Measuring Distances to Stars – Why the weird formulae
... logarithms of the numbers. For instance, the logarithm of 100 is 2. This is the modern way of describing logarithms, they are powers of a particular base. In the case we are looking at, the base is 10. (Sometimes written Log10). What about the logarithm of 101 or 15.27? This is where the tables come ...
... logarithms of the numbers. For instance, the logarithm of 100 is 2. This is the modern way of describing logarithms, they are powers of a particular base. In the case we are looking at, the base is 10. (Sometimes written Log10). What about the logarithm of 101 or 15.27? This is where the tables come ...
A GMOS dissection of the line-of
... Statistical properties of high-z radio quasars may be more useful in determining importance of lensing ...
... Statistical properties of high-z radio quasars may be more useful in determining importance of lensing ...
Conference Abstract Booklet here.
... The era of large-scale photometric variability surveys began a quarter of a century ago, when three microlensing projects - EROS, MACHO, and OGLE - started their operation. These surveys initiated a revolution in the field of variable stars and in the next years they inspired many new observational ...
... The era of large-scale photometric variability surveys began a quarter of a century ago, when three microlensing projects - EROS, MACHO, and OGLE - started their operation. These surveys initiated a revolution in the field of variable stars and in the next years they inspired many new observational ...
THE MONTHLY SKY GUIDE, SIXTH EDITION
... magnitude, and so on. The faintest objects that can be detected by telescopes on Earth are about magnitude 25. ...
... magnitude, and so on. The faintest objects that can be detected by telescopes on Earth are about magnitude 25. ...
3. Cosmology and the Origin and Evolution of Galaxies
... ing whether broad continuum features in the spectral energy distributions (SEDs) of mm galaxies at rest-frame mid-IR to radio wavelengths can provide photometric-redshifts with sufficient accuracy7. There has also been some success in the measurement of optical and IR spectroscopic redshifts for a fr ...
... ing whether broad continuum features in the spectral energy distributions (SEDs) of mm galaxies at rest-frame mid-IR to radio wavelengths can provide photometric-redshifts with sufficient accuracy7. There has also been some success in the measurement of optical and IR spectroscopic redshifts for a fr ...
12-1 - Piscataway High School
... The distances to stars are so large that it is not convenient to use astronomical units. As Reasoning with Numbers 12-1 explains, when you measure distance via parallax, it is convenient to use the unit of distance called a parsec (pc). The word parsec was created by combining parallax and second of ...
... The distances to stars are so large that it is not convenient to use astronomical units. As Reasoning with Numbers 12-1 explains, when you measure distance via parallax, it is convenient to use the unit of distance called a parsec (pc). The word parsec was created by combining parallax and second of ...
Exposing the hidden white dwarf binary origin by means of a
... when compared with the local WD sample of much improved completeness (HOS, d < 13 pc) than there should be when considering a pure single-star population. The question of total WD numbers and completeness of any observed sample is much related to the temperature distribution of the WDs, since the ol ...
... when compared with the local WD sample of much improved completeness (HOS, d < 13 pc) than there should be when considering a pure single-star population. The question of total WD numbers and completeness of any observed sample is much related to the temperature distribution of the WDs, since the ol ...
Do We Know of Any Maunder Minimum Stars?
... stars, S = 0.1451. Zhang et al. (1994) applied this value to an analysis of the effects of stellar activity on brightness and concluded that the Sun was 0.2 − 0.6% dimmer during the Maunder Minimum. However, most Maunder minimum candidates were identified before the advent of accurate parallaxes fro ...
... stars, S = 0.1451. Zhang et al. (1994) applied this value to an analysis of the effects of stellar activity on brightness and concluded that the Sun was 0.2 − 0.6% dimmer during the Maunder Minimum. However, most Maunder minimum candidates were identified before the advent of accurate parallaxes fro ...
Lab 4 Parallax Measurements and Determining
... and then your left eye (you may want to close or cover the other eye as you make the measurements). Your eyes, the thin object, and the parallax ruler should all lie in a line roughly 6 inches above the ground. You assistant will help you to measure the number of inches on the parallax ruler by whic ...
... and then your left eye (you may want to close or cover the other eye as you make the measurements). Your eyes, the thin object, and the parallax ruler should all lie in a line roughly 6 inches above the ground. You assistant will help you to measure the number of inches on the parallax ruler by whic ...
Luminosities and mass-loss rates of SMC and LMC AGB stars and
... shortward of 11.3 μm, and these are better fitted with the constants of Borghesi et al. Section 5.4.1 discusses this point further. Speck et al. also proposed that graphite rather then amorphous carbon dominates the dust, at least in the C-stars with extreme mass-loss rates they considered. Only one ...
... shortward of 11.3 μm, and these are better fitted with the constants of Borghesi et al. Section 5.4.1 discusses this point further. Speck et al. also proposed that graphite rather then amorphous carbon dominates the dust, at least in the C-stars with extreme mass-loss rates they considered. Only one ...
1998 - Universitäts-Sternwarte München
... stellar wind of giant stars, the occurrence of planetary nebulae, or the very spectacular supernova events. Nowadays, it is therefore no surprise that the ancient stars of the Galactic halo are found to be metal-poor objects – as opposed to the understanding when they were first analyzed in the 1950 ...
... stellar wind of giant stars, the occurrence of planetary nebulae, or the very spectacular supernova events. Nowadays, it is therefore no surprise that the ancient stars of the Galactic halo are found to be metal-poor objects – as opposed to the understanding when they were first analyzed in the 1950 ...
File
... The last and final star is called the Alpheratz. This connects all three stars of Pegasus. It is the most prominent in the sky towards the end of Summer and through Autumn for the northern latitudes. ...
... The last and final star is called the Alpheratz. This connects all three stars of Pegasus. It is the most prominent in the sky towards the end of Summer and through Autumn for the northern latitudes. ...
Compare/Order Decimals
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
Stellar populations in the nuclear regions of nearby radio galaxies
... respectively. This configuration provides the spectral resolution necessary to resolve the Mg b and CaT features and, at the same at 5.1-Å time, offers a wide spectral span: l3350–6000 A at 3.5-Å resolution in resolution in the blue and l7900–9400 A the red. In the 1997 run, in which we assess ...
... respectively. This configuration provides the spectral resolution necessary to resolve the Mg b and CaT features and, at the same at 5.1-Å time, offers a wide spectral span: l3350–6000 A at 3.5-Å resolution in resolution in the blue and l7900–9400 A the red. In the 1997 run, in which we assess ...
The Nature of the Stars
... known parallax angle, 0.772 arcsec, and hence is the closest known star (other than the Sun); its distance is 1/(0.772) ⫽ 1.30 pc. ...
... known parallax angle, 0.772 arcsec, and hence is the closest known star (other than the Sun); its distance is 1/(0.772) ⫽ 1.30 pc. ...
Magnitude-range brightness variations of overactive K giants
... 50–200 K. The bolometric flux during maximum of the rotational modulation, i.e., the least spotted states, varied by up to 39% in IL Hya and up to 54% in XX Tri over the course of our observations. We emphasize that for IL Hya this is just about half of the total luminosity variation that can be exp ...
... 50–200 K. The bolometric flux during maximum of the rotational modulation, i.e., the least spotted states, varied by up to 39% in IL Hya and up to 54% in XX Tri over the course of our observations. We emphasize that for IL Hya this is just about half of the total luminosity variation that can be exp ...
bowser - Colorado Space Grant Consortium
... of altitude, wavelength, and angle from the sun • Design Description: – 64 LEDs will measure light in the red, orange, green and blue spectrum • Reasons for Choice: – LEDs do not require the use of filters in order to sense discreet wavelength ranges. – The array will produce over six million altitu ...
... of altitude, wavelength, and angle from the sun • Design Description: – 64 LEDs will measure light in the red, orange, green and blue spectrum • Reasons for Choice: – LEDs do not require the use of filters in order to sense discreet wavelength ranges. – The array will produce over six million altitu ...
preprint, pdf version - LESIA
... It is more advisable to select large TNOs as targets for stellar occultation campaigns. They usually have large apparent sizes (30 mas or more) and thus have a greater chance of a positive detection. In addition, theory indicates that larger TNOs are most likely to possess atmospheres (Elliot & Kern ...
... It is more advisable to select large TNOs as targets for stellar occultation campaigns. They usually have large apparent sizes (30 mas or more) and thus have a greater chance of a positive detection. In addition, theory indicates that larger TNOs are most likely to possess atmospheres (Elliot & Kern ...
Asteroid Rotation Periods
... of a magnitude have been used. Even higher precision can be used, but this is not justified for measurements made by the eye alone, since the accuracy is about ½mag, and this is why the magnitude scale at first had only integer values. However today with the use of electronic sensors it is possible ...
... of a magnitude have been used. Even higher precision can be used, but this is not justified for measurements made by the eye alone, since the accuracy is about ½mag, and this is why the magnitude scale at first had only integer values. However today with the use of electronic sensors it is possible ...
Clusters as laboratories for the study of galaxy evolution
... with cluster radius…It thus appears that the global cluster environment, in the form of cluster mass (Lx), has little influence on the properties of the bright cluster galaxies, whereas the local environment, in the form of galaxy density (radius), has a strong effect. Also, “Homogeneity of early-ty ...
... with cluster radius…It thus appears that the global cluster environment, in the form of cluster mass (Lx), has little influence on the properties of the bright cluster galaxies, whereas the local environment, in the form of galaxy density (radius), has a strong effect. Also, “Homogeneity of early-ty ...
PDF - ASSA
... Pillars, Globules, and Jets in the Carina Nebula [ http:// arxiv.org/abs/1502.03798 ], was published in February, containing a beautiful gallery of images and a detailed guide to the various components. The star eta Carinae is itself a splendid object: one of the most massive and brightest stellar s ...
... Pillars, Globules, and Jets in the Carina Nebula [ http:// arxiv.org/abs/1502.03798 ], was published in February, containing a beautiful gallery of images and a detailed guide to the various components. The star eta Carinae is itself a splendid object: one of the most massive and brightest stellar s ...
Carbon-enhanced metal-poor stars in dwarf galaxies
... a total metallicity of Z ≈ 6.9 × 10−7 (Caffau et al. 2011). The persistent lack of more metal-poor stars seems to confirm the idea that primordial stars were all more massive than ≈ 1M# (e.g. McKee & Tan 2008; Hosokawa et al. 2011; Hirano et al. 2014), and that their formation was possibly quenched ...
... a total metallicity of Z ≈ 6.9 × 10−7 (Caffau et al. 2011). The persistent lack of more metal-poor stars seems to confirm the idea that primordial stars were all more massive than ≈ 1M# (e.g. McKee & Tan 2008; Hosokawa et al. 2011; Hirano et al. 2014), and that their formation was possibly quenched ...
Article PDF - IOPscience
... performed with HSTphot (Dolphin 2000), a photometry package specifically designed to handle the undersampled PSF of the WFPC2/HST data. A number of initial pre-processing steps are required before running the photometry procedure. First, image defects such as bad columns and saturated pixels are ide ...
... performed with HSTphot (Dolphin 2000), a photometry package specifically designed to handle the undersampled PSF of the WFPC2/HST data. A number of initial pre-processing steps are required before running the photometry procedure. First, image defects such as bad columns and saturated pixels are ide ...
WHAT MAKES A STAR SO SPECIAL Abstract
... of the most commonly seen stars? Which stars are rarely seen? What is the relationship between the colour and the life time of stars from the main sequence? How would you explain the fact that one type of star is more common than another type of star? Which type of stars can we see and explore most ...
... of the most commonly seen stars? Which stars are rarely seen? What is the relationship between the colour and the life time of stars from the main sequence? How would you explain the fact that one type of star is more common than another type of star? Which type of stars can we see and explore most ...
Malmquist bias
The Malmquist bias is an effect in observational astronomy which leads to the preferential detection of intrinsically bright objects. It was first described in 1922 by Swedish astronomer Gunnar Malmquist (1893–1982), who then greatly elaborated upon this work in 1925. In statistics, this bias is referred to as a selection bias and affects the survey results in a brightness limited survey, where stars below a certain apparent brightness are not included. Since observed stars and galaxies appear dimmer when farther away, the brightness that is measured will fall off with distance until their brightness falls below the observational threshold. Objects which are more luminous, or intrinsically brighter, can be observed at a greater distance, creating a false trend of increasing intrinsic brightness, and other related quantities, with distance. This effect has led to many spurious claims in the field of astronomy. Properly correcting for these effects has become an area of great focus.