Infrared identification of high-mass X
... The photometric observations were obtained by repeating a set of images for each filter with nine different 3000 offset positions including the targets, following the standard jitter procedure, which enabled us to cleanly subtract the sky emission in NIR. Each individual frame has an integration tim ...
... The photometric observations were obtained by repeating a set of images for each filter with nine different 3000 offset positions including the targets, following the standard jitter procedure, which enabled us to cleanly subtract the sky emission in NIR. Each individual frame has an integration tim ...
System Level # Requirements Document
... InfraRed Multi-Object Spectrometer (IRMOS): near-diffraction limited, R~2000 – 10000 IFU-based spectrometer operating over a wavelength range 0.8-2.5µm. Will use multiple IFUs and access a 5 arcmin diameter field. It is expected to benefit from developments in multi-object adaptive optics (MOAO). ...
... InfraRed Multi-Object Spectrometer (IRMOS): near-diffraction limited, R~2000 – 10000 IFU-based spectrometer operating over a wavelength range 0.8-2.5µm. Will use multiple IFUs and access a 5 arcmin diameter field. It is expected to benefit from developments in multi-object adaptive optics (MOAO). ...
1 Introduction
... measurement techniques. Each technique provides unique information about the object(s) being measured. Typical values used of parameters such as bandwidth, receiver sensitivity, observed field size and angular resolution are, in practice, dependent on the type of measurement performed. Integration t ...
... measurement techniques. Each technique provides unique information about the object(s) being measured. Typical values used of parameters such as bandwidth, receiver sensitivity, observed field size and angular resolution are, in practice, dependent on the type of measurement performed. Integration t ...
THE CASSINI VISUAL AND INFRARED MAPPING SPECTROMETER
... In 1987 this system measured its first spectral images (Green et al., 1998). Also, in the early 1980’s, an instrument development program for future planetary missions was setup at JPL and headed by Larry Soderblom as principal investigator. This collaboration resulted in several similar instruments ...
... In 1987 this system measured its first spectral images (Green et al., 1998). Also, in the early 1980’s, an instrument development program for future planetary missions was setup at JPL and headed by Larry Soderblom as principal investigator. This collaboration resulted in several similar instruments ...
Fundamentals of radio astronomy - Radio Observations of Active
... • Baseline b measured in wavelengths: the (u,v,w) co-ordinate system – w points along reference direction so – (u,v) point east and north in plane normal to w-axis – (u,v,w) are the components of b/l along these directions • In this co-ordinate system, s = (l,m,n) – l,m,n are direction cosines – n = ...
... • Baseline b measured in wavelengths: the (u,v,w) co-ordinate system – w points along reference direction so – (u,v) point east and north in plane normal to w-axis – (u,v,w) are the components of b/l along these directions • In this co-ordinate system, s = (l,m,n) – l,m,n are direction cosines – n = ...
PDF file
... magnetic reconnection model which can explain these active phenomena, at least morphologically. In Chapter 2 we report a detailed examination of the fine structures inside flare ribbons and the temporal evolution of such structures. We examined systems of conjugate footpoints, inside flare ribbons b ...
... magnetic reconnection model which can explain these active phenomena, at least morphologically. In Chapter 2 we report a detailed examination of the fine structures inside flare ribbons and the temporal evolution of such structures. We examined systems of conjugate footpoints, inside flare ribbons b ...
Astronomy Astrophysics
... of the Wolf-Rayet WR 147 at 10 kpc is shown in Fig. 5 after dereddening with the Draine (1989) law (left) and with the Lutz et al. (1996) law (right). The WR 147 spectrum appears as the closest WR one to the Cygnus X-3 spectrum, with almost the same mean flux density at 10 kpc and the same power law ...
... of the Wolf-Rayet WR 147 at 10 kpc is shown in Fig. 5 after dereddening with the Draine (1989) law (left) and with the Lutz et al. (1996) law (right). The WR 147 spectrum appears as the closest WR one to the Cygnus X-3 spectrum, with almost the same mean flux density at 10 kpc and the same power law ...
Descending from on high: Lyman-series cascades and spin
... generated by the first generation of collapsed objects. These highredshift objects are highly biased, leading to large variations in their number density. This, combined with the 1/r 2 dependence of the flux, causes large fluctuations in the Lyα background, which can be probed through their effect o ...
... generated by the first generation of collapsed objects. These highredshift objects are highly biased, leading to large variations in their number density. This, combined with the 1/r 2 dependence of the flux, causes large fluctuations in the Lyα background, which can be probed through their effect o ...
The optical afterglow and z = 0.92 early
... density limit at & 5 ks of Fν (1 keV) . 2.3 × 10−3 µJy. Ground-based follow-up optical observations of the XRT position were first obtained with the Nordic Optical Telescope (NOT) 20.4 min after the burst and led to the marginal detection of a source with R ≈ 22.5 mag (Xu et al. 2010). Inspection of ...
... density limit at & 5 ks of Fν (1 keV) . 2.3 × 10−3 µJy. Ground-based follow-up optical observations of the XRT position were first obtained with the Nordic Optical Telescope (NOT) 20.4 min after the burst and led to the marginal detection of a source with R ≈ 22.5 mag (Xu et al. 2010). Inspection of ...
Fraction of the X-ray selected AGNs with optical emission lines in
... and only the central region (0.9 deg2 ) is covered by the Chandra observations with a higher spatial resolution (Finoguenov et al. 2007; Brusa et al. 2010). With the XM M − N ewton survey of the COSMOS field, there are 1,848 point-like sources detected, at least one of the soft (0.5-2 keV), hard (2- ...
... and only the central region (0.9 deg2 ) is covered by the Chandra observations with a higher spatial resolution (Finoguenov et al. 2007; Brusa et al. 2010). With the XM M − N ewton survey of the COSMOS field, there are 1,848 point-like sources detected, at least one of the soft (0.5-2 keV), hard (2- ...
2. The X-ray-Radio correlation for bulgeless galaxies
... evolution of massive stars and their destruction, suggesting the possibility of using X-ray emission to determine the star formation rates. This work presents a study on the presence of this correlation in bulgeless galaxies at intermediate redshifts ( 0.4≤z≤1.0 ). To this effect, the VLA and Chandr ...
... evolution of massive stars and their destruction, suggesting the possibility of using X-ray emission to determine the star formation rates. This work presents a study on the presence of this correlation in bulgeless galaxies at intermediate redshifts ( 0.4≤z≤1.0 ). To this effect, the VLA and Chandr ...
Power Point Presentation
... Stars like the Sun go gentle into that good night More massive stars rage, rage against the dying of the light ...
... Stars like the Sun go gentle into that good night More massive stars rage, rage against the dying of the light ...
Identifying Young far from Giant Stars Molecular Clouds
... luminosities and effective temperature, implying a potential evolutionary relationship. The dust and gas within the accretion disk may get pulled in to the star, dissipate out , or clump together to form substellar companions (see A.l). However, the transition from a classical to weak T Tauri star o ...
... luminosities and effective temperature, implying a potential evolutionary relationship. The dust and gas within the accretion disk may get pulled in to the star, dissipate out , or clump together to form substellar companions (see A.l). However, the transition from a classical to weak T Tauri star o ...
Composition-Tunable Properties Of CdSxTe1
... combination of elements as it is largely different from the spectral shapes observed in previously studied CdSxSe1-x and CdSexTe1-x nanocrystals, where distinct absorption features centered near band edge energies were reported. The possibility of inhomogeneous broadening of the CdSxTe1-x absorption ...
... combination of elements as it is largely different from the spectral shapes observed in previously studied CdSxSe1-x and CdSexTe1-x nanocrystals, where distinct absorption features centered near band edge energies were reported. The possibility of inhomogeneous broadening of the CdSxTe1-x absorption ...
Development of pixel detectors with integrated
... Construction and tests of the telescope head FPAG and software programming for JTAG communication Study of efficiency of the proposed hit finding algorithm Laboratory calibrations, ALS test and sensors alignment, tests in the STAR environment ...
... Construction and tests of the telescope head FPAG and software programming for JTAG communication Study of efficiency of the proposed hit finding algorithm Laboratory calibrations, ALS test and sensors alignment, tests in the STAR environment ...
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 ...
The Tools of Astronomy
... Astronomical telescopes are often used to make images of their field of view (simply, the portion of the sky that the telescope “sees”). Figure 5.3 illustrates how that is accomplished, in this case by the mirror in a reflecting telescope. Light from a distant object (here, a comet) reaches us as pa ...
... Astronomical telescopes are often used to make images of their field of view (simply, the portion of the sky that the telescope “sees”). Figure 5.3 illustrates how that is accomplished, in this case by the mirror in a reflecting telescope. Light from a distant object (here, a comet) reaches us as pa ...
THE SPECIFIC ACCELERATION RATE IN LOOP
... effects. However, since Lu (E) is equal to the square root of a ratio of integrals, the results do not depend significantly on the values of the s-integration limits used. The forms of Equations (2) and (3) do not result in a closed analytic form for Lu (E) (see Equation (1)), and so a straightforwa ...
... effects. However, since Lu (E) is equal to the square root of a ratio of integrals, the results do not depend significantly on the values of the s-integration limits used. The forms of Equations (2) and (3) do not result in a closed analytic form for Lu (E) (see Equation (1)), and so a straightforwa ...
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 ...
SKA and VLBI synergies
... VLBI observations have remarkably strong impact in the Stellar physics studies. We can mention the study of Gamma Ray Bursts (GRBs), Radio Supernovae (RSNe) and Supernova Remnants (SNRs), Microquasars or Pulsars, among others. Moreover, VLBI astrometry is a unique tool providing stellar parallax mea ...
... VLBI observations have remarkably strong impact in the Stellar physics studies. We can mention the study of Gamma Ray Bursts (GRBs), Radio Supernovae (RSNe) and Supernova Remnants (SNRs), Microquasars or Pulsars, among others. Moreover, VLBI astrometry is a unique tool providing stellar parallax mea ...
Chapter 20
... In 1948, the 200-inch (5-m) “Hale” reflecting telescope opened at the Palomar Observatory, also in California, and was for many years the largest in the world. Current electronic imaging detectors, specifically chargecoupled devices (CCDs) similar to those in camcorders and digital cameras, have mad ...
... In 1948, the 200-inch (5-m) “Hale” reflecting telescope opened at the Palomar Observatory, also in California, and was for many years the largest in the world. Current electronic imaging detectors, specifically chargecoupled devices (CCDs) similar to those in camcorders and digital cameras, have mad ...
H.E.S.S. observations of the binary system PSR B1259
... The class of very high energy (VHE; E > 100 GeV) γ-ray binaries comprises only a handful of known objects in our Galaxy: LS 5039 (Aharonian et al. 2005a), LS I +61 303 (Albert et al. 2006), PSR B1259-63/LS 2883 (Aharonian et al. 2005b) and HESS J0632+057 (Aharonian et al. 2007), the first binary pri ...
... The class of very high energy (VHE; E > 100 GeV) γ-ray binaries comprises only a handful of known objects in our Galaxy: LS 5039 (Aharonian et al. 2005a), LS I +61 303 (Albert et al. 2006), PSR B1259-63/LS 2883 (Aharonian et al. 2005b) and HESS J0632+057 (Aharonian et al. 2007), the first binary pri ...
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.