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 ...
Understanding Variable Stars - Central Florida Astronomical Society
... perspective, an introduction to stars in general, the techniques for discovering and studying variable stars, and a description of the main types of variable stars. It ends with short reflections about the connection between the study of variable stars, and research, education, amateur astronomy, and ...
... perspective, an introduction to stars in general, the techniques for discovering and studying variable stars, and a description of the main types of variable stars. It ends with short reflections about the connection between the study of variable stars, and research, education, amateur astronomy, and ...
act_science_bellringers
... 24. H—“ Gravity causes part of a cloud of gas and dust to collapse and heat up”; gravitational force is the only one mentioned in the passage. 25. B—“ hydrogen to make helium in a shell surrounding its center.” This answer comes straight from the passage, and the question directs you to find the ans ...
... 24. H—“ Gravity causes part of a cloud of gas and dust to collapse and heat up”; gravitational force is the only one mentioned in the passage. 25. B—“ hydrogen to make helium in a shell surrounding its center.” This answer comes straight from the passage, and the question directs you to find the ans ...
Spectroscopic Atlas for Amateur Astronomers
... edition: “Atlas for Objective Prism Spectra” by Waltraut C. Seitter, 1975 [5]). This atlas, covering the spectral types from O5 to M2, is out of print today, but recently available as download [5]! Still based on photographic spectral strips it’s the only reviewed work, documenting most of the lines ...
... edition: “Atlas for Objective Prism Spectra” by Waltraut C. Seitter, 1975 [5]). This atlas, covering the spectral types from O5 to M2, is out of print today, but recently available as download [5]! Still based on photographic spectral strips it’s the only reviewed work, documenting most of the lines ...
Astronomy Astrophysics
... number of member stars Nmem . Each star was ranked according to the number of times it survived after all runs (survival frequency), and only the Nmem highest ranked stars were taken as cluster members. For the present cases we obtained survival frequencies higher than 85%. More details about t ...
... number of member stars Nmem . Each star was ranked according to the number of times it survived after all runs (survival frequency), and only the Nmem highest ranked stars were taken as cluster members. For the present cases we obtained survival frequencies higher than 85%. More details about t ...
Carbon, nitrogen and oxygen abundances in
... stars are selected according to their effective temperatures Teff and surface gravities log g, namely: Teff is between 15 300 and 24 100 K and log g is mostly greater than 3.75; therefore, stars with medium masses of 5–11 M are selected. Theory predicts for the stars with such parameters that the C ...
... stars are selected according to their effective temperatures Teff and surface gravities log g, namely: Teff is between 15 300 and 24 100 K and log g is mostly greater than 3.75; therefore, stars with medium masses of 5–11 M are selected. Theory predicts for the stars with such parameters that the C ...
Book Describing Techniques to Detect Transiting ExoPlanets
... and others are aimed at new discoveries. The various options for exoplanet observing are explained in Chapter 3. The advanced amateur may eventually be recruited to become a member of a professional/amateur team that endeavors to discover exoplanets. This might be the ultimate goal for some readers ...
... and others are aimed at new discoveries. The various options for exoplanet observing are explained in Chapter 3. The advanced amateur may eventually be recruited to become a member of a professional/amateur team that endeavors to discover exoplanets. This might be the ultimate goal for some readers ...
the use of fixed stars in astrology
... 16. In other words, Stars of the First Magnitude are the brightest as seen from the Earth and then receding in brightness so that the Sixteenth Magnitude Stars are the faintest. Mercifully, for predictive astrology, we take into account Stars of the first four Magnitudes only. FOURTHLY, the Fixed St ...
... 16. In other words, Stars of the First Magnitude are the brightest as seen from the Earth and then receding in brightness so that the Sixteenth Magnitude Stars are the faintest. Mercifully, for predictive astrology, we take into account Stars of the first four Magnitudes only. FOURTHLY, the Fixed St ...
Astronomy Astrophysics Gaia-ESO Survey: The analysis of high-resolution The
... of all spectra obtained from the beginning of the Survey up to the end of June 2013, and additional archival data that were included for calibration purposes. For the WG11 analysis, it included a total of 1708 spectra of 1447 FGK-type stars (multiple exposures of benchmark stars were analyzed separa ...
... of all spectra obtained from the beginning of the Survey up to the end of June 2013, and additional archival data that were included for calibration purposes. For the WG11 analysis, it included a total of 1708 spectra of 1447 FGK-type stars (multiple exposures of benchmark stars were analyzed separa ...
A Variability Study of the Typical Red Supergiant Antares A
... with historical radial velocity measures, Hipparcos photometry, and AAVSO photometry. From these data we determine four scales of variability: ~7140 days, 2167 days, ~1260 days, and ~100 days. The longest of these periods is found from the AAVSO photometry and cannot be confirmed by any of the other ...
... with historical radial velocity measures, Hipparcos photometry, and AAVSO photometry. From these data we determine four scales of variability: ~7140 days, 2167 days, ~1260 days, and ~100 days. The longest of these periods is found from the AAVSO photometry and cannot be confirmed by any of the other ...
The CCD Photometric Calibration Cookbook
... independent of each other and you can use just the ones appropriate for your purposes. It is also worth noting that astronomical photometry is a diverse subject. There are many different ways of making and reducing photometric observations. Observations can be made for very different types of progra ...
... independent of each other and you can use just the ones appropriate for your purposes. It is also worth noting that astronomical photometry is a diverse subject. There are many different ways of making and reducing photometric observations. Observations can be made for very different types of progra ...
Stars and Planets Credits and Acknowledgements
... Stars and Planets is a series of nine lessons designed to assist students in grades 6-8 in understanding scale in the solar system and beyond, in time as well as space. Many of the lessons use image data from the Hubble Space Telescope and NASA’s other Great Observatories as they take students on a ...
... Stars and Planets is a series of nine lessons designed to assist students in grades 6-8 in understanding scale in the solar system and beyond, in time as well as space. Many of the lessons use image data from the Hubble Space Telescope and NASA’s other Great Observatories as they take students on a ...
Cassiopeia (constellation)
Cassiopeia is a constellation in the northern sky, named after the vain queen Cassiopeia in Greek mythology, who boasted about her unrivalled beauty. Cassiopeia was one of the 48 constellations listed by the 2nd-century Greek astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is easily recognizable due to its distinctive 'M' shape when in upper culmination but in higher northern locations when near lower culminations in spring and summer it has a 'W' shape, formed by five bright stars. It is bordered by Andromeda to the south, Perseus to the southeast, and Cepheus to the north. It is opposite the Big Dipper.In northern locations above 34ºN latitude it is visible year-round and in the (sub)tropics it can be seen at its clearest from September to early November in its characteristic 'M' shape. Even in low southern latitudes below 25ºS is can be seen low in the North.