Abstract: - Laboratory for Atmospheric and Space Physics
... expected for a near-equatorial interchange flux tube, in that the field interior to the event is larger ...
... expected for a near-equatorial interchange flux tube, in that the field interior to the event is larger ...
and other gamma-ray telescopes
... LAT: 20 MeV – >300 GeV (LAT was originally called GLAST by itself) LAT field of view ~2.5 sr GLAST Burst Monitor GBM: 10 keV – 25 MeV GBM field of view ~9 sr Launch: This Winter Lifetime: 5 years minimum, 10 years goal ...
... LAT: 20 MeV – >300 GeV (LAT was originally called GLAST by itself) LAT field of view ~2.5 sr GLAST Burst Monitor GBM: 10 keV – 25 MeV GBM field of view ~9 sr Launch: This Winter Lifetime: 5 years minimum, 10 years goal ...
Wide-field and High-resolution Integral
... which are then sent in slightly different directions; Usually three mirror arrays to form a pseudo long slit: slicer array (tilted spherical mirrors forming pupil images of each slicer) + pupil array (or capture mirrors, recombines the separate beams into the desired linear image) + field array (f ...
... which are then sent in slightly different directions; Usually three mirror arrays to form a pseudo long slit: slicer array (tilted spherical mirrors forming pupil images of each slicer) + pupil array (or capture mirrors, recombines the separate beams into the desired linear image) + field array (f ...
Universitat Autònoma de Barcelona Observing the VHE Gamma Ray Sky
... indicate particles coming from the cosmos. Later experiments showed that cosmic rays could initiate showers of secondary charged particles, both in cloud chambers and in the atmosphere: in 1938 Pierre Auger using a number of separated detectors discovered (Auger et al., 1938) that some of these air ...
... indicate particles coming from the cosmos. Later experiments showed that cosmic rays could initiate showers of secondary charged particles, both in cloud chambers and in the atmosphere: in 1938 Pierre Auger using a number of separated detectors discovered (Auger et al., 1938) that some of these air ...
GammaRay Bursts, the Strongest Explosions in the Universe.
... the Vela satellites, designed to look for flashes of soft γ‐rays (radiation that is harder than X‐rays) which would have been the characteristic signature of a nuclear explosion in space. ...
... the Vela satellites, designed to look for flashes of soft γ‐rays (radiation that is harder than X‐rays) which would have been the characteristic signature of a nuclear explosion in space. ...
Solar-B FPP
... • 2048 x 4096 back illuminated frame transfer CCD, 0.08 arcsecond pixels. T. Berger ...
... • 2048 x 4096 back illuminated frame transfer CCD, 0.08 arcsecond pixels. T. Berger ...
Superconductive bolometers and calorimeters
... of far-infrared astronomy from low-background platforms or satellites [5]. They are easy to operate and exhibit a flat response over a wide range of energy. The mapping of extraterrestrial infrared sources is for example such an application requiring the ultimate in detector sensitivity. The success ...
... of far-infrared astronomy from low-background platforms or satellites [5]. They are easy to operate and exhibit a flat response over a wide range of energy. The mapping of extraterrestrial infrared sources is for example such an application requiring the ultimate in detector sensitivity. The success ...
ertan et al 11cesme
... AXP/SGRs. For the sources with weaker magnetic dipole fields, rin comes out of the light cylinder earlier than it does for the sources with stronger dipole fields. After this point, P remains almost constant because of decreasing efficiency of the disk torque [2]. As seen in Fig. 1, the model source ...
... AXP/SGRs. For the sources with weaker magnetic dipole fields, rin comes out of the light cylinder earlier than it does for the sources with stronger dipole fields. After this point, P remains almost constant because of decreasing efficiency of the disk torque [2]. As seen in Fig. 1, the model source ...
X-ray Binaries
... Abstract This chapter discusses the implications of X-ray binaries on our knowledge of Type Ibc and Type II supernovae. X-ray binaries contain accreting neutron stars and stellar–mass black holes which are the end points of massive star evolution. Studying these remnants thus provides clues to under ...
... Abstract This chapter discusses the implications of X-ray binaries on our knowledge of Type Ibc and Type II supernovae. X-ray binaries contain accreting neutron stars and stellar–mass black holes which are the end points of massive star evolution. Studying these remnants thus provides clues to under ...
Experimental FLIR study Gruber, James Powell Calhoun: The NPS Institutional Archive 1979-06
... the nonfeedback type mirror is limited much more in its ...
... the nonfeedback type mirror is limited much more in its ...
The low-spin black hole in LMC X-3 Please share
... We adopt the reduction and analysis techniques used by Steiner et al. (2010) while considering the full set of RXTE pointed observations over the mission lifetime. To ensure the most consistent analysis, we only use “Standard-2” data collected for the PCU-2 detector, which has the most stable calibr ...
... We adopt the reduction and analysis techniques used by Steiner et al. (2010) while considering the full set of RXTE pointed observations over the mission lifetime. To ensure the most consistent analysis, we only use “Standard-2” data collected for the PCU-2 detector, which has the most stable calibr ...
Constraining the Warm Dark Matter Particle Mass through Ultra
... constraints (for the points below, see discussions in Abazjian et al. 2011, Watson et al. 2012; Schultz et al. 2014 and references therein; Lovell et al. 2015). Lyman-α is a challenging tool, and requires disentangling the effects of pressure support and thermal broadening from those caused by the D ...
... constraints (for the points below, see discussions in Abazjian et al. 2011, Watson et al. 2012; Schultz et al. 2014 and references therein; Lovell et al. 2015). Lyman-α is a challenging tool, and requires disentangling the effects of pressure support and thermal broadening from those caused by the D ...
X-Ray Spectroscopy of Stars
... of million-degree plasma and the ensuing X-rays. X-rays are therefore tracers of stellar mass loss and sensitive diagnostics of stellar-wind physics. In hot star binaries, winds may collide, thus forming very hot plasma in the wind collision region. The X-ray emission and its modulation with orbital ...
... of million-degree plasma and the ensuing X-rays. X-rays are therefore tracers of stellar mass loss and sensitive diagnostics of stellar-wind physics. In hot star binaries, winds may collide, thus forming very hot plasma in the wind collision region. The X-ray emission and its modulation with orbital ...
Bayesian flux reconstruction in one and two bands
... categorized source catalogs. Source categorization is central to many of these goals, and here one can apply a cut that the spectral index exceed a discrimination threshold αd for one population versus another, P(α > αd) > Pd. In developing the population abundance, one now has a PDF of fluxes for e ...
... categorized source catalogs. Source categorization is central to many of these goals, and here one can apply a cut that the spectral index exceed a discrimination threshold αd for one population versus another, P(α > αd) > Pd. In developing the population abundance, one now has a PDF of fluxes for e ...
Lecture 1
... sits on top of a high ‘mesa’ due to system and background ‘temperature’ (ie noise). • We usually want to subtract the mesa and just leave the spectrum. • We could do that by alternating between onand off-source observations, and subtracting the two: – But this needs 4 times as much observing time to ...
... sits on top of a high ‘mesa’ due to system and background ‘temperature’ (ie noise). • We usually want to subtract the mesa and just leave the spectrum. • We could do that by alternating between onand off-source observations, and subtracting the two: – But this needs 4 times as much observing time to ...
Manufacture of mirror glass substrates for the NuSTAR mission
... the alignment and integration process bends the cylindrical mirror segments into the required conical shapes and attaches them to the mirror assemblies under the monitoring of real-time metrology. As such the first step of making these mirror assemblies is the manufacture of cylindrically shaped gla ...
... the alignment and integration process bends the cylindrical mirror segments into the required conical shapes and attaches them to the mirror assemblies under the monitoring of real-time metrology. As such the first step of making these mirror assemblies is the manufacture of cylindrically shaped gla ...
space telescope imaging spectrograph survey of far
... loop systems that support and heat the coronal gas on the Sun and presumably other late-type stars as well. Thus, the ultraviolet coronal forbidden lines should play an important role in ferreting out the mechanisms responsible for depositing energy into the corona, widely sought over the past sever ...
... loop systems that support and heat the coronal gas on the Sun and presumably other late-type stars as well. Thus, the ultraviolet coronal forbidden lines should play an important role in ferreting out the mechanisms responsible for depositing energy into the corona, widely sought over the past sever ...
Poster VLF GRBs - INFN-LNF
... by CCD observations (Brno 60 cm CCD telescope, Filip Hroch) Stars elongated, OT image not elongated – short OT April 27-May 1, 2005 ...
... by CCD observations (Brno 60 cm CCD telescope, Filip Hroch) Stars elongated, OT image not elongated – short OT April 27-May 1, 2005 ...
The role of black holes in galaxy formation and evolution
... on a stellar mass (Mgal) – colour diagram92. The difference between ultraviolet luminosity and red luminosity, quantified by the magnitude difference u 2 r, is a colour indicator; larger values of u 2 r correspond to redder galaxies. The colour bar has been inserted to convey this notion visually an ...
... on a stellar mass (Mgal) – colour diagram92. The difference between ultraviolet luminosity and red luminosity, quantified by the magnitude difference u 2 r, is a colour indicator; larger values of u 2 r correspond to redder galaxies. The colour bar has been inserted to convey this notion visually an ...
Studying explosive phenomena in astrophysics by the example of
... and that regularities were found between different events suggests that this phenomenon is a natural termination of stellar evolution. Another example of prompt energetic process in the universe are gamma-ray bursts, which were discovered few decades after introduction of the concept of supernovae. ...
... and that regularities were found between different events suggests that this phenomenon is a natural termination of stellar evolution. Another example of prompt energetic process in the universe are gamma-ray bursts, which were discovered few decades after introduction of the concept of supernovae. ...
arXiv:1009.3685
... The 4 detector arrays are readout on a 16 columns by 32 rows format using the multi-channel-electronics (MCE)13 developed at the University of British Columbia (UBC). There are 32 rows of detectors but 33 rows of multiplexer channels due to the addition of a “dark” SQUID channel,10 used to remove co ...
... The 4 detector arrays are readout on a 16 columns by 32 rows format using the multi-channel-electronics (MCE)13 developed at the University of British Columbia (UBC). There are 32 rows of detectors but 33 rows of multiplexer channels due to the addition of a “dark” SQUID channel,10 used to remove co ...
Gamma Ray Burst Afterglows and Host Galaxies
... Effects of Gamma Ray Bursts on their Environments Gamma ray bursts are not nice neighbors. The high energy photons they produce can destroy interstellar dust grains up to 100 pc away, and ionize interstellar gas at similar distances. The ionized gas will fluoresce as it gradually recombines, and ca ...
... Effects of Gamma Ray Bursts on their Environments Gamma ray bursts are not nice neighbors. The high energy photons they produce can destroy interstellar dust grains up to 100 pc away, and ionize interstellar gas at similar distances. The ionized gas will fluoresce as it gradually recombines, and ca ...
G060291-00 - DCC
... • LSC and Virgo have almost concluded negotiations on joint operations and data analysis. • This collaboration will be open to other interferometers at the appropriate sensitivity levels. We will also carry out joint searches with the network of resonant detectors. ...
... • LSC and Virgo have almost concluded negotiations on joint operations and data analysis. • This collaboration will be open to other interferometers at the appropriate sensitivity levels. We will also carry out joint searches with the network of resonant detectors. ...
Astronomy 305/Frontiers in Astronomy - Fermi Gamma
... Unknown magnetic field No repeatable periods seen in bursts No orbital periods seen – not in binaries Thousands of bursts seen to date – no repetitions from same location ...
... Unknown magnetic field No repeatable periods seen in bursts No orbital periods seen – not in binaries Thousands of bursts seen to date – no repetitions from same location ...
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.