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ASI 2017 Abstract Book - Astronomical Society of India
... One of the most outstanding challenges in extragalactic astronomy is to identify the astrophysical processes responsible for transforming simple dark matter haloes into the heterogenous population of galaxies inhabiting today's Universe. How did different morphological types form and evolve? Does th ...
... One of the most outstanding challenges in extragalactic astronomy is to identify the astrophysical processes responsible for transforming simple dark matter haloes into the heterogenous population of galaxies inhabiting today's Universe. How did different morphological types form and evolve? Does th ...
Nucl. Instr Meth A636 (2011) S31.
... present INTPIX has a window area, in which there are no metal or transistors, allowing illumination from the topside to ease testing. It may be possible to shrink the pixel size to less than 10 mm squares. 4.2. Counting-type pixel A pixel circuit of the counting-type pixel (CNTPIX) is shown in Fig. ...
... present INTPIX has a window area, in which there are no metal or transistors, allowing illumination from the topside to ease testing. It may be possible to shrink the pixel size to less than 10 mm squares. 4.2. Counting-type pixel A pixel circuit of the counting-type pixel (CNTPIX) is shown in Fig. ...
Global Properties of Solar Flares
... brightening. The most powerful events have a one-toone association with coronal mass ejections (CMEs), which have the clear appearance of the expansion of the coronal field and the creation of new “open” field that can support solar-wind flow. Sometimes the CME appears to entrain much or all of a pr ...
... brightening. The most powerful events have a one-toone association with coronal mass ejections (CMEs), which have the clear appearance of the expansion of the coronal field and the creation of new “open” field that can support solar-wind flow. Sometimes the CME appears to entrain much or all of a pr ...
The star-forming environment of an ultraluminous X-ray
... The star-forming environment of a ULX in NGC 4559 (Fabrika & Mescheryakov 2001; King et al. 2001; Körding, Falcke & Markoff 2002), or with super-Eddington emission from inhomogeneous discs (Begelman 2002). These different scenarios also predict different duty cycles and time-scales for the X-ray-b ...
... The star-forming environment of a ULX in NGC 4559 (Fabrika & Mescheryakov 2001; King et al. 2001; Körding, Falcke & Markoff 2002), or with super-Eddington emission from inhomogeneous discs (Begelman 2002). These different scenarios also predict different duty cycles and time-scales for the X-ray-b ...
Slides
... We are still very early in our studies but making good progress. We expect to learn much more in our work over next months with arrays plus work on individual devices both in timing and energy resolution. ...
... We are still very early in our studies but making good progress. We expect to learn much more in our work over next months with arrays plus work on individual devices both in timing and energy resolution. ...
The 2–10 keV unabsorbed luminosity function of AGN from the LSS
... AGN LF (e.g. A10; U14; M15) is to amass a very large number of AGN from different surveys made with different instruments, ranging from all-sky and shallow to pencil-beam and deep. Two possible pitfalls with that approach are that different instruments have i) different energy responses, which sometimes ...
... AGN LF (e.g. A10; U14; M15) is to amass a very large number of AGN from different surveys made with different instruments, ranging from all-sky and shallow to pencil-beam and deep. Two possible pitfalls with that approach are that different instruments have i) different energy responses, which sometimes ...
Instrumentation for CCAT
... plane diameter D to be related by s ¼ D=5. Thus, the full 20′ aperture plane defining D ¼ 87:3 cm requires s ¼ 17:5 cm, but we adopt s ¼ 15 cm in order not to overemphasize coverage of the edge of the focal plane where the efficiency will be lower. Another factor in this regard is the field curvatur ...
... plane diameter D to be related by s ¼ D=5. Thus, the full 20′ aperture plane defining D ¼ 87:3 cm requires s ¼ 17:5 cm, but we adopt s ¼ 15 cm in order not to overemphasize coverage of the edge of the focal plane where the efficiency will be lower. Another factor in this regard is the field curvatur ...
Neutron Stars and the Determination of the Dense Matter Equation
... I have a particular thought for friends and colleagues of AstroMcGill. For more than two years now, we have shared our passion of astronomy with kids of all ages and adults alike. It was not always easy, but it was surely rewarding. Friends and colleagues, at McGill or those I met during conferences ...
... I have a particular thought for friends and colleagues of AstroMcGill. For more than two years now, we have shared our passion of astronomy with kids of all ages and adults alike. It was not always easy, but it was surely rewarding. Friends and colleagues, at McGill or those I met during conferences ...
The Balloon-borne Large Aperture Submillimeter Telescope
... A significant amount of additional information contained in the BLAST surveys will be found in one- and twopoint statistics. While one-point statistics (usually referred to as P (D) analysis, i.e. looking at histograms of pixel intensities), allow an estimate of source counts to be made well below th ...
... A significant amount of additional information contained in the BLAST surveys will be found in one- and twopoint statistics. While one-point statistics (usually referred to as P (D) analysis, i.e. looking at histograms of pixel intensities), allow an estimate of source counts to be made well below th ...
Article PDF - IOPscience
... understanding of high-mass X-ray binary formation and evolution. By combining binary population synthesis and detailed mass-transfer models, however, we show that the binary parameters of M82 X-2 are not surprising provided non-conservative mass transfer is allowed. Specifically, the donor-mass lower ...
... understanding of high-mass X-ray binary formation and evolution. By combining binary population synthesis and detailed mass-transfer models, however, we show that the binary parameters of M82 X-2 are not surprising provided non-conservative mass transfer is allowed. Specifically, the donor-mass lower ...
Detector Development and Test Facility Commissioning for SuperCDMS Joseph Fox by
... SuperCDMS, the next stage of the Cryogenic Dark Matter Search (CDMS), uses cylindrical germanium crystals as particle detectors to measure phonon and ionization signals resulting from particle interactions. The aim of CDMS is to identify and measure interactions from dark matter particles (WIMPs). P ...
... SuperCDMS, the next stage of the Cryogenic Dark Matter Search (CDMS), uses cylindrical germanium crystals as particle detectors to measure phonon and ionization signals resulting from particle interactions. The aim of CDMS is to identify and measure interactions from dark matter particles (WIMPs). P ...
(McCullough et al. 2014).
... telescope to improve observations, in this case with the Hubble Space Telescope's Wide Field Camera 3 (HST WFC3). Spatial scanning will turn stars into well-defined streaks on the detector, or, for example, spread a stellar spectrum perpendicular to its dispersion. There are at least two motivations ...
... telescope to improve observations, in this case with the Hubble Space Telescope's Wide Field Camera 3 (HST WFC3). Spatial scanning will turn stars into well-defined streaks on the detector, or, for example, spread a stellar spectrum perpendicular to its dispersion. There are at least two motivations ...
Slide 1
... • Discovery made using the 2XMM catalogue (Watson et al. 2009) during a work to search for new compact objects HLX-1 ...
... • Discovery made using the 2XMM catalogue (Watson et al. 2009) during a work to search for new compact objects HLX-1 ...
ray emission from the distant BL Lac PG 1553+113
... used to set a lower limit of z > 0.78 (Sbarufatti et al. 2005) for PG 1553+113. This redshift limit is based on the assumption of the nucleus being present in a typical host galaxy, and general correlation between photometrically determined redshifts and those determined spectroscopically. However, ...
... used to set a lower limit of z > 0.78 (Sbarufatti et al. 2005) for PG 1553+113. This redshift limit is based on the assumption of the nucleus being present in a typical host galaxy, and general correlation between photometrically determined redshifts and those determined spectroscopically. However, ...
Estudio de la tasa de reacción 30P(alfa, p)33S de interés as
... orders of magnitude smaller than what is available with stable beams, these measurements can not yet be done at astrophysical energies. Consequently experiments are usually studied at higher energies, which are then extrapolated into the region of interest. Other difficulties originate from the pres ...
... orders of magnitude smaller than what is available with stable beams, these measurements can not yet be done at astrophysical energies. Consequently experiments are usually studied at higher energies, which are then extrapolated into the region of interest. Other difficulties originate from the pres ...
doctoral thesis (Dissertation)
... and UV spectroscopy and through detailed physical simulations. Spectroscopic X-ray data is reduced and presented for two targets: The CTTS V4046 Sgr was observed with Chandra for 100 ks, using a high-resolution grating spectrometer. The lightcurve contains one flare and the He-like triplets of Si xi ...
... and UV spectroscopy and through detailed physical simulations. Spectroscopic X-ray data is reduced and presented for two targets: The CTTS V4046 Sgr was observed with Chandra for 100 ks, using a high-resolution grating spectrometer. The lightcurve contains one flare and the He-like triplets of Si xi ...
An X-Ray, Optical and Infra-red study of High-Mass X
... Orbital period against spin period for all the HMXBs for which these two parameters are known. Projections of the orbital and spin distributions are also shown. . . . . . . . . . . . . . . . . . . . . . 153 ...
... Orbital period against spin period for all the HMXBs for which these two parameters are known. Projections of the orbital and spin distributions are also shown. . . . . . . . . . . . . . . . . . . . . . 153 ...
Flare Observations
... 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 orders of magnitude. At about the same time, S.E. Forbush noticed ground-level cosmic ray enhanc ...
... 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 orders of magnitude. At about the same time, S.E. Forbush noticed ground-level cosmic ray enhanc ...
Concept and performance of multiple laser guide stars for 8-m
... considered as the next generation of A0 systems for 8-m telescopes and represents a necessary intermediate step toward A0 systems for Extremely Large Telescopes. Multiple guide stars allow to correct the cone effect which affects single LGS systems and prevents from going to wavelengths shorter than ...
... considered as the next generation of A0 systems for 8-m telescopes and represents a necessary intermediate step toward A0 systems for Extremely Large Telescopes. Multiple guide stars allow to correct the cone effect which affects single LGS systems and prevents from going to wavelengths shorter than ...
High Energy Neutrino Astronomy
... HE neutrino flux implied by UHE cosmic ray • Neutrinos from production ...
... HE neutrino flux implied by UHE cosmic ray • Neutrinos from production ...
Optimization of Signal versus Background in Liquid Xe Detectors
... inner fiducial region is the lowest measured background particle detector in the world at keV energies, with background rates at the level of 10−3 counts keV−1 kg−1 day−1 . Low background rates are essential for identifying WIMP interactions in the detector, which occur with frequencies <1 kg−1 (5 y ...
... inner fiducial region is the lowest measured background particle detector in the world at keV energies, with background rates at the level of 10−3 counts keV−1 kg−1 day−1 . Low background rates are essential for identifying WIMP interactions in the detector, which occur with frequencies <1 kg−1 (5 y ...
General relativistic spectra of accretion discs around rapidly
... parameters: M, V, D, i (for face-on, i ¼ 08Þ, M chosen EOSs. Our results are displayed in Figs 1 – 5. In all the displayed spectra, we have assumed M ¼ 1:4 M( (canonical mass for neutron stars), D ¼ 5 kpc and f ¼ 2:0. In Fig. 1, we have plotted the Newtonian spectrum and general relativistic (GR) sp ...
... parameters: M, V, D, i (for face-on, i ¼ 08Þ, M chosen EOSs. Our results are displayed in Figs 1 – 5. In all the displayed spectra, we have assumed M ¼ 1:4 M( (canonical mass for neutron stars), D ¼ 5 kpc and f ¼ 2:0. In Fig. 1, we have plotted the Newtonian spectrum and general relativistic (GR) sp ...
Hot slumping glass technology and integration process to
... make this approach very attractive and very promising results have been achieved so far, even if a demonstration of imaging capabilities at a level of 5 arcsec it has not yet completely demonstrated and an effort is under way in this direction. In the mean time, the fabrication of large segmented op ...
... make this approach very attractive and very promising results have been achieved so far, even if a demonstration of imaging capabilities at a level of 5 arcsec it has not yet completely demonstrated and an effort is under way in this direction. In the mean time, the fabrication of large segmented op ...
Slides - Indico
... Many accelerators have been proposed in the world, operating up to several MeV, i.e. well suited to study BBN reactions. ...
... Many accelerators have been proposed in the world, operating up to several MeV, i.e. well suited to study BBN reactions. ...
Inspiral Group Report: S1 Preliminary Report
... about 150 instruments covering the full spectrum, from radio to high-energy gamma-rays. • Shortly after a few detections, LSC/Virgo will publicly release GW triggers for follow up: dcc.ligo.org, LIGO-M1200055. ...
... about 150 instruments covering the full spectrum, from radio to high-energy gamma-rays. • Shortly after a few detections, LSC/Virgo will publicly release GW triggers for follow up: dcc.ligo.org, LIGO-M1200055. ...
X-ray astronomy detector
![](https://commons.wikimedia.org/wiki/Special:FilePath/Ill-2_O3.jpg?width=300)
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.