A tale of two tails: exploring stellar populations in the tidal tails of NGC 3256

Rodruck, M.; Konstantopoulos, I. S.; Knierman, Karen; Федотов, К. В.; Mullan, B.; Gallagher, S. C.; Durrell, Patrick R.; Ciardullo, Robin; Grönwall, C.; Charlton, Jane C.

doi:10.1093/mnras/stw1294

Cited by 7 publications

(6 citation statements)

References 41 publications

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“…Hernquist & Quinn 1988;Hendel & Johnston 2015). Blue, low surface brightness tidal streams can, however, be caused by both recent minor (Knierman et al 2012(Knierman et al , 2013 and older major mergers (Rodruck et al 2016). In addition, there are red, quiescent streams which show no active star formation.…”

Section: Introductionmentioning

confidence: 99%

“…The majority of observational work on tidal features in external galaxies to date has been based upon targeted observations of a relatively small number of galaxies (see, e.g. Schweizer & Seitzer 1988;Martínez-Delgado et al 2009Kim et al 2012;Knierman et al 2012Knierman et al , 2013Beaton et al 2014;Martínez-Delgado et al 2015;Rodruck et al 2016;Greco et al 2018b). Amongst those works that are able to derive tidal feature occurrence fractions, where f tidal is the fraction of all galaxies that host tidal features, observed values of f tidal vary by a factor of 7 (Malin & Carter 1983;van Dokkum 2005;Tal et al 2009;Nair & Abraham 2010;Atkinson et al 2013;Hood et al 2018).…”

Section: Introductionmentioning

confidence: 99%

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Tidal Features at 0.05 < z < 0.45 in the Hyper Suprime-Cam Subaru Strategic Program: Properties and Formation Channels

Kado-Fong

Greene

Hendel

et al. 2018

ApJ

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We present 1,201 galaxies at 0.05 < z < 0.45 that host tidal features, detected from the first ∼ 200 deg 2 of imaging from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). All galaxies in the present sample have spectroscopic observations from the Sloan Digital Sky Survey (SDSS) spectroscopic campaigns, generating a sample of 21,208 galaxies. Of these galaxies, we identify 214 shell systems and 987 stream systems. For 575 of these systems, we are additionally able to measure the (g − i) colors of the tidal features. We find evidence for star formation in a subset of the streams, with the exception of streams around massive ellipticals, and find that stream host galaxies span the full range of stellar masses in our sample. Galaxies which host shells are predominantly red and massive: we find that observable shells form more frequently around ellipticals than around disc galaxies of the same stellar mass. Although the majority of the shells in our sample are consistent with being formed by minor mergers, 15% ± 4.4% of shell host galaxies have (g − i) colors as red as their host galaxy, consistent with being formed by major mergers. These "red shell" galaxies are additionally preferentially aligned with the major axis of the host galaxy, as previously predicted from simulations. We suggest that although the bulk of the observable shell population originates from fairly minor mergers, which preferentially form shells that are not aligned with the major axis of the galaxy, major mergers produce a significant number of observable shells.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Tidal Features at 0.05 < z < 0.45 in the Hyper Suprime-Cam Subaru Strategic Program: Properties and Formation Channels

Kado-Fong

Greene

Hendel

et al. 2018

ApJ

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“…This argues against the scenario that the HI filament formed only by the accretion from NGC 6147 and MCG +07-34-022. The shape of HI filament appears to be different to the typical tidal stripped HI tails, which are usually distributed roughly symmetrically on both sides of galaxy (Odenkirchen et al 2001;Klimentowski et al 2007;Rodruck et al 2016), along with disturbed optical morphology and enhanced star formation in galactic center (Fujita 1998;Li et al 2008;Smith et al 2010). NGC 6145 has enhanced star formation activities in the outer region, and not in the galactic center, which is inconsistent with the scenario that the HI filament is due to the tidal stripping by NGC 6146.…”

Section: Summary and Discussionmentioning

confidence: 94%

The Peculiar Filamentary H i Structure of NGC 6145

Wang

Kong

et al. 2017

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In this paper, we report the peculiar HI morphology of the cluster spiral galaxy NGC 6145, which has a 150 kpc HI filament on one side that is nearly parallel to its major axis. This filament is made up of several HI clouds and the diffuse HI gas between them, with no optical counterparts. We compare its HI distribution with other one-sided HI distributions in the literature, and find that the overall HI distribution is very different from the typical tidal and ram-pressure stripped HI shape, and its morphology is inconsistent with being a pure accretion event. Only ∼30% of the total HI gas is anchored on the stellar disk, while most of HI gas forms the filament in the west. At a projected distance of 122 kpc, we find a massive elliptical companion (NGC 6146) with extended radio emission, whose axis points to an HI gap in NGC 6145. The velocity of the HI filament shows an overall light-ofsight motion of 80 to 180 km s −1 with respect to NGC 6145. Using the long-slit spectra of NGC 6145 along its major stellar axis, we find that some outer regions show enhanced star formation, while in contrast, almost no star formation activities are found in its center (<2 kpc). Pure accretion, tidal or ram-pressure stripping is not likely to produce the observed HI filament. An alternative explanation is the jet-stripping from NGC 6146, although direct evidence for a jet-cold gas interaction has not been found.

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“…Oosterloo et al 2004;Mendes de Oliveira et al 2004Ryan-Weber et al 2004;Boquien et al 2007;Torres-Flores et al 2012;de Mello et al 2012;Rodruck et al 2016;Lee-Waddell et al 2016). However, the environments of peculiar merger-candidate elliptical galaxies, with Hi outside their main optical body, have not receive as much attention.…”

Section: Introductionmentioning

confidence: 99%

“…Most of the studies on star-forming regions in the outskirts of galaxies are based in the analysis of ongoing wet mergers, where Hi-rich tidal debris and tidal structures are present, and the interacting galaxies are still separate entities (e.g. Oosterloo et al 2004;Mendes de Oliveira et al 2004Ryan-Weber et al 2004;Boquien et al 2007;Torres-Flores et al 2012;de Mello et al 2012;Rodruck et al 2016;Lee-Waddell et al 2016). However, the environments of peculiar merger-candidate elliptical galaxies, with Hi outside their main optical body, have not receive as much attention.…”

Section: Introductionmentioning

confidence: 99%

Star formation in low density HI gas around the elliptical galaxy NGC 2865

Urrutia-Viscarra

Torres-Flores

Oliveira

et al. 2017

A&A

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Context. Interacting galaxies surrounded by Hi tidal debris are ideal sites for the study of young clusters and tidal galaxy formation. The process that triggers star formation in the low-density environments outside galaxies is still an open question. New clusters and galaxies of tidal origin are expected to have high metallicities for their luminosities. Spectroscopy of such objects is, however, at the limit of what can be done with existing 8-10m class telescopes, which has prevented statistical studies of these objects. Aims. NGC 2865 is an UV-bright merging elliptical galaxy with shells and extended Hi tails. The regions observed in this work were previously detected using multi-slit imaging spectroscopy. Methods. We obtain new multi-slit spectroscopy of six young star-forming regions around NGC 2865, to determine their redshifts and metallicities. Results. The six emission-line regions are located 16-40 kpc from NGC 2865 and they have similar redshifts. They have ages of ∼ 10 Myears and an average metallicity of ∼ 12+log(O/H)∼8.6, suggesting a tidal origin for the regions. It is noted that they coincide with an extended Hi tail, which has projected density of N HI < 10 19 cm −2 , and displays a low surface brightness counterpart. These regions may represent the youngest of the three populations of star clusters already identified in NGC 2865. Conclusions. The high, nearly-solar, oxygen abundances found for the six regions in the vicinity of NGC 2865 suggest that they were formed by pre-enriched material from the parent galaxy, from gas removed during the last major merger. Given the mass and the location of the Hii regions, we can speculate that these young star-forming regions are potential precursors of globular clusters that will be part of the halo of NGC 2865 in the future. Our result supports the use of the multi-slit imaging spectroscopy as a useful tool for finding nearly-formed stellar systems around galaxies.

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A tale of two tails: exploring stellar populations in the tidal tails of NGC 3256

Cited by 7 publications

References 41 publications

Tidal Features at 0.05 < z < 0.45 in the Hyper Suprime-Cam Subaru Strategic Program: Properties and Formation Channels

Tidal Features at 0.05 < z < 0.45 in the Hyper Suprime-Cam Subaru Strategic Program: Properties and Formation Channels

The Peculiar Filamentary H i Structure of NGC 6145

Star formation in low density HI gas around the elliptical galaxy NGC 2865

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