dataesr/scientific-paragraphs-categorization huggingface dataset:
Discussion We conducted a two-sample MR study using summary statistics from the largest genome-wide association meta-analyses data sets currently available for BW and for breast cancer susceptibility in adults. Our study provides no evidence to support the association between higher weight at birth and an increased risk of developing breast cancer in later life that was previously reported in observational studies. In fact, we found that higher genetically-predicted BW might, if anything, be associated with reduced breast cancer risk. Our results were robust to the application of different MR approaches, each with its own distinct set of assumptions. A few observational studies suggest that the association between higher BW and increased future breast cancer risk is confined to premenopausal women but combined analyses of these studies show that this association does not differ by menopausal status  [7, 8].
However, neither SNP was associated with overall or ER-positive or ER-negative breast cancer risks at P < 0. 05 although the alleles that increased BW also conferred breast cancer risk (Supplementary Table  2 ; IVW MR analysis P = 0. 59 for overall breast cancer risk when using just these two SNPs as an IV for BW). Thus, while there is an association between SNPs in the core IGF-1 signalling genes and BW, our data do not provide any evidence that higher BW as predicted by these two IGF pathway SNPs is associated with adult breast cancer risk. While data on the association between BW and breast cancer risk in non-European populations is scarce, it is also worth noting here that a small study from China failed to show any association  [23]. In conclusion, the association between higher BW and increased risk of developing breast cancer in adulthood has been identified in several observational studies published over the last three decades.
Revisiting this association using a comprehensive set of recently-developed MR methods and the largest available genomic data sets provides no evidence to suggest that genetically-predicted higher BW is associated with increased breast cancer risk in adult life. A key unanswered question is whether the association between higher BW and increased breast cancer risk seen in observational studies is largely due to the BW-increasing effect of nongenetic factors such as maternal hormones and nutrition and we are unable to rule out an association between the nongenetically-determined component of BW and breast cancer. Acknowledgements This work builds on multiple, publicly available data sets. Data on birth weight and birth length were obtained from the Early Growth Genetics (EGG) Consortium. Data on adult height and adult body mass index were obtained from the Genetic Investigation of ANthropometric Traits (GIANT) Consortium.
Data on age at menarche and age at menopause were obtained from the Reproductive Genetics (ReproGen) Consortium. Data on age at first birth and number of children ever born were obtained from the Social Science Genetic Association Consortium (SSGAC). Data on type 2 diabetes were obtained from the DIAbetes Genetics Replication And Meta-analysis (DIAGRAM) Consortium. Data on breast cancer were obtained from the Breast Cancer Association Consortium (BCAC).
We report on a detailed X-ray study of the extended emission of the intracluster medium (ICM) around NGC 3268 in the Antlia Cluster of galaxies, together with a characterization of an extended source in the field, namely a background cluster of galaxies at z ≈ 0. 41, which was previously accounted as an X-ray point source. The spectral properties of the extended emission of the gas present in Antlia were studied using data from the XMM-Newton satellite, complemented with optical images of Cerro Tololo Inter-American Observatory (CTIO) Blanco telescope, to attain for associations of the optical sources with the X-ray emission. The XMM-Newton observations show that the intracluster gas is concentrated in a region centred in one of the main galaxies of the cluster, NGC 3268. By means of a spatially resolved spectral analysis, we derived abundances of the ICM plasma.
They were unable to conclude which of the peaks represented the real position of the minimum of the potential well due to limitations of the instrument. Hence, they had to use images from ROSAT PSPC archival data to unveil this issue. In these images, the peak to the west appeared like a point-like source, and they concluded that the only peak of diffuse emission was the one almost coincident with the position of NGC 3268. After extracting spectra of nine different regions around NGC 3268, they fitted a singletemperature model for all the regions and found that the cluster emission appears to be isothermal with a temperature of ∼2. 0 keV and a metallicity of Z = 0. 35 Z¯. However, they found that adding a cool component that represents gas at roughly 1. 0 keV yields a better fit to the spectra at low energies (∼1 keV).
The luminosity share of the cool component that they found is ∼20 per cent of the total luminosity of the gas within 70 h -1 70 kpc. Recently,  Wong et al. (2016)  studied Suzaku observations of the outskirts of Antlia out to 1. 3 R 200 in the east direction, where the cluster seems to be in equilibrium. They used Chandra and XMM-Newton data to identify and exclude point-like sources of their analysis. They found that the extended emission to the west of NGC 3268 is likely a background cluster of galaxies, considering the spectral features of the source. Hess et al. (2015)  studied the substructure of the Antlia Cluster through HI observations of a vast region around NGC 3268 and detected several groups of galaxies that are in the process of infalling into the cluster centre. They concluded that the group of galaxies around NGC 3268 is the central structure of the cluster.
In this work, we analyse X-ray observations of the region around NGC 3268 in the Antlia Cluster obtained by the X-ray Multi-Mirror Mission (XMM-Newton) satellite. The intracluster medium (ICM) is spectroscopically analysed, and new features of the emission are discovered. In particular, we fully characterize an extended source of emission to the west of NGC 3268 and associate it to a hidden group or cluster of galaxies at z ≈ 0. 41. The paper is organized as follows. In Section 2, we present the XMM-Newton observations and the data reduction as well as the Cerro Tololo Inter-American Observatory (CTIO) Blanco optical image. Optical data analysis, X-ray image, and spectral results for the extended emission of the Antlia ICM and the background cluster are presented in Section3, and, finally, the discussion is presented in Section4.
X-ray data SASThe group of galaxies centred around NGC 3268 in the Antlia Cluster was observed with the European Photon Imaging Camera (EPIC) on board the XMM-Newton X-ray observatory, using the PN and MOS1/2 cameras. Three different observations were carried out during 2010 March, 2012 December, and 2013 January. The study presented in this paper is based on the two data sets with longer exposure, which encompasses more than 100 ks each. The XMM data were analysed with the XMM Science Analysis System () version 17. 0 and the latest calibrations available in 2017 June. To exclude background flares, which can affect the observations, we followed the standard procedure to produce Good Time Interval (GTIs) files, using the SAS task ESPFILT. We list detailed information of the observations in Table  1.
Optical data In order to investigate the nature of the two emission peaks of the ICM, we also use wide-field (36 arcmin × 36 arcmin) images in R Kron-Cousins and C Washington filters, obtained with the MOSAIC camera mounted on the 4-m Blanco telescope from CTIO. The observations were carried out during 2001 April 4-5. Refer to  Dirsch et al. (2003)  for further information about these data. In Fig. 1  (right-hand panel), we show the optical image with the usual orientation (north is up, east to the left). The square with dashed lines highlights the XMM-Newton field, and the square with solid lines highlights the region of the Antlia Cluster studied in this paper.
Right: Optical field of the central region of Antlia observed with the Blanco telescope (CTIO) in the R-band  (Dirsch et al. 2003). Highlighted in dashed white lines is the field of the X-ray observations delimited in the left-hand panel and with a solid line the region under consideration in this article. counterpart is present. Only a weak point-like detection lies in the middle of the emission region, but a search through the NED and SIMBAD data bases in the coordinates of the object (α: 10:29:37, δ: -35:19:36. 5, J2000) has thrown negative results. The extended source was detected in the sixth data release of the XMM-Newton Serendipitous Source Catalogue (3XMM-DR6) and named 3XMM J102936. 7-351937. Hereafter, we shall name this region of emission as the SP. The point of maximum emission of this extended X-ray source is offset with respect to the dim object detected in the optical range by 16 arcsec.
6 arcsec according to the image scale of 0. 27 arcsec pixel -1. We used the software ISHAPE  (Larsen 1999 ) in order to fit the luminosity profile of the sources located in the SP region. This software calculates structural parameters of marginally resolved sources by fitting to each source the convolution between the PSF of the image and an analytical profile selected by the user. In order to produce accurate results, the fitted sources should have signal-to-noise (S/N) ratio ≈ 50, thus limiting our analysis to the bright source at SP centre. Previously to fitting the galaxy with ISHAPE, we subtracted a point source located at ∼3 arcsec in order to avoid contamination. This procedure was repeated iteratively in order to minimize the residuals. We applied Sérsic models  (Sersic 1968 ), which have proven to accurately represent the surface brightness profiles of galaxies.
X-ray spectra In this section, we present the X-ray spectral analysis of the regions of interest indicated with circles and ellipses in Fig. 5. We use the HEASARC XSPEC package (v12. 9. 1, from HEASOFT V20; Arnaud 1996) to perform a standard spectral analysis of the sources in order to fit spectral models to the data. Spectra were obtained using the evselect SAS task. A source spectrum was obtained together with a background spectrum. Regions around NGC 3268 and the SP of the extended emission share the same background, obtained in the more external parts of the FOV (see Subsection 3. 4. 1). Ancillary Response Files (ARFs) and Redistribution Matrix Files (RMFs) were produced using the ARFGEN and RMFGEN SAS tasks, respectively. The input of all the detectors was fitted simultaneously with the same model.
We also study the spectral properties of an elliptical region surrounding the wall-like feature to the east of NGC 3268 (tagged as SR). Point-like sources were removed from the data as indicated in the figure. After several tests, the best fit for region A1 was computed using a thermal emission model in equilibrium ionization APEC  (Smith et al. 2001) , widely used in the literature, and modified by an absorption model TBabs. The APEC model has as parameters the temperature of the emitting gas, its abundance, the redshift of the source, and the normalization factor. The version VAPEC adds the individual abundances. The TBabs model uses the cross-sections from  Balucinska-Church & McCammon (1992). The only free parameter of this model is the hydrogen column density N H. In the case of the galactic emission of NGC 3268, in the region A0, we found that the APEC model modified by the absorption model TBabs was not sufficient to fit the counts at higher energies, so we added a power law.
7 keV. Fig. 11  shows a more detailed view of the fitted line. Inspection in the AtomDB web data base reveals that there is no such strong line of emission around that energy. Now, if we consider that the SP of emission can be the Notes. Normalization is defined as 10 -14 /4πD 2 × R n H n e dV, where D is distance (cm), n H is the hydrogen density (cm -3 ), n e is the electron density (cm -3 ), and V is the volume (cm 3 ). Fluxes are given in units of 10 -14 erg cm -2 s -1 and are not absorption-corrected. Error values are given as the 90 per cent confidence level for every single parameter. The redshift parameter in the APEC model corresponding to the Antlia ICM was fixed in z = 0. 0087. The metal abundance A is given relative to the solar abundance calculated by  Anders & Grevesse (1989).
1 R 500. D a is the angular diameter distance. N spec is the normalization of the thermal model fitted using XSPEC. Following  Pascut & Ponman (2015) , we computed the emissivity by means of the analytical expression n e (r) = r (n e /n H ) N spec 4π [D a (1 + z)] 2 V 10 -14 ²(r) C , (3) ²(r) = ² 0 [1 + (r/r c ) 2 ] -η , (4) where η = 3β and ² 0 = S 0 /[2r c R π/2 0 cos α 2(η-1) dα]. β, S 0 , and r c are free parameters of a beta model fitted to the brightness profile of the cluster. For this purpose, we constructed a brightness profile of the Antlia Cluster using annuli centred on NGC 3268 and with 1R = 0. 25 arcmin. The brightness profile was constructed using the Chandra's data analysis system  (CIAO 4. 9 Fruscione; McDowell & Allen 2006). We used an image in the spectral range 0. 3-5. keV and masked pointlike sources and the SP of emission in the image to avoid brightness excesses.
We subtracted the same background used in the spectral analysis. For distances larger than 10 arcmin of the cluster centre, the brightness profile is severely affected because of the background subtraction (see Section 3. 4. 1). Then, we fitted a beta model to the data given by S(r) = S 0 [1 + (r/r c ) 2 ] -3β+0. 5 , ( 5 ) where S 0 and r c are the central surface brightness and core radius, respectively. The fitted values to the brightness profile are β = 0. 7, r c = 6. 16 arcmin, and S 0 = 80. 58. Fig. 12  shows the normalized brightness profile and the best-fitting model with a dotted line. Using the derived parameters, we estimated a cooling time for the Antlia Cluster central region at R = 0. 1 R 500 of t cool = 13. 6 Gyr, which is nearly the age of the Universe within our assumed cosmology.
D I S C U S S I O N The observation of X-ray emission in galaxy clusters has been a useful tool to derive properties that describe their physical state. Here, we present a detailed analysis of two XMM-Newton observations to study the region around NGC 3268 in the Antlia Cluster. In Section 2. 2, we show the images of the region under consideration. A peak of extended emission lies nearly coincident with the position of one of the central galaxies of the Antlia Cluster, NGC 3268. Moreover, an SP of emission is present on the west side. These X-ray sources of emission were already noted by  Nakazawa et al. (2000). They used data from the GIS on board the ASCA satellite to analyse the core of the Antlia Cluster, but the peak of emission to the west of around NGC 3268 fell in the window-support grids and could not be correctly observed.
Therefore, they used data from the PSPC instrument on board the ROSAT satellite to determine which of the observed peaks represented the real minimum of the gravitational potential. They argued that the SP was a point-like source. We also detected the SP of emission at ∼4. 68 arcmin to the west of the peak associated with NGC 3268. However, our images show that the emission is widely extended and it can hardly be accounted as a point-like source, as also noted by  Wong et al. (2016). We examined optical images of these regions looking for an optical counterpart to understand the nature of this emission, and a combined image of filters R and C was needed to reveal an extended object in the coordinates of the emission. Despite the low resolution of the optical images, we performed different fits to the brightness profile of the extended object using a Sérsic model and found that the one with a Sérsic index of n = 3 reproduces more accurately the brightness profile of the source.
AC K N OW L E D G E M E N T S We thank the referee for his/her helpful comments that allowed us to improve this paper. IDG and FG are CONICET fellows. IDG, JPC, and LPB acknowledge support from  Consejo Nacional de Investigaciones Cientificas y Tecnicas de la Republica Argentina, Agencia Nacional de Promocion Cientifica y Tecnologica , and  Universidad Nacional de La Plata (Argentina). FG and JAC were supported by  PIP 0102  (CONICET). JAC was also supported on different aspects of this work by  Consejería de Economía, Innovación, Ciencia y Empleo of Junta de Andalucía , under excellence grant  FQM-1343  and research group FQM-322, as well as FEDER funds. This work is based on observations obtained with  XMM-Newton , an  ESA  science mission with instruments and contributions directly funded by  ESA Member States  and the  USA (NASA).
Techniques SANS measurements were carried out on the D11 beamline at Institut Laue Langevin, France. The samples were contained in 1 mm path-length Hellma cells. Sample temperature (10 1C or 25 1C) was controlled via a thermostated bath coupled to the D11 sample changer. Two sample-detector distances were used: 1. 2 m and 8 m. The incident wavelength was 4. 6 Å and the resulting detectable scattering vector, Q range was approximately 0. 009-0. 7 Å À1. Absolute intensities for the scattered intensity, I(Q) (in cm À1 ) were determined by calibrating the received signal to water and correcting for sample transmission and solvent background, giving the data shown in Fig. 1b  and Fig. S1 (ESI † ). SAXS measurements were carried out on BL40B2 at SPring8, with an incident wavelength of 1. 01 Å, a sample-detector distance of 1.
647 m and a 3000 Â 3000 pixel IP detector, giving a detectable Q range of approximately 0. 03-0. 51 Å À1. The sample temperature was controlled by a hot/cold stage (HCS302, Instec Inc. , CO). Collected data were corrected for natural background radiation, transmission, sample thickness, measurement time, primary beam flux, parasitic background, polarisation and detector solid angle coverage using in-house developed data reduction software written in Python. 9 Sample transmission was established through comparison of the signals from two ion chambers, placed before and after the sample position, intercalibrated by a measurement with no sample in place. The average cylindrical capillary thickness (1. 5 mm capillary), based on a beam width of 8 mm Â 4 mm, was calculated to be 1. 42 mm. The intensity was subsequently binned using 200 linear bins spanning the aforementioned Q range, and scaled to absolute units using a calibrated glassy carbon standard provided by Jan Ilavsky and coworkers.
10 The result was three-column data with Q, and I(Q) in absolute units, in addition an uncertainty estimate, giving data shown in Fig. 1c. Diffusion NMR measurements of 1 in n-hexane-d 14 , n-decane-d 22 and toluene-d 8 were performed as a function of concentration at an observation time, D, of 20 ms, with a gradient duration, d, of 2 ms, a maximum gradient strength, G, of 400 G cm À1 and 32 gradient steps. The diffusion coefficient, D exp , from molecule 1 was determined using the Stejskal-Tanner equation: 11 SðGÞ Sð0Þ ¼ exp Àg 2 d 2 G 2 D exp D À d 3 (1) where g is the gyromagnetic ratio and (S(G))/(S(0)) the normalised signal attenuation, which was acquired by integrating the peak at 2. 85 ppm in the 1 H spectrum for compound 1, which arises from the methyl group attached to the nitrogen atom.
8 sothermal titration calorimetry (ITC) measurements were carried out using a Microcal VP-ITC system. After thorough washing, pure solvent (i. e. n-decane, n-hexane or toluene) was entered into both reference and sample cells. The injector syringe was filled with a solution (124 mM) of molecule 1 in the same solvent. The syringe has a maximum volume of approximately 0. 295 mL and the sample cell volume is 1. 414 mL, so the maximum concentration that could be reached was around 21 mM. A typical run consisted of 36 injections of 8 mL, after an initial injection of 1 mL. Using the OriginPro 8. 1J plugin, datasets were corrected for the baseline signal, giving the raw data plots shown in Fig. 3a. For comparison, the data in Fig. S2  (ESI † ) is shown prior to background subtraction. Finally, for all solvents the peaks were integrated and corrected for concentration, resulting in a plot of response vs.
Small-angle scattering Contrast-variation SANS data was collected for samples of 1 in n-hexane, n-decane and toluene. 12 Fig. 1b  shows the data for 0. 1 M 1 in n-hexane at 25 1C, while the data for 0. 025 M and 0. 05 M in n-hexane at 25 1C, 0. 1 M in n-hexane at 10 1C, and 0. 1 M in n-decane and in toluene at 25 1C are shown in Fig. S1  (ESI † ). In all cases, three contrast profiles were used: SANS from the whole micelle (core + shell) was obtained when a perdeuterated n-alkane solvent was used, while the shell and core were individually highlighted using blends of perdeuterated and perhydrogenated n-alkane solvents contrast-matched to the scattering length density, r of C 60 , r C 60 (CM-C 60 ) or of the alkyl chains in 1, r alkyl (CM-alkyl). Values of r C 60 and r alkyl were estimated to be 5.
However, while these methods gave results that are broadly consistent with the mixed model (Fig. S2 , Tables  S3  and S4 , ESI †), neither showed the same level of agreement with all datasets. Equations for all of the models, and further justification for their use, are given in the ESI. † For the mixed model, fitted parameters were the scale factor N, which is related to the number density of scattering objects, the core radius r core and its dispersity s, the shell width d shell , and the peak amplitude A peak , centre Q peak , and half width at half maximum w peak. An additional flat background contribution, I bkg was allowed for all datasets, as while both the SANS and SAXS data were normalised and the background solvent scattering subtracted, some under-/over-subtraction occurred as a result of (1) the high 1 H content in 1 and (2) displaced volume effects.
23 The SASfit analysis software was used in all cases. 24 For the SANS data, the three different contrast profiles CM-alkyl, CM-C 60 and the 100% deuterated solvent were analysed simultaneously, using the ''multifit'' capability of SASfit. In this case, global parameters N, r core , d shell , s, Q peak and w peak were held constant across the three contrast profiles, apportioning greater reliability to these values and to the overall fit. As the level of solvent penetration into the micelle shell is unknown, the scattering length density of the shell, r shell was additionally allowed to float for the CM-C 60 and 100% deuterated solvent contrast profiles (NB: not for CM-alkyl, as r shell = r solvent ). Fitted values point to a solvent penetration into the shell of around 20%, which seem reasonable based on the molecular dimensions of 1.
However, the R h,scaled value for 0. 1 M 1 in n-hexane is larger than that obtained by SANS. This may be due to a greater level of interaction between neighbouring micelles originating from the larger extent of aggregation in this sample. Such interactions would reduce the diffusion coefficient and lead to an overestimation of R h,scaled. Network formation, implied in the SANS and SAXS analysis, would have the same effect and could also contribute to the overestimation. Values of R h,scaled E 10 Å for all samples in toluene, and for 0. 025 M 1 in n-decane suggest a predominance of nonassociated monomers of 1, given that for bare C 60 in benzene, R h = 6. 4 Å,  30  in line with both the SANS data presented above and previously published SAXS data. 3 The change in R h,scaled between 0. 025 and 0.