Impact of tidal environment on galaxy populations using GAMA

We present constraints on models of the galaxy distribution in the cosmic web using a magnitude limited sample from the Galaxy and Mass Assembly (GAMA) survey. We model the redshift-space behaviour of the 2-point correlation function (2pcf) and the recently proposed Voronoi volume function (VVF) -- which includes information beyond 2-point statistics. We extend the standard halo occupation distribution model by introducing extra satellite degrees of freedom, and also by including two assembly bias parameters, $\alpha_{\rm cen}$ and $\alpha_{\rm sat}$, which respectively correlate the occupation numbers of central and satellite galaxies with their host halo's tidal environment. We measure $\alpha_{\rm sat}=1.44^{+0.25}_{-0.43}$ and $\alpha_{\rm cen}=-0.79^{+0.29}_{-0.11}$ using a combination of 2pcf and VVF measurements. These represent a detection of assembly bias at the 3.3$\sigma$ (2.4$\sigma$) significance level for satellite (central) galaxies, a result that remains robust to possible anisotropies in the halo-centric distribution of satellites as well as technicalities of estimating the data covariance. We show that the growth rate ($f\sigma_8$) deduced using models with assembly bias is about 7\% (i.e. $1.5\sigma$) lower than if assembly bias is ignored. Projecting $f\sigma_8$ onto the $\Omega_m$-$\sigma_8$ plane, we find that the model constraints without assembly bias overlap with Planck expectations, but that allowing assembly bias introduces significant tension with Planck, preferring either a lower $\Omega_m$ or a lower $\sigma_8$. We also study the effect of assembly bias on the weak lensing signal. While the all-galaxy lensing signal is unaffected, both central and satellite sub-populations individually show significantly different signals in the presence of assembly bias. [abridged]Comment: 17 pages, 14 figures, 2 tables, submitted for revie

An Evaluation Of Short-Term Prognostic Significance Of Various Clinical Parameters In Patients Of Stroke

Sonali Saxena', Shadab A. Khan", Jalaj Saxena’" * Consultant Cardiologist, ** Professor (Medicine), *** Assistant Professor (Physiology) Ishwardevi Medical and Cardiology Centre, Kanpur J.N. Medical College, A.M.U., Aligarh and G.S.V.M. Medical College, Kanpur ABSTRACT: Objectives :To predict the short-term prognostic significance of various clinical parameters at the time of admission in patients of stroke. Setting: Department of General Medicine, J.N. Medical College, A.M.U., Aligarh Participants : 100 patients of stroke (Cerebro-vascular accident) comprising 54 males and 46 females. Clinical Parameters : Admission Blood Pressure, Side of paralysis, Extent of Paralysis, Gastro-intestinal Haemorrhage, Level of consciousness at the time of admission. Statistical Analysis: ‘Z’ test (Z>_ 1.96). Results : The admission B.P. was raised in 75% of patients. The mortality was significantly high (57.1%) in the severe grade B.P. while recovery was significantly high (64.3%) in mild or moderate grade B.P patients. The left sided paralysis was having significantly high mortality of patients (49%) while recovery was significantly high (56.2%) in the patients with right sided paralysis. The paralysis with Grade O power was in 58% of stroke patients and was associated with signifi­cantly high (53.4%) mortality while 100% recovery was found in patients with power grade 4 and 5 at the time of admission. The G.l. haemorrhage was associated with 5% of patients but mortality was significantly high (100%) in these patients. The level of consciousness of grade / was highest (34%) while mortality was significantly high (100%) in the patients admitted with grade 3 level of consciousness. The recovery was significantly high (92.9%) in the patients admitted with grade 'O’ level of consciousnes

The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III

The third generation of the Sloan Digital Sky Survey (SDSS-III) took data from 2008 to 2014 using the original SDSS wide-field imager, the original and an upgraded multi-object fiber-fed optical spectrograph, a new near-infrared high-resolution spectrograph, and a novel optical interferometer. All of the data from SDSS-III are now made public. In particular, this paper describes Data Release 11 (DR11) including all data acquired through 2013 July, and Data Release 12 (DR12) adding data acquired through 2014 July (including all data included in previous data releases), marking the end of SDSS-III observing. Relative to our previous public release (DR10), DR12 adds one million new spectra of galaxies and quasars from the Baryon Oscillation Spectroscopic Survey (BOSS) over an additional 3000 deg^2 of sky, more than triples the number of H-band spectra of stars as part of the Apache Point Observatory (APO) Galactic Evolution Experiment (APOGEE), and includes repeated accurate radial velocity measurements of 5500 stars from the Multi-object APO Radial Velocity Exoplanet Large-area Survey (MARVELS). The APOGEE outputs now include the measured abundances of 15 different elements for each star. In total, SDSS-III added 5200 deg^2 of ugriz imaging; 155,520 spectra of 138,099 stars as part of the Sloan Exploration of Galactic Understanding and Evolution 2 (SEGUE-2) survey; 2,497,484 BOSS spectra of 1,372,737 galaxies, 294,512 quasars, and 247,216 stars over 9376 deg^2; 618,080 APOGEE spectra of 156,593 stars; and 197,040 MARVELS spectra of 5513 stars. Since its first light in 1998, SDSS has imaged over 1/3 of the Celestial sphere in five bands and obtained over five million astronomical spectra

Galaxy clustering in the DESI Legacy Survey and its imprint on the CMB

We use data from the DESI Legacy Survey imaging to probe the galaxy density field in tomographic slices covering the redshift range $0<z<0.8$. After careful consideration of completeness corrections and galactic cuts, we obtain a sample of $4.9\times 10^7$ galaxies covering 17 739 deg$^2$. We derive photometric redshifts with precision $\sigma_z/(1+z)=0.012 - 0.015$, and compare with alternative estimates. Cross-correlation of the tomographic galaxy maps with Planck maps of CMB temperature and lensing convergence probe the growth of structure since $z=0.8$. The signals are compared with a fiducial Planck $\Lambda$CDM model, and require an overall scaling in amplitude of $A_\kappa=0.901\pm 0.026$ for the lensing cross-correlation and $A_{\rm ISW} = 0.984 \pm 0.349$ for the temperature cross-correlation, interpreted as the Integrated Sachs-Wolfe effect. The ISW amplitude is consistent with the fiducial $\Lambda$CDM prediction, but lies significantly below the prediction of the AvERA model of R\'acz et al. (2017), which has been proposed as an alternative explanation for cosmic acceleration. Within $\Lambda$CDM, our low amplitude for the lensing cross-correlation requires a reduction either in fluctuation normalization or in matter density compared to the Planck results, so that $\Omega_m^{0.78}\sigma_8=0.297\pm 0.009$. In combination with the total amplitude of CMB lensing, this favours a shift mainly in density: $\Omega_m=0.274\pm0.024$. We discuss the consistency of this figure with alternative evidence. A conservative compromise between lensing and primary CMB constraints would require $\Omega_m=0.296\pm0.006$, where the 95% confidence regions of both probes overlap.Comment: 18 pages, 18 figures, revised to match the accepted version on MNRA

Multi-tracer extension of the halo model:probing quenching and conformity in eBOSS

We develop a new Multi-Tracer Halo Occupation Distribution (\texttt{MTHOD}) framework for the galaxy distribution and apply it to the extended Baryon Oscillation Spectroscopic Survey (eBOSS) final data between $z=0.7-1.1$. We obtain a best fit \mthod\, for each tracer and describe the host halo properties of these galaxies. The mean halo masses for LRGs, ELGs and QSOs are found to be 1.9 \times 10^{13} \msolaroh, 1.1 \times 10^{12} \msolaroh and 5 \times 10^{12} \msolaroh respectively in the eBOSS data. We use the \texttt{MTHOD} framework to create mock galaxy catalogues and predict auto- and cross-correlation functions for all the tracers. Comparing these results with data, we investigate galactic conformity, the phenomenon whereby the properties of neighbouring galaxies are mutually correlated in a manner that is not captured by the basic halo model. We detect \textsl{1-halo} conformity at more than 3$\sigma$ statistical significance, while obtaining upper limit on \textsl{2-halo} conformity. We also look at the environmental dependence of the galaxy quenching efficiency and find that halo mass driven quenching successfully explains the behaviour in high density regions, but it fails to describe the quenching efficiency in low density regions. In particular, we show that the quenching efficiency in low density filaments is higher in the observed data, as compared to the prediction of the \mthod\ with halo mass driven quenching. The mock galaxy catalogue constructed in this paper is publicly available on https://www.roe.ac.uk/~salam/MTHOD/ .Comment: 17 pages, 12 figures, the software and mock catalogue should be made available through: https://www.roe.ac.uk/~salam/MTHOD/ , Accepted for publication in MNRA

Using GAMA to probe the impact of small-scale galaxy physics on nonlinear redshift-space distortions

We present improved modelling of the redshift-space distortions of galaxy clustering that arise from peculiar velocities. We create mock galaxy catalogues in the framework of the halo model, using data from the Bolshoi project. These mock galaxy populations are inserted into the haloes with additional degrees of freedom that govern spatial and kinematical biases of the galaxy populations relative to the dark matter. We explore this generalised halo model with an MCMC algorithm, comparing the predictions to data from the Galaxy And Mass Assembly (GAMA) survey, and thus derive one of the first constraints on the detailed kinematic degrees of freedom for satellite galaxies within haloes. With this approach, the distortions of the redshift-space galaxy autocorrelations can be accounted for down to spatial separations close to 10 kpc, opening the prospect of improved RSD measurements of the perturbation growth rate by the inclusion of data from nonlinear scales.Comment: 19 pages, 10 figures, comments are welcom