NGC 3310 and its tidal debris: remnants of galaxy evolution

Wehner, E. M.; Gallagher, John S.; Papaderos, P.; Alvensleben, U. Fritze-von; Westfall, Kyle B.

doi:10.1111/j.1365-2966.2006.10757.x

Cited by 17 publications

(18 citation statements)

References 26 publications

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“…These authors suggest that "shocks, self-gravity, or possibly external ram pressure" have acted to separate stars and gas. In the starburst NGC 3310, a large stellar loop (Wehner & Gallagher 2005;Wehner et al 2006) is apparently unrelated to the two tidal tails of H i mapped by Kregel & Sancisi (2001). Wehner and collaborators suggest that multiple discrete events, or multiple passes of a single intruding galaxy which is stripped of its gas before being swallowed, are required to explain this morphology.…”

Section: Discussionmentioning

confidence: 99%

NGC 2655: From Inner Polar Ring to Outer Shells and Tails

Sparke

Moorsel

Erwin

et al. 2007

The Astronomical Journal

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NGC 2655, a nearby bright S0/a galaxy in a loose group, has strongly asymmetric central dust lanes and an extended disk of neutral hydrogen gas. Here we present deep optical images showing tidal arms and regions of diffuse starlight well beyond the main galaxy, suggestive of a recent merger. Our maps in the 21 cm line show a layer of neutral hydrogen extending to at least 7.5 or 40 kpc from the center, with a broken streamer of gas trailing off toward the small neighbor galaxy UGC 4714. The global profile has sloping "shoulders" of extreme-velocity gas, usually a sign of interaction. The diffuse stellar light corresponds generally but not in detail with the distribution of H i. In particular, the stellar light of the main tidal arm extends beyond the H i layer, which is limb-brightened as if it had been compressed from outside. The pattern of gas velocities is generally bisymmetric, but the H i layer is strongly warped; it does not share the kinematics of the stellar disk. The gas orbits twist by at least 90• between 1 and 3 of the center, as the H i layer appears to warp through edge-on. The complex optical tails and H i dynamics suggest that the galaxy has undergone multiple mergers. Both at small and at large radii, the gas layer twists in a trailing sense relative to its orbital motion. If the twist results from differential precession in the galaxy's gravitational potential, this would indicate that the dark halo is prolate, elongated along the rotation axis of the disk.

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Section: Discussionmentioning

confidence: 99%

NGC 2655: From Inner Polar Ring to Outer Shells and Tails

Sparke

Moorsel

Erwin

et al. 2007

The Astronomical Journal

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“…However, the system appears to have two HI tails (Kregel & Sancisi 2001), supporting the idea of a major merger. Wehner et al (2006) conclude that either it is the result of a major merger or the result of multiple mergers with smaller companions. For the current study, we assume it is a major merger and classify it as stage 6.…”

Section: 78±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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“…Apart from the absorption features that shape the continuum emission, these sources have been classified as starforming/HII galaxies by several previous works, particularly in the optical region (e.g. González-Delgado et al 1999;Alonso-Herrero et al 2001;Wehner et al 2006;Schweizer & Seitzer 2007). Thus, we measured these nebular atomic emission lines ([SIII] λ9530, HeI λ10830, [FeII] λ12570, Paβ λ12810, [FeII] λ16440 and Brγ λ21650) and the H2 λ21210 line.…”

Section: Emission Gasmentioning

confidence: 99%

Probing the circumnuclear stellar populations of starburst galaxies in the near-infrared

Dametto

Riffel

Pastoriza

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We employ the NASA Infrared Telescope Facility's near-infrared spectrograph SpeX at 0.8-2.4µm to investigate the spatial distribution of the stellar populations (SPs) in four well known Starburst galaxies: NGC 34, NGC 1614, NGC 3310 and NGC 7714. We use the STARLIGHT code updated with the synthetic simple stellar populations models computed by Maraston (2005, M05). Our main results are that the NIR light in the nuclear surroundings of the galaxies is dominated by young/intermediate age SPs (t 2 × 10 9 yr), summing from ∼40% up to 100% of the light contribution. In the nuclear aperture of two sources (NGC 1614 and NGC 3310) we detected a predominant old SP component (t > 2 × 10 9 yr), while for NGC 34 and NGC 7714 the younger component prevails. Furthermore, we found evidence of a circumnuclear star formation ring-like structure and a secondary nucleus in NGC 1614, in agreement with previous studies. We also suggest that the merger/interaction experienced by three of the galaxies studied, NGC 1614, NGC 3310 and NGC 7714 can explain the lower metallicity values derived for the young SP component of these sources. In this scenario the fresh unprocessed metal poorer gas from the destroyed/interacting companion galaxy is driven to the centre of the galaxies and mixed with the central region gas, before star formation takes place. In order to deepen our analysis, we performed the same procedure of SP synthesis using Maraston & Strömbäck (2011, M11) EPS models. Our results show that the newer and higher resolution M11 models tend to enhance the old/intermediate age SP contribution over the younger ages.

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NGC 3310 and its tidal debris: remnants of galaxy evolution

Abstract: The definitive version is available at www.blackwell-synergy.com. Copyright Blackwell Publishing DOI : 10.1111/j.1365-2966.2006.10757.

Cited by 17 publications

References 26 publications

NGC 2655: From Inner Polar Ring to Outer Shells and Tails

NGC 2655: From Inner Polar Ring to Outer Shells and Tails

Diffuse X-Ray-emitting Gas in Major Mergers

Probing the circumnuclear stellar populations of starburst galaxies in the near-infrared

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