J/A+A/675/A105 LeMMINGs V. Nuclear activity and bulge properties (Dullo+, 2023)
LeMMINGs. V. Nuclear activity and bulge properties: A detailed multi-component
decomposition of e-MERLIN Palomar galaxies with HST.
Dullo B.T., Knapen J.H., Beswick R.J., Baldi R.D., Williams D.R.A.,
McHardy I.M., Gallagher J.S., Aalto S., Argo M.K., Gil de Paz A.,
Klockner H.-R., Marcaide J.M., Mundell C.G., Mutie I.M., Saikia P.
<Astron. Astrophys. 675, A105 (2023)>
=2023A&A...675A.105D 2023A&A...675A.105D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Morphology ; Photometry ; Optical ; Radio sources
Keywords: galaxies: elliptical and lenticular, cD - galaxies: spiral -
galaxies: nuclei - galaxies: photometry - galaxies: structure -
radio continuum: galaxies
Abstract:
We use high-resolution HST imaging and e-MERLIN1.5-GHz observations of
galaxy cores from the LeMMINGs survey to investigate the relation
between optical structural properties and nuclear radio emission for a
large sample of galaxies. We perform accurate, multi-component
decompositions of new surface brightness profiles extracted from HST
images for 163 LeMMINGs galaxies and fit up to six galaxy components
(e.g., bulges, discs, AGN, bars, rings, spiral arms, and nuclear star
clusters) simultaneously with Sersic and/or core-Sersic models. By
adding such decomposition data for 10 LeMMINGs galaxies from our past
work, the final sample of 173 nearby galaxies (102 Ss, 42 S0s, 23 Es
plus 6 Irr) with bulge stellar mass (typically)
M*,bulge∼106-1012.5M☉ , encompasses all optical spectral
classes (LINERs, Seyferts, ALG and HII). We show that the bulge mass
can be significantly overestimated in many galaxies when components
such as bars, rings and spirals are not included in the fits. We
additionally implement a Monte Carlo method to determine errors on
bulge, disc and other fitted structural parameters. Moving (in the
opposite direction) across the Hubble sequence, i.e., from the
irregular to elliptical galaxies, we confirm that bulges become
larger, more prominent and round. Such bulge dominance is associated
with a brighter radio core luminosity. We also find that the radio
detection fraction increases with bulge mass. At
M*,bulge≥1011M☉, the radio detection fraction is 77%,
declining to 24% for M*,bulge<1010M☉. Furthermore, we
observe core-Sersic bulges tend to be systematically round and to
possess high radio core luminosities and boxy-distorted or pure
elliptical isophotes. However, there is no evidence for the previously
alleged strong tendency of galaxies' central structures (i.e., a
sharp Sersic/core-Sersic dichotomy) with their radio loudness,
isophote shape and flattening.
Description:
We present an accurate structural analysis of high-resolution
HST imaging for a representative subsample of 173 (23 Es, 43 S0s,
102 Ss and 6 Irrs) galaxies drawn from the full sample of 280 nearby
galaxies in the e-MERLIN legacy survey (LeMMINGs, Beswick et al.,
2014, in Proceedings of the 12th European VLBI Network Symposium and
Users Meeting (EVN 2014). 7-10 October 2014. Cagliari, 10). The aim is
to investigate the nuclear activity, optical and radio properties at
sub-arcsec resolution using HST and 1.5GHz e-MERLIN radio
observations. This work focuses on the results from our HST imaging
analyses, which is coupled in more detail with our 1.5GHz e-MERLIN
radio data in Dullo et al. (2023MNRAS.522.3412D 2023MNRAS.522.3412D). Using HST (ACS,
WFPC2, WFC3 and NICMOS) images, we have extracted new, 1Dmajor-axis
surface brightness, B4, P.A. and ellipticity profiles for a sample 163
LeMMINGs galaxies and these are combined with data for an additional
10 LeMMINGs galaxies from our previous work.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 15 163 Newly analysed LeMMINGs galaxies
tableb2.dat 165 557 Structural parameters for Sersic LeMMINGs
galaxies
tableb3.dat 200 517 Structural parameters for Sersic LeMMINGs
galaxies with a large-scale Gaussian component.
tableb4.dat 158 85 Structural parameters for core-Sersic LeMMINGs
galaxies
tableb5.dat 151 173 LeMMINGs data
tableb2-4.tex 134 2090 LaTeX version of tables B2-B4
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Gal Galaxy Name
7- 15 A9 --- Table Table/Figure (1)
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Note (1): indicates the table, which list the galaxy structural parameters for
our sample of 163 newly analysed LeMMINGs galaxies, and the associated figures
where the fits are shown.
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Byte-by-byte Description of file: tableb2.dat tableb3.dat tableb4.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Gal Galaxy name
6 A1 --- n_Gal [?] Note (2)
7-200 A194 --- Text Text (1)
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Note (1): Table A2:
Best-fitting model parameters for LeMMINGs galaxies from our
1D (major-axis) and 2D decompositions (see Figs.A2 and A6).
Unless labelled otherwise, we present 1D best-fitting parameters.
First line:
Galaxy name, the HST instrument and filter, the goodness of the fit,
the number and nature of the fitted components and the ground-based data
at large radii for galaxies with composite profiles, i.e., inner HST
plus outer ground-based data.
Bulgeless galaxies are indicated with (1)
Quality flag 1 indicates fits with good or higher quality levels whereas
those labeled 2 are questionable primarily as a result of the difficulty in
modelling highly inclined (i≳75deg) galaxies, see the text for further
detail.
Other lines:
For each 2D galaxy component, we present the best-fitting IMFIT ellipticity
(epsilon) and position angle (P.A.). The IMFIT 'boxy'/'discy' parameter c0
is shown for 2D fits that were performed using generalised ellipses
(Erwin, 2015ApJ...799..226E 2015ApJ...799..226E).
We do not show the errors on the best-fitting 2D parameters from IMFIT
as they are unrealistically low, see Erwin (2015ApJ...799..226E 2015ApJ...799..226E).
The fitted models (see Section 3.1) are:
Sersic Bulge (mue, Re [arcsec], Re [pc], n),
Sersic model for galaxy components other than the bulge
(mue, Re [arcsec], n),
exponential model (mudisc,0, h [arcsec])
2-parameter Gaussian function (muGauss,0, mGauss).
mudisc,0 and h are central surface brightness and scale length of the
large-scale exponential disc.
muGauss,0 and mGauss are central surface brightness and apparent
magnitude of nuclear components modelled with a 2-parameter Gaussian
function.
The surface brightnesses mu) are in units of mag/arcsec2,
where the magnitudes are given in the Vega magnitude system.
Unless specified otherwise, the errors associated with
mue, Re, n, mudisc,0, h, muGauss,0 and mGauss are
0.24, 15%, 15%, 0.28, 20%, 0.2 and 0.3, respectively.
Sources:
(a) Dullo et al. (2016MNRAS.462.3800D 2016MNRAS.462.3800D);
(b) Dullo & Graham (2014MNRAS.444.2700D 2014MNRAS.444.2700D);
(c) Dullo et al. (2018MNRAS.475.4670D 2018MNRAS.475.4670D).
Table A3:
Similar to Table A2 but here showing Sersic galaxies with a large-scale
Gaussian component (Figs. A3 and A6).
The fitted 3-parameter Gaussian ring model parameters (see Section 3.1) are
mur, sigma, Rr, where mur denotes the brightest value of the
Gaussian ring with a semi-major axis Rr and a full width at half
maximum of FWHM=2sqrt(2ln2)sigma.
The errors associated with the best-fitting parameters mur, sigma and
Rr are 0.28, 15% and 12%, respectively.
Note that our 2D decomposition for NGC 2859 contains a seventh component:
an inner Gaussian ring (mur∼21.89mag/arcsec2, sigma∼5.8arcsec,
Rr∼38.49arcsec).
Table A4:
As Table A2 but here for core-Sersic LeMMINGs galaxies (see Figs. A4 and
and A6).
The fitted core-Sersic model parameters (see Section 3.1) are
mub, Rb [arcsec], Rb [kpc], n, Re [arcsec], Re [kpc], gamma, and
alpha.
The errors associated with the best-fitting core-Sersic parameters are
0.15, 5%, 5%, 10%, 10%, 10% and 10%, respectively.
Note (2): A "?" shows that we tentatively classify the lenticular galaxies
NGC 1167 and NGC 3665 as core-S'ersic.
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Byte-by-byte Description of file: tableb5.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Gal Galaxy Name
7 A1 --- n_Gal [+] Note on Gal (1)
9- 22 A14 --- Type Morphological type, HyperLeda, from RC3
(de Vaucouleurs et al. 1991, Cat. VII/155)
24- 28 F5.1 Mpc Dist Distance from the NASA/IPAC Extragalactic
Database (NED) if no reference in r_Dist
29 A1 --- r_Dist [kb] Reference for Distance if not NED (2)
31- 37 A7 --- Class Optical spectral class from
Baldi et al. (2021MNRAS...500..4749B) (3)
40- 44 F5.1 km/s sigma ?=- Velocity dispersion (4)
46- 52 F7.3 mag VMAGbul1D ?=- Dust-corrected (1D) bulge absolute
magnitude (V-band) (5)
54- 57 F4.2 mag e_VMAGbul1D ? Dust-corrected (1D) bulge absolute
magnitude (V-band) error
58 A1 --- --- [/]
59- 64 F6.2 mag VMAGbul2D ? Dust-corrected (2D) bulge absolute
magnitude (V-band) (5)
68- 73 F6.2 mag VMAGnuc ?=- Dust-corrected absolute magnitude for
nuclei (V-band) (error = 0.35) (5)
75- 80 F6.2 mag VMAGgal ?=- Dust-corrected galaxy absolute magnitude
(V-band) (error = 0.34) (5)
82- 84 F3.1 --- M/L Mass-to-light ratio (error = 25%) (6)
86- 90 F5.2 [Msun] logM*bul ?=- log bulge stellar mass (7)
92- 95 F4.2 [Msun] e_logM*bul ?=- log bulge stellar mass error (7)
97-100 F4.1 [Msun] logM*nuc ?=- log stellar mass for nuclei
(error = 0.17) (7)
102-106 F5.2 [Msun] logM*gal ?=- log galaxy stellar mass
(error = 0.17) (7)
108-111 F4.2 [Msun] logMBH ?=- log supermassive black hole mass (8)
112-116 F5.2 [Msun] E_logMBH ?=- log supermassive black hole mass
upper error
117 A1 --- --- [-]
118-121 F4.2 [Msun] e_logMBH ?=- log supermassive black hole mass
lower error
123 A1 --- l_logLRcore Limit flag on logLRcore
124-127 F4.1 [10-7W] logLRcore log of 1.5GHz radio core luminosity from
Baldi et al. (2021MNRAS...500..4749B)
in erg/s (error = 1dex)
129-132 F4.2 --- ?=- Average ellipticity of the galaxy inside
the effective radius (Re) after omitting
the PSF-affected region (error = 20%) (9)
134-139 F6.3 --- Med(B4) ?=- Median of the isophote shape parameter
inside Re (error = 35%)
141-145 F5.2 --- gamma ?=- Negative, inner logarithmic slope of the
bulge light profile (error = 15%)
147-151 A5 --- Det Radio detection of the galaxies based on
Baldi et al. (2021MNRAS...500..4749B) (10)
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Note (1): Note on Gal as follows:
+ = bulgeless galaxies
Note (2): Distance reference as followsL
k = Karachentsev et al. (2004AJ..127....2031K, Cat. J/AJ/127/2031)
b = Bonanos et al. (2006ApJ..652....313B, Cat. J/ApJ/652/313)
Note (3): Optical spectral class as follows:
H II = H II galaxy
L = LINER
S = Seyfert
ALG = Absorption Line Galaxy.
RL = radio loud galaxies (Baldi et al. 2021MNRAS...508..2019B).
Note (4): Central velocity dispersion (sigma) from Ho et al.
(2009ApJS..183....1H 2009ApJS..183....1H).
Note (5): VMAGbulge, VMAGnuc and VMAGgal are V-band bulge, nucleus and galaxy
magnitudes calculated by integrating the best-fit Sersic, Gaussian or
core-Sersic functions and applying our colour transformation equations
listed in Table 4 (see Section 3.3).
Note (6): Stellar mass-to-light ratios (M/L) measured in the HST bands listed
in Tables A2--A4.
Note (7): we did not convert the V-band magnitudes into stellar masses, instead
the luminosities of the bulge, nucleus and the galaxy measured in the HST
bands (listed in Tables A2-A4) were converted into stellar masses (M*)
using our M/L values.
Note (8): logarithm of the SMBH mass (MBH) for galaxies with measured MBH from
van den Bosch (2016ApJ...831..134V 2016ApJ...831..134V, Cat. J/ApJ/831/134),
except for NGC 205 which is from Nguyen et al. (2019ApJ...872..104N 2019ApJ...872..104N).
The BH masses are adjusted here to our distance.
Note (9): average ellipticity of the bulge inside Re omitting PSF-affected
region .
Note (10): Radio detection as follows:
I = detected and core identified
unI? = detected but core unidentified
U = undetected
I+unI? = detected and core identified having additional unknown source(s)
in the FOV
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Acknowledgements:
Bililign T. Dullo, bdullo(at)ucm.es
References:
Baldi et al., Paper I 2018MNRAS.476.3478B 2018MNRAS.476.3478B
Baldi et al., Paper II 2021MNRAS.500.4749B 2021MNRAS.500.4749B
Baldi et al., Paper III 2021MNRAS.508.2019B 2021MNRAS.508.2019B
Williams et al., Paper IV 2022MNRAS.510.4909W 2022MNRAS.510.4909W
Dullo et al., Paper VI 2023MNRAS.522.3412D 2023MNRAS.522.3412D
(End) Patricia Vannier [CDS] 16-May-2023