Globular cluster orbits based on Hipparcos proper motions

Odenkirchen, M.; Brosche, P.; Geffert, M.; Tucholke, H. J.

doi:10.1016/s1384-1076(97)00035-3

Cited by 81 publications

(101 citation statements)

References 36 publications

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“…Uncertainties and correlations are not listed, but are available from the TGAS, Tycho2 and RAVE catalogues. worth & Hanson (1993) measured µ α * = 3.4 ± 1.7 mas/yr and µ δ = −1.9 ± 1.5 mas/yr from the ground; Odenkirchen et al (1997) measured µ α * = 7.0 ± 1.0 mas/yr and µ δ = −5.3 ± 1.0 mas/yr using Hipparcos data; Freire et al (2003) measured µ α * = 5.3±0.6 mas/yr and µ δ = −3.3±0.6 mas/yr using radio observations of millisecond pulsars (MSPs); measured µ α * = 5.88 ± 0.18 mas/yr and µ δ = −2.53 ± 0.18 mas/yr using HST/WFPC2 8 ; and 8 We did not use the absolute PM given in ; instead we used their measured motion of NGC 104 relative to the Small Magellanic Cloud (SMC) combined with the SMC PM measurement from Kalli- Cioni et al (2016) measured µ α * = 7.26 ± 0.03 mas/yr and µ δ = −1.25 ± 0.03 mas/yr using ground-based data from VISTA. These points are shown in the PM panel (centre left) of Figure 3 as orange, green, cyan, blue, and purple points, respectively.…”

Section: Ngc 104 (47 Tucanae)mentioning

confidence: 98%

“…Cudworth & Hanson (1993) measured µ α * = −1.2 ± 2.5 mas/yr and µ δ = 2.4 ± 3.0 mas/yr from the ground; Scholz et al (1993) measured µ α * = −3.1 ± 0.2 mas/yr and µ δ = −2.3 ± 0.4 mas/yr using photographic plates; Odenkirchen et al (1997) measured µ α * = 0.9 ± 1.0 mas/yr and µ δ = −2.2 ± 1.0 mas/yr using Hipparcos data; Geffert (1998) measured µ α * = −1.2 ± 0.8 mas/yr and µ δ = −3.2 ± 0.8 mas/yr also using Hipparcos stars; and Wu et al (2002) measured µ α * = −0.06 ± 0.3 mas/yr and µ δ = −2.6 ± 0.3 mas/yr using photographic plates spanning a 70 year baseline. The latter four points are shown in the PM panel (centre left) of Figure 4 as orange, green, cyan, and blue points, respectively.…”

Section: Ngc 5272 (M 3)mentioning

confidence: 99%

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Tycho-Gaia Astrometric Solution Parallaxes and Proper Motions for Five Galactic Globular Clusters

Watkins

Marel

2017

ApJ

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We present a pilot study of Galactic globular cluster (GC) proper motion (PM) determinations using Gaia data. We search for GC stars in the Tycho-Gaia Astrometric Solution (TGAS) catalogue from Gaia Data Release 1 (DR1), and identify five members of NGC 104 (47 Tucanae), one member of NGC 5272 (M 3), five members of NGC 6121 (M 4), seven members of NGC 6397, and two members of NGC 6656 (M 22). By taking a weighted average of member stars, fully accounting for the correlations between parameters, we estimate the parallax (and, hence, distance) and PM of the GCs. This provides a homogeneous PM study of multiple GCs based on an astrometric catalogue with small and well-controlled systematic errors and yields random PM errors similar to existing measurements. Detailed comparison to the available Hubble Space Telescope (HST) measurements generally shows excellent agreement, validating the astrometric quality of both TGAS and HST. By contrast, comparison to ground-based measurements shows that some of those must have systematic errors exceeding the random errors. Our parallax estimates have uncertainties an order of magnitude larger than previous studies, but nevertheless imply distances consistent with previous estimates. By combining our PM measurements with literature positions, distances, and radial velocities, we measure Galactocentric space motions for the clusters and find that these also agree well with previous analyses. Our analysis provides a framework for determining more accurate distances and PMs of Galactic GCs using future Gaia data releases. This will provide crucial constraints on the near end of the cosmic distance ladder and provide accurate GC orbital histories.

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Section: Ngc 104 (47 Tucanae)mentioning

confidence: 98%

Section: Ngc 5272 (M 3)mentioning

confidence: 99%

Tycho-Gaia Astrometric Solution Parallaxes and Proper Motions for Five Galactic Globular Clusters

Watkins

Marel

2017

ApJ

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“…They also observed round contours, but no extratidal halo. NGC 5904 is approaching perigalacticon, starting its crossing of the Galactic disk (Odenkirchen et al 1997). …”

Section: Ngc 5904 (M 5)mentioning

confidence: 99%

Search for extratidal features around 17 globular clusters in the Sloan Digital Sky Survey

Jordi

Grebel

2010

A&A

110

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Context. The dynamical evolution of a single globular cluster and also of the entire Galactic globular cluster system has been studied theoretically in detail. In particular, simulations show how the "lost" stars are distributed in tidal tails emerging from the clusters. Aims. We investigate the distribution of Galactic globular cluster stars on the sky to identify such features as tidal tails. The Sloan Digital Sky Survey provides consistent photometry of a large part of the sky to study the projected two-dimensional structure of the 17 globular clusters in its survey area. Methods. We used a color-magnitude weighted counting algorithm to map (potential) cluster member stars on the sky. Results. We recover the already known tidal tails of Pal 5 and NGC 5466. For NGC 4147 we find a two-arm morphology. Possible indications of tidal tails are also seen around NGC 5053 and NGC 7078, confirming earlier suggestions. Moreover, we find potential tails around NGC 5904 and Pal 14. Especially for Palomar clusters other than Pal 5, deeper data are needed to confirm or to rule out the existence of tails. For many of the remaining clusters in our sample we observe a pronounced extratidal halo, which is particularly large for NGC 7006 and Pal 1. In some cases, the extratidal halos may be associated with the stream of the Sagittarius dwarf spheroidal galaxy (e.g., NGC 4147, NGC 5024, NGC 5053).

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“…For reference we reproduce and update these here in Table 1, in which the escape velocity V esc is from Webbink (1985), the time T since last plane crossing is from Odenkirchen et al (1997), the metallicity is from Sneden et al (1997), the reddening is from Moehler et al (1995) and the distance is from Durrell & Harris (1993); other data are from compilations in Djorkovski & Meylan (1993).…”

Section: Ngc 7078mentioning

confidence: 99%

Far infra-red emission from NGC 7078: First detection of intra-cluster dust in a globular cluster

Evans

Stickel

Loon

et al. 2003

A&A

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Abstract. Improved data analysis of far infrared imaging data of the globular cluster NGC 7078 obtained with the ISO instrument ISOPHOT at 60 µm, 70 µm and 90 µm has detected the thermal emission from dust in its core, the first secure detection of intra-cluster dust in a globular cluster. The amount of dust is broadly consistent with mass-loss from evolved, metal-deficient stars in NGC 7078 in the time since it last crossed the Galactic plane.

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Globular cluster orbits based on Hipparcos proper motions

Cited by 81 publications

References 36 publications

Tycho-Gaia Astrometric Solution Parallaxes and Proper Motions for Five Galactic Globular Clusters

Tycho-Gaia Astrometric Solution Parallaxes and Proper Motions for Five Galactic Globular Clusters

Search for extratidal features around 17 globular clusters in the Sloan Digital Sky Survey

Far infra-red emission from NGC 7078: First detection of intra-cluster dust in a globular cluster

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