J/A+A/673/A44 e-TidalGCs project. Galactic globular cluster (Ferrone+, 2023)
The e-TidalGCs project.
Modeling the extra-tidal features generated by Galactic globular clusters.
Ferrone S., Di Matteo P., Mastrobuono-Battisti A., Haywood M., Snaith O.N.,
Montuori M., Khoperskov S., Valls-Gabaud D.
<Astron. Astrophys., 673, A44 (2023)>
=2023A&A...673A..44F 2023A&A...673A..44F (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, globular ; Models ; Optical
Keywords: globular clusters: general - Galaxy: structure -
Galaxy: kinematics and dynamics - Galaxy: evolution -
methods: numerical
Abstract:
We present the e-TidalGCs project, aimed at modeling and predicting
the extra-tidal features surrounding all Galactic globular clusters
for which 6D phase-space information, masses, and sizes are available
(currently numbering 159 globular clusters). We focus the analysis and
presentation of the results on the distribution of extra-tidal
material on the sky, as well as on the different structures found at
different heliocentric distances. We emphasize the wide variety of
morphologies found: beyond the canonical tidal tails, our models
reveal that the extra-tidal features generated by globular clusters
take a wide variety of shapes, from thin and elongated shapes to thick
and complex halo-like structures. We also compare some of the most
well-studied stellar streams found around Galactic globular clusters
to our model predictions, namely, those associated with the clusters
NGC 3201, NGC 4590, NGC 5466, and Pal 5. Additionally, we investigate
how the distribution and extension in the sky of the simulated streams
vary with the Galactic potential by making use of three different
models, either containing a central spheroid, not containing one, or
containing a stellar bar. Overall, our models predict that the mass
lost by the current globular cluster population in the field from the
last 5Gyrs is between 0.3-2.1x107M☉. This amount is
comparable to a value between 7-55% of the current mass. Most of this
lost mass is found in the inner Galaxy, with the half-mass radius of
this population being between 4-6kpc. The outputs of the simulations
will be publicly available, coinciding with the unique opportunity
presented by the delivery of the ESA Gaia mission and complementary
spectroscopic surveys. Their exquisite data will offer the possibility
to carry out novel comparisons with the models discussed in this work.
Description:
In this work, we have presented the first simulated catalogue of all
Galactic globular clusters for which 6D phase-space information, along
with masses and sizes are available. A total of 159 globular clusters
has been simulated in three Milky Way-like potentials, modeling the
process of tidal stripping that these clusters have experienced over
the past 5Gyr. As a result, for all clusters, we can predict the
distribution of the extra-tidal material in the sky, their proper
motions, distances to the Sun, and line-of-sight velocities.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 100 159 Current positions in the sky, proper motions,
line-of-sight velocities, distances and
relative uncertainties, masses, and half-mass
radii for all globular clusters analyzed
in this study
tableb1.dat 34 159 Crossing time, tcross, and median error in
energy conservation, for all 159 clusters
evolved in isolation
tabled1.dat 28 159 Classification of the 159 globular clusters
studied in this paper
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Cluster Cluster name
16- 21 F6.2 kpc Dist Distance
23- 26 F4.2 kpc e_Dist Distance error
28- 35 F8.4 deg RAdeg Right ascension (J2000)
37- 44 F8.4 deg DEdeg Declination (J2000)
46- 52 F7.3 mas/yr pmRA Proper motion along RA, pmRA*cosDE
54- 58 F5.3 mas/yr e_pmRA Proper motion along RA error
60- 66 F7.3 mas/yr pmDE Proper motion along DE
68- 72 F5.3 mas/yr e_pmDE Proper motion along DE error
74- 80 F7.2 km/s vlos Line-of-sight velocity
82- 86 F5.2 km/s e_vlos Line-of-sight velocity error
88- 94 I7 Msun MGC Mass
96-100 F5.2 pc rh Half-mass radius
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Cluster Cluster name
16- 18 A3 --- n_Cluster [(*)] Note (1)
20- 26 E7.3 --- tcross Crossing time (SQRT(rc3/G.MGC))
28- 34 E7.2 --- merr Median error in energy conservation
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Note (1): All "isolated" simulations have been run with a {DELTA}t=105yr, and
for a total of Nsteps=50000 steps, except for clusters marked
with (*), for which a {DELTA}t=104yr and a a total of
Nsteps=500000 steps have been used.
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Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Cluster Cluster name
15- 20 F6.2 kpc rmax Maximum radius
22- 26 F5.2 deg Angle Angle (arctan(zmax/Rmax))
28 A1 --- Class [DIO] Classification (1)
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Note (1): Classification as follows:
D = disk cluster
I = inner cluster
O = outer cluster
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 04-Aug-2023