Stars and gas in the Medusa merger

Manthey, E.; Hüttemeister, Susanne; Aalto, S.; Horellou, C.; Bjerkeli, P.

doi:10.1051/0004-6361:200810408

Cited by 10 publications

(19 citation statements)

References 33 publications

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“…Neither the simulations by Weil & Hernquist (1993) nor Kojima & Noguchi (1997) show the appearance of two tails in an S+E merger scenario. Furthermore, our H i data of the prototypical S+E merger NGC 4194 show only one gaseous tail in that galaxy, in accordance to the S+E merger simulations (Manthey et al 2008b).…”

Section: Spiral+spiral Merger?supporting

confidence: 88%

The H I content of the advanced merger NGC 4441

Manthey

Aalto

Hüttemeister

et al. 2008

A&A

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Context. NGC 4441 is a candidate for a merger between a spiral and an elliptical galaxy (S+E merger), because it shows typical tidal structures such as an optical tail and two shells. With a far-infrared luminosity of ∼5 × 10 9 L this galaxy belongs to the class of moderate luminosity mergers, in which the merging process induces (if at all) only a moderate starburst. Aims. The study of the atomic gas content allows us to investigate the merger history and the impact on the star formation. In particular, it is not clear from simulations whether an S+E merger leads to a gas concentration in the nucleus, resulting in a starburst, or whether the gas is spread out and therefore too diffuse for new star forming regions.Methods. We used the Westerbork Radio Synthesis Telescope to observe the properties of the H i. By using this interferometer, we are able to study the large-scale H i distribution and kinematics with high spatial and velocity resolution. Results. We found two H i tails extending out to more than 40 kpc. In a central disc, the gas shows a fairly regular rotation pattern indicating that the gas started to settle after the merger. The total H i mass adds up to 1.5 × 10 9 M . By comparing the high resolution H i maps with deep optical images, differences between the stellar and gaseous tidal features are apparent, which indicates an S+E merger origin.

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Section: Spiral+spiral Merger?supporting

confidence: 88%

The H I content of the advanced merger NGC 4441

Manthey

Aalto

Hüttemeister

et al. 2008

A&A

Self Cite

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“…Jütte (2010) reports investigations of minor mergers, i.e., mergers of galaxies with unequal masses, which may be the progenitors of S0 galaxies, or rapidly rotating early-type galaxies. Her results, with those of Manthey et al (2008), suggest that NGC 4194 is an ideal candidate to investigate the contribution to induced star formation of a small spiral galaxy merging with a larger elliptical. NGC 4194 (=Arp 160, Mrk 201, IRAS 12116+5448) is a luminous infrared galaxy (LIRG) which demonstrates the characteristics of a minor merger.…”

Section: Introductionsupporting

confidence: 54%

Characteristics of Star-Forming Regions in the Advanced Minor-Merger, Luminous Infrared Galaxy NGC 4194

Weistrop

Nelson

Angione

et al. 2012

The Astronomical Journal

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We report the results of long-slit spectroscopy at position angles 68• , 131• , and 164• for the minor-merger NGC 4194, a luminous infrared starburst galaxy. The mass within 1.2 kpc of the dynamical center is estimated to be 4.8 × 10 9 to 1.7 × 10 10 M , depending on the assumed inclination to the plane of the sky. The star formation rate (SFR) in the areas sampled is 8 M yr −1 . The metallicity, log(O/H) + 12, ranges from ∼8.8 to >9.0 in regions of significant star formation, suggesting that the metallicity has been enhanced by the current star formation. The star-forming regions range in age from 5 to 9 Myr, with the youngest ages occurring in the regions of high SFR. Electron temperatures and the location of the spectra in emission line diagnostic diagrams suggest the presence of shock waves, presumably due to the presence of supernovae, winds from massive stars, and/or collisions of clouds due to the merger. The presence of massive stars and supernovae is consistent with the ages determined for the star-forming regions. The ages of the continua produced by the stellar population are estimated to range from 10 Myr to 5 Gyr. Much of the stellar population represented in the continua was probably formed before the merger and represents the progenitor galaxies.

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“…It has a long HI tail extending to the south opposite the optical plume (Manthey et al 2008). It has a single nucleus and a near-infrared K band light profile that approximately fits an R 1/4 profile (Rothberg & Joseph 2004).…”

Section: Am 2055−425 (Eso 286-ig 019; Iras 20551-4250)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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Stars and gas in the Medusa merger

Cited by 10 publications

References 33 publications

The H I content of the advanced merger NGC 4441

The H I content of the advanced merger NGC 4441

Characteristics of Star-Forming Regions in the Advanced Minor-Merger, Luminous Infrared Galaxy NGC 4194

Diffuse X-Ray-emitting Gas in Major Mergers

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