Molecular Gas in the Large Magellanic Cloud
... At the Centre for Astrophysics and Supercomputing, I am especially grateful to Matthew Bailes, who convinced me to move to Melbourne and introduced me to astronomy research while I was still a first-year undergraduate. The Centre will be hard-pressed to find a Director who promotes and advocates for s ...
... At the Centre for Astrophysics and Supercomputing, I am especially grateful to Matthew Bailes, who convinced me to move to Melbourne and introduced me to astronomy research while I was still a first-year undergraduate. The Centre will be hard-pressed to find a Director who promotes and advocates for s ...
Composition and Evolution of Interstellar Clouds
... A large fraction of the volume of the Milky Way is filled with the HIM, i.e., a tenuous, ionized coronal gas (McKee and Ostriker, 1977). Supernovae explosions generate the coronal gas (Spitzer, 1990) when their ejecta collide with and shock the surrounding medium. Expanding supernova ejecta sweep up ...
... A large fraction of the volume of the Milky Way is filled with the HIM, i.e., a tenuous, ionized coronal gas (McKee and Ostriker, 1977). Supernovae explosions generate the coronal gas (Spitzer, 1990) when their ejecta collide with and shock the surrounding medium. Expanding supernova ejecta sweep up ...
Probing nuclear activity versus star formation at z ∼ 0.8 using near
... galaxies. However, when they only considered star-forming galaxies in the control sample (i.e. they discarded quiescent galaxies), they found roughly the same level of star formation as in the AGN hosts. A similar result was found by Lutz et al. (2010), based on submillimetre data of a sample of 895 ...
... galaxies. However, when they only considered star-forming galaxies in the control sample (i.e. they discarded quiescent galaxies), they found roughly the same level of star formation as in the AGN hosts. A similar result was found by Lutz et al. (2010), based on submillimetre data of a sample of 895 ...
Revising the census of low luminosity AGN
... WHY AN AGN CENSUS? • A PROPER AGN CENSUS IS NEEDED FOR A VARIETY OF STUDIES, SUCH AS, E.G. , THE AGN/HOST GALAXY CONNECTION, THE PROPERTIES OF THE CENTRAL ENGINE, THE AGN LUMINOSITY FUNCTION … • THE CENSUS SHOULD BE COMPLETE (OR AT LEAST WITH WELL DEFINED BIASES) AND INCLUDE THE LEAST NUMBER OF INT ...
... WHY AN AGN CENSUS? • A PROPER AGN CENSUS IS NEEDED FOR A VARIETY OF STUDIES, SUCH AS, E.G. , THE AGN/HOST GALAXY CONNECTION, THE PROPERTIES OF THE CENTRAL ENGINE, THE AGN LUMINOSITY FUNCTION … • THE CENSUS SHOULD BE COMPLETE (OR AT LEAST WITH WELL DEFINED BIASES) AND INCLUDE THE LEAST NUMBER OF INT ...
Gas and Dust Chemistry in Planet-Forming Disks
... of molecular clouds, hot cores, and comets, consistent with comet formation in the outer regions of disks. The distribution of HDO in LkCa 15 was found to be similar to predictions from chemical models, which suggest a steep gradient as a function of disk radius. Finally, Keck LWS observations of th ...
... of molecular clouds, hot cores, and comets, consistent with comet formation in the outer regions of disks. The distribution of HDO in LkCa 15 was found to be similar to predictions from chemical models, which suggest a steep gradient as a function of disk radius. Finally, Keck LWS observations of th ...
PhD thesis
... 1 Massive star formation 1.1 Massive star formation . . . . . . . . . . . . . . . . . . . . . . 1.1.1 Observational massive star-forming features . . . . . . 1.2 Ionized gas . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1.2.1 Thermal emission from ionized gas . . . . . . . . . . . . 1.2. ...
... 1 Massive star formation 1.1 Massive star formation . . . . . . . . . . . . . . . . . . . . . . 1.1.1 Observational massive star-forming features . . . . . . 1.2 Ionized gas . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1.2.1 Thermal emission from ionized gas . . . . . . . . . . . . 1.2. ...
Spitzer Spectroscopy of Circumstellar Disks in the 5 Myr Old Upper
... Figures 1a–1d are the NextGen stellar atmospheric models of Hauschildt et al. (1999) for solar metallicities and sub-giant surface gravities (log g = 4.0). The main sequence effective temperatures (Teff ) from Kenyon & Hartmann (1995) are adopted for the assigned spectral types of the Upper Scorpius ...
... Figures 1a–1d are the NextGen stellar atmospheric models of Hauschildt et al. (1999) for solar metallicities and sub-giant surface gravities (log g = 4.0). The main sequence effective temperatures (Teff ) from Kenyon & Hartmann (1995) are adopted for the assigned spectral types of the Upper Scorpius ...
Giant molecular clouds in the Local Group galaxy M 33⋆⋆⋆
... at a distance of 840 kpc, is close enough for individual giant molecular clouds (GMCs) to be identified. The goal of this work is to study the properties of the GMCs in this subsolar metallicity galaxy. The CPROPS (Cloud PROPertieS) algorithm was used to identify 337 GMCs in M 33, the largest sample ...
... at a distance of 840 kpc, is close enough for individual giant molecular clouds (GMCs) to be identified. The goal of this work is to study the properties of the GMCs in this subsolar metallicity galaxy. The CPROPS (Cloud PROPertieS) algorithm was used to identify 337 GMCs in M 33, the largest sample ...
Article PDF - IOPscience
... nature of their power source. Specifically, most galaxies which possess a radio-luminous active galactic nucleus (AGN) and rapidly advancing jets show little evidence for a central accreting disk. For example, in Centaurus A and Virgo A (M87) there is no blue continuum or broad emission lines, but a ...
... nature of their power source. Specifically, most galaxies which possess a radio-luminous active galactic nucleus (AGN) and rapidly advancing jets show little evidence for a central accreting disk. For example, in Centaurus A and Virgo A (M87) there is no blue continuum or broad emission lines, but a ...
Gamma-Ray Pulsars - INTEGRAL
... outer co-rotating magnetosphere. As we will see, the number of detected γ-ray pulsars is quite in agreement with expectations based on sensitivities of current telescopes. Moreover, it is quite likely that several of the unidentified γ-ray sources, which belong mostly to a galactic population and ar ...
... outer co-rotating magnetosphere. As we will see, the number of detected γ-ray pulsars is quite in agreement with expectations based on sensitivities of current telescopes. Moreover, it is quite likely that several of the unidentified γ-ray sources, which belong mostly to a galactic population and ar ...
25June2004 - Division of Geological and Planetary Sciences
... •Objects thought to be ~face on have the narrowest line widths, highly inclined systems the largest. •As the excitation energy increases, so does the line width (small effect). •Consistent with disk emission, radii range from 0.5-5 AU at high J. •Low J lines also resonantly scatter 5 mm photons to m ...
... •Objects thought to be ~face on have the narrowest line widths, highly inclined systems the largest. •As the excitation energy increases, so does the line width (small effect). •Consistent with disk emission, radii range from 0.5-5 AU at high J. •Low J lines also resonantly scatter 5 mm photons to m ...
Studies of molecular clouds at the Galactic centre Roland Karlsson DECLINATION (B1950)
... and evolution of star-forming complexes, ignition of starbursts as well as the overall kinematic behaviour of the interstellar medium throughout the Galaxy. In spiral galaxies, radial transport of material is considered essential for the build-up of the energy budget and the evolution of the various ...
... and evolution of star-forming complexes, ignition of starbursts as well as the overall kinematic behaviour of the interstellar medium throughout the Galaxy. In spiral galaxies, radial transport of material is considered essential for the build-up of the energy budget and the evolution of the various ...
Explosive sources of the highest energy radiation
... brightest radio source among known binary systems, with large flares that are attributed to its relativistic jets. The system exhibits a complex X-ray spectrum that fluctuates between two main states: “soft” and “hard”. The source is known to flare in radio when entering the “soft” state with associ ...
... brightest radio source among known binary systems, with large flares that are attributed to its relativistic jets. The system exhibits a complex X-ray spectrum that fluctuates between two main states: “soft” and “hard”. The source is known to flare in radio when entering the “soft” state with associ ...
The Multitude of Molecular Hydrogen Knots in the Helix Nebula 1
... picture of the cometary knots reveals that they are neutral gas condensations that appear as comet like structures with rims bright in Hα and tails that appear as shadows in [OIII] and that point away from the central star. The rim of low-excitation ionize gas has a steep temperature gradient indica ...
... picture of the cometary knots reveals that they are neutral gas condensations that appear as comet like structures with rims bright in Hα and tails that appear as shadows in [OIII] and that point away from the central star. The rim of low-excitation ionize gas has a steep temperature gradient indica ...
SUB-KILOPARSEC IMAGING OF COOL MOLECULAR GAS IN
... evidence that the clumps are offset towards higher star formation efficiency compared to the galaxy as a whole. Bright lensed galaxies are rare, but recent large surveys conducted by the South Pole Telsecope (SPT; Carlstrom et al. 2011; Vieira et al. 2010; Mocanu et al. 2013) and Herschel (Negrello ...
... evidence that the clumps are offset towards higher star formation efficiency compared to the galaxy as a whole. Bright lensed galaxies are rare, but recent large surveys conducted by the South Pole Telsecope (SPT; Carlstrom et al. 2011; Vieira et al. 2010; Mocanu et al. 2013) and Herschel (Negrello ...
Evolution in circumstellar envelopes of Be stars: From disks to rings?
... recognized almost right at the beginning of Be star research, most current models nevertheless omit all time dependencies. It is usually assumed that the associated restructuring of the disk can be described by some suitable sequence of stationary models. The only major exception is the inclusion of ...
... recognized almost right at the beginning of Be star research, most current models nevertheless omit all time dependencies. It is usually assumed that the associated restructuring of the disk can be described by some suitable sequence of stationary models. The only major exception is the inclusion of ...
Multiwavelength properties of γ-ray loud binary systems.
... is found in the directions of known γ-ray-loud binary systems: LSI +61 303, V407 Cyg, Cyg X-3 and PSR B1259-63. Remarkably, there are no signatures of weaker variability which could be clearly associated to other binary systems with black holes and /or neutron stars. Recent discovery of the γ-ray fl ...
... is found in the directions of known γ-ray-loud binary systems: LSI +61 303, V407 Cyg, Cyg X-3 and PSR B1259-63. Remarkably, there are no signatures of weaker variability which could be clearly associated to other binary systems with black holes and /or neutron stars. Recent discovery of the γ-ray fl ...
here - Ira-Inaf
... coverage of the first galactic quadrant. From these 3 sources, we selected candidates on the basis of distance from the Galactic Center (the farther the object, the more preferable it was), CO(1–0) signal strength, and galactic latitude and sidereal time considerations. Of the 70 GMCs that we observ ...
... coverage of the first galactic quadrant. From these 3 sources, we selected candidates on the basis of distance from the Galactic Center (the farther the object, the more preferable it was), CO(1–0) signal strength, and galactic latitude and sidereal time considerations. Of the 70 GMCs that we observ ...
The prebiotic molecules observed in the interstellar gas
... molecules, the dipole moment can be measured from the Stark effect to about 1%, and even for some reactive molecules where the measurement is difficult, it can often be measured to almost the same value. In addition, for many reactive astronomical molecules, dipole moments can now be calculated with ...
... molecules, the dipole moment can be measured from the Stark effect to about 1%, and even for some reactive molecules where the measurement is difficult, it can often be measured to almost the same value. In addition, for many reactive astronomical molecules, dipole moments can now be calculated with ...
1e 1048.1−5937, xte j1810−197 and 4u 0142+61
... line center and black body temperatures) are given in Table 1. What is remarkable is that in each case, the detected emission feature is at an energy of ≈13 keV. In the magnetar model the common interpretation is that these lines are proton-cyclotron in origin, implying a magnetic field of ≈2 × 1015 ...
... line center and black body temperatures) are given in Table 1. What is remarkable is that in each case, the detected emission feature is at an energy of ≈13 keV. In the magnetar model the common interpretation is that these lines are proton-cyclotron in origin, implying a magnetic field of ≈2 × 1015 ...
Optical Spectroscopy of a Flare on Barnard`s Star
... stars (Allred et al. 2006). The simulated line profiles were calculated using the radiative transfer code MULTI (Carlsson 1986) with a 13 level plus continuum model hydrogen atom. Temperature and electron density stratifications for a flaring M dwarf atmosphere were taken at numerous times during th ...
... stars (Allred et al. 2006). The simulated line profiles were calculated using the radiative transfer code MULTI (Carlsson 1986) with a 13 level plus continuum model hydrogen atom. Temperature and electron density stratifications for a flaring M dwarf atmosphere were taken at numerous times during th ...
The Pioneer Effect Discovery and the Amazing Theory that Predicted it
... decade prior to the effect first becoming noticeable to the JPL group and 18 years prior to the publication of the JPL findings, but receiving no mention in their paper. Most would agree that if a theory makes a prediction and that prediction is later verified, then there is good reason to consider ...
... decade prior to the effect first becoming noticeable to the JPL group and 18 years prior to the publication of the JPL findings, but receiving no mention in their paper. Most would agree that if a theory makes a prediction and that prediction is later verified, then there is good reason to consider ...
Part2
... Some things to take away: o Azimuthally averaged, CO emission looks pretty similar to stars (there are important differences, but this is a good place to start): an exponential decline with a scale length ~0.2 to 0.25 times the optical radius. o The exponential decline is a mix of filling factor (e. ...
... Some things to take away: o Azimuthally averaged, CO emission looks pretty similar to stars (there are important differences, but this is a good place to start): an exponential decline with a scale length ~0.2 to 0.25 times the optical radius. o The exponential decline is a mix of filling factor (e. ...
CO OBSERVATIONS OF SPIRAL STRUCTURE AND THE LIFETIME
... By virtue of its broad latitude coverage, the survey of Solomon, Scoville, and Sanders (1978) affords an excellent opportunity to trace large scale galactic features such as spiral arms or cloud clusters which do not necessarily maintain a constant latitude over their full longitude extent. Approxim ...
... By virtue of its broad latitude coverage, the survey of Solomon, Scoville, and Sanders (1978) affords an excellent opportunity to trace large scale galactic features such as spiral arms or cloud clusters which do not necessarily maintain a constant latitude over their full longitude extent. Approxim ...
3.1 Radio Astronomy Research Results For much of PY 2010, radio
... An AGES objective is to investigate the number of low mass gas rich dwarf galaxies that reside around isolated galaxies and within galaxy groups, as hierarchical models of galaxy formation predict hundreds of dwarf companions for each giant galaxy. AGES typically finds only one or two new dwarf gala ...
... An AGES objective is to investigate the number of low mass gas rich dwarf galaxies that reside around isolated galaxies and within galaxy groups, as hierarchical models of galaxy formation predict hundreds of dwarf companions for each giant galaxy. AGES typically finds only one or two new dwarf gala ...