Cold dark matter heats up
... and abundance of isolated, small field galaxies provide stronger constraints on models of feedback and alternative dark matter models64,65. High-mass galaxies Field dwarfs typically fall into the category of ‘low-surface-brightness’ galaxies, defined by their extended diffuse stellar and gaseous dis ...
... and abundance of isolated, small field galaxies provide stronger constraints on models of feedback and alternative dark matter models64,65. High-mass galaxies Field dwarfs typically fall into the category of ‘low-surface-brightness’ galaxies, defined by their extended diffuse stellar and gaseous dis ...
Distribution of streaming rates into high
... The MN simulation uses the AMR code RAMSES (Teyssier 2002). The spatial resolution is ∼1 kpc in physical units. UV heating is included assuming the Haardt & Madau (1996) background model, as in the ART simulation. The code incorporates a simple model of supernovae feedback and metal enrichment using ...
... The MN simulation uses the AMR code RAMSES (Teyssier 2002). The spatial resolution is ∼1 kpc in physical units. UV heating is included assuming the Haardt & Madau (1996) background model, as in the ART simulation. The code incorporates a simple model of supernovae feedback and metal enrichment using ...
doc - Eu-Hou
... charge. It is accelerated and therefore emits radiation as any charged particle, which is accelerated. ...
... charge. It is accelerated and therefore emits radiation as any charged particle, which is accelerated. ...
Molecular Cloud Evolution II. From cloud formation to the early
... Moreover, the thermal pressure in the dense cloud is in pressure balance with the total (thermal + ram) pressure in the inflows, which is significantly larger than the mean thermal pressure in the ISM (Paper I). Consequently, the density in the cold layer can reach densities significantly larger tha ...
... Moreover, the thermal pressure in the dense cloud is in pressure balance with the total (thermal + ram) pressure in the inflows, which is significantly larger than the mean thermal pressure in the ISM (Paper I). Consequently, the density in the cold layer can reach densities significantly larger tha ...
Interstellar Space Not as Empty as you Might Think
... Interstellar clouds are the start and end points of a star’s life. Dying stars release heavy elements back into interstellar space, which becomes richer and richer in heavy elements over time (its metallicity goes up) ...
... Interstellar clouds are the start and end points of a star’s life. Dying stars release heavy elements back into interstellar space, which becomes richer and richer in heavy elements over time (its metallicity goes up) ...
Interstellar Space Not as Empty as you Might Think
... Interstellar clouds are the start and end points of a star’s life. Dying stars release heavy elements back into interstellar space, which becomes richer and richer in heavy elements over time (its metallicity goes up) All the heavy elements in the Earth were made in stars, then spent time in interst ...
... Interstellar clouds are the start and end points of a star’s life. Dying stars release heavy elements back into interstellar space, which becomes richer and richer in heavy elements over time (its metallicity goes up) All the heavy elements in the Earth were made in stars, then spent time in interst ...
Interstellar Space
... Interstellar clouds are the start and end points of a star’s life. Dying stars release heavy elements back into interstellar space, which becomes richer and richer in heavy elements over time (its metallicity goes up) All the heavy elements in the Earth were made in stars, then spent time in interst ...
... Interstellar clouds are the start and end points of a star’s life. Dying stars release heavy elements back into interstellar space, which becomes richer and richer in heavy elements over time (its metallicity goes up) All the heavy elements in the Earth were made in stars, then spent time in interst ...
Numerical Star-Formation Studies-
... sively within this molecular phase of the ISM. Molecular hydrogen is a homonuclear molecule, so its dipole moment vanishes and it radiates extremely weakly. Direct detection of cold interstellar H2 is generally possibly only through ultraviolet absorption studies, such as those made by the the Coper ...
... sively within this molecular phase of the ISM. Molecular hydrogen is a homonuclear molecule, so its dipole moment vanishes and it radiates extremely weakly. Direct detection of cold interstellar H2 is generally possibly only through ultraviolet absorption studies, such as those made by the the Coper ...
The effect of the environment on the HI scaling relations
... already known, but a detailed quantification of their properties, crucial for a comparison with models, was still missing. Luckily, the situation is rapidly changing for 21 cm studies. The advent of large Hi surveys, such as the Arecibo Legacy Fast ALFA Survey (Giovanelli et al. 2005), which eventua ...
... already known, but a detailed quantification of their properties, crucial for a comparison with models, was still missing. Luckily, the situation is rapidly changing for 21 cm studies. The advent of large Hi surveys, such as the Arecibo Legacy Fast ALFA Survey (Giovanelli et al. 2005), which eventua ...
galaxy formation with cold gas accretion and evolving stellar initial
... z = 5. Thus, the VD08 IMF includes more high-mass stars at high redshifts. Observationally, the SFRs and stellar mass are both dependent on the assumed stellar IMF. Therefore, the data should be corrected if a different stellar IMF is used. For this purpose, we use the stellar population synthesis c ...
... z = 5. Thus, the VD08 IMF includes more high-mass stars at high redshifts. Observationally, the SFRs and stellar mass are both dependent on the assumed stellar IMF. Therefore, the data should be corrected if a different stellar IMF is used. For this purpose, we use the stellar population synthesis c ...
powerpoint - Physics @ IUPUI
... Also learn • Since the voids form as a result of the distributions of dark matter in the formation of the universe therefore the sizes and distributions tell you something about the distribution of dark matter when the universe formed! • Also, since the curvature of the universe (aka the cosmologic ...
... Also learn • Since the voids form as a result of the distributions of dark matter in the formation of the universe therefore the sizes and distributions tell you something about the distribution of dark matter when the universe formed! • Also, since the curvature of the universe (aka the cosmologic ...
GRB 021004: A Possible Shell Nebula around a Wolf
... velocity profile for one set of initial conditions. Faster outflowing absorbers can be explained by nearby circumstellar material, while more distant absorbers will evolve slower. After final velocity is achieved the absorbers simply coast along. In particular, the simulations are able to reproduce ...
... velocity profile for one set of initial conditions. Faster outflowing absorbers can be explained by nearby circumstellar material, while more distant absorbers will evolve slower. After final velocity is achieved the absorbers simply coast along. In particular, the simulations are able to reproduce ...
How special are brightest group and cluster galaxies?
... voffset<4σv,cl AND without strong Hα emission. ...
... voffset<4σv,cl AND without strong Hα emission. ...
Pretty Pictures of the Cosmos
... for the constellation in which it resides. About four times smaller (in radius) than our Milky Way Galaxy and the Andromeda Galaxy (M31), it is much larger than the many of the local spheroidal dwarfgalaxies. ...
... for the constellation in which it resides. About four times smaller (in radius) than our Milky Way Galaxy and the Andromeda Galaxy (M31), it is much larger than the many of the local spheroidal dwarfgalaxies. ...
talk at lensing and dark matter conference Ohio state 2004
... RR Lyaes and discovered an old and hot stellar halo! But they say it is too small to account for all the extra microlensing • But the structure of the LMC is being questioned: van der Marel,et al (2002) says the LMC disk is not circular, but Nikolaev, et al. (2004) disagree, saying it is warped. Bot ...
... RR Lyaes and discovered an old and hot stellar halo! But they say it is too small to account for all the extra microlensing • But the structure of the LMC is being questioned: van der Marel,et al (2002) says the LMC disk is not circular, but Nikolaev, et al. (2004) disagree, saying it is warped. Bot ...
systems - Research in Astronomy and Astrophysics
... (1968) as the beginning of research focused on the central parsecs of the Galactic center, the field is only 44 yr old. In that time, the pace of discovery has been breathtaking, and it has not shown any signs of leveling off. This review is intended to illustrate this fact by offering brief descrip ...
... (1968) as the beginning of research focused on the central parsecs of the Galactic center, the field is only 44 yr old. In that time, the pace of discovery has been breathtaking, and it has not shown any signs of leveling off. This review is intended to illustrate this fact by offering brief descrip ...
The Essential Cosmic Perspective, 6e
... Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to travel from the object to us. 3) Starting from the Big Bang, briefly explain how our solar system came to contain the chemic ...
... Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to travel from the object to us. 3) Starting from the Big Bang, briefly explain how our solar system came to contain the chemic ...
sections 23-25 powerpoint
... Lenticular galaxies get their name because they are “lenslike,” but are more like spiral and barred spiral galaxies in possessing a flattened disk, rather than like elliptical galaxies which mostly possess ellipsoidal symmetry. The distinguishing feature of lenticulars is that they do not have spir ...
... Lenticular galaxies get their name because they are “lenslike,” but are more like spiral and barred spiral galaxies in possessing a flattened disk, rather than like elliptical galaxies which mostly possess ellipsoidal symmetry. The distinguishing feature of lenticulars is that they do not have spir ...
The Space Density of Spiral Galaxies as f(magnitude, size and
... observed trends between stellar ages & metallicities and galaxy surface brightness parameters ...
... observed trends between stellar ages & metallicities and galaxy surface brightness parameters ...
San Pedro Mártir observations of microvariability in obscured quasars
... us to detect the variability remains unclear, although there are possible explanations. It is possible that the observed light originates close to the central engine and is then reflected on the corona of charged particles above the dusty torus. Polarimetric observations would be needed to confirm s ...
... us to detect the variability remains unclear, although there are possible explanations. It is possible that the observed light originates close to the central engine and is then reflected on the corona of charged particles above the dusty torus. Polarimetric observations would be needed to confirm s ...
galaxies2_1_complete - Astronomy & Astrophysics Group
... Evidence from e.g. HI rotation curves and the motions of satellite galaxies suggests that halos typically extend to at least 100 kpc. We cannot have (r ) r to arbitrary radii, however, if the halo mass is to remain finite. ...
... Evidence from e.g. HI rotation curves and the motions of satellite galaxies suggests that halos typically extend to at least 100 kpc. We cannot have (r ) r to arbitrary radii, however, if the halo mass is to remain finite. ...
The Formation and Early Evolution of Young Massive Clusters
... We review the formation and early evolution of the most massive (> few 104 M⊙ ) and dense (radius of a few pc) young stellar clusters, focusing on the role that studies of these objects in our Galaxy can play in our understanding of star and planet formation as a whole. Comparing the demographics of ...
... We review the formation and early evolution of the most massive (> few 104 M⊙ ) and dense (radius of a few pc) young stellar clusters, focusing on the role that studies of these objects in our Galaxy can play in our understanding of star and planet formation as a whole. Comparing the demographics of ...
instructor notes: weeks 9/10
... Lenticular galaxies get their name because they are “lenslike,” but are more like spiral and barred spiral galaxies in possessing a flattened disk, rather than like elliptical galaxies which mostly possess an ellipsoidal symmetry. The distinguishing feature of lenticulars relative to spiral galaxie ...
... Lenticular galaxies get their name because they are “lenslike,” but are more like spiral and barred spiral galaxies in possessing a flattened disk, rather than like elliptical galaxies which mostly possess an ellipsoidal symmetry. The distinguishing feature of lenticulars relative to spiral galaxie ...
Inti didn`t form in the X wind (and neither did most CAIs)
... The traditional MMSN is wrong. (1) Planets did not form where we find them today: solar nebula must have been more compact. (2) Mass was lost during planet formation as dust and/or ejected planetesimals: solar nebula must have been more massive. Using Nice model positions, Desch (2007) found new MMS ...
... The traditional MMSN is wrong. (1) Planets did not form where we find them today: solar nebula must have been more compact. (2) Mass was lost during planet formation as dust and/or ejected planetesimals: solar nebula must have been more massive. Using Nice model positions, Desch (2007) found new MMS ...
Phys. Rev. - Cinvestav
... In either case, boson stars or oscillatons, the idea of each halo being a single solitonic configuration runs into some problems: once fundamental scalar field parameters are chosen, the size of the ‘‘boson star halo’’ is fixed 关11兴 so that halos of only one unique size would exist, in stark disagre ...
... In either case, boson stars or oscillatons, the idea of each halo being a single solitonic configuration runs into some problems: once fundamental scalar field parameters are chosen, the size of the ‘‘boson star halo’’ is fixed 关11兴 so that halos of only one unique size would exist, in stark disagre ...