J/MNRAS/445/899 LVL SEDs and physical properties (Cook+, 2014)
Spitzer Local Volume Legacy (LVL) SEDs and physical properties.
Cook D.O., Dale D.A., Johnson B.D., Van Zee L., Lee J.C., Kennicutt R.C.,
Calzetti D., Staudaher S.M., Engelbracht C.W.
<Mon. Not. R. Astron. Soc., 445, 899-912 (2014)>
=2014MNRAS.445..899C 2014MNRAS.445..899C
ADC_Keywords: Surveys ; Galaxies, nearby ; Galaxies, photometry ; Abundances ;
Extinction
Keywords: dust, extinction - galaxies: dwarf - galaxies: ISM - Local Group -
galaxies: spiral - galaxies: star formation
Abstract:
We present the panchromatic spectral energy distributions (SEDs) of
the Local Volume Legacy (LVL) survey which consists of 258 nearby
galaxies (D<11Mpc). The wavelength coverage spans the ultraviolet to
the infrared (1500Å-24µm) which is utilized to derive global
physical properties (i.e. star formation rate, stellar mass, internal
extinction due to dust). With these data, we find colour-colour
relationships and correlated trends between observed and physical
properties (i.e. optical magnitudes and dust properties, optical
colour and specific star formation rate, and ultraviolet-infrared
colour and metallicity). The SEDs are binned by different galaxy
properties to reveal how each property affects the observed shape of
these SEDs. In addition, due to the volume-limited nature of LVL, we
utilize the dwarf-dominated galaxy sample to test star formation
relationships established with higher mass galaxy samples. We find
good agreement with the star-forming `main-sequence' relationship, but
find a systematic deviation in the infrared `main sequence' at low
luminosities. This deviation is attributed to suppressed polycyclic
aromatic hydrocarbon (PAH) formation in low-metallicity environments
and/or the destruction of PAHs in more intense radiation fields
occurring near a suggested threshold in star formation rates (sSFR) at
a value of log(sSFR)~-10.2.
Description:
The LVL sample consists of 258 of our nearest galaxy neighbours
reflecting a statistically complete, representative sample of the
local Universe. The sample selection and description are detailed in
Dale et al. (2009ApJ...703..517D 2009ApJ...703..517D, Cat. J/ApJ/703/517).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 79 258 General galaxy properties
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See also:
J/ApJ/703/517 : The Spitzer Local Volume Legacy: IR photometry (Dale+, 2009)
J/MNRAS/445/881 : LVL global optical photometry (Cook+, 2014)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Galaxy name
16- 17 I2 h RAh Right Ascension (J2000)
19- 20 I2 min RAm Right Ascension (J2000)
22- 26 F5.2 s RAs Right Ascension (J2000)
28 A1 --- DE- Declination sign (J2000)
29- 30 I2 deg DEd Declination (J2000)
32- 33 I2 arcmin DEm Declination (J2000)
35- 38 F4.1 arcsec DEs Declination (J2000)
40- 44 F5.2 Mpc Dist [0.05/20] Distance from Kennicutt et al. 2008
(J/ApJS/178/247)
46- 47 I2 --- TT [-5/11] Optical morphology from Kennicutt et al.
2008 (J/ApJS/178/247)
49- 51 F3.1 [-] Ab(O) [7.2/9.3]?=- Oxygen abundances 12+log(O/H)
(metallicity)
53- 56 F4.2 [-] e_Ab(O) ?=- Error on Ab(O)
58 A1 --- r_Ab(O) [0ab] Reference of Ab(O) (1)
60- 65 A6 --- Meth Method of oxygen abundance determination (2)
67- 71 F5.3 mag AFUV Extinction due to dust in the FUV bandpass
73 A1 --- r_AFUV [0c] AFUV reference (3)
75- 79 F5.2 Msun logM* [5.8/11.1]?=- Stellar mass, derived from
3.6µm measurement
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Note (1): Oxygen abundances (metallicity) reference as follows:
0 = Marble et al. (2010, Cat. J/ApJ/715/506)
a = Metallicity from Moustakas et al. (2010, Cat. J/ApJS/190/233)
b = Metallicity from Berg et al. (2012ApJ...754...98B 2012ApJ...754...98B)
Note (2): Method of oxygen abundance determination as follows:
4363 = [OIII] 4363 line (Marble et al., 2010, Cat. J/ApJ/715/506)
PN = a planetary nebula observation
Mix = mix of [OIII] 4363 line and strong-line methods
Strong = strong-line method (Marble et al., 2010, Cat. J/ApJ/715/506)
none = strong-line method (Marble et al., 2010, Cat. J/ApJ/715/506)
Note (3): Extinction due to dust in the FUV bandpass derived from the following:
0 = Hao et al. (2011ApJ...741..124H 2011ApJ...741..124H)
c = AFUV derived from AHα
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 04-May-2015