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.