Polycyclic Aromatic Hydrocarbons as a Tracer of Star Formation?

By E. Peeters, H. Spoon, A. Tielens. 2004

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In Astronomy and Astrophysics

Citations in the corpus

The Mid-Infrared Properties of Starburst Galaxies from Spitzer-IRS Spectroscopy (2006, background): “If the observed PAH flux is integrated over the whole galaxy, it may predominantly trace B stars, which dominate the Galactic stellar energy budget, rather than very recent massive star formation (Peeters et al. 2004).”
DUSTY INFRARED GALAXIES: Sources of the Cosmic Infrared Background (2005, background): “These features result from C-C and C-H stretching/bending vibrational bands excited by the absorption of a single UV or optical photon and are a good tracer of normal and moderately active star formation activity in spiral and irregular galaxies (e.g., Helou et al. 2000; Peeters et al. 2004).”
Chandra and Spitzer Unveil Heavily Obscured Quasars in the Chandra/SWIRE Survey (2006, background): “…regions is more luminous than that produced by theAGN, e.g., as in the Seyfert 2 galaxiesNGC4945 andNGC6240 (Maiolino et al. 2003; Rigopoulou et al. 1999), the AGN IR emission is fainter or negligible compared to that produced by star formation processes in the host galaxy (Peeters et al. 2004).”
The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields (2007, background): “In general, PAH line equivalent widths appear to be quite independent of the bolometric IR luminosities of star-forming galaxies (Peeters et al. 2004; Brandl et al. 2006).”
PAH and Mid-Infrared Luminosities as Measures of Star Formation Rate in Spitzer First Look Survey Galaxies (2005, background): “Peeters et al. (2004) have pointed out that PAHs may be better tracers of B stars than tracers of massive star formation (O stars).”
Dust covering factor, silicate emission, and star formation in luminous QSOs (2007, background): “…is at∼ 7.7µm) are emitted by very small carbon grains excited in the Photo Dissociation Regions, that are tracers of star forming activity (although PAHs may not be reliable SF tracers for compact HII regions or heavily embedded starbursts, Peeters et al.,2004; Förster Schreiber et al., 2004).”
Mid-Infrared Galaxy Classification Based on Silicate Obscuration and PAH Equivalent Width (2006, background): “…far-infrared) continuum slope, PAH line-to-continuum ratio, PAH to far-infrared luminosity ratio and the ratio of a high to a low ionization forbidden line such as [NeV]/[NeII ] (Genzel et al. 1998; Lutz et al. 1998; Laurent et al. 2000; Peeters et al. 2004; Dale et al. 2006; Sturm et al. 2006).”
Mid-Infrared Spectral Diagnosis of Submillimeter Galaxies (2007, background): “Peeters et al. (2004) showed a correlation between LFIR and LPAH;6:2 for a range of scales of star formation in local massive star-forming regions to normal and starburst galaxies.”
A TWO-PARAMETER MODEL FOR THE INFRARED/SUBMILLIMETER/RADIO SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES AND ACTIVE GALACTIC NUCLEI (2014, background): “…2000; Murphy et al. 1Available at physics.uwyo.edu/∼ddale/research/seds/seds.html 7 2009; Mullaney et al. 2011; Wu et al. 2011) or a combination of the mid-infrared continnum plus mid-infrared fine-structure lines (e.g., Genzel et al. 1998; Peeters et al. 2004; Armus et al. 2007; Dale et al. 2009).”
High-Resolution Mid-Infrared Spectroscopy of Ultraluminous Infrared Galaxies (2007, background): “The origin of PAH features and their use as star formation indicators are still controversial (e.g., Peeters et al. 2004; Förster Schreiber et al. 2004).”
Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample (2009, methodology): “This emission is superimposed by prominent broad emission features of polycyclic aromatic hydrocarbon (PAH) molecules6 ( ee Puget & Léger 1989; Sturm et al. 2000; Draine 2003; Peeters et al. 2004).”
MID-INFRARED SPECTROSCOPY OF SUBMILLIMETER GALAXIES: EXTENDED STAR FORMATION IN MASSIVE HIGH-REDSHIFT GALAXIES (2009, background): “Such diversity in PAH ratios is also present in local ULIRGs (e.g., Rigopoulou et al. 1999; Peeters et al. 2004), indicating that diverse radiation fields are found amongst both low- and high-redshift IR-luminous sources.”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS (2009, background): “…longer wavelength tracers such as the 24 μm emission, with systematic dependences of the emissivity on metal abundance, and local radiation field strength and hardness (e.g., Madden 2000; Peeters et al. 2004; Engelbracht et al. 2005, 2008; Dale et al. 2005; Wu et al. 2006; Smith et al. 2007; C07).”
Variations of the Mid-IR Aromatic Features inside and among Galaxies (2008, methodology): “It has long been surmised that the IR emission features provide a clear mid-IR signature of the interaction of far-UV photons with cloud surfaces and hence a probe of the importance of (massive) star formation in a region (Genzel et al. 1998; Peeters et al. 2004b).”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “…have shown that the PAH luminosity scales relatively well with the SFR in metalrich luminous star-forming galaxies (e.g., Roussel et al. 2001; Peeters et al. 2004; Förster Schreiber et al. 2004; Wu et al. 2005a; Farrah et al. 2007; Calzetti et al. 2007), but the PAH bands weaken…”
WHAT DRIVES THE EXPANSION OF GIANT H ii REGIONS?: A STUDY OF STELLAR FEEDBACK IN 30 DORADUS (2010, result): “This result is consistent with the analyses of Peeters et al. (2004), who showed that the ratio of PAH to far-IR (dust continuum) emission in Galactic HII regions is inversely correlated with the intensity of the UV field absorbed by the dust.”