Leakage of ionizing radiation from the nearby galaxy Tololo 1247
... Incidentally, both models (Razoumov & Sommer-Larsen 2007) and the existing obLyC servations can be interpreted as exhibiting an increase in fesc toward higher redshifts. A very crude estimate using the data collected in Bergvall et al. (2013) shows an increase LyC LyC LyC in the average value of fes ...
... Incidentally, both models (Razoumov & Sommer-Larsen 2007) and the existing obLyC servations can be interpreted as exhibiting an increase in fesc toward higher redshifts. A very crude estimate using the data collected in Bergvall et al. (2013) shows an increase LyC LyC LyC in the average value of fes ...
The Emission Line Spectrum of Active Galactic
... estimate has been made by the reverberation mapping method of the BH mass in 19 Seyfert 1s; these masses range from 0.4 to 40 107 M (Wandel et al. 1999). The ...
... estimate has been made by the reverberation mapping method of the BH mass in 19 Seyfert 1s; these masses range from 0.4 to 40 107 M (Wandel et al. 1999). The ...
On the characterisation of the Galactic warp in the Gaia era
... I would like to thank my supervisors Francesca Figueras and Luis Aguilar for all I have learned from them. You both are the best teachers any student can ask for. Thank you Francesca for all of your support and patience, aspiring guidance and immense knowledge. You always made time to help and advis ...
... I would like to thank my supervisors Francesca Figueras and Luis Aguilar for all I have learned from them. You both are the best teachers any student can ask for. Thank you Francesca for all of your support and patience, aspiring guidance and immense knowledge. You always made time to help and advis ...
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 ...
Extragalactic background light inferred from AEGIS
... The extragalactic background light (EBL) is of fundamental importance both for understanding the entire process of galaxy evolution and for γ -ray astronomy, but the overall spectrum of the EBL between 0.1 and 1000 µm has never been determined directly from galaxy spectral energy distribution (SED) ...
... The extragalactic background light (EBL) is of fundamental importance both for understanding the entire process of galaxy evolution and for γ -ray astronomy, but the overall spectrum of the EBL between 0.1 and 1000 µm has never been determined directly from galaxy spectral energy distribution (SED) ...
Astronomy Astrophysics
... for obvious stellar overdensities towards known star forming regions in the Galactic disk. That procedure was repeated here, but we now include the area encompassing the Galactic bulge. The analysis yielded 58 new cluster candidates. These are not necessarily connected with HII regions, but clearly ...
... for obvious stellar overdensities towards known star forming regions in the Galactic disk. That procedure was repeated here, but we now include the area encompassing the Galactic bulge. The analysis yielded 58 new cluster candidates. These are not necessarily connected with HII regions, but clearly ...
Grand Design and Flocculent Spirals in the Spitzer Survey of Stellar
... that later Hubble types have larger relative bar torques because the bulges are weaker. Combes & Elmegreen (1993) and Athanassoula & Misiriotis (2002) simulated flat and exponential bars by varying the inner rotation curve or halo concentration. Flat bars tend to occur in galaxies with sharply risin ...
... that later Hubble types have larger relative bar torques because the bulges are weaker. Combes & Elmegreen (1993) and Athanassoula & Misiriotis (2002) simulated flat and exponential bars by varying the inner rotation curve or halo concentration. Flat bars tend to occur in galaxies with sharply risin ...
An Atlas of Stellar Spectra
... The problem of a classification according to luminosity is a difficult one. In the first place, lines or blends which may be useful at one spectral type may be quite insensitive at another. In fact, some lines which show a positive absolute-magnitude effect for some spectral classes may show a negat ...
... The problem of a classification according to luminosity is a difficult one. In the first place, lines or blends which may be useful at one spectral type may be quite insensitive at another. In fact, some lines which show a positive absolute-magnitude effect for some spectral classes may show a negat ...
white_paper.word - Space Telescope Science Institute
... from ~ 0.1" to 0.25" in spatially adjacent (but non-contiguous) narrow and wide fields-of-view. Working in space in the NIR (from 0.8 – 2.4 m), NICMOS peers through dusty regions obscured at optical wavelengths that are otherwise compromised by the intrinsic brightness, wavelength-dependent opacity ...
... from ~ 0.1" to 0.25" in spatially adjacent (but non-contiguous) narrow and wide fields-of-view. Working in space in the NIR (from 0.8 – 2.4 m), NICMOS peers through dusty regions obscured at optical wavelengths that are otherwise compromised by the intrinsic brightness, wavelength-dependent opacity ...
i.3. - adaptive optics overview
... from ~ 0.1" to 0.25" in spatially adjacent (but non-contiguous) narrow and wide fields-of-view. Working in space in the NIR (from 0.8 – 2.4 m), NICMOS peers through dusty regions obscured at optical wavelengths that are otherwise compromised by the intrinsic brightness, wavelength-dependent opacity ...
... from ~ 0.1" to 0.25" in spatially adjacent (but non-contiguous) narrow and wide fields-of-view. Working in space in the NIR (from 0.8 – 2.4 m), NICMOS peers through dusty regions obscured at optical wavelengths that are otherwise compromised by the intrinsic brightness, wavelength-dependent opacity ...
Brochure - Institut für Raumfahrtsysteme
... conspicuous dust lane encircles the Sombrero Galaxy (M104, Fig. 2). This region contains most of the galaxy’s molecular gas and dust, both of which are essential ingredients for star formation. While emitting continuous thermal radiation, dust cools the interstellar medium. With thermal pressure dec ...
... conspicuous dust lane encircles the Sombrero Galaxy (M104, Fig. 2). This region contains most of the galaxy’s molecular gas and dust, both of which are essential ingredients for star formation. While emitting continuous thermal radiation, dust cools the interstellar medium. With thermal pressure dec ...
![arXiv:1601.01542v1 [astro-ph.GA] 7 Jan 2016](http://s1.studyres.com/store/data/017487687_1-243c4cbda96da53325dd347b0c588a3e-300x300.png)
Diapositiva 1
... Slow pulsars with low magnetic fields are not observable as radio sources any more ...
... Slow pulsars with low magnetic fields are not observable as radio sources any more ...
X-ray binaries in the Milky Way and other galaxies
... 4.1. Comparison of the differential Log(N)–Log(S) relation for Galactic XRBs from ASM and ASCA . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.2. Comparison of the number-flux relation observed in the ASCA GRS and the predicted Log(N)–Log(S) from ASM luminosity functions. . . . . . . . . ...
... 4.1. Comparison of the differential Log(N)–Log(S) relation for Galactic XRBs from ASM and ASCA . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.2. Comparison of the number-flux relation observed in the ASCA GRS and the predicted Log(N)–Log(S) from ASM luminosity functions. . . . . . . . . ...
The Mass of Quasars Yue Shen
... Zel’dovich & Novikov 1964; Lynden-Bell 1969). The standard picture now is that mass is accreted onto a supermassive black hole (SMBH) at the center of the galaxy, and the gravitational energy is released during this accretion process to power quasar activity. If the SMBH grows mostly via this accret ...
... Zel’dovich & Novikov 1964; Lynden-Bell 1969). The standard picture now is that mass is accreted onto a supermassive black hole (SMBH) at the center of the galaxy, and the gravitational energy is released during this accretion process to power quasar activity. If the SMBH grows mostly via this accret ...
The correlation between galaxy morphology and star
... formation and evolution of galaxies. Massive galaxies in the nearby universe are well described by the Hubble sequence, which correlates with the dominance of galaxy’s central bulge, surface brightness and colors. Hubble types are also broadly correlated with physical parameters, such as the star fo ...
... formation and evolution of galaxies. Massive galaxies in the nearby universe are well described by the Hubble sequence, which correlates with the dominance of galaxy’s central bulge, surface brightness and colors. Hubble types are also broadly correlated with physical parameters, such as the star fo ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.