VCC 2062: an old tidal dwarf galaxy in the Virgo cluster?

Duc, Pierre–Alain; Braine, J.; Lisenfeld, U.; Brinks, E.; Boquien, M.

doi:10.1051/0004-6361:20078335

Cited by 65 publications

(109 citation statements)

References 65 publications

(92 reference statements)

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“…In addition, the luminosities observed for nearby (Duc et al 1997;Duc & Mirabel 1998;Duc et al 2007) and more distant (Weilbacher et al 2000;Temporin et al 2003) TDG candidates are generally more luminous than B = -10.65, as for most of our Hα complexes.…”

Section: Characterization Of the Hα-emitting Complexesmentioning

confidence: 93%

“…Associations of young star-forming regions with a large HI reservoir have been found in TDGs, for instance by Duc et al (2007). We may then consider whether the Hα-emitting complexes in our sample are dynamically unbound associations of objects with masses similar to observed super star clusters (SSCs) or larger, more massive, and self-gravitating objects such as dwarf galaxies.…”

Section: Discussionmentioning

confidence: 99%

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Extranuclear Hα-emitting complexes in low-z(U)LIRGs: precursors of tidal dwarf galaxies?

Miralles-Caballero

Colina

Arribas

2012

A&A

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This paper characterizes the physical and kinematic properties of external massive star-forming regions in a sample of (U)LIRGs. We use high angular resolution ACS images from the Hubble Space Telescope (HST) in F435W (∼B) and F814W (∼I) bands, as well as Hα-line emission maps obtained with integral field spectroscopy. We find 31 external Hα-emitting (i.e., young star-forming) complexes in 11 (U)LIRGs. These complexes have in general similar sizes (from few hundreds of pc to about 2 kpc), luminosities (M F435W < -10.65 and L(Hα) > 10 39 L ), and metallicities (12 + log (O/H) ∼ 8.5-8.7) to extragalactic giant HII regions and TDG candidates found in less luminous mergers and compact groups of galaxies. We assess the mass content and the likelihood of survival as TDGs of the 22 complexes with simple structures in the HST images based on their photometric, structural, and kinematic properties. The dynamical tracers used (radius-σ and luminosity-σ diagrams) indicate that most of the complexes might be self-gravitating entities. The resistance to forces from the parent galaxy is studied by considering the tidal mass of the candidate and its relative velocity with respect to the parent galaxy. After combining the results of previous studies of TDG searches in ULIRGs a total of 9 complexes satisfy most of the applied criteria and thus show a high-medium or high likelihood of survival, their total mass likely being compatible with that of dwarf galaxies. They are defined as TDG candidates. We propose that they probably formed more often during the early phases of the interaction. Combining all data for complexes with IFS data where a significant fraction of the system is covered, we infer a TDG production rate of 0.3 candidates with the highest probabilities of survival per system for the (U)LIRGs class. This rate, though, might decrease to 0.1 after the systems in (U)LIRGs have evolved for 10 Gyr, for long-lived TDGs, which would imply that no more than 5-10% of the overall dwarf population could be of tidal origin.

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Section: Characterization Of the Hα-emitting Complexesmentioning

confidence: 93%

Section: Discussionmentioning

confidence: 99%

Extranuclear Hα-emitting complexes in low-z(U)LIRGs: precursors of tidal dwarf galaxies?

Miralles-Caballero

Colina

Arribas

2012

A&A

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“…Tidal dwarfs are gravitationally bound systems; their DM content may thus simply be derived determining their dynamical mass and subtracting it from the luminous one (consisting of HI, H 2 , stars and dust). This exercise has been carried out for a few systems Duc et al, 2007, Belles et al 2012. Even if the error bars are large, these measurements yield reliable dynamical to luminous mass ratios of 2-3.…”

Section: Constraining the Distribution Of Dark Matter With Tidal Tailsmentioning

confidence: 99%

Tides in Colliding Galaxies

Duc

Renaud

2013

Tides in Astronomy and Astrophysics

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Long tails and streams of stars are the most noticeable upshots of galaxy collisions. Their origin as gravitational, tidal, disturbances has however been recognized only less than fifty years ago and more than ten years after their first observations. This Review describes how the idea of galactic tides emerged, in particular thanks to the advances in numerical simulations, from the first ones that included tens of particles to the most sophisticated ones with tens of millions of them and state-of-the-art hydrodynamical prescriptions. Theoretical aspects pertaining to the formation of tidal tails are then presented. The third part of the review turns to observations and underlines the need for collecting deep multi-wavelength data to tackle the variety of physical processes exhibited by collisional debris. Tidal tails are not just stellar structures, but turn out to contain all the components usually found in galactic disks, in particular atomic / molecular gas and dust. They host star-forming complexes and are able to form star-clusters or even second-generation dwarf galaxies. The final part of the review discusses what tidal tails can tell us (or not) about the structure and content of present-day galaxies, including their dark components, and explains how tidal tails may be used to probe the past evolution of galaxies and their mass assembly history. On-going deep wide-field surveys disclose many new lowsurface brightness structures in the nearby Universe, offering great opportunities for attempting galactic archeology with tidal tails.

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“…In addition to atomic gas pulled from the parent galaxies, these collisional debris actually contain surprisingly large amounts of molecular gas formed in-situ (Braine et al 2000(Braine et al , 2001Lisenfeld et al 2002Lisenfeld et al , 2004Petitpas & Taylor 2005;Duc et al 2007). As the gas subsequently collapses, starforming regions are created with masses ranging from a few hundred solar masses, creating OB associations, the "emission line dots" (Gerhard et al 2002;Yoshida et al 2002;Sakai et al 2002;Weilbacher et al 2003;Ryan-Weber et al 2004;Mendes de Oliveira et al 2004;Cortese et al 2006;Werk et al 2008Werk et al , 2010 to objects as massive as dwarf galaxies named tidal dwarf galaxies (TDGs, Duc 1995;Duc & Mirabel 1998;Duc et al 2000Duc et al , 2007Hancock et al 2007Hancock et al , 2009). These objects, A&A 533, A19 (2011) even though formed from material once pertaining to their parent galaxies, have a radically different and simpler environment.…”

Section: Introductionmentioning

confidence: 99%

Studying the spatially resolved Schmidt-Kennicutt law in interacting galaxies: the case of Arp 158

Boquien¹,

Lisenfeld²,

Duc³

et al. 2011

A&A

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Context. Recent studies have shown that star formation in mergers does not seem to follow the same Schmidt-Kennicutt relation as in spiral disks, presenting a higher star formation rate (SFR) for a given gas column density. Aims. In this paper we study why and how different models of star formation arise. To do so we examine the process of star formation in the interacting system Arp 158 and its tidal debris. Methods. We perform an analysis of the properties of specific regions of interest in Arp 158 using observations tracing the atomic and the molecular gas, star formation, the stellar populations as well as optical spectroscopy to determine their exact nature and their metallicity. We also fit their spectral energy distribution with an evolutionary synthesis code. Finally, we compare star formation in these objects to star formation in the disks of spiral galaxies and mergers. Results. Abundant molecular gas is found throughout the system and the tidal tails appear to have many young stars compared to their old stellar content. One of the nuclei is dominated by a starburst whereas the other is an active nucleus. We estimate the SFR throughout the systems using various tracers and find that most regions follow closely the Schmidt-Kennicutt relation seen in spiral galaxies with the exception of the nuclear starburst and the tip of one of the tails. We examine whether this diversity is due to uncertainties in the manner the SFR is determined or whether the conditions in the nuclear starburst region are such that it does not follow the same Schmidt-Kennicutt law as other regions. Conclusions. Observations of the interacting system Arp 158 provide the first evidence in a resolved fashion that different star-forming regions in a merger may be following different Schmidt-Kennicutt laws. This suggests that the physics of the interstellar medium at a scale no larger than 1 kpc, the size of the largest gravitational instabilities and the injection scale of turbulence, determines the origin of these laws.

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VCC 2062: an old tidal dwarf galaxy in the Virgo cluster?

Cited by 65 publications

References 65 publications

Extranuclear Hα-emitting complexes in low-z(U)LIRGs: precursors of tidal dwarf galaxies?

Extranuclear Hα-emitting complexes in low-z(U)LIRGs: precursors of tidal dwarf galaxies?

Tides in Colliding Galaxies

Studying the spatially resolved Schmidt-Kennicutt law in interacting galaxies: the case of Arp 158

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