GROUND-BASED Paα NARROW-BAND IMAGING OF LOCAL LUMINOUS INFRARED GALAXIES. I. STAR FORMATION RATES AND SURFACE DENSITIES

Ken Tateuchi, Masahiro Konishi, Kentaro Motohara, Hidenori Takahashi, Natsuko Mitani Kato, Yutaro Kitagawa, Soya Todo, Koji Toshikawa, Shigeyuki Sako, Yuka K. Uchimoto, Ryou Ohsawa, Kentaro Asano, Yoshifusa Ita, Takafumi Kamizuka, Shinya Komugi, Shintaro Koshida, Sho Manabe, Tomohiko Nakamura, Asami Nakashima, Kazushi OkadaToshinobu Takagi, Toshihiko Tanabé, Mizuho Uchiyama, Tsutomu Aoki, Mamoru Doi, Toshihiro Handa, Kimiaki Kawara, Kotaro Kohno, Takeo Minezaki, Takashi Miyata, Tomoki Morokuma, Takeo Soyano, Yoichi Tamura, Masuo Tanaka, Ken'Ichi Tarusawa, Yuzuru Yoshii

Research output: Contribution to journalArticlepeer-review

15 Citations (Scopus)

Abstract

Luminous infrared galaxies (LIRGs) are enshrouded by a large amount of dust produced by their active star formation, and it is difficult to measure their activity in optical wavelengths. We have carried out Paα narrow-band imaging observations of 38 nearby star forming galaxies including 33 LIRGs listed in the IRAS Revised Bright Galaxy Sample catalog with the Atacama Near InfraRed camera on the University of Tokyo Atacama Observatory (TAO) 1.0 m telescope (miniTAO). Star formation rates (SFRs) estimated from the Paα fluxes, corrected for dust extinction using the Balmer decrement method (typically AV ∼ 4.3 mag), show a good correlation with those from the bolometric infrared luminosity of the IRAS data within a scatter of 0.27 dex. This suggests that the correction of dust extinction for the Paα flux is sufficient in our sample. We measure the physical sizes and surface densities of infrared luminosities (ΣL(IR)) and the SFR (ΣSFR) of star forming regions for individual galaxies, and we find that most of the galaxies follow a sequence of local ultra-luminous or luminous infrared galaxies (U/LIRGs) on the L(IR)-ΣL(IR) and SFR-ΣSFR plane. We confirm that a transition of the sequence from normal galaxies to U/LIRGs is seen at L(IR) = 8 × 1010 L . Also, we find that there is a large scatter in physical size, different from normal galaxies or ULIRGs. Considering the fact that most U/LIRGs are merging or interacting galaxies, this scatter may be caused by strong external factors or differences in their merging stages.

Original languageEnglish
Article number1
JournalAstrophysical Journal, Supplement Series
Volume217
Issue number1
DOIs
Publication statusPublished - 2015 Mar 1

Keywords

  • HII regions
  • galaxies: interactions
  • galaxies: starburst
  • infrared: galaxies
  • stars: formation

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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