Deep Chandra Observations of the Arches and Quintuplet Clusters at... Hui Dong Q. Daniel Wang ( &
... bright point-like sources that are clearly associated with the clusters. Some of the sources are positionally coincident with known radio sources with strong stellar winds. The sources have similar X-ray spectra, which are dominantly thermal and show an unusually strong 6.7 keV emission line, indica ...
... bright point-like sources that are clearly associated with the clusters. Some of the sources are positionally coincident with known radio sources with strong stellar winds. The sources have similar X-ray spectra, which are dominantly thermal and show an unusually strong 6.7 keV emission line, indica ...
7 November 2012 X-ray Astrophysics
... This principle can be extended to stars, many of which have surfaces at tens of thousands of degrees in temperature and so radiate most strongly in the visible waveband. But not all stars are the same temperature or colour: whilst blue stars are at 15,000-80,000 K, yellower stars like our Sun are at ...
... This principle can be extended to stars, many of which have surfaces at tens of thousands of degrees in temperature and so radiate most strongly in the visible waveband. But not all stars are the same temperature or colour: whilst blue stars are at 15,000-80,000 K, yellower stars like our Sun are at ...
Activity 6 The Electromagnetic Spectrum and Your Community
... primary goals of the HETE mission are the multi-wavelength observation of gamma-ray bursts and the prompt distribution of precise GRB coordinates to the astronomical community for immediate follow-up observations. The HETE science payload consists of one gamma-ray and two x-ray detectors. ...
... primary goals of the HETE mission are the multi-wavelength observation of gamma-ray bursts and the prompt distribution of precise GRB coordinates to the astronomical community for immediate follow-up observations. The HETE science payload consists of one gamma-ray and two x-ray detectors. ...
DTU 8e Chap 17 Quasars and Other Active Galaxies
... Radio galaxy NGC 5128 is 11 million light-years from Earth. At visible wavelengths, a dust lane crosses the face of the galaxy. Superimposed on this visible image is a false-color radio image (green) showing that vast quantities of radio radiation pour from matter ejected from the galaxy perpendicul ...
... Radio galaxy NGC 5128 is 11 million light-years from Earth. At visible wavelengths, a dust lane crosses the face of the galaxy. Superimposed on this visible image is a false-color radio image (green) showing that vast quantities of radio radiation pour from matter ejected from the galaxy perpendicul ...
404.06 Stephen Drake
... You can use `all-sky monitor’ X-ray observations, e.g., Swift BAT, MAXI, etc., => given present sensitivity levels ~10-9 erg cm-2 s-1, only the largest flares will be found: e.g., Swift detections of stellar flares from the active binary systems Algol, II Peg & HR 1099 and the M4.5V star EV Lac an ...
... You can use `all-sky monitor’ X-ray observations, e.g., Swift BAT, MAXI, etc., => given present sensitivity levels ~10-9 erg cm-2 s-1, only the largest flares will be found: e.g., Swift detections of stellar flares from the active binary systems Algol, II Peg & HR 1099 and the M4.5V star EV Lac an ...
Document
... For example, looking for new M7-like NSs one can occasionaly find accretors which are expected to be more abundant than coolers (in the framework of an optimistic scenario) at fluxes <10-13 erg/cm2/s. Recently, Pires and Motch (0710.5192) reported results of a search for INSs in the 2XMMp catalogue. ...
... For example, looking for new M7-like NSs one can occasionaly find accretors which are expected to be more abundant than coolers (in the framework of an optimistic scenario) at fluxes <10-13 erg/cm2/s. Recently, Pires and Motch (0710.5192) reported results of a search for INSs in the 2XMMp catalogue. ...
The phenomena of the satellites of the giant planets
... surface, if there is an atmosphere or not. A planet as Jupiter has a strong limb-centre effect due to its atmosphere: the object seems to be spherical. Contrarily, the Moon has a very small limb-centre effect: its seems to be flat. If this effect remains symmetrical it may not affect the position of ...
... surface, if there is an atmosphere or not. A planet as Jupiter has a strong limb-centre effect due to its atmosphere: the object seems to be spherical. Contrarily, the Moon has a very small limb-centre effect: its seems to be flat. If this effect remains symmetrical it may not affect the position of ...
IMCCE - Observer pages
... surface, if there is an atmosphere or not. A planet as Jupiter has a strong limb-centre effect due to its atmosphere: the object seems to be spherical. Contrarily, the Moon has a very small limb-centre effect: its seems to be flat. If this effect remains symmetrical it may not affect the position of ...
... surface, if there is an atmosphere or not. A planet as Jupiter has a strong limb-centre effect due to its atmosphere: the object seems to be spherical. Contrarily, the Moon has a very small limb-centre effect: its seems to be flat. If this effect remains symmetrical it may not affect the position of ...
Full Poster - Cool Cosmos
... X-rays and Gamma Rays: Since high-energy radiation like X-rays and gamma rays are absorbed by our atmosphere, observatories must be sent into space to study the Universe at these wavelengths. X-rays and gamma rays are produced by matter which is heated to millions of degrees and are often caused by ...
... X-rays and Gamma Rays: Since high-energy radiation like X-rays and gamma rays are absorbed by our atmosphere, observatories must be sent into space to study the Universe at these wavelengths. X-rays and gamma rays are produced by matter which is heated to millions of degrees and are often caused by ...
VLBI of Pulsars with VSOP-2
... Structure of Pulsar Emission Region Scattering of radio waves in the interstellar plasma acts as a large, but very corrupt, lens. This lens has a nominal resolution of about l/D~100’s of km, for some pulsars. Pulsar VLBI allows measurement of the size of the emission region, if it is about this size ...
... Structure of Pulsar Emission Region Scattering of radio waves in the interstellar plasma acts as a large, but very corrupt, lens. This lens has a nominal resolution of about l/D~100’s of km, for some pulsars. Pulsar VLBI allows measurement of the size of the emission region, if it is about this size ...
Our Local Group of Galaxies
... generally elliptical in shape, with the surface brightness largest in the centre decreasing uniformly outwards. With a couple of exceptions, they are found near the large galaxies of the Local Group. • For example, the Milky Way has at least 20 dE/dSph companions while M31 most likely has a similar ...
... generally elliptical in shape, with the surface brightness largest in the centre decreasing uniformly outwards. With a couple of exceptions, they are found near the large galaxies of the Local Group. • For example, the Milky Way has at least 20 dE/dSph companions while M31 most likely has a similar ...
1Cmoles.pdf
... determination are correspondingly rough. At the other extreme in spectral resolution, spectroscopic surveys cannot go as deep as the photometric surveys, reaching only I ≈ 24 with the use of large telescopes. The covered fields are necessarily small and cannot cope with the complex variety of object ...
... determination are correspondingly rough. At the other extreme in spectral resolution, spectroscopic surveys cannot go as deep as the photometric surveys, reaching only I ≈ 24 with the use of large telescopes. The covered fields are necessarily small and cannot cope with the complex variety of object ...
The ultra-luminous x-ray sources near center of M82
... Ultra-Luminous X-ray Sources (ULXs) off-nuclear X-ray sources (not at the center) with isotropic luminosities much higher than the Eddington limit for a solar mass black hole (Lx ~ 1.381038 erg/s) Typical X-ray luminosities of ULXs are in between 1039 erg/s and 1041 erg/s (AGN > 1041 erg/s) ...
... Ultra-Luminous X-ray Sources (ULXs) off-nuclear X-ray sources (not at the center) with isotropic luminosities much higher than the Eddington limit for a solar mass black hole (Lx ~ 1.381038 erg/s) Typical X-ray luminosities of ULXs are in between 1039 erg/s and 1041 erg/s (AGN > 1041 erg/s) ...
Quasars
... this was a very distant object that was masquerading as a star, a quasi-stellar object. • They were first measured to be very small in angular size, but have immense power output. • It is now known that they are actually very ...
... this was a very distant object that was masquerading as a star, a quasi-stellar object. • They were first measured to be very small in angular size, but have immense power output. • It is now known that they are actually very ...
San Pedro Mártir observations of microvariability in obscured quasars
... variations as computed using the approach by Heidt & Wagner (1996) are comparable to the other quantitative measurements of microvariability (Romero et al. 1999). It is highly unlikely that our measurements are affected by systematics because possible effects would also affect the comparison stars, ...
... variations as computed using the approach by Heidt & Wagner (1996) are comparable to the other quantitative measurements of microvariability (Romero et al. 1999). It is highly unlikely that our measurements are affected by systematics because possible effects would also affect the comparison stars, ...
ppt
... For example, looking for new M7-like NSs one can occasionaly find accretors which are expected to be more abundant than coolers (in the framework of an optimistic scenario) at fluxes <10-13 erg/cm2/s. Recently, Pires and Motch (0710.5192) reported results of a search for INSs in the 2XMMp catalogue. ...
... For example, looking for new M7-like NSs one can occasionaly find accretors which are expected to be more abundant than coolers (in the framework of an optimistic scenario) at fluxes <10-13 erg/cm2/s. Recently, Pires and Motch (0710.5192) reported results of a search for INSs in the 2XMMp catalogue. ...
Observational properties of stars
... light. And there was hydrogen in the spectrum, which indicated this to be a type II SN, actually a type IIP. The spectrum of SN1987A also showed relatively high amounts of helium, which indicate that it lost quite a bit of its hydrogen atmosphere before the supernova event. The temperature of the SN ...
... light. And there was hydrogen in the spectrum, which indicated this to be a type II SN, actually a type IIP. The spectrum of SN1987A also showed relatively high amounts of helium, which indicate that it lost quite a bit of its hydrogen atmosphere before the supernova event. The temperature of the SN ...
File
... infrared waves (heat), ultraviolet waves, X-ray waves, and gamma ray waves. The diagram to the right shows the entire spectrum of electromagnetic radiation. Notice that light waves (which can be seen with optical telescopes) occupy only a small portion of the spectrum. But celestial objects such as ...
... infrared waves (heat), ultraviolet waves, X-ray waves, and gamma ray waves. The diagram to the right shows the entire spectrum of electromagnetic radiation. Notice that light waves (which can be seen with optical telescopes) occupy only a small portion of the spectrum. But celestial objects such as ...
Chapter 27 Quasars, Active Galaxies, and Gamma
... from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like stars. ...
... from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like stars. ...
Danish ßrsted Mission In-Orbit Experiences and Status of The
... SAC-C Magnetic Mapping Payload (Ørsted-2) . . . The Ørsted-2 payload will be a direct heritage from the Ørsted mission. Hence, the science objectives for Ørsted-2 are similar to Ørsted, where the mapping of the magnetic field is the primary objective. Secondary science objectives, seen from the Dani ...
... SAC-C Magnetic Mapping Payload (Ørsted-2) . . . The Ørsted-2 payload will be a direct heritage from the Ørsted mission. Hence, the science objectives for Ørsted-2 are similar to Ørsted, where the mapping of the magnetic field is the primary objective. Secondary science objectives, seen from the Dani ...
Solar radioastronomy with the LOFAR (LOw Frequency ARray) radio
... upon early star formation epochs. The most efficient method to date for finding very high redshift radio galaxies uses the correlation between radio spectrum steepness and redshift. At their rest frequency synchrotron losses generate a nonthermal continuum spectrum which steepens above 1 GHz. For di ...
... upon early star formation epochs. The most efficient method to date for finding very high redshift radio galaxies uses the correlation between radio spectrum steepness and redshift. At their rest frequency synchrotron losses generate a nonthermal continuum spectrum which steepens above 1 GHz. For di ...
Spectroscopic confirmation of a galaxy at redshift z=8.6
... constraints on the timing, location and nature of the sources responsible for reionization. Here we report the detection of Lya photons emitted less than 600 million years after the Big Bang. UDFy-38135539 (ref. 5) is at a redshift of z 5 8.5549 6 0.0002, which is greater than those of the previousl ...
... constraints on the timing, location and nature of the sources responsible for reionization. Here we report the detection of Lya photons emitted less than 600 million years after the Big Bang. UDFy-38135539 (ref. 5) is at a redshift of z 5 8.5549 6 0.0002, which is greater than those of the previousl ...
Smallest Kuiper Belt Object Ever Detected
... In fact, the smallest KBO previously seen in reflected light by any telescope is roughly 30 miles across, or 60 times larger. This small KBO represents a missing link between micron-sized dust particles and larger KBOs in the Pluto-size class of 1,000 km. Researchers have long suspected that these b ...
... In fact, the smallest KBO previously seen in reflected light by any telescope is roughly 30 miles across, or 60 times larger. This small KBO represents a missing link between micron-sized dust particles and larger KBOs in the Pluto-size class of 1,000 km. Researchers have long suspected that these b ...
THE DAWN OF X-RAY ASTRONOMY
... outside the absorbing layers of the Earth’s atmosphere has made possible the observation of celestial objects in the x-ray range of wavelength. X-rays of energy greater than several hundreds of electron volts can penetrate the interstellar gas over distances comparable to the size of our own galaxy, ...
... outside the absorbing layers of the Earth’s atmosphere has made possible the observation of celestial objects in the x-ray range of wavelength. X-rays of energy greater than several hundreds of electron volts can penetrate the interstellar gas over distances comparable to the size of our own galaxy, ...
Sample pages 2 PDF
... the vernal equinox; both of them are defined at epoch J2000.0. The ICRS is defined using extra galactic objects, the quasars, that can be considered fixed within some micro arc seconds per year. The technique of Very Long Baseline Interferometry (VLBI) in the radio domain (Chap. 12) allows to estima ...
... the vernal equinox; both of them are defined at epoch J2000.0. The ICRS is defined using extra galactic objects, the quasars, that can be considered fixed within some micro arc seconds per year. The technique of Very Long Baseline Interferometry (VLBI) in the radio domain (Chap. 12) allows to estima ...