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Author: International Astronomical Union. Symposium
Publisher: Cambridge University Press
ISBN: 9780521889872
Category : Science
Languages : en
Pages : 552
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Book Description
This volume presents the most complete and up-to-date accounts of our understanding of the Magellanic Clouds and the astrophysical processes within them. Observations of these nearby dwarf galaxies continue to advance, calibrate and challenge our knowledge of the cosmos. They are rich in gas, they have been actively forming stars throughout their history, and they display a wealth of dynamical features. Poor in metals, they serve as a stepping stone towards understanding the high-redshift Universe. In IAU Symposium 256, scientists from vastly different fields of research discuss galactic dynamics, the physics of the interstellar medium and star formation, and the fundamental properties and evolution of stars. New insight was gained by crossing the traditional boundaries of these fields, placing the findings in the context of the structure and evolution of this interacting pair of galaxies uniquely available to our ever more powerful telescopes and computational machinery.
Author: International Astronomical Union. Symposium
Publisher: Cambridge University Press
ISBN: 9780521889872
Category : Science
Languages : en
Pages : 552
Get Book Here
Book Description
This volume presents the most complete and up-to-date accounts of our understanding of the Magellanic Clouds and the astrophysical processes within them. Observations of these nearby dwarf galaxies continue to advance, calibrate and challenge our knowledge of the cosmos. They are rich in gas, they have been actively forming stars throughout their history, and they display a wealth of dynamical features. Poor in metals, they serve as a stepping stone towards understanding the high-redshift Universe. In IAU Symposium 256, scientists from vastly different fields of research discuss galactic dynamics, the physics of the interstellar medium and star formation, and the fundamental properties and evolution of stars. New insight was gained by crossing the traditional boundaries of these fields, placing the findings in the context of the structure and evolution of this interacting pair of galaxies uniquely available to our ever more powerful telescopes and computational machinery.
Author: Brianna Marie Smart
Publisher:
ISBN:
Category :
Languages : en
Pages : 106
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Book Description
Our understanding of galaxies is limited by our place within the Milky Way and the vast distances to external galaxies. However, our proximity to the Magellanic Clouds, a pair of nearby galaxies in our Galaxy's halo, provides an opportunity to closely examine and survey a galactic system. Many surveys have been conducted of this system, giving a thorough look into some components of the galaxies and providing constraints to dynamic models of the system. But surveys of the ionized gas throughout the Magellanic System have been primarily limited to bright H II regions near young, hot stars and the energetic remnants of recent supernovae. Using the Wisconsin H-Alpha Mapper (WHAM), I have conducted the first survey of diffuse ionized gas throughout the extended Magellanic System, adding an essential view of a key component. First, I present the first extended diffuse ionized gas map of the Small Magellanic Cloud, which includes new kinematic information about the motion of this gas far from the center of the galaxy. Using these results, I calculate the first estimate of the total ionized gas around the SMC. Next, I present a survey of the Large Magellanic Cloud. Using methods developed from the Small Magellanic Cloud survey, I present the first extended diffuse ionized gas maps of the Large Magellanic Cloud and calculated the total ionized gas mass. Finally, I discuss the initial results of an H-alpha survey of Magellanic Stream that I designed and carried out. Covering a large region of the sky (40 by 120 degrees), this is the first attempt to detect and characterize the full extent of ionized gas within the Magellanic Stream. To highlight the progress of the survey reduction, I present four regions along the Stream and compare emission from neutral and ionized components. Together, these studies give new insight into the complex structure of the Magellanic System, explore the warm ionized medium in an interacting galactic system with unprecedented sensitivity, and produce new, more accurate estimates of the total ionized gas mass around the galaxies, providing important constraints for dynamic models of the system.
Author: Stephen Pardy
Publisher:
ISBN:
Category :
Languages : en
Pages : 0
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Book Description
How do low-mass galaxies grow into massive spirals like our Milky Way? How does cold gas reach the inner disks of galaxies to feed ongoing star formation? These are some of the fundamental outstanding questions in galaxy formation and evolution. The Magellanic System holds the key to answering these questions. This system consists of the Large and Small Magellanic Clouds (LMC and SMC), which are the closest example of interacting dwarf galaxies to us, and the Magellanic Stream; an extensive complex of cold and ionized gas that surrounds them. While the Magellanic System contains unambiguous evidence of gas accretion and galaxy interactions, its origin is still unexplained by current models. The LMC is uncommon among late-type galaxies because its stellar bar appears offset from its stellar disk. In addition, the Magellanic Stream is highly ionized, unexpectedly massive, and composed of material from both the LMC and SMC. Finally, there are claims of dwarf satellite galaxies aligned with the Magellanic Stream and the Clouds that support the notion that these dwarf galaxies might have arrived in the Milky Way with the LMC and SMC. In my thesis, I tackle these mysteries of the Magellanic System. My results clarify the origin and properties of the offset between the stellar bar and disk by showing that it is a long-lived feature that arises from the gravitational interaction between the LMC and the SMC. This result matches observational evidence of the tidal interaction between the LMC and SMC, and has implications for our measurements of other galaxies across the universe. My results also elucidate how this tidal interaction between the Clouds can strip gas from both the LMC and SMC into a long stream that both leads and trails the Clouds on the sky. This work makes predictions, which will be tested in future surveys, for the chemical abundances in the Leading Arm of the Stream. The Clouds' interaction history and their proximity to us suggest that they have undergone significant tidal stripping and may have been much more massive in the past. My work demonstrates how an LMC that was more massive would bring a significant amount of warm gas as it fell into the Milky Way. This gas will be the source of the missing ionized component of the Stream required to match the observations. Finally, I hypothesize the number of satellite dwarf galaxies that are expected to arrive with this massive LMC by examining analog galaxies in cosmological simulations. This result also has implications for our understanding of the satellite galaxy population of the Milky Way. This is a complete picture of the Magellanic System where the LMC entered the Milky Way as the largest galaxy of a group of dwarf galaxies with its own bound gas. The interactions between the LMC and SMC in this Magellanic Group combined with ram-pressure stripping from the Milky Way's hot halo create the long, high-mass Stream of ionized and neutral gas. The lessons we learn from the Magellanic Clouds will help us understand galaxy formation and evolution across the universe.
Author: Simon Richard Wayte
Publisher:
ISBN:
Category : Galaxies
Languages : en
Pages : 516
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Book Description
Author: Gurtina Besla
Publisher:
ISBN:
Category :
Languages : en
Pages : 654
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Book Description
Author: Harlow Shapley
Publisher:
ISBN:
Category : Magellanic Clouds
Languages : en
Pages : 18
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Book Description
Author: Drew Austen Ciampa
Publisher:
ISBN:
Category : Astrophysics
Languages : en
Pages : 115
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Book Description
Within our Galactic backyard, the Magellanic System, composed of the Large and Small Magellanic Clouds, is exchanging millions to billions of solar masses worth of material to the Milky Way. In two different studies, we explored this exchange and its impact on the Galactic environment. In the first study, a galactic outflow has erupted due to supernovae explosions within the disk. We present the first spectroscopically resolved H-alpha emission map of this wind. Kinematically, we find that the diffuse gas in the warm-ionized phase of the wind persists at both low (100km/s) and high (100km/s) velocities, relative to the LMC's HI disk. Furthermore, we find that the high-velocity component spatially aligns with the most intense star-forming region, 30~Doradus. We, therefore, conclude that this high-velocity material traces an active outflow. This wind is ejecting an estimated log(Mionized/Mo)=7.51 +/- 0.15 worth of material off the near-side of the galaxy. The second study observes tidally stripped gas that leads the LMC's orbit. This material formed into a massive complex called the Leading Arm that contains multiple sub-structures of gas. We investigate the physical and ionization conditions of this structure using Hubble Space Telescope/Cosmic Origins Spectrograph UV absorption-line and 21\,cm \hi\ emission-line observations along 13 sightlines. Additionally, we use Cloudy radiative transfer modeling to estimate their average temperatures, densities, ionization fractions, and thermal pressures. We find that most Leading Arm sub-structures exhibit multiple absorbers along their lines of sight, indicating a complex three-dimensional structure. Using the ionization fractions, we estimate that the total (neutral plus ionized) hydrogen mass of the LA sub-structures is M_H=3.0x10^8 Mo across a velocity range of +100
Author: Christian Brüns
Publisher:
ISBN:
Category : High-velocity clouds (Astrophysics)
Languages : en
Pages : 189
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Book Description
Author: Bengt E. Westerlund
Publisher: Cambridge University Press
ISBN: 9780521480703
Category : Science
Languages : en
Pages : 304
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Book Description
The first book to provide a synthesised and comprehensive account of the Magellanic Clouds.
Author: Raymond Haynes
Publisher: Springer Science & Business Media
ISBN: 9780792311102
Category : Science
Languages : en
Pages : 534
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Book Description
Symposium 148 "The Magellanic Clouds and their Dynamical Interaction with the Milky Way" was the first IAU Symposium held in Australia since 1973. In all, 23 countries were represented by 149 participants. The Symposium was held from July 9 to 13, 1990 at Womens College, the University of Sydney. The last symposium on the Magellanic Clouds' was held in 1983 in Ttibingen, Germany. Since then new ground-and satellite-based instruments have become available. A range of results from these instruments were presented at IAU Symposium 148 and are published in these proceedings. IAU Symposium 148 was timed to coincide with the commissioning of the Australia Telescope, and indeed, a few of the first results from that instrument were presented at this Symposium Over the next decade the Australia Telescope is destined to make a major impact on Magellanic Cloud research. Papers are arranged in five main sections reflecting the Symposium timetable: • Large-Scale Structure and Kinematics • Star Formation and Clustering • Stellar Evolution • The Interstellar Medium • The LMC-SMC-Galaxy System These are preceeded by both the introduction to and the summary of the Symposium. Questions and answers from the oral sessions are reproduced at the end of each section.
