J/ApJS/190/233 Spectroscopy and abundances of SINGS galaxies (Moustakas+, 2010)
Optical spectroscopy and nebular oxygen abundances of the Spitzer/SINGS
galaxies.
Moustakas J., Kennicutt R.C.Jr, Tremonti C.A., Dale D.A., Smith J.-D.T.,
Calzetti D.
<Astrophys. J. Suppl. Ser., 190, 233-266 (2010)>
=2010ApJS..190..233M 2010ApJS..190..233M
ADC_Keywords: Surveys ; Galaxies, IR ; Spectroscopy ; Equivalent widths ;
Abundances ; H II regions
Keywords: atlases - galaxies: abundances - galaxies: fundamental parameters -
galaxies: ISM - galaxies: stellar content - techniques: spectroscopic
Abstract:
We present intermediate-resolution optical spectrophotometry of 65
galaxies obtained in support of the Spitzer Infrared Nearby Galaxies
Survey (SINGS). For each galaxy we obtain a nuclear, circumnuclear,
and semi-integrated optical spectrum designed to coincide spatially
with mid- and far-infrared spectroscopy from the Spitzer Space
Telescope. We make the reduced, spectrophotometrically calibrated
one-dimensional spectra, as well as measurements of the fluxes and
equivalent widths of the strong nebular emission lines, publically
available. We use optical emission-line ratios measured on all three
spatial scales to classify the sample into star-forming, active
galactic nuclei (AGNs), and galaxies with a mixture of star formation
and nuclear activity. We find that the relative fraction of the sample
classified as star forming versus AGN is a strong function of the
integrated light enclosed by the spectroscopic aperture. We supplement
our observations with a large database of nebular emission-line
measurements of individual HII regions in the SINGS galaxies culled
from the literature. We use these ancillary data to conduct a detailed
analysis of the radial abundance gradients and average HII-region
abundances of a large fraction of the sample. We combine these results
with our new integrated spectra to estimate the central and
characteristic (globally averaged) gas-phase oxygen abundances of all
75 SINGS galaxies. We conclude with an in-depth discussion of the
absolute uncertainty in the nebular oxygen abundance scale.
Description:
The optical spectra were obtained between 2001 November and 2006 May
at the Bok 2.3m telescope on Kitt Peak for galaxies in the northern
hemisphere, and at the CTIO 1.5m telescope for galaxies in the
southern hemisphere.
The SINGS sample (Kennicutt et al., 2003PASP..115..928K 2003PASP..115..928K), comprising
75 galaxies, is intended to be a valuable representative set of local
galaxies that are not ultraluminous, and whose moderate distances
ensure that the properties of the interstellar medium can be studied
at relatively small spatial scales (a few hundreds of parsecs at the
shortest wavelengths).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 84 75 Properties of the SINGS galaxies
table3.dat 146 184 Optical emission-line fluxes for 71 SINGS galaxies
table4.dat 116 184 Optical emission-line equivalent widths
table10.dat 126 561 Oxygen abundances of the HII regions in the
SINGS galaxies
refs.dat 95 54 References for tables 1 and 10
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See also:
J/ApJ/669/959 : Warm molecular hydrogen in SINGS galaxy sample (Roussel+,
2007)
J/MNRAS/361/1063 : Oxygen abundances of HII regions (Perez-Montero+, 2005)
J/ApJ/617/240 : Oxygen abundances in the GOODS-North field (Kobulnicky+,
2004)
J/A+A/391/809i : HII regions in NGC 5457 and NGC 4395 (Cedres+, 2002)
J/AJ/116/2805 : HII regions in spiral galaxies (Van Zee+, 1998)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name SINGS galaxy name
10- 18 A9 --- TType Morphological type from Kennicutt et al.
(2003PASP..115..928K 2003PASP..115..928K)
20- 24 F5.3 mag E(B-V) B-V color excess (1)
26- 30 F5.2 arcmin rho25 Radius of the major axis at the
µB=25mag/arcsec2 isophote
(de Vaucouleurs et al., 1991, Cat. VII/155)
32- 33 I2 deg i Galaxy inclination (2)
35 A1 --- f_i [ce] Flag on inclination (3)
37- 39 I3 deg PA ?=- Position angle (2)
41- 46 F6.2 mag BMAG Absolute B-band magnitude (4)
48- 51 F4.2 mag e_BMAG BMAG uncertainty
53- 57 F5.2 mag B-V B-V color index (4)
59- 62 F4.2 mag e_B-V B-V uncertainty
64- 69 F6.3 Mpc Dist Distance
71- 75 F5.3 Mpc e_Dist Distance uncertainty
76 A1 --- f_Dist [abd] Flag on Dist (5)
78- 81 A4 --- Meth Distance method (6)
83- 84 I2 --- Ref Distance reference; see refs.dat file
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Note (1): used to correct the optical spectroscopy and photometry for
foreground Galactic reddening (Schlegel et al., 1998ApJ...500..525S 1998ApJ...500..525S)
Note (2): Galaxy inclination and position angles (de Vaucouleurs et al.,
1991, Cat. VII/155; Jarrett et al., 2003AJ....125..525J 2003AJ....125..525J). We compute
the inclination angle, i, following Tully et al. (1998AJ....115.2264T 1998AJ....115.2264T):
sin(i)=1.02x(1-(b/a)2)0.5,
where (b/a) is the minor-to-major axis ratio at
µB=25mag/arcsec2 (de Vaucouleurs et al., 1991, Cat. VII/155),
or the isophotal axis ratio at µKs=20mag/arcsec2 (Jarrett et
al., 2003AJ....125..525J 2003AJ....125..525J).
Note (3): Flag as follows:
c = For NGC 5194 we adopt the kinematic inclination angle determined by
Tully (1974ApJS...27..437T 1974ApJS...27..437T).
e = For NGC 6822 we adopt the kinematic inclination and position angle
derived by Brandenburg & Skillman (1998AAS...193.7011B 1998AAS...193.7011B). We have also
adjusted the apparent B- and V-band magnitudes for this object from
Dale et al. (2007ApJ...655..863D 2007ApJ...655..863D) by -0.37mag to better match the B-band
magnitude from Karachentsev et al. (2004, Cat. J/AJ/127/2031).
Note (4): Absolute B-band magnitude and B-V color, both relative to Vega
(Dale et al., 2007ApJ...655..863D 2007ApJ...655..863D; Munoz-Mateos et al.,
2009ApJ...701.1965M 2009ApJ...701.1965M) (see Section 2.1 for more details).
Note (5): Flags as follows:
a = For these objects we adopt the HST Key Project Cepheid distance
uncorrected for metallicity variations (see Freedman et al.,
2001ApJ...553...47F 2001ApJ...553...47F).
b = NGC 4254, NGC 4450, NGC 4569, and NGC 4579 have been placed at the
distance of the Virgo cluster (16.5±0.6Mpc; Mei et al.,
2007ApJ...655..144M 2007ApJ...655..144M).
d = The interacting pair NGC 5194 (M51a) and NGC 5195 has been placed at a
common distance.
Note (6): The distance methods have the following meaning:
Flow = Hubble distance assuming H0=70km/s/Mpc corrected for peculiar
motions;
SBF = Surface-brightness fluctuations;
BS = Bright stars (supergiants);
Ceph = Cepheid variables;
Mult = An average of multiple, cross-calibrated techniques;
TRGB = Tip of the red-giant branch;
Mem = Group/cluster membership;
SN = Supernova;
PNLF = Planetary nebula luminosity function.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Spectrum Spectrum (nuclear, circumnuclear or
semi-integrated)
15- 23 A9 --- Name Galaxy name
25- 31 F7.2 aW/m2 FOII ? The [OII] 3727Å line flux (1)
33- 38 F6.2 aW/m2 e_FOII ? Uncertainty in OII (2)
40- 46 F7.2 aW/m2 FHg ? The Hγ 4340Å line flux (1)
48- 53 F6.2 aW/m2 e_FHg ? Uncertainty in Hg (2)
55- 61 F7.2 aW/m2 FHb ? The Hβ 4861Å line flux (1)
63- 68 F6.2 aW/m2 e_FHb ? Uncertainty in Hb (2)
70- 76 F7.2 aW/m2 FOIII ? The [OIII] 5007Å line flux (1)
78- 83 F6.2 aW/m2 e_FOIII ? Uncertainty in OIII
85- 92 F8.2 aW/m2 FHa ? The Hα 6563Å line flux (1)
94-100 F7.2 aW/m2 e_FHa ? Uncertainty in Ha (2)
102-108 F7.2 aW/m2 FNII ? The [NII] 6584Å line flux (1)
110-116 F7.2 aW/m2 e_FNII ? Uncertainty in NII (2)
118-124 F7.2 aW/m2 FSIIa ? The [SII] 6716Å line flux (1)
126-131 F6.2 aW/m2 e_FSIIa ? Uncertainty in SIIa (2)
133-139 F7.2 aW/m2 FSIIb ? The [SII] 6731Å line flux (1)
141-146 F6.2 aW/m2 e_FSIIb ? Uncertainty in SIIb (2)
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Note (1): Optical emission-line fluxes in units of 10-15erg/s/cm2,
(i.e. 10-18 W/m2),
corrected for foreground Galactic extinction (RV=3.1;
O'Donnell, 1994ApJ...422..158O 1994ApJ...422..158O; Schlegel et al., 1998ApJ...500..525S 1998ApJ...500..525S).
Note (2): Note that the uncertainties include only statistical measurement
uncertainties, and do not include systematic errors due to, for
example, imperfect continuum subtraction. For most applications we
recommend that a minimum S/N>2 signal-to-noise ratio cut be
applied to the fluxes listed in this table.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Spectrum Spectrum, as in table3
15- 23 A9 --- Name Galaxy name
25- 30 F6.2 0.1nm WOII ? The [OII] 3727Å equivalent width (3)
32- 35 F4.2 0.1nm e_WOII ? Uncertainty in WOII (4)
37- 41 F5.2 0.1nm WHg ? The Hγ 4340Å equivalent width (3)
43- 46 F4.2 0.1nm e_WHg ? Uncertainty in WHg (4)
48- 52 F5.2 0.1nm WHb ? The Hβ 4861Å equivalent width (3)
54- 57 F4.2 0.1nm e_WHb ? Uncertainty in WHb (4)
59- 64 F6.2 0.1nm WOIII ? The [OIII] 5007Å equivalent width (3)
66- 70 F5.2 0.1nm e_WOIII ? Uncertainty in WOIII
72- 77 F6.2 0.1nm WHa ? The Hα 6563Å equivalent width (3)
79- 83 F5.2 0.1nm e_WHa ? Uncertainty in WHa (4)
85- 89 F5.2 0.1nm WN ? The [NII] 6584Å equivalent width (3)
91- 94 F4.2 0.1nm e_WNII ? Uncertainty in WNII (4)
96-100 F5.2 0.1nm WSIIa ? The [SII] 6716Å equivalent width (3)
102-105 F4.2 0.1nm e_WSIIa ? Uncertainty in WSIIa (4)
107-111 F5.2 0.1nm WSIIb ? The [SII] 6731Å equivalent width (3)
113-116 F4.2 0.1nm e_WSIIb ? Uncertainty in WSIIb (4)
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Note (3): Rest-frame emission-line equivalent widths in Angstroms.
Note (4): Note that the uncertainties include only statistical measurement
uncertainties, and do not include systematic errors due to, for
example, imperfect continuum subtraction. For most applications we
recommend that a minimum S/N>2 signal-to-noise ratio cut be applied to
the equivalent widths listed in this table.
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Byte-by-byte Description of file: table10.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Unique HII-region identification number
5- 13 A9 --- Name Galaxy name
15- 31 A17 --- Region Alternate HII region name
33- 36 F4.2 arcmin rho25 ? Deprojected galactocentric radius (1)
38- 42 F5.2 --- R23 R23 parameter (2)
44- 47 F4.2 --- e_R23 Uncertainty in R23
49- 53 F5.2 --- O32 O32 parameter (2)
55- 58 F4.2 --- e_O32 Uncertainty in O32
60- 63 F4.2 --- P P parameter (2)
65- 68 F4.2 --- e_P Uncertainty in P
70- 73 F4.2 [-] O/H-a ? Oxygen abundance using KK04 (4)
75- 78 F4.2 [-] e_O/H-a ? Uncertainty in O/H(KK04)
80 A1 --- f_O/H-a [ab] Flag on O/H(KK04) (3)
82- 85 F4.2 [-] O/H-b ? Oxygen abundance using PT05 (4)
87- 90 F4.2 [-] e_O/H-b ? Uncertainty in O/H(PT05)
92 A1 --- f_O/H-b [ab] Flag on O/H(PT05) (3)
94- 95 I2 --- Ref Reference, see refs.dat file
97- 98 I2 h RAh Galaxy hour of right ascension (J2000)
100-101 I2 min RAm Galaxy minute of right ascension (J2000)
103-106 F4.1 s RAs Galaxy second of right ascension (J2000)
108 A1 --- DE- Galaxy sign of declination (J2000)
109-110 I2 deg DEd Galaxy degree of declination (J2000)
112-113 I2 arcmin DEm Galaxy arcminute of declination (J2000)
115-116 I2 arcsec DEs Galaxy arcsecond of declination (J2000)
118-121 I4 arcsec offRA ?=-999 HII region RA offset (from galaxy)
123-126 I4 arcsec offDE ?=-999 HII region DEC offset (from galaxy)
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Note (1): Normalized by the ρ25 radius of the galaxy (see Table 1).
Note (2): The KK04 (Kobulnicky & Kewley, 2004, Cat. J/ApJ/617/240) and PT05
(Pilyugin & Thuan, 2005ApJ...631..231P 2005ApJ...631..231P) calibrations we have chosen
both rely on the metallicity-sensitive R23 parameter (Pagel et al.,
1979MNRAS.189...95P 1979MNRAS.189...95P):
R23=([OII]λ3727+[OIII]4959,5007)/Hβλ4861
O32=[OIII]4959,5007/[OII]λ3727 characterizes the hardness of
the ionizing radiation field (Kewley & Dopita, 2002ApJS..142...35K 2002ApJS..142...35K).
P=[OIII]4959,5007/([OII]λ3727+[OIII]4959,5007) is an excitation
parameter (Pilyugin, 2001A&A...369..594P 2001A&A...369..594P).
See section 4.1 for further details.
Note (3): Flag as follows:
a = The oxygen abundance of this HII region is not defined according to
the criteria described in Section 4.2.
b = The R23 branch of this HII region is ambiguous according to the
criteria described in Section 4.2.
Note (4): 12+log(O/H). Derived using the KK04 (Kobulnicky & Kewley, 2004,
Cat. J/ApJ/617/240) and PT05 (Pilyugin & Thuan, 2005ApJ...631..231P 2005ApJ...631..231P)
strong-line calibrations assuming the R23 branch listed in Table 7,
unless otherwise noted.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Ref Reference number
4- 22 A19 --- BibCode Bibcode
24- 48 A25 --- Aut Author's name
50- 95 A46 --- Comm Comment
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Acknowledgements:
John Moustakas [Siena College] for table 10 galaxy coordinates and offsets.
History:
From electronic version of the journal
28-Nov-2010: Insert into VizieR
20-Jan-2016: Coordinates added in table 10.
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 19-Oct-2010