Galaxy Assembly through Mergers
... a music made from Figure 2.16. Inspiration definitely comes in many forms, shapes and colors. Just like galaxies. The last few years have been nothing short of a roller coaster ride – they have taught me more about science, myself and others, than I could possibly imagine. I cannot wait for the ride ...
... a music made from Figure 2.16. Inspiration definitely comes in many forms, shapes and colors. Just like galaxies. The last few years have been nothing short of a roller coaster ride – they have taught me more about science, myself and others, than I could possibly imagine. I cannot wait for the ride ...
Infall times for Milky Way satellites from their present
... We analyse subhaloes in the Via Lactea II (VL2) cosmological simulation to look for correlations among their infall times and z = 0 dynamical properties. We find that the present-day orbital energy is tightly correlated with the time at which subhaloes last entered within the virial radius. This ene ...
... We analyse subhaloes in the Via Lactea II (VL2) cosmological simulation to look for correlations among their infall times and z = 0 dynamical properties. We find that the present-day orbital energy is tightly correlated with the time at which subhaloes last entered within the virial radius. This ene ...
The correlation between galaxy morphology and star
... Significant improvements are now possible using larger samples of panchromatic images from the CANDELS (Cosmic Assembly Near-infrared Extragalactic Legacy Survey) observations. Wuyts et al. (2011) investigated how the structure of galaxies (Sérsic index and size) depends on galaxy position in the S ...
... Significant improvements are now possible using larger samples of panchromatic images from the CANDELS (Cosmic Assembly Near-infrared Extragalactic Legacy Survey) observations. Wuyts et al. (2011) investigated how the structure of galaxies (Sérsic index and size) depends on galaxy position in the S ...
Galaxy and Mass Assembly (GAMA): the red fraction and radial
... to have a significant effect on the morphology of galaxies. Investigating the red fraction of satellites by mass, they estimate that 70 per cent of satellite galaxies with M∗ = 109 M have undergone satellite quenching in order to be on the red sequence at the present, with 30 per cent already red b ...
... to have a significant effect on the morphology of galaxies. Investigating the red fraction of satellites by mass, they estimate that 70 per cent of satellite galaxies with M∗ = 109 M have undergone satellite quenching in order to be on the red sequence at the present, with 30 per cent already red b ...
The ACS Survey of Galactic Globular Clusters: M54 and Young
... Gyr, LS00). Large surveys of Sgr’s core are dominated by intermediate stellar populations ([Fe/H]=-0.4 to -0.7, 5-8 Gyr; SL95, LS00, Bellazzini et al. 2006a; hereafter B06), though this is likely due to Sgr’s MPPs having been selectively stripped into tidal tails (Chou et al. 2007). There have also ...
... Gyr, LS00). Large surveys of Sgr’s core are dominated by intermediate stellar populations ([Fe/H]=-0.4 to -0.7, 5-8 Gyr; SL95, LS00, Bellazzini et al. 2006a; hereafter B06), though this is likely due to Sgr’s MPPs having been selectively stripped into tidal tails (Chou et al. 2007). There have also ...
Star Formation in the Milky Way and Nearby Galaxies Further
... star formation on all scales, thanks in no small part to new facilities such as the Galaxy Evolution Explorer (GALEX), the Spitzer Space Telescope, and the Herschel Space Observatory; the introduction of powerful new instruments on the Hubble Space Telescope (HST); and a host of ground-based optical ...
... star formation on all scales, thanks in no small part to new facilities such as the Galaxy Evolution Explorer (GALEX), the Spitzer Space Telescope, and the Herschel Space Observatory; the introduction of powerful new instruments on the Hubble Space Telescope (HST); and a host of ground-based optical ...
Isolated elliptical galaxies in the local Universe
... ∼8% are star forming, and ≈10% are recently quenched, while among the Coma ellipticals ≈8% are blue and just < ∼1% are star forming or recently quenched. There are four isolated galaxies (≈4.5%) that are blue and star forming at the same time. These galaxies, with masses between 7 × 109 and 2 × 1010 ...
... ∼8% are star forming, and ≈10% are recently quenched, while among the Coma ellipticals ≈8% are blue and just < ∼1% are star forming or recently quenched. There are four isolated galaxies (≈4.5%) that are blue and star forming at the same time. These galaxies, with masses between 7 × 109 and 2 × 1010 ...
Hubble 2006: Science Year in Review
... The final servicing mission in 2008 will install two new instruments, the Cosmic Origins Spectrograph (COS) and Wide Field Camera 3 (WFC3). COS is the most sensitive ultraviolet spectrograph ever built for Hubble. The instrument will probe the cosmic web—the large-scale structure of the universe—who ...
... The final servicing mission in 2008 will install two new instruments, the Cosmic Origins Spectrograph (COS) and Wide Field Camera 3 (WFC3). COS is the most sensitive ultraviolet spectrograph ever built for Hubble. The instrument will probe the cosmic web—the large-scale structure of the universe—who ...
using WISE to quantify the rarity of warm dust around Kepler stars
... the flux measurements associated with these excesses are spurious. We identify 271 stars with plausible excesses by making a 5MJy/sr cut in the IRAS 100µm emission. The number counts of these excesses, at both 12 and 22µm, have the same distribution as extra-Galactic number counts. Thus, although so ...
... the flux measurements associated with these excesses are spurious. We identify 271 stars with plausible excesses by making a 5MJy/sr cut in the IRAS 100µm emission. The number counts of these excesses, at both 12 and 22µm, have the same distribution as extra-Galactic number counts. Thus, although so ...
Niraj D. Welikala Thesis - D-Scholarship@Pitt
... sampling a wide range of properties such as age, star formation rate (SFR), dust obscuration and metallicity. By summing the SFRs in the pixels, I show that, as found in other studies, the distribution of total galaxy SFR shifts to lower values as the local density of surrounding galaxies increases. ...
... sampling a wide range of properties such as age, star formation rate (SFR), dust obscuration and metallicity. By summing the SFRs in the pixels, I show that, as found in other studies, the distribution of total galaxy SFR shifts to lower values as the local density of surrounding galaxies increases. ...
Catalogue of observed tangents to the spiral
... hot), gas (molecular and atomic), ionized gas and thermal electrons, cosmic rays and relativistic electrons, and magnetic fields. For a review of some physical properties (density, temperature, etc) of the gas phases and the magnetic fields in the interstellar medium, see Heiles & Haverkorn (2012). ...
... hot), gas (molecular and atomic), ionized gas and thermal electrons, cosmic rays and relativistic electrons, and magnetic fields. For a review of some physical properties (density, temperature, etc) of the gas phases and the magnetic fields in the interstellar medium, see Heiles & Haverkorn (2012). ...
Messier 87
Messier 87 (also known as Virgo A or NGC 4486, and generally abbreviated to M87) is a supergiant elliptical galaxy in the constellation Virgo. One of the most massive galaxies in the local universe, it is notable for its large population of globular clusters—M87 contains about 12,000 compared to the 150-200 orbiting the Milky Way—and its jet of energetic plasma that originates at the core and extends outward at least 1,500 parsecs (4,900 light-years), travelling at relativistic speed. It is one of the brightest radio sources in the sky, and is a popular target for both amateur astronomy observations and professional astronomy study.French astronomer Charles Messier discovered M87 in 1781, cataloguing it as a nebulous feature while searching for objects that would confuse comet hunters. The second brightest galaxy within the northern Virgo Cluster, M87 is located about 16.4 million parsecs (53.5 million light-years) from Earth. Unlike a disk-shaped spiral galaxy, M87 has no distinctive dust lanes. Instead, it has an almost featureless, ellipsoidal shape typical of most giant elliptical galaxies, diminishing in luminosity with distance from the centre. Forming around one sixth of M87's mass, the stars in this galaxy have a nearly spherically symmetric distribution, their density decreasing with increasing distance from the core. At the core is a supermassive black hole, which forms the primary component of an active galactic nucleus. This object is a strong source of multiwavelength radiation, particularly radio waves. M87's galactic envelope extends out to a radius of about 150 kiloparsecs (490,000 light-years), where it has been truncated—possibly by an encounter with another galaxy. Between the stars is a diffuse interstellar medium of gas that has been chemically enriched by elements emitted from evolved stars.