The Calibration of Monochromatic Far-Infrared Star Formation Rate Indicators

Calzetti, Daniela; Wu, Szu-Ying; Hong, Sungryong; Kennicutt, Robert C.; Lee, Janice; Dale, Daniel A.; Engelbracht, C. W.; Zee, Liese van; Draine, B. T.; Hao, Cai-Na; Gordon, K. D.; Moustakas, John; Murphy, E. J.; Regan, Michael W.; Begum, Ayesha; Block, M.; Dalcanton, Julianne J.; Funes, J. G.; Paz, A. Gil de; Johnson, Benjamin D.; Sakai, Shoko; Skillman, Evan D.; Walter, Fabian; Weisz, Daniel R.; Williams, Benjamin F.; Wu, Yanling

doi:10.1088/0004-637x/714/2/1256

Cited by 351 publications

(581 citation statements)

References 129 publications

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“…We notice that the 100 μm relation is nearly linear, whereas the 160 μm relation is slightly superlinear. This is similar to what Calzetti et al (2010) found (Eq. (23)), even though individual star-forming regions probe a much smaller range of Σ SFR .…”

Section: μM and 160 μM As Sfr Estimatorssupporting

confidence: 92%

“…For comparison additional integrated galaxies are also plotted: SINGS (Spitzer Infrared Nearby Galaxies Survey, Dale et al 2007, red crosses), LVL (Local Volume Legacy survey, Dale et al 2009, green squares), starburst galaxies from Engelbracht et al (2008) (blue triangles) and LIRGs (luminous infrared galaxies, Calzetti et al 2010, cyan circles). These galaxies belong to the high-metallicity bin of Calzetti et al (2010), which encloses the metallicity of M 33 (Magrini et al 2010). The best fit of selected star-forming regions in M 33, taking into account the uncertainties on both axes, is plotted with a solid black line.…”

Section: Flux Measurementsmentioning

confidence: 99%

“…4.1 assuming an extinction E(B − V) = 0.25, set to reproduce the observed Σ Hα /Σ 24 . Finally the dotted line represents the best fit determined by Calzetti et al (2010) for entire galaxies.…”

Section: Flux Measurementsmentioning

confidence: 99%

“…The ionising flux is determined using Starburst99 (Leitherer et al 1999) with a Kroupa (2001) Calzetti et al (2010) showed that for entire galaxies the emission at 160 μm correlates linearly with Σ S FR . To compare this with the emission of entire galaxies at 100 μm and 160 μm, we plotted in Fig.…”

Section: Modelingmentioning

confidence: 99%

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100 μm and 160 μm emission as resolved star-formation rate estimators in M 33 (HERM33ES)

Boquien¹,

Calzetti²,

Krämer

et al. 2010

A&A

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Context. Over the past few years several studies have provided estimates of the SFR (star-formation rate) or the total infrared luminosity from just one infrared band. However these relations are generally derived for entire galaxies, which are known to contain a large scale diffuse emission that is not necessarily related to the latest star-formation episode. Aims. We provide new relations to estimate the SFR from resolved star-forming regions at 100 μm and 160 μm. Methods. We select individual star-forming regions in the nearby (840 kpc) galaxy M 33. We estimate the SFR combining the emission in Hα and at 24 μm to calibrate the emission at 100 μm and 160 μm as SFR estimators, as mapped with PACS/Herschel. The data are obtained in the framework of the HERM33ES open time key program. Results. There is less emission in the HII regions at 160 μm than at 100 μm. Over a dynamic range of almost 2 dex in Σ S FR we find that the 100 μm emission is a nearly linear estimator of the SFR, whereas that at 160 μm is slightly superlinear. Conclusions. The behaviour of individual star-forming regions is surprisingly similar to that of entire galaxies. At high Σ S FR , star formation drives the dust temperature, whereas uncertainties and variations in radiation-transfer and dust-heated processes dominate at low Σ S FR . Detailed modelling of both galaxies and individual star forming regions will be needed to interpret similarities and differences between the two and assess the fraction of diffuse emission in galaxies.

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Section: μM and 160 μM As Sfr Estimatorssupporting

confidence: 92%

Section: Flux Measurementsmentioning

confidence: 99%

Section: Flux Measurementsmentioning

confidence: 99%

Section: Modelingmentioning

confidence: 99%

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100 μm and 160 μm emission as resolved star-formation rate estimators in M 33 (HERM33ES)

Boquien¹,

Calzetti²,

Krämer

et al. 2010

A&A

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“…Instead, the vast majority of the starforming spirals identified by Herschel and Spitzer lie in the blue cloud, indicating that, at least in the cluster core, the identification of red sequence and blue cloud populations with passive and star-forming galaxy populations is largely valid in the infrared. We used the star formation rate (SFR) calibration of Calzetti et al (2010), which uses L(24 μm) and L(Hα) to measure the obscured and unobscured components of star formation in a galaxy. The Hα luminosities of each galaxy were obtained using Eq.…”

Section: Spatial Distribution Of Star-forming Galaxiesmentioning

confidence: 99%

LoCuSS: Shedding new light on the massive lensing cluster Abell 1689 – the view fromHerschel

Haines¹,

Smith²,

Pereira

et al. 2010

A&A

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We present wide-field Herschel/PACS observations of A 1689, a massive galaxy cluster at z = 0.1832, from our open time key programme. We detect 39 spectroscopically confirmed 100 μm-selected cluster members down to 1.5 × 10 10 L . These galaxies are forming stars at rates in the range 1-10 M /yr, and appear to comprise two distinct populations: two-thirds are unremarkable blue, late-type spirals found throughout the cluster; the remainder are dusty red sequence galaxies whose star formation is heavily obscured with A(Hα) ∼ 2 mag and are found only in the cluster outskirts. The specific-SFRs of these dusty red galaxies are lower than the blue late-types, suggesting that the former are in the process of being quenched, perhaps via pre-processing, the unobscured star formation being terminated first. We also detect an excess of 100 μm-selected galaxies extending ∼6 Mpc in length along an axis that runs NE-SW through the cluster center at > ∼ 95% confidence. Qualitatively this structure is consistent with previous reports of substructure in X-ray, lensing, and near-infrared maps of this cluster, further supporting the view that this cluster is a dynamically active, merging system.

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Star formation rates and the kinematics of gas in the spiral arms of NGC 628

2015

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Relations between star formation rates along the spiral arms and the velocities of gas inflow into the arms in grand-design galaxy NGC 628 were studied. We found that the radial distribution of average star formation rate in individual star formation regions in regular spiral arms correlates with the velocity of gas inflow into the spiral arms. Both distributions have maxima at a galactocentric distance of 4.5-5 kpc. There are no correlations between the radial distributions of average star formation rate in star formation regions in spiral arms and outside spiral arms in the main disc. We also did not find a correlation between the radial distribution of average star formation rate in star formation regions in spiral arms and H I column density.

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The Calibration of Monochromatic Far-Infrared Star Formation Rate Indicators

Abstract: 1 Based on observations obtained with the Spitzer Space Telescope, which is operated by JPL, CalTech, under NASA Contract 1407.

Cited by 351 publications

References 129 publications

100 μm and 160 μm emission as resolved star-formation rate estimators in M 33 (HERM33ES)

100 μm and 160 μm emission as resolved star-formation rate estimators in M 33 (HERM33ES)

LoCuSS: Shedding new light on the massive lensing cluster Abell 1689 – the view fromHerschel

Star formation rates and the kinematics of gas in the spiral arms of NGC 628

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