Advanced information on the Nobel Prize in Physics 2002, 8 October
... The reliability of Davis’ results depends very much on the extraction efficiency of argon. This was very carefully studied. A known amount of 36Ar was introduced regularly and the extraction efficiency was determined to 95%. Radioactive 37Ar was produced in the tank and the extraction efficiency was ...
... The reliability of Davis’ results depends very much on the extraction efficiency of argon. This was very carefully studied. A known amount of 36Ar was introduced regularly and the extraction efficiency was determined to 95%. Radioactive 37Ar was produced in the tank and the extraction efficiency was ...
ULXs: General Properties and Variability - X
... luminous photo-ionized nebulae around them- require high luminosity to photoionize them •Quite a few have “soft” components well fit by low kT black body- consistent with high mass (Miller this meeting). ...
... luminous photo-ionized nebulae around them- require high luminosity to photoionize them •Quite a few have “soft” components well fit by low kT black body- consistent with high mass (Miller this meeting). ...
the orbits of neptune`s outer satellites
... known (Nereid included) outer satellites of Neptune could be imaged on just two Suprime-Cam fields. We thus oriented two Suprime-Cam fields in order to recover all known outer satellites of Neptune. The images were visually blinked in order to recover the known satellites and search for new satellit ...
... known (Nereid included) outer satellites of Neptune could be imaged on just two Suprime-Cam fields. We thus oriented two Suprime-Cam fields in order to recover all known outer satellites of Neptune. The images were visually blinked in order to recover the known satellites and search for new satellit ...
HOPS 383: An Outbursting Class 0 Protostar in Orion
... There were two day-long series of WISE observations at 3.4 and 4.6 µm between the 2009 and 2010 YSOVAR campaigns, on 2010 March 8–9 and 2010 September 15–16. No significant variability from the WISE fluxes shown in the SED (Fig. 3) was detected. The second (2010) YSOVAR season showed a slight fading ...
... There were two day-long series of WISE observations at 3.4 and 4.6 µm between the 2009 and 2010 YSOVAR campaigns, on 2010 March 8–9 and 2010 September 15–16. No significant variability from the WISE fluxes shown in the SED (Fig. 3) was detected. The second (2010) YSOVAR season showed a slight fading ...
VLT identifications in the Chandra/XMM
... a Seyfert-2 galaxy with heavy X-ray absorption and an AGN-type luminosity. The latter spectrum is characteristic for the bulk of the detected galaxies, which show either no or very faint high excitation lines indicating the AGN nature of the object, so that we have to resort to a combination of opti ...
... a Seyfert-2 galaxy with heavy X-ray absorption and an AGN-type luminosity. The latter spectrum is characteristic for the bulk of the detected galaxies, which show either no or very faint high excitation lines indicating the AGN nature of the object, so that we have to resort to a combination of opti ...
Brightness and Flux Density
... Astronomers learn about an astronomical source by measuring the strength of its radiation as a function of direction on the sky (by mapping or imaging) and frequency (spectroscopy), plus other quantities (time, polarization) that we ignore for now. We need precise and quantitative definitions to des ...
... Astronomers learn about an astronomical source by measuring the strength of its radiation as a function of direction on the sky (by mapping or imaging) and frequency (spectroscopy), plus other quantities (time, polarization) that we ignore for now. We need precise and quantitative definitions to des ...
1e 1048.1−5937, xte j1810−197 and 4u 0142+61
... detected emission feature is at an energy of ≈13 keV. In the magnetar model the common interpretation is that these lines are proton-cyclotron in origin, implying a magnetic field of ≈2 × 1015 G. The major challenge with this view is that since all three sources show the line at the same energy, the ...
... detected emission feature is at an energy of ≈13 keV. In the magnetar model the common interpretation is that these lines are proton-cyclotron in origin, implying a magnetic field of ≈2 × 1015 G. The major challenge with this view is that since all three sources show the line at the same energy, the ...
Searching for Dwarf Galaxies and Population III Star
... This multi-step project includes 3 tiers of observations: 1. By 2016, the James Webb Space Telescope will regularly deliver deep infrared images that reveal the most massive star-forming galaxies and proto-clusters of galaxies at z > 7. We will identify the most luminous at z ~ 7.7, where Lyman fa ...
... This multi-step project includes 3 tiers of observations: 1. By 2016, the James Webb Space Telescope will regularly deliver deep infrared images that reveal the most massive star-forming galaxies and proto-clusters of galaxies at z > 7. We will identify the most luminous at z ~ 7.7, where Lyman fa ...
Multiwavelength properties of γ-ray loud binary systems.
... find on the moth-time-scale σ−map less than one lightcurve (on average) with σ > σthr = 4. The most variable Galactic sources are LSI +61 303, Cyg X-3 and V407 Cyg. All the three are γ-ray-loud binaries with rather different types ofvariability. LSI +61 303 is a persistent source, variable on the 26 ...
... find on the moth-time-scale σ−map less than one lightcurve (on average) with σ > σthr = 4. The most variable Galactic sources are LSI +61 303, Cyg X-3 and V407 Cyg. All the three are γ-ray-loud binaries with rather different types ofvariability. LSI +61 303 is a persistent source, variable on the 26 ...
As far as - Sangeeta Malhotra
... As part of the GRAPES project, my team performed spectroscopy on the HUDF target region between October 2002 and January 2003, using about 10 percent of the time that went into imaging. We quickly discovered that GRAPES is not just an extragalactic survey, for the HUDF distance scale starts within o ...
... As part of the GRAPES project, my team performed spectroscopy on the HUDF target region between October 2002 and January 2003, using about 10 percent of the time that went into imaging. We quickly discovered that GRAPES is not just an extragalactic survey, for the HUDF distance scale starts within o ...
Results from the search for tidal disruption flares in the GALEX Deep
... New Confirmed Flare from Inactive Galaxy TOO VLT Spectrum courtesy of Stephane Basa ...
... New Confirmed Flare from Inactive Galaxy TOO VLT Spectrum courtesy of Stephane Basa ...
Document
... This diagram shows a single closed dimension of cosmological space (a huge cosmic great circle) and many local ‘directions’ or dimensions of time. We may think of time in spacetime in much the same way that we think of the gravitational gradient on Earth; time is not a single dimension of spacetime, ...
... This diagram shows a single closed dimension of cosmological space (a huge cosmic great circle) and many local ‘directions’ or dimensions of time. We may think of time in spacetime in much the same way that we think of the gravitational gradient on Earth; time is not a single dimension of spacetime, ...
THE OFFSET AND HOST LIGHT DISTRIBUTIONS OF LONG
... that LGRBs track an exponential light distribution. In addition to the tension between the results of previous studies, and the relatively small samples used in these studies, it is important to note other potential challenges. First, the aforementioned studies were based on LGRB samples collected f ...
... that LGRBs track an exponential light distribution. In addition to the tension between the results of previous studies, and the relatively small samples used in these studies, it is important to note other potential challenges. First, the aforementioned studies were based on LGRB samples collected f ...
English version - Richard de Grijs
... “The tails seem to tell us why that is,” said Posselt, adding that the pulsars’ spin and magnetic axis orientations influence what kind of emission is seen on Earth. Geminga may have magnetic poles quite close to the top and bottom of the object, and nearly aligned spin poles, much like Earth. On ...
... “The tails seem to tell us why that is,” said Posselt, adding that the pulsars’ spin and magnetic axis orientations influence what kind of emission is seen on Earth. Geminga may have magnetic poles quite close to the top and bottom of the object, and nearly aligned spin poles, much like Earth. On ...
Gamma-Ray Pulsars - INTEGRAL
... with periods ranging from ∼ ms to nearly 10s, was the primary characteristic of this new astrophysical object. The lightcurve of a pulsar can be regarded as the cross-section through a rotating beaming pattern cut along the line of sight to the observer. The full beaming pattern on the sphere around ...
... with periods ranging from ∼ ms to nearly 10s, was the primary characteristic of this new astrophysical object. The lightcurve of a pulsar can be regarded as the cross-section through a rotating beaming pattern cut along the line of sight to the observer. The full beaming pattern on the sphere around ...
HWWS 2010 - Monash University
... • Energy released from accretion material onto an object of mass M and radius R is • i.e. the (specific) power-to-mass ratio is just a function of radius… • Neutron stars are the ...
... • Energy released from accretion material onto an object of mass M and radius R is • i.e. the (specific) power-to-mass ratio is just a function of radius… • Neutron stars are the ...
Distances in Cosmology One of the most basic measurements that
... measuring the apparent times at which Venus crossed the Sun’s limb). Then, knowing this distance, parallax has been used to determine the distance to many stars. Parallax, however, has its limits. The problem is that something sufficiently distant has such a tiny angular shift that it can’t be measu ...
... measuring the apparent times at which Venus crossed the Sun’s limb). Then, knowing this distance, parallax has been used to determine the distance to many stars. Parallax, however, has its limits. The problem is that something sufficiently distant has such a tiny angular shift that it can’t be measu ...
No Slide Title - DCC
... were designed conservatively, based on “tabletop” prototypes, but with expected sensitivity gain of ~1000. Given the expected low rate of detectable GW events, it was always planned that in engineering, building and commissioning initial LIGO, one would learn how reliably to build Advanced LIGO with ...
... were designed conservatively, based on “tabletop” prototypes, but with expected sensitivity gain of ~1000. Given the expected low rate of detectable GW events, it was always planned that in engineering, building and commissioning initial LIGO, one would learn how reliably to build Advanced LIGO with ...
Here you can get a Science reprint
... neutron star, leading to the delayed formation of a black hole (1). Recently, it has been found that the black hole x-ray binary GRO J1655-40 was launched far from its birthplace by an energetic SN explosion (2) at a runaway speed (3) of 120 km s⫺1. But so far there has been no observational evidenc ...
... neutron star, leading to the delayed formation of a black hole (1). Recently, it has been found that the black hole x-ray binary GRO J1655-40 was launched far from its birthplace by an energetic SN explosion (2) at a runaway speed (3) of 120 km s⫺1. But so far there has been no observational evidenc ...
Active Galactic Nuclei
... from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like stars. ...
... from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like stars. ...
X-ray Astronomy and the search for Black Holes
... • The hard X-rays are thin thermal emissions, i.e., from plasma accreting onto the white dwarf – Are our inference for very massive white dwarfs correct? ...
... • The hard X-rays are thin thermal emissions, i.e., from plasma accreting onto the white dwarf – Are our inference for very massive white dwarfs correct? ...
has occurred over the past 14 billion years COSMIC DOWNSIZING
... the ultraviolet waveband, at a wavelength of about 912 angstroms. (The cutoff appears because the neutral hydrogen gas in and around the galaxy absorbs radiation with shorter wavelengths.) Because the light from distant galaxies is shifted to the red, the cutoff moves to longer wavelengths; if the r ...
... the ultraviolet waveband, at a wavelength of about 912 angstroms. (The cutoff appears because the neutral hydrogen gas in and around the galaxy absorbs radiation with shorter wavelengths.) Because the light from distant galaxies is shifted to the red, the cutoff moves to longer wavelengths; if the r ...
Finnish Centre for Astronomy with ESO
... in astronomical research. The ultimate goal of FINCA is to improve the scientific and industrial benefit of Finland’s membership in ESO, and Finland’s international competitiveness in astronomical research. The year 2014 marked the 5th year of operation for FINCA, administratively a Special Unit of ...
... in astronomical research. The ultimate goal of FINCA is to improve the scientific and industrial benefit of Finland’s membership in ESO, and Finland’s international competitiveness in astronomical research. The year 2014 marked the 5th year of operation for FINCA, administratively a Special Unit of ...
Document
... 1999: using ASCA, X-1 in M82 was found to vary by up to a factor of four, confirming that this bright source was indeed a single object. *Over half of ULXs are known to be variable, ruling out the multiple source or SNR hypothesis. ...
... 1999: using ASCA, X-1 in M82 was found to vary by up to a factor of four, confirming that this bright source was indeed a single object. *Over half of ULXs are known to be variable, ruling out the multiple source or SNR hypothesis. ...