2010
DOI: 10.1088/0004-637x/715/1/506
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An Aromatic Inventory of the Local Volume

Abstract: Using infrared photometry from the Spitzer Space Telescope, we perform the first inventory of aromatic feature emission (AFE, but also commonly referred to as PAH emission) for a statistically complete sample of star-forming galaxies in the local volume. The photometric methodology involved is calibrated and demonstrated to recover the aromatic fraction of the IRAC 8µm flux with a standard deviation of 6% for a training set of 40 SINGS galaxies (ranging from stellar to dust dominated) with both suitable mid-in… Show more

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Cited by 83 publications
(104 citation statements)
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References 166 publications
(79 reference statements)
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“…According to the results of Andrews & Martini (2013), who used a stacking technique to measure the oxygen abundances of ∼200 000 star-forming galaxies from the SDSS to enhance the signal-to-noise ratio of the weak [Oiii] Thus, in what follows, where there are no direct-Te estimates, we have applied the transformations given by Kewley & Ellison (2008) to convert the original strong-line O/H calibrations for the MEGA dataset (and SDSS10 sample) to the calibrations by D02 and PP04 (PP04N2, PP04O3N2). As reported in Table 1, the original O/H calibrations include: KD02 Cresci et al 2012;Mannucci et al 2010;Troncoso et al 2014); KK04 (Kobulnicky & Kewley 2004;Kennicutt et al 2011;Henry et al 2013;Xia et al 2012);M91 (McGaugh 1991;Marble et al 2010); PP04N2, PP04O3N2 (Pettini & Pagel 2004;Shapley et al 2004Shapley et al , 2005aLiu et al 2008;Yabe et al 2012;Zahid et al 2014;Steidel et al 2014); and T04 (Tremonti et al 2004;de los Reyes et al 2015). .…”
Section: Metallicity Calibrationsmentioning
confidence: 99%
“…According to the results of Andrews & Martini (2013), who used a stacking technique to measure the oxygen abundances of ∼200 000 star-forming galaxies from the SDSS to enhance the signal-to-noise ratio of the weak [Oiii] Thus, in what follows, where there are no direct-Te estimates, we have applied the transformations given by Kewley & Ellison (2008) to convert the original strong-line O/H calibrations for the MEGA dataset (and SDSS10 sample) to the calibrations by D02 and PP04 (PP04N2, PP04O3N2). As reported in Table 1, the original O/H calibrations include: KD02 Cresci et al 2012;Mannucci et al 2010;Troncoso et al 2014); KK04 (Kobulnicky & Kewley 2004;Kennicutt et al 2011;Henry et al 2013;Xia et al 2012);M91 (McGaugh 1991;Marble et al 2010); PP04N2, PP04O3N2 (Pettini & Pagel 2004;Shapley et al 2004Shapley et al , 2005aLiu et al 2008;Yabe et al 2012;Zahid et al 2014;Steidel et al 2014); and T04 (Tremonti et al 2004;de los Reyes et al 2015). .…”
Section: Metallicity Calibrationsmentioning
confidence: 99%
“…Metallicity measurements are available only for a few of our sample galaxies (e.g. Marble et al 2010;Moustakas & Kennicutt 2006). For the rest of our galaxies, we use the MB-Z metallicity relation for dIrs from (Ekta & Chengalur 2010) to estimate their metallicity.…”
Section: Estimation Of the Star Formation Ratementioning
confidence: 99%
“…The total error in ΣSFR is calculated as the quadrature sum of the individual errors. Firstly, 1,2 Galaxies with detected cold HI in Gaussian decomposition and T B method respectively 3,4 Galaxies with available Hα and FUV map respectively References - † : (Marble et al 2010); ‡ : (Moustakas & Kennicutt 2006) we adopt a 10% calibration error in FUV flux and a 15% calibration error in Hα flux measurement. An additional error of ∼ 50% in star formation rate is expected due the variation in IMF and star formation history (Leroy et al 2012(Leroy et al , 2013.…”
Section: Estimation Of the Star Formation Ratementioning
confidence: 99%
“…They found that at a metallicity of 12 + log(O/H) ∼ 8, galaxies transition from having a median q PAH ∼ 3.5%, similar to the Milky Way value of 4.6%, to a median of ∼1%. Spectroscopic (Wu et al 2006;Engelbracht et al 2008) and photometric investigations (Marble et al 2010) of large samples of low-metallicity galaxies provide clear evidence for this deficit.…”
Section: Introductionmentioning
confidence: 97%