THE 2MASS WIDE-FIELD T DWARF SEARCH. II. DISCOVERY OF
... and Ks photometric bands sampled by 2MASS. The optical/near-infrared colors of T dwarfs are also extremely red (RJ e 9; Golimowski et al. 1998); hence, photographic plate surveys, which also cover the whole sky, cannot detect T dwarfs much farther than a few parsecs from the Sun (Scholz et al. 2003 ...
... and Ks photometric bands sampled by 2MASS. The optical/near-infrared colors of T dwarfs are also extremely red (RJ e 9; Golimowski et al. 1998); hence, photographic plate surveys, which also cover the whole sky, cannot detect T dwarfs much farther than a few parsecs from the Sun (Scholz et al. 2003 ...
STARLAB
... you told the first time. If time allows, show the Earth Cylinder or other cylinders. Try some activities from your Planetarium Activities for Student Success (PASS) volumes. (Did you send in your Product Registration form? See Note.) 6. It’s important that the students realize that you are learning ...
... you told the first time. If time allows, show the Earth Cylinder or other cylinders. Try some activities from your Planetarium Activities for Student Success (PASS) volumes. (Did you send in your Product Registration form? See Note.) 6. It’s important that the students realize that you are learning ...
The Lupus clouds - European Southern Observatory
... frequent association of such stars with dark clouds was already noted. The nature of the Lupus clouds as a recent star forming site was thus implicitly recognized later by the works of Herbig (1952) and Walker (1956) where the pre-main sequence character and very young age of T Tauri stars was ident ...
... frequent association of such stars with dark clouds was already noted. The nature of the Lupus clouds as a recent star forming site was thus implicitly recognized later by the works of Herbig (1952) and Walker (1956) where the pre-main sequence character and very young age of T Tauri stars was ident ...
Unfolding the Milky Way bulge - International Max Planck Research
... circles show the results for VVV data at latitudes b = −1◦ and b = +1◦ , respectively. Solid lines show the distance spread along each line of sight correcting for an intrinsic bulge dispersion of 0.17 mag and photometric errors. Black open squares are the results from N05 at b = +1. Dashed lines re ...
... circles show the results for VVV data at latitudes b = −1◦ and b = +1◦ , respectively. Solid lines show the distance spread along each line of sight correcting for an intrinsic bulge dispersion of 0.17 mag and photometric errors. Black open squares are the results from N05 at b = +1. Dashed lines re ...
Communications in Asteroseismology
... “Mi-shell Brezhair” in France and Quebec! Mike is a man of many names, but for his more than 35 postgraduate students and many others he is also known as “mentor”, and all of us know him as “friend” and “colleague”. I (DWK) was Mike’s first PhD student at the University of Texas over 30 years ago. Wh ...
... “Mi-shell Brezhair” in France and Quebec! Mike is a man of many names, but for his more than 35 postgraduate students and many others he is also known as “mentor”, and all of us know him as “friend” and “colleague”. I (DWK) was Mike’s first PhD student at the University of Texas over 30 years ago. Wh ...
... outer rings, inner rings, and stuff dumped onto the center. The results of numerical simulations correspond closely to the morphology of barred galaxies. In the simulations, gas is transported to small radii, where it reaches high densities and plausibly feeds star formation. In the observations, ma ...
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 ...
harlow shapley - National Academy of Sciences
... the truly great are indeed happy fellows; second, men and women of accomplishment have an obligation to search out the best young people that come their way and assist them in every possible way in shaping their careers. During his Princeton days, Harlow Shapley studied the cepheid variable stars, w ...
... the truly great are indeed happy fellows; second, men and women of accomplishment have an obligation to search out the best young people that come their way and assist them in every possible way in shaping their careers. During his Princeton days, Harlow Shapley studied the cepheid variable stars, w ...
THE DEMOGRAPHICS OF LONG-PERIOD COMETS ABSTRACT
... a conservative upper limit: most of these lost objects were most likely either not real to begin with or fastmoving objects only visible for a short window of time. Secondly, some comets might have been inactive at these large heliocentric distances, and hence classified as minor planets. The minor p ...
... a conservative upper limit: most of these lost objects were most likely either not real to begin with or fastmoving objects only visible for a short window of time. Secondly, some comets might have been inactive at these large heliocentric distances, and hence classified as minor planets. The minor p ...
An Atlas of Stellar Spectra
... luminosity classes. It is not possible even to adopt certain criteria as standard, since different criteria may have to be used with different dispersion. In the Atlas some of the most useful features for luminosity classification have been indicated, but it should be emphasized that each dispersion ...
... luminosity classes. It is not possible even to adopt certain criteria as standard, since different criteria may have to be used with different dispersion. In the Atlas some of the most useful features for luminosity classification have been indicated, but it should be emphasized that each dispersion ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... size is 4.6 arcmin (or 33 parsecs) across and the image resolution (\seeing") is 0.5 arcsec. Right panel: A globular cluster in the halo of the giant elliptical galaxy NGC 5128, 3900 kiloparsecs from the Milky Way. The picture shown is an I band image taken with the Hubble Space Telescope (see G. Ha ...
... size is 4.6 arcmin (or 33 parsecs) across and the image resolution (\seeing") is 0.5 arcsec. Right panel: A globular cluster in the halo of the giant elliptical galaxy NGC 5128, 3900 kiloparsecs from the Milky Way. The picture shown is an I band image taken with the Hubble Space Telescope (see G. Ha ...
Chapter 5 The Evolutionary Paths Of Nearby Galaxies
... Figure 5.5: The morphological type distribution of galaxies in the HRS+ sample (dotted histogram). The filled histogram represents galaxies in the transition region, while red and blue sequence galaxies are shown with the empty and dashed histogram, respectively. ...
... Figure 5.5: The morphological type distribution of galaxies in the HRS+ sample (dotted histogram). The filled histogram represents galaxies in the transition region, while red and blue sequence galaxies are shown with the empty and dashed histogram, respectively. ...
Was the bright comet of 1742 discovered from India?
... comet of 1742 as the first recorded apparition of the periodic comet Grant-GriggMellish (P = 164.3 yrs) that subsequently returned as the comet 1907 II. The comet C/1742 C1 was a bright one, having parabolic orbit and inclination 112.948, motion retrograde; it passed its perihelion on February 8.69 ...
... comet of 1742 as the first recorded apparition of the periodic comet Grant-GriggMellish (P = 164.3 yrs) that subsequently returned as the comet 1907 II. The comet C/1742 C1 was a bright one, having parabolic orbit and inclination 112.948, motion retrograde; it passed its perihelion on February 8.69 ...
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 ...
Carbon, nitrogen and oxygen abundances in
... Fundamental parameters and the carbon, nitrogen and oxygen abundances are determined for 22 B-type stars with distances d ≤ 600 pc and slow rotation (v sin i ≤ 66 km s−1 ). The stars are selected according to their effective temperatures Teff and surface gravities log g, namely: Teff is between 15 3 ...
... Fundamental parameters and the carbon, nitrogen and oxygen abundances are determined for 22 B-type stars with distances d ≤ 600 pc and slow rotation (v sin i ≤ 66 km s−1 ). The stars are selected according to their effective temperatures Teff and surface gravities log g, namely: Teff is between 15 3 ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the mai ...
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the mai ...
Stellar Populations of Dwarf Elliptical Galaxies: UBVRI Photometry
... UBVRI images of 16 dwarf elliptical galaxies in the Virgo Cluster were obtained with the VATT 1.8m on 2003 March 29-31. The telescope was equipped with CCD26, a thinned Loral 3 2048 × 2048 CCD with 15µm pixels. CCD26 has a read noise of 5.7 e− and a gain of 1.9 e− per ADU was used. On-chip binning o ...
... UBVRI images of 16 dwarf elliptical galaxies in the Virgo Cluster were obtained with the VATT 1.8m on 2003 March 29-31. The telescope was equipped with CCD26, a thinned Loral 3 2048 × 2048 CCD with 15µm pixels. CCD26 has a read noise of 5.7 e− and a gain of 1.9 e− per ADU was used. On-chip binning o ...
Tuomas Kangas
... Supernova (SN) events have been observed throughout millennia. These transient events were sometimes bright enough to be observed with the naked eye. The earliest recorded SN, observed by the ancient Chinese, dates back to the year 185 – and, using the modern naming convention, is thus known as SN 1 ...
... Supernova (SN) events have been observed throughout millennia. These transient events were sometimes bright enough to be observed with the naked eye. The earliest recorded SN, observed by the ancient Chinese, dates back to the year 185 – and, using the modern naming convention, is thus known as SN 1 ...
- Isaac Newton Group of Telescopes
... the presence of prominent bands of titanium oxide and, especially, vanadium oxide at 750 nm allowed to derive its spectral classification and an estimate of its effective surface temperature, which turned out to be some 2350 K. The spectrum allowed to infere a velocity measurement of this object in ...
... the presence of prominent bands of titanium oxide and, especially, vanadium oxide at 750 nm allowed to derive its spectral classification and an estimate of its effective surface temperature, which turned out to be some 2350 K. The spectrum allowed to infere a velocity measurement of this object in ...
Corona Australis
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.