100 <i>μ</i>m and 160 <i>μ</i>m emission as resolved star-formation rate estimators in M 33 (HERM33ES)

Boquien, M.; Calzetti, Daniela; Krämer, C.; Xilouris, E. M.; Bertoldi, F.; Braine, J.; Buchbender, C.; Combes, F.; Israel, F. P.; Koribalski, B. S.; Lord, S. D.; Quintana-Lacaci, G.; Relaño, M.; Röllig, M.; Stacey, G. J.; Tabatabaei, F. S.; Tilanus, R. P. J.; Tak, F. F. S. van der; Werf, P. van der; Verley, S.

doi:10.1051/0004-6361/201014649

Cited by 34 publications

(43 citation statements)

References 37 publications

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“…For the dust emission, we use Herschel observations taken in the context of the HERM33ES open time key project in combination with Spitzer MIPS data (Verley et al 2007), spanning wavelengths from 24 μm to 500 μm. The Herschel PACS data covering the 100 μm and 160 μm bands have been described in Boquien et al (2010Boquien et al ( , 2011. The SPIRE observations obtained at 250, 350, and 500 μm are displayed in Kramer et al (2010) and Verley et al (2010).…”

Section: Observational Datamentioning

confidence: 99%

Dust and gas power spectrum in M 33 (HERM33ES)

Combes

Boquien

Krämer

et al. 2012

A&A

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Power spectra of deprojected images of late-type galaxies in gas or dust emission are very useful diagnostics of the dynamics and stability of their interstellar medium. Previous studies have shown that the power spectra can be approximated as two power laws, a shallow one on large scales (larger than 500 pc) and a steeper one on small scales, with the break between the two corresponding to the line-of-sight thickness of the galaxy disk. The break separates the 3D behavior of the interstellar medium on small scales, controlled by star formation and feedback, from the 2D behavior on large scales, driven by density waves in the disk. The break between these two regimes depends on the thickness of the plane, which is determined by the natural self-gravitating scale of the interstellar medium. We present a thorough analysis of the power spectra of the dust and gas emission at several wavelengths in the nearby galaxy M 33. In particular, we use the recently obtained images at five wavelengths by PACS and SPIRE onboard Herschel. The wide dynamical range (2-3 dex in scale) of most images allows us to clearly determine the change in slopes from −1.5 to −4, with some variations with wavelength. The break scale increases with wavelength from 100 pc at 24 and 100 μm to 350 pc at 500 μm, suggesting that the cool dust lies in a thicker disk than the warm dust, perhaps because of star formation that is more confined to the plane. The slope on small scales tends to be steeper at longer wavelength, meaning that the warmer dust is more concentrated in clumps. Numerical simulations of an isolated late-type galaxy, rich in gas and with no bulge, such as M 33, are carried out to better interpret these observed results. Varying the star formation and feedback parameters, it is possible to obtain a range of power spectra, with two power-law slopes and breaks, that nicely bracket the data. The small-scale power-law does indeed reflect the 3D behavior of the gas layer, steepening strongly while the feedback smoothes the structures by increasing the gas turbulence. M 33 appears to correspond to a fiducial model with an SFR of ∼0.7 M /yr, with 10% supernovae energy coupled to the gas kinematics.

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Section: Observational Datamentioning

confidence: 99%

Dust and gas power spectrum in M 33 (HERM33ES)

Combes

Boquien

Krämer

et al. 2012

A&A

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“…These sources are mainly HII regions situated in the spiral arms showing enhanced star-formation activity. A detailed analysis of the properties of these sources is presented in Verley et al (2010) as well as in Boquien et al (2010). The emission was modeled with two modified blackbodies of β = 1.5 and fitted to the MIPS 24 and 70 μm, PACS 100 and 160 μm, and SPIRE 250, 350, and 500 μm observations.…”

Section: Morphologymentioning

confidence: 99%

Cool and warm dust emission from M 33 (HerM33es)

Xilouris

Tabatabaei

Boquien

et al. 2012

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In the framework of the open-time key program "Herschel M 33 extended survey (HerM33es)", we study the far-infrared emission from the nearby spiral galaxy M 33 in order to investigate the physical properties of the dust such as its temperature and luminosity density across the galaxy. Taking advantage of the unique wavelength coverage (100, 160, 250, 350, and 500 μm) of the Herschel Space Observatory and complementing our dataset with Spitzer-IRAC 5.8 and 8 μm and Spitzer-MIPS 24 and 70 μm data, we construct temperature and luminosity density maps by fitting two modified blackbodies of a fixed emissivity index of 1.5. We find that the "cool" dust grains are heated to temperatures of between 11 K and 28 K, with the lowest temperatures being found in the outskirts of the galaxy and the highest ones both at the center and in the bright HII regions. The infrared/submillimeter total luminosity (5-1000 μm) is estimated to be 1.9 × 10 9 +4.0×10 8 −4.4×10 8 L . Fifty-nine percent of the total infrared/submillimeter luminosity of the galaxy is produced by the "cool" dust grains (∼15 K), while the remaining 41% is produced by "warm" dust grains (∼55 K). The ratio of the cool-to-warm dust luminosity is close to unity (within the computed uncertainties), throughout the galaxy, with the luminosity of the cool dust being slightly higher at the center than the outer parts of the galaxy. Decomposing the emission of the dust into two components (one emitted by the diffuse disk of the galaxy and one emitted by the spiral arms), we find that the fraction of the emission from the disk in the mid-infrared (24 μm) is 21%, while it gradually rises up to 57% in the submillimeter (500 μm). We find that the bulk of the luminosity comes from the spiral arm network that produces 70% of the total luminosity of the galaxy with the rest coming from the diffuse dust disk. The "cool" dust inside the disk is heated to temperatures in a narrow range between 18 K and 15 K (going from the center to the outer parts of the galaxy).

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“…We also use the Spitzer MIPS 24 μm map presented by Tabatabaei et al (2007), the KPNO Hα map (Hoopes & Walterbos 2000), and the HerM33es PACS and SPIRE maps at 100, 160, 250, 350, and 500 μm Verley et al 2010;Boquien et al 2010). The angular resolution of the 100 and 160 μm PACS maps are ∼6 and 12 .…”

Section: Complementary Data For Comparisonmentioning

confidence: 99%

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

Mookerjea

Krämer

Buchbender

et al. 2011

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ContextResults. The [C ii] line observed with HIFI is significantly broader than that of CO, and slightly blue-shifted. In addition, there is little spatial correlation between [C ii] observed with PACS and CO over the mapped region. There is even less spatial correlation between [C ii] and the atomic gas traced by H i. Detailed comparison of the observed intensities towards the H ii region with models of photo-ionization and photon-dominated regions, confirms that a significant fraction, 20-30%, of the observed [C ii] emission stems from the ionized gas and not from the molecular cloud. The gas heating efficiency, using the ratio of [C ii] to the TIR as a proxy, varies between 0.07 and 1.5%, with the largest variations found outside the H ii region.

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

Cited by 34 publications

References 37 publications

Dust and gas power spectrum in M 33 (HERM33ES)

Dust and gas power spectrum in M 33 (HERM33ES)

Cool and warm dust emission from M 33 (HerM33es)

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

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