Gas dynamics in tidal dwarf galaxies: Disc formation at<i>z</i>= 0

Lelli, Federico; Duc, Pierre–Alain; Brinks, E.; Bournaud, F.; McGaugh, Stacy S.; Lisenfeld, U.; Weilbacher, Peter M.; Boquien, M.; Revaz, Yves; Braine, J.; Koribalski, B. S.; Belles, Pierre-Emmanuel

doi:10.1051/0004-6361/201526613

Cited by 93 publications

(129 citation statements)

References 105 publications

(165 reference statements)

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“…The two brightest (R2 and R3) are near to the HI emission peak, as can be seen in de Mello et al (2012). A similar case is given by the late-stage merger NGC 7252 (Lelli et al 2015), where there are two genuine tidal dwarf galaxies (TDGs) in formation. Through a detailed analysis of the gas dynamics and metallicity in this system, using HI and optical IFS observations, they reinforce that the TDGs in NGC 7252 were not pre-existing dwarfs, but currently forming out of pre-enriched material ejected from the progenitor galaxies.…”

Section: Osiris Line Emission At the Edge Of The Sw Tidal Tailmentioning

confidence: 58%

The spatially resolved stellar population and ionized gas properties in the merger LIRG NGC 2623

Cortijo-Ferrero

Delgado

Pérez

et al. 2017

A&A

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We report on a detailed study of the stellar populations and ionized gas properties in the merger LIRG NGC 2623, analyzing optical integral field spectroscopy from the CALIFA survey and PMAS LArr, multiwavelength HST imaging, and OSIRIS narrow band Hα and [NII]λ6584 imaging. The spectra were processed with the starlight full spectral fitting code, and the results are compared with those for two early-stage merger LIRGs (IC 1623 W and NGC 6090), together with CALIFA Sbc/Sc galaxies. We find that NGC 2623 went through two periods of increased star formation (SF), a first and widespread episode, traced by intermediate-age stellar populations ISP (140 Myr-1.4 Gyr), and a second one, traced by young stellar populations YSP (<140 Myr), which is concentrated in the central regions (<1.4 kpc). Our results are in agreement with the epochs of the first peri-center passage (∼200 Myr ago) and coalescence (<100 Myr ago) predicted by dynamical models, and with high-resolution merger simulations in the literature, consistent with NGC 2623 representing an evolved version of the early-stage mergers. Most ionized gas is concentrated within <2.8 kpc, where LINER-like ionization and high-velocity dispersion (∼220 km s −1 ) are found, consistent with the previously reported outflow. As revealed by the highest-resolution OSIRIS and HST data, a collection of HII regions is also present in the plane of the galaxy, which explains the mixture of ionization mechanisms in this system. It is unlikely that the outflow in NGC 2623 will escape from the galaxy, given the low SFR intensity (∼0.5 M ⊙ yr −1 kpc −2 ), the fact that the outflow rate is three times lower than the current SFR, and the escape velocity in the central areas is higher than the outflow velocity.

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Section: Osiris Line Emission At the Edge Of The Sw Tidal Tailmentioning

confidence: 58%

The spatially resolved stellar population and ionized gas properties in the merger LIRG NGC 2623

Cortijo-Ferrero

Delgado

Pérez

et al. 2017

A&A

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“…However, the TFR scatters for field and cluster samples may differ, with the field samples showing lower values. This is likely the result of a quieter mass accretion history and a less perturbed evolution of the dark matter halos for field systems, as well as the presence of kinematically disturbed systems such as tidal dwarf galaxies (Lelli et al 2015), interacting and stripped galaxies (Mendes de Oliveira et al 2003), and enhanced (Milvang-Jensen et al 2003) or quenched (Nakamura et al 2006) star formation in galaxy clusters. Figure 6 (bottom panel) shows the same data as above, but now comparing various fits (forward, inverse, bisector, orthogonal) of the TFR data by Giovanelli et al (1997), Courteau et al (2007a), Pizagno et al (2007) and this work.…”

Section: Velocity-luminosity (Tully-fisher) Relationsmentioning

confidence: 99%

The Spectroscopy and H-band Imaging of Virgo Cluster Galaxies (SHIVir) Survey: Scaling Relations and the Stellar-to-total Mass Relation

Ouellette

Courteau

Holtzman

et al. 2017

ApJ

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We present parameter distributions and fundamental scaling relations for 190 Virgo cluster galaxies in the SHIVir survey. The distribution of galaxy velocities is bimodal about V circ ∼ 125 km s −1 , hinting at the existence of dynamically unstable modes in the inner regions of galaxies. An analysis of the Tully-Fisher relation (TFR) of late-type galaxies (LTGs) and fundamental plane (FP) of earlytype galaxies (ETGs) is presented, yielding a compendium of galaxy scaling relations. The slope and zero-point of the Virgo TFR match those of field galaxies, while scatter differences likely reflect distinct evolutionary histories. The velocities minimizing scatter for the TFR and FP are measured at large apertures where the baryonic fraction becomes subdominant. While TFR residuals remain independent of any galaxy parameters, FP residuals (i.e. the FP "tilt") correlate strongly with the dynamical-to-stellar mass ratio, yielding stringent galaxy formation constraints. We construct a stellar-to-total mass relation (STMR) for ETGs and LTGs and find linear but distinct trends over the range M * = 10 8−11 M . Stellar-to-halo mass relations (SHMRs), which probe the extended dark matter halo, can be scaled down to masses estimated within the optical radius, showing a tight match with the Virgo STMR at low masses; possibly inadequate halo abundance matching prescriptions and broad radial scalings complicate this comparison at all masses. While ETGs appear to be more compact than LTGs of the same stellar mass in projected space, their mass-size relations in physical space are identical. The trends reported here may soon be validated through well-resolved numerical simulations.

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“…The properties of dwarf satellite galaxies are important for testing cosmological and gravity models on small scales (Gentile et al 2007; Kroupa et al 2010;Lelli et al 2015;Flores et al 2016), and the spacial and velocity distributions of these small galaxies around their hosts probe structure formation models on scales to trigger star formation and hence be observable (the "too big to fail" problem; Boylan-Kolchin et al 2011). These small-scale problems are often seen as mild tensions that can be resolved with the complex processes acting amongst the constituents of the Standard Model of particle physics, i.e.…”

Section: Introductionmentioning

confidence: 99%

DGSAT: Dwarf Galaxy Survey with Amateur Telescopes

Javanmardi

Martínez–Delgado

Kroupa³

et al. 2016

A&A

108

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Context. We introduce the Dwarf Galaxy Survey with Amateur Telescopes (DGSAT) project and report the discovery of eleven low surface brightness (LSB) galaxies in the fields of the nearby galaxies NGC 2683, NGC 3628, NGC 4594 (M 104), NGC 4631, NGC 5457 (M 101), and NGC 7814. Aims. The DGSAT project aims to use the potential of small-sized telescopes to probe LSB features around large galaxies and to increase the sample size of the dwarf satellite galaxies in the Local Volume. Methods. Using long exposure images, fields of the target spiral galaxies are explored for extended LSB objects. After identifying dwarf galaxy candidates, their observed properties are extracted by fitting models to their light profiles. Results. We find three, one, three, one, one, and two new LSB galaxies in the fields of NGC 2683, 3628, 4594, 4631, 5457, and 7814, respectively. In addition to the newly found galaxies, we analyse the structural properties of nine already known galaxies. All of these 20 dwarf galaxy candidates have effective surface brightnesses in the range 25.3 < ∼ µ e < ∼ 28.8 mag arcsec −2 and are fit with Sersic profiles with indices n < ∼ 1. Assuming that they are in the vicinity of the above mentioned massive galaxies, their r-band absolute magnitudes, their effective radii, and their luminosities are in the ranges −15.6 < ∼ M r < ∼ −7.8, 160 pc < ∼ R e < ∼ 4.1 kpc, and 0.1 × 10 6 < ∼ L L r < ∼ 127 × 10 6 , respectively. To determine whether these LSB galaxies are indeed satellites of the above mentioned massive galaxies, their distances need to be determined via further observations. Conclusions. Using small telescopes, we are readily able to detect LSB galaxies with similar properties to the known dwarf galaxies of the Local Group.

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Gas dynamics in tidal dwarf galaxies: Disc formation atz= 0

Cited by 93 publications

References 105 publications

The spatially resolved stellar population and ionized gas properties in the merger LIRG NGC 2623

The spatially resolved stellar population and ionized gas properties in the merger LIRG NGC 2623

The Spectroscopy and H-band Imaging of Virgo Cluster Galaxies (SHIVir) Survey: Scaling Relations and the Stellar-to-total Mass Relation

DGSAT: Dwarf Galaxy Survey with Amateur Telescopes

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