Annual Report 2006/2007
... supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. T ...
... supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. T ...
SPIRAL STRUCTURE IN THE OUTER GALACTIC
... According to the age and the places where they are located, clusters present a variety of challenges in deriving their intrinsic parameters. In the case of very young clusters, they are normally close to the Galactic plane where interstellar absorption and crowded stellar fields make membership assi ...
... According to the age and the places where they are located, clusters present a variety of challenges in deriving their intrinsic parameters. In the case of very young clusters, they are normally close to the Galactic plane where interstellar absorption and crowded stellar fields make membership assi ...
The SAMI Galaxy Survey: extraplanar gas, galactic winds, and their
... et al. 2005 for a review). The optical line-emitting gas usually presents well-defined conical structures, which are the limb-brightened parts of the expanding X-ray bubbles that also entrain the ambient cold gas. As the bubbles expand supersonically, shock waves excite optical emission lines and pr ...
... et al. 2005 for a review). The optical line-emitting gas usually presents well-defined conical structures, which are the limb-brightened parts of the expanding X-ray bubbles that also entrain the ambient cold gas. As the bubbles expand supersonically, shock waves excite optical emission lines and pr ...
GAS ACCRETION AND COUNTER-ROTATION IN DISK GALAXIES
... direction of the slit (N to S). The vertical direction is the direction of the dispersion. The bright vertical line is the spectrum of the galactic nucleus. The dark features are stellar absorption lines. They match into the characteristic X-shape in correspondence to the galactic nucleus, due to th ...
... direction of the slit (N to S). The vertical direction is the direction of the dispersion. The bright vertical line is the spectrum of the galactic nucleus. The dark features are stellar absorption lines. They match into the characteristic X-shape in correspondence to the galactic nucleus, due to th ...
The Collision Between The Milky Way And Andromeda
... time, some of the initial intragroup gas is expected be accreted by each galaxy, and most of the remaining intragroup gas will end up being shock–heated during the collapse and relaxation of the Local Group. The dynamics of the merger 3 The initial scale of the Local group in our simulation is an or ...
... time, some of the initial intragroup gas is expected be accreted by each galaxy, and most of the remaining intragroup gas will end up being shock–heated during the collapse and relaxation of the Local Group. The dynamics of the merger 3 The initial scale of the Local group in our simulation is an or ...
Mapping the Pathways of Galaxy Transformation Across Time and
... Is “quenching” the termination of star formation or the compression of star formation histories (SFHs)? I discuss the deep implications this reframing has for what we see as and how we study core processes shaping galaxy life-cycles. As a lens, I use two outcomes from the IMACS Cluster-Building Surv ...
... Is “quenching” the termination of star formation or the compression of star formation histories (SFHs)? I discuss the deep implications this reframing has for what we see as and how we study core processes shaping galaxy life-cycles. As a lens, I use two outcomes from the IMACS Cluster-Building Surv ...
2. The X-ray-Radio correlation for bulgeless galaxies
... Fig. 20: The bulgeless galaxies detected in the X-ray band by the C-COSMOS survey. The continuous line represents the luminosity detection limit for the survey in respect to the redshift. The dashed line represents the limit above which galaxies are considered AGN................................... ...
... Fig. 20: The bulgeless galaxies detected in the X-ray band by the C-COSMOS survey. The continuous line represents the luminosity detection limit for the survey in respect to the redshift. The dashed line represents the limit above which galaxies are considered AGN................................... ...
witnessing the birth of the red sequence
... ALMA pipeline and by executing different ALMA calibration scripts depending on the date when the data were released. The calibrated visibilities for the calibrators and science target were visually inspected and only very minor further flagging was required. The calibrated visibilities of the science ...
... ALMA pipeline and by executing different ALMA calibration scripts depending on the date when the data were released. The calibrated visibilities for the calibrators and science target were visually inspected and only very minor further flagging was required. The calibrated visibilities of the science ...
Science with the Constellation
... Universe. Today we are confident that their ultimate power source is the release of gravitational energy sustained by an accretion disk, which is feeding matter directly into a central supermassive black hole. Such black holes appear to reside at the centers of most galaxies, and they have masses of ...
... Universe. Today we are confident that their ultimate power source is the release of gravitational energy sustained by an accretion disk, which is feeding matter directly into a central supermassive black hole. Such black holes appear to reside at the centers of most galaxies, and they have masses of ...
Infrared Properties of Star-Forming Dwarf Galaxies. I. Dwarf Irregular
... 1. Detection of the [O iii] k4363 emission line for the determination of oxygen abundances. 2. A reliable distance (i.e., determined from stellar constituents, such as Cepheids and the tip of the RGB [TRGB]). ...
... 1. Detection of the [O iii] k4363 emission line for the determination of oxygen abundances. 2. A reliable distance (i.e., determined from stellar constituents, such as Cepheids and the tip of the RGB [TRGB]). ...
![THE SPATIALLY RESOLVED [Cii] COOLING LINE DEFICIT IN](http://s1.studyres.com/store/data/023160905_1-0e54338357f8801ad3946849a853f5fc-300x300.png)
THE SPATIALLY RESOLVED [Cii] COOLING LINE DEFICIT IN
... is found to vary by orders of magnitude among different galaxy types and environments (Malhotra et al. 1997, 2001; Luhman et al. 2003; Brauher et al. 2008; Stacey et al. 2010; GraciáCarpio et al. 2011; Díaz-Santos et al. 2013). This so-called [C II] cooling line deficit problem, first revealed as an u ...
... is found to vary by orders of magnitude among different galaxy types and environments (Malhotra et al. 1997, 2001; Luhman et al. 2003; Brauher et al. 2008; Stacey et al. 2010; GraciáCarpio et al. 2011; Díaz-Santos et al. 2013). This so-called [C II] cooling line deficit problem, first revealed as an u ...
Probing Dark Energy with Lensing Magnification in Photometric
... attempting to minimize both wgg and wgµ to measure wµµ . This latter term is typically an order-of-magnitude smaller than even wgµ , which would require unrealistically large galaxy samples for a statistically significant measurement. Ref. [20] showed that the clustering (wgg ) and magnification (wg ...
... attempting to minimize both wgg and wgµ to measure wµµ . This latter term is typically an order-of-magnitude smaller than even wgµ , which would require unrealistically large galaxy samples for a statistically significant measurement. Ref. [20] showed that the clustering (wgg ) and magnification (wg ...
Quantitative constraints on starburst cycles in galaxies with stellar
... galaxies with strong emission lines (BCD galaxies), which are clearly undergoing strong starbursts at the present day (e.g. Searle & Sargent 1972; Meurer et al 1995). In very nearby galaxies where individual stars can be resolved in high quality images, star formation histories for individual system ...
... galaxies with strong emission lines (BCD galaxies), which are clearly undergoing strong starbursts at the present day (e.g. Searle & Sargent 1972; Meurer et al 1995). In very nearby galaxies where individual stars can be resolved in high quality images, star formation histories for individual system ...
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.