The Arches Cluster: Extended Structure and Tidal Radius

Hosek, Matthew W.; Lu, Jessica R.; Anderson, Jay; Ghez, A. M.; Morris, Mark; Clarkson, W. I.

doi:10.1088/0004-637x/813/1/27

Cited by 34 publications

(44 citation statements)

References 84 publications

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“…Local Group dwarf irregular galaxies show [α/Fe] ratios that cluster around [α/Fe] ⊙ with some scatter, with much lower values than MW stars of similar iron content (see review by Tolstoy et al 2009). In particular, sub-solar values have also been found in Sextans A (Kaufer et al 2004), WLM (Venn et al (2003), but also see Urbaneja et al (2008)) and NGC3109 (Hosek al. 2014).…”

Section: Ic 1613's Metal Contentmentioning

confidence: 82%

WINDS OF LOW-METALLICITY OB-TYPE STARS:HST-COS SPECTROSCOPY IN IC 1613

García

Herrero

Najarro

et al. 2014

ApJ

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We present the first quantitative UV spectroscopic analysis of resolved OB stars in IC 1613. Because of its alleged very low metallicity ( 1/10 Z ⊙ , from H II regions), studies in this Local Group dwarf galaxy could become a significant step forward from the SMC towards the extremely metal-poor massive stars of the early Universe. We present HST-COS data covering the ∼1150-1800Å wavelength range with resolution R∼2500. We find that the targets do exhibit wind features, and these are similar in strength to SMC stars. Wind terminal velocities were derived from the observed P Cygni profiles with the SEI method. The v ∞ -Z relationship has been revisited. The terminal velocity of IC 1613 O-stars is clearly lower than Milky Way counterparts, but there is no clear difference between IC 1613 and SMC or LMC analogue stars. We -2find no clear segregation with host galaxy in the terminal velocities of B-supergiants, nor in the v ∞ /v esc ratio of the whole OB star sample in any of the studied galaxies. Finally, we present first evidence that the Fe-abundance of IC 1613 OB stars is similar to the SMC, in agreement with previous results on red supergiants. With the confirmed ∼1/10 solar oxygen abundances of B-supergiants, our results indicate that IC 1613's α/Fe ratio is sub-solar.

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Section: Ic 1613's Metal Contentmentioning

confidence: 82%

WINDS OF LOW-METALLICITY OB-TYPE STARS:HST-COS SPECTROSCOPY IN IC 1613

García

Herrero

Najarro

et al. 2014

ApJ

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“…Current observations of the Quintuplet allow us to directly observe the projected stellar density as a function of projected distance to the cluster center-the radial profilewhich ultimately encodes information about a cluster's spatial extent and dynamical history. Portegies Zwart et al (2010) note that, counterintuitively, YMCs tend to lack sharp tidal truncations, a conclusion corroborated in part by observations of extragalactic star clusters (Mackey & Gilmore 2003a,b,c) as well as the Arches cluster (Hosek et al 2015).…”

Section: Introductionmentioning

confidence: 90%

“…Nevertheless, it appears clear that mass segregation in the Quintuplet, if it exists, is less substantial than it is in the Arches (Hosek et al 2015). This is quite an intriguing result-dynamical mass segregation is known to segregate clusters over a relaxation time, and the Quintuplet, as the older of the two, would naïvely be expected to be more mass segregated than the Arches.…”

Section: Mass Segregation In Ymcsmentioning

confidence: 99%

The Quintuplet Cluster: Extended Structure and Tidal Radius

Rui

Hosek

et al. 2019

ApJ

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The Quintuplet star cluster is one of only three known young (< 10 Myr) massive (M > 10 4 M ) clusters within ∼ 100 pc of the Galactic Center. In order to explore star cluster formation and evolution in this extreme environment, we analyze the Quintuplet's dynamical structure. Using the HST WFC3-IR instrument, we take astrometric and photometric observations of the Quintuplet covering a 120 × 120 field-of-view, which is 19 times larger than those of previous proper motion studies of the Quintuplet. We generate a catalog of the Quintuplet region with multi-band, near-infrared photometry, proper motions, and cluster membership probabilities for 10, 543 stars. We present the radial density profile of 715 candidate Quintuplet cluster members with M 4.7 M out to 3.2 pc from the cluster center. A 3σ lower limit of 3 pc is placed on the tidal radius, indicating the lack of a tidal truncation within this radius range. Only weak evidence for mass segregation is found, in contrast to the strong mass segregation found in the Arches cluster, a second and slightly younger massive cluster near the Galactic Center. It is possible that tidal stripping hampers a mass segregation signature, though we find no evidence of spatial asymmetry. Assuming that the Arches and Quintuplet formed with comparable extent, our measurement of the Quintuplet's comparatively large core radius of 0.62 +0.10 −0.10 pc provides strong empirical evidence that young massive clusters in the Galactic Center dissolve on a several Myr timescale.

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“…Proper motion studies have been used to identify cluster members in the Quintuplet cluster (Stolte et al 2008(Stolte et al , 2014Hosek et al 2015;Rui et al 2019). In order to test if our proper motion measurements are robust, we measured the proper motions of the Quintuplet cluster by using the HST data in the field that covers this cluster and the corresponding field of GNS (chip #2 of F10; see Fig.…”

Section: Methods Validationmentioning

confidence: 99%

First results from a large-scale proper motion study of the Galactic centre

Shahzamanian

Schödel

Nogueras-Lara

et al. 2019

A&A

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Proper motion studies of stars in the centre of the Milky Way have been typically limited to the Arches and Quintuplet clusters and to the central parsec. Here, we present the first results of a large-scale proper motion study of stars within several tens of parsecs of Sagittarius A* based on our 0.2 angular resolution GALACTICNUCLEUS survey (epoch 2015) combined with NICMOS/HST data from the Paschen-α survey (epoch 2008). This study will be the first extensive proper motion study of the central ∼ 36 × 16 of the Galaxy, which is not covered adequately by any of the existing astronomical surveys such as Gaia because of its extreme interstellar extinction (AV 30 mag). Proper motions can help us to disentangle the different stellar populations along the line-of-sight and interpret their properties in combination with multi-wavelength photometry from GALACTICNUCLEUS and other sources. It also allows us to infer the dynamics and interrelationship between the different stellar components (Galactic bulge, nuclear stellar disk, nuclear stellar cluster) of the Galactic Centre (GC). In particular, we use proper motions to detect co-moving groups of stars which can trace low mass or partially dissolved young clusters in the GC that can hardly be discovered by any other means. Our pilot study in this work is on a field in the nuclear bulge associated by HII regions that show the presence of young stars. We detect the first group of co-moving stars coincident with an HII region. Using colour-magnitude diagrams, we infer that the co-moving stars are consistent with being the post-main sequence stars with ages of few Myrs. Simulations show that this group of stars is a real group that can indicate the existence of a dissolving or low to intermediate mass young cluster. A census of these undiscovered clusters will ultimately help us to constrain star formation at the GC in the past few ten Myrs.

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The Arches Cluster: Extended Structure and Tidal Radius

Cited by 34 publications

References 84 publications

WINDS OF LOW-METALLICITY OB-TYPE STARS:HST-COS SPECTROSCOPY IN IC 1613

WINDS OF LOW-METALLICITY OB-TYPE STARS:HST-COS SPECTROSCOPY IN IC 1613

The Quintuplet Cluster: Extended Structure and Tidal Radius

First results from a large-scale proper motion study of the Galactic centre

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