The outer envelopes of globular clusters. II. NGC 1851, NGC 5824 and NGC 1261*

Kuzma, Pete; Costa, G. S. Da; Mackey, A. D.

doi:10.1093/mnras/stx2353

Cited by 85 publications

(85 citation statements)

References 65 publications

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“…In fact, the animation associated with Figure 4 suggests that these putative tidal tails may extend ±15°or more from NGC 1851. The detection of extratidal structure associated with NGC 1851 agrees with recent work by Kuzma et al (2018) and Carballo-Bello et al (2018). The DES data greatly extend the coverage around NGC 1851 and make a strong case for a "vast stellar structure" (Carballo-Bello et al 2018) extending both northward and southward of this cluster.…”

Section: Ngc 1851supporting

confidence: 87%

“…The analysis of Leon et al (2000) suggests the existence of a tidal tail oriented in the direction of the Galactic center. Recent observations with DECam have similarly detected evidence that the stellar halo of NGC 1261 extends beyond its nominal Wilson tidal radius (Carballo-Bello et al 2018;Kuzma et al 2018) but do not see any evidence of tail-like structure. Our observations support the existence of extratidal structure around NGC 1261.…”

Section: Ngc 1261mentioning

confidence: 96%

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Stellar Streams Discovered in the Dark Energy Survey

Shipp

Drlica-Wagner

Balbinot

et al. 2018

ApJ

246

254

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We perform a search for stellar streams around the Milky Way using the first 3 yr of multiband optical imaging data from the Dark Energy Survey (DES). We use DES data covering ∼5000 deg 2 to a depth of g>23.5 with a relative photometric calibration uncertainty of <1%. This data set yields unprecedented sensitivity to the stellar density field in the southern celestial hemisphere, enabling the detection of faint stellar streams to a heliocentric distance of ∼50 kpc. We search for stellar streams using a matched filter in color-magnitude space derived from a synthetic isochrone of an old, metal-poor stellar population. Our detection technique recovers four previously known thin stellar streams: Phoenix, ATLAS, Tucana III, and a possible extension of Molonglo. In addition, we report the discovery of 11 new stellar streams. In general, the new streams detected by DES are fainter, more distant, and lower surface brightness than streams detected by similar techniques in previous photometric surveys. As a by-product of our stellar stream search, we find evidence for extratidal stellar structure associated with four globular clusters: NGC 288, NGC 1261, NGC 1851, and NGC 1904. The ever-growing sample of stellar streams will provide insight into the formation of the Galactic stellar halo, the Milky Way gravitational potential, and the large-and small-scale distribution of dark matter around the Milky Way.

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Section: Ngc 1851supporting

confidence: 87%

Section: Ngc 1261mentioning

confidence: 96%

Stellar Streams Discovered in the Dark Energy Survey

Shipp

Drlica-Wagner

Balbinot

et al. 2018

ApJ

246

254

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“…These are expected for stripped galaxy nuclei, as the inner component tracks the original NSC, while the outer section is the remnants of the remaining galaxy (Pfeffer & Baumgardt 2013). Low surface brightness halos found around galactic GCs have also been suggested to track tidally stripped nuclei (e.g., Olszewski et al 2009;Kuzma et al 2018). Thus the twocomponent profile provides perhaps the strongest evidence for UCD 330 being a stripped nucleus.…”

mentioning

confidence: 92%

Upper Limits on the Presence of Central Massive Black Holes in Two Ultra-compact Dwarf Galaxies in Centaurus A

Voggel

Seth

Neumayer

et al. 2018

ApJ

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The recent discovery of massive black holes (BHs) in the centers of high-mass ultra-compact dwarf galaxies (UCDs) suggests that at least some are the stripped nuclear star clusters of dwarf galaxies. We present the first study that investigates whether such massive BHs, and therefore stripped nuclei, also exist in low-mass (M<10 7 M e ) UCDs. We constrain the BH masses of two UCDs located in Centaurus A (UCD 320 and UCD 330) using Jeans modeling of the resolved stellar kinematics from adaptive optics data obtained with the SINFONI integral field spectrograph at the Very Large Telescope (VLT/SINFONI). No massive BHs are found in either UCD. We find a 3σ upper limit on the central BH mass in UCD 330 of M • <1.0 × 10 5 M e , which corresponds to 1.7% of the total mass. This excludes a high-mass fraction BH and would only allow low-mass BHs similar to those claimed to be detected in Local Group globular clusters. For UCD 320, poorer data quality results in a less constraining 3σ upper limit of M • <1 × 10 6 M e , which is equal to 37.7% of the total mass. The dynamical massto-light ratios of UCD 320 and UCD 330 are not inflated compared to predictions from stellar population models. The non-detection of BHs in these low-mass UCDs is consistent with the idea that elevated dynamical mass-tolight ratios do indicate the presence of a substantial BH. Although no massive BHs are detected, these systems could still be stripped nuclei. The strong rotation (v/σ of 0.3-0.4) in both UCDs and the two-component light profile in UCD 330 support the idea that these UCDs may be stripped nuclei of low-mass galaxies whose BH occupation fraction is not yet known.

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“…These streams range from events as massive as the accretion of the Sagittarius (Sgr) dwarf spheroidal galaxy (Ibata et al 1994;Belokurov et al 2006) to observations of more The full Tables C.1 and C.3 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/. elusive stellar streams and envelopes attributed to globular clusters (GCs) that are in the process of being tidally disrupted (e.g., Odenkirchen et al 2001;Grillmair & Dionatos 2006;Jordi & Grebel 2010;Kuzma et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Purveyors of fine halos

Hanke

Koch

Prudil

et al. 2020

A&A

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A long-lasting open question in the field of Galactic archeology refers to the size of the contribution from former globular cluster (GC) stars to the formation of the stellar halo of the Milky Way. We contribute to answering this important question by establishing observational links between the present-day halo field star population and GCs. To this end, we combined astrometric information such as space motions and parallaxes from the second data release of the Gaia mission (Gaia DR2) with spectroscopic radial velocities and metallicities ([Fe/H]) from the Sloan Digital Sky Survey (SDSS-IV, DR14) to end up with a seven-dimensional chemodynamical information space for more than 3 · 10 5 stars. Moreover, from our previous study, we incorporated the sample of halo giant stars with a distinct chemical signature (strong CN bandheads) that resembles the light-elements anomaly otherwise only seen in the second generation of globular cluster stellar populations. Using three different tagging techniques -among which is the exploration of conservative integrals of motion -we are able to establish unique associations between 151 extratidal stars in the neighborhood of eight GCs, which coincide with earlier findings of stellar envelopes beyond the tidal radius and even beyond (out to several tens of tidal radii). In addition, we trace the possible origin of about 62% of the sample of CN-strong giants to their potential host clusters. We find a connection between several of the involved GCs and the Gaia-Enceladus and Sequoia merger events. By establishing kinematic and chemical connections between 17 CN-strong stars and their surrounding fields, we identify co-moving groups of stars at the same [Fe/H] with a possible cluster origin. Some of these associations contain RR Lyrae variables, which allows meaningful distance inferences to be made. From these, we find strong evidence that four CN-strong stars and their associates are connected to the Sagittarius stream whilst their tightly confined [Fe/H] may hint to a birth site in M 54, the massive cluster in Sagittarius' core remnant. Finally, by employing the counts of CN-strong and bona-fide CN-normal giants from our novel sample, we provide tentative estimates for the fraction of first-generation cluster stars among all stars lost to the halo. In the immediate cluster vicinity, this value amounts to 50.0 ± 16.7% while the associations in the halo field rather imply 80.2 +4.9 −5.2 %. We speculate that -if proven real by spectroscopic follow-up -the disparity between these numbers could indicate a major contribution of low-mass clusters to the overall number of stars escaped to the halo or could alternatively suggest strong mass loss from the first generation during early cluster dissolution.

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The outer envelopes of globular clusters. II. NGC 1851, NGC 5824 and NGC 1261*

Cited by 85 publications

References 65 publications

Stellar Streams Discovered in the Dark Energy Survey

Stellar Streams Discovered in the Dark Energy Survey

Upper Limits on the Presence of Central Massive Black Holes in Two Ultra-compact Dwarf Galaxies in Centaurus A

Purveyors of fine halos

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