Stellar Tidal Streams in Spiral Galaxies of the Local Volume: A Pilot Survey With Modest Aperture Telescopes

Martínez–Delgado, David; Gabany, R. Jay; Crawford, Ken; Zibetti, S.; Majewski, Steven R.; Rix, Hans─Walter; Fliri, J.; Carballo‐Bello, J. A.; Gagliuffi, Daniella Bardalez; Peñarrubia, Jorge; Chonis, Taylor S.; Madore, Barry F.; Trujillo, Ignacio; Schirmer, M.; McDavid, D.

doi:10.1088/0004-6256/140/4/962

Cited by 368 publications

(355 citation statements)

References 37 publications

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“…Tidal streams or little tails are also kinematically distinct components, and they turn out to be quite common in the local universe. At least 6 % of the local galaxies show distinct stream-like features, and a total of 19 % show some sort of faint tail (e.g., Miskolczi et al 2011;Martínez-Delgado et al 2010). They are thought to be leftovers of tidally disrupted gas-rich satellites on their way to reach the center of the global gravitational potential.…”

Section: Kinematical Distortionsmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

183

130

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Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

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Section: Kinematical Distortionsmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

183

130

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“…There remains a possibility that a component of the halo formed dissipationally during the Galaxy formation process (Eggen et al, 1962;Samland & Gerhard, 2003). Halobuilding accretion events continue to the present time: the disrupting Sgr dwarf is an example in our Galaxy, and the faint disrupting system around NGC 5907 is another example of such an event (Martínez-Delgado et al, 2010). The metallicity distribution function (MDF) of the major surviving satellites around the Milky way is not like the MDF in the stellar halo (e.g.…”

Section: The Galactic Stellar Halomentioning

confidence: 99%

Structure and Evolution of the Milky Way

Freeman

2011

Astrophysics and Space Science Proceedings

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This review discusses the structure and evolution of the Milky Way, in the context of opportunities provided by asteroseismology of red giants. The review is structured according to the main Galactic components: the thin disk, thick disk, stellar halo, and the Galactic bar/bulge. The review concludes with an overview of Galactic archaeology and chemical tagging, and a brief account of the upcoming HERMES survey with the AAT. The Thin Disk: Formation and EvolutionHere are some of the issues related to the formation and evolution of the Galactic thin disk:• Building the thin disk: its exponential radial structure, and the role of mergers.• The star formation history: chemical evolution and continued gas accretion.• Evolutionary processes in the disk: disk heating, radial mixing.• The outer disk: chemical properties and chemical gradients.Many of the basic observational constraints on the properties of the Galactic disk are still uncertain. At this time, we do not have reliable information about the star formation history of the disk. We do not know how the metallicity distribution and the stellar velocity dispersions in the disk have evolved with time. One might have expected that these observational questions were well understood by now, but this is not yet so. The basic observational problem is the difficulty of measuring ages for individual stars.The younger stars of the Galactic disk show a clear abundance gradient of about 0.07 dex kpc −1 , outlined nicely by the cepheids (Luck et al., 2006). In the outer disk, for the older stars, the abundance gradient appears to be even stronger: the

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“…In the recent years, a big effort has been made to develop deep photometric surveys aimed at studying galaxy structures up to the faintest levels of surface brightness, which reveal lowluminosity structures and trace the stellar halos at very large distances from the galaxy center (Mihos et al 2005;Janowiecki et al 2010;Martínez-Delgado et al 2010;Roediger et al 2011;Ferrarese et al 2012;van Dokkum et al 2014;Duc et al 2015;Muñoz et al 2015;Trujillo & Fliri 2015). Recently, deep images of the Virgo cluster have revealed several faint (μ V =26-29 mag arcsec −2 ) streams of ICL among the galaxy members and made it possible to map the stellar halos of the bright cluster galaxies (BCGs) at very large distances from the center (Janowiecki et al 2010).…”

Section: Introductionmentioning

confidence: 99%

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

Iodice

Capaccioli

Grado

et al. 2016

ApJ

174

342

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We have started a new, deep multi-imaging survey of the Fornax cluster, dubbed the Fornax Deep Survey (FDS), at the VLT Survey Telescope (VST). In this paper we present the deep photometry inside two square degrees around the bright galaxy NGC1399 in the core of the cluster. We found that the core of the Fornax cluster is characterized by a very extended and diffuse envelope surrounding the luminous galaxy NGC1399: we map the surface brightness out to 33 arcmin (∼192 kpc) from the galaxy center and down to μ g ∼31 mag arcsec −2 in the g band. The deep photometry allows us to detect a faint stellar bridge in the intracluster region on the west side of NGC1399 and toward NGC1387. By analyzing the integrated colors of this feature, we argue that it could be due to the ongoing interaction between the two galaxies, where the outer envelope of NGC1387 on its east side is stripped away. By fitting the light profile, we found that there exists a physical break radius in the total light distribution at R=10 arcmin (∼58 kpc) that sets the transition region between the bright central galaxy and the outer exponential halo, and that the stellar halo contributes 60% of the total light of the galaxy (Section 3.5). We discuss the main implications of this work on the build-up of the stellar halo at the center of the Fornax cluster. By comparing with the numerical simulations of the stellar halo formation for the most massive bright cluster galaxies (i.e., M M 13 log 14, we find that the observed stellar halo mass fraction is consistent with a halo formed through the multiple accretion of progenitors with stellar mass in the range 10 8 -10 11 M e . This might suggest that the halo of NGC1399 has also gone through a major merging event. The absence of a significant number of luminous stellar streams and tidal tails out to 192 kpc suggests that the epoch of this strong interaction goes back to an early formation epoch. Therefore, different from the Virgo cluster, the extended stellar halo around NGC1399 is characterized by a more diffuse and well-mixed component, including the intracluster light.

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Stellar Tidal Streams in Spiral Galaxies of the Local Volume: A Pilot Survey With Modest Aperture Telescopes

Cited by 368 publications

References 37 publications

Star formation sustained by gas accretion

Star formation sustained by gas accretion

Structure and Evolution of the Milky Way

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

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