J/MNRAS/505/4289 Chemical abundances of nearby galaxies (Perez-diaz+, 2021)
Chemical abundances in the nuclear region of nearby galaxies from the Palomar
Survey
Perez-Diaz B., Masegosa J., Marquez I., Perez-Montero E.
<Mon. Not. R. Astron. Soc., 505, 4289-4309 (2021)>
=2021MNRAS.505.4289P 2021MNRAS.505.4289P (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Galaxy catalogs ; Active gal. nuclei ;
Black holes ; Nebulae ; Spectroscopy ; Abundances ;
Infrared sources ; Optical ; Photometry ; Ultraviolet
Keywords: galaxies: abundances - galaxies: active - galaxies: ISM -
galaxies: nuclei
Abstract:
We estimate chemical abundances and ionization parameters in the
nuclear region of a sample of 143 galaxies from the Palomar
Spectroscopic Survey, composed by star-forming galaxies (87), Seyferts
2 (16), and LINERs (40) using the HII-CHI-MISTRY code. We also study
for each spectral type the correlation of the derived quantities with
other different properties of the host galaxies, such as morphology,
stellar mass, luminosity, and mass of their supermassive black holes.
The results obtained for star-forming galaxies are used to check the
soundness of our methodology. Then, we replicate a similar study for
our sample of AGN, distinguishing between Seyferts 2 and LINERs. We
report a saturation of Oxygen abundances for the nuclear regions of
SFG. The correlations between chemical abundances and their host
galaxy properties for SFG are in good agreement with previous studies.
We find that Seyferts 2 present slightly higher chemical abundances
but this result must be reexamined in larger samples of Seyfert
galaxies. In contrast, we obtain lower chemical abundances for LINERs
than for SFG. We confirm these relatively lower abundances for another
sample of infrared luminous LINERs in the same stellar mass range. Our
analysis of AGNs (both LINERs and Seyferts) shows that their host
galaxy properties are not correlated with our estimated chemical
abundances.
Description:
We compile our sample of 486 galaxies from those observed in the
Palomar Spectroscopic Survey (Ho et al. 1995ApJS...98..477H 1995ApJS...98..477H, Cat.
J/ApJS/98/477 ; Ho et al. 1997ApJS..112..315H 1997ApJS..112..315H, Cat.
J/ApJS/112/315). The Palomar Survey constitutes a magnitude-limited
spectroscopic optical survey of the nuclear emission for galaxies in
the local Universe (the median distance is 17.9 Mpc and the maximum
is 108.8 Mpc).
We take from Ho et al. (1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315)
all the nuclear spectroscopic data, and their corresponding emission
line fluxes once the stellar continuum is subtracted. Moreover, a
considerable amount of complementary data (Ho et al.
2009ApJS..183....1H 2009ApJS..183....1H, Cat. J/ApJS/183/1 ; Ho et al.
2003ApJ...583..159H 2003ApJ...583..159H) can be used to study chemical abundances of the
nuclear region in relation to the properties of their host galaxies.
Both star-formation and AGN activity lead to the presence of emission
lines which are key to estimate chemical abundances in the gas-phase
of nuclear regions of galaxies. The galaxies that do not show any
intrinsic emission once the stellar contribution is subtracted, are
omitted hence from the sample. The original sample of 486 galaxies is
then reduced to 418 (Ho et al. 1997ApJS..112..315H 1997ApJS..112..315H, Cat.
J/ApJS/112/315).
To get reliable chemical abundances and a good spectral classification
only emission lines with accurate measures can be used. We hence only
consider galaxies with relative errors up to 20 percent in the flux of
the emission lines Hα, Hβ, [O III]λ5007 Å,
[N II]λ6584 Å, and [S II]λλ6717,6731o Å. The
choice of these emission lines is based on they are needed to
spectroscopically classify the galaxies (see Section 2.2); and they
are used for the code HCM to estimate chemical abundances (see Section
2.4). Thus reducing our sample to 232 galaxies. Hereafter, this
classification allows our to omits composite galaxies which leads to a
sample of 185 galaxies: 107 SFG, 23 Seyferts 2, and 55 LINERs.
After reddening correction and chemical abundances determination, we
filtered our sample by using grids of models that have a step of
σ of chemical abundance ratio or ionization parameter. So any
galaxies whose uncertainty is greater than 3σ is omitted in this
study. Therefore, our final sample of galaxies amounts to 143
galaxies: 87 SFG, 16 Seyferts 2, and 40 LINERs.
Thus the tablec1.dat lists host galaxy properties used in the study
taken and calculated with above surveys. For its part, the tablec2.dat
contains nebular line ratios corrected from the reddening. As results
of HCM code and using tablec2.dat values, the tablec3.dat regroups
chemical abundances and ionization parameters for our 143 galaxies.
Further in the study, due to the lack of [O II] measurements of LINERs
galaxies in our sample, we perform an additional test. It's on the
chemical abundances in the nuclear region of LINERs by selecting
another sample of LINERs. We use the sample of luminous infrared
LINERs observed by Povic et al. (2016MNRAS.462.2878P 2016MNRAS.462.2878P,
Cat. J/MNRAS/462/2878). We do an analogous analysis on 25 LINERs
galaxies in order to compare it from our previous LINERs galaxies
sample. The results are presented in tablec4.dat.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablec1.dat 139 143 List of host galaxy properties used in the
study of the Palomar Survey
tablec2.dat 128 143 Emission line ratios for our sample of galaxies
corrected for reddening
tablec3.dat 145 143 *Chemical abundances and ionization parameters
for our sample of galaxies
tablec4.dat 76 25 Chemical abundances and ionization parameters
for sample of LINERs galaxies
--------------------------------------------------------------------------------
Note on tablec3.dat: Computed according to with photoionization models via
HCM code developed by Perez-Montero (2014MNRAS.441.2663P 2014MNRAS.441.2663P, 2019MNRAS.489.2652P 2019MNRAS.489.2652P),
which uses the code cloudy v17.01 (Ferland et al. 2017RMxAA..53..385F 2017RMxAA..53..385F) as
explained in the section 2.4 Chemical abundances determination.
--------------------------------------------------------------------------------
See also:
J/MNRAS/462/2878 : SFR & AGN in most luminous local universe LINERs
(Povic+, 2016)
J/ApJS/98/477 : Optical spectral atlas of Seyfert nuclei (Ho+ 1995)
J/ApJS/112/315 : Spectroscopic parameters of Seyfert nuclei (Ho+ 1997)
J/ApJS/183/1 : Catalog of central stellar velocity dispersions (Ho+, 2009)
Byte-by-byte Description of file: tablec1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Galaxy name (Name) (1)
10- 12 A3 --- MType Hubble morphological type (Type) (1)
14- 16 A3 --- f_MType [AMB] Ambiguous galaxies (f_MType) (2)
18- 22 F5.2 --- T Numerical Hubble type index (T) (1)
24- 30 F7.3 deg RAdeg Right Ascension (J2000) from SIMBAD (RAdeg)
32- 39 F8.4 deg DEdeg Declination (J2000) from SIMBAD (DEdeg)
41- 44 F4.1 Mpc D Distance (d) (1)
46- 63 F18.13 pc R Radius observed (Radius) (3)
65- 69 F5.1 km/s sigma Stellar velocity dispersion in the galactic
centres (sigma*) (4)
71- 78 F8.5 [Msun] log(MSMBH) ? Logarithm of the mass of the
supermassive black hole (5)
80- 83 F4.2 mag Ag ? Galactic extinction (Ag) (6)
85- 89 F5.2 mag Bmag Total asymptotic apparent B magnitude (mB)
(1)
91- 98 F8.4 mag BMAG Absolute B-magnitude corrected for
galactic extinction (M0B)
100-105 F6.3 mag W1mag ? WISE W1 at 3.4um band apparent
magnitude (w1) (7)
107-112 F6.3 mag W2mag ? WISE W2 at 4.6um band apparent
magnitude (w2) (7)
114-121 F8.4 mag W1Mag ? WISE W1 at 3.4um band absolute
magnitude (W1) (7)
123-130 F8.4 mag W2Mag ? WISE W2 at 4.6um band absolute
magnitude (W2) (7)
132-139 F8.5 [Msun] logM* ? Stellar mass (logM*) (8)
-------------------------------------------------------------------------------
Note (1): Taken from Ho et al. (1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315).
Note (2): Furthermore, the Kewley's criteria allow us to distinguish
among SFG, Seyferts 2, LINERs, and composite galaxies. However,
it also contemplates the possibility that some galaxies may fall
in different regions from one diagram to another. These galaxies
are called ambiguous galaxies (Kewley et al. 2006MNRAS.372..961K 2006MNRAS.372..961K).
Note (3): Radius observed with the Double Spectrograph mounted on the Hale
5 m telescope, using an effective aperture of 2 * 4 arcsec2
(Ho et al. 1995ApJS...98..477H 1995ApJS...98..477H, Cat. J/ApJS/98/477).
Note (4): Adopted velocity dispersion taken from Ho et al. (2009ApJS..183....1H 2009ApJS..183....1H,
Cat. J/ApJS/183/1).
Note (5): To estimate the mass of the supermassive black hole, we use the
empirical relation given by McConnell & Ma (2013ApJ...764..184M 2013ApJ...764..184M) which
relates MSMBH and the stellar velocity dispersion σ* in the
galactic centre (within the effective radius of the galaxy) such as
the equation 4 in section 4.4 shows.
We also omit the LINER NGC 185 that has a low-massive black hole
(M_SMBH ∼ 102.7 M☉) due to its low stellar velocity dispersion
σ* ~= 19.9 km/s. This low stellar velocity dispersion
might be explained because this dwarf elliptical galaxy
presents several bright knots that may be identified as its nucleus
(Lira et al. 2007MNRAS.382.1552L 2007MNRAS.382.1552L, Cat. J/MNRAS/382/1552).
Note (6): Reddening correction obtained via the procedure explained in
section 2.3.
Note (7): Data are available in the INFRARED SCIENCE ARCHIVE
(IRSA: https://irsa.ipac.caltech.edu/frontpage/).
Note (8): Stellar mass derived with the equation 3 section 4.3 Stellar mass
using the absolute magnitude W1 and W2.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Galaxy name (Name) (1)
10- 12 A3 --- MType Hubble morphological type (Type) (1)
14- 16 A3 --- f_MType [AMB] Ambiguous galaxies (f_MType) (2)
18- 26 F9.5 deg RAdeg Right Ascension (J2000) from SIMBAD (RAdeg)
28- 36 F9.5 deg DEdeg Declination (J2000) from SIMBAD (DEdeg)
38- 45 F8.6 --- cHb Reddening or extinction coefficient described
in the section 2.3 (cHb)
47- 54 F8.6 --- e_cHb Mean error of cHb (e_cHb)
56- 63 F8.6 --- [OIII]4363 ? Doubly ionized O III line-intensity ratio
at 436.3 nm ([OIII]4363Å) (3)
65- 72 F8.6 --- e_[OIII]4363 ? Mean error of [OIII]4363 (e_[OIII]4363A)
74- 82 F9.6 --- [OIII]5007 Doubly ionized O III line-intensity ratio
at 500.7 nm ([OIII]5007Å) (3)
84- 91 F8.6 --- e_[OIII]5007 Mean error of [OIII]5007 (e_[OIII]5007)
93-101 F9.6 --- [NII]6584 Simply ionized N II line-intensity ratio
at 658.4 nm ([NII]6584Å) (3)
103-110 F8.6 --- e_[NII]6584 Mean error of [NII]6584 (e_[NII]6584)
112-119 F8.6 --- [SII] Simply ionized S II lines sum at 671.7 nm
and 673.1 nm ([SII]6717,6731Å) (3)
121-128 F8.6 --- e_[SII] Mean error of [SII] (e_[SII])
-------------------------------------------------------------------------------
Note (1): Taken from Ho et al. (1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315).
Note (2): Furthermore, the Kewley's criteria allow us to distinguish
among SFG, Seyferts 2, LINERs, and composite galaxies. However,
it also contemplates the possibility that some galaxies may fall
in different regions from one diagram to another. These galaxies
are called ambiguous galaxies (Kewley et al. 2006MNRAS.372..961K 2006MNRAS.372..961K).
Note (3): [N II], [S II], [O III] are so-called forbidden lines commonly
observed in astrophysical gases.
Emission line ratio Iλ/IHβ corrected from the reddening
as the equation 2 shows in section 2.3.
Taken from Ho et al. (1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315),
before reddening correction.
Moreover, we denote the lack of measurements for the auroral line
[O III] at 436.3 nm (only measured in 5 galaxies of the sample).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Galaxy name (Name) (1)
10- 12 A3 --- MType Hubble morphological type (Type) (1)
14- 16 A3 --- f_MType [AMB] Ambiguous galaxies (f_MType) (2)
18- 26 F9.5 deg RAdeg Right Ascension (J2000) from SIMBAD (RAdeg)
28- 36 F9.5 deg DEdeg Declination (J2000) from SIMBAD (DEdeg)
38- 54 F17.15 [-] 12+log(O/H) Logarithm of oxygen abundance 12+log(O/H)
(12+logO/H)
56- 72 F17.15 [-] e_12+log(O/H) Mean error of 12+log(O/H) (e_12+logO/H)
74- 91 F18.15 [-] log(N/O) Logarithm of nitrogen-to-oxygen abundance
ratio (logN/O)
93-109 F17.15 [-] e_log(N/O) Mean error of log(N/O) (e_logN/O)
111-127 F17.14 [-] logU Logarithm of the ionization parameter U (logU)
129-145 F17.15 [-] e_logU Mean error of logU (e_logU)
--------------------------------------------------------------------------------
Note (1): Taken from Ho et al. (1997ApJS..112..315H 1997ApJS..112..315H, Cat. J/ApJS/112/315).
Note (2): Furthermore, the Kewley's criteria allow us to distinguish
among SFG, Seyferts 2, LINERs, and composite galaxies. However,
it also contemplates the possibility that some galaxies may fall
in different regions from one diagram to another. These galaxies
are called ambiguous galaxies (Kewley et al. 2006MNRAS.372..961K 2006MNRAS.372..961K).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- Name LINER Galaxy name (1)
5- 20 F16.11 pc R ? Radius observed (Radius) (2)
22- 29 F8.4 mag BMAG ? Absolute B-magnitude corrected for
galactic extinction (M0B)
31- 38 F8.5 [Msun] logM* Stellar mass logM* (3)
40- 44 F5.3 --- 12+log(O/H) Logarithm of oxygen abundance 12+log(O/H)
(12+logO/H) (4)
46- 50 F5.3 --- e_12+log(O/H) Mean error of 12+log(O/H) (e_12+logO/H)
52- 57 F6.3 --- log(N/O) Logarithm of nitrogen-to-oxygen abundance
ratio (logN/O) (4)
59- 63 F5.3 --- e_log(N/O) Mean error of log(N/O) (e_logN/O)
65- 70 F6.3 --- logU Logarithm of the ionization parameter U
(logU) (4)
72- 76 F5.3 --- e_logU Mean error of logU (e_logU)
--------------------------------------------------------------------------------
Note (1): LINERs galaxies taken from Povic et al. (2016MNRAS.462.2878P 2016MNRAS.462.2878P,
Cat. J/MNRAS/462/2878).
Note (2): Radius observed by Povic et al. (2016MNRAS.462.2878P 2016MNRAS.462.2878P,
Cat. J/MNRAS/462/2878). The median radius of the region observed
is ∼ 1839.9 pc, larger than the median region r ∼ 82.4 pc observed
in the tablec1.dat.
Note (3): Stellar mass derived with the equation 3 section 4.3 Stellar mass
using the absolute magnitude W1 and W2.
Note (4): Computed according to with photoionization models via
HCM code developed by Perez-Montero (2014MNRAS.441.2663P 2014MNRAS.441.2663P,
2019MNRAS.489.2652P 2019MNRAS.489.2652P), which uses the code cloudy v17.01
(Ferland et al. 2017RMxAA..53..385F 2017RMxAA..53..385F) as explained in the section 2.4
Chemical abundances determination.
-------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 04-Jun-2024