J/A+A/617/A113 GalMer S0 remnants morphological properties (Eliche-Moral+, 2018)
Formation of S0 galaxies through mergers. Morphological properties: tidal
relics, lenses, ovals, and other inner components.
Eliche-Moral M.C., Rodriguez-Perez C., Borlaff A., Querejeta M., Tapia T.
<Astron. Astrophys. 617, A113 (2018)>
=2018A&A...617A.113E 2018A&A...617A.113E (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, optical ; Galaxies, peculiar ; Models ;
Models, evolutionary ; Morphology
Keywords: galaxies: bulges - galaxies: elliptical and lenticular, cD -
galaxies: evolution - galaxies: formation - galaxies: interactions -
galaxies: structure
Abstract:
Major mergers are popularly considered too destructive to produce the
relaxed regular structures and the morphological inner components
(ICs) usually observed in lenticular (S0) galaxies. We have tested if
major mergers can produce remnants with realistic S0 morphologies. We
have selected a sample of relaxed discy remnants resulting from the
dissipative merger simulations of the GalMer database and derived
their morphological properties mimicking the typical conditions of
current observational data. Only ∼1-2Gyr after the full merger, we
find that: 1) many remnants (67 major and 29 minor events) present
relaxed structures and typical S0 or E/S0 morphologies, for a wide
variety of orbits and even in gas-poor cases. 2) Most of them do not
exhibit any morphological traces of their past merger origin under
typical observing conditions and at distances as nearby as 30Mpc. 3)
The merger relics are more persistent in minor mergers than in major
ones for similar relaxing time periods. 4) No major-merger S0-like
remnant develops a significant bar. 5) Nearly 58% of the major-merger
S0 remnants host visually detectable ICs, such as embedded inner
discs, rings, pseudo-rings, inner spirals, nuclear bars, and compact
sources, very frequent in real S0s too. 6) All remnants contain a lens
or oval, identically ubiquitous in local S0s. 7) These lenses and
ovals do not come from bar dilution in major-merger cases, but are
associated with stellar halos or embedded inner discs instead (thick
or thin). We conclude that the relaxed morphologies, lenses, ovals,
and other ICs of real S0s do not necessarily come from internal
secular evolution, gas infall, or environmental mechanisms, as
traditionally assumed, but they can result from major mergers as well.
Description:
Dynamical status properties, relevant orbital times, visual
morphological types, and visual morphological features of a set of
remnants resulting from the SPH galaxy merger simulations of the
GalMer database. The dynamical status is provided for the 287
pre-selected models producing apparently relaxed remnants hosting disc
components in the database (Table A.2). For 204 out of them, which are
fully merged and structurally relaxed, the relevant orbital times and
visual morphological types are listed in Table A.3. Table A.4
tabulates the morphological features visually identified in the mock
V-band photometric images of the 96 S0 and E/S0 remnants that are
dynamically relaxed. We have identified inner components (such as
ovals, lenses, inner discs, inner spirals, rings, pseudo-rings, and
nuclear bars), features in the main disc (large bars, warps, and outer
spiral relics), and tidal relics (as disc asymmetries, tidal debris,
tidal tails, plumes, shells, and collisional rings). Models with tidal
satellites are also indicated.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea2.dat 28 287 Dynamical status of the 287 pre-selected models
with apparently relaxed remnants hosting
disc components from GalMer
tablea3.dat 76 204 Orbital times and visual morphological types of
the 204 fully merged and structurally relaxed
remnants with discs from GalMer
tablea4.dat 103 96 Visual morphological features detected in mock
photometric images of the 96 dynamically relaxed
remnants of GalMer with S0 and E/S0 morphology
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- No Ordering number (1)
5- 14 A10 --- Model Model identifier in GalMer database
16 A1 --- Criter1 [Y/N] Whether the model obeys the first
criterion to be considered fully merged and
structurally relaxed commented in Sect. 3
18 A1 --- Criter2 [Y/N] Whether the model obeys the
second criterion
20 A1 --- Criter3 [Y/N] Whether the model obeys the
third criterion
22- 23 A2 --- MergStat Merging status on the basis of the three
criteria (2)
25- 28 A4 --- DynStat Dynamical status of the structurally relaxed
remnants (3)
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Note (1): The dynamical status is provided for the 287 pre-selected models from
the database with apparently relaxed final remnants and hosting disc
components in their projected density maps.
The three criteria differ for major and minor merger events (see Sect. 3
in the paper).
Note (2): Merging status as follows:
OM = on-going merger
NR = non- structurally relaxed
SR = structurally relaxed
Note (3): Dynamical status as follows:
DR = dynamically relaxed or virialised
N-DR = non-dynamically relaxed or virialised
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Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
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1- 3 I3 --- No Ordering number (1)
5- 14 A10 --- Model Model identifier in GalMer database
16- 19 A4 --- Type Visual morphological type
21- 26 F6.2 kpc D0 Initial distance between the mass centroids
of the progenitors
28- 31 F4.2 Gyr Tper1 Time of the 1st pericentre passage in orbit
33- 37 F5.2 kpc Dper1 Distance between the mass centroids of the
two progenitors in the 1st pericentre passage
39- 42 F4.2 Gyr Tper2 Time of the 2nd pericentre passage in orbit
44- 48 F5.2 kpc Dper2 Distance between the mass centroids of the
two progenitors in the 2nd pericentre passage
50- 53 F4.2 Gyr Tfull Time for the full merger of both galaxies
55- 59 F5.3 kpc Dfull Distance between mass centroids of the two
progenitors in full merger
61- 64 F4.2 Gyr Tfinal Total time computed in the model
66- 71 F6.4 kpc Dfinal Distance between the centroids of the two
progenitors in the final remnant
73- 76 F4.2 Gyr Trelax Total relaxation time experienced by the
remnant after full merger
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Note (1): The orbital times and visual morphological type of the 204 fully
merged and structurally relaxed remnants in the sample are provided.
Models gE0gSdo71 and gSagSdo74 are not dynamically relaxed finally.
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- No Ordering number (1)
4- 13 A10 --- Model Model identifier in GalMer database
15- 18 A4 --- Type Visual morphological type
21- 66 A46 --- Merger Morphological features visually detected in
the photometric images of the remnant
indicating past merger activity (2) (3)
68 A1 --- Bar [Y/N?] Whether the final remnant is barred or
not (2)
70-101 A32 --- Morph Relevant morphological features detected in
the photometric images of the remnant, not
necessarily linked to a merger origin (2) (4)
103 A1 --- TidSat [Y/N] Are there any tidal satellites? (2) (5)
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Note (1): The morphological features of the 96 S0 and E/S0 dynamically relaxed
remnants resulting from major and minor mergers are described.
Note (2): The morphological features have been visually detected using the mock
photometric images of the S0-like remnants in the V-band, assuming D=30Mpc
to the remnant, mulim=26mag/arcsec2 (for S/N=5), and FWHM=0.5".
Note (3): Codes as follows:
DA = disc asymmetry
TD = tidal debris
TT = tidal tail
Note (4): Codes as follows:
FL = flat lens
ID = inner disc
IID = inclined inner disc
IPR = inner pseudo-ring
IR = inner ring
LL = lentil-shaped lens
NB = nuclear bar
ISp = inner spiral
OR = outer ring
OSR = outer spiral relics
SL = spheroidal lens
Note (5): The satellites are identified within a FoV of 100x100kpc2 in the
face-on and edge-on views of the remnants.
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Acknowledgements:
M. Carmen Eliche-Moral, carmen.eliche(at)gmail.com
References:
Chilingarian et al., 2010A&A...518A..61C 2010A&A...518A..61C, The GalMer database:
galaxy mergers in the virtual observatory.
Borlaff et al., 2014A&A...570A.103B 2014A&A...570A.103B, Formation of S0 galaxies through
mergers. Antitruncated stellar discs resulting from major mergers.
Querejeta et al., 2015A&A...573A..78Q 2015A&A...573A..78Q, Formation of S0 galaxies through
mergers. Bulge-disc structural coupling resulting from major mergers.
Querejeta et al., 2015A&A...579L...2Q 2015A&A...579L...2Q, Formation of S0 galaxies through
mergers. Explaining angular momentum and concentration change from spirals
to S0s.
Tapia et al., 2017A&A...604A.105T 2017A&A...604A.105T, Formation of S0 galaxies through
mergers. Evolution in the Tully-Fisher relation since z ∼ 1.
Costantin et al., 2018A&A...609A.132C 2018A&A...609A.132C, The intrinsic shape of bulges in
the CALIFA survey.
Eliche-moral et al., 2006A&A...457...91E 2006A&A...457...91E, Growth of galactic bulges by
mergers. II. Low-density satellites.
Eliche-moral et al., 2011A&A...533A.104E 2011A&A...533A.104E, A minor merger origin for stellar
inner discs and rings in spiral galaxies.
Eliche-moral et al., 2012A&A...547A..48E 2012A&A...547A..48E, Evolution along the sequence of S0
Hubble types induced by dry minor mergers.
I. Global bulge-to-disk structural relations.
Eliche-moral et al., 2013A&A...552A..67E 2013A&A...552A..67E, Evolution along the sequence of S0
Hubble types induced by dry minor mergers.
II. Bulge-disk coupling in the photometric relations through
merger-induced internal secular evolution.
(End) M. Carmen Eliche-Moral [IAC], Patricia Vannier [CDS] 28-Jun-2018