• 천문학논총
• /
• 제27권4호
• /
• pp.321-324
• /
• 2012

Using extensive mid-IR datasets from AKARI, i.e. 9-band photometry covering the wavelength range from $2{\mu}m$ to $24{\mu}m$ and the unbiased spectroscopic survey for sources with $S_{\nu}$($9{\mu}m$)>0.3 mJy, we study starburst galaxies specifically at the redshift of z ~ 0.5, whose mid-IR spectra are clearly dominated by the PAH emission features. PAH-selected galaxies, selected with extremely red mid-IR colour due to PAHs, have high rest-frame PAH-to-stellar luminosity ratios, comparable to those in the most active regions in nearby starburst galaxies. Thus, they seem to have active starburst regions spreading over the whole body. Furthermore, some of PAH-selected galaxies are found to have peculiar rest-frame 11-to-$8{\mu}m$ flux ratios, which is systematically smaller than nearby starburst/AGN spectral templates. This may indicate a systematic difference in the physical condition of ISM between nearby and distant starburst galaxies.

• 천문학회보
• /
• 제42권2호
• /
• pp.78.2-78.2
• /
• 2017

Post-starburst (E+A) galaxies are thought to be in the green valley transition phase between star-forming blue galaxies and quiescent red galaxies. They are identified by their unusual spectra characterized by strong Balmer absorption lines and weak emission lines, indicating a period of starburst followed by abrupt quenching. However, the underlying mechanism that drives the formation of E+A galaxies still remains contradictory or inconclusive. Thus, in order to differentiate between the different formation scenarios of E+A galaxies, we perform a statistical analysis of the environments of E+A galaxies. We spectroscopically identify a large sample of post-starburst galaxies from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) using a selection criteria based on $H{\delta}$ equivalent width. We report our findings and discuss their implications in the context of post-starburst galaxy formation.

• 천문학논총
• /
• 제30권2호
• /
• pp.499-502
• /
• 2015

Starburst galaxies have strong star formation activity and generate large scale outflows which eject a huge amount of gas mass. This process affects galaxy activity, and therefore, the detailed study of nearby starburst galaxies could provide valuable information for the study of distant ones. So far there have been only a few studies of galactic-scale molecular outflows due to the sensitivity limitation of telescopes. Our study provides two nearby examples, NGC 2146 and NGC 3628. We used Nobeyama Millimeter Array (NMA) CO(1-0) data, Chandra soft X-ray data, and NMA 3 mm data to study the kinematics of molecular outflows, their interaction with ionized outflows, and the star forming activity in the starburst region. We found that the gas ejected through molecular outflows is much more significant than that used to form stars.

• 반도체디스플레이기술학회지
• /
• 제13권1호
• /
• pp.83-90
• /
• 2014

Using a ray tracing simulation, we have investigated the moir${\acute{e}}$ and starburst phenomena of touch screen panels (TSPs) based on opaque metallic grids (square, hexagonal, and random grids). It is demonstrated that employing a random metal mesh is the most effective way to suppress the moir${\acute{e}}$ and starburst phenomena at the same time. At high crossing angles between metal mesh of TSPs and black matrix (BM) of displays, however, a random metal mesh brings in stronger moir${\acute{e}}$ phenomenon than a square metal mesh due to point defects. Though the square metal mesh suppresses the moir${\acute{e}}$ effect substantially at high crossing angles, yet it results in the strongest starburst patterns. We have also provided the simulation scheme that can capture the moir${\acute{e}}$ and starburst patterns observed experimentally and useful design guidelines for metal grids.

• 한국정보통신학회논문지
• /
• 제18권5호
• /
• pp.1162-1170
• /
• 2014

본 논문에서는 두 개의 카메라를 이용하여 보다 정확한 동공 인식을 통한 원격방식의 시선 추적을 제안한다. 헤드 장착형 시선추적용으로 개발된 Starburst 알고리즘은 원격방식의 시선추적에서는 카메라가 보다 넓은 영역을 보기 때문에 눈썹, 눈꼬리 등 외란이 많아 스타버스트 알고리즘을 바로 적용하면 동공 중심 추출에 실패하는 경우가 많았다. 이에 템플렛매칭을 이용하여 대략적인 동공영역을 찾고, 찾은 영역 내에서만 스타버스트 알고리즘으로 동공의 경계 후보점들을 찾은 후 보완된 RANSAC 알고리즘으로 타원근사하여 동공의 중심을 추출하였다. 추출된 동공중심을 머리의 움직임에 거의 영향을 받지 않도록 4개의 적외선 LED를 모니터 네 구석에 부착하고 Homography normalization을 적용하였다. 스크린 좌표계로 변환할 때 기존에는 호모그래피를 사용하였으나, 카메라 렌즈의 비선형왜곡을 보상하기 위해 여기서는 고차다항식을 이용한 캘리브레이션 기법을 이용하였다. 끝으로, 두 대의 카메라를 사용하여 정확도와 신회성이 향상됨을 보인다.

• 천문학회지
• /
• 제29권spc1호
• /
• pp.159-160
• /
• 1996

Recent high resolution CO observations of normal and starburst galaxies at Owens Valley Millimeter Array are summarized. While normal disk galaxies generally show exponential distribution which follows the optical blue light, starburst galaxies are often characterized by a compact ($\~$1 kpc) nuclear complex whose surface gas mass density is strongly correlated with the observed large infrared luminosity and thus the ongoing massive star formation.

• 천문학회보
• /
• 제43권1호
• /
• pp.31.1-31.1
• /
• 2018

While astronomers are working hard to detect the earliest galaxies and to follow their evolution to redshift z~0, they remain baffled by the present-day dichotomy between disky, star forming (aka late-type) galaxies and quiescent, spheroidal (aka early-type) galaxies. The key is to find galaxies in transition from one class to the other, whose spectra indicate intense recent star formation that has now ended. We have identified thousands of such "post-starburst galaxies" and discovered that they are often the products of late-type galaxy-galaxy mergers. Their current kinematics, stellar populations, and morphologies are consistent with late- to early-type galaxy evolution. I will discuss recent work that suggests new connections between this violent history and the central supermassive black hole. In particular, the molecular gas reservoir of a post-starburst galaxy declines rapidly after the starburst ends and in a manner consistent with feedback from an active nucleus. Furthermore, a star is ~300x more likely to be tidally disrupted by the nucleus of a post-starburst galaxy than in other galaxies. Like the well-known black hole-bulge mass correlation, these surprising links between the properties of a galaxy on kpc scales and its supermassive black hole on pc scales require explanation.

• 천문학회보
• /
• 제36권2호
• /
• pp.55.1-55.1
• /
• 2011

Luminous infrared galaxies (LIRGs; $L_{IR}$ > ${10^{11}}_{Lsun}$) are the most powerful objects in the local Universe. Previous work suggested that dust re-processing of starburst and/or active galactic nuclei (AGN) activity, triggered by galaxy interactions, is responsible for their enormous infrared emission. To understand the nature of LIRGs, it is essential to determine their spectral types. Optical spectral types of 115 ultraluminous infrared galaxies in the southern sky are presented using CTIO observations. The AGN fraction is on average 50% and increases with infrared luminosity. Near-infrared spectral types of 36 LIRGs are also presented based on AKARI observations. In the sample, 12 optically elusive buried AGNs are found. To investigate the evolutionary sequence of LIRGs, star formation histories of ~6000 LIRGs in the SDSS and IRAS/AKARI matched sample are derived by comparing observed optical spectra and stellar population models. AGN-dominated LIRGs are currently massive relative to starburst-dominated LIRGs, which originates from an enhancement of star formation at intermediate-ages. For ~1100 early-type LIRGs, optical and NIR fundamental planes (FPs) are constructed. The FP of LIRGs is significantly different from that of normal early-type galaxies, but the difference is minimized in low luminous and AGN-like LIRGs. These findings support that the importance of AGN is growing as infrared luminosity increases and that LIRGs follow at least in the high mass regime the standard evolutionary scenario: starburst LIRGs evolve into AGN LIRGs and finally into normal early-type galaxies.

• 천문학회보
• /
• 제39권1호
• /
• pp.39.2-39.2
• /
• 2014

We present a photometric study of star clusters in the nuclear starburst region of NGC 253 using gVI, YJ, and H band images in the Hubble Space Telescope archive. We find about one thousand star clusters in about 200"x200" field by visual inspection with I<21. We also find about ten thousand star clusters in the same field by automated classification method with magnitude range of 21< I $$\leq_-$$ 24. Ages and masses of star clusters are estimated using spectral energy distribution fitting method. Age distribution of star cluster shows two distinguished young populations with peak ages at 3.5 Myr and 18 Myr. Old populations (>100 Myr) are exist, but their number is small. About thirty young massive star clusters (<10 Myr, ) are found in nuclear region of NGC 253 which are regarded as a result of the recent starburst. Mass function of young star clusters in NGC 253 is somewhat different with those of star clusters in other galaxies. This result suggests that initial cluster mass functions (ICMFs) for star clusters are not universial. Especially ICMF in starburst galaxies may be distinguishable compared with those in normal spiral galaxies. We discuss the implications of these results.

• 천문학회보
• /
• 제45권1호
• /
• pp.37.1-37.1
• /
• 2020

Cosmic-ray protons (CRp) are efficiently produced at starburst galaxies (SBGs), where the star formation rate (SFR) rate is high. In this talk, we present estimates of gamma-ray and neutrino emissions from nearby SBGs, M82, NGC253, and Arp220. Inside the starburst nucleus (SBN), CRp are accelerated at supernova remnant (SNR) shocks as well as at stellar wind (SW) termination shocks, and their transport is governed by the advection due to starburst-driven wind and diffusion mediated by turbulence. We here model the momentum distributions of SNR and SW-produced CRp with single or a double power-law forms. We also employ two different diffusion models, where CRp are resonantly scattered off large-scale turbulence in SBN or self-excited waves driven by CR streaming instability. We then calculate gamma-ray/neutrino fluxes. The observed gamma-ray fluxes by Fermi-LAT, Veritas, and H.E.S.S are well reproduced with double power-law distribution for SNR-produced CRp and the CRp diffusion by self-excited turbulence. The estimated neutrino fluxes are <~10-3 of the atmospheric neutrino flux in the energy range of Eneutrino <~100 GeV and <~10-1 of the IceCube point source sensitivity in the energy range of Eneutrino >~60 TeV.