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Additionally we can include the BAO information ($D_V/r_s$), where we however have to fix the sound horizon size $r_s$. In Figure REF we show the constraint using the sound horizon of Planck (blue contours) and WMAP9 (green contours). We use the sound horizon in co-moving units $r_s^{\rm Planck}(z_d) = 98.79,$Mpc$/h$ and $r^{\rm WMAP9}_s(z_d) = 102.06,$Mpc$/h$, which includes information about the Hubble constant. Our constraint on $D_V/r_s$ together with the sound horizon from the CMB allows tight constraints on $\Omega_m$, while the constraint on $\sigma_8$ does not improve significantly (see Table REF for details). | 625 | 1312.4611 | 11,002,388 | 2,013 | 12 | 17 | true | false | 2 | MISSION, MISSION |
In principle it is assumed that a low-energy effective description of quantum gravity phenomena can be considered as an expansion in energy over a mass scale, which is probably related to the Planck scale. The leading-order term in such an expansion comprises the ordinary Standard Model of elementary particle physics plus General Relativity. The next-to-leading order term is the minimal Standard-Model Extension (SME) [CIT], which is a framework to study and test Lorentz violation at energies much smaller than the Planck scale. The minimal SME includes all Lorentz-violating operators that are invariant under the gauge group of the Standard Model plus power-counting renormalizable. Since gravity itself is nonrenormalizable one may expect higher-order terms in the expansion to be made up of operators of nonrenormalizable dimension. These are included in the nonminimal SME. | 882 | 1312.4916 | 11,005,263 | 2,013 | 12 | 17 | false | true | 2 | UNITS, UNITS |
In Fig. REF we plot the improvement in the likelihood to the Planck data with respect to the best fit concordance model for each level of Crossing function. Green line is for the case where the mean function is fixed to be the best fit concordance model and the blue line is for the case where we allow the parameters of the mean function (concordance model) to vary. | 367 | 1401.0595 | 11,038,330 | 2,014 | 1 | 3 | true | false | 1 | MISSION |
Due to the Hawking radiation, a PBH with a mass $M$ emits particles and loses its mass [CIT]. The energy spectrum of the Hawking radiation are similar to the Planck distribution, FORMULA where $E$ is the total radiation energy, $T\equiv M_{\rm Pl}^2/M_0$ is the Hawking temperature, $g$ is the degrees of freedom of particles being radiated, and $\nu$ is the frequency of the particles. Note that a PBH emits only particles which are lighter than the Hawking temperature. [^1] | 476 | 1401.1909 | 11,051,811 | 2,014 | 1 | 9 | true | true | 1 | LAW |
The plan of the paper is as follows: in §[2] we review the main effects of varying cosmological parameters, including $f_b$ and radiation density, on CMB and BAO observations. In §[3] we present numerical predictions of the BAO feature for a set of models (selected to give a good match to WMAP) with varying matter density and $N_{\rm eff}$, and we derive a statistic based on the galaxy correlation function which is sensitive to $f_b$ and $N_{\rm eff}$, but cancels galaxy bias and dark energy to leading order. We summarize our conclusions in §[4]. Most of this work was completed before the Planck release in March 2013, so we mainly use WMAP-9 fit parameters [CIT] as our baseline. The adjustments post-Planck are moderate, and we discuss the implications of recent Planck results (Planck Collaboration, [CIT] -xvi) in §[3.3]. | 832 | 1401.3240 | 11,064,597 | 2,014 | 1 | 14 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
Holographic calculations of the entanglement entropy in higher dimensions also suggest this behavior. Using the AdS/CFT correspondence, the corner-induced logarithm from an angle $\theta$ and its analogs in arbitrary dimensions obey the scaling form [CIT] FORMULA where $L$ is the length scale set by the AdS curvature and $L_P$ is the Planck length, while the ellipses include a $\log^2(\ell/\delta)$ term for odd $d>1$. The Planck length arises from Newton's constant, which appears in Ryu and Takayangi's famous formula relating the entanglement entropy to an area of a minimal surface in the AdS space. [CIT] The factor $(L/L_P)^d$ scales appropriately for counting the degrees of freedom in $d$-dimensional space with the Planck length as a short-distance cutoff, and the cutoff-independent function $q(\theta)$ has been computed for $d<6$. In $d=1$, the coefficient indeed becomes precisely $c/3$, [CIT] and in $d>2$ other relations with conformal central charges can be found. [CIT] Thus it is natural to believe that the coefficient of the log term in our case $d=2$ is also proportional to some universal quantity like a central charge giving a measure for the degrees of freedom. Our results provide support for this idea. | 1,232 | 1401.3504 | 11,066,856 | 2,014 | 1 | 15 | false | true | 3 | UNITS, UNITS, UNITS |
To begin with, we check our cluster matching by visually inspecting the SDSS and WISE images for each of the PSZ1clusters that resulted in a redshift conflict in Section [3.1]. Our goal is to ensure that every PSZ1cluster is matched to the best possible redMaPPermatch. We emphasize that "best possible" does not mean correct; we sometimes find Plancksources that have no convincing redMaPPermatch. In such cases, we let the original match stand, with the expectation that subsequent analysis will confirm those clusters as poor matches. It should also be noted that "unconvincing" is a qualitative decision made by us based on the visual inspection. Quantitative tests will be presented in subsequent sections. Our visual inspection also revealed several Planckdetections where the SZ signal is likely to be affected by projection effects, i.e., there are multiple rich galaxy clusters along the line-of-sight of the Planckdetection. These clusters are flagged as such. | 970 | 1401.7716 | 11,108,844 | 2,014 | 1 | 30 | true | false | 3 | MISSION, MISSION, MISSION |
There are 245 PlanckSZ-detections in PSZ1labeled as confirmed that fall within the SDSS redMaPPerfootprint with an assigned redshift $z$ in the range $z\in[0.08,0.6]$. These have allowed us to identify three failures in the redMaPPercluster catalog. One (Planck1216) is a low ($z\leq 0.6$) redshift cluster missing from the redMaPPercatalog because of a combination of miscentering and angular masking, reflecting $\approx 0.5\%$ incompleteness in redMaPPer. One (Planck500) is a redshift failure because of bad photometry in the SDSS, and one (Planck617, Section [3.2]) has an unusually low richness because of bad SDSS photometry. Our estimate of the catastrophic failure rate for the SDSS redMaPPercatalog from this analysis is therefore $3/245\approx 1.2\%$. In addition, we identified 4 redMaPPerclusters as having two obvious galaxy concentrations, which can lead to large centering uncertainties (Planck728, 249, 472, and 587, Section [3.3]), and one obvious centering failure in redMaPPer(Planck113, Section [3.3]). Note that the centering failure rate of redMaPPeris, in fact, higher, as evidenced by utilizing high resolution X-ray data [CIT]. The low rate of miscentering identifications from this analysis reflects the fact that Planckcluster centering is noisy. | 1,274 | 1401.7716 | 11,108,861 | 2,014 | 1 | 30 | true | false | 7 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
3\) These perturbations are gaussian. In non-inflationary models, the parameter $f_{NL}^{\rm local}$ describing the level of the so-called local non-Gaussianity can be as large as $O(10^{4})$, but it is predicted to be $O(1)$ in all single-field inflationary models. Prior to the Planck data release, there were rumors that $f_{NL}^{\rm local} \sim 30$, which would rule out all or nearly all single field inflationary models. | 426 | 1402.0526 | 11,119,238 | 2,014 | 2 | 3 | true | true | 1 | MISSION |
**1)** The present status of the SM strengthens the status of the SM as a low energy effective (LEESM) theory of a cutoff system residing at the Planck scale, with the Planck mass $M_{\rm Pl}\simeq1.22\times 10^{19} \mbox{GeV}$ as a cutoff. It renders the now finite relationship between bare and renormalized parameters to have a precise physical meaning. We thus can calculate the parameters of the bare system residing at the Planck scale. | 442 | 1402.3738 | 11,150,518 | 2,014 | 2 | 16 | false | true | 3 | UNITS, UNITS, UNITS |
The Higgs discovery, together with the fact than non-SM physics has not yet shown up at the LHC, may have a dramatic impact on particle theory and particle physics all-together. We have shown that, under the conditions that the SM vacuum remains stable up to the Planck scale and that the quadratically enhanced Higgs mass counterterm exhibits a zero not far below the Planck scale, likely the SM largely summarizes the all-driving laws of physics which govern the evolution of the universe from its birth and possibly for all future. This likely brings high precision physics and high precision SM calculations in the focus of future developments as a tool to learn more about early cosmology. We note that close-by non-SM low energy emergent new physics is naturally expected to exist. The origin of dark energy or the strong CP problem definitely may find their solution in new not yet fully uncovered low energy emergent physics [CIT]. Should vacuum stability in the SM fail all this could be completely different [CIT]. | 1,024 | 1402.3738 | 11,150,566 | 2,014 | 2 | 16 | false | true | 2 | UNITS, UNITS |
The best constraint for $n_s$ is 0.00145 from Table REF for $10^6$ detectors, $1'$ beam, and 75% $f_{sky}$. For reference, the constraints from TT, EE, TE spectra alone is 0.00151. This is a factor of five improvement from current Planck best constraints (0.0073). We note that the gain over going to larger sky area plateaus once $f_{sky}$ hits 0.3 and adding BAO information helps by about 30%. For $n_s$, the major input that changes the constraints is $f_{sky}$. In the CMB only case, going from $10^4$ to $10^5$ $N_{\rm det}$ and from $10^5$ to $10^6$ $N_{\rm det}$ improves the constraints by 5-10% respectively. The improvement is better for smaller beam cases. Improvement from decreasing beam sizes per arc-minute is on the percent-level. | 747 | 1402.4108 | 11,153,170 | 2,014 | 2 | 17 | true | true | 1 | MISSION |
where $A$ is the cross-sectional surface area, $\epsilon$ = 0.9 is the emissivity, $B$ is the Planck function and $T$ is the temperature at each piece of the surface. Assuming a solar flux at 70 $\mu$m of $S$ at the distance of Haumea, $R$, then $T$ is calculated for an edge-on rotating body and | 296 | 1402.4456 | 11,156,355 | 2,014 | 2 | 18 | true | false | 1 | LAW |
Let us note that consistent formulation of renormalization group for both cosmological constant and Newton constant (related to the inverse $,\kappa,$ of the re-scaled Planck mass) is definitely impossible since we are working in the framework of the on-shell renormalization group. The form of the classical action (REF) and the counterterms (REF) indicate that there is no possibility to study renormalization of $\kappa$ in this framework, so in what follows we will pursue only the aim of constructing the renormalization group equations for effective charges $\lambda_1$, $\lambda_2$, $\lambda_3$ and $\lambda_4$, defined in (REF). One can also see this method as working in the Planck units, where all quantities become dimensionless. | 740 | 1402.4854 | 11,160,520 | 2,014 | 2 | 20 | false | true | 2 | UNITS, UNITS |
The largest $C_l$ residuals for the 5eV neutrino model are at $l>1000$ so these are at least within range of the possible CMB systematics such as lensing and beam profile effects discussed by [CIT]. The Planck power spectrum results agree with those of ACT [CIT] and SPT [CIT] at small scales, making systematics due to Planck beam smoothing less likely. Therefore we concentrate here on smoothing by lensing to improve the fit of the model at small scales. Lensing has been detected in the Planck CMB maps at a level comparable with the $\Lambda$CDM prediction [CIT]. Given the uncertainty about how to produce a plausible matter power spectrum from the neutrino model (see below) here we follow [CIT] and use an ad hoc lensing model based on equn A7 of [CIT]. We assume a constant magnification rms dispersion of $\sigma=0.0005$, a factor of 10 lower than previously used by [CIT] and so closer to the $\Lambda$CDM case (see their Fig. 3). The results of lensing the neutrino model with this assumed $\sigma$ are shown in Fig. REF. We see that the fit of the fourth, fifth and sixth peaks are improved, although the fourth peak demands still more smoothing. This is all reflected in the reduced $\chi^2=21.4$, down from $\chi^2=126.3$ for the unlensed model. Most of the significant residuals still lie at $l>1000$; when these are excluded the reduced $\chi^2=5.8$, down from $\chi^2=9.0$. But we must still conclude that formally the neutrino model is rejected and could only be rescued by appeal to an unknown further systematic effect in the CMB data. Meanwhile the $\Lambda$CDM model continues to produce a much better fit over a wide range of scales. | 1,657 | 1402.5502 | 11,166,470 | 2,014 | 2 | 22 | true | false | 3 | MISSION, MISSION, MISSION |
The purpose of this paper is twofold. First, we will show that the predicted spectral index for the axion hilltop inflation can be increased with respect to the hilltop quartic inflation case by including a relative phase between two sinusoidal functions. This gives a better fit to the Planck data. Second, we consider a UV completion of multi-natural inflation within supergravity(SUGRA)/string theory. This is because a viable inflation model can be easily realized for large decay constants close to the GUT or Planck scale, and because the string theory offers many axions through compactifications [CIT], some of which could play an important role in inflation. Also, non-perturbative dynamics which explicitly break the axionic shift symmetry can be studied rigorously in a supersymmetric (SUSY) framework. | 813 | 1403.0410 | 11,186,402 | 2,014 | 3 | 3 | true | true | 2 | MISSION, UNITS |
A separate but related method of determining the calibration factor $y$ is to compare ACT and Planck measurements of unresolved sources. Determining the flux density of a compact source requires both a calibrated map and knowledge of the relevant beam solid angle. Comparing Planck and ACT measurements can thus test our understanding of both instruments' beams. | 362 | 1403.0608 | 11,188,413 | 2,014 | 3 | 3 | true | false | 2 | MISSION, MISSION |
Figure REF and REF compare the ACT and Planck flux densities. For both frequencies, the linear fits were forced to pass through the origin (see Planck Collaboration XIV, 2011) to reduce the effect of source boosting, sometimes called Eddington bias, in the Planck data. Relaxing this constraint typically changes the slope of the fits by less than $1 \sigma$. At 148 GHz, the agreement is excellent, despite the evident scatter introduced by variability. ACT's flux densities agree with Planck's to within 1$\%$; from this comparison we find $y=1.002 \pm 0.028$. The uncertainties in flux density in the Planck measurements, at 30 to 40 mJy, are typically 10 times those in the ACT measurements: the size of the symbols used in the figures is roughly equivalent to the $1 \sigma$ Planck errors. | 794 | 1403.0608 | 11,188,417 | 2,014 | 3 | 3 | true | false | 6 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
We conducted several tests of the stability of these results on compact sources. First, as noted, allowing an unconstrained fit to the data changed the slope of the fits (and hence $y$) by less than $1\sigma$. Another test of the effect of possible Eddington bias in the Planck data was to drop the weakest sources (around 20$\%$ of the total). There was little effect on the values of the calibration factor $y$. We also repeated the fits with unweighted averages of the 2009 and 2010 ACT data, rather than inverse-variance weighted averages. At 148 GHz, using unweighted averages raised $y$ by 2$\%$ or less than 1$\sigma$. At 218 GHz, with J0217+017 omitted, the value of $y$ shifted only slightly, from 1.016 to 1.020. Next, we omitted all the 2008 ACT data, taken before Plancks launch. At 218 GHz, $y$ changed minimally from 1.016 to 1.004 (again excluding J0217+017). The same test at 148 GHz resulted in a small change in $y$, from 0.983 to $0.971 \pm 0.017$. Finally, we tried dropping $\sim$ 5 -10 sources at low Galactic latitude or those flagged in the PCCS as possibly contaminated by Galactic cirrus emission (with the CIRRUS flag $>$ 10; see Planck Collaboration XXVIII, 2013). Two of the 148 GHz sources dropped were known variables, J0253-544 and J0739+016. The result was to lower $y$ by $\sim 2 \%$ at 148 GHz, with a much smaller effect at 218 GHz. None of these tests resulted in a change of $y$ greater than 1$\sigma$. | 1,440 | 1403.0608 | 11,188,421 | 2,014 | 3 | 3 | true | false | 3 | MISSION, MISSION, MISSION |
Regarding inflation, the Coleman-Weinberg type of potential is a simple and well motivated one, since it naturally arises when loop corrections are taken into account, and it is typical for the new inflation scenario [CIT] where inflation takes place near the maximum. Recently it has been studied in [CIT] in a B-L extension of the Standard Model, and a few years ago in [CIT] in a GUT inflationary model. As shown in [CIT] in the context of the effective theory of inflation, Cosmic Microwave Background together with Large Scale Structure data prefer double-well inflaton potentials. The 2013 Planck data confirmed this result, and not surprisingly the Coleman-Weinberg potential considered here belongs to this class, and succeeds to reproduce the $n_s$ value and the r bound from the 2013 Planck release. However, in [CIT] the inflaton was minimally coupled to gravity. Setting $\xi=0$, although it is a popular choice, is often unacceptable as was pointed out in [CIT]. Non-minimal couplings are generated by quantum corrections even if they are absent in the classical action [CIT], and as a matter of fact the coupling is required if the scalar field theory is to be renormalizable in a classical gravitational background [CIT]. For early works on non-minimal inflation see for example [CIT] and references therein. | 1,323 | 1403.0931 | 11,191,428 | 2,014 | 3 | 4 | false | true | 2 | MISSION, MISSION |
The naturalness argument implies that some new physics should come in at the PeV scale to cut off the quartic divergence and make the $\phi$ mass natural. We will now explore some possibilities for what this PeV-scale physics can be. As in the more familiar hierarchy problem arising from the Higgs boson mass, the physics that explains why $\phi$ is light could arise from compositeness or from supersymmetry. Let us first address the less appealing case of compositeness. We could begin with a Dirac fermion $\chi$ charged under some SU($N$) gauge group, coupling to photons through the dimension-7 Rayleigh operator $\frac{1}{\Lambda_R^3} \chi{\bar \chi} F_{\mu \nu} F^{\mu \nu}$. Such an operator can be readily UV completed by loops of electrically charged particles that could also carry SU($N$) quantum numbers [CIT]. We could then imagine that SU($N$) confines, binding the $\chi$ particles into a composite scalar $\phi$ with a mass set by the compositeness scale, i.e. $\Lambda_{\rm comp} \sim m_\phi \sim 10 {\rm keV}$. In that case, we expect that FORMULA There are several reasons that this seems unlikely: first, it would require new charged particles at the weak scale, also charged under a hidden gauge group, that we have not yet seen. Second, it requires a light stable scalar in the composite sector, built out of fermionic constituents, whereas confinement typically favors pseudoscalars as the lightest states. (Glueballs are an exception, but more difficult to UV complete.) Third, it involves a gauge group that confines at the keV scale, which could pose cosmological difficulties (though our favored alternative is also cosmologically problematic). Finally, if nature has handed us a scale like $7 \times 10^{17} {\rm GeV}$ suppressing an operator, it would be disappointing if it is completed by such mundane physics. Instead, the obvious temptation is to view this very large scale as a fundamental one, near the Planck scale for a good reason rather than an accidental one. | 2,001 | 1403.1240 | 11,194,743 | 2,014 | 3 | 5 | false | true | 1 | UNITS |
To estimate the stellar age more reliably, one could adopt the average value from various Th/X chronometers, since the ages determined from different Th/X chronometers are consistent within uncertainties. The corresponding uncertainty of the average value is calculated with $\sqrt{\sum_i (\delta t)_i^2}/n$, where $(\delta t)_i$ denotes the error of the corresponding Th/X chronometer and $n$ is the number of the Th/X chronometers used in the calculations. In this way, the average age of all Th/X chronometers and the corresponding error are $16.35\pm 1.52$ Gyr. By taking the Th/X ages, whose $r$-fraction exceeds $60\%$ for the element X, as a group, the average cosmic age and the related error are $15.68\pm 1.95$ Gyr. This value is smaller than the average value on all Th/X ages, but it is still larger than the latest cosmic age $13.813\pm 0.058$ Gyr determined from Planck 2013 results [CIT], while they are still consistent within the uncertainties. It should be noted that if the cosmic age determined with the CMB data is indeed smaller than the stellar age, then there would be something wrong about either the Big Bang theory or the theory of radiometric dating. However, the uncertainty of $1.95$ Gyr is relatively large to confirm this age deviation. Since this uncertainty of determined cosmic age mainly originates from the error on thorium abundance observed in metal-poor star CS 22892-052, so future high-precision abundance observations on CS 22892-052 are needed to understand this age discrepancy. | 1,523 | 1403.1644 | 11,199,304 | 2,014 | 3 | 7 | true | false | 1 | MISSION |
The last term in the righthand side of Eq. (REF) represents the contribution to the emission coefficient coming from atoms that are collisionally excited. Since collisions are assumed to be isotropic, this term only contributes to Stokes $I$. The profile FORMULA is the normalized absorption profile of the multiplet (in the absence of magnetic fields, and under the hypothesis of unpolarized lower term). The quantity $B_T(\nu_0)$ is the Planck function in the Wien limit (consistently with the hypothesis of neglecting stimulated emission), at the temperature $T$. | 566 | 1403.1701 | 11,199,654 | 2,014 | 3 | 7 | true | false | 1 | LAW |
Another interesting feature is the value of the extrapolation at $z=0$ (as already pointed out and studied by Ref. [CIT]). While the error at $z=0$ is larger than the one from Planck [^1], it is fully compatible with it. It however points to the central value of the locally determined $H_0$ being slightly high. Here we use the Ref. [CIT] "world average\" value for $H_0$ obtained from the [CIT] determinations. | 412 | 1403.2181 | 11,203,600 | 2,014 | 3 | 10 | true | false | 1 | MISSION |
The parameters $M$ and $\phi_*$ are determined from the slow-roll parameters, which in turn are determined by $r$ and $n_s$. $V_0$ is fixed by the amplitude, $A_s \simeq 22.2 \times 10^{-10}$ [CIT], via Eq. REF. With ${\epsilon}, \eta$ and $\xi$ known, we also compute $n_t$, and the running of the spectral indices. In Table REF, we display the parameters of the model together with $n_t$, $\alpha_s$ and $\alpha_t$ for values of $n_s$ and $r$ within their $1\sigma$ uncertainties. The values of $M$ agree with (REF) modulo logarithmic corrections from the high field contributions to $N$. The predictions for $\alpha_s$ are within the 95% C.L. region favored by Planck data [CIT]. Note that $[V(\phi_*)]^{1/4}$ is of the order of $10^{16}$ GeV, the grand unification scale. | 775 | 1403.4578 | 11,227,929 | 2,014 | 3 | 18 | true | true | 1 | MISSION |
We now use the MCMC chains of [CIT] :2013rxa, where the neutrino mass is varied freely and importance sample these chains. The chains we use include the A$_{\rm L}$-lensing signal, meaning they do not marginalise over $A_{\rm L}$. The CMB lensing signal from the $4$-point function is not included. The result is shown in Figure REF (bottom), Figure REF and Table REF. Combining Spergel2013 with the results of [CIT] :2013b yields $\sum m_{\nu} = 0.24\pm0.12,$eV. Including CFHTLenS, GGlensing and further BAO constraints gives $\sum m_{\nu} = 0.29\pm0.10,$eV ($2.9\sigma$). These results are within $1\sigma$ with the results we obtained when importance sampling the Planck and the Planck-$A_{\rm L}$ chains. Overall we see small (below $1\sigma$) shifts towards WMAP. | 769 | 1403.4599 | 11,228,179 | 2,014 | 3 | 18 | true | false | 2 | MISSION, MISSION |
The fact that the thresholds are near $\sqrt { N }$ rather than $N^{1/4}$ is rather intriguing. This has been discussed in [CIT]. Angular momenta of $J \approx N^{ 1 / 4 }$ correspond to momenta comparable to the ten-dimensional Planck scale. This may be a sign that $AdS_5 \times S^5$ physics is just very different from expectations derived from effective field theory in flat space $\mathbb{R}^{ 9, 1 }$. On the other hand, it could be that a clever interpretation of the link between the extremal correlators and flat space scattering would account for the thresholds we see from the CFT. Potentially, the correct interpretation has to recognise that extremal correlators correspond to collinear graviton scatterings. We would need to consider the flat space expectations in the light of collinear effective theories of gravitons, along the lines developed in [CIT], to understand the difference between the threshold scale and the Planck scale. An early discussion of the subtleties of connecting bulk AdS spacetime physics to the flat space limit is given in [CIT]. | 1,071 | 1403.5281 | 11,237,085 | 2,014 | 3 | 20 | false | true | 2 | UNITS, UNITS |
The Planck satellite measured the dark matter abundance of the universe, in unites of the critical density, to be $\Omega_\chi h^2=0.1196\pm 0.0031$ [CIT]. For a thermal relic this abundance can be predicted as FORMULA Here $h$ is the present value of Hubble parameter in units of 100 $\rm km/(s\cdot Mpc)$, $G$ is Newton's constant, $s_0$ is the present entropy density, and $Y_0$ is the present co-moving number density of the dark matter particles [CIT]. | 457 | 1403.5829 | 11,241,780 | 2,014 | 3 | 24 | false | true | 1 | MISSION |
Taken at face value, the BICEP2 results strongly suggest large-field inflation such as chaotic inflation [CIT]. For various large-field inflation models and their concrete realization in the standard model as well as supergravity and superstring theory, see e.g. [CIT]. It is worth noting, however, that the BICEP2 results are in tension with the Planck + WP + highL data. Explicitly, there is a tension on the relative size of scalar density perturbations on large and small scales. This tension suggests another extension of the Lambda CDM model such as a running spectral index, dark radiation, hot dark matter (HDM), non-zero neutrino mass [CIT], anti-correlation between tensor and scalar modes [CIT] or between tensor and isocurvature modes [CIT], and a sharp cut-off in the scalar modes [CIT].[^4] If it is due to the running spectral index, it would provide us with invaluable information on the inflation sector.[^5] | 925 | 1403.5883 | 11,242,216 | 2,014 | 3 | 24 | true | true | 1 | MISSION |
In order to use the sfermions to generate flavor, there must be large flavor breaking in the sfermion sector. Unfortunately, if sfermions are at the weak scale, low energy flavor tests require them to be nearly flavor diagonal [CIT], a difficulty encountered by many of the early attempts to build such a model [CIT]. Because the Yukawa couplings are dimensionless parameters, they are quite insensitive to the scale at which they are generated. On the other hand, the flavor observables that constrain the flavor breaking in the sfermion sector correspond to higher dimension operators, so they decouple quickly with heavier sfermion masses. Therefore, spectra where the sfermions are much above the weak scale such as Split [CIT] and Supersplit [CIT] Supersymmetry can be used for radiative flavor generation with sfermions potentially as heavy as the GUT or Planck scale [CIT]. | 880 | 1403.6118 | 11,243,983 | 2,014 | 3 | 24 | false | true | 1 | UNITS |
The first year Planck data have been analysed [CIT] within the framework of $\Lambda$CDM cosmology for a simple adiabatic model with an extra string contribution expressed in terms of the fractional contribution, $f_{10}$, of strings to the CMB temperature spectrum at multipole $\ell=10$. For an Abelian-Higgs (AH) field theory model, the constraint turned out to be $f_{10}<0.028$, or equivalently $G\mu_{\rm AH}/c^2<3.2\times 10^{-7}$ [CIT]. Moreover, the Planck data impose severe constraints on any primordial non-Gaussianity [CIT]. The evident question is whether the theoretical models can be compatible with the observational data [CIT]. | 645 | 1403.6688 | 11,249,733 | 2,014 | 3 | 26 | true | true | 2 | MISSION, MISSION |
The shapes of the effective scalar potential in various projections are shown in Fig. REF, REF and REF. We see explicitly in Fig. REF the form of the effective potential for the real and imaginary components of $\phi$, assuming that $m= 10^{-5}, \tilde{m} =10^{-13}$ for $\Lambda=10^{-2}$ the fixed value $2 {\rm Re}, T = 1$ and ${\rm Im}, T = 0$. By construction, the real part of $\phi$ has the desired quadratic potential, and we see that the effective potential for the imaginary part has a minimum at ${\rm Im}, \phi = 0$. Secondly, Fig. REF shows, correspondingly, that the real parts of $T$ and $\phi$ are indeed stabilized in the neighborhood of ${\rm Re}, T = 1$ and ${\rm Re}, \phi = 0$. The curvature of the potential for the degree of freedom corresponding to ${\rm Re}, T$ is difficult to see in this figure, as its mass is ${\cal O}(\tilde{m} /\Lambda)$ in Planck units, which is hierarchically smaller than the mass of the inflaton ${\rm Re}, \phi$, $m$ in this example. Thirdly, Fig. REF shows, correspondingly, that both the real and imaginary parts of $T$ are indeed stabilized in the neighborhood of ${2 \rm Re}, T = 1$ and ${\rm Im}, T = 0$ when $\phi = 0$. | 1,177 | 1403.7518 | 11,258,348 | 2,014 | 3 | 28 | true | true | 1 | UNITS |
We find that the Planck $r$-likelihood peaks $1.6\sigma$ below zero, indicating a deficit of large-scale power. The power deficit has been extensively studied by the Planck collaboration [CIT]; its formal statistical significance can be as high as 3$\sigma$ if an *a posteriori* choice of $\ell$-range is made. Note that the preference for negative $r$ is hidden when an $r \ge 0$ prior is imposed throughout the analysis (as is typically done when quoting upper limits on $r$ from WMAP/Planck). Indeed, a primary purpose of this Letter is to point out that the tension between Planck and BICEP2 is larger than would be expected by comparing the $r$ constraints with an $r \ge 0$ prior imposed. | 694 | 1404.0373 | 11,266,876 | 2,014 | 4 | 1 | true | true | 4 | MISSION, MISSION, MISSION, MISSION |
The action we propose is FORMULA where $\omega$ is a dimensionless coupling constant, $R$ is the scalar curvature of the spacetime metric $g$, $F^{\mu\nu}$ is the electromagnetic field strength tensor, $A_{\mu}$ and $B$ are vector and scalar fields, respectively. Here the constant $m$ is the mass of the Stueckelberg fields and is defined as a real valued positive number, so that we also avoid an imaginary (tachyonic) mass for the vector field that leads to a ghost instability [CIT]. The action $S_{\rm M}$ stands for the matter source. We use natural units with $\hbar=c=1$ and hence the reduced Planck mass is given by $M_{\rm pl}=1/\sqrt{8\pi G}$, where $G$ is the gravitational coupling. We note that the Stueckelberg action, given in REF(#action){reference-type="eqref" reference="action"}, preserves gauge invariance under FORMULA transformations provided that $\lambda$ satisfies FORMULA Neglecting gravity and investigating in Minkowski spacetime, the action under consideration reduces to the free Stueckelberg action. For free Stueckelberg theory, i.e., for Stueckelberg photon interacting with fermions, the Stueckelberg scalar field $B$ satisfies the free wave equation so that the gauge function $\lambda$ which also satisfies the free wave equation can be used to choose a gauge where $B$ is zero. This is the Proca limit of the Stueckelberg mechanism. However, for our action, in curved spacetime $B$ field does not satisfy the free wave equation so it cannot be set to zero with a gauge transformation. | 1,522 | 1404.0892 | 11,271,895 | 2,014 | 4 | 3 | true | false | 1 | UNITS |
A common but dangerous assumption is that sufficient geometric separation of two sectors, $A$ and $B$, makes the couplings between the sectors negligible. (More refined criteria involve separation along a warped direction, or separation without any branes stretched between the sectors, but the principle is the same.) To check this assumption, one has to compute the couplings between the sectors by integrating out massive fields that couple to both $A$ and $B$. In particular, open strings with one end on $A$ and another end on $B$ lead to massive fields in the four-dimensional theory. Integrating out these strings leads to operators of the form[^4] FORMULA where ${\cal{O}}_A^{(\delta_A)}$ is an operator of dimension $\delta_A$ consisting of the fields of sector $A$, and similarly for ${\cal{O}}_B^{(\delta_B)}$, while $M_{AB}$ is the mass of the strings stretched between the sectors. For example, if ${\cal{O}}_B^{(4)} \equiv V_0$ is a constant contribution to the vacuum energy originating in sector $B$, and taking $\phi$ to be a scalar field in sector $A$, then with ${\cal{O}}_A^{(2)} \equiv \phi^2$ we find the coupling FORMULA This is precisely the dimension-six ultraviolet-sensitive inflaton mass term discussed in §REF. The problematic interaction (REF), and kindred couplings, will be negligible if $M_{AB} \gg M_{\rm pl}$, but will otherwise alter the inflationary dynamics. Notice that two sectors decouple, for the purposes of inflation, if the interactions between the sectors are *more than Planck-suppressed*. The general expectation in effective field theory is that Planck-mass degrees of freedom that participate in the ultraviolet completion of gravity will induce Planck-suppressed interactions: the absence of such couplings requires a special structure or symmetry in the quantum gravity theory. We will see that this expectation is borne out in string theory.[^5] | 1,898 | 1404.2601 | 11,289,232 | 2,014 | 4 | 9 | true | true | 3 | UNITS, UNITS, UNITS |
First, we will examine the size of the moduli space for a D$p$-brane in a simple toroidal compactification. Consider a D$p$-brane that fills the four-dimensional spacetime and wraps a $(p-3)$-cycle of volume ${\cal V}_{p-3}=(2\pi L)^{p-3}$ on an isotropic six-torus of volume ${\cal V} = (2\pi L)^6$. The dynamics of the brane is then that of a point particle in $9-p$ compact dimensions. We will derive a kinematic constraint on the canonical range of this particle. Suppose that the D$p$-brane moves along one of the circles in the $T^6$, with coordinate $y$; the maximum possible distance from its starting point is then $\Delta y = \pi L$. Dimensional reduction of the DBI action defines the canonically-normalized field as $\phi^2 = T_p {\cal V}_{p-3}, y^2$, so that the maximal displacement is \^2 \< ()\^p-1. It may appear that we can make this field range arbitrarily large by choosing $L \gg \ell_{\rm s}$ and/or $g_{\rm s}\ll 1$. However, what is relevant for the Lyth bound is the canonical field range in units of the four-dimensional Planck mass (REF), M\_pl\^2 = ()\^6. We find \< ()\^7-p. []{#isotorus label="isotorus"} For $p < 8$, the Planck mass grows faster with $L$ than $\Delta \phi$ does, so that in the limit of theoretical control ($L > \ell_{\rm s}$ and $g_{\rm s} < 1$), the field excursion is sub-Planckian. | 1,334 | 1404.2601 | 11,289,251 | 2,014 | 4 | 9 | true | true | 2 | UNITS, UNITS |
Since general relativity is not a renormalizable theory, it is expected that deviation from it will show up at some scale between the Planck scale and the lowest length scale we have currently accessed. It is tempting to consider a scenario where those deviation persist all the way to cosmological scales and account for Dark Matter and/or Dark Energy. After all, we do only detect these dark component through gravity. However, there is a major problem with this way of thinking. There is no sign of these modifications in the range of scales for which we have exhaustively tested gravity. So, they would have to be relevant at very small scales, then somehow switch off at intermediate scales, then switch on again at larger scales. It is hard to imagine what can lead to such behaviour, which actually contradicts our basic theoretical intuition about separation of scales and effective field theory. Nonetheless, intuition is probably not a good enough reason to not rigorously explore an idea that could solve two of the major problem of contemporary physics at once. This explain the considerable surge of interest in alternative theories of gravity in the last decade or so. | 1,182 | 1404.2955 | 11,293,995 | 2,014 | 4 | 10 | true | true | 1 | UNITS |
Moreover, we have analyzed the spectral index $n_{\mathrm{s}}$ of scalar modes of the primordial density perturbations and those tensor-to-scalar ratio $r$, and make the comparison of the theoretical predictions with the observational data obtained by the Planck satellite as well as the BICEP2 experiments. Consequently, it has explicitly been shown that for sets of the wider ranges of the parameters, the value of $n_{\mathrm{s}}$ can explain the Planck analysis of $n_{\mathrm{s}} = 0.9603 \pm 0.0073, (68\%,\mathrm{CL})$, while the value of $r$ is not within the 1 $\sigma$ error range of the BICEP2 result $r = 0.20_{-0.05}^{+0.07}, (68\%,\mathrm{CL})$. For instance, $n_s\sim 0.968$ and $r=0.0028$ can be realized (when the values of model parameters are $M\sim0.1,M_P$, $\mu\sim M$, and $\phi_k (=\phi(\tilde{t}_k)) \sim7.756 M_P$, as presented in Sec. 5.2). These resultant values mainly depend on the quite-large value of $\phi_k$, and therefore they are basically independent of the other model parameters. Since these results are similar to those in the Starobinsky inflation model, it is considered that quantum gravity might present only small corrections to the values of $n_{\mathrm{s}}$ and $r$. | 1,212 | 1404.4311 | 11,306,785 | 2,014 | 4 | 16 | true | true | 2 | MISSION, MISSION |
Here we assume that a gauge group, for example $SU(5)$, is broken in a hidden sector and a singlet field acquires a vacuum expectation value. The latter field, propagates the breaking of the gauge group to the visible sector through its interactions with a messenger superfield. Finally, mass terms for the fields in the visible sector and a splitting in mass between the components of a same supermultiplet are generated which induces supersymmetry breaking.\ The two mechanisms described here are not the only ones. Other solutions to the problem of supersymmetry breaking have been considered such as the anomaly gauge mediated supersymmetry breaking (AMSB) or extra-dimensional supersymmetry breaking (XMSB) [CIT]. In any case, it is always supposed that supersymmetry breaking is induced by some mechanism at high scale (generally unification scale or Planck scale) inducing, in the low energy limit, a new Lagrangian called the soft supersymmetry breaking Lagrangian which reads: \_soft = h\^ijk\_i_j_k - b\^ij \_i_j - a\^i \_i - (m\^2)\_i\^j \^i \_j - M +h.c. These new parameters are related to the high energy ones through the renormalization group equations. | 1,168 | 1404.4564 | 11,309,853 | 2,014 | 4 | 17 | false | true | 1 | UNITS |
One must recall, however, that baryons are not the dominant matter component in the universe and, in particular, the total isocurvature perturbation corresponds to a weighted sum of the contributions from baryons and cold dark matter: FORMULA with $\Omega_c=0.845\Omega_m$ and $\Omega_b=0.155\Omega_m$ according to the best fit Planck model [CIT]. Planck has in fact placed bounds on the amount of matter isocurvature perturbations for different types of correlation with the main adiabatic component. For anti-correlated isocurvature perturbations, the bound obtained by Planck for the effective CDM matter isocurvature component corresponds to $|B_b|<0.51$ (95% CL) in the absence of CDM perturbations [CIT], so that the quartic potential predictions are well within these bounds. Interestingly, the Planck collaboration has reported a significant improvement of their fit to the CMB temperature data when anti-correlated matter isocurvature modes are included, although no unambiguous evidence for their existence, such as a shift in the position of the acoustic peaks, could be claimed. This is also supported by the more recent analysis in [CIT], so that the observational effects of matter isocurvature perturbations deserve a closer look. | 1,245 | 1404.4976 | 11,313,539 | 2,014 | 4 | 19 | true | true | 4 | MISSION, MISSION, MISSION, MISSION |
In standard big-bang cosmology with $c=c_0$: FORMULA where $\Omega=\rho/\rho_c$, $\rho_c=3H^2/8\pi G$ and the Planck time $t_{\rm PL}\sim 10^{-43},{\rm sec}$. This implies that the radius of curvature $R_{\rm curv}$ at the Planck time was very large compared to the Hubble radius $R_H=c_0/H$: FORMULA This means that the universe in standard big-bang cosmology was very special at the Planck time. The universe has survived some $10^{60}$ Planck times without re-collapsing or becoming curvature dominated. | 506 | 1404.5567 | 11,314,242 | 2,014 | 4 | 20 | true | false | 4 | UNITS, UNITS, UNITS, UNITS |
The indication from the LHC of a scalar resonance compatible with perturbative electroweak symmetry breaking reinforces the Standard Model parameterisation of all subatomic experimental data. The logarithmic evolution of the Standard Model gauge and matter parameters suggests that the Standard Model provides a viable parameterisation up to the Planck scale. Supersymmetry preserves the logarithmic running also in the scalar sector, which provides reasonable motivation to seek experimental evidence for its validity in the LHC, VLHC (Very Large Hadron Collider) and other future machines. It should be stressed that the viability of the experimental program rests on its ability to deliver a working machine in the first place and to measure the parameters of the Standard Model to better accuracy in the second. Discovering new physics is an added bonus. | 858 | 1404.5180 | 11,314,964 | 2,014 | 4 | 21 | false | true | 1 | UNITS |
Both $n_s$ and $r$ are suppressed if $\alpha \neq 0$ and has negative values, but, for $\alpha > 0$, those are enhanced. These results are completely opposite compared to Ref. [CIT], in which $r$ is enhanced for negative $\alpha$ and reduced for positive $\alpha$ for $V=V_0 \phi^n$ with $\xi=\xi_0 \phi^{-n}$. Because $r$ becomes suppressed as $n$ decreases, Planck data alone favor the $n=1$ model, but the BICEP2 + Planck favors $n=2$. Even for $\alpha \neq 0$, BICEP2 with Planck seems to rule out $n=1$ at $95\%$ CL (Fig. REF). For $n=2$ with $\alpha \neq 0$ (Fig. REF), negative $\alpha$ with $N=60$ lies within the contour of $95\%$ CL according to Planck data, but positive $\alpha$ is located outside of the contour. We find that Planck alone favors $\alpha < 0$ model with $N> 50$. However, Planck combining with BICEP2 allows both the positive and negative $\alpha$ models with $N=50$ and $N=60$ at $95\%$ CL and favors $N \lesssim 60$. Although the $n=4$ model seems to be ruled out by Planck at $99.7\%$ CL [CIT], it can be survived according to Planck combining by BICEP2 (Fig. REF) for $N> 50$ at $95\%$ CL. | 1,122 | 1404.6096 | 11,325,496 | 2,014 | 4 | 24 | false | true | 8 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
Figure REF shows the $1\sigma$ and $2\sigma$ marginalized allowed regions in the planes $m_s$--$\Delta{N}_{\text{eff}}$ and $H_0$--$\Delta{N}_{\text{eff}}$ obtained by fitting the CMB data (Planck+WP+high-$\ell$+BICEP2(9bins); see Ref. [CIT]) with the SBL prior in a model with free $\Delta{N}_{\text{eff}}$ and a massive sterile neutrino which decays invisibly. The corresponding numerical values of the cosmological parameters are listed in Tab. REF. From the values of $\Delta\chi^2(\text{A})$ and $\Delta\chi^2(\text{B})$ one can see that the fit of cosmological data is even slightly better than that obtained with a stable sterile neutrino without mass constraints (A) and much better than that obtained with a stable sterile neutrino with the SBL mass prior (B). | 769 | 1404.6160 | 11,326,290 | 2,014 | 4 | 24 | true | true | 1 | MISSION |
The value of this parameter can be constrained using the astronomical observations and astrophysical experiments. In the scale of the solar system the Cassini spacecraft mission experiment gave a very stringent bound on $\omega_{\textrm{\tiny BD}}> 4000$ for spherically symmetric solutions in the parametrized post-Newtonian (PPN) formalism [CIT]. On the other hand the data from the cosmological experiments conducted during the WMAP and Planck missions gave substantially lower values of limits on the parameter $\omega_{\textrm{\tiny BD}}$. Liddle et al. in [CIT] studied the transition form radiation domination to matter domination epoch in Brans-Dicke theory and showed how the Hubble length at equality depends on the coupling parameter $\omega_{\textrm{\tiny BD}}$ for large values of this parameter. Acquaviva et al. in [CIT] using structure formation constraints found lower bound $\omega_{\textrm{\tiny BD}}>120$ at $95\%$ confidence level. Recently Avilez and Scordis, using CMB data, have obtained the smaller value of the limit $\omega_{\textrm{\tiny BD}}> 692$ at a $99\%$ confidence level [CIT]. Li et al. [CIT] using data coming from the Planck satellite and others cosmological observations determined the $\omega_{\textrm{\tiny BD}}$ parameter region $-407.0 < \omega_{\textrm{\tiny BD}}< 175.87$ at the $95\%$ confidence level, while for positive values of this parameter they obtained $\omega_{\textrm{\tiny BD}}> 181.65$ at the $95\%$ confidence level. On the other hand Fabris et al. in [CIT] using the supernovae Ia data obtained the best fit value of $\omega_{\textrm{\tiny BD}}= -1.477$. We must remember that all these limits are model dependent. In some estimations the potential of the scalar field is ignored while in others the Newtonian approximation and spherical symmetry is assumed at the starting point. | 1,840 | 1404.7112 | 11,333,202 | 2,014 | 4 | 28 | true | true | 2 | MISSION, MISSION |
Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US 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 is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, Cambridge University, Case Western Reserve University, University of Chicago, Drexel University, Fermi National Accelerator Laboratory, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, The Chinese Academy of Sciences (LAMOST), the Leibniz Institute for Astrophysics, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the US Naval Observatory and the University of Washington. | 1,320 | 1404.7138 | 11,333,986 | 2,014 | 4 | 28 | true | false | 3 | MPS, MPS, MPS |
[Abridged.] It is conceivable that no single statistical estimator can be sensitive to all forms and levels of non-Gaussianity that may be present in observed CMB data. In recent works a statistical procedure based upon the calculation of the skewness and kurtosis of the patches of CMB sky-sphere has been proposed and used to find out significant large-angle deviation from Gaussianity in the foreground-reduced WMAP maps. Here we address the question as to how the analysis of Gaussianity of WMAP maps is modified if the foreground-cleaned Planck maps are used, therefore extending and complementing the previous analyses in several regards. We carry out a new analysis of Gaussianity with the available nearly full-sky foreground-cleaned Planck maps. As the foregrounds are cleaned through different component separation procedures, each of the resulting Planck maps is then tested for Gaussianity. We determine quantitatively the effects for Gaussianity of masking the foreground-cleaned Planck maps with the INPMASK, VALMASK, and U73 Planck masks. We show that although the foreground-cleaned Planck maps present significant deviation from Gaussianity of different degrees when the less severe INPMASK and VALMASK are used, they become consistent with Gaussianity as detected by our indicator $S$ when masked with the union U73 mask. A slightly smaller consistency with Gaussianity is found when the $K$ indicator is employed, which seems to be associated with large-angle anomalies reported by the Planck team. Finally, we examine the robustness of the Gaussianity analyses with respect to the noise pixel's as given by the Planck team, and show that no appreciable changes arise when is incorporated into the maps. The results of our analyses provide important information about the suitability of the foreground-cleaned Planck maps as Gaussian reconstructions of the CMB sky. | 1,884 | 1405.1128 | 11,354,916 | 2,014 | 5 | 6 | true | true | 9 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
Although the above comparison of the power spectra can be used as a first indication of deviation from Gaussianity of different degrees for distinct masks, to have a quantitative overall assessment of this deviation on a large angular scale, we employed the power spectra $S_\ell$ and $K_\ell$ (calculated from the foreground-cleaned Planck maps) to carry out a $\chi^2$ analysis to determine the goodness of fit of these power spectra obtained from the Planck maps as compared to the mean power spectra calculated from simulated Gaussian maps ($\overline{S}^{G}_{\ell}$ and $\overline{K}^{G}_{\ell}$). Thus, for the power spectrum $S_\ell$ obtained from a given Planck map one has FORMULA where $\overline{S}^{G}_{\ell}$ are the mean multipole values for each $\ell$ mode, $(\sigma_{\ell}^{G})^2$ is the variance calculated from $1,000$ Gaussian simulated maps, and $n$ is the highest multipole one chooses to analyze the Gaussianity. We took this to be $\ell = 10$ in this paper, since we are concerned with large-angle non-Gaussianity. Obviously a similar expression and reasoning can be used for $K_\ell$. | 1,109 | 1405.1128 | 11,355,103 | 2,014 | 5 | 6 | true | true | 3 | MISSION, MISSION, MISSION |
We also addressed the question of how the results of Gaussianity analyses are modified when the noise is added to the foreground-cleaned Planck maps, a point that has not been considered in Planck Collaboration XXIII ([CIT]). Tables REF and REF show that the results of the analyses do not change appreciably when the noise is incorporated into the Planck maps. | 361 | 1405.1128 | 11,355,118 | 2,014 | 5 | 6 | true | true | 3 | MISSION, MISSION, MISSION |
For one thing, inflationary cosmology does not resolve the problem of the initial singularity inherited from the hot big bang cosmology [CIT]. On the other hand, it is well known that the Planck mass suppressed corrections to the inflaton potential generally lead to the masses of the order of the Hubble scale and then spoil the slow roll conditions rendering a sustained inflationary stage impossible [CIT]. This issue would be even worse if the field variation of the inflaton is super-Planckian as indicated by the BICEP2 [CIT]. Moreover, if we trace backward along the cosmological perturbations observed today, their length scales could go beyond the Planck length at the onset of inflation [CIT]. Additionally, in order to study quantum field theory during inflation, it is inevitably necessary to systematically study the nonlinear corrections of field fluctuations that are on one side not ultraviolet (UV) complete, and on the other side yield observably large infrared effects that were not detected in experiments [CIT]. | 1,032 | 1405.1369 | 11,357,189 | 2,014 | 5 | 6 | true | true | 2 | UNITS, UNITS |
Inflation, and in particular slow-roll inflation, has emerged as the leading framework to understand and explain the recent cosmological CMB observations, most notably by PLANCK mission [CIT] and BICEP2 [CIT]. The most common models of inflation are those involving one or more scalars with canonical kinetic terms and a (carefully) chosen or designed potential (minimally) coupled to Einstein gravity. Despite the theoretical simplicity and addressing some theoretical issues in Big Bang early Universe cosmology, the wealth of the new observational data has made it increasingly difficult to find inflationary models which do well with data, as well as being free of theoretical issues, like naturalness, stability of inflaton potential and having a natural appearance and embedding into high energy physics models, such as beyond SM particle physics models or string theory. | 877 | 1405.1685 | 11,360,564 | 2,014 | 5 | 7 | true | true | 1 | MISSION |
Models of the Universe with large additional dimensions were proposed around the year 2000 to bypass the constraints of not having observable Kaluza-Klein modes. In these scenarios the Standard Model particles and interactions are confined on a thin "brane" embedded in a higher-dimensional space-time, while gravity leaks into the extra dimensions [CIT]. Because gravity propagates in the entire "bulk\" space-time, its fundamental scale $M_{\rm G}$ is related to the observed Planck mass $M_{\rm P}\simeq 10^{16},$TeV by a coefficient determined by the volume of the (large or warped) extra dimensions. Therefore in these models there appear several length scales, namely the spatial extension(s) $L$ of the extra dimensions in the ADD scenario [CIT], or the anti-de Sitter scale in the RS scenario $\ell$ [CIT], and possibly the finite thickness $\Delta$ of the brane in either. The size $L$ of the extra dimensions or the scale $\ell$, determines the value of the effective Planck mass $M_{\rm P}$ from the fundamental gravitational mass $M_{\rm G}$. At the same time all of them determine the scale below which one should measure significant departures from the Newton law. | 1,178 | 1405.1692 | 11,360,632 | 2,014 | 5 | 7 | false | true | 2 | UNITS, UNITS |
Now, the question is whether the large values of the primordial bispectra are supported by the Planck data. To answer this we need to compare the angular bispectra obtained from these models with the Planck bispectrum data. From a first look, it may be argued that since the violent oscillations in the primordial power spectrum leads to a large and oscillating $f_{_{\rm NL}}$, in a finite bin width of Planck resolution the $f_{_{\rm NL}}$ will be averaged out. However, to have a full understanding of the issue, we need to wait for Planck polarization data to confirm the oscillations in Wiggly Whipped First order - II case and then compare the bispectrum directly. Till then we can at least say that Wiggly Whipped First order - I and Second order (for a smooth transition) are completely consistent with Planck bounds. | 825 | 1405.2012 | 11,363,219 | 2,014 | 5 | 8 | true | true | 5 | MISSION, MISSION, MISSION, MISSION, MISSION |
But in the presence of a magnetic field $\mathbf{B}$ the component of momentum perpendicular to $\mathbf{B}$ becomes quantised, an effect known as Landau quantization. The solution of the relativistic Dirac equation of an electron of mass $m_{\rm e}$ in the presence of magnetic field $\mathbf{B}$ along z-axis gives, for $z$-momentum $p_z$, the energy eigenvalue of $\nu$-th quantised level as FORMULA where $B$ is the magnitude of magnetic field $\mathbf B$, $B_c=\frac{m_{\rm e}^2c^2}{\hbar e}=4.414\times10^9$T, $c$ is speed of light, $h$ is the Planck's constant, $\hbar=h/2\pi$, $\nu=(n_L+\frac{1}{2}+\sigma)$, $n_L$=0,1,2\.... and $\sigma=\pm\frac{1}{2}$ [CIT]. | 668 | 1405.2282 | 11,367,149 | 2,014 | 5 | 9 | true | false | 1 | CONSTANT |
Figure REF shows our PS1 map, followed by the difference between our PS1 map and the two Planck reddening maps. Consistent with [5.3], we have rescaled the Planck $\tau_{353}$ map by 30% to provide a better match to the PS1 map. The high-latitude sky is in close agreement, and subtracts well in the difference maps. However, the lower latitude and higher $E(B-V)$ sky shows large differences between the maps. Both Planck maps substantially underpredict the amount of extinction outside the plane east of the the Galactic center, as well as in the Cepheus Flare and at high latitudes towards the anticenter. Meanwhile at low latitudes the Planck $E(B-V)$ are generally larger than the PS1 $E(B-V)$, which is expected as the PS1 maps saturate at about 1.5 mag and there is often significant dust beyond 4.5 kpc in this area. | 824 | 1405.2922 | 11,371,953 | 2,014 | 5 | 12 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
We are grateful to Aninda Sinha for valuable suggestions and remarks. We also thank Joan Camps and Rajesh Gopakumar for discussions. A.B thanks the string theory group at Harish-Chandra Research Institute, Allahabad for hospitality during part of this work. A.B also thanks the members of the department of particle physics, University of Santiago de Compostela, specially Jose Edelstein, the Max Planck Institute of Gravitational Physics, Golm specially Axel Kleinschmidt and the theory division of Max Planck Institute for Physics, Munich specially Johanna Erdmenger for hospitality and the opportunity to present part of this work. | 634 | 1405.3511 | 11,378,148 | 2,014 | 5 | 14 | false | true | 2 | MPS, MPS |
Thus we have a broad class of consistent large field inflation models, which have identical model-independent observational predictions. This universality is closely related to the existence of the UV cutoff in the original conformal formulation of the theory. Note that we did not need to invent a cutoff, or speculate about its existence as in (REF): It is a part of the theory, and it is directly proportional to the Planck mass. The value of the cutoff becomes infinitely large in terms of the canonically normalized inflaton field in the Einstein frame, but the consequences of its original existence are reflected in the universality of the observational predictions of this class of theories. | 699 | 1405.3646 | 11,379,039 | 2,014 | 5 | 14 | true | true | 1 | UNITS |
One relevant approach to dark energy suggests that the universe is composed by a single fluid, which unifies dark matter and dark energy in a single description. A barotropic perfect fluid with vanishing adiabatic sound speed reproduces the $\Lambda$CDM behavior at the background, as proposed in [CIT] and it is compatible with small perturbations, as shown in [CIT]. The corresponding equation of state reads FORMULA while the total equation of state for the $\Lambda + \text{dm}$ total dark fluid in the $\Lambda$CDM model reads FORMULA Thus, both models, i.e. $\Lambda$CDM and the negligible sound speed model, exactly behave in the same way and hence they are degenerate. There are several other options for a unified dark fluid which does not degenerate with $\Lambda$CDM. One of these frameworks is represented by the Chaplygin gas [CIT] and its generalizations [CIT] and constant adiabatic speed of sound models [CIT], among others. Therefore, we parameterize the dark fluid equation of state by a Taylor series: FORMULA where FORMULA Knowing the value of $\Omega_b$, in order to estimate up to $w_i$, we need to use the first $i$th cosmographic parameters. If we use Padé approximants up to $P_{23}$, then we truncate the expansion series at third order. The Hubble rate easily reads FORMULA where $\Omega_{df} = 1-\Omega_{b}$ and we define FORMULA The parameters to estimate are given implicitly by FORMULA which reduce to the flat-$\Lambda$CDM values when $w_0 = -1$, $w_1=w_2=0$, and by considering $\Omega_b \rightarrow \Omega_m$. From several independent observations we have measurements of the baryon species in the universe. In this section we will take the best-fit from the Planck Collaboration $\Omega_b = 0.0488$ [CIT]. We report the estimated values from Padé approximants $P_{21}$, $P_{31}$ and $P_{23}$: | 1,827 | 1405.6935 | 11,411,604 | 2,014 | 5 | 27 | true | false | 1 | MISSION |
Finally, in Fig. REF we also consider the different contributions for the equilateral shape at the highest Planck frequencies. This is interesting in terms of a possible detection of the CIB-lensing bispectrum. Due to its strong signal at these frequencies, it should be detectable with high significance for Planck at $\nu\ge217$,GHz. However, IR galaxies give rise themselves to a strong contribution at high frequencies and they can be therefore a strong contaminant for the detection of the CIB--lensing bispectrum. We discuss later how to tackle this problem. | 564 | 1405.7029 | 11,412,433 | 2,014 | 5 | 27 | true | false | 2 | MISSION, MISSION |
center $\Omega_\mathrm m$ $\sigma_8$ $n_s$ $w_0$ $w_a$ $\Omega_\mathrm b$ $h_0$ ---------------------- ---------------------- ------------- -------------- ------- ------- -------------------- ------------- Fiducial 0.315 0.829 0.9603 -1.0 0.0 0.049 0.673 Min 0.1 0.6 0.85 -2.0 -2.5 0.04 0.6 Max 0.6 0.95 1.06 0.0 2.5 0.055 0.76 Planck+WP 1-$\sigma$ $^{+0.016}_{-0.018}$ $\pm 0.012$ $\pm 0.0073$ \- \- $\pm 0.00062$ $\pm 0.012$ | 427 | 1405.7423 | 11,417,095 | 2,014 | 5 | 28 | true | false | 1 | MISSION |
However, it is permissible for $|\eta_V|$ be of order unity over a number of e-foldings. Indeed, for the very same Planck fat to Planck flat inflationary trajectory discussed in Section [1], this fat to flat transition occurs at the point in the inflaton trajectory where $|\eta_V|$ becomes order unity and $\epsilon_V$ becomes tiny while the inflaton sources primordial modes smaller than those that have been observed. This behavior can be seen in Figure REF. The inflaton can come to near rest ($\epsilon_V \ll 1$) rather abruptly, which requires $|\eta_V|\gtrsim1$ over some amount of the field trajectory. The question then becomes whether the width of the trajectory in e-folds multiplied by the average large value of $\left\langle \eta_V - 2\epsilon_V \right\rangle$ in this region is greater than $\sim \mathcal{O}(1)$. If it is, the Antusch and Nolde bound as stated does not necessarily restrict these models. For example if $\eta_V - 2\epsilon_V$ is zero over 50 e-folds, but $|\eta_V|>10$ over 10 e-folds, this inflaton technically evades the bound of Antusch and Nolde. | 1,083 | 1405.7563 | 11,419,116 | 2,014 | 5 | 29 | true | true | 2 | MISSION, MISSION |
For instance, the Starobinsky model [CIT] has only one mass parameter $M$ that is fixed by the observational (CMB) data as $M=(3.0 \times10^{-6})(50/N_e)$ where $N_e$ is the e-foldings number. The predictions of the Starobinsky model for the spectral index $n_{\text{s}}\approx 1-2/N_e\approx 0.96$ (for $N_e =50$), the tensor-to-scalar ratio $r\approx 12/N^2_e\approx0.0048$ and low non-Gaussianity are in agreement with the WMAP and Planck data ($r<0.13$ and $r<0.11$, respectively, at 95% CL) [CIT], but are in disagreement with the BICEP2 measurements ($r=0.2^{+0.07}_{-0.05}$, or $r=0.16^{+0.06}_{-0.05}$ when dust subtracted) [CIT]. The competitive model of chaotic inflation with a quadratic scalar potential, proposed by Linde [CIT], predicts $r\approx 8/N_e = 0.16\left(50/N_e \right)$ in good agreement with the BICEP2 data, though in apparent disagreement with the Planck data (when running of the spectral index is ignored). | 936 | 1406.0252 | 11,426,190 | 2,014 | 6 | 2 | false | true | 2 | MISSION, MISSION |
The global variable $\lambda$ sets the hierarchy between the matter scales and the Planck scale, since FORMULA where $m_{phys}$ is a physical mass scale of a canonically normalized matter theory, and $m$ is the bare mass in the Lagrangian. As an illustration, consider a scalar field with bare mass $m$, FORMULA where $\varphi=\lambda \phi$ is the canonical scalar and the physical mass is $m_{phys}=\lambda m$. | 411 | 1406.0711 | 11,431,028 | 2,014 | 6 | 3 | true | true | 1 | UNITS |
The original motivation for warped extra-dimensions, or Randall-Sundrum models (RS), was to address the hierarchy problem. In RS the fundamental scale of gravity is exponentially reduced from the Planck mass scale to a TeV size due to a Higgs sector localized near the boundary of the extra dimension [CIT]. If SM fermions are allowed to propagate in the extra dimension [CIT], and become localized towards either boundary, the scenario also addresses the flavor problem of the SM and suppresses generic flavor-violating higher-order operators present in the original RS setup. However, KK-mediated processes still generate dangerous contributions to electroweak and flavor observables [CIT], pushing the KK scale to $5-10$ TeV [CIT]. One realization of the model is based on the so-called flavor anarchy [CIT], in which one assumes that no special structure governs the flavor of Yukawa couplings and bulk fermion masses, as natural ${\cal O}(1)$ values for these 5D parameters already generate viable masses and mixings. The neutrino sector must behave differently, first due to the possibility of Majorana mass terms, and second because this setup generates large mass hierarchies and small mixing angles, at odds with neutrino observations. An interesting property of warped scenarios was investigated in [CIT], for the case of a bulk Higgs wave function leaking into the extra dimension. There one would obtain small mixing angles and hierarchical masses for all charged fermions, and at the same time very small Dirac masses, with large mixing angles and negligible mass hierarchy for neutrinos. Thus the flavor anarchy paradigm could still work in these scenarios. | 1,671 | 1406.2331 | 11,446,783 | 2,014 | 6 | 9 | false | true | 1 | UNITS |
The consistency relations are *physical* statements and can be related to late-time observables, such as the CMB bispectrum [CIT] and the large-scale structure [CIT]. Their violations can be tested observationally. For instance, had the Planck satellite detected a significant primordial local $f_{\rm NL}$, this would have violated Maldacena's consistency relation and immediately ruled out in one shot all of the simplest inflationary models. More precisely, we would have learned that one of the three standard assumptions listed above is invalid. Instead, the Planck result [CIT] $f_{\rm NL}^{\rm local} = 2.7\pm 5.8$ is so far consistent with Maldacena's relation. What REF(#schematicintro){reference-type="eqref" reference="schematicintro"} shows is that there are in fact an infinite number of additional checks that the simplest inflationary scenarios must pass to be validated. | 886 | 1406.2689 | 11,451,385 | 2,014 | 6 | 10 | true | true | 2 | MISSION, MISSION |
In Fig. REF we show the best fit TT spectrum from this analysis and we compare this with the best fit concordance cosmology. Quite interestingly, the resulting plot has a strong overlap at all $100\leq \ell \leq 3500$. The larger value of the tilt compensates for any deviations at large $\ell$ from the oscillation. In Fig. REF we show the anticipated difference with the EE and TE spectra. The difference between the concordance model for TE is relatively largest, and a Planck polarization measurements might be able to give further evidence for a large feature. These are relatively large scales, so they are cosmic variance limited. For TE over the range $\ell = 2-40$ the difference is about 20$\%$. We can estimate a detection by computing the signal to noise of the difference, i.e. for a full sky experiment FORMULA Given the difference of around $20\%$, and in the assumption we are limited by cosmic variance, we obtain $S/N\sim 8$, i.e. such a difference should be detectible. If one includes noise (which will be there for Planck) and the fact that for cosmology the sky fraction is about 30$\%$, we expect that Planck will be near the detection limit. What should be emphasized is that this simple estimate shown that a combined analysis of TT, TE and EE would help discriminate between the axion model and concordance cosmology. | 1,343 | 1406.3243 | 11,457,371 | 2,014 | 6 | 12 | true | false | 3 | MISSION, MISSION, MISSION |
Charged particles with energy $E$, mass $m$ and charge number $Z$ spiralling in a magnetic field $\vec{B}$ emit synchrotron radiation at a rate FORMULA where $m_e$ is the electron mass and $\sigma_T$ is the Thompson cross section. The synchrotron spectrum radiated by a distribution of particles $N(E)$ (see appendix A) as function of the scattered photon energy $(E_\gamma)$ (in units of power per unit area) is FORMULA where $V_{vol}$ is the volume of the emission region, $d$ is the distance of the source from us, $h$ is the Planck constant, $K_{5/3}(\xi)$ is the modified Bessel function of 5/3 order, and the characteristic energy $E_c$ is FORMULA In these calculations we assumed that the particle velocity is perpendicular to the local magnetic field. | 759 | 1406.5664 | 11,484,651 | 2,014 | 6 | 22 | true | false | 1 | CONSTANT |
We adopt the BAO measurements from four different redshift surveys, following the analysis by the Planck team [CIT] :the BOSS DR9 measurement [CIT] at $z=0.57$; the 6dF Galaxy Survey measurement [CIT] at $z=0.1$; the WiggleZ measurement [CIT] at $z=0.44,0.60$ and $0.73$; the SDSS DR7 measurement [CIT] at $z=0.2$ and $z=0.35$. | 327 | 1406.6822 | 11,498,513 | 2,014 | 6 | 26 | true | false | 1 | MISSION |
In conclusion, the overall amplitude of the peaks is less affected by a change in $m_{\rm e}$ than by a change in $\alpha$, due to the different effect on the damping tail. This is the reason why high resolution data on the damping tail, as provided by Planck, allow one to break the degeneracy between $\alpha$ and $H_0$, while one can hardly do this for $m_{\rm e}$ and $H_0$. Further details of these effects can be found in Appendix [8]. | 441 | 1406.7482 | 11,504,541 | 2,014 | 6 | 29 | true | false | 1 | MISSION |
To summarize, in the present article, I have established a methodology for generating sub-Planckian field excursion along with large tensor-to-scalar ratio in a single brane RS braneworld scenario for generic model of inflation with and without ${\bf Z_{2}}$ symmetry in the most generalized form of inflationary potential. I have investigated this scenario by incorporating various parametrization in the power spectrum for scalar and tensor modes as well as in the tensor-to-scalar ratio as required by the observational probes. Using the proposed technique I have further derived a analytical as well as the numerical constraints on the positive brane tension, 5D Planck scale and 5D bulk cosmological constant in terms of the 4D Planck scale. Finally, I have given an estimation of the field excursion which lies within a sub-Planckian regime and makes the embedding of inflationary paradigm in RS single braneworld via effective field theory prescription consistent. | 971 | 1406.7618 | 11,505,566 | 2,014 | 6 | 30 | true | true | 2 | UNITS, UNITS |
In this paper we extend the method further, applying a clustering-based redshift inference technique to a field of unresolved sources. Using data from the Planck satellite and the SDSS, we will benefit from the availability of a large fraction of the sky, therefore reducing sample variance effects. The outline of the paper is as follows: in §,[2] we present the method; in §,[3] we describe the Planck maps and spectroscopic quasar datasets; in §,[4] we present the intensity measurements, as well as estimates of the dust mass density and star formation rate density as a function of redshift; in §,[5] we offer conclusions and future directions; and finally, in an Appendix we summarize other findings from Planck maps that may be of interest. We assume a cosmology with $\Omega_{M}=0.274$, $\Omega_{\Lambda}=0.726$, and $H_{0}=70.5$ km/s/Mpc [CIT]. All error bars on the distributions are computed via spatial jackknife. | 925 | 1407.0031 | 11,509,354 | 2,014 | 6 | 30 | true | false | 3 | MISSION, MISSION, MISSION |
The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. | 928 | 1407.1619 | 11,524,373 | 2,014 | 7 | 7 | true | false | 2 | MPS, MPS |
Hints of Bohm-like diffusion in CR precursors have already been outlined by [CIT], who used a MHD-kinetic code that exploits a spherical harmonic expansion of the Vlasov--Fokker--Planck equation to calculate a self-consistent magnetic field configuration starting from an initial CR current of mono-energetic ions. These authors inferred diffusion faster than Bohm in $B_0$, but slower than Bohm in $B_{tot}$, possibly because simulations were not converged (see their section 4.3). Our hybrid simulations, instead, test CR diffusion for an ion power-law distribution that forms and grows spontaneously because of DSA, without any need to prescribe particle injection or escape; therefore, we can self-consistently study the connection between CR spectrum, wave spectrum, and momentum dependence of the diffusion coefficient. We also distinguish between different regimes of field amplification, and confirm that for strong shocks Bohm diffusion in $B_{tot}$ provides a reasonable description for the transport of particles of any energy. Finally, we attest to the relative relevance of NRH and resonant instability in amplifying the magnetic field in the far upstream and in the precursor, providing the theoretical framework for calculating both self-generated turbulence and diffusion for a given CR distribution, in different shock regions. | 1,344 | 1407.2261 | 11,531,498 | 2,014 | 7 | 8 | true | false | 1 | FOKKER |
However, a few alterations/variations have been incorporated in the present discussion. Instead of expanding $\langle \sigma v_{\rm rel} \rangle$ into the leading $s$ and $p$ wave contributions (ignoring the higher partial waves, and assuming no threshold or pole in the vicinity), we have used `micrOMEGAs` [CIT] for an accurate estimate of $\langle \sigma v_{rel} \rangle$, and therefore, of the relic density. `SuSpect` [CIT] has been used as the spectrum generator. Assuming standard cosmology, we have used the recent estimates for the right (thermal) relic density from the CMBR measurements by `PLANCK` [CIT] and `WMAP` (9 year data) [CIT]. In addition, we have taken into account the recent bounds on the sparticle spectrum, especially on the CP-even Higgs mass (125 GeV) from the LHC [CIT]. | 799 | 1407.3030 | 11,540,445 | 2,014 | 7 | 11 | false | true | 1 | MISSION |
[^1]: Based on data acquired using the Large Binocular Telescope (LBT) and Gemini Observatory. The LBT is an international collaboration among institutions in Germany, Italy, and the United States. LBT Corporation partners are LBT Beteiligungsgesellschaft, Germany, representing the Max Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; Istituto Nazionale di Astrofisica, Italy; The University of Arizona on behalf of the Arizona university system; The Ohio State University, and The Research Corporation, on behalf of the University of Notre Dame, University of Minnesota, and University of Virginia. Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciěncia, Tecnologia e Inovaç ao (Brazil) and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina)." | 1,092 | 1407.3900 | 11,548,836 | 2,014 | 7 | 15 | true | false | 1 | MPS |
In the following section, we report the results that have been obtained for all the *Encyclopædia Inflationaris* scenarios. To make the comparison with the current Planck (and BICEP2) constraints realistic, let us stress that the fiducial models, having zero free parameters and used to generate the mock data, *are not* included in the list of models tested. | 359 | 1407.4034 | 11,549,734 | 2,014 | 7 | 15 | true | true | 1 | MISSION |
Following [CIT], the opacities are estimated as: FORMULA Here, $G_{F}=1.166\times 10^{-5}$ GeV$^{-2}$ is Fermi's constant, $\hbar=1.054\times10^{-27}$ cm$^{2}$ g s$^{-1}$ is the reduced Planck constant, $Q=1.29$ MeV is the difference in mass between a neutron and proton, $n_{n}$ is the number density of neutrons, $c_{V}$ and $c_{A}$ are weak interaction constants,[^6] $f_{e}$ is the distribution function for electrons and $n$ is the number density of nucleons. For deriving typical values we used $n_{n}=n_{p}=n/2$, where $n_{p}$ is the number density of protons. The composition is assumed to be completely dissociated to free protons and neutrons. We have neglected stimulated absorption effects for simplicity. | 717 | 1407.4653 | 11,556,976 | 2,014 | 7 | 17 | true | false | 1 | CONSTANT |
Finally, let us discuss how inflation begins in our set up. Since we assume that the VEVs of $\phi$ and $S$ are below the Planck scale, it is natural to expect that the universe is in a symmetric phase at a very early epoch at around the Planck time. Then, it is generically expected that cosmic strings are formed when the universe experiences the $U(1)$ phase transition. [^4] Then, as the energy of the universe further drops, the explicit breaking of the $U(1)$ symmetry becomes important, and domain walls are formed in between cosmic strings. As a result, the universe is dominated by networks of strings and domain walls. [^5] This situation is quite similar to the evolution of the string-domain wall network in the case of the QCD-axion [CIT] which is confirmed by numerical simulations, [CIT]. | 803 | 1407.4893 | 11,559,812 | 2,014 | 7 | 18 | true | true | 2 | UNITS, UNITS |
Our optical spectra of GW Ori were taken with the Fiber-fed Extended Range Optical Spectrograph [FEROS, [CIT]], which is mounted on the 2.2 m MPG/ESO (Max-Planck Gesellschaft/European Southern Observatory) telescope, and the High Accuracy Radial velocity Planet Searcher [HARPS, [CIT]], which is mounted on the 3.6 m telescope. Both telescopes are located at La Silla Observatory. The FEROS has a spectral resolution of $\lambda/\Delta\lambda FORMULA \sim$ 115000), but a narrower wavelength coverage (3800--6900Å). With the two instruments, a total of 58 spectra were obtained during 2007--2010 (see Table REF for a detailed description of these observations). Both FEROS and HARPS have their own online data reduction pipelines, which can automatically produce science-quality spectra with calibrated wavelengths from observational raw data. Recently, [CIT] found that the barycentric correction of the FEROS data reduction pipeline is inaccurate, as it induces an artificial one-year period with a semi-amplitude of 62,m,s$^{-1}$. Following [CIT], we apply a more precise barycentric correction that is calculated with the IDL code "baryvel.pro", which is based on the method in [CIT] and gives an accuracy of $\sim$ 1,m,s$^{-1}$. The corrected FEROS spectra are then used in our analysis. | 1,292 | 1407.4959 | 11,560,466 | 2,014 | 7 | 18 | true | false | 1 | MPS |
As shown in section [4.5], while this coupling to matter does not lead to any ghost in the decoupling limit, the BD ghost still appears below the Planck scale although above the strong coupling scale $\Lambda$. In order to trust the exact FLRW solutions found previously, it is therefore essential to establish whether or not this background excites the BD ghost. | 363 | 1408.1678 | 11,613,831 | 2,014 | 8 | 7 | true | true | 1 | UNITS |
In the first part of this work, we reconsidered LTB models without cosmological constant to investigate whether highly flexible, radially fine-tuned mass profiles allow us to simultaneously fit the high local Hubble rate and the CMB data from the Planck satellite [CIT]. To this end, we consecutively compared numerous LTB models with different combinations of observational data. The main results of this first part can be summarised as follows: | 446 | 1408.1872 | 11,616,237 | 2,014 | 8 | 8 | true | false | 1 | MISSION |
A detailed statistical analysis to constrain $\theta$ would be a substantial project, and was not undertaken. Instead, the fact that the alpha-mode effects were most distinctive at very low multipoles was used to get some crude estimates. The effects are then proportional to the amplitude of the scalar perturbations, the tensor-to-scalar ratio $r$, and $\sin\theta$ or $\sin ^2\theta /2$. If $r\gtrsim.1$, then data from Planck [CIT], make values of $|\theta |$ larger than around $.4$ (modulo $2\pi$) unlikely, but if $r\lesssim.01$, no significant constraints were found. More refined analyses may provide more information. | 627 | 1408.2729 | 11,623,133 | 2,014 | 8 | 12 | true | false | 1 | MISSION |
We work with ${\cal N}=1$ supergravity in $d=3+1$ dimensions. Throughout the paper, we focus on the minimal theory containing only a graviton and gravitino. The bulk four-dimensional action is given by FORMULA We use the notation of the (reduced) Planck mass $M_{\rm pl}^2 = 1/8\pi G_N$ instead of the Newton constant $G_N$. Here ${\cal R}_{(4)}$ is the 4d Ricci scalar, with the subscript to distinguish it from its 3d counterpart that we will introduce shortly. There is also the standard Gibbons-Hawking boundary term which we have not written explicitly. | 558 | 1408.3418 | 11,630,942 | 2,014 | 8 | 14 | false | true | 1 | UNITS |
*Suzaku*reveals the source to be reflection-dominated over $\sim$,2--10 keV. The combination of *Suzaku*and *Swift*/BAT data is used to model the broadband X-ray spectrum and show the source to be a bona fide CTAGN. We discuss the origin of the broadband X-ray emission, constraints on the intrinsic source power, and implications for multiwavelength studies of the CTAGN population in general. Luminosities quoted herein are based upon a redshift $z$,=,0.01311 corrected to the reference frame of the Cosmic Microwave Background and with a flat Planck cosmology with $H_{\rm 0}$,=,67.3,km,s$^{-1}$,Mpc$^{-1}$ and $\Omega_\Lambda$,=,0.685 [CIT], corresponding to a distance of 59,Mpc. Note that a Tully-Fisher based distance of 49.6 Mpc is reported in the literature [CIT], but other complementary redshift-independent measurements are lacking. So we use the redshift-based distance herein. All X-ray spectral fitting is carried out with the xspecpackage v12.8.1g [CIT] and uncertainties are quoted at 90% confidence, unless stated otherwise. | 1,042 | 1408.4453 | 11,640,968 | 2,014 | 8 | 19 | true | false | 1 | MISSION |
We wish to know whether allowing a greater active neutrino mass alleviates the tension between Planck+WP and CFHTLenS. We allow the mass, $m_{\nu}$ of the massive neutrino eigenstate in our base $\Lambda$CDM model to vary, above a lower bound of 0.06 eV. We call this model $m_{\nu}\Lambda$CDM. | 294 | 1408.4742 | 11,643,832 | 2,014 | 8 | 20 | true | false | 1 | MISSION |
The results on $A_{\rm mod}$ are shown in Figures REF and in Table REF for different multipole ranges and assuming two different fiducial modulation directions: (i) $(l,b)=(225^\circ, 1^\circ)$, found in [CIT] to maximize the hemispherical asymmetry; (ii) the dipole direction. Note that $(l,b)=(225^\circ, 1^\circ)$ is also very close (actually within the error bars) to the direction $(l,b) = (226^\circ,-17^\circ)$, found in [CIT] to maximize this dipolar modulation. We split the data intro 3 ranges: $\ell\in[2,600]$, which corresponds to the cosmic-variance-limited region of WMAP, $\ell\in[601,1500]$ which are the extra modes precisely measured by Planck (well within the cosmic-variance region) and $\ell\in[2,2000]$, which is the full range of modes accessible ($\ell \gtrsim 2000$ are clearly dominated by noise). Figure REF explores further the maximal asymmetry direction by depicting the measured $A_{\rm mod}$ using $\ell \in [2, \ell_{\rm max}]$ as a function of $\ell_{\rm max}$, together with the corresponding discrepancy with the fiducial, isotropic model. As it can clearly be seen in both figures, neglecting the boost makes the data look anomalous at high-$\ell$. When properly treating the boost we do not find any significant detection for a modulation along the dipole direction, but there is still some nonzero value along the *maximal asymmetry* direction, where for the full range of scales we find $A_{\rm mod} = 0.0044\pm 0.0014$. Such result has an error and a central value which is one order of magnitude smaller than the official Planck results [CIT] which is limited to scales of about $\ell\lesssim 100$, and deviates from zero at the 3.2$\sigma$ level. | 1,690 | 1408.5792 | 11,654,197 | 2,014 | 8 | 25 | true | false | 2 | MISSION, MISSION |
**Introduction.** Recent years have seen staggering progress in the field of CMB observation. High accuracy measurements have transformed the once speculative field of cosmology into a precision science. Combined data from WMAP and Planck [CIT] provides strong evidence for a very early phase of cosmological inflation. The CMB gives constraints on inflation that are by and large consistent with the picture of simple single-field slow-roll inflation. Yet the very same observations contain hints [CIT] that the power of the CMB temperature spectrum may be suppressed by 5%-10% at large angular scales ($\ell\lesssim 40$) compared to a spectrum with $n_s$=$0.960$ and no running. Similarly, the COBE results [CIT] already contain evidence towards the same effect. Cosmic variance [CIT] limits any measurement of the $c_\ell$ to $\Delta c_\ell \sim (2\ell+1)^{-1/2}$. At low-$\ell$, the Planck temperature TT data already reaches this limit. At smaller scales, $\Delta c_{\ell}$ is not yet reached experimentally everywhere, and adding future data may still lead to slight variations of the value of $n_s$. Adding future polarization data will provide additional independent data at low-$\ell$ in form of the TE and EE correlations. Moreover, future large-scale structure surveys and 21-cm tomography may provide even more modes at low-$\ell$ due to an increased sample volume compared to the CMB alone [CIT]. Thus the significance of the observed power loss may still change considerably in the future [CIT]. Finally, if the B-mode polarization detected by BICEP2 [CIT] corresponds to a primordial tensor mode signal from inflation with $r\sim 0.1$, this would roughly double the amount of power suppression hinted for by the CMB data at low-$\ell$ [CIT]. | 1,756 | 1408.5904 | 11,655,184 | 2,014 | 8 | 25 | true | true | 2 | MISSION, UNITS |
However, despite significant progress that has been made towards a reliable description of pitch-angle scattering [e.,g., [CIT] :hom; [CIT] :pit; [CIT] :pit; [CIT] :sto], an all-encompassing theoretical understanding is still elusive. Here, we show the modifications obtained for the Fokker-Planck coefficient of pitch-angle scattering by introducing a new unperturbed orbit under the assumption of a (constant) adiabatic focusing length for the magnetic field. While the classic quasi-linear result is retained in the limit of a homogeneous magnetic field, it will be shown that in general the Fokker-Planck coefficient---and thus the parallel mean-free path---is strongly altered. | 682 | 1408.6947 | 11,665,831 | 2,014 | 8 | 29 | true | false | 2 | FOKKER, FOKKER |
The noise is simulated at the map level, and is uncorrelated from pixel to pixel. The noise standard deviation maps are designed to be consistent with the scanning strategy chosen for the Planck spacecraft and is therefore anisotropic. In the harmonic domain the noise is characterized by one white power spectrum per frequency, derived from the noise standard deviation maps. Our inference approximate the noise as isotropic. The impact of this approximation will be assessed in Sect. [5]. | 490 | 1409.0858 | 11,676,549 | 2,014 | 9 | 2 | true | false | 1 | MISSION |
These algorithms inconveniently both require us to really capture the full state of the evaporation. As soon as we start making mistakes, for example because it is rather difficult to detect gravitons, they don't work. In particular if we try to use the swap test to compare subsystems of the two states then the states would be mixed and as just argued the test would fail. To deal with missing (or corrupted) radiation we need to do some kind of quantum error correction. A brief introduction to quantum error correction and its computational complexity is given in section 4 of [CIT]. The upshot is that quantum error correction is possible provided that we don't lose too much of the radiation; we can lose or corrupt up to almost half if we know which part is affected, while if we don't know we can lose or corrupt up to a quarter. Recalling our observation in section [4.3] that black holes radiate less into higher spin particles, losing gravitons is thus not really a principled obstruction: even if we don't measure any of them we will be able to correct for the loss. Unfortunately it seems likely that this error correction procedure will take exponential time in the number of affected qubits, so if an $O(1)$ fraction of the radiation is lost then the correction procedure will probably take a time which is exponential in the black hole entropy. To deal with this exponential we thus need to take the entropy to be at most $O(10-20)$, which corresponds to a black hole whose radius is only slightly larger than the Planck scale. | 1,543 | 1409.1231 | 11,680,388 | 2,014 | 9 | 3 | false | true | 1 | UNITS |
In order to remove contaminating radio sources from the SB data, the LB CARMA-8 data were used to identify the location of the compact radio sources and provide an initial estimate of their peak flux density. This initial set of source parameters was fit directly to the LB visibility data and the best-fit parameters were determined using the task ([CIT]). Using these best-fit parameters, the contribution to the SB data from detected LB radio sources was removed. Radio source-subtracted, ed[^7] maps were produced, see Figure REF for CARMA-8 SZ-detected clusters, and Figure REF for candidate clusters without a CARMA-8 detection. Details on the SZ signal detected by CARMA and Planck are given in Table REF. For those CARMA-8 data that required the contribution from LB-detected radio sources to be removed, the reader should note that the source-subtracted SB images represent the map with the most-likely source parameters and, thus, uncertainties in the source parameters are not reflected in the final map. Given that the cluster and source parameters can be degenerate, a quantitative analysis should fit for the cluster and radio-source contributions jointly. This analysis is undertaken in paper II of this work (Rodríguez-Gonzálvez et al. *in prep*). | 1,263 | 1409.1978 | 11,690,348 | 2,014 | 9 | 6 | true | false | 1 | MISSION |
Therefore, as just mentioned, the Maldacena's consistency condition plays important roles in tensor fossil effects. In models which violate the consistency condition, this fossil effect can be large. With this motivation in mind, recently in [CIT], the tensor fossil effects in solid inflation and non-attractor models [CIT], as two known examples of single field models which violate the Maldacena's consistency condition, have been studied. The tensor-scalar-scalar bispectrum which they used is obtained with the assumption of $F_Y\sim F$, which as we already pointed out, is in some tensions with the Planck constraints on non-Gaussianity. In order to ease the tension, the authors of [CIT] extended the results of [CIT] to the limits $F_Y \lesssim \epsilon F$. However, as we have discussed in Section [3], in this limit there are other contributions to the bispectrum which can not be neglected and are not captured in the analysis of [CIT]. Now, with the tensor-scalar-scalar bispectrum calculated in Eq. (REF) valid for general values of $F_Y/F$ and $F_Z/F$ (subject to the upper bound REF(#Superluminal){reference-type="eqref" reference="Superluminal"}), we are ready to calculate the tensor fossils in solid inflation in the regime which leads to non-Gaussianity consistent with the Planck. | 1,300 | 1409.3004 | 11,699,720 | 2,014 | 9 | 10 | true | true | 2 | MISSION, MISSION |
Excited KK modes of the graviton, $G^*$, which are localized on the SM brane, are predicted in Randal--Sundrum (RS) models with a warped spacetime metric. Two parameters determine graviton couplings and widths: the constant $k/\overline{M}_{PL}$, where $k$ is the curvature scale of the extra dimension, and $\overline{M}_{PL}= M_{PL}/\sqrt{8}$ is the reduced Planck scale, and graviton excitation, $M_1$. The D0 [CIT] and the CDF experiments [CIT] searched for evidence of single RS graviton production and decay via $G^*\to \ell\ell$ or $VV$. No significant excess of events in the dilepton ($e$ or $\mu$) or $\gamma\gamma$ was found and limits are shown in Fig. REF(a,b). The results from the searches for the other diboson resonances described in the previous section were also interpreted as limits on the RS graviton production [CIT]. Limits from the $G^*\to WW$ are set for a mass $m_{G^*}<754$ GeV when $k/\overline{M}_{PL}=0.1$. In $G^*\to ZZ$ an excess of events is observed in low yield four--lepton channel at the $M_{G^*}=327$ GeV, but it was not confirmed in the more sensitive searches in the $\ell\ell jj$ and $\ell\ell\mbox{$\not\!\!E_T$}$ final states [CIT]. Figure REF(c) shows the results. | 1,209 | 1409.4910 | 11,720,079 | 2,014 | 9 | 17 | false | true | 1 | UNITS |
Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. 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, University of Cambridge, 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. | 1,202 | 1409.7389 | 11,744,096 | 2,014 | 9 | 25 | true | false | 2 | MPS, MPS |
The Sloan Digital Sky Survey (SDSS) is a photometric and spectroscopic survey that covers one-quarter of the celestial sphere in the north Galactic cap [CIT]. Observations were performed using a $2.5$ m wide-field optical telescope. The spectra have an instrumental velocity resolution $\sigma$ of $\sim 65$ km/s and the spectral coverage is $3,800-9,200$Å. The measured galaxies have a median redshift of $z\sim0.1$. Spectra were taken with $3\arcsec$ diameter fibers ($5.7$ kpc at $z\sim0.1$), which makes the sample sensitive to aperture effects (see Sect. 2.4). Low redshift objects are likely to be dominated by nuclear emission [e.g., [CIT]]. The Max-Planck-Institute for Astrophysics (MPA)-Johns Hopkins University (JHU) Data Release 7 (DR7) of spectral measurements[^1] contains the derived galaxy properties from the MPA-JHU emission line analysis for the $\sim10^6$ objects in the SDSS DR7 [CIT]. Stellar population synthesis spectra [updated [CIT]] have been used for the stellar continuum subtraction. The MPA-JHU contains, in particular, the emission-line measurements of the low-ionization lines that are used in diagnostic diagrams to separate star-forming galaxies from the AGN families (Seyferts and LINERs, or high- and low-excitation systems). Optical images are available as well. Total stellar masses are also provided and estimated by fitting broad-band spectral energy distributions (SEDs) with stellar population models. | 1,444 | 1409.7396 | 11,744,594 | 2,014 | 9 | 25 | true | false | 1 | MPS |
Figure REF shows examples of the emissivity, normalized to the blackbody intensity, as a function of the photon energy $E=\hbar\omega$, in both the free- and fixed-ion limits, for the wave-vector inclination angle $\theta_\mathrm{k}=45^\circ$, $B=10^{13}$ G and $10^{14}$ G, and different values of the magnetic-field inclination $\theta_\mathrm{n}$ and azimuthal angles $\varphi_k$. The characteristic energies $E_\mathrm{ci}=\hbar\omega_\mathrm{ci}$, $E_\mathrm{pe}=\hbar\omega_{\mathrm{pe}}$, and $E_\mathrm{C}=E_\mathrm{ci}+E_\mathrm{pe}^2/\hbar\omega_\mathrm{c}$ are marked. The spectral features near these energies are explained in [CIT]. For instance, the emissivity suppression at $E_\mathrm{ci}\lesssim E\lesssim E_\mathrm{C}$ is due to the strong damping of one of the two normal modes in the plasma in this energy range. There is a resonant absorption, depending on the directions of the incident wave and the magnetic field, near $E_\mathrm{pe}$. The local flux density of radiation from a condensed surface is equal to the Planck function $\mathcal{B}_{\omega,T}$ multiplied by the normalized emissivity. | 1,118 | 1409.7666 | 11,746,827 | 2,014 | 9 | 26 | true | false | 1 | LAW |
Depending on how one chooses to characterize the dark energy and its equation-of-state $p_\Lambda=w_\Lambda\rho_\Lambda$, $\Lambda$CDM can have as many as 7 free parameters, including the Hubble constant $H_0$, the matter energy density $\Omega_m\equiv \rho_m/\rho_c$ normalized to today's critical density $\rho_c\equiv (3c^2/8\pi G)H_0^2$, the similarly defined dark energy density $\Omega_\Lambda$, and $\Omega_k$, representing the spatial curvature of the Universe---appearing as a term proportional to the spatial curvature constant $k$ in the Friedmann equation. In this paper, we will take the minimalist approach and consider only the most essential parameters needed to fit the AGN data. For this purpose, we will take guidance from other observations (such as those with WMAP and Planck), which indicate that $k=0$ (i.e., that the Universe is spatially flat). In other words, we will treat $k$ as a prior and not include it in the optimization procedure, which means that $\Omega_m+ \Omega_\Lambda=1$ in the redshift range of interest. As such, the $\Lambda$CDM model we use here for comparison with the $R_{\rm h}=ct$ Universe is characterized by three essential parameters: $H_0$, $\Omega_m$ and $w_\Lambda$, with the additional restriction that the Universe has no phantom energy, i.e., that $w_\Lambda\ge -1$. | 1,323 | 1409.7815 | 11,748,364 | 2,014 | 9 | 27 | true | false | 1 | MISSION |
[^6]: The observed spectrum is expected to deviate from the Planck function due to the fact that photons arriving at any given time at the observer in fact originated at different radii and time. Hence, the observed spectrum is a superposition of Planck functions of different temperatures. In particular, the observed spectrum below the peak is likely flattened to $f_\nu \aprop \nu^{1.4}$ from the original $f_\nu\propto \nu^2$ shape [CIT]. And if the LF of the jet has an angular dependence such that it peaks at the jet axis and decreases with angle then the observed spectrum is flattened even further and can become $f_\nu \propto \nu^{0}$ [CIT]. | 652 | 1410.0679 | 11,763,779 | 2,014 | 10 | 2 | true | false | 2 | LAW, LAW |
A natural explanation for the negative values of [Fe I/H]$-$[Fe II/H] measured for our AGB sample would be that these stars suffer for departures from the LTE condition, which mainly affects the less abundant species (in this case Fe I), while leaving virtually unaltered the dominant species [i.e. Fe II; [CIT]]. In late-type stars, NLTE effects are mainly driven by overionization mechanisms, occurring when the intensity of the radiation field overcomes the Planck function [see [CIT] for a complete review of these effects]. These effects are predicted to increase for decreasing metallicity and for decreasing atmospheric densities (i.e., lower surface gravities at a given $T_{\rm eff}$), as pointed out by a vast literature [see e.g. [CIT]]. At the metallicity of 47 Tuc, significant deviations are expected only for stars approaching the RGB-Tip. [CIT] computed a grid of NLTE corrections for a sample of Fe I and Fe II lines in late-type stars over a large range of metallicity. Assuming the atmospheric parameters of the 11 RGB stars in our sample and the measured EWs of the iron lines in common with their grid (25 Fe I and 9 Fe II lines), the predicted NLTE corrections are [Fe/H]$_{\rm NLTE}-$[Fe/H]$_{\rm LTE}\simeq +0.04$ dex. This is consistent with no significant differences between [Fe I/H] and [Fe II/H] found in our analysis (Section [4.1]) and in previous studies [see e.g. [CIT]]. Instead, a larger difference ([Fe I/H]$-$[Fe II/H]$= -0.08$ dex) has been found for the brightest RGB stars in 47 Tuc [CIT], as expected. [^6] | 1,547 | 1410.3841 | 11,794,888 | 2,014 | 10 | 14 | true | false | 1 | LAW |
The recent measurements based on BICEP2 [CIT] and Planck [CIT] results of CMB B-mode polarization indicate two different values for the tensor-to-scalar modes perturbation ratios, given by $r_{BICEP2} \approx 0.2$ and $r_{Planck} \le 0.11$. Note that $r_{BICEP2}$ is a specific value while $r_{Planck}$ gives an upper bound. There is an impression that the Planck data is more reliable and probably gives the correct number (there is question about the BICEP2 results -- that some or all of the signal may be due to dust). But as we see below this variation does not affect our conclusion by much. The energy scale of inflation, ${\cal E}_{inf}$, is related to $r$ via the following relationship FORMULA Since ${\cal E}_{inf}$ depends on the one-fourth power of the ratio $r$, its contribution corresponding to both observations is of the order of unity (if one assumes that $r_{Planck}$ is not too far below its upper value of $0.11$). This approximately gives the energy scale of inflation as ${\cal E}_{inf} \sim 10^{16} GeV$, which corresponds to the GUT energy scale. Converting this energy scale to a timescale gives an inflationary time scale of $t_{inf} \sim 10^{-38} - 10^{-39} s$. This matches the time scale of our model for inflation driven by Hawking-like radiation with the chosen value of $K_0\sim 10^{6}$ which was fixed so as to obtain the observed value of $\eta$ needed to generate the correct amount of baryogenesis in our model. | 1,449 | 1410.6785 | 11,798,405 | 2,014 | 10 | 15 | true | true | 5 | MISSION, MISSION, MISSION, MISSION, MISSION |
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