ERRATUM: “SPIRALS, BRIDGES, AND TAILS: A<i>GALAXY EVOLUTION EXPLORER</i>UV ATLAS OF INTERACTING GALAXIES” (2010, AJ, 139, 1212)

Smith, Beverly J.; Giroux, Mark L.; Struck, Curtis; Hancock, Mark H.; Hurlock, Sabrina

doi:10.1088/0004-6256/139/6/2719

Cited by 90 publications

(233 citation statements)

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“…To this end, we have extracted UV and IR fluxes for these galaxies from archival Spitzer and Galaxy Evolution Explorer (GALEX) images using the method described in Smith et al (2007Smith et al ( , 2010. In this study we use GALEX far-ultraviolet (FUV; λ ef f = 1516Å) and near-ultraviolet (NUV; λ ef f = 2267Å) data, as well as Spitzer 3.6 µm and 24 µm fluxes.…”

Section: Uv/ir Data and Sfrsmentioning

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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Section: Uv/ir Data and Sfrsmentioning

confidence: 99%

Diffuse X-Ray-emitting Gas in Major Mergers

Smith

Campbell

Struck

et al. 2018

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“…These are summarised in Table 3 and discussed in more detail below. The Mice have been observed in the mid-IR with the MIPS instrument on board Spitzer (Smith et al 2007) and the near-UV (NUV) and far-UV (FUV) with GALEX (Smith et al 2010). This provides us with two alternative SFR estimates which account for optically thick dust obscuration by direct detection of the thermal dust emission.…”

Section: Multiwavelength Analysis Of Total Star Formation Ratesmentioning

confidence: 99%

The Mice at play in the CALIFA survey

Wild

Rosales-Ortega

Falcón-Barroso

et al. 2014

A&A

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We present optical integral field spectroscopy (IFS) observations of the Mice, a major merger between two massive ( 10 11 M ) gas-rich spirals NGC 4676A and B, observed between first passage and final coalescence. The spectra provide stellar and gas kinematics, ionised gas properties, and stellar population diagnostics, over the full optical extent of both galaxies with ∼1.6 kpc spatial resolution. The Mice galaxies provide a perfect case study that highlights the importance of IFS data for improving our understanding of local galaxies. The impact of first passage on the kinematics of the stars and gas has been significant, with strong bars most likely induced in both galaxies. The barred spiral NGC 4676B exhibits a strong twist in both its stellar and ionised gas disk. The edge-on disk galaxy NGC 4676A appears to be bulge free, with a strong bar causing its "boxy" light profile. On the other hand, the impact of the merger on the stellar populations has been minimal thus far. By combining the IFS data with archival multiwavelength observations we show that star formation induced by the recent close passage has not contributed significantly to the total star formation rate or stellar mass of the galaxies. Both galaxies show bicones of high ionisation gas extending along their minor axes. In NGC 4676A the high gas velocity dispersion and Seyfert-like line ratios at large scaleheight indicate a powerful outflow. Fast shocks (v s ∼ 350 km s −1 ) extend to ∼6.6 kpc above the disk plane. The measured ram pressure (P/k = 4.8 × 10 6 K cm −3 ) and mass outflow rate (∼8−20 M yr −1 ) are similar to superwinds from local ultra-luminous infrared galaxies, although NGC 4676A only has a moderate infrared luminosity of 3 × 10 10 L . Energy beyond what is provided by the mechanical energy of the starburst appears to be required to drive the outflow. Finally, we compare the observations to mock kinematic and stellar population maps extracted from a hydrodynamical merger simulation. The models show little enhancement in star formation during and following first passage, in agreement with the observations. We highlight areas where IFS data could help further constrain the models.

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“…In many cases spiral-like features are observed in the UV range beyond the main disc of a galaxy and reveal continuing star formation, although with low efficiency (see Bigiel et al 2010, and references therein). Another type of outer structure is connected with the gaseous tidal tails of interacting galaxies -weak star formation may also take place there, in spite of the extremely low mean gas density (Smith et al 2010). …”

Section: Introductionmentioning

confidence: 99%

Magnetic fields near the peripheries of galactic discs

Михайлов

Kasparova

Moss

et al. 2014

A&A

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Context. Magnetic fields are observed beyond the peripheries of optically detected galactic discs, while numerical models of their origin and the typical magnitudes are still absent. Previously, studies of galactic dynamo have avoided considering the peripheries of galactic discs because of the very limited (though gradually growing) knowledge about the local properties of the interstellar medium. Aims. Here we investigate the possibility that magnetic fields can be generated in the outskirts of discs, taking the Milky Way as an example. Methods. We consider a simple evolving galactic dynamo model in the "no-z" formulation, applicable to peripheral regions of galaxies, for various assumptions about the radial and vertical profiles of the ionized gas disc.Results. The magnetic field may grow as galaxies evolve, even in the more remote parts of the galactic disc, out to radii of 15 to 30 kpc, becoming substantial after times of about 10 Gyr. This result depends weakly on the adopted distributions of the half thickness and surface density of the ionized gas component. The model is robust to changes in the amplitude of the initial field and the position of its maximum strength. The magnetic field in the remote parts of the galactic disc could be generated in situ from a seed field by local dynamo action. Another possibility is field production in the central regions of a galaxy, followed by transport to the disc's periphery by the joint action of the dynamo and turbulent diffusivity.Conclusions. Our results demonstrate the possibilities for the appearance and strengthening of magnetic fields at the peripheries of disc galaxies and emphasize the need for observational tests with new and anticipated radio telescopes (LOFAR, MWA, and SKA).

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ERRATUM: “SPIRALS, BRIDGES, AND TAILS: AGALAXY EVOLUTION EXPLORERUV ATLAS OF INTERACTING GALAXIES” (2010, AJ, 139, 1212)

Cited by 90 publications

References 0 publications

Diffuse X-Ray-emitting Gas in Major Mergers

Diffuse X-Ray-emitting Gas in Major Mergers

The Mice at play in the CALIFA survey

Magnetic fields near the peripheries of galactic discs

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