[논문]THE LUMINOSITY OF TYPE IA SUPERNOVA AND THE PROPERTIES OF THEIR EARLY-TYPE HOST GALAXIES

KANG, YIJUNG; KIM, YOUNG-LO; LEE, YOUNG-WOOK; LIM, DONGWOOK; CHUNG, CHUL; SUNG, EON-CHANG

doi:10.5303/pkas.2015.30.2.487

[국내논문] THE LUMINOSITY OF TYPE IA SUPERNOVA AND THE PROPERTIES OF THEIR EARLY-TYPE HOST GALAXIES 원문보기

천문학논총 = Publications of the Korean Astronomical Society, v.30 no.2, 2015년, pp.487 - 488

KANG, YIJUNG (Center for Galaxy Evolution Research & Department of Astronomy, Yonsei University) , KIM, YOUNG-LO (Center for Galaxy Evolution Research & Department of Astronomy, Yonsei University) , LEE, YOUNG-WOOK (Center for Galaxy Evolution Research & Department of Astronomy, Yonsei University) , LIM, DONGWOOK (Center for Galaxy Evolution Research & Department of Astronomy, Yonsei University) , CHUNG, CHUL (Center for Galaxy Evolution Research & Department of Astronomy, Yonsei University) , SUNG, EON-CHANG (Korea Astronomy and Space Science Institute)

Abstract ▼ AI-Helper

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.

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제안 방법

Basic data reduction and analysis were performed using IRAF, including pre-processing, extraction, wavelength calibration, flux calibration, and heliocentric velocity correction. We also removed weak emission lines from absorption lines using pPXF+GANDALF (Cappellari & Emsellem, 2004; Sarzi et al.

이론/모형

Luminosity-weighted mean age and metallicity of host galaxies were determined using Lick indices by employing the EPS models (Chung et al., 2013; Thomas et al., 2003, 2011; Schiavon, 2007).

참고문헌 (8)

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Chung, C., Yoon, S.-J., Lee, S. -Y., & Lee, Y. -W., 2013, Yonsei Evolutionary Population Synthesis (YEPS) Model. I. Spectroscopic Evolution of Simple Stellar Populations, ApJS, 204, 3

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Sarzi, M., Falcon-Barroso, J., & Davies, R. L., et al., 2006, The SAURON Project - V. Integral-eld emission-line Kinematics of 48 Elliptical and Lenticular Galaxies, MNRAS, 366, 1151

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Schiavon, R. P., 2007, Population Synthesis in the Blue. IV. Accurate Model Predictions for Lick Indices and UBV Colors in Single Stellar Populations, ApJS, 171, 146

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Thomas, D., Maraston, C., & Bender, R., 2003, Stellar Population Models of Lick Indices with Variable Element Abundance Ratios, MNRAS, 339, 897

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Thomas, D., Maraston, C., & Johansson, J., 2011, Flux-calibrated Stellar Population Models of Lick Absorptionline Indices with Variable Element Abundance Ratios, MNRAS, 412, 2183

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