Day 622

Sunday.  Monday.

1404.0677
Massive compact galaxies with high-velocity outflows: morphological analysis and constraints on AGN activity
Sell et al

Investigate the process of rapid SF quenching in a sample f 12 massive galaxies at intermediate redshift (z~0.6) that host high-velocity ionized gas outflows (v>1000 km/s).  Conclude that these fast outflows are most likely driven by feedback from SF rather than AGN.  Use multi wavelength survey and targeted observations of the galaxies to assess their SF, AGN activity, and morphology.  Common attributes include diffuse tidal features indicative of recent mergers accompanied by bright, unresolved cores with effective radii less than a few hundred parsecs.  The galaxies are extraordinarily compact for their stellar mass, even when compared with galaxies at z~2-3.  For 9/12 galaxies, rule out an AGN contribution to the nuclear light and hypothesize that the unresolved core comes from a compact central starburst triggered by the dissipative collapse of very gas-rich progenitor merging disks.  Find evidence of AGN activity in half the sample but argue that it accounts for only a small fraction (<10%) of the total bolometric luminosity.  Find no correlation between AGN activity and outflow velocity and conclude that the fast outflows in the galaxies are not powered by on-going AGN activity, but rather by recent, extremely compact starbursts.

1404.0680
Annual modulation of cosmic relic neutrinos
Safdi et al

Neutrino capture on beta-decaying nuclei (NCB) a clear path forward towards the detection of the CvB (cosmic neutrino background).  Show that gravitational focusing by the Sun causes the expected neutrino capture rate to modulate annually.  The amplitude and phase of the modulation depend on the phase-space distribution of the local neutrino background, which is perturbed by structure formation.  These results also apply to searches for sterile neutrinos at NCB experiments.  Gravitational focusing is the only source of modulation for neutrino capture experiments, in contrast to dark-matter direct-detection searches where the Earth's time-dependent velocity relative to the Sun also plays a role.

1404.1080
Rapidly growing black holes and host galaxies in the distant Universe from the Herschel radio galaxy evolution project
Drouart et al

Present results from 70 radio galaxies (RGs) at 1<z<5.2 using PACS and SPIRE on Herschel.  Combined with existing MIR photometry from Spitzer and observations from LABOCA, the SEDs of galaxies in sample are continuously covered across 3.6-870um.  The total IR luminosities of these RGs are such that they almost all are either ULIRG or hyper-LIRGs.  Fit the IR SEDs with a set of empirical templates which represent dust heated (1) by a variety of SB and (2) by a AGN.  Find the the SEDs of RGs require the dust to be heated by both AGN and SB, but the luminosities of these two components are not strongly correlated.  Assuming empirical relations and simple physical assumptions, calculate the SFR, the BH mass accretion rate (MdotBH), and the black hole mass (MBH) for each RG.  Find the the host galaxies and their BHs are growing extremely rapidly, having SFR~100-5000 Msunyr and MdotBH~1-100 Msun/yr.  The mean sSFR of RGs at z>2.5 are higher than the sSFR of typical SF galaxies over the same z range but are similar or perhaps lower than the galaxy population for RGs at z<2.5.  By comparing the sSFR and the specific BH mass accretion rate, conclude the BHs in radio loud AGN are already, or soon will be, overly massive compared to their host galaxies in terms of expectations from the local MBH-MGal relation.  In order to "catch up" with the BH, the galaxies require about an order-of magnitude more time to grow in mass, at the observed SFRs, compared to the time the BH is actively accreting.  However, during the current cycle of activity, argue that this catching-up is likely to be difficult due to the short gas depletion times.  Finally, speculate on how the host galaxies might grow sufficiently in stellar mass to ultimately fall onto the local MBH-MGal relation.