J/A+A/610/A8 NGC3447/NGC3447A maps (Mazzei+, 2018)
Galaxy evolution in groups. NGC3447/NGC3447A: the odd couple in LGG 225.
Mazzei P., Marino A., Rampazzo R., Plana H., Rosado M., Arias L.
<Astron. Astrophys. 610, A8 (2018)>
=2018A&A...610A...8M 2018A&A...610A...8M (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Radial velocities ; Photometry, H-alpha
Keywords: galaxies: groups: individual: LGG 225 -
galaxies: individual: NGC 3447/NGC 3447A -
galaxies: interactions - galaxies: kinematics and dynamics -
galaxy: photometry - galaxies: evolution
Abstract:
Local Group (LG) Analogs (LGAs) are galaxy associations dominated by a
few bright spirals reminiscent of the LG. The NGC3447/NGC3447A
system is a member of the LGG 225 group, a nearby LGA. This system is
considered a physical pair composed of an intermediate-luminosity
late-type spiral, NGC3447 itself, and an irregular companion,
NGC3447A, linked by a faint, short filament of matter. A ring-like
structure in the NGC3447 outskirts has been emphasised by Galaxy
Evolution Explorer (GALEX) observations. This work aims to contribute
to the study of galaxy evolution in low-density environments, a
favourable habitat to highly effective encounters, shedding light on
the evolution of the NGC3447/NGC3447A system. We performed a
multi-λ analysis of the surface photometry of this system to
derive its spectral energy distribution and structural properties
using ultraviolet (UV), Swift UVOT, and optical Sloan Digital Sky
Survey (SDSS) images complemented with available far-IR observations.
We also characterised the velocity field of the pair using
two-dimensional Hα kinematical observations of the system
obtained with PUMA Fabry-Perot interferometer at the 2.1m telescope of
San Pedro Martir (Mexico). All these data are used to constrain
smooth particle hydrodynamic simulations with chemo-photometric
implementation to shed light on the evolution of this system. The
luminosity profiles, from UV to optical wavelengths, are all
consistent with the presence of a disc extending and including
NGC3447A. The overall velocity field does not emphasise any
significant rotation pattern, rather a small velocity gradient between
NGC3447 and NGC3447A. Our simulation, detached from a large grid
explored to best-fit the global properties of the system, suggests
that this arises from an encounter between two halos of equal mass.
Description:
Observations were carried out with the PUMA Fabry-Perot (FP,
hereafter) interferometer at the 2.1m telescope of the Observatorio
Astronomico Nacional at San Pedro Martir (OAN-SPM) Baja California,
Mexico, (PUMA@2.1-mSPM) on March 13, 2013. The PUMA instrument is
formed by a Queensgate ET50 etalon in the pupil of a focal reducer
with the Marconi2 2Kx2K CCD detector as receptor. Marconi has a
physical pixel size of 13um and a scale on the sky of 0.33"/pix. We
performed 4x4 spatial binning giving a pixel equivalent of 1.3" on the
sky.
Objects:
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RA (2000) DE Designation(s)
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10 53 23.98 +16 46 20.7 NGC3447/NGC3447A = NGC 3447
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 121 4 List of fits files
fits/* . 4 Individual fits files
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 22 I3 --- Nx Number of pixels along X-axis
24- 26 I3 --- Ny Number of pixels along Y-axis
28- 29 I2 --- Nz ? Number of slices
31- 37 F7.3 km/s bVel ? Lower value of velocity interval
for the datacube
39- 45 F7.2 km/s BVel ? Upper value of velocity interval
for the datacube
47- 52 F6.3 km/s dVel ? Velocity resolution for the datacube
54- 58 I5 Kibyte size Size of FITS file
60- 80 A21 --- FileName Name of FITS file, in subdirectory fits
82-121 A40 --- Title Title of the FITS file
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Acknowledgements:
Paola Mazzei, paola.mazzei(at)oapd.inaf.it
(End) Patricia Vannier [CDS] 24-Oct-2017