Search

Your search keyword '"Furusawa H"' showing total 501 results
Start Over Author "Furusawa H"
501 results on '"Furusawa H"'

1. Combining the CLAUDS & HSC-SSP surveys: U+grizy(+YJHKs) photometry and photometric redshifts for 18M galaxies in the 20 deg2 of the HSC-SSP Deep and ultraDeep fields

Author

Desprez, G., Picouet, V., Moutard, T., Arnouts, S., Sawicki, M., Coupon, J., Gwyn, S., Chen, L., Huang, J., Golob, A., Furusawa, H., Ikeda, H., Paltani, S., Cheng, C., Hartley, W., Hsieh, B. C., Ilbert, O., Kauffmann, O. B., McCracken, H. J., Shuntov, M., Tanaka, M., Toft, S., Tresse, L., and Weaver, J. R.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the combination of the Canada-France-Hawaii Telescope (CHFT) Large Area $U$-bands Deep Survey (CLAUDS) and the Hyper-Suprime-Cam (HSC) Subaru Strategic Program (HSC-SSP) data over their four deep fields. We provide photometric catalogs for $u$, $u^*$ (CFHT--MegaCam), $g$, $r$, $i$, $z$, and $y$ (Subaru--HSC) bands over $\sim 20~{\rm deg}^2$, complemented in two fields by data from the Visible and Infrared Survey Telescope for Astronomy (VISTA) Deep Extragalactic Observations (VIDEO) survey and the UltraVISTA survey, thus extending the wavelength coverage toward near-infrared with VIRCAM $Y$, $J$, $H$, and $K_s$ observations over $5.5~{\rm deg}^2$. The extraction of the photometry was performed with two different softwares: the HSC pipeline hscPipe and the standard and robust SExtractor software. Photometric redshifts were computed with template-fitting methods using the new Phosphoros code for the hscPipe photometry and the well-known Le Phare code for the SExtractor photometry. The products of these methods were compared with each other in detail. We assessed their quality using the large spectroscopic sample available in those regions, together with photometry and photometric redshifts from COSMOS2020, the latest version of the Cosmic Evolution Survey catalogs. We find that both photometric data sets are in good agreement in $Ugrizy$ down to magnitude$\sim26$, and to magnitude$\sim24.5$ in the $YJHK_s$ bands. We achieve good performance for the photometric redshifts, reaching precisions of $\sigma_{NMAD} \lesssim 0.04$ down to ${m}_i\sim25$, even using only the CLAUDS and HSC bands. At the same magnitude limit, we measured an outlier fraction of $\eta \lesssim 10\%$ when using the $Ugrizy$ bands, and down to $\eta \lesssim 6\%$ when considering near-infrared data. [abridged], Comment: 25 pages (20+5 Appendices), 17 figures (+4 in appendices), 4 Tables (+2 in appendices), Accepted for publication in A&A

Published
2023
Full Text
View/download PDF

2. Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). IV. Discovery of 41 Quasars and Luminous Galaxies at 5.7 < z < 6.9

Author

Matsuoka, Y., Iwasawa, K., Onoue, M., Kashikawa, N., Strauss, M. A., Lee, C. -H., Imanishi, M., Nagao, T., Akiyama, M., Asami, N., Bosch, J., Furusawa, H., Goto, T., Gunn, J. E., Harikane, Y., Ikeda, H., Izumi, T., Kawaguchi, T., Kato, N., Kikuta, S., Kohno, K., Komiyama, Y., Lupton, R. H., Minezaki, T., Miyazaki, S., Morokuma, T., Murayama, H., Niida, M., Nishizawa, A. J., Oguri, M., Ono, Y., Ouchi, M., Price, P. A., Sameshima, H., Schulze, A., Shirakata, H., Silverman, J. D., Sugiyama, N., Tait, P. J., Takada, M., Takata, T., Tanaka, M., Tang, J. -J., Toba, Y., Utsumi, Y., Wang, S. -Y., and Yamashita, T.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We report discovery of 41 new high-z quasars and luminous galaxies, which were spectroscopically identified at 5.7 < z < 6.9. This is the fourth in a series of papers from the Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) project, based on the deep multi-band imaging data collected by the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. We selected the photometric candidates by a Bayesian probabilistic algorithm, and then carried out follow-up spectroscopy with the Gran Telescopio Canarias and the Subaru Telescope. Combined with the sample presented in the previous papers, we have now spectroscopically identified 137 extremely-red HSC sources over about 650 deg2, which include 64 high-z quasars, 24 high-z luminous galaxies, 6 [O III] emitters at z ~ 0.8, and 43 Galactic cool dwarfs (low-mass stars and brown dwarfs). The new quasars span the luminosity range from M1450 ~ -26 to -22 mag, and continue to populate a few magnitude lower luminosities than have been probed by previous wide-field surveys. In a companion paper, we derive the quasar luminosity function at z ~ 6 over an unprecedentedly wide range of M1450 ~ -28 to -21 mag, exploiting the SHELLQs and other survey outcomes., Comment: ApJS in press. arXiv admin note: substantial text overlap with arXiv:1704.05854

Published
2018
Full Text
View/download PDF

3. The Hyper Suprime-Cam SSP Survey: Overview and Survey Design

Author

Aihara, H., Arimoto, N., Armstrong, R., Arnouts, S., Bahcall, N. A., Bickerton, S., Bosch, J., Bundy, K., Capak, P. L., Chan, J. H. H., Chiba, M., Coupon, J., Egami, E., Enoki, M., Finet, F., Fujimori, H., Fujimoto, S., Furusawa, H., Furusawa, J., Goto, T., Goulding, A., Greco, J. P., Greene, J. E., Gunn, J. E., Hamana, T., Harikane, Y., Hashimoto, Y., Hattori, T., Hayashi, M., Hayashi, Y., Hełminiak, K. G., Higuchi, R., Hikage, C., Ho, P. T. P., Hsieh, B. -C., Huang, K., Huang, S., Ikeda, H., Imanishi, M., Inoue, A. K., Iwasawa, K., Iwata, I., Jaelani, A. T., Jian, H. -Y., Kamata, Y., Karoji, H., Kashikawa, N., Katayama, N., Kawanomoto, S., Kayo, I., Koda, J., Koike, M., Kojima, T., Komiyama, Y., Konno, A., Koshida, S., Koyama, Y., Kusakabe, H., Leauthaud, A., Lee, C. -H., Lin, L., Lin, Y. -T., Lupton, R. H., Mandelbaum, R., Matsuoka, Y., Medezinski, E., Mineo, S., Miyama, S., Miyatake, H., Miyazaki, S., Momose, R., More, A., More, S., Moritani, Y., Moriya, T. J., Morokuma, T., Mukae, S., Murata, R., Murayama, H., Nagao, T., Nakata, F., Niida, M., Niikura, H., Nishizawa, A. J., Obuchi, Y., Oguri, M., Oishi, Y., Okabe, N., Okura, Y., Ono, Y., Onodera, M., Onoue, M., Osato, K., Ouchi, M., Price, P. A., Pyo, T. -S., Sako, M., Okamoto, S., Sawicki, M., Shibuya, T., Shimasaku, K., Shimono, A., Shirasaki, M., Silverman, J. D., Simet, M., Speagle, J., Spergel, D. N., Strauss, M. A., Sugahara, Y., Sugiyama, N., Suto, Y., Suyu, S. H., Suzuki, N., Tait, P. J., Takata, T., Takada, M., Tamura, N., Tanaka, M. M., Tanaka, M., Tanaka, Y., Terai, T., Terashima, Y., Toba, Y., Toshikawa, J., Turner, E. L., Uchida, T., Uchiyama, H., Umetsu, K., Uraguchi, F., Urata, Y., Usuda, T., Utsumi, Y., Wang, S. -Y., Wang, W. -H., Wong, K. C., Yabe, K., Yamada, Y., Yamanoi, H., Yasuda, N., Yeh, S., Yonehara, A., and Yuma, S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Hyper Suprime-Cam (HSC) is a wide-field imaging camera on the prime focus of the 8.2m Subaru telescope on the summit of Maunakea in Hawaii. A team of scientists from Japan, Taiwan and Princeton University is using HSC to carry out a 300-night multi-band imaging survey of the high-latitude sky. The survey includes three layers: the Wide layer will cover 1400 deg$^2$ in five broad bands ($grizy$), with a $5\,\sigma$ point-source depth of $r \approx 26$. The Deep layer covers a total of 26~deg$^2$ in four fields, going roughly a magnitude fainter, while the UltraDeep layer goes almost a magnitude fainter still in two pointings of HSC (a total of 3.5 deg$^2$). Here we describe the instrument, the science goals of the survey, and the survey strategy and data processing. This paper serves as an introduction to a special issue of the Publications of the Astronomical Society of Japan, which includes a large number of technical and scientific papers describing results from the early phases of this survey., Comment: 14 pages, 7 figures, 5 tables. Corrected for a typo in the coordinates of HSC-Wide spring equatorial field in Table 5

Published
2017
Full Text
View/download PDF

4. SILVERRUSH. III. Deep optical and near-infrared spectroscopy for Lyα and UV-nebular lines of bright Lyα emitters at z = 6-7

Author

Shibuya, T, Ouchi, M, Harikane, Y, Rauch, M, Ono, Y, Mukae, S, Higuchi, R, Kojima, T, Yuma, S, Lee, CH, Furusawa, H, Konno, A, Martin, CL, Shimasaku, K, Taniguchi, Y, Kobayashi, MAR, Kajisawa, M, Nagao, T, Goto, T, Kashikawa, N, Komiyama, Y, Kusakabe, H, Momose, R, Nakajima, K, Tanaka, M, and Wang, SY

Subjects
early universe, galaxies: formation, galaxies: high-redshift, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We present Lyα and UV-nebular emission line properties of bright Lyα emitters (LAEs) at z = 6-7 with a luminosity of log LLyα/[erg s-1] = 43-44 identified in the 21 deg2 area of the SILVERRUSH early sample developed with the Subaru Hyper Suprime-Cam survey data. Our optical spectroscopy newly confirms 21 bright LAEs with clear Lyα emission, and contributes to making a spectroscopic sample of 96 LAEs at z = 6-7 in SILVERRUSH. From the spectroscopic sample, we select seven remarkable LAEs as bright as Himiko and CR7 objects, and perform deep Keck/MOSFIRE and Subaru/nuMOIRCS near-infrared spectroscopy reaching the 3 σ flux limit of ∼2 × 10-18 erg s-1 for the UV-nebular emission lines of He II λ1640, CIV λλ1548,1550, and OIII]λλ1661,1666. Except for one tentative detection of C IV, we find no strong UV-nebular lines down to the flux limit, placing the upper limits of the rest-frame equivalent widths (EW0) of ∼2-4 A for CIV, He II, and OIII] lines. We also investigate the VLT/X-SHOOTER spectrum of CR7 whose 6 σ detection of He II is claimed by Sobral et al. Although two individuals and the ESO archive service carefully reanalyzed the X-SHOOTER data that are used in the study of Sobral et al., no He II signal of CR7 is detected, supportive of weak UV-nebular lines of the bright LAEs even for CR7. The spectral properties of these bright LAEs are thus clearly different from those of faint dropouts at z ∼ 7 that have strong UV-nebular lines shown in the various studies. Comparing these bright LAEs and the faint dropouts, we find anti-correlations between the UV-nebular line EW0 and the UV-continuum luminosity, which are similar to those found at z ∼ 2-3.

Published
2018

6. A Fast Radio Burst Host Galaxy

Author

Keane, E. F., Johnston, S., Bhandari, S., Barr, E., Bhat, N. D. R., Burgay, M., Caleb, M., Flynn, C., Jameson, A., Kramer, M., Petroff, E., Possenti, A., van Straten, W., Bailes, M., Burke-Spolaor, S., Eatough, R. P., Stappers, B. W., Totani, T., Honma, M., Furusawa, H., Hattori, T., Morokuma, T., Niino, Y., Sugai, H., Terai, T., Tominaga, N., Yamasaki, S., Yasuda, N., Allen, R., Cooke, J., Jencson, J., Kasliwal, M. M., Kaplan, D. L., Tingay, S. J., Williams, A., Wayth, R., Chandra, P., Perrodin, D., Berezina, M., Mickaliger, M., and Bassa, C.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In recent years, millisecond duration radio signals originating from distant galaxies appear to have been discovered in the so-called Fast Radio Bursts. These signals are dispersed according to a precise physical law and this dispersion is a key observable quantity which, in tandem with a redshift measurement, can be used for fundamental physical investigations. While every fast radio burst has a dispersion measurement, none before now have had a redshift measurement, due to the difficulty in pinpointing their celestial coordinates. Here we present the discovery of a fast radio burst and the identification of a fading radio transient lasting $\sim 6$ days after the event, which we use to identify the host galaxy; we measure the galaxy's redshift to be $z=0.492\pm0.008$. The dispersion measure and redshift, in combination, provide a direct measurement of the cosmic density of ionised baryons in the intergalactic medium of $\Omega_{\mathrm{IGM}}=4.9 \pm 1.3\%$, in agreement with the expectation from WMAP, and including all of the so-called "missing baryons". The $\sim6$-day transient is largely consistent with a short gamma-ray burst radio afterglow, and its existence and timescale do not support progenitor models such as giant pulses from pulsars, and supernovae. This contrasts with the interpretation of another recently discovered fast radio burst, suggesting there are at least two classes of bursts., Comment: Published in Nature, 2016 Feb 25

Published
2016
Full Text
View/download PDF

7. A SYSTEMATIC SURVEY of PROTOCLUSTERS at z ∼ 3-6 in the CFHTLS DEEP FIELDS

Author

Toshikawa, J, Kashikawa, N, Overzier, R, Malkan, MA, Furusawa, H, Ishikawa, S, Onoue, M, Ota, K, Tanaka, M, Niino, Y, and Uchiyama, H

Subjects
early universe, galaxies: clusters: general, galaxies: high-redshift, large-scale structure of universe, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present the discovery of three protoclusters at z ∼ 3-4 with spectroscopic confirmation in the Canada-France-Hawaii Telescope Legacy Survey Deep Fields. In these fields, we investigate the large-scale projected sky distribution of z ∼ 3-6 Lyman-break galaxies and identify 21 protocluster candidates from regions that are overdense at more than 4σ overdensity significance. Based on cosmological simulations, it is expected that more than 76% of these candidates will evolve into a galaxy cluster of at least a halo mass of 1014 M o at z = 0. We perform follow-up spectroscopy for eight of the candidates using Subaru/FOCAS, Keck II/DEIMOS, and Gemini-N/GMOS. In total we target 462 dropout candidates and obtain 138 spectroscopic redshifts. We confirm three real protoclusters at z = 3-4 with more than five members spectroscopically identified and find one to be an incidental overdense region by mere chance alignment. The other four candidate regions at z ∼ 5-6 require more spectroscopic follow-up in order to be conclusive. A z = 3.67 protocluster, which has 11 spectroscopically confirmed members, shows a remarkable core-like structure composed of a central small region (

Published
2016

8. The galaxy luminosity function at z ~ 6 and evidence for rapid evolution in the bright end from z ~ 7 to 5

Author

Bowler, R. A . A., Dunlop, J. S., McLure, R. J., McCracken, H. J., Milvang-Jensen, B., Furusawa, H., Taniguchi, Y., Fevre, O. Le, Fynbo, J. P. U., Jarvis, M. J., and Häußler, B.

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

We present the results of a search for bright (-22.7 < M_UV < -20.5) Lyman-break galaxies at z ~ 6 within a total of 1.65 square degrees of imaging in the UltraVISTA/COSMOS and UKIDSS UDS/SXDS fields. The deep near-infrared imaging available in the two independent fields, in addition to deep optical (including z'-band) data, enables the sample of z ~ 6 star-forming galaxies to be securely detected long-ward of the break (in contrast to several previous studies). We show that the expected contamination rate of our initial sample by cool galactic brown dwarfs is < 3 per cent and demonstrate that they can be effectively removed by fitting brown dwarf spectral templates to the photometry. At z ~ 6 the galaxy surface density in the UltraVISTA field exceeds that in the UDS by a factor of ~ 1.8, indicating strong cosmic variance even between degree-scale fields at z > 5. We calculate the bright end of the rest-frame Ultra-Violet (UV) luminosity function (LF) at z ~ 6. The galaxy number counts are a factor of ~1.7 lower than predicted by the recent LF determination by Bouwens et al.. In comparison to other smaller area studies, we find an evolution in the characteristic magnitude between z ~ 5 and z ~ 7 of dM* ~ 0.4 mag, and show that a double power-law or a Schechter function can equally well describe the LF at z = 6. Furthermore, the bright-end of the LF appears to steepen from z ~ 7 to z ~ 5, which could indicate the onset of mass quenching or the rise of dust obscuration, a conclusion supported by comparing the observed LFs to a range of theoretical model predictions., Comment: 27 pages, 13 figures, updated to match MNRAS accepted version

Published
2014
Full Text
View/download PDF

9. The bright end of the galaxy luminosity function at z ~ 7: before the onset of mass quenching?

Author

Bowler, R. A . A., Dunlop, J. S., McLure, R. J., Rogers, A. B., McCracken, H. J., Milvang-Jensen, B., Furusawa, H., Fynbo, J. P. U., Taniguchi, Y., Afonso, J., Bremer, M. N., and Fevre, O. Le

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

We present the results of a new search for bright star-forming galaxies at z ~ 7 within the UltraVISTA DR2 and UKIDSS UDS DR10 data, which together provide 1.65 sq deg of near-infrared imaging with overlapping optical and Spitzer data. Using a full photo-z analysis to identify high-z galaxies and reject contaminants, we have selected a sample of 34 luminous (-22.7 < M_UV < -21.2) galaxies with 6.5 < z < 7.5. Crucially, the deeper imaging provided by UltraVISTA DR2 confirms all of the robust objects previously uncovered by Bowler et al. (2012), validating our selection technique. Our sample includes the most massive galaxies known at z ~ 7, with M_* ~ 10^{10} M_sun, and the majority are resolved, consistent with larger sizes (r_{1/2} ~ 1 - 1.5 kpc) than displayed by less massive galaxies. From our final sample, we determine the form of the bright end of the rest-frame UV galaxy luminosity function (LF) at z ~ 7, providing strong evidence that the bright end of the z = 7 LF does not decline as steeply as predicted by the Schechter function fitted to fainter data. We consider carefully, and exclude the possibility that this is due to either gravitational lensing, or significant contamination of our galaxy sample by AGN. Rather, our results favour a double power-law form for the galaxy LF at high z, or, more interestingly, a LF which simply follows the form of the dark-matter halo mass function at bright magnitudes. This suggests that the physical mechanism which inhibits star-formation activity in massive galaxies (i.e. AGN feedback or some other form of `mass quenching') has yet to impact on the observable galaxy LF at z ~ 7, a conclusion supported by the estimated masses of our brightest galaxies which have only just reached a mass comparable to the critical `quenching mass' of M_* = 10 ^{10.2} M_sun derived from studies of the mass function of star-forming galaxies at lower z., Comment: 36 pages, 13 figures, accepted to MNRAS

Published
2013
Full Text
View/download PDF

10. Discovery of bright z ~ 7 galaxies in the UltraVISTA survey

Author

Bowler, R. A. A., Dunlop, J. S., McLure, R. J., McCracken, H., Milvang-Jensen, B., Furusawa, H., Fynbo, J. P. U., Fevre, O. Le, Holt, J., Ideue, Y., Ihara, Y., Rogers, A. B., and Taniguchi, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We have exploited the new, deep, near-infrared UltraVISTA imaging of the COSMOS field, in tandem with deep optical and mid-infrared imaging, to conduct a new search for luminous galaxies at redshifts z ~ 7. The unique multi-wavelength dataset provided by VISTA, CFHT, Subaru, HST and Spitzer over a common area of 1 deg^2 has allowed us to select galaxy candidates at z > 6.5 by searching first for Y+J-detected (< 25 AB mag) objects which are undetected in the CFHT+HST optical data. This sample was then refined using a photometric redshift fitting code, enabling the rejection of lower-redshift galaxy contaminants and cool galactic M,L,T dwarf stars.The final result of this process is a small sample of (at most) ten credible galaxy candidates at z > 6.5 which we present in this paper. The first four of these appear to be robust galaxies at z > 6.5, and fitting to their stacked SED yields z = 6.98+-0.05 with a stellar mass M* = 5x10^9 Msun, and rest-frame UV spectral slope beta = -2.0+-0.2. The next three are also good candidates for z > 6.5 galaxies, but the possibility that they are low-redshift galaxies or dwarf stars cannot be excluded. Our final subset of three additional candidates is afflicted not only by potential dwarf-star contamination, but also contains objects likely to lie at redshifts just below z = 6.5. We show that the three even-brighter z > 7 galaxy candidates reported in the COSMOS field by Capak et al. (2011) in fact all lie at z ~ 1.5-3.5. Consequently the new z ~ 7 galaxies reported here are the first credible z ~ 7 Lyman-break galaxies discovered in the COSMOS field and, as the most UV-luminous discovered to date at these redshifts, are prime targets for deep follow-up spectroscopy. We explore their physical properties, and briefly consider the implications of their inferred number density for the form of the galaxy luminosity function at z = 7., Comment: Updated to accepted version, MNRAS. 18 pages, 9 figures, 3 tables

Published
2012
Full Text
View/download PDF

11. Detection of an ultra-bright submillimeter galaxy in the Subaru/XMM-Newton Deep Field using AzTEC/ASTE

Author

Ikarashi, S., Kohno, K., Aguirre, J. E., Aretxaga, I., Arumugam, V., Austermann, J. E., Bock, J. J., Bradford, C. M., Cirasuolo, M., Earle, L., Ezawa, H., Furusawa, H., Furusawa, J., Glenn, J., Hatsukade, B., Hughes, D. H., Iono, D., Ivison, R. J., Johnson, S., Kamenetzky, J., Kawabe, R., Lupu, R., Maloney, P., Matsuhara, H., Mauskopf, P. D., Motohara, K., Murphy, E. J., Nakajima, K., Nakanishi, K., Naylor, B. J., Nguyen, H. T., Perera, T. A., Scott, K. S., Shimasaku, K., Takagi, T., Takata, T., Tamura, Y., Tanaka, K., Tsukagoshi, T., Wilner, D. J., Wilson, G. W., Yun, M. S., and Zmuidzinas, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the detection of an extremely bright ($\sim$37 mJy at 1100 $\mu$m and $\sim$91 mJy at 880 $\mu$m) submillimeter galaxy (SMG), AzTEC-ASTE-SXDF1100.001 (hereafter referred to as SXDF1100.001 or Orochi), discovered in 1100 $\mu$m observations of the Subaru/XMM-Newton Deep Field using AzTEC on ASTE. Subsequent CARMA 1300 $\mu$m and SMA 880 $\mu$m observations successfully pinpoint the location of Orochi and suggest that it has two components, one extended (FWHM of $\sim$ 4$^{\prime\prime}$) and one compact (unresolved). Z-Spec on CSO has also been used to obtain a wide band spectrum from 190 to 308 GHz, although no significant emission/absorption lines are found. The derived upper limit to the line-to-continuum flux ratio is 0.1--0.3 (2 $\sigma$) across the Z-Spec band. Based on the analysis of the derived spectral energy distribution from optical to radio wavelengths of possible counterparts near the SMA/CARMA peak position, we suggest that Orochi is a lensed, optically dark SMG lying at $z \sim 3.4$ behind a foreground, optically visible (but red) galaxy at $z \sim 1.4$. The deduced apparent (i.e., no correction for magnification) infrared luminosity ($L_{\rm IR}$) and star formation rate (SFR) are $6 \times 10^{13}$ $L_{\odot}$ and 11000 $M_{\odot}$ yr$^{-1}$, respectively, assuming that the $L_{\rm IR}$ is dominated by star formation. These values suggest that Orochi will consume its gas reservoir within a short time scale ($3 \times 10^{7}$ yr), which is indeed comparable to those in extreme starbursts like the centres of local ULIRGs., Comment: 18 pages, 13 figures

Published
2010
Full Text
View/download PDF

12. Spectra and Light Curves of Six Type Ia Supernovae at 0.511 < z < 1.12 and the Union2 Compilation

Author

Amanullah, R., Lidman, C., Rubin, D., Aldering, G., Astier, P., Barbary, K., Burns, M. S., Conley, A., Dawson, K. S., Deustua, S. E., Doi, M., Fabbro, S., Faccioli, L., Fakhouri, H. K., Folatelli, G., Fruchter, A. S., Furusawa, H., Garavini, G., Goldhaber, G., Goobar, A., Groom, D. E., Hook, I., Howell, D. A., Kashikawa, N., Kim, A. G., Knop, R. A., Kowalski, M., Linder, E., Meyers, J., Morokuma, T., Nobili, S., Nordin, J., Nugent, P. E., Ostman, L., Pain, R., Panagia, N., Perlmutter, S., Raux, J., Ruiz-Lapuente, P., Spadafora, A. L., Strovink, M., Suzuki, N., Wang, L., Wood-Vasey, W. M., and Yasuda, N.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

We report on work to increase the number of well-measured Type Ia supernovae (SNe Ia) at high redshifts. Light curves, including high signal-to-noise HST data, and spectra of six SNe Ia that were discovered during 2001 are presented. Additionally, for the two SNe with z>1, we present ground-based J-band photometry from Gemini and the VLT. These are among the most distant SNe Ia for which ground based near-IR observations have been obtained. We add these six SNe Ia together with other data sets that have recently become available in the literature to the Union compilation (Kowalski et al. 2008). We have made a number of refinements to the Union analysis chain, the most important ones being the refitting of all light curves with the SALT2 fitter and an improved handling of systematic errors. We call this new compilation, consisting of 557 supernovae, the Union2 compilation. The flat concordance LambdaCDM model remains an excellent fit to the Union2 data with the best fit constant equation of state parameter w=-0.997^{+0.050}_{-0.054} (stat) ^{+0.077}_{-0.082} (stat+sys\ together) for a flat universe, or w=-1.035^{+0.055}_{-0.059} (stat)^{+0.093}_{-0.097} (stat+sys together) with curvature. We also present improved constraints on w(z). While no significant change in w with redshift is detected, there is still considerable room for evolution in w. The strength of the constraints depend strongly on redshift. In particular, at z > 1, the existence and nature of dark energy are only weakly constrained by the data., Comment: 33 pages, 18 figures; accepted for publication in Astrophysical Journal. For data tables, code for cosmological analysis and full-resolution figures, see http://supernova.lbl.gov/Union/

Published
2010
Full Text
View/download PDF

13. 'Dark' GRB 080325 in a Dusty Massive Galaxy at z ~ 2

Author

Hashimoto, T., Ohta, K., Aoki, K., Tanaka, I., Yabe, K., Kawai, N., Aoki, W., Furusawa, H., Hattori, T., Iye, M., Kawabata, K. S., Kobayashi, N., Komiyama, Y., Kosugi, G., Minowa, Y., Mizumoto, Y., Niino, Y., Nomoto, K., Noumaru, J., Ogasawara, R., Pyo, T. -S., Sakamoto, T., Sekiguchi, K., Shirasaki, Y., Suzuki, M., Tajitsu, A., Takata, T., Tamagawa, T., Terada, H., Totani, T., Watanabe, J., Yamada, T., and Yoshida, A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present optical and near infrared observations of GRB 080325 classified as a "Dark GRB". Near-infrared observations with Subaru/MOIRCS provided a clear detection of afterglow in Ks band, although no optical counterpart was reported. The flux ratio of rest-wavelength optical to X-ray bands of the afterglow indicates that the dust extinction along the line of sight to the afterglow is Av = 2.7 - 10 mag. This large extinction is probably the major reason for optical faintness of GRB 080325. The J - Ks color of the host galaxy, (J - Ks = 1.3 in AB magnitude), is significantly redder than those for typical GRB hosts previously identified. In addition to J and Ks bands, optical images in B, Rc, i', and z' bands with Subaru/Suprime-Cam were obtained at about one year after the burst, and a photometric redshift of the host is estimated to be z_{photo} = 1.9. The host luminosity is comparable to L^{*} at z \sim 2 in contrast to the sub-L^{*} property of typical GRB hosts at lower redshifts. The best-fit stellar population synthesis model for the host shows that a large dust extinction (Av = 0.8 mag) attributes to the red nature of the host and that the host galaxy is massive (M_{*} = 7.0 \times 10^{10} Msun) which is one of the most massive GRB hosts previously identified. By assuming that the mass-metallicity relation for star-forming galaxies at z \sim 2 is applicable for the GRB host, this large stellar mass suggests the high metallicity environment around GRB 080325, consistent with inferred large extinction., Comment: 22 pages, 10 figures, accepted for publication in The Astrophysical Journal

Published
2010
Full Text
View/download PDF

14. Strange filamentary structures ('fireballs') around a merger galaxy in the Coma cluster of galaxies

Author

Yoshida, M., Yagi, M., Komiyama, Y., Furusawa, H., Kashikawa, N., Koyama, Y., Yamanoi, H., Hattori, T., and Okamura, S.

Subjects
Astrophysics
Abstract

We found an unusual complex of narrow blue filaments, bright blue knots, and H-alpha emitting filaments and clouds, which morphologically resembled a complex of ``fireballs,'' extending up to 80 kpc south from an E+A galaxy RB199 in the Coma cluster. The galaxy has a highly disturbed morphology indicative of a galaxy--galaxy merger remnant. The narrow blue filaments extend in straight shapes toward the south from the galaxy, and several bright blue knots are located at the southern ends of the filaments. The Rc band absolute magnitudes, half light radii and estimated masses of the bright knots are -12 - -13 mag, 200 - 300 pc and 10^6-7 Msolar, respectively. Long, narrow H-alpha emitting filaments are connected at the south edge of the knots. The average color of the fireballs is B - Rc = 0.5, which is bluer than RB199 (B - R = 0.99), suggesting that most of the stars in the fireballs were formed within several times 10^8 yr. The narrow blue filaments exhibit almost no H-alpha emission. Strong H-alpha and UV emission appear in the bright knots. These characteristics indicate that star formation recently ceased in the blue filaments and now continues in the bright knots. The gas stripped by some mechanism from the disk of RB199 may be traveling in the intergalactic space, forming stars left along its trajectory. The most plausible fireball formation mechanism is ram pressure stripping by high-speed collision between the galaxy and the hot intra-cluster medium. The fireballs may be a snapshot of diffuse intra-cluster population formation, or halo star population formation in a cluster galaxy., Comment: 13 pages, 14 figures, submitted to ApJ

Published
2008
Full Text
View/download PDF

15. Detections of Lyman Continuum from Star-forming Galaxies at z~3 Through Subaru/Suprime-Cam Narrow-band Imaging

Author

Iwata, I., Inoue, A. K., Matsuda, Y., Furusawa, H., Hayashino, T., Kousai, K., Akiyama, M., Yamada, T., Burgarella, D., and Deharveng, J. -M.

Subjects
Astrophysics
Abstract

Knowing the amount of ionizing photons from young star-forming galaxies is of particular importance to understanding the reionization process. Here we report initial results of Subaru/Suprime-Cam deep imaging observation of the SSA22 proto-cluster region at z=3.09, using a special narrow-band filter to optimally trace Lyman continuum (LyC) from galaxies at z~3. The unique wide field-of-view of Suprime-Cam enabled us to search for ionizing photons from 198 galaxies (73 Lyman break galaxies (LBGs) and 125 Ly-alpha emitters (LAEs)) with spectroscopically measured redshifts z~3.1. We detected LyC from 7 LBGs, as well as from 10 LAE candidates. Some of the detected galaxies show significant spatial offsets of LyC from non-ionizing UV emission. For some LBGs the observed non-ionizing UV to LyC flux density ratios are smaller than values expected from population synthesis models with a standard Salpeter initial mass function (IMF) with moderate dust attenuation (which is suggested from the observed UV slopes), even if we assume very transparent IGM along the sightlines of these objects. This implies an intrinsically bluer spectral energy distribution, e.g, that produced by a top-heavy IMF, for these LBGs. The observed flux desity ratios of non-ionizing UV to LyC of 7 detected LBGs range from 2.4 to 23.8 and the median is 6.6. The observed flux density ratios of the detected LAEs are even smaller than LBGs, if they are truly at z~3.1. We find that the median value of the flux density ratio for the deteced LBGs suggest that their escape fractions is likely to be higher than 4%, if the LyC escape is isotropic. The results imply that some of the LBGs in the proto-cluster at z~3 have the escape fraction significantly higher than that of galaxies (in a general field) at z~1 studied previously., Comment: 9 pages, 5 figures. Accepted for publication in ApJ

Published
2008
Full Text
View/download PDF

16. The SCUBA Half-Degree Extragalactic Survey (SHADES) - VIII. The Nature of Faint Submm Galaxies in SHADES, SWIRE and SXDF Surveys

Author

Clements, D. L., Vaccari, M., Babbedge, T., Oliver, S., Rowan-Robinson, M., Davoodi, P., Ivison, R., Farrah, D., Dunlop, J., Shupe, Dave, Waddington, I., Simpson, C., Furusawa, H., Serjeant, S., Afonso-Luis, A., Alexander, D. M., Aretxaga, I., Blain, A., Borys, C., Chapman, S., Coppin, K., Dunne, L., Dye, S., Eales, S. A., Evans, T., Fang, F., Frayer, D., Fox, M., Gear, W. K., Greve, T. R., Halpern, M., Hughes, D. H., Jenness, T., Lonsdale, C. J., Mortier, A. M. J., Page, M. J., Pope, A., Priddey, R. S., Rawlings, S., Savage, R. S., Scott, D., Scott, S. E., Sekiguchi, K., Smail, I., Smith, H. E., Stevens, J. A., Surace, J., Takagi, T., and van Kampen, E.

Subjects
Astrophysics
Abstract

We present the optical-to-submm spectral energy distributions for 33 radio & mid-IR identified submillimetre galaxies discovered via the SHADES 850 micron SCUBA imaging in the Subaru-XMM Deep Field (SXDF). Optical data for the sources comes from the Subaru-XMM Deep Field (SXDF) and mid- and far-IR fluxes from SWIRE. We obtain photometric redshift estimates for our sources using optical and IRAC 3.6 and 4.5 micron fluxes. We then fit spectral energy distribution (SED) templates to the longer wavelength data to determine the nature of the far-IR emission that dominates the bolometric luminosity of these sources. The infrared template fits are also used to resolve ambiguous identifications and cases of redshift aliasing. The redshift distribution obtained broadly matches previous results for submm sources and on the SHADES SXDF field. Our template fitting finds that AGN, present in about 10% of sources, do not contribute significantly to their bolometric luminosity. Dust heating by starbursts, with either Arp220 or M82 type SEDs, appears to be responsible for the luminosity in most sources (23/33 are fitted by Arp220 templates, 2/33 by the warmer M82 templates). 8/33 sources, in contrast, are fit by a cooler cirrus dust template, suggesting that cold dust has a role in some of these highly luminous objects. Three of our sources appear to have multiple identifications or components at the same redshift, but we find no statistical evidence that close associations are common among our SHADES sources. Examination of rest-frame K -band luminosity suggests that 'downsizing' is underway in the submm galaxy population, with lower redshift systems lying in lower mass host galaxies. Of our 33 identifications six are found to be of lower reliability but their exclusion would not significantly alter our conclusions., Comment: MNRAS in press

Published
2008
Full Text
View/download PDF

17. The Subaru/XMM-Newton Deep Survey (SXDS) - II. Optical Imaging and Photometric Catalogs

Author

Furusawa, H., Kosugi, G., Akiyama, M., Takata, T., Sekiguchi, K., Tanaka, I., Iwata, I., Kajisawa, M., Yasuda, N., Doi, M., Ouchi, M., Simpson, C., Shimasaku, K., Yamada, T., Furusawa, J., Morokuma, T., Ishida, C. M., Aoki, K., Fuse, T., Imanishi, M., Iye, M., Karoji, H., Kobayashi, N., Kodama, T., Komiyama, Y., Maeda, Y., Miyazaki, S., Mizumoto, Y., Nakata, F., Noumaru, J., Ogasawara, R., Okamura, S., Saito, T., Sasaki, T., Ueda, Y., and Yoshida, M.

Subjects
Astrophysics
Abstract

We present multi-waveband optical imaging data obtained from observations of the Subaru/XMM-Newton Deep Survey (SXDS). The survey field, centered at R.A.=02:18:00, decl.=-05:00:00, has been the focus of a wide range of multi-wavelength observing programs spanning from X-ray to radio wavelengths. A large part of the optical imaging observations are carried out with Suprime-Cam on Subaru Telescope at Mauna Kea in the course of Subaru Telescope Observatory Projects. This paper describes our optical observations, data reduction and analysis procedures employed, and the characteristics of the data products. A total area of 1.22 sqdeg is covered in five contiguous sub-fields, each of which corresponds to a single Suprime-Cam field of view (34'x27'), in five broad-band filters B, V, Rc, i', z' to the depths of B=28.4, V=27.8, Rc=27.7, i'=27.7 and z'=26.6 (AB, 3-sigma, 2-arcsec aperture). The data are reduced and compiled into five multi-waveband photometric catalogs, separately for each Suprime-Cam pointing. The i'-band catalogs contain about 900,000 objects, making the SXDS catalogs one of the largest multi-waveband catalogs in corresponding depth and area coverage. The SXDS catalogs can be used for an extensive range of astronomical applications such as the number density of the Galactic halo stars to the large scale structures at the distant universe. The number counts of galaxies are derived and compared with those of existing deep extragalactic surveys. The optical data, the source catalogs, and configuration files used to create the catalogs are publicly available via the SXDS web page (http://www.naoj.org/Science/SubaruProject/SXDS/index.html), Comment: 55 pages, 22 figures, 9 tables, accepted by ApJS, a higher-resolution version is available at http://step.mtk.nao.ac.jp/sxds/

Published
2008
Full Text
View/download PDF

18. SuprimeCam Observation of Sporadic Meteors during Perseids 2004

Author

Iye, M., Tanaka, M., Yanagisawa, M., Ebizuka, N., Ohnishi, K., Hirose, C., Asami, N., Komiyama, Y., and Furusawa, H.

Subjects
Astrophysics
Abstract

We report the serendipitous findings of 13 faint meteors and 44 artificial space objects by Subaru SuprimeCam imaging observations during 11-16 August 2004. The meteors, at about 100km altitude, and artificial satellites/debris in orbit, at 500km altitude or higher, were clearly discriminated by their apparent defocused image sizes. CCD photometry of the 13 meteors, including 1 Perseid, 1 Aquarid, and 11 sporadic meteors, was performed. We defined a peak video-rate magnitude by comparing the integrated photon counts from the brightest portion of the track traversed within 33ms to those from a 0-mag star during the same time duration. This definition gives magnitudes in the range 4.0< V_{vr} <6.4 and 4.1< I_{vr}<5.9 for these 13 meteors. The corresponding magnitude for virtual naked-eye observers could be somewhat fainter especially for the V-band observation, in which the [OI] 5577 line lasting about 1 sec as an afterglow could contribute to the integrated flux of the present 5-10 min CCD exposures. Although the spatial resolution is insufficient to resolve the source size of anything smaller than about 1 m, we developed a new estimate of the collisionally excited column diameter of these meteors. A diameter as small as a few mm was derived from their collisionally excited photon rates, meteor speed, and the volume density of the oxygen atoms at the 100km altitude. The actual column diameter of the radiating zone, however, could be as large as few 100m because the excited atoms travel that distance before they emit forbidden lines in 0.7 sec of its average lifetime. Among the 44 artificial space objects, we confirmed that 17 were cataloged satellites/space debris., Comment: 14 pages, 13 figures, 5 tables, submitted to PASJ

Published
2007
Full Text
View/download PDF

19. The Galaxy Luminosity Functions down to M~-10 in the Hydra I Cluster

Author

Yamanoi, H., Tanaka, M., Hamabe, M., Yagi, M., Okamura, S., Iye, M., Shimasaku, K., Doi, M., Komiyama, Y., and Furusawa, H.

Subjects
Astrophysics
Abstract

We study the galaxy population in the central region and a region about 0.6 Mpc away from the center of the Hydra I cluster in B- and Rc-bands down to M~-10 using the Subaru Suprime-Cam photometry. We find that the luminosity function of the entire population has a slightly steeper slope (alpha~-1.6) in the range of -20-14) increases in the cluster center as well as bright galaxies. The Hydra I cluster is dominated by red dwarfs and the luminosity function shows a significant upturn at M~-16 as is seen in several other nearby clusters, but not in the field. This upturn and the variation in the faint-end slope of the luminosity function may be caused by the cluster environment or the evolution history of individual clusters., Comment: 21 pages, 6 figures, submitted to AJ

Published
2007
Full Text
View/download PDF

20. Search for the host galaxy of GRB 050904 at z=6.3

Author

Aoki, K., Furusawa, H., Ohta, K., Yamada, T., and Kawai, N.

Subjects
Astrophysics
Abstract

We present the results of deep imaging of the field of GRB 050904 with Suprime-Cam on the Subaru 8.2m telescope. We have obtained a narrow-band (130 A) image centered at 9200 A (NB921) and an i'-band image with total integration times of 56700 and 24060 s, respectively. The host galaxy was not detected within 1'' of the afterglow position. An object was found at 1.5'' NE from the position of the afterglow, but clear detection of this object in the i'-band image rules out its association with the burst. We obtained a limit of > 26.4 AB magnitude (2'' diameter, 3 sigma) in the NB921 image for the host galaxy, corresponding to a flux of 6.0 x 10^{28} erg/s/Hz at rest 1500 A assuming a flat spectrum of the host galaxy. The star formation rate should be less than 7.5 (M_{solar}/yr) based on the conversion rate by Madau et al (1998). This upper limit for the host of GRB 050904 is consistent with the star formation rate of other gamma-ray burst host galaxies around redshift of 2 or less., Comment: To be published in the proceedings of the conference "SWIFT and GRBs: Unveiling the Relativistic Universe", Venice, June 5-9, 2006. To appear in "Il Nuovo Cimento"

Published
2006
Full Text
View/download PDF

21. In-plane thermal conductivity of large single crystals of Sm-substituted (Y$_{1-x}$Sm$_{x}$)Ba$_{2}$Cu$_{3}$O$_{7-\delta}$

Author

Matsukawa, M., Noto, H., Furusawa, H., and Yao, X.

Subjects
Condensed Matter - Superconductivity, Condensed Matter - Materials Science
Abstract

We have investigated the in-plane thermal conductivity $\kappa_{ab}(T,H)$ of large single crystals of optimally oxygen-doped (Y$_{1-x}$,Sm$_{x}$)Ba$_{2}$Cu$_{3}$O$_{7-\delta}$ ($x$=0, 0.1, 0.2 and 1.0) and YBa$_{2}$(Cu$_{1-y}$Zn$_{y}$)$_{3}$O$_{7-\delta}$($y$=0.0071) as functions of temperature and magnetic field (along the c axis). For comparison, the temperature dependence of $\kappa_{ab}$ for as-grown crystals with the corresponding compositions are presented. The nonlinear field dependence of $\kappa_{ab}$ for all crystals was observed at relatively low fields near a half of $T_{c}$. We make fits of the $\kappa(H)$ data to an electron contribution model, providing both the mean free path of quasiparticles $\ell_{0}$ and the electronic thermal conductivity $\kappa_{e}$, in the absence of field. The local lattice distortion due to the Sm substitution for Y suppresses both the phonon and electron contributions. On the other hand, the light Zn doping into the CuO $_{2}$ planes affects solely the electron component below $T_{c}$, resulting in a substantial decrease in $\ell_{0}$ ., Comment: 7 pages,4 figures,1 table

Published
2006
Full Text
View/download PDF

22. Afterglow spectrum of a gamma-ray burst with the highest known redshift z=6.295

Author

Kawai, N., Kosugi, G., Aoki, K., Yamada, T., Totani, T., Ohta, K., Iye, M., Hattori, T., Aoki, W., Furusawa, H., Hurley, K., Kawabata, K., Kobayashi, N., Komiyama, Y., Mizumoto, Y., Nomoto, K., Noumaru, J., Ogasawara, R., Sato, R., Sekiguchi, K., Shirasaki, Y., Suzuki, M., Takata, T., Tamagawa, T., Terada, H., Watanabe, J., Yatsu, Y., and Yoshida, A.

Subjects
Astrophysics
Abstract

Gamma-ray bursts (GRBs) and their afterglows have been proposed as an excellent probe to study the evolution of cosmic star formation, the reionization of the intergalactic medium, and the metal enrichment history of the universe, since the prompt gamma-ray emission of GRBs should be detectable out to distances z>10. Hitherto, the highest measured redshift for a GRB has been z=4.50. Here we report the optical spectrum of the afterglow of GRB 050904 obtained 3.4 days after the burst. The spectrum shows a clear continuum at the long wavelength end of the spectrum with a sharp cutoff at around 9000 A due to Ly alpha absorption at a redshift of 6.3 with a damping wing. Little flux is present in the waveband shortward of the Ly alpha break. A system of absorption lines of heavy elements at redshift z=6.295 +- 0.002 were also detected, yielding a precise measurement of the largest known redshift of a GRB. Analysis of the Si II fine structure lines suggest a dense metal-enriched environment around the GRB progenitor, providing unique information on the properties of the gas in a galaxy when the universe was younger than one billion years., Comment: 12 pages, 1 figure (figure only in PostScript format, not in PDF)

Published
2005

23. Number Density of Bright Lyman-Break Galaxies at z~6 in the Subaru Deep Field

Author

Shimasaku, K., Ouchi, M., Furusawa, H., Yoshida, M., Kashikawa, N., and Okamura, S.

Subjects
Astrophysics
Abstract

We report on the bright Lyman-break galaxies (LBGs) selected in a 767 arcmin^2 area of the Subaru Deep Field. The selection is made in the i-zR vs zB-zR plane, where zB and zR are new bandpasses with a central wavelength of 8842A and 9841A, respectively. This set of bandpasses enables us to separate well z~6 LBGs from foreground galaxies and Galactic cool stars. We detect 12 LBG candidates down to zR=25.4, and calculate the normalization of the rest-frame far-ultraviolet (FUV: 1400A) luminosity function at MFUV = -21.6 to be \phi(-21.6) = (2.6+/-0.7) x 10^{-5} mag^{-1} Mpc^{-3}. This must be the most reliable measurement ever obtained of the number density of bright z~6 LBGs, because it is more robust against both contamination and cosmic variance than previous values. The FUV luminosity density contributed from LBGs brighter than MFUV = -21.3 is (2.8+/-0.8) x 10^{24} ergs/s/Hz/Mpc^3, which is equivalent to a star formation rate density of (3.5+/-1.0) x 10^{-4} Msun/yr/Mpc^3. Combining our measurement with those at z<6 in the literature, we find that the FUV luminosity density of bright galaxies increases by an order of magnitude from z~6 to z~3 and then drops by 10^3 from z~3 to the present epoch, while the evolution of the total luminosity density is much milder. The evolutionary behavior of bright LBGs resembles that of luminous dusty star-forming galaxies and bright QSOs. The redshift of z~3 appears to be a remarkable era in the cosmic history when massive galaxies were being intensively formed., Comment: 12 pages, accepted for PASJ, a high resolution version is available at http://hikari.astron.s.u-tokyo.ac.jp/~shima/z6LBGs/

Published
2005
Full Text
View/download PDF

24. The Discovery of Primeval Large-Scale Structures with Forming Clusters at Redshift 6

Author

Ouchi, M., Shimasaku, K., Akiyama, M., Sekiguchi, K., Furusawa, H., Okamura, S., Kashikawa, N., Iye, M., Kodama, T., Saito, T., Sasaki, T., Simpson, C., Takata, T., Yamada, T., Yamanoi, H., and Yoshida, M.

Subjects
Astrophysics
Abstract

We report the discovery of primeval large-scale structures (LSSs) including two proto-clusters in a forming phase at z=5.7. We carried out extensive deep narrow-band imaging in the 1 deg^2 sky of the Subaru/XMM-Newton Deep Field, and obtained a cosmic map of 515 Ly alpha emitters (LAEs) in a volume with a transverse dimension of 180 Mpc x 180 Mpc and a depth of ~40 Mpc in comoving units. This cosmic map shows filamentary LSSs, including clusters and surrounding 10-40 Mpc scale voids, similar to the present-day LSSs. Our spectroscopic follow-up observations identify overdense regions in which two dense clumps of LAEs with a sphere of 1-Mpc diameter in physical units are included. These clumps show about 130 times higher star-formation rate density, mainly due to a large overdensity, ~80, of LAEs. These clumps would be clusters in a formation phase involving a burst of galaxy formation., Comment: 8 pages, 4 figures, to be published in ApJL. The paper with high resolution figures is available at http://www-int.stsci.edu/~ouchi/work/astroph/sxds_LSS/

Published
2004
Full Text
View/download PDF

25. The Subaru Deep Field: The Optical Imaging Data

Author

Kashikawa, N., Shimasaku, K., Yasuda, N., Ajiki, M., Akiyama, M., Ando, H., Aoki, K., Doi, M., Fujita, S. S., Furusawa, H., Hayashino, T., Iwamuro, F., Iye, M., Karoji, H., Kobayashi, N., Kodaira, K., Kodama, T., Komiyama, Y., Matsuda, Y., Miyazaki, S., Mizumoto, Y., Morokuma, T., Motohara, K., Murayama, T., Nagao, T., Nariai, K., Ohta, K., Okamura, S., Ouchi, M., Sasaki, T., Sato, Y., Sekiguchi, K., Shioya, Y., Tamura, H., Taniguchi, Y., Umemura, M., Yamada, T., and Yoshida, M.

Subjects
Astrophysics
Abstract

The Subaru Deep Field (SDF) project is a program of Subaru Observatory to carry out a deep galaxy survey over a blank field as large as 34'x27'. The program consists of very deep multi-band optical imaging, near infrared imaging for smaller portions of the field and follow-up optical spectroscopy. Major scientific goals of the project are to construct large samples of Lyman-break galaxies at z~4-5 and Lyman alpha emitters at z~5.7 and 6.6, and to make detailed studies these very high-redshift galaxy populations. In this paper, we describe the optical imaging observations and data reduction, presenting mosaicked images and object catalogs in seven bandpasses.The optical imaging was made through five broad-band filters, B, V, R, i', z', and two narrow-band filters, NB816 (lambda_c=8150A) and NB921 (lambda_c=9196A) with almost 10 hours long integrations for each band. The limiting magnitudes measured at 3-sigma on a 2" aperture are B=28.45, V=27.74, R=27.80, i'=27.43, z'=26.62, NB816=26.63, and NB921=26.54 in the AB system. The object catalog constructed for each of the seven bands contains more than 10^5 objects. The galaxy number counts corrected for detection incompleteness and star count contribution are found to be consistent with previous results in the literature. The mosaicked images and catalogs of all the bands have been made open to the public on Oct. 1, 2004 on the SDF project website at http://soaps.naoj.org/sdf/., Comment: 18 pages, 10figures, accepted for publication in PASJ, and see also http://step.mtk.nao.ac.jp/sdf/ [Japan site], http://soaps.naoj.org/sdf/ [US site]

Published
2004
Full Text
View/download PDF

26. Subaru Deep Spectroscopy of the Very Extended Emission-Line Region of NGC 4388: Ram Pressure Stripped Gas Ionized by the Nuclear Radiation

Author

Yoshida, M., Ohyama, Y., Iye, M., Aoki, K., Kashikawa, N., Sasaki, T., Shimasaku, K., Yagi, M., Okamura, S., Doi, M., Furusawa, H., Hamabe, M., Kimura, M., Komiyama, Y., Miyazaki, M., Miyazaki, S., Nakata, F., Ouchi, M., Sekiguchi, M., and Yasuda, N.

Subjects
Astrophysics
Abstract

We report here the results of deep optical spectroscopy of the very extended emission-line region (VEELR) found serendipitously around the Seyfert 2 galaxy NGC 4388 in the Virgo cluster using the Subaru Telescope. The H-alpha recession velocities of most of the filaments of the region observed are highly blue-shifted with respect to the systemic velocity of the galaxy. The velocity field is complicated, and from the kinematic and morphological points of view, there seem to be several streams of filaments: low velocity (v = -100 km/s) filaments, high velocity (v = -300 km/s) filaments, and a very high velocity (v > -500 km/s) cloud complex. The emission-line ratios of the VEELR filaments are well explained by power-law photoionization models with solar abundances, suggesting that the Seyfert nucleus of NGC 4388 is the dominant ionization source of the VEELR and that the VEELR gas has moderate metallicity. In addition to photoionization, shock heating probably contributes to the ionization of the gas. In particular, the filaments outside the ionization cone of the Seyfert nucleus are mainly excited by shocks. We conclude that the VEELR was formerly the disk gas of NGC 4388, which has been stripped by ram pressure due to the interaction between the hot intra-cluster medium (ICM) and the galaxy. The velocity field and the morphology of the VEELR closely resemble snapshots from some numerical simulations of this process. In the case of NGC 4388, the ram pressure-stripped gas, which is normally seen as extended HI filaments, happens to be exposed and ionized by the radiation from the AGN, and so can be seen as optical emission-line gas., Comment: 20 pages, LaTeX, Accepted by Astron. J

Published
2003
Full Text
View/download PDF

27. Subaru Deep Survey V. A Census of Lyman Break Galaxies at z=4 and 5 in the Subaru Deep Fields: Photometric Properties

Author

Ouchi, M., Shimasaku, K., Okamura, S., Furusawa, H., Kashikawa, N., Ota, K., Doi, M., Hamabe, M., Kimura, M., Komiyama, Y., Miyazaki, M., Miyazaki, S., Nakata, F., Sekiguchi, M., Yagi, M., and Yasuda, N.

Subjects
Astrophysics
Abstract

(abridged) We investigate photometric properties of Lyman Break Galaxies (LBGs) at z=3.5-5.2 based on large samples of 2,600 LBGs detected in deep (i'~27) and wide-field (1,200 arcmin^2) images taken in the Subaru Deep Field (SDF) and the Subaru/XMM Deep Field (SXDF). The selection criteria for the LBG samples are examined with 85 spectroscopically identified objects and by Monte Carlo simulations. We find in the luminosity functions of LBGs (i) that the number density of bright galaxies (M_{1700}<-22; corresponding to SFR_{corr}>100 Msolar yr^{-1}) decreases significantly from z=4 to 5 and (ii) that the faint-end slope of the luminosity function may become steeper towards higher redshifts. We estimate dust extinction of z=4 LBGs with M~0.13., Comment: 41 pages, 22 figures, ApJ in press. Paper with high resolution figures is available at http://hikari.astron.s.u-tokyo.ac.jp/~ouchi/work/astroph/SDS_V_VI/SDS_V.pdf (PDF)

Published
2003
Full Text
View/download PDF

28. Subaru Deep Survey VI. A Census of Lyman Break Galaxies at z=4 and 5 in the Subaru Deep Fields: Clustering Properties

Author

Ouchi, M., Shimasaku, K., Okamura, S., Furusawa, H., Kashikawa, N., Ota, K., Doi, M., Hamabe, M., Kimura, M., Komiyama, Y., Miyazaki, M., Miyazaki, S., Nakata, F., Sekiguchi, M., Yagi, M., and Yasuda, N.

Subjects
Astrophysics
Abstract

We investigate the clustering properties of 2,600 Lyman Break Galaxies (LBGs) at z=3.5-5.2 in two large blank fields, the Subaru Deep Field and the Subaru/XMM Deep Field (600arcmin^2 each). The angular correlation functions of these LBGs show a clear clustering at both z~4 and 5. The correlation lengths are r_0= 4.1^{+0.2}_{-0.2} and 5.9^{+1.3}_{-1.7} h_{100}^{-1} Mpc (r_0= 5.1^{+1.0}_{-1.1} and 5.9^{+1.3}_{-1.7} h_{100}^{-1} Mpc) for all the detected LBGs (for L>L* LBGs) at z~4 and 5, respectively. These correlation lengths correspond to galaxy-dark matter biases of b_g= 2.9^{+0.1}_{-0.1} and 4.6^{+0.9}_{-1.2} (b_g=3.5^{+0.6}_{-0.7} and 4.6^{+0.9}_{-1.2}), for all the detected LBGs (for L>L^* LBGs) at z~4 and 5, respectively. These results, combined with estimates for z~3 LBGs in the literature, show that the correlation length of L>L^* LBGs is almost constant, ~5 h_{100}^{-1} Mpc, over z~3-5, while the bias monotonically increases with redshift at z>3. We also find that for LBGs at z~4 the clustering amplitude increases with UV-continuum luminosity and with the amount of dust extinction. We estimate the mass of dark halos hosting various kinds of high-z galaxies including LBGs with the analytic model given by Sheth & Tormen (1999). We find that the typical mass of dark halos hosting L>L^* LBGs is about 1x10^{12} h_{70}^{-1}Msol over z~3-5, which is comparable to that of the Milky Way Galaxy. A single dark halo with ~10^{12} h_{70}^{-1} Msol is found to host 0.1-0.3 LBG on average but host about four K-band selected galaxies., Comment: 33 pages, 12 figures, ApJ in press. Paper with high resolution figures is available at http://hikari.astron.s.u-tokyo.ac.jp/~ouchi/work/astroph/SDS_V_VI/SDS_VI.pdf (PDF) (The abstract was reduced by the revision.)

Published
2003
Full Text
View/download PDF

29. Subaru Deep Survey. IV. Discovery of a Large-Scale Structure at Redshift \simeq 5

Author

Shimasaku, K., Ouchi, M., Okamura, S., Kashikawa, N., Doi, M., Furusawa, H., Hamabe, M., Hayashino, T., Kawabata, K., Kimura, M., Kodaira, K., Komiyama, Y., Matsuda, Y., Miyazaki, M., Miyazaki, S., Nakata, F., Ohta, K., Ohyama, Y., Sekiguchi, M., Shioya, Y., Tamura, H., Taniguchi, Y., Yagi, M., Yamada, T., and Yasuda, N.

Subjects
Astrophysics
Abstract

We report the discovery of a large-scale structure of Lyman alpha emitters (LAEs) at z=4.86 based on wide-field imaging with the prime-focus camera (Suprime-Cam) on the Subaru telescope. We observed a 25' x 45' area of the Subaru Deep Field in a narrow band (NB, lambdaC=7126 A and FWHM=73 A) together with R and i'. We isolate from these data 43 LAE candidates down to NB=25.5 mag using color criteria. Follow-up spectroscopy of five candidates suggests the contamination by low-z objects to be ~ 20%. We find that the LAE candidates are clustered in an elongated region on the sky of 20 Mpc in width and 50 Mpc in length at z=4.86, which is comparable in size to present-day large-scale structures (we adopt H0=70 km/s/Mpc, Omega0=0.3, lambda0=0.7). This elongated region includes a circular region of 12 Mpc radius of higher surface overdensity (delta=2), which may be the progenitor of a cluster of galaxies. Assuming this circular region to be a sphere with a spatial overdensity of 2, we compare our observation with predictions by Cold Dark Matter models. We find that an Omega0=0.3 flat model with sigma8=0.9 predicts the number of such spheres consistent with the observed number (one sphere in our survey volume) if the bias parameter of LAEs is b \simeq 6. This value suggests that the typical mass of dark haloes hosting LAEs at z \simeq 5 is of the order of 10^12 Msolar. Such a large mass poses an interesting question about the nature of LAEs., Comment: 4 pages, 4 figures, uses emulateapj5.sty, ApJL, accepted

Published
2003
Full Text
View/download PDF

30. Narrow band imaging in [OIII] and Halpha to search for ICPNe in the Virgo cluster

Author

Arnaboldi, M., Freeman, K. C., Okamura, S., Yasuda, N., Gerhard, O., Napolitano, N. R., Pannella, M., Ando, H., Do, M., Furusawa, H., Hamabe, M., Kimura, M., Kajino, T., Komiyama, Y., Miyazaki, S., Nakata, F., Ouchi, M., Sekiguchi, M., Shimasaku, K., and Yagi, M.

Subjects
Astrophysics
Abstract

We have identified intracluster planetary nebulae in a Virgo cluster core field by imaging with the Subaru Suprime-Cam through two narrow band filters centered at the redshifted wavelengths of the [OIII] $\lambda=5007$ \AA and the H$\alpha$ $\lambda = 6563$ \AA lines; broad-band images in V and R were acquired to check for emission in the adjacent continuum. Emission line objects in Virgo are then selected from the two-color diagram ([OIII] -- Halpha) vs. ([OIII] -- (V+R)), which is calibrated using PNe in M84 (Jacoby et al. 1990). Using both [OIII] and Halpha allows us to distinguish bona-fide planetary nebulae from high redshift emission-line galaxies at the bright end of the [OIII] luminosity function. Spectroscopic observations of a subsample of these objects were made at the TNG and at the VLT, in a region around M84 and in an intracluster field respectively. The observations confirm the efficiency of the combined [OIII]+H$\alpha$ imaging to identify true PNe. We also obtained the first spectrum of an intracluster PN which shows the [OIII] doublet with S/N > 10 and its Halpha emission. From the results based on the spectroscopic follow-up, we derive a lower limit to the fraction of the Virgo cluster light contributed by the intracluster stars at the surveyed position in the cluster core: it amounts to 10%., Comment: 32 pages,11 figures, in press on AJ, February 2003

Published
2002
Full Text
View/download PDF

31. Candidates for Intracluster Planetary Nebulae in the Virgo Cluster based on the Suprime-Cam Narrow-Band Imaging in O[III] and Halpha

Author

Okamura, S., Yasuda, N., Arnaboldi, M., Freeman, K. C., Ando, H., Doi, M., Furusawa, H., Gerhard, O., Hamabe, M., Kimura, M., Kajino, T., Komiyama, Y., Miyazaki, S., Nakata, F., Napolitano, N. R., Ouchi, M., Pannella, M., Sekiguchi, M., Shimasaku, K., and Yagi, M.

Subjects
Astrophysics
Abstract

We have identified 38 candidates of intracluster planetary nebulae (ICPNe) in a $34'\times27'$ field in the core of the Virgo cluster based on the Suprime-Cam imaging through two narrow-band filters centered at the redshifted wavelengths of the [OIII]$\lambda=5007\AA$ and the Halpha \lambda=6563\AA lines. Broad-band images in V and R bands are used to check for any emissions in the adjacent continuum. We describe the method briefly and present the list of intracluster planetary nebulae candidates, together with their finding charts. The ICPN candidates show a highly inhomogeneous distribution, which may suggest an association with the M86-M84 subcluster. Fraction of diffuse intracluster light with respect to total light in galaxies is estimated to be about 10%, leading to an estimate of about 20% for the baryon fraction. Spectroscopic follow up and a wider survey are critical to reveal the nature of intracluster stellar population., Comment: 8 pages, 3 figures, in press on PASJ, December 2002

Published
2002
Full Text
View/download PDF

32. Evolution of Elliptical Galaxies at z >~ 1 Revealed from a Large, Multicolor Sample of Extremely Red Objects

Author

Miyazaki, M., Shimasaku, K., Kodama, T., Okamura, S., Furusawa, H., Ouchi, M., Nakata, F., Doi, M., Hamabe, M., Kimura, M., Komiyama, Y., Miyazaki, S., Nagashima, C., Nagata, T., Nagayama, T., Nakajima, Y., Nakaya, H., Pickles, A. J., Sato, S., Sekiguchi, K., Sekiguchi, M., Sugitani, K., Takata, T., Tamura, M., Yagi, M., and Yasuda, N.

Subjects
Astrophysics
Abstract

We study the evolution of elliptical galaxies at z >~ 1 on the basis of a sample of 247 Extremely Red Objects (EROs) with R-Ks >= 3.35 (AB) and Ks <= 22.1 (AB) constructed from BVRi'z'JHKs multicolor data of a 114 arcmin2 area in the Subaru/XMM Deep Survey Field. By fitting template spectra of old ellipticals (OEs) and young, dusty starbursts (DSs) to the multicolor data, we classify EROs into these two classes and estimate their redshifts. We find that 58% of the EROs in our sample belong to the OE class and that 24% of the OEs are fit by a spectrum having a disk component with the B-band bulge-to-total luminosity ratio of <= 0.9. We compare the observed surface density of OEs with predictions from passive evolution models. We then derive rest-frame B-band luminosity functions (LFs) of OEs in our sample at z=1-1.5 and 1.5-2.5. We find that the LF at z=1-1.5 roughly agrees with the LF of local ellipticals if a dimming of 1.3 mag from z=1.25 to the present epoch is assumed. On the other hand, the amplitude of the LF at z=1.5-2.5 is found to be lower than that of the local LF by a factor of ~ 3 over the whole range of magnitude observed. Taking account of a strong decrease in the number density of morphologically classified early-type galaxies at z >~ 1.5 found by several authors, we conclude that the majority of ellipticals seen at present have not established either a red color or a smooth 1/4-law profile before z ~ 1.5$. (abridged), Comment: 46 pages, 15 PostScript figures. Submitted to ApJ

Published
2002
Full Text
View/download PDF

33. Searching for dark matter halos in the Suprime-Cam 2 sq deg field

Author

Miyazaki, S., Hamana, T., Shimasaku, K., Furusawa, H., Doi, M., Hamabe, M., Imi, K., Kimura, M., Komiyama, Y., Nakata, F., Okada, N., Okamura, S., Ouchi, M., Sekiguchi, M., Yagi, M., and Yasuda, N.

Subjects
Astrophysics
Abstract

We report the first result of weak gravitational lensing survey on a 2.1 sq deg Rc-band image taken with a wide field camera (Suprime-Cam) on the prime focus of 8.2 m Subaru Telescope. The weak lensing mass reconstruction is applied to the data to search for dark matter halos of cluster scale; M >= 10^14 solar mass. The reconstructed convergence field is divided by 1-sigma noise to obtain the signal-to-noise ratio map (S/N-map) of the detection. Local maxima and minima are searched on the S/N-map and the probability distribution function (PDF) of the peaks are created to compare with model predictions. We found excess over noise PDF created from the randomized realization on both positive and negative sides. Negative peaks imply the presence of voids in the dark matter distribution and this is the first report of the detection. Positive peaks, on the other hand, represent the dark matter halos and the number count of the halos on the 2.1 sq deg image is 4.9 +- 2.3 for S/N > 5 where the Gaussian smoothing radius of the convergence map is 1'. The result is consistent with the prediction assuming the Press-Schechter mass function and the NFW halo profile under the cluster normalized CDM cosmology. Although the present statistics is not enough due to the limited field of view, this work demonstrates that dark matter halo count via weak lensing is a promising way to test the paradigm of structure formation and cosmological model., Comment: 4 pages, 3 figures, Accepted for publication in ApJL

Published
2002
Full Text
View/download PDF

34. Cosmic shear statistics in the Suprime-Cam 2.1 sq deg field: Constraints on Omega_m and sigma_8

Author

Hamana, T., Miyazaki, S., Shimasaku, K., Furusawa, H., Doi, M., Hamabe, M., Imi, K., Kimura, M., Komiyama, Y., Nakata, F., Okada, N., Okamura, S., Ouchi, M., Sekiguchi, M., Yagi, M., and Yasuda, N.

Subjects
Astrophysics
Abstract

We present measurements of the cosmic shear correlation in the shapes of galaxies in the Suprime-Cam 2.1 deg^2 R_c-band imaging data. As an estimator of the shear correlation originated from the gravitational lensing, we adopt the aperture mass variance. We detect a non-zero E mode variance on scales between 2 and 40arcmin. We also detect a small but non-zero B mode variance on scales larger than 5arcmin. We compare the measured E mode variance to the model predictions in CDM cosmologies using maximum likelihood analysis. A four-dimensional space is explored, which examines sigma_8, Omega_m, Gamma and zs (a mean redshift of galaxies). We include three possible sources of error: statistical noise, the cosmic variance estimated using numerical experiments, and a residual systematic effect estimated from the B mode variance. We derive joint constraints on two parameters by marginalizing over the two remaining parameters. We obtain an upper limit of Gamma<0.5 for zs>0.9 (68% confidence). For a prior Gamma\in[0.1,0.4] and zs\in[0.6,1.4], we find sigma_8=(0.50_{-0.16}^{+0.35})Omega_m^{-0.37} for flat cosmologies and sigma_8=(0.51_{-0.16}^{+0.29})Omega_m^{-0.34}$ for open cosmologies (95% confidence). If we take the currently popular LCDM model, we obtain a one-dimensional confidence interval on sigma_8 for the 95.4% level, 0.62<\sigma_8<1.32 for zs\in[0.6,1.4]. Information on the redshift distribution of galaxies is key to obtaining a correct cosmological constraint. An independent constraint on Gamma from other observations is useful to tighten the constraint., Comment: 12 pages, 12 figures, accepted for publication in ApJ

Published
2002
Full Text
View/download PDF

35. Subaru Deep Survey II. Luminosity Functions and Clustering Properties of Lya Emitters at z=4.86 in the Subaru Deep Field

Author

Ouchi, M., Shimasaku, K., Furusawa, H., Miyazaki, M., Doi, M., Hamabe, M., Hayashino, T., Kimura, M., Kodaira, K., Komiyama, Y., Matsuda, Y., Miyazaki, S., Nakata, F., Okamura, S., Sekiguchi, M., Shioya, Y., Tamura, H., Taniguchi, Y., Yagi, M., and Yasuda, N.

Subjects
Astrophysics
Abstract

We report on early results from deep and wide-field narrow-band imaging on a 543 arcmin^2 area of the Subaru Deep Field. We find 87 Lya emitters (LAEs) at z=4.86(+/-0.03) which are photometrically selected by a combination of two broad bands (R and i') and one narrow band (NB711; 7126A FWHM=73A). We derive the luminosity functions (LFs) of the LAEs at Lya luminosity and at UV-continuum (1700A) luminosity. The LFs show little evolution between z=3.4 and z=4.86 either in Lya or UV-continuum emission. The amplitude of the LAE LF tends to decline at the bright magnitudes more rapidly than that of the LBG LF at similar redshifts. We calculate the angular correlation function of our LAEs up to ~15 arcmin separations. The angular correlation w(theta) is found to increase with decreasing angular separations, showing a clear signal of clustering. It is also found that the distribution of LAEs shows a large density gradient with a scale of >~15 arcmin, which would indicate the existence of a large-scale structure of LAEs on >~20h^(-1) Mpc scales.We fit the observed correlation function by Aw theta^(-0.8) to find Aw=29arcsec^(0.8). The estimated correlation length is r0=3.5(+/-0.3)h^(-1)Mpc in comoving units (Omega_m=0.3 and Omega_Lambda=0.7), which is slightly larger than the value for z~4 LBGs with i'<26. We calculate the angular correlation function for two sub-samples of the 87 LAEs divided by Lya luminosity, UV-continuum luminosity, and Lya equivalent width (EW). The Lya bright sub-sample shows a larger correlation amplitude than the Lya faint sub-sample, while no significant difference is found for the sub-samples divided by UV-continuum luminosity or EW., Comment: 14 pages, 7 figures, Accepted for publication in ApJ. High resolution versions of Fig. 2 and Fig. 3 are available at http://ichou.astron.s.u-tokyo.ac.jp/~ouchi/work/0202204fig23.tar.gz

Published
2002
Full Text
View/download PDF

36. Completing the census of Lyα emitters at the reionization Epoch

Author

Kashikawa, N, Shimasaku, K, Matsuda, Y, Egami, E, Jiang, L, Nagao, T, Ouchi, M, Malkan, MA, Hattori, T, Ota, K, Taniguchi, Y, Okamura, S, Ly, C, Iye, M, Furusawa, H, Shioya, Y, Shibuya, T, Ishizaki, Y, and Toshikawa, J

Subjects
cosmology: observations, early universe, galaxies: formation, galaxies: high-redshift, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We carried out extended spectroscopic confirmations of Lyα emitters (LAEs) at z = 6.5 and 5.7 in the Subaru Deep Field. Now, the total number of spectroscopically confirmed LAEs is 45 and 54 at z = 6.5 and 5.7, respectively, and at least 81% (70%) of our photometric candidates at z = 6.5 (5.7) have been spectroscopically identified as real LAEs. We made careful measurements of the Lyα luminosity, both photometrically and spectroscopically, to accurately determine the Lyα and rest-UV luminosity functions (LFs). The substantially improved evaluation of the Lyα LF at z = 6.5 shows an apparent deficit from z = 5.7 at least at the bright end, and a possible decline even at the faint end, though small uncertainties remain. The rest-UV LFs at z = 6.5 and 5.7 are in good agreement, at least at the bright end, in clear contrast to the differences seen in the Lyα LF. These results imply an increase in the neutral fraction of the intergalactic medium from z = 5.7 to 6.5. The rest-frame equivalent width (EW0) distribution at z = 6.5 seems to be systematically smaller than z = 5.7, and it shows an extended tail toward larger EW0. The bright end of the rest-UV LF can be reproduced from the observed Lyα LF and a reasonable EW0-UV luminosity relation. Integrating this rest-UV LF provides the first measurement of the contribution of LAEs to the photon budget required for reionization. The derived UV LF suggests that the fractional contribution of LAEs to the photon budget among Lyman break galaxies significantly increases toward faint magnitudes. Low-luminosity LAEs could dominate the ionizing photon budget, though this inference depends strongly on the uncertain faint-end slope of the Lyα LF. © 2011. The American Astronomical Society. All rights reserved.

Published
2011

38. The SVBABU/XMM-Newton deep survey (SXDS). V. Optically faint variable object survey

Author

Morokuma, T, Doi, M, Yasuda, N, Akiyama, M, Sekiguchi, K, Furusawa, H, Ueda, Y, Totani, T, Oda, T, Nagao, T, Kashikawa, N, Murayama, T, Ouchi, M, Watson, MG, Richmond, MW, Lidman, C, Perlmutter, S, Spadafora, AL, Aldering, G, Wang, L, Hook, IM, and Knop, RA

Subjects
galaxies : active, stars : variables : other, supernovae : general, surveys, astro-ph, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present our survey for optically faint variable objects using multiepoch (8-10 epochs over 2-4 years) i′-band imaging data obtained with Subaru Suprime-Cam over 0.918 deg2 in the Subaru/XMM-Newton Deep Field (SXDF). We found 1040 optically variable objects by image subtraction for all the combinations of images at different epochs. This is the first statistical sample of variable objects at depths achieved with 8-10 m class telescopes or the Hubble Space Telescope. The detection limit for variable components is i′vari ∼ 25.5 mag. These variable objects were classified into variable stars, supernovae (SNe), and active galactic nuclei (AGNs), based on the optical morphologies, magnitudes, colors, and optical-mid-infrared colors of the host objects, spatial offsets of variable components from the host objects, and light curves. Detection completeness was examined by simulating light curves for periodic and irregular variability. We detected optical variability for 36% ± 2% (51% ± 3% for a bright sample with i′ < 24.4 mag) of X-ray sources in the field. Number densities of variable objects as functions of time intervals Δt and variable component magnitudes i′vari are obtained. Number densities of variable stars, SNe, and AGNs are 120, 489, and 579 objects deg-2, respectively. Bimodal distributions of variable stars in the color-magnitude diagrams indicate that the variable star sample consists of bright (V ∼ 22 mag) blue variable stars of the halo population and faint (V ∼ 23.5 mag) red variable stars of the disk population. There are a few candidates of RR Lyrae providing a possible number density of ∼10-2 kpc-3 at a distance of >150 kpc from the Galactic center. © 2008. The American Astronomical Society. All rights reserved.

Published
2008

39. Clustering of Lyman break galaxies at z = 4 and 5 in the Subaru Deep Field: Luminosity dependence of the correlation function slope

Author

Kashikawa, N, Yoshida, M, Shimasaku, K, Nagashima, M, Yahagi, H, Ouchi, M, Matsuda, Y, Malkan, MA, Doi, M, Iye, M, Ajiki, M, Akiyama, M, Ando, H, Aoki, K, Furusawa, H, Hayashino, T, Iwamuro, F, Karoji, H, Kobayashi, N, Kodaira, K, Kodama, T, Komiyama, Y, Miyazaki, S, Mizumoto, Y, Morokuma, T, Motohara, K, Murayama, T, Nagao, T, Nariai, K, Ohta, K, Okamura, S, Sasaki, T, Sato, Y, Sekiguchi, K, Shioya, Y, Tamura, H, Taniguchi, Y, Umemura, M, Yamada, T, and Yasuda, N

Subjects
cosmology : observations, cosmology : theory, galaxies : high-redshift, large-scale structure of universe, astro-ph, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We explored the clustering properties of Lyman break galaxies at z = 4 and 5 with an angular two-point correlation function on the basis of the very deep and wide Subaru Deep Field data. We confirmed the previous result that the clustering strength of LBGs depends on the UV luminosity in the sense that brighter LBGs are more strongly clustered. In addition, we found an apparent dependence of the correlation function slope on UV luminosity for LBGs at both z = 4 and 5. More luminous LBGs have a steeper correlation function. The bias parameter was found to be a scale-dependent function for bright LBGs, whereas it appears to be almost scale-independent for faint LBGs. Luminous LBGs have a higher bias at smaller angular scales, which decreases as the scale increases. To compare these observational results, we constructed numerical mock LBG catalogs based on a semianalytic model of hierarchical clustering combined with high-resolution N-body simulation, carefully mimicking the observational selection effects. The luminosity functions and the overall correlation functions for LBGs at z = 4 and 5 predicted by this mock catalog were found to be almost consistent with the observation. The observed dependence of the clustering on UV luminosity was not reproduced by the model, unless subsamples of distinct halo mass were considered. That is, LBGs belonging to more massive dark halos had steeper and larger amplitude correlation functions. With this model, we found that LBG multiplicity in massive dark halos amplifies the clustering strength at small scales, which steepens the correlation function. The hierarchical clustering model could therefore be reconciled with the observed luminosity dependence of the correlation function if there is a tight correlation between UV luminosity and halo mass. Our finding that the slope of the correlation function depends on luminosity could be an indication that massive dark halos hosted multiple bright LBGs. © 2006. The American Astronomical Society. All rights reserved.

Published
2006

40. Combining the CLAUDS and HSC-SSP surveys U plus grizy(+YJHK(s)) photometry and photometric redshifts for 18M galaxies in the 20 deg(2) of the HSC-SSP Deep and ultraDeep fields

Author

Desprez, G., Picouet, V., Moutard, T., Arnouts, S., Sawicki, M., Coupon, J., Gwyn, S., Chen, L., Huang, J., Golob, A., Furusawa, H., Ikeda, H., Paltani, S., Cheng, C., Hartley, W., Hsieh, B. C., Ilbert, O., Kauffmann, O. B., McCracken, H. J., Shuntov, M., Tanaka, M., Toft, S., Tresse, L., Weaver, J. R., Desprez, G., Picouet, V., Moutard, T., Arnouts, S., Sawicki, M., Coupon, J., Gwyn, S., Chen, L., Huang, J., Golob, A., Furusawa, H., Ikeda, H., Paltani, S., Cheng, C., Hartley, W., Hsieh, B. C., Ilbert, O., Kauffmann, O. B., McCracken, H. J., Shuntov, M., Tanaka, M., Toft, S., Tresse, L., and Weaver, J. R.

Abstract

We present the combination of the Canada-France-Hawaii Telescope (CHFT) Large Area U-bands Deep Survey (CLAUDS) and the Hyper-Suprime-Cam (HSC) Subaru Strategic Program (HSC-SSP) data over their four deep fields. We provide photometric catalogs for u, u* (CFHT-MegaCam), g, r, i, z, and y (Subaru-HSC) bands over similar to 20 deg(2), complemented in two fields by data from the Visible and Infrared Survey Telescope for Astronomy (VISTA) Deep Extragalactic Observations (VIDEO) survey and the UltraVISTA survey, thus extending the wavelength coverage toward near-infrared with VIRCAM Y, J, H, and K-s observations over 5.5 deg(2). The extraction of the photometry was performed with two different softwares: the HSC pipeline hscPipe and the standard and robust SExtractor software. Photometric redshifts were computed with template-fitting methods using the new Phosphoros code for the hscPipe photometry and the well-known Le Phare code for the SExtractor photometry. The products of these methods were compared with each other in detail. We assessed their quality using the large spectroscopic sample available in those regions, together with photometry and photometric redshifts from COSMOS2020, the latest version of the Cosmic Evolution Survey catalogs. We find that both photometric data sets are in good agreement in Ugrizy down to magnitude similar to 26, and to magnitude similar to 24.5 in the YJHK(s) bands. We achieve good performance for the photometric redshifts, reaching precisions of sigma(NMAD) less than or similar to 0.04 down to m(i) similar to 25, even using only the CLAUDS and HSC bands. At the same magnitude limit, we measured an outlier fraction of eta less than or similar to 10% when using the Ugrizy bands, and down to eta less than or similar to 6% when considering near-infrared data. The hscPipe plus Phosphoros pipeline performs slightly worse in terms of photometric-redshifts precision and outlier fraction than its SExtractor plus Le Phare counterpart, which

Published
2023

42. Combining the CLAUDS and HSC-SSP surveys

Author

Desprez, G., primary, Picouet, V., additional, Moutard, T., additional, Arnouts, S., additional, Sawicki, M., additional, Coupon, J., additional, Gwyn, S., additional, Chen, L., additional, Huang, J., additional, Golob, A., additional, Furusawa, H., additional, Ikeda, H., additional, Paltani, S., additional, Cheng, C., additional, Hartley, W., additional, Hsieh, B. C., additional, Ilbert, O., additional, Kauffmann, O. B., additional, McCracken, H. J., additional, Shuntov, M., additional, Tanaka, M., additional, Toft, S., additional, Tresse, L., additional, and Weaver, J. R., additional

Published
2023
Full Text
View/download PDF

43. The host galaxy of a fast radio burst

Author

Keane, E.F., Johnston, S., Bhandari, S., Barr, E., Bhat, N.D.R., Burgay, M., Caleb, M., Flynn, C., Jameson, A., Kramer, M., Petroff, E., Possenti, A., van Straten, W., Bailes, M., Burke-Spolaor, S., Eatough, R.P., Stappers, B.W., Totani, T., Honma, M., Furusawa, H., Hattori, T., Morokuma, T., Niino, Y., Sugai, H., Terai, T., Tominaga, N., Yamasaki, S., Yasuda, N., Allen, R., Cooke, J., Jencson, J., Kasliwal, M.M., Kaplan, D.L., Tingay, S.J., Williams, A., Wayth, R., Chandra, P., Perrodin, D., Berezina, M., Mickaliger, M., and Bassa, C.

Subjects
Telescope -- Usage -- Research, Pulsars -- Observations -- Research, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

In recent years, millisecond-duration radio signals originating in distant galaxies appear to have been discovered in the so-called fast radio bursts (1-9). These signals are dispersed according to a precise physical law and this dispersion is a key observable quantity, which, in tandem with a redshift measurement, can be used for fundamental physical investigations (10,11). Every fast radio burst has a dispersion measurement, but none before now have had a redshift measurement, because of the difficulty in pinpointing their celestial coordinates. Here we report the discovery of a fast radio burst and the identification of a fading radio transient lasting ~6 days after the event, which we use to identify the host galaxy; we measure the galaxy's redshift to be z = 0.492 ± 0.008. The dispersion measure and redshift, in combination, provide a direct measurement of the cosmic density of ionized baryons in the intergalactic medium of [Ω.sub.IGM] = 4.9 ± 1.3 per cent, in agreement with the expectation from the Wilkinson Microwave Anisotropy Probe (12), and including all of the so-called 'missing baryons'. The ~6-day radio transient is largely consistent with the radio afterglow of a short γ-ray burst (13), and its existence and timescale do not support progenitor models such as giant pulses from pulsars, and supernovae. This contrasts with the interpretation (8) of another recently discovered fast radio burst, suggesting that there are at least two classes of bursts., As part of the SUrvey for Pulsars and Extragalactic Radio Bursts (SUPERB) project at the Parkes radio telescope, we perform real-time searches of the sky at high time resolution (see [...]

Published
2016

45. Subaru/XMM-Newton Deep Survey (SXDS)

Author

The SXDS Team, Sekiguchi, K., Akiyama, M., Furusawa, H., Simpson, C., Takata, T., Ueda, Y., Watson, M. W., Burton, W. B., editor, Kuijpers, J. M. E., editor, van den Heuvel, E. P. J., editor, van der Laan, H., editor, Appenzeler, I., editor, Bahcall, J. N., editor, Bertola, F., editor, Cassinelli, J. P., editor, Cesarsky, C. J., editor, Engvold, O., editor, McCray, R., editor, Murdin, P. G., editor, Pacini, F., editor, Radhakrishnan, V., editor, Sato, K., editor, Shu, F. H., editor, Somov, B. V., editor, Sunyaev, R. A., editor, Tanaka, Y., editor, Tremaine, S., editor, Weiss, N. O., editor, and Plionis, Manolis, editor

Published
2004
Full Text
View/download PDF

47. Worldwide trends in hypertension prevalence and progress in treatment and control from 1990 to 2019: a pooled analysis of 1201 population-representative studies with 104 million participants

Author

Zhou, B, Carrillo-Larco, Rm, Danaei, G, Riley, Lm, Paciorek, Cj, Stevens, Ga, Gregg, Ew, Bennett, Je, Solomon, B, Singleton, Rk, Sophiea, Mk, Iurilli, Mlc, Lhoste, Vpf, Cowan, Mj, Savin, S, Woodward, M, Balanova, Y, Cifkova, R, Damasceno, A, Elliott, P, Farzadfar, F, He, J, Ikeda, N, Kengne, Ap, Khang, Yh, Kim, Hc, Laxmaiah, A, Lin, Hh, Maira, Pm, Miranda, Jj, Neuhauser, H, Sundstrom, J, Varghese, C, Widyahening, Is, Zdrojewski, T, Ezzati, M, Abarca-Gomez, L, Abdeen, Za, Rahim, Hfa, Abu-Rmeileh, Nm, Acosta-Cazares, B, Adams, Rj, Aekplakorn, W, Afsana, K, Afzal, S, Agdeppa, Ia, Aghazadeh-Attari, J, Aguilar-Salinas, Ca, Agyemang, C, Ahmad, Na, Ahmadi, A, Ahmadi, N, Ahmadizar, F, Ahmed, Sh, Ahrens, W, Ajlouni, K, Al-Raddadi, R, Alarouj, M, Albuhairan, F, Aldhukair, S, Ali, Mm, Alkandari, A, Alkerwi, A, Allin, K, Aly, E, Amarapurkar, Dn, Amougou, N, Amouyel, P, Andersen, Lb, Anderssen, Sa, Anjana, Rm, Ansari-Moghaddam, A, Ansong, D, Aounallah-Skhiri, H, Araujo, J, Ariansen, I, Aris, T, Arku, Re, Arlappa, N, Aryal, Kk, Aspelund, T, Assah, Fk, Assuncao, Mcf, Auvinen, J, Avdicova, M, Azevedo, A, Azimi-Nezhad, M, Azizi, F, Azmin, M, Babu, Bv, Bahijri, S, Balakrishna, N, Bamoshmoosh, M, Banach, M, Banadinovic, M, Bandosz, P, Banegas, Jr, Baran, J, Barbagallo, Cm, Barcelo, A, Barkat, A, Barreto, M, Barros, Ajd, Barros, Mvg, Bartosiewicz, A, Basit, A, Bastos, Jld, Bata, I, Batieha, Am, Batyrbek, A, Baur, La, Beaglehole, R, Belavendra, A, Ben Romdhane, H, Benet, M, Benson, Ls, Berkinbayev, S, Bernabe-Ortiz, A, Bettiol, H, Bezerra, J, Bhagyalaxmi, A, Bhargava, Sk, Bia, D, Biasch, K, Lele, Ecb, Bikbov, Mm, Bista, B, Bjerregaard, P, Bjertness, E, Bjertness, Mb, Bjorkelund, C, Bloch, Kv, Blokstra, A, Bo, S, Bobak, M, Boeing, H, Boggia, Jg, Boissonnet, Cp, Bojesen, Se, Bongard, V, Bonilla-Vargas, A, Bopp, M, Borghs, H, Bovet, P, Boyer, Cb, Braeckman, L, Brajkovich, I, Branca, F, Breckenkamp, J, Brenner, H, Brewster, Lm, Briceno, Y, Brito, M, Bruno, G, Bueno-de-Mesquita, Hb, Bueno, G, Bugge, A, Burns, C, Bursztyn, M, de Leon, Ac, Cacciottolo, J, Cameron, C, Can, G, Candido, Apc, Capanzana, Mv, Capkova, N, Capuano, E, Capuano, V, Cardoso, Vc, Carlsson, Ac, Carvalho, J, Casanueva, Ff, Censi, L, Cervantes-Loaiza, M, Chadjigeorgiou, Ca, Chamukuttan, S, Chan, Aw, Chan, Q, Chaturvedi, Hk, Chaturvedi, N, Chee, Ml, Chen, Cj, Chen, Ff, Chen, Hs, Chen, Sh, Chen, Zm, Cheng, Cy, Cheraghian, B, Dekkaki, Ic, Chetrit, A, Chien, Kl, Chiolero, A, Chiou, St, Chirita-Emandi, A, Chirlaque, Md, Cho, B, Christensen, K, Christofaro, Dg, Chudek, J, Cinteza, E, Claessens, F, Clarke, J, Clays, E, Cohen, E, Concin, H, Cooper, C, Coppinger, Tc, Costanzo, S, Cottel, D, Cowell, C, Craig, Cl, Crampin, Ac, Crujeiras, Ab, Cruz, Jj, Csilla, S, Cui, Lf, Cureau, Fv, Cuschieri, S, D'Arrigo, G, D'Orsi, E, Dallongeville, J, Dankner, R, Dantoft, Tm, Dauchet, L, Davletov, K, De Backer, G, De Bacquer, D, De Curtis, A, de Gaetano, G, De Henauw, S, de Oliveira, Pd, De Ridder, D, De Smedt, D, Deepa, M, Deev, Ad, Degennaro, V, Delisle, H, Demarest, S, Dennison, E, Deschamps, V, Dhimal, M, Di Castelnuovo, Af, Dias-da-Costa, Js, Diaz, A, Dickerson, Tt, Dika, Z, Djalalinia, S, Htp, Do, Dobson, Aj, Donfrancesco, C, Donoso, Sp, Doring, A, Dorobantu, M, Dorr, M, Doua, K, Dragano, N, Drygas, W, Duante, Ca, Duboz, P, Duda, Rb, Dulskiene, V, Dushpanova, A, Dzakula, A, Dzerve, V, Dziankowska-Zaborszczyk, E, Eddie, R, Eftekhar, E, Eggertsen, R, Eghtesad, S, Eiben, G, Ekelund, U, El-Khateeb, M, El Ati, J, Eldemire-Shearer, D, Eliasen, M, Elosua, R, Erasmus, Rt, Erbel, R, Erem, C, Eriksen, L, Eriksson, Jg, Escobedo-de la Pena, J, Eslami, S, Esmaeili, A, Evans, A, Faeh, D, Fakhretdinova, Aa, Fall, Ch, Faramarzi, E, Farjam, M, Fattahi, Mr, Fawwad, A, Felix-Redondo, Fj, Felix, Sb, Ferguson, Ts, Fernandes, Ra, Fernandez-Berges, D, Ferrante, D, Ferrao, T, Ferrari, M, Ferrario, Mm, Ferreccio, C, Ferreira, Hs, Ferrer, E, Ferrieres, J, Figueiro, Th, Fink, G, Fischer, K, Foo, Lh, Forsner, M, Fouad, Hm, Francis, Dk, Grego, Franco, Frikke-Schmidt, R, Frontera, G, Fuchs, Fd, Fuchs, Sc, Fujita, Y, Fumihiko, M, Furdela, V, Furer, A, Furusawa, T, Gaciong, Z, Galbarczyk, A, Galenkamp, H, Galvano, F, Gao, Jl, Gao, P, Garcia-de-la-Hera, M, Garcia, P, Gareta, D, Garnett, Sp, Gaspoz, Jm, Gasull, M, Gazzinelli, A, Gehring, U, Geleijnse, Jm, George, R, Ghanbari, A, Ghasemi, E, Gheorghe-Fronea, Of, Ghimire, A, Gialluisi, A, Giampaoli, S, Gieger, C, Gill, Tk, Giovannelli, J, Gironella, G, Giwercman, A, Gkiouras, K, Goldberg, M, Goldsmith, Ra, Gomez, Lf, Gomula, A, da Silva, Bgc, Goncalves, H, Goncalves, M, Gonzalez-Chica, Da, Gonzalez-Gross, M, Gonzalez-Rivas, Jp, Gonzalez-Villalpando, C, Gonzalez-Villalpando, Me, Gonzalez, Ar, Gorbea, Mb, Gottrand, F, Graff-Iversen, S, Grafnetter, D, Grajda, A, Grammatikopoulou, Mg, Gregor, Rd, Grodzicki, T, Grosso, G, Gruden, G, Df, Gu, Guan, Op, Gudmundsson, Ef, Gudnason, V, Guerrero, R, Guessous, I, Guimaraes, Al, Gulliford, Mc, Gunnlaugsdottir, J, Gunter, Mj, Gupta, Pc, Gupta, R, Gureje, O, Gurzkowska, B, Gutierrez, L, Gutzwiller, F, Ha, S, Hadaegh, F, Haghshenas, R, Hakimi, H, Halkjaer, J, Hambleton, Ir, Hamzeh, B, Hange, D, Hanif, Aam, Hantunen, S, Hao, J, Hardman, Cm, Kumar, Rh, Hashemi-Shahri, Sm, Hata, J, Haugsgjerd, T, Hayes, Aj, Yn, He, Heier, M, Hendriks, Me, Henrique, Rd, Henriques, A, Cadena, Lh, Herrala, S, Heshmat, R, Hill, Ag, Sy, Ho, Sc, Ho, Hobbs, M, Holdsworth, M, Homayounfar, R, Dinc, Gh, Horimoto, Arvr, Hormiga, Cm, Horta, Bl, Houti, L, Howitt, C, Htay, Tt, Htet, As, Htike, Mmt, Yh, Hu, Huerta, Jm, Huhtaniemi, It, Huiart, L, Huisman, M, Husseini, As, Huybrechts, I, Hwalla, N, Iacoviello, L, Iannone, Ag, Ibrahim, Mm, Wong, Ni, Ikram, Ma, Iotova, V, Irazola, Ve, Ishida, T, Isiguzo, Gc, Islam, M, Islam, Sms, Iwasaki, M, Jackson, Rt, Jacobs, Jm, Jaddou, Hy, Jafar, T, James, K, Jamrozik, K, Janszky, I, Janus, E, Jarvelin, Mr, Jasienska, G, Jelakovic, A, Jelakovic, B, Jennings, G, Jha, Ak, Jiang, Cq, Jimenez, Ro, Jockel, Kh, Joffres, M, Johansson, M, Jokelainen, Jj, Jonas, Jb, Jorgensen, T, Joshi, P, Joukar, F, Jozwiak, J, Juolevi, A, Jurak, G, Juresa, V, Kaaks, R, Kafatos, A, Kajantie, Eo, Kalmatayeva, Z, Kalpourtzi, N, Kalter-Leibovici, O, Kampmann, Fb, Kannan, S, Karaglani, E, Karhus, Ll, Karki, Kb, Katibeh, M, Katz, J, Kauhanen, J, Kaur, P, Kavousi, M, Kazakbaeva, Gm, Keil, U, Boker, Lk, Keinanen-Kiukaanniemi, S, Kelishadi, R, Kemper, Hcg, Keramati, M, Kerimkulova, A, Kersting, M, Key, T, Khader, Ys, Khalili, D, Khaw, Kt, Kheiri, B, Kheradmand, M, Khosravi, A, Kiechl-Kohlendorfer, U, Kiechl, S, Killewo, J, Kim, Dw, Kim, J, Klakk, H, Klimek, M, Klumbiene, J, Knoflach, M, Kolle, E, Kolsteren, P, Kontto, Jp, Korpelainen, R, Korrovits, P, Kos, J, Koskinen, S, Kouda, K, Kowlessur, S, Koziel, S, Kratenova, J, Kriaucioniene, V, Kristensen, Pl, Krokstad, S, Kromhout, D, Kruger, Hs, Kubinova, R, Kuciene, R, Kujala, Um, Kulaga, Z, Kumar, Rk, Kurjata, P, Kusuma, Ys, Kutsenko, V, Kuulasmaa, K, Kyobutungi, C, Laatikainen, T, Lachat, C, Laid, Y, Lam, Th, Landrove, O, Lanska, V, Lappas, G, Larijani, B, Latt, Ts, Le Coroller, G, Bao, Kln, Le, THUY DUNG, Lee, J, Lehmann, N, Lehtimaki, T, Lemogoum, D, Levitt, Ns, Yp, Li, Lilly, Cl, Lim, Wy, Lima-Costa, Mf, Lin, X, Lin, Yt, Lind, L, Lingam, V, Linneberg, A, Lissner, L, Litwin, M, Wc, Lo, Loit, Hm, Lopez-Garcia, E, Lopez, T, Lotufo, Pa, Lozano, Je, Lovrencic, Il, Lukrafka, Jl, Luksiene, D, Lundqvist, A, Lundqvist, R, Lunet, N, Lustigova, M, Luszczki, E, Gs, Ma, Ma, J, Machado-Coelho, Gll, Machado-Rodrigues, Am, Macia, E, Macieira, Lm, Madar, Aa, Maggi, S, Magliano, Dj, Magriplis, E, Mahasampath, G, Maire, B, Majer, M, Makdisse, M, Malekzadeh, F, Malekzadeh, R, Malhotra, R, Mallikharjuna, K, Malyutina, Sk, Maniego, Lv, Manios, Y, Mann, Ji, Mansour-Ghanaei, F, Manzato, E, Marcil, A, Margozzini, P, Marild, Sb, Glavic, Mm, Marques-Vidal, P, Marques, Lp, Marrugat, J, Martorell, R, Mascarenhas, Lp, Matasin, M, Mathiesen, Eb, Mathur, P, Matijasevich, A, Matlosz, P, Matsha, Te, Mavrogianni, C, Mbanya, Jcn, Posso, Ajm, Mcfarlane, Sr, Mcgarvey, St, Mclachlan, S, Mclean, Rm, Mclean, Sb, Mcnulty, Ba, Benchekor, Sm, Medzioniene, J, Mehdipour, P, Mehlig, K, Mehrparvar, Ah, Meirhaeghe, A, Meisinger, C, Montano, Cm, Menezes, Amb, Menon, Gr, Mereke, A, Meshram, Ii, Metspalu, A, Meyer, He, Mi, J, Michels, N, Mikkel, K, Milkowska, K, Miller, Jc, Minderico, Cs, Mini, Gk, Mirjalili, Mr, Mirrakhimov, E, Misigoj-Durakovic, M, Modesti, Pa, Moghaddam, Ss, Mohajer, B, Mohamed, Mk, Mohamed, Sf, Mohammad, K, Mohammadi, Mr, Mohammadi, Z, Mohammadifard, N, Mohammadpourhodki, R, Mohan, V, Mohanna, S, Yusoff, Mfm, Mohebbi, I, Mohebi, F, Moitry, M, Mollehave, Lt, Molnar, D, Momenan, A, Mondo, Ck, Monterrubio-Flores, E, Monyeki, Kdk, Moon, Js, Moosazadeh, M, Moreira, Lb, Morejon, A, Moreno, La, Morgan, K, Moschonis, G, Mossakowska, M, Mostafa, A, Mostafavi, Sa, Mota, J, Motlagh, Me, Motta, J, Moura-dos-Santos, Ma, Mridha, Mk, Msyamboza, Kp, Tt, Mu, Muhihi, Aj, Muiesan, Ml, Muller-Nurasyid, M, Murphy, N, Mursu, J, Musa, Ki, Milanovic, Sm, Musil, V, Mustafa, N, Nabipour, I, Naderimagham, S, Nagel, G, Naidu, Bm, Najafi, F, Nakamura, H, Namesna, J, Nang, Eek, Nangia, Vb, Narake, S, Ndiaye, Nc, Neal, Wa, Nejatizadeh, A, Nenko, I, Neovius, M, Neuhauser, Hk, Nguyen, Ct, Nguyen, Nd, Nguyen, Qv, Nguyen, Qn, Nieto-Martinez, Re, Niiranen, Tj, Nikitin, Yp, Ninomiya, T, Nishtar, S, Njelekela, Ma, Noale, M, Noboa, Oa, Noorbala, Aa, Norat, T, Nordendahl, M, Nordestgaard, Bg, Noto, D, Nowak-Szczepanska, N, Al Nsour, M, Nunes, B, O'Neill, Tw, O'Reilly, D, Ochimana, C, Oda, E, Odili, An, Oh, K, Ohara, K, Ohtsuka, R, Olie, V, Olinto, Mta, Oliveira, Io, Omar, Ma, Onat, A, Ong, Sk, Ono, Lm, Ordunez, P, Ornelas, R, Ortiz, Pj, Osmond, C, Ostojic, Sm, Ostovar, A, Otero, Ja, Overvad, K, Owusu-Dabo, E, Paccaud, Fm, Padez, C, Pahomova, E, de Paiva, Km, Pajak, A, Palli, D, Palmieri, L, Pan, Wh, Panda-Jonas, S, Panza, F, Paoli, M, Papandreou, D, Park, Sw, Park, S, Parnell, Wr, Parsaeian, M, Pasquet, P, Patel, Nd, Pavlyshyn, H, Pecin, I, Pednekar, Ms, Pedro, Jm, Peer, N, Peixoto, Sv, Peltonen, M, Pereira, Ac, Peres, Kgda, Peres, Ma, Peters, A, Petkeviciene, J, Peykari, N, Pham, St, Pichardo, Rn, Pigeot, I, Pikhart, H, Pilav, A, Pilotto, L, Pitakaka, F, Piwonska, A, Pizarro, An, Plans-Rubio, P, Polasek, O, Porta, M, Poudyal, A, Pourfarzi, F, Pourshams, A, Poustchi, H, Pradeepa, R, Price, Aj, Price, Jf, Providencia, R, Puhakka, Se, Puiu, M, Punab, M, Qasrawi, Rf, Qorbani, M, Queiroz, D, Bao, Tq, Radic, I, Radisauskas, R, Rahimikazerooni, S, Rahman, M, Raitakari, O, Raj, M, Rakhimova, Em, Rao, Sr, Ramachandran, A, Ramos, E, Rampal, L, Rampal, S, Reina, Dar, Rarra, V, Rech, Cr, Redon, J, Reganit, Pfm, Regecova, V, Revilla, L, Rezaianzadeh, A, Ribeiro, R, Riboli, E, Richter, A, Rigo, F, de Wit, Tfr, Ritti-Dias, Rm, Robitaille, C, Rodriguez-Artalejo, F, Rodriguez-Perez, Md, Rodriguez-Villamizar, La, Roggenbuck, U, Rojas-Martinez, R, Romaguera, D, Romeo, El, Rosengren, A, Roy, Jgr, Rubinstein, A, Ruidavets, Jb, Ruiz-Betancourt, Bs, Ruiz-Castell, M, Rusakova, Ia, Russo, P, Rutkowski, M, Sabanayagam, C, Sabbaghi, H, Sachdev, Hs, Sadjadi, A, Safarpour, Ar, Safi, S, Safiri, S, Saidi, O, Sakarya, S, Saki, N, Salanave, B, Martinez, Es, Salmeron, D, Salomaa, V, Salonen, Jt, Salvetti, M, Sanchez-Abanto, J, Sans, S, Santos, Da, Santos, Is, Santos, Lc, Santos, Mp, Santos, R, Saramies, Jl, Sardinha, Lb, Sarganas, G, Sarrafzadegan, N, Sathish, T, Saum, Ku, Savva, S, Sawada, N, Sbaraini, M, Scazufca, M, Schaan, Bd, Schargrodsky, H, Schipf, S, Schmidt, Co, Schnohr, P, Schottker, B, Schramm, S, Schultsz, C, Schutte, Ae, Sebert, S, Sein, Aa, Sen, A, Senbanjo, Io, Sepanlou, Sg, Servais, J, Shalnova, Sa, Shamah-Levy, T, Shamshirgaran, M, Shanthirani, Cs, Sharafkhah, M, Sharma, Sk, Shaw, Je, Shayanrad, A, Shayesteh, Aa, Shi, Zm, Shibuya, K, Shimizu-Furusawa, H, Shin, Dw, Shirani, M, Shiri, R, Shrestha, N, Si-Ramlee, K, Siani, A, Siantar, R, Sibai, Am, Silva, Crd, Silva, Das, Simon, M, Simons, J, Simons, La, Sjostrom, M, Slowikowska-Hilczer, J, Slusarczyk, P, Smeeth, L, Hk, So, Soares, Fc, Sobngwi, E, Soderberg, S, Soemantri, A, Sofat, R, Solfrizzi, V, Somi, Mh, Sonestedt, E, Song, Y, Sorensen, Tia, Sorgjerd, Ep, Soric, M, Jerome, Cs, Soumare, A, Sparboe-Nilsen, B, Sparrenberger, K, Staessen, Ja, Starc, G, Stavreski, B, Steene-Johannessen, J, Stehle, P, Stein, Ad, Stergiou, Gs, Stessman, J, Stieber, J, Stockl, D, Stocks, T, Stokwiszewski, J, Stronks, K, Strufaldi, Mw, Suka, M, Sun, Ca, Sung, Yt, Suriyawongpaisal, P, Rg, Sy, Syddall, He, Sylva, Rc, Szklo, M, Tai, Es, Tammesoo, Ml, Tamosiunas, A, Tan, Ej, Tang, X, Tanser, F, Tao, Y, Tarawneh, Mr, Tarqui-Mamani, Cb, Taylor, A, Taylor, J, Tebar, Wr, Tell, Gs, Tello, T, Tham, Yc, Thankappan, Kr, Theobald, H, Theodoridis, X, Thijs, L, Thinggaard, M, Thomas, N, Thorand, B, Thuesen, Bh, Timmermans, Ej, Tjandrarini, Dh, Tjonneland, A, Toft, U, Tolonen, Hk, Tolstrup, Js, Topbas, M, Topor-Madry, R, Tormo, Mj, Tornaritis, Mj, Torrent, M, Torres-Collado, L, Touloumi, G, Traissac, P, Triantafyllou, A, Trichopoulos, D, Trichopoulou, A, Trinh, Oth, Trivedi, A, Tshepo, L, Tsugane, S, Tuliakova, Am, Tulloch-Reid, Mk, Tullu, F, Tuomainen, Tp, Tuomilehto, J, Turley, Ml, Twig, G, Tynelius, P, Tzourio, C, Ueda, P, Ugel, E, Ulmer, H, Uusitalo, Hmt, Valdivia, G, Valvi, D, van Dam, Rm, van den Born, Bj, Van der Heyden, J, van der Schouw, Yt, Van Herck, K, Minh, Hv, Van Schoor, Nm, van Valkengoed, Igm, van Zutphen, Em, Vanderschueren, D, Vanuzzo, D, Varbo, A, Vasan, Sk, Vega, T, Veidebaum, T, Velasquez-Melendez, G, Veronesi, G, Verschuren, Wmm, Verstraeten, R, Victora, Cg, Viet, L, Villalpando, S, Vineis, P, Vioque, J, Virtanen, Jk, Visvikis-Siest, S, Viswanathan, B, Vlasoff, T, Vollenweider, P, Voutilainen, A, Wade, An, Walton, J, Wambiya, Eoa, Bebakar, Wmw, Mohamud, Wnw, Wanderley, Rd, Wang, Md, Wang, Nl, Wang, Q, Wang, Xj, Wang, Yx, Wang, Yw, Wannamethee, Sg, Wareham, N, Wei, Wb, Weres, A, Werner, B, Whincup, Ph, Widhalm, K, Wiecek, A, Wilks, Rj, Willeit, J, Willeit, P, Williams, Ea, Wilsgaard, T, Wojtyniak, B, Wong-McClure, Ra, Wong, A, Wong, Ty, Woo, J, Fc, Wu, Sl, Wu, Wyszynska, J, Hq, Xu, Xu, L, Yaacob, Na, Yan, Wl, Yang, L, Yang, Xg, Yang, Y, Yasuharu, T, Xw, Ye, Yiallouros, Pk, Yoosefi, M, Yoshihara, A, You, Sl, Younger-Coleman, No, Yusoff, Af, Zainuddin, Aa, Zakavi, Sr, Zamani, F, Zambon, S, Zampelas, A, Zapata, Me, Zaw, Kk, Zejglicova, K, Vrkic, Tz, Zeng, Y, Zhang, Lx, Zhang, Zy, Zhao, D, Zhao, Mh, Zhen, Sq, Zheng, Yf, Zholdin, B, Zhu, D, Zins, M, Zitt, E, Zocalo, Y, Zoghlami, N, Cisneros, Jz, Borghs, Herman, Claessens, Frank, Staessen, Jan, Thijs, Lutgarde, Vanderschueren, Dirk, Zhang, Zhen-Yu, Imperial Coll London, Harvard TH Chan Sch Publ Hlth, WHO, Univ Calif Berkeley, Univ New South Wales, Natl Med Res Ctr Therapy & Prevent Med, Charles Univ Prague, Thomayer Hosp, Eduardo Mondlane Univ, Noncommunicable Dis Res Ctr, Tulane Univ, Natl Inst Biomed Innovat Hlth & Nutr, South African Med Res Council, Seoul Natl Univ, Yonsei Univ, ICMR Natl Inst Nutr, Natl Taiwan Univ, Pontificia Univ Catolica Chile, Univ Peruana Cayetano Heredia, Robert Koch Inst, Uppsala Univ, Univ Indonesia, Med Univ Gdansk, Univ Ghana, Caja Costarricense Seguro Social, Al Quds Univ, Qatar Univ, Birzeit Univ, Inst Mexicano Seguro Social, Flinders Univ S Australia, Mahidol Univ, BRAC Univ, Univ Copenhagen, Copenhagen Univ Hosp, Food & Nutr Res Inst, Urmia Univ Med Sci, Inst Nacl Ciencias Med & Nutr Salvador Zubiran, Univ Amsterdam, Minist Hlth, Modeling Hlth Res Ctr, Shahid Sadoughi Univ Med Sci, Erasmus MC, Univ Oslo, Leibniz Inst Prevent Res & Epidemiol BIPS, Natl Ctr Diabet Endocrinol & Genet, King Abdulaziz Univ, Dasman Diabet Inst, Aldara Hosp & Med Ctr, King Abdullah Int Med Res Ctr, Luxembourg Inst Hlth, Bispebjerg, Frederiksberg Univ Hosp, WHO Reg Off Eastern Mediterranean, Bombay Hosp & Med Res Ctr, CNRS, Univ Lille, Lille Univ Hosp, Western Norway Univ Appl Sci, Norwegian Sch Sport Sci, Madras Diabet Res Fdn, Zahedan Univ Med Sci, Kwame Nkrumah Univ Sci & Technol, Natl Inst Publ Hlth, Univ Porto, Norwegian Inst Publ Hlth, Univ Massachusetts, Abt Associates Inc, Univ Iceland, Univ Yaounde I, Univ Fed Pelotas, Univ Oulu, Oulu Univ Hosp, Banska Bystr Reg Author Publ Hlth, Neyshabur Univ Med Sci, Res Inst Endocrine Sci, Indian Council Med Res, Univ Sci & Technol, Med Univ Lodz, Univ Zagreb, Univ Autonoma Madrid CIBERESP, Univ Rzeszow, Univ Palermo, Pan Amer Hlth Org, Mohammed V Univ Rabat, Natl Inst Hlth Doutor Ricardo Jorge, NOVA Univ Lisbon, Univ Pernambuco, Baqai Inst Diabetol & Endocrinol, Universidade Federal de Santa Catarina (UFSC), Dalhousie Univ, Jordan Univ Sci & Technol, Al Farabi Kazakh Natl Univ, Univ Sydney, Univ Auckland, Christian Med Coll Vellore, Univ Tunis El Manar, Cafam Univ Fdn, Univ Utah, Kazakh Natl Med Univ, Lithuanian Univ Hlth Sci, Universidade de São Paulo (USP), BJ Med Coll, Sunder Lal Jain Hosp, Univ Republica, Univ Strasbourg, Inst Med Res & Med Plant Studies, Ufa Eye Res Inst, Nepal Hlth Res Council, Univ Southern Denmark, Univ Gothenburg, Universidade Federal do Rio de Janeiro (UFRJ), Natl Inst Publ Hlth & Environm, Univ Turin, UCL, German Inst Human Nutr, Ctr Educ Med & Invest Clin, Toulouse Univ, Univ Zurich, Univ Hosp KU Leuven, Unisante, Univ Ghent, Univ Cent Venezuela, Bielefeld Univ, German Canc Res Ctr, Univ Andres, Inst Politecn Lisboa, Univ Zaragoza, Univ Coll Copenhagen, Munster Technol Univ, Hadassah Univ, Univ La Laguna, Univ Malta, Canadian Fitness & Lifestyle Res Inst, Istanbul Univ Cerrahpasa, Univ Fed Juiz de Fora, Gaetano Fucito Hosp, Karolinska Inst, Santiago Compostela Univ, Council Agr Res & Econ, Res & Educ Inst Child Hlth, India Diabet Res Fdn, Duke NUS Med Sch, ICMR Natl Inst Med Stat, Singapore Eye Res Inst, Acad Sinica, Capital Inst Pediat, Duke Univ, Kailuan Gen Hosp, Univ Oxford, Ahvaz Jundishapur Univ Med Sci, Gertner Inst Epidemiol & Hlth Policy Res, Univ Bern, Minist Hlth & Welf, Victor Babes Univ Med & Pharm Timisoara, CIBER Epidemiol & Salud Publ, Universidade Estadual Paulista (UNESP), Med Univ Silesia, Carol Davila Univ Med & Pharm, Katholieke Univ Leuven, STAT Canada, Agcy Prevent & Social Med, Univ Southampton, IRCCS Neuromed, Inst Pasteur, Malawi Epidemiol & Intervent Res Unit, CIBEROBN, Univ Autonoma Madrid, Univ Debrecen, Univ Fed Rio Grande do Sul, CNR, Geneva Univ Hosp, Innovating Hlth Int, Univ Montreal, Sciensano, French Publ Hlth Agcy, Mediterranea Cardioctr, Univ Vale Rio dos Sinos, Natl Council Sci & Tech Res, Minist Hlth & Med Educ, Natl Inst Nutr, Univ Queensland, Ist Super Sanita, Univ Cuenca, Helmholtz Zentrum Munchen, Univ Med Greifswald, Minist Sante & Hyg Publ, Univ Hosp Dusseldorf, Natl Inst Cardiol, IRL 3189 ESS, Beth Israel Deaconess Med Ctr, Harvard Med Sch, Scuola Super Sant Anna, Univ Latvia, Minist Hlth & Med Serv, Hormozgan Univ Med Sci, Univ Tehran Med Sci, Univ Skovde, Natl Inst Nutr & Food Technol, Univ West Indies, Inst Hosp Mar Invest Med, CIBERCV, Univ Stellenbosch, Univ Duisburg Essen, Karadeniz Tech Univ, Univ Helsinki, Mashhad Univ Med Sci, Rafsanjan Univ Med Sci, Queens Univ Belfast, Tabriz Univ Med Sci, Fasa Univ Med Sci, Shiraz Univ Med Sci, Baqai Med Univ, Ctr Salud Villanueva Norte, Hosp Don Benito Villanueva de la Serena, Univ Insubria, Univ Fed Alagoas, Swiss Trop & Publ Hlth Inst, Univ Basel, Univ Tartu, Univ Sains Malaysia, Umea Univ, Universidade Federal de São Paulo (UNIFESP), Hosp Univ Son Espases, Hosp Clin Porto Alegre, Kindai Univ, Kyoto Univ, I Horbachevsky Ternopil Natl Med Univ, Tel Aviv Univ, Hebrew Univ Jerusalem, Med Univ Warsaw, Jagiellonian Univ Med Coll, Univ Catania, Peking Univ, Wuqu Kawoq, Africa Hlth Res Inst, Univ Geneva, Universidade Federal de Minas Gerais (UFMG), Univ Utrecht, Wageningen Univ, Med Res Fdn, BP Koirala Inst Hlth Sci, Univ Adelaide, Lund Univ, Aristotle Univ Thessaloniki, Inst Natl Sante & Rech Med, Paris Univ, Pontificia Univ Javeriana, PASs Hirszfeld Inst Immunol & Expt Therapy, Univ Agostinho Neto, Univ Politecn Madrid, Int Clin Res Ctr, Ctr Estudios Diabet AC, Univ Autonoma Santo Domingo, Natl Inst Hyg Epidemiol & Microbiol, Inst Clin & Expt Med, Childrens Mem Hlth Inst, Int Hellen Univ, Natl Ctr Cardiovasc Dis, Iceland Heart Assoc, Univ ICESI, Univ Estadual Montes Claros, Kings Coll London, Int Agcy Res Canc, Healis Sekhsaria Inst Publ Hlth, Eternal Heart Care Ctr & Res Inst, Univ Ibadan, Inst Clin Effectiveness & Hlth Policy, Natl Hlth Insurance Serv, Prevent Metab Disorders Res Ctr, Danish Canc Soc Res Ctr, Kermanshah Univ Med Sci, BRAC James P Grant Sch Publ Hlth, Univ Eastern Finland, Beijing Inst Ophthalmol, Universidade Federal de Pernambuco (UFPE), Kyushu Univ, Univ Bergen, Chinese Ctr Dis Control & Prevent, Joep Lange Inst, Chron Dis Res Ctr, Univ Hong Kong, Chinese Univ Hong Kong, Univ Western Australia, French Natl Res Inst Sustainable Dev, Celal Bayar Univ, Fdn Oftalmol Santander, Univ Oran 1, Minist Hlth & Sports, Sante Publ France, Vrije Univ Amsterdam Med Ctr, Amer Univ Beirut, Cairo Univ, Med Univ Varna, Univ Tokyo, Universidade Estadual de Maringá (UEM), Hosp Sick Children, Deakin Univ, Tokyo Metropolitan Inst Gerontol, Hadassah Univ Med Ctr, Norwegian Univ Sci & Technol, Univ Melbourne, Univ Hosp Ctr Zagreb, Heart Fdn, Guangzhou 12th Hosp, Univ Eugenio Maria Hostos, Simon Fraser Univ, Inst Mol & Clin Ophthalmol Basel, WHO Country Off, Guilan Univ Med Sci, Univ Opole, Finnish Inst Hlth & Welf, Univ Ljubljana, Univ Crete, Natl & Kapodistrian Univ Athens, Sree Chitra Tirunal Inst Med Sci & Technol, Harokopio Univ, Maharajgunj Med Campus, Aarhus Univ, Johns Hopkins Bloomberg Sch Publ Hlth, Natl Inst Epidemiol, Univ Munster, Israel Ctr Dis Control, Res Inst Primordial Prevent Noncommunicable Dis, Amsterdam UMC Publ Hlth Res Inst, Kyrgyz State Med Acad, Res Inst Child Nutr, Shahid Beheshti Univ Med Sci, Univ Cambridge, Mazandaran Univ Med Sci, Hypertens Res Ctr, Med Univ Innsbruck, VASCage, Muhimbili Univ Hlth & Allied Sci, Natl Canc Ctr, Univ Coll South Denmark, Oulu Deaconess Inst Fdn, Tartu Univ Clin, Kansai Med Univ, Minist Hlth & Wellness, Univ Groningen, North West Univ, Amrita Inst Med Sci, All India Inst Med Sci, African Populat & Hlth Res Ctr, Minist Salud Publ, Sahlgrens Acad, Endocrinol & Metab Res Ctr, Univ Publ Hlth, Natl Univ Singapore, Tampere Univ Hosp, Tampere Univ, Univ Douala, Univ Cape Town, West Virginia Univ, Oswaldo Cruz Fdn Rene Rachou Res Inst, Shanghai Inst Nutr & Hlth, Taipei Med Univ, Natl Inst Hlth Dev, Univ San Martin de Porres, Consejeria Sanidad Junta Castilla & Leon, Univ Fed Ciencias Saude Porto Alegre, Norrbotten Cty Council, Univ Fed Ouro Preto, Univ Coimbra, Coimbra Univ Hosp Ctr, Inst Neurosci Natl Res Council, Baker Heart & Diabet Inst, Agr Univ Athens, Hosp Israelita Albert Einstein, SB RAS Fed Res Ctr Inst Cytol & Genet, Univ Otago, Univ Padua, Gothenburg Univ, Univ Rijeka, Lausanne Univ Hosp, Univ Lausanne, Escola Nacl Saude Publ Sergio Arouca, Emory Univ, Univ Estadual Centro Oeste, UiT Arctic Univ Norway, ICMR Natl Ctr Dis Informat & Res, Cape Peninsula Univ Technol, Inst Conmemorat Gorgas Estudios Salud, Brown Univ, Univ Edinburgh, Univ Coll Dublin, Inst Nutr Ctr Amer & Panama, Univ Lisbon, Womens Social & Hlth Studies Fdn, Univ Firenze, Ain Shams Univ, Psychiat & Psychol Res Canter, Isfahan Cardiovasc Res Ctr, Strasbourg Univ Hosp, Univ Pecs, Mulago Hosp, Univ Limpopo, Univ Med Sci Cienfuegos, Royal Coll Surgeons Ireland, La Trobe Univ, Int Inst Mol & Cell Biol, Dept Publ Hlth, Univ Brescia, Ludwig Maximilians Univ Munchen, Croatian Inst Publ Hlth, Univ Kebangsaan Malaysia, Bushehr Univ Med Sci, Ulm Univ, Dept Stat, Kobe Univ, Suraj Eye Inst, Natl Inst Hyg & Epidemiol, Univ Med & Pharm Ho Chi Minh City, Natl Hosp Endocrinol, Hanoi Med Univ, LifeDoc Hlth, Univ Turku, Heartfile, Eastern Mediterranean Publ Hlth Network, Univ Manchester, Tachikawa Gen Hosp, Univ Abuja, Korea Ctr Dis Control & Prevent, Japan Wildlife Res Ctr, Istanbul Univ, Univ Fed Parana, Univ Madeira, Univ Novi Sad, Osteoporosis Res Ctr, UniSante, Inst Canc Res Prevent & Clin Network, Inst Clin & Sci Ophthalmol & Acupuncture Jonas, IRCCS Ente Osped Specializzato Gastroenterol S de, Zayed Univ, Catholic Univ Daegu, Jivandeep Hosp, Ctr Invest Saude Angola, Griffith Univ, Natl Dent Care Ctr Singapore, Vietnam Natl Heart Inst, Clin Med Avanzada Dr Abel Gonzalez, Univ Sarajevo, Cardiovasc Prevent Ctr Udine, Publ Hlth Agcy Catalonia, Univ Split, Ardabil Univ Med Sci, London Sch Hyg & Trop Med, Alborz Univ Med Sci, Pure Earth, Univ Putra Malaysia, Univ Malaya, Sotiria Hosp, Univ Valencia, Univ Philippines, Slovak Acad Sci, Univ San Martin Porres, Minas Gerais State Secretariat Hlth, CS S Agustin Ibsalut, Amsterdam Inst Global Hlth & Dev, Univ Nove de Julho, Publ Hlth Agcy Canada, Canarian Hlth Serv, Univ Ind Santander, Assoc Calabrese Epatol, Sahlgrens Univ Hosp, Sitaram Bhartia Inst Sci & Res, Koc Univ, Natl Inst Hlth, Catalan Dept Hlth, South Karelia Social & Hlth Care Dist, German Ctr Cardiovasc Res, McMaster Univ, Hosp Italiano Buenos Aires, Acad Med Ctr Univ Amsterdam, George Inst Global Hlth, Ctr Oral Hlth Serv & Res Mid Norway, Lagos State Univ, Nippon Med Sch, Sungkyunkwan Univ, Shahrekord Univ Med Sci, Finnish Inst Occupat Hlth, Publ Hlth Promot & Dev Org, St Vincents Hosp, Diponegoro Univ, Univ Bari, Inst Reg Sante Publ, Univ Bordeaux, Oslo Metropolitan Univ, Univ Leuven, Univ Bonn, Natl Inst Hyg, Jikei Univ, Fu Jen Catholic Univ, Natl Stat Off, Univ Lincoln, Cent Univ Kerala, Amsterdam Publ Hlth Res Inst, Natl Inst Hlth Res & Dev, Hlth Serv Murcia, Inst Invest Sanitaria Illes Balears, CIBER Epidemiol Salud Publ, Hellen Hlth Fdn, Govt Med Coll, Sefako Makgatho Hlth Sci Univ, Addis Ababa Univ, Israel Def Forces Med Corps, Univ Ctr Occidental Lisandro Alvarado, Univ Tampere, Icahn Sch Med Mt Sinai, Hanoi Univ Publ Hlth, Inst Trop Med, Univ Miguel Hernandez, Univ Lorraine, North Karelia Ctr Publ Hlth, Univ Witwatersrand, Inst Med Res, Capital Med Univ, Xinjiang Med Univ, Shanghai Educ Dev Co Ltd, Orebro Univ, St Georges Univ London, Med Univ Vienna, Komfo Anokye Teaching Hosp, Minist Agr & Rural Affairs, Fudan Univ, Shanghai Educ Dev, Univ Cyprus, Niigata Univ, Iran Univ Med Sci, Ctr Estudios Nutr Infantil, Jiangsu Prov Ctr Dis Control & Prevent, Sun Yat Sen Univ, West Kazakhstan Med Univ, Inner Mongolia Med Univ, Éco-Anthropologie (EAE), Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Universitas Indonesia (UI ), Montpellier Interdisciplinary center on Sustainable Agri-food systems (Social and nutritional sciences) (UMR MoISA), Centre de Coopération Internationale en Recherche Agronomique pour le Développement (Cirad)-Institut de Recherche pour le Développement (IRD)-Centre International de Hautes Etudes Agronomiques Méditerranéennes - Institut Agronomique Méditerranéen de Montpellier (CIHEAM-IAMM), Centre International de Hautes Études Agronomiques Méditerranéennes (CIHEAM)-Centre International de Hautes Études Agronomiques Méditerranéennes (CIHEAM)-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Interactions Gène-Environnement en Physiopathologie Cardio-Vasculaire (IGE-PCV), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Lorraine (UL), Clinicum, Research Programs Unit, Johan Eriksson / Principal Investigator, Department of General Practice and Primary Health Care, University of Helsinki, HUS Helsinki and Uusimaa Hospital District, Department of Public Health, Tampere University, Clinical Medicine, Department of Clinical Chemistry, Eye Centre, Wellcome Trust, Epidemiology, Radiology & Nuclear Medicine, Éco-Anthropologie (EA), Cohortes épidémiologiques en population (CONSTANCES), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Paris-Saclay-Université Paris Cité (UPCité), Université Paris Cité (UPCité), Centre International de Hautes Études Agronomiques Méditerranéennes (CIHEAM)-Centre International de Hautes Études Agronomiques Méditerranéennes (CIHEAM)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut Agro - Montpellier SupAgro, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro), Epidemiology and Data Science, APH - Aging & Later Life, APH - Societal Participation & Health, Public and occupational health, APH - Health Behaviors & Chronic Diseases, VU University medical center, APH - Personalized Medicine, Psychiatry, APH - Mental Health, Bin Zhou, Rodrigo M Carrillo-Larco, Goodarz Danaei, Leanne M Riley, Christopher J Paciorek, Gretchen A Stevens, Edward W Gregg, James E Bennett, Bethlehem Solomon, Rosie K Singleton, Marisa K Sophiea, Maria Lc Iurilli, Victor Pf Lhoste, Melanie J Cowan, Stefan Savin, Mark Woodward, Yulia Balanova, Renata Cifkova, Albertino Damasceno, Paul Elliott, Farshad Farzadfar, Jiang He, Nayu Ikeda, Andre P Kengne, Young-Ho Khang, Hyeon Chang Kim, Avula Laxmaiah, Hsien-Ho Lin, Paula Margozzini Maira, J Jaime Miranda, Hannelore Neuhauser, Johan Sundström, Cherian Varghese, Indah S Widyahening, Tomasz Zdrojewski, Leandra Abarca-Gómez, Ziad A Abdeen, Hanan F Abdul Rahim, Niveen M Abu-Rmeileh, Benjamin Acosta-Cazares, Robert J Adams, Wichai Aekplakorn, Kaosar Afsana, Shoaib Afzal, Imelda A Agdeppa, Javad Aghazadeh-Attari, Carlos A Aguilar-Salinas, Charles Agyemang, Noor Ani Ahmad, Ali Ahmadi, Naser Ahmadi, Nastaran Ahmadi, Fariba Ahmadizar, Soheir H Ahmed, Wolfgang Ahrens, Kamel Ajlouni, Rajaa Al-Raddadi, Monira Alarouj, Fadia AlBuhairan, Shahla AlDhukair, Mohamed M Ali, Abdullah Alkandari, Ala'a Alkerwi, Kristine Allin, Eman Aly, Deepak N Amarapurkar, Norbert Amougou, Philippe Amouyel, Lars Bo Andersen, Sigmund A Anderssen, Ranjit Mohan Anjana, Alireza Ansari-Moghaddam, Daniel Ansong, Hajer Aounallah-Skhiri, Joana Araújo, Inger Ariansen, Tahir Aris, Raphael E Arku, Nimmathota Arlappa, Krishna K Aryal, Thor Aspelund, Felix K Assah, Maria Cecília F Assunção, Juha Auvinen, Mária Avdićová, Ana Azevedo, Mohsen Azimi-Nezhad, Fereidoun Azizi, Mehrdad Azmin, Bontha V Babu, Suhad Bahijri, Nagalla Balakrishna, Mohamed Bamoshmoosh, Maciej Banach, Maja Banadinović, Piotr Bandosz, José R Banegas, Joanna Baran, Barbagallo Carlo Maria, Alberto Barceló, Amina Barkat, Marta Barreto, Aluisio Jd Barros, Mauro Virgílio Gomes Barros, Anna Bartosiewicz, Abdul Basit, Joao Luiz D Bastos, Iqbal Bata, Anwar M Batieha, Assembekov Batyrbek, Louise A Baur, Robert Beaglehole, Antonisamy Belavendra, Habiba Ben Romdhane, Mikhail Benet, Lowell S Benson, Salim Berkinbayev, Antonio Bernabe-Ortiz, Gailute Bernotiene, Heloísa Bettiol, Jorge Bezerra, Aroor Bhagyalaxmi, Santosh K Bhargava, Daniel Bia, Katia Biasch, Elysée Claude Bika Lele, Mukharram M Bikbov, Bihungum Bista, Peter Bjerregaard, Espen Bjertness, Marius B Bjertness, Cecilia Björkelund, Katia V Bloch, Anneke Blokstra, Simona Bo, Martin Bobak, Heiner Boeing, Jose G Boggia, Carlos P Boissonnet, Stig E Bojesen, Vanina Bongard, Alice Bonilla-Vargas, Matthias Bopp, Herman Borghs, Pascal Bovet, Christopher B Boyer, Lutgart Braeckman, Imperia Brajkovich, Francesco Branca, Juergen Breckenkamp, Hermann Brenner, Lizzy M Brewster, Yajaira Briceño, Miguel Brito, Graziella Bruno, H Bas Bueno-de-Mesquita, Gloria Bueno, Anna Bugge, Con Burns, Michael Bursztyn, Antonio Cabrera de León, Joseph Cacciottolo, Christine Cameron, Günay Can, Ana Paula C Cândido, Mario V Capanzana, Naděžda Čapková, Eduardo Capuano, Vincenzo Capuano, Viviane C Cardoso, Axel C Carlsson, Joana Carvalho, Felipe F Casanueva, Laura Censi, Marvin Cervantes-Loaiza, Charalambos A Chadjigeorgiou, Snehalatha Chamukuttan, Angelique W Chan, Queenie Chan, Himanshu K Chaturvedi, Nish Chaturvedi, Miao Li Chee, Chien-Jen Chen, Fangfang Chen, Huashuai Chen, Shuohua Chen, Zhengming Chen, Ching-Yu Cheng, Bahman Cheraghian, Imane Cherkaoui Dekkaki, Angela Chetrit, Kuo-Liong Chien, Arnaud Chiolero, Shu-Ti Chiou, Adela Chirita-Emandi, María-Dolores Chirlaque, Belong Cho, Kaare Christensen, Diego G Christofaro, Jerzy Chudek, Eliza Cinteza, Frank Claessens, Janine Clarke, Els Clays, Emmanuel Cohen, Hans Concin, Cyrus Cooper, Tara C Coppinger, Simona Costanzo, Dominique Cottel, Chris Cowell, Cora L Craig, Amelia C Crampin, Ana B Crujeiras, Juan J Cruz, Semánová Csilla, Liufu Cui, Felipe V Cureau, Sarah Cuschieri, Graziella D'Arrigo, Eleonora d'Orsi, Jean Dallongeville, Rachel Dankner, Thomas M Dantoft, Luc Dauchet, Kairat Davletov, Guy De Backer, Dirk De Bacquer, Amalia De Curtis, Giovanni de Gaetano, Stefaan De Henauw, Paula Duarte de Oliveira, David De Ridder, Delphine De Smedt, Mohan Deepa, Alexander D Deev, Vincent Jr DeGennaro, Hélène Delisle, Stefaan Demarest, Elaine Dennison, Valérie Deschamps, Meghnath Dhimal, Augusto F Di Castelnuovo, Juvenal Soares Dias-da-Costa, Alejandro Diaz, Ty T Dickerson, Zivka Dika, Shirin Djalalinia, Ha Tp Do, Annette J Dobson, Chiara Donfrancesco, Silvana P Donoso, Angela Döring, Maria Dorobantu, Marcus Dörr, Kouamelan Doua, Nico Dragano, Wojciech Drygas, Charmaine A Duante, Priscilla Duboz, Rosemary B Duda, Virginija Dulskiene, Anar Dushpanova, Aleksandar Džakula, Vilnis Dzerve, Elzbieta Dziankowska-Zaborszczyk, Ricky Eddie, Ebrahim Eftekhar, Robert Eggertsen, Sareh Eghtesad, Gabriele Eiben, Ulf Ekelund, Mohammad El-Khateeb, Jalila El Ati, Denise Eldemire-Shearer, Marie Eliasen, Roberto Elosua, Rajiv T Erasmus, Raimund Erbel, Cihangir Erem, Louise Eriksen, Johan G Eriksson, Jorge Escobedo-de la Peña, Saeid Eslami, Ali Esmaeili, Alun Evans, David Faeh, Albina A Fakhretdinova, Caroline H Fall, Elnaz Faramarzi, Mojtaba Farjam, Mohammad Reza Fattahi, Asher Fawwad, Francisco J Felix-Redondo, Stephan B Felix, Trevor S Ferguson, Romulo A Fernandes, Daniel Fernández-Bergés, Daniel Ferrante, Thomas Ferrao, Marika Ferrari, Marco M Ferrario, Catterina Ferreccio, Haroldo S Ferreira, Eldridge Ferrer, Jean Ferrieres, Thamara Hubler Figueiró, Günther Fink, Krista Fischer, Leng Huat Foo, Maria Forsner, Heba M Fouad, Damian K Francis, Maria do Carmo Franco, Ruth Frikke-Schmidt, Guillermo Frontera, Flavio D Fuchs, Sandra C Fuchs, Yuki Fujita, Matsuda Fumihiko, Viktoriya Furdela, Ariel Furer, Takuro Furusawa, Zbigniew Gaciong, Andrzej Galbarczyk, Henrike Galenkamp, Fabio Galvano, Jingli Gao, Pei Gao, Manoli Garcia-de-la-Hera, Pablo Garcia, Dickman Gareta, Sarah P Garnett, Jean-Michel Gaspoz, Magda Gasull, Andrea Gazzinelli, Ulrike Gehring, Johanna M Geleijnse, Ronnie George, Ali Ghanbari, Erfan Ghasemi, Oana-Florentina Gheorghe-Fronea, Anup Ghimire, Alessandro Gialluisi, Simona Giampaoli, Christian Gieger, Tiffany K Gill, Jonathan Giovannelli, Glen Gironella, Aleksander Giwercman, Konstantinos Gkiouras, Marcel Goldberg, Rebecca A Goldsmith, Luis F Gomez, Aleksandra Gomula, Helen Gonçalves, Mauer Gonçalves, Bruna Gonçalves Cordeiro da Silva, David A Gonzalez-Chica, Marcela Gonzalez-Gross, Juan P González-Rivas, Clicerio González-Villalpando, María-Elena González-Villalpando, Angel R Gonzalez, Mariano Bonet Gorbea, Frederic Gottrand, Sidsel Graff-Iversen, Dušan Grafnetter, Aneta Grajda, Maria G Grammatikopoulou, Ronald D Gregor, Tomasz Grodzicki, Giuseppe Grosso, Gabriella Gruden, Dongfeng Gu, Ong Peng Guan, Elias F Gudmundsson, Vilmundur Gudnason, Ramiro Guerrero, Idris Guessous, Andre L Guimaraes, Martin C Gulliford, Johanna Gunnlaugsdottir, Marc J Gunter, Prakash C Gupta, Rajeev Gupta, Oye Gureje, Beata Gurzkowska, Laura Gutierrez, Felix Gutzwiller, Seongjun Ha, Farzad Hadaegh, Rosa Haghshenas, Hamid Hakimi, Jytte Halkjær, Ian R Hambleton, Behrooz Hamzeh, Dominique Hange, Abu Am Hanif, Sari Hantunen, Jie Hao, Carla Menêses Hardman, Rachakulla Hari Kumar, Seyed Mohammad Hashemi-Shahri, Jun Hata, Teresa Haugsgjerd, Alison J Hayes, Yuna He, Margit Heier, Marleen Elisabeth Hendriks, Rafael Dos Santos Henrique, Ana Henriques, Leticia Hernandez Cadena, Herqutanto, Sauli Herrala, Ramin Heshmat, Allan G Hill, Sai Yin Ho, Suzanne C Ho, Michael Hobbs, Michelle Holdsworth, Reza Homayounfar, Gonul Horasan Dinc, Andrea Rvr Horimoto, Claudia M Hormiga, Bernardo L Horta, Leila Houti, Christina Howitt, Thein Thein Htay, Aung Soe Htet, Maung Maung Than Htike, Yonghua Hu, José María Huerta, Ilpo Tapani Huhtaniemi, Laetitia Huiart, Martijn Huisman, Abdullatif S Husseini, Inge Huybrechts, Nahla Hwalla, Licia Iacoviello, Anna G Iannone, Mohsen M Ibrahim, Norazizah Ibrahim Wong, M Arfan Ikram, Violeta Iotova, Vilma E Irazola, Takafumi Ishida, Godsent C Isiguzo, Muhammad Islam, Sheikh Mohammed Shariful Islam, Masanori Iwasaki, Rod T Jackson, Jeremy M Jacobs, Hashem Y Jaddou, Tazeen Jafar, Kenneth James, Konrad Jamrozik, Imre Janszky, Edward Janus, Marjo-Riitta Jarvelin, Grazyna Jasienska, Ana Jelaković, Bojan Jelaković, Garry Jennings, Anjani Kumar Jha, Chao Qiang Jiang, Ramon O Jimenez, Karl-Heinz Jöckel, Michel Joffres, Mattias Johansson, Jari J Jokelainen, Jost B Jonas, Torben Jørgensen, Pradeep Joshi, Farahnaz Joukar, Jacek Jóżwiak, Anne Juolevi, Gregor Jurak, Vesna Jureša, Rudolf Kaaks, Anthony Kafatos, Eero O Kajantie, Zhanna Kalmatayeva, Natasa Kalpourtzi, Ofra Kalter-Leibovici, Freja B Kampmann, Srinivasan Kannan, Eva Karaglani, Line L Kårhus, Khem B Karki, Marzieh Katibeh, Joanne Katz, Jussi Kauhanen, Prabhdeep Kaur, Maryam Kavousi, Gyulli M Kazakbaeva, Ulrich Keil, Lital Keinan Boker, Sirkka Keinänen-Kiukaanniemi, Roya Kelishadi, Han Cg Kemper, Maryam Keramati, Alina Kerimkulova, Mathilde Kersting, Timothy Key, Yousef Saleh Khader, Davood Khalili, Kay-Tee Khaw, Bahareh Kheiri, Motahareh Kheradmand, Alireza Khosravi, Ursula Kiechl-Kohlendorfer, Stefan Kiechl, Japhet Killewo, Dong Wook Kim, Jeongseon Kim, Heidi Klakk, Magdalena Klimek, Jurate Klumbiene, Michael Knoflach, Elin Kolle, Patrick Kolsteren, Jukka P Kontto, Raija Korpelainen, Paul Korrovits, Jelena Kos, Seppo Koskinen, Katsuyasu Kouda, Sudhir Kowlessur, Slawomir Koziel, Jana Kratenova, Vilma Kriaucioniene, Peter Lund Kristensen, Steiner Krokstad, Daan Kromhout, Herculina S Kruger, Ruzena Kubinova, Renata Kuciene, Urho M Kujala, Zbigniew Kulaga, R Krishna Kumar, Pawel Kurjata, Yadlapalli S Kusuma, Vladimir Kutsenko, Kari Kuulasmaa, Catherine Kyobutungi, Tiina Laatikainen, Carl Lachat, Youcef Laid, Tai Hing Lam, Orlando Landrove, Vera Lanska, Georg Lappas, Bagher Larijani, Tint Swe Latt, Gwenaëlle Le Coroller, Khanh Le Nguyen Bao, Tuyen D Le, Jeannette Lee, Jeonghee Lee, Nils Lehmann, Terho Lehtimäki, Daniel Lemogoum, Naomi S Levitt, Yanping Li, Christa L Lilly, Wei-Yen Lim, M Fernanda Lima-Costa, Xu Lin, Yi-Ting Lin, Lars Lind, Vijaya Lingam, Allan Linneberg, Lauren Lissner, Mieczyslaw Litwin, Wei-Cheng Lo, Helle-Mai Loit, Esther Lopez-Garcia, Tania Lopez, Paulo A Lotufo, José Eugenio Lozano, Iva Lukačević Lovrenčić, Janice L Lukrafka, Dalia Luksiene, Annamari Lundqvist, Robert Lundqvist, Nuno Lunet, Michala Lustigová, Edyta Luszczki, Guansheng Ma, Jun Ma, George Ll Machado-Coelho, Aristides M Machado-Rodrigues, Enguerran Macia, Luisa M Macieira, Ahmed A Madar, Stefania Maggi, Dianna J Magliano, Emmanuella Magriplis, Gowri Mahasampath, Bernard Maire, Marjeta Majer, Marcia Makdisse, Fatemeh Malekzadeh, Reza Malekzadeh, Rahul Malhotra, Kodavanti Mallikharjuna Rao, Sofia K Malyutina, Lynell V Maniego, Yannis Manios, Jim I Mann, Fariborz Mansour-Ghanaei, Enzo Manzato, Anie Marcil, Staffan B Mårild, Mihalea Marinović Glavić, Pedro Marques-Vidal, Larissa Pruner Marques, Jaume Marrugat, Reynaldo Martorell, Luis P Mascarenhas, Marija Matasin, Ellisiv B Mathiesen, Prashant Mathur, Alicia Matijasevich, Piotr Matlosz, Tandi E Matsha, Christina Mavrogianni, Jean Claude N Mbanya, Anselmo J Mc Donald Posso, Shelly R McFarlane, Stephen T McGarvey, Stela McLachlan, Rachael M McLean, Scott B McLean, Breige A McNulty, Sounnia Mediene Benchekor, Jurate Medzioniene, Parinaz Mehdipour, Kirsten Mehlig, Amir Houshang Mehrparvar, Aline Meirhaeghe, Christa Meisinger, Carlos Mendoza Montano, Ana Maria B Menezes, Geetha R Menon, Alibek Mereke, Indrapal I Meshram, Andres Metspalu, Haakon E Meyer, Jie Mi, Nathalie Michels, Kairit Mikkel, Karolina Milkowska, Jody C Miller, Cláudia S Minderico, G K Mini, Mohammad Reza Mirjalili, Erkin Mirrakhimov, Marjeta Mišigoj-Duraković, Pietro A Modesti, Sahar Saeedi Moghaddam, Bahram Mohajer, Mostafa K Mohamed, Shukri F Mohamed, Kazem Mohammad, Mohammad Reza Mohammadi, Zahra Mohammadi, Noushin Mohammadifard, Reza Mohammadpourhodki, Viswanathan Mohan, Salim Mohanna, Muhammad Fadhli Mohd Yusoff, Iraj Mohebbi, Farnam Mohebi, Marie Moitry, Line T Møllehave, Dénes Molnár, Amirabbas Momenan, Charles K Mondo, Eric Monterrubio-Flores, Kotsedi Daniel K Monyeki, Jin Soo Moon, Mahmood Moosazadeh, Leila B Moreira, Alain Morejon, Luis A Moreno, Karen Morgan, George Moschonis, Malgorzata Mossakowska, Aya Mostafa, Seyed-Ali Mostafavi, Jorge Mota, Mohammad Esmaeel Motlagh, Jorge Motta, Marcos André Moura-Dos-Santos, Malay K Mridha, Kelias P Msyamboza, Thet Thet Mu, Alfa J Muhihi, Maria L Muiesan, Martina Müller-Nurasyid, Neil Murphy, Jaakko Mursu, Kamarul Imran Musa, Sanja Musić Milanović, Vera Musil, Norlaila Mustafa, Iraj Nabipour, Shohreh Naderimagham, Gabriele Nagel, Balkish M Naidu, Farid Najafi, Harunobu Nakamura, Jana Námešná, Ei Ei K Nang, Vinay B Nangia, Sameer Narake, Ndeye Coumba Ndiaye, William A Neal, Azim Nejatizadeh, Ilona Nenko, Martin Neovius, Chung T Nguyen, Nguyen D Nguyen, Quang V Nguyen, Quang Ngoc Nguyen, Ramfis E Nieto-Martínez, Teemu J Niiranen, Yury P Nikitin, Toshiharu Ninomiya, Sania Nishtar, Marina A Njelekela, Marianna Noale, Oscar A Noboa, Ahmad Ali Noorbala, Teresa Norat, Maria Nordendahl, Børge G Nordestgaard, Noto Davide, Natalia Nowak-Szczepanska, Mohannad Al Nsour, Baltazar Nunes, Terence W O'Neill, Dermot O'Reilly, Caleb Ochimana, Eiji Oda, Augustine N Odili, Kyungwon Oh, Kumiko Ohara, Ryutaro Ohtsuka, Valérie Olié, Maria Teresa A Olinto, Isabel O Oliveira, Mohd Azahadi Omar, Altan Onat, Sok King Ong, Lariane M Ono, Pedro Ordunez, Rui Ornelas, Pedro J Ortiz, Clive Osmond, Sergej M Ostojic, Afshin Ostovar, Johanna A Otero, Kim Overvad, Ellis Owusu-Dabo, Fred Michel Paccaud, Cristina Padez, Elena Pahomova, Karina Mary de Paiva, Andrzej Pająk, Domenico Palli, Luigi Palmieri, Wen-Harn Pan, Songhomitra Panda-Jonas, Francesco Panza, Mariela Paoli, Dimitrios Papandreou, Soon-Woo Park, Suyeon Park, Winsome R Parnell, Mahboubeh Parsaeian, Patrick Pasquet, Nikhil D Patel, Halyna Pavlyshyn, Ivan Pećin, Mangesh S Pednekar, João M Pedro, Nasheeta Peer, Sergio Viana Peixoto, Markku Peltonen, Alexandre C Pereira, Karen Gda Peres, Marco A Peres, Annette Peters, Janina Petkeviciene, Niloofar Peykari, Son Thai Pham, Rafael N Pichardo, Iris Pigeot, Hynek Pikhart, Aida Pilav, Lorenza Pilotto, Freda Pitakaka, Aleksandra Piwonska, Andreia N Pizarro, Pedro Plans-Rubió, Ozren Polašek, Miquel Porta, Anil Poudyal, Farhad Pourfarzi, Akram Pourshams, Hossein Poustchi, Rajendra Pradeepa, Alison J Price, Jacqueline F Price, Rui Providencia, Soile E Puhakka, Maria Puiu, Margus Punab, Radwan F Qasrawi, Mostafa Qorbani, Daniel Queiroz, Tran Quoc Bao, Ivana Radić, Ricardas Radisauskas, Salar Rahimikazerooni, Mahfuzar Rahman, Olli Raitakari, Manu Raj, Ellina M Rakhimova, Sudha Ramachandra Rao, Ambady Ramachandran, Elisabete Ramos, Lekhraj Rampal, Sanjay Rampal, Daniel A Rangel Reina, Vayia Rarra, Cassiano Ricardo Rech, Josep Redon, Paul Ferdinand M Reganit, Valéria Regecová, Luis Revilla, Abbas Rezaianzadeh, Robespierre Ribeiro, Elio Riboli, Adrian Richter, Fernando Rigo, Tobias F Rinke de Wit, Raphael M Ritti-Dias, Cynthia Robitaille, Fernando Rodríguez-Artalejo, María Del Cristo Rodriguez-Perez, Laura A Rodríguez-Villamizar, Ulla Roggenbuck, Rosalba Rojas-Martinez, Dora Romaguera, Elisabetta L Romeo, Annika Rosengren, Joel Gr Roy, Adolfo Rubinstein, Jean-Bernard Ruidavets, Blanca Sandra Ruiz-Betancourt, Maria Ruiz-Castell, Iuliia A Rusakova, Paola Russo, Marcin Rutkowski, Charumathi Sabanayagam, Hamideh Sabbaghi, Harshpal S Sachdev, Alireza Sadjadi, Ali Reza Safarpour, Sare Safi, Saeid Safiri, Olfa Saidi, Sibel Sakarya, Nader Saki, Benoit Salanave, Eduardo Salazar Martinez, Diego Salmerón, Veikko Salomaa, Jukka T Salonen, Massimo Salvetti, Jose Sánchez-Abanto, Susana Sans, Diana A Santos, Ina S Santos, Lèlita C Santos, Maria Paula Santos, Rute Santos, Jouko L Saramies, Luis B Sardinha, Giselle Sarganas, Nizal Sarrafzadegan, Thirunavukkarasu Sathish, Kai-Uwe Saum, Savvas Savva, Norie Sawada, Mariana Sbaraini, Marcia Scazufca, Beatriz D Schaan, Herman Schargrodsky, Sabine Schipf, Carsten O Schmidt, Peter Schnohr, Ben Schöttker, Sara Schramm, Constance Schultsz, Aletta E Schutte, Sylvain Sebert, Aye Aye Sein, Abhijit Sen, Idowu O Senbanjo, Sadaf G Sepanlou, Jennifer Servais, Svetlana A Shalnova, Teresa Shamah-Levy, Morteza Shamshirgaran, Coimbatore Subramaniam Shanthirani, Maryam Sharafkhah, Sanjib K Sharma, Jonathan E Shaw, Amaneh Shayanrad, Ali Akbar Shayesteh, Zumin Shi, Kenji Shibuya, Hana Shimizu-Furusawa, Dong Wook Shin, Majid Shirani, Rahman Shiri, Namuna Shrestha, Khairil Si-Ramlee, Alfonso Siani, Rosalynn Siantar, Abla M Sibai, Caroline Ramos de Moura Silva, Diego Augusto Santos Silva, Mary Simon, Judith Simons, Leon A Simons, Michael Sjöström, Jolanta Slowikowska-Hilczer, Przemyslaw Slusarczyk, Liam Smeeth, Hung-Kwan So, Fernanda Cunha Soares, Eugène Sobngwi, Stefan Söderberg, Agustinus Soemantri, Reecha Sofat, Vincenzo Solfrizzi, Mohammad Hossein Somi, Emily Sonestedt, Yi Song, Thorkild Ia Sørensen, Elin P Sørgjerd, Maroje Sorić, Charles Sossa Jérome, Aïcha Soumaré, Bente Sparboe-Nilsen, Karen Sparrenberger, Jan A Staessen, Gregor Starc, Bill Stavreski, Jostein Steene-Johannessen, Peter Stehle, Aryeh D Stein, George S Stergiou, Jochanan Stessman, Jutta Stieber, Doris Stöckl, Tanja Stocks, Jakub Stokwiszewski, Karien Stronks, Maria Wany Strufaldi, Machi Suka, Chien-An Sun, Yn-Tz Sung, Paibul Suriyawongpaisal, Rody G Sy, Holly E Syddall, René Charles Sylva, Moyses Szklo, E Shyong Tai, Mari-Liis Tammesoo, Abdonas Tamosiunas, Eng Joo Tan, Xun Tang, Frank Tanser, Yong Tao, Mohammed Rasoul Tarawneh, Carolina B Tarqui-Mamani, Anne Taylor, Julie Taylor, William R Tebar, Grethe S Tell, Tania Tello, Yih Chung Tham, K R Thankappan, Holger Theobald, Xenophon Theodoridis, Lutgarde Thijs, Mikael Thinggaard, Nihal Thomas, Barbara Thorand, Betina H Thuesen, Erik J Timmermans, Dwi H Tjandrarini, Anne Tjonneland, Ulla Toft, Hanna K Tolonen, Janne S Tolstrup, Murat Topbas, Roman Topór-Madry, María José Tormo, Michael J Tornaritis, Maties Torrent, Laura Torres-Collado, Giota Touloumi, Pierre Traissac, Areti Triantafyllou, Dimitrios Trichopoulos, Antonia Trichopoulou, Oanh Th Trinh, Atul Trivedi, Lechaba Tshepo, Shoichiro Tsugane, Azaliia M Tuliakova, Marshall K Tulloch-Reid, Fikru Tullu, Tomi-Pekka Tuomainen, Jaakko Tuomilehto, Maria L Turley, Gilad Twig, Per Tynelius, Christophe Tzourio, Peter Ueda, Eunice Ugel, Hanno Ulmer, Hannu Mt Uusitalo, Gonzalo Valdivia, Damaskini Valvi, Rob M van Dam, Bert-Jan van den Born, Johan Van der Heyden, Yvonne T van der Schouw, Koen Van Herck, Hoang Van Minh, Natasja M Van Schoor, Irene Gm van Valkengoed, Elisabeth M van Zutphen, Dirk Vanderschueren, Diego Vanuzzo, Anette Varbo, Senthil K Vasan, Tomas Vega, Toomas Veidebaum, Gustavo Velasquez-Melendez, Giovanni Veronesi, Wm Monique Verschuren, Roosmarijn Verstraeten, Cesar G Victora, Lucie Viet, Salvador Villalpando, Paolo Vineis, Jesus Vioque, Jyrki K Virtanen, Sophie Visvikis-Siest, Bharathi Viswanathan, Tiina Vlasoff, Peter Vollenweider, Ari Voutilainen, Alisha N Wade, Janette Walton, Elvis Oa Wambiya, Wan Mohamad Wan Bebakar, Wan Nazaimoon Wan Mohamud, Rildo de Souza Wanderley Júnior, Ming-Dong Wang, Ningli Wang, Qian Wang, Xiangjun Wang, Ya Xing Wang, Ying-Wei Wang, S Goya Wannamethee, Nicholas Wareham, Wenbin Wei, Aneta Weres, Bo Werner, Peter H Whincup, Kurt Widhalm, Andrzej Wiecek, Rainford J Wilks, Johann Willeit, Peter Willeit, Emmanuel A Williams, Tom Wilsgaard, Bogdan Wojtyniak, Roy A Wong-McClure, Andrew Wong, Tien Yin Wong, Jean Woo, Frederick C Wu, Shouling Wu, Justyna Wyszynska, Haiquan Xu, Liang Xu, Nor Azwany Yaacob, Weili Yan, Ling Yang, Xiaoguang Yang, Yang Yang, Tabara Yasuharu, Xingwang Ye, Panayiotis K Yiallouros, Moein Yoosefi, Akihiro Yoshihara, San-Lin You, Novie O Younger-Coleman, Ahmad Faudzi Yusoff, Ahmad A Zainuddin, Seyed Rasoul Zakavi, Farhad Zamani, Sabina Zambon, Antonis Zampelas, Maria Elisa Zapata, Ko Ko Zaw, Kristyna Zejglicova, Tajana Zeljkovic Vrkic, Yi Zeng, Luxia Zhang, Zhen-Yu Zhang, Dong Zhao, Ming-Hui Zhao, Shiqi Zhen, Yingfeng Zheng, Bekbolat Zholdin, Dan Zhu, Marie Zins, Emanuel Zitt, Yanina Zocalo, Nada Zoghlami, Julio Zuñiga Cisneros, Majid Ezzati, Sakarya, Sibel (ORCID 0000-0002-9959-6240 & YÖK ID 172028), Zhou, Bin, Carrillo-Larco, Rodrigo M., Danaei, Goodarz, Riley, Leanne M., Paciorek, Christopher J., Stevens, Gretchen A., Gregg, Edward W., Bennett, James E., Solomon, Bethlehem, Singleton, Rosie K., Sophiea, Marisa K., Iurilli, Maria L. C., Lhoste, Victor P. F., Cowan, Melanie J., Savin, Stefan, Woodward, Mark, Balanova, Yulia, Cifkova, Renata, Damasceno, Albertino, Elliott, Paul, Farzadfar, Farshad, He, Jiang, Ikeda, Nayu, Kengne, Andre P., Khang, Young-Ho, Kim, Hyeon Chang, Laxmaiah, Avula, Lin, Hsien-Ho, Margozzini Maira, Paula, Miranda, J. Jaime, Neuhauser, Hannelore, Sundstrom, Johan, Varghese, Cherian, Widyahening, Indah S., Zdrojewski, Tomasz, Ezzati, Majid, Abarca-Gomez, Leandra, Abdeen, Ziad A., Rahim, Hanan F. Abdul, Abu-Rmeileh, Niveen M., Acosta-Cazares, Benjamin, Adams, Robert J., Aekplakorn, Wichai, Afsana, Kaosar, Afzal, Shoaib, Agdeppa, Imelda A., Aghazadeh-Attari, Javad, Aguilar-Salinas, Carlos A., Agyemang, Charles, Ahmad, Noor Ani, Ahmadi, Ali, Ahmadi, Naser, Ahmadi, Nastaran, Ahmadizar, Fariba, Ahmed, Soheir H., Ahrens, Wolfgang, Ajlouni, Kamel, Al-Raddadi, Rajaa, Alarouj, Monira, AlBuhairan, Fadia, AlDhukair, Shahla, Ali, Mohamed M., Alkandari, Abdullah, Alkerwi, Ala'a, Allin, Kristine, Aly, Eman, Amarapurkar, Deepak N., Amougou, Norbert, Amouyel, Philippe, Andersen, Lars Bo, Anderssen, Sigmund A., Anjana, Ranjit Mohan, Ansari-Moghaddam, Alireza, Ansong, Daniel, Aounallah-Skhiri, Hajer, Araujo, Joana, Ariansen, Inger, Aris, Tahir, Arku, Raphael E., Arlappa, Nimmathota, Aryal, Krishna K., Aspelund, Thor, Assah, Felix K., Assuncao, Maria Cecilia F., Auvinen, Juha, Avdicova, Maria, Azevedo, Ana, Azimi-Nezhad, Mohsen, Azizi, Fereidoun, Azmin, Mehrdad, Babu, Bontha V., Bahijri, Suhad, Balakrishna, Nagalla, Bamoshmoosh, Mohamed, Banach, Maciej, Banadinovic, Maja, Bandosz, Piotr, Banegas, Jose R., Baran, Joanna, Barbagallo, Carlo M., Barcelo, Alberto, Barkat, Amina, Barreto, Marta, Barros, Aluisio J. D., Gomes Barros, Mauro Virgilio, Bartosiewicz, Anna, Basit, Abdul, Bastos, Joao Luiz D., Bata, Iqbal, Batieha, Anwar M., Batyrbek, Assembekov, Baur, Louise A., Beaglehole, Robert, Belavendra, Antonisamy, Ben Romdhane, Habiba, Benet, Mikhail, Benson, Lowell S., Berkinbayev, Salim, Bernabe-Ortiz, Antonio, Bettiol, Heloisa, Bezerra, Jorge, Bhagyalaxmi, Aroor, Bhargava, Santosh K., Bia, Daniel, Biasch, Katia, Lele, Elysee Claude Bika, Bikbov, Mukharram M., Bista, Bihungum, Bjerregaard, Peter, Bjertness, Espen, Bjertness, Marius B., Bjorkelund, Cecilia, Bloch, Katia V., Blokstra, Anneke, Bo, Simona, Bobak, Martin, Boeing, Heiner, Boggia, Jose G., Boissonnet, Carlos P., Bojesen, Stig E., Bongard, Vanina, Bonilla-Vargas, Alice, Bopp, Matthias, Bovet, Pascal, Boyer, Christopher B., Braeckman, Lutgart, Brajkovich, Imperia, Branca, Francesco, Breckenkamp, Juergen, Brenner, Hermann, Brewster, Lizzy M., Briceno, Yajaira, Brito, Miguel, Bruno, Graziella, Bueno-de-Mesquita, H. Bas, Bueno, Gloria, Bugge, Anna, Burns, Con, Bursztyn, Michael, Cabrera de Leon, Antonio, Cacciottolo, Joseph, Cameron, Christine, Can, Gunay, Candido, Ana Paula C., Capanzana, Mario V., Capkova, Nadezda, Capuano, Eduardo, Capuano, Vincenzo, Cardoso, Viviane C., Carlsson, Axel C., Carvalho, Joana, Casanueva, Felipe F., Censi, Laura, Cervantes-Loaiza, Marvin, Chadjigeorgiou, Charalambos A., Chamukuttan, Snehalatha, Chan, Angelique W., Chan, Queenie, Chaturvedi, Himanshu K., Chaturvedi, Nish, Chee, Miao Li, Chen, Chien-Jen, Chen, Fangfang, Chen, Huashuai, Chen, Shuohua, Chen, Zhengming, Cheng, Ching-Yu, Cheraghian, Bahman, Dekkaki, Imane Cherkaoui, Chetrit, Angela, Chien, Kuo-Liong, Chiolero, Arnaud, Chiou, Shu-Ti, Chirita-Emandi, Adela, Chirlaque, Maria-Dolores, Cho, Belong, Christensen, Kaare, Christofaro, Diego G., Chudek, Jerzy, Cinteza, Eliza, Clarke, Janine, Clays, Els, Cohen, Emmanuel, Concin, Hans, Cooper, Cyrus, Coppinger, Tara C., Costanzo, Simona, Cottel, Dominique, Cowell, Chris, Craig, Cora L., Crampin, Amelia C., Crujeiras, Ana B., Cruz, Juan J., Csilla, Semanova, Cui, Liufu, Cureau, Felipe V., Cuschieri, Sarah, D'Arrigo, Graziella, d'Orsi, Eleonora, Dallongeville, Jean, Dankner, Rachel, Dantoft, Thomas M., Dauchet, Luc, Davletov, Kairat, De Backer, Guy, De Bacquer, Dirk, De Curtis, Amalia, de Gaetano, Giovanni, De Henauw, Stefaan, de Oliveira, Paula Duarte, De Ridder, David, De Smedt, Delphine, Deepa, Mohan, Deev, Alexander D., DeGennaro, Vincent Jr, Delisle, Helene, Demarest, Stefaan, Dennison, Elaine, Deschamps, Valerie, Dhimal, Meghnath, Di Castelnuovo, Augusto F., Dias-da-Costa, Juvenal Soares, Diaz, Alejandro, Dickerson, Ty T., Dika, Zivka, Djalalinia, Shirin, Do, Ha T. P., Dobson, Annette J., Donfrancesco, Chiara, Donoso, Silvana P., Doering, Angela, Dorobantu, Maria, Doerr, Marcus, Doua, Kouamelan, Dragano, Nico, Drygas, Wojciech, Duante, Charmaine A., Duboz, Priscilla, Duda, Rosemary B., Dulskiene, Virginija, Dushpanova, Anar, Dzakula, Aleksandar, Dzerve, Vilnis, Dziankowska-Zaborszczyk, Elzbieta, Eddie, Ricky, Eftekhar, Ebrahim, Eggertsen, Robert, Eghtesad, Sareh, Eiben, Gabriele, Ekelund, Ulf, El-Khateeb, Mohammad, El Ati, Jalila, Eldemire-Shearer, Denise, Eliasen, Marie, Elosua, Roberto, Erasmus, Rajiv T., Erbel, Raimund, Erem, Cihangir, Eriksen, Louise, Eriksson, Johan G., Escobedo-de la Pena, Jorge, Eslami, Saeid, Esmaeili, Ali, Evans, Alun, Faeh, David, Fakhretdinova, Albina A., Fall, Caroline H., Faramarzi, Elnaz, Farjam, Mojtaba, Fattahi, Mohammad Reza, Fawwad, Asher, Felix-Redondo, Francisco J., Felix, Stephan B., Ferguson, Trevor S., Fernandes, Romulo A., Fernandez-Berges, Daniel, Ferrante, Daniel, Ferrao, Thomas, Ferrari, Marika, Ferrario, Marco M., Ferreccio, Catterina, Ferreira, Haroldo S., Ferrer, Eldridge, Ferrieres, Jean, Figueiro, Thamara Hubler, Fink, Gunther, Fischer, Krista, Foo, Leng Huat, Forsner, Maria, Fouad, Heba M., Francis, Damian K., Franco, Maria do Carmo, Frikke-Schmidt, Ruth, Frontera, Guillermo, Fuchs, Flavio D., Fuchs, Sandra C., Fujita, Yuki, Fumihiko, Matsuda, Furdela, Viktoriya, Furer, Ariel, Furusawa, Takuro, Gaciong, Zbigniew, Galbarczyk, Andrzej, Galenkamp, Henrike, Galvano, Fabio, Gao, Jingli, Gao, Pei, Garcia-de-la-Hera, Manoli, Garcia, Pablo, Gareta, Dickman, Garnett, Sarah P., Gaspoz, Jean-Michel, Gasull, Magda, Gazzinelli, Andrea, Gehring, Ulrike, Geleijnse, Johanna M., George, Ronnie, Ghanbari, Ali, Ghasemi, Erfan, Gheorghe-Fronea, Oana-Florentina, Ghimire, Anup, Gialluisi, Alessandro, Giampaoli, Simona, Gieger, Christian, Gill, Tiffany K., Giovannelli, Jonathan, Gironella, Glen, Giwercman, Aleksander, Gkiouras, Konstantinos, Goldberg, Marcel, Goldsmith, Rebecca A., Gomez, Luis F., Gomula, Aleksandra, Cordeiro da Silva, Bruna Goncalves, Goncalves, Helen, Goncalves, Mauer, Gonzalez-Chica, David A., Gonzalez-Gross, Marcela, Gonzalez-Rivas, Juan P., Gonzalez-Villalpando, Clicerio, Gonzalez-Villalpando, Maria-Elena, Gonzalez, Angel R., Bonet Gorbea, Mariano, Gottrand, Frederic, Graff-Iversen, Sidsel, Grafnetter, Dusan, Grajda, Aneta, Grammatikopoulou, Maria G., Gregor, Ronald D., Grodzicki, Tomasz, Grosso, Giuseppe, Gruden, Gabriella, Gu, Dongfeng, Guan, Ong Peng, Gudmundsson, Elias F., Gudnason, Vilmundur, Guerrero, Ramiro, Guessous, Idris, Guimaraes, Andre L., Gulliford, Martin C., Gunnlaugsdottir, Johanna, Gunter, Marc J., Gupta, Prakash C., Gupta, Rajeev, Gureje, Oye, Gurzkowska, Beata, Gutierrez, Laura, Gutzwiller, Felix, Ha, Seongjun, Hadaegh, Farzad, Haghshenas, Rosa, Hakimi, Hamid, Halkjaer, Jytte, Hambleton, Ian R., Hamzeh, Behrooz, Hange, Dominique, Hanif, Abu A. M., Hantunen, Sari, Hao, Jie, Hardman, Carla Meneses, Kumar, Rachakulla Hari, Hashemi-Shahri, Seyed Mohammad, Hata, Jun, Haugsgjerd, Teresa, Hayes, Alison J., He, Yuna, Heier, Margit, Hendriks, Marleen Elisabeth, Henrique, Rafael dos Santos, Henriques, Ana, Cadena, Leticia Hernandez, Herrala, Sauli, Heshmat, Ramin, Hill, Allan G., Ho, Sai Yin, Ho, Suzanne C., Hobbs, Michael, Holdsworth, Michelle, Homayounfar, Reza, Dinc, Gonul Horasan, Horimoto, Andrea R. V. R., Hormiga, Claudia M., Horta, Bernardo L., Houti, Leila, Howitt, Christina, Htay, Thein Thein, Htet, Aung Soe, Htike, Maung Maung Than, Hu, Yonghua, Huerta, Jose Maria, Huhtaniemi, Ilpo Tapani, Huiart, Laetitia, Huisman, Martijn, Husseini, Abdullatif S., Huybrechts, Inge, Hwalla, Nahla, Iacoviello, Licia, Iannone, Anna G., Ibrahim, Mohsen M., Wong, Norazizah Ibrahim, Ikram, M. Arfan, Iotova, Violeta, Irazola, Vilma E., Ishida, Takafumi, Isiguzo, Godsent C., Islam, Muhammad, Islam, Sheikh Mohammed Shariful, Iwasaki, Masanori, Jackson, Rod T., Jacobs, Jeremy M., Jaddou, Hashem Y., Jafar, Tazeen, James, Kenneth, Jamrozik, Konrad, Janszky, Imre, Janus, Edward, Jarvelin, Marjo-Riitta, Jasienska, Grazyna, Jelakovic, Ana, Jelakovic, Bojan, Jennings, Garry, Jha, Anjani Kumar, Jiang, Chao Qiang, Jimenez, Ramon O., Joeckel, Karl-Heinz, Joffres, Michel, Johansson, Mattias, Jokelainen, Jari J., Jonas, Jost B., Jorgensen, Torben, Joshi, Pradeep, Joukar, Farahnaz, Jozwiak, Jacek, Juolevi, Anne, Jurak, Gregor, Juresa, Vesna, Kaaks, Rudolf, Kafatos, Anthony, Kajantie, Eero O., Kalmatayeva, Zhanna, Kalpourtzi, Natasa, Kalter-Leibovici, Ofra, Kampmann, Freja B., Kannan, Srinivasan, Karaglani, Eva, Karhus, Line L., Karki, Khem B., Katibeh, Marzieh, Katz, Joanne, Kauhanen, Jussi, Kaur, Prabhdeep, Kavousi, Maryam, Kazakbaeva, Gyulli M., Keil, Ulrich, Boker, Lital Keinan, Keinanen-Kiukaanniemi, Sirkka, Kelishadi, Roya, Kemper, Han C. G., Keramati, Maryam, Kerimkulova, Alina, Kersting, Mathilde, Key, Timothy, Khader, Yousef Saleh, Khalili, Davood, Khaw, Kay-Tee, Kheiri, Bahareh, Kheradmand, Motahareh, Khosravi, Alireza, Kiechl-Kohlendorfer, Ursula, Kiechl, Stefan, Killewo, Japhet, Kim, Dong Wook, Kim, Jeongseon, Klakk, Heidi, Klimek, Magdalena, Klumbiene, Jurate, Knoflach, Michael, Kolle, Elin, Kolsteren, Patrick, Kontto, Jukka P., Korpelainen, Raija, Korrovits, Paul, Kos, Jelena, Koskinen, Seppo, Kouda, Katsuyasu, Kowlessur, Sudhir, Koziel, Slawomir, Kratenova, Jana, Kriaucioniene, Vilma, Kristensen, Peter Lund, Krokstad, Steiner, Kromhout, Daan, Kruger, Herculina S., Kubinova, Ruzena, Kuciene, Renata, Kujala, Urho M., Kulaga, Zbigniew, Kumar, R. Krishna, Kurjata, Pawel, Kusuma, Yadlapalli S., Kutsenko, Vladimir, Kuulasmaa, Kari, Kyobutungi, Catherine, Laatikainen, Tiina, Lachat, Carl, Laid, Youcef, Lam, Tai Hing, Landrove, Orlando, Lanska, Vera, Lappas, Georg, Larijani, Bagher, Latt, Tint Swe, Le Coroller, Gwenaelle, Khanh Le Nguyen Bao, Le, Tuyen D., Lee, Jeannette, Lee, Jeonghee, Lehmann, Nils, Lehtimaki, Terho, Lemogoum, Daniel, Levitt, Naomi S., Li, Yanping, Lilly, Christa L., Lim, Wei-Yen, Lima-Costa, M. Fernanda, Lin, Xu, Lin, Yi-Ting, Lind, Lars, Lingam, Vijaya, Linneberg, Allan, Lissner, Lauren, Litwin, Mieczyslaw, Lo, Wei-Cheng, Loit, Helle-Mai, Lopez-Garcia, Esther, Lopez, Tania, Lotufo, Paulo A., Lozano, Jose Eugenio, Lovrencic, Iva Lukacevic, Lukrafka, Janice L., Luksiene, Dalia, Lundqvist, Annamari, Lundqvist, Robert, Lunet, Nuno, Lustigova, Michala, Luszczki, Edyta, Ma, Guansheng, Ma, Jun, Machado-Coelho, George L. L., Machado-Rodrigues, Aristides M., Macia, Enguerran, Macieira, Luisa M., Madar, Ahmed A., Maggi, Stefania, Magliano, Dianna J., Magriplis, Emmanuella, Mahasampath, Gowri, Maire, Bernard, Majer, Marjeta, Makdisse, Marcia, Malekzadeh, Fatemeh, Malekzadeh, Reza, Malhotra, Rahul, Mallikharjuna, Kodavanti, Malyutina, Sofia K., Maniego, Lynell V., Manios, Yannis, Mann, Jim I., Mansour-Ghanaei, Fariborz, Manzato, Enzo, Marcil, Anie, Margozzini, Paula, Marild, Staffan B., Glavic, Mihalea Marinovic, Marques-Vidal, Pedro, Marques, Larissa Pruner, Marrugat, Jaume, Martorell, Reynaldo, Mascarenhas, Luis P., Matasin, Marija, Mathiesen, Ellisiv B., Mathur, Prashant, Matijasevich, Alicia, Matlosz, Piotr, Matsha, Tandi E., Mavrogianni, Christina, Mbanya, Jean Claude N., Mc Donald Posso, Anselmo J., McFarlane, Shelly R., McGarvey, Stephen T., McLachlan, Stela, McLean, Rachael M., McLean, Scott B., McNulty, Breige A., Benchekor, Sounnia Mediene, Medzioniene, Jurate, Mehdipour, Parinaz, Mehlig, Kirsten, Mehrparvar, Amir Houshang, Meirhaeghe, Aline, Meisinger, Christa, Mendoza Montano, Carlos, Menezes, Ana Maria B., Menon, Geetha R., Mereke, Alibek, Meshram, Indrapal I., Metspalu, Andres, Meyer, Haakon E., Mi, Jie, Michels, Nathalie, Mikkel, Kairit, Milkowska, Karolina, Miller, Jody C., Minderico, Claudia S., Mini, G. K., Mirjalili, Mohammad Reza, Mirrakhimov, Erkin, Misigoj-Durakovic, Marjeta, Modesti, Pietro A., Moghaddam, Sahar Saeedi, Mohajer, Bahram, Mohamed, Mostafa K., Mohamed, Shukri F., Mohammad, Kazem, Mohammadi, Mohammad Reza, Mohammadi, Zahra, Mohammadifard, Noushin, Mohammadpourhodki, Reza, Mohan, Viswanathan, Mohanna, Salim, Yusoff, Muhammad Fadhli Mohd, Mohebbi, Iraj, Mohebi, Farnam, Moitry, Marie, Mollehave, Line T., Molnar, Denes, Momenan, Amirabbas, Mondo, Charles K., Monterrubio-Flores, Eric, Monyeki, Kotsedi Daniel K., Moon, Jin Soo, Moosazadeh, Mahmood, Moreira, Leila B., Morejon, Alain, Moreno, Luis A., Morgan, Karen, Moschonis, George, Mossakowska, Malgorzata, Mostafa, Aya, Mostafavi, Seyed-Ali, Mota, Jorge, Motlagh, Mohammad Esmaeel, Motta, Jorge, Andre Moura-dos-Santos, Marcos, Mridha, Malay K., Msyamboza, Kelias P., Mu, Thet Thet, Muhihi, Alfa J., Muiesan, Maria L., Muller-Nurasyid, Martina, Murphy, Neil, Mursu, Jaakko, Musa, Kamarul Imran, Milanovic, Sanja Music, Musil, Vera, Mustafa, Norlaila, Nabipour, Iraj, Naderimagham, Shohreh, Nagel, Gabriele, Naidu, Balkish M., Najafi, Farid, Nakamura, Harunobu, Namesna, Jana, Nang, Ei Ei K., Nangia, Vinay B., Narake, Sameer, Ndiaye, Ndeye Coumba, Neal, William A., Nejatizadeh, Azim, Nenko, Ilona, Neovius, Martin, Neuhauser, Hannelore K., Nguyen, Chung T., Nguyen, Nguyen D., Nguyen, Quang V., Quang Ngoc Nguyen, Nieto-Martinez, Ramfis E., Niiranen, Teemu J., Nikitin, Yury P., Ninomiya, Toshiharu, Nishtar, Sania, Njelekela, Marina A., Noale, Marianna, Noboa, Oscar A., Noorbala, Ahmad Ali, Norat, Teresa, Nordendahl, Maria, Nordestgaard, Borge G., Noto, Davide, Nowak-Szczepanska, Natalia, Al Nsour, Mohannad, Nunes, Baltazar, O'Neill, Terence W., O'Reilly, Dermot, Ochimana, Caleb, Oda, Eiji, Odili, Augustine N., Oh, Kyungwon, Ohara, Kumiko, Ohtsuka, Ryutaro, Olie, Valerie, Olinto, Maria Teresa A., Oliveira, Isabel O., Omar, Mohd Azahadi, Onat, Altan, Ong, Sok King, Ono, Lariane M., Ordunez, Pedro, Ornelas, Rui, Ortiz, Pedro J., Osmond, Clive, Ostojic, Sergej M., Ostovar, Afshin, Otero, Johanna A., Overvad, Kim, Owusu-Dabo, Ellis, Paccaud, Fred Michel, Padez, Cristina, Pahomova, Elena, de Paiva, Karina Mary, Pajak, Andrzej, Palli, Domenico, Palmieri, Luigi, Pan, Wen-Harn, Panda-Jonas, Songhomitra, Panza, Francesco, Paoli, Mariela, Papandreou, Dimitrios, Park, Soon-Woo, Park, Suyeon, Parnell, Winsome R., Parsaeian, Mahboubeh, Pasquet, Patrick, Patel, Nikhil D., Pavlyshyn, Halyna, Pecin, Ivan, Pednekar, Mangesh S., Pedro, Joao M., Peer, Nasheeta, Peixoto, Sergio Viana, Peltonen, Markku, Pereira, Alexandre C., Peres, Karen G. D. A., Peres, Marco A., Peters, Annette, Petkeviciene, Janina, Peykari, Niloofar, Son Thai Pham, Pichardo, Rafael N., Pigeot, Iris, Pikhart, Hynek, Pilav, Aida, Pilotto, Lorenza, Pitakaka, Freda, Piwonska, Aleksandra, Pizarro, Andreia N., Plans-Rubio, Pedro, Polasek, Ozren, Porta, Miquel, Poudyal, Anil, Pourfarzi, Farhad, Pourshams, Akram, Poustchi, Hossein, Pradeepa, Rajendra, Price, Alison J., Price, Jacqueline F., Providencia, Rui, Puhakka, Soile E., Puiu, Maria, Punab, Margus, Qasrawi, Radwan F., Qorbani, Mostafa, Queiroz, Daniel, Tran Quoc Bao, Radic, Ivana, Radisauskas, Ricardas, Rahimikazerooni, Salar, Rahman, Mahfuzar, Raitakari, Olli, Raj, Manu, Rakhimova, Ellina M., Rao, Sudha Ramachandra, Ramachandran, Ambady, Ramos, Elisabete, Rampal, Lekhraj, Rampal, Sanjay, Rangel Reina, Daniel A., Rarra, Vayia, Rech, Cassiano Ricardo, Redon, Josep, Reganit, Paul Ferdinand M., Regecova, Valeria, Revilla, Luis, Rezaianzadeh, Abbas, Ribeiro, Robespierre, Riboli, Elio, Richter, Adrian, Rigo, Fernando, de Wit, Tobias F. Rinke, Ritti-Dias, Raphael M., Robitaille, Cynthia, Rodriguez-Artalejo, Fernando, del Cristo Rodriguez-Perez, Maria, Rodriguez-Villamizar, Laura A., Roggenbuck, Ulla, Rojas-Martinez, Rosalba, Romaguera, Dora, Romeo, Elisabetta L., Rosengren, Annika, Roy, Joel G. R., Rubinstein, Adolfo, Ruidavets, Jean-Bernard, Sandra Ruiz-Betancourt, Blanca, Ruiz-Castell, Maria, Rusakova, Iuliia A., Russo, Paola, Rutkowski, Marcin, Sabanayagam, Charumathi, Sabbaghi, Hamideh, Sachdev, Harshpal S., Sadjadi, Alireza, Safarpour, Ali Reza, Safi, Sare, Safiri, Saeid, Saidi, Olfa, Saki, Nader, Salanave, Benoit, Salazar Martinez, Eduardo, Salmeron, Diego, Salomaa, Veikko, Salonen, Jukka T., Salvetti, Massimo, Sanchez-Abanto, Jose, Sans, Susana, Santos, Diana A., Santos, Ina S., Santos, Lelita C., Santos, Maria Paula, Santos, Rute, Saramies, Jouko L., Sardinha, Luis B., Sarganas, Giselle, Sarrafzadegan, Nizal, Sathish, Thirunavukkarasu, Saum, Kai-Uwe, Savva, Savvas, Sawada, Norie, Sbaraini, Mariana, Scazufca, Marcia, Schaan, Beatriz D., Schargrodsky, Herman, Schipf, Sabine, Schmidt, Carsten O., Schnohr, Peter, Schoettker, Ben, Schramm, Sara, Schultsz, Constance, Schutte, Aletta E., Sebert, Sylvain, Sein, Aye Aye, Sen, Abhijit, Senbanjo, Idowu O., Sepanlou, Sadaf G., Servais, Jennifer, Shalnova, Svetlana A., Shamah-Levy, Teresa, Shamshirgaran, Morteza, Shanthirani, Coimbatore Subramaniam, Sharafkhah, Maryam, Sharma, Sanjib K., Shaw, Jonathan E., Shayanrad, Amaneh, Shayesteh, Ali Akbar, Shi, Zumin, Shibuya, Kenji, Shimizu-Furusawa, Hana, Shin, Dong Wook, Shirani, Majid, Shiri, Rahman, Shrestha, Namuna, Si-Ramlee, Khairil, Siani, Alfonso, Siantar, Rosalynn, Sibai, Abla M., de Moura Silva, Caroline Ramos, Santos Silva, Diego Augusto, Simon, Mary, Simons, Judith, Simons, Leon A., Sjostrom, Michael, Slowikowska-Hilczer, Jolanta, Slusarczyk, Przemyslaw, Smeeth, Liam, So, Hung-Kwan, Soares, Fernanda Cunha, Sobngwi, Eugene, Soderberg, Stefan, Soemantri, Agustinus, Sofat, Reecha, Solfrizzi, Vincenzo, Somi, Mohammad Hossein, Sonestedt, Emily, Song, Yi, Sorensen, Thorkild I. A., Sorgjerd, Elin P., Soric, Maroje, Jerome, Charles Sossa, Soumare, Aicha, Sparboe-Nilsen, Bente, Sparrenberger, Karen, Staessen, Jan A., Starc, Gregor, Stavreski, Bill, Steene-Johannessen, Jostein, Stehle, Peter, Stein, Aryeh D., Stergiou, George S., Stessman, Jochanan, Stieber, Jutta, Stoeckl, Doris, Stocks, Tanja, Stokwiszewski, Jakub, Stronks, Karien, Strufaldi, Maria Wany, Suka, Machi, Sun, Chien-An, Sung, Yn-Tz, Suriyawongpaisal, Paibul, Sy, Rody G., Syddall, Holly E., Sylva, Rene Charles, Szklo, Moyses, Tai, E. Shyong, Tammesoo, Mari-Liis, Tamosiunas, Abdonas, Tan, Eng Joo, Tang, Xun, Tanser, Frank, Tao, Yong, Tarawneh, Mohammed Rasoul, Tarqui-Mamani, Carolina B., Taylor, Anne, Taylor, Julie, Tebar, William R., Tell, Grethe S., Tello, Tania, Tham, Yih Chung, Thankappan, K. R., Theobald, Holger, Theodoridis, Xenophon, Thinggaard, Mikael, Thomas, Nihal, Thorand, Barbara, Thuesen, Betina H., Timmermans, Erik J., Tjandrarini, Dwi H., Tjonneland, Anne, Toft, Ulla, Tolonen, Hanna K., Tolstrup, Janne S., Topbas, Murat, Topor-Madry, Roman, Jose Tormo, Maria, Tornaritis, Michael J., Torrent, Maties, Torres-Collado, Laura, Touloumi, Giota, Traissac, Pierre, Triantafyllou, Areti, Trichopoulos, Dimitrios, Trichopoulou, Antonia, Trinh, Oanh T. H., Trivedi, Atul, Tshepo, Lechaba, Tsugane, Shoichiro, Tuliakova, Azaliia M., Tulloch-Reid, Marshall K., Tullu, Fikru, Tuomainen, Tomi-Pekka, Tuomilehto, Jaakko, Turley, Maria L., Twig, Gilad, Tynelius, Per, Tzourio, Christophe, Ueda, Peter, Ugel, Eunice, Ulmer, Hanno, Uusitalo, Hannu M. T., Valdivia, Gonzalo, Valvi, Damaskini, van Dam, Rob M., van den Born, Bert-Jan, Van der Heyden, Johan, van der Schouw, Yvonne T., Van Herck, Koen, Hoang Van Minh, Van Schoor, Natasja M., van Valkengoed, Irene G. M., van Zutphen, Elisabeth M., Vanuzzo, Diego, Varbo, Anette, Vasan, Senthil K., Vega, Tomas, Veidebaum, Toomas, Velasquez-Melendez, Gustavo, Veronesi, Giovanni, Verschuren, W. M. Monique, Verstraeten, Roosmarijn, Victora, Cesar G., Viet, Lucie, Villalpando, Salvador, Vineis, Paolo, Vioque, Jesus, Virtanen, Jyrki K., Visvikis-Siest, Sophie, Viswanathan, Bharathi, Vlasoff, Tiina, Vollenweider, Peter, Voutilainen, Ari, Wade, Alisha N., Walton, Janette, Wambiya, Elvis O. A., Bebakar, Wan Mohamad Wan, Mohamud, Wan Nazaimoon Wan, Wanderley Junior, Rildo de Souza, Wang, Ming-Dong, Wang, Ningli, Wang, Qian, Wang, Xiangjun, Wang, Ya Xing, Wang, Ying-Wei, Wannamethee, S. Goya, Wareham, Nicholas, Wei, Wenbin, Weres, Aneta, Werner, Bo, Whincup, Peter H., Widhalm, Kurt, Wiecek, Andrzej, Wilks, Rainford J., Willeit, Johann, Willeit, Peter, Williams, Emmanuel A., Wilsgaard, Tom, Wojtyniak, Bogdan, Wong-McClure, Roy A., Wong, Andrew, Wong, Tien Yin, Woo, Jean, Wu, Frederick C., Wu, Shouling, Wyszynska, Justyna, Xu, Haiquan, Xu, Liang, Yaacob, Nor Azwany, Yan, Weili, Yang, Ling, Yang, Xiaoguang, Yang, Yang, Yasuharu, Tabara, Ye, Xingwang, Yiallouros, Panayiotis K., Yoosefi, Moein, Yoshihara, Akihiro, You, San-Lin, Younger-Coleman, Novie O., Yusoff, Ahmad Faudzi, Zainuddin, Ahmad A., Zakavi, Seyed Rasoul, Zamani, Farhad, Zambon, Sabina, Zampelas, Antonis, Elisa Zapata, Maria, Zaw, Ko Ko, Zejglicova, Kristyna, Vrkic, Tajana Zeljkovic, Zeng, Yi, Zhang, Luxia, Zhao, Dong, Zhao, Ming-Hui, Zhen, Shiqi, Zheng, Yingfeng, Zholdin, Bekbolat, Zhu, Dan, Zins, Marie, Zitt, Emanuel, Zocalo, Yanina, Zoghlami, Nada, Zuniga Cisneros, Julio., School of Medicine, ACS - Diabetes & metabolism, APH - Global Health, Pulmonology, Medical Informatics, Adult Psychiatry, Global Health, APH - Quality of Care, APH - Methodology, Vascular Medicine, ACS - Atherosclerosis & ischemic syndromes, Anesthesiology, Graduate School, and ACS - Heart failure & arrhythmias

Subjects
Male, Latin Americans, Nutrition and Disease, Epidemiology, [SDV]Life Sciences [q-bio], Medizin, BLOOD-PRESSURE, 030204 cardiovascular system & hematology, Worldwide trends in hypertension prevalence and progress in treatment and control from 1990 to 2019: a pooled analysis of 1201 population-representative studies with 104 million participants, Hypertension, Prevalence, Control, Tretament, GUIDELINES, Global Health, Worldwide trends, 0302 clinical medicine, Hypertension prevalence, Voeding en Ziekte, Medicine and Health Sciences, kohonnut verenpaine, Medicine, 030212 general & internal medicine, Prevention and Control, 11 Medical and Health Sciences, ComputingMilieux_MISCELLANEOUS, education.field_of_study, food and beverages, Public Health, Global Health, Social Medicine and Epidemiology, General Medicine, Noncommunicable diseases, Period prevalence, Middle Aged, kansainvälinen vertailu, 3142 Public health care science, environmental and occupational health, 3. Good health, MIDDLE-INCOME, Pooled analysis, SYSTEMATIC ANALYSIS, INCOME COUNTRIES, ADULTS, PREVENTION, MANAGEMENT, ADHERENCE, DIAGNOSIS, Western europe, [SDE]Environmental Sciences, Hypertension/diagnosis, NCD Risk Factor Collaboration (NCD-RisC), Female, B990 Subjects Allied to Medicine not elsewhere classified, Life Sciences & Biomedicine, Adult, health-care, esiintyvyys, Central asia, Population, Nursing, 3121 Internal medicine, 03 medical and health sciences, Medicine, General & Internal, Drug Therapy, General & Internal Medicine, Life Science, Humans, ddc:610, education, Antihypertensive Agents, VLAG, Aged, Science & Technology, Antihypertensive Agents/therapeutic use, business.industry, Omvårdnad, fungi, General and internal medicine, Estados de Saúde e de Doença, Taking medication, Treatment, Folkhälsovetenskap, global hälsa, socialmedicin och epidemiologi, Blood pressure, Faculdade de Ciências Sociais, 3121 General medicine, internal medicine and other clinical medicine, lääkehoito, 1182 Biochemistry, cell and molecular biology, business, Demography
Abstract

Background: hypertension can be detected at the primary health-care level and low-cost treatments can effectively control hypertension. We aimed to measure the prevalence of hypertension and progress in its detection, treatment, and control from 1990 to 2019 for 200 countries and territories. Methods: we used data from 1990 to 2019 on people aged 30-79 years from population-representative studies with measurement of blood pressure and data on blood pressure treatment. We defined hypertension as having systolic blood pressure 140 mm Hg or greater, diastolic blood pressure 90 mm Hg or greater, or taking medication for hypertension. We applied a Bayesian hierarchical model to estimate the prevalence of hypertension and the proportion of people with hypertension who had a previous diagnosis (detection), who were taking medication for hypertension (treatment), and whose hypertension was controlled to below 140/90 mm Hg (control). The model allowed for trends over time to be non-linear and to vary by age. Findings: the number of people aged 30-79 years with hypertension doubled from 1990 to 2019, from 331 (95% credible interval 306-359) million women and 317 (292-344) million men in 1990 to 626 (584-668) million women and 652 (604-698) million men in 2019, despite stable global age-standardised prevalence. In 2019, age-standardised hypertension prevalence was lowest in Canada and Peru for both men and women; in Taiwan, South Korea, Japan, and some countries in western Europe including Switzerland, Spain, and the UK for women; and in several low-income and middle-income countries such as Eritrea, Bangladesh, Ethiopia, and Solomon Islands for men. Hypertension prevalence surpassed 50% for women in two countries and men in nine countries, in central and eastern Europe, central Asia, Oceania, and Latin America. Globally, 59% (55-62) of women and 49% (46-52) of men with hypertension reported a previous diagnosis of hypertension in 2019, and 47% (43-51) of women and 38% (35-41) of men were treated. Control rates among people with hypertension in 2019 were 23% (20-27) for women and 18% (16-21) for men. In 2019, treatment and control rates were highest in South Korea, Canada, and Iceland (treatment >70%; control >50%), followed by the USA, Costa Rica, Germany, Portugal, and Taiwan. Treatment rates were less than 25% for women and less than 20% for men in Nepal, Indonesia, and some countries in sub-Saharan Africa and Oceania. Control rates were below 10% for women and men in these countries and for men in some countries in north Africa, central and south Asia, and eastern Europe. Treatment and control rates have improved in most countries since 1990, but we found little change in most countries in sub-Saharan Africa and Oceania. Improvements were largest in high-income countries, central Europe, and some upper-middle-income and recently high-income countries including Costa Rica, Taiwan, Kazakhstan, South Africa, Brazil, Chile, Turkey, and Iran. Interpretation Improvements in the detection, treatment, and control of hypertension have varied substantially across countries, with some middle-income countries now outperforming most high-income nations. The dual approach of reducing hypertension prevalence through primary prevention and enhancing its treatment and control is achievable not only in high-income countries but also in low-income and middle-income settings., British Heart Foundation Centre of Research Excellence Grant; World Health Organization (WHO); Abdul Latif Jameel Institute for Disease and Emergency Analytics Fellowship

Published
2021
Full Text
View/download PDF

48. Heterogeneous contributions of change in population distribution of body mass index to change in obesity and underweight

Author

Iurilli, M.L.C. Zhou, B. Bennett, J.E. Carrillo-Larco, R.M. Sophiea, M.K. Rodriguez-Martinez, A. Bixby, H. Solomon, B.D. Taddei, C. Danaei, G. Di Cesare, M. Stevens, G.A. Riley, L.M. Savin, S. Cowan, M.J. Bovet, P. Damasceno, A. Chirita-Emandi, A. Hayes, A.J. Ikeda, N. Jackson, R.T. Khang, Y.-H. Laxmaiah, A. Liu, J. Miranda, J.J. Saidi, O. Sebert, S. Sorić, M. Starc, G. Gregg, E.W. Abarca-Gómez, L. Abdeen, Z.A. Abdrakhmanova, S. Ghaffar, S.A. Rahim, H.F.A. Abu-Rmeileh, N.M. Garba, J.A. Acosta-Cazares, B. Adams, R.J. Aekplakorn, W. Afsana, K. Afzal, S. Agdeppa, I.A. Aghazadeh-Attari, J. Aguilar-Salinas, C.A. Agyemang, C. Ahmad, M.H. Ahmad, N.A. Ahmadi, A. Ahmadi, N. Ahmed, S.H. Ahrens, W. Aitmurzaeva, G. Ajlouni, K. Al-Hazzaa, H.M. Al-Lahou, B. Al-Raddadi, R. Alarouj, M. AlBuhairan, F. AlDhukair, S. Ali, M.M. Alkandari, A. Alkerwi, A. Allin, K. Alvarez-Pedrerol, M. Aly, E. Amarapurkar, D.N. Amiri, P. Amougou, N. Amouyel, P. Andersen, L.B. Anderssen, S.A. Ängquist, L. Anjana, R.M. Ansari-Moghaddam, A. Aounallah-Skhiri, H. Araújo, J. Ariansen, I. Aris, T. Arku, R.E. Arlappa, N. Aryal, K.K. Aspelund, T. Assah, F.K. Assunção, M.C.F. Aung, M.S. Auvinen, J. Mária Avdicová Avi, S. Azevedo, A. Azimi-Nezhad, M. Azizi, F. Azmin, M. Babu, B.V. Bæksgaard Jørgensen, M. Baharudin, A. Bahijri, S. Baker, J.L. Balakrishna, N. Bamoshmoosh, M. Banach, M. Bandosz, P. Banegas, J.R. Baran, J. Barbagallo, C.M. Barceló, A. Barkat, A. Barros, A.J.D. Barros, M.V.G. Basit, A. Bastos, J.L.D. Bata, I. Batieha, A.M. Batista, R.L. Battakova, Z. Batyrbek, A. Baur, L.A. Beaglehole, R. Bel-Serrat, S. Belavendra, A. Romdhane, H.B. Benedics, J. Benet, M. Bergh, I.H. Berkinbayev, S. Bernabe-Ortiz, A. Bernotiene, G. Bettiol, H. Bezerra, J. Bhagyalaxmi, A. Bharadwaj, S. Bhargava, S.K. Bhutta, Z.A. Bi, H. Bi, Y. Bia, D. Lele, E.C.B. Bikbov, M.M. Bista, B. Bjelica, D.J. Bjerregaard, P. Bjertness, E. Bjertness, M.B. Björkelund, C. Bloch, K.V. Blokstra, A. Bo, S. Bobak, M. Boddy, L.M. Boehm, B.O. Boeing, H. Boggia, J.G. Bogova, E. Boissonnet, C.P. Bojesen, S.E. Bonaccio, M. Bongard, V. Bonilla-Vargas, A. Bopp, M. Borghs, H. Braeckevelt, L. Braeckman, L. Bragt, M.C.E. Brajkovich, I. Branca, F. Breckenkamp, J. Breda, J. Brenner, H. Brewster, L.M. Brian, G.R. Brinduse, L. Brophy, S. Bruno, G. Bueno-de-Mesquita, H.B. Bugge, A. Buoncristiano, M. Burazeri, G. Burns, C. de León, A.C. Cacciottolo, J. Cai, H. Cama, T. Cameron, C. Camolas, J. Can, G. Candido, A.P.C. Cañete, F. Capanzana, M.V. Capková, N. Capuano, E. Capuano, V. Cardol, M. Cardoso, V.C. Carlsson, A.C. Carmuega, E. Carvalho, J. Casajús, J.A. Casanueva, F.F. Celikcan, E. Censi, L. Cervantes-Loaiza, M. Cesar, J.A. Chamukuttan, S. Chan, A.W. Chan, Q. Chaturvedi, H.K. Chaturvedi, N. Rahim, N.C.A. Chee, M.L. Chen, C.-J. Chen, F. Chen, H. Chen, S. Chen, Z. Cheng, C.-Y. Cheraghian, B. Chetrit, A. Chikova-Iscener, E. Chiolero, A. Chiou, S.-T. Chirlaque, M.-D. Cho, B. Christensen, K. Christofaro, D.G. Chudek, J. Cifkova, R. Cilia, M. Cinteza, E. Claessens, F. Clarke, J. Clays, E. Cohen, E. Concin, H. Confortin, S.C. Cooper, C. Coppinger, T.C. Corpeleijn, E. Costanzo, S. Cottel, D. Cowell, C. Craig, C.L. Crampin, A.C. Crujeiras, A.B. Csilla, S. Cucu, A.M. Cui, L. Cureau, F.V. Czenczek-Lewandowska, E. D’Arrigo, G. d’Orsi, E. Dacica, L. Dal Re Saavedra, M.A. Dallongeville, J. Damsgaard, C.T. Dankner, R. Dantoft, T.M. Dasgupta, P. Dastgiri, S. Dauchet, L. Davletov, K. De Backer, G. De Bacquer, D. de Gaetano, G. De Henauw, S. de Oliveira, P.D. De Ridder, D. De Ridder, K. de Rooij, S.R. De Smedt, D. Deepa, M. Deev, A.D. DeGennaro, V., Jr Dehghan, A. Delisle, H. Delpeuch, F. Demarest, S. Dennison, E. Dereń, K. Deschamps, V. Dhimal, M. Di Castelnuovo, A.F. Dias-da-Costa, J.S. Díaz-Sánchez, M.E. Diaz, A. Dika, Z. Djalalinia, S. Djordjic, V. Do, H.T.P. Dobson, A.J. Donati, M.B. Donfrancesco, C. Donoso, S.P. Döring, A. Dorobantu, M. Dorosty, A.R. Doua, K. Dragano, N. Drygas, W. Duan, J.L. Duante, C.A. Duboz, P. Duda, R.B. Duleva, V. Dulskiene, V. Dumith, S.C. Dushpanova, A. Dzerve, V. Dziankowska-Zaborszczyk, E. Eddie, R. Eftekhar, E. Egbagbe, E.E. Eggertsen, R. Eghtesad, S. Eiben, G. Ekelund, U. El-Khateeb, M. Ati, J.E. Eldemire-Shearer, D. Eliasen, M. Elliott, P. Engle-Stone, R. Enguerran, M. Erasmus, R.T. Erbel, R. Erem, C. Eriksen, L. Eriksson, J.G. Escobedo-de la Peña, J. Eslami, S. Esmaeili, A. Evans, A. Faeh, D. Fakhretdinova, A.A. Fall, C.H. Faramarzi, E. Farjam, M. Sant’Angelo, V.F. Farzadfar, F. Fattahi, M.R. Fawwad, A. Felix-Redondo, F.J. Ferguson, T.S. Fernandes, R.A. Fernández-Bergés, D. Ferrante, D. Ferrao, T. Ferrari, M. Ferrario, M.M. Ferreccio, C. Ferrer, E. Ferrieres, J. Figueiró, T.H. Fijalkowska, A. Fink, G. Fischer, K. Foo, L.H. Forsner, M. Fouad, H.M. Francis, D.K. Maria do Carmo Franco Frikke-Schmidt, R. Frontera, G. Fuchs, F.D. Fuchs, S.C. Fujiati, I.I. Fujita, Y. Fumihiko, M. Furusawa, T. Gaciong, Z. Gafencu, M. Galbarczyk, A. Galenkamp, H. Galeone, D. Galfo, M. Galvano, F. Gao, J. Garcia-de-la-Hera, M. García-Solano, M. Gareta, D. Garnett, S.P. Gaspoz, J.-M. Gasull, M. Gaya, A.C.A. Gaya, A.R. Gazzinelli, A. Gehring, U. Geiger, H. Geleijnse, J.M. Ghanbari, A. Ghasemi, E. Gheorghe-Fronea, O.-F. Giampaoli, S. Gianfagna, F. Gill, T.K. Giovannelli, J. Gironella, G. Giwercman, A. Gkiouras, K. Godos, J. Gogen, S. Goldberg, M. Goldsmith, R.A. Goltzman, D. Gómez, S.F. Gomula, A. da Silva, B.G.C. Gonçalves, H. Gonzalez-Chica, D.A. Gonzalez-Gross, M. González-Leon, M. González-Rivas, J.P. González-Villalpando, C. González-Villalpando, M.-E. Gonzalez, A.R. Gottrand, F. Graça, A.P. Graff-Iversen, S. Grafnetter, D. Grajda, A. Grammatikopoulou, M.G. Gregor, R.D. Grodzicki, T. Grøholt, E.K. Grøntved, A. Grosso, G. Gruden, G. Gu, D. Gualdi-Russo, E. Guallar-Castillón, P. Gualtieri, A. Gudmundsson, E.F. Gudnason, V. Guerrero, R. Guessous, I. Guimaraes, A.L. Gulliford, M.C. Gunnlaugsdottir, J. Gunter, M.J. Guo, X.-H. Guo, Y. Gupta, P.C. Gupta, R. Gureje, O. Gurzkowska, B. Gutiérrez-González, E. Gutierrez, L. Gutzwiller, F. Ha, S. Hadaegh, F. Hadjigeorgiou, C.A. Haghshenas, R. Hakimi, H. Halkjær, J. Hambleton, I.R. Hamzeh, B. Hange, D. Hanif, A.A.M. Hantunen, S. Hao, J. Kumar, R.H. Hashemi-Shahri, S.M. Hassapidou, M. Hata, J. Haugsgjerd, T. He, J. He, Y. He, Y. Heidinger-Felso, R. Heinen, M. Hejgaard, T. Hendriks, M.E. dos Santos Henrique, R. Henriques, A. Cadena, L.H. Herrala, S. Herrera, V.M. Herter-Aeberli, I. Heshmat, R. Hill, A.G. Ho, S.Y. Ho, S.C. Hobbs, M. Holdsworth, M. Homayounfar, R. Homs, C. Hopman, W.M. Horimoto, A.R.V.R. Hormiga, C.M. Horta, B.L. Houti, L. Howitt, C. Htay, T.T. Htet, A.S. Htike, M.M.T. Hu, Y. Huerta, J.M. Huhtaniemi, I.T. Huiart, L. Petrescu, C.H. Huisman, M. Husseini, A. Huu, C.N. Huybrechts, I. Hwalla, N. Hyska, J. Iacoviello, L. Ibarluzea, J.M. Ibrahim, M.M. Wong, N.I. Ikram, M.A. Iotova, V. Irazola, V.E. Ishida, T. Islam, M. Islam, S.M.S. Iwasaki, M. Jacobs, J.M. Jaddou, H.Y. Jafar, T. James, K. Jamil, K.M. Jamrozik, K. Janszky, I. Janus, E. Jarani, J. Jarvelin, M.-R. Jasienska, G. Jelakovic, A. Jelakovic, B. Jennings, G. Jha, A.K. Jiang, C.Q. Jimenez, R.O. Jöckel, K.-H. Joffres, M. Johansson, M. Jokelainen, J.J. Jonas, J.B. Jonnagaddala, J. Jørgensen, T. Joshi, P. Joukar, F. Jovic, D.P. Jóźwiak, J.J. Juolevi, A. Jurak, G. Simina, I.J. Juresa, V. Kaaks, R. Kaducu, F.O. Kafatos, A. Kajantie, E.O. Kalmatayeva, Z. Kalter-Leibovici, O. Kameli, Y. Kampmann, F.B. Kanala, K.R. Kannan, S. Kapantais, E. Karakosta, A. Kårhus, L.L. Karki, K.B. Katibeh, M. Katz, J. Katzmarzyk, P.T. Kauhanen, J. Kaur, P. Kavousi, M. Kazakbaeva, G.M. Keil, U. Boker, L.K. Keinänen-Kiukaanniemi, S. Kelishadi, R. Kelleher, C. Kemper, H.C.G. Kengne, A.P. Keramati, M. Kerimkulova, A. Kersting, M. Key, T. Khader, Y.S. Khalili, D. Khaw, K.-T. Kheiri, B. Kheradmand, M. Khosravi, A. Khouw, I.M.S.L. Kiechl-Kohlendorfer, U. Kiechl, S. Killewo, J. Kim, D.W. Kim, H.C. Kim, J. Kindblom, J.M. Klakk, H. Klimek, M. Klimont, J. Klumbiene, J. Knoflach, M. Koirala, B. Kolle, E. Kolsteren, P. König, J. Korpelainen, R. Korrovits, P. Korzycka, M. Kos, J. Koskinen, S. Kouda, K. Kovacs, V.A. Kowlessur, S. Koziel, S. Kratenova, J. Kratzer, W. Kriemler, S. Kristensen, P.L. Krokstad, S. Kromhout, D. Kruger, H.S. Kubinova, R. Kuciene, R. Kujala, U.M. Kujundzic, E. Kulaga, Z. Kumar, R.K. Kunešová, M. Kurjata, P. Kusuma, Y.S. Kuulasmaa, K. Kyobutungi, C. La, Q.N. Laamiri, F.Z. Laatikainen, T. Lachat, C. Laid, Y. Lam, T.H. Lambrinou, C.-P. Landais, E. Lanska, V. Lappas, G. Larijani, B. Latt, T.S. Lauria, L. Lazo-Porras, M. Le Coroller, G. Bao, K.L.N. Le Port, A. Le, T.D. Lee, J. Lee, J. Lee, P.H. Lehmann, N. Lehtimäki, T. Lemogoum, D. Levitt, N.S. Li, Y. Liivak, M. Lilly, C.L. Lim, W.-Y. Lima-Costa, M.F. Lin, H.-H. Lin, X. Lin, Y.-T. Lind, L. Linneberg, A. Lissner, L. Litwin, M. Liu, L. Lo, W.-C. Loit, H.-M. Long, K.Q. Lopes, L. Lopes, O. Lopez-Garcia, E. Lopez, T. Lotufo, P.A. Lozano, J.E. Lukrafka, J.L. Luksiene, D. Lundqvist, A. Lundqvist, R. Lunet, N. Lunogelo, C. Lustigová, M. Łuszczki, E. Ma, G. Ma, J. Ma, X. Machado-Coelho, G.L.L. Machado-Rodrigues, A.M. Macieira, L.M. Madar, A.A. Maggi, S. Magliano, D.J. Magnacca, S. Magriplis, E. Mahasampath, G. Maire, B. Majer, M. Makdisse, M. Mäki, P. Malekzadeh, F. Malekzadeh, R. Malhotra, R. Rao, K.M. Malyutina, S.K. Maniego, L.V. Manios, Y. Mann, J.I. Mansour-Ghanaei, F. Manzato, E. Margozzini, P. Markaki, A. Markey, O. Ioannidou, E.M. Marques-Vidal, P. Marques, L.P. Marrugat, J. Martin-Prevel, Y. Martin, R. Martorell, R. Martos, E. Maruszczak, K. Marventano, S. Mascarenhas, L.P. Masoodi, S.R. Mathiesen, E.B. Mathur, P. Matijasevich, A. Matsha, T.E. Mavrogianni, C. Mazur, A. Mbanya, J.C.N. McFarlane, S.R. McGarvey, S.T. McKee, M. McLachlan, S. McLean, R.M. McLean, S.B. McNulty, B.A. Benchekor, S.M. Medzioniene, J. Mehdipour, P. Mehlig, K. Mehrparvar, A.H. Meirhaeghe, A. Meisfjord, J. Meisinger, C. Menezes, A.M.B. Menon, G.R. Mensink, G.B.M. Menzano, M.T. Mereke, A. Meshram, I.I. Metspalu, A. Meyer, H.E. Mi, J. Michaelsen, K.F. Michels, N. Mikkel, K. Milkowska, K. Miller, J.C. Minderico, C.S. Mini, G.K. Miquel, J.F. Mirjalili, M.R. Mirkopoulou, D. Mirrakhimov, E. Mišigoj-Durakovic, M. Mistretta, A. Mocanu, V. Modesti, P.A. Moghaddam, S.S. Mohajer, B. Mohamed, M.K. Mohamed, S.F. Mohammad, K. Mohammadi, Z. Mohammadifard, N. Mohammadpourhodki, R. Mohan, V. Mohanna, S. Yusoff, M.F.M. Mohebbi, I. Mohebi, F. Moitry, M. Molbo, D. Møllehave, L.T. Møller, N.C. Molnár, D. Momenan, A. Mondo, C.K. Monroy-Valle, M. Monterrubio-Flores, E. Monyeki, K.D.K. Moon, J.S. Moosazadeh, M. Moreira, L.B. Morejon, A. Moreno, L.A. Morgan, K. Morin, S.N. Mortensen, E.L. Moschonis, G. Mossakowska, M. Mostafa, A. Mota-Pinto, A. Mota, J. Motlagh, M.E. Motta, J. Moura-dos-Santos, M.A. Mridha, M.K. Msyamboza, K.P. Mu, T.T. Muc, M. Mugoša, B. Muiesan, M.L. Mukhtorova, P. Müller-Nurasyid, M. Murphy, N. Mursu, J. Murtagh, E.M. Musa, K.I. Milanovic, S.M. Musil, V. Mustafa, N. Nabipour, I. Naderimagham, S. Nagel, G. Naidu, B.M. Najafi, F. Nakamura, H. Námešná, J. Nang, E.E.K. Nangia, V.B. Nankap, M. Narake, S. Nardone, P. Nauck, M. Neal, W.A. Nejatizadeh, A. Nekkantti, C. Nelis, K. Nelis, L. Nenko, I. Neovius, M. Nervi, F. Nguyen, C.T. Nguyen, N.D. Nguyen, Q.N. Nieto-Martínez, R.E. Nikitin, Y.P. Ning, G. Ninomiya, T. Nishtar, S. Noale, M. Noboa, O.A. Nogueira, H. Norat, T. Nordendahl, M. Nordestgaard, B.G. Noto, D. Nowak-Szczepanska, N. Al Nsour, M. Nuhoglu, I. Nurk, E. O’Neill, T.W. O’Reilly, D. Obreja, G. Ochimana, C. Ochoa-Avilés, A.M. Oda, E. Oh, K. Ohara, K. Ohlsson, C. Ohtsuka, R. Olafsson, O. Olinto, M.T.A. Oliveira, I.O. Omar, M.A. Onat, A. Ong, S.K. Ono, L.M. Ordunez, P. Ornelas, R. Ortiz, A.P. Ortiz, P.J. Osler, M. Osmond, C. Ostojic, S.M. Ostovar, A. Otero, J.A. Overvad, K. Owusu-Dabo, E. Paccaud, F.M. Padez, C. Pagkalos, I. Pahomova, E. de Paiva, K.M. Pajak, A. Palli, D. Palloni, A. Palmieri, L. Pan, W.-H. Panda-Jonas, S. Pandey, A. Panza, F. Papandreou, D. Park, S.-W. Park, S. Parnell, W.R. Parsaeian, M. Pascanu, I.M. Pasquet, P. Patel, N.D. Pecin, I. Pednekar, M.S. Peer, N. Pei, G. Peixoto, S.V. Peltonen, M. Pereira, A.C. Peres, M.A. Pérez-Farinós, N. Pérez, C.M. Peterkova, V. Peters, A. Petersmann, A. Petkeviciene, J. Petrauskiene, A. Pettenuzzo, E. Peykari, N. Pham, S.T. Pichardo, R.N. Pierannunzio, D. Pigeot, I. Pikhart, H. Pilav, A. Pilotto, L. Pistelli, F. Pitakaka, F. Piwonska, A. Pizarro, A.N. Plans-Rubió, P. Poh, B.K. Pohlabeln, H. Pop, R.M. Popovic, S.R. Porta, M. Posch, G. Poudyal, A. Poulimeneas, D. Pouraram, H. Pourfarzi, F. Pourshams, A. Poustchi, H. Pradeepa, R. Price, A.J. Price, J.F. Providencia, R. Puder, J.J. Pudule, I. Puhakka, S.E. Puiu, M. Punab, M. Qasrawi, R.F. Qorbani, M. Bao, T.Q. Radic, I. Radisauskas, R. Rahimikazerooni, S. Rahman, M. Rahman, M. Raitakari, O. Raj, M. Rakhimova, E. Rakhmatulloev, S. Rakovac, I. Rao, S.R. Ramachandran, A. Ramke, J. Ramos, E. Ramos, R. Rampal, L. Rampal, S. Rarra, V. Rascon-Pacheco, R.A. Rasmussen, M. Rech, C.R. Redon, J. Reganit, P.F.M. Regecová, V. Revilla, L. Rezaianzadeh, A. Ribas-Barba, L. Ribeiro, R. Riboli, E. Richter, A. Rigo, F. Rinaldo, N. de Wit, T.F.R. Rito, A. Ritti-Dias, R.M. Rivera, J.A. Robitaille, C. Roccaldo, R. Rodrigues, D. Rodríguez-Artalejo, F. del Cristo Rodriguez-Perez, M. Rodríguez-Villamizar, L.A. Roggenbuck, U. Rojas-Martinez, R. Rojroongwasinkul, N. Romaguera, D. Romeo, E.L. Rosario, R.V. Rosengren, A. Rouse, I. Roy, J.G.R. Rubinstein, A. Rühli, F.J. Ruidavets, J.-B. Ruiz-Betancourt, B.S. Ruiz-Castell, M. Moreno, E.R. Rusakova, I.A. Jonsson, K.R. Russo, P. Rust, P. Rutkowski, M. Sabanayagam, C. Sacchini, E. Sachdev, H.S. Sadjadi, A. Safarpour, A.R. Safiri, S. Saki, N. Salanave, B. Martinez, E.S. Salmerón, D. Salomaa, V. Salonen, J.T. Salvetti, M. Samoutian, M. Sánchez-Abanto, J. Sans, S. Marina, L.S. Santos, D.A. Santos, I.S. Santos, L.C. Santos, M.P. Santos, O. Santos, R. Sanz, S.S. Saramies, J.L. Sardinha, L.B. Sarrafzadegan, N. Sathish, T. Saum, K.-U. Savva, S. Savy, M. Sawada, N. Sbaraini, M. Scazufca, M. Schaan, B.D. Rosario, A.S. Schargrodsky, H. Schienkiewitz, A. Schipf, S. Schmidt, C.O. Schmidt, I.M. Schnohr, P. Schöttker, B. Schramm, S. Schramm, S. Schröder, H. Schultsz, C. Schutte, A.E. Sein, A.A. Selamat, R. Sember, V. Sen, A. Senbanjo, I.O. Sepanlou, S.G. Sequera, V. Serra-Majem, L. Servais, J. Ševcíková, L. Shalnova, S.A. Shamah-Levy, T. Shamshirgaran, M. Shanthirani, C.S. Sharafkhah, M. Sharma, S.K. Shaw, J.E. Shayanrad, A. Shayesteh, A.A. Shengelia, L. Shi, Z. Shibuya, K. Shimizu-Furusawa, H. Shin, D.W. Shirani, M. Shiri, R. Shrestha, N. Si-Ramlee, K. Siani, A. Siantar, R. Sibai, A.M. Silva, A.M. Silva, D.A.S. Simon, M. Simons, J. Simons, L.A. Sjöberg, A. Sjöström, M. Skodje, G. Slowikowska-Hilczer, J. Slusarczyk, P. Smeeth, L. So, H.-K. Soares, F.C. Sobek, G. Sobngwi, E. Sodemann, M. Söderberg, S. Soekatri, M.Y.E. Soemantri, A. Sofat, R. Solfrizzi, V. Somi, M.H. Sonestedt, E. Song, Y. Sørensen, T.I.A. Sørgjerd, E.P. Jérome, C.S. Soto-Rojas, V.E. Soumaré, A. Sovic, S. Sparboe-Nilsen, B. Sparrenberger, K. Spinelli, A. Spiroski, I. Staessen, J.A. Stamm, H. Stathopoulou, M.G. Staub, K. Stavreski, B. Steene-Johannessen, J. Stehle, P. Stein, A.D. Stergiou, G.S. Stessman, J. Stevanovic, R. Stieber, J. Stöckl, D. Stocks, T. Stokwiszewski, J. Stoyanova, E. Stratton, G. Stronks, K. Strufaldi, M.W. Sturua, L. Suárez-Medina, S. Suka, M. Sun, C.-A. Sundström, J. Sung, Y.-T. Sunyer, J. Suriyawongpaisal, P. Swinburn, B.A. Sy, R.G. Syddall, H.E. Sylva, R.C. Szklo, M. Szponar, L. Tai, E.S. Tammesoo, M.-L. Tamosiunas, A. Tan, E.J. Tang, X. Tanrygulyyeva, M. Tanser, F. Tao, Y. Tarawneh, M.R. Tarp, J. Tarqui-Mamani, C.B. Braunerová, R.T. Taylor, A. Taylor, J. Tchibindat, F. Tebar, W.R. Tell, G.S. Tello, T. Tham, Y.C. Thankappan, K.R. Theobald, H. Theodoridis, X. Thijs, L. Thomas, N. Thuesen, B.H. Tichá, L. Timmermans, E.J. Tjonneland, A. Tolonen, H.K. Tolstrup, J.S. Topbas, M. Topór-Madry, R. Torheim, L.E. Tormo, M.J. Tornaritis, M.J. Torrent, M. Torres-Collado, L. Toselli, S. Touloumi, G. Traissac, P. Tran, T.T.-H. Trichopoulos, D. Trichopoulou, A. Trinh, D.T.H. Trivedi, A. Tshepo, L. Tsigga, M. Tsugane, S. Tuliakova, A.M. Tulloch-Reid, M.K. Tullu, F. Tuomainen, T.-P. Tuomilehto, J. Turley, M.L. Twig, G. Tynelius, P. Tzotzas, T. Tzourio, C. Ueda, P. Ugel, E. Ukoli, F.A.M. Ulmer, H. Unal, B. Usupova, Z. Uusitalo, H.M.T. Uysal, N. Vaitkeviciute, J. Valdivia, G. Vale, S. Valvi, D. van Dam, R.M. Van der Heyden, J. van der Schouw, Y.T. Van Herck, K. Van Minh, H. Van Schoor, N.M. van Valkengoed, I.G.M. Vanderschueren, D. Vanuzzo, D. Varbo, A. Varela-Moreiras, G. Varona-Pérez, P. Vasan, S.K. Vega, T. Veidebaum, T. Velasquez-Melendez, G. Velika, B. Veronesi, G. Verschuren, W.M.M. Victora, C.G. Viegi, G. Viet, L. Villalpando, S. Vineis, P. Vioque, J. Virtanen, J.K. Visser, M. Visvikis-Siest, S. Viswanathan, B. Vladulescu, M. Vlasoff, T. Vocanec, D. Vollenweider, P. Völzke, H. Voutilainen, A. Voutilainen, S. Vrijheid, M. Vrijkotte, T.G.M. Wade, A.N. Wagner, A. Waldhör, T. Walton, J. Wambiya, E.O.A. Bebakar, A.M.W. Mohamud, W.N.W. de Souza Wanderley Júnior, R. Wang, M.-D. Wang, N. Wang, Q. Wang, X. Wang, Y.X. Wang, Y.-W. Wannamethee, S.G. Wareham, N. Weber, A. Wedderkopp, N. Weerasekera, D. Weghuber, D. Wei, W. Weres, A. Werner, B. Whincup, P.H. Widhalm, K. Widyahening, I.S. Wiecek, A. Wilks, R.J. Willeit, J. Willeit, P. Williams, J. Wilsgaard, T. Wojtyniak, B. Wong-McClure, R.A. Wong, A. Wong, J.E. Wong, T.Y. Woo, J. Woodward, M. Wu, F.C. Wu, J. Wu, L.J. Wu, S. Xu, H. Xu, L. Yaacob, N.A. Yamborisut, U. Yan, W. Yang, L. Yang, X. Yang, Y. Yardim, N. Yaseri, M. Yasuharu, T. Ye, X. Yiallouros, P.K. Yoosefi, M. Yoshihara, A. You, Q.S. You, S.-L. Younger-Coleman, N.O. Yusof, S.M. Yusoff, A.F. Zaccagni, L. Zafiropulos, V. Zainuddin, A.A. Zakavi, S.R. Zamani, F. Zambon, S. Zampelas, A. Zamrazilová, H. Zapata, M.E. Zargar, A.H. Zaw, K.K. Zdrojewski, T. Zejglicova, K. Vrkic, T.Z. Zeng, Y. Zhang, L. Zhang, Z.-Y. Zhao, D. Zhao, M.-H. Zhao, W. Zhen, S. Zheng, W. Zheng, Y. Zholdin, B. Zhou, M. Zhu, D. Zins, M. Zitt, E. Zocalo, Y. Cisneros, J.Z. Zuziak, M. Ezzati, M. Filippi, S. NCD Risk Factor Collaboration (NCD-RisC)

Subjects
nutritional and metabolic diseases, sense organs, skin and connective tissue diseases
Abstract

From 1985 to 2016, the prevalence of underweight decreased, and that of obesity and severe obesity increased, in most regions, with significant variation in the magnitude of these changes across regions. We investigated how much change in mean body mass index (BMI) explains changes in the prevalence of underweight, obesity, and severe obesity in different regions using data from 2896 population-based studies with 187 million participants. Changes in the prevalence of underweight and total obesity, and to a lesser extent severe obesity, are largely driven by shifts in the distribution of BMI, with smaller contributions from changes in the shape of the distribution. In East and Southeast Asia and sub-Saharan Africa, the underweight tail of the BMI distribution was left behind as the distribution shifted. There is a need for policies that address all forms of malnutrition by making healthy foods accessible and affordable, while restricting unhealthy foods through fiscal and regulatory restrictions. © Copyright.

Published
2021

Catalog

Books, media, physical & digital resources
See catalog results