Epsilon Aurigae: a rare stellar eclipse - Project VS
... Flat-bottomed eclipses of 2-years duration and their depth (2.9 to 3.8) optically suggest that the cold disk covers half the surface area of the F star (Huang 1965). A lot of information was collected during the eclipse of 1982 -1984. At the end of the campaign, in 1985 a workshop was held at the Am ...
... Flat-bottomed eclipses of 2-years duration and their depth (2.9 to 3.8) optically suggest that the cold disk covers half the surface area of the F star (Huang 1965). A lot of information was collected during the eclipse of 1982 -1984. At the end of the campaign, in 1985 a workshop was held at the Am ...
Infrared Astronomy
... 1. Introduction – the discovery and use of infrared ............................................................................... 1 1.1 Herschel and his discovery of infrared ................................................................................... 1 1.2 Black body radiation – the first ...
... 1. Introduction – the discovery and use of infrared ............................................................................... 1 1.1 Herschel and his discovery of infrared ................................................................................... 1 1.2 Black body radiation – the first ...
Comprehensive search for natural satellites of Vesta by the Dawn
... motion. For these image sets, the stars are fixed in the frame while Vesta moves. If a satellite were present it would be noticed by its motion relative to stationary stars. This search technique was more useful than the Motion-Vesta technique until Dawn was nearer Vesta. At close range, the star fiel ...
... motion. For these image sets, the stars are fixed in the frame while Vesta moves. If a satellite were present it would be noticed by its motion relative to stationary stars. This search technique was more useful than the Motion-Vesta technique until Dawn was nearer Vesta. At close range, the star fiel ...
Revising the census of low luminosity AGN
... A LOW EW (~1 Å) IS CHARACTERISTIC OF STELLAR PROCESSES AGN 10 - Roma 10/09/2012 ...
... A LOW EW (~1 Å) IS CHARACTERISTIC OF STELLAR PROCESSES AGN 10 - Roma 10/09/2012 ...
12 Introduction to Cepheid Variable Stars Exercise
... Miss Henrietta Leavitt (1868 - 1921), working at the Harvard Observatory, determined the apparent magnitude and periods of 25 cepheid variables in the Large and Small Magellanic Clouds. Miss Leavitt noted that when the cepheids were ordered by increasing period that the variable stars were also orde ...
... Miss Henrietta Leavitt (1868 - 1921), working at the Harvard Observatory, determined the apparent magnitude and periods of 25 cepheid variables in the Large and Small Magellanic Clouds. Miss Leavitt noted that when the cepheids were ordered by increasing period that the variable stars were also orde ...
astronomical objects detection-paper-06-25-2014
... and applied this method for the segmentation of regions of interest in images. Later, Mangan & Whitaker (1999) found a new application of watersheds to partition 3D surfaces meshes for improved rendering. Inspired by this approach, we present a novel non-linear partitioning method which divides an i ...
... and applied this method for the segmentation of regions of interest in images. Later, Mangan & Whitaker (1999) found a new application of watersheds to partition 3D surfaces meshes for improved rendering. Inspired by this approach, we present a novel non-linear partitioning method which divides an i ...
PP Chapter 28 Text
... Life cycle of stars: • Begins as a nebula • Advances to a protostar • Becomes a star when fusion in its core occurs Depending on its mass, the star may become a red giant and then burn out to become a white dwarf. ...
... Life cycle of stars: • Begins as a nebula • Advances to a protostar • Becomes a star when fusion in its core occurs Depending on its mass, the star may become a red giant and then burn out to become a white dwarf. ...
DUSTiNGS III: Distribution of Intermediate
... et al. (2005). All observations that are part of the DUSTiNGS program had a combined exposure time from epochs 1 and 2 of 1080 sec with a 5σ sensitivity limit of 1.6 µJy. Epoch 0 observations consist of archival data for three of our selected sample which were processed in a uniform manner as Epochs ...
... et al. (2005). All observations that are part of the DUSTiNGS program had a combined exposure time from epochs 1 and 2 of 1080 sec with a 5σ sensitivity limit of 1.6 µJy. Epoch 0 observations consist of archival data for three of our selected sample which were processed in a uniform manner as Epochs ...
comet panstarrs
... night sky. The brightening trend continues to speed up so that by mid-February, Comet PANSTARRS should be an unaided eye “fuzzy” located in the vicinity of the southern constellation of Microscopium. As it dives toward the Sun, it will move into the constellation of Pisces, easily visible in the S ...
... night sky. The brightening trend continues to speed up so that by mid-February, Comet PANSTARRS should be an unaided eye “fuzzy” located in the vicinity of the southern constellation of Microscopium. As it dives toward the Sun, it will move into the constellation of Pisces, easily visible in the S ...
FIRST STELLAR ABUNDANCES IN THE DWARF IRREGULAR
... evolution of more distant galaxies to date (Matteucci & Tosi 1985). So far, only a very limited number of elements can be examined and quantified when using this approach. The chemical evolution of a galaxy depends on the contributions of all its constituents, e.g., SNe type Ia and II, high mass sta ...
... evolution of more distant galaxies to date (Matteucci & Tosi 1985). So far, only a very limited number of elements can be examined and quantified when using this approach. The chemical evolution of a galaxy depends on the contributions of all its constituents, e.g., SNe type Ia and II, high mass sta ...
Axisymmetry in protoplanetary nebulae: using imaging polarimetry
... the core of the surface brightness image is quite centrally peaked in both wavebands (Table 1), the J-band image shows evidence for a diffuse halo that extends to the NE of 1710623046 and encompasses the faint source found there. This source appears to be a faint star and may be in association with ...
... the core of the surface brightness image is quite centrally peaked in both wavebands (Table 1), the J-band image shows evidence for a diffuse halo that extends to the NE of 1710623046 and encompasses the faint source found there. This source appears to be a faint star and may be in association with ...
THE OFFSET AND HOST LIGHT DISTRIBUTIONS OF LONG
... present our measurements. In Section 4 we present our resulting offset and fractional flux distributions, and in ...
... present our measurements. In Section 4 we present our resulting offset and fractional flux distributions, and in ...
Galileo`s miraculous year: 1609 and the revolutionary telescope
... notebooks have been identified that suggest Galileo was aware of the possibility of a new planet. If Galileo had used his observations to propose the discovery of a new planet, it would have been the first time a planet had been discovered by humanity since deep antiquity, and would be without precede ...
... notebooks have been identified that suggest Galileo was aware of the possibility of a new planet. If Galileo had used his observations to propose the discovery of a new planet, it would have been the first time a planet had been discovered by humanity since deep antiquity, and would be without precede ...
here - NASA/IPAC Extragalactic Database
... standards have been defined. Even a high-luminosity O star in the SMC may fail to show He II λ4686 and be labeled a “giant” or even a “dwarf”, when its absolute visual magnitude demonstrates it’s a supergiant; see discussion in Massey et al. (2005b). The other thing to keep in mind about the evoluti ...
... standards have been defined. Even a high-luminosity O star in the SMC may fail to show He II λ4686 and be labeled a “giant” or even a “dwarf”, when its absolute visual magnitude demonstrates it’s a supergiant; see discussion in Massey et al. (2005b). The other thing to keep in mind about the evoluti ...
Astronomy 112 - Solar Physics and Space Weather
... Mons, a massive volcano many times larger than the Island of Hawaii. Olympus Mons is only one of four huge volcanoes in a 3000 km-wide region called Tharsis. These volcanoes erupted repeatedly over many millions of years, growing higher with each lava flow. Enormous collapsed calderas are found on t ...
... Mons, a massive volcano many times larger than the Island of Hawaii. Olympus Mons is only one of four huge volcanoes in a 3000 km-wide region called Tharsis. These volcanoes erupted repeatedly over many millions of years, growing higher with each lava flow. Enormous collapsed calderas are found on t ...
IAC_L2_thindisk
... So far, radial migration is a theoretical concept: we do not know how important it is in reality. It could move metal-rich stars from the inner galaxy out to the outer galaxy, and invert the abundance gradient. z ...
... So far, radial migration is a theoretical concept: we do not know how important it is in reality. It could move metal-rich stars from the inner galaxy out to the outer galaxy, and invert the abundance gradient. z ...
MEarth
... There are two issues that help compensate for the sparse cadence. Firstly, typical levels and timescales of correlated noise in photometric surveys (see, e.g., Pont et al. 2006) suppress the benefit of dense time sampling such that the “standard” N 1=2 improvement in precision generally does not ap ...
... There are two issues that help compensate for the sparse cadence. Firstly, typical levels and timescales of correlated noise in photometric surveys (see, e.g., Pont et al. 2006) suppress the benefit of dense time sampling such that the “standard” N 1=2 improvement in precision generally does not ap ...
Chemical abundances and winds of massive stars in M31: a Btype
... The CCD frames were reduced to wavelength-calibrated spectra using the IRAF reduction system.1 Standard procedures were used to bias correct and flat field the stellar images. There is considerable background Balmer line emission from the nebular region of OB 10, which can vary over small spatial sc ...
... The CCD frames were reduced to wavelength-calibrated spectra using the IRAF reduction system.1 Standard procedures were used to bias correct and flat field the stellar images. There is considerable background Balmer line emission from the nebular region of OB 10, which can vary over small spatial sc ...
Catch an Asteroid - Odysseus Contest
... international student project. Using the astronomical software Astrometrica we found the asteroid in each image and measured its ascension and declination. After this we prepared a report for the Minor Planet Center in Harvard. We send it there, where all the astronomical observations are gathered – ...
... international student project. Using the astronomical software Astrometrica we found the asteroid in each image and measured its ascension and declination. After this we prepared a report for the Minor Planet Center in Harvard. We send it there, where all the astronomical observations are gathered – ...
Galaxy Assembly through Mergers
... larger structures are built from smaller ones, more massive galaxies can then be assembled from less massive galaxies, thus contributing to shape the galaxy mass function. However, disentangling the role of mergers in the build up of this mass function is a complex process, not only due to the short ...
... larger structures are built from smaller ones, more massive galaxies can then be assembled from less massive galaxies, thus contributing to shape the galaxy mass function. However, disentangling the role of mergers in the build up of this mass function is a complex process, not only due to the short ...
IAU GA, Prague, Aug 2006 - Spanish Virtual Observatory
... star-formation regions (e.g Taurus-Auriga). Depending on the ejection velocity BDs may have travelled far from their birth sites and not revealed by the previously mentioned surveys. Check the ejection model by cross-correlating IPHAS and 2MASS to search young BD by their Hα emission and IR colo ...
... star-formation regions (e.g Taurus-Auriga). Depending on the ejection velocity BDs may have travelled far from their birth sites and not revealed by the previously mentioned surveys. Check the ejection model by cross-correlating IPHAS and 2MASS to search young BD by their Hα emission and IR colo ...
Hubble Deep Field
The Hubble Deep Field (HDF) is an image of a small region in the constellation Ursa Major, constructed from a series of observations by the Hubble Space Telescope. It covers an area 2.5 arcminutes across, about one 24-millionth of the whole sky, which is equivalent in angular size to a 65 mm tennis ball at a distance of 100 metres. The image was assembled from 342 separate exposures taken with the Space Telescope's Wide Field and Planetary Camera 2 over ten consecutive days between December 18 and December 28, 1995.The field is so small that only a few foreground stars in the Milky Way lie within it; thus, almost all of the 3,000 objects in the image are galaxies, some of which are among the youngest and most distant known. By revealing such large numbers of very young galaxies, the HDF has become a landmark image in the study of the early universe, with the associated scientific paper having received over 900 citations by the end of 2014.Three years after the HDF observations were taken, a region in the south celestial hemisphere was imaged in a similar way and named the Hubble Deep Field South. The similarities between the two regions strengthened the belief that the universe is uniform over large scales and that the Earth occupies a typical region in the Universe (the cosmological principle). A wider but shallower survey was also made as part of the Great Observatories Origins Deep Survey. In 2004 a deeper image, known as the Hubble Ultra-Deep Field (HUDF), was constructed from a few months of light exposure. The HUDF image was at the time the most sensitive astronomical image ever made at visible wavelengths, and it remained so until the Hubble Extreme Deep Field (XDF) was released in 2012.