but to obtain a reliable upper limit on the possible population of X-ray undetected, obscured AGNs, a cle ...
... • Deep MIR and radio images are an obvious avenue for searching for highly-obscured AGNs, since extinction in the MIR & radio is small • People have tried to use combined MIR & radio selections, but to obtain a reliable upper limit on the possible population of X-ray undetected, obscured AGNs, a cle ...
Aryabhatta Research Institute of Observational Sciences
... a minor planet, near-IR and Fabry-Perot spectroscopic observations, optical data of a GRB afterglow and micro-lensing event have been taken at the Institute. • The Institute actively participated in the discovery of rings around Neptune, Uranus and two additional rings around Saturn. • The Institute ...
... a minor planet, near-IR and Fabry-Perot spectroscopic observations, optical data of a GRB afterglow and micro-lensing event have been taken at the Institute. • The Institute actively participated in the discovery of rings around Neptune, Uranus and two additional rings around Saturn. • The Institute ...
Copyright © 2010 Pearson Education, Inc. Chapter 13 Neutron Stars
... bursts have been observed shows no “clumping” of bursts anywhere, particularly not within the Milky Way. Therefore, the bursts must originate from outside our Galaxy. ...
... bursts have been observed shows no “clumping” of bursts anywhere, particularly not within the Milky Way. Therefore, the bursts must originate from outside our Galaxy. ...
X-ray spectrometer
... * The duration and cadence of monitoring will become more clear once GLAST is in orbit * Sensitivity: for the brightest GLAST blazars, average 10-80 keV flux is ~ 10-11 erg cm-2 s-1 -> we should get about 0.1 NuSTAR count/s -> Dflux ~ 7% , Da~0.1 in a NuSTAR orbit * Probably will do “continuous look ...
... * The duration and cadence of monitoring will become more clear once GLAST is in orbit * Sensitivity: for the brightest GLAST blazars, average 10-80 keV flux is ~ 10-11 erg cm-2 s-1 -> we should get about 0.1 NuSTAR count/s -> Dflux ~ 7% , Da~0.1 in a NuSTAR orbit * Probably will do “continuous look ...
ALMA_BoJun605_Gruppioni
... Detecting normal galaxies at z=3 • Total CO luminosity of Milky Way: L’co(1-0) = 3.7x108 K km s-1pc2 (Solomon & Rivolo 1989). • COBE found slightly higher luminosities in higher transitions (Bennett et al 1994) → adopt L’co = 5x108 K km s-1pc2. • At z=3 → observe (3-2) or (4-3) transition in the 84 ...
... Detecting normal galaxies at z=3 • Total CO luminosity of Milky Way: L’co(1-0) = 3.7x108 K km s-1pc2 (Solomon & Rivolo 1989). • COBE found slightly higher luminosities in higher transitions (Bennett et al 1994) → adopt L’co = 5x108 K km s-1pc2. • At z=3 → observe (3-2) or (4-3) transition in the 84 ...
POISE AND EVOLUTION OF THE GALAXY : STRUCTURE ,
... the whole, within the last 2000 years. The reason is clear : this is just an instant phenomenon, with absolutely no warning before, and as soon disappearing with only quite ephemeral fossil remnants testifying. There is however, nowadays, a current opinion that SUPERNOVAE should actually be many tim ...
... the whole, within the last 2000 years. The reason is clear : this is just an instant phenomenon, with absolutely no warning before, and as soon disappearing with only quite ephemeral fossil remnants testifying. There is however, nowadays, a current opinion that SUPERNOVAE should actually be many tim ...
Strongly Interacting Supernovae - The National Centre for Radio
... Shock Formation in Supernovae: Blast wave shock : Ejecta expansion speed is much higher than sound speed. Shocked Circumstellar Medium: Interaction of blast wave with CSM . CSM is accelerated, compressed, heated and shocked. Reverse Shock Formation: Due to deceleration of shocked ejecta around cont ...
... Shock Formation in Supernovae: Blast wave shock : Ejecta expansion speed is much higher than sound speed. Shocked Circumstellar Medium: Interaction of blast wave with CSM . CSM is accelerated, compressed, heated and shocked. Reverse Shock Formation: Due to deceleration of shocked ejecta around cont ...
color-stellar mass diagram
... more recent studies based on 39,000 galaxies from surveys DEEP2 and COMBO-17 (Faber et al 2007) have provided evidence also for evolution of the LF of red galaxies, with a decrease of MB* and an increase of φ* (parameters of the Schechter LF) ...
... more recent studies based on 39,000 galaxies from surveys DEEP2 and COMBO-17 (Faber et al 2007) have provided evidence also for evolution of the LF of red galaxies, with a decrease of MB* and an increase of φ* (parameters of the Schechter LF) ...
The population of young stars in Orion A: X-rays and... Ignazio Pillitteri , S. J. Wolk , L. Allen
... Through Spitzer and XMM-Newton we identify ∼ 702 PMS stars that emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean ...
... Through Spitzer and XMM-Newton we identify ∼ 702 PMS stars that emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean ...
AST1001.ch13
... something that falls in. It increases the hole’s mass, changes its spin or charge, but otherwise loses its identity. ...
... something that falls in. It increases the hole’s mass, changes its spin or charge, but otherwise loses its identity. ...
On the composition of GRBs` Collapsar jets
... ≤95 per cent (2σ ).5 The best-fitting plateaus extend from 5 to 25 s in the BATSE data (7.19/4 χ 2 /DOF), from 2.5 to 17 s in the FermiGBM data (10/5 χ 2 /DOF) and from 1 to 20 s in the Swift data (15.85/9 χ 2 /DOF). We account for three free parameters in our fit: the height of the plateau and the ...
... ≤95 per cent (2σ ).5 The best-fitting plateaus extend from 5 to 25 s in the BATSE data (7.19/4 χ 2 /DOF), from 2.5 to 17 s in the FermiGBM data (10/5 χ 2 /DOF) and from 1 to 20 s in the Swift data (15.85/9 χ 2 /DOF). We account for three free parameters in our fit: the height of the plateau and the ...
Galaxies - Stockton University
... – Material coming into the black-hole is hot and ionized. Photons radiated by the black-hole interact mostly with electrons and exert an outward force on them. The electrons are electrostatically coupled to protons which are gravitationally attracted to the black-hole. ...
... – Material coming into the black-hole is hot and ionized. Photons radiated by the black-hole interact mostly with electrons and exert an outward force on them. The electrons are electrostatically coupled to protons which are gravitationally attracted to the black-hole. ...
Lecture 2: ppt, 5 MB
... way to the moon! Chandra can observe X-rays from clouds of gas so vast that it takes light five million years to go from one side to the other! During maneuvers from one target to the next, Chandra slews more slowly than the minute hand on a clock. At 45 feet long, Chandra is the largest satel ...
... way to the moon! Chandra can observe X-rays from clouds of gas so vast that it takes light five million years to go from one side to the other! During maneuvers from one target to the next, Chandra slews more slowly than the minute hand on a clock. At 45 feet long, Chandra is the largest satel ...
Exploration of the Kuiper Belt by High-Precision Photometric
... diffraction shadow and the velocity of the occulter in the sky plane. With the assumption of a circular orbit around the Sun, the velocity of the object in the sky plane depends on !, the angle between the occulter and the antisolar direction. In our observations, ! ¼ 36 , 7 , and 35 for fields 1 ...
... diffraction shadow and the velocity of the occulter in the sky plane. With the assumption of a circular orbit around the Sun, the velocity of the object in the sky plane depends on !, the angle between the occulter and the antisolar direction. In our observations, ! ¼ 36 , 7 , and 35 for fields 1 ...
Article “What Astronomers Do” (appendix C) one per student
... disregarded as gaps between colors). Though lacking the necessary theoretical knowledge to account for these lines, he catalogued about 600 of them [Freedman, Kaufmann, 2002], introducing in the process an alphabetical classification system that is still sometimes used. Later, Fraunhofer made pione ...
... disregarded as gaps between colors). Though lacking the necessary theoretical knowledge to account for these lines, he catalogued about 600 of them [Freedman, Kaufmann, 2002], introducing in the process an alphabetical classification system that is still sometimes used. Later, Fraunhofer made pione ...
Some Examples of Virtual Observatory Enabled Science What Are the Some Distinguishing
... Radio Galaxies: Typical Examples Radio overlayed on optical images ...
... Radio Galaxies: Typical Examples Radio overlayed on optical images ...
Planetplanet scattering alone cannot explain the freefloating planet
... the compact object due to its strong gravity. Bosch-Ramon et al. (2007) analysed the XMM–Newton data of LS 5039 during the periastron and apastron passages to study the effect of stellar wind on the X-ray absorption properties in this source. The spectral fitting of the data gave a value of equivale ...
... the compact object due to its strong gravity. Bosch-Ramon et al. (2007) analysed the XMM–Newton data of LS 5039 during the periastron and apastron passages to study the effect of stellar wind on the X-ray absorption properties in this source. The spectral fitting of the data gave a value of equivale ...
Document
... Legacy Survey optical catalog. • Rule out sources with optical hosts with the colors and morphology of a star or quasar. • Follow up galaxy hosts that do not have an hard X-ray detection with optical spectroscopy to look for signs of an AGN. • Trigger Chandra TOO X-ray observations of our best candi ...
... Legacy Survey optical catalog. • Rule out sources with optical hosts with the colors and morphology of a star or quasar. • Follow up galaxy hosts that do not have an hard X-ray detection with optical spectroscopy to look for signs of an AGN. • Trigger Chandra TOO X-ray observations of our best candi ...
The High Resolution Camera CXC Newsletter
... for all of them. We classified sources as highly variable or outbursting (with subclasses short vs. long outbursts and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supe ...
... for all of them. We classified sources as highly variable or outbursting (with subclasses short vs. long outbursts and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supe ...
Projet d`observation
... But … • The photo – (and highly) – ionized absorber approach has only been tested at 0.5 – 10 keV energy band (XMM-Newton EPIC detector) so far. ...
... But … • The photo – (and highly) – ionized absorber approach has only been tested at 0.5 – 10 keV energy band (XMM-Newton EPIC detector) so far. ...
EXPLORATION OF THE KUIPER BELT BY HIGH
... diffraction shadow and the velocity of the occulter in the sky plane. With the assumption of a circular orbit around the Sun, the velocity of the object in the sky plane depends on !, the angle between the occulter and the antisolar direction. In our observations, ! ¼ 36 , 7 , and 35 for fields 1 ...
... diffraction shadow and the velocity of the occulter in the sky plane. With the assumption of a circular orbit around the Sun, the velocity of the object in the sky plane depends on !, the angle between the occulter and the antisolar direction. In our observations, ! ¼ 36 , 7 , and 35 for fields 1 ...