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35 results on '"Zhao, G.-B."'

1. The Sloan Digital Sky Survey Quasar Catalog: Fourteenth Data Release

Author

Pâris, I., Petitjean, P., Aubourg, E., Myers, A. D., Streblyanska, A., Lyke, B. W., Anderson, S. F., Armengaud, E., Bautista, J., Blanton, M. R., Blomqvist, M., Brinkmann, J., Brownstein, J. R., Brandt, W. N., Burtin, E., Dawson, K., de la Torre, S., Georgakakis, A., Gil-Marin, H., Green, P. J., Hall, P. B., Kneib, J. -P., LaMassa, S. M., Goff, J. -M. Le, MacLeod, C., Mariappan, V., McGreer, I. D., Merloni, A., Noterdaeme, P., Delabrouille, N. Palanque, Percival, W. J., Ross, A. J., Rossi, G., Schneider, D. P., Seo, H. -J., Tojeiro, R., Weaver, B. A., Weijmans, A. -M., Yèche, C., Zarrouk, P., and Zhao, G. -B.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the Data Release 14 Quasar catalog (DR14Q) from the extended Baryon Oscillation Spectroscopic Survey (eBOSS) of the Sloan Digital Sky Survey IV (SDSS-IV). This catalog includes all SDSS-IV/eBOSS objects that were spectroscopically targeted as quasar candidates and that are confirmed as quasars via a new automated procedure combined with a partial visual inspection of spectra, have luminosities $M_{\rm i} \left[ z=2 \right] < -20.5$ (in a $\Lambda$CDM cosmology with $H_0 = 70 \ {\rm km \ s^{-1} \ Mpc ^{-1}}$, $\Omega_{\rm M} = 0.3$, and $\Omega_{\rm \Lambda} = 0.7$), and either display at least one emission line with a full width at half maximum (FWHM) larger than $500 \ {\rm km \ s^{-1}}$ or, if not, have interesting/complex absorption features. The catalog also includes previously spectroscopically-confirmed quasars from SDSS-I, II and III. The catalog contains 526,356 quasars 144,046 are new discoveries since the beginning of SDSS-IV) detected over 9,376 deg$^2$ (2,044 deg$^2$ having new spectroscopic data available) with robust identification and redshift measured by a combination of principal component eigenspectra. The catalog is estimated to have about 0.5% contamination. The catalog identifies 21,877 broad absorption line quasars and lists their characteristics. For each object, the catalog presents SDSS five-band CCD-based photometry with typical accuracy of 0.03 mag. The catalog also contains X-ray, ultraviolet, near-infrared, and radio emission properties of the quasars, when available, from other large-area surveys., Comment: Accepted for publication in A&A. The catalog is available at https://data.sdss.org/sas/dr14/eboss/qso/DR14Q/DR14Q_v4_4.fits

Published
2017
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2. The SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: final Emission Line Galaxy Target Selection

Author

Raichoor, A., Comparat, J., Delubac, T., Kneib, J. -P., Yèche, Ch., Dawson, K. S., Percival, W. J., Dey, A., Lang, D., Schlegel, D. J., Gorgoni, C., Bautista, J., Brownstein, J. R., Mariappan, V., Seo, H. -J., Tinker, J. L., Ross, A. J., Wang, Y., Zhao, G. -B., Moustakas, J., Palanque-Delabrouille, N., Jullo, E., Newmann, J. A., Prada, F., and Zhu, G. B.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We describe the algorithm used to select the Emission Line Galaxy (ELG) sample at $z \sim 0.85$ for the extended Baryon Oscillation Spectroscopic Survey of the Sloan Digital Sky Survey IV, using photometric data from the DECam Legacy Survey. Our selection is based on a selection box in the $g-r$ vs. $r-z$ colour-colour space and a cut on the $g$-band magnitude, to favour galaxies in the desired redshift range with strong [OII] emission. It provides a target density of 200 deg$^{-2}$ on the North Galactic Cap (NGC) and of 240 deg$^{-2}$ on the South Galactic Cap (SGC), where we use a larger selection box because of deeper imaging. We demonstrate that this selection passes the eBOSS requirements in terms of homogeneity. About 50,000 ELGs have been observed since the observations have started in 2016, September. These roughly match the expected redshift distribution, though the measured efficiency is slightly lower than expected. The efficiency can be increased by enlarging the redshift range and with incoming pipeline improvement. The cosmological forecast based on these first data predict $\sigma_{D_V}/D_V = 0.023$, in agreement with previous forecasts. Lastly, we present the stellar population properties of the ELG SGC sample. Once observations are completed, this sample will be suited to provide a cosmological analysis at $z \sim 0.85$, and will pave the way for the next decade of massive spectroscopic cosmological surveys, which heavily rely on ELGs. The target catalogue over the SGC will be released along with DR14., Comment: Submitted to MNRAS, 18 pages

Published
2017
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3. The Low Redshift survey at Calar Alto (LoRCA)

Author

Comparat, J., Chuang, C. -H., Rodriguez-Torres, S., Pellejero-Ibanez, M., Prada, F., Yepes, G., Courtois, H. M., Zhao, G. -B., Wang, Y., Sanchez, J., Maraston, C., Metcalf, R. Benton, Peiro-Perez, J., Kitaura, F. S., Perez, E., and Delgado, R. M. Gonzalez

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Baryon Acoustic Oscillation (BAO) feature in the power spectrum of galaxies provides a standard ruler to measure the accelerated expansion of the Universe. To extract all available information about dark energy, it is necessary to measure a standard ruler in the local, z<0.2, universe where dark energy dominates most the energy density of the Universe. Though the volume available in the local universe is limited, it is just big enough to measure accurately the long 100 Mpc/h wave-mode of the BAO. Using cosmological N-body simulations and approximate methods based on Lagrangian perturbation theory, we construct a suite of a thousand light-cones to evaluate the precision at which one can measure the BAO standard ruler in the local universe. We find that using the most massive galaxies on the full sky (34,000 sq. deg.), i.e. a K(2MASS)<14 magnitude-limited sample, one can measure the BAO scale up to a precision of 4\% and 1.2\% using reconstruction). We also find that such a survey would help to detect the dynamics of dark energy.Therefore, we propose a 3-year long observational project, named the Low Redshift survey at Calar Alto (LoRCA), to observe spectroscopically about 200,000 galaxies in the northern sky to contribute to the construction of aforementioned galaxy sample. The suite of light-cones is made available to the public., Comment: 15 pages. Accepted in MNRAS. Please visit our website: http://lorca-survey.ft.uam.es/

Published
2015
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4. Radio Continuum Surveys with Square Kilometre Array Pathfinders

Author

Norris, Ray P., Afonso, J., Bacon, D., Beck, Rainer, Bell, Martin, Beswick, R. J., Best, Philip, Bhatnagar, Sanjay, Bonafede, Annalisa, Brunetti, Gianfranco, Budavari, Tamas, Cassano, Rossella, Condo, J. J., Cress, Catherine, Dabbech, Arwa, Feain, I., Fender, Rob, Ferrari, Chiara, Gaensler, B. M., Giovannini, G., Haverkorn, Marijke, Heald, George, van der Heyden, Kurt, Hopkins, A. M., Jarvis, M., Johnston-Hollitt, Melanie, Kothes, Roland, van Langevelde, Huib, Lazio, Joseph, Mao, Minnie Y., Martınez-Sansigre, Alejo, Mary, David, McAlpine, Kim, Middelberg, E., Murphy, Eric, Padovani, P., Paragi, Zsolt, Prandoni, I., Raccanelli, A., Rigby, Emma, Roseboom, I. G., Rottgering, H., Sabater, Jose, Salvato, Mara, Scaife, Anna M. M., Schilizzi, Richard, Seymour, N., Smith, Dan J. B., Umana, Grazia, Zhao, G. -B., and Zinn, Peter-Christian

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

In the lead-up to the Square Kilometre Array (SKA) project, several next-generation radio telescopes and upgrades are already being built around the world. These include APERTIF (The Netherlands), ASKAP (Australia), eMERLIN (UK), VLA (USA), e-EVN (based in Europe), LOFAR (The Netherlands), Meerkat (South Africa), and the Murchison Widefield Array (MWA). Each of these new instruments has different strengths, and coordination of surveys between them can help maximise the science from each of them. A radio continuum survey is being planned on each of them with the primary science objective of understanding the formation and evolution of galaxies over cosmic time, and the cosmological parameters and large-scale structures which drive it. In pursuit of this objective, the different teams are developing a variety of new techniques, and refining existing ones. Here we describe these projects, their science goals, and the technical challenges which are being addressed to maximise the science return., Comment: Accepted by PASA, 22 October 2012

Published
2012
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5. EMU: Evolutionary Map of the Universe

Author

Norris, Ray P., Hopkins, A. M., Afonso, J., Brown, S., Condon, J. J., Dunne, L., Feain, I., Hollow, R., Jarvis, M., Johnston-Hollitt, M., Lenc, E., Middelberg, E., Padovani, P., Prandoni, I., Rudnick, L., Seymour, N., Umana, G., Andernach, H., Alexander, D. M., Appleton, P. N., Bacon, D., Banfield, J., Becker, W., Brown, M. J. I., Ciliegi, P., Jackson, C., Eales, S., Edge, A. C., Gaensler, B. M., Giovannini, G., Hales, C. A., Hancock, P., Huynh, M. Y., Ibar, E., Ivison, R. J., Kennicutt, R., Kimball, Amy E., Koekemoer, A. M., Koribalski, B. S., López-Sánchez, Á. R., Mao, M. Y., Murphy, T., Messias, H., Pimbblet, K. A., Raccanelli, A., Randall, K. E., Reiprich, T. H., Roseboom, I. G., Röttgering, H., Saikia, D. J., Sharp, R. G., Slee, O. B., Smail, Ian, Thompson, M. A., Urquhart, J. S., Wall, J. V., and Zhao, G. -B.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

EMU is a wide-field radio continuum survey planned for the new Australian Square Kilometre Array Pathfinder (ASKAP) telescope. The primary goal of EMU is to make a deep (rms ~ 10 microJy/beam) radio continuum survey of the entire Southern Sky at 1.3 GHz, extending as far North as +30 degrees declination, with a resolution of 10 arcsec. EMU is expected to detect and catalogue about 70 million galaxies, including typical star-forming galaxies up to z~1, powerful starbursts to even greater redshifts, and AGNs to the edge of the visible Universe. It will undoubtedly discover new classes of object. This paper defines the science goals and parameters of the survey, and describes the development of techniques necessary to maximise the science return from EMU., Comment: Accepted by PASA; see http://www.atnf.csiro.au/people/rnorris/papers/n252.pdf for higher-resolution figures

Published
2011
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6. The design of the Ali CMB Polarization Telescope receiver

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Salatino, M., Austermann, J., Thompson, K. L., Ade, P. A. R., Bai, X., Beall, J. A., Becker, D. T., Cai, Y., Chang, Z., Chen, D., Connors, J., Chen, P., Dober, B., Delabrouille, J., Duff, S. M., Gao, G., Givhan, R. C., Ghosh, S., Hilton, G., Hu, B., Hubmayr, J., Karpel, E., Kuo, C.-L., Li, H., Li, M., Li, S.-Y., Li, X., Link, M., Li, Y., Liu, H., Liu, L., Liu, Y., Lu, F., Lukas, T., Lu, X., Mates, J. A. B., Mathewson, J., Mauskopf, P., Meinke, J., Montana-Lopez, J., Moore, J., Shi, J., Sinclair, A. K., Stephenson, R., Sun, W., Tseng, Y.‐H., Tucker, C., Ullom, J., Vale, L., van Lanen, J., Vissers, M., Walker, S., Wang, B., Wang, G., Wang, J., Weeks, E., Wu, Di, Wu, Y.-H., Xia, J., Xu, H., Yao, J., Yao, Y., Yoon, K. W., Yue, B., Zhai, H., Zhang, A., Zhang, Laiyu, Zhang, Le, Zhang, P., Zhang, T., Zhang, Xinmin, Zhang, Yifei, Zhang, Yongjie, Zhao, G.-B., and Zhao, W.

Published
2020
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7. The SDSS-IV extended Baryon Oscillation Spectroscopic Survey: final emission line galaxy target selection

Author

Raichoor, A., primary, Comparat, J., additional, Delubac, T., additional, Kneib, J.-P., additional, Yèche, Ch, additional, Dawson, K. S., additional, Percival, W. J., additional, Dey, A., additional, Lang, D., additional, Schlegel, D. J., additional, Gorgoni, C., additional, Bautista, J., additional, Brownstein, J. R., additional, Mariappan, V., additional, Seo, H.-J., additional, Tinker, J. L., additional, Ross, A. J., additional, Wang, Y., additional, Zhao, G.-B., additional, Moustakas, J., additional, Palanque-Delabrouille, N., additional, Jullo, E., additional, Newmann, J. A., additional, Prada, F., additional, and Zhu, G. B., additional

Published
2017
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9. The Low Redshift survey at Calar Alto (LoRCA)

Author

Comparat, J., primary, Chuang, C.-H., additional, Rodríguez-Torres, S., additional, Pellejero-Ibanez, M., additional, Prada, F., additional, Yepes, G., additional, Courtois, H. M., additional, Zhao, G.-B., additional, Wang, Y., additional, Sanchez, J., additional, Maraston, C., additional, Metcalf, R. Benton, additional, Peiro-Perez, J., additional, Kitaura, F. S., additional, Pérez, E., additional, and González Delgado, R. M., additional

Published
2016
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10. Jagged2 promotes cancer stem cell properties of triple negative breast cancer cells and paclitaxel resistance via regulating microRNA-200.

Author

LI, C. Y., MIAO, K. L., LIU, L. Y., ZHAO, G. B., JIANG, C., CHEN, Y., and LIN, M. H.

Abstract

OBJECTIVE: To investigate the role of Jagged2 in triple negative breast cancer (TNBC) and its underlying mechanism. PATIENTS AND METHODS: Breast cancer tissues of patients diagnosed with TNBC in Fujian Medical University Affiliated MinDong Hospital from January 2015 to September 2017 were selected. TNBC patients were divided into the paclitaxel-resistant group (n=34) and non-resistance group (n=11). Jagged2 expression in paclitaxel-resistant group and non-resistance group before and after treatment was detected by quantitative Real-time-polymerase chain reaction (qRT-PCR), respectively. After Jagged2 knockdown in paclitaxel-resistant MDAMB- 231 cells (MDA-MB-231/TXR), expression of CD44+CD24-ESA+ subset was detected by flow cytometry. MicroRNA-200 expression was detected after Jagged2 knockdown in MDAMB- 231/TXR cells. RESULTS: Jagged2 was highly expressed in paclitaxel-resistant TNBC tissues and cells. Jagged2 expression was found to be associated with cancer stem cell (CSC) properties of TNBC cells. Knockdown of Jagged2 inhibited CSC properties and paclitaxel resistance, whereas upregulated microRNA-200 expression. The inhibited CSC properties and paclitaxel resistance induced by Jagged2 knockdown were reversed by microRNA-200 knockdown. CONCLUSIONS: Jagged2 maintains CSC properties of TNBC cells and paclitaxel resistance via regulating microRNA-200. [ABSTRACT FROM AUTHOR]

Published
2018

11. The Clustering of Galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: Testing Deviations from \u039b and General Relativity using anisotropic clustering of galaxies

Author

Samushia, L., Reid, B. A., White, M., Percival, W. J., Cuesta, A. J., Lombriser, L., Manera, M., Nichol, R. C., Schneider, D. P., Bizyaev, D., Brewington, H., Malanushenko, E., Malanushenko, V., Oravetz, D., Pan, K., Simmons, A., Shelden, A., Snedden, S., Tinker, J. L., Weaver, B. A., York, D. G., and Zhao, G.-B.

Published
2012
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12. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : measurements of the growth of structure and expansion rate at z = 0.57 from anisotropic clustering

Author

Reid, B. A., Samushia, L., White, M., Percival, W. J., Manera, M., Padmanabhan, N., Ross, A. J., Sánchez, A. G., Bailey, S., Bizyaev, D., Bolton, A. S., Brewington, H., Brinkmann, J., Brownstein, J. R., Cuesta, A. J., Eisenstein, D. J., Gunn, J. E., Honscheid, K., Malanushenko, E., Malanushenko, V., Maraston, C., McBride, C. K., Muna, D., Nichol, R. C., Oravetz, D., Pan, K., de Putter, R., Roe, N. A., Ross, N. P., Schlegel, D. J., Schneider, D. P., Seo, H.-J., Shelden, A., Sheldon, E. S., Simmons, A., Skibba, R. A., Snedden, S., Swanson, M. E. C., Thomas, D., Tinker, J., Tojeiro, R., Verde, L., Wake, D. A., Weaver, B. A., Weinberg, D. H., Zehavi, I., Zhao, G.-B., and University of St Andrews. School of Physics and Astronomy

Subjects
QC Physics, haloes [Galaxies], statistics [Galaxies], Cosmological parameters, QB Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Large-scale structure of the Universe, Astrophysics::Galaxy Astrophysics, QC, QB
Abstract

We analyse the anisotropic clustering of massive galaxies from the Sloan Digital Sky Survey III Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) sample, which consists of 264 283 galaxies in the redshift range 0.43 < z < 0.7 spanning 3275 deg2. Both peculiar velocities and errors in the assumed redshift–distance relation (‘Alcock–Paczynski effect’) generate correlations between clustering amplitude and orientation with respect to the line of sight. Together with the sharp baryon acoustic oscillation (BAO) standard ruler, our measurements of the broad-band shape of the monopole and quadrupole correlation functions simultaneously constrain the comoving angular diameter distance (2190 ± 61 Mpc) to z = 0.57, the Hubble expansion rate at z = 0.57 (92.4 ± 4.5 km s−1 Mpc−1) and the growth rate of structure at that same redshift (dσ8/d ln a = 0.43 ± 0.069). Our analysis provides the best current direct determination of both DA and H in galaxy clustering data using this technique. If we further assume a Λcold dark matter expansion history, our growth constraint tightens to dσ8/d ln a = 0.415 ± 0.034. In combination with the cosmic microwave background, our measurements of DA, H and dσ8/d ln a all separately require dark energy at z > 0.57, and when combined imply ΩΛ = 0.74 ± 0.016, independent of the Universe's evolution at z < 0.57. All of these constraints assume scale-independent linear growth, and assume general relativity to compute both 퓞 (10 per cent) non-linear model corrections and our errors. In our companion paper, Samushia et al., we explore further cosmological implications of these observations. Publisher PDF

Published
2012

13. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Analysis of potential systematics

Author

Ross, A. J., Percival, W. J., Sánchez, A. G., Samushia, L., Ho, S., Kazin, E., Manera, M., Reid, B., White, M., Tojeiro, R., McBride, C. K., Xu, X., Wake, D. A., Strauss, M. A., Montesano, F., Swanson, M. E. C., Bailey, S., Bolton, A. S., Dorta, A. M., Eisenstein, D. J., Guo, H., Hamilton, J.-C., Nichol, R. C., Padmanabhan, N., Prada, F., Schlegel, D. J., Magaña, M. V., Zehavi, I., Blanton, M., Bizyaev, D., Brewington, H., Cuesta, A. J., Malanushenko, E., Malanushenko, V., Oravetz, D., Parejko, J., Pan, K., Schneider, D. P., Shelden, A., Simmons, A., Snedden, S., Zhao, G.-b., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), SDSS-III, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and University of St Andrews. School of Physics and Astronomy

Subjects
Cosmology and Gravitation, Distance scale, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology and Extragalactic Astrophysics, Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], QC Physics, QB Astronomy, observations [Cosmology], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], QC, Astrophysics::Galaxy Astrophysics, QB, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We analyze the density field of galaxies observed by the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS) included in the SDSS Data Release Nine (DR9). DR9 includes spectroscopic redshifts for over 400,000 galaxies spread over a footprint of 3,275 deg^2. We identify, characterize, and mitigate the impact of sources of systematic uncertainty on large-scale clustering measurements, both for angular moments of the redshift-space correlation function and the spherically averaged power spectrum, P(k), in order to ensure that robust cosmological constraints will be obtained from these data. A correlation between the projected density of stars and the higher redshift (0.43 < z < 0.7) galaxy sample (the `CMASS' sample) due to imaging systematics imparts a systematic error that is larger than the statistical error of the clustering measurements at scales s > 120h^-1Mpc or k < 0.01hMpc^-1. We find that these errors can be ameliorated by weighting galaxies based on their surface brightness and the local stellar density. We use mock galaxy catalogs that simulate the CMASS selection function to determine that randomly selecting galaxy redshifts in order to simulate the radial selection function of a random sample imparts the least systematic error on correlation function measurements and that this systematic error is negligible for the spherically averaged correlation function. The methods we recommend for the calculation of clustering measurements using the CMASS sample are adopted in companion papers that locate the position of the baryon acoustic oscillation feature (Anderson et al. 2012), constrain cosmological models using the full shape of the correlation function (Sanchez et al. 2012), and measure the rate of structure growth (Reid et al. 2012). (abridged), Matches version accepted by MNRAS. Clarifications and references have been added. See companion papers that share the "The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey:" title

Published
2012

14. Radio Continuum Surveys with Square Kilometre Array Pathfinders

Author

Norris, Ray P., primary, Afonso, J., additional, Bacon, D., additional, Beck, Rainer, additional, Bell, Martin, additional, Beswick, R. J., additional, Best, Philip, additional, Bhatnagar, Sanjay, additional, Bonafede, Annalisa, additional, Brunetti, Gianfranco, additional, Budavári, Tamás, additional, Cassano, Rossella, additional, Condon, J. J., additional, Cress, Catherine, additional, Dabbech, Arwa, additional, Feain, I., additional, Fender, Rob, additional, Ferrari, Chiara, additional, Gaensler, B. M., additional, Giovannini, G., additional, Haverkorn, Marijke, additional, Heald, George, additional, Van der Heyden, Kurt, additional, Hopkins, A. M., additional, Jarvis, M., additional, Johnston-Hollitt, Melanie, additional, Kothes, Roland, additional, Van Langevelde, Huib, additional, Lazio, Joseph, additional, Mao, Minnie Y., additional, Martínez-Sansigre, Alejo, additional, Mary, David, additional, Mcalpine, Kim, additional, Middelberg, E., additional, Murphy, Eric, additional, Padovani, P., additional, Paragi, Zsolt, additional, Prandoni, I., additional, Raccanelli, A., additional, Rigby, Emma, additional, Roseboom, I. G., additional, Röttgering, H., additional, Sabater, Jose, additional, Salvato, Mara, additional, Scaife, Anna M. M., additional, Schilizzi, Richard, additional, Seymour, N., additional, Smith, Dan J. B., additional, Umana, Grazia, additional, Zhao, G.-B., additional, and Zinn, Peter-Christian, additional

Published
2013
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15. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Data Release 9 spectroscopic galaxy sample

Author

Anderson, L., primary, Aubourg, E., additional, Bailey, S., additional, Bizyaev, D., additional, Blanton, M., additional, Bolton, A. S., additional, Brinkmann, J., additional, Brownstein, J. R., additional, Burden, A., additional, Cuesta, A. J., additional, da Costa, L. A. N., additional, Dawson, K. S., additional, de Putter, R., additional, Eisenstein, D. J., additional, Gunn, J. E., additional, Guo, H., additional, Hamilton, J.-C., additional, Harding, P., additional, Ho, S., additional, Honscheid, K., additional, Kazin, E., additional, Kirkby, D., additional, Kneib, J.-P., additional, Labatie, A., additional, Loomis, C., additional, Lupton, R. H., additional, Malanushenko, E., additional, Malanushenko, V., additional, Mandelbaum, R., additional, Manera, M., additional, Maraston, C., additional, McBride, C. K., additional, Mehta, K. T., additional, Mena, O., additional, Montesano, F., additional, Muna, D., additional, Nichol, R. C., additional, Nuza, S. E., additional, Olmstead, M. D., additional, Oravetz, D., additional, Padmanabhan, N., additional, Palanque-Delabrouille, N., additional, Pan, K., additional, Parejko, J., additional, Paris, I., additional, Percival, W. J., additional, Petitjean, P., additional, Prada, F., additional, Reid, B., additional, Roe, N. A., additional, Ross, A. J., additional, Ross, N. P., additional, Samushia, L., additional, Sanchez, A. G., additional, Schlegel, D. J., additional, Schneider, D. P., additional, Scoccola, C. G., additional, Seo, H.-J., additional, Sheldon, E. S., additional, Simmons, A., additional, Skibba, R. A., additional, Strauss, M. A., additional, Swanson, M. E. C., additional, Thomas, D., additional, Tinker, J. L., additional, Tojeiro, R., additional, Magana, M. V., additional, Verde, L., additional, Wagner, C., additional, Wake, D. A., additional, Weaver, B. A., additional, Weinberg, D. H., additional, White, M., additional, Xu, X., additional, Yeche, C., additional, Zehavi, I., additional, and Zhao, G.-B., additional

Published
2012
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17. EMU: Evolutionary Map of the Universe

Author

Norris, Ray P., primary, Hopkins, A. M., additional, Afonso, J., additional, Brown, S., additional, Condon, J. J., additional, Dunne, L., additional, Feain, I., additional, Hollow, R., additional, Jarvis, M., additional, Johnston-Hollitt, M., additional, Lenc, E., additional, Middelberg, E., additional, Padovani, P., additional, Prandoni, I., additional, Rudnick, L., additional, Seymour, N., additional, Umana, G., additional, Andernach, H., additional, Alexander, D. M., additional, Appleton, P. N., additional, Bacon, D., additional, Banfield, J., additional, Becker, W., additional, Brown, M. J. I., additional, Ciliegi, P., additional, Jackson, C., additional, Eales, S., additional, Edge, A. C., additional, Gaensler, B. M., additional, Giovannini, G., additional, Hales, C. A., additional, Hancock, P., additional, Huynh, M. T., additional, Ibar, E., additional, Ivison, R. J., additional, Kennicutt, R., additional, Kimball, Amy E., additional, Koekemoer, A. M., additional, Koribalski, B. S., additional, López-Sánchez, Á. R., additional, Mao, M. Y., additional, Murphy, T., additional, Messias, H., additional, Pimbblet, K. A., additional, Raccanelli, A., additional, Randall, K. E., additional, Reiprich, T. H., additional, Roseboom, I. G., additional, Röttgering, H., additional, Saikia, D. J., additional, Sharp, R. G., additional, Slee, O. B., additional, Smail, Ian, additional, Thompson, M. A., additional, Urquhart, J. S., additional, Wall, J. V., additional, and Zhao, G.-B., additional

Published
2011
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19. Effect of CO<INF>2</INF> on Nonthermal-Plasma Reactions of Nitrogen Oxides in N<INF>2</INF>. 2. Percent-Level Concentrations

Author

Zhao, G.-B., Hu, X., Argyle, M. D., and Radosz, M.

Abstract

Both NOx conversion and CO2 conversion decrease with increasing percent-level CO2 concentration in nonthermal nitrogen plasma. The rate constants of electron collision reactions of both N2 and CO2 decrease with increasing CO2 concentration because electronegative CO2 reduces electron concentrations in the reactor due to the electron attachment process. The rate constant of CO2 dissociation through electron collision is 1−2 orders of magnitude higher than that of N2 dissociation because of low dissociation energy of CO2. Model data for reactor outlet NOx and COx concentrations agree well with experimental data. The effect of CO2 on NO, NO2, N2O, and CO concentrations can be explained on the basis of the proposed reaction mechanism and kinetic modeling.

Published
2005

20. Effect of CO<INF>2</INF> on Nonthermal-Plasma Reactions of Nitrogen Oxides in N<INF>2</INF>. 1. PPM-Level Concentrations

Author

Zhao, G.-B., Hu, X., Argyle, M. D., and Radosz, M.

Abstract

PPM-level concentrations of CO2 are added to NO/N2 mixtures to determine the effect of CO2 on plasma generation and to investigate the mechanism of CO2 reactions. Addition of 599.9 ppm CO2 does not affect the electric discharge in NOx in N2 nonthermal plasma. However, CO2 slightly dissociates, with CO2 conversion reaching a maximum of about 5.5% at the power input at which NO conversion ceases. NO(A), the first-excited electronic state of NO, is detected by corona-induced optical emission and is found to contribute to CO2 dissociation. A kinetic model including 38 reactions is required to adequately model decomposition of NOx and CO2 in the presence of CO2. About 18% of the NO(A) that is formed reacts with CO2 to form NO, CO, and O.

Published
2005

21. Nonthermal-Plasma Reactions of Dilute Nitrogen Oxide Mixtures:  NO<INF>x</INF><INF></INF>-in-Argon and NO<INF>x</INF><INF></INF> + CO-in-Argon

Author

Hu, X., Zhao, G.-B., Zhang, J.-J., Wang, L., and Radosz, M.

Abstract

Analysis of conversion mechanisms for NO and N2O in Ar plasma suggests that NO is converted through the reaction Ar+ + NO + e- → Ar + N + O, whereas N2O is converted through the reaction Ar+ + N2O + e- → Ar + N2 + O. A time-averaged lumped model developed on the basis of this analysis matches the experimental data. CO inhibits N2O conversion but not NO conversion. However, parts-per-million levels of CO affect neither N2O nor NO conversion. Compared to N2 plasma, which produces a weak streamer glow discharge and a small temperature increase along the reactor, Ar plasma produces a strong streamer discharge and a small temperature decrease along the reactor.

Published
2004

22. N Atom Radicals and N<INF>2</INF>(A<SUP>3</SUP>∑<INF>u</INF><SUP>+</SUP>) Found To Be Responsible for Nitrogen Oxides Conversion in Nonthermal Nitrogen Plasma

Author

Zhao, G.-B., Hu, X., Argyle, M. D., and Radosz, M.

Abstract

All species that are likely to be responsible for nitrogen oxides (N2O, NO, and NO2) conversion in nitrogen plasma are analyzed in detail through carefully designed systematic experiments and theoretical analysis. The effect of ppm-level CO2, CO, and 1% CO on N2O conversion reveals that the N2O conversion occurs mainly by interaction with N2(A3∑u+) excited species. The effect of 1% CO on the NO conversion suggests that only N atom radicals are predominantly involved in NO conversion. NO2 conversion, on the other hand, occurs by interaction with both N2(A3∑u+) and N atom radicals. Therefore, only two active species, N2(A3∑u+) and N atom radicals, are found to be responsible for nitrogen oxides conversion in nitrogen plasma.

Published
2004

23. Nonthermal Plasma Reactions of Dilute Nitrogen Oxide Mixtures:  NO<INF>x</INF><INF></INF> in Nitrogen

Author

Zhao, G.-B., Hu, X., Yeung, M.-C., Plumb, O. A., and Radosz, M.

Abstract

A lumped kinetic model of a pulsed corona discharge reactor, where the high-voltage discharge-induced electron density fluctuation and hence the electron collision rate fluctuation are approximated with a uniform electron distribution and a new Arrhenius-type rate model, is found to capture the effect of power input, NOx composition, and residence time. An N atom and N2(A) are found to control the conversion of nitrogen oxides and the evolution of byproducts; the N atom controls the NO conversion, N2(A) controls the N2O conversion, and the N atom and N2(A) control the NO2 conversion.

Published
2004

25. The Sloan Digital Sky Survey Quasar Catalog: Fourteenth Data Release

Author

Pâris, I., Petitjean, P., Aubourg, E., Myers, A. D., Streblyanska, A., Lyke, B. W., Anderson, S. F., Armengaud, E., Bautista, J., Blanton, M. R., Brinkmann, J., Brownstein, J. R., Brandt, W. N., Burtin, E., Dawson, K., La Torre, S., Georgakakis, A., Gil-Marin, H., Green, P. J., Hall, P. B., Kneib, J. -P, Lamassa, S. M., Le Goff, J. -M, Macleod, C., Mariappan, V., Mcgreer, I. D., Merloni, A., Noterdaeme, P., Palanque Delabrouille, N., Percival, W. J., Ross, A. J., Rossi, G., Schneider, D. P., Seo, H. -J, Tojeiro, R., Weaver, B. A., Anne-Marie Weijmans, Yèche, C., Zarrouk, P., Zhao, G. -B, Laboratoire d'Astrophysique de Marseille ( LAM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Aix Marseille Université ( AMU ) -Centre National d'Etudes Spatiales ( CNES ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), and SDSS

Subjects
surveys, quasars: general, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, catalogs
Abstract

International audience; We present the data release 14 Quasar catalog (DR14Q) from the extended Baryon Oscillation Spectroscopic Survey (eBOSS) of the Sloan Digital Sky Survey IV (SDSS-IV). This catalog includes all SDSS-IV/eBOSS objects that were spectroscopically targeted as quasar candidates and that are confirmed as quasars via a new automated procedure combined with a partial visual inspection of spectra, have luminosities Mi [z = 2] < −20.5 (in a Λ CDM cosmology with H0 = 70 km s−1 Mpc−1, Ω M =0.3, and Ω Λ = 0.7), and either display at least one emission line with a full width at half maximum larger than 500 km s−1 or, if not, have interesting/complex absorption features. The catalog also includes previously spectroscopically-confirmed quasars from SDSS-I, II, and III. The catalog contains 526 356 quasars (144 046 are new discoveries since the beginning of SDSS-IV) detected over 9376 deg2 (2044 deg2 having new spectroscopic data available) with robust identification and redshift measured by a combination of principal component eigenspectra. The catalog is estimated to have about 0.5% contamination. Redshifts are provided for the Mg II emission line. The catalog identifies 21 877 broad absorption line quasars and lists their characteristics. For each object, the catalog presents five-band (u, g, r, i, z) CCD-based photometry with typical accuracy of 0.03 mag. The catalog also contains X-ray, ultraviolet, near-infrared, and radio emission properties of the quasars, when available, from other large-area surveys. The calibrated digital spectra, covering the wavelength region 3610–10 140 Å at a spectral resolution in the range 1300 < R < 2500, can be retrieved from the SDSS Science Archiver Server.Key words: catalogs / surveys / quasars: general★ http://www.sdss.org/dr14/algorithms/qso_catalog

29. Cosmology intertwined: A review of the particle physics, astrophysics, and cosmology associated with the cosmological tensions and anomalies

Author

Elcio Abdalla, Guillermo Franco Abellán, Amin Aboubrahim, Adriano Agnello, Özgür Akarsu, Yashar Akrami, George Alestas, Daniel Aloni, Luca Amendola, Luis A. Anchordoqui, Richard I. Anderson, Nikki Arendse, Marika Asgari, Mario Ballardini, Vernon Barger, Spyros Basilakos, Ronaldo C. Batista, Elia S. Battistelli, Richard Battye, Micol Benetti, David Benisty, Asher Berlin, Paolo de Bernardis, Emanuele Berti, Bohdan Bidenko, Simon Birrer, John P. Blakeslee, Kimberly K. Boddy, Clecio R. Bom, Alexander Bonilla, Nicola Borghi, François R. Bouchet, Matteo Braglia, Thomas Buchert, Elizabeth Buckley-Geer, Erminia Calabrese, Robert R. Caldwell, David Camarena, Salvatore Capozziello, Stefano Casertano, Geoff C.-F. Chen, Jens Chluba, Angela Chen, Hsin-Yu Chen, Anton Chudaykin, Michele Cicoli, Craig J. Copi, Fred Courbin, Francis-Yan Cyr-Racine, Bożena Czerny, Maria Dainotti, Guido D'Amico, Anne-Christine Davis, Javier de Cruz Pérez, Jaume de Haro, Jacques Delabrouille, Peter B. Denton, Suhail Dhawan, Keith R. Dienes, Eleonora Di Valentino, Pu Du, Dominique Eckert, Celia Escamilla-Rivera, Agnès Ferté, Fabio Finelli, Pablo Fosalba, Wendy L. Freedman, Noemi Frusciante, Enrique Gaztañaga, William Giarè, Elena Giusarma, Adrià Gómez-Valent, Will Handley, Ian Harrison, Luke Hart, Dhiraj Kumar Hazra, Alan Heavens, Asta Heinesen, Hendrik Hildebrandt, J. Colin Hill, Natalie B. Hogg, Daniel E. Holz, Deanna C. Hooper, Nikoo Hosseininejad, Dragan Huterer, Mustapha Ishak, Mikhail M. Ivanov, Andrew H. Jaffe, In Sung Jang, Karsten Jedamzik, Raul Jimenez, Melissa Joseph, Shahab Joudaki, Marc Kamionkowski, Tanvi Karwal, Lavrentios Kazantzidis, Ryan E. Keeley, Michael Klasen, Eiichiro Komatsu, Léon V.E. Koopmans, Suresh Kumar, Luca Lamagna, Ruth Lazkoz, Chung-Chi Lee, Julien Lesgourgues, Jackson Levi Said, Tiffany R. Lewis, Benjamin L'Huillier, Matteo Lucca, Roy Maartens, Lucas M. Macri, Danny Marfatia, Valerio Marra, Carlos J.A.P. Martins, Silvia Masi, Sabino Matarrese, Arindam Mazumdar, Alessandro Melchiorri, Olga Mena, Laura Mersini-Houghton, James Mertens, Dinko Milaković, Yuto Minami, Vivian Miranda, Cristian Moreno-Pulido, Michele Moresco, David F. Mota, Emil Mottola, Simone Mozzon, Jessica Muir, Ankan Mukherjee, Suvodip Mukherjee, Pavel Naselsky, Pran Nath, Savvas Nesseris, Florian Niedermann, Alessio Notari, Rafael C. Nunes, Eoin Ó Colgáin, Kayla A. Owens, Emre Özülker, Francesco Pace, Andronikos Paliathanasis, Antonella Palmese, Supriya Pan, Daniela Paoletti, Santiago E. Perez Bergliaffa, Leandros Perivolaropoulos, Dominic W. Pesce, Valeria Pettorino, Oliver H.E. Philcox, Levon Pogosian, Vivian Poulin, Gaspard Poulot, Marco Raveri, Mark J. Reid, Fabrizio Renzi, Adam G. Riess, Vivian I. Sabla, Paolo Salucci, Vincenzo Salzano, Emmanuel N. Saridakis, Bangalore S. Sathyaprakash, Martin Schmaltz, Nils Schöneberg, Dan Scolnic, Anjan A. Sen, Neelima Sehgal, Arman Shafieloo, M.M. Sheikh-Jabbari, Joseph Silk, Alessandra Silvestri, Foteini Skara, Martin S. Sloth, Marcelle Soares-Santos, Joan Solà Peracaula, Yu-Yang Songsheng, Jorge F. Soriano, Denitsa Staicova, Glenn D. Starkman, István Szapudi, Elsa M. Teixeira, Brooks Thomas, Tommaso Treu, Emery Trott, Carsten van de Bruck, J. Alberto Vazquez, Licia Verde, Luca Visinelli, Deng Wang, Jian-Min Wang, Shao-Jiang Wang, Richard Watkins, Scott Watson, John K. Webb, Neal Weiner, Amanda Weltman, Samuel J. Witte, Radosław Wojtak, Anil Kumar Yadav, Weiqiang Yang, Gong-Bo Zhao, Miguel Zumalacárregui, Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre Pierre Binétruy (CPB), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Helsinki Institute of Physics, Universitat Politècnica de Catalunya. Departament de Matemàtiques, Universitat Politècnica de Catalunya. EDP - Equacions en Derivades Parcials i Aplicacions, European Commission, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Eusko Jaurlaritza, Generalitat Valenciana, Generalitat de Catalunya, Abdalla, Elcio, Abellán, Guillermo Franco, Aboubrahim, Amin, Agnello, Adriano, Akarsu, Özgür, Akrami, Yashar, Alestas, George, Aloni, Daniel, Amendola, Luca, Anchordoqui, Luis A., Anderson, Richard I., Arendse, Nikki, Asgari, Marika, Ballardini, Mario, Barger, Vernon, Basilakos, Spyro, Batista, Ronaldo C., Battistelli, Elia S., Battye, Richard, Benetti, Micol, Benisty, David, Berlin, Asher, de Bernardis, Paolo, Berti, Emanuele, Bidenko, Bohdan, Birrer, Simon, Blakeslee, John P., Boddy, Kimberly K., Bom, Clecio R., Bonilla, Alexander, Borghi, Nicola, Bouchet, François R., Braglia, Matteo, Buchert, Thoma, Buckley-Geer, Elizabeth, Calabrese, Erminia, Caldwell, Robert R., Camarena, David, Capozziello, Salvatore, Casertano, Stefano, Chen, Geoff C. -F., Chluba, Jen, Chen, Angela, Chen, Hsin-Yu, Chudaykin, Anton, Cicoli, Michele, Copi, Craig J., Courbin, Fred, Cyr-Racine, Francis-Yan, Czerny, Bożena, Dainotti, Maria, D'Amico, Guido, Davis, Anne-Christine, de Cruz Pérez, Javier, de Haro, Jaume, Delabrouille, Jacque, Denton, Peter B., Dhawan, Suhail, Dienes, Keith R., Di Valentino, Eleonora, Du, Pu, Eckert, Dominique, Escamilla-Rivera, Celia, Ferté, Agnè, Finelli, Fabio, Fosalba, Pablo, Freedman, Wendy L., Frusciante, Noemi, Gaztañaga, Enrique, Giarè, William, Giusarma, Elena, Gómez-Valent, Adrià, Handley, Will, Harrison, Ian, Hart, Luke, Hazra, Dhiraj Kumar, Heavens, Alan, Heinesen, Asta, Hildebrandt, Hendrik, Hill, J. Colin, Hogg, Natalie B., Holz, Daniel E., Hooper, Deanna C., Hosseininejad, Nikoo, Huterer, Dragan, Ishak, Mustapha, Ivanov, Mikhail M., Jaffe, Andrew H., Jang, In Sung, Jedamzik, Karsten, Jimenez, Raul, Joseph, Melissa, Joudaki, Shahab, Kamionkowski, Marc, Karwal, Tanvi, Kazantzidis, Lavrentio, Keeley, Ryan E., Klasen, Michael, Komatsu, Eiichiro, Koopmans, Léon V. E., Kumar, Suresh, Lamagna, Luca, Lazkoz, Ruth, Lee, Chung-Chi, Lesgourgues, Julien, Levi Said, Jackson, Lewis, Tiffany R., L'Huillier, Benjamin, Lucca, Matteo, Maartens, Roy, Macri, Lucas M., Marfatia, Danny, Marra, Valerio, Martins, Carlos J. A. P., Masi, Silvia, Matarrese, Sabino, Mazumdar, Arindam, Melchiorri, Alessandro, Mena, Olga, Mersini-Houghton, Laura, Mertens, Jame, Milaković, Dinko, Minami, Yuto, Miranda, Vivian, Moreno-Pulido, Cristian, Moresco, Michele, Mota, David F., Mottola, Emil, Mozzon, Simone, Muir, Jessica, Mukherjee, Ankan, Mukherjee, Suvodip, Naselsky, Pavel, Nath, Pran, Nesseris, Savva, Niedermann, Florian, Notari, Alessio, Nunes, Rafael C., Ó Colgáin, Eoin, Owens, Kayla A., Özülker, Emre, Pace, Francesco, Paliathanasis, Androniko, Palmese, Antonella, Pan, Supriya, Paoletti, Daniela, Perez Bergliaffa, Santiago E., Perivolaropoulos, Leandro, Pesce, Dominic W., Pettorino, Valeria, Philcox, Oliver H. E., Pogosian, Levon, Poulin, Vivian, Poulot, Gaspard, Raveri, Marco, Reid, Mark J., Renzi, Fabrizio, Riess, Adam G., Sabla, Vivian I., Salucci, Paolo, Salzano, Vincenzo, Saridakis, Emmanuel N., Sathyaprakash, Bangalore S., Schmaltz, Martin, Schöneberg, Nil, Scolnic, Dan, Sen, Anjan A., Sehgal, Neelima, Shafieloo, Arman, Sheikh-Jabbari, M. M., Silk, Joseph, Silvestri, Alessandra, Skara, Foteini, Sloth, Martin S., Soares-Santos, Marcelle, Solà Peracaula, Joan, Songsheng, Yu-Yang, Soriano, Jorge F., Staicova, Denitsa, Starkman, Glenn D., Szapudi, István, Teixeira, Elsa M., Thomas, Brook, Treu, Tommaso, Trott, Emery, van de Bruck, Carsten, Vazquez, J. Alberto, Verde, Licia, Visinelli, Luca, Wang, Deng, Wang, Jian-Min, Wang, Shao-Jiang, Watkins, Richard, Watson, Scott, Webb, John K., Weiner, Neal, Weltman, Amanda, Witte, Samuel J., Wojtak, Radosław, Yadav, Anil Kumar, Yang, Weiqiang, Zhao, Gong-Bo, Zumalacárregui, Miguel, Abdalla E., Abellan G.F., Aboubrahim A., Agnello A., Akarsu O., Akrami Y., Alestas G., Aloni D., Amendola L., Anchordoqui L.A., Anderson R.I., Arendse N., Asgari M., Ballardini M., Barger V., Basilakos S., Batista R.C., Battistelli E.S., Battye R., Benetti M., Benisty D., Berlin A., de Bernardis P., Berti E., Bidenko B., Birrer S., Blakeslee J.P., Boddy K.K., Bom C.R., Bonilla A., Borghi N., Bouchet F.R., Braglia M., Buchert T., Buckley-Geer E., Calabrese E., Caldwell R.R., Camarena D., Capozziello S., Casertano S., Chen G.C.-F., Chluba J., Chen A., Chen H.-Y., Chudaykin A., Cicoli M., Copi C.J., Courbin F., Cyr-Racine F.-Y., Czerny B., Dainotti M., D'Amico G., Davis A.-C., de Cruz Perez J., de Haro J., Delabrouille J., Denton P.B., Dhawan S., Dienes K.R., Di Valentino E., Du P., Eckert D., Escamilla-Rivera C., Ferte A., Finelli F., Fosalba P., Freedman W.L., Frusciante N., Gaztanaga E., Giare W., Giusarma E., Gomez-Valent A., Handley W., Harrison I., Hart L., Hazra D.K., Heavens A., Heinesen A., Hildebrandt H., Hill J.C., Hogg N.B., Holz D.E., Hooper D.C., Hosseininejad N., Huterer D., Ishak M., Ivanov M.M., Jaffe A.H., Jang I.S., Jedamzik K., Jimenez R., Joseph M., Joudaki S., Kamionkowski M., Karwal T., Kazantzidis L., Keeley R.E., Klasen M., Komatsu E., Koopmans L.V.E., Kumar S., Lamagna L., Lazkoz R., Lee C.-C., Lesgourgues J., Levi Said J., Lewis T.R., L'Huillier B., Lucca M., Maartens R., Macri L.M., Marfatia D., Marra V., Martins C.J.A.P., Masi S., Matarrese S., Mazumdar A., Melchiorri A., Mena O., Mersini-Houghton L., Mertens J., Milakovic D., Minami Y., Miranda V., Moreno-Pulido C., Moresco M., Mota D.F., Mottola E., Mozzon S., Muir J., Mukherjee A., Mukherjee S., Naselsky P., Nath P., Nesseris S., Niedermann F., Notari A., Nunes R.C., O Colgain E., Owens K.A., Ozulker E., Pace F., Paliathanasis A., Palmese A., Pan S., Paoletti D., Perez Bergliaffa S.E., Perivolaropoulos L., Pesce D.W., Pettorino V., Philcox O.H.E., Pogosian L., Poulin V., Poulot G., Raveri M., Reid M.J., Renzi F., Riess A.G., Sabla V.I., Salucci P., Salzano V., Saridakis E.N., Sathyaprakash B.S., Schmaltz M., Schoneberg N., Scolnic D., Sen A.A., Sehgal N., Shafieloo A., Sheikh-Jabbari M.M., Silk J., Silvestri A., Skara F., Sloth M.S., Soares-Santos M., Sola Peracaula J., Songsheng Y.-Y., Soriano J.F., Staicova D., Starkman G.D., Szapudi I., Teixeira E.M., Thomas B., Treu T., Trott E., van de Bruck C., Vazquez J.A., Verde L., Visinelli L., Wang D., Wang J.-M., Wang S.-J., Watkins R., Watson S., Webb J.K., Weiner N., Weltman A., Witte S.J., Wojtak R., Yadav A.K., Yang W., Zhao G.-B., and Zumalacarregui M.

Subjects
Planck, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Física::Astronomia i astrofísica::Cosmologia i cosmogonia [Àrees temàtiques de la UPC], anomaly, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, Gamma ray bursts, large-scale structure, Gravitational waves, NO, High Energy Physics - Phenomenology (hep-ph), gravitation: lens, Cosmic physics, energy: density, fine-structure constant, structure, dark energy survey, Cosmologia, Hubble constant, matter: energy, new physics, PE9_14, large-angle correlations, Astrophysics -- Mathematical models, Astronomy and Astrophysics, universal rotation curve, tension, oscillation spectroscopic survey, 115 Astronomy, Space science, redshift, Cosmology, astrophysics, cosmological tensions, Cosmology, High Energy Physics - Phenomenology, microwave-anisotropy-probe, calibration: geometrical, Dark matter (Astronomy), Space and Planetary Science, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], matter power spectrum, baryon acoustic-oscillations, hubble-space-telescope, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

E. Abdalla, G. F. Abellán, A. Aboubrahim et al., The standard Λ Cold Dark Matter (ΛCDM) cosmological model provides a good description of a wide range of astrophysical and cosmological data. However, there are a few big open questions that make the standard model look like an approximation to a more realistic scenario yet to be found. In this paper, we list a few important goals that need to be addressed in the next decade, taking into account the current discordances between the different cosmological probes, such as the disagreement in the value of the Hubble constant H0, the σ8–S8 tension, and other less statistically significant anomalies. While these discordances can still be in part the result of systematic errors, their persistence after several years of accurate analysis strongly hints at cracks in the standard cosmological scenario and the necessity for new physics or generalisations beyond the standard model. In this paper, we focus on the 5.0σ tension between the Planck CMB estimate of the Hubble constant H0 and the SH0ES collaboration measurements. After showing the H0 evaluations made from different teams using different methods and geometric calibrations, we list a few interesting new physics models that could alleviate this tension and discuss how the next decade's experiments will be crucial. Moreover, we focus on the tension of the Planck CMB data with weak lensing measurements and redshift surveys, about the value of the matter energy density Ωm, and the amplitude or rate of the growth of structure (σ8, fσ8). We list a few interesting models proposed for alleviating this tension, and we discuss the importance of trying to fit a full array of data with a single model and not just one parameter at a time. Additionally, we present a wide range of other less discussed anomalies at a statistical significance level lower than the H0–S8 tensions which may also constitute hints towards new physics, and we discuss possible generic theoretical approaches that can collectively explain the non-standard nature of these signals. Finally, we give an overview of upgraded experiments and next-generation space missions and facilities on Earth that will be of crucial importance to address all these open questions., Amin Aboubrahim is supported by the BMBF under contract 05P21PMCAA and by the DFG through the Research Training Network 2149 “Strong and Weak Interactions - from Hadrons to Dark Matter”. Adriano Agnello is supported by a Villum Experiment Grant, project number 36225. Özgür Akarsu acknowledges the support by the Turkish Academy of Sciences in the scheme of the Outstanding Young Scientist Award (TÜBA-GEBİP). Yashar Akrami is supported by Richard S. Morrison Fellowship and LabEx ENS-ICFP: ANR-10-LABX-0010/ANR-10-IDEX-0001-02 PSL*. George Alestas is supported by the project “Dioni: Computing Infrastructure for Big-Data Processing and Analysis” (MIS No. 5047222) co-funded by European Union (ERDF) and Greece through Operational Program “Competitiveness, Entrepreneurship and Innovation”, NSRF 2014-2020. Luca Amendola acknowledges support from DFG project 456622116 and from the CAPES-DAAD bilateral project “Data Analysis and Model Testing in the Era of Precision Cosmology”. Luis A. Anchordoqui and Jorge F. Soriano are supported by the U.S. National Science Foundation (NSF Grant PHY-2112527). Mario Ballardini acknowledges financial support from the contract ASI/INAF for the Euclid mission n.2018-23-HH.0. Micol Benetti acknowledges the Istituto Nazionale di Fisica Nucleare (INFN), sezione di Napoli, iniziativa specifica QGSKY. David Benisty acknowledges the support the supports of the Blavatnik and the Rothschild fellowships. John Blakeslee is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the US National Science Foundation. Thomas Buchert has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement ERC advanced grant 740021–ARTHUS, PI: Thomas Buchert). Erminia Calabrese acknowledges support from the STFC Ernest Rutherford Fellowship ST/M004856/2, STFC Consolidated Grant ST/S00033X/1 and from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (Grant agreement No. 849169). Salvatore Capozziello acknowledges the Istituto Nazionale di Fisica Nucleare (INFN), sezione di Napoli, iniziative specifiche QGSKY and MOONLIGHT2. Javier de Cruz Pérez is supported by a FPI fellowship associated to the project FPA2016-76005-C2-1-P. Peter Denton acknowledges support from the US Department of Energy under Grant Contract DE-SC0012704. Eleonora Di Valentino is supported by a Royal Society Dorothy Hodgkin Research Fellowship. Keith R. Dienes was supported in part by the U.S. Department of Energy under Grant DE-FG02-13ER41976 / DE-SC0009913, and also by the U.S. National Science Foundation through its employee IR/D program. Celia Escamilla-Rivera is supported by DGAPA-PAPIIT UNAM Project TA100122 and acknowledges the Royal Astronomical Society as FRAS 10147 and the Cosmostatistics National Group (CosmoNag) project. Noemi Frusciante is supported by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-OUT/29048/2017, CERN/FIS-PAR/0037/2019 and the personal FCT grant “CosmoTests – Cosmological tests of gravity theories beyond General Relativity” with ref. number CEECIND/00017/2018 and the FCT project “BEYLA–BEYond LAmbda” with ref. number PTDC/FIS-AST/0054/2021. Adrià Gómez-Valent is funded by the Instituto Nazionale di Fisica Nucleare (INFN) through the project “Dark Energy and Modified Gravity Models in the light of Low-Redshift Observations” (n. 22425/2020). Asta Heinesen has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement ERC advanced grant 740021–ARTHUS, PI: Thomas Buchert). J. Colin Hill acknowledges support from NSF grant AST-2108536. The Flatiron Institute is supported by the Simons Foundation. Mustapha Ishak acknowledges that this material is based upon work supported in part by the Department of Energy, Office of Science, under Award Number DE-SC0022184. Michael Klasen is supported by the BMBF under contract 05P21PMCAA and by the DFG through the Research Training Network 2149 “Strong and Weak Interactions - from Hadrons to Dark Matter”. Suresh Kumar gratefully acknowledges support from the Science and Engineering Research Board (SERB), Govt. of India (File No. CRG/2021/004658). Ruth Lazkoz is supported by the Spanish Ministry of Science and Innovation through research projects FIS2017-85076-P (comprising FEDER funds), and also by the Basque Government and Generalitat Valenciana through research projects GIC17/116-IT956-16 and PROMETEO/2020/079 respectively. Benjamin L'Huillier would like to acknowledge the support of the National Research Foundation of Korea (NRF-2019R1I1A1A01063740) and the support of the Korea Institute for Advanced Study (KIAS) grant funded by the government of Korea. Jackson Levi Said would like to acknowledge support from Cosmology@MALTA which is supported by the University of Malta. Roy Maartens is supported by the South African Radio Astronomy Observatory and the National Research Foundation (Grant No. 75415). Valerio Marra thanks CNPq (Brazil) and FAPES (Brazil) for partial financial support. The work of Yuto Minami was supported in part by the Japan Society for the Promotion of Science (JSPS) KAKENHI, Grants No. JP20K14497. The work of Carlos Martins was financed by FEDER—Fundo Europeu de Desenvolvimento Regional funds through the COMPETE 2020—Operational Programme for Competitiveness and Internationalisation (POCI), and by Portuguese funds through FCT - Fundação para a Ciência e a Tecnologia in the framework of the project POCI-01-0145-FEDER-028987 and PTDC/FIS-AST/28987/2017. Olga Mena is supported by the Spanish grants PID2020-113644GB-I00, PROMETEO/2019/083 and by the European ITN project HIDDeN (H2020-MSCA-ITN-2019//860881-HIDDeN). Cristian Moreno-Pulido is funded by PID2019-105614GB-C21 and FPA2016-76005-C2-1-P (MINECO, Spain), 2017-SGR-929 (Generalitat de Catalunya) and CEX2019-000918-M (ICCUB) and partially supported by the fellowship 2019 FI_B 00351. Michele Moresco acknowledges support from MIUR, PRIN 2017 (grant 20179ZF5KS) and grants ASI n.I/023/12/0 and ASI n.2018-23-HH.0. Suvodip Mukherjee is supported by the Simons Foundation. Research at Perimeter Institute is supported in part by the Government of Canada through the Department of Innovation, Science and Economic Development and by the Province of Ontario through the Ministry of Colleges and Universities. Pran Nath is supported in part by the NSF Grant PHY-1913328. Savvas Nesseris acknowledges support from the Research Project No. PGC2018-094773-B-C32 and the Centro de Excelencia Severo Ochoa Program No. CEX2020-001007-S. Rafael Nunes acknowledges support from the Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP, São Paulo Research Foundation) under the project No. 2018/18036-5. Eoin Ó Colgáin was supported by the National Research Foundation of Korea grant funded by the Korea government (MSIT) (NRF-2020R1A2C1102899). Supriya Pan acknowledges the financial supports from the Science and Engineering Research Board, Govt. of India, under Mathematical Research Impact-Centric Support Scheme (File No. MTR/2018/000940) and The Department of Science and Technology (DST), Govt. of India, under the Scheme “Fund for Improvement of S&T Infrastructure (FIST)” [File No. SR/FST/MS-I/2019/41]. Santiago E. Perez Bergliaffa acknowledges partial support from Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)- Código de Financiamento 001, and Universidade do Estado do Rio de Janeiro (Brazil). Leandros Perivolaropoulos acknowledges support by the Hellenic Foundation for Research and Innovation (H.F.R.I.), under the “First call for H.F.R.I. Research Projects to support Faculty members and Researchers and the procurement of high-cost research equipment Grant” (Project Number: 789). Fabrizio Renzi is supported by the NWO and the Dutch Ministry of Education, Culture and Science (OCW), and from the D-ITP consortium, a program of the NWO that is funded by the OCW. Nils Schöneberg acknowledges the support of the following Maria de Maetzu fellowship grant: Esta publicación es parte de la ayuda CEX2019-000918-M, financiado por MCIN/AEI/10.13039/501100011033. Anjan A Sen acknowledges the funding from SERB, Govt of India under the research grants no: CRG/2020/004347 and MTR/20l9/000599. Arman Shafieloo would like to acknowledge the support by National Research Foundation of Korea NRF-2021M3F7A1082053, and the support of the Korea Institute for Advanced Study (KIAS) grant funded by the government of Korea. M.M. Sheikh-Jabbari acknowledges the support by SarAmadan grant No. ISEF/M/400122. Joan Solà Peracaula is funded by PID2019-105614GB-C21 and FPA2016-76005-C2-1-P (MINECO, Spain), 2017-SGR-929 (Generalitat de Catalunya), CEX2019-000918-M (ICCUB) and also partially supported by the COST Association Action CA18108 “Quantum Gravity Phenomenology in the Multimessenger Approach (QG-MM)”. Denitsa Staicova is supported by Bulgarian NSF grant KP-06-N 38/11. Glenn Starkman is partly supported by a Department of Energy grant DESC0009946 to the particle astrophysics theory group at CWRU. Brooks Thomas is supported in part by the National Science Foundation under Grant PHY-2014104. Luca Visinelli has received support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement “TALeNT” No. 754496 (H2020-MSCA-COFUND-2016 FELLINI). Shao-Jiang Wang is supported by the National Key Research and Development Program of China Grant No. 2021YFC2203004, No. 2021YFA0718304, the National Natural Science Foundation of China Grant No. 12105344, and the China Manned Space Project with NO.CMS-CSST-2021-B01. Weiqiang Yang has been supported by the National Natural Science Foundation of China under Grants No. 12175096 and No. 11705079, and Liaoning Revitalization Talents Program under Grant no. XLYC1907098. Gong-Bo Zhao is supported by the National Key Basic Research and Development Program of China (No. 2018YFA0404503), NSFC Grants 11925303, 11720101004, and a grant of CAS Interdisciplinary Innovation Team.

Published
2022

30. Emulators for the nonlinear matter power spectrum beyond ΛCDM

Author

Gong-Bo Zhao, Kazuya Koyama, Marco Baldi, Baojiu Li, Lucas Lombriser, Hans A. Winther, S. Casas, Winther H.A., Casas S., Baldi M., Koyama K., Li B., Lombriser L., Zhao G.-B., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))

Subjects
gr-qc, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, Theoretical physics, 0103 physical sciences, 010306 general physics, STFC, Weak gravitational lensing, Physics, 010308 nuclear & particles physics, Matter power spectrum, RCUK, Spectral density, Function (mathematics), ST/P000541/1, Redshift, Nonlinear system, Alternative gravity theories, Cosmology, Astrophysical and Cosmological Simulations, astro-ph.CO, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], ST/N000668/1, ST/L00075X/1, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Accurate predictions for the non-linear matter power spectrum are needed to confront theory with observations in current and near future weak lensing and galaxy clustering surveys. We propose a computationally cheap method to create an emulator for modified gravity models by utilizing existing emulators for $\Lambda$CDM. Using a suite of $N$-body simulations we construct a fitting function for the enhancement of both the linear and non-linear matter power spectrum in the commonly studied Hu-Sawicki $f(R)$ gravity model valid for wave-numbers $k \lesssim 5-10\, h\text{Mpc}^{-1}$ and redshifts $z \lesssim 3$. We show that the cosmology dependence of this enhancement is relatively weak so that our fit, using simulations coming from only one cosmology, can be used to get accurate predictions for other cosmological parameters. We also show that the cosmology dependence can, if needed, be included by using linear theory, approximate $N$-body simulations (such as COLA) and semi-analytical tools like the halo model. Our final fit can easily be combined with any emulator or semi-analytical models for the non-linear $\Lambda$CDM power spectrum to accurately, and quickly, produce a non-linear power spectrum for this particular modified gravity model. The method we use can be applied to fairly cheaply construct an emulator for other modified gravity models. As an application of our fitting formula we use it to compute Fisher-forecasts for how well galaxy clustering and weak lensing in a Euclid-like survey will be at constraining modifications of gravity., Comment: 12 pages, 10 figures. Version accepted for publication in PRD. Data can be found at https://github.com/HAWinther/FofrFittingFunction

Published
2019

31. Radio Continuum Surveys with Square Kilometre Array Pathfinders

Author

Gianfranco Brunetti, Grazia Umana, Roland Kothes, Zsolt Paragi, Bryan Gaensler, Isabella Prandoni, Joseph Lazio, David Mary, Peter-Christian Zinn, Tamás Budavári, Eric J. Murphy, Ray P. Norris, Mara Salvato, J. Sabater, Marijke Haverkorn, Gong-Bo Zhao, Martin Bell, Gabriele Giovannini, Andrew M. Hopkins, Arwa Dabbech, Philip Best, Anna M. M. Scaife, Paolo Padovani, Huib Jan van Langevelde, Rainer Beck, Rob Fender, A. Martinez-Sansigre, C. M. Cress, Richard Schilizzi, Enno Middelberg, Annalisa Bonafede, Chiara Ferrari, David Bacon, J. J. Condo, Jose Afonso, George Heald, Sanjay Bhatnagar, H. J. A. Röttgering, Kurt van der Heyden, Isaac Roseboom, E. E. Rigby, Minnie Mao, Daniel J. B. Smith, Rossella Cassano, Matt J. Jarvis, Robert Beswick, Ilana Feain, Nick Seymour, Kim McAlpine, Melanie Johnston-Hollitt, Alvise Raccanelli, Norris, Ray P., Afonso, J., Bacon, D., Beck, Rainer, Bell, Martin, Beswick, R.J., Best, Philip, Bhatnagar, Sanjay, Bonafede, Annalisa, Brunetti, Gianfranco, Budavári, Tamá, Cassano, Rossella, Condon, J.J., Cress, Catherine, Dabbech, Arwa, Feain, I., Fender, Rob, Ferrari, Chiara, Gaensler, B.M., Giovannini, G., Haverkorn, Marijke, Heald, George, Van Der Heyden, Kurt, Hopkins, A.M., Jarvis, M., Johnston-Hollitt, Melanie, Kothes, Roland, Van Langevelde, Huib, Lazio, Joseph, Mao, Minnie Y., Martínez-Sansigre, Alejo, Mary, David, McAlpine, Kim, Middelberg, E., Murphy, Eric, Padovani, P., Paragi, Zsolt, Prandoni, I., Raccanelli, A., Rigby, Emma, Roseboom, I.G., Röttgering, H., Sabater, Jose, Salvato, Mara, Scaife, Anna M. M., Schilizzi, Richard, Seymour, N., Smith, Dan J. B., Umana, Grazia, Zhao, G.-B., and Zinn, Peter-Christian

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), radiotelescope, Astronomy, FOS: Physical sciences, galaxy evolution, Murchison Widefield Array, Primary science, Astrophysics, 01 natural sciences, Radio telescope, 0103 physical sciences, survey, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Physics, Continuum (measurement), 010308 nuclear & particles physics, business.industry, Astronomy and Astrophysics, LOFAR, Astronomy and Astrophysic, Square kilometre array, Space and Planetary Science, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Telecommunications, business, Astrophysics - Instrumentation and Methods for Astrophysics, cosmology, Cosmic time, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In the lead-up to the Square Kilometre Array (SKA) project, several next-generation radio telescopes and upgrades are already being built around the world. These include APERTIF (The Netherlands), ASKAP (Australia), eMERLIN (UK), VLA (USA), e-EVN (based in Europe), LOFAR (The Netherlands), Meerkat (South Africa), and the Murchison Widefield Array (MWA). Each of these new instruments has different strengths, and coordination of surveys between them can help maximise the science from each of them. A radio continuum survey is being planned on each of them with the primary science objective of understanding the formation and evolution of galaxies over cosmic time, and the cosmological parameters and large-scale structures which drive it. In pursuit of this objective, the different teams are developing a variety of new techniques, and refining existing ones. Here we describe these projects, their science goals, and the technical challenges which are being addressed to maximise the science return., Accepted by PASA, 22 October 2012

Published
2016

32. The Low Redshift survey at Calar Alto (LoRCA)

Author

Sergio Rodríguez-Torres, Claudia Maraston, Enrique Pérez, R. M. González Delgado, Chia-Hsun Chuang, R. Benton Metcalf, Johan Comparat, Marcos Pellejero-Ibanez, Hélène M. Courtois, Gong-Bo Zhao, J. Peiro-Perez, Francisco-Shu Kitaura, Gustavo Yepes, Justo Sanchez, Francisco Prada, Y. Wang, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Statistique de l'ENS (LPS), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Comparat, J., Chuang, C.-H., Rodríguez-Torres, S., Pellejero-Ibanez, M., Prada, F., Yepes, G., Courtois, H.M., Zhao, G.-B., Wang, Y., Sanchez, J., Maraston, C., Metcalf, R. Benton, Peiro-Perez, J., Kitaura, F.S., Pérez, E., González Delgado, R.M., Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris Diderot - Paris 7 (UPD7)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Ministerio de Economía, Industria y Competitividad (España), Chinese Academy of Sciences, European Commission, Ministerio de Ciencia e Innovación (España), Universidad Autónoma de Madrid (UAM), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, 010308 nuclear & particles physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmology: observations, Library science, FOS: Physical sciences, Astronomy and Astrophysics, Galaxies: Abundance, Abundances [Galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy and Astrophysic, 01 natural sciences, Chinese academy of sciences, Galaxies: Abundances, Cosmology: Observation, Space and Planetary Science, 0103 physical sciences, observations [Cosmology], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Baryon Acoustic Oscillation (BAO) feature in the power spectrum of galaxies provides a standard ruler to measure the accelerated expansion of the Universe. To extract all available information about dark energy, it is necessary to measure a standard ruler in the local, z < 0.2, universe where dark energy dominates most the energy density of the Universe. Though the volume available in the local universe is limited, it is just big enough to measure accurately the long 100 h Mpc wave-mode of the BAO. Using cosmological N-body simulations and approximate methods based on Lagrangian perturbation theory, we construct a suite of a thousand light-cones to evaluate the precision at which one can measure the BAO standard ruler in the local universe. We find that using the most massive galaxies on the full sky (34 000 deg), i.e. a K < 14 magnitude-limited sample, one can measure the BAO scale up to a precision of 4 per cent (~1.2 per cent using reconstruction). We also find that such a survey would help to detect the dynamics of dark energy. Therefore, we propose a 3-year long observational project, named the Low Redshift survey at Calar Alto, to observe spectroscopically about 200 000 galaxies in the northern sky to contribute to the construction of aforementioned galaxy sample. The suite of light-cones is made available to the public. © 2016 The Authors., JC, CC, SRT, MPI, FP, JS and FK acknowledge support from the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064, MINECO Centro de Excelencia Severo Ochoa Programme under grant SEV-2012-0249, and grant AYA2014-60641-C2-1-P. JC and GY acknowledge financial support from MINECO (Spain) under project number AYA2012-31101 and FPA2012-34694. MPI acknowledges support from MINECO under the grant AYA2012-39702-C02-01. MPI thanks the Instituto de Fisica Teorica for its hospitality and support during the completion of this work. HC acknowledges support from the Lyon Institute of Origins under grant ANR-10-LABX-66. GBZ is supported by the 1000 Young Talents programme in China, and by the Strategic Priority Research Programme `The Emergence of Cosmological Structures' of the Chinese Academy of Sciences, Grant No. XDB09000000. YW is supported by the National Science Foundation of China under Grant No. 11403034. RBM's research is funded under the European Seventh Framework Programme, Ideas, Grant no. 259349 (GLENCO). The BigMD simulation suite have been performed in the Supermuc supercomputer at LRZ using time granted by PRACE. This work made use of the HDAP, which was produced at Landessternwarte Heidelberg-Konigstuhl under grant No. 00.071.2005 of the Klaus-Tschira-Foundation.

Published
2016

33. [Determination of flavonoids in Ginkgo biloba L. leaves from different producing areas].

Author

Wang H, Zhao GB, Liu SQ, and Zheng JH

Subjects
Plant Leaves chemistry, Quercetin analogs & derivatives, Quercetin analysis, Flavonoids analysis, Flavonols, Ginkgo biloba chemistry, Kaempferols, Plants, Medicinal chemistry
Abstract

Objective: To compare the contents of flavonoids in the leaves of Ginkgo biloba gathered from 35 producing areas., Methods: Separating and determining 3 flavonoid aglycones, quercetin, kaempferol and isorhamnetin, by high performance liquid chromatography, and there by calculating the total contents of flavonoids., Results: The contents of flavonoids in the leaves of G. biloba gathered from different producing areas are different, but in those gathered from Pizhou, Zheng'an Xing'an, Anlu, etc. appear higher.

Published
2000

34. [Impairment of the digestive system in high altitude erythrocythemia].

Author

Zhao GB and Li L

Subjects
Adolescent, Adult, Alanine Transaminase blood, Bilirubin blood, Female, Gastroscopy, Hepatomegaly etiology, Humans, L-Lactate Dehydrogenase blood, Male, Middle Aged, Altitude Sickness complications, Duodenitis etiology, Gastritis etiology, Peptic Ulcer etiology, Polycythemia complications
Abstract

Among 203 patients with high altitude erythrocythemia (HAE), 89% had various kinds of alimentary canal symptoms, while these were present only in 31% of a control group (P less than 0.01). 49% of the HAE group had stomach, while only 8% of the control group had it. Endoscopic examination revealed 44% of the HAE group had peptic ulcer, being much higher than 6% of the control group. The ratio of gastric to duodenal ulcer in the HAE group was 2 to 1. The HAE patients had higher values of ALT, total bilirubin, LDH activity, LDH1 and LDHs, but lower values of AKP, LDH2, LDH4 and gamma-GT than the controls. The difference was, however, of no statistical significance. B mode ultrasonography showed that the incidence of hepatomegaly and splenomegaly was 24% and 11% respectively in the HAE group, while it was only 4% and 2% in the control group. HAE patients usually had symptoms of digestive system two years after the onset and the incidence at that time was 67%. With the extended course of the disease, the incidence gradually came down. The mechanism of digestive system impairment in HAE was probed and it was shown that treatment of digestive system impairment would promote the healing of HAE.

Published
1991

35. [Analysis of the etiology and clinical characteristics of Tibetan cirrhosis in Tibet].

Author

Zhao GB and Li L

Subjects
Adult, Aged, Altitude, China, Ethnicity, Female, Humans, Liver Cirrhosis ethnology, Liver Cirrhosis, Alcoholic ethnology, Liver Cirrhosis, Alcoholic etiology, Male, Middle Aged, Sex Factors, Liver Cirrhosis etiology
Abstract

The authors collected 41 cases of cirrhosis in native Tibetans with pathological verification. It is found that 60.98% of the cases were alcoholic cirrhosis, with an incidence significantly higher than that of 7.6% reported in the inland (P less than 0.01). 74.19% and 20% of the cirrhosis in male and female patients respectively were alcoholic, while 50% of the cirrhosis in the female were due to malnutrition. Among the Tibetan cirrhotics 12.2% was due to hepatitis and 4.88% each to hydatid disease and tuberculosis. The average age of these cirrhotics was 47.05. The frequent occurring age was between 41-50 (about 41.46%). The Tibetan cirrhosis in peasants and herdsmen were 51.28%. At the first admission, 84.49% got jaundice and 90.2% got ascites. These percentages were higher respectively than 43.2% and 50.5% from the Lanzou report (P less than 0.01). Ascites was serious, portal vein expanded, but splenomegaly were merely 17.07% (normal were 82.93%). These spleens expanded just a little, macrosplenopathy was not found.

Published
1989

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