Day 295

Tuesday.

1209.1635
SDSS 0956+5128: a broad-line quasar with extreme velocity offsets
Steinhardt, et al

z~0.714 on narrow emission lines, and MgII emission lines z~0.707 (1200 km/s bluer), also with broad Halpha and Hbeta at z~0.690 (4100 km/s bluer).

1209.1636
Galaxy and mass assembly (GAMA): the mass-metallicity relationship
Foster et al

Stellar mass-metallicity relation can vary significantly depending on the sample selection criteria.  

1209.1640
Accreting SMBHs in the COSMOS field and the connection to their host galaxies
Bongiorno et al

AGNs found in all type of galaxies (no bimodality) but mostly in massive red galaxies; Find: "specific accretion rate" alsmot independent of host galaxy mass, but decreases with Lx/M.  Incidence of AGN increases with redshift as (1+z)^4, in close resemblance with overall evolution of the sSFR of galaxy population.  Although AGN activity and SF in galaxies do appear to have a common triggering mechanism, in COSMOS find no strong evidence of any signal of AGN influencing the SF properties of their host galaxies.

1209.1646
Size magnification as a complement to cosmic shear
Casaponsa, Heavens, Kitching, Miller, Barreiro, Martinez-Gonzalez

Hoes does magnification complement cosmic shear in WL surveys?  Simulated images used, find that size estimation can be an excellent complement; unbiased estimation of the convergence field is possible with galaxies with angular sizes larger than the PSF and S/N ratio in excess of 10.  Statistical power similar to cosmic shear; subject to different systematic effects.  Ground-based data application requires large empirical corrections (mostly due to size wrt PSF), but for 0.1 arcsecond resolution, size distribution of galaxies brighter than i=24 is ideal for accurate estimation of cosmic size magnification.

1209.1786
Theories of the massive star formation: a (short) review
Hennebelle, Commercon

Formation of massive star, a review.  Discuss (i) problem of building stars >20 Msun (ii) how to prevent the massive cores to fragment in many objects.  Circumvent radiative pressure leading to the formation of massive stars although some questions are still debated regarding how accretion exactly proceeds.  Core fragmentation slightly reduced by radiative feedback and the B-field when they are treated separately; almost entirely suppressed when both included.  B-field by removing angular momentum focusses the flow in a compact regions.  This makes radiative feedback efficient, leading to a significant increase of the temperature.

1209.1812
Scenarios to explain extreme Be depletion in solar-like stars: accretion or rotation effects ?
Viallet, Baraffe

Be abundance in stars: small fraction are extremely Be-deficient.  2 possible scenarios: early accretion and rotational mixing.  In both cases, conditions to reach observed level of Be depletion are quite extreme.  Substantial Be depletion can be obtained in stars if they were fast rotators in the past, with high initial rotational velocities and short disc lifetimes.  [??]  Rotational mixing may not be efficient enough to deplete Be in <10 Myr; will be able to tell if there is a Be-deficiency derived from accretion process.

1209.1835
Finding new signature effects on galactic dynamics to constrain Bose-Einstein-condensed cold dark matter
Rindler-Daller, Shapiro

If CDM is light bosonic particles, then can form a BE Condensate.  Quite dynamically different, may lead to observable signatures in galactic haloes.

1209.1915
THe radio signatures of the first supernovae
Meiskin, Whalen

The PopIII SNe remnants may soon be detectable in the radio.  Calculate radio synchrotron signatures between 0.5-35 GHz from hydro sim of PopIII SNe in minihalos.  Hypernovae radio remnants should be detectable by existing radio facilities like eVLA and eMERLIN, while Type II SNe remnants will require the SKA.  Expected number count at z>20 with flux >1 muJy hypernovas are 1 per 50 sq deg field, increasing to few per sqdeg for z=10.  Hypernova and SNeII are easily distinguishable by their light curves---constrain IMF of PopIII stars!

1209.2043
NEXUS: tracing the cosmic web connection
Cautun et al

Identification of cosmic web environments: clusters, filaments, walls and voids.

1209.1480
AGN feedback and triggering of star formation in galaxies
Ishibashi, Fabian

Feedback from AGN may be responsible for the MBH-sigma relation, and limiting the bulge stellar mass of the host galaxy.  Explore the possibility of AGN feedback triggering SF in the host galaxy: shell of dusty gas, driven outwards by radiation pressure, and analyze its escape/trapping condition in the galactic halo for different underlying DM potentials.  In isothermal potential, the standard MBH-sigma relation not sufficient to clear gas out of the entire galaxy, but is sufficient for the case of Hernquist and NFW profiles.  The squeezing and compression of the inhomogeneous interstellar medium during the ejection process can trigger star formation within the feedback-driven shell.  Estimate SFR and total additional stellar mass; new stars are formed at increasingly larger radii and successively populate the outer regions of the host galaxy.  This characteristic pattern may be compared with the observed 'inside-out' growth of massive galaxies.

1209.1484
The molecular gas content of z=3 Lyman break galaxies; evidence of a non evolving gas fraction in main sequence galaxies at z > 2
Magdis et al

Observation of CO[3-2] emission towards two massive and IR luminous LBGs at z=3.21 and 2.92; place constraints on the molecular gas masses (Mgas) of non-lensed LBGs.  Consistent with MS galaxies at their redshifts, despite their high IR luminosity.  Existence of a plateau in the evolution of sSFR at z>2.5 (Mgas/M*).  

1209.1497
LOFT: the large observatory for X-ray timing
Feroci et al

One of the 4 candidates selected by ESA for M3 launch, medium size mission of Cosmic Vision programme, for 2022-2024 launch.  Exploit the diagnostics of rapid X-ray flux and spectral variability that directly probe the motion of matter down to distances very close to BHs and NSs, as well as physical state of ultra-dense matter.  Large area detector (LAD) and wide field monitor (WFM).  Investigate variability from submillisecond QPO's to year-long transient outbursts.