Chandra and NIR Observations of Galactic HII Regions
... detected with Chandra, with LX in the range 5.3´1030 – 1.8x1032 ergs s-1, LX/Lbol in the range 1.4x10-8 – 6.8x10-8, and kT from 0.49–0.96 keV. • The 2-Myr old O stars in NGC 6611 have relatively soft X-ray spectra and low LX/Lbol , like many nearby O stars whose winds are thought to drive instabilit ...
... detected with Chandra, with LX in the range 5.3´1030 – 1.8x1032 ergs s-1, LX/Lbol in the range 1.4x10-8 – 6.8x10-8, and kT from 0.49–0.96 keV. • The 2-Myr old O stars in NGC 6611 have relatively soft X-ray spectra and low LX/Lbol , like many nearby O stars whose winds are thought to drive instabilit ...
Polarimeter - Raman Research Institute
... Fabrication of an engineering model is in final stages. The instrument consists of position sensitive proportional counter detectors and works in the 5-30 keV energy band. This instrument will be suitable for X-ray polarisation measurement in about 50 hard X-ray sources. The accretion powered X-ray ...
... Fabrication of an engineering model is in final stages. The instrument consists of position sensitive proportional counter detectors and works in the 5-30 keV energy band. This instrument will be suitable for X-ray polarisation measurement in about 50 hard X-ray sources. The accretion powered X-ray ...
DoAr21_AAS2005 - Astronomy at Swarthmore College
... One of the few PMS stars that is x-ray bright enough to produce a highquality grating spectrum, DoAr 21 is perhaps the youngest PMS star observed with the Chandra gratings. In terms of its disk properties, it is an intermediate case between the CTTS TW Hya, which has x-ray properties that have been ...
... One of the few PMS stars that is x-ray bright enough to produce a highquality grating spectrum, DoAr 21 is perhaps the youngest PMS star observed with the Chandra gratings. In terms of its disk properties, it is an intermediate case between the CTTS TW Hya, which has x-ray properties that have been ...
X-ray Sources in Nearby Galaxies Q. Daniel Wang University of Massachusetts
... • Feeding of AGNs • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scat ...
... • Feeding of AGNs • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scat ...
Xray_image_chain
... – Count up the number of photons that landed in each grid cell (pixel) during the observation • For a 30,000 (1/3 day) second observation, 10,000 CCD frames are obtained • Hopefully, each grid cell will contain only 1 photon per frame ...
... – Count up the number of photons that landed in each grid cell (pixel) during the observation • For a 30,000 (1/3 day) second observation, 10,000 CCD frames are obtained • Hopefully, each grid cell will contain only 1 photon per frame ...
Hitomi Observation of the Highly Obscured High-Mass X-ray
... of continuum and line components significantly decreased in this ten years while the equivalent widths increased. Unabsorbed luminosity in 2 to 10 keV is 5.8×1035 ergs/s, which is far below the Eddington limit of 1.8×1038 ergs/s for a neutron star of 1.4 M⊙ and hence permits moderate accretion. The ...
... of continuum and line components significantly decreased in this ten years while the equivalent widths increased. Unabsorbed luminosity in 2 to 10 keV is 5.8×1035 ergs/s, which is far below the Eddington limit of 1.8×1038 ergs/s for a neutron star of 1.4 M⊙ and hence permits moderate accretion. The ...
PowerPoint - Chandra X
... solar system is shown in the image. The image is brighter to the upper right -- the side of the nebula nearest the Earth -- where there is less obscuring material to block the X-ray emission. NGC 7027 is the remains of a sun-like star that has ejected much of its mass to expose its hot core. The X-r ...
... solar system is shown in the image. The image is brighter to the upper right -- the side of the nebula nearest the Earth -- where there is less obscuring material to block the X-ray emission. NGC 7027 is the remains of a sun-like star that has ejected much of its mass to expose its hot core. The X-r ...
X-Ray Astronomy Poster_Final
... X-rays are electromagnetic radiation of energy ranging from 0.1keV to a few 100keV. We see many objects in the sky that emit visible light but some objects emit X-rays and some are even more bright in X-rays than in visible light. ...
... X-rays are electromagnetic radiation of energy ranging from 0.1keV to a few 100keV. We see many objects in the sky that emit visible light but some objects emit X-rays and some are even more bright in X-rays than in visible light. ...
poster
... Abstract. DG Tau is a classical T Tauri star showing an unusual X-ray spectrum, best described by two thermal components with different absorption columns. The soft X-rays are less absorbed than the hard X-rays, presumably coronal, component. This rules out stellar accretion as the origin of the sof ...
... Abstract. DG Tau is a classical T Tauri star showing an unusual X-ray spectrum, best described by two thermal components with different absorption columns. The soft X-rays are less absorbed than the hard X-rays, presumably coronal, component. This rules out stellar accretion as the origin of the sof ...
X-ray Binaries and Cygnus X-1
... X-rays. Since the object cycles through the two states, a transition period also exists, which is a combination of both the high/soft and low/hard states. Data is collected by the high energy transmission grating (HETG) on the X-ray satellite Chandra. The HETG is a diffraction grating for high and m ...
... X-rays. Since the object cycles through the two states, a transition period also exists, which is a combination of both the high/soft and low/hard states. Data is collected by the high energy transmission grating (HETG) on the X-ray satellite Chandra. The HETG is a diffraction grating for high and m ...
High Energy Observational Astrophysics
... X-rays from about 12 keV to 120 keV are classified as "hard" X-rays ...
... X-rays from about 12 keV to 120 keV are classified as "hard" X-rays ...
XMM - advanced X-ray Astronomy school - X
... (this is the light from a point source will be spread in (almost) a Gaussian with the above dimensions). Although the spatial resolution in all telescopes is dictated by Airy’s law which says that for a given telescope diameter, the resolution (decreases) gets better with decreasing wavelength. Howe ...
... (this is the light from a point source will be spread in (almost) a Gaussian with the above dimensions). Although the spatial resolution in all telescopes is dictated by Airy’s law which says that for a given telescope diameter, the resolution (decreases) gets better with decreasing wavelength. Howe ...
H. W. Schnopper, Chlorine K Absorption Edge in Single Crystal... ` in R ntgenspektren und Chemische Bindung
... The raw data is divided into N bins, the kth bin containing A(k) events. The total number of events detected is NT = 'A(k) N ...
... The raw data is divided into N bins, the kth bin containing A(k) events. The total number of events detected is NT = 'A(k) N ...
Complex Spatio-Spectral Structure of Diffuse X-Ray
... - Hard X-ray light curve increases with a lower rate of ~20% /yr (f ~ t4). As of 2008-1, f (3-10 keV) = 5.2 x 10-13 erg/cm2/s, Lx = 1.6 x 1035 erg/s. - Cross-comparisons among different X-ray instruments are consistent. - Radio emission shows an evolution of the spectral index: currently S ~ -0.8 ...
... - Hard X-ray light curve increases with a lower rate of ~20% /yr (f ~ t4). As of 2008-1, f (3-10 keV) = 5.2 x 10-13 erg/cm2/s, Lx = 1.6 x 1035 erg/s. - Cross-comparisons among different X-ray instruments are consistent. - Radio emission shows an evolution of the spectral index: currently S ~ -0.8 ...
Variable Sources Summary 4u1822-37:
... energy spectrum seems to introduce an anomalous peak at ~2 keV. Fitting a blackbody model to the higher energy part of the spectrum yields a “good” fit, but with a questionable temperature (144 keV). Difference in flux between high and low state is clear. In this case, no color change indicates that ...
... energy spectrum seems to introduce an anomalous peak at ~2 keV. Fitting a blackbody model to the higher energy part of the spectrum yields a “good” fit, but with a questionable temperature (144 keV). Difference in flux between high and low state is clear. In this case, no color change indicates that ...
Atomic Physics Explaining the Universe
... • Strong iron emission lines, Fe XVII – XXIV • Continuum emission between 1.5-10A • Detection of non-thermal electrons from small flares • Modeling of X-ray Spectra is well developed and allow scientists to compare detailed forward models with state-of-the-art observations. ...
... • Strong iron emission lines, Fe XVII – XXIV • Continuum emission between 1.5-10A • Detection of non-thermal electrons from small flares • Modeling of X-ray Spectra is well developed and allow scientists to compare detailed forward models with state-of-the-art observations. ...
PowerPoint - Chandra X
... X-ray spectra of the wind show that the composition of the material in the wind is roughly similar to that of the Sun’s atmosphere, except for a deficit of oxygen atoms, and that it has a temperature of about 100,000 K. The average gas speed is about 500 km/s. ...
... X-ray spectra of the wind show that the composition of the material in the wind is roughly similar to that of the Sun’s atmosphere, except for a deficit of oxygen atoms, and that it has a temperature of about 100,000 K. The average gas speed is about 500 km/s. ...
The Main Features of the X
... Galactic Bulge: not well understood, but definitely consists of some component beyond the NPS LMC: a nearby dwarf irregular galaxy ...
... Galactic Bulge: not well understood, but definitely consists of some component beyond the NPS LMC: a nearby dwarf irregular galaxy ...
Initial Results from the Chandra Shallow X
... source free fields using archival ACIS-I background data Scale to 126 fields: ...
... source free fields using archival ACIS-I background data Scale to 126 fields: ...
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 ...
X-ray polarimetry in Xenon gas filled detectors
... 2D-MHSP:The images registered with a 2D position-sensitive detector based on the new Micro-Hole & Strip Plate structure further reinforce that evidence and confirm that a photoelectric polarimeter based on Micro Pattern Gas Chambers is a viable option for X-ray polarimetry. ...
... 2D-MHSP:The images registered with a 2D position-sensitive detector based on the new Micro-Hole & Strip Plate structure further reinforce that evidence and confirm that a photoelectric polarimeter based on Micro Pattern Gas Chambers is a viable option for X-ray polarimetry. ...
Presentazione di PowerPoint
... 29 galaxies with good spectra in the CDFS and emission line ratios consistent with starbursts or normal galaxies give the X-ray priors. A Bayesian approach allows us to identify 74 galaxies in the CDFS and 136 in the CDFN (2 Ms) Norman et al. 2004 ...
... 29 galaxies with good spectra in the CDFS and emission line ratios consistent with starbursts or normal galaxies give the X-ray priors. A Bayesian approach allows us to identify 74 galaxies in the CDFS and 136 in the CDFN (2 Ms) Norman et al. 2004 ...
X-ray Astronomy
... Photon knocks out a bound electron, losing all of its energy to the electron ...
... Photon knocks out a bound electron, losing all of its energy to the electron ...
Document
... For improvements to detector systems for solar and night-time UV and EUV (approx. 20-300nm) observing, the following areas are of interest: ...
... For improvements to detector systems for solar and night-time UV and EUV (approx. 20-300nm) observing, the following areas are of interest: ...
X-ray astronomy detector
X-ray astronomy detectors are instruments that detect X-rays for use in the study of X-ray astronomy.X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray emission from celestial 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 part of space science.X-ray astronomy detectors have been designed and configured primarily for energy and occasionally for wavelength detection using a variety of techniques usually limited to the technology of the time.