The spiral galaxy M 33 mapped in the FIR by ISOPHOT

Hippelein, H.; Haas, Martín; Tuffs, R.; Lemke, D.; Stickel, M.; Klaas, U.; Völk, H. J.

doi:10.1051/0004-6361:20030769

Cited by 91 publications

(140 citation statements)

References 29 publications

Supporting

Mentioning

119

Contrasting

Order By: Relevance

“…The absolute calibration uncertainty is 5% at 100 μm and 10% at 160 μm. The total fluxes of M 33 agree to within a few percent with those from ISO (Hippelein et al 2003) and MIPS. In addition, for all radial averages the PACS 160 flux is within 20% of the MIPS 160 one.…”

Section: Pacssupporting

confidence: 57%

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

Boquien¹,

Calzetti²,

Krämer

et al. 2010

A&A

View full text Add to dashboard Cite

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.

show abstract

Section: Pacssupporting

confidence: 57%

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

Boquien¹,

Calzetti²,

Krämer

et al. 2010

A&A

View full text Add to dashboard Cite

show abstract

“…A&A 518, L67 (2010) In this first HERM33ES paper, we use continuum maps covering the full extent of M 33, at 100, 160, 250, 350, and 500 μm. These data are an improvement over previous data sets of M 33, obtained with ISO and Spitzer (Hippelein et al 2003;Hinz et al 2004;Tabatabaei et al 2007), in terms of wavelength coverage and angular resolution.…”

Section: Introductionmentioning

confidence: 52%

PACS and SPIRE photometer maps of M 33: First results of theHERschel M 33 Extended Survey (HERM33ES)

Krämer¹,

Buchbender²,

Xilouris

et al. 2010

A&A

View full text Add to dashboard Cite

Context. Within the framework of the HERM33ES key program, we are studying the star forming interstellar medium in the nearby, metal-poor spiral galaxy M 33, exploiting the high resolution and sensitivity of Herschel. Aims. We use PACS and SPIRE maps at 100, 160, 250, 350, and 500 μm wavelength, to study the variation of the spectral energy distributions (SEDs) with galacto-centric distance. Methods. Detailed SED modeling is performed using azimuthally averaged fluxes in elliptical rings of 2 kpc width, out to 8 kpc galacto-centric distance. Simple isothermal and two-component grey body models, with fixed dust emissivity index, are fitted to the SEDs between 24 μm and 500 μm using also MIPS/Spitzer data, to derive first estimates of the dust physical conditions. Results. The far-infrared and submillimeter maps reveal the branched, knotted spiral structure of M 33. An underlying diffuse disk is seen in all SPIRE maps (250-500 μm). Two component fits to the SEDs agree better than isothermal models with the observed, total and radially averaged flux densities. The two component model, with β fixed at 1.5, best fits the global and the radial SEDs. The cold dust component clearly dominates; the relative mass of the warm component is less than 0.3% for all the fits. The temperature of the warm component is not well constrained and is found to be about 60 K ± 10 K. The temperature of the cold component drops significantly from ∼24 K in the inner 2 kpc radius to 13 K beyond 6 kpc radial distance, for the best fitting model. The gas-to-dust ratio for β = 1.5, averaged over the galaxy, is higher than the solar value by a factor of 1.5 and is roughly in agreement with the subsolar metallicity of M 33.

show abstract

“…0.05 mag) or the average metallicity (≤0.15 dex; see Table 2). According to the detailed dust maps of M 33 by Hippelein et al (2003) the effect of the intrinsic extinction should be negligible in the fields considered here.…”

Section: Trgb Distancementioning

confidence: 91%

The distance of M 33 and the stellar population in its outskirts

Galleti¹,

Bellazzini²,

Ferraro³

2004

A&A

View full text Add to dashboard Cite

Abstract. We present deep V, I photometry of two 9.4 × 9.4 field in the outer regions of the M 33 galaxy. We obtain a robust detection of the luminosity of the Red Giant Branch Tip (I TRGB = 20.72 ± 0.08) from which we derived a new estimate of Our observations demonstrate that Red Giant Branch and Asymptotic Giant Branch stars have a radial distribution that is much more extended than the young MS stars associated with the star-forming disc.

show abstract

The spiral galaxy M 33 mapped in the FIR by ISOPHOT

Cited by 91 publications

References 29 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)

PACS and SPIRE photometer maps of M 33: First results of theHERschel M 33 Extended Survey (HERM33ES)

The distance of M 33 and the stellar population in its outskirts

Contact Info

Product

Resources

About