The Anatomy of Star Formation in NGC 300

By G. Helou, H. Roussel, P. Appleton, D. Frayer, S. Stolovy, L. Storrie-Lombardi, R. Hurt, P. Lowrance, D. Makovoz, F. Masci and 15 more. 2004

234 citations recorded by the source corpus.

The Spitzer Space Telescope was used to study the mid- to far-infrared properties of NGC 300 and to compare dust emission to Hα to elucidate the heating of the interstellar medium (ISM) and the star formation cycle at scales smaller than 100 pc. The new data allow us to discern clear differences in the spatial distribution of 8 μm dust emission with respect to 24 μm dust and to H II regions traced by Hα light. The 8 μm emission highlights the rims of H II regions, and the 24 μm emission is more strongly peaked in star-forming regions than 8 μm. We confirm the existence and approximate amplitude of interstellar dust emission at 4.5 μm, detected statistically in Infrared Space Observatory (ISO) data, and conclude it arises in star-forming regions. When averaging over regions larger than ∼1 kpc, the ratio of Hα to aromatic feature emission in NGC 300 is consistent with the values observed in disks of spiral galaxies. The mid- to far-infrared spectral energy distribution of dust emission is generally consistent with pre-Spitzer models.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b02a0efc140b4243f435016f136ae375143c6bec

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

RADIAL DISTRIBUTION OF STARS, GAS, AND DUST IN SINGS GALAXIES. II. DERIVED DUST PROPERTIES (2009, methodology): “To check the possible systematic effects introduced by the stellar emission correction, we fitted the models twice for all galaxies, using our flux ratios and the ones estimated by Helou et al. (2004) using stellar population modeling from Starburst99 (Leitherer et al. 1999).”
TESTING THE UNIFICATION MODEL FOR ACTIVE GALACTIC NUCLEI IN THE INFRARED: ARE THE OBSCURING TORI OF TYPE 1 AND 2 SEYFERTS DIFFERENT? (2011, background): “As found by Spitzer, the ∼8 µm PAH emission of nearby galaxies appears to be more extended than at ∼24 µm (e.g., Helou et al. 2004; Calzetti et al. 2005).”
Star Formation in NGC 5194 (M51a): The Panchromatic View from GALEX to Spitzer (2005, background): “This implies that the very small grains responsible for the IR emission closely trace the young ionizing stars (Cesarsky et al. 1996; Helou 2000; Haas, Klaas & Bianchi 2002; Helou et al. 2004).”
A Multiwavelength Study of M17: The Spectral Energy Distribution and PAH Emission Morphology of a Massive Star Formation Region (2007, methodology): “S. Holt & C. L. Bennett (New York: AIP), 161 Helfand, D. J., Becker, R. L., Fallon, A., & Tuttle, S. 2006, AJ, 131, 2525 Helou et al. 2004, ApJS, 154, 253 Houck, J. R., et al. 2004, Proc.”
Dust spectral energy distributions of nearby galaxies: an insight from the Herschel Reference Survey (2014, methodology): “Our coefficients are in good agreement with those of Helou et al. (2004) and Draine et al. (2007), i.e. 0.589, 0.396, 0.244 and 0.044 at 4.5, 5.8, 8.0 and 24.0 µm, respectively for the late-type galaxies.”
BULGES OF NEARBY GALAXIES WITH SPITZER: SCALING RELATIONS IN PSEUDOBULGES AND CLASSICAL BULGES (2010, background): “We calculate M8,dust using the relation from Helou et al. (2004), where M8,dust = −2.5 × log10(L8 − 0.232 × L3.”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “Interestingly PAH emission appears to correlate the most strongly with the longer-wavelength component of the thermal dust emission (e.g., Bendo et al. 2008), though it often also appears as resolved shells around the young star-forming regions (Helou et al. 2004).”
The Calibration of Mid-Infrared Star Formation Rate Indicators (2007, background): “Helou et al. (2004) have shown that the 8 µm emission is brighter at the edges of an HII region (i.e., in the PDR) than at its center.”
CALIBRATING EXTINCTION-FREE STAR FORMATION RATE DIAGNOSTICS WITH 33 GHz FREE–FREE EMISSION IN NGC 6946 (2011, methodology): “We note that the 8µm map was corrected for stellar light using a scaled 3.6µm image following Helou et al. (2004).”
Warm Molecular Hydrogen in the Spitzer SINGS Galaxy Sample (2007, methodology): “To this effect, we scaled 3.6 m fluxes, assumed to be dominated by stellar emission, as described in Helou et al. (2004).”
EXTENDING THE NEARBY GALAXY HERITAGE WITH WISE: FIRST RESULTS FROM THE WISE ENHANCED RESOLUTION GALAXY ATLAS (2012, methodology): “Using the three elliptical galaxies in the sample, which trace only the photospheric continuum contribution, we determine that the W3 to W1 scale factor is ∼15% (which may be compared with the IRAC-4 to IRAC-1 ratio of 23%; Helou et al. 2004).”
An Ultraviolet-to-Radio Broadband Spectral Atlas of Nearby Galaxies (2006, unknown): “In fact, the 24 µm emission can be spatially closely associated with H II regions, and in such cases is probably dominated by dust from within these regions (Helou et al. 2004; Murphy et al. 2006).”
A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) (2015, background): “…considers the 3.6 and 4.5µm filters as near-IR and the 5.8 and 8.0µm filters as mid- 2 Buta et al. tic spectrum: the 3.6 and 4.5µm bands largely sample the photospheric light of old stars (Pahre et al. 2004), while the 5.8 and 8.0µm bands reveal the dusty interstellar medium (Helou et al. 2004).”
RECONSTRUCTING THE STELLAR MASS DISTRIBUTIONS OF GALAXIES USING S4G IRAC 3.6 AND 4.5 μm IMAGES. I. CORRECTING FOR CONTAMINATION BY POLYCYCLIC AROMATIC HYDROCARBONS, HOT DUST, AND INTERMEDIATE-AGE STARS (2011, methodology): “…comparison to the 8µm emission provides as accurate quantification of the quality of our contaminant correction as is currently possible, given that corrections for the contaminants in the IRAC bands are typically based on such images, where available (Kendall et al. 2008; Helou et al. 2004).”
Modelling the spectral energy distribution of galaxies - V. The dust and PAH emission SEDs of disk galaxies (2010, methodology): “Before comparison with the model, the 8µm image had the stellar component subtracted off. light at 8µm (estimated by multiplying a Spitzer 3.6µm image by a factor of 0.26; Helou et al. 2004).”
WHAT DRIVES THE EXPANSION OF GIANT H ii REGIONS?: A STUDY OF STELLAR FEEDBACK IN 30 DORADUS (2010, background): “The coefficients 0.232 and 0.032 are given in Helou et al. (2004).”
EXTRAGALACTIC CHEMICAL ABUNDANCES: DO H ii REGIONS AND YOUNG STARS TELL THE SAME STORY? THE CASE OF THE SPIRAL GALAXY NGC 300 (2009, background): “…al. 2001), planetary nebulae (Soffner et al. 1996; Peña et al. 2009), variable stars (Pietrzyński et al. 2002; Mennickent et al. 2004), dust content (Helou et al. 2004; Roussel et al. 2005), X-ray sources (Read & Pietsch 2001; Carpano et al. 2005), supernova remnants (Blair & Long 1997; Pannuti…”
Infrared Spectral Energy Distributions of Nearby Galaxies (2005, background): “These results suggest that both 24 and 70 m trace warmer dust phases, consistent with morphological studies carried out by Hinz et al. (2004) for M33, Helou et al. (2004) for NGC 300, Gordon et al. (2004), and G. Rieke et al. (2005, private communication) for M31.”