Multiple minor mergers: formation of elliptical galaxies and
... The nomenclature for each run is as follows: NxM:1 indicates that the galaxy has undergone N mergers with companions of mass 1/M of the target galaxy mass. We have simulated mass ratios M of 1, 3, 5, 7, 10, 15, and N varying from 1 to M (by steps of 2 for M=15). In sequences with mass ratios up to 1 ...
... The nomenclature for each run is as follows: NxM:1 indicates that the galaxy has undergone N mergers with companions of mass 1/M of the target galaxy mass. We have simulated mass ratios M of 1, 3, 5, 7, 10, 15, and N varying from 1 to M (by steps of 2 for M=15). In sequences with mass ratios up to 1 ...
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 ...
Identifying the progenitor set of present-day early
... evolve without interactions thereafter, while in the field the corresponding value is ∼30 percent. Averaging across all environments at z ∼ 1, less than 50 percent of the stellar mass which ends up in early-types today is actually in early-type progenitors at this redshift, in agreement with recent ...
... evolve without interactions thereafter, while in the field the corresponding value is ∼30 percent. Averaging across all environments at z ∼ 1, less than 50 percent of the stellar mass which ends up in early-types today is actually in early-type progenitors at this redshift, in agreement with recent ...
CH16.AST1001.S15.EDS
... Our goals for learning: • What is the evidence for supermassive black holes at the centers of galaxies? • Why do we think the growth of central black holes is related to galaxy evolution? ...
... Our goals for learning: • What is the evidence for supermassive black holes at the centers of galaxies? • Why do we think the growth of central black holes is related to galaxy evolution? ...
Galaxy Morphology - The University of Alabama
... facilitating citizen science at its best. Galaxy Zoo images are also in color, thus allowing the recognition of special galaxy types and features based on stellar populations or gaseous emission. 5. Finally, deep surveys with the Hubble Space Telescope have extended morphological studies well beyond ...
... facilitating citizen science at its best. Galaxy Zoo images are also in color, thus allowing the recognition of special galaxy types and features based on stellar populations or gaseous emission. 5. Finally, deep surveys with the Hubble Space Telescope have extended morphological studies well beyond ...
Abstract book
... Topic A (Day 1 and 2): Observational properties of active galactic nuclei This session should discuss the most relevant photometric, spectroscopic, polarimetric, and variability observations over the full SED, together with their interpretation, with attention to both statistical results and case st ...
... Topic A (Day 1 and 2): Observational properties of active galactic nuclei This session should discuss the most relevant photometric, spectroscopic, polarimetric, and variability observations over the full SED, together with their interpretation, with attention to both statistical results and case st ...
Isolated elliptical galaxies in the local Universe
... Context. We have studied a sample of 89 very isolated, elliptical galaxies at z < 0.08 and compared their properties with elliptical galaxies located in a high-density environment such as the Coma supercluster. Aims. Our aim is to probe the role of environment on the morphological transformation and ...
... Context. We have studied a sample of 89 very isolated, elliptical galaxies at z < 0.08 and compared their properties with elliptical galaxies located in a high-density environment such as the Coma supercluster. Aims. Our aim is to probe the role of environment on the morphological transformation and ...
GRB 990123 - University of Iowa Astrophysics
... • Edge of sphere (photosphere) will expand at a speed close to c as long as kT > mec2 • If baryons are added, most energy goes into accelerating baryons to ~ E/Mc2 ...
... • Edge of sphere (photosphere) will expand at a speed close to c as long as kT > mec2 • If baryons are added, most energy goes into accelerating baryons to ~ E/Mc2 ...
Galaxy pairs in the Sloan Digital Sky Survey III. Evidence of induced
... if one detects differences between interacting and non-interacting galaxies, it is difficult to distinguish between interaction-induced effects (such as triggered star formation) and pre-interaction differences (e.g. if interacting and non-interacting galaxies reside in different environments). One ...
... if one detects differences between interacting and non-interacting galaxies, it is difficult to distinguish between interaction-induced effects (such as triggered star formation) and pre-interaction differences (e.g. if interacting and non-interacting galaxies reside in different environments). One ...
Molecular gas in the barred spiral galaxy M 83 Andreas Andersson Lundgren
... Molecular gas is one of the most important constituents to consider in any study of the structure and evolution of spiral galaxies. It is the fuel for future star formation, and, due to its dissipative nature, it will respond quickly and strongly to dynamical influences. Despite its ubiquity, hydrog ...
... Molecular gas is one of the most important constituents to consider in any study of the structure and evolution of spiral galaxies. It is the fuel for future star formation, and, due to its dissipative nature, it will respond quickly and strongly to dynamical influences. Despite its ubiquity, hydrog ...
Stars and Galaxies PowerPoint
... truck moves towards you, and lower as it moves away from you Visible wavelengths emitted by objects moving away from us are shifted towards the red part of the visible spectrum The faster they move away from us, the more they are redshifted. Thus, redshift is a reasonable way to measure the spee ...
... truck moves towards you, and lower as it moves away from you Visible wavelengths emitted by objects moving away from us are shifted towards the red part of the visible spectrum The faster they move away from us, the more they are redshifted. Thus, redshift is a reasonable way to measure the spee ...
Stars and Galaxies - Lunar and Planetary Institute
... truck moves towards you, and lower as it moves away from you Visible wavelengths emitted by objects moving away from us are shifted towards the red part of the visible spectrum The faster they move away from us, the more they are redshifted. Thus, redshift is a reasonable way to measure the spee ...
... truck moves towards you, and lower as it moves away from you Visible wavelengths emitted by objects moving away from us are shifted towards the red part of the visible spectrum The faster they move away from us, the more they are redshifted. Thus, redshift is a reasonable way to measure the spee ...
A simple model to interpret the ultraviolet, optical and infrared
... infrared wavelengths. We compute the spectral evolution of stellar populations using the Bruzual & Charlot (2003) population synthesis code. To describe the attenuation of starlight by dust, we appeal to the two-component model of Charlot & Fall (2000). This has been shown to account for the observe ...
... infrared wavelengths. We compute the spectral evolution of stellar populations using the Bruzual & Charlot (2003) population synthesis code. To describe the attenuation of starlight by dust, we appeal to the two-component model of Charlot & Fall (2000). This has been shown to account for the observe ...
Molecular gas and dust in Arp 94: The formation of a recycled galaxy
... where we also detect large quantities of molecular gas (Braine et al. 2000, 2001, Lisenfeld et al. 2002) and where enough tidal material is often available to build a dwarf galaxy (Tidal Dwarf Galaxies, hereafter TDGs). Indeed, tidal interactions between approximately equalmass gas-rich galaxies hav ...
... where we also detect large quantities of molecular gas (Braine et al. 2000, 2001, Lisenfeld et al. 2002) and where enough tidal material is often available to build a dwarf galaxy (Tidal Dwarf Galaxies, hereafter TDGs). Indeed, tidal interactions between approximately equalmass gas-rich galaxies hav ...
The redshift evolution of the distribution of star formation among dark
... of mid-infrared-to-radio number counts. It contains two types of star-forming galaxies with different spectral energy distributions (SEDs): secularly star-forming MS galaxies and a population of episodic, probably merger-driven starbursts with a strong excess of SFR compared to the main sequence foll ...
... of mid-infrared-to-radio number counts. It contains two types of star-forming galaxies with different spectral energy distributions (SEDs): secularly star-forming MS galaxies and a population of episodic, probably merger-driven starbursts with a strong excess of SFR compared to the main sequence foll ...
Universe 8e Lecture Chapter 23 Our Galaxy
... According to the density-wave theory, spiral arms are created by density waves that sweep around the Galaxy. The gravitational field of this spiral pattern compresses the interstellar clouds through which it passes, thereby triggering the formation of the OB associations and H II regions that illumi ...
... According to the density-wave theory, spiral arms are created by density waves that sweep around the Galaxy. The gravitational field of this spiral pattern compresses the interstellar clouds through which it passes, thereby triggering the formation of the OB associations and H II regions that illumi ...
lecture
... UGC 8877) 2)planar model with noncircular velocity also fits observation. ◆ Peterson & Huntley (1980,ApJ,242,913) NGC 1300 (prototypical barred galaxy, SBb) Observations: long-slit emission line spectroscopy at various positions (Hα, [NII], [SII]) Stellar absorption line spectroscopy along the bar ...
... UGC 8877) 2)planar model with noncircular velocity also fits observation. ◆ Peterson & Huntley (1980,ApJ,242,913) NGC 1300 (prototypical barred galaxy, SBb) Observations: long-slit emission line spectroscopy at various positions (Hα, [NII], [SII]) Stellar absorption line spectroscopy along the bar ...
ALMA 50 antennas: 1225 baselines
... incoming wavefront arrives at each antenna at a different phase. For good image quality: many baselines n antennas: n(n-1)/2 spacings (ALMA 50 antennas: 1225 baselines) ...
... incoming wavefront arrives at each antenna at a different phase. For good image quality: many baselines n antennas: n(n-1)/2 spacings (ALMA 50 antennas: 1225 baselines) ...
Lifetime of merger features of equal
... and stars from numerical simulations (Silva et al. 1998; Jonsson 2006). Although this method provides detailed and extensive panchromatic data for galaxies, it requires high computational costs. The other method is to directly assign spectral data to a single stellar population using population synt ...
... and stars from numerical simulations (Silva et al. 1998; Jonsson 2006). Although this method provides detailed and extensive panchromatic data for galaxies, it requires high computational costs. The other method is to directly assign spectral data to a single stellar population using population synt ...
Ch. 23
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students exc ...
... the use of instructors in teaching their courses and assessing student learning. Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students exc ...
Molecular Gas in Late-stage Merging Galaxies
... low gas mass fractions requires further studies to investigate whether a large amount of cold gas will settle on the extended gas disks by the returning of the ejected cold gas via tidal tails and cold gas stream/accretion. For six merger remnants whose velocity fields cannot be modeled with circula ...
... low gas mass fractions requires further studies to investigate whether a large amount of cold gas will settle on the extended gas disks by the returning of the ejected cold gas via tidal tails and cold gas stream/accretion. For six merger remnants whose velocity fields cannot be modeled with circula ...
Stars
... objects are scattered • The smallest type of galaxy • Caused by other nearby objects disturbing the gravity or by colliding galaxies • Young galaxies Back to Galaxies Menu ...
... objects are scattered • The smallest type of galaxy • Caused by other nearby objects disturbing the gravity or by colliding galaxies • Young galaxies Back to Galaxies Menu ...
Star Formation in Galaxies Along the Hubble Sequence
... of galaxies, Roberts’ analysis established the basic elements of the contemporary picture of the Hubble sequence as a monotonic sequence in present-day SFRs and past star formation histories. Quantifying this picture required the development of more precise diagnostics of global SFRs in galaxies. T ...
... of galaxies, Roberts’ analysis established the basic elements of the contemporary picture of the Hubble sequence as a monotonic sequence in present-day SFRs and past star formation histories. Quantifying this picture required the development of more precise diagnostics of global SFRs in galaxies. T ...
Seyfert galaxy
Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.Seyfert galaxies account for about 10% of all galaxies and are some of the most intensely studied objects in astronomy, as they are thought to be powered by the same phenomena that occur in quasars, although they are closer and less luminous than quasars. These galaxies have supermassive black holes at their centers which are surrounded by accretion discs of in-falling material. The accretion discs are believed to be the source of the observed ultraviolet radiation. Ultraviolet emission and absorption lines provide the best diagnostics for the composition of the surrounding material.Seen in visible light, most Seyfert galaxies look like normal spiral galaxies, but when studied under other wavelengths, it becomes clear that the luminosity of their cores is of comparable intensity to the luminosity of whole galaxies the size of the Milky Way.Seyfert galaxies are named after Carl Seyfert, who first described this class in 1943.