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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
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), 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:
FileName Lrecl Records Explanations
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 95 561 Oxygen abundances of the HII regions in the SINGS galaxies refs.dat 95 54 References for tables 1 and 10
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
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) 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
Note (1): used to correct the optical spectroscopy and photometry for foreground Galactic reddening (Schlegel et al., 1998ApJ...500..525S) Note (2): Galaxy inclination and position angles (de Vaucouleurs et al., 1991, Cat. VII/155; Jarrett et al., 2003AJ....125..525J). We compute the inclination angle, i, following Tully et al. (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). Note (3): Flag as follows: c = For NGC 5194 we adopt the kinematic inclination angle determined by Tully (1974ApJS...27..437T). e = For NGC 6822 we adopt the kinematic inclination and position angle derived by Brandenburg & Skillman (1998AAS...193.7011B). We have also adjusted the apparent B- and V-band magnitudes for this object from Dale et al. (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; Munoz-Mateos et al., 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). 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). 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.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
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)
Note (1): Optical emission-line fluxes in units of 10-15erg/s/cm2, corrected for foreground Galactic extinction (RV=3.1; O'Donnell, 1994ApJ...422..158O; Schlegel et al., 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.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
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)
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.
Byte-by-byte Description of file: table10.dat
Bytes Format Units Label Explanations
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
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) calibrations we have chosen both rely on the metallicity-sensitive R23 parameter (Pagel et al., 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). P=[OIII]4959,5007/([OII]λ3727+[OIII]4959,5007) is an excitation parameter (Pilyugin, 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) strong-line calibrations assuming the R23 branch listed in Table 7, unless otherwise noted.
Byte-by-byte Description of file: refs.dat
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
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 19-Oct-2010
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