Ionized gas in E/S0 galaxies with dust lanes

Finkelman, Ido; Brosch, Noah; Funes, Guillermo; Kniazev, A. Y.; Vaïsänen, P.

doi:10.1111/j.1365-2966.2010.17070.x

Cited by 37 publications

(73 citation statements)

References 95 publications

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“…In addition, a recent minor merger is consistent with the presence of prominent dust lanes around the nucleus of the S0 galaxy (e.g. Finkelman et al 2010;Shabala et al 2012) and the evidence of UV emission centred on its bulge (S10), indicating ongoing star formation (SF, e.g. Kaviraj et al 2009).…”

Section: The Puzzling Nature Of the Hlx-1 Counterpartmentioning

confidence: 69%

A disrupted bulgeless satellite galaxy as counterpart of the ultraluminous X-ray source ESO 243-49 HLX-1

Mapelli

Annibali

Zampieri

et al. 2013

A&A

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The point-like X-ray source HLX-1, close to the S0 galaxy ESO 243-49, is one the strongest intermediate-mass black hole candidates, but the nature of its counterpart is still puzzling. By means of N-body/smoothed particle hydrodynamics simulations, we investigate the hypothesis that the HLX-1 counterpart is the nucleus of a bulgeless satellite galaxy, which undergoes a minor merger with the S0 galaxy. We derived synthetic surface brightness profiles for the simulated counterpart of HLX-1 in six Hubble Space Telescope (HST) filters, ranging from far ultraviolet (FUV) to infrared wavelengths, and we compared them with the observed profiles. Our model matches the emission associated with the HLX-1 counterpart in all considered filters, including the bluer ones, even without requiring the contribution of an irradiated disc. The simulation can also account for an extended FUV emission, which is hinted at by the analysis of the F140LP HST filter. This matching is impossible to achieve by assuming either a bulgy satellite, a young star cluster, or an irradiated disc component.

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Section: The Puzzling Nature Of the Hlx-1 Counterpartmentioning

confidence: 69%

A disrupted bulgeless satellite galaxy as counterpart of the ultraluminous X-ray source ESO 243-49 HLX-1

Mapelli

Annibali

Zampieri

et al. 2013

A&A

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“…HCG 22 does not present clear signs of ongoing interaction. However, NGC 1199 presents a central dust lane in its centre similar to the more local case of NGC 5128 (CenA) of approximately 3 kpc and about 10 7 M (Nieto 1983;Sparks et al 1985;Veron-Cetty & Veron 1988;Finkelman et al 2010). This is a quite strong indication of a gas-rich merger, old enough to have settled in a single remanent, that likely has triggered the formation of star clusters.…”

Section: Ucd Formationmentioning

confidence: 97%

Two formation channels of ultra-compact dwarf galaxies in Hickson compact groups

Rocha

Mieske

Georgiev

et al. 2010

A&A

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Context. The formation of ultra-compact dwarf galaxies (UCDs) is believed to be driven by interaction, and UCDs are abundant in the cores of galaxy clusters, environments that mark the end-point of galaxy evolution. Nothing is known about the properties of UCDs in compact groups of galaxies, environments where most of galaxy evolution and interaction is believed to occur and where UCDs in an intermediate stage in their evolution may be expected. Aims. The main goal of this study is to detect and characterize, for the first time, the UCD population of compact groups of galaxies. For that, two nearby groups in different evolutionary stages, HCG 22 and HCG 90, were targeted. Methods. We selected about 40 UCD candidates from pre-existing photometry of both groups, and obtained spectra of these candidates using the VLT FORS2 instrument in MXU mode. Archival HST/ACS imaging was used to measure their structural parameters. Results. We detect 16 and 5 objects belonging to HCG 22 and HCG 90, respectively, covering the magnitude range −10.0 > M R > −11.5 mag. Their integrated colours are consistent with old ages covering a broad range in metallicities (metallicities confirmed by the spectroscopic measurements). Photometric mass estimates put 4 objects in HCG 90 and 9 in HCG 22 in the mass range of UCDs (>2 × 10 6 M ) for an assumed age of 12 Gyr. These UCDs are on average 2−3 times larger than the typical size of Galactic GCs, covering a range of 2 < ∼ r h < ∼ 21 pc. The UCDs in HCG 22 are more concentrated around the central galaxy than in HCG 90, at the 99% confidence level. They cover a broad range in [α/Fe] abundances from sub-to super-solar. The spectra of 3 UCDs (2 in HCG 22, 1 in HCG 90) show tentative evidence of intermediate age stellar populations. The clearest example is the largest and most massive UCD (∼10 7 M ) in our sample, which is detected in HCG 22. Its properties are most consistent with a stripped dwarf galaxy nucleus. We calculate the specific frequency (S N ) of UCDs for both groups, finding that HCG 22 has about three times higher S N than HCG 90. Conclusions. The ensemble properties of the detected UCDs supports two co-existing formation channels: a star cluster origin (lowluminosity, compact sizes, old ages, super-solar α/Fe), and an origin as tidally stripped dwarf nuclei (more extended and younger stellar populations). Our results imply that the UCDs detected in both groups do not, in their majority, originate from relatively recent galaxy interactions. Most of the detected UCDs have likely been brought into the group along with their host galaxies.

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“…Combining the extinction measurements made by Finkelman et al (2010) and Annibali et al (2010) for nearby S0s, the average extinction (A) of an E-S0 galaxy is A B ∼ 1.2 mag and A K ∼ 0.15 mag in the B and K bands, respectively. However, this extinction can be as high as A B ∼ 7 mag for some of their local objects, which is much higher than the A B 0.3 mag typically predicted for local galaxies (see e.g.…”

Section: Appendix A: Dust Extinctionmentioning

confidence: 99%

Formation of S0 galaxies through mergers

Tapia

Eliche‐Moral

Aceves

et al. 2017

A&A

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Context. Lenticular (S0) galaxies are known to derive from spiral galaxies. The fact that S0s nearly obey the Tully-Fisher relation (TFR) at z ∼ 0 (as spirals have done in the last ∼9 Gyr) is considered an argument against their major-merger origin because equal mergers of two disc galaxies produce remnants that are outliers of the TFR. Aims. We explore whether a scenario that combines an origin by mergers at z ∼ 1.8 − 1.5 with a subsequent passive evolution of the resulting S0 remnants since z ∼ 0.8-1 is compatible with observational data of S0s in the TFR both at z ∼ 0.8 and z ∼ 0. Methods. We studied a set of major and minor merger experiments from the GalMer database that generate massive S0 remnants that are dynamically relaxed and have realistic properties. We analysed the location of these remnants in the photometric and stellar TFRs assuming that they correspond to z ∼ 0.8 galaxies. We then estimated their evolution in these planes over the last ∼ 7 Gyr considering that they have evolved passively in isolation. The results were compared with data of real S0s and spirals at different redshifts. We also tested how the use of V circ or V rot,max affects the results. Results. Just after ∼ 1-2 Gyr of coalescence, major mergers generate S0 remnants that are outliers of the local photometric and stellar TFRs (as already stated in previous studies), in good agreement with observations at z ∼ 0.8. After ∼ 4 -7 Gyr of passive evolution in isolation, the S0 remnants move towards the local TFR, although the initial scatter among them persists. This scatter is sensitive to the indicator used for the rotation velocity: V circ values yield a lower scatter than when V rot,max values are considered instead. In the planes involving V rot,max , a clear segregation of the S0 remnants in terms of the spin-orbit coupling of the model is observed, in which the remnants of retrograde encounters overlap with local S0s hosting counter-rotating discs. The location of the S0 remnants at z ∼ 0 agrees well with the observed distribution of local S0 galaxies in the σ 0 -M K , V circ -σ 0 , and V rot,max -σ 0 planes. Conclusions. Massive S0 galaxies may have been formed through major mergers that occurred at high redshift and have later evolved towards the local TFR through passive evolution in relative isolation, a mechanism that would also contribute to the scatter observed in this relation.

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Ionized gas in E/S0 galaxies with dust lanes

Cited by 37 publications

References 95 publications

A disrupted bulgeless satellite galaxy as counterpart of the ultraluminous X-ray source ESO 243-49 HLX-1

A disrupted bulgeless satellite galaxy as counterpart of the ultraluminous X-ray source ESO 243-49 HLX-1

Two formation channels of ultra-compact dwarf galaxies in Hickson compact groups

Formation of S0 galaxies through mergers

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