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

Tateuchi, Ken; Konishi, Masahiro; Motohara, Kentaro; Takahashi, H.; Kato, Natsuko; Kitagawa, Yoichi; Todo, Soya; Toshikawa, Koji; Sako, Shigeyuki; Uchimoto, Yuka Katsuno; Ohsawa, Ryou; Asano, Kentaro; Ita, Yoshifusa; Kamizuka, Takafumi; Komugi, Shinya; Koshida, Shintaro; Manabe, Sho; Nakamura, Tomohiko; Nakashima, A.; Okada, Kazushi; Takagi, Toshinobu; Tanabé, Toshihiko; Uchiyama, Mitsuru; Aoki, Tsutomu; Doi, Mamoru; Handa, Toshihiro; Kawara, Kimiaki; Kohno, Kotaro; Minezaki, Takeo; Miyata, Takashi; Morokuma, Tomoki; Soyano, T.; Tamura, Motohide; Tanaka, Masuo; Tarusawa, K.; Yoshii, Yuzuru

doi:10.1088/0067-0049/217/1/1

Cited by 25 publications

(25 citation statements)

References 103 publications

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“…They also report about our IRAM-30m observations of CO emission, which were not published, with a molecular mass of M(H 2 ) = 8.5 10 9 M . The star formation rate of the ensemble has been estimated to be 21.9 M /yr from Paα by Tateuchi et al (2015).…”

Section: Arp 295nmentioning

confidence: 99%

Molecular gas content of shell galaxies

Mancillas

Combes

Duc

2019

A&A

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Shells are fine stellar structures identified by their arc-like shapes present around a galaxy and currently thought to be vestiges of galaxy interactions and/or mergers. The study of their number, geometry, stellar populations and gas content can help to derive the interaction/merger history of a galaxy. Numerical simulations have proposed a mechanism of shell formation through phase wrapping during a radial minor merger. Alternatively, there could be merely a space wrapping, when particles have not made any radial oscillation yet, but are bound by their radial expansion, or produce an edge-brightened feature. These can be distinguished, because they are expected to keep a high radial velocity. While shells are first a stellar phenomenon, HI and CO observations have revealed neutral gas associated with shells. Some of the gas, the most diffuse and dissipative, is expected to be driven quickly to the center if it is travelling on nearly radial orbits. Molecular gas, distributed in dense clumps, is less dissipative, and may be associated to shells. It can then determine the shell velocity, too difficult to obtain from stars. We present here a search for molecular gas in nine shell galaxies with the IRAM-30m telescope. Six of them are detected in their galaxy center, and in three galaxies, we clearly detect molecular gas in shells. The derived amount of molecular gas varies from 1.5 10 8 to 3.4 10 9 M in the shells. For two of them (Arp 10 and NGC 3656), the shells are characteristic of an oblate system. Their velocity is nearly systemic, and we conclude that these shells are phase-wrapped. For the third one (NGC 3934) the shells appear to participate in the rotation. Follow up with higher spatial resolution is required to conclude.

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Section: Arp 295nmentioning

confidence: 99%

Molecular gas content of shell galaxies

Mancillas

Combes

Duc

2019

A&A

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“…UGC 2238 is classified as a LINER by Veilleux et al (1995). Tateuchi et al (2015) note extended Paα emission over a 3 kpc region in the disk. The Chandra data for UGC 2238 have not previously been published.…”

Section: Mrk 231 (Iras 12540+5708)mentioning

confidence: 99%

Diffuse X-Ray-emitting Gas in Major Mergers

Smith

Campbell

Struck

et al. 2018

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Using archived data from the Chandra X-ray telescope, we have extracted the diffuse Xray emission from 49 equal-mass interacting/merging galaxy pairs in a merger sequence, from widely separated pairs to merger remnants. After removal of contributions from unresolved point sources, we compared the diffuse thermal X-ray luminosity from hot gas (L X (gas)) with the global star formation rate (SFR). After correction for absorption within the target galaxy, we do not see strong trend of L X (gas)/SFR with SFR or merger stage for galaxies with SFR > 1 M ⊙ yr −1 . For these galaxies, the median L X (gas)/SFR is 5.5 × 10 39 ((erg s −1 )/M ⊙ yr −1 )), similar to that of normal spiral galaxies. These results suggest that stellar feedback in star forming galaxies reaches an approximately steady state condition, in which a relatively constant fraction of about 2% of the total energy output from supernovae and stellar winds is converted into X-ray flux. Three late-stage merger remnants with low SFRs and high K band luminosities (L K ) have enhanced L X (gas)/SFR; their UV/IR/optical colors suggest that they are post-starburst galaxies, perhaps in the process of becoming ellipticals. Systems with L K < 10 10 L ⊙ have lower L X (gas)/SFR ratios than the other galaxies in our sample, perhaps due to lower gravitational fields or lower metallicities. We see no relation between L X (gas)/SFR and Seyfert activity in this sample, suggesting that feedback from active galactic nuclei is not a major contributor to the hot gas in our sample galaxies.

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“…The total star formation rate (SFR) is ∼75M e yr −1 based on the measurement of extinction-corrected Paschen α emission (Tateuchi et al 2015). Merging signatures such as a tidal tail are clearly seen in the H I ( Figure 1(a); Hibbard & Yun 1996, p. 47) and optical images ( Figure 1(b); AlonsoHerrero et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Spatially Resolved CO SLED of the Luminous Merger Remnant NGC 1614 with ALMA

Saito

Iono

et al. 2017

ApJ

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We present high-resolution (1 0) Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO(1-0) and CO(2-1) rotational transitions toward the nearby IR-luminous merger NGC1614 supplemented with ALMA archival data of CO(3-2)and CO(6-5) transitions. The CO(6-5) emission arises from the starburst ring (central 590 pc in radius), while the lower-J CO lines are distributed over the outer disk (∼3.3 kpc in radius). Radiative transfer and photon-dominated region (PDR) modeling reveals that the starburst ring has a single warmer gas component with more a intense far-ultraviolet radiation field (ñ 10 A two-phase molecular interstellar medium with a warm and cold (>70 and ∼19 K) component is also an applicable model for the starburst ring. A possible source for heating the warm gas component is mechanical heating due to stellar feedback rather than PDR. Furthermore, we find evidence for non-circular motions along the north-south optical bar in the lower-J CO images, suggesting a cold gas inflow. We suggest that star formation in the starburst ring is sustained by the bardriven cold gas inflowand that starburst activities radiatively and mechanically power the CO excitation. The absence of a bright active galactic nucleus can be explained by a scenario wherecold gas accumulating on the starburst ring is exhausted as the fuel for star formationor is launched as an outflow before being able to feed to the nucleus.

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

Cited by 25 publications

References 103 publications

Molecular gas content of shell galaxies

Molecular gas content of shell galaxies

Diffuse X-Ray-emitting Gas in Major Mergers

Spatially Resolved CO SLED of the Luminous Merger Remnant NGC 1614 with ALMA

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