2. The X-ray-Radio correlation for bulgeless galaxies
... The study of integrated light measurements in both the X-ray and Radio bands in galaxies allows for the identification of populations of new stars – and therefore, star formation processes – as well as markers for the presence of Active Galactic Nuclei. Correlations between the X-ray and Radio emiss ...
... The study of integrated light measurements in both the X-ray and Radio bands in galaxies allows for the identification of populations of new stars – and therefore, star formation processes – as well as markers for the presence of Active Galactic Nuclei. Correlations between the X-ray and Radio emiss ...
UvA-DARE (Digital Academic Repository) Multi
... just a fraction of a second to a few seconds, than our own Sun will over its entire lifetime. This energy is generated by super hot plasma travelling at relativistic speeds. The plasma is ejected from near the horizon of a newly created black hole in the form of a narrow jet pointing straight toward ...
... just a fraction of a second to a few seconds, than our own Sun will over its entire lifetime. This energy is generated by super hot plasma travelling at relativistic speeds. The plasma is ejected from near the horizon of a newly created black hole in the form of a narrow jet pointing straight toward ...
Observations of Jets and Outflows from Young Stars
... simple, analytical model, which can estimate the expected X-ray luminosity of an HH flow. The detected X-ray-bright HH objects have plasma temperatures in the range TX = 106 to 107 K. The X-ray spectrum is dominated by soft photons with energies below 1 keV. The soft-portion of the X-ray spectra are ...
... simple, analytical model, which can estimate the expected X-ray luminosity of an HH flow. The detected X-ray-bright HH objects have plasma temperatures in the range TX = 106 to 107 K. The X-ray spectrum is dominated by soft photons with energies below 1 keV. The soft-portion of the X-ray spectra are ...
PDF hosted at the Radboud Repository of the Radboud University
... Despite the importance of type Ia supernovae for stellar astrophysics, galactic evolution and cosmology, the nature of the progenitor systems giving rise to these events remains mysterious, and no direct, unambiguous detection of a type Ia supernova progenitor has been made at the time of the writin ...
... Despite the importance of type Ia supernovae for stellar astrophysics, galactic evolution and cosmology, the nature of the progenitor systems giving rise to these events remains mysterious, and no direct, unambiguous detection of a type Ia supernova progenitor has been made at the time of the writin ...
PowerPoint - Herschel Space Observatory
... • A black body is a perfect emitter and absorber of radiation – It emits and absorbs radiation with a particular “spectrum” – The shape of the spectrum is always the same, but the peak wavelength changes with temperature. – But not all objects are black bodies. – Atoms, molecules and electrons emit ...
... • A black body is a perfect emitter and absorber of radiation – It emits and absorbs radiation with a particular “spectrum” – The shape of the spectrum is always the same, but the peak wavelength changes with temperature. – But not all objects are black bodies. – Atoms, molecules and electrons emit ...
INFRARED DUST BUBBLES: PROBING THE DETAILED
... zone where temperature sharply decreases and density rapidly increases (with radius); and a thin, dense shell of shocked H+ gas surrounded by a very thin shell of nonshocked H+ gas at about 104 K. The outer thin shell of 104 K H+ gas is the region classically thought to represent the photoionized H ...
... zone where temperature sharply decreases and density rapidly increases (with radius); and a thin, dense shell of shocked H+ gas surrounded by a very thin shell of nonshocked H+ gas at about 104 K. The outer thin shell of 104 K H+ gas is the region classically thought to represent the photoionized H ...
ON THE POLAR CAPS OF THE THREE MUSKETEERS1
... ( Bignami et al. 1983). The discovery of a common 237 ms pulsation clicked the identification, the first ever, of an unidentified -ray source with its X-ray counterpart ( Halpern & Holt 1992; Bertsch et al. 1992). The first good-quality spectral data on Geminga were collected by ROSAT. Halpern & Ru ...
... ( Bignami et al. 1983). The discovery of a common 237 ms pulsation clicked the identification, the first ever, of an unidentified -ray source with its X-ray counterpart ( Halpern & Holt 1992; Bertsch et al. 1992). The first good-quality spectral data on Geminga were collected by ROSAT. Halpern & Ru ...
Accreting millisecond X-ray pulsars: a search for pulsed radio
... > 8 M⊙ ) during a Type II, Type Ib or Type Ic collapse of a massive star (M ∼ supernova event, which occurs when a massive star runs out of nuclear fuel in its core at the end of its life. A typical neutron star has a mass between 1 M⊙ – 2.1 M⊙ , with a corresponding radius range of 8 – 15 km and th ...
... > 8 M⊙ ) during a Type II, Type Ib or Type Ic collapse of a massive star (M ∼ supernova event, which occurs when a massive star runs out of nuclear fuel in its core at the end of its life. A typical neutron star has a mass between 1 M⊙ – 2.1 M⊙ , with a corresponding radius range of 8 – 15 km and th ...
PDF file
... regions of dark nebulosity (Joy, 1945). Stars resembling the original variables first identified as TTS are currently called ”strong emission” or Classical TTS (CTTS). Subsequent spectroscopic studies of the Ca II H and K lines and the first X-ray observations with the Einstein X-ray observatory (Fe ...
... regions of dark nebulosity (Joy, 1945). Stars resembling the original variables first identified as TTS are currently called ”strong emission” or Classical TTS (CTTS). Subsequent spectroscopic studies of the Ca II H and K lines and the first X-ray observations with the Einstein X-ray observatory (Fe ...
Gamma-Ray Pulsars - INTEGRAL
... Table 1 (Kanbach, 2001) gives an overview of the highenergy pulsars and their multi-frequency detections, ranging from the radio band to gamma rays, after the decade of discoveries with the CGRO instruments. Next to the column with the spin period the rank of the quantity Ė/d2 , i.e. the spin-down ...
... Table 1 (Kanbach, 2001) gives an overview of the highenergy pulsars and their multi-frequency detections, ranging from the radio band to gamma rays, after the decade of discoveries with the CGRO instruments. Next to the column with the spin period the rank of the quantity Ė/d2 , i.e. the spin-down ...
Flare Observations
... and blast waves (Moreton, 1964) were noted. Meter wave radio emissions, detected serendipitously in 1942 during military radar operations, revealed the presence of non-thermal electrons in the corona (Hey, 1983). During a radio burst, the total solar luminosity in radio waves may increase by several ...
... and blast waves (Moreton, 1964) were noted. Meter wave radio emissions, detected serendipitously in 1942 during military radar operations, revealed the presence of non-thermal electrons in the corona (Hey, 1983). During a radio burst, the total solar luminosity in radio waves may increase by several ...
OBSERVATIONS OF PHYSICAL PROCESSES IN
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
Non-thermal emission processes in massive binaries*
... within stellar winds is clearly revealed in their spectra by emission lines associated to highly ionized elements such as O, N, Si, Mg, Ne or Fe. Such emission line spectra have been observed by the XMM-Newton and Chandra X-ray observatories (Schulz et al 2000; Kahn et al 2001). Beside these intrins ...
... within stellar winds is clearly revealed in their spectra by emission lines associated to highly ionized elements such as O, N, Si, Mg, Ne or Fe. Such emission line spectra have been observed by the XMM-Newton and Chandra X-ray observatories (Schulz et al 2000; Kahn et al 2001). Beside these intrins ...
Untitled - METU Astrophysics Home Page
... suggestions on these issues. I would like to thank my colleagues at METU Astrophysics Group for useful discussions and for their help at all levels of this tedious work. My deep gratitudes are to M. Miraç Serim for his great help, advice and insights related to data analysis and interpretation. It w ...
... suggestions on these issues. I would like to thank my colleagues at METU Astrophysics Group for useful discussions and for their help at all levels of this tedious work. My deep gratitudes are to M. Miraç Serim for his great help, advice and insights related to data analysis and interpretation. It w ...
Session 1: Stellar winds, diagnostics across the electromagnetic
... rates? J.O. Sundqvist, J. Puls, A. Feldmeier, S.P. Owocki Small-scale inhomogeneities, or "clumping", in the winds of hot, massive stars are conventionally included in spectral analyses by the so-called microclumping technique. To reconcile investigations of different diagnostics using this techniqu ...
... rates? J.O. Sundqvist, J. Puls, A. Feldmeier, S.P. Owocki Small-scale inhomogeneities, or "clumping", in the winds of hot, massive stars are conventionally included in spectral analyses by the so-called microclumping technique. To reconcile investigations of different diagnostics using this techniqu ...
THE LUMINOSITY FUNCTION OF X
... XMM-Newton are not identified. Mainieri et al. (2005) find that the peak of the redshift distribution shifts to higher values (z 1:2Y1:5) when incorporating photometric redshifts for objects too faint for optical spectroscopy. (2) Barger et al. (2005) demonstrate that the XLF can be fitted equally ...
... XMM-Newton are not identified. Mainieri et al. (2005) find that the peak of the redshift distribution shifts to higher values (z 1:2Y1:5) when incorporating photometric redshifts for objects too faint for optical spectroscopy. (2) Barger et al. (2005) demonstrate that the XLF can be fitted equally ...
Particle kinematics in solar flares: observations - ETH E
... In X-rays, the Sun looks completely different from what we are used to by observing it with backyard telescopes. Fig. 1.2 shows the changing face of the Sun observed in visible light, Hα, UV and X-rays. The peak of the solar irradiance is in the optical light, which constitutes mostly of continuum e ...
... In X-rays, the Sun looks completely different from what we are used to by observing it with backyard telescopes. Fig. 1.2 shows the changing face of the Sun observed in visible light, Hα, UV and X-rays. The peak of the solar irradiance is in the optical light, which constitutes mostly of continuum e ...
Slide 1
... a large fraction of gas & stars tidally stripped from the dwarf galaxy during interaction leaving only stars most closely bound to the BH (GC-like) star formation triggered by tidal interactions compatible with eccentric binary scenario presence of dust lanes in ESO243-49 could provide evide ...
... a large fraction of gas & stars tidally stripped from the dwarf galaxy during interaction leaving only stars most closely bound to the BH (GC-like) star formation triggered by tidal interactions compatible with eccentric binary scenario presence of dust lanes in ESO243-49 could provide evide ...
SPECTRAL STATE DEPENDENCE OF THE 0.4–2 MEV
... truncated at a large distance from the accretor (see however Reynolds & Miller 2013, for examples of results contradicting this picture). The X-ray spectrum shows a strong power-law like component extending up to hundreds of keV, usually with a roll-over at typically 50–200 keV. The level of rapid v ...
... truncated at a large distance from the accretor (see however Reynolds & Miller 2013, for examples of results contradicting this picture). The X-ray spectrum shows a strong power-law like component extending up to hundreds of keV, usually with a roll-over at typically 50–200 keV. The level of rapid v ...
The Early-time Optical Properties of Gamma
... Gamma Ray Bursts (GRBs) are brief, intense flashes of high energy gamma rays originating at cosmological distances and often associated with subsequent radiation emitted at longer wavelengths from X-ray to radio waves on times scales of minutes to days after the initial gamma ray burst. In the stand ...
... Gamma Ray Bursts (GRBs) are brief, intense flashes of high energy gamma rays originating at cosmological distances and often associated with subsequent radiation emitted at longer wavelengths from X-ray to radio waves on times scales of minutes to days after the initial gamma ray burst. In the stand ...
Global Properties of Solar Flares
... historical progression, the development of radio astronomy and then UV and X-ray astronomy made coronal observations possible even in front of the solar disk. At these extreme wavelengths the photosphere becomes dark (for the short wavelengths) or elevated in altitude (for radio waves), and flare ef ...
... historical progression, the development of radio astronomy and then UV and X-ray astronomy made coronal observations possible even in front of the solar disk. At these extreme wavelengths the photosphere becomes dark (for the short wavelengths) or elevated in altitude (for radio waves), and flare ef ...
Quasars and Blazars
... For many years, BL Lacs were divided into two categories: radio-selected (RBLs) and X-ray selected (XBLs). The two categories had very different broad-band spectral energy distributions (SEDs): the RBLs peaked4 in the IR to optical part of the spectrum, and were generally brighter at radio frequenci ...
... For many years, BL Lacs were divided into two categories: radio-selected (RBLs) and X-ray selected (XBLs). The two categories had very different broad-band spectral energy distributions (SEDs): the RBLs peaked4 in the IR to optical part of the spectrum, and were generally brighter at radio frequenci ...
X-ray astronomy
X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray observation and detection from astronomical objects. X-radiation is absorbed by the Earth's atmosphere, so instruments to detect X-rays must be taken to high altitude by balloons, sounding rockets, and satellites. X-ray astronomy is the space science related to a type of space telescope that can see farther than standard light-absorption telescopes, such as the Mauna Kea Observatories, via x-ray radiation.X-ray emission is expected from astronomical objects that contain extremely hot gasses at temperatures from about a million kelvin (K) to hundreds of millions of kelvin (MK). Although X-rays have been observed emanating from the Sun since the 1940s, the discovery in 1962 of the first cosmic X-ray source was a surprise. This source is called Scorpius X-1 (Sco X-1), the first X-ray source found in the constellation Scorpius. The X-ray emission of Scorpius X-1 is 10,000 times greater than its visual emission, whereas that of the Sun is about a million times less. In addition, the energy output in X-rays is 100,000 times greater than the total emission of the Sun in all wavelengths. Based on discoveries in this new field of X-ray astronomy, starting with Scorpius X-1, Riccardo Giacconi received the Nobel Prize in Physics in 2002. It is now known that such X-ray sources as Sco X-1 are compact stars, such as neutron stars or black holes. Material falling into a black hole may emit X-rays, but the black hole itself does not. The energy source for the X-ray emission is gravity. Infalling gas and dust is heated by the strong gravitational fields of these and other celestial objects.Many thousands of X-ray sources are known. In addition, the space between galaxies in galaxy clusters is filled with a very hot, but very dilute gas at a temperature between 10 and 100 megakelvins (MK). The total amount of hot gas is five to ten times the total mass in the visible galaxies.