The Extragalactic Group of MPE and USM
... • Advantage of photo z: no color selection bias, fainter luminosities, larger sample (~10000 galaxies in FDF and GOODS S sub-sample) • FORS Deep Field (IAB=26.8): 98% of all galaxies with dz/(1+z)<0.03; GOODS S (KAB=25.4): dz/(1+z)<0.055 • Deep I-selection misses only a small fraction of deep K sele ...
... • Advantage of photo z: no color selection bias, fainter luminosities, larger sample (~10000 galaxies in FDF and GOODS S sub-sample) • FORS Deep Field (IAB=26.8): 98% of all galaxies with dz/(1+z)<0.03; GOODS S (KAB=25.4): dz/(1+z)<0.055 • Deep I-selection misses only a small fraction of deep K sele ...
Here`s - Abrams Planetarium
... Moon’s bright edge and reappear at the dark edge between 10:05 p.m. and 11:46 p.m. (telescope needed). By 1:41 a.m. EDT, the sunlit edge of the Moon will cover firstmagnitude Aldebaran, eye of Taurus, the Bull. Aldebaran remains hidden by the Moon until 2:27 a.m., when the star reappears at the Moon ...
... Moon’s bright edge and reappear at the dark edge between 10:05 p.m. and 11:46 p.m. (telescope needed). By 1:41 a.m. EDT, the sunlit edge of the Moon will cover firstmagnitude Aldebaran, eye of Taurus, the Bull. Aldebaran remains hidden by the Moon until 2:27 a.m., when the star reappears at the Moon ...
Doppler imaging of stellar surfaces
... rise to doubts about the reliability of specific types of features. The potential for generating artifacts in DI reconstructions have led some of us to run tests comparing the reconstruction of images from artificial data, where incorrect parameters have been used in the reconstruction, with the ori ...
... rise to doubts about the reliability of specific types of features. The potential for generating artifacts in DI reconstructions have led some of us to run tests comparing the reconstruction of images from artificial data, where incorrect parameters have been used in the reconstruction, with the ori ...
powerpoint - High Energy Physics at Wayne State
... Astronomy is a Time Machine When we observe a star that is 100 light-years distant, then the light took 100 years to reach us. We are seeing it as it was 100 years ago. The nearest galaxy is about a million light-years from Earth. We see it as it was 1 million years ago. The most distant objects ob ...
... Astronomy is a Time Machine When we observe a star that is 100 light-years distant, then the light took 100 years to reach us. We are seeing it as it was 100 years ago. The nearest galaxy is about a million light-years from Earth. We see it as it was 1 million years ago. The most distant objects ob ...
Notes on Stars
... distances up to 10 pc can me measured with about 10% accruacy, the Hipparcos-satellite derived distances up to 1kpc (in orbit there are no disturbing effects of the earth’s atmosphere like seeing and deflection!). ...
... distances up to 10 pc can me measured with about 10% accruacy, the Hipparcos-satellite derived distances up to 1kpc (in orbit there are no disturbing effects of the earth’s atmosphere like seeing and deflection!). ...
Fast Auto-Focus Method and Software for CCD
... In a typical run the telescope can be routinely brought to focus in only one minute with a LX200, ST-8E system. The process is: 1. A non-precision move of the focuser is made to a point that is known to be sufficiently far from Best Focus (user selected inside or outside of Best Focus) 2. A full fra ...
... In a typical run the telescope can be routinely brought to focus in only one minute with a LX200, ST-8E system. The process is: 1. A non-precision move of the focuser is made to a point that is known to be sufficiently far from Best Focus (user selected inside or outside of Best Focus) 2. A full fra ...
Fast Auto-Focus Method and Software for CCD-based
... waist. The measured left and right sides of the V Curve are delightfully linear with slopes that depend only on the hardware characteristics such as the optics fnumber, the CCD pixel size and the focuser gear ratios. We have found these slopes to be remarkably constant over temperature and time. The ...
... waist. The measured left and right sides of the V Curve are delightfully linear with slopes that depend only on the hardware characteristics such as the optics fnumber, the CCD pixel size and the focuser gear ratios. We have found these slopes to be remarkably constant over temperature and time. The ...
Homework Assignment 6 — Solutions
... at the low temperature end to NII /Nt ≈ 1 at the high temperature end, with a transition at temperatures where b ≈ 1 (in fact, NII /Nt = 0.5 when b = 0.5). Looking at the plot, we see that these predictions are correct—the transition from fully neutral to fully ionized happens at a temperature of ab ...
... at the low temperature end to NII /Nt ≈ 1 at the high temperature end, with a transition at temperatures where b ≈ 1 (in fact, NII /Nt = 0.5 when b = 0.5). Looking at the plot, we see that these predictions are correct—the transition from fully neutral to fully ionized happens at a temperature of ab ...
Preview Sample 2
... 4) Suppose that you live in Sydney, Australia (latitude 34°S). Describe the path of the Sun through your sky for each of the following days: a. the day of the spring equinox b. the day of the summer solstice c. the day of the winter solstice Answer: a. On the vernal equinox, the Sun rises due east, ...
... 4) Suppose that you live in Sydney, Australia (latitude 34°S). Describe the path of the Sun through your sky for each of the following days: a. the day of the spring equinox b. the day of the summer solstice c. the day of the winter solstice Answer: a. On the vernal equinox, the Sun rises due east, ...
Red supergiants around the obscured open cluster Stephenson 2
... visitor mode). AF2 uses 150 science fibres with diameter 1.′′ 6, and 10 fiducial bundles for acquisition and guiding. Fibres can be positioned over a field of radius 30′ , though there is some vignetting starting at r = 20′ , and image quality outside r = 25′ ...
... visitor mode). AF2 uses 150 science fibres with diameter 1.′′ 6, and 10 fiducial bundles for acquisition and guiding. Fibres can be positioned over a field of radius 30′ , though there is some vignetting starting at r = 20′ , and image quality outside r = 25′ ...
Life Histories Of Some Stars
... all? Describe the shape of the graph? Is it a straight line? A curve? 5. Give each group the list of stars attached and the HR diagram attached. Instead of height and weight, the information is in Luminosity (compared to sun) and Surface Temperature (in K). The chart also gives the star’s current st ...
... all? Describe the shape of the graph? Is it a straight line? A curve? 5. Give each group the list of stars attached and the HR diagram attached. Instead of height and weight, the information is in Luminosity (compared to sun) and Surface Temperature (in K). The chart also gives the star’s current st ...
The Formation of High Mass Stars
... (Diffuse clouds such as Taurus, Perseus and Ophiuchus; typical galactic massive star forming regions; extra-galactic super star clusters) • Surface density determines effectiveness of trapping radiation and accretion luminosities of forming stars (Krumholz, McKee 2008) • As surface density increases ...
... (Diffuse clouds such as Taurus, Perseus and Ophiuchus; typical galactic massive star forming regions; extra-galactic super star clusters) • Surface density determines effectiveness of trapping radiation and accretion luminosities of forming stars (Krumholz, McKee 2008) • As surface density increases ...
28.2 Calculating Luminosity
... describes how much light is coming from the star each second. Luminosity can be measured in watts (W). Measuring the luminosity of something as far away as a star is difficult to do. However, we can measure its brightness. Brightness describes the amount of the star’s light that reaches a square met ...
... describes how much light is coming from the star each second. Luminosity can be measured in watts (W). Measuring the luminosity of something as far away as a star is difficult to do. However, we can measure its brightness. Brightness describes the amount of the star’s light that reaches a square met ...
1. INTRODUCTION - Institut für Theoretische Astrophysik
... We calculate time-dependent models of acoustically heated chromospheres for main-sequence stars between spectral type F0 V and M0 V and for two giants of spectral type K0 III and K5 III assuming monochromatic waves. The hydrodynamic equations are solved together with the radiative transfer and stati ...
... We calculate time-dependent models of acoustically heated chromospheres for main-sequence stars between spectral type F0 V and M0 V and for two giants of spectral type K0 III and K5 III assuming monochromatic waves. The hydrodynamic equations are solved together with the radiative transfer and stati ...
First Census of Galaxies Near Cosmic Dawn The Night Sky
... First Census of Galaxies Near Cosmic Dawn ...
... First Census of Galaxies Near Cosmic Dawn ...
The High Resolution Camera CXC Newsletter
... or outbursting (with subclasses short vs. long outbursts and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supernova remnants, one of which is a new candidate, and also ...
... or outbursting (with subclasses short vs. long outbursts and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supernova remnants, one of which is a new candidate, and also ...
Ursa Minor
Ursa Minor (Latin: ""Smaller She-Bear"", contrasting with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the name Little Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, due to Polaris being the North Star.Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from apparent magnitude 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the ""guardians of the pole star"". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered with a surface temperature of 200,000 K.