J/A+A/573/A59 Gas kinematics in CALIFA survey (Garcia-Lorenzo+, 2015)
Ionized gas kinematics of galaxies in the CALIFA survey.
I. Velocity fields, kinematic parameters of the dominant component, and
presence of kinematically distinct gaseous systems.
Garcia-Lorenzo B., Marquez I., Barrera-Ballesteros J.K., Masegosa J.,
Husemann B., Falcon-Barroso J., Lyubenova M., Sanchez S.F., Walcher J.,
Mast D., Garcia-Benito R., Mendez-Abreu J., Van De Ven G., Spekkens K.,
Holmes L., Monreal-Ibero A., Del Olmo A., Ziegler B., Bland-Hawthorn J.,
Sanchez-Blazquez P., Iglesias-Paramo J., Aguerri J.A.L., Papaderos P.,
Gomes J.M., Marino R.A., Gonzalez Delgado R.M., Cortijo-Ferrero C.,
Lopez-Sanchez A.R., Bekeraite S., Wisotzki L., Bomans D., (the Califa team)
<Astron. Astrophys., 573, A59-59 (2015)>
=2015A&A...573A..59G 2015A&A...573A..59G
ADC_Keywords: Surveys ; Galaxy catalogs ; Morphology
Keywords: galaxies: evolution - galaxies: kinematics and dynamics -
galaxies: star formation - galaxies: spiral -
techniques: spectroscopic - galaxies: elliptical and lenticular, cD
Abstract:
Ionized gas kinematics provide important clues to the dynamical
structure of galaxies and hold constraints to the processes driving
their evolution.
The motivation of this work is to provide an overall characterization
of the kinematic behavior of the ionized gas of the galaxies included
in the Calar Alto Legacy Integral field Area (CALIFA), offering
kinematic clues to potential users of the CALIFA survey for including
kinematical criteria in their selection of targets for specific
studies. From the first 200 galaxies observed by CALIFA survey in its
two configurations, we present the two-dimensional kinematic view of
the 177 galaxies satisfaying a gas content/detection threshold.
After removing the stellar contribution, we used the cross-correlation
technique to obtain the radial velocity of the dominant gaseous
component for each spectrum in the CALIFA data cubes for different
emission lines (namely, [OII] λλ3726,3729, [OIII]
λλ4959,5007, Hα+[NII] λλ6548,6584,
and [SII]λλ6716,6730). The main kinematic parameters
measured on the plane of the sky were directly derived from the radial
velocities with no assumptions on the internal prevailing motions.
Evidence of the presence of several gaseous components with different
kinematics were detected by using [OIII] λλ4959,5007
emission line profiles.
Description:
The galaxies presented in this work are included in the CALIFA survey
mother sample (Sanchez et al., 2012A&A...538A...8S 2012A&A...538A...8S), that comprises
939 galaxies selected from the SDSS DR7 (Abazajian et al.,
2009ApJS..182..543A 2009ApJS..182..543A).
Observations were carried out using the PMAS fiber Package (PPak)
of the Potsdam Multi-Aperture Spectrophotometer (PMAS) at the 3.5m
telescope of the Calar Alto Observatory (Almeria, Spain).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 89 177 Morphological parameters of the sample of CALIFA
galaxies analized in this work
tablea2.dat 71 177 *Kinematic parameters estimated directly from
the radial velocity derived for each spectra of
the CALIFA data cubes
tablea3.dat 78 177 *Types and classes of asymmetries detected from
the [OIII] emission line profiles
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Note on tablea2.dat: with a S/N>6 (in both the stellar and ionized gas
components) through the application of the cross-correlation technique in the
Hα+[NII] spectral range.
Note on tablea3.dat: and systemic velocity derived from different emission lines
([OII],[OIII], Hα+[NII] and [SII].
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See also:
J/A+A/559/A114 : Updated O3N2 and N2 abundance indicators (Marino+, 2013)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Galaxy name
16- 18 I3 --- CAL [1/939] CALIFA unique ID number for the galaxy
20- 23 I4 km/s Vsys Systemic velocity from NED
25- 27 I3 deg PA [0/180]?=- Position angle of the apparent
major axis from NED
29- 30 I2 arcsec reff [5/43]?=- Effective radius of the disk estimated
as detailed in Sanchez et al. 2014A&A...563A..49S 2014A&A...563A..49S
32- 34 F3.1 --- rout [1/8]?=- Radial distance (in units of the
effective radii) used to estimate the large-scale
photometric position angles and ellipticities
36- 40 F5.1 deg PA1 [0/180]?=- Morphological position angle at one
effective radius (1)
42- 45 F4.1 deg e_PA1 ? rms uncertainty on PA1
47- 51 F5.1 deg PAout [0/180]?=- Morphological position angle at the
largest scale of the SDSS images (1)
53- 56 F4.1 deg e_PAout ? rms uncertainty on PAout
58- 61 F4.2 --- ell [0/1]?=- Ellipticity ε of the outer
isophotes of the SDSS r-band image obtained
using the IRAF task ellipse
63- 66 F4.2 --- e_ell ? rms uncertainty on Ell
68- 72 A5 --- Stage [IoM G] Galaxy situation (2)
75- 78 A4 --- MType Morphological type from visual classification
performed by the CALIFA collaboration (3)
81- 82 A2 --- Bar [AB ] Bar strength of the galaxy; B=barred (4)
85- 89 A5 --- Nuc Nuclear type of the object (5)
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Note (1): Both measurements were inferred from the SDSS r-band image of the
galaxy using the IRAF task ellipse.
Note (2): Classes are (see Sect. 2.3):
I G = Isolated Galaxies
IoM G = interacting/merging galaxies (includes mergers with tidal features)
GoG = group of galaxies (includs pair and small groups)
Note (3): See Husemann et al. (2013A&A...549A..87H 2013A&A...549A..87H) and Walcher et al.
(in prep.), for details.
Note (4): as an additional outcome of the CALIFA visual classification (see
Husemann et al. (2013A&A...549A..87H 2013A&A...549A..87H) and Walcher at al. (in prep.), for
details). We divided the galaxies into non-barred (A), weakly barred (AB)
and strongly barred (B).
Note (5): Nuclear type of the object indicating the main ionization mechanisms
in the central region determined through diagnostic diagrams (see Sect. 2.3):
SF = pure star formation
AGN = Active galaxy nucleus
LINER = low-ionization nuclear emission-line region
INDEF = nuclear type could not be inferred
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- CAL [1/939] CALIFA identification number of galaxy
5- 7 A3 --- Grad Classification from the velocity gradient (6)
9- 12 F4.1 arcsec oRAkc ? Position of the kinematic center right
ascension relative to the central spaxel
of the CALIFA data cube (7)
14- 16 F3.1 arcsec e_oRAkc ? rms uncertainty on oRAkc
18- 21 F4.1 arcsec oDEkc ? Position of the kinematic center declination
relative to the central spaxel of the
CALIFA data cube (7)
23- 25 F3.1 arcsec e_oDEkc ? rms uncertainty on oDEkc
27- 32 F6.1 km/s Vkc ?=- Average velocity in an aperture of 3.7"
in radius centered at the location of
the kinematic center
34- 38 F5.1 km/s e_Vkc ? Standard deviation of average radial velocity
40- 44 F5.1 deg PArec [0/393]? Position angle PAkin,re of the major
kinematic pseudo-axis estimated from the
receding sides of the velocity field (8)
46- 49 F4.1 deg e_PArec ? Standard deviation of the polar coordinates
of the spaxels tracing these axes
(see Sect. 3.2.3)
51- 55 F5.1 deg PAapp [-2/361]? Position angle PAkin,app of the
major kinematic pseudo-axis estimated from the
approaching sides of the velocity field (8)
57- 60 F4.1 deg e_PAapp ? Standard deviation of the polar coordinates
of the spaxels tracing these axes
(see Sect. 3.2.3)
62- 66 F5.1 deg PAmin ? Position angle of the minor kinematic
pseudo-axis
68- 71 F4.1 deg e_PAmin [0/180]? Standard deviation of the polar
coordinates tracing these axes (see Sect. 3.2.3)
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Note (6): Classification of the galaxy according to the structures in the
velocity gradient map obtained from the Hα+[NII] velocity field
(see Sect. 4.1.2):
SGP = Single velocity Gradient Peak
MGP = Multiple velocity Gradient Peak
UGP = Unclear velocity Gradient Peak
Note (7): see Table 4 in Husemann et al. (2013A&A...549A..87H 2013A&A...549A..87H) for keyword
(see Sect. 3.2.2).
Note (8): and taking the reference position at the kinematic center.
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Galaxy name
16- 19 I4 km/s V[OII] ?=- Systemic velocity derived from [OII]
emission line
21- 23 I3 km/s e_V[OII] ? rms uncertainty on V[OII]
25- 28 I4 km/s V[OIII] ?=- Systemic velocity derived from [OIII]
emission line
30- 32 I3 km/s e_V[OIII] ? rms uncertainty on V[OIII]
34- 37 I4 km/s VHa+ ?=- Systemic velocity derived from
Hα+[NII] emission line
39- 41 I3 km/s e_VHa+ ? rms uncertainty on VHa+
43- 46 I4 km/s V[SII] ?=- Systemic velocity derived from [SII]
emission line
48- 50 I3 km/s e_V[SII] ? rms uncertainty on Vsys[SII]
52- 59 A8 --- AclA Asymmetries Class A (A0 A1 A2) (9)
62- 69 A8 --- AclB Asymmetries Class B (B0 B1 B2) (9)
71- 78 A8 --- AclC Asymmetries Class C (C0 C1 C2) (9)
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Note (9): We classified the detected asymmetries into three categories according
to the number of bisector levels at which the profiles appear asymmetric:
Class A = |ΔVb|>FΔVb(S/N) in >5 bisector levels.
In general, class A profiles correspond to asymmetries first
detected over a 30% of the peak intensity level.
Class B = |ΔVb|>FΔVb(S/N) 3 to 5 bisector levels.
Frequently, class B profiles correspond to asymmetries first
detected at intensity levels between 20% and 30% of the
intensity peak.
Class C = |ΔVb|>FΔVb(S/N) only in two bisector levels.
Commonly, class C corresponds to profiles with asymmetries
in the 10% and 15% bisector levels.
FΔVb(S/N) = A(l) + B(l).(S/N),
significance of the asymmetry level approximated linearly
in signal-to-noise (S/N) (see Appendix B1)
Moreover, we can classify the detected asymmetries according to the maximum
deviation of the bisector from a Gaussian (ΔVb):
Type 0: max(|ΔVb|) - FΔVb(S/N) ≤ FΔVb(S/N)
Type 1: FΔVb(S/N) < max(|ΔVb|)-FΔVb(S/N)
≤ 2.FΔVb(S/N)
Type 2: max(|ΔVb|) - FΔVb(S/N) > 2.FΔVb(S/N)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 10-Feb-2015