miniTAO/ANIR Paα SURVEY OF LOCAL LIRGs

Tateuchi, Ken; Motohara, Kentaro; Konishi, Masahiro; Takahashi, H.; Kato, Natsuko; Uchimoto, Yuka Katsuno; Toshikawa, Koji; Ohsawa, Ryou; Kitagawa, Yoichi; Yoshii, Yuzuru; Doi, M.; Kohno, Kotaro; Kawara, Kimiaki; Tanaka, Masuo; Miyata, Takashi; Tanabé, Toshihiko; Minezaki, Takeo; Sako, Shigeyuki; Morokuma, Tomoki; Tamura, Motohide; Aoki, Tsutomu; Soyano, T.; Tarusawa, Kenfichi; Koshida, Shintaro; Kamizuka, Takafumi; Nakamura, Tomohiko; Asano, Kentaro; Uchiyama, Mitsuru; Okada, Kazushi; Ita, Yoshifusa

doi:10.5303/pkas.2012.27.4.297

Cited by 6 publications

(24 citation statements)

References 4 publications

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“…We observed the blended set of 2 1 -1 1 (ν rest = 96.756 GHz, E up /k = 28.0 K), 2 0 -1 0 E (ν rest = 96.745 GHz, E up /k = 20.1 K), 2 0 -1 0 A + (ν rest = 96.741 GHz, E up /k = 7.0 K), and 2 −1 -1 −1 E (ν rest = 96.739 GHz, E up /k = Table 2). The red cross shows the position of the eastern nucleus defined by the peak position of the Ks-band observation (Tateuchi et al 2012).…”

Section: Co (1-0)mentioning

confidence: 99%

“…The (box-averaged) kinetic temperature near the eastern nucleus (R21a) is constrained to within 25 -90 K (the best fit is 50 K), as shown in (4-3). The white cross shows the position of the eastern nucleus defined by the peak position of the Ks-band observation (Tateuchi et al 2012). (bottom) 1.…”

Section: Casementioning

confidence: 99%

“…There is a dust lane from north to south in front of the eastern galaxy. The red crosses show the positions of the nuclei defined by the peak positions of the Ks-band observation (Tateuchi et al 2012). The white ellipse shows a field of view of 3-point mosaic observation with band 7, while the white circle shows a field of view of 7-point mosaic observation with band 7 (see §2).…”

Section: Introductionmentioning

confidence: 99%

“…The beam size of each line is shown in the bottom-left of the images ( Table 2). The red crosses show the positions of the nuclei defined by the peak positions of the Ks-band observation (Tateuchi et al 2012). levels of the channel maps with 30 km s −1 resolution are 1.0 mJy beam −1 and 0.8 mJy beam −1 , respectively. Furthermore, we made continuum maps at each observing frequency by adding the line-free channels.…”

Section: Introductionmentioning

confidence: 99%

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Alma Multi-Line Observations of the Ir-Bright Merger Vv 114

Saito

Iono

Yun

et al. 2015

ApJ

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We present ALMA cycle 0 observations of the molecular gas and dust in the IR-bright mid-stage merger VV 114 obtained at 160 -800 pc resolution. The main aim of this study is to investigate the distribution and kinematics of the cold/warm gas and to quantify the spatial variation of the excitation conditions across the two merging disks. The data contain 10 molecular lines, including the first detection of extranuclear CH 3 OH emission in interacting galaxies, as well as continuum emission. We map the 12 CO (3-2)/ 12 CO (1-0) and the 12 CO (1-0)/ 13 CO (1-0) line ratio at 800 pc resolution (in the units of K km s −1 ), and find that these ratios vary from 0.2 -0.8 and 5 -50, respectively. Conversely, the 200 pc resolution HCN (4-3)/HCO + (4-3) line ratio shows low values (< 0.5) at a filament across the disks except for the unresolved eastern nucleus which is three times higher (1.34 ± 0.09). We conclude from our observations and a radiative transfer analysis that the molecular gas in the VV 114 system consists of five components with different physical and chemical conditions; i.e., 1) dust-enshrouded nuclear starbursts and/or AGN, 2) wide-spread star forming dense gas, 3) merger-induced shocked gas, 4) quiescent tenuous gas arms without star formation, 5) H 2 gas mass of (3.8 ± 0.7) × 10 7 M ⊙ (assuming a conversion factor of α CO = 0.8 M ⊙ (K km s −1 pc 2 ) −1 ) at the tip of the southern tidal arm, as a potential site of tidal dwarf galaxy formation.

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Section: Co (1-0)mentioning

confidence: 99%

Section: Casementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Alma Multi-Line Observations of the Ir-Bright Merger Vv 114

Saito

Iono

Yun

et al. 2015

ApJ

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“…We have carried out Paα narrow-band imaging survey of local LIRGs (Tateuchi et al 2012;Tateuchi et al 2013;Tateuchi et al 2015) with Atacama Near InfraRed camera (ANIR; Motohara et al 2008;Motohara et al 2010;Konishi et al 2015) on the University of Tokyo Atacama Observatory 1.0 m telescope (miniTAO; Minezaki et al 2010;Yoshii et al 2010) installed at the summit of Co. Chajnantor (5640m altitude) in northern Chile. Thanks to the high altitude and the extremely low water vapor of the site, we can stably observe Paα emission line even from the ground (Motohara et al 2010).…”

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confidence: 99%

Ground-based Paα narrow-band imaging of local luminous infrared galaxies. II. Bulge structure and star formation activity

Tateuchi

Motohara

Konishi

et al. 2019

Publications of the Astronomical Society of Japan

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We present properties of two types of bulges (classical and pseudo-bulges) in 20 luminous infrared galaxies (LIRGs) observed in the near infrared of the H, K s and 1.91µm narrow-band targeting at the hydrogen Paα emission line by the University of Tokyo Atacama Observatory (TAO) 1.0 m telescope. To classify the two types of bulges, we first perform a two-dimensional bulge-disk decomposition analysis in the K s -band images. The result shows a tentative bimodal distribution of Sérsic indices with a separation at log(n b ) ∼ 0.5, which is consistent with that of classical and normal galaxies. We next measure extents of the distribution of star forming regions in Paα emission line images, normalized with the size of the bulges, and find that they decrease with increasing Sérsic indices. These results suggest that star-forming galaxies with classical bulges have compact star forming regions concentrated within the bulges, while those with pseudobulges have extended star forming regions beyond the bulges, suggesting that there are different formation scenarios at work in classical and pseudobulges.

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Investigating AGN/Starburst activities through ALMA multi-line observations in the mid-stage IR-bright merger VV 114

et al. 2014

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We present ALMA cycle 0 observations of the luminous merger VV 114. One of the main goals is to investigate mechanisms of molecular line ratio enhancement. Regions with the high 12CO (1–0)/13CO (1–0) and 12CO (3–2)/12CO (1–0) is located at a central filamentary structure (∼6 kpc) in VV 114. The filament consists of the eastern nucleus and the overlap region, where the galaxy disks are colliding. We also investigate these molecular line ratios on the Kennicutt-Schmidt law. VV 114 fills a gap between the “starburst” sequence and the “normal disk” sequence, and regions with the high ratios show the high ΣSFR and ΣH2. We suggest that the high ratios in VV 114 are due to star-forming activities in the both progenitor's nuclei and the merger-induced overlap region.

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miniTAO/ANIR Paα SURVEY OF LOCAL LIRGs

Cited by 6 publications

References 4 publications

Alma Multi-Line Observations of the Ir-Bright Merger Vv 114

Alma Multi-Line Observations of the Ir-Bright Merger Vv 114

Ground-based Paα narrow-band imaging of local luminous infrared galaxies. II. Bulge structure and star formation activity

Investigating AGN/Starburst activities through ALMA multi-line observations in the mid-stage IR-bright merger VV 114

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