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*WMAP* provided maps at five frequency bands between 23 and 94,GHz [CIT]. In the lower three frequencies the sky polarisation is dominated by Galactic synchrotron emission, with a brightness temperature that drops steeply with frequency ($T_\nu \propto \nu^{\beta}$, with $\beta \approx -3$). Since the brightness temperature sensitivity is similar in all bands, the highest SNR is at 23,GHz (K band), where large areas of diffuse polarised emission have $\mbox{SNR}>3$ after smoothing to 1$^{\circ}$FWHM resolution. In these bands the synchrotron polarisation angle reflects the Galactic magnetic field direction in the source regions, and is expected to be almost independent of frequency. The most likely cause of any frequency variation is superposition on the line of sight of regions with different field directions and also difference spectral indices $\beta$; however, the variation of $\beta$ for the synchrotron component is small as has been shown by [CIT]. On the other hand, the higher *WMAP* bands begin to be sensitive to dust polarisation, which has $\beta \approx +1.7$, and Planck data confirm that this is generally significantly misaligned with synchrotron [CIT]. For this reason we only consider the three lowest *WMAP* bands below. | 1,253 | 1410.4436 | 11,799,526 | 2,014 | 10 | 16 | true | false | 1 | MISSION |
The cross-correlation APS between the Plancklensing map and the *Fermi-LAT* $\gamma$-ray map is estimated using a pseudo-$C_\ell$ approach [CIT]. To this aim, we make use of the publicly available tool PolSpice [CIT]. Although the PolSpice algorithm properly deconvolves the signal APS from mask effects, it is known not to be a minimum variance algorithm [CIT]. Thus the associated covariance matrix is likely to be an overestimation of the actual uncertainty, and the significances reported throughout the paper can in turn be considered as conservative. | 556 | 1410.4997 | 11,805,474 | 2,014 | 10 | 18 | true | true | 1 | MISSION |
We reported the first indication of a cross-correlation between the unresolved $\gamma$-ray sky and CMB lensing. The analysis also points towards a direct evidence that the IGRB is of extragalactic origin. The analysis has been based on the $\gamma$-ray data of the first 68 month of operation of the *Fermi-LAT* and on the 2013 public release by the PlanckCollaboration of the CMB lensing potential map. Current models of AGN and SFG can fit well the amplitude, angular dependence and energy spectrum of the observed APS. The size of the signal appears to be robust against variations of the analysis assumptions. Data exhibit a preference for a signal with the correct features expected from the extragalactic gamma-ray emission with a $3.0\sigma$ significance. | 763 | 1410.4997 | 11,805,490 | 2,014 | 10 | 18 | true | true | 1 | MISSION |
These results call for the study of the evolution of electron spectra at the energies far exceeding that of equilibrium. At that, the last term in a Fokker-Planck Eq. (7) can be omitted since $\theta_0 \ll \theta_{in}$, so that in terms of number density $\rho^{(e)} \propto \mu^2 g^{(e)}$ it can be reduced to FORMULA which is essentially a continuity-like equation. Again, it is fully integrable, and its general solution is FORMULA where $\Phi (x)$ is an arbitrary function of $x$ defined here by initial conditions, e. g. a MJ-distribution with $\theta_{in} \gg 1$. A resulting analytic solution for $\rho^{(e)} (\mu, \tau)$ with $f = f_{_M}$, Eq. (15), for $\rho^{(e)}$ $vs$ $\mu$ for various ${\tau} = (\theta^3 / q) t / t_C$ is plotted in Fig. 3 for initial temperature, $\theta_{in} = 10^5 \mu_{_C}$ or $k_B T_{in} = 10^{19} eV$. | 837 | 1410.6953 | 11,825,362 | 2,014 | 10 | 25 | true | false | 1 | FOKKER |
Since the standard model couplings are weak at the unification point, whilst the inflationary model is still strongly coupled at this scale (now identified with $\Lambda$). this feature allows us to decouple the contributions of the SM from inflationary theory and ensures that the action formulating inflation does not include any contributions from the SM. For this model, we show that inflation starts at energy scales just below or near the energy scales above which the underlying gauge dynamic is perturbative and expect the perturbative dynamic of the gauge theory to set in before arriving at the Planck scale. | 618 | 1410.7547 | 11,831,485 | 2,014 | 10 | 28 | false | true | 1 | UNITS |
As there are several interferometric experiments at or close to Planck sensitivity, it is important to generate consistent predictions for those experiments in order to make sure that this hypothesis is not already ruled out. Here we will focus on two of the most sensitive experiments, first GEO-600 and then LIGO in the following section. We will be mostly following the assumptions made for the baseline prediction in the previous section. | 442 | 1410.8197 | 11,839,264 | 2,014 | 10 | 29 | false | true | 1 | MISSION |
We have presented new low-frequency observations of Fornax A at 154 MHz from the MWA and used these data, along with previously published data at 1510 MHz, to conduct a spatially resolved study of the spectral index of Fornax A. We have also presented microwave flux densities obtained from Planck and *WMAP* data and $\gamma$-ray flux densities from *Fermi*-LAT data and used these, in combination with previously published flux-density measurements at radio and X-ray energies, to model the spectral energy density of Fornax A. Our results best support a scenario where the X-ray photons are produced by inverse-Compton scattering of the cosmic microwave background and extragalactic background light by the radio-synchrotron emitting electrons in the lobes, while the $\gamma$-rays are the result of proton-proton collisions localised in the lobe filaments. | 860 | 1411.1487 | 11,860,396 | 2,014 | 11 | 6 | true | false | 1 | MISSION |
Here we study the predictions for asymmetry in polarization auto-correlations and cross-correlations, assuming that only one type of mode generates the asymmetry. In what follows we always fix the six parameters in the $\Lambda CDM$ model to the best fit values from Planck data [CIT]. In addition, the spectral index of isocurvature mode is also assumed to be the same as the adiabatic mode for simplicity. In this and next sections whenever any of sub-dominant modes (i.e. tensor and isocurvature modes) do not contribute to the dipole asymmetry (i.e. their power spectrum is symmetric) we neglect their sub-leading contributions to the symmetric part of the power spectrum as well (i.e. by setting either $r=0$ or $\beta=0$). | 728 | 1411.5312 | 11,897,843 | 2,014 | 11 | 19 | true | true | 1 | MISSION |
The dark matter particle in this model can be a neutral scalar ($\eta_{R,I}$) or a singlet fermion ($N_1$). Both possibilities have been examined in the previous literature and it is known that they give rise to a different phenomenology. We assume in the following that the dark matter is the singlet fermion and that its relic density is the result of a freeze-out process in the early Universe (freeze-in [CIT] is an alternative possibility we do not consider), as this is the most interesting scenario from the point of view of LFV processes. In this case, the dark matter relic density is determined by the $N_1$ annihilation rate, which depends on the Yukawa couplings. Since they must be large enough to explain the observed dark matter density, the rates of LFV processes, which are proportional to these Yukawas, are generally expected to be observable. We examine two different dark matter scenarios depending on the process that sets the value of the relic density: $N_1$-$N_1$ annihilations or $N_1$-$\eta$ coannihilations ($N_1$-$N_2$ coannihilations are rarely relevant as they depend on the same Yukawa couplings as $N_1$-$N_1$). For each case, we require the corresponding process to be dominant. We have implemented the scotogenic model into micrOMEGAs [CIT], which accurately computes the relic density taking into account all relevant effects, including resonances and coannihilations. All our viable models are consistent with the observed value of the dark matter density, as determined by WMAP [CIT] and PLANCK [CIT]. | 1,539 | 1412.2545 | 11,949,136 | 2,014 | 12 | 8 | false | true | 1 | MISSION |
We thank the anonymous referee for thorough reviews, critical comments and numerous, constructive suggestions that greatly improved this paper, and in particular, for bringing the Lanza et al. modification of the Applegate mechanism to our attention. We are very grateful to Antonino F. Lanza for explanations regarding the Applegate effect and its observational constraints. This work has been supported by Polish National Science Centre MAESTRO grant DEC-2012/06/A/ST9/00276 (K.G.), SONATA grant DEC-2011/03/D/ST9/00656 (A.S., K.K., M.Ż.), and SONATA BIS DEC-2011/01/D/ST9/00735 (M.G.). We thank the Skinakas Observatory for their support and allocation of telescope time. Skinakas Observatory is a collaborative project of the University of Crete, the Foundation for Research and Technology -- Hellas, and the Max-Planck-Institute for Extraterrestrial Physics. This work is based on observations made with the 2-m telescope operated by the National Astronomical Observatory in Rozhen (Bulgaria). We thank the staff of NAO for their generous support and telescope time. This work has made use of data obtained at the Thai National Observatory on Doi Inthanon, operated by NARIT. We also provide observations with the 1.55-m Carlos Sánchez Telescope operated on the island of Tenerife by the Instituto de Astrofísica de Canarias in the Spanish Observatorio del Teide. We would like to thank Yucel Kilic for his help with observations at the TÜBİTAK National Observatory. K.G. thanks the Poznań Supercomputer and Network Centre (PCSS, Poland) for computational grant No. 195 and technical support. Computations in this work were carried out on the `cane` and `chimera` supercomputers of the PCSS. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. | 1,847 | 1412.5899 | 11,987,034 | 2,014 | 12 | 18 | true | false | 1 | MPS |
Recently an unprecedented amount of data has become available to constrain the properties of primordial fluctuations which source structure in our universe. This includes the results from the Planck satellite [CIT], the BICEP2 collaboration [CIT], and the South Pole Telescope (SPT) [CIT], as well as many others. Single field slow roll inflation, based on a scalar field, the inflaton, appears compatible with all the data. However, in addition to the inflaton, there might be other scalars present during inflation. Indeed, unless the Standard Model couplings are drastically modified at inflationary energies, we know that there is at least one light isocurvature scalar, the Higgs, which was present during inflation and acted as a spectator field [CIT]. | 758 | 1412.5973 | 11,988,019 | 2,014 | 12 | 18 | true | false | 1 | MISSION |
The amplitude of the tSZ power spectrum was predicted analytically by [CIT], with an expected value of $8-10 {\mu\mathrm{K}^2}$ around $\ell = 3000$. Later semi-analytic modeling predicted similar values [CIT], but experimental results have confirmed these early predictions to be too high. The first conclusive measurement of the combined tSZ$+$kSZ power spectrum came from the South Pole Telescope [SPT; [CIT]]. Successive data releases from the SPT and ACT (Atacama Cosmology Telescope) have provided increasingly sensitive and consistent measurements of the tSZ power on arcminute scales ($\ell \sim \mathrm{few}\times 1000$) where the contributions from galaxy groups and clusters are expected to peak [CIT]. Recent results from the Planck spacecraft are also consistent with the SPT value within $2\sigma$ [CIT], although the Planck resolution cannot resolve the position of the peak of the tSZ power, and is more sensitive on roughly degree angular scales. At these low multipoles, the two-halo correlation term might be important, or the contribution from the warm-hot intergalactic medium (WHIM) might dominate [e.g., [CIT]]. | 1,134 | 1412.6023 | 11,988,618 | 2,014 | 12 | 18 | true | false | 2 | MISSION, MISSION |
We revisit the scenario where inflation is preceded by a radiation era by considering that the inflaton too could have been in thermal equilibrium early in the radiation era. Hence we take into account not only the effect of a pre-inflationary era on the inflaton mode functions but also that of a frozen thermal distribution of inflaton quanta. We initially discuss in detail the issues relevant to our scenario of a pre-inflationary radiation dominated era and then obtain the scalar power spectrum for this scenario. We find that the power spectrum is free from infrared divergences. We then use the WMAP and Planck data to determine the constraints on the inflaton comoving `temperature' and on the duration of inflation. We find that the best fit value of the duration of inflation is less than 1 e-folding more than what is required to solve cosmological problems, while only an upper bound on the inflaton temperature can be obtained. | 941 | 1412.7093 | 11,997,285 | 2,014 | 12 | 22 | true | true | 1 | MISSION |
As we will discuss below, conical defects are curvature singularities. Thus a given defect carries some mass/energy on its infinitely thin hyperplane. In 2+1-dimensional gravity the Newton's constant $G$ has the dimension of inverse mass[^1] (it is the inverse Planck mass) and hence provides a natural mass scale for the theory. The quantity $\mu := Gm$ is the dimensionless "rest energy per point\", which is proportional to the deficit angle of a particle at rest $\alpha = 8\pi Gm$. If we generalize this picture to $n + 1$ dimensions, $G$ will have the dimension of length to the power $n - 2$ times inverse mass. Similarly to the three-dimensional case we can then define the dimensionless energy density $\mu := G\rho$, where $\rho$ is the mass per unit of volume of the defect's hyperplane (e.g. length of the string in 3+1 dimensions). | 844 | 1412.8452 | 12,013,467 | 2,014 | 12 | 29 | false | true | 1 | UNITS |
In 2013 the Planck mission has delivered its measurements of the CMB temperature anisotropies. The CMB angular power spectrum has been measured with a high accuracy down to very small scales. It is found to be in a very good agreement with the best fit of the standard cosmological model, assuming that primordial perturbations are well described by the amplitude and the spectral index of their power spectrum. With Planck combined to observations of the Baryon Acoustic Oscillations and type 1-a supernovae, the cosmological parameters have been measured with an unprecedented accuracy [CIT]. As already mentioned, the scalar power spectrum amplitude and spectral index are respectively given by $A_{\mathrm s} = 2.196^{+0.051}_{-0.06} \times 10^{-9}$ and $n_{\mathrm s} = 0.9603 \pm 0.0073$. An important point is that $n_s <1$ at more than $4\sigma$, which rules out models predicting a scale invariant or a blue tilted scalar power spectrum (such as the original hybrid model). An upper bound on the tensor to scalar ratio ($r \lesssim 0.11$) has also been derived by combining Planck data to the measurements by WMAP of the CMB polarization. The Planck limits in the plane $(n_{\mathrm s},r)$ are given in Fig. REF, together with the predictions of some of the most well-known inflation models. One can observe that the limit where convex potentials will be disfavored at the 95% C.L. is not far, and that simple potentials like $V\propto \phi^4$ and $V \propto \phi^3$ are already strongly disfavored. Simple supersymmetric models like F-term and D-term inflation are also in strong tension with Planck data, because they predict typically that $0.98 \lesssim n_{\mathrm s} \lesssim 1$. | 1,693 | 1501.00460 | 12,021,421 | 2,015 | 1 | 2 | true | true | 5 | MISSION, MISSION, MISSION, MISSION, MISSION |
When it comes to testing the quadratic term for LIV, having a very high energy component compensates for a lack of distance. Pulsars represent a fast varying, relatively well understood source population with very different intrinsic source physics processes to GRBs and AGN. The Crab pulsar has a pulsed VHE component to its spectrum up to hundreds of GeV and little evidence of a cut-off (within event statistics). Whilst the LIV limits from current generation instruments are presently inferior to those from AGN and GRBs [CIT], a millisecond pulsar observed at 1,TeV with CTA has the potential to place stringent limits (even above the Planck scale on the linear term). As a pulsar has a very well measured lightcurve profile it also makes for an interesting source to test for any lightcurve broadening that might occur from a polarisation dependent superluminal correction (see e.g. [CIT]). | 896 | 1501.00824 | 12,023,918 | 2,015 | 1 | 5 | true | true | 1 | UNITS |
We have set an upper bound on the RH sneutrino relic abundance, $\Omega_{{\tilde N}_1} h^2<0.13$, consistent with the latest Planck results [CIT]. Besides, we have considered the possibility that RH sneutrinos only contribute to a fraction of the total relic density and set for concreteness a lower bound on the relic abundance, $0.001<\Omega_{{\tilde N}_1} h^2$. To deal with these cases, the fractional density, $\xi=\min[1,\Omega_{{\tilde N}_1}h^2/0.11]$, has been introduced to account for the reduction in the rates for direct and indirect searches (assuming that the RH sneutrino is present in the DM halo in the same proportion as in the Universe). | 656 | 1501.01296 | 12,028,177 | 2,015 | 1 | 6 | true | true | 1 | MISSION |
So far most CMB experiments indicate that CMB anisotropies are statistically isotropic and Gaussian and so can be completely characterized by their two-point correlations or power spectrum [CIT]. Although, almost all the CMB observations confirm that the six parameter $\Lambda$CDM cosmological model best fits the observed data, still there are some anomalies which have always been present from COBE to Planck. One of such anomalies has been the lack of power in the CMB-TT power spectrum ($C_l^{TT}$) at large angular scales or low-$\ell$ [CIT]. Recently, [CIT] studied the consistency of the standard $\Lambda$CDM model with the Planck data using the Crossing statistic [CIT]. Their results indicate that the Planck data is consistent to the concordance $\Lambda$CDM only at 2-3$\sigma$ confidence level and lack of power at both high and low $\ell$'s with respect to concordance model. The low power at large angular scales can be attributed to cosmic variance [CIT], still there have been efforts to explain this anomaly by changing the potential of inflation field (for a comprehensive review check [CIT]), considering different initial conditions at the beginning of inflation [CIT], ISW effect [CIT], spatial curvature [CIT], non-trivial topology [CIT], geometry [CIT], violation of statistical anisotropies [CIT], cosmological-constant type dark energy during the inflation [CIT], bounce from contracting phase to inflation [CIT], production of primordial micro black holes (MBH) remnants in the very early universe [CIT], hemispherical anisotropy and non-gaussianity [CIT], string theory [CIT], loop quantum cosmology [CIT] etc. Although, inflationary $\Lambda$CDM model with almost scale-invariant power spectrum has emerged most successful model from the recent observations, it is important to note it does not uniquely confirm the generic picture of the universe and the generalization of primordial power spectrum having additional features like cut off, oscillations would be crucial in identifying specific inflationary models. | 2,045 | 1501.02647 | 12,040,775 | 2,015 | 1 | 12 | true | false | 3 | MISSION, MISSION, MISSION |
Our numerical study based on a more advanced approximation as described in App. [7] shows that already with moderately small values $\lambda_6\approx 0.25$ the cutoff scale can be increased by approximately two orders of magnitude while retaining the full stability of the electroweak vacuum. This can be seen from the green region I in Fig. REF. Increasing the possible cutoff scales by further orders of magnitude is difficult since there is a strongly infrared-attractive pseudo-fixed point at $|\lambda_6|\approx 0$ for those scales, see Sec. [2.5] below. Next, there is a large pseudo-stable region (blue) where the UV-potential as well as the low-energy effective potential are stable, but our polynomially expanded potentials exhibit further minima at intermediate scales. As already explained, this is beyond the strict validity of our approximation and further studies are needed. Already relatively small values of $\lambda_{6}$ are sufficient to stabilize the UV-potential --- although not the minimum at $H=0$ --- up to the Planck scale, since $\lambda_{4}$ is negative, but its absolute value remains quite small. Finally, in the red region III the UV-potential is already meta-stable, as might be the effective potential. In this region the cutoff can easily take values beyond the Planck scale even for tiny values of $\lambda_{6}$, because the tunneling rates are always small enough to guarantee the longevity of the electroweak vacuum. | 1,453 | 1501.02812 | 12,042,906 | 2,015 | 1 | 12 | false | true | 2 | UNITS, UNITS |
Here the first sum is over all *RedMaPPer* clusters that have been detected by Planck and the second sum is over all *RedMaPPer* clusters that have not been detected by Planck. Figure REF shows the photo-z distribution of the Planck sample (black) compared to the subsample (red) defined by the selection algorithm based on detection probability. The data agree in most bins within 1$\sigma$ (of the Poissonian errors) and in all bins within 2$\sigma$. To validate the quality of the comparison sample we drew 1000 random subsamples of 250 clusters according to their $P_{\mathrm{det}}$ and determined the likelihood of each subsample. Comparing to the likelihood of the original Planck sample, we obtain a p-value of 0.27, so we consider our comparison sample as reasonable (i.e., 27% of subsamples have lower likelihood than the actual Planck sample). | 853 | 1501.02840 | 12,043,427 | 2,015 | 1 | 12 | true | false | 5 | MISSION, MISSION, MISSION, MISSION, MISSION |
In this review article we have studied the overall dynamics of the FLRW flat cosmological models in which the vacuum energy varies with the Hubble parameter, namely $\Lambda(H)=\Lambda_{0}+3\nu(H^{2}-H^{2}_{0})$. First we have performed a joint likelihood analysis in order to put constraints on the main cosmological parameters by using the current observational data (SNIa, BAOs and CMB shift parameter together with the growth rate of galaxy clustering). We have shown that the $\Lambda(H)$ model fits slightly better the observational data than that of the traditional $\Lambda$ cosmology. In particular, we have found that the $\Lambda$CDM model can not simultaneously accommodate the Planck priors and the growth data implying that this kind of data favor the $\Lambda(H)$ vacuum scenario. Subsequently we have investigated the nonlinear regime and considered the predicted redshift distribution of cluster-size collapsed structures as a powerful method to distinguish the $\Lambda(H)$ and $\Lambda$CDM cosmological scenarios. Finally, we have generalized the properties (virial theorem, collapse factor, virial and turnaround densities) of the spherical collapse model in the case when the vacuum energy is a running function of the Hubble rate, $\Lambda=\Lambda(H)$. Overall, we have found that the virial density contrast is affected by the considered status of the vacuum energy model (homogeneous or clustered). | 1,422 | 1501.03749 | 12,053,001 | 2,015 | 1 | 15 | true | true | 1 | MISSION |
Primordial non-Gaussianity is a powerful test of inflationary models---and Planck has already ruled out those models that generate large non-Gaussianity. The key target is the simple single-field inflation models. These models generate negligible non-Gaussianity, but a nonlinear GR correction to the Poisson equation means that large-scale structure would measure $f_{\rm NL}\sim -2$. (We will discuss this and the new techniques to improve constraints on primordial non-Gaussianity via a proper accounting of the relativistic effects in detail in [CIT].) SKA HI galaxy redshift surveys will greatly help on this effort. Indeed, [CIT] showed that a HI galaxy redshift survey covering the range $0<z\leq3$ is able, thanks to the huge volume it probes, to put the currently most stringent constraint on $f_{\rm NL}$ from a single threshold tracer, i.e. $\sigma(f_{\rm NL})=1.54$. Moreover, their analysis has been performed for the first time by fully accounting for the GR effects described above. More specifically, the numbers used for the bias and galaxy redshift distribution for different flux cuts were taken directly from simulations. The other parameters required for the relativistic corrections were in turn directly derived from these parameters, which allowed for a fully consistent analysis of the fluctuations on ultra-large scales taking into account the GR corrections. | 1,385 | 1501.04035 | 12,056,382 | 2,015 | 1 | 16 | true | false | 1 | MISSION |
The spectral distribution of a photon gas which is in equilibrium with matter (e.g rarefied gases) at temperature $T$ is given by the Planck distribution which can be written in terms of the a-dimensional frequency $x=h \nu/k_B T$ as FORMULA For the case of the CMB, $T=T_{\text{CMB}}=2.725 \pm0.001$ K [CIT] and $h$ is the Planck constant, $k_B$ is the Boltzmann constant and $c$ is the speed of light. In a ionized plasma with electron plasma frequency $x_p$, deviations from Planck distribution in eq.(REF) are possible because photons are suppressed at frequencies lower than $x_p$. By taking in consideration this effect, we can write the generalized Planck distribution for the CMB photons as follows [CIT] FORMULA where $\text{H}(x-x_p)$ is the Heaviside step function (with values 1 for $x > x_p$ and 0 for $x \leq x_p$). The step-function $\text{H}(x-x_p)$ takes into account the fact that photons are suppressed at frequencies below $x_p$. The difference between the two distributions is more pronounced if $x_p$ is larger than 1 but nonetheless there are appreciable differences even for values of $x_p < 1$. The largest contrast between the generalized Planck distribution in eq.(REF) and the standard Planck distribution in eq.(REF) is that the former has a cut-off frequency which depends on $x_p$. We also notice that the frequency at which the maximum of the CMB spectrum occurs shifts to higher frequencies as the cuff-frequency $x_p$ increases [CIT] and that the CMB peak intensity decreases as the value of $x_p$ increases. | 1,542 | 1501.04818 | 12,064,206 | 2,015 | 1 | 20 | true | false | 6 | LAW, CONSTANT, LAW, LAW, LAW, LAW |
The Planck satellite has completed the first all-sky cluster survey since ROSAT [see e.g. [CIT]]. Planck, however, is not well-suited for the discovery of high-$z$ systems, whose arcminute-scale SZ signals are heavily diluted inside Planck's 7.--9. beams at the detecting 2 & 3 mm bands. As such, Planck detects only the most prominent, rare systems at high-$z$. The Planck XMM-*Newton*cluster validation program [CIT] used the 15.5-month nominal survey data to identify likely cluster candidates and understand Planck's selection function. It suggests that the high-$z$ detections are likely dynamically-disturbed massive systems, which are far from being virialized and, on average, less X-ray luminous than X-ray selected clusters of the same mass. | 751 | 1501.05051 | 12,066,779 | 2,015 | 1 | 21 | true | false | 6 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
In this talk, we extend SM by a $SU(2)_L$ triplet scalar with hypercharge $Y=0,2$. The lightest component of triplet field is neutral and provides suitable candidate for DM [CIT]. Then, we review allowed parameters space of ITM by PLANCK data and invisible higgs decay measurement, direct and indirect detection. | 312 | 1501.06176 | 12,077,829 | 2,015 | 1 | 25 | false | true | 1 | MISSION |
The authors thank the anonymous referee for comments and suggestions which have improved the paper. BH would like to thank Kerstin Paech for useful discussions. S.Seitz and M. M. Rau are supported by the Transregional Collaborative Research Centre TRR 33 - The Dark Universe and the DFG cluster of excellence "Origin and Structure of the Universe". CB: Funding for this project was partially provided by the Spanish Ministerio de Economa y Com- petitividad (MINECO) under projects FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. | 931 | 1501.06759 | 12,083,779 | 2,015 | 1 | 27 | true | false | 1 | MPS |
Using the $\rm Planck+BAO+SNLS3+HST$ and $\rm Planck+BAO+SNLS3+SDSS-Ly\alpha$ datasets, we investigate the dynamical properties and cosmic expansion history of the $\Lambda$HDE model. The results shows that the goodness-of-fit of the $\Lambda$HDE model are $\chi^2_{\rm min}$=426.27 ($\rm Planck+SNLS3+BAO+HST$) and $\chi^2_{\rm min}$=431.79 ($\rm Planck+SNLS3+BAO+HST+SDSS-Ly\alpha$) which is smaller then the results of the original HDE model ($\rm Planck+SNLS3+BAO+HST$:428.20; $\rm Planck+SNLS3+BAO+HST+SDSS-Ly\alpha$:438.19) and the concordant $\Lambda$CDM model ($\rm Planck+BAO+SNLS3+HST$:431.35; $\rm Planck+SNLS3+BAO+HST+SDSS-Ly\alpha$:438.22) obtained using the same datasets. Especially when constrained by the $\rm Planck+SNLS3+BAO+HST+SDSS-Ly\alpha$ dataset, The $\chi^2_{\rm min}$ of $\Lambda$HDE model shrinks more than 6, compared with both the HDE and $\Lambda$HDE model. Thus, the $\Lambda$HDE model provides a nice fit to the cosmological data. | 963 | 1502.01156 | 12,108,284 | 2,015 | 2 | 4 | true | false | 9 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
Let us note that due to stronger limits on the tensor-to-scalar ratio $r$ the PLANCK data favour the plateau-like potentials (like in Starobinsky inflation) and disfavour the power-law potentials (like $m^2\phi^2$). Nevertheless, the plateau-like models of inflation struggle with some difficulties mentioned in the Ref. [CIT]. One of the problems, which appears within the analysis of the Starobinsky model, is the fact that the Einstein frame potential is limited from above by the scale of the order of $M^2\ll M_{p}^4$. Thus, if one would set initial conditions at the Planck scale the potential term would be always subdominant and the $(\partial_i \phi)^2$ term may dominate the universe, which would lead to strong inhomogeneities. While potentials without the upper bound generate the Planck scale initial conditions $(\partial_i \phi)^2 \sim \dot{\phi}^2 \sim V(\phi)$ [^2], for which the potential term can dominate the evolution of the field and homogenize the universe.\ \* | 985 | 1502.01371 | 12,111,163 | 2,015 | 2 | 4 | false | true | 3 | MISSION, UNITS, UNITS |
We study the implications of Planck data for models of dark energy (DE) and modified gravity (MG), beyond the cosmological constant scenario. We start with cases where the DE only directly affects the background evolution, considering Taylor expansions of the equation of state, principal component analysis and parameterizations related to the potential of a minimally coupled DE scalar field. When estimating the density of DE at early times, we significantly improve present constraints. We then move to general parameterizations of the DE or MG perturbations that encompass both effective field theories and the phenomenology of gravitational potentials in MG models. Lastly, we test a range of specific models, such as k-essence, f(R) theories and coupled DE. In addition to the latest Planck data, for our main analyses we use baryonic acoustic oscillations, type-Ia supernovae and local measurements of the Hubble constant. We further show the impact of measurements of the cosmological perturbations, such as redshift-space distortions and weak gravitational lensing. These additional probes are important tools for testing MG models and for breaking degeneracies that are still present in the combination of Planck and background data sets. All results that include only background parameterizations are in agreement with LCDM. When testing models that also change perturbations (even when the background is fixed to LCDM), some tensions appear in a few scenarios: the maximum one found is \sim 2 sigma for Planck TT+lowP when parameterizing observables related to the gravitational potentials with a chosen time dependence; the tension increases to at most 3 sigma when external data sets are included. It however disappears when including CMB lensing. | 1,762 | 1502.01590 | 12,111,522 | 2,015 | 2 | 5 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
The contribution of thermally produced axions to the energy budget of the universe and hence the axion mass $m_a$ can be constrained by observations of CMB anisotropies and the large-scale structure distribution in the same way as we constrain neutrino hot dark matter and hence the neutrino mass sum. Our group has previously published limits on $m_a$ in a series of papers based on a sequence of cosmological data releases [CIT]; our most recent limit is $m_a\lesssim 0.67$ eV at 95% C.L. for a minimal cosmological model and using Planck-era cosmological data [CIT], a number comparable to the results of other authors [CIT]. Hot dark matter constraints do not apply to axion masses exceeding $\sim20$ eV because the aforementioned $a\to 2 \gamma$ decay removes the axion population. However, we note that axions masses up to $\sim300$ keV are nonetheless cosmologically forbidden owing primarily to modifications to the primordial deuterium abundance instigated by the decay photons [CIT]. | 993 | 1502.03325 | 12,129,980 | 2,015 | 2 | 11 | true | false | 1 | EPOCH |
Throughout this thesis we will use the metric convention $\eta_{\mu\nu}=\textrm{diag}\left(-,+,+,+\right)$ for the Minkowski metric and will use the same signature convention when dealing with curved space-times. Greek letters refer to four-dimensional Lorentzian coordinates when used as indices and Roman letters likewise for three-dimensional Euclidean coordinates. When describing identical theories of gravity in different frames the Jordan frame quantities are distinguished from their Einstein frame counterparts using tildes, for example, the Jordan frame metric is $\tilde{g}_{\mu\nu}$. $\nabla$ denotes a covariant derivative and $\partial$ a partial derivative. We will work in units where $\hbar=c=1$. The Planck mass is $\mpl^2=1/8\pi G$. We will often use abbreviations for cumbersome expressions and, for convenience, a complete list is given in table REF. | 871 | 1502.04503 | 12,140,342 | 2,015 | 2 | 16 | true | true | 1 | UNITS |
From Fig. REF, $\alpha =2/3$ can be consistent with Planck bounds, but assuming an equation of state $w_{re} \geq 0$, the model would tend to predict smaller reheating temperatures if one considers Planck's $1 \sigma$ bound on $n_{s}$; using Planck's 2$\sigma$ bounds, any reheating temperature up to the maximum instantaneous case is still allowed. | 349 | 1502.04673 | 12,141,595 | 2,015 | 2 | 16 | true | true | 3 | MISSION, MISSION, MISSION |
Since the noise power spectrum after beam deconvolution enters into this calculation, the impact of noise depends on the instrumental beam size (as seen in Eq. 7). We will thus consider two reference experiments in our analysis. The first reference experiment, which we will designate the *highRes* experiment, has high resolution -- a 1.4 arcmin FWHM Gaussian beam -- and is thus capable of efficient internal delensing when noise levels are low. This experiment should be taken as a proxy for ground-based telescopes such as ACTPol, POLARBEAR-I/II, SPTpol, and their successors [CIT], as well as high-resolution satellites such as COrE or PRISM [CIT]. The second reference experiment, which we term the *lowRes* experiment, is a lower angular resolution CMB telescope targeted towards measuring large-scale CMB polarization. We take it to have a 30 arcmin FWHM Gaussian beam; this resolution is too low for efficient internal delensing. The *lowRes* experiment is intended to represent CMB telescopes such as Keck Array, BICEP3 or LiteBIRD [CIT]. For the *lowRes* experiment, we assume that the measured E-mode can be co-added with Planck maps of the E-mode polarization on smaller scales (for which we assume 60$\mu$K-arcmin in polarization and a 7-arcmin beam, as in [CIT]). | 1,278 | 1502.05356 | 12,147,501 | 2,015 | 2 | 18 | true | false | 1 | MISSION |
Planck $2013$ (i.e. PlanckTT+WP using the terminology introduced before) found the following results ($68\%$ confidence limits) [CIT] FORMULA On the other hand, Planck $2015$ with PlanckTT, TE, EE+lowP (as already mentioned, using the other likelihoods described before would lead to slightly different numbers) gives [CIT] FORMULA The consistency between Planck $2013$ and Planck $2015$ is evidently very good. | 411 | 1502.05733 | 12,152,257 | 2,015 | 2 | 19 | true | true | 4 | MISSION, MISSION, MISSION, MISSION |
In this section we will discuss another intriguing possibility of NMC fluids. In fact, one can speculate whether there could be more than one fluid which is NMC. In particular, one can imagine the situation in which there are two NMC fluids one playing the role of DM and another one related to DE, such that couplings of the form FORMULA can be available. The last term in particular, represents an interaction, mediated by gravity, between DE and DM fluids. Recently, it has been shown that Planck data allow for this possibility [CIT] or even more, they seems to favour such interaction [CIT] so that coupling as those presented above may represent an interesting extension to the model presented in this paper able to include such experimental hints. Interactions of this kind are also interesting in connection to other models like the one investigated in [CIT], where a Lorentz breaking vector field is coupled to a fluid DM fluid, or the one investigated in [CIT] where a vector version of the Horndeski action is constructed. | 1,033 | 1502.06613 | 12,159,433 | 2,015 | 2 | 23 | true | false | 1 | MISSION |
We have constrained the deviation of the adiabatic evolution of the CMB black-body temperature applying two different estimators to a sample of X-ray selected clusters and using foreground cleaned Planck Nominal maps. By not including clusters selected by their TSZ signature, we avoid biasing our sample to those clusters that are closest to adiabatic evolution. Following [CIT] we distributed our cluster in six bins of redshift. The constrains using the ratio and fit methods were $\alpha=-0.03\pm 0.06$ and $\alpha=-0.007\pm 0.013$, respectively; the fit method producing statistically more significant results than the ratio method since the latter is very sensitive to small denominators. The constrains are weakened if we add a hypothetical systematic effect due to the component separation method used to construct the LGMCA map and become $\alpha=-0.007\pm 0.013\; (-0.02)$ and $\alpha=-0.03\pm 0.06\; (-0.02)$, compatible with the results given in the literature at the $2\sigma$ confidence level. | 1,007 | 1502.06707 | 12,161,091 | 2,015 | 2 | 24 | true | false | 1 | MISSION |
With the discovery of a Higgs-like particle at the Large Hadron Collider (LHC) [CIT], all the parameters of the Standard Model (SM) are now known and the fate of the SM is sealed. Taking all the uncertainties of the current experimental data into account, it has been found that the SM scalar potential becomes unstable somewhere within $10^8$-$10^{10}$ GeV [CIT]. In fact, it has been shown that for the SM scalar potential to be stable all the way up to the Planck scale $(M_P = 10^{19} \rm GeV)$ the Higgs mass $(m_h)$ needs to be in the following range [CIT] : FORMULA where, $M_t$ denotes the top quark pole mass and $\alpha_s(M_Z)$ is the strong coupling constant at the $Z$-boson mass scale. Hence, an SM Higgs boson with mass in the range 124-126 GeV certainly disfavors the possibility of having an absolutely stable vacuum up to $M_P$. As a way out of this vexing situation, it has been suggested that while absolute stability of the SM potential might be a tall ask, a metastable vacuum is entirely consistent with the current experimental value of the Higgs mass [CIT]. Nevertheless, the problem of vacuum stability in the SM remains one of the most discussed topics after the Higgs discovery and often has been taken as a hint for the intervention of some new physics. | 1,281 | 1503.02135 | 12,193,006 | 2,015 | 3 | 7 | false | true | 1 | UNITS |
In this subsection, we derive the path-integral formula for the Massieu-Planck functional $\Psi$. We show that the action has a form in the curved spacetime background, whose metric depends on parameters $\beta^\mu$ and $\nu$. We also show that the result is in accordance with those of recent studies, in which the Massieu-Planck functional is derived on the basis of symmetric and scaling properties [CIT]. Although we only consider a neutral scalar field here, the discussion covers the essential feature of the Massieu-Planck functional. | 541 | 1503.04535 | 12,214,692 | 2,015 | 3 | 16 | false | true | 3 | POTENTIAL, POTENTIAL, POTENTIAL |
[CIT] presented a study on the possible gamma-ray emission based on a number of CO surveys [CIT]. We find candidate clouds from these surveys and identify them in the Planck CO map. We choose several of the brightest high latitude clouds from these surveys. Three other, fainter clouds are chosen to explore the low limits for gamma-ray detection. Two bright clouds, G313.1-28.6 and G315.1-29.0, are identified via visual inspection of the Planck CO map. These were observed in an earlier CO catalog towards dark clouds [CIT] and named Chamaeleon-East II [CIT], but were not part of the surveys described in [CIT], nor mapped by [CIT]. | 636 | 1503.05100 | 12,219,988 | 2,015 | 3 | 17 | true | false | 2 | MISSION, MISSION |
The second case corresponds to the traditional studies of time variations, e.g. [CIT], where one does not impose the local values of $\alpha$ or $m_e/m_p$. In this case, the shape-determined values of $m_p\eta_b/m_\chi\eta_\chi$ and $\alpha^2m_e/m_p\eta_b$ are not sufficient to separately measure the cosmological and fundamental parameters. These studies therefore also use the angular scale, assuming that it is given by the flat-$\Lambda$CDM result (REF) and assume that $Gm_\chi m_p$ has not varied in time. In this case, equation (REF) provides a third constraint, determining $\eta_b$. The shape-determined value of $\alpha^2m_e/m_p\eta_b$ then determines $\alpha^2m_e/m_p$. This pre-recombination value can then be compared with the $(\alpha^2m_e/m_p)_0$. This is a simplified version of what is done in traditional CMB studies of time variations. Studies using WMAP data [CIT] confirm that in the $(\alpha,m_e)$ space, the best determined combination is indeed $\sim\alpha^2m_e$. (Those studies assume a fixed $m_p$.). The Planck data extends to sufficiently high $\ell$ to give tight constraints on other combinations of $(\alpha,m_e)$ [CIT]. | 1,152 | 1503.06012 | 12,229,845 | 2,015 | 3 | 20 | true | false | 1 | MISSION |
Where $n_{gv}\equiv \frac{1}{V}$ and $\Delta \varepsilon _{vac}\equiv$ h-.2em $\omega.$ Note that $Eq.(31)$ reduces to $Eq.(17)$ for $n=1,$ therefore $% Eq.(31)$ can be rewritten for Planck scale cutoff correction (where Planck series of energy $(n$ h-.2em $\omega)$ is taken to be the Planck energy $(E_{Pl})$): | 312 | 1503.06041 | 12,230,077 | 2,015 | 3 | 20 | false | true | 3 | UNITS, UNITS, UNITS |
A number of $Planck$ detections of cold clumps have been confirmed with the $Herschel$ Space Observatory observations (100$-$ 500 $\muup$m) to be cold (T$_{\rm dust} \sim$ 14 K or below) and also dense. For the present study, we selected clumps from fields covered in the $Herschel$ open time key program Galactic Cold Cores [CIT]. The aim of this $Herschel$ program is to examine a representative cross section of the source population of cold clumps observed with $Planck$ and to determine the physical properties of these clumps. The $Herschel$ results suggest that many of the sources are already past the prestellar phase [CIT]. In this paper, we refer to sources that are gravitationally bound as prestellar objects. If the estimated mass exceeds the virial mass, the object is expected to be gravitationally bound. Bonnor-Ebert (BE) spheres are used as an alternative model to recognize prestellar cores [CIT]. | 917 | 1503.06158 | 12,231,402 | 2,015 | 3 | 20 | true | false | 2 | MISSION, MISSION |
Black holes are among the most fascinating objects populating our universe. Their characteristic features, encompassing spacetime singularities, event horizons, and black hole thermodynamics, provide a rich testing ground for quantum gravity ideas. In this note we observe that the renormalization group improved Schwarzschild black holes constructed by Bonanno and Reuter within Weinberg's asymptotic safety program constitute a prototypical example of a Hayward geometry used to model non-singular black holes within quantum gravity phenomenology. Moreover, they share many features of a Planck star: their effective geometry naturally incorporates the one-loop corrections found in the effective field theory framework, their Kretschmann scalar is bounded, and the black hole singularity is replaced by a regular de Sitter patch. The role of the cosmological constant in the renormalization group improvement process is briefly discussed. | 941 | 1503.06472 | 12,233,300 | 2,015 | 3 | 22 | false | true | 1 | STAR |
Here, the solution for $\bar{\rho}$ will explicitly depend on both $\theta$ and $\rho_0$. However, the dynamics in $\rho$ is such that its time derivatives are still negligible in the e.o.m. Because $\bar{\rho}(\theta)$ is a complicated function of $\theta$, it is not easy to find an effective potential. Fortunately, we can solve the system by considering the slow roll parameters as given in (REF). The solution of this system is such that $\epsilon$ becomes *bigger* as we decrease $\rho_0$. In principle this is bad news since we would not like to move away from the $1\sigma$ contour of Planck data (see figure REF). | 622 | 1503.07486 | 12,242,662 | 2,015 | 3 | 25 | true | true | 1 | MISSION |
As the angular resolution of Planckis substantially coarser than those of *Chandra*and *XMM-Newton*, it cannot resolve closely interacting subclusters or close cluster pairs. Because of the size-flux degeneracy, Planckhas to use the X-ray determined position and radius to refine the SZ flux measurement (e.g., Planck Collaboration XXIX 2014). Much of this information comes from MCXC, which collects cluster parameters from publicly available *ROSAT*All-Sky Survey based and serendipitous based catalogues (Piffaretti et al. 2011). These catalogues usually consist of observations too shallow to resolve clusters in much detail. Consequently, clusters with small projected separations might not be resolved and are treated as a single cluster, which is then adopted by MCXC and Planck. If such close clusters occupy a considerable fraction, the consequence is that the Planckall-sky survey will overestimate the number of massive clusters. Using this biased mass function to constrain cosmological parameter will result in lower $\Omega _{\rm M}$ and higher $\sigma _8$. Thus, higher resolution X-ray observations by *Chandra*and *XMM-Newton*of the Planckcluster sample are necessary to identify the fraction of previously unresolved clusters like PLCK G036.7+14.9and correct for this bias before applying the PlanckSZ mass function to constrain cosmological parameters. | 1,371 | 1503.07694 | 12,245,531 | 2,015 | 3 | 26 | true | false | 7 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
- data products from the Sloan Digital Sky Survey (SDSS and SDSS-II), funded by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. 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. | 1,337 | 1503.07953 | 12,248,512 | 2,015 | 3 | 27 | true | false | 3 | MPS, MPS, MPS |
Last year, the Background Imaging of Cosmic Extragalactic Polarization (BICEP2) collaboration reported their observation of CMB $B$-mode polarization [CIT], which was interpreted as the primordial gravity waves with $r=0.20^{+0.07}_{-0.05}$ (68% confidence level) generated by inflation. Motived by the BICEP2 result of the large tensor-to-scalar ratio of ${\cal O}(0.1)$, various inflationary models and their predictions have been reexamined/updated. See, for example, Ref. [CIT] for an update of the inflationary predictions of simple models in the standard cosmology. In [CIT], we have examined simple inflationary models in the context of the RS brane-world cosmology, and found that the brane-world cosmological effect enhances the tensor-to-scalar ratio to nicely fit the BICEP2 result.[^1] However, recent joint analysis of BICEP2/Keck Array and Planck data [CIT] has concluded that uncertainty of dust polarization dominates the excess observed by the BICEP2 experiment. Now the Planck 2015 results set an upper bound on the tensor-to-scalar ratio to be $r \lesssim 0.1$. The purpose of this paper is to update simple brane-world inflationary models discussed in [CIT], in light of the Planck 2015 results. The fact that the brane-world inflationary models could nicely fit the BICEP2 result implies that the Planck 2015 results constrain the brane-world cosmological effect. | 1,384 | 1504.00683 | 12,261,678 | 2,015 | 3 | 31 | true | true | 4 | MISSION, MISSION, MISSION, MISSION |
[^3]: It is often assumed that the natural value from quantum field fluctuations is given by the Planck scale. However, this cannot be so. Consider for simplicity the flat space case (since we are primarily discussing ultraviolet issues, due to the adiabaticity of the ultraviolet, the conclusions reached here are easily carried over to expanding backgrounds). The Planckian value for the cosmological constant is obtained by setting the (physical) UV cutoff, $\Lambda_{\rm UV}$ at the Planck scale, $\Lambda_{\rm UV}\sim m_{\rm P}$, $m_{\rm P} = \sqrt{8\pi} M_{\rm P}$. In this case the one-loop contribution to the stress energy tensor can be described by an ideal fluid with the energy density and pressure [CIT], $\rho_{\rm UV} = \Lambda_{\rm UV}^4/(16\pi^2)=3p_{\rm UV}$, implying an equation of state parameter of radiation, $w_{\rm UV}=1/3$. Then the covariant energy conservation in a (homogenous) Universe dominated by such a vacuum energy, $\rho_{\rm UV}+3H(\rho_{\rm UV}+p_{\rm UV})\simeq 0$ tells us that $\rho_{\rm UV}\propto 1/a^4$. That then implies that one either has to give up imposing a physical momentum cutoff, or cutoff regularization altogether. Here we assume that cutoff regularization is incorrect, since it violates the (observed) Lorentz symmetry of the (quantum) vacuum. When a Lorentz symmetric regularisation is used [CIT], one gets a universal (regularization independent) result for the vacuum energy and pressure induced by (one-loop) vacuum fluctuations that is of the order the electroweak scale, which we assume here to be the physical contribution to $\Lambda$ from (the vacuum fluctuations of) quantum fields. Moreover, this result depends only logarithmically on the regularisation energy scale [CIT], rendering this contribution stable under a change of the renormalization scale. | 1,823 | 1504.00842 | 12,267,631 | 2,015 | 4 | 2 | true | false | 2 | UNITS, UNITS |
This Lagrangian constitutes a very well-motivated portal into hidden sectors for a variety of reasons. First and foremost, the operator $|H|^2$ is the lowest-dimension gauge- and Lorentz-singlet that can be constructed from SM fields, and is thus one of only a few possible candidates to mediate the leading interactions between the SM and hidden-sector matter that is neutral under all SM gauge groups (see e.g. [CIT]). For a hidden sector made of scalar fields, the portal operators appearing in Eq. (REF) are renormalizable, meaning that if the interactions between the extra scalar and the Higgs boson were generated at very high scales such as the GUT, or even Planck scale, then they may remain as a relevant interaction down to the energy scales probed by experiments today. And also, as it is believed that dark matter is neutral under all SM gauge interactions, and the Higgs portal can provide a bridge between the SM and neutral sectors, it is natural to speculate that scalars coupled through the Higgs portal may play a role in dark sector physics, or perhaps themselves constitute the dark matter within the present day Universe.[^1] | 1,147 | 1504.04855 | 12,309,512 | 2,015 | 4 | 19 | false | true | 1 | UNITS |
In the 2015 release [CIT] such a source was replaced by the Doppler effect due to the motion with velocity $\boldsymbol{\beta_O}$ of the Planck satellite around the Sun, called the "orbital dipole". Although it is one order of magnitude smaller than the solar dipole (${\beta_O} = 1.0 \times 10^{-4}$) it has the great advantages of both being time-dependent (on a scale of 1 year) and having a very well known amplitude and direction. The very small uncertainties come only from the motion of the satellite inside the solar system, which is known to very high accuracy. The uncertainties are of the order $10^{-10}c$, which corresponds to just one part in a million. For this reason the 2015 release is thought to be more accurate and the new absolute calibration of the Planck 2015 HFI instrument is higher by $2\%$ (in power) compared to 2013, resolving the calibration differences noted between WMAP and Planck, which goes down from $2.6\%$ in 2013 to $0.3\%$ in 2015. | 972 | 1504.04897 | 12,310,199 | 2,015 | 4 | 19 | true | false | 3 | MISSION, MISSION, MISSION |
where $C_1(N)=N+N\ln\Big(\frac{\kappa_0^3}{8\pi{N}}\Big)$ and also we have substituted $\kappa= \kappa_0,p_{_{\rm Pl}}=\kappa_0/l_{_{\rm Pl}}$ with $\kappa_0$ is the dimensionless parameter and $l_{_{\rm Pl}}$ is the Planck length. The dimensionless parameter $\kappa_0\sim{\mathcal O}(1)$ determines the boundary at which the noncommutative effects will become important and it should be fixed only by the experiments (see Ref. [CIT] in which some upper bounds for this dimensionless parameter are obtained in different contexts). The entropy bound (REF) shows that the photon gas is saturated at high temperature regime in noncommutative spacetime and the entropy could not increase by increasing the temperature in this regime. More precisely, the entropy bound (REF) for the photon gas originates from the existence of an ultraviolet cutoff in this setup which also, as we shall see, leads to an upper bound for the internal energy. | 936 | 1504.06839 | 12,329,524 | 2,015 | 4 | 26 | false | true | 1 | UNITS |
The Planck 2015 data, combined with the BICEP2/Keck Array data, have placed strong constraints on the level of primordial tensor modes by B-mode polarization of the Cosmic Microwave Background (CMB) [CIT], and upcoming CMB observations will constrain the amplitude of tensor modes in the CMB at much stronger levels. However, detection of a tensor-to-scalar ratio of $r\lesssim 0.1$ may be still possible in the near future, fixing the energy scale of inflation. In the canonical single field inflation models [CIT], such a value of $r$ implies that the change in the inflaton value during inflation is at least of the order of the (reduced) Planck mass $M_P\equiv (8\pi G)^{-1/2}$ [CIT], FORMULA where $\Delta N \simeq 7$ is the number of $e$-folds corresponding to the observable CMB scales [CIT]. If we extrapolate this estimation up to the total number of $e$-folds $N \simeq 50-60$, which is valid in the simple chaotic inflation models [CIT], the field excursion fairly exceeds the Planck scale. This is called the Lyth bound [CIT]. | 1,038 | 1504.06946 | 12,330,374 | 2,015 | 4 | 27 | true | true | 3 | MISSION, UNITS, UNITS |
One may worry about isocurvature perturbations which are currently severely constrained by the Planck collaboration [CIT]. The light mode contributing to isocurvature perturbations is regarded as a massless particle during inflation. In our model this is the axionic partner of the overall volume modulus. The other fields are heavy enough and hence the adiabatic perturbations are essentially driven by the single inflaton field. The mass of $\theta_1$ is generated by a non-perturbative effect on $T_1$, that is sub-dominant in LVS and we did not specify in our model. If the mass scale is large enough to be a dark matter, this axion also contributes to the CDM isocurvature perturbations. Since the magnitude of CDM isocurvature perturbation crucially depends on the initial mis-alignment angle and the fraction of CDM consisting of axion, we believe that the CDM isocurvature constraint is satisfied (see e.g. Figure 6 of [CIT] at $H_{\rm inf} \sim 10^{10} {\rm GeV}, f_a \sim 10^{16} {\rm GeV}$ of our illustrative example). On the other hand, when the mass scale is negligible even at the minimum of LVS, this lightest axion could play a role of dark radiation. In this case, although the direct entropy production from axion perturbations would not be subject to the constraint as the axion only has derivative couplings and hence the entropy is diluted away quickly, the dark radiation produced by the decay of the volume modulus may contribute to the neutrino isocurvature density perturbations [CIT]. However, a more conclusive discussion requires more details of the setup including the location of the matter sector in the compact manifold. Hence, we consider this is beyond the scope of the paper. | 1,711 | 1504.07202 | 12,332,413 | 2,015 | 4 | 27 | true | true | 1 | MISSION |
SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. | 937 | 1504.08044 | 12,341,135 | 2,015 | 4 | 29 | true | false | 2 | MPS, MPS |
Before we discuss the non-perturbative effects, we consider briefly the perturbative part at high energies, i.e. above the scale of the dynamical chiral symmetry breaking in the hidden sector. As explained in the Introduction, it is essential for our scenario of explaining the origin of the EW scale to work that the scaler potential is unbounded below and the theory remains perturbative (no Landau pole) below the Planck scale. So, we require: FORMULA In the following discussion we assume that the perturbative regime (of the hidden sector) starts around $q_0=1$ TeV and $g_H^2 (q_0)/4\pi \simeq1$. Although in this model the Higgs mass depends mainly on two parameters, $\lambda_H$ and $\lambda_{HS}$, lowering $\lambda_H(q_0)<0.13$ will destabilize the Higgs potential while increasing $\lambda_H(q_0)> 0.14$ will require a larger mixing with $S$, which is strongly constrained. Therefore, we consider the RG running of the couplings with $\lambda_H(q_0)$ fixed at $0.135$ and rely on one-loop approximations. In the case that the hypercharge $Q$ of the hidden fermions is different from zero, these fermions contribute to the renormalization group (RG) running of the $U(1)_Y$ gauge coupling considerably. We found that $Q \mathrel{\mathpalette\ [CIT] <}0.8$ should be satisfied for $g'$ to remain perturbative below the Planck scale. | 1,341 | 1505.00128 | 12,345,136 | 2,015 | 5 | 1 | false | true | 2 | UNITS, UNITS |
In the last two decades, cosmologists have been making great efforts for establishing standard cosmological model to describe the contents and evolution of the Universe. With precise measurements of the cosmic microwave background from the *Wilkinson Microwave Anisotropy Probe* (*WMAP*) [CIT] and Planck [CIT] satellites, the cosmological parameters have been measured in a higher and higher precision, making it possible to test whether the standard $\Lambda$ cold dark matter ($\Lambda$CDM) model can describe the cosmic evolution throughout the history of the Universe. In fact, after Planck has published its 2013 results [CIT], it was found that the previously measured value of Hubble constant $H_{0}$ through $600$ Cepheid variables [CIT] is higher than the Planck measured value by $3\sigma$ confidence level, although later it is shown that by correcting the NGC 4258 distance one can obtain a lower value of $H_{0}$ which is compatible with Planck 2013 results [CIT]. In addition, it is shown that the Planck constrained $\Omega_{\rm M}$--$\sigma_{8}$ parameter plane is in tension with CFHTLenS data [CIT], thermal Sunyaev-Zeldovich effect [CIT], and statistics of cluster number counts [CIT]. These interesting tensions between cosmological data sets drive us to consider more, and robust test on $\Lambda$CDM model at different periods of cosmic evolution. | 1,370 | 1505.03584 | 12,379,428 | 2,015 | 5 | 14 | true | false | 5 | MISSION, MISSION, MISSION, MISSION, MISSION |
In this paper we have shown that the scale invariant PMF can be generated by the simple model ${f^2}FF$, Eq.(REF), in ${R^2}$-inflationary model, which is mostly favored by the latest result of Planck, 2015 [CIT]. Unlike, in non-standard inflationary models like NI [CIT], LFI [CIT], and some standard models of inflation [CIT] at which ${f^2}FF$ model suffers from the backreaction problem, we can avoid this problem in ${R^2}$-inflation. It is easily to avoid this problem as long as, the rate of inflationary expansion, $H$, is in the order of or less than the upper bound reported by Planck ($\le 3.6 \times {10^{ - 5}}{M_{{\rm{Pl}}}}$) [CIT]. In principle, the electric spectrum starts exceeds the magnetic spectrum at relatively high, $H(> 0.2{\rm{ }}{M_{{\rm{Pl}}}})$. The corresponding e-folds number is, $N \sim 68$. Thus, we can consider these two values as upper bounds to the model. We do this investigation for both simple exponential (de Sitter) and power law expansion. At sufficiently high e-folds number, $N$, there is no significant differences in their results. | 1,080 | 1505.05204 | 12,396,843 | 2,015 | 5 | 19 | true | false | 2 | MISSION, MISSION |
We compute the ionisation history and corresponding CMB optical depth for a variety of model parameterisations with and without LW feedback and metal enrichment and find that without LW feedback or metal enrichment, massive Pop III stars cannot form efficiently in minihaloes without violating the Planck constraints. When LW feedback and metal enrichment are included, massive Pop III stars could form efficiently early on, but they are suppressed at lower redshifts, reducing the optical depth sufficiently to be consistent with Planck. We also find that, irrespective of the feedback prescription used, the total density of Pop III stars formed over all cosmic time cannot exceed $\approx 10^{4-5} M_\odot {\rm Mpc^{-3}}$ without violating the Planck optical depth constraints. | 780 | 1505.06359 | 12,409,408 | 2,015 | 5 | 23 | true | false | 3 | MISSION, MISSION, MISSION |
We have also considered how X-rays emitted due to the accretion of black hole remnants from Pop III stars would impact the IGM. We performed a simple estimate of X-ray ionisation from black holes produced by our fiducial model with $f_{\rm *,m}=0.001$ and found that unless the duty cycle of black hole accretion is $\epsilon_{\rm BH, duty} \lesssim 0.01$, early ionisation produces an optical depth greater than the Planck 1$\sigma$ limits. While we emphasise that our rough estimate is somewhat model dependent (e.g. a very hard X-ray spectrum could lead to free-streaming of X-rays and weaker constraints), the result is intriguing. To form the first super massive black holes (SMBHs), which are more massive than $10^9M_\odot$ at $z\approx6$, would require that Pop III remnants grow at the Eddington limit with a duty cycle of nearly unity. This suggests that either some type of feedback [e.g. [CIT].425.2974T] acts on most, but not all Pop III remnants if they are the seeds of the first SMBHs or that SMBHs are seeded by a different mechanism such as direct collapse black holes [e.g. [CIT].409.1022V; [CIT].442.2036D; [CIT].445.1056V; [CIT]]. | 1,151 | 1505.06359 | 12,409,450 | 2,015 | 5 | 23 | true | false | 1 | MISSION |
Now we could formulate results in a rather different manner. We have two interesting values for possible cut-off $\Lambda$. The low value (REF), which is compatible with previous results [CIT] by the order of magnitude, and the Planck mass. Let us consider set of equations (REF, REF, REF) for these values of the cut-off. Earlier we have fixed actual value for electromagnetic constant $\alpha(M_Z)$ and calculated values for the cutoff (REF, REF). Now we fix $\Lambda$ and calculate $\alpha(M_Z)$. In this way for values (REF) and the Planck mass we obtain respectively FORMULA Both values differ from actual value $\alpha(M_Z),=,0.007756$ by 2%. Thus it might be possible to interpret results (REF) as a calculation of a value of $\alpha$ with this precision. Just contributions of order of magnitude of few % are expected at the next approximation in the development in powers of $\alpha_{ew}$. | 898 | 1505.07269 | 12,417,680 | 2,015 | 5 | 27 | false | true | 2 | UNITS, UNITS |
[^8]: In our analysis, we assume that 100% of dark matter consists of the neutralino. If there is other dark matter components, we need to regard the measurement of the dark matter density determined by Planck satellite as an upper limit, and follow some scaling ansaz studied in, e.g., [CIT]. This is however beyond the scope of this paper. | 341 | 1506.01529 | 12,443,299 | 2,015 | 6 | 4 | true | true | 1 | MISSION |
An unexpected benefit from the new tools for moduli stabilization during inflation was realized very recently. Many examples of previously known supergravity models, compatible with current and future cosmological observations, can now easily describe dark energy via tiny de Sitter vacua, and spontaneous breaking of supersymmetry. In this paper we provide examples of such generalizations of $\alpha$-attractor models [CIT]. These models interpolate between various polynomial models $\varphi^{2m}$ at very large $\alpha$ and attractor line for $\alpha\leq 1$, see Figs. 1, 2. Therefore they are flexible with regard to data on B-modes, $r$. They provide a seamless natural fit to Planck data. For these kinds of cosmological models we have shown that it is possible to break supersymmetry without an additional hidden sector, with a controllable parameter of supersymmetry breaking. With inflationary scale $\sim 10^{-5} M_{p}$ the scale of supersymmetry breaking can be $M\sim (10 ^{-13}- 10^{-14}) M_{p}$, compatible with the discovery of supersymmetry at LHC. With $M \gg 100- 1000$ TeV we will have equally good inflationary models, compatible with an absence of observed supersymmetry at LHC. In fact, such inflationary models are even easier to construct. | 1,264 | 1506.01708 | 12,445,216 | 2,015 | 6 | 4 | true | true | 1 | MISSION |
Having obtained the signature of bubble collisions in the CMB, we now describe the method whereby we forecast constraints on the underlying parameters. We assume that the data --- in this case, the observed spherical harmonic coefficients $d_{\ell m}^X$, where $X = \{T,E\}$ --- consist of the stochastic Gaussian CMB ($a_{\ell m}^X$), the beam-deconvolved instrumental white noise ($n_{\ell m}^X$), and a deterministic bubble collision ($b_{\ell m}^X$). Under these assumptions the moments of the (Gaussian) data are simple to define: the noise and CMB anisotropies do not contribute to the mean, which is determined entirely by the collision to be FORMULA and the deterministic bubble collision signature does not contribute to the covariance, which is defined purely by the CMB and noise power spectra to be FORMULA We generate the CMB power spectra $C_{\ell}$ using CAMB, fixing the cosmological parameters to their 2013 Planck+WP+highL+BAO best-fit values [CIT] | 967 | 1506.01716 | 12,445,334 | 2,015 | 6 | 4 | true | true | 1 | UNITS |
We would like to thank the staff at the IRAM 30-m telescope, in particular N. Billot and S. Trevino for their excellent support during observations. We are also very grateful to the former director of IRAM, P. Cox, the director of the SMA, R. Blundell, the director of the CFHT, D. Simons, and the director of ESO, T. de Zeew, for the generous allocation of Director's Discretionary Time. We thank the referee, S. Bussman, for constructive comments that helped improve our manuscript. We would also like to thank A. Sajina and several other colleagues unknown to us and sollicited by the Planck collaboration as external referees for their valuable comments on an earlier version of the paper. We would also like to thank C. Kramer for having made his `CLASS` routine FTSPlatformingCorrection5 available to us. We thank the Planck Editorial Board for ensuring that our manuscript is in accordance with the internal Planck publication rules and standards. MN acknowledges financial support from ASI/INAF agreement 2014-024-R.0 and from PIRN-INAF 2012 project "Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the *Herschel* Astrophysical Large Area Survey." IFC, LM and EP acknowledge the support of grant ANR-11-BS56-015. | 1,259 | 1506.01962 | 12,448,105 | 2,015 | 6 | 5 | true | false | 3 | MISSION, MISSION, MISSION |
We carried out a detailed COSMOMC analysis in Ref. [CIT], using Planck 2013 and WMAP nine year data and the power spectrum in Eq. (REF). In addition to the 6 standard parameters for the Monte Carlo simulation we included two extra parameters -- $\delta N$, the number of e-foldings of inflation in excess of the minimum required to solve the horizon and flatness problems, and $T$, the comoving temperature. (The factor ${\cal C}(k)$ in the power spectrum depends on $\delta N$ through the time when the change from the radiation era to the inflationary era takes place.) For an inflationary scale of $10^{15}{\rm,Ge\kern-0.125em V}$ we found that the best fit value of $\delta N$ is 0.08 (the marginalized value is consistent with zero with 68 % confidence). This indicates that the data favours a 'just enough' inflationary scenario. As discussed earlier, there are also theoretical motivations for considering such a scenario. We also obtained an upper limit on the comoving temperature as $T< 1.3\times10^{-4},{\rm Mpc}^{-1}$ at 68% C.L. (for the GUT and the electroweak scale). | 1,082 | 1506.04808 | 12,476,217 | 2,015 | 6 | 16 | true | true | 1 | MISSION |
In Section 2, we describe our investigation of how the stellar mass-density and star-formation rate per unit comoving volume depend on galaxy morphology in the Universe today. Section 3 describes the caloriometry method that we have used to estimate how the mass of stars that has formed over the history of the Universe depends on the morphology of the galaxy in which those stars were formed. Section 4 gives the results of the calorimetry method. The results and their implications are discussed in §5 and the conclusions are given in §6. We assume the cosmological parameters given from the Planck 2013 cosmological analysis (Planck Collaboration XVI 2014): a spatially-flat universe with $\Omega_M = 0.315$ and a Hubble constant of 67.3 $\rm km s^{-1} Mpc^{-1}$. | 767 | 1506.05466 | 12,482,807 | 2,015 | 6 | 17 | true | false | 2 | MISSION, MISSION |
A primary motivation for studying extra-dimensional models was to resolve the hierarchy problem between the (effective) Planck scale, $M_{Pl} = {\cal O}(10^{18}GeV)$, and the electroweak scale, $M_{EW} = {\cal O}(100GeV)$. This stems from the expectation that the bare Higgs mass would obtain corrections of the order of $M_{Pl}$, meaning some extreme fine-tuning of the Higgs sector parameters is required for the electroweak scale to be so low. The ADD model can solve this by virtue of the true Planck scale being related to the four dimensional Planck scale via the volume of the extra-dimensions. This is the result of gravity being able to propagate in the full spacetime, such that the Planck scale we measure is effective and valid for energies smaller than the inverse radius of compactification of these extra-dimensions. As such, if the volume of the extra-dimensions is large enough, then the true scale of gravity can be as low as the electroweak scale. However, the ADD model's hierarchy problem resolution replaces the hierarchy between $M_{EW}$ and $M_{Pl}$ with another hierarchy, that between $M_{EW}$ and the inverse radius of compactification for the extra-dimensions. Thus this ADD resolution only raises another question, why is the inverse radius of compactification so large when compared to the electroweak scale? | 1,338 | 1506.05598 | 12,484,431 | 2,015 | 6 | 18 | false | true | 4 | UNITS, UNITS, UNITS, UNITS |
It should be noted that the combination of CMB and Ly$\alpha$ is a very efficient way of constraining cosmological parameters, especially $\sum m_\nu$. As one can see in Figure 5, the Planck and +$H_0$ contours in the $\sum m_\nu-\Omega_m$ and $\sum m_\nu-\sigma_8$ planes are complementary. The Ly$\alpha$ data constrain $\Omega_m$ and $\sigma_8$ largely independently of $\sum m_\nu$ because they have different impact on the shape of the power spectrum (see discussion in §5.1 of Paper I). For the Planck constraints, high $\sum m_\nu$ corresponds to low $\sigma_8$ because of the suppression of power on small scales by neutrino free streaming. The positive correlation between $\Omega_m$ and $\sum m_\nu$ is more subtle: with $\Omega_c h^2$ and $\Omega_b h^2$ well constrained by the acoustic peaks, raising $\sum m_\nu$ increases the matter density at low redshift after neutrinos become non-relativistic, and within $\Lambda$CDM this requires a decrease in $h$ to maintain the well determined angular diameter distance to last scattering, and this in turn corresponds to higher $\Omega_m$ (see, e.g., §6.4 of [CIT]). The end result is that the and Planck contours intersect only near $\sum m_\nu=0$. As shown in Figure REF, adding polarization or BAO to the Planck + Ly$\alpha$ contours does not lead to significant further improvement of the constraints in these planes, at least within the $\Lambda$CDM framework. | 1,422 | 1506.05976 | 12,488,448 | 2,015 | 6 | 19 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
Let us now turn back to the hypothesis about equality to zero of the average DP (see Part I, section 2.5), expressed by Lima [CIT]. Over the last nine years of cosmic microwave background observations, the Wilkinson Microwave Anisotropy Probe (WMAP) results were consistent with the $\Lambda$CDM cosmological model in which the age of the Universe is one Hubble time, and the time-averaged value of the DP is consistent with zero. As was noted in [CIT], this curious observation has been put forward as a new coincidence problem for the $\Lambda$CDM concordance cosmology, which is in fact a 'greater' coincidence than the near equality of the density parameters of matter and the cosmological constant. However recent Planck's results [CIT] make the new coincidence problem not so important. Let us convince ourself in this. Setting $t=t_0$ and $a=a_0=1$ in (REF), the $H_0t_0=1$ condition transforms to FORMULA The only positive solution to equation (REF) is $\Omega_{\Lambda0}\approx0.737125$. In general, we can write the time-averaged DP $\langle q\rangle$ as a function of scale factor: FORMULA Figure REF shows the $95\%$ confidence levels of $\Omega_{\Lambda0}$ from both the Planck data ($0.686^{+0.037}_{-0.040}$) and the WMAP $9$-year data ($0.721\pm0.050$). The probability density function of the posterior distribution is indicated by the colorscale. Note that $\bar q(t_0)$ is close to zero only during a brief period in cosmic time. Moreover, $\bar q(t_0)\approx0$ in the WMAP 9-year data, however, $\bar q(t_0)\ne0$ for the Planck data. | 1,553 | 1506.08918 | 12,518,235 | 2,015 | 6 | 30 | true | true | 3 | MISSION, MISSION, MISSION |
For both datasets we used the publicly available Markov chains from Planck, analyzed by using python scripts from CosmoMC [CIT]. These chains were produced considering $n_s$, $n_{sk}$ and $r$ as free parameters. The primordial scalar power spectrum is determined by $A_s$, $n_s$ and $n_{sk}$, while the primordial tensor power spectrum will have an amplitude determined by $r$, with $n_t$ satisfying the consistency relation (REF) at first order. | 446 | 1506.09172 | 12,520,735 | 2,015 | 6 | 30 | true | true | 1 | MISSION |
The canonical form of the brane world scenario, however, was fully realized later in the work of Arkadi-Hamed, Dimopoulos and Dvali [CIT], which is described in the third section. Their model, known as the ADD model, rather than hide additional dimensions under the carpet, used the bulk as an instrument to explain phenomenological truths about the nature. In ADD scenario the extra dimensions are compactified, but in contrast to the Kaluza-Klein scenario, not to the Planck scale $M_P\sim 10^{19}$ GeV, but rather to experimentally more accessible Weak scale $M_{W}\sim 10^3$ GeV. As a consequence, they are called *large extra dimensions*, even though from human perspective they are still rather small (around micrometer or less). The reason for this is to account for apparent weakness of gravity. In the brane world scenario, gravitons are not, like ordinary matter, trapped on the brane, but they are free to roam in the bulk. This results in weakening of gravitation from a point of view of a brane-bound matter. We also briefly describe different approach to the brane world scenario, which is the work of Randall and Sundrum [CIT]. To localize particles on the brane, they use warped extra-dimension, compactified on a ${S^1/\mathbb{Z}_2}$ orbifold and a negative cosmological constant in the bulk. In contrast to ADD scenario, the fundamental scale in models of Randall and Sundrum is the Planck scale. However, the warping of the extra dimension causes exponential screening of the fundamental scale down to $M_W$. | 1,527 | 1507.01246 | 12,532,759 | 2,015 | 7 | 5 | false | true | 2 | UNITS, UNITS |
This possibility is realized within the brane world scenario quite naturally. There are two typical models of the brane world scenario. One of them is proposed by Arkani-Hamed, Dimopoulos and Dvali (ADD) [CIT]. The mechanism in this model is the following. One can argue that gravity, connected with the geometry of space-time, cannot be confined to the brane and must "leak out" into the bulk. This will lower the apparent strength of gravitational force from a point of view of brane-bound observers, setting the effective four-dimensional Planck scale $M_P^{(4)}$ much higher than what the actual $(4+n)$-dimensional Planck scale $M_P^{(4+n)}$ is. This "diluting effect" of $n$ compact extra dimensions can be easily quantified. Let us assume that typical size of extra dimensions is $R$. Then, for distances $r\ll R$, the effective four-dimensional gravitational force may be written either in terms of effective Planck scale $M_P^{(4)}$ or in terms of actual Planck scale $M_P^{(4+n)}$ as FORMULA This is giving us the relation FORMULA If we set $M_P^{(4)} \sim 10^{19}$ GeV, then the radius of extra dimensions must be of the order FORMULA | 1,146 | 1507.01246 | 12,532,782 | 2,015 | 7 | 5 | false | true | 4 | UNITS, UNITS, UNITS, UNITS |
To date, experimental results have not confirmed the existence of large extra dimensions [CIT]. These null results set upper bounds on the size of the large extra dimensions, or equivalently, lower bounds on the the fundamental Planck scale. Models with one or two large extra dimensions have been ruled out [CIT], such as the Fermi Large Area Telescope [CIT]. Constraints on space-times with three large extra dimensions from astrophysical and cosmological experiments are generally very stringent, although they typically suffer from large systematic errors. The observation of Supernova SN1987A sets a lower limit on $M_D$ of 2.4 TeV for $n=3$ [CIT], where the reduced Planck mass $M_D$ is related to $M_*$ by [CIT], FORMULA Neutron star-derived limits constrain $M_D$ to be larger than 76 TeV for $n=3$ [CIT]. Collider experiments provide less stringent, albeit more accurate limits on $M_D$ for $n\ge3$ from non-observation of perturbative processes. These limits (in units of TeV) are shown in Table REF. | 1,010 | 1507.01632 | 12,536,032 | 2,015 | 7 | 6 | false | true | 2 | UNITS, UNITS |
The Lagrangian in the Standard Model (SM) contains only one scale parameter, the negative Higgs mass squared term, $-\mu^2_{\text{\tiny SM}}$, which is quite small compared to the Planck scale; therefore, it seems reasonable to expect that it can be generated from the dynamics of the underlying theory. The concept of classical scale invariance (CSI) states that there should be no mass scales in the Lagrangian at a classical level and all the mass scales must be generated by the dynamics of the theory. In this framework it then becomes difficult to generate vastly different scales in the theory. These ideas have attracted a lot of attention recently [CIT]. In our work we will follow the approach taken by the authors of ref. [CIT], where the only mass scale in the Standard Model is generated via the Coleman-Weinberg (CW) mechanism [CIT] in a hidden sector and then transmitted to the Standard Model through a Higgs portal interaction. | 944 | 1507.04996 | 12,567,504 | 2,015 | 7 | 17 | false | true | 1 | UNITS |
Large plots encompassing full parameter sets are pushed off to Appendix [7]. In particular, Figs. REF and REF are our forecast parameter constraints from the default simulated Y1 and Y5 likelihood analyses. As discussed in Section [4], these results represent our conservative and optimistic estimates at the eventual DES constraining power on the growth function for the respective data stages. The takeaway is that parameter constraints are very well centered with respect to their true values, an indication that the 20-parameter MCMC is working well. Note that we are not showing constraints on the cosmological parameters, as these are largely dominated by Planck priors. Therefore, we suppress these columns but come away with the knowledge that for the cosmological parameters that we consider -- $\Omega_M$, $h$, and $A_s$ -- we expect CMB constraints to be dominant over constraints from combining small scale lensing and large scale clustering. Also, as the two lens bins show very similar parameter behaviors, we only show contours for the first lens bin and simply tabulate results for the second lens bin. | 1,118 | 1507.05353 | 12,570,211 | 2,015 | 7 | 19 | true | false | 1 | MISSION |
For observational purpose and also for comparison with the $y$-type distortions [CIT] it is convenient to define the dimensionless frequency not with respect to the temperature of the Bose-Einstein spectrum but with respect to the temperature of a Planck spectrum which has the same number density of photons as the Bose-Einstein spectrum, $N_{\rm BE}(T,\mu)\equiv N_{\rm Pl}(T_{\rm ref}) \Rightarrow (T-T_{\rm ref})/T_{\rm ref}\approx 0.456\mu$,$x_{\rm ref}\equiv \nu/T_{\rm ref}$. In terms of this reference temperature we have FORMULA where the first term is the Planck spectrum and the second term defines the $\mu$-type distortion in the limit of small distortions [CIT]. Note that at linear order, for small $\mu$, we have $\mu\equiv -\mu_E/T \approx -\mu_E/T_{\rm ref}$. We should emphasize that this re-definition is just for convenience of visualization and does not affect the analysis of data. This is because the monopole temperature of the CMB is also uncertain, at the sensitivity we will be working, and we must fit for the reference temperature simultaneously giving us the freedom to choose the reference temperature. We will use the definition $n_{\mu}$ from Eq. REF throughout the rest of the paper with $T=2.725 {\rm K}$ as the reference temperature dropping the subscript ${}_{\rm ref}$. | 1,308 | 1507.05615 | 12,573,778 | 2,015 | 7 | 20 | true | true | 2 | LAW, LAW |
In this paper, we have addressed the formation and the growth of supermassive BHs in the presence of scale-dependent non-Gaussianities. We use two identical simulations except for their initial conditions, with either Gaussian or scale-dependent non-Gaussian primordial perturbations ($f_{\rmn{NL}}(k) = f_{\rmn{NL}, 0},\left(k/k_0\right)^{\alpha}$, with $\alpha=4/3$ and $f_{\rmn{NL}, 0}=10^{4}$). The introduction of these non-Gaussianities on galactic scales, consistent at larger scales with the Planck results, produces an enhancement in the low-mass end of the halo and galaxy mass functions, increasing with redshift. As a consequence, changes in the BH population arise as well. We explore the impact of scale-dependent non-Gaussian primordial perturbations on two models of BH formation, and on the growth of the putative BHs. Sherkatghanad & Brandenberger (2015) also investigate local-type non-Gaussianities, i.e. with both skewness ($f_\rmn{NL}$) and kurtosis (described by the parameter $g_\rmn{NL}$), in the context of BH formation. They do not include scale-dependent non-Gaussianities, and conclude that non-Gaussianities do not strongly affect the number density of dark matter halos at high redshifts (and of BHs as a consequence). This is in agreement with our previous work [CIT] where we showed that non-Gaussian models closest to a non-scale dependent $f_\rmn{NL}$ do not show significant differences in halo and stellar mass functions compared to the Gaussian model. On a related note, [CIT] find that varying the slope of the primordial power spectrum impacts the formation of structures as well: an enhanced power spectrum at small length scales (or blue-tilted power spectrum) pushes to the formation of the first stars at much higher redshifts, and the higher CMB temperature leads to more massive stars, which can be precursor of massive BHs. | 1,870 | 1507.05971 | 12,578,231 | 2,015 | 7 | 21 | true | false | 1 | MISSION |
Why the value of the cosmological constant $\Lambda$ is neither zero nor of the order of the Planck density (the Planck mass to the fourth power, $M_{\rm Pl}^4$) remains one of the deepest mysteries of nature. Refs [CIT] have argued that in order for observers (and thus cosmic structure) to exist, the value of $\Lambda$ could not be larger than $10^{-120} M_{\rm Pl}^4$. This was the first indication that the value of $\Lambda$ could not be arbitrary and that requiring the existence of observers bounded $\Lambda$ from above. Subsequent works (e.g., [CIT]) have firmed up this argument. However, to this date no argument has been given to provide a lower bound to $\Lambda$; in particular, it is not clear why $\Lambda$ does not simply vanish[^1]. Interestingly, the necessity to avoid massive life extinction events by GRBs can shed a new light on this issue. | 864 | 1508.01034 | 12,617,783 | 2,015 | 8 | 5 | true | true | 2 | UNITS, UNITS |
An illustration of the Planck observed power spectrum in this region is visible on Figure REF from Mathews et al. [CIT]. Although the error bars are large, there is a noticeable systematic deviation in the range $\ell = 10-30$ below the best fit based upon the standard $\Lambda$CDM cosmology with a power-law primordial power spectrum. This same feature is visible in the CMB power spectrum from the Wilkinson Microwave Anisotropy Probe (*WMAP*) [CIT], and hence, is likely a true feature in the CMB power spectrum. This can be interpreted as an artifact of the cosmic variance [CIT], or a phase transition in the inflation-generating potential [CIT]. However, here we adopt the the premise that this could be a real feature in the primordial power spectrum produced by new trans-Planckian physics occurring near the end of the inflation epoch. In particular, we show that this feature is well represented by the resonant creation [CIT] of Planck-scale particles that couple to the inflaton field as shown by the solid line in Figure REF and we now describe in detail. | 1,069 | 1508.01214 | 12,619,711 | 2,015 | 8 | 5 | true | false | 2 | MISSION, UNITS |
The outcome is illustrated in Fig. 2 for three representative values of the limiting UV magnitude at the faint end: red lines are for $M_{\rm UV} \lesssim -17$, green lines refer to $M_{\rm UV} \lesssim -13$ and blue lines to $M_{\rm UV} \lesssim -11$; these produce integrated optical depths $\tau_{\rm es}$ covering the $1\sigma$ region measured by Planck, with the value $M_{\rm UV}^{\rm lim}\approx -13$ approximately yielding the Planck best fit $\tau_{\rm es}\approx 0.066$ [CIT] (to be precise, we obtain asymptotically $\tau_{\rm es}\approx 0.06$, while we find $\tau_{\rm es}\approx 0.055$ if truncating the cosmic SFR at $z\gtrsim 8-10$, cf. [CIT]). For reference, the dotted line represents the optical depth expected in a fully ionized Universe up to redshift $z$; this is to show that the bulk of the reionization process occurred at $z \sim 8-10$ and was almost completed at $z \sim 6$ [CIT]. Note that from this perspective, the detailed behavior of the luminosity functions at $z \gtrsim 10$ (that have been computed by extrapolation of the lower-redshift behavior), and the related ionizing background, are only marginally relevant. This is also apparent from the inset of Fig. 2, where the evolution with redshift of the ionizing fraction $Q_{\rm HII}$ is illustrated, and confronted with various observational constraints [CIT]. | 1,347 | 1508.02147 | 12,628,196 | 2,015 | 8 | 10 | true | false | 2 | MISSION, MISSION |
On the other hand, recent developments in observational cosmology using high quality data including Type Ia supernovae (SNe Ia), cosmic microwave background (CMB), baryonic acoustic oscillations (BAO) and Large Scale Structure (LSS), converge to a standard cosmological model in a spatially flat geometry with a cosmic dark sector usually in the form of pressureless cold dark matter (CDM) and dark energy (DE) with negative pressure, respectively, in order to interpret the observed flat rotation curves of spiral galaxies and the accelerated expansion of the Universe [CIT]. On the basis of the Planck experiment results [CIT], DE amounts to $\sim68\%$, CDM and usual baryons to $\sim27\%$ and $\sim5\%$ of the total energy budget of the Universe, respectively. | 763 | 1508.04697 | 12,651,661 | 2,015 | 8 | 18 | true | false | 1 | MISSION |
In this paper, we calculate instantaneous halo mass accretion rates from the Bolshoi-Planck simulation, as well as halo mass accretion rates averaged over the dynamical time ($\dot{M}_{\rm vir,dyn}$), defined as FORMULA The dynamical time of the halo is $t_{\rm dyn}(z) = [G \Delta_{\rm vir}(z) \rho_{\rm m}]^{-1/2}$, which is $\sim 20\%$ of the Hubble time. Simulations [e.g., [CIT] +2009] suggest that most star formation results from cold gas flowing inward at about the virial velocity -- i.e., roughly a dynamical time after the gas enters. As instantaneous accretion rates for distinct halos near clusters can also be negative [CIT], using time-averaged accretion rates allows galaxies in these halos to continue forming stars. | 733 | 1508.04842 | 12,655,668 | 2,015 | 8 | 20 | true | false | 1 | MISSION |
Before giving a derivation of the previous results, we stress that both the bounds REF(#Tmass){reference-type="eqref" reference="Tmass"} and REF(#Tcharge){reference-type="eqref" reference="Tcharge"} are relevant only for $q \ge q_{\rm P}$ and $m \ge m_{\rm P}$. Indeed for systems below the Planck mass/charge, even if the bounds are formally correct, their meaning is trivial since any measurement of the state must at least interact with both parts of the superposition and this process requires at least a time $d/c$. | 520 | 1509.02408 | 12,710,760 | 2,015 | 9 | 8 | false | true | 1 | UNITS |
In accordance with Eqs. (REF), (REF), (REF), and (REF), in both cases $\alpha = \frac{1}{2}$ and $\alpha = \frac{2}{3}$, classical theory predicts the existence of the initial cosmological singularity at the point $a = 0$ in the domain of real values of the scale factor. The solution of Eq. (REF) which takes into account the domination of quantum correction (REF) on scales $a < 1$ demonstrates that, according to Eq. (REF), the initial cosmological singularity lies in the non-physical region of imaginary values of $a$ and it is inaccessible from the point of view of general relativity. Moreover, if one takes into account quantum effects in the region $a < 1$, it will allow one to revise the properties of the universe on sub-Planck scales. Quantum-mechanical description of the universe in semiclassical approximation admits the possibility of an origin of the universe from the sub-Planck domain. As is shown in Refs. [CIT], the origin of the universe is accompanied by a change in space-time topology, so that the geometry conformal to a unit four-sphere in a five-dimensional Euclidean flat space changes into the geometry conformal to a unit four-hyperboloid embedded in a five-dimensional Lorentz-signatured flat space. On the boundary, where these two subregions adjoin each other, there is a jump with change of metric signature [CIT]. | 1,350 | 1509.02740 | 12,713,764 | 2,015 | 9 | 9 | true | false | 2 | UNITS, UNITS |
Figure REF shows the expected 1-$\sigma$ uncertainties in $h$ from strong lenses combined with the Planck distance priors. As $D_{\Delta t}$ is mostly sensitive to $H_0$, the constraining power of $D_{\Delta t}$ + Planck (red dotted line) is more powerful than that of $D_A$ + Planck (blue dashed line). When $w$ is fixed as a constant (o$w$CDM model, left panel), $D_{\Delta t}$ + Planck are more powerful than $D_{\Delta t}$ + $D_A$ (black dot-dashed line). When $w$ is allowed to vary (o$w_z$CDM model, right panel), however, $D_{\Delta t}$ + $D_A$ is more powerful than $D_{\Delta t}$ + Planck. This is due to the degeneracies between $H_0$, $\Omega_k$ and $w$ from the linear CMB constraints alone [CIT], which cannot be broken by $D_{\Delta t}$. However, ref. [CIT] has shown that the main degeneracy from CMB constraints is between $w$ and $H_0$, and as shown in section [3.1], the combination of lensing distances is powerful in breaking the degeneracy between $\Omega_k$ and $w$. Thus, the combination of Planck and the lensing distances shows 30% improvement in constraining $h$. | 1,089 | 1509.03310 | 12,718,577 | 2,015 | 9 | 10 | true | false | 6 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
For CMB data, we use the distance priors data extracted from Planck 2015 [CIT], Planck 2013 [CIT] and WMAP9 [CIT] samples. To make a comparison, we also use the full "$Planck TT+lowP$" data given by the Planck 2015 data release [CIT]. For simplicity, hereafter we will call them "Planck2015", "Planck2013", "WMAP9" and "Planck2015(full data)", respectively. | 357 | 1509.03461 | 12,719,674 | 2,015 | 9 | 11 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
This research was partially supported by Scientific Research Fund of the Bulgarian Ministry of Education and Sciences under grant DO 02-137 (BIn-13/09). The Skinakas Observatory is a collaborative project of the University of Crete, the Foundation for Research and Technology -- Hellas, and the Max-Planck-Institut für Extraterrestrische Physik. | 345 | 1509.04936 | 12,733,114 | 2,015 | 9 | 16 | true | false | 1 | MPS |
Figure REF shows the tSZ power spectrum measured by Planck at 150 GHz [red symbols with error bars; [CIT]]. Two dashed lines show the tSZ power spectrum from the local universe at low multipoles and that from the light-cone at high multipoles, while the black solid line shows the sum of the two. This division in multipoles is consistent with the previous work showing that the nearby structures dominate at low multipoles simply because they appear larger in the sky [CIT]. | 475 | 1509.05134 | 12,735,654 | 2,015 | 9 | 17 | true | false | 1 | MISSION |
In short, the main conclusion from our study is that all the properties of tSZ found in the Magneticum Pathfinder simulation and the local universe simulation agree well with the Planck data. This includes the tSZ power spectrum, which was previously found to be in tension with the Planck 2013 parameters [CIT]. Now, the tSZ power spectrum calculated for the Planck 2015 parameters including CMB lensing information agrees with the measurement at all multipoles up to $l\approx 1000$. | 485 | 1509.05134 | 12,735,684 | 2,015 | 9 | 17 | true | false | 3 | MISSION, MISSION, MISSION |
We modeled the synchrotron emission in the microwave portion of the electromagnetic spectrum due to DM annihilation, making various assumptions about the DM density distribution, the DM particle model, as well as the MF and CR propagation models. DM emission intensity sky maps for various DM/MF/propagation models were created and compared with the data at seven WMAP-Planck frequencies. To test the consistency of the DM models with the data, we adopted two approaches. First we adopted a conservative approach which only considered CMB fluctuations and DM as contributing to the total sky intensity, while second we attempted to separate all the emission components including a potential DM signal using template fitting. The first approach yields relatively weak, but very robust DM constraints (see Fig. REF). | 814 | 1509.05135 | 12,735,701 | 2,015 | 9 | 17 | true | true | 1 | MISSION |
We test the validity of our method by computing our Fisher matrix forecast for the complete Planck mission and comparing our results to those obtained by Planck measurements. For that purpose, we shall use the $100$, $143$ and $217$ GHz channels of Planck with its accounted foreground removal as shown in Table REF, and following the specifications detailed in Table REF of the Appendix B. From the results depicted in Table REF, notice that there is an excellent agreement between the forecasted parameter errors and the errors quoted by the Planck collaboration, with the differences always below the $20\%$ level. In addition, we have verified that the correlations between the cosmological parameters are well accounted for. | 729 | 1509.05419 | 12,738,664 | 2,015 | 9 | 17 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
The plan of our paper is the following. In Sec. [2], we describe the observational samples and the methods we use to measure differential lensing surface density profiles and two-point autocorrelation functions. Our N-body simulations and the galaxy formation models based on them are introduced in Sec. [3]. We present results for differential lensing surface density profiles for SDSS LBGs in Sec. [4] and compare them with predictions from models with varying cosmologies, N-body realisations and physical models for galaxy formation. Galaxy clustering measurements for the SDSS LBGs are compared with various models in Sec. [5]. Finally, we recalibrate the scaling relations of [CIT] in Sec. [6], providing new relations which account consistently for the uncertainties both in effective halo mass and in stacked SZ and X-ray flux for each bin of LBG stellar mass. In a companion paper, [CIT] compare lensing signals for active and passive (e.g. blue and red) subsamples of our LBG sample, finding red LBGs to have significantly more massive halos than blue ones of the same stellar mass, while the same conclusion is reached by [CIT] through halo modelling to both lensing and clustering measurements. When quoting observational results, we adopt as our fiducial cosmological model the first-year Planck cosmology [CIT]. Our simulations assume a variety of other cosmologies as described in Sec. [3]. In the following we will define the reduced Hubble parameter h as $\mathrm{h}=H_0/100\mathrm{ km s^{-1}/Mpc}$. | 1,516 | 1509.05784 | 12,741,574 | 2,015 | 9 | 18 | true | false | 1 | MISSION |
We now illustrate this method by applying it to a realistic situation. We add a point source map to a simulated Gaussian CMB map with anisotropic noise, generated as described in the caption of Table REF. The point source simulation was created with the Planck Sky Model, at 143 GHz, with a beam with a FWHM of 5 arcmin, and contains faint infrared sources, as described in [CIT], and faint radio sources with the improved parameters described in [CIT]. The galactic and point source masks were applied as described in Section REF. | 531 | 1509.08107 | 12,764,446 | 2,015 | 9 | 27 | true | false | 1 | MISSION |
where $M_\mathrm{SZ}$ is the tSZ mass estimate and $M_\mathrm{true}$ is the *true* mass or the physically relevant mass, in this case replaced by the weak-lensing mass ($M_\mathrm{WL}$). The measured bias parameters for the Planck clusters [e.g., [CIT]] are used as priors in the likelihood for Planck tSZ cosmological results [CIT]. There is a disagreement between $1-b$ as determined directly from cluster observations and the $1-b$ inferred by fixing the cosmological parameters to the Planck primary CMB results [CIT]. This tension may point towards new phenomena or may be a systematic effect. | 598 | 1509.08930 | 12,772,460 | 2,015 | 9 | 29 | true | false | 3 | MISSION, MISSION, MISSION |
To demonstrate the compatibility of the tSZ measurements made by ACT and Planck, we recompute the ACT tSZ masses without correcting for Eddington bias and recover on average the same masses as Planck for the 31 common clusters (see Figure REF right panel). We exclude three outliers ($>2.5\sigma$) in this comparison. The most significant outlier is ACT-CL J0516-5430, which appears to be a more extended source than is typical for its redshift, $z = 0.294$. The clusters ACT-CL J2135.1-0102 and ACT-CL J0104.8+0002 appear to be contaminated by lensed high redshift sub-millimeter sources and radio sources, respectively. Further discussion of these three cases is found in [CIT]. We note that these three clusters were identified as outliers in [CIT] and their removal may lead to a possible selection bias. A $\chi^2$ test for the hypothesis that the remaining Planck and ACT cluster masses agree yields a probability to exceed of 0.15. A direct comparison of the published masses, for which ACT has included an Eddington bias correction, yields a systematic difference between the two masses, described by $M^\mathrm{ACT}_{500} = 0.86 M^\mathrm{Planck}_{500}$. The Eddington bias correction to the Planck tSZ masses is significant. This bias is accounted for in the Planck tSZ cluster cosmology likelihood when forward modeling the tSZ signal [CIT], but is not included in the public tSZ catalog of individual cluster masses provided by the Planck collaboration in [CIT]. | 1,474 | 1509.08930 | 12,772,492 | 2,015 | 9 | 29 | true | false | 7 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
Let us briefly review the main ingredients of the black hole deconstruction proposal. We start from the setup first introduced and studied by Maldacena, Strominger and Witten (MSW) [CIT] : consider M-theory on the background $\mathbb{R}^{1,3}\times S^1 \times X$, with $X$ a Calabi-Yau threefold. When the radius of the circle is small in 11D Planck units, the type IIA string theory picture is appropriate. One can consider BPS states which are point-like in $\mathbb{R}^{1,3}$, arising from wrapped (D6, D4, D2, D0) branes[^2] and labelled by a charge vector $\Gamma=(p^0, p^A, q_A, q_0)$. In the M-theory frame, these lift to (KK monopole, M5, M2, momentum) charges respectively, but we choose to use the IIA language throughout this paper. It is possible to construct a regular black hole carrying D4-D0 charges $(0, p^A, 0, q_0)$ which breaks half of the supersymmetry of the background[^3] and whose Bekenstein-Hawking entropy can be computed to be: FORMULA where $p^3 \equiv D_{ABC} p^A p^B p^C$ where is triple self-intersection of the four-cycle in $X$ wrapped by the D4-brane. | 1,086 | 1510.00583 | 12,780,648 | 2,015 | 10 | 2 | false | true | 1 | UNITS |
$B$ is defined on scalar fields on any causal set but is physically relevant for causal sets that are well-approximated by a four dimensional Lorentzian manifold, $(\mathcal{M},g)$. A causet, $(\mathcal{C}, \preceq)$ is well approximated by $(\mathcal{M},g)$ if there exists a *faithful embedding* of $\mathcal{C}$ into $\mathcal{M}$ in which the causal order of the embedded elements respects the order of $\mathcal{C}$ and in which the number of causet elements embedded in any sufficiently nice, large region of $\mathcal{M}$ approximates the spacetime volume of that region in fundamental units. These manifold-like, faithfully embeddable causets are typical in the random process of *sprinkling* into $(\mathcal{M},g)$: a Poisson process of selecting points in $\mathcal{M}$ with density $\rho$ so that the expected number of points sprinkled in a region of spacetime volume $V$ is $\rho V$. To do justice to our expectations for quantum gravity, the density $\rho = l^{-4}$, where $l$ is the fundamental length scale of the order of the Planck length. The probability for sprinkling $m$ elements into a region of volume V is FORMULA This process generates a causet, $\mathcal{C}$ whose elements are the sprinkled points and whose order, $\preceq$ is that induced by the manifold's causal order restricted to the sprinkled points. | 1,335 | 1510.04656 | 12,820,201 | 2,015 | 10 | 15 | false | true | 1 | UNITS |
Given the non-blackbody nature of the emergent spectrum, the turn-over that one begins to see at bluer wavelengths cannot necessarily be extrapolated with a Planck function. This suggests caution when inferring a bolometric luminosity by fitting a single blackbody temperature to the optical continuum. In both models of Figure REF, the bolometric luminosity is $10^{45}$ erg s$^{-1}$, much larger than one might estimate based on fitting a single blackbody to the optical/UV data. | 481 | 1510.08454 | 12,859,821 | 2,015 | 10 | 28 | true | false | 1 | LAW |
In this paper, we revisit the properties of the Surprise and compare it to other proposed measures of agreement between cosmological datasets. We derive expressions for these different measures in the limit of Gaussian likelihoods and a linear model and illustrate the results using a one-dimensional toy model. As an application of the Surprise, we reexamine the consistency of Planck and WMAP in light of the 2015 data release from Planck [CIT]. Motivated by the functional form of the Surprise, we analyze how we can identify directions in parameter space that are causing it. We discuss how these results illustrate the versatility of the Surprise as an information metric for concordance in cosmology. | 706 | 1510.08483 | 12,860,763 | 2,015 | 10 | 28 | true | false | 2 | MISSION, MISSION |
In this paper, we have addressed a number of outstanding issues in forecasts for upcoming $21,\textrm{cm}$ power spectrum and global signal measurements. First, we provided updated forecasts for $21,\textrm{cm}$ power spectrum measurements seeking to constrain astrophysical and cosmological parameters. Our forecasts are based on two sets of fiducial parameters from the Planck satellite. One set is based on the *Planck's* TT+lowP dataset and features a relatively high optical depth $\tau$, while the other is based on *Planck's* TT,TE,EE+lowP+lensing+ext dataset and features a relatively low $\tau$. Using a Fisher matrix formalism, we find that the projected parameter constraints from a power spectrum measurement are better for the TT,TE,EE+lowP+lensing+ext dataset than the TT+lowP dataset. The lower $\tau$ of the latter dataset implies a lower redshift of reionization, which is favourable to $21,\textrm{cm}$ experiments. This is because lower redshifts translate into higher frequencies for $21,\textrm{cm}$ observations, where the foregrounds are dimmer and instrumental noise is lower. Additionally, the cosmological constraints from the TT,TE,EE+lowP+lensing+ext dataset alone (i.e., without $21,\textrm{cm}$ information) are tighter than those from TT+lowP. This also contributes to better parameter constraints because instruments like HERA are sensitive enough to make cosmological parameter uncertainties non-negligible in one's data analysis. | 1,463 | 1510.08815 | 12,863,180 | 2,015 | 10 | 29 | true | false | 3 | MISSION, MISSION, MISSION |
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