First detection of cold dust in the northern shell of NGC 5128 (Centaurus A)

Stickel, M.; Hulst, J. M. van der; Gorkom, Jacqueline van; Schiminovich, David; Carilli, C. L.

doi:10.1051/0004-6361:20034314

Cited by 20 publications

(30 citation statements)

References 51 publications

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“…This material could remain outside the areas of the galaxies and would have low temperature (see Xilouris et al 2006). Such a case has been detected in the nearby giant elliptical galaxy Centaurus A, where ∼15 K dust has been detected outside the main body of the galaxy (see Stickel et al 2004). This was understood as a consequence of the accretion by a number of gas-rich dwarf companion galaxies that surround Centaurus A and have led to the formation of its dust lane, as well as to the filaments of atomic and molecular gas that surrounds it (see Schiminovich et al 1994;Charmandaris et al 2000).…”

Section: Cold Dust In Hickson Compact Groupsmentioning

confidence: 94%

A mid-IR study of Hickson compact groups

Bitsakis¹,

Charmandaris

Floc’h

et al. 2010

A&A

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Hickson compact groups (HCGs) are among the densest galaxy environments of the local universe. To examine the effects of the environment on the infrared properties of these systems, we present an analysis of Spitzer and ISO mid-infrared imaging, as well as of deep ground-based near-infrared imaging of 14 HCGs containing a total of 69 galaxies. Based on mid-infrared color diagnostics we identify the galaxies that appear to host an active nucleus, while using a suite of templates, and fit the complete infrared spectral energy distribution for each group member. We compare our estimates of galaxy mass, star formation rate, total infrared luminosities, and specific star formation rates (sSFR) for our HCG sample to samples of isolated galaxies and interacting pairs and find that overall there is no discernible difference among them. However, HCGs that can be considered as dynamically "old" host late-type galaxies with a slightly lower sSFR than the one found in dynamically "young" groups. This could be attributed to multiple past interactions among the galaxies in old groups, that have led to the build up of their stellar mass. It is also consistent with our prediction of the presence of diffuse cold dust in the intergalactic medium of 9 of the dynamically "old" groups.

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Section: Cold Dust In Hickson Compact Groupsmentioning

confidence: 94%

A mid-IR study of Hickson compact groups

Bitsakis¹,

Charmandaris

Floc’h

et al. 2010

A&A

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“…In addition, a temperature range 15−20 K was chosen to estimate the dust mass. As an upper limit we used the ISM cold dust temperature of our galaxies derived from the model and as a lower limit the estimated temperature of the cold dust stream ∼15 kpc from the centre of NGC5128 (Stickel et al 2004).The results are presented in the last column of Table 5. As we see, the amount of extended dust we detect near our galaxies is not enough to explain the high dust deficiencies of these systems (presented in Col. 6 of the same table).…”

Section: Diffuse Cold Dust In the Intragroup Mediummentioning

confidence: 99%

Herschelobservations of Hickson compact groups of galaxies: Unveiling the properties of cold dust

Bitsakis

Charmandaris

Appleton

et al. 2014

A&A

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We present a Herschel far-infrared and sub-millimetre (sub-mm) study of a sample of 120 galaxies in 28 Hickson compact groups (HCGs). Fitting their UV to sub-mm spectral energy distributions with the model of da Cunha et al. (2008), we accurately estimate the dust masses, luminosities, and temperatures of the individual galaxies. We find that nearly half of the late-type galaxies in dynamically "old" groups, those with more than 25% of early-type members and redder UV-optical colours, also have significantly lower dustto-stellar mass ratios compared to those of actively star-forming galaxies of the same mass found both in HCGs and in the field. Examining their dust-to-gas mass ratios, we conclude that dust was stripped out of these systems as a result of the gravitational and hydrodynamic interactions, experienced owing to previous encounters with other group members. About 40% of the early-type galaxies (mostly lenticulars), in dynamically "old" groups, display dust properties similar to those of the UV-optical red late-type galaxies. Given their stellar masses, star formation rates, and UV-optical colours, we suggest that red late-type and dusty lenticular galaxies represent transition populations between blue star-forming disk galaxies and quiescent early-type ellipticals. On the other hand, both the complete absence of any correlation between the dust and stellar masses of the dusty ellipticals and their enhanced star formation activity, suggest the increase in their gas and dust content due to accretion and merging. Our deep Herschel observations also allow us to detect the presence of diffuse cold intragroup dust in 4 HCGs. We also find that the fraction of 250 μm emission that is located outside of the main bodies of both the red late-type galaxies and the dusty lenticulars is 15−20% of their integrated emission at this band. All these findings are consistent with an evolutionary scenario in which gas dissipation, shocks, and turbulence, in addition to tidal interactions, shape the evolution of galaxies in compact groups.

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“…Another possibility is based on theory: it has been shown that it is possible for gas or dust to remain connected with the shell stars after a small merger (Kojima & Noguchi 1997;Charmandaris & Combes 2000). Observational evidence for significant amounts of dust residing in a shell was found in NGC 5128 (Stickel et al 2004). HI gas in shells has been found in M 83, NGC 2865 and NGC 3656 (Schiminovich et al 1995;Balcells et al 2001).…”

Section: Shell Coloursmentioning

confidence: 99%

HST/ACS observations of shell galaxies: inner shells, shell colours and dust

Sikkema

Carter²,

Peletier

et al. 2007

A&A

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Context. Shells in Elliptical Galaxies are faint, sharp-edged features, believed to provide evidence for a merger event. Accurate photometry at high spatial resolution is needed to learn on presence of inner shells, population properties of shells, and dust in shell galaxies. Aims. Learn more about the origin of shells and dust in early type galaxies. Methods. V − I colours of shells and underlying galaxies are derived, using HST Advanced Camera for Surveys (ACS) data. A galaxy model is made locally in wedges and subtracted to determine shell profiles and colours. We applied Voronoi binning to our data to get smoothed colour maps of the galaxies. Comparison with N-body simulations from the literature gives more insight to the origin of the shell features. Shell positions and dust characteristics are inferred from model galaxy subtracted images. Results. The ACS images reveal shells well within the effective radius in some galaxies (at 0.24 r e = 1.7 kpc in the case of NGC 5982). In some cases, strong nuclear dust patches prevent detection of inner shells. Most shells have colours which are similar to the underlying galaxy. Some inner shells are redder than the galaxy. All six shell galaxies show out of dynamical equilibrium dust features, like lanes or patches, in their central regions. Our detection rate for dust in the shell ellipticals is greater than that found from HST archive data for a sample of normal early-type galaxies, at the 95% confidence level.Conclusions. The merger model describes better the shell distributions and morphologies than the interaction model. Red shell colours are most likely due to the presence of dust and/or older stellar populations. The high prevalence and out of dynamical equilibrium morphologies of the central dust features point towards external influences being responsible for visible dust features in early type shell galaxies. Inner shells are able to manifest themselves in relatively old shell systems.

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First detection of cold dust in the northern shell of NGC 5128 (Centaurus A)

Cited by 20 publications

References 51 publications

A mid-IR study of Hickson compact groups

A mid-IR study of Hickson compact groups

Herschelobservations of Hickson compact groups of galaxies: Unveiling the properties of cold dust

HST/ACS observations of shell galaxies: inner shells, shell colours and dust

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