RAS_WEB (Page 2,341)

Radial velocity map of solar wind transients in the field of view of STEREO/HI1 on 3 and 4 April 2010. (arXiv:2103.04740v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_X/0/1/0/all/0/1">Xiaolei Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Y/0/1/0/all/0/1">Yuming Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guo_J/0/1/0/all/0/1">Jingnan Guo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_R/0/1/0/all/0/1">Rui Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhuang_B/0/1/0/all/0/1">Bin Zhuang</a> The solar wind transients propagating out in the inner heliosphere can be observed in white-light images from Heliospheric Imager-1 (HI1), an instrument of the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) on board the Solar Terrestrial Relations Observatory (STEREO), from two perspectives. The spatial velocity distribution inside solar wind transients is key to understanding their dynamic evolution processes. We generated a velocity map of transients inRead More →

Packing fraction of clusters formed in free-falling granular streams based on flash X-ray radiography. (arXiv:2103.04017v2 [cond-mat.soft] UPDATED) <a href="http://arxiv.org/find/cond-mat/1/au:+Nagaashi_Y/0/1/0/all/0/1">Yuuya Nagaashi</a>, <a href="http://arxiv.org/find/cond-mat/1/au:+Nakamura_A/0/1/0/all/0/1">Akiko M. Nakamura</a>, <a href="http://arxiv.org/find/cond-mat/1/au:+Hasegawa_S/0/1/0/all/0/1">Sunao Hasegawa</a>, <a href="http://arxiv.org/find/cond-mat/1/au:+Wada_K/0/1/0/all/0/1">Koji Wada</a> We study the packing fraction of clusters in free-falling streams of spherical and irregularly shaped particles using flash X-ray radiography. The estimated packing fraction of clusters is low enough to correspond to coordination numbers less than 6. Such coordination numbers in numerical simulations correspond to aggregates that collide and grow without bouncing. Moreover, the streams of irregular particles evolved faster and formed clusters of larger sizes with lower packing fraction. This result on granular streamsRead More →

Quantitative estimates of impact induced crustal erosion during accretion and its influence on the Sm/Nd ratio of the Earth. (arXiv:2103.02571v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Allibert_L/0/1/0/all/0/1">Laetitia Allibert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charnoz_S/0/1/0/all/0/1">S&#xe9;bastien Charnoz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siebert_J/0/1/0/all/0/1">Julien Siebert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jacobson_S/0/1/0/all/0/1">Seth A. Jacobson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raymond_S/0/1/0/all/0/1">Sean N. Raymond</a> Dynamical scenarios of terrestrial planets formation involve strong perturbations of the inner part of the solar system by the giant-planets, leading to enhanced impact velocities and subsequent collisional erosion. We quantitatively estimate the effect of collisional erosion on the resulting composition of Earth, and estimate how it may provide information on the dynamical context of its formation. We simulate and quantify the erosion of Earth’s crustRead More →

Photometric and spectroscopic investigations of the Galactic field RRc candidates V764 Mon and HY Com. (arXiv:2103.02367v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Benko_J/0/1/0/all/0/1">Jozsef M. Benko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sodor_A/0/1/0/all/0/1">Adam Sodor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pal_A/0/1/0/all/0/1">Andras Pal</a> By analyzing photometric and spectroscopic time series in this paper, we show that the pulsator V764 Mon, assumed to be the brightest RR Lyrae star in the sky, is in fact a rapidly rotating delta Scuti star with an unusually long dominant period (P1=0.29 d). Our spectroscopy confirmed the discovery of the Gaia satellite about the binarity of V764 Mon. In the case of HY Com, a `bona fide’ RRc star, we present its first complete radialRead More →

A model independent approach to the study of $f(R)$ cosmologies with expansion histories close to $Lambda$CDM. (arXiv:2103.02274v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Chakraborty_S/0/1/0/all/0/1">Saikat Chakraborty</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+MacDevette_K/0/1/0/all/0/1">Kelly MacDevette</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Dunsby_P/0/1/0/all/0/1">Peter Dunsby</a> We propose a new framework for studying the cosmology of $f(R)$ gravity which completely avoids using the reconstruction programme. This allows us to easily obtain a qualitative feel of how much the $Lambda$CDM model differs from other $f(R)$ theories of gravity at the level of linear perturbation theory for theories that share the same background dynamics. This is achieved by using the standard model independent cosmographic parameters to develop a new dynamical system formulation of $f(R)$ gravityRead More →

A low-mass dark matter project, ALETHEIA: A Liquid hElium Time projection cHambEr In dArk matter. (arXiv:2103.02161v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Liao_J/0/1/0/all/0/1">Junhui Liao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gao_Y/0/1/0/all/0/1">Yuanning Gao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liang_Z/0/1/0/all/0/1">Zhuo Liang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peng_Z/0/1/0/all/0/1">Zhaohua Peng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_L/0/1/0/all/0/1">Lifeng Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_L/0/1/0/all/0/1">Lei Zhang</a> Dark Matter (DM) is one of the most critical questions to be understood and answered in fundamental physics today. Observations with varied astronomical and cosmological technologies already pinned down that DM exists in the Universe, the Milky Way, and the Solar System. However, the understanding of DM under the language of elementary physics is still in progress. DM direct detection aims to test the interactive cross-section between galactic DMRead More →

Probing non-Gaussianities with the high frequency tail of induced gravitational waves. (arXiv:2103.01056v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Atal_V/0/1/0/all/0/1">Vicente Atal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Domenech_G/0/1/0/all/0/1">Guillem Dom&#xe8;nech</a> We investigate in detail the spectrum of gravitational waves induced by a peaked primordial curvature power spectrum generated in single field inflationary models. We argue that the $f_{rm NL}$ parameter can be inferred by measuring the high frequency spectral tilt of the induced gravitational waves. We also show that the intrinsically non-Gaussian impact of $f_{rm NL}$ in $Omega_{rm GW}$ is to broaden its peak, although at a negligible level in order not to overproduce primordial black holes. We discuss possible degeneracies in the high frequencyRead More →

Small-scale Bright Blobs Ejected from a Sunspot Light Bridge. (arXiv:2102.13545v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_F/0/1/0/all/0/1">Fuyu Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yajie Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hou_Y/0/1/0/all/0/1">Yijun Hou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tian_H/0/1/0/all/0/1">Hui Tian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_X/0/1/0/all/0/1">Xianyong Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Song_Y/0/1/0/all/0/1">Yongliang Song</a> Light bridges (LBs) are bright lanes that divide an umbra into multiple parts in some sunspots. Persistent oscillatory bright fronts at a temperature of $sim$$10^5$ K are commonly observed above LBs in the 1400/1330 AA~passbands of the Interface Region Imaging Spectrograph (IRIS). Based on IRIS observations, we report small-scale bright blobs from the oscillating bright front above a light bridge. Some of these blobs reveal a clear acceleration, whereas the others do not. The averageRead More →

Significant H I and Metal Differences around the z = 0.83 Lens Galaxy Towards the Doubly Lensed Quasar SBS 0909+532. (arXiv:2102.13523v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Cashman_F/0/1/0/all/0/1">Frances H. Cashman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kulkarni_V/0/1/0/all/0/1">Varsha P. Kulkarni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_S/0/1/0/all/0/1">Sebastian Lopez</a> We report a large difference in neutral hydrogen (H I) and metal column densities between the two sight lines probing opposite sides of the lensing galaxy at $z_mathrm{lens}$ = 0.83 toward the doubly lensed quasar SBS 0909+532. Using archival HST-STIS and Keck HIRES spectra of the lensed quasar images, we measure log $N_mathrm{H;I}$ = 18.77 $pm$ 0.12 cm$^{-2}$ toward the brighter image ($A$) at an impact parameter of $r_A$ = 3.15Read More →

Connecting multi-lepton anomalies at the LHC and in Astrophysics and the prospects of MeerKAT/SKA. (arXiv:2102.10596v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Beck_G/0/1/0/all/0/1">Geoff Beck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_M/0/1/0/all/0/1">Mukesh Kumar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malwa_E/0/1/0/all/0/1">Elias Malwa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mellado_B/0/1/0/all/0/1">Bruce Mellado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Temo_R/0/1/0/all/0/1">Ralekete Temo</a> Multi-lepton anomalies at the Large Hadron Collider are reasonably well described by a two Higgs doublet model with an additional singlet scalar. Here, we demonstrate that using this model we are also able to describe the excesses in gamma-ray flux from the galactic centre and the cosmic-ray spectra from AMS-02. This is achieved through Dark Matter (DM) annihilation via the singlet scalar. Of great interest is the flux of synchrotron emissions which resultsRead More →

Impact of rotation on the evolution of convective vortices in collapsing stars. (arXiv:2012.06710v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Abdikamalov_E/0/1/0/all/0/1">E. Abdikamalov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foglizzo_T/0/1/0/all/0/1">T. Foglizzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mukazhanov_O/0/1/0/all/0/1">O. Mukazhanov</a> We study the impact of rotation on the hydrodynamic evolution of convective vortices during stellar collapse. Using linear hydrodynamics equations, we study the evolution of the vortices from their initial radii in convective shells down to smaller radii where they are expected to encounter the supernova shock. We find that the evolution of vortices is mainly governed by two effects: the acceleration of infall and the accompanying speed up of rotation. The former effect leads to the radial stretching of vortices,Read More →

The jet collimation profile at high resolution in BL Lacertae. (arXiv:2102.08952v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Casadio_C/0/1/0/all/0/1">C. Casadio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacDonald_N/0/1/0/all/0/1">N. R. MacDonald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boccardi_B/0/1/0/all/0/1">B. Boccardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jorstad_S/0/1/0/all/0/1">S. G. Jorstad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marscher_A/0/1/0/all/0/1">A. P. Marscher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krichbaum_T/0/1/0/all/0/1">T. P. Krichbaum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hodgson_J/0/1/0/all/0/1">J. A. Hodgson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_J/0/1/0/all/0/1">J-Y. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Traianou_E/0/1/0/all/0/1">E. Traianou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weaver_Z/0/1/0/all/0/1">Z. R. Weaver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garrido_M/0/1/0/all/0/1">M. G&#xf3;mez Garrido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_J/0/1/0/all/0/1">J. Gonz&#xe1;lez Garc&#xed;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kallunki_J/0/1/0/all/0/1">J. Kallunki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lindqvist_M/0/1/0/all/0/1">M. Lindqvist</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_S/0/1/0/all/0/1">S. S&#xe1;nchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_J/0/1/0/all/0/1">J. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zensus_J/0/1/0/all/0/1">J. A. Zensus</a> Controversial studies on the jet collimation profile of BL Lacertae (BL Lac), the eponymous blazar of BL Lac objects class, complicate the scenario in this already puzzling class of objects. Understanding theRead More →

The substructure of the Perseus star forming region: A survey with Gaia DR2. (arXiv:2102.08263v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Pavlidou_T/0/1/0/all/0/1">Tatiana Pavlidou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scholz_A/0/1/0/all/0/1">Aleks Scholz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Teixeira_P/0/1/0/all/0/1">Paula S. Teixeira</a> (University of St Andrews) We use photometric and kinematic data from Gaia DR2 to explore the structure of the star forming region associated with the molecular cloud of Perseus. Apart from the two well known clusters, IC 348 and NGC 1333, we present five new clustered groups of young stars, which contain between 30 and 300 members, named Autochthe, Alcaeus, Heleus, Electryon and Mestor. We demonstrate these are co-moving groups of young stars, based on how the candidate membersRead More →

Revealing Gravitational Collapse in Serpens G3-G6 Molecular Cloud using Velocity Gradients. (arXiv:2102.06225v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Hu_Y/0/1/0/all/0/1">Yue Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lazarian_A/0/1/0/all/0/1">A. Lazarian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stanimirovic_S/0/1/0/all/0/1">Snezana Stanimirovic</a> The relative role of turbulence, magnetic fields, self-gravity in star formation is a subject of intensive debate. We present IRAM 30m telescope observations of the $^{13}$CO (1-0) emission in the Serpens G3-G6 molecular cloud and apply to the data a set of statistical methods. Those include the probability density functions (PDFs) of column density and the Velocity Gradients Technique (VGT). We combine our data with the Planck 353 GHz polarized dust emission observations, Hershel H$_2$ column density. We suggest that the SerpensRead More →

Dissecting the Energy Budget of a Gamma-Ray Burst Fireball. (arXiv:2102.04968v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_B/0/1/0/all/0/1">Bing Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Y/0/1/0/all/0/1">Yu Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_L/0/1/0/all/0/1">Liang Li</a> The jet composition and radiative efficiency of GRBs are poorly constrained from the data. If the jet composition is matter-dominated (i.e. a fireball), the GRB prompt emission spectra would include a dominant thermal component originating from the fireball photosphere, and a non-thermal component presumably originating from internal shocks whose radii are greater than the photosphere radius. We propose a method to directly dissect the GRB fireball energy budget into three components and measure their values by combining the prompt emission and early afterglow data.Read More →

Efficient application of the Radiance Enhancement method for detection of the forest fires due to combustion-originated reflectance. (arXiv:2102.02136v2 [physics.ao-ph] UPDATED) <a href="http://arxiv.org/find/physics/1/au:+Siddiqui_R/0/1/0/all/0/1">Rehan Siddiqui</a>, <a href="http://arxiv.org/find/physics/1/au:+Jagpal_R/0/1/0/all/0/1">Rajinder K. Jagpal</a>, <a href="http://arxiv.org/find/physics/1/au:+Abrarov_S/0/1/0/all/0/1">Sanjar M. Abrarov</a>, <a href="http://arxiv.org/find/physics/1/au:+Quine_B/0/1/0/all/0/1">Brendan M. Quine</a> The existing methods detect the cloud scenes are applied at relatively small spectral range within shortwave upwelling radiative wavelength flux. We have reported a new method for detection of the cloud scenes based on the Radiance Enhancement (RE). This method can be used to cover a significantly wider spectral range from 1100 nm to 1700 nm (Siddiqui et al., 2015) by using datasets from the space-orbiting micro-spectrometer Argus 1000. DueRead More →

Strongly lensed cluster substructures are not in tension with $Lambda$CDM. (arXiv:2101.12112v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Bahe_Y/0/1/0/all/0/1">Yannick M. Bah&#xe9;</a> Strong gravitational lensing observations can test structure formation models by constraining the masses and concentrations of subhaloes in massive galaxy clusters. Recent work has concluded that cluster subhaloes are more abundant and/or concentrated than predicted by $Lambda$CDM simulations; this finding has been interpreted as arising from unidentified issues with simulations or an incorrect understanding of the nature of dark matter. We test these hypotheses by comparing observed subhalo masses and maximum circular velocities $v_mathrm{max}$ to predictions from the high resolution Hydrangea galaxy cluster simulation suite, which is basedRead More →

Jupiter as an Exoplanet: Insights from Cassini Phase Curves. (arXiv:2101.09984v3 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Heng_K/0/1/0/all/0/1">Kevin Heng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_L/0/1/0/all/0/1">Liming Li</a> Due to its proximity to Earth, Jupiter of the Solar System serves as a unique case study for gas-giant exoplanets. In the current study, we perform fits of ab initio, reflective, semi-infinite, homogeneous model atmospheres to 61 phase curves from 0.40 to 1.00 $mu$m, obtained from the Cassini spacecraft, within a Bayesian framework. We reproduce the previous finding that atmospheric models using classic reflection laws (Lambertian, Rayleigh, single Henyey-Greenstein) provide poor fits to the data. Using the double Henyey-Greenstein reflection law, we extract posterior distributions of theRead More →

Orbital evolution of binary black holes in active galactic nucleus disks: a disk channel for binary black hole mergers?. (arXiv:2101.09406v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Y/0/1/0/all/0/1">Ya-Ping Li</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Dempsey_A/0/1/0/all/0/1">Adam M. Dempsey</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_S/0/1/0/all/0/1">Shengtai Li</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">Hui Li</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_J/0/1/0/all/0/1">Jiaru Li</a> (1) ((1) LANL) We perform a series of high-resolution 2D hydrodynamical simulations of equal-mass binary black holes (BBHs) embedded in active galactic nucleus (AGN) accretion disks to study whether these binaries can be driven to merger by the surrounding gas. We find that the gravitational softening adopted for the BBH has a profound impact on this result. When the softening is less thanRead More →

Pushing automated morphological classifications to their limits with the Dark Energy Survey. (arXiv:2012.07858v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Vega_Ferrero_J/0/1/0/all/0/1">J. Vega-Ferrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_H/0/1/0/all/0/1">H. Dom&#xed;nguez S&#xe1;nchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardi_M/0/1/0/all/0/1">M. Bernardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huertas_Company_M/0/1/0/all/0/1">M. Huertas-Company</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morgan_R/0/1/0/all/0/1">R. Morgan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Margalef_B/0/1/0/all/0/1">B. Margalef</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguena_M/0/1/0/all/0/1">M. Aguena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allam_S/0/1/0/all/0/1">S. Allam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Annis_J/0/1/0/all/0/1">J. Annis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_S/0/1/0/all/0/1">S. Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bacon_D/0/1/0/all/0/1">D. Bacon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_E/0/1/0/all/0/1">E. Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">D. Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosell_A/0/1/0/all/0/1">A. Carnero Rosell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kind_M/0/1/0/all/0/1">M. Carrasco Kind</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">J. Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_A/0/1/0/all/0/1">A. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conselice_C/0/1/0/all/0/1">C. Conselice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costanzi_M/0/1/0/all/0/1">M. Costanzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_L/0/1/0/all/0/1">L. N. da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pereira_M/0/1/0/all/0/1">M. E. S. Pereira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vicente_J/0/1/0/all/0/1">J. De Vicente</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desai_S/0/1/0/all/0/1">S. Desai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrero_I/0/1/0/all/0/1">I. Ferrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fosalba_P/0/1/0/all/0/1">P. Fosalba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frieman_J/0/1/0/all/0/1">J. Frieman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Bellido_J/0/1/0/all/0/1">J. Garc&#xed;a-Bellido</a>, <aRead More →