• 천문학논총
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• 제30권2호
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• pp.565-568
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• 2015

In this work, we study the correlation between the photon index (${\Gamma}$) of the X-ray spectrum and the 2-10 keV X-ray luminosity ($L_X$) for black hole X-ray binaries (BHBs). The BHB sample is mainly from the quiescent, hard and intermediate states, with values of $L_X$ ranging from ${\sim}10^{30.5}$ to $10^{37.5}$ erg $s^{-1}$. We find that the photon index ${\Gamma}$ is positively or negatively correlated with the X-ray luminosity $L_X$, for $L_X$ above or below a critical value, ${\sim}10^{36.5}$ erg $s^{-1}$. This result is consistent with previous works. Moreover, when $L_X{\leq}{\sim}10^{33}$ erg $s^{-1}$, we found that the photon index is roughly independent of the X-ray luminosity. We interpret the above correlations in the framework of a coupled hot accretion flow - jet model. Besides, we also find that in the moderate-luminosity region, different sources may have different anti-correlation slopes, and we argue this diversity is caused by the different value of ${\delta}$, which describes the fraction of turbulent dissipation that directly heats electrons.

• 천문학논총
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• 제30권2호
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• pp.487-488
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• 2015

In type Ia supernovae (SNe Ia) cosmology, a well-established correlation exists between the mass of host galaxies and the Hubble residual (HR) of SNe Ia. In order to investigate the origin of this correlation, we used low-resolution spectroscopic data of early-type host galaxies obtained from our YOnsei Nearby Supernovae Evolution Investigation (YONSEI) project. We measured velocity dispersions and Lick/IDS absorption line indices from these fully calibrated spectra. These indices were used to estimate the luminosity-weighted mean age, metallicity and mass of host galaxies. We found a tight correlation between host mass and population age, which is consistent with the "downsizing" trend in early-type galaxies. This suggests that the well-established correlation between HR and host mass is most likely due to the difference in population age. More observations, which are in progress, are required to understand the impact of luminosity evolution on SNe Ia cosmology.

• 천문학논총
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• 제30권2호
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• pp.321-325
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• 2015

Determining the absolute neutrino mass scale and the neutrino mass hierarchy are central goals in particle physics, with important implications for the Standard Model. However, the final answer may come from cosmology, as laboratory experiments provide measurements for two of the squared mass differences and a stringent lower bound on the total neutrino mass - but the upper bound is still poorly constrained, even when considering forecasted results from future probes. Cosmological tracers are very sensitive to neutrino properties and their total mass, because massive neutrinos produce a specific redshift-and scale-dependent signature in the power spectrum of the matter and galaxy distributions. Stringent upper limits on ${\sum}m_v$ will be essential for understanding the neutrino sector, and will nicely complement particle physics results. To this end, we describe here a series of cosmological hydrodynamical simulations which include massive neutrinos, specifically designed to meet the requirements of the Baryon Acoustic Spectroscopic Survey (BOSS) and focused on the Lyman-${\alpha}$ ($Ly{\alpha}$) forest - also a useful theoretical ground for upcoming surveys such as SDSS-IV/eBOSS and DESI. We then briefly highlight the remarkable constraining power of the $Ly{\alpha}$ forest in terms of the total neutrino mass, when combined with other state-of-the-art cosmological probes, leaving to a stringent upper bound on ${\sum}m_v$.

• 수완나부미
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• 제6권1호
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• pp.161-191
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• 2014

The entry of the logging industry in the once heavily forested riverine middle Agusan Valley where aboriginal Manobos live meant the entry of the material practice of wage labor into this out-of-the-way place. Wage labor converted the once relatively isolated, subsistence animist Manobos into laborers of the expanding capitalist regime. A symptom of modernity, this wage labor also accompanied the coming of Visayan settlers (also loggers paid by wage) who introduced indigenous Manobos the compadrazgo social relationship. This friendly relationship across ethnic identities legitimated social ties and is a social material practice represented in recent bilingual Manobo possession rituals where the Visayan spirit is incarnated along with Manobo spirits. To understand the idea behind spirit embodiment, I explore Manobo ritual as mimesis or poeisis. This representation is shaped by concrete material realities as much as these realities, in turn, are reconfigured by ritual practice. In the older Manobo cosmology, which is based on subsistence economy and dependent on the forest and rivers, individuals have an externalized self (as manifest in the idea of twin soul), in which the inner vital principle is co-extensive with a spirit double in cosmos. Manobos imitate the perceived workings of nature in ritual so as to control them in times of illnesses. In contrast, the mimesis of the Visayan spirit is based on a different political economic set up with its attendant asymmetrical interpersonal relationship. By symbolically representing the Visayan patron as friend, Manobos are able to negotiate the predicament of their subalternity in local modernity.

• Monthly Notices of the Royal Astronomical Society
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• 제501권4호
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• pp.5616-5645
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• 2021

We analyse the large-scale clustering in Fourier space of emission line galaxies (ELG) from the Data Release 16 of the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey. The ELG sample contains 173 736 galaxies covering 1170 deg² in the redshift range 0.6 eff = 0.845 we measure D_V(z_eff)/r_drag = 18.33^+0.57_-0.62, with D_V the volume-averaged distance and r_drag the comoving sound horizon at the drag epoch. In combination with the RSD measurement, at z_eff = 0.85 we find fσ₈(z_eff) = 0.289^+0.085_-0.096, with f the growth rate of structure and σ₈ the normalization of the linear power spectrum, D_H(z_eff)/r_drag = 20.0^+2.4_-2.2 and D_M(z_eff)/r_drag = 19.17 ± 0.99 with D_H and D_M the Hubble and comoving angular distances, respectively. These results are in agreement with those obtained in configuration space, thus allowing a consensus measurement of fσ₈(z_eff) = 0.315 ± 0.095, D_H(z_eff)/r_drag = 19.6^+2.2_-2.1 and D_M(z_eff)/r_drag = 19.5 ± 1.0. This measurement is consistent with a flat ΛCDM model with Planck parameters.

• 천문학회보
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• 제43권1호
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• pp.48.3-48.3
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• 2018

We present the methodology to probe the initial condition of the universe using SPHEREx.

• 천문학회지
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• 제29권spc1호
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• pp.31-33
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• 1996

The role of gravitational lenses as valuable tools for astrophysics and cosmology is highlighted.

• 천문학회보
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• 제40권1호
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• pp.41.1-41.1
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• 2015

Hierarchical galaxy formation models under LCDM cosmology predict that the most massive structures such as galaxy clusters (M > $10^{14}M_{\odot}$) appear late (z < 1) in the history of the universe through hierarchical clustering of small objects. Galaxy formation is also expected to be accelerated in overdense environments, with the star formation rate-density relation to be established at z ~ 2. In this talk, we present our search of massive structures of galaxies at 0.7 < z < 4, using the data from GOODS survey and our own imaging survey, Infrared Medium-deep Survey (IMS). From these studies, we find that there are excess of massive structures of galaxies at z > 2 in comparison to the Millennium simulation data. At 1 < z < 2, the number density of massive structures is consistent with the simulation data, but the star formation history is more or less identical between field and cluster. The star formation quenching process is dominated by internal process (stellar mass). The environmental effect becomes important only at z < 1, which contributes to create the well known star formation-density relation in the local universe. Our results suggest that galaxy formation models under LCDM cosmology may require further refinements to match the observation.

• 천문학회지
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• 제37권5호
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• pp.533-541
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• 2004

The origin of magnetic fields in the universe remains an outstanding problem in cosmology. We propose that these fields are produced by shocks during the large-scale structure formation. We discuss the mechanism of the field generation via the counter-streaming (Weibel) instability. We also show that these Weibel-generated fields are long-lived and weakly coupled to dissipation. Subsequent field amplification by the intra-cluster turbulence may also take place, thus maintaining the magnetic energy density close to equipartition.

• 천문학회지
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• 제38권2호
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• pp.129-133
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• 2005

The temperature (T) and entropy (S) fields of baryonic gas, or intergalactic medium (IGM), in the ACDM cosmology are analyzed using simulation samples produced by a hybrid cosmological hydrodynamic/N-body code based on the weighted essentially non-oscillatory scheme. We demonstrate that, in the nonlinear regime, the dynamical similarity between the IGM and dark matter will be broken in the presence of strong shocks in the IGM. The heating and entropy production by the shocks breaks the IGM into multiple phases. The multiphase and non-Gaussianity of the IGM field would be helpful to account for the high-temperature and high-entropy gas observed in groups and clusters with low-temperature IGM observed by Ly$\alpha$ forest lines and the intermittency observed by the spikes of quasi-stellar object's absorption spectrum.