Day 399

Saturday.

2006MNRAS.371.1188H  (arXiv:astro-ph/0511416)
On measuring the covariance matrix of the non-linear power spectrum from simulations
Hamilton, Rimes, Scoccimarro

Estimate the covariance of PS of a statistically homogeneous and isotropic density field from a single periodic simulation by applying a set of weightings to the density field, and by measuring the scatter in PS between different weightings.  Recommend a specific set of 52 weightings containing only combinations of fundamental modes, constructed to yield a minimum variance estimate of the covariance of power.  Numerical tests reveal that at non-linear scales the variance of power estimated by the weighting method substantially exceeds that estimated from a simple ensemble method.  Argue that this discrepancy is caused by beat-coupling, in which products of closely spaced Fourier modes couple by NL gravitational growth to the beat mode between them.  Beat-coupling appears whenever NL power is measured from Fourier modes with a finite spread of wavevector, and is therefore preset in the weightings method but not in the ensemble method.  Beat-coupling inevitably affects real galaxy surveys, whose Fourier modes have finite width.  Surprisingly, the beat-coupling contribution dominates the covariance of power at NL scales, so that, counter-intuitively, it is expected that the covariance of NL power in galaxy surveys is dominated not by small-scale structure, but rather by beat-coupling to the largest scales of the survey.

Day 398

Good Friday.


1303.6783
Space based microlensing planet searches
Beaulieu, Tisserand, Batista

EUCLID and WFIRST combine exoplanet search and DE characterization.  Space-based microlensing is the optimal approach to providing a true statistical census of planetary systems in the Galaxy, over a range of likely semi-moajor axes.  This census, combined with Kepler, will determine how common Earth-like planets are over a wide range of orbital parameters.  Preset a status report of the results obtained by microlensing on exoplanets and the new objectives of the next generation of ground based wide field imager networks.  Discuss the prospect offered by space based microlensing at 2020-2025.

1303.6896
Gravitational lensing evidence against extended dark matter haloes
Magain, Chantry

Dark matter around early-type galaxies, detected by BG quasar lensing: a robust measure of total mass within the Einstein ring.  The M/L ratio of the lensing galaxies does not depend on radius, from inner galactic regions out to several half-light radii; its value does not exceed the value predicted by stellar population models by more than a factor two, which may be explained by baryonic dark matter alone, without any need for exotic matter.  Results suggest that if DM is present in early-type galaxies, its amount does not exceed the amount of luminous matter and its density follows that of luminous matter, in sharp contrast to what is found from rotation curves of spiral galaxies.

1303.6949
The pesky power asymmetry
Dai, Jeong (Donghui!), Kamionkowski, Chluba

Physical models for the hemispherical power asymmetry in the CMB reported by Planck must satisfy CMB constraints to the homogeneity of the Universe and quasar constraints to power asymmetries.  Survey a variety of models for the power asymmetry and show that consistent models include (1) a modulated scale-dependent isocurvature contribution to the matter power spectrum or (2) a modulation of the reionization optical depth, (3) gravitational-wave amplitude, or (4) scalar spectral index.  Propose further tests to distinguish between the different scenarios.

1303.6959
Cosmological zoom simulations of z=2 galaxies: the impact of galactic outflows
Angles-Alcazar, Dave, Ozel, Oppenheimer

High-res cosmo zoom sims with 200pc resolution at z=2 and various prescriptions for galactic outflows in order to explore the impact of winds on the morphological, dynamical, and structural properties of eight individual z=2 galaxies.  Present a detailed comparison to spatially- and spectrally-resolved Ha and other observations of z~2 galaxies.  Find that simulations without winds produce massive, compact galaxies with low gas fractions, super-solar metallicities, high bulge fractions, and much of the SF concentrated within the inner kpc.  Strong winds are required to maintain high gas fractions, redistribute SF gas over larger scales, and increase the velocity dispersion of simulated galaxies, more in agreement with the large, extended, turbulent disks typical of high-z SF galaxies.  Winds also suppress early SF to produce high-z cosmic SF efficiencies in better agreement with observations.  Sizes, rotation velocities, and velocity dispersions all scale with stellar mass in accord with observations.  Find a diversity of morphological characteristics - among the two most massive galaxies, one resembles a quiescent grand-design spiral while the other is a clumpy disk undergoing a minor merger; the clumps are evident in Ha but not in the stars.  Some galaxies have stellar densities above the threshold for compact ellipticals seen at these redshifts, although these galaxies are SF since quenching feedback are not included.  Rotation curves are generally slowly rising, particularly when calculated using azimuthal velocities rather than enclosed mass.  These results show that cosmological simulations including outflows can produce disk galaxies similar to those observed during the peak epoch of cosmic galaxy growth.

1303.6960
Finding core collapse supernova from the epoch of reionization behind cluster lenses
Pan, Loeb

Utilize GL by galaxy clusters with Einstein radii > 35" in the search for the highest redshift galaxies.  Associated SNe from the epoch of reionization would have their fluxes boosted above the detection threshold, extending their duration of visibility.  Predict JWST will be able to discover lensed core-collapse SNe at z>7-8.

1303.6961
Are super-luminous supernovae and long GRBs produced exclusively in young dense stellar clusters?
van den Heuvel, Zwart

Argue that both the super luminal SNe and long-duration GRBs are exclusive products of dynamical interactions and collisions in young dense star clusters, which are abundant in dwarf galaxies with active SF; present a model.

1303.7121
Cosmological magnetic fields: their generation, evolution and observation
Durrer, Neronov

Review the possible mechanisms for the generation of cosmological B-fields, discuss their evolution in an expanding Universe filled with the cosmic plasma and provide a critical review of the literature on the subject.  Put special emphasis on the prospects for observational tests of the proposed cosmological magneto genesis scenarios using radio and gamma-ray astronomy and UHE CRs.  Argue that primordial B-fields are observationally testable.  Lead to B-fields in the IGM with B-field strength and correlation length in a well-defined range.  Also state the unsolved questions in this open problem, and propose future observations to address them.

1303.7124
Potential of EBL and cosmology studies with the Cherenkov telescope array
Mazin, ... Totani, et al, for the CTA consortium

VHE (E>100 GeV) gamma-rays are absorbed via interactions with low-energy photons from the extragalactic background light (EBL) if the involved photon energies are above the threshold for electron-positron pair production.  The VHE gamma-ray absorption, which is energy dependent and increases strongly with z, distorts the VHE spectra observed from distant objects.  The observed energy spectra of the AGNs carry, therefore, and imprint of the EBL.  The detection of VHE gamma-ray spectra of distant sources (z=0.11-0.54) by current generation imaging atmospheric Cherenkov telescopes (IACTs) enabled to set stronger upper limits on the EBL density, using certain basic assumptions about blazar physics.  Study how the improved sensitivity of Cherenkov Telescope Array (CTA) and its enlarged energy coverage will enlarge knowledge about EBL and its sources.  CTA will deliver a large sample of AGN at different z with detailed measured spectra.  In addition, it will provide the exciting opportunity to use GRBs as probes for the EBL density at high z.  [what is there to EBL besides the CMB?  The CIB?  Why is the EBL so interesting at different z?]

1303.7194
Evidence for AGN-driven outflows in young radio quasars
Kim, etal

NIR spectra of young radio quasars from WFISE; typical redshifts of 1.6-2.5 and bolometric luminosities ~1e47 erg/s.  Based on the intensity ratios of narrow emission lines, find that these objects are mainly powered by AGNs, although SF contribution cannot be completely ruled out.  The host galaxies experience moderate levels of extinction, A(V)~0-1.3 mag [meaning, some dust].  The observed [OIII] luminosities and rest-frame J-band magnitudes constrain the BH masses to lie in the range 1e8.9-9.7 Msun.  From the empirical correlation between BH mass and host galaxy mass, infer stellar masses of 1e11.3-12.2 Msun.  The [OIII] line is exceptionally broad, with FWHM ~1300 to 2100 km/s, significantly larger than that of ordinary distant quasars.  Argue that these large line widths can be explained by jeg-induced outflows, as predicted by theoretical models of AGN feedback.

1303.7206
Ripple effects & oscillations in the broad FeKa line as a prove of massive black hole mergers
McKernan, Ford, Kocsis, Haiman

If a sufficiently massive satellite BH is embedded in a gas disk around a primary SMBH, it can open a empty gap in the disk.  A gap-opening secondary close to the primary will leave an imprint in the broad component of the FeKa emission line, which varies in a unique and predictable manner.  If the gap persists into the innermost disk, the effect consists of a pari of dips in the broad line which ripple blue-ward and red-ward from the line centroid energy respectively, as the gap moves closer to the primary.  This ripple effect could be unambiguously detectable and allow an EM monitoring of massive BH mergers as they occur.  As the mass ratio of the secondary to the primary BH increases to q>0.01, expect the gap to widen, possibly clearing a central cavity in the inner disk, which shows up in the broad FeKa line component.  If the secondary stalls at >100 r_g in its in-migration, due to low co-rotating gas mass, a detectable ripple effect occurs in the broad line component on the disk viscous timescale as the inner disk drains and the outer disk is dammed.  If the secondary maintains an accretion disk within a central cavity, due to dam bursting or leakage, a periodic 'see-saw' oscillation effect is exhibited in the observed line profile.  Demonstrate the range of ripple effect signatures potentially detectable with Astro-H and IXO/Athena, and oscillation effects potentially detectable with XMM or LOFT for a wide variety of merger and disk conditions.  Observations of the ripple effect and periodic oscillations can be used to provide an early warning of gravitational radiation emission from the AGN.

1212.4097
Search for dark matter annihilations in the Sun with the 79-string IceCube detector
IceCube collaboration

Search for muon neutrinos from DM annihilation in the center of the Sun with the 79-string configuration of IceCube.  The DeepCore sub-array is included in the analysis, lowering the energy threshold and extending the search to the austral summer.  The 317 days of data collected between June 2010 and May 2011 are consistent with the expected background from atmospheric muons and neutrinos.  Upper limits are therefore set on the dark matter annihilation rate, with conversions to limits on spin-dependent and spin-independent WIMP-proton cross-sections for WIMP masses in the range 20-5000 GeV.   These are the most stringent spin-dependent WIMP-proton cross-sections limits to date above 35GeV.

Day 397

Thursday.

1102.4349
Integral field spectroscopy of massive, kiloparsec-scale outflows in the infrared-luminous QSO Mrk 231
Rupke, Veilleux

Unambiguous detection of a wide-angle, kpc scale outflow from this QSO, using neutral gas absorption.  how that the nuclear region hosts an outflow with blueshifted velocities reaching 110 km/s, extending 2-3 kpc from the nucleus in all directions in the plane of the sky [wow].  A radio jet impacts the outflow north of the nucleus, accelerating it to even higher velocities (up to 1400 km/s).  3.5 kpc south of the nucleus, SF is simultaneously powering an outflow that reaches more modest velocities of only 570 km/s.  Blueshifted ionized gas is also detected around the nucleus at lower velocities and smaller scales.  The mass and energy flux from the outflow are >2.5x the SFR and >~0.7% of the AGN luminosity, consistent with feedback models of QSOs.

1303.6629
Early-type galaxy archeology: ages, abundance ratios, and effective temperatures from full-spectrum fitting
Conroy, Graves, van Dokkum

Model stacked spectra of early-type galaxies from SDSS as a function of sigma (dispersion velocity) from 90 to 300 km/s.  High quality spectra used (S/N~1000/A), covering 4000A-8800A.  Population synthesis model includes variation in 16 elements from C to Ba, the shift in effective temperature of the stars wrt a solar metallicity isochrone, and other params.  Fit the full optical spectra, measure the abundances of the elements V, Cr, Mn, Co and Ni from the integrated light of distance galaxies.  Main results: (1) light-weighted stellar ages range from 6-12 Gyr from low to high sigma, (2) [Fe/H] varies by less than 0.1 dex across the entire sample, (3) Mg closely tracks O, and both increase from 0.0 at log sigma to 0.25 at high sigma; Si and Ti show a shallower rise with sigma, and Ca tracks Fe rather than O; (4) The iron peak elements V, Cr, Mn, and Ni track Fe, while Co tracks O, suggesting that Co forms primarily in massive stars, (5) C and N track O over the full sample, and [C/Fe] and [N/Fe] exceed 0.2 at high sigma; and (6) the variation in Delta (T_eff) with total metallicity follows theoretical predictions based on stellar evolution theory.  Derived [Mg/Fe] and [O/Fe] abundance ratios are 0.05-0.1 dex lower than most previous determinations.  Under the conventional interpretation that the variation in these ratios is due to star formation timescale variations, results suggest longer SF timescales for massive early-type galaxies than previous studies.

1303.6631
Insights into the content and spatial distribution of dust from the integrated spectral properties of galaxies
Chevallard, Charlot, Wandelt, Wild

Content and spatial distribution of dust in structurally unresolved SF galaxies from the observed dependence of the integrated spectral properties on galaxy inclination.  Combine radiative transfer (RT) model in dusty media with prescription for the spectral evolution of galaxies, via the association of different geometric components of galaxies with stars in different age ranges.  Show that a wide range of RT models all predict a quasi-universal relation between slope of the attenuation curve at any wavelength and V-band attenuation optical depth in the diffuse ISM, at all galaxy inclinations.  The relation predicts steeper (shallower) dust attenuation curves than both the Calzetti and MW curves at small (large) attenuation optical depths, which implies that geometry and orientation effects havae a stronger influence on the shape of the attenuation curve than changes in the optical properties of dust grains.  Interpret 23k SF galaxy attenuation curves.  Measure the face-on B-band optical depth of this sample to be tau_B perp ~1.8pm0.2.  Quantify the enhanced optical depth towards newly formed stars in birth clouds, find it to be significantly larger in galaxies with bulges than in disc-dominated galaxies, while tau_Bperp is roughly similar in both cases.  Show that neglecting the effect of geometry and orientation on attenuation can severely bias the interpretation of galaxy spectral energy distributions, ad the impact of broadband colors can reach up to 0.3-0.4 mag at optical wavelengths and 0.1 mag at NIR ones.

1303.6644
The WiggleZ dark energy survey: constraining galaxy bias and cosmic growth with 3-point correlation functions
Marin, Blake, et al

3pt corroation function for 187k galaxies; scale and shape dependence at z=0.35, 0.55, and 0.68, the highest redshifts where these measurements have been made to date.  Compare with N-body sim results, constrain linear and NL bias of galaxies wrt DM, marginalise over them to obtain sigma_8(z).  Consistent with LCDM predictions.

1303.6689
Evolution of galaxies and their environments at z=0.1 to 3 in COSMOS
Scoville et al

The galaxy properties (M*, SEDs and SFRs) are strongly correlated with environmental density and redshift, particularly at z<1.0-1.2.  Classifying the spectral type of each galaxy using the rest-frame b-i color (from the photoz SED fitting), find a strong correlation of early type galaxies (E-Sa) with high density environments, while the degree of environmental segregation varies systematically with redshift out to z~1.3.  In the highest density regions, 80% of the galaxies are early types at z=0.2 compared to only 20% at z=1.5.  The SFRs and the SF timescales exhibit clear environmental correlations.  At z>0.8, the SFR density is uniformly distributed over all environmental density percentiles, while at lower z the dominant contribution is shifted to galaxies in lower density environments.
1303.6725
HerMES: a deficit in the surface brightness of the cosmic infrared background due to galaxy cluster gravitational lensing
Zemcov, Blain, Coorey, ... Haltern, Jullo, Kneib, ... et al

Observation of 4 massive clusters with Herschel SPIRE: measure a deficit of surface brightness within their central region, after subtracting sources.  Simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit.  The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources.  Find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the CIB.  Integrated total intensity of CIB of L(250 um)>0.69 pm 0.1ish MJy/sr, with more CIB possible from both low-z sources and from sources within the target clusters.  Should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB.

Day 396

Wednesday.

1303.6279
Recurring flares from supermassive black hole binaries: implications for tidal disruption candidates and OJ 287
Tanaka (Taka!)

Possible: accreting SMBH binaries with sub-parsec separations produce luminous, periodically recurring outbursts that interrupt periods of relative quiescence.  Simulations of binaries embedded in prograde accretion disks motivates this: (i) the formation of a central, low-density cavity, and (ii) the leakage of circumbinary gas into this cavity, occurring once per orbit, via discrete streams on nearly radial trajectories.  (i) diminishes AGN optical/UV flux compared to single SMBHs, while the second is likely to trigger periodic fluctuations in the emergent flux.  Toy model: a leaked stream crosses its own orbit and shocks, converting its bulk KE to heat, resulting in a hot, optically thick flow that is quickly accreted and produces a flare with an AGN-like spectrum that peaks in the UV and ranges from optical to soft X-ray.  The preceding quiescence causes the flare to be mistaken from the tidal disruption of a star.  For typical binary periods of years to decades, the event rate in an individual system can be much higher than predicted for stellar tidal disruptions, but infrequent enough to hinder tests of periodicity.  The flares proposed here can be produced by very massive (>1e8 Msun) SMBHs that would not tidally disrupt solar-type stars.  They could be discovered serendipitously in the future by observatories such as LSST or eROSITA.  Apply the model to the active galaxy OJ 287, whose production of periodic optical flares has long fueled speculation that it hosts a SMBH binary.

1303.6281
Absorption signatures of warm-hot gas at low redshift: NeVIII
Tepper-Garcia, Richter, Schaye

Strong NeVIII absorbers are robust probes of shock-heated diffuse gas.

1303.6283
Galactic accretion and the outer structure of galaxies in the CDM model
Cooper, D'Souza, Kauffmann, Wang, Boylan-Kolchin, Guo, Frenk, White

Combine SAM with the particle-tagging technique to predict galaxy surface brightness profiles in a representative sample of ~1900 massive DM haloes (1e12-14 Msun) from Millennium II LCDM N-body sim.  Focus on outer regions of galaxies consisting of stars accreted in mergers.  These simulations cover scales from the stellar haloes of MW-like galaxies to the 'cD envelopes' of groups and clusters, and resolve low SB substructure such as tidal streams.  Find that the surface density of accreted stellar mass around the central galaxies of DM haloes is well described by a Sersic profile, the radial scale and amplitude of which vary systematically with halo mass (M_200).  The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself.  This break disappears with increasing M_200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between stellar mass and halo mass.  To test our model, derive average stellar mass surface density profiles for massive galaxies at z~0.08 by stacking SDSS images.  Model agrees well with these stacked profiles and with other data from the literature, but can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes.  Conclude that it is likely that the structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly.

1303.6285
Nonlinear color-metallicity relations of globular clusters.  IV.  Testing the nonlinearity scenario for color bimodality via HST/WFC3 u-band photometry of M84 (NGC 4374)
Yoon et al

Globular cluster (GC) color distributions in most massive galaxies are bimodal; viewed as presence of merely two GC subsystems with distinct metallicities, forming backbone of various galaxy formation theories.  Recent studies however show that color-metallicity relations (CMRs) often used to derive GC metallicities are in fact inflected.  Such inflection can create bimodal color distributions if the underlying GC metallicity spread is simply broad as expected from the hierarchical merging paradigm of galaxy formation.  In order to test the NL-CMR scenario for GC color bimodality, the u-band photometry is proposed, because the u-related CMRs are theoretically predicted to be least inflected and most distinctive among commonly used optical CMRs.  Present HST WFC3 F336W (u-band) photometry of the GC system in M84, a giant elliptical in the Virgo cluster.  Combine u-band with existing g and z data, find that the u-z and u-g color distributions are different from the g-z distribution in a very systematic manner and remarkably consistent with model predictions based on the NL-CMR hypothesis.  Results lend further confidence to validity of the NL-CMR scenario as an explanation for GC color bimodality.  There are some GC systems showing bimodal spectroscopic metallicity, and in such systems, the inflected CMRs often create stronger bimodality in the color domain.

1303.6286
What controls star formation in the central 500 pc of the Galaxy?
Kruijssen et al

The SFR in the central molecular zone (CMZ, the central 500 pc) of the MW is lower by a factor of >10 than expected for the substantial amount of dense gas it contains, which challenges current SF theories.  Quantify which physical mechanism could be causing this observations.  On scales larger than the disc scale height, the low SFR is found to be consistent with episodic SF due to secular instabilities [what are they?] or variations of the gas inflow along the Galactic bar.  The CMZ is marginally Toomre-stable [condition for differentially rotating disk to be stable] when including gas and stars, but highly Toomre-stable when only accounting for the gas, indicating that the condensation of self-gravitating clouds may be limited.  On small scales, find that the SFR in the CMZ is consistent with an elevated critical density for SF due to the high turbulent pressure - potentially aided by weak magnetic effects and an underproduction of massive stars due to a bottom-heavy IMF.  The existence of a universal density threshold for SF is ruled out, as well as the importance of the HI-H_2 phase transition of hydrogen, the tidal field, the B-field, radiation pressure, and CR heating.  Propose observational and numerical tests to distinguish between the remaining candidate SF inhibitors, in which ALMA play a key role.  Conclude by proposing a self-consistent cycle of SF in the CMZ, in which the plausible SF inhibitors are combined.  Ubiquity suggests that the perception of a lowered central SFR should be a common phenomenon in other galaxies.  Discuss the implications for galactic SF and SMBH growth, including a prediction that the recently reported bimodality of SF in high-z galaxies may emanate from a difference in the gas inflow rates.

1303.6287
Dark matter halo properties from Galaxy-galaxy lensing
Brimioulle, Seitz, Lerchster, Bender, Snigula

CFHTLS, 124 deg sq in ugriz, photoz scatter of Delta z/(1+z)=0.033, outlier rate of 2% for i<=22.5, and extract galaxy shapes down to i=24.0.  Lens: 0.05<z<=1, and source 0.05<z_s<2.  Fit 3 different galaxy halo profiles to the lensing signal: SIS, truncated isothermal sphere (BBS), and NFW.  Derive velocity dispersions, luminosity scaling relations, separate red and blue lenses, as well as the combined sample.

1303.6396
Cold gas in the inner regions of intermediate redshift clusters
Jablonka et al

CO observations of LIRGs inside the virial radii of 2 intermediate redshift clusters (z~0.4-0.5).  Detect 3 galaxies at high S/N (5-10 sigma), and provide robust estiamtes of their CO luminosities.  Find evidence that at fixed LIR (or fixed stellar mass), the frequency of high L'CO galaxies is lower in cluster than in the field, suggesting environmental depletion of the reservoir of cold gas.  Level of SF activity in a galaxy is primarily linked to the amount of cold gas.  In clusters (just as in the field), the conversion between gas and stars seems universal. ... find evidence of a decrease in CO towards cluster centers.

1303.6506
Large-scale inhomogeneities of the intracluster medium: improving mass estimates using the observed azimuthal scatter
Roncarelli, Ettori, et al

Hydro-sims of 62 galaxy clusters and groups: study ICM of inhomogeneities.  Intorduce the concept of residual clumsiness, C_R, that quantifies the LS inhomogeneity of the ICM.  Can be robustly defined, study dependence on radius, mass and dynamical state of the halo.  Observe that it introduces an overestimate in the determination of the density profile from the X-ray emission, which translates into a systematic overestimate of 5(12)% in the measurement of M_gas at R_200 for relaxed (perturbed) cluster sample.  ..other biases.. Residual clumpiness of the ICM is not directly observable, so study its correlation with azimuthal scatter in the X-ray SB of the halo and in the y-parameter profiles.  Find that their correlation is highly significant (0.6-0.7), allowing to define a function that connects the 2 quantities.  Obtain that correcting the observed gas density profiles using the azimuthal scatter eliminates the bias in the measurement of M_gas for relaxed objects, which becomes 0pm2% up to 2R_200, and reduces it by a factor of 3 for perturbed ones.  Method allows to eliminate the systematics on the measurements of M_he and f_gas, although a significant halo to halo scatter remains.

1303.6550
High precision simulations of weak lensing effect on cosmic microwave background polarization
Fabbian, Stompor

As the title says.  Code publicly available.

1303.6564
Reconstructing the lensing mass in the universe from photometric catalogue data
Collett, Marshall, Auger, Hilbert, Suyu, Greene, Treu, Fassnacht, Koopmans, Bradac, Blandford

High precision cosmological distance measurements towards individual objects such as time delay gravitational lenses or type Ia SNe are affected by WL perturbations by galaxies and groups along the line of sight  In time delay gravitational lenses, "external convergence" kappa can dominate the uncertainty in the inferred distances and hence cosmological parameters.  Attempt to reconstruct kappa along LoS using a simple halo model.  Use mock catalogues from MS, and calibrate and compare reconstructed P(kappa) to ray-traced true kappa, including observational uncertainties.  Find that reconstruction of kappa improves precision of ~50% over galaxy number ocunts.  Find that the lowest-kappa LoS have the best constrained P(kappa).  Find: selecting the thrid of the systems with the highest precision kappa estimates gives a sample of unbiased time delay distance measurements with just ~1% uncertainty due to LoS external convergence effects.  Photometric data sufficient to pre-select the best constrained LoS, and can be done before investment in light-curve monitoring.  Conversely, show that selecting LoS with high external shear could induce biases of up to 1% in time delay distance [??what's different from low shear LoS??]; this could introduce ~2% biases on the time-delay distance if ignored.  Suggest areas for improvement of the analysis framework.

1303.6583
A lower growth rate from recent redshift space distortions than expected from Planck
Macaulay, Wehus, Eriksen

Results from 6dFGS, BOSS, LRG, WIggleZ and VIPERS: the RSD measurements are consistently less than the values expected from Planck, and the relative scatter between the RSD meausrements is lower than expected.  

1303.6588
Cluster lensing profiles derived from a redshift enhancement of magnified BOSS-SUrvey galaxies
Coupon, Broadhurst, Umetsu

Detection of z-depth enhancement of BG galaxies magnified by FG clusters.  A clear trend of increasing mean redshift towards the cluster centers is found (use 300k BOSS redshifts, 5-15k SDSS clusters).  Similar but noisier results for (158) X-ray clusters.  The radial form of this z enhancement is well fitted by richness-to-mass weighted composite NFW profile with an effective mass ranging between M_200~1.4-1.8 e14 Msun for the optical cluster sample, and 5e14 Msun for X-ray.  Lensing detection helps to establish the credibility of SDSS cluster surveys; provides a normalization for their respective mass-richness relations.  An independent means of deriving the masses of cluster samples for examining the cosmological evolution, and provides a relatively clean consistency check of WL measurements, free from systematic limitations of shear calibration.

Day 395

Tuesday.

1303.5787
Effect of a high opacity on the light curves of radioactively powered transients from compact object mergers
Barnes, Kasen

Coalescence of compact objects are a promising astrophysical sources of GW signals.  The ejection of r-process material from such mergers may lead to a radioactively-powered EM counterpart which, if discovered, would enhance the science return of a GW detection.  Very little is known about the optical properties of heavy r-process elements; previous light curve models have adopted opacities similar to those of Fe group elements.  Report that the presence of heavier elements, particularly the lanthanides, increase the ejecta opacity by several orders of magnitude.  Include these higher opacities in time dependent, multi-wavelength radiative transport calculations to predict the broadband light curves of one-dimensional models over a range of parameters (eject masses from 0.001 to 0.1 Msun and velocities from 0.1 to 0.3c).  Find that the higher opacities lead to much longer duration light curves which can last a week or more.  The emission is shifted toward to IR bands due to strong optical line blanketing, and the colors at later times are representative of a BB near the recombination temperature of the lanthanides (T~2500K).  Further consider the case in which a second mass outflow, composed of 56Ni, is ejected from a disk wind, and show that the net result is a distinctive 2 component spectral energy distribution, with a bright optical peak due to 56Ni and an IR peak due to r-process ejecta.  Briefly consider the prospects for detection and identification of these transients.

1303.5788
Opacities and spectra of the r-process ejecta from neutron star mergers
Kasen, Badnell, Barnes

Material ejected during (or immediately following) the merger of 2 NSs may assemble into heavy elements by the r-process.  Subsequent decay of the nuclei can power EM emission similar to, but significantly dimmer than, and ordinary SNe.  Predictions of the transient light curves and spectra, however, have suffered from the uncertain optical properties of heavy ions.  Consider the opacity of expanding r-process material, argue that it tis dominated by the line transitions from those ions with the most complex valence electron structure, namely the lanthanides.  For a few representative ions, run atomic structure models to calculate radiative data for ~1e7 lines.  Find: resulting r-process opacities are orders of magnitude larger than that of ordinary (i.e., Fe-rich) SNe ejecta.  Radiative transport calculations using these new opacities indicate that the transient emission should be dimmer and redder than previously thought.  The spectra appear pseudo-BB, with broad absorption features, and peak in the IR (~1um).  Uncertainties in opacities needed to quantify their impact on the spectral predictions.    Implications for observational strategies for studies of radioactively powered EM counterparts to compact object mergers.

1303.5987
The chemical evolution of star-forming galaxies over the last 11 billion years
Zahid, Geller, Kewley, Hwang, Fabricant, Kurtz

Measure the stellar mass-metallicity relation at 5 epochs out to z~2.3.  Quantify evolution in the shape of mass-metallicity relation as a function of redshift; the mass-metallicity relation flattens at late times.  Empirical upper limit to the gas-phase O abundance in SF galaxies that is independent of z.  From examination of the mass-metllicity relation and its observed scatter, show that the flattening at late times is a consequence of evolution in the stellar mass where galaxies enrich to this empirical upper metallicity limit; there is also evolution in the fraction of galaxies at a fixed stellar mass that enrich to this limit.  The stellar mass where metallicities begin to saturate is ~0.7 dex smaller in the local universe than it is at z~0.8.  These observations provide a benchmark for theoretical and observational studies of the chemical evolution of SF galaxies.

1303.6109
A candidate z~8 galaxy lensed by a foreground z~1.7 group
Barone-Nugent, Wyithe, Trenti, Treu, Oesch, Bradley, Schmidt

As the title says.  Find in pure-parallel HST as part of BoRG survey.  A Y-dropout galaxy with m=25.9 which appears to be SL by a FG group with a photo-z~1.7, which would be the highest-z deflector discovered to date.  Multiple evidence: (1) the z~8 dropout is close in project to the FG group, (2) it is lightly elongated tangentially in the direction of the putative critical curve, (3) a possible counter image marginally detected, (4) the Y-dropout is not clustered (intrinsically fainter than it appears---i.e., magnified) [clustered?].  SIE deflector model with Sersic SB (with index 0.92) appears to work.  Magnification factor of 3.7.  Lens group mass of 1e12 Msun, M/L_B=30 Msun/Lsun within the Einstein radius.  If confirmed, the system provides a unique opportunity to obtain spectroscopy of a typical z~8 galaxy, and an absolute measure of mass for a galaxy at z~1.7.  Qualitatively consistent with theoretical expectation that 10% of z~8 galaxies with L>2L* are significantly magnified.

1303.6110
Resolving the molecular gas around the lensed quasar RXJ0911.4+0551
Anh, ... Kneib, ... et al

High angular resolution observations of CO(7-6) line and mm continuum in the host galaxy of the gravitationally lensed (z~2.8) quasar.  Resolves molecular disk of the source; 1pm0.2 kpc disk radius, inclination of 70 deg (observed in CO).  Continuum is more compact, only marginally resolved by observations.  Relatively low mass, a scaled-down version of the QSOs usually found at high-z.  ...

1303.6158
Reconciling extremely different concentration-mass relations
Meneghetti, Rasia

Concentration estimates are sensitive to the largely different radial scales probed by a particular measurement method.

Day 394

Monday.

1303.5443
Toward a comprehensive model for feedback by active galactic nuclei: new insights from M87 observations by LOFAR, Fermi and H.E.S.S.
Pfrommer

AGN appears to be critical in balancing radiative cooling of the low-entropy gas at the centers of galaxy clusters and in mitigating the SF of elliptical galaxies.  New observations of M87 enable a comprehensive model for the physical heating mechanism.  Low-frequency radio observations by LOFAR revealed the absence of fossil CR electrons [what the heck is that?] in the radio halo surrounding M87.  This can be resolved by accounting for the CR release from the radio cocoons and the subsequent mixing of CRs with the dense ambient IC gas, which thermalizes the electrons on a timescale similar to the radio halo age of 40 Myrs.  Hadronic interactions of similarly injected CR protons with the ambient gas should produce an observable gamma-ray signal in accordance with the steady emission of the low state [low state?] of M87 detected by Fermi and HESS.  Hence, normalize the CR population to the gamma-ray emission, which shows the same spectral slope as the CR injection spectrum probed by LOFAR, thereby supporting a common origin.  Show that CRs, which stream at the Alfven velocity wrt the plasma rest frame, heat the surrounding thermal plasma at a rate that balances that of radiative cooling on average at each radius, thereby setting the thermal pressure profile equal to that of the streaming CRs.  However, the resulting global thermal equilibrium is locally unstable and allows for the formation of the observed cooling multi-phase medium through thermal instability.  Provided CR heating balances cooling during the emerging "cooling flow", the collapse of the majority of the gas is halted at 1 keV, which is in accordance with x-ray data.  Show that both the existence of a temperature floor and the similar radial scaling of the heating and cooling rates are generic predictions of the CR heating model.


1303.5445
Describing galaxy weak lensing measurements from tenths to tens of Mpc and up to z~0.6 with a single model
Cacciato, van Uitert, Hoekstra

The clustering of galaxies and the matter distribution around them can be described using the halo model complemented with a realistic description of the way galaxies populate dark matter haloes.  This has been used successfully to describe statistical properties of samples of galaxies at z<0.2.  Without adjusting any model parameters, compare the predicted WL signal induced by LRGs to measurements from SDSS DR7 on much larger scales (up to ~90 Mpc/h, h=0.7) and at higher redshift (z~0.4).  Find excellent agreement, suggesting that the model captures the main properties of the galaxy-DM connection.  To extend the comparison to lenses at even higher redshifts, complement the SDSS data with shape measurements from the deeper RCS2, resulting in precise lensing measurements for lenses up to z~0.6.  These measurements are also well described using the same model.  Considering solely these WL meausrements, robustly assess that, up to z~0.6, the number of central galaxies as a function of halo mass is well described by a log-normal distribution with scatter sigma_log(L_c) = 0.146 pm 0.011, in agreement with previous independent studies at lower z. Results demonstrate the value of complementing the information about the properties of the lens galaxies provided by SDSS with deeper, high-quality imaging data.

1303.5490
The supermassive black hole mass - spheriod stellar mass relation for S\'ersic and Core-S\'ersic galaxies
Scott, Graham, Schombert

For core-Sersic galaxies (typically massive and luminous, with M_BH>2e8Msun), find M_BH propto M*_sph^0.97, consistent with other literature relations.  However, for the Sersic galaxies (typically lower masses, M*_sph < 3e10 Msun), find M_BH propto M*_sph^2.22, a dramatically steeper slope that differs by more than 2 std devs.  For Sersic galaxies, M_BH is not a constant fraction of M*_sph.  Sersic galaxies can grow via the accretion of gas which fuels both SF and the central BH, as well as through merging.  Their BH grows significantly more rapidly than their host spheroid, prior to growth by dry merging events that produce core-Sersic galaxies, where the BH and spheroid grow in lock step.  Additional compare Sersic relation with the corresponding relation for nuclear star clusters, confirming that the two classes of central massive object follow significantly different scaling relations.

1303.5528
What determines the grain size distribution in galaxies?
Asano et al

Dust production by SNeII and AGB stars, additional 3 other processes: (i) dust destruction by SN shocks, (i) metal accretion onto the surface of preexisting grains in the cold neutral medium (CNM) -- "grain growth", and (iii) grain-grain collisions (shattering and coagulation) in the warm neutral medium (WNM) and CNM.  Find: grain size distribution in galaxies controlled by stellar sources in early stage of galaxy evolution, and that afterwards the main processes that govern the size distribution changes to those in the ISM.  Since shattering produces a large abundance of small grains (surface-to-vlue ratio of grains increases), it enhances the efficiency of grain growth, contributing to the increase in total dust mass.  Grain growth creates a large bump in the grain size distribution around ~0.01 um.  Coagulation occurs effectively after the number of small grains is enhanced by shattering, and the grain size distribution is deformed to have bump at a ~0.03-0.05 um at t~10 Gyr.  Conclude that the evolutions of the total dust mass and the grain size distribution in galaxies are closely related to each other, and the grain size distribution changes considerably through the galaxy evolution because the dominant dust processes which regulate the grain size distribution change.

1303.5577
Recent variability of the solar spectral irradiance and its impact on climate modelling
Ermolli, etal

More variability in UV spectral range; changes in the visible and NIR bands in anti-phase with the solar cycle.  Chemistry-climent model (CCM) sims show that this might have significant implications on the Earth's atmosphere.  Motivated by these results, summarize current knowledge of SSI (solar spectral irradiance) variability and its impact on Earth's climent.  SSI changes influence the Earth's atmosphere, both directly (due to changes in shortwave heating, and hence temperature and ozone distributions in the stratosphere), and indirectly (dynamical feedbacks).  Investigate these effects with CCM sims with measured and modeled SSI changes.  Discuss the reliability of the available data and propose adidtional coordinated work.

1303.5586
Star formation and metallicity gradients in semi-analytic models of disk galaxy formation
Fu, Kaufmann, Huang, Yates, Moran, Heckman, Dave, Guo

Update radially-resolved SAMs to track the radial distribution of stars, metals, atomic and molecular gas in galactic disks.  MS and MSII sims, modify to (1) simpler SF law, (2) inject heavy elements by SNe directly into the halo (no prior mixing with disk cold gas), (3) include radial gas inflows in disks using a model of the form v_inflow=alpha r.  The sigma_H2 profiles in L* strongly constraints the inflow velocities to (7 km/s at r=10 kpc).  Metallicity gradients affected more strongly by the fraction of metals that are directly injected into the halo gas.  Metals ejected out of the galaxy at early epochs result in late infall of pre-enriched gas and flatter present-day gas metallicity gradients.  Prescription in which 80% of the metals produced by stars are injected into the halo gas provides the best fit to the relative flat observed metallicity gradients of galaxies with stellar masses >1e10 Msun.  Also results in a good fit to the relation between gas metallicity and sSFR in the outer parts of disks.  Examine the correlation between gas metallicity gradient and some global galaxy properties, finding that it is most strongly correlated with the B/T ratio of the galaxy.  This is because gas is consumed when the bulge forms during the galaxy merger, and the gas metallicity gradient is then set by newly-accreted gas.  THese model predictions appear to be in good agreement with observations.

Day 393

Friday.  Planck-on-Astro-ph Day.  Saturday.  Saw a gold ring.

1303.5058
Black hole-galaxy correlations without self-regulations
Angles-Alcazar, Ozel, Dave

Models of BH growth in cosmo context: forwarded a paradigm in which the growth is self-regulated by feedback from the BH itself.  Use cosmo zoom sims of galaxy foramtion down to z=2 to show taht such strong self-regulation is required in the popular spheriacl Bondi accretion model, but that a plausible alternative model in which BH growth is limited by galaxy-scale torques does not require self-regulation.  Instead, this torque-limited accretion model yields BHs and galaxies evolving on average along the observed scaling relations by relying only on a fixed, 5% mass retention rate onto the BH from the radius at which the accretion flow is fed.  Feedback from the BH may (and likely does) occur, but does not need to couple to galaxy-scale gas in order to regulate BH growth.  Show that this results is insensitive to variations in the initial HB mass, stellar feedback, or other implementation details.  The torque-limited model allows for high accretion rates at very early epochs (unlike the Bondi case), which if viable can help explain the rapid early growth of BHs, while by z=2 it yeilds Eddington factors of 1-10%.  This model also yields a less direct correspondence between major merger events and rapid phases of BH growth.  Instead, growth is more closely tied to cosmological disk feeding, which may help explain observational studies showing that, at least at z>1, active galaxies do not preferentially show merger signatures.

1303.5059
Gas-regulation of galaxies: the evolution of the cosmic sSFR, the metallicity-mass-SFR relation and the stellar content of haloes
Lilly, Carollo, Pipino, Renzini, Peng

A simple physical model of galaxies, in which the formation of stars is instantaneously regulated by the mass of gas in a reservoir, links together 3 different aspects of the evolving galaxy population: (a) the cosmic time evolution of the sSFR relative to the growth of haloes, (b) the gas-phase metallicities across the galaxy population and over cosmic time, and (c) the ratio of the stellar to DM mass of haloes,  If the SFR efficiency and wind mass loading are constant, the sSFR is set to the specific accretion rate of the galaxy: more realistic situations lead to an sSFR which is perturbed from this identity.  The metallicity is set by the instantaneous operation of the regulator system rather than by the past history of the system.  The regulator system naturally produces a Z(M*, SFR) relation, with SFR as a second parameter in the mass-metallicity relation.  This will be the same at all epochs unless the efficiency and mass-loading change with time, naturally producing a so-called "fundamental metallicity relation".  The observed Z(M*) relation of SDSS relation of SDSS galaxies implies a strong dependence of stellar mass on halo mass that reconciles the different faint end slopes of the stellar and halo mass-functions in standard LCDM.  It also boosts the sSFR relative to the specific accretion rate and produces a different dependence on mass, both of which are observed.  The derived Z(M*, SFR) relation for the regulator system is fit to published Z(M*, SFR) data.  The fitted efficiency is consistent with observed molecular gas-depletion timescales in galaxies while the fitting mass-loading is also plausible.  The model also successfully reproduces the mass-metallicity relation of star-forming galaxies at z~2.

Planck 2013 resutls. I. through XXIX.
Planck collaboration.

I. Overview of products and scientific results

First 15.5 months of Planck operations, along with a set of scientific and technical papers and a web-based explanatory supplement.  Main science results: robust support for the standard, 6 parameter LCDM model of cosmology and improved measurements for the parameters that define this model, including a highly significant deviation from scale invariance of the primordial power spectrum.  The Planck values for some of these parameters and others derived from them are significantly different from those previously determined.  Several large scale anomalies in the CMB temperature distribution detected earlier by WMAP are confirmed with higher confidence.  Planck sets new limits on the number and mass of neutrinos, and has measured gravitational lensing of CMB anisotropies at 25 sigma [cool!].  Planck finds no evidence for non-Gaussian statistics of CMB anisotropies.  Some tension between Planck and WMAP results; this is evident in the power spectrum and results for some of the cosmology parameters.  In general, Planck results agree well with results from the measurements of baryon acoustic oscillations.  Because the analysis of Planck polarization data is not yet as mature as the analysis of the temperature data, polarization results are not released.  Illustrate the robust detection of the E-mode polarization around CMB hot-and cold-spots.

II. The low frequency instrument data processing
III. LFI systematic uncertainties
IV. Low frequency instrument beams and window functions
V. LFI calibration
VI. High frequency instrument data processing
VII. HFI time response and beams
VIII. HFI photometric calibration and mapmaking
IX. HFI spectral response
X. Energetic particle effects: characterization, removal and simulation

Most of the detected glitches are from galactic protons incident on the Si die from supporting the micromachined bolometric detectors.  At HFI, the particle flux is ~5 per square cm and per second and is dominated by protons incident on the spacecraft with an energy > 39 MeV, leading to a rate of typically one event per second and per detector.  Different categories of glitches have different signature in time streams.  Simulations show glitch removal method does not bias signal.

XII. Component separation

9 frequency bands available; allow robust reconstruction of primordial CMB over nearly the full sky, and constrain Galactic foregrounds.  Describe Planck framework; test 4 FG-cleaned CMB maps using qualitatively different component separation algorithms.  Quality of reconstructions evaluated through detailed simulations and internal comparisons [Euclid with WL would definitely have to do the same], and shown through various tests to be internally consistent and robust for CMB power spectrum and cosmological parameter estimation up to l=2000.  The parameter constraints on LCDM cosmologies derived from these maps are consistent with those presented in the cross-spectrum based Planck likelihood analysis.  Choose two of the CMB maps for specific scientific goals.  Also present maps and frequency spectra of the Galactic low-frequency, CO, and thermal dust emission.  The component maps are found to provide a faithful representation of the sky, as evaluated by simulations.  For the low-frequency component, the spectral index varies widely over the sky, ranging from about beta=-4 to -2.  Considering both morphology and prior knowledge of the low frequency components, the index map allows: to associate a steep spectral index (beta < -3.2) with strong anomalous microwave emission, corresponding to a spinning dust spectrum peaking below 20 GHz, a flat index of beta > -2.3 with strong free-free emission, and intermediate values with synchrotron emission.

XIII. Galactic CO emission

Rotational CO transition lines play a large role in study of SF and Galactic structure.  Such all-sky surveys can be constructed using the Planck HFI data because the 3 lowest CO rotational transition lines at 115,230, and 345 GHz significantly contribute to the signal of the 100, 217 and 353 GHz HFI channels respectively.  2 different component separation methods used to extract the CO maps from Planck HFI data.  The maps obtained are then compared to one another and to existing external CO surveys.  From these quality checks the best CO maps in terms of signal to noise and/or residual FG contamination are selected.  3 sets of velocity-integrated CO emission maps are produced: Type 1 maps of the CO 1-0, 2-1 and 3-2 rotation transitions with low FG contamination but moderate S/N ratio, Type 2 maps for 1-0 and 2-1 transitions with a better S/N; and one Type 3 map, a line composite map with the best S/N in order to locate the faintest molecular regions.  The maps are described in detail.  They are shown to be fully compatible with previous surveys of parts of the Galactic Plane and also of fainter regions out of the Galactic plane.  The Planck HFI velocity-integrated CO maps for the 1-0, 2-1, and 3-2 rotation transitions provide an unprecedented all-sky CO view of the Galaxy.  These maps are also of great interest to monitor potential CO contamination on CMB Planck studies.

XIV. Zodiacal emission

Planets, minor bodies, and diffuse interplanetary dust (IPD) contribute to the submm and mm sky emission.  The diffuse emission can be effectively separated from Galactic and other emissions, because Planck views a given point on the distant celestial sphere multiple times, through different columns of IPD.  Us the Planck data to investigate the behavior of Zodiacal emission over the whole sky in the submm and mm.  Fit the COBE Zodiacal model to the Planck data to find the emissivities of the various components of this model --- a diffuse cloud, 3 astroidal dust bands, a circumsolar ring, and an Earth-trailing feature.  The emissivity of the diffuse Zodiacal cloud decreases with increasing wavelength, as expected from earlier analysis.  The emissivities of the dust bands, however, decrease less rapidly, indicating that the properties of the grains in the bands are different than those in the diffuse cloud.  As part of the analysis, fit the small amount of Galactic emission seen through the instrument's far sidelobes and place limits on possible contamination of the CMB results from both Zodiacal and Galactic emission seen through these far sidelobes.  When necessary, these results are used in the Planck pipeline to make maps with Zodiacal emission and far sidelobes removed. Show that the spectrum of the Zodiacal correction  to the CMB maps is small compared to the Planck CMB temperature power spectrum.

XV. CMB power spectra and likelihood

Derive CMB PS in 2<=l<=2500.  Main source of error at l<=1500 is cosmic variance.  Uncertainties in small-scale FG modeling and instrumental noise dominate the error budget at higher l's.  For l<50, likelihood exploits all Planck frequency channels from 30 to 353 GHz through a physically motivated Bayesian component separations technique.  At l>=50, employ a correlated Gaussian likelihood approximation based on angular cross-spectra derived from 3 channels.  Validate likelihood through an extensive suite of consistency tests, and assess the impact of residual FG and instrumental uncertainties on cosmological parameters.  Find good internal agreement among the high-l cross-sepctra with residual of a few uK^2 at l<=1000.  Compare results with FG-cleaned CMB maps, and with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters.  The best-fit LCDM cosmology is in excellent agreement with preliminary Planck polarization spectra.  The standard LCDM cosmology is well constrained by Planck by l<=1500.  Report a 5.4 sigma deviation from n_s=1.  Consider various extensions beyond the standard model; find not indication of significant departures from the LCDM framework.  Finally, report a tension between the best-fit LCDM model and the low-l spectrum in the form of a power deficit of 5-10% at l<~40, significant at 2.5-3 sigma.  Do not elaborate further on its cosmological implications, but note that this is the most puzzling finding in a otherwise remarkably consistent dataset.

XVI. Cosmological parameters

Results based on CMB temperature and lensing-potential PS.  Planck spectra at high multipoles are extremely well described by the standard spatially-flat 6 param LCDM cosmology.  Find low Hubble constant, H0=67.3pm1.2 km/s/Mpc, and high value of Omega_m=0.315pm0.017, in excellent agreement with constraints from BAO surveys.  Including curvature, find that the Universe is consistent with spatial flatness to percent-level precision using Planck CMB data alone.  Present results from an analysis of extensions to the standard cosmology, using astrophysical data sets in addition to Planck and high-res CMB data; none of these models are favored significantly over standard LCDM.  The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe.  Find a 95% upper limit of r<0.11 on the tensor-to-scalar ratio. No evidence for additional neutrino-like relativistic particles.  Using BAO and CMB data, find N_eff=3.3pm0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the summed neutrino mass.  Results are in excellent agreement with BBN and the standard value of N_eff=3.046.  Find no evidence for dynamical DE.  Despite the success of the standard LCDM model, this cosmology does not provide a good fit to the CMB PS at low multipoles, as noted previously by the WMAP team.  While not of decisive significance, this is an anomaly in the otherwise self-consistent analysis of the Planck temperature data.

XVII. Gravitational lensing by large-scale structure

On the arcminute scales probed by Planck, the CMB anisotropies are gently perturbed by gravitational lensing.  Present studies of the effect, independent detection in the 3 bands with an overall significance of 25 sigma.  Use the temperature-tradient correlations induced by lensing to reconstruct a (noisy) map of the CMB lensing potential, which provides an integrated measure of the mass distribution back to the CMB last-scattering surface.  Lensing potential map is significantly correlated with other tracers of mass, a fact demonstrated using several representative tracers of LSS.  Estimate the PS of the lensing potential, finding generally good agreement with expectations from the best-fitting LCDM model of the Planck temperature PS, showing that this measurement at z=1100 correctly predicts the properties of the lower z, later-time structures which source the lensing potential.  When combined with the temperature PS, measurement provides degeneracy-breaking power for parameter constraints; improves CMB-alone constraints on curvature bay a factor of 2 and also partly breaks the degeneracy between the amplitude of the primordial perturbation PS and the optical depth to reionization, allowing a measurement of the optical depth to reionization which is independent of large-scale polarization data.  Discarding scale information, measurement corresponds to a 4% constraint on the amplitude of the lensing potential PS, or a 2% constraint on the RMS amplitude of matter fluctuations at z~2.

XVIII. Gravitational lensing-infrared background correlation

Planck provides info both on CIB (integrated history of SF) and CMB lensing (distribution of DM).  The conjunction of these 2 unique probes allows direct measurement of the connection between dark and luminous matter in the 1<z<3 universe.  Use 3pt statistic optimized to detect the correlation between the two tracers.  Follow a thorough discussion of possible contaminants and a suite of consistency tests, using lens reconstructions at 3 bands and CIB measurements, report the first detection of the correlation between CIB and CMB lensing.  The well matched z distribution of these two signals leads to a detection significance wit ha peak value of 42 sigma at 545 GHz and a correlation as high as 80%.  Full set of multi-frequency measurements (both auto and cross-spectra) are consistent with a simple halo-based model, with a characteristic mass scale for the haloes hosting CIB sources of M=1e(10.5 pm 0.6) Msun.  Leveraging the frequency dependence of the signal, isolate the high redshift contribution to the CIB, and constrain the SFR density at z>1.  Measure directly the SFR density with around 2 sigma significance for 3 z bins between 1<z<7, thus opening a new window into the study of the formation of stars at early times.

XIX. The integrated Sachs-Wolfe effect

Detection of the ISW (correlation between CMB and LS evolving gravitational potentials), with significance of 2-4 sigma (method dependent).  Investigate 3 separate approaches, which cover essentially all previous studies, as well as breaking new ground.  (i) correlation of the CMB with Planck reconstructed gravitational lensing potential.  Detection made via lensing-induced bispectrum; the correlation between lensing and ISW has significance close to 2.5 sigma.  (ii) Cross-correlation with tracers of LSS, yielding around 3 sigma, based on combination of NVSS and SDSS data.  (iii) Aperture photometry on stacked CMB fields at the locations of known LSS, which yields a 4 sigma signal when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale compared to expectations. Recent catalogues give more moderate results, ranging from negligible to 2.5 sigma at most, but with a more consistent scale and amplitude, the latter being still slightly above what is expected from numerical simulations within [LCDM].  Where they can be compared, these measurements are compatible with previous work using data from WMAP, which had already mapped these scales to the limits of cosmic variance.  Planck's broader frequency coverage confirms that the signal is achromatic, bolstering the case for ISW detection.  As a final step, use tracers of LSS to filter the CMB data, presenting maps of the ISW temperature perturbation.  These results provide complementary and independent evidence for the existence of DE component that governs the current accelerated expansion of the Universe.

XX. Cosmology from Sunyaev-Zeldovich cluster counts

Constraints from 189 galaxy clusters from Planck SZ catalog (PSZ).  S/N threshold of 7, each object confirmed as a clusters, and all but one with a z estimate.  Discuss the calculation of the expected cluster counts as a function cosmo parameters, the completeness of the sample, and the likelihood construction method.  Using a relation between mass M and SZ signal Y based on comparison to X-ray measurements, derive constraints on sigma_8 and Omega_m in the flat LCDM model.  Test the robustness of estimates and find that possible biases in Y-M relation and the halo mass function appear larger than the statistical uncertainties from the cluster sample.  Assuming a bias between the X-ray determined mass and the true mass of 20%, motivated by comparison of observation with sims, find that sigma_8(Omega_m/0.27)^0.3=0.78pm0.01, with 1d ranges sigma_8=0.77pm0.02 and Omega_m=0.29pm0.02.  The values of the cosmological parameters are degenerate with the mass bias, and it is found that the larger values of sigma_8 and Omega_m preferred by the Planck's measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 45%.  Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales, such as a component of massive neutrinos.  Place results in the context of other determinations of cosmological parameters, and discuss issues that need to be resolved in order to make progress in this field.

XXI. Cosmology with the all-sky \Planck\ Compton parameter $y$-map

All-sky map of tSZ from 100 to 857 GHz channel maps from Planck.  Map shows correspondence with PSZ catalogue.  Compute it's angular PS.  At large angular scales (l<60), the major FG contaminant is the diffuse thermal dust emission.  At small angular scales (l>500), the clustered CIB and residual point sources are the major contaminants.  These FGs are carefully modeled and subtracted.  Measure the tSZ PS in angular scales, 0.17<theta<3.0, that were previously unexplored.  The measured tSZ PS is consistent with that expected from the Planck catalogue of SZ sources, with additional clear evidence of signal from unresolved clusters and, potentially, diffuse warm baryons.  Use the tSZ PS to obtain the cosmo constraints: sigma_8(Omega_m/0.28)^(3.2/8.1)=0.784pm0.016.  Marginalized band-powers of tSZ spectrum and best-fit models given.  The non-Gaussianity of the Compton parameter map is further characterized by computing its 1d probability distribution function and its bispectrum.  These are used to place additional independent constraints on sigma_8.

XXII. Constraints on inflation

Analyze implications of Planck data for cosmic inflation.  Constraint of n_s=0.960 pm 0.0073, ruling out exact scale invariance at >5 sigma.  Planck establishes and upper bound on the tensor-to-scalar ratio at r<0.11.  Planck data shrink the space of allowed standard inflationary models, preferring potentials with V"<0.  Exponential potential models, the simplest hybrid inflationary models, and monomial potential models of n>2 do not provide a good fit to the data.  Planck does not find any statistically significant running of the scalar spectral index, obtaining dn_s/dlnk=-0.0134 pm 0.0090.  Several analysis dropping the slow-roll approximation are carried out, including detailed model comparison and inflationary potential reconstruction.  Investigate whether the primordial PS contains any features.  .... Constrain several single-field inflation models with generalized Lagrangians by combining PS data with bounds of f_NL measured by Planck.  The fractional primordial contribution of CDM isocurvature modes in the curvaton and axion scenarios has upper bounds of 0.25% (95% CL), respectively.  In models with arbitrarily correlated CDM or neutrino isocurvature modes, an anti-correlation can improve chi^2 by ~4 dues to a moderate tension between l<40 and higher multipoles.  Nonetheless, the data are consistent with adiabatic initial conditions.

XXIII. Isotropy and statistics of the CMB

Fundamental assumptions of the standard cosmological model: initial fluctuations are statistically isotropic and Gaussian; rigorously tested using maps of the CMB anisotropy from Planck.  Results based on studies of 4 independent estimates of CMB compared to simulations using a fiducial LCDM model and incorporating essential aspects of Planck measurement process. Deviations from isotropy have been found and demonstrated to be robust against component separation algorithm, mask and frequency dependence.  Many of these anomalies were previously observed in the WMAP data, and are now confirmed at similar levels of significance (~3 sigma).  However, find little evidence for non-Gaussianity with the exception for a few statistical signatures that seem to be associated with specific anomalies.  In particular, find that the quadrupole-octopole alignment is also connected to a low observed variance of the CMB signal.  The dipolar power asymmetry is now found to persist to much smaller angular scales, and can be described in the low-l regime by a phenomenological dipole modulation model.  Finally, it is plausible that some of these features may be reflected in the angular PS of the data which shows a deficit of power on the same scales.  When the PS of two hemispheres defined by a preferred direction are considered separately, one shows evidence for a deficit in power, while its opposite contains oscillations between odd and even modes that may be related to the parity voilation and phase correlations also detected in the data.  While these analyses represent a step forward in building an understanding of the anomalies, a satisfactory explanation based on physically motivated models is still lacking.

XXIV. Constraints on primordial non-Gaussianity

Use 3 optimal bispectrum estimators, separable template-fitting (KSW), binned, and model, obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting final result of: f_NL^local=2.7pm5.8, f_NL^equil=-42pm75, and f_NL^ortho=-25 pm 39; Find the ISFW-lensing bispectrum expected in the LCDM scenario.  Results based on comprehensive simulations, are stable across component separation techniques, pass tests, and confirmed by skew-C_l, wavelet bispectrum and Minkowski functional estimators.  Beyond estimates of individual shape amplitudes, present model-independent, 3d reconstructions of the Planck CMB bispectrum and derive constraints on early-Universe scenarios that generate primordial NG, including general single-field models of inflation, excited initial states, and directionally-dependent vector models.  Provide an initial survey of scale-dependent feature and resonance models.  ... 

XXV. Searches for cosmic strings and other topological defects

As the title says---upper limits found.

XXVI. Background geometry and topology of the universe

Detect departures from homogeneity and isotropy on the largest scales.  Search for topology with a fundamental domain (nearly) intersecting the last scattering surface (comoving distance X_r).  Some preference for multi-connected models just larger than X_r.  This efect also present in simulated realizations of isotropic maps, interpret it as the inevitable alignment of mild anisotropic correlations with chance features in a single sky realization.  Test for: cubic torus (matched-circles search), chimney, slab, dodecahedron, truncated cube, octahedron, Bianchi VII_h geometry.  A Bianchi pattern is quite efficient at accounting for some large-scale anomalies seen in Planck data.  Cosmological parameters are in strong disagreement with those found from CMB anisotropy data alone.  In the physically motivated setting where the Bianchi parameters are fitted simultaneously with the standard cosmological parameters, find no evidence for a Bianchi VII_h cosmology; constrain vorticity of such models.

XXVII. Doppler boosting of the CMB: Eppur si muove

Velocity relative to the rest frame of CMB generates a dipole temperature anisotropy on the sky, with amplitude of v=369 km/s.  Motion also modulates and aberrates the CMB temperature fluctuations (as well as every other source of radiation at cosmological distances).  This is an order 0.1% effect applied to fluctuations which are already one part in roughly one hundred thousand, so it is quite small.  Neverthless, it becomes detectable with the all-sky coverage, high angular resolution, and low noise levels of the Planck satellite.  Report a first measurement of this velocity signature using the aberration and modulation effects on the CMB temperature anisotropies, finding a component in the known dipole direction, (l,b)=(264,48) deg, of 384 km/s pm 78 (stat) pm 115 (sys).  This is a significant confirmation of the expected velocity.

XXVIII. The Planck catalogues of compact sources

PCCS: catalogues of sources detected in Planck nominal mission data.  9 single-frequency catalogues of compact sources containing reliable sources, both Galactic and extragalactic, detected over the entire sky.  90% complete in the best band, angular resolution from ~33' to 5'.  reliability is >80% and >65% of the sources have been detected at least in 2 contiguous Planck channels.  The Planck PCCS sources have known associations to stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features.  In this paper present the construction and validation of the PCCS, its contents and statistical characterization.

XXIX. Planck catalogue of Sunyaev-Zeldovich sources

Catalogue of clusters and cluster candidates from SZ, containing 1227 entries, 861 confirmed; 178 confirmed as clusters and further 683 previously-known clusters.  The remaining 366 have the status of cluster candidates, and divide them into 3 classes according to the quality of evidence that they are likely to be true clusters.  The Planck SZ catalogue is the deepest all-sky cluster catalogue, with redshifts up to about one, and spans the broadest cluster mass range from 0.1 to 1.5 e15 Msun.  Completeness and statistical reliability; comparison with existing surveys or catalogues described.  An ensemble of 813 cluster z, and for all these Planck clusters, also include a mass estimated from a newly-proposed SZ-mass proxy.  A refined measure of the SZ Compton parameter for the cluters with X-ray counter-parts is provided, as is an X-ray flux for all the Planck clusters not previously detected in X-ray surveys.

1303.5090
Planck intermediate results. XIII. Constraints on peculiar velocities
Planck collaboration 

At average z of 0.18, kSZ monopole amounts to 72 pm 60 km/s, less than 1% of the relative Hubble velocity of the cluster sample wrt local CMB frame.  From a subset, find raidal peculiar velocity rms to be <800km/s, ~3x the LCDM prediction for athe typical cluster radial velocity rms at z=0.155.  No detection of bulk flow as measured in any comoving sphere extending to the maximum z covered by the cluster sample.  A blind search for bulk flows in this sample has an upper limit of 254 km/s dominated by CMB confusion and instrumental noise, indicating that the Universe is largely homogeneous on Gpc scales  IN conjunction with SNe observations, Planck is able to rule out a large class of inhomogeneous void models as alternatives to DE or modified gravity.  Planck constraints on peculiar velocities and bulk flows are thus consistent with the LCDM scenario.
1303.5328
Updated nearby galaxy catalog
Karachentsev, Makarov, Kaisina

All-sky catalog of 869 nearby galaxies, distance estimates within 11 Mpc or corrected radial velocities V_LG < 600 km/s.  The catalog is a renewed and expanded version of the Catalog of Neighboring Galaxies by Karachentsev+2004.  Collects data on: angular diameters, apparent magnitudes (FUV, B, K_s), H_alpha and HI fluxes, morphological types, HI-line widths, radial velocities and distance estimates.  Local volume (LV) sample 108 dwarf galaxies remaint obe still without measured radial velocities.  Catalog yields also calculated global galaxy parameters: linear Holmberg diameter, absolute B-magnitude, surface brightness, HI-mass, stellar mass estimated via K-band luminosity, HI rotational velocity corrected for galaxy inclination, indicative mass within the Holmberg radius, and 3 kinds of "tidal index", which quantify the local density environment.  Catlog is supplemented with the data based on the local galaxies, which presents their optical and available H_alpha images, as well as other service.  Briefly discuss the Hubble flow within the LV, and different scaling relations that characterize galaxy structure and global star formation in them.  Also trace the behavior of the mean stellar mass density, HI-mass density and SFR density within the considered volume.