The DOI matches its Crossref record; 40 of the 51 references it cites were found in a registry or an index.
ESTIMATING THE STAR FORMATION RATE AT 1 kpc SCALES IN NEARBY GALAXIES
Open accessAbstract
Using combinations of Hα, ultraviolet (UV), and infrared (IR) emission, we estimate the star formation rate (SFR) surface density, Σ SFR , at 1 kpc resolution for 30 disk galaxies that are targets of the IRAM HERACLES CO survey. We present a new physically motivated IR spectral-energy-distribution-based approach to account for possible contributions to 24 μm emission not associated with recent star formation. Considering a variety of "reference" SFRs from the literature, we revisit the calibration of the 24 μm term in hybrid (UV+IR or Hα+IR) tracers. We show that the overall calibration of this term remains uncertain at the factor of two level because of the lack of wide-field, robust reference SFR estimates. Within this uncertainty, published calibrations represent a reasonable starting point for 1 kpc-wide areas of star-forming disk galaxies, but we re-derive and refine the calibration of the IR term in these tracers to match our resolution and approach to 24 μm emission. We compare a large suite of Σ SFR estimates and find that above Σ SFR ∼ 10 −3 M ☉ yr −1 kpc −2 the systematic differences among tracers are less than a factor of two across two orders of magnitude dynamic range. We caution that methodology and data both become serious issues below this level. We note from simple model considerations that when focusing on a part of a galaxy dominated by a single stellar population, the intrinsic uncertainty in Hα- and FUV-based SFRs is ∼0.3 and ∼0.5 dex.
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“In nearby spirals, analyses of the radial energy budget find that a significant fraction of the 24 µ m flux, particularly in bulges and inner disks, arises from dust heated by older stars rather than embedded HII regions (e.g., Boquien et al. 2011; Leroy et al. 2012).”
From The Panchromatic Hubble Andromeda Southern Treasury (PHAST). II. The Spatially Resolved Recent Star Formation History in M31 (2026) · cites this paper as Leroy et al. 2012
Citations
Cites
Schlegel, D. J., Finkbeiner, D. P., & Davis, M. (1998) · The Astrophysical Journal · doi:10.1086/305772 · Cited by 15,126 · cited 2×
“We correct the maps for the effect of Galactic extinction following Schlegel et al. (1998).”
MethodAstrophysics of Gaseous Nebulae and Active Galactic Nuclei
Osterbrock, D., & Ferland, G. (1989) · Choice Reviews Online · doi:10.5860/choice.26-6270 · Cited by 6,966 · cited 1×
“We also use UV and Hα, corrected for extinction based on astrophysical expectations, e.g., by the “Balmer decrement” or IRX-β approach (Storey & Hummer 1995; Osterbrock & Ferland 2006; Kennicutt 1998; Cortese et al. 2008).”
MethodThe Milky Way in Molecular Clouds: A New Complete CO Survey
Dame, T., Hartmann, D., & Thaddeus, P. (2000) · The Astrophysical Journal · doi:10.1086/318388 · Cited by 1,774 · cited 1×
“This value is intermediate among recent determinations of the Milky Way αCO (e.g., Strong & Mattox 1996; Dame et al. 2001; Heyer et al. 2009; Abdo et al. 2010) and represents a commonly adopted ”best single value” for work on nearby disk galaxies (e.g., Wong & Blitz 2002; Leroy et al. 2008).”
ResultAstrophysics of Gaseous Nebulae
Osterbrock, D., & Gull, T. (1976) · doi:10.1063/1.3023426 · Cited by 1,727 · cited 5×
“…Moustakas et al. (2010), supplement these with extinctions estimated from the gas column following Wong & Blitz (2002, their “hybrid” model) and extinctions inferred from comparing thermal radio continuum flux estimates from Niklas et al. (1995, 1997) to our Hα maps (following Wong & Blitz 2002).”
MethodInfluentialMeurer, G., Heckman, T., & Calzetti, D. (1999) · The Astrophysical Journal · doi:10.1086/307523 · Cited by 924 · cited 1×
“Adding UV and IR emission has an established pedigree (Buat 1992; Meurer et al. 1995, 1999; Cortese et al. 2008), while the combination of Hα and IR has been explored more recently (Calzetti et al. 2007; Kennicutt et al. 2007, 2009).”
BackgroundDust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample
Draine, B., Dale, D., Bendo, G. J., Gordon, K., Smith, J. D., Armus, L., Engelbracht, C., Helou, G., Kennicutt, R., Li, A., et al. (2007) · The Astrophysical Journal · doi:10.1086/518306 · Cited by 820 · cited 4×
“To calculate χ2 we use uncertainties estimated from the scatter in the convolved maps away from the galaxy or 10% of the observed intensity, whichever is higher (this approach follows Draine et al. 2007).”
BackgroundMethodInfluentialSelf-citationThe Calibration of Mid-Infrared Star Formation Rate Indicators
Calzetti, D., Kennicutt, R., Engelbracht, C., Leitherer, C., Draine, B., Kewley, L., Moustakas, J., Sosey, M., Dale, D., Gordon, K., et al. (2007) · The Astrophysical Journal · doi:10.1086/520082 · Cited by 758 · cited 35×
“Assuming the Paα to trace the true SFR, Calzetti et al. (2007) found: ΣSFR [ M⊙ yr −1 kpc−2 ] = 634 IHα [ erg s−1 sr−1 ] +(10) 13 AHα refers to the extinction (in magnitudes) of Hα emission by dust.”
BackgroundMethodInfluentialSelf-citationDUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS
Kennicutt, R. C., Hao, C.-N., Calzetti, D., Moustakas, J., Dale, D. A., Bendo, G., Engelbracht, C. W., Johnson, B. D., & Lee, J. C. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/703/2/1672 · Cited by 604 · cited 15×
“Note that the Calzetti et al. (2010) results are partially anchored to the Kennicutt et al. (2009) results, which we consider somewhat uncertain for these targets.”
BackgroundMethodResultInfluentialMOLECULAR GAS AND STAR FORMATION IN NEARBY DISK GALAXIES
Leroy, A., Walter, F., Sandstrom, K., Schruba, A., Muńoz-Mateos, J., Bigiel, F., Bolatto, A., Brinks, E., de Blok, W. D., Meidt, S., et al. (2013) · The Astronomical Journal · doi:10.1088/0004-6256/146/2/19 · Cited by 492
Self-citationRE-EXAMINING LARSON'S SCALING RELATIONSHIPS IN GALACTIC MOLECULAR CLOUDS
Heyer, M., Krawczyk, C., Duval, J., & Jackson, J. (2008) · The Astrophysical Journal · doi:10.1088/0004-637x/699/2/1092 · Cited by 460 · cited 1×
“This value is intermediate among recent determinations of the Milky Way αCO (e.g., Strong & Mattox 1996; Dame et al. 2001; Heyer et al. 2009; Abdo et al. 2010) and represents a commonly adopted ”best single value” for work on nearby disk galaxies (e.g., Wong & Blitz 2002; Leroy et al. 2008).”
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Items 201–202 of 202
Eibensteiner, C., Leroy, A. K., Sun, J., Rosolowsky, E. W., Koch, E. W., Pingel, N. M., Kim, C., Chomiuk, L. B., Chown, R., Bolatto, A. D., et al. (2026) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ae9080
“In that case, the contamination will have a distribution that reflects both the location of the ISM material and the radiation field ( e.g., see A. K. Leroy et al. 2012, 2023 ) .”
Self-citationPolimera, M., Kannappan, S. J., Richardson, C. T., Stark, D. V., Eckert, K., Jarrett, T. H., Carr, D. S., Hutchens, Z. L., Bellovary, J., & Norris, M. A. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae9baf
Metadata
- Authors
- Leroy, A. K., Bigiel, F., de Blok, W. J. G., Boissier, S., Bolatto, A., Brinks, E., Madore, B., Munoz-Mateos, J.-C., Murphy, E., Sandstrom, K., Schruba, A., & Walter, F.
- Affiliations
- National Radio Astronomy Observatory (US)
- University of Cape Town (ZA)
- Centre National de la Recherche Scientifique (FR)
- University of Maryland, College Park (US)
- University of Hertfordshire (GB)
- Carnegie Institution for Science (US)
- Max Planck Institute for Astronomy (DE)
- Venue
- The Astronomical Journal
- Publisher
- American Astronomical Society
- Published
- 2012-05-24
- Volume
- 144
- Issue
- 1
- Pages
- 3
- ISSN
- 0004-6256 (ISSN-L)
- 1538-3881
- OpenAlex
- W2140570487
- Cited by
- 203
- References
- 51
- Citations by year
- 2026: 9 · 2025: 7 · 2024: 8 · 2023: 15 · 2022: 10 · 2021: 8 · 2020: 10 · 2019: 16 · 2018: 13 · 2017: 20 · 2016: 19 · 2015: 19 · 2014: 20 · 2013: 22 · 2012: 7
- FWCI
- 11.91
- Type
- journal article
- Language
- en
- Open access
- green
- hal.science
- Locations
- The Astronomical Journal (publishedVersion)
- University of Hertfordshire Research Archive (University of Hertfordshire) (acceptedVersion)
- HAL (submittedVersion)
- arXiv (Cornell University) (submittedVersion)
- University of Hertfordshire Research Archive (University of Hertfordshire) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Science Foundation (0955836, NAS 5-26555)
- National Aeronautics and Space Administration (NAS 526555, 526555)
- Research Corporation for Science Advancement
- California Institute of Technology
- Aspen Center for Physics
- Space Telescope Science Institute (NAS5- 26555, 5-26555, 26555)
- Jet Propulsion Laboratory
- Science and Technology Facilities Council (ST/G002630/1)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- star formation rate surface density, 24 micron emission, SFR calibration, H-alpha emission, ultraviolet emission, infrared emission, spectral energy distribution, simple stellar populations
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