Vireo Manual - Gettysburg College
... database includes data from the Hubble Guide Star Catalog (about 16 million objects), plus additional data on 24 thousand galaxies, 2269 quasi-stellar objects and 558 pulsars. In addition, VIREO data files contain the orbital elements of about 29 thousand asteroids. When used with a broad-band inter ...
... database includes data from the Hubble Guide Star Catalog (about 16 million objects), plus additional data on 24 thousand galaxies, 2269 quasi-stellar objects and 558 pulsars. In addition, VIREO data files contain the orbital elements of about 29 thousand asteroids. When used with a broad-band inter ...
SkyProdigy Series Manual
... sky, which is processed internally to positively identify the stars in the image. Once a positive match is found, SkyProdigy determines the coordinates of the center of the captured image. The process is automatically repeated two more times so that the system has three known alignment points that c ...
... sky, which is processed internally to positively identify the stars in the image. Once a positive match is found, SkyProdigy determines the coordinates of the center of the captured image. The process is automatically repeated two more times so that the system has three known alignment points that c ...
A catalogue of the Chandra Deep Field South with multi
... 1999 and February 2001. They encompass a total exposure time of 195 ksec of which 35 ksec were taken in the R-band during the best seeing conditions. We needed several observing runs to collect the full 17filter data set. Hence, for some long-term variable stars and QSOs, the observed 17-passband sp ...
... 1999 and February 2001. They encompass a total exposure time of 195 ksec of which 35 ksec were taken in the R-band during the best seeing conditions. We needed several observing runs to collect the full 17filter data set. Hence, for some long-term variable stars and QSOs, the observed 17-passband sp ...
April 2016 - Central Arkansas Astronomical Society
... The gravita onal waves were detected on September 14, The existence of gravita onal waves was first demonstrated 2015 at 5:51 a.m. Eastern Daylight Time (09:51 UTC) by both in the 1970s and 80s by Joseph Taylor, Jr., and colleagues. of the twin Laser Interferometer Gravita onal‐wave Taylor and Russel ...
... The gravita onal waves were detected on September 14, The existence of gravita onal waves was first demonstrated 2015 at 5:51 a.m. Eastern Daylight Time (09:51 UTC) by both in the 1970s and 80s by Joseph Taylor, Jr., and colleagues. of the twin Laser Interferometer Gravita onal‐wave Taylor and Russel ...
The Celestial Origin of Atoms
... Aims and aspirations of nuclear astrophysics The aim of nuclear astrophysics is threefold. Firstly, it seeks to determine the mechanisms whereby the various nuclear species occurring in nature are built up, from deuterium with its two nucleons to uranium with 238 nucleons. Secondly, it seeks to iden ...
... Aims and aspirations of nuclear astrophysics The aim of nuclear astrophysics is threefold. Firstly, it seeks to determine the mechanisms whereby the various nuclear species occurring in nature are built up, from deuterium with its two nucleons to uranium with 238 nucleons. Secondly, it seeks to iden ...
Digital STARLAB Teachers Guide
... projection system in its price range for portable and small fixed domes. The projector features a custom fisheye lens (patent pending) capable of depicting an accurate, high-contrast, simulated night sky with the capacity to explore a multitude of motions and displays eliminating the need for addition ...
... projection system in its price range for portable and small fixed domes. The projector features a custom fisheye lens (patent pending) capable of depicting an accurate, high-contrast, simulated night sky with the capacity to explore a multitude of motions and displays eliminating the need for addition ...
A Zoo of Galaxies - Cambridge University Press
... The variety of different galaxies observed in the sky naturally caused people to wonder what they were. The scientific arguments surrounding this question at the start of the 20th century, are best represented perhaps, by the public debate held in 1920 between Heber Curtis and Harlow Shapley. Many oth ...
... The variety of different galaxies observed in the sky naturally caused people to wonder what they were. The scientific arguments surrounding this question at the start of the 20th century, are best represented perhaps, by the public debate held in 1920 between Heber Curtis and Harlow Shapley. Many oth ...
Structure in the first quadrant of the Galaxy: an analysis of TMGS star
... The original SKY model described in WCVWS incorporates six fully detailed Galactic components: an exponential disc; a Bahcalltype bulge; a de Vaucouleurs halo; a 4-armed spiral with 2 local spurs; Gould’s Belt and a circular molecular ring. Each geometrical element may contain up to 87 source catego ...
... The original SKY model described in WCVWS incorporates six fully detailed Galactic components: an exponential disc; a Bahcalltype bulge; a de Vaucouleurs halo; a 4-armed spiral with 2 local spurs; Gould’s Belt and a circular molecular ring. Each geometrical element may contain up to 87 source catego ...
Super-Eddington outburst in a binary system: V4641 Sgr Mikhail Revnivtsev, Marat Gilfanov
... • Usually the increase of optical brightness of X-ray Novae is caused by the contribution of the accretion disk • It is common for X-ray Novae to demonstrate ∆mv ∼ 5. But only if the X-ray Nova is the low mass X-ray binary ! Such huge change of the optical brightness was never observed in high mass ...
... • Usually the increase of optical brightness of X-ray Novae is caused by the contribution of the accretion disk • It is common for X-ray Novae to demonstrate ∆mv ∼ 5. But only if the X-ray Nova is the low mass X-ray binary ! Such huge change of the optical brightness was never observed in high mass ...
Spectroscopic Atlas for Amateur Astronomers
... which systematically covers the classes O, B, A, F, G, K, M, by commenting most of the lines, visible in a medium resolved spectral profile was still missing. In the Internet we find many professional papers, mostly focused on small sections of a spectral profile. Nevertheless, they often contribute ...
... which systematically covers the classes O, B, A, F, G, K, M, by commenting most of the lines, visible in a medium resolved spectral profile was still missing. In the Internet we find many professional papers, mostly focused on small sections of a spectral profile. Nevertheless, they often contribute ...
Quiescent and flaring X-ray emission from the nearby M/T dwarf
... However, the detected signal in the RGS (Reflection Grating Spectrometer) detectors is rather weak; while we clearly see a few photons from prominent emission lines, e.g. O viii at 19 Å and O vii at 21.6–22.1 Å, the RGS spectra are not suitable for a quantitative analysis. Thus we considered only X- ...
... However, the detected signal in the RGS (Reflection Grating Spectrometer) detectors is rather weak; while we clearly see a few photons from prominent emission lines, e.g. O viii at 19 Å and O vii at 21.6–22.1 Å, the RGS spectra are not suitable for a quantitative analysis. Thus we considered only X- ...
Galactic Stellar and Substellar Initial Mass Function Invited Review Gilles Chabrier
... kinematic shear between the thick-disk population, present in local samples, and the genuine spheroid one. This enables us to derive only an upper limit for the spheroid mass density and IMF. Within all the uncertainties, the latter is found to be similar to the one derived for globular clusters and ...
... kinematic shear between the thick-disk population, present in local samples, and the genuine spheroid one. This enables us to derive only an upper limit for the spheroid mass density and IMF. Within all the uncertainties, the latter is found to be similar to the one derived for globular clusters and ...
The low-mass dispersed population around the Lupus clouds
... for the classification of stars in the range of temperatures expected from the spectral energy distribution fits carried out by CSL (T eff . 3700 K in Lupus 1, T eff . 3400 K in Lupus 3 and 4), providing diagnostic features of temperature and surface gravity as well as accretion/outflow diagnostic l ...
... for the classification of stars in the range of temperatures expected from the spectral energy distribution fits carried out by CSL (T eff . 3700 K in Lupus 1, T eff . 3400 K in Lupus 3 and 4), providing diagnostic features of temperature and surface gravity as well as accretion/outflow diagnostic l ...
N-Body/SPH simulations of induced star formation in dwarf galaxies
... 1 Figures front page: Density evolution projected on the xy plane. This density evolution belongs to sim1058 and shows the density evolution during an extreme peak in the SFR and right afterwards. The extreme star formation has caused extreme feedback, and the gas is entirely blown apart by supernov ...
... 1 Figures front page: Density evolution projected on the xy plane. This density evolution belongs to sim1058 and shows the density evolution during an extreme peak in the SFR and right afterwards. The extreme star formation has caused extreme feedback, and the gas is entirely blown apart by supernov ...
A physical interpretation of the `red Sirius` anomaly
... would need to suffer reddening E B 2 V < 1:5 [Bonnet-Bidaud & Gry 1991 adopt E B 2 V < 1:0, but this value raises its colour index only to the value for Pollux, the least red of the comparison stars]. To convert from reddening, E B 2 V, to total visual extinction, AV, we must assume a value for t ...
... would need to suffer reddening E B 2 V < 1:5 [Bonnet-Bidaud & Gry 1991 adopt E B 2 V < 1:0, but this value raises its colour index only to the value for Pollux, the least red of the comparison stars]. To convert from reddening, E B 2 V, to total visual extinction, AV, we must assume a value for t ...
Where stars form: inside-out growth and coherent star formation from
... We present Hα maps at 1 kpc spatial resolution for star-forming galaxies at z ∼ 1, made possible by the WFC3 grism on HST. Employing this capability over all five 3D-HST/CANDELS fields provides a sample of 2676 galaxies enabling a division into subsamples based on stellar mass and star formation rat ...
... We present Hα maps at 1 kpc spatial resolution for star-forming galaxies at z ∼ 1, made possible by the WFC3 grism on HST. Employing this capability over all five 3D-HST/CANDELS fields provides a sample of 2676 galaxies enabling a division into subsamples based on stellar mass and star formation rat ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... used by Shapley to estimate the centroid of the system and thus { again for the rst time { to determine the distance from the Sun to the Galactic center. The second graph shows us exactly the same plot with the most modern measurements. The data have improved dramatically over the intervening 80 ye ...
... used by Shapley to estimate the centroid of the system and thus { again for the rst time { to determine the distance from the Sun to the Galactic center. The second graph shows us exactly the same plot with the most modern measurements. The data have improved dramatically over the intervening 80 ye ...
Angular Momentum Evolution of Young Low
... contrast, the lowest-mass stars significantly spin up. Henderson and Stassun (2012) suggested that the increasing period-mass slope for lower-mass stars can be used as an age proxy for very young clusters. Littlefairet al. (2010), however, reported that the similarly aged (5 Ma) NGC 2362 and Cep OB3 ...
... contrast, the lowest-mass stars significantly spin up. Henderson and Stassun (2012) suggested that the increasing period-mass slope for lower-mass stars can be used as an age proxy for very young clusters. Littlefairet al. (2010), however, reported that the similarly aged (5 Ma) NGC 2362 and Cep OB3 ...
Science with IMACS on Magellan
... arcsec, sharp enough to result in only 10% degradation of the best images that are expected, FWHM ∼ 0.25 arsec. The f/2.4 camera’s performance is remarkable considering the field size, with rms image size of 0.25 arcsec over the field. The working performance of the cameras with band-limiting filter ...
... arcsec, sharp enough to result in only 10% degradation of the best images that are expected, FWHM ∼ 0.25 arsec. The f/2.4 camera’s performance is remarkable considering the field size, with rms image size of 0.25 arcsec over the field. The working performance of the cameras with band-limiting filter ...
Sample syllabus 2 - Johns Hopkins Center for Talented Youth
... Course Description: When the sun runs out of fuel, will it explode in a giant supernova or fade out into a white dwarf? Does every galaxy revolve around a super-massive black hole? Will the universe continue to expand, or will it eventually collapse back upon itself in a reversal of the Big Bang? As ...
... Course Description: When the sun runs out of fuel, will it explode in a giant supernova or fade out into a white dwarf? Does every galaxy revolve around a super-massive black hole? Will the universe continue to expand, or will it eventually collapse back upon itself in a reversal of the Big Bang? As ...
The Celestial Sphere CHAPTER 1
... motion was a good approximation. Furthermore, since a geocentric model maintains circular motion, it was very difficult to make any observational distinction between geocentric and heliocentric universes. (Parallax effects are far too small to be noticeable with the naked eye.) ...
... motion was a good approximation. Furthermore, since a geocentric model maintains circular motion, it was very difficult to make any observational distinction between geocentric and heliocentric universes. (Parallax effects are far too small to be noticeable with the naked eye.) ...
Chandra Characterization of X-ray Emission in the Young F
... The total program observing time was 39 ksec, and the total on-target observing time was 37.3 ksec, in which 1509 total raw photons were detected using a source extraction radius of 20ʺ and an energy filter in the range 0.3-2.0 keV. The extraction region was centered halfway between the two resolved ...
... The total program observing time was 39 ksec, and the total on-target observing time was 37.3 ksec, in which 1509 total raw photons were detected using a source extraction radius of 20ʺ and an energy filter in the range 0.3-2.0 keV. The extraction region was centered halfway between the two resolved ...
– 1 – 1. Galaxy Observations 1.1.
... proceeds to use the above characterizations to study the relations between stellar mass, star formation history, size, and internal structure (concentration of light and surface mass density) in low redshift SDSS galaxies. Many of these trends (for example, that lower mass galaxies have younger stel ...
... proceeds to use the above characterizations to study the relations between stellar mass, star formation history, size, and internal structure (concentration of light and surface mass density) in low redshift SDSS galaxies. Many of these trends (for example, that lower mass galaxies have younger stel ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.