SXDF-ALMA 2 arcmin $^ 2$ Deep Survey: 1.1
... ALMA number counts obtained in the Extended Chandra Deep Field South (ECDFS) by Karim et al. (2013) (870 µm) and in the UKIRT InfraRed Deep Sky Surveys (UKIDSS) Ultra Deep Survey (UDS) field by Simpson et al. (2015) (870 µm), and ALMA number counts derived from serendipitously-detected sources by Ha ...
... ALMA number counts obtained in the Extended Chandra Deep Field South (ECDFS) by Karim et al. (2013) (870 µm) and in the UKIRT InfraRed Deep Sky Surveys (UKIDSS) Ultra Deep Survey (UDS) field by Simpson et al. (2015) (870 µm), and ALMA number counts derived from serendipitously-detected sources by Ha ...
Influence of extreme ultraviolet radiation on the Pv ionization fraction
... reconcile with each other. The widely accepted presence of clumping in hot star winds implies a significant reduction of observational mass-loss rate estimates from diagnostics that depend on the square of the density. Moreover, the ultraviolet P V resonance lines indicate a possible need for an eve ...
... reconcile with each other. The widely accepted presence of clumping in hot star winds implies a significant reduction of observational mass-loss rate estimates from diagnostics that depend on the square of the density. Moreover, the ultraviolet P V resonance lines indicate a possible need for an eve ...
VLVNT_APP_Roadmaps_Ch_Spiering_
... for looking deeper into black hole environments and, at energies beyond 100 TeV, further out into the Universe than possible with gamma-rays. Together with gammaray and cosmic ray observations (and with IceCube), it could pave the way to real multi-messenger astronomy. • However, in absence of estab ...
... for looking deeper into black hole environments and, at energies beyond 100 TeV, further out into the Universe than possible with gamma-rays. Together with gammaray and cosmic ray observations (and with IceCube), it could pave the way to real multi-messenger astronomy. • However, in absence of estab ...
radioactive 26a1 in the galaxy: observations versus theory
... is supported by a large body of observational data, concerning the abundances of the chemical elements in the solar system, in stars of different ages, in the interstellar medium of our Galaxy and in external galaxies as well [ 1601. In the vast majority of cases observations reveal only elemental a ...
... is supported by a large body of observational data, concerning the abundances of the chemical elements in the solar system, in stars of different ages, in the interstellar medium of our Galaxy and in external galaxies as well [ 1601. In the vast majority of cases observations reveal only elemental a ...
New challenges for adaptive optics: extremely large telescopes
... to obtain the full potential in angular resolution, to avoid source confusion for extragalactic studies at high redshifts, and to reduce the background contribution, dramatically increasing limiting magnitude (the signal-to-noise ratio is then proportional to the square of telescope diameter). Compe ...
... to obtain the full potential in angular resolution, to avoid source confusion for extragalactic studies at high redshifts, and to reduce the background contribution, dramatically increasing limiting magnitude (the signal-to-noise ratio is then proportional to the square of telescope diameter). Compe ...
"IR Detector Arrays for Astronomy", ARAA, 45
... Space Observatory (ISO), and for the far-infrared channels on the Spitzer Space Telescope (Spitzer). In the latter case, rather elaborate strategies both in the instrument and in the data pipeline have tamed the calibration problems to a large extent. In addition, there are inherent contradictions i ...
... Space Observatory (ISO), and for the far-infrared channels on the Spitzer Space Telescope (Spitzer). In the latter case, rather elaborate strategies both in the instrument and in the data pipeline have tamed the calibration problems to a large extent. In addition, there are inherent contradictions i ...
PRESPEC – towards gamma-ray spectroscopy of exotic nuclei at FAIR
... Which are the nuclei relevant for astrophysical processes and what are their properties? What is the origin of the heavy elements? ...
... Which are the nuclei relevant for astrophysical processes and what are their properties? What is the origin of the heavy elements? ...
models for low-mass x-ray binaries in the elliptical
... binaries. The formation rates associated with these two possibilities are not understood well enough to give accurate predictions and are based on the relative numbers in the samples. Juett (2005) has shown that the observed relationship between the fraction of LMXBs found in GCs and the GC-specific ...
... binaries. The formation rates associated with these two possibilities are not understood well enough to give accurate predictions and are based on the relative numbers in the samples. Juett (2005) has shown that the observed relationship between the fraction of LMXBs found in GCs and the GC-specific ...
Untitled - METU Astrophysics Home Page
... calculations of neutron star mass and radii. However, the first observational evidence of a rotation powered pulsar hasn’t come until 1967, when Bell detected radio pulsations from outside the solar system which later was understood to be the first detection of a pulsar by the humankind. Following t ...
... calculations of neutron star mass and radii. However, the first observational evidence of a rotation powered pulsar hasn’t come until 1967, when Bell detected radio pulsations from outside the solar system which later was understood to be the first detection of a pulsar by the humankind. Following t ...
PACS Calibration Status and Plans
... 5) Refinement of PV calibrations along the progress in data processing (e.g. more sensitive set-up, design of measurement to avoid disturbing effects). ...
... 5) Refinement of PV calibrations along the progress in data processing (e.g. more sensitive set-up, design of measurement to avoid disturbing effects). ...
Slide 1
... Low Energy Solar Neutrinos SNO+ will detect solar neutrinos with lower energies than SNO. This will enable precision studies of neutrino oscillations and the coupling between neutrinos and dense matter. SNO+ will detect the pep and CNO solar neutrinos, helping us understand the nuclear reactions tha ...
... Low Energy Solar Neutrinos SNO+ will detect solar neutrinos with lower energies than SNO. This will enable precision studies of neutrino oscillations and the coupling between neutrinos and dense matter. SNO+ will detect the pep and CNO solar neutrinos, helping us understand the nuclear reactions tha ...
PowerPoint - Herschel Space Observatory
... – 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 radiation with a different ...
... – 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 radiation with a different ...
Cathode MCP Anode -100V
... of the Mesosphere and lower Thermosphere between an altitude of approximately 60 to 180 kilometers. • GUVI is a far-ultraviolet (115 to 180 nm), scanning imaging spectrograph that provides horizon-tohorizon images in five selectable wavelength intervals www.photek.co.uk ...
... of the Mesosphere and lower Thermosphere between an altitude of approximately 60 to 180 kilometers. • GUVI is a far-ultraviolet (115 to 180 nm), scanning imaging spectrograph that provides horizon-tohorizon images in five selectable wavelength intervals www.photek.co.uk ...
Discussion about Noise Equivalent Power and its use for photon
... Definitions of NEP. Contrary of what could be thought regarding the wide use of the Noise Equivalent Power in literature to characterize the measurements limits of detectors, it is not easy to find a clear mathematical definition of the NEP in the literature! The first definition given here comes fr ...
... Definitions of NEP. Contrary of what could be thought regarding the wide use of the Noise Equivalent Power in literature to characterize the measurements limits of detectors, it is not easy to find a clear mathematical definition of the NEP in the literature! The first definition given here comes fr ...
Accreting millisecond X-ray pulsars, from accretion disk to magnetic
... controlled by the magnetic stresses. Electrons spiraling around such extreme fields emit cyclotron radiation as a flow of X-rays and γ−rays, and when B > BQED the electron cyclotron energy equals the electron rest mass energy and quantum mechanical effects are dominant, like photon splitting and pai ...
... controlled by the magnetic stresses. Electrons spiraling around such extreme fields emit cyclotron radiation as a flow of X-rays and γ−rays, and when B > BQED the electron cyclotron energy equals the electron rest mass energy and quantum mechanical effects are dominant, like photon splitting and pai ...
Rich Clusters of Galaxies
... The Chandra X-ray observations reveal a large cloud of hot gas that extends throughout the cluster. The gas cloud is several million light years across and has a temperature of about 40 million degrees in the outer parts decreasing to about 15 million degrees in the inner region. In the very central ...
... The Chandra X-ray observations reveal a large cloud of hot gas that extends throughout the cluster. The gas cloud is several million light years across and has a temperature of about 40 million degrees in the outer parts decreasing to about 15 million degrees in the inner region. In the very central ...
Systematic variation in the apparent burning area of thermonuclear
... 2 A N A LY S I S A N D R E S U LT S The large area and good time resolution of the proportional counter array (PCA) detector of the Rossi X-ray Timing Explorer (RXTE) satellite make it an ideal instrument for measuring the burst spectral evolution. In order to find a pattern in the R ∞ evolution dur ...
... 2 A N A LY S I S A N D R E S U LT S The large area and good time resolution of the proportional counter array (PCA) detector of the Rossi X-ray Timing Explorer (RXTE) satellite make it an ideal instrument for measuring the burst spectral evolution. In order to find a pattern in the R ∞ evolution dur ...
potenza dei jet nei nuclei galattici attivi radio
... radiation fields responsible for photoionizing the galactic nebulae where they came from. AGNs are thought to host at their centers a massive compact object with mass M ∼ 106 –109 M , where M = 1.9891 · 1033 g corresponds to the unit solar mass. Another feature of an AGN’s optical-UV (Ultra Violet ...
... radiation fields responsible for photoionizing the galactic nebulae where they came from. AGNs are thought to host at their centers a massive compact object with mass M ∼ 106 –109 M , where M = 1.9891 · 1033 g corresponds to the unit solar mass. Another feature of an AGN’s optical-UV (Ultra Violet ...
The Next Error Committed by the Nobel Committee
... It results from the localization constant k 0 m r const (1) of the photon that its mass m and, consequently, energy E mC 2 are decreased when the photon radius is increased (r ) . It has been established that these changes depend on a coincidence or an opposition of the directions of mot ...
... It results from the localization constant k 0 m r const (1) of the photon that its mass m and, consequently, energy E mC 2 are decreased when the photon radius is increased (r ) . It has been established that these changes depend on a coincidence or an opposition of the directions of mot ...
Clumpy wind accretion in supergiant neutron star high mass X
... (mostly 2D and pseudo 3D), however, were so far unable to account for the thermal structure of the wind and thus they could not make any clear prediction on the intensity of the produced X-ray radiation to be compared with observations of isolated OB supergiants and massive stars in SGXBs (see, e.g. ...
... (mostly 2D and pseudo 3D), however, were so far unable to account for the thermal structure of the wind and thus they could not make any clear prediction on the intensity of the produced X-ray radiation to be compared with observations of isolated OB supergiants and massive stars in SGXBs (see, e.g. ...
Hint of a transiting extended atmosphere on 55 Cancri b⋆
... of 55 Cnc e, with precise start times of 2012-03-07 UT 02:13 and 2012-04-05 UT 12:50. The scheduled exposure times were 20 ks, but the first observation was cut short to 12 ks by safing of ACIS due to high Solar radiation levels. Since 55 Cnc is a bright optical source, we operated the ACIS-S CCD in ...
... of 55 Cnc e, with precise start times of 2012-03-07 UT 02:13 and 2012-04-05 UT 12:50. The scheduled exposure times were 20 ks, but the first observation was cut short to 12 ks by safing of ACIS due to high Solar radiation levels. Since 55 Cnc is a bright optical source, we operated the ACIS-S CCD in ...
The X-ray/radio and UV luminosity expected from symbiotic systems
... owing to the existence of the CSM, the possibility of significant blueshifts for some absorption lines can be expected in the spectra of some SNe Ia, even though the true nature of the blueshift is not fully understood (Sternberg et al. 2014). Sternberg et al. (2011) checked the absorption propertie ...
... owing to the existence of the CSM, the possibility of significant blueshifts for some absorption lines can be expected in the spectra of some SNe Ia, even though the true nature of the blueshift is not fully understood (Sternberg et al. 2014). Sternberg et al. (2011) checked the absorption propertie ...
Fundamental properties of Ana González Galán
... The aim of this thesis is to characterise a sample of High Mass X-ray Binaries (HMXBs) formed by: IGR J00370+6122, XTE J1855-026, AX J1841.0-0535 and AX J1845.0-0433. These objects are composed of pulsars (rotating neutron stars) accreting material from the wind of their supergiant companions. The X ...
... The aim of this thesis is to characterise a sample of High Mass X-ray Binaries (HMXBs) formed by: IGR J00370+6122, XTE J1855-026, AX J1841.0-0535 and AX J1845.0-0433. These objects are composed of pulsars (rotating neutron stars) accreting material from the wind of their supergiant companions. The X ...
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. ...
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.