The Kuiper Belt Explored by Serendipitous Stellar Occultations
... The characteristic scale of the Fresnel diffraction effect (i.e., roughly speaking, the broadening of the object shadow) is the so-called Fresnel scale Fs = (λD/2) (Warner, 1988). [Note that some authors give different definitions for the Fresnel scale: (λD/2π) , (λD) , or (λD)/2 .] The Fresnel scal ...
... The characteristic scale of the Fresnel diffraction effect (i.e., roughly speaking, the broadening of the object shadow) is the so-called Fresnel scale Fs = (λD/2) (Warner, 1988). [Note that some authors give different definitions for the Fresnel scale: (λD/2π) , (λD) , or (λD)/2 .] The Fresnel scal ...
Astronomical signs of Korean tombs
... be uniform for the all Goguryeo mural star paintings. Jinpari #4 tomb is famous for 136 stars painted with gold. Although North Korean Ree (1981b) and Kim (1996) identified the stars in Jinpari #4 with Big Dipper and 28 major constellations, Park & Yang (2009) confirmed only a few stars from several ...
... be uniform for the all Goguryeo mural star paintings. Jinpari #4 tomb is famous for 136 stars painted with gold. Although North Korean Ree (1981b) and Kim (1996) identified the stars in Jinpari #4 with Big Dipper and 28 major constellations, Park & Yang (2009) confirmed only a few stars from several ...
A Budget and Accounting of Metals at z~ 0: Results from the COS
... galaxies, although it does predict too much downsizing for M⋆,0 . 109 M⊙ galaxies (i.e., it predicts that these dwarf galaxies have formed all of their stars at late times, contrary to what is observed). Fortuitously, the bulk of 9 Throughout this paper, when we refer to the mass of metals “made”, “ ...
... galaxies, although it does predict too much downsizing for M⋆,0 . 109 M⊙ galaxies (i.e., it predicts that these dwarf galaxies have formed all of their stars at late times, contrary to what is observed). Fortuitously, the bulk of 9 Throughout this paper, when we refer to the mass of metals “made”, “ ...
INSTRUCTION MANUAL
... sophisticated and easy to use telescopes available on the market today. Take time to read through this manual before embarking on your journey through the Universe. It may take a few observing sessions to become familiar with your NexStar, so you should keep this manual handy until you have fully ma ...
... sophisticated and easy to use telescopes available on the market today. Take time to read through this manual before embarking on your journey through the Universe. It may take a few observing sessions to become familiar with your NexStar, so you should keep this manual handy until you have fully ma ...
The new X-ray universe
... have confirmed that hot gas exists within groups of galaxies that have low X-ray luminosity, and in some with very low velocity dispersion. These groups are in the majority; if otherwise invisible hot gas is a general feature of them, then this may account for the bulk of the baryonic mass at this s ...
... have confirmed that hot gas exists within groups of galaxies that have low X-ray luminosity, and in some with very low velocity dispersion. These groups are in the majority; if otherwise invisible hot gas is a general feature of them, then this may account for the bulk of the baryonic mass at this s ...
Influence of the Gould Belt on Interstellar Extinction
... (2008a) but in the extinction, whose accuracy depends primarily on the accuracy of the multiband photometry used. Therefore, for this study, the stars with photometry less accurate than 0.05m at least in one of the Tycho-2 and 2MASS bands under consideration were excluded from our sample: BT , VT , ...
... (2008a) but in the extinction, whose accuracy depends primarily on the accuracy of the multiband photometry used. Therefore, for this study, the stars with photometry less accurate than 0.05m at least in one of the Tycho-2 and 2MASS bands under consideration were excluded from our sample: BT , VT , ...
here
... minutes to 24.8 arc minutes but increases in illumination from 27% to 48% during the course of the month. As the sun rises in late May, Venus will reach an altitude of about 23 degrees for observers at 40 degrees north. The brightest planet is at the descending node on May 9th. On May 22nd, Venus li ...
... minutes to 24.8 arc minutes but increases in illumination from 27% to 48% during the course of the month. As the sun rises in late May, Venus will reach an altitude of about 23 degrees for observers at 40 degrees north. The brightest planet is at the descending node on May 9th. On May 22nd, Venus li ...
Physical Properties of the Gas and Dust in the Orion B Molecular
... are located (see Goudis 1982 for a review). Their strong UV radiation field and stellar winds impinge on the “surface” of the molecular cloud form this side. The main internal heating source of L 1630 is the H II region NGC 2024 which is the second most luminous source in the Orion region and the on ...
... are located (see Goudis 1982 for a review). Their strong UV radiation field and stellar winds impinge on the “surface” of the molecular cloud form this side. The main internal heating source of L 1630 is the H II region NGC 2024 which is the second most luminous source in the Orion region and the on ...
Stars and Planets Credits and Acknowledgements
... techniques astronomers use to find planets without “seeing” them. In part 2, students learn about the discoveries of Jupiter-like planets around other stars and make scale models of several of these planetary systems to compare to our own solar system. The students are also be introduced to current ...
... techniques astronomers use to find planets without “seeing” them. In part 2, students learn about the discoveries of Jupiter-like planets around other stars and make scale models of several of these planetary systems to compare to our own solar system. The students are also be introduced to current ...
Star formation rates from young-star counts and the structure of the
... YSOs is calculated in the low-surface-density regime as they use the nth nearest neighbour centred on the detected YSOs. We further note that, given the steep dependence on SFR and the low number counts, distinguishing between a threshold and this power law is difficult and almost a matter of sema ...
... YSOs is calculated in the low-surface-density regime as they use the nth nearest neighbour centred on the detected YSOs. We further note that, given the steep dependence on SFR and the low number counts, distinguishing between a threshold and this power law is difficult and almost a matter of sema ...
Determination of accurate stellar radial
... ELODIE (Baranne et al. 1996) is an échelle spectrometer physically located in a coudé room at the 1.93 m telescope at Observatoire de Haute-Provence (OHP). For this programme, the spectrometer was fed via one optical fibre from the Cassegrain focus. The instrument FWHM is '7.2 km s−1 , correspondi ...
... ELODIE (Baranne et al. 1996) is an échelle spectrometer physically located in a coudé room at the 1.93 m telescope at Observatoire de Haute-Provence (OHP). For this programme, the spectrometer was fed via one optical fibre from the Cassegrain focus. The instrument FWHM is '7.2 km s−1 , correspondi ...
Scientific Requirements for Basic Angle Stability and Monitoring
... observed by Gaia down to 20th magnitude, 75% are fainter than 19th mag, 21% between 19th and 18th mag, and only 4% brighter than 18th mag. Potentially, they could jointly define the parallax zero point to an accuracy of about 0.2 µas. However, even a small fraction of contaminating stars could upset ...
... observed by Gaia down to 20th magnitude, 75% are fainter than 19th mag, 21% between 19th and 18th mag, and only 4% brighter than 18th mag. Potentially, they could jointly define the parallax zero point to an accuracy of about 0.2 µas. However, even a small fraction of contaminating stars could upset ...
Detection of the Stochastic Background of nHz Gravitational Radiation from Massive Black
... seeks ripples from final stages of coalescing binary MBHs and other systems: minutes time scale (milliHertz). 2003 Summer School, SLAC ...
... seeks ripples from final stages of coalescing binary MBHs and other systems: minutes time scale (milliHertz). 2003 Summer School, SLAC ...
Stars Evolution of High Mass Stars Nucleosynthesis Supernovae
... Today Stars Evolution of High Mass Stars Nucleosynthesis Supernovae - the explosive deaths of massive stars ...
... Today Stars Evolution of High Mass Stars Nucleosynthesis Supernovae - the explosive deaths of massive stars ...
GALAXIES 626
... The α-enhancement indicates that star formation in this inner disk/bulge region proceeded rapidly. The bulge structure may be younger than its stars. ...
... The α-enhancement indicates that star formation in this inner disk/bulge region proceeded rapidly. The bulge structure may be younger than its stars. ...
The spectroscopic Hertzsprung
... that the absolute brightnesses, i.e., the distances, are required to properly order the stars in the HR diagram. Order can also be achieved for stars in star clusters where the distance may still be unknown, but the distances of all stars are roughly equal, in what we now call color-magnitude diagra ...
... that the absolute brightnesses, i.e., the distances, are required to properly order the stars in the HR diagram. Order can also be achieved for stars in star clusters where the distance may still be unknown, but the distances of all stars are roughly equal, in what we now call color-magnitude diagra ...
Radio Emission Toward Regions of Massive Star Formation
... Our understanding of high-mass star formation is not that simple. In this dissertation and per convention, stars with enough mass to end their lives as core-collapse supernovae (M∗ ≥ 8.0 M ) are considered ‘high-mass’ stars. High-mass stars have difficulty forming in this fashion, because the onset ...
... Our understanding of high-mass star formation is not that simple. In this dissertation and per convention, stars with enough mass to end their lives as core-collapse supernovae (M∗ ≥ 8.0 M ) are considered ‘high-mass’ stars. High-mass stars have difficulty forming in this fashion, because the onset ...
Discovery and spectroscopy of the young Jovian planet
... Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA. 2Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94040, USA. 3Department of Astronomy, University of California–Berkeley, Berkeley, CA, 94720, USA. 4Lunar and Planetary Labo ...
... Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA. 2Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94040, USA. 3Department of Astronomy, University of California–Berkeley, Berkeley, CA, 94720, USA. 4Lunar and Planetary Labo ...
arXiv:astro-ph/9701131v1 18 Jan 1997
... quietly fade from prominence as helium white dwarfs. This general evolutionary scenario is detailed in Figure 1 (adapted from Laughlin et al., 1996), which charts the path in the Hertzsprung-Russell diagram followed by low mass stars of several different masses in the range 0.08M⊙ ≤ M∗ ≤ 0.25M⊙. Upo ...
... quietly fade from prominence as helium white dwarfs. This general evolutionary scenario is detailed in Figure 1 (adapted from Laughlin et al., 1996), which charts the path in the Hertzsprung-Russell diagram followed by low mass stars of several different masses in the range 0.08M⊙ ≤ M∗ ≤ 0.25M⊙. Upo ...
On the elemental abundance and isotopic mixture of mercury in
... Spectra taken with the EMMI spectrograph at the 3.5 m NTT telescope cover a large wavelength interval (4070– 6740 Å) at a resolving power of R ∼ 80 000 and S/N ∼ 100. The spectrum of AV Scl was taken with the UVES spectrograph at the 8.0 m VLT. The UVES is a two-arm crossdispersed echelle spectrogra ...
... Spectra taken with the EMMI spectrograph at the 3.5 m NTT telescope cover a large wavelength interval (4070– 6740 Å) at a resolving power of R ∼ 80 000 and S/N ∼ 100. The spectrum of AV Scl was taken with the UVES spectrograph at the 8.0 m VLT. The UVES is a two-arm crossdispersed echelle spectrogra ...
Rest-frame Optical Spectra: A Window into Galaxy Formation at z~2
... • At low-z (e.g., SDSS), spectral diagnostics, Dn(4000), HδA, others, have been used to infer M/L, fraction of mass formed in burst, stellar velocity dispersion, metallicity. • The samples for which such measurements have been assembled at z>1.4 are in the “handfuls.” (Kauffmann et al. 2003) ...
... • At low-z (e.g., SDSS), spectral diagnostics, Dn(4000), HδA, others, have been used to infer M/L, fraction of mass formed in burst, stellar velocity dispersion, metallicity. • The samples for which such measurements have been assembled at z>1.4 are in the “handfuls.” (Kauffmann et al. 2003) ...
Corvus (constellation)
Corvus is a small constellation in the Southern Celestial Hemisphere. Its name comes from the Latin word ""raven"" or ""crow"". It includes only 11 stars with brighter than 4.02 magnitudes. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The four brightest stars, Gamma, Delta, Epsilon, and Beta Corvi from a distinctive quadrilateral in the night sky. The young star Eta Corvi has been found to have two debris disks.