Date: Thu, 29 Nov 12 01:08:46 GMT Subject: astro-ph daily 57 new + 6 crosses received by eprepget ------------------------------------------------------------------------------ ------------------------------------------------------------------------------ Send any comments regarding submissions directly to submitter. ------------------------------------------------------------------------------ Archives at http://arxiv.org/ To unsubscribe, e-mail To: astro-ph@arXiv.org, Subject: cancel ------------------------------------------------------------------------------ received by eprepget from Tue 27 Nov 12 21:00:00 GMT to Wed 28 Nov 12 21:00:00 GMT ------------------------------------------------------------------------------ \\ arXiv:1211.6425 Date: Tue, 27 Nov 2012 21:00:00 GMT (445kb) Title: Implementation of Sink Particles in the Athena Code Authors: Hao Gong and Eve C. Ostriker Categories: astro-ph.IM astro-ph.GA Comments: 39 pages, 14 figures, Accepted to ApJS \\ We describe implementation and tests of sink particle algorithms in the Eulerian grid-based code Athena. Introduction of sink particles enables long-term evolution of systems in which localized collapse occurs, and it is impractical (or unnecessary) to resolve the accretion shocks at the centers of collapsing regions. We discuss similarities and differences of our methods compared to other implementations of sink particles. Our criteria for sink creation are motivated by the properties of the Larson-Penston collapse solution. We use standard particle-mesh methods to compute particle and gas gravity together. Accretion of mass and momenta onto sinks is computed using fluxes returned by the Riemann solver. A series of tests based on previous analytic and numerical collapse solutions is used to validate our method and implementation. We demonstrate use of our code for applications with a simulation of planar converging supersonic turbulent flow, in which multiple cores form and collapse to create sinks; these sinks continue to interact and accrete from their surroundings over several Myr. \\ ( http://arxiv.org/abs/1211.6425 , 445kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6426 Date: Tue, 27 Nov 2012 21:00:00 GMT (380kb,D) Title: Constraining Self-Interacting Dark Matter with the Milky Way's dwarf spheroidals Authors: Jesus Zavala (1,2), Mark Vogelsberger (3), Matthew G. Walker (3) ((1) UW, (2) PI, (3) Harvard/CfA) Categories: astro-ph.CO Comments: 6 pages, 4 figures, submitted to MNRAS Letters \\ Self-Interacting Dark Matter is an attractive alternative to the Cold Dark Matter paradigm only if it is able to substantially reduce the central densities of dwarf-size haloes while keeping the densities and shapes of cluster-size haloes within current constraints. Given the seemingly stringent nature of the latter, it was thought for nearly a decade that SIDM would be viable only if the cross section for self-scattering was strongly velocity-dependent. However, it has recently been suggested that a constant cross section per unit mass of sigma_T/m~0.1cm^2/g is sufficient to accomplish the desired effect. We explicitly investigate this claim using high resolution cosmological simulations of a Milky-Way size halo and find that, similarly to the Cold Dark Matter case, such cross section produces a population of massive subhaloes that is inconsistent with the kinematics of the classical dwarf spheroidals, in particular with the inferred slopes of the mass profiles of Fornax and Sculptor. This problem is resolved if sigma_T/m~1cm^2/g at the dwarf spheroidal scales. Since this value is likely inconsistent with the halo shapes of several clusters, our results leave only a small window open for a velocity-independent Self-Interacting Dark Matter model to work as a distinct alternative to Cold Dark Matter. \\ ( http://arxiv.org/abs/1211.6426 , 380kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6427 Date: Tue, 27 Nov 2012 21:00:00 GMT (82kb) Title: High Frequency Gravitational Waves from Supermassive Black Holes: Prospects for LIGO-Virgo Detections Authors: Bence Kocsis Categories: astro-ph.HE astro-ph.CO Comments: 7 pages, 2 figures, submitted to ApJ, comments welcome \\ It is commonly assumed that ground-based gravitational wave (GW) instruments will not be sensitive to supermassive black holes (SMBHs) because the characteristic GW frequencies are far below the ~ 10 - 1000 Hz sensitivity bands of terrestrial detectors. Here, however, we explore the possibility of SMBH gravitational waves to leak to higher frequencies. In particular, if the high frequency spectral tail asymptotes to h(f) ~ f^(-alpha), where alpha<=2, then the spectral amplitude is a constant or increasing function of the mass M at a fixed frequency f>>c^3/GM. This will happen if the time domain waveform or its derivative exhibits a discontinuity. Ground based instruments could search for these universal spectral tails to detect or rule out such features irrespective of their origin. We identify the following processes which may generate high frequency signals: (i) gravitational bremsstrahlung of ultrarelativistic objects in the vicinity of a SMBH, (ii) ringdown modes excited by an external process that has a high frequency component or terminates abruptly, (iii) gravitational lensing echos and diffraction. More specifically for (iii), SMBHs produce GW echos of inspiraling stellar mass binaries in galactic nuclei with a delay of a few minutes to hours. We estimate the order of magnitude of the detection signal to noise ratio for each mechanism (i, ii, and iii) as a function of the waveform parameters. \\ ( http://arxiv.org/abs/1211.6427 , 82kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6429 Date: Tue, 27 Nov 2012 21:00:01 GMT (938kb,D) Title: An Over-Massive Black Hole in the Compact Lenticular Galaxy NGC1277 Authors: Remco C. E. van den Bosch (1), Karl Gebhardt (2), Kayhan G\"ultekin (3), Glenn van de Ven (1), Arjen van der Wel (1) and Jonelle L. Walsh (2) ((1) MPIA (2) UT (3) UMich) Categories: astro-ph.CO Comments: 7 pages. 6 figures. Nature. Animation at http://www.mpia.de/~bosch/blackholes.html Journal-ref: Nature, 2012, vol 491, issue 7426, pp 729-731 DOI: 10.1038/nature11592 \\ All massive galaxies likely have supermassive black holes at their centers, and the masses of the black holes are known to correlate with properties of the host galaxy bulge component. Several explanations have been proposed for the existence of these locally-established empirical relationships; they include the non-causal, statistical process of galaxy-galaxy merging, direct feedback between the black hole and its host galaxy, or galaxy-galaxy merging and the subsequent violent relaxation and dissipation. The empirical scaling relations are thus important for distinguishing between various theoretical models of galaxy evolution, and they further form the basis for all black hole mass measurements at large distances. In particular, observations have shown that the mass of the black hole is typically 0.1% of the stellar bulge mass of the galaxy. The small galaxy NGC4486B currently has the largest published fraction of its mass in a black hole at 11%. Here we report observations of the stellar kinematics of NGC 1277, which is a compact, disky galaxy with a mass of 1.2 x 10^11 Msun. From the data, we determine that the mass of the central black hole is 1.7 x 10^10 Msun, or 59% its bulge mass. Five other compact galaxies have properties similar to NGC 1277 and therefore may also contain over-sized black holes. It is not yet known if these galaxies represent a tail of a distribution, or if disk-dominated galaxies fail to follow the normal black hole mass scaling relations. \\ ( http://arxiv.org/abs/1211.6429 , 938kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6431 Date: Tue, 27 Nov 2012 21:00:02 GMT (113kb,D) Title: Hints on halo evolution in SFDM models with galaxy observations Authors: Alma X. Gonzalez-Morales, Alberto Diez-Tejedor, L. Arturo Urena-Lopez and Octavio Valenzuela Categories: astro-ph.CO gr-qc Comments: 5 pages, 2 figures, 1 table \\ A massive, self-interacting scalar field has been considered as a possible candidate for the dark matter in the universe. We present an observational constraint to the model arising from strong lensing observations in galaxies. The result points to a discrepancy in the properties of scalar field dark matter halos for dwarf and lens galaxies, mainly because halo parameters are directly related to physical quantities in the model. This is an important indication that it becomes necessary to have a better understanding of halo evolution in scalar field dark matter models, where the presence of baryons can play an important role. \\ ( http://arxiv.org/abs/1211.6431 , 113kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6432 Date: Tue, 27 Nov 2012 21:00:02 GMT (1534kb,D) Title: On the effects of optically thick gas (disks) around massive stars Authors: Rolf Kuiper, Harold W. Yorke Categories: astro-ph.SR Comments: accepted at ApJ \\ Numerical simulations have shown that the often cited radiation pressure barrier to accretion onto massive stars can be circumvented, when the radiation field is highly anisotropic in the presence of a circumstellar accretion disk with high optical depth. Here, these studies of the so-called flashlight effect are expanded by including the opacity of the innermost dust-free but potentially optically thick gas regions around forming massive stars. In addition to frequency-dependent opacities for the dust grains, we use temperature- and density-dependent Planck- and Rosseland mean opacities for the gas. The simulations show that the innermost dust-free parts of the accretion disks are optically thick to the stellar radiation over a substantial fraction of the solid angle above and below the disk's midplane. The temperature in the shielded disk region decreases faster with radius than in a comparison simulation with a lower constant gas opacity, and the dust sublimation front is shifted to smaller radii. The shielding by the dust-free gas in the inner disk thus contributes to an enhanced flashlight effect, which ultimately results in a smaller opening angle of the radiation pressure driven outflow and in a much longer timescale of sustained feeding of the circumstellar disk by the molecular cloud core. We conclude that it is necessary to properly account for the opacity of the inner dust-free disk regions around forming massive stars in order to correctly assess the effectiveness of the flashlight effect, the opening angle of radiation pressure driven outflows, and the lifetime and morphological evolution of the accretion disk. \\ ( http://arxiv.org/abs/1211.6432 , 1534kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6433 Date: Tue, 27 Nov 2012 21:00:03 GMT (4719kb,D) Title: On the Star Formation Efficiency of Turbulent Magnetized Clouds Authors: Christoph Federrath and Ralf S. Klessen Categories: astro-ph.SR astro-ph.CO astro-ph.GA astro-ph.IM physics.data-an Comments: 23 pages, 14 figures, submitted to ApJ, more info at http://www.ita.uni-heidelberg.de/~chfeder/pubs/sfe/sfe.shtml?lang=en \\ We study the star formation efficiency (SFE) in simulations and observations of turbulent, magnetized, molecular clouds. We find that the volumetric and column density probability distributions (PDFs) of our simulations with solenoidal, mixed, and compressive forcing of turbulence, sonic Mach numbers of 3-50, and magnetic fields in the super- to the trans-Alfvenic regime, all develop power-law tails of flattening slope with increasing SFE. The high-density tails of the PDFs are consistent with equivalent radial density profiles, rho ~ r^(-kappa) with kappa ~ 1.5-2.5, in agreement with observations. Studying velocity-size scalings, we find that all the simulations are consistent with the observed v ~ l^(1/2) scaling of supersonic turbulence, and seem to approach Kolmogorov turbulence with v ~ l^(1/3) below the sonic scale. The velocity-size scaling is, however, largely independent of the SFE. In contrast, the density-size and column density-size scalings are highly sensitive to star formation. We find that the power-law slope alpha of the density power spectrum, P(rho,k) ~ k^alpha, or equivalently the Delta-variance spectrum of column density, DV(Sigma,l) ~ l^(-alpha), switches sign from alpha < 0 for SFE ~ 0 to alpha > 0 when star formation proceeds (SFE > 0). We provide a relation to compute the SFE from a measurement of alpha. Studying the literature, we find values ranging from alpha = -1.6 to +1.6 in observations covering scales from the large-scale atomic medium, over cold molecular clouds, down to dense star-forming cores. From those alpha values, we infer SFEs and find good agreement with independent measurements based on young stellar object (YSO) counts, where available. Our SFE-alpha relation provides an independent estimate of the SFE based on the column density map of a cloud alone, without requiring a priori knowledge of star-formation activity or YSO counts. \\ ( http://arxiv.org/abs/1211.6433 , 4719kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6434 Date: Tue, 27 Nov 2012 21:00:03 GMT (478kb) Title: Precision cosmology in muddy waters: Cosmological constraints and N-body codes Authors: Robert E. Smith, Darren S. Reed, Doug Potter, Laura Marian, Martin Crocce, Ben Moore Categories: astro-ph.CO astro-ph.GA Comments: 21 Pages; 20 Figures. Submitted to MNRAS. Comments welcome \\ Future large-scale structure surveys of the Universe will aim to constrain the cosmological model and the true nature of dark energy with unprecedented accuracy. In order for these surveys to achieve their designed goals, they will require predictions for the nonlinear matter power spectrum to sub-percent accuracy. Through the use of a large ensemble of cosmological N-body simulations, we demonstrate that if we do not understand the uncertainties associated with simulating structure formation, i.e. knowledge of the `true' simulation parameters, and simply seek to marginalize over them, then the constraining power of such future surveys can be significantly reduced. However, for the parameters {n_s, h, Om_b, Om_m}, this effect can be largely mitigated by adding the information from a CMB experiment, like Planck. In contrast, for the amplitude of fluctuations sigma8 and the time-evolving equation of state of dark energy {w_0, w_a}, the mitigation is mild. On marginalizing over the simulation parameters, we find that the dark-energy figure of merit can be degraded by ~2. This is likely an optimistic assessment, since we do not take into account other important simulation parameters. A caveat is our assumption that the Hessian of the likelihood function does not vary significantly when moving from our adopted to the 'true' simulation parameter set. This paper therefore provides strong motivation for rigorous convergence testing of N-body codes to meet the future challenges of precision cosmology. \\ ( http://arxiv.org/abs/1211.6434 , 478kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6436 Date: Tue, 27 Nov 2012 21:00:04 GMT (404kb) Title: Widespread and Hidden Active Galactic Nuclei in Star-Forming Galaxies at Redshift > 0.3 Authors: St\'ephanie Juneau, Mark Dickinson, Fr\'ed\'eric Bournaud, David M. Alexander, Emanuele Daddi, James R. Mullaney, Benjamin Magnelli, Jeyhan S. Kartaltepe, Ho Seong Hwang, S. P. Willner, Alison L. Coil, David J. Rosario, Jonathan R. Trump, Benjamin J. Weiner, Christopher N. A. Willmer, Michael C. Cooper, David Elbaz, S. M. Faber, David T. Frayer, Dale D. Kocevski, Elise S. Laird, Jacqueline A. Monkiewicz, Kirpal Nandra, Jeffrey Newman, Samir Salim and Myrto Symeonidis Categories: astro-ph.CO astro-ph.HE Comments: 21 pages, 15 figures. Submitted to the Astrophysical Journal, revised based on referee's comments \\ We characterize the incidence of active galactic nuclei (AGNs) is 0.3 < z < 1 star-forming galaxies by applying multi-wavelength AGN diagnostics (X-ray, optical, mid-infrared, radio) to a sample of galaxies selected at 70-micron from the Far-Infrared Deep Extragalactic Legacy survey (FIDEL). Given the depth of FIDEL, we detect "normal" galaxies on the specific star formation rate (sSFR) sequence as well as starbursting systems with elevated sSFR. We find an overall high occurrence of AGN of 37+/-3%, more than twice as high as in previous studies of galaxies with comparable infrared luminosities and redshifts but in good agreement with the AGN fraction of nearby (0.05 < z < 0.1) galaxies of similar infrared luminosities. The more complete census of AGNs comes from using the recently developed Mass-Excitation (MEx) diagnostic diagram. This optical diagnostic is also sensitive to X-ray weak AGNs and X-ray absorbed AGNs, and reveals that absorbed active nuclei reside almost exclusively in infrared-luminous hosts. The fraction of galaxies hosting an AGN appears to be independent of sSFR and remains elevated both on the sSFR sequence and above. In contrast, the fraction of AGNs that are X-ray absorbed increases substantially with increasing sSFR, possibly due to an increased gas fraction and/or gas density in the host galaxies. \\ ( http://arxiv.org/abs/1211.6436 , 404kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6438 Date: Tue, 27 Nov 2012 21:00:04 GMT (83kb) Title: Constraints on Shallow 56Ni from the Early Lightcurves of Type Ia Supernovae Authors: Anthony L. Piro (Caltech), Ehud Nakar (Tel Aviv University) Categories: astro-ph.HE astro-ph.SR Comments: 9 pages, 9 figures, submitted for publication in The Astrophysical Journal \\ Ongoing transient surveys are presenting an unprecedented account of the rising lightcurves of Type Ia supernovae (SNe Ia). This early emission probes the shallowest layers of the exploding white dwarf, which can provide constraints on the progenitor star and the properties of the explosive burning. We use semi-analytic models of radioactively-powered rising lightcurves to analyze these observations. As we have summarized in previous work, the main limiting factor in determining the surface distribution of 56Ni is the lack of an unambiguously identified time of explosion, as would be provided by detection of shock breakout or shock-heated cooling. Without this the SN may in principle exhibit a "dark phase" for a few hours to days, where the only emission is from shock-heated cooling that is too dim to be detected. Nevertheless, by considering the time-dependent velocity evolution, the explosion time can be better constrained, albeit with considerable uncertainty. This technique is used to infer the surface 56Ni distribution of three recent SNe Ia that were caught especially early in their rise. Although we cannot constrain the explosion times to better than ~1 day, in all three we find fairly similar 56Ni distributions. Observations of SN 2011fe and SN 2012cg probe shallower depths than in SN 2009ig, and in these two cases 56Ni is present merely ~0.01Msun from the WD's surface. We also use our conclusions about the explosion times to reassess radius constraints for the progenitor of SN 2011fe, as well as discuss the roughly t^2 power law that is inferred for many observed rising lightcurves. \\ ( http://arxiv.org/abs/1211.6438 , 83kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6439 Date: Tue, 27 Nov 2012 21:00:20 GMT (840kb) Title: A search for the hidden population of AM CVn binaries in the Sloan Digital Sky Survey Authors: P. J. Carter, T. R. Marsh, D. Steeghs, P. J. Groot, G. Nelemans, D. Levitan, A. Rau, C. M. Copperwheat, T.Kupfer and G. H. A. Roelofs Categories: astro-ph.SR Comments: 19 pages, 14 figures. Accepted for publication in MNRAS \\ We present the latest results from a spectroscopic survey designed to uncover the hidden population of AM Canum Venaticorum (AM CVn) binaries in the photometric database of the Sloan Digital Sky Survey (SDSS). We selected ~2000 candidates based on their photometric colours, a relatively small sample which is expected to contain the majority of all AM CVn binaries in the SDSS (expected to be ~50). We present two new candidate AM CVn binaries discovered using this strategy: SDSS J104325.08+563258.1 and SDSS J173047.59+554518.5. We also present spectra of 29 new cataclysmic variables, 23 DQ white dwarfs and 21 DZ white dwarfs discovered in this survey. The survey is now approximately 70 per cent complete, and the discovery of seven new AM CVn binaries indicates a lower space density than previously predicted. From the essentially complete g <= 19 sample, we derive an observed space density of (5 +/- 3) x10^-7 pc^-3; this is lower than previous estimates by a factor of 3. The sample has been cross-matched with the GALEX All-Sky Imaging Survey database, and with Data Release 9 of the UKIRT (United Kingdom Infrared Telescope) Infrared Deep Sky Survey (UKIDSS). The addition of UV photometry allows new colour cuts to be applied, reducing the size of our sample to ~1100 objects. Optimising our followup should allow us to uncover the remaining AM CVn binaries present in the SDSS, providing the larger homogeneous sample required to more reliably estimate their space density. \\ ( http://arxiv.org/abs/1211.6439 , 840kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6440 Date: Tue, 27 Nov 2012 21:00:24 GMT (175kb) Title: Herschel-ATLAS/GAMA: a difference between star-formation rates in strong-line and weak-line radio galaxies Authors: M. J. Hardcastle, J. H. Y. Ching, J. S. Virdee, M. J. Jarvis, S. M. Croom, E. M. Sadler, T. Mauch, D. J. B. Smith, J. A. Stevens, M. Baes, I. K. Baldry, S. Brough, A. Cooray, A. Dariush, G. De Zotti, S. Driver, L. Dunne, S. Dye, S. Eales, R. Hopwood, J. Liske, S. Maddox, M. J. Michalowski, E. E. Rigby, A. S. G. Robotham, O. Steele, D. Thomas, and E. Valiante Categories: astro-ph.CO Comments: 19 pages, 10 colour figures. Accepted by MNRAS \\ We have constructed a sample of radio-loud objects with optical spectroscopy from the Galaxy and Mass Assembly (GAMA) project over the Herschel-ATLAS Phase 1 fields. Classifying the radio sources in terms of their optical spectra, we find that strong-emission-line sources (`high-excitation radio galaxies') have, on average, a factor ~4 higher 250-micron Herschel luminosity than weak-line (`low-excitation') radio galaxies and are also more luminous than magnitude-matched radio-quiet galaxies at the same redshift. Using all five H-ATLAS bands, we show that this difference in luminosity between the emission-line classes arises mostly from a difference in the average dust temperature; strong-emission-line sources tend to have comparable dust masses to, but higher dust temperatures than, radio galaxies with weak emission lines. We interpret this as showing that radio galaxies with strong nuclear emission lines are much more likely to be associated with star formation in their host galaxy, although there is certainly not a one-to-one relationship between star formation and strong-line AGN activity. The strong-line sources are estimated to have star-formation rates at least a factor 3-4 higher than those in the weak-line objects. Our conclusion is consistent with earlier work, generally carried out using much smaller samples, and reinforces the general picture of high-excitation radio galaxies as being located in lower-mass, less evolved host galaxies than their low-excitation counterparts. \\ ( http://arxiv.org/abs/1211.6440 , 175kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6441 Date: Tue, 27 Nov 2012 21:00:38 GMT (400kb) Title: Dynamics of stellar black holes in young star clusters with different metallicities - I. Implications for X-ray binaries Authors: M. Mapelli, L. Zampieri, E. Ripamonti, A. Bressan Categories: astro-ph.HE astro-ph.SR Comments: 19 pages, 11 figures, 8 tables, MNRAS, accepted \\ We present N-body simulations of intermediate-mass (3000-4000 Msun) young star clusters (SCs) with three different metallicities (Z=0.01, 0.1 and 1 Zsun), including metal-dependent stellar evolution recipes and binary evolution. Following recent theoretical models of wind mass loss and core collapse supernovae, we assume that the mass of the stellar remnants depends on the metallicity of the progenitor stars. In particular, massive metal-poor stars (Z<=0.3 Zsun) are enabled to form massive stellar black holes (MSBHs, with mass >=25 Msun) through direct collapse. We find that three-body encounters, and especially dynamical exchanges, dominate the evolution of the MSBHs formed in our simulations. In SCs with Z=0.01 and 0.1 Zsun, about 75 per cent of simulated MSBHs form from single stars and become members of binaries through dynamical exchanges in the first 100 Myr of the SC life. This is a factor of >~3 more efficient than in the case of low-mass (<25 Msun) stellar black holes. A small but non-negligible fraction of MSBHs power wind-accreting (10-20 per cent) and Roche lobe overflow (RLO, 5-10 per cent) binary systems. The vast majority of MSBH binaries that undergo wind accretion and/or RLO were born from dynamical exchange. This result indicates that MSBHs can power X-ray binaries in low-metallicity young SCs, and is very promising to explain the association of many ultraluminous X-ray sources with low-metallicity and actively star forming environments. \\ ( http://arxiv.org/abs/1211.6441 , 400kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6443 Date: Tue, 27 Nov 2012 21:01:05 GMT (1124kb) Title: X-ray Proper Motions and Shock Speeds along the Northwest Rim of SN 1006 Authors: Satoru Katsuda, Knox S. Long, Robert Petre, Stephen P. Reynolds, Brian J. Williams, and P. Frank Winkler Categories: astro-ph.GA astro-ph.HE Comments: 19 pages, 5 figures \\ We report the results of an X-ray proper motion measurement for the NW rim of SN1006, carried out by comparing Chandra observations from 2001 and 2012. The NW limb has predominantly thermal X-ray emission, and it is the only location in SN1006 with significant optical emission: a thin, Balmer-dominated filament. For most of the NW rim, the proper motion is about 0.30 arcsec/yr, essentially the same as has been measured from the H-alpha filament. Isolated regions of the NW limb are dominated by nonthermal emission, and here the proper motion is much higher, 0.49 arcsec/yr, close to the value measured in X-rays along the much brighter NE limb, where the X-rays are overwhelmingly nonthermal. At the 2.2 kpc distance to SN1006, the proper motions imply shock velocities of about 3000 km/s and 5000 km/s in the thermal and nonthermal regions, respectively. A lower velocity behind the H-alpha filament is consistent with the picture that SN1006 is encountering denser gas in the NW, as is also suggested by its overall morphology. In the thermally-dominated portion of the X-ray shell, we also see an offset in the radial profiles at different energies; the 0.5-0.6 keV peak dominated by O VII is closer to the shock front than that of the 0.8-3 keV emission--due to the longer times for heavier elements to reach ionization states where they produce strong X-ray emission. \\ ( http://arxiv.org/abs/1211.6443 , 1124kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6444 Date: Tue, 27 Nov 2012 21:01:30 GMT (2999kb,D) Title: The CORALIE survey for southern extrasolar planets XVII. New and updated long period and massive planets Authors: M. Marmier, D. S\'egransan, S. Udry, M. Mayor, F. Pepe, D. Queloz, C. Lovis, D. Naef, N. C. Santos, R. Alonso, S. Alves, S. Berthet, B. Chazelas, B.-O. Demory, X. Dumusque, A. Eggenberger, P. Figueira, M. Gillon, J. Hagelberg, M. Lendl, R. A. Mardling, D. M\'egevand, M. Neveu, J. Sahlmann, D. Sosnowska, M. Tewes and A. H. M. J. Triaud Categories: astro-ph.EP Comments: 14 pages, 16 figures \\ Since 1998, a planet-search program around main sequence stars within 50 pc in the southern hemisphere, is carried out with the CORALIE echelle spectrograph at La Silla Observatory. With an observing time span of more than 14 years, the CORALIE survey is now able to unveil Jovian planets on Jupiter's period domain. This growing period-interval coverage is important regarding to formation and migration models since observational constraints are still weak for periods beyond the ice line. Long-term precise Doppler measurements with the CORALIE echelle spectrograph, together with a few additional observations made with the HARPS spectrograph on the ESO 3.6m telescope, reveal radial velocity signatures of massive planetary companions in long period orbits. In this paper we present seven new planets orbiting HD27631, HD98649, HD106515A, HD166724, HD196067, HD219077, and HD220689 together with the CORALIE orbital parameters for three already known planets around HD10647, HD30562, and HD86226. The period range of the new planetary companions goes from 2200 to 5500 days and covers a mass domain between 1 and 10.5 MJup. Surprisingly, five of them present quite high eccentricities above e>0.57. A pumping scenario by Kozai mechanism may be invoked for HD106515Ab and HD196067b which are both orbiting stars in multiple systems. As the presence of a third massive body can't be inferred from the data of HD98649b, HD166724b, and HD219077b, the origin of the eccentricity of these systems remains unknown. Except for HD10647b, no constraint on the upper mass of the planets is provided by Hipparcos astrometric data. Finally it is interesting to note that the hosts of these long period planets show no metallicity excess. \\ ( http://arxiv.org/abs/1211.6444 , 2999kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6449 Date: Tue, 27 Nov 2012 21:05:22 GMT (788kb,D) Title: Missing Lensed Images and the Galaxy Disk Mass in CXOCY J220132.8-320144 Authors: Jacqueline Chen (MIT), Samuel K. Lee (Princeton), Francisco-Javier Castander (ICE/CSIC), Jos\'e Maza (U Chile), and Paul L. Schechter (MIT) Categories: astro-ph.CO Comments: 9 pages, 8 figures, 6 tables. Submitted to ApJ \\ The CXOCY J220132.8-320144 system consists of an edge-on spiral galaxy lensing a background quasar into two bright images. Previous efforts to constrain the mass distribution in the galaxy have suggested that at least one additional image must be present (Castander et al. 2006). These extra images may be hidden behind the disk which features a prominent dust lane. We present and analyze Hubble Space Telescope (HST) observations of the system. We do not detect any extra images, but the observations further narrow the observable parameters of the lens system. We explore a range of models to describe the mass distribution in the system and find that a variety of acceptable model fits exist. All plausible models require 2 magnitudes of dust extinction in order to obscure extra images from detection, and some models may require an offset between the center of the galaxy and the center of the dark matter halo of 1 kiloparsec. Currently unobserved images will be detectable by future James Webb Space Telescope (JWST) observations and will provide strict constraints on the fraction of mass in the disk. \\ ( http://arxiv.org/abs/1211.6449 , 788kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6450 Date: Tue, 27 Nov 2012 21:09:09 GMT (4340kb) Title: Exploring the Cosmic Reionization Epoch in Frequency Space: An Improved Approach to Remove the Foreground in 21 cm Tomography Authors: Jingying Wang, Haiguang Xu, Tao An, Junhua Gu, Xueying Guo, Weitian Li, Yu Wang, Chengze Liu, Olivier Martineau-Huynh, and Xiang-Ping Wu Categories: astro-ph.CO astro-ph.IM Comments: 33 pages, 14 figures. Accepted for publication in ApJ \\ Aiming to correctly restore the redshifted 21 cm signals emitted by the neutral hydrogen during the cosmic reionization processes, we re-examine the separation approaches based on the quadratic polynomial fitting technique in frequency space to investigate whether they works satisfactorily with complex foreground, by quantitatively evaluate the quality of restored 21 cm signals in terms of sample statistics. We construct the foreground model to characterize both spatial and spectral substructures of the real sky, and use it to simulate the observed radio spectra. By comparing between different separation approaches through statistical analysis of restored 21 cm spectra and corresponding power spectra, as well as their constraints on the mean halo bias $b$ and average ionization fraction $x_e$ of the reionization processes, at $z=8$ and the noise level of 60 mK we find that, although the complex foreground can be well approximated with quadratic polynomial expansion, a significant part of Mpc-scale components of the 21 cm signals (75% for $\gtrsim 6h^{-1}$ Mpc scales and 34% for $\gtrsim 1h^{-1}$ Mpc scales) is lost because it tends to be mis-identified as part of the foreground when single-narrow-segment separation approach is applied. The best restoration of the 21 cm signals and the tightest determination of $b$ and $x_e$ can be obtained with the three-narrow-segment fitting technique as proposed in this paper. Similar results can be obtained at other redshifts. \\ ( http://arxiv.org/abs/1211.6450 , 4340kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6455 Date: Tue, 27 Nov 2012 21:27:10 GMT (6089kb) Title: Radio Astronomy Transformed: Aperture Arrays - Past, Present & Future Authors: Michael A. Garrett (ASTRON, Univ. of Leiden) Categories: astro-ph.IM Comments: 9 pages, Paper presented at "From Antikythera to the Square Kilometre Array: Lessons from the Ancients, Kerastari, Greece 12-15 June 2012" eds. A.K. Tzioumis et al; Proceedings of Science, 2012, http://pos.sissa.it/cgi-bin/reader/conf.cgi?confid=170 \\ I review the early development of Aperture Arrays and their role in radio astronomy. The demise of this technology at the end of the 1960's, and the reasons for the rise of parabolic dishes is also considered. The parallels with the Antikythera mechanism (see these proceedings) as a lost technology are briefly presented. Aperture Arrays re-entered the world of radio astronomy as the idea to build a huge radio telescope with a collecting area of one square kilometre (the Square Kilometre Array, SKA) arose. Huge ICT technology advances had transformed Aperture Arrays in terms of their capability, flexibility and reliability. In the mid-1990s, ASTRON started to develop and experiment with the first high frequency aperture array tiles for radio astronomy - AAD, OSMA, THEA & EMBRACE. In the slipstream of these efforts, Phased Array Feeds (PAFs) for radio astronomy were invented and LOFAR itself emerged as a next generation telescope and a major pathfinder for the SKA. Meanwhile, the same advantages that aperture arrays offered to radio astronomy had already made dishes obsolete in many different civilian and military applications. The first commissioning results from LOFAR and other Aperture Arrays (MWA, LWA and PAPER) currently demonstrate that this kind of technology can transform radio astronomy over 2 decades of the radio spectrum, and at frequencies up to at least 1.5 GHz. This "reinvention of radio astronomy" has important implications for the design and form of the full SKA. Building a SKA that is simply the "VLA on steroids" is simply not good enough. Like the Antikythera mechanism itself, we must amaze future generations of astronomers - they and the current generation deserve nothing less. \\ ( http://arxiv.org/abs/1211.6455 , 6089kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6457 Date: Tue, 27 Nov 2012 21:30:47 GMT (218kb) Title: Search for gamma-ray emission from four accreting millisecond pulsars with Fermi/LAT Authors: Yi Xing and Zhongxiang Wang Categories: astro-ph.HE Comments: 8 pages, 2 figures, 2 tables, submitted to ApJ \\ We report our search for \gamma-ray emission in the energy range from 100 MeV to 300 GeV from four Accreting Millisecond Pulsars (AMPs), SAX J1808.4-3658, IGR J00291+5934, XTE J1814-338, and XTE J0929-314. The data are from four-year observations carried out by Large Area Telescope (LAT) onboard the Fermi \gamma-ray Space Telescope. The AMPs were not detected, and their \gamma-ray luminosity upper limits we obtain are 5.1*10^33 ergs/s for SAX J1808.4-3658, 2.1*10^33 ergs/s for IGR J00291+5934, 1.2*10^34 ergs/s for XTE J1814-338, and 2.2*10^33 ergs/s for XTE J0929-314. We compare our results with \gamma-ray irradiation luminosities required for producing optical modulations seen from the companions in the AMPs, which has been suggested by Takata et al. (2012), and our upper limits have excluded \gamma-ray emission as the heating source in these systems except XTE J0929-314, the upper limit of which is not deep enough. Our results also do not support the model proposed by Takata et al. (2012) that relatively strong \gamma-ray emission could arise from the outer gap of a high-mass neutron star controlled by the photon-photon pair-creation for the AMPs. Two AMPs, SAX J1808.4-3658 and IGR J00291+5934, have the measurements of their spin-down rates, and we derive the upper limits of their \gamma-ray conversion efficiencies, which are 57% and 3%, respectively. We discuss the implications to the AMP systems by comparing the efficiency upper limit values with that of 20 \gamma-ray millisecond pulsars (MSP) detected by Fermi and the newly discovered transitional MSP binary J1023+0038. \\ ( http://arxiv.org/abs/1211.6457 , 218kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6467 Date: Tue, 27 Nov 2012 22:27:07 GMT (933kb) Title: Habitable Planets Around White and Brown Dwarfs: The Perils of a Cooling Primary Authors: Rory Barnes and Rene Heller Categories: astro-ph.EP Comments: 28 pages, 7 figures, accepted to Astrobiology. A version with full resolution images is available at http://www.astro.washington.edu/users/rory/publications/bh12.pdf \\ White and brown dwarfs are astrophysical objects that are bright enough to support an insolation habitable zone (IHZ). Unlike hydrogen-burning stars, they cool and become less luminous with time, and hence their IHZ moves in with time. The inner edge of the IHZ is defined as the orbital radius at which a planet may enter a moist or runaway greenhouse, phenomena that can remove a planet's surface water forever. Thus, as the IHZ moves in, planets that enter it may no longer have any water, and are still uninhabitable. Additionally, the close proximity of the IHZ to the primary leads to concern that tidal heating may also be strong enough to trigger a runaway greenhouse, even for orbital eccentricities as small as 10^-6. Water loss occurs due to photolyzation by UV photons in the planetary stratosphere, followed by hydrogen escape. Young white dwarfs emit a large amount of these photons as their surface temperatures are over 10^4 K. The situation is less clear for brown dwarfs, as observational data do not constrain their early activity and UV emission very well. Nonetheless, both types of planets are at risk of never achieving habitable conditions, but planets orbiting white dwarfs may be less likely to sustain life than those orbiting brown dwarfs. We consider the future habitability of the planet candidates KOI 55.01 and 55.02 in these terms and find they are unlikely to become habitable. \\ ( http://arxiv.org/abs/1211.6467 , 933kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6470 Date: Tue, 27 Nov 2012 22:44:02 GMT (1926kb) Title: A new class of SETI beacons that contain information (22-aug-2010) Authors: G. R. Harp, R. F. Ackermann, Samantha K. Blair, J. Arbunich, P. R. Backus, J. C. Tarter, and the ATA Team Categories: astro-ph.IM cs.OH Comments: 33 pages, 8 figures, 1 table \\ In the cm-wavelength range, an extraterrestrial electromagnetic narrow band (sine wave) beacon is an excellent choice to get alien attention across interstellar distances because 1) it is not strongly affected by interstellar / interplanetary dispersion or scattering, and 2) searching for narrowband signals is computationally efficient (scales as Ns log(Ns) where Ns = number of voltage samples). Here we consider a special case wideband signal where two or more delayed copies of the same signal are transmitted over the same frequency and bandwidth, with the result that ISM dispersion and scattering cancel out during the detection stage. Such a signal is both a good beacon (easy to find) and carries arbitrarily large information rate (limited only by the atmospheric transparency to about 10 GHz). The discovery process uses an autocorrelation algorithm, and we outline a compute scheme where the beacon discovery search can be accomplished with only 2x the processing of a conventional sine wave search, and discuss signal to background response for sighting the beacon. Once the beacon is discovered, the focus turns to information extraction. Information extraction requires similar processing as for generic wideband signal searches, but since we have already identified the beacon, the efficiency of information extraction is negligible. \\ ( http://arxiv.org/abs/1211.6470 , 1926kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6475 Date: Tue, 27 Nov 2012 23:21:22 GMT (993kb) Title: Changes Of Dust Opacity With Density in the Orion A Molecular Cloud Authors: Arabindo Roy, Peter G. Martin, Danae Polychroni, Sylvain Bontemps, Alain Abergel, Philippe Andre, Doris Arzoumanian, James Di Francesco, Tracey Hill, Vera Konyves, Quang Nguyen-Luong, Stefano Pezzuto, Nicola Schneider, Leonardo Testi, and Glenn White Categories: astro-ph.GA Comments: 13 pages, 11 Figures, To appear in the Astrophysical Journal \\ We have studied the opacity of dust grains at submillimeter wavelengths by estimating the optical depth from imaging at 160, 250, 350, and 500 um from the Herschel Gould Belt Survey and comparing this to a column density obtained from the 2MASS-derived color excess E(J-Ks). Our main goal was to investigate the spatial variations of the opacity due to "big" grains over a variety of environmental conditions and thereby quantify how emission properties of the dust change with column (and volume) density. The central and southern areas of the Orion A molecular cloud examined here, with NH ranging from 1.5X10^21 cm^-2 to 50X10^21 cm^-2, are well suited to this approach. We fit the multi-frequency Herschel spectral energy distributions (SEDs) of each pixel with a modified blackbody to obtain the temperature, T, and optical depth, \tau(1200), at a fiducial frequency of 1200 GHz (250 um). Using a calibration of NH/E(J-Ks)for the interstellar medium (ISM) we obtained the opacity (dust emission cross-section per H nucleon), \sigma_e(1200), for every pixel. From a value of ~ 1X10^-25 cm^2 H^-1 at the lowest column densities that is typical of the high latitude diffuse ISM, \sigma_e(1200) increases as NH^0.28 over the range studied. This is suggestive of grain evolution. Integrating the SEDs over frequency, we also calculated the specific power P (emission power per H) for the big grains. In low column density regions where dust clouds are optically thin to the interstellar radiation field (ISRF), P is typically 3.7 X 10^-31 W H^-1, again close to that in the high latitude diffuse ISM. However, we find evidence for a decrease of P in high column density regions, which would be a natural outcome of attenuation of the ISRF that heats the grains, and for localized increases for dust illuminated by nearby stars or embedded protostars. \\ ( http://arxiv.org/abs/1211.6475 , 993kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6478 Date: Tue, 27 Nov 2012 23:35:30 GMT (27kb) Title: A conceptual problem for non-commutative inflation and the new approach for non-relativistic inflationary equation of state Authors: U. D. Machado and R. Opher Categories: astro-ph.CO gr-qc hep-th \\ In a previous paper, we connected the phenomenological non-commutative inflation of Alexander, Brandenberger and Magueijo (2003, 2005 and 2007) with the formal representation theory of groups and algebras. In that paper, the fundamental equations of inflation followed as a consequence of a deformation of the Poincar\'e group, which induces a particular quantum representation. In this paper, we show that there exists a conceptual problem with the kind of representation that leads to the fundamental equations of the model and that the procedure to obtain those equations should be modified according to one of two possible proposals. One of them relates to the general theory of Hopf algebras. The other is based on a representation theorem of Von Neumann algebras, a proposal already suggested by us to take into account interactions in the inflationary equation of state. This reopens the problem of finding inflationary deformed dispersion relations and all developments which followed the first paper of Non-commutative Inflation. \\ ( http://arxiv.org/abs/1211.6478 , 27kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6481 Date: Tue, 27 Nov 2012 23:56:00 GMT (55kb) Title: Parameters of Recent Transits of HAT-P-23b Authors: Felipe G. Ram\'on-Fox and Pedro V. Sada Categories: astro-ph.EP Comments: 11 pages, 2 figures, 2 tables - Accepted for publication at the Revista Mexicana de Astronom\'ia y Astrof\'isica \\ Four transits of the exoplanet HAT-P-23b were recently observed with the 0.36m telescope at the Universidad de Monterrey Observatory. The four light curves were successfully combined to obtain a resulting one with reduced scattering per bin. This one was modeled using a Monte Carlo method to obtain the essential parameters that characterize the system. Assuming orbital parameters such as eccentricity, e, and longitude of periastron, w, from the discovery paper, we found values of Rp/R* = 0.1105 +0.0015-0.0013 for the planet-to-star radius ratio, a/R* = 4.23 +0.06-0.12 for the scaled semimajor axis, and an orbital inclination of the system of i = 87.9d +1.5-2.2. We also derive an improved orbital period of 1.2128868 +- 0.0000004 days (To = 2,454,852.26542 +- 0.00018 BJD_TDB) for the system. \\ ( http://arxiv.org/abs/1211.6481 , 55kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6482 Date: Tue, 27 Nov 2012 23:56:36 GMT (1518kb,D) Title: Superionic to superionic phase change in water: consequences for the interiors of Uranus and Neptune Authors: Hugh F. Wilson, Michael L. Wong, Burkhard Militzer Categories: astro-ph.EP cond-mat.mtrl-sci \\ Using density functional molecular dynamics free energy calculations, we show that the body-centered-cubic phase of superionic ice previously believed to be the only phase is in fact thermodynamically unstable compared to a novel phase with oxygen positions in fcc lattice sites. The novel phase has a lower proton mobility than the bc phase and may exhibit a higher melting temperature. We predict a transition between the two phases at a pressure of 1 +/- 0.5 Mbar, with potential consequences for the interiors of ice giants such as Uranus and Neptune. \\ ( http://arxiv.org/abs/1211.6482 , 1518kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6485 Date: Wed, 28 Nov 2012 00:14:30 GMT (285kb) Title: BoA: a versatile software for bolometer data reduction Authors: F. Schuller Categories: astro-ph.IM Comments: 10 pages, 4 figures Journal-ref: Proc. SPIE, 8452, 84521T (2012) DOI: 10.1117/12.926696 \\ Together with the development of the Large APEX Bolometer Camera (LABOCA) for the Atacama Pathfinder Experiment (APEX), a new data reduction package has been written. This software naturally interfaces with the telescope control system, and provides all functionalities for the reduction, analysis and visualization of bolometer data. It is used at APEX for real time processing of observations performed with LABOCA and other bolometer arrays, providing feedback to the observer. Written in an easy-to-script language, BoA is also used offline to reduce APEX continuum data. In this paper, the general structure of this software is presented, and its online and offline capabilities are described. \\ ( http://arxiv.org/abs/1211.6485 , 285kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6487 Date: Wed, 28 Nov 2012 00:28:47 GMT (1624kb) Title: Effects of Kerr Strong Gravity on Quasar X-ray Microlensing Authors: Bin Chen, Xinyu Dai, Eddie Baron, Ronald Kantowski Categories: astro-ph.HE astro-ph.CO astro-ph.GA gr-qc Comments: 26 pages, 7 figures, ApJ submitted \\ Recent quasar microlensing observations have constrained the sizes of X-ray emission regions to be within about 10 gravitational radii of the central supermassive black hole. Therefore, the X-ray emission from lensed quasars is first strongly lensed by the black hole before it is lensed by the foreground galaxy and star fields. We present a scheme that combines the initial strong lensing of a Kerr black hole with standard linearized microlensing by intervening stars. We find that X-ray microlensed light curves incorporating Kerr strong gravity can differ significantly from standard curves. The amplitude of the fluctuations in the light curves can increase or decrease by ~0.65-0.75 mag by including Kerr strong gravity. Larger inclination angles give larger amplitude fluctuations in the microlensing light curves. Consequently, current X-ray microlensing observations might have under or overestimated the sizes of the X-ray emission regions. We estimate this bias using a simple metric based on the amplitude of magnitude fluctuations. The half light radius of the X-ray emission region can be underestimated up to ~50% or overestimated up to ~20%. Underestimates are found in most situations we have investigated. The only exception is for a disk with large spin, radially flat emission profile, and observed nearly face on, where an overestimate is found. Thus, more accurate microlensing size constraints should be obtainable by including Kerr lensing. The caustic crossing time can differ by months after including Kerr strong gravity. A simultaneous monitoring of gravitational lensed quasars in both X-ray and optical bands with densely sampled X-ray light curves might reveal this feature. We conclude that it should be possible to constrain important parameters such as inclination angles and black hole spins from combined Kerr and microlensing effects. \\ ( http://arxiv.org/abs/1211.6487 , 1624kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6492 Date: Wed, 28 Nov 2012 00:56:36 GMT (253kb) Title: The Galactic Census of High- and Medium-mass Protostars. II. Luminosities and Evolutionary States of a Complete Sample of Dense Gas Clumps Authors: Bo Ma (1), Jonathan C. Tan (1,2) and Peter J. Barnes (1) ((1) Dept. of Astronomy, University of Florida, (2) Dept. of Physics, University of Florida) Categories: astro-ph.GA astro-ph.CO Comments: 25 pages, 11 figures. Submitted to ApJ. Comments welcome \\ (Abridged) The Census of High- and Medium-mass Protostars (CHaMP) is the first large-scale (280 degree 10^4$ clusters), shows an opposite result: the mean temperature rises to about 10 uK. The unexpected qualitative scenario implies that the main foreground effect of most clusters is NOT always the expected SZ effect. This is maybe the reason why the SZ signal detection result is lower than what is expected by the model. \\ ( http://arxiv.org/abs/1211.6515 , 21kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6524 Date: Wed, 28 Nov 2012 05:45:14 GMT (5297kb,D) Title: The Driver of Coronal Mass Ejections in the Low Corona: A Flux Rope Authors: X. Cheng, J. Zhang, D. M. Ding, Y. Liu and W. Poomvises Categories: astro-ph.SR physics.plasm-ph physics.space-ph Comments: 18 pages, 12 figures, 1 table, accepted for publication in ApJ \\ Recent Solar Dynamic Observatory observations reveal that coronal mass ejections (CMEs) consist of a multi-temperature structure: a hot flux rope and a cool leading front (LF). The flux rope first appears as a twisted hot channel in the Atmospheric Imaging Assembly 94 A and 131 A passbands. The twisted hot channel initially lies along the polarity inversion line and then rises and develops into the semi-circular flux rope-like structure during the impulsive acceleration phase of CMEs. In the meantime, the rising hot channel compresses the surrounding magnetic field and plasma, which successively stack into the CME LF. In this paper, we study in detail two well-observed CMEs occurred on 2011 March 7 and 2011 March 8, respectively. Each of them is associated with an M-class flare. Through a kinematic analysis we find that: (1) the hot channel rises earlier than the first appearance of the CME LF and the onset of the associated flare; (2) the speed of the hot channel is always faster than that of the LF, at least in the field of view of AIA. Thus, the hot channel acts as a continuous driver of the CME formation and eruption in the early acceleration phase. Subsequently, the two CMEs in white-light images can be well reproduced by the graduated cylindrical shell flux rope model. These results suggest that the pre-existing flux rope plays a key role in CME initiation and formation. \\ ( http://arxiv.org/abs/1211.6524 , 5297kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6527 Date: Wed, 28 Nov 2012 06:27:46 GMT (1484kb) Title: Comparative study between N-body and Fokker-Planck simulations for rotating star clusters - II. 2-component models Authors: Jongsuk Hong, Eunhyeuk Kim, Hyung Mok Lee and Rainer Spurzem Categories: astro-ph.SR Comments: 14 pages 21 figures 5 tables \\ To understand the effects of the initial rotation on the evolution of the tidally limited clusters with mass spectrum, we have performed N-body simulations of the clusters with different initial rotations and compared the results with those of the Fokker-Planck (FP) simulations. We confirmed that the cluster evolution is accelerated by not only the initial rotation but also the mass spectrum. For the slowly rotating models, the time evolutions of mass, energy and angular momentum show good agreements between N-body and FP simulations. On the other hand, for the rapidly rotating models, there are significant differences between these two approaches at the early stage of the evolutions because of the development of bar instability in N-body simulations. The shape of the cluster for N-body simulations becomes tri-axial or even prolate, which cannot be produced by the 2-dimensional FP simulations. The total angular momentum and the total mass of the cluster decrease rapidly while bar-like structure persists. After the rotational energy becomes smaller than the critical value for the bar instability, the shape of the cluster becomes nearly axisymmetric again, and follows the evolutionary track predicted by the FP equation. We have confirmed again that the energy equipartiton is not completely achieved when M2/M1(m2>/m1)^(3/2) > 0.16. By examining the angular momentum at each mass component, we found that the exchange of angular momentum between different mass components occurs, similar to the energy exchange leading to the equipartition. \\ ( http://arxiv.org/abs/1211.6527 , 1484kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6528 Date: Wed, 28 Nov 2012 06:28:27 GMT (1052kb) Title: An Independent Measurement of the Incidence of MgII Absorbers along Gamma-Ray Burst Sightlines: the End of the Mystery? Authors: A. Cucchiara, J. X. Prochaska, G. Zhu, B. M\'enard, J. P. U. Fynbo, D. B. Fox, H.-W. Chen, K. L. Cooksey, S. B. Cenko, D. Perley, J. S. Bloom, E. Berger, N. R. Tanvir, V. D'Elia, S. Vergani, S. Lopez, R. Chornock, Thomas deJaeger Categories: astro-ph.CO Comments: 42 pages, 22 figures, submitted to ApJ \\ In 2006, Prochter et al. reported a statistically significant enhancement of very strong Mg II absorption systems intervening the sightlines to gamma-ray bursts (GRBs) relative to the in- cidence of such absorption along quasar sightlines. This counterintuitive result, has inspired a diverse set of astrophysical explanations (e.g. dust, gravitational lensing) but none of these has obviously resolved the puzzle. Using the largest set of GRB afterglow spectra available, we reexamine the purported enhancement. In an independent sample of GRB spectra with a survey path 3 times larger than Prochter et al., we measure the incidence per unit redshift of $\geq 1$\AA rest-frame equivalent width Mg II absorbers at $z \approx 1$ to be l(z)= 0.18 $\pm$ 0.06. This is fully consistent with current estimates for the incidence of such absorbers along quasar sightlines. Therefore, we do not confirm the original enhancement and suggest those results suffered from a statistical fluke. Signatures of the original result do remain in our full sample (l(z) shows an $\approx 1.5$ enhancement over l(z)QSO), but the statistical significance now lies at $\approx 90%$ c.l. Restricting our analysis to the subset of high-resolution spectra of GRB afterglows (which overlaps substantially with Prochter et al.), we still reproduce a statistically significant enhancement of Mg II absorption. The reason for this excess, if real, is still unclear since there is no connection between the rapid afterglow follow-up process with echelle (or echellette) spectrographs and the detectability of strong Mg II doublets. Only a larger sample of such high-resolution data will shed some light on this matter. \\ ( http://arxiv.org/abs/1211.6528 , 1052kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6532 Date: Wed, 28 Nov 2012 07:39:51 GMT (2260kb) Title: ACCESS - V. Dissecting ram-pressure stripping through integral-field spectroscopy and multi-band imaging Authors: P. Merluzzi, G. Busarello, M. A. Dopita, C. P. Haines, D. Steinhauser, A. Mercurio, A. Rifatto, R. J. Smith, S. Schindler Categories: astro-ph.CO Comments: 46 pages, 21 figures, accepted for publication; MNRAS 2012 \\ We study the case of a bright (L>L*) barred spiral galaxy from the rich cluster A3558 in the Shapley supercluster core (z=0.05) undergoing ram-pressure stripping. Integral-field spectroscopy, complemented by multi-band imaging, allows us to reveal the impact of ram pressure on the interstellar medium. We study in detail the kinematics and the physical conditions of the ionized gas and the properties of the stellar populations. We observe one-sided extraplanar ionized gas along the full extent of the galaxy disc. Narrow-band Halpha imaging resolves this outflow into a complex of knots and filaments. The gas velocity field is complex with the extraplanar gas showing signature of rotation. In all parts of the galaxy, we find a significant contribution from shock excitation, as well as emission powered by star formation. Shock-ionized gas is associated with the turbulent gas outflow and highly attenuated by dust. All these findings cover the whole phenomenology of early-stage ram-pressure stripping. Intense, highly obscured star formation is taking place in the nucleus, probably related to the bar, and in a region 12 kpc South-West from the centre. In the SW region we identify a starburst characterized by a 5x increase in the star-formation rate over the last ~100 Myr, possibly related to the compression of the interstellar gas by the ram pressure. The scenario suggested by the observations is supported and refined by ad hoc N-body/hydrodynamical simulations which identify a rather narrow temporal range for the onset of ram-pressure stripping around t~60 Myr ago, and an angle between the galaxy rotation axis and the intra-cluster medium wind of ~45 deg. Taking into account that the galaxy is found ~1 Mpc from the cluster centre in a relatively low-density region, this study shows that ram-pressure stripping still acts efficiently on massive galaxies well outside the cluster cores. \\ ( http://arxiv.org/abs/1211.6532 , 2260kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6545 Date: Wed, 28 Nov 2012 08:57:58 GMT (3606kb,D) Title: The Sun's Global Photospheric and Coronal Magnetic Fields: Observations and Models Authors: D. H. Mackay, A. R. Yeates Categories: astro-ph.SR Comments: 61 pages, 18 figures. Published version available via http://www.livingreviews.org/lrsp-2012-6 Journal-ref: Living Rev. Solar Phys., 9 (2012) 6 \\ In this review, our present day understanding of the Sun's global photospheric and coronal magnetic fields is discussed from both observational and theoretical viewpoints. Firstly, the large-scale properties of photospheric magnetic fields are described, along with recent advances in photospheric magnetic flux transport models. Following this, the wide variety of theoretical models used to simulate global coronal magnetic fields are described. From this, the combined application of both magnetic flux transport simulations and coronal modeling techniques to describe the phenomena of coronal holes, the Sun's open magnetic flux and the hemispheric pattern of solar filaments is discussed. Finally, recent advances in non-eruptive global MHD models are described. While the review focuses mainly on solar magnetic fields, recent advances in measuring and modeling stellar magnetic fields are described where appropriate. In the final section key areas of future research are identified. \\ ( http://arxiv.org/abs/1211.6545 , 3606kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6550 Date: Wed, 28 Nov 2012 09:16:28 GMT (1378kb) Title: A study of the performance of the transit detection tool DST in space-based surveys. Application of the CoRoT pipeline to Kepler data Authors: J. Cabrera, Sz. Csizmadia, A. Erikson, H. Rauer, S. Kirste Categories: astro-ph.EP Comments: 18 pages, 23 figures, published in A&A Journal-ref: Astronomy & Astrophysics, 2012, Volume 548, id.A44, 16 pp DOI: 10.1051/0004-6361/201219337 \\ Context. Transit detection algorithms are mathematical tools used for detecting planets in the photometric data of transit surveys. In this work we study their application to space-based surveys. Aims: Space missions are exploring the parameter space of the transit surveys where classical algorithms do not perform optimally, either because of the challenging signal-to-noise ratio of the signal or its non-periodic characteristics. We have developed an algorithm addressing these challenges for the mission CoRoT. Here we extend the application to the data from the space mission Kepler. We aim at understanding the performances of algorithms in different data sets. Methods: We built a simple analytical model of the transit signal and developed a strategy for the search that improves the detection performance for transiting planets. We analyzed Kepler data with a set of stellar activity filtering and transit detection tools from the CoRoT community that are designed for the search of transiting planets. Results: We present a new algorithm and its performances compared to one of the most widely used techniques in the literature using CoRoT data. Additionally, we analyzed Kepler data corresponding to quarter Q1 and compare our results with the most recent list of planetary candidates from the Kepler survey. We found candidates that went unnoticed by the Kepler team when analyzing longer data sets. We study the impact of instrumental features on the production of false alarms and false positives. These results show that the analysis of space mission data advocates the use of complementary detrending and transit detection tools also for future space-based transit surveys such as PLATO. \\ ( http://arxiv.org/abs/1211.6550 , 1378kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6556 Date: Wed, 28 Nov 2012 09:54:14 GMT (1757kb,D) Title: The mid-infrared extinction law in the darkest cores of the Pipe Nebula Authors: J. Ascenso, C. J. Lada, J. Alves, C. G. Rom\'an-Z\'u\~niga, and M. Lombardi Categories: astro-ph.GA Comments: 8 pages, 6 figures. Accepted to A&A \\ Context. The properties of dust grains, in particular their size distribution, are expected to differ from the interstellar medium to the high-density regions within molecular clouds. Aims. We measure the mid-infrared extinction law produced by dense material in molecular cloud cores. Since the extinction at these wavelengths is caused by dust, the extinction law in cores should depart from that found in low-density environments if the dust grains have different properties. Methods. We use the unbiased LINES method to measure the slope of the reddening vectors in color-color diagrams. We derive the mid-infrared extinction law toward the dense cores B59 and FeSt 1-457 in the Pipe Nebula over a range of visual extinction between 10 and 50 magnitudes, using a combination of Spitzer/IRAC, and ESO NTT/VLT data. Results. The mid-infrared extinction law in both cores departs significantly from a power-law between 3.6 and 8 micron, suggesting that these cores contain dust with a considerable fraction of large dust grains. We find no evidence for a dependence of the extinction law with column density up to 50 magnitudes of visual extinction in these cores, and no evidence for a variation between our result and those for other clouds at lower column densities reported elsewhere in the literature. This suggests that either large grains are present even in low column density regions, or that the existing dust models need to be revised at mid-infrared wavelengths. We find a small but significant difference in the extinction law of the two cores, that we tentatively associate with the onset of star formation in B59. \\ ( http://arxiv.org/abs/1211.6556 , 1757kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6569 Date: Wed, 28 Nov 2012 10:31:45 GMT (5869kb) Title: A solar tornado triggered by flares? Authors: N. K. Panesar, D. E. Innes, S. K. Tiwari, and B. C. Low Categories: astro-ph.SR Comments: 7 pages, 8 Figures, accepted for publication in A&A, Movies can be found at http://www.mps.mpg.de/data/outgoing/panesar/tornado/ \\ Solar tornados are dynamical, conspicuously helical magnetic structures mainly observed as a prominence activity. We investigate and propose a triggering mechanism for the solar tornado observed in a prominence cavity by SDO/AIA on September 25, 2011. High-cadence EUV images from the SDO/AIA and the Ahead spacecraft of STEREO/EUVI are used to correlate three flares in the neighbouring active-region (NOAA 11303), and their EUV waves, with the dynamical developments of the tornado. The timings of the flares and EUV waves observed on-disk in 195\AA\ are analyzed in relation to the tornado activities observed at the limb in 171\AA. Each of the three flares and its related EUV wave occurred within 10 hours of the onset of the tornado. They have an observed causal relationship with the commencement of activity in the prominence where the tornado develops. Tornado-like rotations along the side of the prominence start after the second flare. The prominence cavity expands with acceleration of tornado motion after the third flare. Flares in the neighbouring active region may have affected the cavity prominence system and triggered the solar tornado. A plausible mechanism is that the active-region coronal field contracted by the `Hudson effect' due to the loss of magnetic energy as flares. Subsequently the cavity expanded by its magnetic pressure to fill the surrounding low corona. We suggest that the tornado is the dynamical response of the helical prominence field to the cavity expansion. \\ ( http://arxiv.org/abs/1211.6569 , 5869kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6574 Date: Wed, 28 Nov 2012 10:56:02 GMT (394kb) Title: On the surface structure of sunspots Authors: Morten Franz Categories: astro-ph.SR Comments: 5 Pages, 2 Figures, 3 Movies To appear in Astronomical Notes Vol 333, Issue 10, pp.1009-1012 DOI: 10.1002/asna.201211789 \\ A precise knowledge of the surface structure of sunspots is essential to construct adequate input models for helioseismic inversion tools. We summarize our recent findings about the velocity and magnetic field in and around sunspots using HINODE observation. To this end we quantize the horizontal and vertical component of the penumbral velocity field at different levels of precision and study the moat flow around sunspot. Furthermore, we find that a significant amount of the penumbral magnetic fields return below the surface within the penumbra. Finally, we explain why the related opposite polarity signals remain hidden in magnetograms constructed from measurements with limited spectral resolution. \\ ( http://arxiv.org/abs/1211.6574 , 394kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6586 Date: Wed, 28 Nov 2012 11:57:55 GMT (1517kb) Title: Supernovae and Cosmology with Future European Facilities Authors: I. M. Hook Categories: astro-ph.CO Comments: To appear in proceedings of the Royal Society scientific discussion meeting "New windows on transients across the Universe", 23-24 April 2012 \\ Prospects for future supernova surveys are discussed, focusing on the ESA Euclid mission and the European Extremely Large Telescope(E-ELT), both expected to be in operation around the turn of the decade. Euclid is a 1.2m space survey telescope that will operate at visible and near-infrared wavelengths, and has the potential to find and obtain multi-band lightcurves for thousands of distant supernovae. The E-ELT is a planned general-purpose ground-based 40m-class optical-IR telescope with adaptive optics built in, which will be capable of obtaining spectra of Type Ia supernovae to redshifts of at least four. The contribution to supernova cosmology with these facilities will be discussed in the context of other future supernova programs such as those proposed for DES, JWST, LSST and WFIRST. \\ ( http://arxiv.org/abs/1211.6586 , 1517kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6589 Date: Wed, 28 Nov 2012 12:12:03 GMT (80kb) Title: Neutrino Lump Fluid in Growing Neutrino Quintessence Authors: Youness Ayaita, Maik Weber, Christof Wetterich Categories: astro-ph.CO Comments: 11 pages, 6 figures \\ Growing neutrino quintessence addresses the "why now" problem of dark energy by assuming that the neutrinos are coupled to the dark energy scalar field. The coupling mediates an attractive force between the neutrinos leading to the formation of large neutrino lumps. This work proposes an effective, simplified description of the subsequent cosmological dynamics. We treat neutrino lumps as effective particles and investigate their properties and mutual interactions. The neutrino lump fluid behaves as cold dark matter coupled to dark energy. The methods developed here may find wider applications for fluids of composite objects. \\ ( http://arxiv.org/abs/1211.6589 , 80kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6592 Date: Wed, 28 Nov 2012 12:22:53 GMT (4364kb,D) Title: Analytical modeling of pulse-pileup distortion using the true pulse shape, with applications to Fermi-GBM Authors: Vandiver Chaplin, Narayana Bhat, Michael Briggs, Valerie Connaughton Categories: astro-ph.IM hep-ex nucl-ex physics.ins-det physics.med-ph Comments: 23 pages, 21 figures \\ Pulse-pileup affects most photon counting systems and occurs when photon detections occur faster than the detector's registration and recovery time. At high input rates, shaped pulses interfere and the source spectrum, as well as intensity information, get distorted. For instruments using bipolar pulse shaping there are two aspects to consider: `peak' and `tail' pileup effects, which raise and lower the measured energy, respectively. Peak effects have been extensively modeled in the past. Tail effects have garnered less attention due to the increased complexity: bipolar tails mean the tail pulse-height measurement depends on events in more than one time interval. We leverage previous work to derive an accurate, semi-analytical prediction for peak and tail pileup, up to high orders. We use the true pulse shape from the detectors of the Fermi Gamma-ray Burst Monitor. The measured spectrum is calculated by writing exposure time as a state-space expansion of overlapping pileup states and is valid up to very high rates. This expansion models losses due to fixed and extendable deadtime by averaging overlap configurations. Additionally, the model correctly predicts energy-dependent losses due to tail subtraction (sub-threshold) effects. We discuss pileup losses in terms of the true rate of photon detections versus the recorded count rate. \\ ( http://arxiv.org/abs/1211.6592 , 4364kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6605 Date: Wed, 28 Nov 2012 14:04:34 GMT (351kb,D) Title: Warm water deuterium fractionation in IRAS 16293-2422 - The high-resolution ALMA and SMA view Authors: Magnus V. Persson, Jes K. J{\o}rgensen, Ewine F. van Dishoeck Categories: astro-ph.SR Comments: Accepted for publication in Astronomy & Astrophysics DOI: 10.1051/0004-6361/201220638 \\ Measuring the water deuterium fractionation in the inner warm regions of low-mass protostars has so far been hampered by poor angular resolution obtainable with single-dish ground- and space-based telescopes. Observations of water isotopologues using (sub)millimeter wavelength interferometers have the potential to shed light on this matter. Observations toward IRAS 16293-2422 of the 5(3,2)-4(4,1) transition of H2-18O at 692.07914 GHz from Atacama Large Millimeter/submillimeter Array (ALMA) as well as the 3(1,3)-2(2,0) of H2-18O at 203.40752 GHz and the 3(1,2)-2(2,1) transition of HDO at 225.89672 GHz from the Submillimeter Array (SMA) are presented. The 692 GHz H2-18O line is seen toward both components of the binary protostar. Toward one of the components, "source B", the line is seen in absorption toward the continuum, slightly red-shifted from the systemic velocity, whereas emission is seen off-source at the systemic velocity. Toward the other component, "source A", the two HDO and H2-18O lines are detected as well with the SMA. From the H2-18O transitions the excitation temperature is estimated at 124 +/- 12 K. The calculated HDO/H2O ratio is (9.2 +/- 2.6)*10^(-4) - significantly lower than previous estimates in the warm gas close to the source. It is also lower by a factor of ~5 than the ratio deduced in the outer envelope. Our observations reveal the physical and chemical structure of water vapor close to the protostars on solar-system scales. The red-shifted absorption detected toward source B is indicative of infall. The excitation temperature is consistent with the picture of water ice evaporation close to the protostar. The low HDO/H2O ratio deduced here suggests that the differences between the inner regions of the protostars and the Earth's oceans and comets are smaller than previously thought. \\ ( http://arxiv.org/abs/1211.6605 , 351kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6608 Date: Wed, 28 Nov 2012 14:17:41 GMT (322kb) Title: Multiple stellar-mass black holes in globular clusters: theoretical confirmation Authors: Anna C. Sippel and Jarrod R. Hurley Categories: astro-ph.GA Comments: accepted for publication in MNRAS letters. 5 pages, 4 figures \\ While tens or hundreds of stellar-remnant black holes are expected to form in globular star clusters, it is still unclear how many of those will be retained upon formation, and how many will be ejected through subsequent dynamical interactions. No such black holes have been found in any Milky Way globular cluster until the recent discovery of stellar-mass black holes in the globular cluster M22 (NGC 6656) with now an estimated population of 5-100 black holes. We present a direct N-body model of a star cluster of the same absolute and dynamical age as M22. Imposing an initial retention fraction of approx. 10% for black holes, 16 stellar-remnant black holes are retained at a cluster age of 12 Gyr, in agreement with the estimate for M22. Of those 16 BHs, two are in a binary system with a main sequence star each while also one pure black hole binary is present. We argue that multiple black holes can be present in any Milky Way cluster with an extended core radius, such as M22 or the model presented here. \\ ( http://arxiv.org/abs/1211.6608 , 322kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6642 Date: Wed, 28 Nov 2012 15:54:16 GMT (33kb) Title: Exponents of non-linear clustering in scale-free one dimensional cosmological simulations Authors: David Benhaiem, Michael Joyce and Fran\c{c}ois Sicard Categories: astro-ph.CO Comments: 11 pages, 4 figures \\ One dimensional versions of cosmological N-body simulations have been shown to share many qualitative behaviours of the three dimensional problem. They can resolve a large range of time and length scales, and admit exact numerical integration. We use such models to study how non-linear clustering depends on initial conditions and cosmology. More specifically, we consider a family of models which, like the 3D EdS model, lead for power-law initial conditions to self-similar clustering characterized in the strongly non-linear regime by power-law behaviour of the two point correlation function. We study how the corresponding exponent \gamma depends on the initial conditions, characterized by the exponent n of the power spectrum of initial fluctuations, and on a single parameter \kappa controlling the rate of expansion. The space of initial conditions/cosmology divides very clearly into two parts: (1) a region in which \gamma depends strongly on both n and \kappa and where it agrees very well with a simple generalisation of the so-called stable clustering hypothesis in three dimensions, and (2) a region in which \gamma is more or less independent of both the spectrum and the expansion of the universe. We explain the observed location of the boundary in (n, \kappa) space dividing the "stable clustering" region from the "universal" region. We compare and contrast our findings to results in three dimensions, and discuss in particular the light they may throw on the question of "universality" of non-linear clustering in this context. \\ ( http://arxiv.org/abs/1211.6642 , 33kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6650 Date: Wed, 28 Nov 2012 16:43:11 GMT (648kb) Title: Characterizing two solar-type Kepler subgiants with asteroseismology: KIC10920273 and KIC11395018 Authors: G. Dogan, T. S. Metcalfe, S. Deheuvels, M. P. Di Mauro, P. Eggenberger, O. L. Creevey, M. J. P. F. G. Monteiro, M. Pinsonneault, A. Frasca, C. Karoff, S. Mathur, S. G. Sousa, I. M. Brandao, T. L. Campante, R. Handberg, A.O. Thygesen, K. Biazzo, H. Bruntt, E. Niemczura, T. R. Bedding, W. J. Chaplin, J. Christensen-Dalsgaard, R. A. Garcia, J. Molenda-Zakowicz, D. Stello, J. L. Van Saders, H. Kjeldsen, M. Still, S. E. Thompson and J. Van Cleve Categories: astro-ph.SR Comments: 12 pages, 3 figures, 5 tables. Accepted by ApJ \\ Determining fundamental properties of stars through stellar modeling has improved substantially due to recent advances in asteroseismology. Thanks to the unprecedented data quality obtained by space missions, particularly CoRoT and Kepler, invaluable information is extracted from the high-precision stellar oscillation frequencies, which provide very strong constraints on possible stellar models for a given set of classical observations. In this work, we have characterized two relatively faint stars, KIC10920273 and KIC11395018, using oscillation data from Kepler photometry and atmospheric constraints from ground-based spectroscopy. Both stars have very similar atmospheric properties; however, using the individual frequencies extracted from the Kepler data, we have determined quite distinct global properties, with increased precision compared to that of earlier results. We found that both stars have left the main sequence and characterized them as follows: KIC10920273 is a one-solar-mass star (M=1.00 +/- 0.04 M_sun), but much older than our Sun (t=7.12 +/- 0.47 Gyr), while KIC11395018 is significantly more massive than the Sun (M=1.27 +/- 0.04 M_sun) with an age close to that of the Sun (t=4.57 +/- 0.23 Gyr). We confirm that the high lithium abundance reported for these stars should not be considered to represent young ages, as we precisely determined them to be evolved subgiants. We discuss the use of surface lithium abundance, rotation and activity relations as potential age diagnostics. \\ ( http://arxiv.org/abs/1211.6650 , 648kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6657 Date: Wed, 28 Nov 2012 16:57:09 GMT (1913kb) Title: Interacting warm dark matter Authors: Norman Cruz, Guillermo Palma, David Zambrano, Arturo Avelino Categories: astro-ph.CO gr-qc Comments: 22 pages, 20 figures, 1 table. Submitted to the Journal of Cosmology and Astroparticle Physics (JCAP) \\ We explore a cosmological model composed by a dark matter fluid interacting with a dark energy fluid. The interaction term has the non-linear "lambda * rho_m^alpha * rho_e^beta" form, where rho_m and rho_e are the energy densities of the dark matter and dark energy, respectively. The parameters alpha and beta in principle are not constraint to take any particular values. We perform an analytical study of the evolution equations, finding the fixed points and their stability properties in order to characterize suitable physical regions in the space of the dark matter and dark energy densities. The constants (lambda, alpha, beta) as well as (w_m, w_e) of the EoS of dark matter and dark energy respectively were estimated using the cosmological observations of the type Ia supernovae data set and the Hubble parameter H(z) at different redshift. We found that the best fit to data is for a model with a phantom dark energy interacting with a warm dark matter, where the energy transfer comes from the dark energy to the dark matter and with an interacting term of the simple form "rho_m * rho_e". This result is consistent with stable solutions of the dynamical system analysis. \\ ( http://arxiv.org/abs/1211.6657 , 1913kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6659 Date: Wed, 28 Nov 2012 17:02:04 GMT (244kb) Title: Evidence for CO shock excitation in NGC 6240 from Herschel SPIRE spectroscopy Authors: R. Meijerink, L. E. Kristensen, A. Weiss, P. P. van der Werf, F. Walter, M. Spaans, A. F. Loenen, J. Fischer, F. P. Israel, K. Isaak, P. P. Papadopoulos, S. Aalto, L. Armus, V. Charmandaris, K. M. Dasyra, T. Diaz-Santos, A. Evans, Y. Gao, E. Gonzalez-Alfonso, R. Guesten, C. Henkel, C. Kramer, S. Lord, J. Martin-Pintado, D. Naylor, D. B. Sanders, H. Smith, L. Spinoglio, G. Stacey, S. Veilleux, M. C. Wiedner Categories: astro-ph.CO astro-ph.GA Comments: Accepted by Astrophysical Journal Letters \\ We present Herschel SPIRE FTS spectroscopy of the nearby luminous infrared galaxy NGC 6240. In total 20 lines are detected, including CO J=4-3 through J=13-12, 6 H2O rotational lines, and [CI] and [NII] fine-structure lines. The CO to continuum luminosity ratio is 10 times higher in NGC 6240 than Mrk 231. Although the CO ladders of NGC 6240 and Mrk 231 are very similar, UV and/or X-ray irradiation are unlikely to be responsible for the excitation of the gas in NGC 6240. We applied both C and J shock models to the H2 v=1-0 S(1) and v=2-1 S(1) lines and the CO rotational ladder. The CO ladder is best reproduced by a model with shock velocity v_s=10 km s^-1 and a pre-shock density n_H=5 * 10^4 cm^-3. We find that the solution best fitting the H2 lines is degenerate: The shock velocities and number densities range between v_s = 17 - 47 km s^-1 and n_H=10^7 - 5 * 10^4 cm^-3, respectively. The H2 lines thus need a much more powerful shock than the CO lines. We deduce that most of the gas is currently moderately stirred up by slow (10 km s^-1) shocks while only a small fraction (< 1 percent) of the ISM is exposed to the high velocity shocks. This implies that the gas is rapidly loosing its highly turbulent motions. We argue that a high CO line-to-continuum ratio is a key diagnostic for the presence of shocks. \\ ( http://arxiv.org/abs/1211.6659 , 244kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6661 Date: Wed, 28 Nov 2012 17:04:34 GMT (237kb) Title: Impact of a revised $^{25}$Mg(p,$\gamma$)$^{26}$Al reaction rate on the operation of the Mg-Al cycle Authors: O. Straniero, G. Imbriani, F. Strieder, D. Bemmerer, C. Broggini, A. Caciolli, P. Corvisiero, H. Costantini, S. Cristallo, A. DiLeva, A. Formicola, Z. Elekes, Zs. F\"ul\"op, G. Gervino, A. Guglielmetti, C. Gustavino, Gy. Gy\"urky, M. Junker, A. Lemut, B. Limata, M. Marta, C. Mazzocchi, R. Menegazzo, L. Piersanti, P. Prati, V. Roca, C. Rolfs, C. Rossi Alvarez, E. Somorjai, F. Terrasi, H.P. Trautvetter Categories: astro-ph.SR astro-ph.GA astro-ph.HE nucl-ex \\ Proton captures on Mg isotopes play an important role in the Mg-Al cycle active in stellar H-burning regions. In particular, low-energy nuclear resonances in the $^{25}$Mg(p,$\gamma$)$^{26}$Al reaction affect the production of radioactive $^{26}$Al$^{gs}$ as well as the resulting Mg/Al abundance ratio. Reliable estimations of these quantities require precise measurements of the strengths of low-energy resonances. Based on a new experimental study performed at LUNA, we provide revised rates of the $^{25}$Mg(p,$\gamma$)$^{26}$Al$^{gs}$ and the $^{25}$Mg(p,$\gamma$)$^{26}$Al$^{m}$ reactions with corresponding uncertainties. In the temperature range 50 to 150 MK, the new recommended rate of the $^{26}$Al$^{m}$ production is up to 5 times higher than previously assumed. In addition, at T$=100$ MK, the revised total reaction rate is a factor of 2 higher. Note that this is the range of temperature at which the Mg-Al cycle operates in an H-burning zone. The effects of this revision are discussed. Due to the significantly larger $^{25}$Mg(p,$\gamma$)$^{26}$Al$^{m}$ rate, the estimated production of $^{26}$Al$^{gs}$ in H-burning regions is less efficient than previously obtained. As a result, the new rates should imply a smaller contribution from Wolf-Rayet stars to the galactic $^{26}$Al budget. Similarly, we show that the AGB extra-mixing scenario does not appear able to explain the most extreme values of $^{26}$Al/$^{27}$Al, i.e. $>10^{-2}$, found in some O-rich presolar grains. Finally, the substantial increase of the total reaction rate makes the hypothesis of a self-pollution by massive AGBs a more robust explanation for the Mg-Al anticorrelation observed in Globular-Cluster stars. \\ ( http://arxiv.org/abs/1211.6661 , 237kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6668 Date: Wed, 28 Nov 2012 17:24:03 GMT (502kb) Title: The SCUBA-2 Cosmology Legacy Survey: blank-field number counts of 450um-selected galaxies and their contribution to the cosmic infrared background Authors: J. E. Geach (McGill), E. L. Chapin (ESAC), K. E. K. Coppin (McGill), J. S. Dunlop (ROE), M. Halpern (UBC), Ian Smail (Durham), P. van der Werf (Leiden), S. Serjeant (Open), D. Farrah (Virginia), I. Roseboom (ROE), T. Targett (ROE), V. Arumugam (ROE), V. Asboth (UBC), A. Blain (Leicester), A. Chrysostomou (Herts), C. Clarke (Sussex), R. J. Ivison (ROE/ATC), S. L. Jones (Leicester), A. Karim (Durham), T. Mackenzie (UBC), R. Meijerink (Kapteyn), M. J. Michalowski (ROE), D. Scott (UBC), J. Simpson (Durham), A. M. Swinbank (Durham), D. Alexander (Durham), O. Almaini (Nottingham), I. Aretxaga (INAO), P. Best (ROE), S. Chapman (Dalhousie), D. L. Clements (Imperial), C. Conselice (Nottingham), A. L. R. Danielson (Durham), S. Eales (Cardiff), A. C. Edge (Durham), A. Gibb (JAC), D. Hughes (INAO), T. Jenness (JAC), et al. (15 additional authors not shown) Categories: astro-ph.CO Comments: 9 pages, 5 figures, submitted to MNRAS \\ The first deep blank-field 450um map (1-sigma~1.3mJy) from the SCUBA-2 Cosmology Legacy Survey (S2CLS), conducted with the James Clerk Maxwell Telescope (JCMT) is presented. Our map covers 140 arcmin^2 of the COSMOS field, in the footprint of the HST CANDELS area. Using 60 submillimetre galaxies (SMGs) detected at >3.75-sigma, we evaluate the number counts of 450um-selected galaxies with flux densities S_450>5mJy. The 8-arcsec JCMT beam and high sensitivity of SCUBA-2 now make it possible to directly resolve a larger fraction of the cosmic infrared background (CIB, peaking at ~200um) into the individual galaxies responsible for its emission than has previously been possible at this wavelength. At S_450>5mJy we resolve (7.4[+/-]0.7)x10^-2 MJy/sr of the CIB at 450um (equivalent to 16[+/-]7% of the absolute brightness measured by COBE at this wavelength) into point sources. A further ~40% of the CIB can be recovered through a statistical stack of 24um emitters in this field, indicating that the majority (~60%) of the CIB at 450um is emitted by galaxies with S_450>2mJy. The average redshift of 450um emitters identified with an optical/near-infrared counterpart is estimated to be =1.3, implying that the galaxies in the sample are in the ultraluminous class (L_IR~1.1x10^12 L_sun). If the galaxies contributing to the statistical stack lie at similar redshifts, then the majority of the CIB at 450um is emitted by galaxies in the LIRG class with L_IR>3.6x10^11 L_sun. \\ ( http://arxiv.org/abs/1211.6668 , 502kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6701 Date: Wed, 28 Nov 2012 18:51:32 GMT (2844kb,D) Title: Cosmological perturbations during the Bose-Einstein condensation of dark matter Authors: R. C. Freitas and S. V. B. Gon\c{c}alves Categories: astro-ph.CO gr-qc Comments: 19 pages, 8 figures \\ In the present work, we analyze the evolution of the scalar and tensorial perturbations and the quantities relevant for the physical description of the Universe, as the density contrast of the scalar perturbations and the gravitational waves energy density during the Bose-Einstein condensation of dark matter. The behavior of these parameters during the Bose-Einstein phase transition of dark matter is analyzed in details. To study the cosmological dynamics and evolution of scalar and tensorial perturbations in a Universe with and without cosmological constant we use both analytical and numerical methods. The Bose-Einstein phase transition modifies the evolution of gravitational waves of cosmological origin, as well as the process of large-scale structure formation. \\ ( http://arxiv.org/abs/1211.6701 , 2844kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6713 Date: Wed, 28 Nov 2012 19:26:08 GMT (732kb,D) Title: Large-Scale Image Processing with the ROTSE Pipeline Authors: L. K. Nuttall, D. J. White, P. J. Sutton, E. J. Daw, V. S. Dhillon, W. Zheng, C. Akerlof Categories: astro-ph.IM gr-qc Report-no: LIGO-P1200131-v4 \\ Electromagnetic (EM) observations of gravitational-wave (GW) sources would bring unique insights into a source which are not available from either channel alone. However EM followup of GW events presents new challenges. GW events will have large sky error regions, on the order of 10-100 square degrees, which can be made up of many disjoint patches. When searching such large areas there is potential contamination by EM transients unrelated to the GW event. Furthermore, the characteristics of possible EM counterparts to GW events are also uncertain. It is therefore desirable to be able to assess the statistical significance of a candidate EM counterpart, which can only be done by performing background studies of large data sets. Current image processing pipelines such as that used by ROTSE are not usually optimised for large-scale processing. We have automated the ROTSE image analysis, and supplemented it with a post-processing unit for candidate validation and classification. We also propose a simple ad hoc statistic for ranking candidates as more likely to be associated with the GW trigger. We demonstrate the performance of the automated pipeline and ranking statistic using archival ROTSE data. EM candidates from a randomly selected set of images are compared to a background estimated from analysis of 102 additional sets of archival images. The pipeline's detection efficiency is computed empirically by re-analysis of the images after adding simulated optical transients that follow typical light curves for gamma-ray burst afterglows and kilonovae. We show that the automated pipeline rejects most background events and is sensitive to simulated transients to limiting magnitudes consistent with the limiting magnitude of the images. \\ ( http://arxiv.org/abs/1211.6713 , 732kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6717 Date: Wed, 28 Nov 2012 19:50:25 GMT (1166kb) Title: A Detailed Morpho-Kinematic Model of the Eskimo, NGC 2392. A Unifying View with the Cat's Eye and Saturn Planetary Nebulae Authors: Ma. T. Garc\'ia-D\'iaz, J. A. L\'opez, W. Steffen, M. G. Richer Categories: astro-ph.SR Comments: 26 pages, 9 figures, accepted for publication in The Astrophysical Journal \\ The 3-D and kinematic structure of the Eskimo nebula, NGC 2392, has been notoriously difficult to interpret in detail given its complex morphology, multiple kinematic components and its nearly pole-on orientation along the line of sight. We present a comprehensive, spatially resolved, high resolution, long-slit spectroscopic mapping of the Eskimo planetary nebula. The data consist of 21 spatially resolved, long-slit echelle spectra tightly spaced over the Eskimo and along its bipolar jets. This data set allows us to construct a velocity-resolved [NII] channel map of the nebula with a resolution of 10 km/s that disentangles the different kinematic components of the nebula. The spectroscopic information is combined with HST images to construct a detailed three dimensional morpho-kinematic model of the Eskimo using the code SHAPE. With this model we demonstrate that the Eskimo is a close analog to the Saturn and the Cat's Eye nebulae, but rotated 90 degrees to the line of sight. Furthermore, we show that the main characteristics of our model apply to the general properties of the group of elliptical planetary nebulae with ansae or FLIERS, once the orientation is considered. We conclude that these kind of nebulae belongs to a class with a complex common evolutionary sequence of events. \\ ( http://arxiv.org/abs/1211.6717 , 1166kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6721 Date: Wed, 28 Nov 2012 20:00:52 GMT (30kb) Title: Does the CMB prefer a leptonic Universe? Authors: Dominik J. Schwarz, Maik Stuke Categories: astro-ph.CO Comments: 9 pages, 1 figure Report-no: BI-TP2012/47 \\ Recent observations of the cosmic microwave background (CMB) at smallest angular scales and updated abundances of primordial elements, indicate an increase of the energy density and the helium-4 abundance with respect to standard big bang nucleosynthesis with three neutrino flavour. This calls for a reanalysis of the observational bounds on neutrino chemical potentials, which encode the number asymmetry between cosmic neutrinos and anti-neutrinos and thus measures the lepton asymmetry of the Universe. We compare recent data with a big bang nucleosynthesis code, assuming neutrino flavour equilibration via neutrino oscillations before the onset of big bang nucleosynthesis. We find a slight preference for negative neutrino chemical potentials, which would imply an excess of anti-neutrinos and thus a negative lepton number of the Universe. This lepton asymmetry could exceed the baryon asymmetry by orders of magnitude. \\ ( http://arxiv.org/abs/1211.6721 , 30kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6722 Date: Wed, 28 Nov 2012 20:01:41 GMT (1088kb,D) Title: The nature of filamentary cold gas in the core of the Virgo Cluster Authors: N. Werner, J. B. R. Oonk, R. E. A. Canning, S. W. Allen, A. Simionescu, J. Kos, R. J. van Weeren, A. C. Edge, A. C. Fabian, A. von der Linden, P. E. J. Nulsen, C. S. Reynolds, M. Ruszkowski Categories: astro-ph.CO Comments: submitted to ApJ \\ We present a multi-wavelength study of the emission-line nebulae located southeast of the nucleus of M87, the central dominant galaxy of the Virgo Cluster. We report the detection of far-infrared (FIR) [CII] line emission from the nebulae using observations made with Herschel PACS. The infrared line emission is extended and cospatial with optical H{\alpha}+[NII], far-ultraviolet CIV lines, and soft X-ray emission. The filamentary nebulae evidently contain multi-phase material spanning a temperature range of at least 5 orders of magnitude, from ~100 K to ~10^7 K. This material has most likely been uplifted by the AGN from the center of M87. The thermal pressure of the 10^4 K phase appears to be significantly lower than that of the surrounding hot intra-cluster medium (ICM) indicating the presence of additional turbulent and magnetic pressure in the filaments. If the turbulence in the filaments is subsonic then the magnetic field strength required to balance the pressure of the surrounding ICM is B~30-70 {\mu}G. The spectral properties of the soft X-ray emission from the filaments indicate that it is due to thermal plasma with kT~0.5-1 keV, which is cooling by mixing with the cold gas and/or radiatively. Charge exchange can be ruled out as a significant source of soft X-rays. Both cooling and mixing scenarios predict gas with a range of temperatures. This is at first glance inconsistent with the apparent lack of X-ray emitting gas with kT<0.5 keV. However, we show that the missing very soft X-ray emission could be absorbed by the cold gas in the filaments with an average absorption column density of ~10^21 cm^-2, providing a natural explanation for the apparent temperature floor to the X-ray emission at kT~0.5 keV. The FIR through ultra-violet line emission is most likely primarily powered by the ICM particles penetrating the cold gas following a shearing induced mixing process. \\ ( http://arxiv.org/abs/1211.6722 , 1088kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6723 Date: Wed, 28 Nov 2012 20:04:18 GMT (3308kb,D) Title: Galaxy Zoo: A Catalog of Overlapping Galaxy Pairs for Dust Studies Authors: William C. Keel, Anna Manning, Benne W. Holwerda, Massimo Mezzoprete, Chris J. Lintott, Kevin Schawinski, Pamela Gay, and Karen L. Masters Categories: astro-ph.CO Comments: PASP, in press. Full catalog and additional data are available at http://data.galaxyzoo.org/overlaps.html \\ Analysis of galaxies with overlapping images offers a direct way to probe the distribution of dust extinction and its effects on the background light. We present a catalog of 1990 such galaxy pairs selected from the Sloan Digital Sky Survey (SDSS) by volunteers of the Galaxy Zoo project. We highlight subsamples which are particularly useful for retrieving such properties of the dust distribution as UV extinction, the extent perpendicular to the disk plane, and extinction in the inner parts of disks. The sample spans wide ranges of morphology and surface brightness, opening up the possibility of using this technique to address systematic changes in dust extinction or distribution with galaxy type. This sample will form the basis for forthcoming work on the ranges of dust distributions in local disk galaxies, both for their astrophysical implications and as the low-redshift part of a study of the evolution of dust properties. Separate lists and figures show deep overlaps, where the inner regions of the foreground galaxy are backlit, and the relatively small number of previously-known overlapping pairs outside the SDSS DR7 sky coverage. \\ ( http://arxiv.org/abs/1211.6723 , 3308kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6726 Date: Wed, 28 Nov 2012 20:08:53 GMT (698kb) Title: The effect of electron beam pitch angle and density gradient on solar type III radio bursts Authors: Roman Pechhacker and David Tsiklauri Categories: astro-ph.SR physics.plasm-ph Comments: supplemental material at http://astro.qmul.ac.uk/~tsiklauri/sp.html. to be published in Physics of Plasmas December 2012 issue \\ 1.5D Particle-In-Cell simulations of a hot, low density electron beam injected into magnetized, maxwellian plasma were used to further explore the alternative non-gyrotropic beam driven electromagnetic emission mechanism, first studied in Tsiklauri (2011). Variation of beam injection angle and background density gradient showed that the emission process is caused by the perpendicular component of the beam injection current, whereas the parallel component only produces Langmuir waves, which play no role in the generation of EM waves in our mechanism. Particular emphasis was put on the case, where the beam is injected perpendicularly to the background magnetic field, as this turned off any electrostatic wave generation along the field and left a purely electromagnetic signal in the perpendicular components. The simulations establish the following key findings: i) Initially waves at a few w_ce/gamma are excited, mode converted and emitted at w_pe ii) The emission intensity along the beam axis is proportional to the respective component of the kinetic energy of the beam; iii) The frequency of the escaping EM emission is independent of the injection angle; iv) A stronger background density gradient causes earlier emission; v) The beam electron distribution function in phase space shows harmonic oscillation in the perpendicular components at the relativistic gyrofrequency; vi) The requirement for cyclotron maser emission, df/dv_perp > 0, is fulfilled; vii) The degree of linear polarization of the emission is strongly dependent on the beam injection angle; viii) The generated electromagnetic emission is left-hand elliptically polarized as the pitch angle tends to 90 deg; ix) The generated electromagnetic energy is of the order of 0.1% of the initial beam kinetic energy. \\ ( http://arxiv.org/abs/1211.6726 , 698kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6729 Date: Wed, 28 Nov 2012 20:20:17 GMT (174kb) Title: Electron cyclotron maser emission mode coupling to the z-mode on a longitudinal density gradient in the context of solar type III bursts Authors: Roman Pechhacker and David Tsiklauri Categories: astro-ph.SR Comments: supplemental material at http://astro.qmul.ac.uk/~tsiklauri/sp.html. to be published in Physics of Plasmas December 2012 issue \\ A beam of super-thermal, hot electrons was injected into maxwellian plasma with a density gradient along a magnetic field line. 1.5D particle-in-cell simulations were carried out which established that the EM emission is produced by the perpendicular component of the beam injection momentum. The beam has a positive slope in the distribution function in perpendicular momentum phase space, which is the characteristic feature of a cyclotron maser. The cyclotron maser in the overdense plasma generates emission at the electron cyclotron frequency. The frequencies of generated waves were too low to propagate away from the injection region, hence the wavelet transform shows a pulsating wave generation and decay process. The intensity pulsation frequency is twice the relativistic cyclotron frequency. Eventually, a stable wave packet formed and could mode couple on the density gradient to reach frequencies of the order of the plasma frequency, that allowed for propagation. The emitted wave is likely to be a z-mode wave. The total electromagnetic energy generated is of the order of 0.1% of the initial beam kinetic energy. The proposed mechanism is of relevance to solar type III radio bursts, as well as other situations, when the injected electron beam has a non-zero perpendicular momentum, e.g. magnetron. \\ ( http://arxiv.org/abs/1211.6729 , 174kb) %-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%- ------------------------------------------------------------------------------ \\ arXiv:1211.6272 (*cross-listing*) Date: Tue, 27 Nov 2012 11:07:41 GMT (185kb) Title: Reconstruction of Scalar Potentials in Modified Gravity Models Authors: A.Yu. Kamenshchik, A. Tronconi, G. Venturi, S.Yu. Vernov Categories: gr-qc astro-ph.CO Comments: 20 pages, 2 figures \\ We employ the superpotential technique for the reconstruction of cosmological models with a non-minimally coupled scalar field evolving on a spatially flat Friedmann-Robertson-Walker background. The key point in this method is that the Hubble parameter is considered as a function of the scalar field and this allows one to reconstruct the scalar field potential and determine the dynamics of the field itself, without a priori fixing the Hubble parameter as a function of time or of the scale factor. The scalar field potentials which lead to de Sitter or asymptotic de Sitter solutions, and those which reproduce the cosmological evolution given by Einstein-Hilbert action plus a barotropic perfect fluid, have been obtained. \\ ( http://arxiv.org/abs/1211.6272 , 185kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6516 (*cross-listing*) Date: Wed, 28 Nov 2012 04:38:54 GMT (318kb,D) Title: Smooth hybrid inflation in a supersymmetric axion model Authors: Masahiro Kawasaki, Naoya Kitajima and Kazunori Nakayama Categories: hep-ph astro-ph.CO Comments: 27 pages, 17 figures Report-no: ICRR-Report-639-2012-28; IPMU 12-6216; UT-12-36 \\ We show that the smooth hybrid inflation is naturally realized in a framework of supersymmetric axion model. Identifying the Peccei-Quinn scalar fields as a part of the infaton sector, successful inflation takes place reproducing the amplitude and spectral index of the curvature perturbation observed by WMAP. A relatively large axion isocurvature perturbation and its non-Gaussianity are predicted in our model. The saxion coherent oscillation has a large amplitude and dominates the Universe. The subsequent decay of the saxion produces huge amount of entropy, which dilutes unwanted relics. Winos, the lightest supersymmetric particles in this scenario, are produced non-thermally in the decay and account for dark matter. \\ ( http://arxiv.org/abs/1211.6516 , 318kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6558 (*cross-listing*) Date: Wed, 28 Nov 2012 09:55:13 GMT (17kb) Title: New tests of local Lorentz invariance and local position invariance of gravity with pulsars Authors: Lijing Shao, Norbert Wex, Michael Kramer Categories: gr-qc astro-ph.GA Comments: 3 pages, 1 figure; submitted to Proceedings of the Thirteenth Marcel Grossmann Meeting, (eds.) Kjell Rosquist, Robert T Jantzen, Remo Ruffini \\ New tests are proposed to constrain possible deviations from local Lorentz invariance and local position invariance in the gravity sector. By using precise timing results of two binary pulsars, i.e., PSRs J1012+5307 and J1738+0333, we are able to constrain (strong-field) parametrized post-Newtonian parameters $\hat{\alpha}_1$, $\hat{\alpha}_2$, $\hat{\xi}$ to high precision, among which, $|\hat{\xi}| < 3.1\times10^{-4}$ (95% C.L.) is reported here for the first time. \\ ( http://arxiv.org/abs/1211.6558 , 17kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6619 (*cross-listing*) Date: Wed, 28 Nov 2012 14:55:04 GMT (309kb) Title: Generation of Cosmological Flows in General Relativity (Features and Properties of Integrable Singularities) Authors: V. N. Lukash, E. V. Mikheeva, and V. N. Strokov Categories: gr-qc astro-ph.CO hep-th Comments: 21 pages, 3 figures, extended Introduction and minor changes as compared to the published version Journal-ref: Phys. Usp. 55 831-837 (2012) DOI: 10.3367/UFNe.0182.201208k.0894 \\ We discuss status of the singularity problem in General Relativity and argue that the requirement that a physical solution must be completely free of singularities may be too strong. As an example, we consider properties of the integrable singularities and show that they represent light horizons separating T-regions of black and white holes. Connecting an astrophysical black hole to a white hole, they lead to a natural mechanism of generating new universes. Under favorable conditions the new universes will also contain black holes which, in their turn, will give rise to another generation of universes. In this case the cosmological evolutionary tree will continue to grow to form the "hyperverse". This scenario essentially differs from other known mechanisms, such as bounce, birth from "nothing", baby-universe scenario, etc. \\ ( http://arxiv.org/abs/1211.6619 , 309kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6632 (*cross-listing*) Date: Wed, 28 Nov 2012 15:23:04 GMT (190kb,D) Title: Numerical Relativity in Spherical Polar Coordinates: Evolution Calculations with the BSSN Formulation Authors: Thomas W. Baumgarte, Pedro J. Montero, Isabel Cordero-Carri\'on, Ewald M\"uller Categories: gr-qc astro-ph.SR Comments: 14 pages, 10 figures, submitted to PRD \\ In the absence of symmetry assumptions most numerical relativity simulations adopt Cartesian coordinates. While Cartesian coordinates have some desirable properties, spherical polar coordinates appear better suited for certain applications, including gravitational collapse and supernova simulations. Development of numerical relativity codes in spherical polar coordinates has been hampered by the need to handle the coordinate singularities at the origin and on the axis, for example by careful regularization of the appropriate variables. Assuming spherical symmetry and adopting a covariant version of the BSSN equations, Montero and Cordero-Carri\'on recently demonstrated that such a regularization is not necessary when a partially implicit Runge-Kutta (PIRK) method is used for the time evolution of the gravitational fields. Here we report on an implementation of the BSSN equations in spherical polar coordinates without any symmetry assumptions. Using a PIRK method we obtain stable simulations in three spatial dimensions without the need to regularize the origin or the axis. We perform and discuss a number of tests to assess the stability, accuracy and convergence of the code, namely weak gravitational waves, "hydro-without-hydro" evolutions of spherical and rotating relativistic stars in equilibrium, and single black holes. \\ ( http://arxiv.org/abs/1211.6632 , 190kb) ------------------------------------------------------------------------------ \\ arXiv:1211.6708 (*cross-listing*) Date: Wed, 28 Nov 2012 19:11:43 GMT (242kb) Title: On the Distribution of Plasmoids In High-Lundquist-Number Magnetic Reconnection Authors: Yi-Min Huang, A. Bhattacharjee Categories: physics.plasm-ph astro-ph.SR physics.flu-dyn physics.space-ph Comments: Accepted for publication in Phys. Rev. Lett \\ The distribution function $f(\psi)$ of magnetic flux $\psi$ in plasmoids formed in high-Lundquist-number current sheets is studied by means of an analytic phenomenological model and direct numerical simulations. The distribution function is shown to follow a power law $f(\psi)\sim\psi^{-1}$, which differs from other recent theoretical predictions. Physical explanations are given for the discrepant predictions of other theoretical models. \\ ( http://arxiv.org/abs/1211.6708 , 242kb) %%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%% ------------------------------------------------------------------------------ \\ arXiv:1106.5866 replaced with revised version Wed, 28 Nov 2012 13:31:38 GMT (117kb) Title: Particle motion in weak relativistic gravitational fields Authors: Miki Obradovic, Martin Kunz, Mark Hindmarsh and Ilian T. Iliev Categories: astro-ph.CO Comments: 9 pages, 5 figures DOI: 10.1103/PhysRevD.86.064018 \\ ( http://arxiv.org/abs/1106.5866 , 117kb) ------------------------------------------------------------------------------ \\ arXiv:1109.6566 (*cross-listing*) replaced with revised version Wed, 28 Nov 2012 07:36:22 GMT (580kb,D) Title: The Inflationary Wavefunction and its Initial Conditions Authors: Daniel Carney, Willy Fischler, Sonia Paban and Navin Sivanandam Categories: hep-th astro-ph.CO Comments: 17 pages, 1 figure, numerical example and analysis thereof added in this version Report-no: UTTG-14-11 \\ ( http://arxiv.org/abs/1109.6566 , 580kb) ------------------------------------------------------------------------------ \\ arXiv:1111.2305 (*cross-listing*) replaced with revised version Wed, 28 Nov 2012 14:51:38 GMT (318kb) Title: New Q-ball Solutions in Gauge-Mediation, Affleck-Dine Baryogenesis and Gravitino Dark Matter Authors: Francesca Doddato, John McDonald Categories: hep-ph astro-ph.CO hep-th Comments: 13 pages, 9 figures. Some corrections and additional discussion. Version published in JCAP \\ ( http://arxiv.org/abs/1111.2305 , 318kb) ------------------------------------------------------------------------------ \\ arXiv:1202.3107 replaced with revised version Wed, 28 Nov 2012 15:55:10 GMT (120kb) Title: MASSIV: Mass Assembly Survey with SINFONI in VVDS. IV. Fundamental relations of star-forming galaxies at 1