Friday.
1209.2705
The bizarre chemical inventory of NGC 2419, an extreme outer halo globular cluster
Cohen, Kirby
NGC2419 appears to be like no other globular cluster, but rather the core of an accreted dwarf galaxy.
1209.2706
Cosmological implications of the effective field theory of cosmic acceleration
Mueller, Bean, Watson
Both leading correction and scalar couplings each modify the MD and/or accelerative eras that allow to place cosmological constraints. Find scalar fieldEFT with a coupled Gauss-Bonnet term and data are discrepant.
1209.2707
Evidence for a wide range of UV obscuration in z~2 dusty galaxies from the GOODS-Herschel survey
Penner et al
What is the physical mechanism for this diversity? Abnormal bright in MIR, or abnormally faint in UV? MIR is not abnormally bright. Only 24% have sSFR which indicate the dominance of compact SF regions. Supports idea that the UV- and IR-emitting regions in these galaxies are spatially coincident--supports connection between UV faintness of DOGs (dust obscured galaxies) and dust obscuration. It's due to different amounts of UV obscuration.
1209.2708
Constraints on the shape of the milky way dark matter halo from Jeans equations applied to SDSS data
Loebman, Ivezic, et al
Evidence of DM in MW: stellar number density distribution and kinematics from SDSS stars >10kpc from the sun. Employ cylindrically symmetric form of Jean equations, focus on the morphology of the resulting acceleration maps. The implied gravitational potential assuming Newtonian framework cannot be explained by visible matter alone. Estimate DM halo axis ratio: z_DM=0.47.
1209.2709
Predicting the number of giant arcs expected in the next generation wide-field surveys from space
Boldrin, Giocoli, Meneghetti, Moscardini
Use simulation (MOKA to obtain angle deflection maps of mock gravitational lenses, ray-traced SL). (1) generate light cone populated with lenses derived from mass-function, (2) model each single lens using a triaxial halo with NFW profile, concentration-mass relation, substructures, (3) lensing cross section determination as a function of redshift for each lens in light cone, (4) simulation of mock observations to characterize the z distribution of sources that will be detectable in the Euclid images. At 15000 sq deg for Euclid, about several thousand giant arcs.
1209.2737
Comparisons of cosmological MHD galaxy cluster simulations to radio observations
Xu, ... Cen, et al
Use AMR MHD simulations, simulation agree with observations (radio power vs cluster X-ray luminosity, radio power vs. radio halo size) Show that cluster wide magnetic fields that originate from AGNs are then amplified by the ICM turbulence can explain observation.
1209.2856
The star formation rate of turbulent magnetized clouds: comparing theory, simulations, and observations
Federrath, Klessen
Study role of turbulence and B-fields for SF in molecular clouds. Compare 6 theoretical models of SFR. Conclude that the SFR is primarily controlled by interstellar turbulence, with a secondary effect coming from B-fields.
1209.2705
The bizarre chemical inventory of NGC 2419, an extreme outer halo globular cluster
Cohen, Kirby
NGC2419 appears to be like no other globular cluster, but rather the core of an accreted dwarf galaxy.
1209.2706
Cosmological implications of the effective field theory of cosmic acceleration
Mueller, Bean, Watson
Both leading correction and scalar couplings each modify the MD and/or accelerative eras that allow to place cosmological constraints. Find scalar fieldEFT with a coupled Gauss-Bonnet term and data are discrepant.
1209.2707
Evidence for a wide range of UV obscuration in z~2 dusty galaxies from the GOODS-Herschel survey
Penner et al
What is the physical mechanism for this diversity? Abnormal bright in MIR, or abnormally faint in UV? MIR is not abnormally bright. Only 24% have sSFR which indicate the dominance of compact SF regions. Supports idea that the UV- and IR-emitting regions in these galaxies are spatially coincident--supports connection between UV faintness of DOGs (dust obscured galaxies) and dust obscuration. It's due to different amounts of UV obscuration.
1209.2708
Constraints on the shape of the milky way dark matter halo from Jeans equations applied to SDSS data
Loebman, Ivezic, et al
Evidence of DM in MW: stellar number density distribution and kinematics from SDSS stars >10kpc from the sun. Employ cylindrically symmetric form of Jean equations, focus on the morphology of the resulting acceleration maps. The implied gravitational potential assuming Newtonian framework cannot be explained by visible matter alone. Estimate DM halo axis ratio: z_DM=0.47.
1209.2709
Predicting the number of giant arcs expected in the next generation wide-field surveys from space
Boldrin, Giocoli, Meneghetti, Moscardini
Use simulation (MOKA to obtain angle deflection maps of mock gravitational lenses, ray-traced SL). (1) generate light cone populated with lenses derived from mass-function, (2) model each single lens using a triaxial halo with NFW profile, concentration-mass relation, substructures, (3) lensing cross section determination as a function of redshift for each lens in light cone, (4) simulation of mock observations to characterize the z distribution of sources that will be detectable in the Euclid images. At 15000 sq deg for Euclid, about several thousand giant arcs.
1209.2737
Comparisons of cosmological MHD galaxy cluster simulations to radio observations
Xu, ... Cen, et al
Use AMR MHD simulations, simulation agree with observations (radio power vs cluster X-ray luminosity, radio power vs. radio halo size) Show that cluster wide magnetic fields that originate from AGNs are then amplified by the ICM turbulence can explain observation.
1209.2856
The star formation rate of turbulent magnetized clouds: comparing theory, simulations, and observations
Federrath, Klessen
Study role of turbulence and B-fields for SF in molecular clouds. Compare 6 theoretical models of SFR. Conclude that the SFR is primarily controlled by interstellar turbulence, with a secondary effect coming from B-fields.
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