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We have considered Poincaré maps for magnetic field lines corresponding to runs $R_{0.2}^{80}$, $R_{0.08}^{80}$ and $R_{0.08}^{86}$. The first two runs differ by the amplitude of the turbulent fluctuations, while the third one is characterized by the same level of fluctuations as the second one but has the same parameter $A$, and essentially the same nonlinearity parameter $\chi$, as the first one. Figure REF displays the 50 intersections for the 32 considered magnetic lines (each of them characterized by a different color), in the three simulations. Interestingly, although they correspond to a different level of fluctuations, runs $R_{0.2}^{80}$ and $R_{0.08}^{86}$ (that display the same $\chi$) both display an erratic distribution of the intersection points of magnetic field lines in the transverse plane and a significant mixing of these lines, a situation that appears to be associated to a regime of strong turbulence. On the other hand, for run $R_{0.08}^{80}$ that corresponds to a regime of weak turbulence, the successive intersection points of individual field lines form distinct clusters, a configuration which is not significantly affected when increasing the extension of the considered field lines and thus the number of intersections. These observations indicate that the degree of meandering of the magnetic field lines is not associated with the amplitude of the turbulence fluctuations but rather to the value of the nonlinearity parameter, which governs the weak or strong character of the turbulence. This remark could be of interest in the context of propagation of solar energetic particles (SEP) for which the sole Fokker-Planck equation cannot explain the fast longitudinal diffusion [CIT].
| 1,726 |
1511.01256
| 12,879,415 | 2,015 | 11 | 4 | true | false | 1 |
FOKKER
|
The Participating Institutions in SDSS-IV include the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatório Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.
| 1,234 |
1511.01496
| 12,881,953 | 2,015 | 11 | 4 | true | false | 3 |
MPS, MPS, MPS
|
Our MCMC algorithm computes the probability needed for the model sequence only from the temperature angular power spectrum ${\cal D}_l^{\hbox{\scriptsize TT}}$, so the match with the polarization data is completely ignored for the generation of the MCMC sequence. However, it is nevertheless important to compare the Planck polarization data [CIT] with the spectrum of the best-fit model. In figure REF, the polarization power spectra ${\cal D}_l^{\hbox{\scriptsize TE}} := l(l+1) C^{\hbox{\scriptsize TE}}_l/(2\pi)$ and ${\cal D}_l^{\hbox{\scriptsize EE}} := l(l+1) C^{\hbox{\scriptsize EE}}_l/(2\pi)$ are shown in panels (a) and (b), respectively, in comparison to the binned TE and EE data of the Planck 2015 data release [CIT]. The best-fit model with $c^2_{\hbox{\scriptsize eff}}=0$ is plotted as a full curve, while the model with the slightly enhanced value of $c^2_{\hbox{\scriptsize eff}}=0.01$ is shown as the dashed curve. With respect to the fact that the best-fit model is solely determined from the temperature power spectrum ${\cal D}_l^{\hbox{\scriptsize TT}}$, it is assuring that also the polarization data agree well with the best-fit model. The comparison with the model with $c^2_{\hbox{\scriptsize eff}}=0.01$ reveals discrepancies as it is the case for the temperature power spectrum ${\cal D}_l^{\hbox{\scriptsize TT}}$ shown in figure REF. The largest deviations can be found for the EE spectrum around $l\simeq 700$.
| 1,443 |
1511.01691
| 12,884,690 | 2,015 | 11 | 5 | true | false | 2 |
MISSION, MISSION
|
We investigated the variation of the spectral indices with frequency for the PACO Bright Source sample, for which we have a larger probability to find detections at Planck frequencies. Table REF and Fig. REF summarize the median values of spectral indices in the 4--217,GHz frequency range. No break is clearly visible at high frequencies. The spectral indices in the ranges 70--100,GHz and 100--150,GHz (-0.65 and -0.67 respectively) have 98.3,% probability to be drawn from the same distribution according to a Kolmogorov-Smirnov test. At even higher frequencies spectral indices seem to increase, probably as a consequence of the arising of Galactic dust contamination in the vicinity of the sources.
| 703 |
1511.02605
| 12,891,962 | 2,015 | 11 | 9 | true | false | 1 |
MISSION
|
The Planck 2015 CMB data have provided the tight limits on the total mass of active neutrinos, $\sum m_\nu$ [CIT]. The base $\Lambda$CDM model assumes a normal mass hierarchy of neutrinos with $\sum m_\nu\approx 0.06$ eV (dominated by the heaviest neutrino mass eigenstate). When the model is extended to allow for larger neutrino masses, a reasonable assumption is that the three species of neutrinos have degenerate masses, neglecting the small differences between mass eigenstates. For the $\Lambda$CDM model, the Planck data (Planck TT+lowP) give the constraint $\sum m_\nu<0.72$ eV.[^1] Here, "lowP" denotes the Planck low-$\ell$ temperature-polarization data. It is known that the CMB data alone have a limitation to constrain the neutrino mass due to the acoustic scale degeneracy with $H_0$. So, it is necessary to combine the CMB data with other late-time cosmological probes in order to break the degeneracy. Adding the baryon acoustic oscillation (BAO) data could help to break the acoustic scale degeneracy and tighten the constraint on $\sum m_\nu$ substantially. The Planck TT+lowP+BAO data combination changes the limit to: $\sum m_\nu<0.21$ eV. Since the full Planck mission released the first analysis of the Planck polarization data, one could add the polarization data to the constraint, which will further tighten the neutrino mass limit. The combination of Planck TT, TE, EE+lowP+BAO leads to the limit $\sum m_\nu<0.17$ eV. Note that all the upper limit values for neutrino mass quoted in this paper refer to the 95% confidence level (CL).
| 1,561 |
1511.02651
| 12,892,233 | 2,015 | 11 | 9 | true | true | 8 |
MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION
|
As seen in the autocorrelation measurements, the lensing cross-correlations are generally scale-independent over the chosen fitting range. However, beyond this range toward smaller scales (larger $l$), there is a clear increase in cross-correlation power that is particularly strong for the obscured sample, though more prevalent for both samples when PlanckDR1 is used. While the measurement is noisy at the largest $l$, with the PlanckDR2 lensing map the unobscured cross-correlation stays consistent with flat out to the smallest scales ($\sim$ 0.1$^{\circ}$, consistent with the clustering measurement). The scale-dependence for the obscured sample is reduced somewhat with DR2, but is still present. The obscured sample cross-correlation with DR2 also shows a prominent bump around $l \sim 600$, about the scales for which there may be an unknown correlated feature in the DR2 lensing map [CIT].
| 900 |
1511.04469
| 12,913,609 | 2,015 | 11 | 13 | true | false | 2 |
MISSION, MISSION
|
In this paper, we extend the analysis performed in [CIT] in two ways. In order to study the effects of BH rotation, we first calculate the greybody factors in section [2], and thus the gravity wave spectrum at emission time in section [3]. The evolution of the PBH parameters like mass and angular momentum is then also computable, as shown in section [4]. Second, we discuss the physical requirements in choosing parameters in section [5]. The effects of cosmic expansion on the observed signal is derived in section [6]. After completing this preliminary setup, we perform our calculations of gravity wave spectrum for small PBHs that evaporate before the big-bang nucleosynthesis (BBN) in section [7]. In addition, after taking into account the observational astrophysical limits (summarized in section [8]) we also compute the gravity wave spectrum for larger black holes that evaporated before or are still evaporating today in sections [9]. The results are summarized in section [10]. Throughout the paper we use Planck units, i.e. $\hbar=c=G=k_B=1$, unless otherwise specified.
| 1,084 |
1511.05642
| 12,924,853 | 2,015 | 11 | 18 | true | false | 1 |
UNITS
|
A modified black body spectrum was then fit to the mid- to far-IR observations to model the contribution due to excess dust emission (See Figure REF). The black body equation in Jy/sr can be seen in Equation REF where $h$ is Planck's constant, $c$ is the speed of light, and $k$ is Boltzmann's constant. The main independent variables over a given wavelength range are the temperature and effective emitting area of dust in steradians ($\Omega$) which can vary to fit the flux density ($\rm F_{\nu}$) of the observations in Jy (Eq. REF). Uncertainties are determined from the diagonal elements of the covariance matrices from the least-square fit. The fit itself is weighted by the measured magnitude uncertainties.
| 715 |
1511.05919
| 12,926,935 | 2,015 | 11 | 18 | true | false | 1 |
CONSTANT
|
In Section 2, we present details of new searches for SLSNe. In Section 3, we provide the methodology used to create our mock Hubble Diagrams for a number of on-going and planned surveys. Section 4 outlines how we then analyse those mock data with cosmological fitting discussed in Section 5. We present results on Section 6 and conclude in Section 7. We assume throughout a flat $\Lambda$CDM Universe with $\Omega_m=0.3$ and $H_0=68$ km,s$^{-1}$,Mpc$^{-1}$ as our fiducial cosmology, consistent with Planck [CIT].
| 513 |
1511.06670
| 12,933,348 | 2,015 | 11 | 20 | true | false | 1 |
MISSION
|
As shown in Table REF, unlike the other cases considered, these three scenarios yield purely adiabatic initial conditions when $r_D = 1$. This has important implications for Planck/BAO constraints to $\xi_{\rm lep}^2$ in these scenarios. From Eq. (REF), it is clear that the level of neutrino isocurvature in these models is negligible. As a result, the sensitivity of Planck/BAO data to $\xi_{\rm lep}^2$ comes solely from its contribution to the total radiative energy density of the universe.
| 495 |
1511.07431
| 12,939,504 | 2,015 | 11 | 23 | true | true | 2 |
MISSION, MISSION
|
The rate at which stars of energy ${\cal E}$ to ${\cal E}+d{\cal E}$ cross the loss cone boundary is easily shown to be FORMULA Evaluating this quantity in the steady-state models, one finds a clear separation between the low- and high-binding-energy regimes. The reason, of course, is the presence of the GW terms in the Fokker-Planck equation, which "grab" stars at high binding energies and keep them from crossing the loss cone boundary until their eccentricities have been sharply reduced.
| 494 |
1511.08169
| 12,946,597 | 2,015 | 11 | 25 | true | false | 1 |
FOKKER
|
In 2010 de Rham and Gabadadze studied generic extensions of the Fierz-Pauli Lagrangian (REF) by higher-order interactions of the massive spin-2 fluctuation $h_{\mu\nu}$ [CIT]. Their analysis went to quintic order in the longitudinal component of the massive spin-2 field and demonstrated that its interactions could in fact be made ghost-free in a decoupling limit, correcting the conclusions of [CIT]. The decoupling limit analysis relies heavily on the aforementioned Goldstone boson analogy suggested by Arkani-Hamed, Georgi and Schwartz and requires taking a double scaling limit in order to study the dynamics of the longitudinal mode separately. As a follow up to [CIT], de Rham, Gabadadze and Tolley (henceforth dRGT) presented a nonlinear theory of massive gravity in whose decoupling limit they proved the absence of ghost for all nonlinear self-interactions of the longitudinal component [CIT]. The dRGT action is of the form, FORMULA where the first term is the ordinary Einstein-Hilbert term of GR with Planck mass $m_g$ and the second term is the interaction potential for the graviton whose mass is set by the scale $m$. Furthermore, $\alpha_2=1$ while the two remaining $\alpha_n$ are arbitrary interaction parameters. The $e_n(\mathcal{K})$ are the elementary symmetric polynomials (see appendix REF) constructed out of the matrix $\mathcal{K}^\mu_{\phantom\mu\nu}=\delta^\mu_\nu-[\sqrt{g^{-1}\eta}]^\mu_{\phantom\mu\nu}$.[^2] Expanding the action in terms of $h_{\mu\nu}=m_g(g_{\mu\nu}-\eta_{\mu\nu})$ indeed results in a nonlinear extension of the Fierz-Pauli theory (REF).
| 1,591 |
1512.00021
| 12,960,581 | 2,015 | 11 | 30 | false | true | 1 |
UNITS
|
[^20]: [CIT] also finds consistent $\tau_{\rm es}$ when they (1) reanalyze the WMAP polarization data using the newer Planck foreground maps and, remarkably, (2) do not use any polarization data and instead use CMB lensing to break the $\tau_{\rm es} - \sigma_8$ degeneracy that is present in the temperature anisotropies (which results in just $50\%$ larger errors on $\tau_{\rm es}$).
| 386 |
1512.00086
| 12,961,824 | 2,015 | 11 | 30 | true | false | 1 |
MISSION
|
In previous related work, [CIT] predicted the polarization asymmetry given a simplified procedure for fitting to the $T$ data, for modulations of various cosmological parameters. Reference [CIT] considered what the $T$ asymmetry predicts for polarization asymmetry via modulated primordial spectra, using a similar fitting procedure. Importantly, they found that the polarization predictions are strongly dependent on the $k$-space model. Refs. [CIT] performed more careful fitting, but restricted their models. None of these groups considered lensing. Ref. [CIT] looked for a power asymmetry in the Plancklensing map, finding no significant signal in the low-$\ell$ $T$ asymmetry direction. Additionally, a recent study [CIT] claimed that lensing $B$ modes could confirm a physical modulation at high significance, due to the mode mixing that takes low-$\ell$ lensing modes to high-$\ell$ $B$ modes. However, this paper treated the statistics of the lensed $B$ field as Gaussian, whereas it is known that non-Gaussianity reduces the total signal-to-noise ratio of the lensing $B$ power spectrum by a large factor (see, e.g., [CIT]). Also, [CIT] did not consider a physical lensing modulation mechanism and simply took the expected lensing modulation amplitude to be $7\%$ to $\ell = 70$.
| 1,288 |
1512.02618
| 12,985,547 | 2,015 | 12 | 8 | true | false | 1 |
MISSION
|
A new scenario for gravitational collapse has been recently proposed by Haggard and Rovelli. Presenting the model under the name of black hole fireworks, they claim that the accumulation of quantum gravitational effects outside the horizon can cause the tunneling of geometry from a black hole to a white hole, allowing a bounce of the collapsing star which can eventually go back to infinity. In this paper we discuss the instabilities of this model and propose a simple minimal modification which eliminates them, as well as other related instabilities discussed in the literature. The new scenario is a time-asymmetric version of the original model with a time-scale for the final explosion that is shorter than m log m in Planck units. Our analysis highlights the importance of irreversibility in gravitational collapse which, in turn, uncovers important issues that cannot be addressed in detail without a full quantum gravity treatment.
| 942 |
1512.04566
| 13,001,973 | 2,015 | 12 | 14 | false | true | 1 |
UNITS
|
The strategy to evolve the distribution function can in principle be applied to any underlying evolution equations, and we pay special attention to keep the derivation general. For the equations of a pressureless perfect fluid and at a fixed order of perturbation theory the TSPT approach gives the same results as SPT. Nonetheless, we will show that TSPT has the important advantage that all building blocks of the diagrammatic expansion, i.e. propagators and vertices, as well as individual diagrams themselves are free from IR divergences. This can be traced back to the property that within TSPT one deals only with equal-time objects which are protected from spurious divergences by the equivalence principle. TSPT is thus a convenient framework for implementing IR resummation --- a subject that is addressed in [CIT]. On the UV side, TSPT allows to reformulate the effective field theory of LSS in the language of Wilsonian renormalization group within the 3-dimensional Euclidean QFT describing the statistical averaging. This formulation appears promising to shed new light on the properties of the effective operators. The inclusion of stochastic noise in the evolution [CIT] can, in principle, be incorporated by promoting the Liouville equation for the distribution function to a Fokker-Planck equation. Finally, the structure of TSPT is also suitable to include primordial non-Gaussianity in a straightforward manner.
| 1,430 |
1512.05807
| 13,022,139 | 2,015 | 12 | 17 | true | true | 1 |
FOKKER
|
The wealth of recent observational data has dramatically reduced the number of viable inflationary models and opened a debate on the possibilities that are left [CIT]. For instance, in the context of single-field inflation, the data from Planck [CIT] basically exclude all potentials of the type $V\sim \phi^{p}$ with $p\geq 2$, thus leaving only a handful of feasible alternatives. Among these, there is the Starobinsky model [CIT], which is based on a minimal extension of general relativity obtained by the addition of a term quadratic in the Ricci scalar $R$. Originally motivated by quantum corrections, this model has been generalised to the class of so-called $f(R)$ gravity (see [CIT] for comprehensive reviews).
| 720 |
1512.07186
| 13,037,871 | 2,015 | 12 | 22 | true | true | 1 |
MISSION
|
Another interesting research line within modified gravity theories is massive gravity. Since the carrier of the gravitational force would be massive in this case, the mediated force would be Yukawa suppressed on large scales and this could yield a natural explanation of the recent cosmological acceleration. The unique mass term at the linear level was already constructed in the 1940's by Fierz and Pauli [CIT]. This constitutes the unique linear theory at the classical level without introducing any additional ghost degree of freedom. Even theoretically being viable, this simple linear theory gives rise to the vDVZ discontinuity [CIT], which reflects the fact that the massless limit of the theory yields a discrete difference to General Relativity. However, this discontinuity can be avoided by restoring non-linear interactions that become appreciable on small scales to freeze out the field fluctuations [CIT]. The inclusion of these non-linear interactions has to be performed in a way that maintains the Boulware-Deser ghost absent [CIT], which was finally accomplished in 2010 [CIT]. Besides being the unique ghost-free non-linear theory of massive gravity, it is technically natural in the sense that it is not subject to strong renormalization by quantum loops [CIT]. The potential interactions have to be tuned in a very specific way to ensure the absence of the Boulware-Deser ghost, however the one-loop contributions from the gravitons usually destabilize this special structure. Notwithstanding this detuning of the potential interactions is irrelevant below the Planck scale.
| 1,595 |
1601.02180
| 13,080,640 | 2,016 | 1 | 10 | true | true | 1 |
UNITS
|
After some experimentation, we found that the values of these parameters vary smoothly with redshift, $z$, and can be calibrated once a cosmological model has been adopted. For the Planck cosmology, their values may be reproduced as follows: FORMULA FORMULA FORMULA FORMULA and FORMULA where $a=(1+z)^{-1}$ and $D(z)$ is the linear growth factor. These expressions are valid over the redshift range $1\geq\log(1+z)\geq 0$, and for masses $-8\leq \log {\rm M}/[h^{-1},{\rm M}_\odot]\leq 16.5$.
| 492 |
1601.02624
| 13,085,072 | 2,016 | 1 | 11 | true | false | 1 |
MISSION
|
The partial wave decomposition employed here should be distinguished from the usual partial wave decompositions in first- or second-quantized particle theories. We are forced to treat particles not as being point-like, but as forming a finite set of membranes that each take the shape of a partial wave. So, introducing a cut-off in $\ell$ would not restrict total angular momenta of all particles any way. Although these partial waves have a classical appearance, we insist that they form legitimate representations of our operator algebra. They can be interpreted as a reformulation of the coordinates of all particles entering and leaving the black hole, a number that is roughly equal to $R^2$ (in Planck units), [CIT]. The partial waves are then nothing but a band-limited mode decomposition as was described in Ref [CIT].
| 827 |
1601.03447
| 13,093,976 | 2,016 | 1 | 14 | false | true | 1 |
UNITS
|
The paper is organized as follows. In Sec. REF we describe the meson-baryon effective interactions used to compute the scattering amplitudes and cross sections of $\Lambda_c$ and $\Lambda_b$ baryons in a light-meson bath. In addition, we review the interactions of $D$ and $\bar B$ mesons in the same medium. In Sec. REF we present the theory of the transport coefficients using the Fokker-Planck approach. Moreover, we show our results for the transport coefficients for $\Lambda_c$ and $\Lambda_b$, and investigate the applicability of certain nonrelativistic estimates of these coefficients. We, furthermore, compare our result for the spatial diffusion coefficient with the one resulting from a direct solution of the Boltzmann equation, as described in Appendix REF. Finally, in Sec. REF, we present our conclusions.
| 821 |
1601.03743
| 13,096,879 | 2,016 | 1 | 14 | false | true | 1 |
FOKKER
|
We now compute the predicted number density of virialised haloes in the Press-Schechter formalism for homogeneous models in ST cosmologies. In the case of homogeneous cosmologies we use equations (REF) and (REF) to determine the number density of virialised haloes. In this case the total mass of haloes is defined by the pressureless matter perturbations. In order to calculate $\sigma^2$, we adopt the formulation presented in [CIT]. On the basis of latest observational results by the Planck Collaboration team [CIT], we adopt the concordance $\Lambda$CDM model with the normalization of the matter power spectrum $\sigma_8=0.815$.
| 634 |
1601.04593
| 13,104,405 | 2,016 | 1 | 18 | true | false | 1 |
MISSION
|
Up till now, we have considered the classical version of $q$-theory [CIT], in which the quantum-dissipative energy exchange between vacuum and matter has been neglected. In the classical theory, the analog of the chemical potential $\mu$ -- the variable thermodynamically conjugate to the variable $q$ -- becomes an integration constant. In a perfect equilibrium vacuum, $\mu$ has the value $\mu_0$ determined by the microscopic parameters of the physical vacuum, which gives a zero value for the cosmological constant. After a cosmic catastrophe, the energy density of the perturbed vacuum may be huge, of the order of the Planck energy scale. Still, if the cosmic catastrophe occurs in the original Minkowski vacuum (i.e., with $\mu=\mu_0$), the state with a huge cosmological constant will relax back to the Minkowski state with zero cosmological constant (see Figs. 1--5 in Ref. [CIT]).
| 890 |
1601.04676
| 13,105,402 | 2,016 | 1 | 18 | false | true | 1 |
UNITS
|
Moreover, from the CMB normalization, $A_s=\frac{1}{24\pi^2},\frac{V_*}{\epsilon_*}\simeq 2.196\times 10^{-9}$, at the Planck pivot scale of $k=0.05,{\rm Mpc}^{-1}$, we obtain FORMULA Then, the sufficient number of efoldings and the spectral index constrain the following combination of the model parameters, FORMULA Therefore, we can express the model parameters in terms of the tensor-to-scalar ratio $r$, $N_{\rm max}$ and $\cos\Theta$ as FORMULA
| 450 |
1601.05979
| 13,119,607 | 2,016 | 1 | 22 | true | true | 1 |
UNITS
|
In 1997 Pinkse *et al.* [CIT] experimentally demonstrated that adiabatically changing the trap shape could increase the phase-space density of an atomic gas by up to a factor of two and conjectured that this effect could be exploited to cross the BEC transition in a thermodynamically reversible fashion. This scenario was subsequently realised in the MIT group by Stamper-Kurn *et al.* [CIT] by slowly ramping on a tight "dimple" trap formed from an optical dipole potential on top of a weaker harmonic magnetic trap. This experiment was the setting for the first application of a stochastic Gross--Pitaevskii methodology [CIT], previously developed from a nonequilibrium formalism for Bose gases by Stoof [CIT]. This is based on the many-body T-matrix approximation, and uses the Schwinger--Keldysh path integral formulation of nonequilibrium quantum field theory to derive a Fokker-Planck equation for both the coherent and incoherent dynamics of a Bose gas. The classical modes of the gas were represented by a Gross--Pitaevskii equation, with additional dissipative and noise terms resulting from a collisional coupling to a thermal bath with a temperature $T$ and chemical potential $\mu$.
| 1,195 |
1601.06197
| 13,121,367 | 2,016 | 1 | 22 | false | true | 1 |
FOKKER
|
- Out of the 71 clusters with $Y_X$-based mass listed in Planck Collaboration et al. (2014), 11 are also in Table 1. The mass comparison is shown in Fig. 10. There is a good agreement, except for Abell 1795, a cluster with a complex X-ray morphology (a cavity, a cold front, and a cooling wake; see Walker et al. 2014 and Ehlert et al. 2015 and references therein). Although the agreement is promising, we emphasize once more that because the parent sample (the 71 clusters with $Y_X$) does not have a selection function, this comparison should be taken with caution, as discussed in detail for the larger sample of the Planck clusters in our Appendix B.
| 654 |
1601.06912
| 13,126,765 | 2,016 | 1 | 26 | true | false | 2 |
MISSION, MISSION
|
As shown by [CIT], the CPL expression (and alike) is not exempt of pitfalls either. Moreover, Figure REF indicates that some tension exists between Planck outputs and CFHTLensS weak lensing data [^1] [CIT], leadind to include values $|w_a| \gg 1$ in the likelihood ellypse, for which a CPL parametrization [eq. (REF)] looses significance [CIT].
| 344 |
1601.07230
| 13,129,176 | 2,016 | 1 | 26 | true | false | 1 |
MISSION
|
It is important to note that the critical temperature, $T_C$, we found here is three times lower than the Planck temperature. This means that our calculations are under control and quantum gravity corrections will not ruin the result. We indeed used the process of black hole production by two particles, but this is purely classical process as long as the energy densities and temperatures are below the Planck scale.
| 418 |
1601.07563
| 13,132,997 | 2,016 | 1 | 27 | false | true | 2 |
UNITS, UNITS
|
The Drummond-Hathrell contribution to the light deflection is negligibly small with respect to the Euler-Heisenberg one if FORMULA Note that the higher-order curvature/derivative terms are also suppressed in comparison with the Euler-Heisenberg term. The angle of the light deflection could be of the order one or even larger with respect to the standard result of general relativity (GR) if FORMULA where the lower bound is due to our assumption $|\delta{c}_U/c| \lesssim 1/10$. Therefore, we come to a conclusion that the black-hole evaporation considerably influences the light propagation if the black-hole mass is sufficiently small, i.e. FORMULA Note that the condition REF(#eq:dh-less-eh){reference-type="eqref" reference="eq:dh-less-eh"} as well as the weak gravity condition are then automatically satisfied if the black-hole mass lies in this range. However, the semi-classical approximation is reliable if the black hole is not too small, namely $M \gg M_\text{Pl}$ should be fulfilled. Thus, the above effects of the black-hole evaporation on the low-energy electromagnetic wave propagation are still trustable if the black-hole mass $M$ is much bigger than the Planck mass $M_\text{Pl}$, so that $M_\text{Pl} \ll M \lesssim 10^{19},M_\text{Pl}$.
| 1,258 |
1602.01475
| 13,150,817 | 2,016 | 2 | 3 | false | true | 1 |
UNITS
|
In this paper we set up to investigate the effects induced by noncommutativity on the coupling of matter to gravity. For that purpose, the dynamics of the scalar matter in the background of the BTZ geometry [CIT] has been sampled out as a working model for describing the matter coupled to gravity. On the other hand, as a conceptual framework for mimicking the noncommutative nature of spacetime at the Planck scale, the $\kappa$-deformed Minkowski spacetime has been envisioned as a convenient and sufficiently general one, as explained above. Likewise, it is noteworthy that a non-smooth, grain-like nature of spacetime calls for a different types of symmetries which are compatible with it, since those embraced by the ordinary Poincaré are not. Symmetries that underlie $\kappa$-deformed systems are however embodied within the $\kappa$-deformed Poincaré algebra [CIT], a specific type of quantum deformation of the Poincaré algebra.
| 938 |
1602.01488
| 13,151,197 | 2,016 | 2 | 3 | false | true | 1 |
UNITS
|
The strength of the signal, parameterized by $\Lambda$, is a combination of the higher-dimensional Planck mass, and the scale $r_1$ determining the density of the wavefunction in the extra dimensions, as in REF(#Lambdarel){reference-type="eqref" reference="Lambdarel"}. If $r_1$ is the same scale as $1/m_1$, as might be typically expected, this then determines $M_D$. Specifically, in the example of RS1, this happens through REF(#rsl_m5){reference-type="eqref" reference="rsl_m5"}, which with $\Lambda=60$ TeV, determines $M_5=33$ TeV.
| 537 |
1602.02793
| 13,163,673 | 2,016 | 2 | 8 | false | true | 1 |
UNITS
|
The spectrum is contained in $[-E, \frac{ 8 \hbar^2}{ 2 \mu^2} -E]$. Hence $\mu$ determines the maximal energy and, by duality, the minimal step-size. This is analogous to loop quantum cosmology, where the minimal step-size is set by the Planck scale and the energy density is bounded by the Planck density [CIT].
| 313 |
1602.03237
| 13,168,123 | 2,016 | 2 | 10 | false | true | 2 |
UNITS, UNITS
|
The performed numerical studies are illustrated with plots in Figs.,REF, REF. It is worth noting that the region $\Delta m^2\gtrsim 100$,eV$^2$ is excluded for $\sin^22\theta>0.1$ by the peak searches in $\beta$-decays, the strongest limits are placed by the Troitsk $\nu$-mass experiment, [CIT]. Note also, that sterile neutrino of mass $m_s\simeq 1$,eV noticeably changes the cosmological prediction of the standard $\Lambda$CDM model. In particular, the Planck experiment [CIT] excludes masses above $0.5$,eV for the fully thermalized sterile neutrino. However, this cosmological limit considerably depends on the cosmological data set used in the analysis. Also, this limit is inapplicable if the sterile neutrinos are not thermalized in the early Universe plasma of the Standard Model particles, which can happen in specific extensions of the Standard Model, see e.g., [CIT]. Thus, cosmology still allows for the presence of light sterile neutrinos (introduced to explain the Gallium anomaly) with extended particle physics and/or cosmological model. In turn, direct searches for light sterile neutrinos, like that provided by BEST, can test such extensions.
| 1,163 |
1602.03826
| 13,173,270 | 2,016 | 2 | 11 | true | true | 1 |
MISSION
|
In this paper we showed that the vacuum energy density in a theory with matching commuting and anticommuting degrees of freedom is equal to zero. This may or may not have bearing on issues related to the smallness of the cosmological constant $\rho_{\Lambda}=1.48\pm0.11\times 10^{-123}\rho_{Planck}$ ([CIT]) for several reasons. First we could not in our approach generate any small quantity. If one considers a model with mismatching degrees of freedom then the corresponding vacuum energy density will be proportional to $\Lambda^4f(N)$ where $\Lambda$ is the cut-off of the theory and $f(N)$ is an integer function of the degrees of freedom and thus cannot be small. Thus our results agree with the standard estimates for the vacuum energy density for theories outside the class considered here. On the other hand our results refer exclusively to the Minkowski space and we do not know in what measure a curved space time may alter them. According to some authors [CIT] it is possible that the space time curvature may have tiny effects on the vacuum energy. If this is the case in our context the smallness of the cosmological constant may be associated to these effects.
| 1,176 |
1602.06146
| 13,192,462 | 2,016 | 2 | 19 | false | true | 1 |
MISSION
|
Fig. REF shows that the simplest T-models with $n=1$ are vulnerable for $N_k\lesssim54$ since they leads to $n_s$ which is out of $1\sigma$ confidence region from the Planck 2015 data although it is still in $2\sigma$ confidence region. On the other hand, considering the upper bound on the tensor-to-scalar ratio $r< 0.07$ (95% CL) by BICEP2/Keck plus Planck data [CIT], this figure indicates that T-models with $n=1$ and $\alpha>25$ are unfavorable.\ Fig. REF displays the behavior of $n_s$ and $r$ for T-models with $n=2$. In this case, $N_k\lesssim53.5$ leads to $n_s$ which is out of $1\sigma$ region but it is still in $2\sigma$ region. On the other hand, the maximum allowable value for $\alpha$ which keeps $n_s$ within 95% CL is $\alpha=7$.\ From Fig. REF, the starobinsky model ($\alpha=1$) is a bit unfavorable for $N_k<52$ as it is out of $1\sigma$ region, but for $\alpha\geq 5$, E-models are very safe as compared to Planck data (68% CL). However, $r$ varies very slowly with $\alpha$ for E-models.
| 1,012 |
1602.07914
| 13,207,057 | 2,016 | 2 | 25 | true | true | 3 |
MISSION, MISSION, MISSION
|
The extreme and uncertain degree of host-galaxy dust reddening toward SN 2015Umakes estimating bolometric properties quite difficult. In §[3.1] we assume that the emission from SN 2015Uis roughly blackbody in spectral shape; here we further discuss this assumption. It has long been known that the continua of young SNe II exhibit "diluted blackbody" spectral energy distributions (SEDs), which (at optical wavelengths) are similar to the Planck function at a lower temperature [e.g., [CIT]]. Though SN 2015Uis certainly not a SN II, it is continuum-dominated, and in the sections above we present evidence that SN 2015Uwas shrouded in an optically thick CSM. In addition, [CIT] show that modeled shock breakouts from the hydrogen-dominated CSM around red supergiants exhibit roughly blackbody SEDs. [CIT] explore shock breakouts from He or He/CO stellar envelopes in detail; for He-dominated stellar envelopes, they show that the colour temperature of the system deviates from the photosphere's temperature by a (time-dependent) factor of only $\sim20$%, largely owing to diffusion effects as a helium recombination wave moves through the material.
| 1,149 |
1603.04866
| 13,265,998 | 2,016 | 3 | 15 | true | false | 1 |
LAW
|
I will focus on the perturbation growth in the matter domination phase, starting from the matter-radiation equality at about $z_{\rm eq} \approx 3370$ to $z_\Lambda \approx 0.5$ when the vacuum energy takes over. Setting the sound speed to be zero, one obtains the well-known result that the dark matter perturbation grows linearly with the scale factor $a$ (or equivalently $t^{2/3}$) in the matter domination phase. For negligible self-interactions, one finds the usual Jeans instability scale FORMULA where $\bar{\rho}_0$ is the current dark matter energy density and $M_p = 1/\sqrt{8\pi G} = 2.4 \times 10^{18}$ GeV is the reduced Planck scale. For length scale below the Jeans scale $L_J=2\pi/k_J$ or equivalently $k > k_J$, quantum pressure due to the uncertainty principle (an increase in momentum delocalizes the particles more) dominates. In this case, the density perturbation stops growing and oscillates with time. Since the comoving Jeans scale is almost scale invariant, perturbation growth below $k_J$ generates a sharp break in the matter power spectrum at about $k_J^{\rm eq}$, the comoving wavenumber at the matter-radiation equality [CIT]. The Jeans scale in this case is also roughly the de Broglie wavelength of the particle in the ground state. When dark matter mass is around $10^{-22}$ eV, more careful numerical studies show that the power spectrum drops at about 4.5 Mpc$^{-1}$ and could give reasonable fits to the data of dwarf spheroidal galaxies [CIT].
| 1,482 |
1603.06580
| 13,281,948 | 2,016 | 3 | 21 | true | true | 1 |
UNITS
|
In LED scenario, RN metric can be written as follows [CIT] FORMULA where FORMULA and $d\Omega^2_{D-2}$ is the line element on the $(D-2)$-dimensional unit sphere and the volume of the $(D-2)$-dimensional unit sphere is given by $\Omega_{D-2} = \frac{2\pi^{\frac{D-1}{2}}}{\Gamma(\frac{D-1}{2})}$. The mass and electric charge of the black hole are given by FORMULA Here, $G_D$ is gravitational constant in $D$-dimensional spacetime such that in ADD model is given by FORMULA where $M_{Pl}$ is the $D$-dimensional Planck mass and there is an effective 4-dimensional Newton constant related to $M_{Pl}$ by FORMULA where $R$ is the size of extra dimensions. It is necessary to note that in this work, the conventions for definition of the fundamental Planck scale $M_{Pl}$ are the same as which have been used by ADD. The location of the outer and inner horizons, determined by $F(r)=0$, are given by FORMULA and the horizon area is given by $A_D={\Omega_{D-2}}{r^{D-2}_+}$. Moreover, the entropy reads $S=\frac {A_D}{4}$.
| 1,019 |
1603.07976
| 13,295,014 | 2,016 | 3 | 25 | false | true | 2 |
UNITS, UNITS
|
In all but one case the zones were selected from Planck maps. To estimate masses above given cut-off level of the $N$-pdf, we adopted a linear conversion formula from dust opacity $\tau_{353}$ at 353 GHz to hydrogen column density: FORMULA as suggested in [CIT], with coefficients $C_0$ and $C_1$ obtained like in the work of [CIT]. The possible uncertainty of the calculated column-density is about a factor of 2. Comparing the derived mass-size relationships with our models, we prefer a conservative approach to neglect this uncertainty and cling only to estimates due to uncertainty of distance to the considered star-forming regions (see Table REF, column 2).
| 664 |
1603.08441
| 13,299,243 | 2,016 | 3 | 28 | true | false | 1 |
MISSION
|
Let us now consider the inclusion of the LGC data set in the cosmological fit. As discussed in Section REF and in Ref. [CIT], the measured amount of clustering of galaxies [CIT] is smaller than that obtained by evolving the primordial density fluctuations with the relatively large matter density at recombination measured precisely by Planck [CIT]. The correlation of a relatively large matter density and the clustering of galaxies can be quantified through the approximate relation $\sigma_{8} \propto \Omega_{m}^{0.563}$ [CIT] which relates the rms amplitude of linear fluctuations today at a scale of $8 h^{-1} \Mpc$, $\sigma_{8}$, with the present matter density $\Omega_{m}$. The value of $\sigma_{8}$ and the amount of clustering of galaxies can be lowered by adding hot dark matter in the form of sterile neutrinos with eV-scale masses[^4] to the cosmological model. The free-streaming of these sterile neutrinos suppresses the growth of structures at distances smaller than the free-streaming length, leading to a suppression of $\sigma_{8}$ with respect to the approximate relation $\sigma_{8} \propto \Omega_{m}^{0.563}$. In this way, the relatively large Planck value of $\Omega_{m}$ can be reconciled with the relatively small amount of local galaxy clustering in the LGC data set.
| 1,295 |
1603.09102
| 13,305,816 | 2,016 | 3 | 30 | true | true | 2 |
MISSION, MISSION
|
Having now established a relation between $\eta_{B}$ and $\eta_{X}$, the final ingredient is to relate the particle asymmetries to the mass density ratio of DM and baryons [CIT] FORMULA where $r_{\infty} \equiv n_{-}/n_{+}$ with $n_{\pm}$ being the number density of (anti-)DM. Notice that the fractional asymmetry, $r_{\infty}$ is not uniquely determined by the DM asymmetry $\eta_{X}$ but instead also depends on the annihilation cross section [CIT] FORMULA where $g_{*}$ is the relativistic degrees of freedom, $M_{{\rm Pl}}$ is the Planck mass, and $\langle \sigma v\rangle = \sigma_{0}(T/m_{X})^{n}$ where $n=0$ and $n=1$ are for $s$- and $p$-wave annihilation respectively. Lastly, $x_{f} = m_{X}/T_{f}$ is a dimensionless measure of the DM freeze-out temperature when DM annihilation processes cease being more rapid than the Hubble rate. This number is only logarithmically dependent on the DM mass and cross section, being typically $x_{f} \simeq 20$.
| 960 |
1603.09354
| 13,308,974 | 2,016 | 3 | 30 | false | true | 1 |
UNITS
|
SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.
| 937 |
1604.01050
| 13,322,922 | 2,016 | 4 | 4 | true | false | 2 |
MPS, MPS
|
The Sunyaev-Zeldovich amplitude, $y$, contains information about the properties of the galaxy cluster which in turn are sensitive to the cosmological parameters. The Planck collaboration as well as independent groups have used the $y$ maps created using the Planck data to study the clusters themselves as well as to measure the cosmological parameters (e.g., [CIT]) In particular, the Planck collaboration has used the $y$ parameter measurements of the Coma and Virgo cluster to constrain the average properties of these clusters [CIT]. Since these nearby clusters are well resolved by Planck, detecting $y$ signal out to several Mpc, it opens up the possibility of studying the $y$ fluctuations -- and hence the ICM pressure perturbations -- on large scales, complementing the X-ray studies focusing on smaller scales (e.g., [CIT] :2004; [CIT] :2012; [CIT] :2013 [CIT] and references within). The smallest scale we can study with Planck is limited by the angular resolution of $10'$ of the 100 GHz channel. We need the 100 GHz channel to be able to do component separation and minimize contamination from the other components.
| 1,128 |
1604.03106
| 13,341,604 | 2,016 | 4 | 11 | true | false | 5 |
MISSION, MISSION, MISSION, MISSION, MISSION
|
The ISW amplitude can be parametrized in terms of $A_{e\text{ISW}}$ and $A_{l\text{ISW}}$, which rescale the contribution of the ISW to the temperature anisotropies. A Markov-chain Monte-Carlo (MCMC) analysis was performed with a baseline standard $\Lambda$CDM model and flat priors on the parameters. [CIT] We also check the impact of a Gaussian prior $A_{l\text{ISW}} = 1.00\pm 0.25$, consistent with the 68% confidence level (C.L.) bounds on the same parameter from the estimation of the ISW-lensing bispectrum, which has been obtained by cross-correlating the PlanckCMB maps with the Planckmap of the lensing potential. Various datasets were tested: the high-$\ell$ Plancktemperature and temperature+polarization APS in the range $30\leq\ell<2500$ (hereafter $TT$ and $TT,TE,EE$, respectively) in combination with the low-$\ell$ Plancktemperature and polarization APS in the range $2\leq\ell<30$ (lowP). We also tested the WMAP APS including both temperature and polarization up to $\ell=1200$.
| 998 |
1604.03819
| 13,349,228 | 2,016 | 4 | 13 | true | false | 4 |
MISSION, MISSION, MISSION, MISSION
|
The dust opacities are calculated by Mie theory using the method by [CIT]. To calculate the opacity we assume a range of silicate and carbon particles between ($\rm a_{min}=5 \mu m$ and $\rm a_{max}=100 \mu m$) with a size distribution profile $\rm \sim a^{-3.5}$ and a silicate abundance of 62.5%. The profile of the dust opacity is plotted in Fig REF. For comparison we plot also opacity values by [CIT] and by [CIT] which assume slightly smaller dust sizes. To reduce the complexity of the problem we use gray opacities for the simulations. E.g. we define the Planck mean opacity as FORMULA with the Planck function $\rm B(\nu,T)$. We note that in this work we assume the same evaporation temperature for silicate and carbon grains. Especially refractory carbon grains could survive to higher temperatures. We will address this in a future work.
| 848 |
1604.04601
| 13,356,337 | 2,016 | 4 | 15 | true | false | 2 |
OPACITY, LAW
|
The resulting inflationary scenarios are in agreement with the Planck and the last BICEP2/Keck Array data and bring to an amount of inflation compatible with the thermalization of the observable universe. Note that as it is clearly seen from the explicit expressions for slow-roll parameters the analysis of Jordan frame inflation seems to be much more complicated than the corresponding analysis in convinient Einstein frame.
| 426 |
1604.06088
| 13,368,578 | 2,016 | 4 | 20 | false | true | 1 |
MISSION
|
It is known that a higgsino type of LSP in MSSM that is supposed to satisfy the PLANCK data on DM relic density has a mass of around 1 TeV. In pMSSM this obviously increases the electroweak fine-tuning due to the sufficiently large value of $\mu$. In contrast, NHSSM is able to produce a drastic reduction of the electroweak fine-tuning measure even for such a large mass of higgsino. The dependence of electroweak fine-tuning on $\mu$ rather than $\mu'$, the bilinear Higgs nonholomorphic parameter whereas the fact that electroweakino masses are related to the difference of $\mu$ and $\mu'$ indeed isolates the two sectors[^13]. The electroweak fine-tuning can either decrease or increase depending on the relative contributions of $\mu$ and $\mu'$ to the difference $\mu-\mu'$.
| 781 |
1604.06367
| 13,372,450 | 2,016 | 4 | 21 | false | true | 1 |
MISSION
|
Relations (REF)-(REF) prove to be very useful, since they allow us to compare the predictions of our scenario with the observational data. In particular, in Fig. REF we use (REF) and we present the estimated tensor-to-scalar ratio of the specific scenario (REF)-(REF) of inflation in unimodular $F(T)$ gravity, for two cases, on top of the 1$\sigma$ and 2$\sigma$ contours of the Planck 2013 results [CIT] as well as of the Planck 2015 results [CIT]. Additionally, in Fig. REF we use (REF) and we show the predictions of our scenario for the running spectral index $\alpha_\mathrm{s}$ on top of the 1$\sigma$ and 2$\sigma$ contours of the Planck 2013 results [CIT] as well as of the Planck 2015 results [CIT]. The agreement with observations is inside the 2$\sigma$ region for the tensor-to-scalar ratio and it is very satisfactory for the running spectral index. We mention that the agreement with observations is obtained through the unimodular construction, since taking $\lambda$ to zero, i.e. for $\alpha_2,\alpha_3\rightarrow0$, one arrives to unacceptable deviations.
| 1,074 |
1605.02461
| 13,420,487 | 2,016 | 5 | 9 | true | true | 4 |
MISSION, MISSION, MISSION, MISSION
|
In Table REF, these CMB priors are compared to the previous WMAP9 priors [CIT] that were used in and to Planck priors derived from temperature data only. Compared to, uncertainties on the priors are approximately divided by a factor of 5, with central values compatible within uncertainties. The gain on the cosmological constraints is detailed in Section [3]. We checked that the priors are consistent with those already derived by [CIT] using the 2013 data release from the Planck collaboration.
| 497 |
1605.02627
| 13,421,497 | 2,016 | 5 | 9 | true | false | 2 |
MISSION, MISSION
|
Fig. REF shows the shape of the reconstructed $f_\mathrm{esc} (z)$ using the non-parametric techniques described in Sect. [4]. Again, we marginalize over $C_\mathrm{HII}$, $\xi_\mathrm{ion}$, and $d M_\mathrm{SF} /dz$ (for the B15 model). The mean value of the escape fraction increases with increasing redshift due to our requirement of monotonicity. The recovered functions again demonstrate the strong consistency between the results obtained using the two GLFs. There is substantial variability in the allowed $f_\mathrm{esc} (z)$, with no obvious difference in the shapes that are allowed by Scorch compared to B15. Similar to Fig. REF, Planck 2016 lowE predicts a lower $f_\mathrm{esc}$ than Planck 2015 TT,TE,EE+lowP at all redshifts, as expected. However, the difference is relatively minor given the large difference in the measured values of the Thomson optical depth for these datasets.
| 897 |
1605.03970
| 13,437,074 | 2,016 | 5 | 12 | true | false | 2 |
MISSION, MISSION
|
The discussions above only adopt the SNLS3+BAO1d+Planck 2015+GF data. In this subsection, we explore the impact of adopting different types of observational data on the cosmic evolutions and the cosmic fates of $\Lambda$HDE. It should be pointed out that this topic has not been studied in the previous literatures.
| 315 |
1605.04356
| 13,440,659 | 2,016 | 5 | 14 | true | false | 1 |
MISSION
|
The gauge hierarchy problem has become more urgent with the discovery of the Higgs boson [CIT]. Although the SM is conceptually complete, the Higgs boson mass, together with the electroweak scale, is unstable against enormous corrections from loop processes, which pull the Higgs mass to the cutoff scale of the theory, for example, the Planck scale. This outcome can be avoided within the framework of the SM only with extreme fine tuning of the bare Higgs mass parameter, a situation that is regarded as unnatural, although not excluded. This problem suggests that additional symmetries and associated degrees of freedom may be present that ameliorate these effects. So-called natural SUSY models [CIT], in which sufficiently light SUSY partners are present, are a major focus of current new physics searches at the CERN LHC. In natural models, several of the SUSY partners are constrained to be light [CIT] : both top squarks, $\PSQt_L$ and $\PSQt_R$, which have the same electroweak couplings as the left- ($L$) and right- ($R$) handed top quarks, respectively; the bottom squark with $L$-handed couplings ($\PSQb_L$); the gluino ($\PSg$); and the Higgsinos ($\widetilde\Ph$). While the gluino mass is not constrained by naturalness considerations as strongly as that of the lighter top squark mass eigenstate, $\PSQt_1$, the cross section for gluino pair production is substantially larger than that for top squark pair production, for a given mass. As a consequence, the two types of searches can have comparable sensitivity to these models. Both types of searches are currently of intense interest, and CMS and ATLAS data taken at $\sqrt{s}=8\TeV$ have provided significant constraints [CIT] on natural SUSY scenarios.
| 1,725 |
1605.04608
| 13,442,088 | 2,016 | 5 | 15 | false | true | 1 |
UNITS
|
TR acknowledges support from The International Max Planck Research School on Astrophysics at the Ludwig Maximilian University Munich, EM & TM acknowledge support from the Max-Planck-Princeton Center for Plasma Physics, and MA, PCD, TR and MO acknowledge support from the European Research Council (grant CAMAP-259276). We also acknowledge support from grants AYA2013-40979-P and PROMETEOII/2014-069. The computations have been performed at the Leibniz Supercomputing Center of the Bavarian Academy of Sciences and Humanities (LRZ), the Max Planck Computing & Data Facility (MPCDF), and at the Servei d'Informàtica of the University of Valencia.
| 644 |
1605.05200
| 13,448,756 | 2,016 | 5 | 17 | true | false | 3 |
MPS, MPS, MPS
|
Indeed, notice that in the standard geometry of a collapse a generic spacetime point outside the horizon is *only a single Planck space-like distance away from the singularity*. This is counter-intuitive at first, but true, due to the Lorentzian nature of spacetime (see Figure REF). Therefore there is no surprise, nor violation of any known fundamental physical low that we know, if quantum effects leak outside the horizon. This cannot happen in quantum field theory over a fixed background, but there is no reason we know it should not happen when the full quantum dynamics of the gravitational field is taken into account, including the non-perturbative effects that are not accounted for by quantum field theory on curved spacetime. Here we see clearly the limitation of local quantum field theory. See [CIT], and in particular the contributions by Giddings and Rovelli therein, for a recent discussion of this essential point.
| 933 |
1605.05268
| 13,449,106 | 2,016 | 5 | 17 | true | true | 1 |
UNITS
|
To calculate the cross correlation coefficients between the $\gamma$-ray maps and dust opacity maps we first smooth both map into the same angular resolution. This is done by following the relation that $\sigma^2_{f}=\sigma^2_{s}+\sigma^2_{o}$, where $\sigma_{f}$ and $\sigma_{o}$ are the final and origin map resolution and $\sigma_{s}$ is the width of the smoothing kernel. The angular resolution for *Fermi*-LAT and beam width for Planck maps can be found in the calibration database (CALDB) files in *Fermi Science tools* and [CIT], respectively. If the point spread function has a gaussian form, the 68% containment angle is identical to $\sigma$ of the gaussian function by definition. Although the PSF of *Fermi*-LAT is not a perfectly gaussian [^4], the tail is not relevant for the analysis described here. Thus we assume for *Fermi*-LAT maps $\sigma_{o} = 0.35^{\circ}$. To make full use of the *Fermi*-LAT angular resolution we chose $\sigma_{f}$ to be $0.4^{\circ}$ in this work.
| 991 |
1606.00270
| 13,494,013 | 2,016 | 6 | 1 | true | false | 1 |
MISSION
|
As far as the other quantities are concerned, we find that the best-fit value of $\Delta_{\rm crit}$ is slightly larger for the model without He $\scriptstyle\rm II$data, as it allows higher contribution from the QSOs than the model with He $\scriptstyle\rm II$data. However, both the models support a much broader range for this parameter; $\Delta_{\rm crit}\sim25-60$ within the 2-$\sigma$ limits. Thus, our results do not vary considerably for the choice of $\Delta_{\rm crit}$ as long as it is within this limit. We also find that, the electron scattering optical depths $\tau_{\rm el}$ for all the best-fit models are in good agreement with the Planck 2016 value. Interestingly, when we include He $\scriptstyle\rm II$data, the best-fit model predicts slightly higher $\tau_{\rm el}$ than the other models, as it allows the highest stellar contributions among them.
| 870 |
1606.02719
| 13,515,460 | 2,016 | 6 | 8 | true | false | 1 |
MISSION
|
We show that if the $\alpha$-attractor model is realized by the spontaneous breaking of the scale symmetry, then the stability and the dynamics of the vector field that gauges the scale symmetry can severely constrain the $\alpha$-parameter as $5/6 < \alpha < 1$ restricting the inflationary predictions in a very tiny region in the $n_s - r$ plane that are in great agreement with the latest Planck data. Although the different values of $\alpha$ do not make a tangible difference for $n_s$ and $r$, they provide radically different scenarios for the post-inflationary dynamics which determines the standard BBN processes and the large scale isotropy of the universe.
| 668 |
1606.05308
| 13,535,528 | 2,016 | 6 | 16 | true | true | 1 |
MISSION
|
While the two lensing analyses (KiDS-450, CFHTLenS) and the pre-Planck CMB results are consistent with each other, with overlapping 1-$\sigma$ contours, there is tension between the KiDS-450 and Planck results, similar to that found for CFHTLenS. The tension with respect to Planck is significant at the $2.3$-$\sigma$ level. We explore concordance in the full parameter space in Section [1.9]. Note that a recent re-analysis of the Planck data [CIT] finds slightly different values for $\sigma_8$ and $\Omega_{\rm m}$ but essentially the same $S_8$. Hence the tension with respect to this KiDS-450 study is not affected.
| 621 |
1606.05338
| 13,538,076 | 2,016 | 6 | 16 | true | false | 4 |
MISSION, MISSION, MISSION, MISSION
|
Our internal consistency tests show some interesting results. While we expect to see a proper consistency between derived values of $H_0\ensuremath{r_\text{d}}$ using LOWZ and CMASS data considering both $d_A(z)$ and $H(z)$ observations, we realized some considerable tensions. Having the expansion history directly derived from supernovae data we noticed that only by considering lower values of $H_0\ensuremath{r_\text{d}}$ (around × 10^4^ km s^−1^ and also considering larger expansion history rate (darker lines in Fig. REF for $D(z)$), we can have consistent results between all measurements. This is particularly important looking at the results from CMASS data. This somehow supports the cosmological parameters from Planck concordance model cosmology (lower $H_0$ and higher $\ensuremath{\Omega_\text{m}}$) without using the cosmic microwave background data. Future surveys, such as DESI, will measure $H(z)\ensuremath{r_\text{d}}$ at several redshifts with smaller uncertainties. Using these values, we can test the flatness and the metrics in a wider range and with much higher precision and accuracy.
| 1,112 |
1606.06832
| 13,551,350 | 2,016 | 6 | 22 | true | false | 1 |
MISSION
|
We use the Planck 2015 lensing map provided by the Planck collaboration [CIT]. We convert the provided $\kappa_{l,m}$ values to a convergence map using healpy [CIT], with n$_\text{side} FORMULA =1024$, we test the effects of changing the pixel size (using n$_\text{side} FORMULA =512$ is somewhat greater than the smoothing scale in the lensing map, we do expect to gain some information by using smaller pixels with n$_\text{side} FORMULA =2048$ should not make a very significant difference except at very small scales, in case there is some information left in the lensing maps at those scales. Similarly, smoothing with a Gaussian beam with $\sigma=1'$ should not significantly affect our results given the resolution of the Planck maps and the scales used for our measurements, though $\sigma=10'$ should change the signal on scales up to the FWHM ($\approx25'$) of the smoothing kernel. Hence we will omit the measurements with $\sigma=1\arcmin$ and will show results with $\sigma=10\arcmin$ smoothing for comparison with the main results, which have no additional smoothing applied to maps.
| 1,097 |
1606.08841
| 13,569,743 | 2,016 | 6 | 28 | true | false | 3 |
MISSION, MISSION, MISSION
|
Substitution into Eq. REF(#eq:relevance){reference-type="eqref" reference="eq:relevance"} yields the critical or *Einstein--Cartan number density* $n_\text{EC} \approx m/(\kappa\hbar)^2$. Defining the reduced Compton wavelength of the fermion under consideration, $\lambda{}_\text{Compton} := \hbar/(mc)$, one finally has for the critical Einstein--Cartan density FORMULA For a typical nucleon, $m \approx 1,\text{GeV}/(c^2)$, and hence $\rho_\text{EC} \approx 10^{59}, \text{kg}/\text{m}^3$, which is much smaller than the reduced Planck density of $\rho{}_\text{Planck} = 10^{96}, \text{kg}/\text{m}^3$ at the big bang. For comparison, a typical nuclear density is $\rho_\text{nucl} = 10^{18}, \text{kg}/\text{m}^3$. Analogously, the *Einstein--Cartan length* scale $\ell{}_\text{EC} = \left(\lambda{}_\text{Compton}, \ell{}_\text{Planck}^2\right)^{1/3} \approx 10^{-29}, \text{m}$ is seven orders of magnitude larger than the reduced Planck scale $\ell{}_\text{Planck} \approx 10^{-36},\text{m}$.
| 999 |
1606.09273
| 13,574,601 | 2,016 | 6 | 29 | false | true | 5 |
UNITS, UNITS, UNITS, UNITS, UNITS
|
We thank Aleksi Halkola for his contributions to this project. This work is based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, and is supported by JSPS KAKENHI Grant Numbers JP15K17617, JP26800093, and JP15H05892. SHS gratefully acknowledges support from the Max Planck Society through the Max Planck Research Group. We thank the referee for a helpful report. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code freely available[^1]. The Pan-STARRS1 (PS1) Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy and the Max Planck Institute for Extraterrestrial Physics, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE).
| 2,331 |
1606.09363
| 13,575,489 | 2,016 | 6 | 30 | true | false | 5 |
MPS, MPS, MPS, MPS, MPS
|
We have extended our study to measure the sum of neutrino mass using different methodologies including double probe analysis (introduced in this study), full-likelihood analysis, and single probe analysis. We found that double probe has weaker constraint on the neutrino mass since it does not include the constraining power on the neutrino mass from Planck data. While including lensing information, we have performed the analyses with varying $A_{\rm L}$ or fixing $A_{\rm L}=1$. We found that varying $A_{\rm L}$ would shift the $\Sigma m_\nu$ to a larger value. From the full-likelihood analysis with varying $A_{\rm L}$, we obtained $\Sigma m_\nu=0.17^{+0.08}_{-0.13}$ assuming $\Lambda$CDM; $\Sigma m_\nu=0.34^{+0.17}_{-0.22}$ assuming o$\Lambda$CDM; $\Sigma m_\nu=0.33^{+0.16}_{-0.18}$ assuming $w$CDM; $\Sigma m_\nu=0.44^{+0.23}_{-0.22}$ assuming o$w$CDM. We found $\sim2\sigma$ detection of $\Sigma m_\nu$ when allowing $w$ and $\Omega_k$ to be free.
| 959 |
1607.03152
| 13,611,447 | 2,016 | 7 | 11 | true | false | 1 |
MISSION
|
The tachyon potential is derived from string theory and has to satisfy some definite properties to describe tachyon condensation and other requirements in string theory. However, Kofman and Linde have shown [CIT] that the slow-roll conditions are not compatible with a string coupling much smaller than one, and the compactification length scale much larger than the Planck length. This leads to the density fluctuations produced during inflation being incompatible with observational constraint on the amplitude of the scalar perturbations. This criticism is based on the string theory motivated values of the parameters in the tachyon potential, i.e., the brane tension and the parameters in the four-dimensional Newton constant obtained via conventional string compactification. Of course, if one relaxes the string theory constraints on the above mentioned parameters, the effective tachyon theory will naturally lead to a type of inflation which will slightly deviate from the conventional inflation based on the canonical scalar field theory. Steer and Vernizzi [CIT] have noted a deviation from the standard single field inflation in the second order consistency relations. Based on their analysis they concluded that the tachyon inflation could not be ruled out by the then available observations. It seems like the present observations [CIT] could perhaps discriminate between different tachyon models and disfavor or rule out some of these models (for a recent discussion on phenomenological constraints imposed by Planck 2015, see, e.g., ref [CIT]).
| 1,560 |
1607.04524
| 13,624,508 | 2,016 | 7 | 15 | false | true | 2 |
UNITS, MISSION
|
The scenario of Higgs compositeness [CIT] offers a powerful resolution to the Hierarchy Problem. The Standard Model (SM) Higgs degrees of freedom remain much lighter than the Planck scale in the face of radiative corrections because they are only assembled at $\sim$ TeV scale, as tightly bound composites of some new strongly interacting "preons". This is in close analogy to how the ordinary charged pion remains much lighter than the Planck scale in the face of QED radiative corrections, by being assembled as a quark-gluon composite at $\sim$ GeV. But despite the simple plot, composite Higgs dynamics is notoriously difficult to model in detail because it requires understanding a new strongly-coupled dynamics, operating outside perturbative control.
| 757 |
1608.00526
| 13,671,437 | 2,016 | 8 | 1 | false | true | 2 |
UNITS, UNITS
|
In fact, there has been a large number of work on the issue of investigating neutrino mass and dark radiation using cosmological observations in the literature. For example, [CIT] presented the effects of $N_{\rm eff}$ on the CMB peaks; [CIT] discussed forecasted constraints on massive neutrinos and dark energy; [CIT] presented constraints on massive neutrinos and dark energy with reference to clustering (but also contained physical descriptions); [CIT] presented constraints on massive neutrinos and dark energy after the first release of Planck mission. In addition, [CIT] discussed a variety of combinations to address the possible discordance between the Planck constraints and low$-$redshift probes. [CIT] considered a 12-parameter extended cosmological model that allows for dark energy, massive neutrinos and dark radiation, simultaneously; see also [CIT]. In particular, [CIT] recently considered constraints on the neutrino mass in the $w$CDM model and the holographic dark energy model (without and with the consideration of mass hierarchies, respectively).
| 1,071 |
1608.01219
| 13,677,121 | 2,016 | 8 | 3 | true | true | 2 |
MISSION, MISSION
|
The measure weight $v(x)\sim 1/|x|$ arises as the ultraviolet limit of a multifractional measure with logarithmic oscillations. In this limit, the fundamental scale $\ell_\infty$ appearing in the oscillatory part is factored out of the asymptotic measure as an overall constant. Thus, the theoretical problem of the disappearance of the Planck length in the $\kappa$-Minkowski cyclic-invariant measure was solved in [CIT] by regarding $\kappa$-Minkowski spacetime as the limit of noncommutative multifractional Minkowski spacetime and by identifying $\ell_\infty$ with the Planck scale. This embedding would be fully valid only if the symmetries of $\kappa$-Minkowski exactly matched those of the multifractional $q$-theory. Here we checked this correspondence at the level of the Heisenberg algebra and, in the next subsection, we will give another proof at the level of the Poincaré algebra. Therefore, the geometrical and physical interpretation of [CIT] is confirmed. Note that there is no contradiction between this result and the fact that we cannot identify multifractional field theories with noncommutative field theories, first because the embedding of $\kappa$-Minkowski in the multifractional framework is at the level of spacetime, not of field theory; and, second, because such embedding is of a noncommutative spacetime within another, while the negative results of the previous section involve noncommutative theories on one hand and commutative multifractional theories on the other hand.
| 1,505 |
1608.01667
| 13,682,008 | 2,016 | 8 | 4 | false | true | 2 |
UNITS, UNITS
|
Having described the shifts fairly pragmatically, we now turn to trying to understand what, physically, is driving them. It is clear that the oscillatory residuals are important, and qualitatively we can see that they look like extra smoothing of the peaks and hence resemble the effects of gravitational lensing. Indeed, along with the parameter shifts themselves, much attention has been given in the literature to the fact that the Planck high-$\ell$ data appear to favour an overly enhanced gravitational lensing potential with respect to that expected from $\Lambda$CDM [CIT]. Given this, and noting that the parameters shift to increase $A_{\rm s}$ and $\omega_{\rm m}$ (both of which increase the gravitational lensing potential) it may be tempting to think that the parameter shifts are dominantly driven by a desire to increase lensing and hence increase peak smoothing at high $\ell$. We will see, however, that this only explains about a third of the total shifts and instead most of the change in the best-fit model spectrum is related to non-lensing effects such as changing the matter envelope (Sect. [4.1]) and the primordial tilt (Sect. [4.4]).
| 1,160 |
1608.02487
| 13,689,379 | 2,016 | 8 | 8 | true | false | 1 |
MISSION
|
In this paper, we use the likelihood function for observations of CMB [CIT] and lensing by Planck, and low-$\ell$ polarization from the WMAP (WP) in the following form FORMULA where $\mathbb{C}$ is the covariance matrix with the errors, $\mathbf{x}$ is a vector of the acoustic scale $l_{A}$, the shift parameter $R$ and $\Omega_{b}h^2$ where FORMULA where $z^{*}$ is the redshift of the epoch of the recombination [CIT].
| 421 |
1608.03196
| 13,695,674 | 2,016 | 8 | 10 | true | false | 1 |
MISSION
|
To summarize, we have studied a scenario based on gauge-Higgs unification where the scale at which the Higgs quartic coupling vanishes in the SM corresponds to the KK scale of the 5D compactified spacetime. The KK scale is related with the 5D Planck scale. Since the 1st generation fermions are mostly localized at an orbifold fixed point, quantum gravity can give rise to operators involving four 1st generation fermions suppressed by the square of the 5D Planck scale. Hence, the 5D Planck scale, or equivalently the KK scale, determines the partial width of the $p \to \pi^0 e^+$ process induced by 5D Planck suppressed operators. We have thus obtained a correlation between the top quark mass, which controls the RG running of the Higgs quartic coupling, and the proton partial decay width. The correlation indicates that the future Hyper-Kamiokande experiment may discover the proton decay if the top quark pole mass is larger than about 172.5 GeV.\
| 954 |
1608.04065
| 13,702,784 | 2,016 | 8 | 14 | false | true | 4 |
UNITS, UNITS, UNITS, UNITS
|
Fig.,REF shows the ratio of the averaged power spectra with respect to the standard Bunch-Davies power spectrum in the standard inflationary scenario for the Starobinsky and quadratic potentials. The solid (red) and dashed (blue) curves correspond, respectively, to positive and negative $\dot\phi_{{}_{\rm B}}$. In all cases, there is suppression of power at $k\lesssim0.002 {\rm Mpc^{-1}}$ with respect to the standard BD prediction. Note that the form of this suppression is the same for both potentials and the two choices of $\dot\phi_{{}_{\rm B}}$. This property can be traced back to the fact that the underlying mechanism has its origin in the dynamics of perturbations in the well behaved Planck regime of LQC and Principle 1 implies that the bounce is highly kinetic energy dominated. Therefore the Planck scale dynamics is quite insensitive to the details of the potential. In this sense, the power suppression at $k\lesssim k_{\star} =0.002 {\rm Mpc^{-1}}$ is a robust feature of the Planck scale dynamics of LQC, supplemented with the two principles that provided us with the preferred background fields $\tilde{g}_{ab},, \phi$ and the quantum state $\psi$ of scalar perturbations. {width="47%"} {width="47%"}
| 1,288 |
1608.04228
| 13,703,947 | 2,016 | 8 | 15 | true | true | 3 |
UNITS, UNITS, UNITS
|
The coupled dark energy model provides a possible approach to mitigate the coincidence problem of cosmological standard model. Here, the coupling term is assumed as $\bar{Q}=3H\xi_x\bar{\rho}_x$, which is related to the interaction rate and energy density of dark energy. We derive the background and perturbation evolution equations for several coupled models. Then, we test these models by currently available cosmic observations which include cosmic microwave background radiation from Planck 2015, baryon acoustic oscillation, type Ia supernovae, $f\sigma_8(z)$ data points from redshift-space distortions, and weak gravitational lensing. The constraint results tell us there is no evidence of interaction at 2$\sigma$ level, it is very hard to distinguish different coupled models from other ones.
| 802 |
1608.07039
| 13,730,895 | 2,016 | 8 | 25 | true | false | 1 |
MISSION
|
Perhaps the most intriguing result of Planck's dust-polarization measurements is the observation that the power in the E-mode polarization is twice that in the B mode, as opposed to pre-Planck expectations of roughly equal dust powers in E and B modes. Here we show how the E- and B-mode powers depend on the detailed properties of the fluctuations in the magnetized interstellar medium. These fluctuations are classified into the slow, fast, and Alfv\'en magnetohydrodynamic (MHD) waves, which are determined once the ratio of gas to magnetic-field pressures is specified. We also parametrize models in terms of the power amplitudes and power anisotropies for the three types of waves. We find that the observed EE/BB ratio (and its scale invariance) and positive TE correlation cannot be easily explained in terms of favored models for MHD turbulence. The observed power-law index for temperature/polarization fluctuations also disfavors MHD turbulence. We thus speculate that the 0.1--30 pc length scales probed by these dust-polarization measurements are not described by MHD turbulence but, rather, probe the large-scale physics that drives ISM turbulence. We develop a simple phenomenological model, based on random displacements of the magnetized fluid, that produces EE/BB $\simeq2$ and a positive TE cross-correlation. According to this model, the EE/BB and TE signals are due to longitudinal, rather than transverse, modes in the random-displacement field, providing, perhaps, some clue to the mechanism that stirs the ISM. Future investigations involving the spatial dependence of the EE/BB ratio, TE correlation, and local departures from statistical isotropy in dust-polarization maps, as well as further tests of some of the assumptions in this analysis, are outlined. This work may also aid in the improvement of foreground-separation techniques for studies of CMB polarization.
| 1,893 |
1608.08138
| 13,730,972 | 2,016 | 8 | 25 | true | false | 2 |
MISSION, MISSION
|
There is also a disparity between the spectral index $\nu\simeq 2.4$ measured for the TE/EE/BB/TT power spectra, $C_\ell \propto \ell^{-\nu}$, and that, $\kappa \simeq 3.67$, in the three-dimensional power spectrum, $P(k)\propto k^{-\kappa}$ expected in MHD turbulence. The two exponents are related through the Limber equation, Eq. (REF). If the three-dimensional power spectrum is well-approximated by a single power law over the relevant distance scales, then the two-dimensional power spectrum $C_\ell$ will also be a power law and, moreover, with the same spectral index, $\nu=\kappa$. Given that the maximum distance from which we see dust emission (at least at high Galactic latitudes) is $r_{\rm max} \simeq 100-200$ pc, the range of physical length scales probed by Planck measurements over $\ell\simeq 30-600$ is roughly $L\sim 0.1-30$ pc, where $L=2 \pi/k$.
| 868 |
1608.08138
| 13,734,161 | 2,016 | 8 | 25 | true | false | 1 |
MISSION
|
CMB data is associated with each point on the spherical sky. So in order to apply the TMFCode, we use stereographic projection of the CMB field onto a plane. We calculate $W_2^{1,1}$, and then compute $\alpha$ and $\beta$ as functions of different threshold levels for simulated Gaussian and isotropic CMB temperature and $E$ mode fields. We find that the standard $\Lambda$CDM predicts that the level of intrinsic anisotropy of hotspots and coldspots in both the CMB fields to be $\beta = 0.62$, where correction due to pixelization has been taken into account. Further, we find the value of $\alpha$ to be one for botih temperature and $E$ mode fields, which implies that there is no net orientation in the structures of these fields. This is a recovery of the statistical isotropy of density fluctuations that we have input into the CMB simulations. Then, we use TMFCode to compute $\alpha$ and $\beta$ for temperature and $E$ mode data from PLANCK mission. We find that $\beta$ for both temperature and $E$ mode data are consistent with the expectations from standard $\Lambda$CDM simulations within $3-\sigma$. Further, we find that the temperature field agrees with the standard $\Lambda$CDM prediction of no net orientation within $3-\sigma$. However, we find $14-\sigma$ evidence for a net orientation in $E$ mode data. The reason behind this may be instrumental effects that we have not included in the simulated CMB maps, or this may be due to the contamination present in the PLANCK $E$ mode data. This may also be a signature of the existence of some net orientation in the structures of the $E$ mode field. The exact reason can only be revealed by further investigation and we plan to come back to this issue after the PLANCK team releases the full polarization data.
| 1,780 |
1608.07452
| 13,735,029 | 2,016 | 8 | 26 | true | false | 3 |
MISSION, MISSION, MISSION
|
Under the same condition which allows the Planck function to be simplified, $\kappa_{\mathrm{\mathrm{ff}}} (x,y,z)$ can be re-expressed as a function of frequency and temperature such that FORMULA This expression retains its spacial dependence due to $n_{\mathrm{e}}$ and $n_{\mathrm{i}}$, which are the local electron and ion number densities respectively. $_{\mathrm{ff}}$ is the free-free Gaunt factor (see Section [3.4]) given by: FORMULA [CIT].
| 449 |
1608.08380
| 13,743,177 | 2,016 | 8 | 30 | true | false | 1 |
LAW
|
We review the uncertainties in high-z star-formation rate (SFR) measures and the constraints that one obtains from high-z gamma-ray burst (GRB) rates on them. We show that at the present time, the GRB rates per unit star-formation at z>3 are higher than at lower redshift. We also compare metallicity predictions made using a hierarchical model of cosmic chemical evolution based on two recently proposed SFRs, one based on the observed galaxy luminosity function at high redshift and one based on the GRB rate and find that within the considerable scatter in metal abundance measures, they both are consistent with the data. Analyzing the ensemble of different measurements together, we conclude that despite metallicity biases, GRBs may be a less biased probe of star-formation at z>3 than at z<2. There is likely to be a common origin to the high GRB rate per unit star-formation and the high observed Lyman-continuum production rate in high redshift galaxies and that this may be due to a relative overabundance of stars with mass $>$25Msun which are likely GRB progenitors. We also find that to reconcile these measurements with the Thomson scattering cross section of cosmic microwave background (CMB) photons measured by Planck, the escape fraction of Lyman-continuum photons from galaxies must be low, about 15 percent or less and that the clumping factor of the IGM is likely to be small, about 3. Finally, we demonstrate that GRBs are unique probes of metallicity evolution in low-mass galaxy samples and that GRB hosts likely lost a significant fraction of metals to the intergalactic medium (IGM) due to feedback processes such as stellar winds and supernovae.
| 1,672 |
1609.00764
| 13,754,786 | 2,016 | 9 | 2 | true | false | 1 |
MISSION
|
For all our analysis, we use the Planck TT,TE,EE+lowP+lensing+BAO fiducial cosmology for all our calculations; $\Omega_m = 0.3089$, $\Omega_\Lambda = 0.6911$, and $h = 67.74{\rm km/s/Mpc}$. We use for data the NILC - MILCA F/L cross-power spectrum after foreground subtraction as described in [CIT] and the ACT value at high $l$ from [CIT].
| 340 |
1609.01850
| 13,768,305 | 2,016 | 9 | 7 | true | false | 1 |
MISSION
|
In this work we showed that by embedding simplified dark matter models in a general $E_6$ and $SO(10)$ grand unification theory constructions, we can combine and use the complementary of spin independent and spin dependent constraints from direct detection with LUX and PICO data, and observations from Planck, to derive stringent bounds on the thermally produced dark matter scenario and exclude dark matter masses below $\sim 100$ GeV in several different models in this setup without specific assumptions on the dark matter couplings. Collider analysis have been performed in general extensions of the standard model involving a $Z^\prime$, and combining cosmological measurements and constraints from the upcoming direct detection experiments and results from run II of the LHC will be a powerful tool to probe a larger parameter space in our framework and might lead to a reconsideration of the thermally produced dark matter paradigm.
| 940 |
1609.02424
| 13,773,534 | 2,016 | 9 | 8 | false | true | 1 |
MISSION
|
Next, we want to compare with constraints from reionization. In this case the comparison is more complicated because the physics of the baryons plays a very important role. Establishing such bounds rigorously, in any given model of DM, requires dedicated studies of the evolution of the mass power spectrum in the quasi-linear regime and modeling of the intergalactic medium (IGM). Some work along these lines has been done by [CIT]. The limit on ULA mass from our analysis of the dSph data, $m_{22}<0.4$, gives a considerable small value for the CMB optical depth, $\tau$, which is in tension with the Planck+ Low-l WMAP 9 (Planck + WP) constraints on $\tau$, yet this is consistent with the Planck High Frequency Instrument (Planck+HFI) constraint. This demonstrates the power that future constraints on the epoch of reionization from CMB polarization will have to probe the nature of DM [e.g. [CIT]], and the importance of understanding possible low-$\ell$ polarization systematic errors that could be causing a tension between Planck and WMAP $\tau$ measurements. See appendix [9] for wider explanation on how we derived these constraints based on [CIT].
| 1,158 |
1609.05856
| 13,804,039 | 2,016 | 9 | 19 | true | true | 5 |
MISSION, MISSION, MISSION, MISSION, MISSION
|
Note that a modified dispersion relation like REF(#mod-disp){reference-type="eqref" reference="mod-disp"} may result from a theory which explicitly breaks Lorentz invariance near the Planck scale, like Hořava-Lifshitz gravity for example, but can also arise due to deformations of the Lorentz symmetries [CIT]. While many Lorentz-violating theories are ruled out by low energy quantum field theory---for example, all theories that predict a Planck-scale discreteness in a preferred frame [CIT] ---theories that merely deform the Lorentz symmetries are not immediately ruled out by these constraints.
| 599 |
1609.06891
| 13,813,674 | 2,016 | 9 | 22 | true | false | 2 |
UNITS, UNITS
|
Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is <http://www.sdss.org/>.
| 384 |
1610.00429
| 13,843,434 | 2,016 | 10 | 3 | true | false | 1 |
MPS
|
Given the internal consistency of the spectra, we proceed to calibrate the maps by cross-correlating with the Planck-2015 143 GHz temperature maps. The cross correlation of the D56 PA2 maps with the Planck maps is shown in Figure REF. Here we follow the same method as in [CIT] /etal/2014. We find the ACT x Planck (AxP) cross-spectra to be consistent with the ACT auto-spectra (AxA): their differences have a reduced $\chi^2$ of 0.68, 1.10, 1.17, with PTE of 0.93, 0.31, 0.22, for TT, TE and EE. No obvious shape dependence or anomalies are detected. The temperature calibration factor is found to be $0.998 \pm 0.007$. Cross-correlating the D5, D6, D56 PA1 maps with D56 PA2 gives relative calibrations of $1.002 \pm 0.012$, $0.996 \pm 0.01$, and $1.009 \pm 0.007$. We then rescale all the maps to have unit calibration. We do not calibrate our data to polarization data, but we test the cross-correlation of the D56 polarization maps with the Planck-2015 143 GHz Q and U maps. The spectra appear consistent, as shown in Figure REF, and the correlation implies an ACTPol polarization efficiency of $0.990\pm 0.025$.
| 1,117 |
1610.02360
| 13,861,561 | 2,016 | 10 | 7 | true | false | 4 |
MISSION, MISSION, MISSION, MISSION
|
In this section, we generalize the idea of the gravitational baryogenesis from a PBH [CIT] by taking the direct effect of the decay of the PBH mass $M(t)$. Since the scalar curvature $\mathcal{R}$ vanishes outside of the BH in vacuum[^9], we consider an operator such as in (REF). More generally, we can consider a class of higher dimensional operators[^10], FORMULA It can be further generalized to FORMULA where $F(\mathcal{R_{....}})$ is any scalar function made of the curvature tensors. For the square of the Riemann curvature of the Schwartzschild BH is given by[^11] FORMULA a non-vanishing chemical potential $\mu=a_n \partial_0 \left(\mathcal{R}_{\mu\nu\rho\sigma}\mathcal{R}^{\mu\nu\rho\sigma}\right)^n /M_*^{4n}$ is generated if the BH mass $M$ is decaying. Here we have introduced the reduced Planck scale, FORMULA where $G$ is the Newton constant. Note that the chemical potential is dependent on time through $M(t)$. It also changes with the distance $r$ from the BH. Since the Hawking radiation is generated by the Bogoliubov transformation between the vacua of quantum fields near the horizon and at far-infinity from the BH, the chemical potential near the horizon is relevant to generate the asymmetry of the Hawking radiation. The propagations of baryon and anti-baryon become different in the vicinity of the horizon, which shift the energy between them. Accordingly the generated asymmetry is proportional to the chemical potential evaluated at the horizon $r=r_H$. Here we note that even if we instead evaluate the chemical potential at, e.g., $r \simeq 2 r_H$, it does not change our conclusion very much (see the 2nd paragraph of Sec. [5]).
| 1,664 |
1610.02586
| 13,863,765 | 2,016 | 10 | 8 | true | true | 1 |
UNITS
|
In modern cosmology, the spatial topology of the Universe is an unresolved issue. The recent observational data measures the curvature density as $\Omega_k = 0.000 \pm 0.005$ ($95\%$, Planck TT+lowP+lensing+BAO) [CIT]. It is never manifest from the current observation to conclude if the Universe is flat, closed, or open. Apart from analyzing the observational data, investigating the primordial density perturbation in different topologies would give an insight for the topology of the Universe. Study of inflation in the closed and the open universe tells that there are models which is viable with the current observational data [CIT]. They predict some peculiar phenomena distinguishable from flat models, but they are still beyond the current observational resolution. Therefore, it is not very possible to rule out any specific topology from the cosmological studies at the current stage.
| 895 |
1610.04087
| 13,878,425 | 2,016 | 10 | 13 | false | true | 1 |
MISSION
|
A large number of protoclusters were discovered serendipitously using data from the Planck survey. The Planck all-sky (sub-)millimeter maps contain a large number of compact (unresolved) "cold" sources [CIT]. A large fraction of these sources are believed to be overdensities of star-forming galaxies in overdense regions at $z\simeq2-4$ with significant far-infrared emission redshifted into the 353--857 GHz frequency range [CIT]. The Planck selection resulted in over one thousand candidates over 26 % of the sky, of which about two hundred were followed up with Herschel to obtain higher resolution data. [CIT] -cacho15 showed that at least one of the structures is due to two overlapping high redshift structures along the line of sight, at $z\sim1.7$ and $z\sim2$. Although most of the Planck sources remain to be confirmed spectroscopically, the uniform selection method and the large survey area make this a highly promising new search technique. The Planck selection is also interesting because it complements other protocluster selections that are based on optical- and NIR-selected galaxies (relatively dust-free, star-forming galaxies and passive galaxies).
| 1,169 |
1610.05201
| 13,887,995 | 2,016 | 10 | 17 | true | false | 5 |
MISSION, MISSION, MISSION, MISSION, MISSION
|
A necessary requirement for REF(#model_action){reference-type="eqref" reference="model_action"} to describe post-inflationary physics is to reduce to the standard Einstein-Hilbert action after symmetry breaking. Thus, the quartic self-interaction term for the scalar field and the quadratic term for the Ricci scalar need to cancel out, implying $\alpha = \xi^2 / \lambda$. The model, therefore, is left with only two free parameters. Finally, the non-minimal coupling term in the action, at the stable point, reduces to $M_p^2 R / 2$ (where $M_p$ is the Planck mass) provided that $M_p = \sqrt{\xi / 3} \phi_0$.
| 612 |
1610.06478
| 13,900,905 | 2,016 | 10 | 20 | true | true | 1 |
UNITS
|
At last, our analysis reveals something interesting that seems to be important interpreting the Planck CMB angular power spectrum data. Considering Crossing functions along with the concordance model (as the mean function) and using Planck 2015 temperature data the probability distribution function of the Hubble parameter $H_0$ broadens towards larger $H_0$ values resulting to $H_0=69.4^{+1.76}_{-2}$ which shows proper agreement with all local observations [CIT]. This clearly reflects the fact that Planck CMB temperature data has no fundamental tension with the local $H_0$ measurements and there are in fact forms of the angular power spectrum that are fully consistent with Planck data as well as with local $H_0$ measurements. Setting a strong prior on $H_0$ from [CIT] while our mean functions are from the background concordance $\Lambda$CDM model, data suggest a systematic suppression at low and high multiples. This can hints towards some possible physical effects such as having running in the spectrum of the primordial fluctuations, having an additional relativistic species or a massive neutrino. However, analysis of the TE and EE data suggest something different as the marginalized confidence contours of $H_0$ broadens towards lower values (and higher values of matter density). In other words the tension between the Planck 2015 polarization data (EE and TE) and local measurement of $H_0$ from [CIT] seems to be serious and beyond model assumption or choice of parametric fitting.
| 1,504 |
1610.07402
| 13,909,784 | 2,016 | 10 | 24 | true | false | 5 |
MISSION, MISSION, MISSION, MISSION, MISSION
|
[CIT] :2014dba show that the scale-dependence of the pairwise kSZ signal can be used to constrain neutrino masses. In particular, the authors forecast 68% upper limits on the sum of the neutrino masses, $\sum m_{\nu} = 290$ meV, $220$ meV, $96$ meV for Stage II, Stage III, and Stage IV surveys, respectively. The authors further show that percent-level constraints on $\tau$ will improve these constraints to 120 meV, 90 meV and 33 meV, respectively. For comparison, [CIT] :2016qvy find $\sum m_{\nu} = 140\pm80,$meV, by combining data from SPT clusters with Planck CMB data and baryon acoustic oscillation data.
| 614 |
1610.08029
| 13,917,235 | 2,016 | 10 | 25 | true | false | 1 |
MISSION
|
Using the [CIT] aperture flux measurements at 44, 70, 100 and 143,GHz, a spectral index $\alpha$ and normalisation factor C were derived by fitting a function F(C,$\alpha$) = C $\times$ $\nu^{\alpha}$ ($\nu$ in GHz) with spectral index $\alpha$ and scaling factor $C$ to these Planck and IRAC,3.6,$\mu$m fluxes. Relying on the Levenberg-Marquardt least-square fitting minimisation routine MPFIT in IDL, we derived a best fitting spectral index $\alpha$ = -0.644$\pm$ 0.020 and normalisation factor C=1706.7$\pm$ 199.2,Jy. Figure REF shows the Planck fluxes reported by [CIT] indicated as black squares, with the red diamonds corresponding to flux measurements for Cas,A from other facilities. The best fitting power law is indicated as a solid black line. The data point at the highest Planck frequency is significantly higher compared to the extrapolation of this power law, due to an increasing contribution of thermal dust emission towards higher frequencies. The dashed red lines correspond to the lower and upper limits of this synchrotron spectrum calculated based on the uncertainties of the spectral index fitting results. These uncertainties on the synchrotron spectrum are considered in the synchrotron models at every photometric wavelength.
| 1,252 |
1611.00774
| 13,944,772 | 2,016 | 11 | 2 | true | false | 3 |
MISSION, MISSION, MISSION
|
As low-$\ell$ temperature data, we always employ the Planck`Commander` CMB map, obtained combining the Planckobservations between 30 and 857 GHz [CIT], the 9-year WMAP observations between 23 and 94 GHz [CIT], and the 408 MHz sky maps from [CIT] :1982zz, as described in Refs. [CIT] (see also Refs. [CIT] for a description of the `Commander` component-separation algorithm), The `Commander` map covers 94% of the sky and will hereafter be denoted as "PlancklowT".
| 463 |
1611.01123
| 13,947,440 | 2,016 | 11 | 3 | true | false | 3 |
MISSION, MISSION, MISSION
|
The Compton and Schwarzschild lines intersect at around the Planck scales, FORMULA and naturally divide the $(M,R)$ diagram in Fig. REF into three regimes, which for convenience we label quantum, relativistic and classical. (As discussed in Appendix [9], a more comprehensive discussion involves three dichotomies -- classical/quantum, non-relativistic/relativistic, weak-gravitational/strong-gravitational -- and different combinations of these then give $8$ possible regimes.) There are several other interesting lines in Fig. REF. The vertical line $M=M_{P}$ marks the division between elementary particles ($M <M_{P}$) and black holes ($M > M_{P}$), since the event horizon of a black hole is usually required to be larger than the Compton wavelength associated with its mass. The horizontal line $R=R_{P}$ is significant because quantum fluctuations in the metric should become important below this [CIT]. Quantum gravity effects should also be important whenever the density exceeds the Planck value, $\rho_{P} = c^5/(G^2 \hbar) \sim 10^{94} \mathrm {g, cm^{-3}}$, corresponding to the sorts of curvature singularities associated with the big bang or the centres of black holes [CIT]. This implies $R < R_{P}(M/M_{P})^{1/3}$, which is well above the $R = R_{P}$ line in Fig. REF for $M \gg M_P$, so one might regard the shaded region as specifying the 'quantum gravity' domain. This point has recently been invoked to support the notion of Planck stars [CIT] and could have important implications for the detection of evaporating black holes [CIT].
| 1,554 |
1611.01913
| 13,953,741 | 2,016 | 11 | 7 | false | true | 3 |
UNITS, CONSTANT, STAR
|
For several decades, the study of black hole (BH) thermodynamics has provided crucial information about the underlying structure of the spacetime. In particular, the fact that the BH entropy is proportional to the BH surface area in Planck units seems to tell us something important regarding the microstructure of spacetime.
| 325 |
1611.03525
| 13,966,497 | 2,016 | 11 | 10 | false | true | 1 |
UNITS
|
Fig. REF shows the thermal relic abundance of the first KK photon $\Omega h^2$ as a function of the compactification scale $1/R$ in the mUED model. The cases with $\Lambda R=5$ (red line), $20$ (orange) and $50$ (blue) are plotted from the top. The green band shows the DM abundance at the $2\sigma$ level determined by Planck [CIT]. Here, we include all the coannihilation processes taking the production of second KK particles into account. In computing the KK mass spectrum and the thermal relic abundance of $\gamma^{(1)}$, we use the same model files as Ref. [CIT] employs. Namely, these model files are generated by `LanHEP` [CIT] and implemented into `CalcHEP` [CIT] and `micrOMEGAs4.3` [CIT]. For the details of the computations, see Ref. [CIT]. The mass of the Higgs boson is set at $m_h^{}=125$ GeV. From this figure, the cosmologically favored compactification scale, which is roughly the mass of the fist KK photon $\gamma^{(1)}$, is shown to range typically from around $1300$ GeV to $1500$ GeV in the mUED model.
| 1,026 |
1611.06760
| 13,996,994 | 2,016 | 11 | 21 | false | true | 1 |
MISSION
|
Extensive efforts have been made to search for and identify such obscured star-forming galaxies in protoclusters at $z>2$, using submm/mm bolometer cameras onboard single-dish telescopes, such as AzTEC (e.g., [CIT].440.3462U), SCUBA (e.g., [CIT]), SCUBA2 (e.g., [CIT]), and LABOCA (e.g., [CIT]) as well as FIR to submm/mm satellites, including *Herschel* (e.g., [CIT].460.3861K) and Planck (e.g., [CIT]). While these single-dish telescopes are beneficial to cover wide area and find bright SMGs, their relatively poor angular resolution (FWHM $\gtrsim15^{\prime\prime}-30^{\prime\prime}$) and sensitivity limits due to source confusion have prevented us from obtaining accurate identifications for sources and/or revealing less extreme dusty galaxies. The advent of the Atacama Large Millimeter/submillimeter Array (ALMA) allows us to break through these limitations. Contiguous ALMA mosaic imaging is able to open a window for submm/mm deep surveys with sub-arcsec resolution (e.g., [CIT]). [^1]
| 996 |
1611.09857
| 14,026,679 | 2,016 | 11 | 29 | true | false | 1 |
MISSION
|
In the previous sections we have reported the constraints achievable from CORE-M5 on the $6$ parameters of the $\Lambda$CDM model and for one or two parameters extensions as, for example, the helium abundance and the neutrino effective number $Y_p+N_{\rm eff}$ (Section VI), or the neutrino mass and effective number $M_{\nu} + N_{\rm eff}$ (Section VII). In this section, along the lines of recent analyses as [CIT], we further extend the parameter space by considering $3$ or $4$ more parameters with respect to $\Lambda$CDM. The reason of this kind of analysis is clear: we need to assess the stability of the constraints under the assumption of $\Lambda$CDM. Moreover, if we extend the parameter space the CORE constraints will be clearly relaxed since degeneracies are present between the parameters. It is therefore useful to quantify how much future datasets as DESI will help in breaking these degeneracies and what is the gain of CORE-M5 in this case with respect to current results from Planck.
| 1,004 |
1612.00021
| 14,032,239 | 2,016 | 11 | 30 | true | true | 1 |
MISSION
|
The current accelerated expansion of the universe could be also explained by introducing modifications to general relativity and considering an energy content made just of dark matter and baryons and no dark energy. Several modified gravity scenarios have been proposed. One possible way to check for hints for modified gravity in the data, without relying on a particular model, is to introduce additional parameters to perturbation theory that can modify the evolution of the gravitational potentials $\Phi$ and $\Psi$ (see, for example [CIT]). For example, a now common approach, presented in the publicly available code `MGCAMB` [CIT] and also recently applied in [CIT] to the Planck data, is to firstly modify the Poisson equation for $\Psi$:
| 747 |
1612.00021
| 14,032,253 | 2,016 | 11 | 30 | true | true | 1 |
MISSION
|
SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.
| 937 |
1612.04748
| 14,079,462 | 2,016 | 12 | 14 | true | false | 2 |
MPS, MPS
|
In the 4 decades since those early tests, interest in Lorentz violation has surged [CIT], as have theoretical and experimental developments [CIT]. In addition to the search for preferred frame effects as a signal of alternatives to GR [CIT], more general types of Lorentz violation are now actively sought as a possible signal of new physics at the Planck scale [CIT]. Though performing Planck-scale experiments directly will likely remain infeasible for the foreseeable future, experimental information about the nature of the underlying theory can be attained by searching for tiny Planck-suppressed effects in experiments at presently accessible energies. Lorentz violation provides a useful candidate Planck-suppressed effect [CIT], and the gravitational Standard-Model Extension (SME) provides a field-theory based framework for organizing a systematic search [CIT]. While sensitivities to SME coefficients for Lorentz violation have been achieved in a variety of gravitational systems [CIT], including pioneering work with an atom-interferometer gravimeter [CIT], this work provides the first exploration of superconducting gravimeters in the SME framework and the first search for matter-sector Lorentz violation using gravimeters of any kind. Sensitivity improvements over prior gravimeter work [CIT] are achieved for 7 coefficients for Lorentz violation, and the best laboratory sensitivity to 6 coefficients not previously explored in gravimeter experiments is achieved. In some cases, sensitivities are improved by more than a factor of 10.
| 1,551 |
1612.08495
| 14,119,617 | 2,016 | 12 | 27 | false | true | 4 |
UNITS, UNITS, UNITS, UNITS
|
The observational results from the satellite borne experiment WMAP [CIT] and more recently Planck [CIT] have now firmly established the presence of dark matter (DM) in the Universe. Their results reveal that more than 80% matter content of the Universe are in the form of mysterious unknown matter called the dark matter. Until now, only the gravitational interactions of DM have been manifested by most of its indirect evidences namely the flatness of rotation curves of spiral galaxies [CIT], gravitational lensing [CIT], phenomena of Bullet cluster [CIT] and other various colliding galaxy clusters etc. However, the particle nature of DM still remains an enigma. There are various ongoing dark matter direct detection experiments such as LUX [CIT], XENON-1T [CIT], $\text{PandaX-II}$ [CIT] etc. which have been trying to investigate the particle nature as well as the interaction type (spin dependent or spin independent) of DM with the visible sector by measuring the recoil energy of the scattered detector nuclei. However, the null results of these experiments have severely constrained the DM-nucleon spin independent scattering cross-section and thereby at present, $\sigma_{\rm SI}>2.2\times 10^{-46}$ cm$^2$ has been excluded by the LUX experiment [CIT] for the mass of a 50 GeV dark matter particle at 90% C.L. Like the spin independent case, the present upper bound on DM-proton spin dependent scattering cross-section is $\sigma_{\rm SD} \sim 5\times 10^{-40}$ cm$^2$ [CIT] for a dark matter of mass $\sim 20$ to 60 GeV. The DM-nucleon scattering cross-sections are approaching towards the regime of coherent neutrino-nucleon scattering cross-section and within next few years $\sigma_{\rm SI}$ may hit the "neutrino floor". Therefore, it will be difficult to discriminate the DM signal from that of background neutrinos. However, if the DM is detected in direct direction experiments then that will be a "smoking gun signature" of the existence of beyond Standard Model (BSM) scenario as the Standard Model of particle physics does not have any viable cold dark matter candidate.
| 2,094 |
1612.08621
| 14,120,322 | 2,016 | 12 | 27 | false | true | 1 |
MISSION
|
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