dataesr/scientific-paragraphs-categorization huggingface dataset:
Free radicals Raw 264. 7 cells were cultured under irradiation and the level of production of free radicals evaluated at different times after the beginning of the irradiation using a chemoluminescent method. In order to normalize the data between experiments, the results were expressed as an irradiated/control ratio of free radical levels. The dots in Figure !1A indicate this ratio as a function of time. We observed that the Raw264. 7 cells cultivated under irradiation had a statistically higher capacity of free radicals production when compared to controls. This capacity was maximal after 3 and 4 weeks of irradiation (p<0. 01 and p<0. 05 respectively) corresponding to total cumulative doses respectively estimated at 2. 7 cGy and 3. 6 cGy) and returned to control level after 6 weeks (total cumulative dose respectively estimated at 5.
Apoptosis assay The characteristic apoptotic bodies were observed both in extracellular space and in the macrophage cytoplasm. Early-stage apoptosis was also detected as intact cell with nuclear condensation. The mean values of percentages of apoptotic bodies were similar in the two groups at 32 weeks (3 ± 0. 8 % in controls and 3. 16 ± 0. 3 % in irradiated) and at 42 weeks (3. 78 ± 0. 6 % versus 3. 16 ± 0. 4 % in controls), without significant changes (data not shown).
We study cosmological models involving scalar fields coupled to radiation and discuss their effect on the redshift evolution of the cosmic microwave background temperature, focusing on links with varying fundamental constants and dynamical dark energy. We quantify how allowing for the coupling of scalar fields to photons, and its important effect on luminosity distances, weakens current and future constraints on cosmological parameters. In particular, for evolving dark energy models, joint constraints on the dark energy equation of state combining BAO radial distance and SN luminosity distance determinations, will be strongly dominated by BAO. Thus, to fully exploit future SN data one must also independently constrain photon number non-conservation arising from the possible coupling of SN photons to the dark energy scalar field.
Therefore, not allowing for such couplings may significantly bias the analysis of current and future cosmological datasets. In this paper, which is a sequel to  [3] , we focus on potentially observable signatures of the interaction of cosmological scalar fields with the electromagnetic sector, specifically changes to the standard evolution of the Cosmic Microwave Background temperature with redshift, T (z) = T 0 (1 + z). ( Rather than focusing on a particular favoured model and obtaining specific constraints, we consider two general classes of models from the Cosmology literature, described in a phenomenological way. These include models in which a scalar field drives variations of the fine-structure constant, and models where the scalar field is responsible for cosmic acceleration. Since scalars can in general couple to the electromagnetic sector, our goal is to demonstrate that such scalar-photon couplings, if not accounted for, can strongly bias cosmological parameter determination.
We quantify how important an effect these couplings can have on constraints derived from current and future datasets, and show how the degeneracy can be broken through the independent reconstruction of the CMB temperature evolution. The two canonical ways to reconstruct the evolution of the CMB temperature with redshift rely on spectroscopy of molecular/ionic transitions triggered by CMB photons  [4] [5] [6]  and on the thermal Sunyaev-Zel'dovich (SZ) effect towards clusters  [7] [8] [9] [10]. New sources will soon become available for measurements by the above methods, and entirely new methods for measuring T (z) are also being developed, so it is timely to consider their impact on cosmology and on searches for new physics. There is also complementarity with other techniques that are now becoming available.
3(κh) × 10 -17 s -1 , (3. 9) where the inequality is due to dark energy. According to Rosenband et al. [20]  this variation is constrained to be when the inequality in (3. 9) is saturated. In practice, κ can be significantly larger due to the effect of dark energy suppressing α variations in the present era, but note that even this figure is consistent with the aforementioned dipole hint  [19] : if one ignores the direction of sources on the sky and naively fits the entire dataset to the above function, there is no strong evidence for a non-zero κ. The spatial dependence of these measurements will be addressed in subsequent work. There is thus no tension with atomic clock constraints. As discussed in  [3]  the typical precision expected for temperature measurements will significantly increase with the next generation of facilities.
17) where d L and d A are the luminosity and angular diameter distance measures respectively. Therefore for this class of varying-α models we predict that d L (z) = d A (z)(1 + z) 2 α(z) α 0 3/8 ∼ d A (z)(1 + z) 2 1 + 3 8 ∆α α (3. 18) ∼ d A (z)(1 + z) 2 1 - 3 2 k ln (1 + z). Again, this relation can be tested for both time and/or spatial variations of α; even though the effect is small, there are hundreds (and in the future there will be thousands) of type Ia supernova measurements. Recently  [29]  found a 2σ hint for a 'supernova dipole' aligned with the α dipole. Their analysis does not take into account the effects of varying α on the supernova brightness (see  [30]  for a succinct discussion). Such effects are negligible with current supernova sensitivities but they could soon become relevant as datasets of a few thousands of supernovae became available.
As was pointed out above, in the models we are considering, in which the deviation from the standard T (z) relation is due to a coupling of CMB photons with the dark energy scalar field, one generally expects that the same field also couples to optical photons, thus affecting luminosity distances, as discussed in  [3]. Within a given model, one can then translate T (z) deviations to violations of the distance duality relation  (3. 17). Note that on general grounds, the coupling is expected to be weaker for lower photon frequencies, so assuming a frequency-independent coupling should yield conservative bounds on T (z) violations from SN (or other optical) data. We use the Union2. 1 SNIa compilation  [34]  and a number of different determinations of H(z): cosmic chronometers  [35] [36] [37]  (11 data points in the redshift range 0.
Fig. 4  shows current constraints from combining the above luminosity distance and radial distance data on our (flat) CPL-CDM models, allowing for a non-zero k in equation (4. 5). The top left panel of Fig. 4  shows 2-parameter joint constraints (68% and 95%, having marginalised over k and Ω m ) for the SN (blue filled contours), H(z) (dashed lines) and combined SN+H(z) data (solid line contours). Having allowed for violation of photon number conservation through the parameter k, the SN constraints on the dark energy equation of state are weak, but the constraints improve dramatically with the inclusion of H(z) data that are not affected by k. The region near w 0 = 0, favoured (at the 1σ level) by the SN data, corresponds to negative values of k (i. e. photon dimming due to decay to scalar particles) as is evident from the top right panel of Fig.
4. The bottom left panel then shows that corresponds to large values of Ω m , so low values for the dark energy density parameter. This is the well-known degeneracy between dark energy and photon number non-conservation, which gets broken by including the H(z) data favouring Ω m near 0. 25. For comparison, in the bottom right panel we show the corresponding constraint on the w 0 -w a plane but now assuming that photon-number is conserved, k = 0. In Fig. 5  we show constraints on the dark energy equation of state w for flat wCDM models, again allowing for k ∈ [-5, 5] × 10 -5 (left), and enforcing photon number conservation, k = 0 (right). This again highlights the dramatic effect of k on constraints derived from the SN data. On the contrary, the effect of k for the H(z) data is insignificant; that is, H(z) alone does not significantly constrain k as mentioned and combined SN+H(z) data (solid line contours).
Having allowed for photon number nonconservation, the SN data alone do not strongly constrain dark energy (and favour w 0 ∼ 0 at the 1σ level), but the inclusion of the H(z) data strongly improves dark energy constraints. Top Right-Bottom Left: The SN data favoured region w 0 ∼ 0 corresponds to negative k (photon dimming) and large Ω m , exemplifying the well-known dark energy-photon dimming degeneracy. This gets broken by using the H(z) data which favour Ω m ≃ 0. 25. Bottom Right: As in top left plot but now assuming that photon-number is conserved k = 0. Note the dramatic effect of k on SN constraints (blue filled contours). above-refer to equation (4. 3) and the ranges of w 0 and k. The important effect of photon-number violation on weakening SN constraints, shown in Figs. 4 5 , makes clear that, in order to efficiently exploit current and future SN data for dark energy parameter determinations, one must independently constrain photon-number violations, which can be done through independent T (z) determinations  [3, 6, 10] , as discussed above.
3, k ∼ 0} (also refer to Fig. 4 ). However, the degeneracy is not broken, and the region around w 0 ∼ 0 is still allowed by the SN data. The overall constraint on w 0 is still controlled by the H(z) data, even though the bound on w a is now much stronger. In the same figure, we also show the corresponding SN contours that one would obtain if k was constrained at the 10 -5 level (dotted lines). The SN contours shrink a little, but w 0 ∼ 0 is still allowed, and the total constraint is again controlled by the H(z) data. For the Union2. 1 SN dataset to become competitive with the current H(z) determinations, k must be independently constrained at the ∼ 10 -6 level, resulting in a SN contour similar to that of  Fig 4, bottom right. This is at a level attainable using current Sunyaev-Zel'dovich T(z) measurements: namely the stacked Planck SZ clusters of  [44]  and the constraints from SPT clusters  [45].
We will present a detailed T(z) analysis based both on SZ clusters and on atomic and molecular absorption lines in a follow-up publication. Such T(z) constraints will therefore provide an independent means of breaking the degeneracy between dark energy parameters and photon number non-conservation, subject to completely different systematics. Currently, this degeneracy can only be broken by combining SN constraints with a k-independent dataset like H(z), as we have demonstrated, and it is important to be able to also break the degeneracy by directly constraining the photon violation parameter k. Similarly, if one is instead interested in constraining photon-number violations in the context of evolving dark energy cosmologies (rather than constraining dark energy in a way that accounts for photon-number violations), then T(z) measurements offer a more direct Figure  6.
Constraints from future datasets Let us now proceed to present forecasts for future datasets. We will be particularly interested in studying the impact of the Euclid mission, and will start by considering one of its probes, BAO from the Euclid wide survey, which is expected to cover ∼15000 deg 2 of extragalactic sky down to a redshift of order 2. Assuming the same conservative priors as in Fig. 4 , we repeat the above analysis with simulated data for Euclid BAO and a SNAP-like SN mission. BAO radial distance errors have been estimated using the code developed by Seo & Eisenstein  [46]  adapted for Euclid estimated parameters  [15]. For SN we follow  [47]  for a Dark Energy Task Force Stage IV SN mission. The relevant constraints are shown in Fig. 7. As before, we show 68% and 95% likelihood contours for the SN data in blue (filled contours), while the transparent dashed line contours are for BAO H(z) data.
Note, in particular, that the horizontal band around w 0 (bottom left plot) for the SN data disappears, as it corresponds to a region with k ≃ -10 -5 (cf. top plots). The main message arising from this analysis is that constraining k at a level 10 -6 will rule out this region, shrinking the SN contours by a factor of a few and improving the joint SN+H(z) constraint by a factor of ∼ 2 in the context of CPL-CDM models (Fig. 7 , middle left plot). We will discuss current and future constraints on k from T(z) measurements, and their quantitative effect on dark energy parameter bounds, in a follow-up publication. In the rest of this section we will examine the ability of future BAO and SN surveys to jointly constrain dark energy parameters and k in the absence of such an independent bound on k.
11. We empahsise that the numbers we use for the E-ELT and the TMT come from assumptions made in Phase A studies of their relevant instruments; the amounts of telescope time required for gathering each dataset are not necessarily comparable. We can see that these high-redshift supernovae lead to significantly improved constraints, compared to the previous Euclid+SNAP case. On the other hand, the constraints from the E-ELT and the TMT are comparable, indicating that the larger redshift lever arm partially compensates the smaller number of supernovae. Note, however, that these improvements on SN constraints from the inclusion of high-redshift supernovae, will only have a moderate effect on the joint BAO+SN result, unless k is independently constrained as discussed above. Table  1  provides a comparison of the uncertainties in the various model parameters obtainable in each case.
Conclusions We have studied two typical classes of phenomenological scenarios involving scalar fields coupled to radiation, specifically considering their effects on the redshift evolution of the cosmic microwave background temperature. In the first of these a BSBM-type field provides a time variation of the fine-structure constant α, while in the other the dynamical scalar field is responsible for the recent acceleration of the universe. Our analysis shows that the effects of the coupling of scalar fields to photons, which include effects on luminosity distances, dramatically weaken current and future constraints on cosmological parameters. In particular, our results strongly suggest that in order to fully exploit forthcoming SN data one must also independently constrain photon-number non-conservation arising from the possible coupling of SN photons to the dark energy scalar field.
We have also considered the role of the increased redshift lever arm provided by type Ia supernovae at high redshift (z > 2), such as can be found by JWST and ground-based extremely large telescopes. Specifically, we have considered two different samples which are meant to be representative of the E-ELT and TMT, with the former going deeper into the matter era while the latter has five times more supernovae. The constrains from both datasets (in combination with lower-redshift measurements) are quite comparable: the E-ELT provides a better constraint on the matter density (for which the increased redshift lever arm is the dominant factor) while the TMT provides better constraints on the dark energy parameters w 0 and w a (since, at least in the models we considered, dark energy is negligible at the higher redshifts, the larger number of supernovae provides the dominant effect).
On the left plot, note that the horizontal band around w 0 for the SN data corresponds to a region with k ≃ -10 -5 (cf. top plots), and it disappears when k is constrained at the 10 -6 level. 7. While Euclid alone cannot strongly constrain k (violations of photon number conservation) it will still provide useful constraints on dark energy parameters, especially within the wCDM model. However, the joint constraints (solid transparent contours) are determined predominantly by the BAO data (dashed transparent contours), while the SN-only bounds (blue filled contours) are weak. Therefore, these constraints become much stronger when a low-redshift SN sample is a also included, cf. Fig. 9.
Acknowledgments This work was done in the context of the project  PTDC/FIS/111725/2009  from  FCT (Portugal)  and the cooperation grant ' Probing Fundamental Physics with Planck' (PHC-EGIDE/Programa PESSOA , grant  FCT/1562/25/1/2012/S ), with additional support from Grant No. PP-IJUP2011-212  (funded by  U. Porto  and  Santander-Totta ). AA was supported by the  Marie Curie  grant  FP7-PEOPLE-2010-IEF-274326  and a  University of Nottingham Research Fellowship. We acknowledge useful comments and suggestions from  Isobel Hook  and other members of the  Euclid Cosmology Theory and Transients & Supernovae Science Working Groups. We also acknowledge use of the  Planck Mission Cosmological Parameters Products , which are publicly available from the  Planck Legacy Archive  (http://www. sciops. esa.
Bti application: At t0, measured quantity of Vectobac GR was dispensed manually taking necessary safety precautions using gloves and facial masks. Cohort monitoring: Larvicidal activity might last longer than the developmental period. In this context, cohort of 30 to 50 second instars larvae of An. gambiae or Cx. qinquefasciatus were released in each container every 7 to 10 days, depending on the larval development time frame. Each An. gambiae and Cx. quinquefasciatus larvae cohort was fed with 0. 5 g and 1 g of cat food respectively when released. Each day after treatment, pupae were counted and removed from the containers and placed in plastic cups with water and covered with a netting piece. Temperature and pH of water in the containers were recorded daily and meteorological data were obtained from the National Meteorology Department.
Data Analysis The data analyses were performed using R software (version 2. 11. 1). Data from the simulated field trial were used to estimate the Emergence Inhibition Rates (% EIR) for each treatment according to the following formula: % EIR~CT ð Þ=C ð Þ |100 where C is the emergence rate in the control and T is the emergence rate in the treated containers at the same period of time  [13]. A logistic regression model with a logit link was fitted to the data to investigate the effect of the treatments on the emergence rate. The influence explanatory covariables on the emergence rate was investigated by including in the models the dose, the number of day post-treatment and the replicates. The number of day after which the emergence rates significantly increased to more than 20% with 95% Confidence Intervals was estimated for each treatment based on the logistic regression model.
Concerning data from the field trials, the mean number of larvae and pupae collected (i. e. density) per sampling day was calculated for both treated and control groups. The first and second instars larvae (L1+L2) were pooled as early instars and the third and fourth instars (L3+L4) as late instars. Density Reduction (DR) of early and late instars larvae as well as pupae was estimated post-treatment using Mulla's formula as follows: DR~100{ C 1 =T 1 ð Þ| T 2 =C 2 ð Þ|100 where C 1 is the average number of larvae or pupae in control breeding sites prior to treatment and C 2 is the average number of larvae in control breeding sites at each day of sampling. T 1 is the average number of larvae or pupae in breeding sites to be treated with Vectobac GR and T 2 is the average number of larvae or pupae in treated breeding sites for each sampling day  [13].
ACKNOWLEDGMENTS Valérian Chambon was supported by a  Post-doctoral Fellowship  of the  Région Île-de-France (Paris) , and by  ANR-10-LABX-0087 IEC  and  ANR-10-IDEX-0001-02 PSL*. Nura Sidarus  was supported by  UCL Impact Scholarship  and the  Belgian Science Policy Office  project " Mechanisms of conscious and unconscious learning " ( IAP P7/33 ). Patrick Haggard  was supported by an  ESRC   Professorial Fellowship , an  ESRC/ESF  ECRP Research Project, an  ERC Advanced Grant  (HUMVOL) and by  EU   FP7 Project VERE, Work Package 1.
Acknowledgements We thank all the members of the  Lenne and Bertrand labs , in particular  Olivier Blanc  for software development and  Jérémie Capoulade  for discussion. We also thank the PICsL-IBDM imaging facility, in particular  Claude Moretti  and  Brice Detailleur  for technical support. This work was supported by  ATIP  grants from  CNRS  (to P. -F. L. and V. B. ), the  Labex INFORM  grant (to P. -F. L. and V. B. ) and a grant from  Sanofi-Aventis  (to V. B. ). We acknowledge  France-BioImaging  infrastructure supported by the  Agence Nationale de la Recherche  ( ANR-10-INSB-04-01 , call " Investissements d'Avenir ").
Acknowledgments: This work has been partially supported by the  Agence Nationale de la Recherche  and  Japanese Science and Technology Agency within the framework of the 'WITH' ANR/JST Franco-Japanese  project, and was partly supported by the  Ministry of Higher Education and Research, Nord-Pas de Calais Regional Council and FEDER  through the  Contrat de Projets Etat Région  ' Campus Intelligente Ambiante ' (CPER-CIA) 2007-2013.
In T. gondii, loss of BCKDH leads to global defects in glucose metabolism, increased gluconeogenesis and a marked attenuation of growth in host cells and virulence in animals. In P. bergei, loss of BCKDH leads to a defect in parasite proliferation in mature red blood cells, although the mutant retains the capacity to proliferate within 'immature' reticulocytes, highlighting the role of host metabolism/physiology on the development of Plasmodium asexual stages. Intracellular growth of RH (blue) and Tge1a_ko (red) was assessed after 24 h in complete media, media lacking glutamine, or glucose. Following 24 h of growth in glucose-depleted environment, glucose was added back to the media and rescue of the parasite's growth was assessed. Data are represented as means 6 SD from three independent biological replicates.
2C ). Collectively, these findings show that the BCKDH is required for the conversion of pyruvate to mitochondrial acetyl-CoA and operation of a cyclical TCA cycle. In the absence of BCKDH, the continued production of C4 dicarboxylic acids derived from glutamine by the oxidative TCA cycle leads to Intracellular growth assay at 32 h post transient transfection of Tge1a_ko with pTub8-SOD3mycPDHE1a, pTub8-SOD3mycBCKDHE1a and pTub8-mycNtGAP45 (negative control) in complete media or media depleted in glucose. Data are represented as means 6 SD from three independent biological replicates. Only vacuoles containing parasites transiently expressing the transgene were taken into account. Over 200 vacuoles were counted per replicate. (G) CD1 mice were infected with RH (in blue) or Tge1a_ko (in red) tachyzoites (,15 parasites per mouse) and survival was assessed over 21 days.
(D) Mass isotopologue abundances of citrate generated in 13 C-glucose and 13 C-glutamine-fed RH and Tge1a_ko tachyzoites. 'M' indicates the monoisotopic mass containing no 13 C atoms. Error bars indicate standard deviation (n = 3). (E) Intracellular growth of RH (blue) and Tge1a_ko (red) was assessed after 24 h in medium depleted of glucose complemented or not with 5 mM exogenous acetate. Data are represented as means 6 SD from three independent biological replicates. doi:10. 1371/journal. ppat. 1004263. g002 shown in (Fig. 4E ). Indeed, we observed no difference in invasion efficiency between WT and Pbe1a_ko parasites when using purified normocytes and reticulocytes as target host cells. In vitro maturation was examined following in vitro invasion of purified normocytes or reticulocytes. This selective distribution appears to be due to rapid loss of viability of Pbe1a_ko in the normocytes.