Tidal dwarfs in the M81 group: The second generation?

Макарова, Л. Н.; Grebel, Eva K.; Караченцев, И. Д.; Dolphin, Andrew E.; Караченцева, В. Е.; Шарина, М. Е.; Geisler, Doug; Guhathakurta, Puragra; Hodge, P. W.; Sarajedini, Ata; Seitzer, Patrick

doi:10.1051/0004-6361:20021426

Cited by 92 publications

(124 citation statements)

References 31 publications

(52 reference statements)

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“…These features, already noticed by Arp (1965) and Efremov et al (1986), are due to dust in the ring, indicating that part of it should be situated between the observer and M 81. In the north-eastern part of this feature (in the region where HI strong emission was found by Yun et al 1994) a significant overdensity of stellar complexes is also apparent and suggests that new stars are still forming (Makarova et al 2002;Mouhcine & Ibata 2010).…”

Section: The Datamentioning

confidence: 84%

“…We adopted the relation by Muñoz-Mateos et al (2009;see their Eq. (A8)) to convert fluxes in masses adopting a distance for M 81 of 3.7 Mpc (Makarova et al 2002). In order to obtain total gas masses, we measured the HI fluxes from the M 81 intensity map obtained by the THINGS survey (Walter et al 2008).…”

Section: Comparison Between Far-infrared and Hi Emissionmentioning

confidence: 99%

“…Numerical simulations of the system by Yun (1999) successfully reproduced the HI tidal debris assuming M 82 and NGC 3077 approached M 81 during recent epochs. More recently, Makarova et al (2002) and De Mello et al (2008) resolved the nebular region characterized by strong HI emission into stars using deep Hubble Space Telescope (HST) observations. Their color-magnitude diagrams (CMD) showed a significant population of young stars (with an age of ∼40-160 Myr) and an old population characterized by a well defined Red Giant Branch.…”

Section: Introductionmentioning

confidence: 99%

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A multi-wavelength analysis of M 81: insight on the nature of Arp's loop

Sollima

Paz

Martínez–Delgado

et al. 2010

A&A

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Context. The optical ring-like structure detected by Arp (1965) around M 81 (commonly referenced as "Arp's loop") represents one of the most spectacular features observed in nearby galaxies. Arp's loop is commonly interpreted as a tail resulting from the tidal interaction between M 81 and M 82. However, since its discovery the nature of this feature has remained controversial. Aims. Our primary purpose was to identify the sources of optical and infrared emission observed in Arp's loop. Methods. The morphology of Arp's loop has been investigated with deep wide-field optical images. We also measured its colors using IRAS and Spitzer-MIPS infrared images and compared them with those of the disk of M 81 and Galactic dust cirrus that fills the area where M 81 is located. Results. Optical images reveal that this peculiar object has a filamentary structure characterized by many dust features overlapping M 81's field. The ratios of far-infrared fluxes and the estimated dust-to-gas ratios indicate the infrared emission of Arp's loop is dominated by the contribution of cold dust that is most likely from Galactic cirrus. Conclusions. The above results suggest that the light observed at optical wavelengths is a combination of emission from i) a few recent star-forming regions located close to M 81, where both bright UV complexes and peaks in the HI distribution are found, ii) the extended disk of M 81 and iii) scattered light from the same Galactic cirrus that is responsible for the bulk of the far-infrared emission.

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Section: The Datamentioning

confidence: 84%

Section: Comparison Between Far-infrared and Hi Emissionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A multi-wavelength analysis of M 81: insight on the nature of Arp's loop

Sollima

Paz

Martínez–Delgado

et al. 2010

A&A

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“…This fact should be considered when comparing the results of N-body simulations with the observational data. In addition to the presence of ultra-faint dwarfs of extremely low surface brightness, resolved into stars only at nearby distances, the Local Group stands out among the neighboring groups by the absence in it of blue compact dwarfs (BCD), as well as HI-filaments and tidal dwarfs like Holm-IX, BK3N, Garland, A0952+69, which are visible around M 81 (Makarova et al 2002). It should be added here that the stellar masses of MW and M 31, their virial masses, as well as the linear dimensions of the suite of companions around the MW and M 31 are notably inferior to other highluminosity galaxies in the Local Volume.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 99%

Companions around the nearest luminous galaxies: Segregation and selection effects

Караченцев

Kudrya

2015

Astron Nachr

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Using the "Updated Nearby Galaxy Catalog", we consider different properties of companion galaxies around luminous hosts in the Local Volume. The data on stellar masses, linear diameters, surface brightnesses, HI-richness, specific star formation rate (sSF R), and morphological types are discussed for members of the nearest groups, including the Milky Way and M 31 groups, as a function of their separation from the hosts. Companion galaxies in groups tend to have lower stellar masses, smaller linear diameters and fainter mean surface brightnesses as the distance to their host decreases. The hydrogen-to-stellar mass ratio of the companions increases with their linear projected separation from the dominant luminous galaxy. This tendency is more expressed around the bulge-dominated hosts. While linear separation of the companions decreases, their mean sSF R becomes lower, accompanied with the increasing sSF R scatter. Typical linear projected separation of dSphs around the bulge-dominated hosts, 350 kpc, is substantially larger than that around the disk-dominated ones, 130 kpc. This difference probably indicates the presence of larger hot/warm gas haloes around the early-type host galaxies. The mean fraction of dSph (quenched) companions in 11 the nearest groups as a function of their projected separation Rp can be expressed as f (E) = 0.55 − 0.69 × Rp. The fraction of dSphs around the Milky Way and M 31 looks much higher than in other nearby groups because the quenching efficiency dramatically increases towards the ultra-low mass companions. We emphasize that the observed properties of the Local Group are not typical for other groups in the Local Volume due to the role of selection effects caused by our location inside the Local Group.

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“…Walter et al 2006). Some of them, such as the Garland object or Holmberg IX, may qualify as TDG candidates (Makarova et al 2002) although their dynamical status and real age are still unknown. Finally, even more nearby, a tidal origin has been speculated for the old Local Group dwarf spheroidals by Kroupa (1997) and Metz & Kroupa (2007); however whether they really have a relatively low dark matter content, as claimed by these authors, is highly controversial (Mateo 1998).…”

Section: Introductionmentioning

confidence: 99%

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

Duc¹,

Braine

Lisenfeld

et al. 2007

A&A

103

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Context. Numerical simulations predict the existence of old Tidal Dwarf Galaxies (TDGs) that would have survived several Gyr after the collision lying at their origin. Such survivors, which would by now have become independent relaxed galaxies, would be ideal laboratories, if nearby enough, to tackle a number of topical issues, including the distribution of Dark Matter in and around galaxies. However finding old dwarf galaxies with a confirmed tidal origin is an observational challenge. Aims. A dwarf galaxy in the nearby Virgo Cluster, VCC 2062, exhibits several unusual properties that are typical of a galaxy made out of recycled material. We discuss whether it may indeed be a TDG. Methods. We analysed multi-wavelength observations of VCC 2062, including a CO map acquired with the IRAM 30 m dish, an optical spectrum of its HII regions, GALEX ultraviolet and archival broad-band and narrow-band optical images as well as a VLA HI datacube, originally obtained as part of the VIVA project. Results. VCC 2062 appears to be the optical, low surface brightness counterpart of a kinematically detached, rotating condensation that formed within an HI tail apparently physically linked to the disturbed galaxy NGC 4694. In contrast to its faint optical luminosity, VCC 2062 is characterised by strong CO emission and a high oxygen abundance more typical of spiral disks. Its dynamical mass however, is that of a dwarf galaxy. Conclusions. VCC 2062 was most likely formed within a pre-enriched gaseous structure expelled from a larger galaxy as a result of a tidal interaction. The natural provider for the gaseous tail is NGC 4694 or rather a former companion which subsequently has been accreted by the massive galaxy. According to that scenario, VCC 2062 has been formed by a past tidal encounter. Since its parent galaxies have most probably already totally merged, it qualifies as an old Tidal Dwarf Galaxy.

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Tidal dwarfs in the M81 group: The second generation?

Cited by 92 publications

References 31 publications

A multi-wavelength analysis of M 81: insight on the nature of Arp's loop

A multi-wavelength analysis of M 81: insight on the nature of Arp's loop

Companions around the nearest luminous galaxies: Segregation and selection effects

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

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