searching for dark matter annihilation in the smith high
... Galactic substructures which may host significant dark matter content. HVCs are detected as cold clouds of neutral hydrogen (H i), and are characterized by their large peculiar velocities, which are often incompatible with Galactic rotation (Wakker & van Woerden 1997). Multiple HVCs exhibit cometary ...
... Galactic substructures which may host significant dark matter content. HVCs are detected as cold clouds of neutral hydrogen (H i), and are characterized by their large peculiar velocities, which are often incompatible with Galactic rotation (Wakker & van Woerden 1997). Multiple HVCs exhibit cometary ...
aaswinter07ppt
... three epochs have been reduced. Typical angular resolutions of the VLBA observations are 600 x 200 microarcseconds. The observations were made in phase-referencing mode to the nearby quasar J0656-0323, in order to measure astrometric positions and eventually, the parallax. For the v=2 transition, us ...
... three epochs have been reduced. Typical angular resolutions of the VLBA observations are 600 x 200 microarcseconds. The observations were made in phase-referencing mode to the nearby quasar J0656-0323, in order to measure astrometric positions and eventually, the parallax. For the v=2 transition, us ...
script
... Background: Very few people have a comprehensive view of our place in the universe. They think about astronomical objects as disconnected elements, rather than an integrated system. This demonstration takes visitors from our Solar System, the part of the universe with which they are most familiar, o ...
... Background: Very few people have a comprehensive view of our place in the universe. They think about astronomical objects as disconnected elements, rather than an integrated system. This demonstration takes visitors from our Solar System, the part of the universe with which they are most familiar, o ...
Origin and Evolution of the Abundance Gradient along the Milky
... the framework of a phenomenological scenario of disk formation, several mechanisms may play roles in shaping the abundance gradient and its evolution. One is the star formation processes in the disk. Observations of local disk and starburst galaxies show that the star formation rate (SFR) per unit a ...
... the framework of a phenomenological scenario of disk formation, several mechanisms may play roles in shaping the abundance gradient and its evolution. One is the star formation processes in the disk. Observations of local disk and starburst galaxies show that the star formation rate (SFR) per unit a ...
Chemistry of Silicate Atmospheres of Evaporating Super
... gravitational acceleration. We assumed the planetary properties for CoRot-7b (R = 1.72R/, M ~11M/) to calculate g = 36.2 m/s2. The major gas at all temperatures shown is monatomic Na, followed by O2 and monatomic O. As temperature increases, the SiO abundance increases and approaches the abundances ...
... gravitational acceleration. We assumed the planetary properties for CoRot-7b (R = 1.72R/, M ~11M/) to calculate g = 36.2 m/s2. The major gas at all temperatures shown is monatomic Na, followed by O2 and monatomic O. As temperature increases, the SiO abundance increases and approaches the abundances ...
Practical cosmology with the Local Volume galaxies
... dark matter distribution on scales of 0.3 – 3 Mpc. In this respect we note that the sum of virial mass for 7 nearest groups (around the Milky Way, M31, M81, CenA, M83, IC342, and Maffei) consists of 1.3·1013 M☼. But the sum of their total masses estimated via R0 from external galaxy motions is 0.86· ...
... dark matter distribution on scales of 0.3 – 3 Mpc. In this respect we note that the sum of virial mass for 7 nearest groups (around the Milky Way, M31, M81, CenA, M83, IC342, and Maffei) consists of 1.3·1013 M☼. But the sum of their total masses estimated via R0 from external galaxy motions is 0.86· ...
the formation of giant molecular clouds
... This introduction reviews observations of interstellar gas clouds of mass M > 10 4 M¯ . It then critically reviews theories of cloud formation and discusses what constraints observations place on these theories. 1. Introduction The existence of dense clouds of interstellar material has long been app ...
... This introduction reviews observations of interstellar gas clouds of mass M > 10 4 M¯ . It then critically reviews theories of cloud formation and discusses what constraints observations place on these theories. 1. Introduction The existence of dense clouds of interstellar material has long been app ...
Document
... between yearly epochs at the 5 level with the CFHT Legacy Survey optical catalog. • Rule out sources with optical hosts with the colors and morphology of a star or quasar. • Follow up galaxy hosts that do not have an hard X-ray detection with optical spectroscopy to look for signs of an AGN. • Trig ...
... between yearly epochs at the 5 level with the CFHT Legacy Survey optical catalog. • Rule out sources with optical hosts with the colors and morphology of a star or quasar. • Follow up galaxy hosts that do not have an hard X-ray detection with optical spectroscopy to look for signs of an AGN. • Trig ...
Investigating the Effects of Milky Way Globular Clusters
... Dark matter is believed to be matter that gives off so little light, if any at all, that we are unable to detect its presence (Weintraub 261). However, scientists have been able to infer its existence from numerous observations and calculations surrounding the nature of the Milky Way galaxy, oth ...
... Dark matter is believed to be matter that gives off so little light, if any at all, that we are unable to detect its presence (Weintraub 261). However, scientists have been able to infer its existence from numerous observations and calculations surrounding the nature of the Milky Way galaxy, oth ...
two dozen compact sources and a massive disk
... cluster begins to emerge MIR - mm 4. Young cluster cluster has emerged from cloud ...
... cluster begins to emerge MIR - mm 4. Young cluster cluster has emerged from cloud ...
P - Inaf
... Fig. 6 shows the average metallicity and mass-weighted stellar ages of the W08 model galaxies as functions of stellar and halo mass, with central and satellite galaxies in grey and black, respectively. The vertical bars in the left-hand panels indicate the typical ±1σ scatter in the model. For compa ...
... Fig. 6 shows the average metallicity and mass-weighted stellar ages of the W08 model galaxies as functions of stellar and halo mass, with central and satellite galaxies in grey and black, respectively. The vertical bars in the left-hand panels indicate the typical ±1σ scatter in the model. For compa ...
16 Hubble s Law and Dark Matter
... Dark Matter in the Universe Galaxy mass measurements show that galaxies need between 3 and 10 times more mass than can be observed to explain their rotation curves. The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the ...
... Dark Matter in the Universe Galaxy mass measurements show that galaxies need between 3 and 10 times more mass than can be observed to explain their rotation curves. The discrepancy is even larger in galaxy clusters, which need 10 to 100 times more mass. The total needed is more than the sum of the ...
sections 16-18 instructor notes
... For disk stars that are not drifting either perpendicular to the Galactic plane or in the direction of the Galactic centre, it is reasonable to expect that: ≡ 0 and ≡ 0.
However, ≠ 0 since a typical group of stars selected
observationally will always tend to lag behind the solar
LSR. ...
... For disk stars that are not drifting either perpendicular to the Galactic plane or in the direction of the Galactic centre, it is reasonable to expect that: ≡ 0 and
arXiv:astro-ph/9510089 v1 17 Oct 95
... the baryonic content of the Universe must be between 0.01 < Ωb h2 < 0.015 [13,14,15]. Given the large uncertainty in h this means 0.01 < Ωb < 0.1. These values are far below unity, so the theoretical predilection for Ωtotal = 1 (or the observational evidence for Ω > 0.3) forces the bulk of the dark ...
... the baryonic content of the Universe must be between 0.01 < Ωb h2 < 0.015 [13,14,15]. Given the large uncertainty in h this means 0.01 < Ωb < 0.1. These values are far below unity, so the theoretical predilection for Ωtotal = 1 (or the observational evidence for Ω > 0.3) forces the bulk of the dark ...
Power Point
... • another 6dF Galaxy Survey data release in Dec 2003 – more data with new gratings on 6dF spectrograph with higher S/N – the eventually completed survey will have ~13 times more data Exploring the Stellar Populations of Early-Type Galaxies in the 6dF Galaxy Survey ...
... • another 6dF Galaxy Survey data release in Dec 2003 – more data with new gratings on 6dF spectrograph with higher S/N – the eventually completed survey will have ~13 times more data Exploring the Stellar Populations of Early-Type Galaxies in the 6dF Galaxy Survey ...
What is a standard candle?
... Both stars have the same average apparent brightness. The star in galaxy A has a bright-dim-bright period of 10 days, while the one in galaxy B has a bright-dim-bright period of 30 days. Which of the two galaxies is at a greater distance from us? a) ...
... Both stars have the same average apparent brightness. The star in galaxy A has a bright-dim-bright period of 10 days, while the one in galaxy B has a bright-dim-bright period of 30 days. Which of the two galaxies is at a greater distance from us? a) ...
Neutron Stars and Black Holes
... Both stars have the same average apparent brightness. The star in galaxy A has a bright-dim-bright period of 10 days, while the one in galaxy B has a bright-dim-bright period of 30 days. Which of the two galaxies is at a greater distance from us? a) ...
... Both stars have the same average apparent brightness. The star in galaxy A has a bright-dim-bright period of 10 days, while the one in galaxy B has a bright-dim-bright period of 30 days. Which of the two galaxies is at a greater distance from us? a) ...
implication on the mass and
... ! Connection between LIRGs and disks (z>0.4) (HST morphologies and color maps) : 40% of LIRGs are large disks (Zheng et al, 2004, A&A) ! Lilly et al (1998) large disk sample (rdisk > 4 h50-1 kpc) at 0.5 < z < 1: 32 (+/-13)% of them are LIRGs ! LIRGs have large stellar masses: 1.4 1010MO
... ! Connection between LIRGs and disks (z>0.4) (HST morphologies and color maps) : 40% of LIRGs are large disks (Zheng et al, 2004, A&A) ! Lilly et al (1998) large disk sample (rdisk > 4 h50-1 kpc) at 0.5 < z < 1: 32 (+/-13)% of them are LIRGs ! LIRGs have large stellar masses: 1.4 1010MO
KINEMATIC DISCOVERY OF A STELLAR STREAM LOCATED IN
... In the top left and top right panels of Figure 3 we show color–magnitude diagrams (CMDs) of all stars having SDSS DR8 spectra within the on- and off-stream fields, respectively. We also show subsets of the spectra with properties expected for the PSS. The subscripts on the magnitudes g0 and (g − r)0 ...
... In the top left and top right panels of Figure 3 we show color–magnitude diagrams (CMDs) of all stars having SDSS DR8 spectra within the on- and off-stream fields, respectively. We also show subsets of the spectra with properties expected for the PSS. The subscripts on the magnitudes g0 and (g − r)0 ...
Stars and Galaxies
... Parallax (let’s model it) As Earth orbits the Sun, we see nearby stars move relative to more distant stars How many degrees did the plate move, relative to the background? ...
... Parallax (let’s model it) As Earth orbits the Sun, we see nearby stars move relative to more distant stars How many degrees did the plate move, relative to the background? ...
lec09_14oct2011
... Basic result: Disks dissipate within a few Myr, but with a large disp. for any SINGLE system. When they go, however, the dissipation is FAST in comparison w/ disk “lifetime.” Gas??? ...
... Basic result: Disks dissipate within a few Myr, but with a large disp. for any SINGLE system. When they go, however, the dissipation is FAST in comparison w/ disk “lifetime.” Gas??? ...
Review 3 (11-18-10)
... • Exam based on material covered in class, i,e., study class notes and use book only to help you understand the material covered in class. Several questions presented in class are included in the exam almost verbatim • I will put up a list of formulas, you do not need to memorize them, BUT you need ...
... • Exam based on material covered in class, i,e., study class notes and use book only to help you understand the material covered in class. Several questions presented in class are included in the exam almost verbatim • I will put up a list of formulas, you do not need to memorize them, BUT you need ...
IAC_L3_thickdisk
... the disk, e.g. via Jeans equation. Is there more matter in the disk that we can account for from census of visible objects ? The tracer sample must be in equilibrium so the stars need to be older than a few Gyr. The last few estimates have used K dwarfs and K giants - probably OK but they do include ...
... the disk, e.g. via Jeans equation. Is there more matter in the disk that we can account for from census of visible objects ? The tracer sample must be in equilibrium so the stars need to be older than a few Gyr. The last few estimates have used K dwarfs and K giants - probably OK but they do include ...
m82 as a galaxy: morphology and stellar content of the disk and halo
... profiles at RG > 6000 can be very well fitted by an exponential function, with the scale-lengths systematically increasing at shorter wavelengths — again a property characteristic of dusty disks (Evans 1994). The shortest scale-length is reached in the K-band, where the observed scale-length (4700 = ...
... profiles at RG > 6000 can be very well fitted by an exponential function, with the scale-lengths systematically increasing at shorter wavelengths — again a property characteristic of dusty disks (Evans 1994). The shortest scale-length is reached in the K-band, where the observed scale-length (4700 = ...