J/A+A/699/A300 Informations on VMC survey LII (Cioni+, 2025)
The VMC survey. LII. Data release #7.
Complete survey data and data from additional programmes.
Cioni M.-R.L., Cross N.J.G., Ripepi V., Girardi L., de Grijs R.,
Clementini G., van Loon J.T., Groenewegen M., Ivanov V.D., Oliveira J.M.,
Marconi M., Bekki K., Blake R.P., Holliman M.J., Irwin J., Irwin M.J.,
Mann R.G., Read M., Sutorius E., Craig J.E.M., Cusano F., Dresbach F.,
Maitra C., Molinaro R., Niederhofer F., Omkumar A.O., Pennock C.M.,
Sicignano T., Subramanian S., Tatton B.L., Vijayasree S., Zaggia S.
<Astron. Astrophys. 699, A300 (2025)>
=2025A&A...699A.300C 2025A&A...699A.300C (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Magellanic Clouds ; Infrared sources
Keywords: surveys - Magellanic Clouds - infrared: Stars
Abstract:
The near-infrared YJKs Visual and Infrared Survey Telescope for
Astronomy (VISTA) survey of the Magellanic Clouds (VMC) is complete,
along with data from additional programmes contributing to the
enhancement of its quality over the original footprints. This work
presents the final data release of the VMC survey, which includes
additional observations and provides an overview of the scientific
results. The overall data quality has been revised and reprocessed
standard data products that have previously appeared in earlier data
releases are made available together with new data products. These
include the individual stellar proper motions, reddening towards red
clump stars, and source classifications. Several data products, such
as the parameters of some variable stars and of background galaxies,
from the VMC publications have been associated with a data release for
the first time. The data were processed using the VISTA Data Flow
System and additional products (e.g. catalogues with
point-spread-function photometry and tables with stellar proper
motions) were obtained with software developed by the survey team.
This release supersedes all previous data releases of the VMC survey
for the combined (deep-stacked) data products, whilst providing
additional (complementary) images and catalogues of single
observations per filter. Overall, it includes about 64 million
detections, split nearly evenly between sources with stellar or galaxy
profiles. The VMC survey provides a homogeneous data set resulting
from deep and multi-epoch YJKs-band imaging observations of the Large
and Small Clouds, the Bridge, and two fields in the Stream. The VMC
data represent a valuable counterpart for sources detected at other
wavelengths for both stars and background galaxies.
Description:
Table B.1 provides information about the VISTA tile images that were
obtained outside the VMC sky-quality criteria, including those with
significant (0.1mag or larger) zero-point variations across the tile.
Each line refers to a single tile observation and indicates: the tile,
the date of observation, the filter, and the type (deep or shallow),
which refers to the exposure time of the individual pawprints. Then it
shows the FWHM, ellipticity, zero-point and airmass, as well as the
reason(s) of the low-quality, namely which attribute(s) were violated
with respect to the requirements e.g. FWHM, ellipticity, transparency
or airmass. The phrasing 'zero-point' refers to observations for which
the zero-point variation among the six pawprints that make up a tile
is at least 0.1mag, whereas `exposure time' indicates that
observations were acquired with DIT=1s rather than 5s as for all
others tiles in the Ks band. An asterisk next to a value of FWHM or
ellipticity indicates that the value corresponding to the worst
pawprint is listed instead of the one provided by CASU for the
combined tile. This is because the latter (without a dispersion
associated with it) may not reflect the poor quality of the data. For
observations of tiles with a pointing different from that of the other
observations of the same tile a double asterisk is placed next to the
entry for the low-quality reason.
Table B.2 reports the same information as in Table B.1 for the
additional programmes, where the corresponding ESO programme
identification is also listed. Table B.3 reports the same quantities
for single pawprints from both the VMC and the additional programmes,
which could not result into complete tiles.
The format of Table B.3 is the same as that of Table B.2. We note that
the wording '<5 images' indicates pawprints with an incomplete number
of dithering offsets.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 91 497 Low quality VMC tile images
tableb2.dat 114 63 Low quality tile images from additional programmes
tableb3.dat 114 255 Low quality pawprints
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See also:
II/351 : VISTA Magellanic Survey (VMC) catalog (Cioni+, 2011)
Byte-by-byte Description of file: tableb1.dat tableb2.dat tableb3.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Tile Name of tile within the VMC survey
10- 19 A10 "date" Date Date of observation
22- 23 A2 --- Filter Y, J or Ks band filter
26- 32 A7 --- Type deep or shallow observation
35- 38 F4.2 arcsec FWHM FWHM
39 A1 --- n_FWHM [*] Note on FWHM (1)
42- 45 F4.2 --- Ell source ellipticity
46 A1 --- n_Ell [*] Note on Ell (1)
48- 52 F5.2 mag ZP Zero Point
54 A1 --- --- [(] open parenthesis
55- 58 F4.2 mag sigma sigma of Zero Point
59 A1 --- --- [)] closed parenthesis
62- 66 F5.3 --- Airmass Airmass of observations
69-102 A34 --- Reason Reson(s) for low-quality classifications
104-114 A11 --- Program ESO programme ID of observation
(for tables B2 and B3 only)
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Note (1): Note as follows:
* = value corresponding to the worst pawprint is listed instead of the one
provided by CASU for the combined tile
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Acknowledgements:
Maria-Rosa L. Cioni, mcioni(at)aip.de
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(End) Patricia Vannier [CDS] 08-Jul-2025