Tuesday. No JC this week, hiking instead.
1209.0005
The temperature-density relation in the intergalacitic medium at redshift <z>=2.4
Rudie, Steidel, Pettini
T-rho relation for neutral H in 2.0<z<2.8 IGM from 6000 HI absorbers fitted with Voigt profiles. Find positive correlation between the column density of HI and minimum observed velocity width of absorbers.
1209.0006
A galactic-scale origin for stellar clustering
Kruijssen
Cluster formation efficiency (CFE) from: SF occuring across a continuous spectrum of ISM densities, bound stellar clusters arising from high-density end of this density spectrum. Short free-fall times allow high SFEs, unaffected by gas expulsion; opposite for lower-density regions. Summary of model physics presented, agreement with observations.
1209.0008
Discovery of 100 supernovae among 700,000 Sloan spectra: the Type-Ia supernova rate versus galaxy mass and star formation rate at redshift ~0.1
Graur, Maoz
SNIa spectra found in SDSS; confirm the inverse dependence on galaxy mass of the SNIa rate per unit mass. Explained by the combination of galaxy "downsizing" and a power-law delay-time distribution (delay between starburst and subsequent SNIa explosions) with an index of -1, inherent to the double-degenerate progenitor scenario. Obtained by comparing number of SNIa hosted by each galaxy with the SFH of the stellar population within the spectral aperture. Sample dominated by old and massive galaxies; delay time of 4.5e-14 /Msun /yr: delays in the range >2.4 Gyr. Volumetric rate: 0.25e-4 /yr /Mpc^3.
1209.0014
The 2200 A bump and the UV extinction curve
Zagury
2200 A bump is a major figure of interstellar extinction. No bump extinctions curves are rare, and are linear from NIR down to 2500A over all the visible-UV spectrum. ... The continuum of the extinction curve of the bump contain no information concerning the chemical composition of the interstellar cloud.
1209.0052
An analysis of the FIR/RADIO continuum correlation in the Small Magellanic Cloud
Leverenz, Filipovic
Over scales of 3kpc to 0.01 kpc: Good correlation down to ~15 kpc. Reciprocal slope of FIR/ RC emission correlation greatest in the most active SF regions: indicate RC emission increases faster than the FIR emission. Results consistent with common source for UV photons heating dust and CR electrons diffusing away from SF regions. If CR e- escape the gas readily, cannot provide support for coupling between the local gas density and the B-field density, which is the case for SMC here.
1209.0101
THe spin effect on planetary radial velocimetry of exoplanets
Kawaraha
Effect of planetary spin on the planetary radial velocity in dayside spectra of exoplanets. Curve of PRV distorted by planetary spin; anomaly characterized by spin radial velocity at equator and projected angle on a celestial plane between the spin axis; can constrain planetary obliquity. Can constrain planetary spin.
1209.0168
The jet feedback mechanism (JFM): from supernovae to clusters of galaxies
Soker et al
Common to cooling flow clusters of galaxies, core-collapse SNe, Planetary nebulae, and common envelope evolution. Similarities: hot bubbles inflated by jets in a bipolar structure, vorticies on the sides of the jets, vorticies inside the inflated bubbles, fragmentation of bubbles to two and more bubbles, and buoyancy of bubbles. Activities regulated by a negative feedback mechanism (higher accretion rate leads to stronger jet activity that in turn suppresses the accretion process). Common process in many astrophysical objects.
1209.0216
A multi-waveband study of the Magellanic Bridge
Bahgeri et al
Magellanic system: LMC, SMC, Magellanic Bridge (with stars and gas) and Magellanic Stream (gas only). Find old and new stellar population in the Stream as well, albeit low density. (Foreground star removal was challenging.)
1209.0005
The temperature-density relation in the intergalacitic medium at redshift <z>=2.4
Rudie, Steidel, Pettini
T-rho relation for neutral H in 2.0<z<2.8 IGM from 6000 HI absorbers fitted with Voigt profiles. Find positive correlation between the column density of HI and minimum observed velocity width of absorbers.
1209.0006
A galactic-scale origin for stellar clustering
Kruijssen
Cluster formation efficiency (CFE) from: SF occuring across a continuous spectrum of ISM densities, bound stellar clusters arising from high-density end of this density spectrum. Short free-fall times allow high SFEs, unaffected by gas expulsion; opposite for lower-density regions. Summary of model physics presented, agreement with observations.
1209.0008
Discovery of 100 supernovae among 700,000 Sloan spectra: the Type-Ia supernova rate versus galaxy mass and star formation rate at redshift ~0.1
Graur, Maoz
SNIa spectra found in SDSS; confirm the inverse dependence on galaxy mass of the SNIa rate per unit mass. Explained by the combination of galaxy "downsizing" and a power-law delay-time distribution (delay between starburst and subsequent SNIa explosions) with an index of -1, inherent to the double-degenerate progenitor scenario. Obtained by comparing number of SNIa hosted by each galaxy with the SFH of the stellar population within the spectral aperture. Sample dominated by old and massive galaxies; delay time of 4.5e-14 /Msun /yr: delays in the range >2.4 Gyr. Volumetric rate: 0.25e-4 /yr /Mpc^3.
1209.0014
The 2200 A bump and the UV extinction curve
Zagury
2200 A bump is a major figure of interstellar extinction. No bump extinctions curves are rare, and are linear from NIR down to 2500A over all the visible-UV spectrum. ... The continuum of the extinction curve of the bump contain no information concerning the chemical composition of the interstellar cloud.
1209.0052
An analysis of the FIR/RADIO continuum correlation in the Small Magellanic Cloud
Leverenz, Filipovic
Over scales of 3kpc to 0.01 kpc: Good correlation down to ~15 kpc. Reciprocal slope of FIR/ RC emission correlation greatest in the most active SF regions: indicate RC emission increases faster than the FIR emission. Results consistent with common source for UV photons heating dust and CR electrons diffusing away from SF regions. If CR e- escape the gas readily, cannot provide support for coupling between the local gas density and the B-field density, which is the case for SMC here.
1209.0101
THe spin effect on planetary radial velocimetry of exoplanets
Kawaraha
Effect of planetary spin on the planetary radial velocity in dayside spectra of exoplanets. Curve of PRV distorted by planetary spin; anomaly characterized by spin radial velocity at equator and projected angle on a celestial plane between the spin axis; can constrain planetary obliquity. Can constrain planetary spin.
1209.0168
The jet feedback mechanism (JFM): from supernovae to clusters of galaxies
Soker et al
Common to cooling flow clusters of galaxies, core-collapse SNe, Planetary nebulae, and common envelope evolution. Similarities: hot bubbles inflated by jets in a bipolar structure, vorticies on the sides of the jets, vorticies inside the inflated bubbles, fragmentation of bubbles to two and more bubbles, and buoyancy of bubbles. Activities regulated by a negative feedback mechanism (higher accretion rate leads to stronger jet activity that in turn suppresses the accretion process). Common process in many astrophysical objects.
1209.0216
A multi-waveband study of the Magellanic Bridge
Bahgeri et al
Magellanic system: LMC, SMC, Magellanic Bridge (with stars and gas) and Magellanic Stream (gas only). Find old and new stellar population in the Stream as well, albeit low density. (Foreground star removal was challenging.)
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