The Attitude of Kazakhstani Millennials to Images with Traditional Overtones

Gulnara Z. Karimova,Christopher Marquette,Yevgeniya D. Kim 한국외국어대학교(글로벌캠퍼스) 러시아연구소 2020 REGION Vol.9 No.2

The purpose of this article is to use questionnaires and interviews to gain insight into how the young generation in Kazakhstan perceives images with traditional overtones. Respondents were exposed to images of female figures with Central Asian facial features dressed in traditional Kazakh clothing, a male hunter holding a golden eagle, and a nomad’s tent set against the backdrop of a steppe landscape. These images of pre-Soviet nomadic life—preliminarily designated by the interviewees as traditional Kazakh images—may serve as further attestation to “localization” by means of distancing from Soviet-era symbols. Qualitative and quantitative analysis are used to reveal the attitude of Generation Y individuals toward these images with Kazakh traditional overtones. Research analysis is used to map the preference of Kazakhstani youth as a response to the nationalization policy of the Nazarbayev regime. The findings lead to the important discovery that Kazakhstani cultural representation, which is essentially based on Kazakh pre-Soviet ethnic representation, is nonetheless shared by Kazakhstani youth of varying ethnicities.

REVISITING THE MICROLENSING EVENT OGLE 2012-BLG-0026: A SOLAR MASS STAR WITH TWO COLD GIANT PLANETS

Beaulieu, J.-P.,Bennett, D. P.,Batista, V.,Fukui, A.,Marquette, J.-B.,Brillant, S.,Cole, A. A.,Rogers, L. A.,Sumi, T.,Abe, F.,Bhattacharya, A.,Koshimoto, N.,Suzuki, D.,Tristram, P. J.,Han, C.,Gould, A American Astronomical Society 2016 The Astrophysical Journal Vol.824 No.2

<P>Two cold gas giant planets orbiting a G-type main-sequence star in the galactic disk were previously discovered in the high-magnification microlensing event OGLE-2012-BLG-0026. Here, we present revised host star flux measurements and a refined model for the two-planet system using additional light curve data. We performed high angular resolution adaptive optics imaging with the Keck and Subaru telescopes at two epochs while the source star was still amplified. We detected the lens flux, H = 16.39 +/- 0.08. The lens, a disk star, is brighter than predicted from the modeling in the original study. We revisited the light curve modeling using additional photometric data from the B&C telescope in New Zealand and CTIO 1.3 m H-band light curve. We then include the Keck and Subaru adaptive optic observation constraints. The system is composed of a similar to 4-9 Gyr lens star of M-lens = 1.06 +/- 0.05 M circle dot at a distance of D-lens = 4.0 +/- 0.3 kpc, orbited by two giant planets of 0.145 +/- 0.008 M-Jup and 0.86 +/- 0.06 M-Jup, with projected separations of 4.0 +/- 0.5 au and 4.8 +/- 0.7 au, respectively. Because the lens is brighter than the source star by 16 +/- 8% in H, with no other blend within one arcsec, it will be possible to estimate its metallicity using subsequent IR spectroscopy with 8-10 m class telescopes. By adding a constraint on the metallicity it will be possible to refine the age of the system.</P>

The EPOCH Project : I. Periodic variable stars in the EROS-2 LMC database⋆

Kim, Dae-Won,Protopapas, Pavlos,Bailer-Jones, Coryn A. L.,Byun, Yong-Ik,Chang, Seo-Won,Marquette, Jean-Baptiste,Shin, Min-Su Springer-Verlag 2014 Astronomy and astrophysics Vol.566 No.-

SUB-SATURN PLANET MOA-2008-BLG-310Lb: LIKELY TO BE IN THE GALACTIC BULGE

Janczak, Julia,Fukui, A.,Dong, Subo,Monard, L. A. G.,Kozłowski, Szymon,Gould, A.,Beaulieu, J. P.,Kubas, Daniel,Marquette, J. B.,Sumi, T.,Bond, I. A.,Bennett, D. P.,Abe, F.,Furusawa, K.,Hearnshaw, J. B IOP Publishing 2010 The Astrophysical journal Vol.711 No.2

<P>We report the detection of sub-Saturn-mass planet MOA-2008-BLG-310Lb and argue that it is the strongest candidate yet for a bulge planet. Deviations from the single-lens fit are smoothed out by finite-source effects and therefore are not immediately apparent from the light curve. Nevertheless, we find that a model in which the primary has a planetary companion is favored over the single-lens model by Delta chi(2) similar to 880 for an additional 3 degrees of freedom. Detailed analysis yields a planet/star mass ratio q = (3.3 +/- 0.3) x 10(-4) and an angular separation between the planet and star within 10% of the angular Einstein radius. The small angular Einstein radius, theta(E) = 0.155 theta 0.011 mas, constrains the distance to the lens to be D(L) > 6.0 kpc if it is a star (M(L) > 0.08 M(circle dot)). This is the only microlensing exoplanet host discovered so far that must be in the bulge if it is a star. By analyzing VLT NACO adaptive optics images taken near the baseline of the event, we detect additional blended light that is aligned to within 130 mas of the lensed source. This light is plausibly from the lens, but could also be due to a companion to the lens or source, or possibly an unassociated star. If the blended light is indeed due to the lens, we can estimate the mass of the lens, M(L) = 0.67 +/- 0.14 M(circle dot), planet mass m = 74 +/- 17 M(circle plus), and projected separation between the planet and host, 1.25 +/- 0.10 AU, putting it right on the 'snow line.' If not, then the planet has lower mass, is closer to its host and is colder. To distinguish among these possibilities on reasonable timescales would require obtaining Hubble Space Telescope images almost immediately, before the source-lens relative motion of mu = 5 mas yr(-1) causes them to separate substantially.</P>

THE FIRST NEPTUNE ANALOG OR SUPER-EARTH WITH A NEPTUNE-LIKE ORBIT: MOA-2013-BLG-605LB

Sumi, T.,Udalski, A.,Bennett, D. P.,Gould, A.,Poleski, R.,Bond, I. A.,Skowron, J.,Rattenbury, N.,Pogge, R. W.,Bensby, T.,Beaulieu, J. P.,Marquette, J. B.,Batista, V.,Brillant, S.,Abe, F.,Asakura, Y.,B American Astronomical Society 2016 The Astrophysical journal Vol.825 No.2

<P>We present the discovery of the first Neptune analog exoplanet or super-Earth with a Neptune-like orbit, MOA-2013-BLG-605Lb. This planet has a mass similar to that of Neptune or a super-Earth and it orbits at 9 similar to 14 times the expected position of the snow line, a(snow), which is similar to Neptune's separation of 11 a(snow) from the Sun. The planet/host-star mass ratio is q = (3.6 +/- 0.7) x 10(-4) and the projected separation normalized by the Einstein radius is s = 2.39 +/- 0.05. There are three degenerate physical solutions and two of these are due to a new type of degeneracy in the microlensing parallax parameters, which we designate 'the wide degeneracy.' The three models have (i) a Neptune-mass planet with a mass of M-p = 21(-7)(+6)M(circle plus) orbiting a low-mass M-dwarf with a mass of M-h = 0.19(-0.06)(+0.05)M(circle dot), (ii) a mini-Neptune with M-p = 7.9(-1.2)(+1.8)M(circle plus) orbiting a brown dwarf host with M-h = 0.068(-0.011)(+0.019)M(circle dot), and (iii) a super-Earth with M-p = 3.2(-0.3)(+0.5)M(circle plus) orbiting a low-mass brown dwarf host with M-h = 0.025(-0.004)(+0.005)M(circle dot), which is slightly favored. The 3D planet-host separations are 4.6(-1.2)(+4.7) au, 2.1(-0.2) (+1.0) au, and 0.94(-0.02)(+0.67) au, which are 8.9(-1.4)(+10.5), 12(-1)(+7), or 14(-1)(+11) times larger than a(snow) for these models, respectively. Keck adaptive optics observations confirm that the lens is faint. This discovery suggests that low-mass planets with Neptune-like orbits are common. Therefore processes similar to the one that formed Neptune in our own solar system or cold super-Earths may be common in other solar systems.</P>

MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT

Bachelet, E.,Shin, I.-G.,Han, C.,Fouqué,, P.,Gould, A.,Menzies, J. W.,Beaulieu, J.-P.,Bennett, D. P.,Bond, I. A.,Dong, Subo,Heyrovský,, D.,Marquette, J.-B.,Marshall, J.,Skowron, J.,Street, IOP Publishing 2012 The Astrophysical journal Vol.754 No.1

<P>Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 +/- 0.004) x 10(-3) and the projected separation is s = 1.1228 +/- 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large theta(E) = 1.38 +/- 0.11 mas. Combining this measurement with constraints on the 'microlens parallax' and the lens flux, we can only limit the host mass to the range 0.13 < M/M-circle dot < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M-* = 0.67(-0.13)(+0.33) M-circle dot and m(p) = 1.5(-0.3)(+0.8) M-JUP at a distance of D = 2.3 +/- 0.6 kpc, and with a semi-major axis of a = 2(-1)(+3) AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric.</P>