![IR-excesses around nearby Lambda Boo stars are caused by debris](http://s1.studyres.com/store/data/016731829_1-505dbf1b190751a7c8ddb12a558fbc40-300x300.png)
IR-excesses around nearby Lambda Boo stars are caused by debris
... bow waves have been referred to as “bow shocks” in the literature, but this implies that the gas is being shocked, which is not what is being modelled, so we will not refer to it as such. Since the gas density can be low and dust does not shock like a fluid, the dust is rather pushed around a cone o ...
... bow waves have been referred to as “bow shocks” in the literature, but this implies that the gas is being shocked, which is not what is being modelled, so we will not refer to it as such. Since the gas density can be low and dust does not shock like a fluid, the dust is rather pushed around a cone o ...
astronomical oxygen isotopic evidence for supernova
... Both 17 O and 18 O are secondary nuclides, produced by H and He burning, respectively (Meyer et al. 2008). One expects their solar ratio to be that of the bulk of the Galaxy at the time of solar system formation unless the abundances of the oxygen isotopes were affected by some local perturbation. Q ...
... Both 17 O and 18 O are secondary nuclides, produced by H and He burning, respectively (Meyer et al. 2008). One expects their solar ratio to be that of the bulk of the Galaxy at the time of solar system formation unless the abundances of the oxygen isotopes were affected by some local perturbation. Q ...
Optical and Infrared Colors of Stars Observed by the
... sample) that do not have a cataloged SDSS source within 2A. Visual inspection of SDSS images shows that 70% of these do not have an optical counterpart at the cataloged 2MASS position. Such sources are either spurious 2MASS detections (roughly 80% of the unmatched 2MASS sources have S/N \ 10 in all ...
... sample) that do not have a cataloged SDSS source within 2A. Visual inspection of SDSS images shows that 70% of these do not have an optical counterpart at the cataloged 2MASS position. Such sources are either spurious 2MASS detections (roughly 80% of the unmatched 2MASS sources have S/N \ 10 in all ...
Gravitationally lensed galaxies at 2 z 3.5: direct abundance
... With the boost of the fluxes from gravitational lensing, it also becomes feasible to detect emission lines such as [O III] λ4363 or [N III] λ5755 which, when related to other transitions from the same ionization stage, are sensitive to the gas temperature. Combining this with the knowledge of the de ...
... With the boost of the fluxes from gravitational lensing, it also becomes feasible to detect emission lines such as [O III] λ4363 or [N III] λ5755 which, when related to other transitions from the same ionization stage, are sensitive to the gas temperature. Combining this with the knowledge of the de ...
X-ray Binaries
... as proved by dynamical studies. Relatively precise masses have been measured in quiescence through exploiting the photometric and spectroscopic detection of the companion star. These are listed in Table 2. Only in the case of GX 339-4 is the constraint on the black hole mass aided by the Bowen techn ...
... as proved by dynamical studies. Relatively precise masses have been measured in quiescence through exploiting the photometric and spectroscopic detection of the companion star. These are listed in Table 2. Only in the case of GX 339-4 is the constraint on the black hole mass aided by the Bowen techn ...
Dark matter scaling relations and the assembly epoch of Coma early
... K2000 galaxies are brighter (and have higher stellar mass) than Coma early-types with a similar halo. Can this be an artifact related to differences in the dynamical models? Many of the K2000 models are based on B-band photometry, while we used RC -band images for the Coma galaxies. Elliptical galax ...
... K2000 galaxies are brighter (and have higher stellar mass) than Coma early-types with a similar halo. Can this be an artifact related to differences in the dynamical models? Many of the K2000 models are based on B-band photometry, while we used RC -band images for the Coma galaxies. Elliptical galax ...
Astronomy Astrophysics - Niels Bohr Institutet
... of such ages has been obtained. Finally, we have computed individual Galactic orbits for all stars with adequate data. The resulting data set should place a wide range of studies of the evolution of the Galactic disk on a new and considerably improved footing. We caution, however, that no such thing ...
... of such ages has been obtained. Finally, we have computed individual Galactic orbits for all stars with adequate data. The resulting data set should place a wide range of studies of the evolution of the Galactic disk on a new and considerably improved footing. We caution, however, that no such thing ...
Cold Gas and Star Formation in Elliptical Galaxies
... shown by the detection and mapping of powerful H2 O maser emission (Claussen et al. 1998). It should be emphasized that, like the infrared emission, the CO data for elliptical galaxies are not, at present, individually very reliable (with a few exceptions). The lines are weak, and are typically obse ...
... shown by the detection and mapping of powerful H2 O maser emission (Claussen et al. 1998). It should be emphasized that, like the infrared emission, the CO data for elliptical galaxies are not, at present, individually very reliable (with a few exceptions). The lines are weak, and are typically obse ...
Period Changes of Delta Scuti Stars and Stellar Evolution
... Mazzitelli (1994), and then computed radial oscillations of these models. The envelopes were integrated from the surface to a layer with temperature log T = 7.2 which corresponds to relative radius r/R = 0.03 − 0.13 in all models considered. For such deep envelopes, the periods of radial oscillation ...
... Mazzitelli (1994), and then computed radial oscillations of these models. The envelopes were integrated from the surface to a layer with temperature log T = 7.2 which corresponds to relative radius r/R = 0.03 − 0.13 in all models considered. For such deep envelopes, the periods of radial oscillation ...
Stellarium User Guide - Skolekonsulenterne.dk
... planetarium. It will calculate the positions of the Sun and Moon, planets and stars, and draw how the sky would look to an observer depending on their location and the time. It can also draw the constellations and simulate astronomical phenomena such as meteor showers, and solar or lunar eclipses. S ...
... planetarium. It will calculate the positions of the Sun and Moon, planets and stars, and draw how the sky would look to an observer depending on their location and the time. It can also draw the constellations and simulate astronomical phenomena such as meteor showers, and solar or lunar eclipses. S ...
Hewitt/Lyons/Suchocki/Yeh, Conceptual Integrated Science
... We measure the Sun’s luminosity as LSun. If we were on a spaceship twice as far away from the Sun, its apparent brightness would appear A. B. C. D. ...
... We measure the Sun’s luminosity as LSun. If we were on a spaceship twice as far away from the Sun, its apparent brightness would appear A. B. C. D. ...
Sunday, March 24, 2013
... 1 in 100) that the alignments were chance. When I first started reading these papers, I was often frustrated that many of these authors did not publish just what assumptions went into the probability calculation or did not provide clear direct references to the papers that did. I eventually found th ...
... 1 in 100) that the alignments were chance. When I first started reading these papers, I was often frustrated that many of these authors did not publish just what assumptions went into the probability calculation or did not provide clear direct references to the papers that did. I eventually found th ...
The Life and Work of Edward Emerson Barnard
... his sick bed long enough to note that the ring was still visible in the 40-inch telescope, though 'very thin' and with a satellite at each end. 'Without occultation it was almost impossible to see any trace of the ring on the sky,' he noted 'The condensations were feebly seen as slightly brighter pa ...
... his sick bed long enough to note that the ring was still visible in the 40-inch telescope, though 'very thin' and with a satellite at each end. 'Without occultation it was almost impossible to see any trace of the ring on the sky,' he noted 'The condensations were feebly seen as slightly brighter pa ...
The distribution of the ISM in the Milky Way A three
... emission from the Galaxy by fitting exponential dust distributions to the COBE/DIRBE maps. In this study, the authors find that the best fit could be achieved by assuming that the dust distribution is more extended than that of the stars, namely that the scalelength of the dust is 1.5 times that of ...
... emission from the Galaxy by fitting exponential dust distributions to the COBE/DIRBE maps. In this study, the authors find that the best fit could be achieved by assuming that the dust distribution is more extended than that of the stars, namely that the scalelength of the dust is 1.5 times that of ...
arXiv:0705.3323v2 [astro-ph] 12 Oct 2007
... 2007). These are easily affected by smooth changes to the galaxy clustering amplitude as a function of scale. In this paper, we use a more robust approach: the BAO scale is defined via the locations where the BAO cross a smooth fit to the power spectrum. Ideally we would use the BAO within two galax ...
... 2007). These are easily affected by smooth changes to the galaxy clustering amplitude as a function of scale. In this paper, we use a more robust approach: the BAO scale is defined via the locations where the BAO cross a smooth fit to the power spectrum. Ideally we would use the BAO within two galax ...
Red Supergiants and Extinction Law in the Large Magelanic Cloud
... equal weights were adopted for all pass-bands. The great advantage of the method lays in its differentiallity. In practice, there is no need to know how big the real extinctions are. Among the strengths of the method is the possibility to obtain true extinction curve if an appropriate pairs are chos ...
... equal weights were adopted for all pass-bands. The great advantage of the method lays in its differentiallity. In practice, there is no need to know how big the real extinctions are. Among the strengths of the method is the possibility to obtain true extinction curve if an appropriate pairs are chos ...
Chemical abundances of metal-poor RR Lyrae stars in the Magellanic Clouds
... can cover an age range of more than ten Gyr. Thus one can either turn to globular clusters as easily identifiable and reliably age-dateable populations or to uniquely identifiable, old tracer stars among field populations. For field stars the exclusively old Population II can only be traced with cer ...
... can cover an age range of more than ten Gyr. Thus one can either turn to globular clusters as easily identifiable and reliably age-dateable populations or to uniquely identifiable, old tracer stars among field populations. For field stars the exclusively old Population II can only be traced with cer ...
Anisotropy of the Hectometer Cosmic Radio Background
... existing estimates for the diffuse interstellar medium, κ = 4 × 10–3 (f[MHz])–2.1 [pc–1]. In this case, the value of r, which may be called a visibility horizon, is smaller than the characteristic half-thickness of the Galactic gas disk (~500 pc) even near 1 MHz, decreasing to 15 pc at f = 260 kHz. ...
... existing estimates for the diffuse interstellar medium, κ = 4 × 10–3 (f[MHz])–2.1 [pc–1]. In this case, the value of r, which may be called a visibility horizon, is smaller than the characteristic half-thickness of the Galactic gas disk (~500 pc) even near 1 MHz, decreasing to 15 pc at f = 260 kHz. ...
May 8 Matter & Chemistry
... What is the variable in this experiment? *ask yourself this question-what did he change during the experiment that would effect the outcome or results? C changing the mass, (increasing it) made the trolley gain speed. ...
... What is the variable in this experiment? *ask yourself this question-what did he change during the experiment that would effect the outcome or results? C changing the mass, (increasing it) made the trolley gain speed. ...
A Rotational and Variability Study of a Large Sample of... in NGC 2264 M. H. Lamm , C. A. L. Bailer-Jones
... Nebular cluster (ONC). They found that the period distribution for higher mass stars (i. e. M ≥ 0.25M ) is bimodal with peaks at 2 and 8 days. The bimodality is interpreted as an effect of disk-star interactions in PMS stars: Slow rotators have been magnetically locked to their disks which prevent ...
... Nebular cluster (ONC). They found that the period distribution for higher mass stars (i. e. M ≥ 0.25M ) is bimodal with peaks at 2 and 8 days. The bimodality is interpreted as an effect of disk-star interactions in PMS stars: Slow rotators have been magnetically locked to their disks which prevent ...
Morphology and dynamics of the cosmic web Aragón Calvo
... The results presented in this chapter are based on a galaxy sample selected from the largest galaxy survey to date, the Sloan Digital Sky Survey (SDSS). The SDSS is a wide-field photometric and spectroscopic survey carried out with a dedicated 2.5 meter telescope at Apache Point, New Mexico (York et ...
... The results presented in this chapter are based on a galaxy sample selected from the largest galaxy survey to date, the Sloan Digital Sky Survey (SDSS). The SDSS is a wide-field photometric and spectroscopic survey carried out with a dedicated 2.5 meter telescope at Apache Point, New Mexico (York et ...
preprint, pdf version - LESIA
... Aims. We derive precise astrometric predictions for stellar occultations by Eris, Haumea, Ixion, Makemake, Orcus, Quaoar, Sedna, Varuna, 2002 TX300 , and 2003 AZ84 for 2011–2015. We construct local astrometric catalogs of stars complete to magnitudes as faint as R = 18−19 in the UCAC2 (Second US Nav ...
... Aims. We derive precise astrometric predictions for stellar occultations by Eris, Haumea, Ixion, Makemake, Orcus, Quaoar, Sedna, Varuna, 2002 TX300 , and 2003 AZ84 for 2011–2015. We construct local astrometric catalogs of stars complete to magnitudes as faint as R = 18−19 in the UCAC2 (Second US Nav ...
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”, “ ...
Lecture 2
... • In recent years, the same group has been extending their survey to z=1-3 Current Topics: Lyman Break Galaxies - Lecture 2 ...
... • In recent years, the same group has been extending their survey to z=1-3 Current Topics: Lyman Break Galaxies - Lecture 2 ...
Head–tail Galaxies: beacons of high
... wide-angle tailed galaxies (WATs) believed to be the result of ‘cluster weather’ (Klamer et al. 2004). NATs are most likely to be caused by the passage of the galaxy through the cluster (Odea & Owen 1985) while WATs are more likely to be associated with dominant cluster galaxies (Owen & Rudnick 1976 ...
... wide-angle tailed galaxies (WATs) believed to be the result of ‘cluster weather’ (Klamer et al. 2004). NATs are most likely to be caused by the passage of the galaxy through the cluster (Odea & Owen 1985) while WATs are more likely to be associated with dominant cluster galaxies (Owen & Rudnick 1976 ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.