Carbon, nitrogen and oxygen abundances in
... velocity v sin i for 102 B stars. The v sin i values were found to range from 5 to 280 km s−1 ; such a large variation allowed us to analyse a relation between the helium abundances and rotational velocities. The used He I lines are strong in spectra of early and medium B stars, so their equivalent ...
... velocity v sin i for 102 B stars. The v sin i values were found to range from 5 to 280 km s−1 ; such a large variation allowed us to analyse a relation between the helium abundances and rotational velocities. The used He I lines are strong in spectra of early and medium B stars, so their equivalent ...
Understanding Variable Stars - Central Florida Astronomical Society
... Understanding Variable Stars Variable stars are those that change brightness. Their variability may be due to geometric processes such as rotation, or eclipse by a companion star, or physical processes such as vibration, flares, or cataclysmic explosions. In each case, variable stars provide unique ...
... Understanding Variable Stars Variable stars are those that change brightness. Their variability may be due to geometric processes such as rotation, or eclipse by a companion star, or physical processes such as vibration, flares, or cataclysmic explosions. In each case, variable stars provide unique ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... M/L defined in units of M /L For galaxies, M/L reflects the average M/L over the population Pop I (young) : massive stars dominate light; low mass stars dominate mass Pop II (old) : giants dominate light; M.S. stars dominate mass Typical galaxy (& solar neighborhood) has M/LV 6, M/LB ∼ 10 In gener ...
... M/L defined in units of M /L For galaxies, M/L reflects the average M/L over the population Pop I (young) : massive stars dominate light; low mass stars dominate mass Pop II (old) : giants dominate light; M.S. stars dominate mass Typical galaxy (& solar neighborhood) has M/LV 6, M/LB ∼ 10 In gener ...
Astronomy Astrophysics Gaia-ESO Survey: The analysis of high-resolution The
... science verification papers were based on iDR1, and it is therefore important to document how this analysis was conducted. We stress again that the Gaia-ESO spectrum analysis is under continous development. With improvements in the analysis, the complete Survey data set will be reanalyzed. Therefore ...
... science verification papers were based on iDR1, and it is therefore important to document how this analysis was conducted. We stress again that the Gaia-ESO spectrum analysis is under continous development. With improvements in the analysis, the complete Survey data set will be reanalyzed. Therefore ...
Stellar Populations of Dwarf Elliptical Galaxies: UBVRI Photometry
... Cluster with previously measured kinematic properties. The global optical colors are red, with median values for the sample of 0.24 ± 0.03 in (U–B), 0.77 ± 0.02 in (B– V), and 1.02 ± 0.03 in (V–I). We recover the well known color-magnitude relation for cluster galaxies, but find no significant diffe ...
... Cluster with previously measured kinematic properties. The global optical colors are red, with median values for the sample of 0.24 ± 0.03 in (U–B), 0.77 ± 0.02 in (B– V), and 1.02 ± 0.03 in (V–I). We recover the well known color-magnitude relation for cluster galaxies, but find no significant diffe ...
Full Text - Departement Natuurkunde en Sterrenkunde
... Strömgren photometric system . . . . . . . . . . . . . . . . . . . . . 165 ...
... Strömgren photometric system . . . . . . . . . . . . . . . . . . . . . 165 ...
THE MORPHOLOGICAL DEMOGRAPHICS OF GALAXIES IN THE
... types provided by BPZ are a linear combination from a template library of SEDs. We use the CWWSB_Benitez2003 template set as described in Benítez et al. (2004). These are based on the templates from Coleman, Wu, & Weedman (1980) and Kinney et al. (1996) consisting of El, Sbc, Scd, Im, SB3, and SB2, ...
... types provided by BPZ are a linear combination from a template library of SEDs. We use the CWWSB_Benitez2003 template set as described in Benítez et al. (2004). These are based on the templates from Coleman, Wu, & Weedman (1980) and Kinney et al. (1996) consisting of El, Sbc, Scd, Im, SB3, and SB2, ...
abstracts book - Instituto de Astrofísica e Ciências do Espaço
... For the last 30 years, since the meeting on Seismology of the Sun and the Distant Stars held in Cambridge, in 1985, the range of seismic data and associated science results obtained has far exceeded the expectations of the community. The continuous observation of the Sun has secured major advances i ...
... For the last 30 years, since the meeting on Seismology of the Sun and the Distant Stars held in Cambridge, in 1985, the range of seismic data and associated science results obtained has far exceeded the expectations of the community. The continuous observation of the Sun has secured major advances i ...
Gaia 1 and 2. A pair of new satellites of the Galaxy
... i.e. without an entry in any of the clusters/galaxies catalogues available to us, has an estimated significance of ∼ 10. Note however, that initially, this candidate, dubbed here Gaia 1, was rejected as it is located in close proximity of the brightest star on the sky – Sirius2 . Figure 3 shows the ...
... i.e. without an entry in any of the clusters/galaxies catalogues available to us, has an estimated significance of ∼ 10. Note however, that initially, this candidate, dubbed here Gaia 1, was rejected as it is located in close proximity of the brightest star on the sky – Sirius2 . Figure 3 shows the ...
Tuomas Kangas
... Stars are divided into spectral classes depending on their effective (surface) temperatures, which determine their intrinsic colors. The sequence from hottest to coolest is O–B–A–F–G–K–M, followed by the even cooler brown dwarfs. O-type stars are blue, with temperatures T & 20000 K, while red M-type ...
... Stars are divided into spectral classes depending on their effective (surface) temperatures, which determine their intrinsic colors. The sequence from hottest to coolest is O–B–A–F–G–K–M, followed by the even cooler brown dwarfs. O-type stars are blue, with temperatures T & 20000 K, while red M-type ...
THE COMET`S TALE - Institute of Astronomy
... Than Ours, from his Sunday school library which led him to an interest in astronomy. This interest was further inspired by the conjunction of Jupiter and Mars on May 7th, 1879, when the planets were slightly over one degree apart, and/or July 22nd, 1881, when the two planets were separated by only s ...
... Than Ours, from his Sunday school library which led him to an interest in astronomy. This interest was further inspired by the conjunction of Jupiter and Mars on May 7th, 1879, when the planets were slightly over one degree apart, and/or July 22nd, 1881, when the two planets were separated by only s ...
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 ...
the PDF program book
... The registration desk is located in the south-east corner of UKK, behind the escalators near the entrance to Hall D. ...
... The registration desk is located in the south-east corner of UKK, behind the escalators near the entrance to Hall D. ...
Development of a Software Package for the Reduction and Analysis
... for the reduction and analysis of meteor videos. The uncertainty in determining the position of a meteor was computed to be 0.2−3.0 pixels, with a median value of 0.3 pixels. Sub-pixel accuracy (0.2−0.5 pixels) was also reached for the uncertainties in the astrometric transformation. Different modul ...
... for the reduction and analysis of meteor videos. The uncertainty in determining the position of a meteor was computed to be 0.2−3.0 pixels, with a median value of 0.3 pixels. Sub-pixel accuracy (0.2−0.5 pixels) was also reached for the uncertainties in the astrometric transformation. Different modul ...
Digital Universe Guide - American Museum of Natural History
... The Digital Universe, developed by the American Museum of Natural History’s Hayden Planetarium with support from NASA, incorporates data from dozens of organizations worldwide to create the most complete and accurate 3-D atlas of the Universe from the local solar neighborhood out to the edge of the ...
... The Digital Universe, developed by the American Museum of Natural History’s Hayden Planetarium with support from NASA, incorporates data from dozens of organizations worldwide to create the most complete and accurate 3-D atlas of the Universe from the local solar neighborhood out to the edge of the ...
Search For Gas Giants Around Late-m Dwarfs - STARS
... atomic lines, the measurement of pseudo-equivalent widths, masses, surface gravity, effective temperature, absolute radial velocities, rotational velocities and rotation periods. The identification of neutral atomic lines was carried out using the Vienna Atomic line Database. We were able to confirm ...
... atomic lines, the measurement of pseudo-equivalent widths, masses, surface gravity, effective temperature, absolute radial velocities, rotational velocities and rotation periods. The identification of neutral atomic lines was carried out using the Vienna Atomic line Database. We were able to confirm ...
The CCD Photometric Calibration Cookbook
... CCD (Charge-Coupled Device) photometric calibration is concerned with converting the arbitrary units in which CCD images are recorded into standard, reproducible units. In principle the observed brightness could be calibrated into genuine physical units, such as W m , and indeed this is occasionally ...
... CCD (Charge-Coupled Device) photometric calibration is concerned with converting the arbitrary units in which CCD images are recorded into standard, reproducible units. In principle the observed brightness could be calibrated into genuine physical units, such as W m , and indeed this is occasionally ...
Astronomy Astrophysics
... crowded regions, we performed point spread function (PSF) photometry of 10 × 10 arcmin fields surrounding each selected candidate. We used the VVV-SkZ pipeline, which is an automatic PSF-fitting photometric pipeline for the VVV survey (Mauro et al. 2013). Where possible, the saturated stars (usually ...
... crowded regions, we performed point spread function (PSF) photometry of 10 × 10 arcmin fields surrounding each selected candidate. We used the VVV-SkZ pipeline, which is an automatic PSF-fitting photometric pipeline for the VVV survey (Mauro et al. 2013). Where possible, the saturated stars (usually ...
Clusters as laboratories for the study of galaxy evolution
... exploit the coeval populations of stars to understand how stars evolve, but do not expect that the evolution of these stars has been influenced by the cluster environment. Given this difference, my “laboratories” statement would have been an imperfect analogy, at best. In this talk I will review evi ...
... exploit the coeval populations of stars to understand how stars evolve, but do not expect that the evolution of these stars has been influenced by the cluster environment. Given this difference, my “laboratories” statement would have been an imperfect analogy, at best. In this talk I will review evi ...
THE DEMOGRAPHICS OF LONG-PERIOD COMETS ABSTRACT
... is not a major source of incompleteness. It also shows that most comets down to the LINEAR magnitude limit are still active out to 10AU from the Sun. Fig 3 shows an intriguing correlation between perihelion distance and semi-major axis in the LINEAR sample. This correlation was first noted by Marsden ...
... is not a major source of incompleteness. It also shows that most comets down to the LINEAR magnitude limit are still active out to 10AU from the Sun. Fig 3 shows an intriguing correlation between perihelion distance and semi-major axis in the LINEAR sample. This correlation was first noted by Marsden ...
sections 23-25 powerpoint
... tied to overall dimensions: cD galaxies. Huge elliptical galaxies dominating some clusters of galaxies. “cD” stands for “cluster dominating” galaxy. Some are incredibly large, massive, and luminous. Normal ellipticals. Standard E galaxies comparable in luminosity to supergiant spiral galaxies. Dwarf ...
... tied to overall dimensions: cD galaxies. Huge elliptical galaxies dominating some clusters of galaxies. “cD” stands for “cluster dominating” galaxy. Some are incredibly large, massive, and luminous. Normal ellipticals. Standard E galaxies comparable in luminosity to supergiant spiral galaxies. Dwarf ...
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 ...
Boötes
Boötes /boʊˈoʊtiːz/ is a constellation in the northern sky, located between 0° and +60° declination, and 13 and 16 hours of right ascension on the celestial sphere. The name comes from the Greek Βοώτης, Boōtēs, meaning herdsman or plowman (literally, ox-driver; from βοῦς bous “cow”). The ""ö"" in the name is a diaeresis, not an umlaut, meaning that each 'o' is to be pronounced separately.One of the 48 constellations described by the 2nd century astronomer Ptolemy, Boötes is now one of the 88 modern constellations. It contains the fourth brightest star in the night sky, the orange-hued Arcturus. Boötes is home to many other bright stars, including eight above the fourth magnitude and an additional 21 above the fifth magnitude, making a total of 29 stars easily visible to the naked eye.