Astronomy Astrophysics
... The VIRCAM (VISTA Infrared CAMera; Dalton et al. 2006) is a 16 detector-array infrared camera that samples 1.65 deg2 . Each 2048 × 2048 detector is sensitive over λ = 0.8–2.5 μm and delivers images with an average pixel scale of 0.34 arcsec px−1 . A single exposure corresponds to a patchy individual ...
... The VIRCAM (VISTA Infrared CAMera; Dalton et al. 2006) is a 16 detector-array infrared camera that samples 1.65 deg2 . Each 2048 × 2048 detector is sensitive over λ = 0.8–2.5 μm and delivers images with an average pixel scale of 0.34 arcsec px−1 . A single exposure corresponds to a patchy individual ...
Astronomy Astrophysics Gaia-ESO Survey: The analysis of high-resolution The
... box is defined in a color-magnitude diagram with limits 12 < J < 14 and 0.23 < (J − K) < 0.45 + 0.5 × E(B − V). The Schlegel et al. (1998) maps are used to determine the extinction E(B − V). The targets selected before April 2012 had a brightest cut on J = 11 instead of 12. When there were not enoug ...
... box is defined in a color-magnitude diagram with limits 12 < J < 14 and 0.23 < (J − K) < 0.45 + 0.5 × E(B − V). The Schlegel et al. (1998) maps are used to determine the extinction E(B − V). The targets selected before April 2012 had a brightest cut on J = 11 instead of 12. When there were not enoug ...
X-Ray Spectroscopy of Stars
... High-resolution X-ray spectroscopy has been provided by grating instruments on the XMM-Newton and C HANDRA X-ray observatories which both were launched in 1999. Their broad wavelength coverage (0.07-15 keV), effective areas (up to ≈ 200 cm2 ) and their impressive spectral resolving power (up to ≈ 10 ...
... High-resolution X-ray spectroscopy has been provided by grating instruments on the XMM-Newton and C HANDRA X-ray observatories which both were launched in 1999. Their broad wavelength coverage (0.07-15 keV), effective areas (up to ≈ 200 cm2 ) and their impressive spectral resolving power (up to ≈ 10 ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... Much of the recent success in finding new Local Group members is due to the availability of the many largescale photographic surveys of the sky carried out since the seminal Palomar Sky Survey of the 1950s. Soon after these surveys were begun, visual searches of the photographic plates identified ne ...
... Much of the recent success in finding new Local Group members is due to the availability of the many largescale photographic surveys of the sky carried out since the seminal Palomar Sky Survey of the 1950s. Soon after these surveys were begun, visual searches of the photographic plates identified ne ...
148 Jun - British Astronomical Association
... system with the stars separated though still quite close. It appears that the orbit of the eclipsing stars is ellipitical as the secondary minimum does not occur at 0.5 of the system’s phase. RX Herculis is roughly midway between Rasalhague and Altair. AK Herculis Although this system is not on our ...
... system with the stars separated though still quite close. It appears that the orbit of the eclipsing stars is ellipitical as the secondary minimum does not occur at 0.5 of the system’s phase. RX Herculis is roughly midway between Rasalhague and Altair. AK Herculis Although this system is not on our ...
Book Describing Techniques to Detect Transiting ExoPlanets
... of a regular telephoto camera lens attached to an astronomer’s CDD, monitors a set of star fields for several months before moving on to another set of star fields. When a star appears to fade by a small amount for a short time (e.g., <0.030 magnitude for ~3 hours), and when these fading events occu ...
... of a regular telephoto camera lens attached to an astronomer’s CDD, monitors a set of star fields for several months before moving on to another set of star fields. When a star appears to fade by a small amount for a short time (e.g., <0.030 magnitude for ~3 hours), and when these fading events occu ...
Digital Universe Guide - American Museum of Natural History
... Partiview’s graphical user interface (GUI) was written to be simple and compact. However, for a new user, parts of the interface may seem cryptic. The buttons, sliders, and menus are designed to make navigation, data manipulation, and data group toggling effortless, but they result in an interface t ...
... Partiview’s graphical user interface (GUI) was written to be simple and compact. However, for a new user, parts of the interface may seem cryptic. The buttons, sliders, and menus are designed to make navigation, data manipulation, and data group toggling effortless, but they result in an interface t ...
the stebbins galaxy: the origins of interstellar medium studies
... form a symmetric halo around the center of the Galaxy, their apparent distribution in our sky and, critically, their distances tell us that the Sun is far from that center, which must lie roughly in the direction of the constellation Sagittarius. This was a most important result and a transformative ...
... form a symmetric halo around the center of the Galaxy, their apparent distribution in our sky and, critically, their distances tell us that the Sun is far from that center, which must lie roughly in the direction of the constellation Sagittarius. This was a most important result and a transformative ...
The CCD Photometric Calibration Cookbook
... Cape photographic Dm data about such magnitudes are contained for all the stars south of declination , down to about 9.5, together with a great mass of fainter ones. The difficulty of reducing all these magnitudes to one and the same homogeneous and rational scale has however, not been altogether ov ...
... Cape photographic Dm data about such magnitudes are contained for all the stars south of declination , down to about 9.5, together with a great mass of fainter ones. The difficulty of reducing all these magnitudes to one and the same homogeneous and rational scale has however, not been altogether ov ...
X-ray astronomy of stellar coronae (Review)
... evolution predict that the young Zero-Age Main-Sequence (ZAMS) Sun was fainter by ≈ 25% than at present, stellar X-ray astronomy has revealed that the solar high-energy emission was likely to be hundreds of times more intense at such young ages. The increased level of ionizing and UV radiation must ...
... evolution predict that the young Zero-Age Main-Sequence (ZAMS) Sun was fainter by ≈ 25% than at present, stellar X-ray astronomy has revealed that the solar high-energy emission was likely to be hundreds of times more intense at such young ages. The increased level of ionizing and UV radiation must ...
A Variability Study of the Typical Red Supergiant Antares A
... many of the features of this variability have been associated with large convective cells. Unfortunately, due to the long timescales of these variations they are not well studied, with the exception of the bright M-class supergiant Betelgeuse (α Orionis, M2 Iab). Betelgeuse has been well studied bot ...
... many of the features of this variability have been associated with large convective cells. Unfortunately, due to the long timescales of these variations they are not well studied, with the exception of the bright M-class supergiant Betelgeuse (α Orionis, M2 Iab). Betelgeuse has been well studied bot ...
Introduction_to_pulsar_astronomy
... The repetition rates imply that the source is very compact. A star pulsating with a period of 0.25 seconds cannot be larger than 0.25 x c (of 75.000 km). This is confirmed by radio scintillation: extended objects do not scintillate, pulsars scintillate a lot. Is the fundamental periodicity caused by ...
... The repetition rates imply that the source is very compact. A star pulsating with a period of 0.25 seconds cannot be larger than 0.25 x c (of 75.000 km). This is confirmed by radio scintillation: extended objects do not scintillate, pulsars scintillate a lot. Is the fundamental periodicity caused by ...
A catalogue of the Chandra Deep Field South with multi
... The spectral shapes of the objects in the R-band selected catalogue were measured with a different approach. Photometry in all 17 passbands was done by projecting the object coordinates into the frames of reference of each single exposure and measuring the object fluxes at the given locations. In or ...
... The spectral shapes of the objects in the R-band selected catalogue were measured with a different approach. Photometry in all 17 passbands was done by projecting the object coordinates into the frames of reference of each single exposure and measuring the object fluxes at the given locations. In or ...
Lab 14 Galaxy Morphology
... across a faint, fuzzy patch of light. Many of these “nebulae” (Latin for cloud-like) ...
... across a faint, fuzzy patch of light. Many of these “nebulae” (Latin for cloud-like) ...
constellations - Richmond and Glen Allen Weather
... What is a constellation? Constellation is derived from the Latin "constellatus," set with stars; from "com-," together, and "stellare," to shine; stella, a star. A constellation is a group of stars, which might form a pattern or shape within a specific area of the sky and is often named after people ...
... What is a constellation? Constellation is derived from the Latin "constellatus," set with stars; from "com-," together, and "stellare," to shine; stella, a star. A constellation is a group of stars, which might form a pattern or shape within a specific area of the sky and is often named after people ...
Article PDF - IOPscience
... ([Fe H] < -0.5 dex), pulsating horizontal branch stars with periodically variable light curves (periods ranging from 0.2 to 0.9 days; Smith 2004). They are bright stars (MV = 0.6 0.1 mag) with distinct light curves, which makes them easy to identify with time-domain imaging surveys, even to large ...
... ([Fe H] < -0.5 dex), pulsating horizontal branch stars with periodically variable light curves (periods ranging from 0.2 to 0.9 days; Smith 2004). They are bright stars (MV = 0.6 0.1 mag) with distinct light curves, which makes them easy to identify with time-domain imaging surveys, even to large ...
Astronomy Astrophysics - Niels Bohr Institutet
... The resulting data set should place a wide range of studies of the evolution of the Galactic disk on a new and considerably improved footing. We caution, however, that no such thing as a fully unbiased sample exists in Galactic astronomy, and the reader is strongly urged to carefully study Sect. 5, ...
... The resulting data set should place a wide range of studies of the evolution of the Galactic disk on a new and considerably improved footing. We caution, however, that no such thing as a fully unbiased sample exists in Galactic astronomy, and the reader is strongly urged to carefully study Sect. 5, ...
The Ages of Stars
... • Many gas-giant planets have now been found around nearby solar-type stars. We can estimate rough ages for those stars, but a better understanding of, for instance, the dynamics of such systems and the inward migration of planets requires accurate ages. • We could better understand the behavior and ...
... • Many gas-giant planets have now been found around nearby solar-type stars. We can estimate rough ages for those stars, but a better understanding of, for instance, the dynamics of such systems and the inward migration of planets requires accurate ages. • We could better understand the behavior and ...
Galaxies - WordPress.com
... A an enormous luminous cloud of gas and dust in the interstellar space. B a collection of planets with a parent star similar to the solar system. C a collection of hundreds of billions of stars sometimes called a galaxy. D a figment of the imagination of early astronomers like, the "seas" of the moo ...
... A an enormous luminous cloud of gas and dust in the interstellar space. B a collection of planets with a parent star similar to the solar system. C a collection of hundreds of billions of stars sometimes called a galaxy. D a figment of the imagination of early astronomers like, the "seas" of the moo ...
X. Nuclear star clusters in low-mass early-type galaxies
... sizes of the NSCs, although not without some uncertainty, since also a widely accepted theory for the formation of GCs is still lacking. Bekki et al. (2004) present scaling relations for the sizes of NSCs based on N-body simulations of the merging of equal-mass star clusters; however, they do not pr ...
... sizes of the NSCs, although not without some uncertainty, since also a widely accepted theory for the formation of GCs is still lacking. Bekki et al. (2004) present scaling relations for the sizes of NSCs based on N-body simulations of the merging of equal-mass star clusters; however, they do not pr ...
Stars, Galaxies, and Beyond
... I have prepared this summary to assist in learning some of the materials relevant to the courses named. These 300–level (junior) college courses have provided a satisfying opportunity to take a more detailed but still manageable look at astronomy and astrophysics applying to space well beyond the so ...
... I have prepared this summary to assist in learning some of the materials relevant to the courses named. These 300–level (junior) college courses have provided a satisfying opportunity to take a more detailed but still manageable look at astronomy and astrophysics applying to space well beyond the so ...
Spitzer Spectroscopy of Circumstellar Disks in the 5 Myr Old Upper
... the collision of planetesimals. Of particular interest, none of the ∼30 F or G-type stars (1.2– 1.8 M⊙ ) included in the Spitzer survey exhibit infrared excess emission at wavelengths <16 µm. These results imply that the mechanisms responsible for disk dispersal operate more efficiently for high mas ...
... the collision of planetesimals. Of particular interest, none of the ∼30 F or G-type stars (1.2– 1.8 M⊙ ) included in the Spitzer survey exhibit infrared excess emission at wavelengths <16 µm. These results imply that the mechanisms responsible for disk dispersal operate more efficiently for high mas ...
Corona Australis
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.