H<i>α</i>, SCUBA and MERLIN imaging of NGC 4490

Clemens, M.; Alexander, Paul

doi:10.1046/j.1365-8711.2002.05444.x

Cited by 11 publications

(16 citation statements)

References 23 publications

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“…This is most likely due to the high internal extinction in this dense area. High extinction of the thermal flux density has also been noticed by Clemens & Alexander (2002), who suggested a possibility that the obscuring dust is related not to the region itself, but to the surrounding atomic gas.…”

Section: S-srcmentioning

confidence: 72%

“…Such a value clearly indicates an almost purely thermal character of the emission, as it agrees with the theoretical value of 0.1 (Pacholczyk 1973). This conclusion is not astounding in the light of its identification as an Hii region (Clemens & Alexander 2002). Radio emission from such a structure should be dominated by the thermal radiation with the synchrotron component almost negligible.…”

Section: S-srcmentioning

confidence: 93%

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Probing the magnetic field of the nearby galaxy pair Arp 269

Nikiel-Wroczyński

Jamrozy

Soida

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a multiwavelength radio study of the nearby galaxy pair Arp 269 (NGC 4490/85). High sensitivity to extended structures gained by using the merged interferometric and single dish maps allowed us to reveal a previously undiscovered extension of the radio continuum emission. Its direction is significantly different from that of the neutral gas tail, suggesting that different physical processes might be involved in their creation. The population of radio-emitting electrons is generally young, signifying an ongoing, vigorous star formation -this claim is supported by strong magnetic fields (over 20 µG), similar to the ones found in much larger spiral galaxies. From the study of the spectral energy distribution we conclude that the electron population in the intergalactic bridge between member galaxies originates from the disk areas, and therefore its age (app. 3.7-16.9 Myrs, depending on the model used) reflects the timescale of the interaction. We have also discovered an angularly near Compact Steep Source -which is a member of a different galaxy pair -at a redshift of approximately 0.125.

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Section: S-srcmentioning

confidence: 72%

Section: S-srcmentioning

confidence: 93%

Probing the magnetic field of the nearby galaxy pair Arp 269

Nikiel-Wroczyński

Jamrozy

Soida

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Gas outflows from galaxies owing to supernova feedback is a different gas removal process that could move gas out to large distances (e.g. Hopkins et al 2014, Arraki et al 2014, Pontzen & Governato 2012, Tolstoy et al 2009, Clemens & Alexander 2002. Furthermore, it has been proposed that mergers between gas rich dwarfs can trigger starbursts and potentially transform the dwarfs into gas poor systems (e.g.…”

Section: Star Formation In the Dwarfsmentioning

confidence: 99%

Local Volume TiNy Titans: gaseous dwarf–dwarf interactions in the Local Universe

Pearson¹,

Besla²,

Putman³

et al. 2016

Mon. Not. R. Astron. Soc.

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In this paper, we introduce the Local Volume TiNy Titans sample (LV-TNT), which is a part of a larger body of work on interacting dwarf galaxies: TNT (Stierwalt et al. 2015). This LV-TNT sample consists of 10 dwarf galaxy pairs in the Local Universe (< 30 Mpc from Milky Way), which span mass ratios of M * ,1 /M * ,2 < 20, projected separations < 100 kpc, and pair member masses of log(M * /M ) < 9.9. All 10 LV-TNT pairs have resolved synthesis maps of their neutral hydrogen, are located in a range of environments and captured at various interaction stages. This enables us to do a comparative study of the diffuse gas in dwarf-dwarf interactions and disentangle the gas lost due to interactions with halos of massive galaxies, from the gas lost due to mutual interaction between the dwarfs. We find that the neutral gas is extended in the interacting pairs when compared to non-paired analogs, indicating that gas is tidally pre-processed. Additionally, we find that the environment can shape the HI distributions in the form of trailing tails and that the gas is not unbound and lost to the surroundings unless the dwarf pair is residing near a massive galaxy. We conclude that a nearby, massive host galaxy is what ultimately prevents the gas from being reaccreted. Dwarf-dwarf interactions thus represent an important part of the baryon cycle of low mass galaxies, enabling the "parking" of gas at large distances to serve as a continual gas supply channel until accretion by a more massive host.

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“…The size and the mass of NGC 4490 are ∼15 kpc (Clemens, & Alexander 2002) and ∼1.6×10 10 M ⊙ (Viallefond et al 1980), respectively, while those of NGC 4485 are ∼5.6 kpc (Clemens, & Alexander 2002) and ∼2×10 9 M ⊙ (Clemens et al 1999), respectively. Radio observations identified many H II regions in NGC 4490, indicating an on-going star forming activity at a star formation rate of ∼4.7 M ⊙ yr −1 (Clemens et al 1999;Clemens, & Alexander 2002). Two core-collapse SNe recently occurred in the galaxy 4 .…”

Section: Ngc 4490/85mentioning

confidence: 99%

Long-Term Spectral Variations of Ultraluminous X-Ray Sources in the Interacting Galaxy Systems M 51 and NGC 4490/85

Yoshida¹,

Ebisawa²,

Matsushita³

et al. 2010

ApJ

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Variable ultraluminous X-ray sources (ULXs), which are considered to be black hole binaries (BHBs), are known to show state transitions similarly to Galactic BHBs. However, the relation between the ULX states and the Galactic BHB states is still unclear primarily due to less well-understood behaviors of ULXs in contrast to the Galactic BHBs. Here, we report a statistical X-ray spectral study of 34 energy spectra from seven bright ULXs in the interacting galaxy systems M 51 and NGC 4490/85, using archive data from multiple Chandra and XMM-Newton observations spanning for a few years. In order to compare with Galactic BHB states, we applied representative spectral models of BHBs; a power-law (PL), a multi-color disk black body (MCD), and a slim disk model to all the ULX spectra. We found a hint of a bimodal structure in the luminosity distribution of the samples, suggesting that ULXs have two states with typical luminosities of 3-6×10 39 and 1.5-3×10 39 ergs s −1 . Most spectra in the brighter state are explained by the MCD or the slim disk model, whereas those in the fainter state are explained by the PL model. In particular, the slim disk model successfully explains the observed spectral variations of NGC 4490/85 ULX-6 and ULX-8 by changes of the mass accretion rate to a black hole of an estimated mass of <40 M ⊙ . From the best-fit model parameters of each state, we speculate that the brighter state in these two ULXs corresponds to the brightest state of Galactic BHBs, which is often called the "apparently standard state". The fainter state of the ULXs has a PL shaped spectrum, but the photon index range is much wider than that seen in any single state of Galactic BHBs. We thus speculate that it is a state unique to ULXs. Some sources show much fainter and steeper spectra than the faint state, which we identified as another state.

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Hα, SCUBA and MERLIN imaging of NGC 4490

Cited by 11 publications

References 23 publications

Probing the magnetic field of the nearby galaxy pair Arp 269

Probing the magnetic field of the nearby galaxy pair Arp 269

Local Volume TiNy Titans: gaseous dwarf–dwarf interactions in the Local Universe

Long-Term Spectral Variations of Ultraluminous X-Ray Sources in the Interacting Galaxy Systems M 51 and NGC 4490/85

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