A Method of Correcting Near-Infrared Spectra for Telluric Absorption
... spectra of all A0 V stars can be considered nearly identical to one another. It is a fortunate circumstance that Vega, the object that defines the zero point of the magnitude system, is also a bright A0 V star whose spectrum has been accurately modeled. Assuming that the model provides an accurate r ...
... spectra of all A0 V stars can be considered nearly identical to one another. It is a fortunate circumstance that Vega, the object that defines the zero point of the magnitude system, is also a bright A0 V star whose spectrum has been accurately modeled. Assuming that the model provides an accurate r ...
Multiplicity in Early Stellar Evolution
... tree (level 1). Inner pairs associated with primary and secondary components of the outer pair are called levels 11 and 12, respectively, and this notation continues to deeper levels. Triple systems can have inner pairs at level 11 or 12. When both sub-systems are present, we get the so-called 2+2 q ...
... tree (level 1). Inner pairs associated with primary and secondary components of the outer pair are called levels 11 and 12, respectively, and this notation continues to deeper levels. Triple systems can have inner pairs at level 11 or 12. When both sub-systems are present, we get the so-called 2+2 q ...
Stars and Planets Credits and Acknowledgements
... NASA’s exploration of the cosmos is highlighted in multiple lessons along with cuttingedge science. New Horizons is introduced in the Scale Model Solar System lesson and the Kepler Mission, a distribution partner for Stars and Planets, is highlighted in Planet Hunting. Three of the lessons feature s ...
... NASA’s exploration of the cosmos is highlighted in multiple lessons along with cuttingedge science. New Horizons is introduced in the Scale Model Solar System lesson and the Kepler Mission, a distribution partner for Stars and Planets, is highlighted in Planet Hunting. Three of the lessons feature s ...
Stars sensors terminology and performance
... This Standard specifies star tracker performances as part of a space project. The Standard covers all aspects of performances, including nomenclature, definitions, and performance requirements for the performance specification of star sensors. The Standard focuses on performance specifications (incl ...
... This Standard specifies star tracker performances as part of a space project. The Standard covers all aspects of performances, including nomenclature, definitions, and performance requirements for the performance specification of star sensors. The Standard focuses on performance specifications (incl ...
Galaxies
... The radiation from these galaxies is called nonstellar radiation Many luminous galaxies are experiencing an outburst of star formation, probably due to interactions with a neighbor These galaxies are called starburst galaxies, and we will discuss them later The galaxies we will discuss now are those ...
... The radiation from these galaxies is called nonstellar radiation Many luminous galaxies are experiencing an outburst of star formation, probably due to interactions with a neighbor These galaxies are called starburst galaxies, and we will discuss them later The galaxies we will discuss now are those ...
Evolution in circumstellar envelopes of Be stars: From disks to rings?
... FV CMa (= HD 54 309 = HR 2690; B2 IVe): unfortunately, this star was observed during one observing run only so that nothing can be stated about a possible temporal evolution. Thirteen spectra were taken with Feros at the ESO 1.52-m telescope over a period of 17 days in January, 2000. All spectral fe ...
... FV CMa (= HD 54 309 = HR 2690; B2 IVe): unfortunately, this star was observed during one observing run only so that nothing can be stated about a possible temporal evolution. Thirteen spectra were taken with Feros at the ESO 1.52-m telescope over a period of 17 days in January, 2000. All spectral fe ...
FLARE SWG theme 3: high
... Quasars/AGNs appear to become rarer wrt galaxies at z>5 but need direct measurements FLARE+Athena (also E-ELT) can directly measure out to (potentially) z~10 ...
... Quasars/AGNs appear to become rarer wrt galaxies at z>5 but need direct measurements FLARE+Athena (also E-ELT) can directly measure out to (potentially) z~10 ...
The Collision Between The Milky Way And Andromeda
... therefore the most powerful tool, to study the formation and evolution of galactic structure. Like most extragalactic groups, the Local Group is very likely to be decoupled from the cosmological expansion and is now a gravitationally bound collection of galaxies. This notion is supported by the obse ...
... therefore the most powerful tool, to study the formation and evolution of galactic structure. Like most extragalactic groups, the Local Group is very likely to be decoupled from the cosmological expansion and is now a gravitationally bound collection of galaxies. This notion is supported by the obse ...
User`s Manual for DAOPHOT II This manual is intended as a guide
... fits visually on an image display before accepting the final product. (3) The shape of the point-spread function is assumed to be spatially constant or to vary smoothly with position within the frame; it is assumed not to depend at all on apparent magnitude. If these conditions are not met, systemat ...
... fits visually on an image display before accepting the final product. (3) The shape of the point-spread function is assumed to be spatially constant or to vary smoothly with position within the frame; it is assumed not to depend at all on apparent magnitude. If these conditions are not met, systemat ...
Radio Emission Toward Regions of Massive Star Formation
... stars with accretion disks and bipolar outflows have been directly observed (Kraus et al. 2010). Therefore, there must be some other important physics simple models do not take into account. The review by Zinnecker & Yorke (2007) discusses three prevailing theories: monolithic collapse in cores with ...
... stars with accretion disks and bipolar outflows have been directly observed (Kraus et al. 2010). Therefore, there must be some other important physics simple models do not take into account. The review by Zinnecker & Yorke (2007) discusses three prevailing theories: monolithic collapse in cores with ...
Type Ia Supernovae
... eternity. Theory predicts that such stars will self ignite when close to 1.38 M (called the Chandrasekhar Mass). Most stars however leave white dwarfs with 0.6 M and no star leaves a remnant as heavy as 1.38 M , which suggests that they somehow need to acquire mass if they are to explode as SN Ia. C ...
... eternity. Theory predicts that such stars will self ignite when close to 1.38 M (called the Chandrasekhar Mass). Most stars however leave white dwarfs with 0.6 M and no star leaves a remnant as heavy as 1.38 M , which suggests that they somehow need to acquire mass if they are to explode as SN Ia. C ...
Stellar Structure and Evolution
... and to Karlheinz Langanke for translating it from the Danish original (‘Stjerneudviklingens slutstadier’). I also thank Langanke for very substantial contributions to the revised Chapters 14 and 15. Discussions with A. V. Sweigart and J. Lattanzio were very helpful in bringing my ideas about late st ...
... and to Karlheinz Langanke for translating it from the Danish original (‘Stjerneudviklingens slutstadier’). I also thank Langanke for very substantial contributions to the revised Chapters 14 and 15. Discussions with A. V. Sweigart and J. Lattanzio were very helpful in bringing my ideas about late st ...
Gaia 1 and 2. A pair of new satellites of the Galaxy
... Gaia-detected sources is indeed very prominent (top left and top middle panels). Note a white patch corresponding to a dearth of Gaia sources near the centre of the over-density. This is the location of Sirius, where Gaia struggles to detect genuine stars3 . The area affected by Sirius is much large ...
... Gaia-detected sources is indeed very prominent (top left and top middle panels). Note a white patch corresponding to a dearth of Gaia sources near the centre of the over-density. This is the location of Sirius, where Gaia struggles to detect genuine stars3 . The area affected by Sirius is much large ...
Book Describing Techniques to Detect Transiting ExoPlanets
... those who studied objects in our solar system had the lowest status. My studies were of the moon, which was about as low a status as possible. Some would say that at that time there was only one level lower than mine: those who speculated about other worlds and the possibilities for intelligent life ...
... those who studied objects in our solar system had the lowest status. My studies were of the moon, which was about as low a status as possible. Some would say that at that time there was only one level lower than mine: those who speculated about other worlds and the possibilities for intelligent life ...
Introduction_to_pulsar_astronomy
... are expelled and form a Planetary Nebula. The core of the star remains bound, and forms a white dwarf. ...
... are expelled and form a Planetary Nebula. The core of the star remains bound, and forms a white dwarf. ...
Article PDF - IOPscience
... communication) places the star inside the 20 pc region, and the DC star LHS 1247 (0123−262) since its distance, estimated from the photometric observations of Bergeron et al. (1997, hereafter BRL97), places this candidate inside our region of interest, within the uncertainties. We also include two D ...
... communication) places the star inside the 20 pc region, and the DC star LHS 1247 (0123−262) since its distance, estimated from the photometric observations of Bergeron et al. (1997, hereafter BRL97), places this candidate inside our region of interest, within the uncertainties. We also include two D ...
Deneb - Emmi
... Deneb, which means tail in Arabic, is the 19th brightest star in the universe, and one of the most well known stars in our very own Milky Way. ...
... Deneb, which means tail in Arabic, is the 19th brightest star in the universe, and one of the most well known stars in our very own Milky Way. ...
Chapter 24
... somewhat larger than dwarf ellipticals. They typically contain between 108 and 1010 stars. The smallest such galaxies are called dwarf irregulars. As with elliptical galaxies, the dwarf type is the most common irregular. Dwarf ellipticals and dwarf irregulars occur in approximately equal numbers and ...
... somewhat larger than dwarf ellipticals. They typically contain between 108 and 1010 stars. The smallest such galaxies are called dwarf irregulars. As with elliptical galaxies, the dwarf type is the most common irregular. Dwarf ellipticals and dwarf irregulars occur in approximately equal numbers and ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... reliably from our unfavorable vantage point inside the Galaxy. Various indirect indicators suggest that our Galaxy can be classified as an Sbc galaxy, intermediate between the properties described for M31 and M33. Some recent studies at radio, infrared and optical wavelengths also suggest that our G ...
... reliably from our unfavorable vantage point inside the Galaxy. Various indirect indicators suggest that our Galaxy can be classified as an Sbc galaxy, intermediate between the properties described for M31 and M33. Some recent studies at radio, infrared and optical wavelengths also suggest that our G ...
- Isaac Newton Group of Telescopes
... 1996 we had the additional distraction of the Prior Options process the then UK Governments requirement for public services to be subject to competitive tendering, in this case the management of the telescopes and delivery of the instrumentation programme. So my main emotion on reading this annua ...
... 1996 we had the additional distraction of the Prior Options process the then UK Governments requirement for public services to be subject to competitive tendering, in this case the management of the telescopes and delivery of the instrumentation programme. So my main emotion on reading this annua ...
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 ...
Mapping of the extinction in giant molecular clouds using optical star
... between m − 1/2 and m + 1/2) in each cell of a regular rectangular grid in an obscured area and to compare the result with the counts obtained in a supposedly unextinguished region. In order to improve the spatial resolution, Bok (1956) proposed to make count up to the completeness limiting magnitud ...
... between m − 1/2 and m + 1/2) in each cell of a regular rectangular grid in an obscured area and to compare the result with the counts obtained in a supposedly unextinguished region. In order to improve the spatial resolution, Bok (1956) proposed to make count up to the completeness limiting magnitud ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.