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Sexual Violence against Women in Japanese Society
Megumu Kimoto BROWNSTEIN 이화여자대학교 아시아여성학센터 2017 이화여자대학교 아시아여성학센터 학술대회자료집 Vol.2017 No.01
According to the national statistics published by the Gender Equality Bureau Cabinet Office in 2014, approximately one in 15 women in Japan reported being forced to have sex. Nearly 70% of these women responded not reporting the assaults to the police, other individuals or organizations. There is also currently no systematic data collection mechanism which accurately captures the extent of a wide range of sexual crimes committed against women. Japan’s damaging rape culture has long been reinforced and sustained by a persistent, archaic belief in “danson johi” (male domination of women or male chauvinism). This sadly results in the sexual objectification and commercialization of female bodies, and it continues to harm thousands of women each year. In this paper, an overview of various forms of sexual violence taking place in the Japanese societies including some culturally specific ones such as peep chikan (physical molestation on public transportation), and sexual assaults and human rights violation in pornography and entertainment industries, will be provided. In addition, possible causes and efforts put forth by prominent women activists in Japan thus far will be discussed. While much advancement has been made to address sexual violence against women, Japan has a long road ahead in order to bring about drastic changes required to create a society free of violence and gender inequality.
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Megumu Kimoto Brownstein 이화여자대학교 아시아여성학센터 2017 Asian Journal of Women's Studies(AJWS) Vol.23 No.3
This case study on the Association of Women for Action and Research (AWARE) in Singapore relates a simple and powerful tenet of social justice; all children deserve government and social support regardless of their parents’ marital status. Despite single parenthood becoming increasingly common, some single mothers and their children in Singapore face numerous challenges, such as finding suitable housing. Significant factors regarding this may be attributed to the housing policies and regulations that reward traditional families and underserve other forms of family structures. While more than 80 percent of Singapore’s population enjoy access to public housing, unwed mothers seem to be systematically excluded from this entitlement until they reach the age of 35, in addition to other welfare and tax benefits that are consistently awarded to traditional families. Divorced single mothers also often experience poor housing situations and sometimes homelessness, apparently due to excessively stringent eligibility criteria. To address these issues, AWARE conducted “evidence-based” advocacy using a multi-actor and multi-level approach. The method, commitment, and coordination that AWARE has demonstrated may indeed serve as a blueprint for other organizations seeking to assist deserving single parents and their dependents.
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Slepian, Zachary,Eisenstein, Daniel J.,Brownstein, Joel R.,Chuang, Chia-Hsun,Gil-Marí,n, Hé,ctor,Ho, Shirley,Kitaura, Francisco-Shu,Percival, Will J.,Ross, Ashley J.,Rossi, Graziano,Seo, H Oxford University Press 2017 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.469 No.2
<P>We present the large-scale three-point correlation function (3PCF) of the Sloan Digital Sky Survey DR12 Constant stellar Mass (CMASS) sample of 777 202 Luminous Red Galaxies, the largest-ever sample used for a 3PCF or bispectrum measurement. We make the first high-significance (4.5 sigma) detection of baryon acoustic oscillations (BAO) in the 3PCF. Using these acoustic features in the 3PCF as a standard ruler, we measure the distance to z = 0.57 to 1.7 per cent precision (statistical plus systematic). We find DV = 2024 +/- 29 Mpc (stat) +/- 20 Mpc (sys) for our fiducial cosmology (consistent with Planck 2015) and bias model. This measurement extends the use of the BAO technique from the two-point correlation function (2PCF) and power spectrum to the 3PCF and opens an avenue for deriving additional cosmological distance information from future large-scale structure redshift surveys such as DESI. Our measured distance scale from the 3PCF is fairly independent from that derived from the pre-reconstruction 2PCF and is equivalent to increasing the length of BOSS by roughly 10 per cent; reconstruction appears to lower the independence of the distance measurements. Fitting a model including tidal tensor bias yields a moderate-significance (2.6 sigma) detection of this bias with a value in agreement with the prediction from local Lagrangian biasing.</P>
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A TOPOLOGICAL ANALYSIS OF LARGE-SCALE STRUCTURE, STUDIED USING THE CMASS SAMPLE OF SDSS-III
Parihar, Prachi,Vogeley, Michael S.,Gott III, J. Richard,Choi, Yun-Young,Kim, Juhan,Kim, Sungsoo S.,Speare, Robert,Brownstein, Joel R.,Brinkmann, J. IOP Publishing 2014 The Astrophysical journal Vol.796 No.2
<P>We study the three-dimensional genus topology of large-scale structure using the northern region of the CMASS Data Release 10 (DR10) sample of the SDSS-III Baryon Oscillation Spectroscopic Survey. We select galaxies with redshift 0.452 < z < 0.625 and with a stellar mass M-stellar > 10(11.56) M-circle dot. We study the topology at two smoothing lengths: R-G = 21 h(-1) Mpc and R-G = 34 h(-1) Mpc. The genus topology studied at the R-G = 21 h(-1) Mpc scale results in the highest genus amplitude observed to date. The CMASS sample yields a genus curve that is characteristic of one produced by Gaussian random phase initial conditions. The data thus support the standard model of inflation where random quantum fluctuations in the early universe produced Gaussian random phase initial conditions. Modest deviations in the observed genus from random phase are as expected from shot noise effects and the nonlinear evolution of structure. We suggest the use of a fitting formula motivated by perturbation theory to characterize the shift and asymmetries in the observed genus curve with a single parameter. We construct 54 mock SDSS CMASS surveys along the past light cone from the Horizon Run 3 (HR3) N-body simulations, where gravitationally bound dark matter subhalos are identified as the sites of galaxy formation. We study the genus topology of the HR3 mock surveys with the same geometry and sampling density as the observational sample and find the observed genus topology to be consistent with ACDM as simulated by the HR3 mock samples. We conclude that the topology of the large-scale structure in the SDSS CMASS sample is consistent with cosmological models having primordial Gaussian density fluctuations growing in accordance with general relativity to form galaxies in massive dark matter halos.</P>
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Spectroscopic needs for imaging dark energy experiments
Newman, J.A.,Abate, A.,Abdalla, F.B.,Allam, S.,Allen, S.W.,Ansari, R.,Bailey, S.,Barkhouse, W.A.,Beers, T.C.,Blanton, M.R.,Brodwin, M.,Brownstein, J.R.,Brunner, R.J.,Carrasco Kind, M.,Cervantes-Cota, North-Holland 2015 Astroparticle physics Vol.63 No.-
Ongoing and near-future imaging-based dark energy experiments are critically dependent upon photometric redshifts (a.k.a. photo-z's): i.e., estimates of the redshifts of objects based only on flux information obtained through broad filters. Higher-quality, lower-scatter photo-z's will result in smaller random errors on cosmological parameters; while systematic errors in photometric redshift estimates, if not constrained, may dominate all other uncertainties from these experiments. The desired optimization and calibration is dependent upon spectroscopic measurements for secure redshift information; this is the key application of galaxy spectroscopy for imaging-based dark energy experiments. Hence, to achieve their full potential, imaging-based experiments will require large sets of objects with spectroscopically-determined redshifts, for two purposes:*Training: Objects with known redshift are needed to map out the relationship between object color and z (or, equivalently, to determine empirically-calibrated templates describing the rest-frame spectra of the full range of galaxies, which may be used to predict the color-z relation). The ultimate goal of training is to minimize each moment of the distribution of differences between photometric redshift estimates and the true redshifts of objects, making the relationship between them as tight as possible. The larger and more complete our ''training set'' of spectroscopic redshifts is, the smaller the RMS photo-z errors should be, increasing the constraining power of imaging experiments. Requirements: Spectroscopic redshift measurements for ~30,000 objects over >~15 widely-separated regions, each at least ~20arcmin in diameter, and reaching the faintest objects used in a given experiment, will likely be necessary if photometric redshifts are to be trained and calibrated with conventional techniques. Larger, more complete samples (i.e., with longer exposure times) can improve photo-z algorithms and reduce scatter further, enhancing the science return from planned experiments greatly (increasing the Dark Energy Task Force figure of merit by up to ~50%). Options: This spectroscopy will most efficiently be done by covering as much of the optical and near-infrared spectrum as possible at modestly high spectral resolution (λ/Δλ>~3000), while maximizing the telescope collecting area, field of view on the sky, and multiplexing of simultaneous spectra. The most efficient instrument for this would likely be either the proposed GMACS/MANIFEST spectrograph for the Giant Magellan Telescope or the OPTIMOS spectrograph for the European Extremely Large Telescope, depending on actual properties when built. The PFS spectrograph at Subaru would be next best and available considerably earlier, c. 2018; the proposed ngCFHT and SSST telescopes would have similar capabilities but start later. Other key options, in order of increasing total time required, are the WFOS spectrograph at TMT, MOONS at the VLT, and DESI at the Mayall 4m telescope (or the similar 4MOST and WEAVE projects); of these, only DESI, MOONS, and PFS are expected to be available before 2020. Table 2-3 of this white paper summarizes the observation time required at each facility for strawman training samples. To attain secure redshift measurements for a high fraction of targeted objects and cover the full redshift span of future experiments, additional near-infrared spectroscopy will also be required; this is best done from space, particularly with WFIRST-2.4 and JWST. Calibration: The first several moments of redshift distributions (the mean, RMS redshift dispersion, etc.), must be known to high accuracy for cosmological constraints not to be systematics-dominated (equivalently, the moments of the distribution of differences between photometric and true redshifts could be determined instead). The ultimate goal of calibration is to characterize these moments for every subsample used in analyses - i.e., to minimi
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