J/A+A/663/A107 VMC survey XLV. (Schmidt+, 2022)
The VMC survey. XLV. Proper motion of the outer LMC and the impact of the SMC.
Schmidt T., Cioni M.-R., Niederhofer F., Bekki K., Bell C.P.M., de Grijs R.,
El Youssoufi D., Ivanov V., Oliveira, J.M., Ripepi V., van Loon J.T.
<Astron. Astrophys. 663, A107 (2022)>
=2022A&A...663A.107S 2022A&A...663A.107S (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Associations, stellar ; Proper motions ;
Optical
Keywords: Galaxy: kinematics and dynamics - Magellanic Clouds -
galaxies: interactions - proper motions - surveys
Abstract:
The Large Magellanic Cloud (LMC) is the most luminous satellite galaxy
of the Milky Way and, owing to its companion, the Small Magellanic
Cloud (SMC), represents an excellent laboratory to study the
interaction of dwarf galaxies.
The aim of this study is to investigate the kinematics of the outer
regions of the LMC by using stellar proper motions to understand the
impact of interactions, e.g. with the SMC about 250Myr ago.
We calculate proper motions using multi-epoch Ks-band images from the
VISTA survey of the Magellanic Clouds system. Observations span a time
baseline of 2-5yr. We combine the VMC data with data from the Gaia
early Data Release 3 and introduce a new method to distinguish between
Magellanic and Milky Way stars based on a machine learning algorithm.
This new technique enables a larger and cleaner sample selection of
fainter sources as it reaches below the red clump of the LMC.
We investigate the impact of the SMC on the rotational field of the
LMC and find hints of stripped SMC debris. The south-eastern region of
the LMC shows a slow rotational speed compared to the overall
rotation.
N-body simulations suggest that this could be caused by a fraction of
stripped SMC stars located in that particular region that move
opposite to the expected rotation.
Description:
Tables 5-8 in their entirety for all 257 bins.
Columns (from left to right) refer to the bin number as created by the
Voronoi routine, right ascension and declination of the bin centre,
angular distance of the bin from the LMC centre, number of stars
within each bin, their average proper motion in right ascension and
declination, and rotational velocity with respect to the LMC centre.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 69 258 Gaia EDR3 proper motion of LMC stars
table6.dat 69 258 Gaia EDR3 proper motion of old stars
table7.dat 69 258 Gaia EDR3 proper motion of young stars
table8.dat 69 258 VMC proper motion of LMC stars
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See also:
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
Byte-by-byte Description of file: table5.dat table6.dat table7.dat table8.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Bin Bin number as created by the Voronoi routine
5- 13 F9.6 deg RAdeg Right ascension (ICRS) at Ep=2016.0
of the bin centre (Gaia EDR3)
15- 24 F10.6 deg DEdeg Declination (ICRS) at Ep=2016.0
of the bin centre (Gaia EDR3)
26- 29 F4.2 deg d Angular distance from the LMC centre
31- 35 I5 --- N Number of sources
37- 40 F4.2 mas/yr pmRA Proper motion in Right ascension
42- 45 F4.2 mas/yr e_pmRA Proper motion error in Right ascension
47- 51 F5.2 mas/yr pmDE Proper motion in Declination
53- 56 F4.2 mas/yr e_pmDE Proper motion error in Declination
58- 63 F6.2 km/s VR Rotational velocity with respect to LMC centre
65- 69 F5.2 km/s e_VR Rotational velocity error
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Acknowledgements:
Thomas Schmidt, tschmidt(at)aip.de
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(End) Patricia Vannier [CDS] 31-May-2022