J/AJ/152/73 Stellar nuclei and bulges of nearby S0 galaxies (Sil'chenko, 2016)
Stellar nuclei and inner polar disks in lenticular galaxies.
Sil'chenko O.K.
<Astron. J., 152, 73 (2016)>
=2016AJ....152...73S 2016AJ....152...73S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Spectroscopy
Keywords: galaxies: elliptical and lenticular, cD - galaxies: ISM -
galaxies: kinematics and dynamics - galaxies: stellar content
Abstract:
I analyze statistics of the stellar population properties for stellar
nuclei and bulges of nearby lenticular galaxies in different
environments by using panoramic spectral data of the integral-field
spectrograph SAURON retrieved from the open archive of the Isaac
Newton Group. I also estimate the fraction of nearby lenticular
galaxies having inner polar gaseous disks by exploring the
volume-limited sample of early-type galaxies of the ATLAS-3D survey.
By inspecting the two-dimensional velocity fields of the stellar and
gaseous components with the running tilted-ring technique, I have
found seven new cases of inner polar disks. Together with those, the
frequency of inner polar disks in nearby S0 galaxies reaches 10%,
which is much higher than the frequency of large-scale polar rings.
Interestingly, the properties of the nuclear stellar populations in
the inner polar ring hosts are statistically the same as those in the
whole S0 sample, implying similar histories of multiple gas-accretion
events from various directions.
Description:
The integral-field spectrograph Spectrographic Areal Unit for Research
on Optical Nebulae (SAURON) was operating at the 4.2m William Herschel
Telescope belonging to the ING of telescopes on La Palma. It worked in
"TIGER mode", giving about 1500 spectra simultaneously, each for a
0.94''*0.94'' square element ("spaxel") from a (central) part of a
galaxy. A total set of spectra covers an area of 41''*33''. The
spectral range of the unit is rather narrow, 4800-5350Å, and its
spectral resolution has been fixed since 2007 at about 4.3Å.
There were two surveys of nearby early-type galaxies with SAURON. The
first one, which started in 1999 and finished in 2004, involved 72
galaxies, among those 48 early-type ones and 24 spirals (de Zeeuw et
al. 2002MNRAS.329..513D 2002MNRAS.329..513D). The second one undertaken in 2007-2008 added
more early-type galaxies, including dwarfs, to complete the
volume-limited (D<42Mpc) sample (Cappellari et al. 2011, Cat.
J/MNRAS/413/813). The total sample of early-type galaxies investigated
in these two surveys includes 260 objects, and 200 of them are
lenticular galaxies. For my analysis I have selected a subsample of
143 S0 galaxies that were observed in 2007-2008.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 40 143 Lick indices and Simple Stellar Populations
(SSP)-equivalent parameters for the nuclei
table2.dat 63 86 Lick indices and Simple Stellar Populations
(SSP)-equivalent parameters for the bulges
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See also:
J/ApJS/219/4 : S4G pipeline 4: multi-component decompositions (Salo+, 2015)
J/MNRAS/448/3484 : ATLAS3D Project. XXX (McDermid+, 2015)
J/MNRAS/416/1680 : ATLAS3D project. VII. (Cappellari+, 2011)
J/MNRAS/414/940 : ATLAS3D project. IV. (Young+, 2011)
J/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011)
J/MNRAS/405/1089 : Photometric scaling for L/S0 galaxies (Laurikainen+ 2010)
J/A+A/478/353 : Structural properties of disk galaxies (Mendez-Abreu+, 2008)
J/AJ/116/1626 : Galaxy brightness profiles (Baggett+, 1998)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Galaxy name
10- 13 F4.2 0.1nm W5007 [0/5.5] Equivalent width of [OIII]λ5007;
in Å
15- 19 F5.2 0.1nm Hb [-0.3/5.3] Hβ Lick index; in Å (G1)
21- 24 F4.2 0.1nm Mgb [1.8/6.1] Mgb Lick index; in Å (G1)
26- 29 F4.2 0.1nm Fe5270 [2.1/3.7] Fe5270 Lick index; in Å (G1)
31- 34 F4.1 Gyr Age [1/15] Simple Stellar Populations (SSP)-equivalent
age (G1)
36- 40 F5.2 [Sun] [Z/H] [-0.3/1] SSP-equivalent metallicity (G1)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Galaxy name
10- 13 F4.1 arcsec Reff [1.7/14.4] Bulge effective radius re(bul)
15- 17 F3.1 arcsec e_Reff [0.1/3.9]? Error in Reff
19- 23 A5 --- r_Reff Reference for Reff (1)
25- 29 F5.3 0.1nm W5007 [0/1.7] Equivalent width of [OIII]λ5007;
in Å
31- 34 F4.2 0.1nm Hb [1/2.6] Hβ Lick index; in Å (G1)
36- 39 F4.2 0.1nm Mgb [2.1/4.9] Mgb Lick index; in Å (G1)
41- 44 F4.2 0.1nm Fe5270 [1.7/3.2] Fe5270 Lick index; in Å (G1)
46 A1 --- l_Age [>] Lower limit flag on Age
47- 50 F4.1 Gyr Age [1.5/15] Simple Stellar Populations
(SSP)-equivalent age (G1)
52 A1 --- l_[Z/H] [<] Upper limit flag on [Z/H]
53- 57 F5.2 [Sun] [Z/H] [-0.4/0.25] SSP-equivalent metallicity (G1)
59- 63 F5.2 [Sun] [Mg/Fe] [0/0.4] Magnesium-to-iron ratio (G1)
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Note (1): The sources of the re(bull) are numbered as follows:
1 = Laurikainen et al. 2010 (Cat. J/MNRAS/405/1089);
2 = Laurikainen et al. 2005MNRAS.362.1319L 2005MNRAS.362.1319L;
3 = Salo et al. 2015 (Cat. J/ApJS/219/4);
4 = Krajnovic et al. 2013MNRAS.432.1768K 2013MNRAS.432.1768K;
5 = Mendez-Abreu et al. 2008 (Cat. J/A+A/478/353);
6 = D'Onofrio 2001MNRAS.326.1517D 2001MNRAS.326.1517D;
7 = Baggett et al. 1998 (Cat. J/AJ/116/1626);
8 = Il'ina & Sil'chenko 2012ARep...56..578I 2012ARep...56..578I.
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Global Notes:
Note (G1): Mean (close to luminosity-weighted) parameters of the stellar
populations were calculated in the frame of the evolutionary synthesis
models of Simple Stellar Populations (SSP). The SSP-equivalent ages,
metallicities, and magnesium-to-iron ratios were determined by comparing
Mgb versus Fe5270 and Hβ versus [MgFe52]=(Mgb*Fe5270)1/2; I compared
my index measurements to the SSP models by Thomas et al.
2003MNRAS.339..897T 2003MNRAS.339..897T, which are calculated for a set of the
magnesium-to-iron ratios. The typical internal (statistical) accuracy of
the indices is around 0.1Å; subsequently the internal accuracy of the
ages is 0.5Gyr for young populations, T<3Gyr, 1Gyr for intermediate ages,
3<T<8Gyr, and 3Gyr for older ones. The accuracy of the metallicities is
about 0.1dex.
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History:
From electronic version of the journal
(End) Sylvain Guehenneux [CDS] 27-Sep-2016