The distribution of far-infrared emission from edge-on galaxies

Alton, P. B.; Davies, Jonathan Ivor; Trewhella, M.

doi:10.1046/j.1365-8711.1998.01488.x

Cited by 29 publications

(42 citation statements)

References 18 publications

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“…The ISOPHOT data at 100 and 200 µm give a better measure of the dust temperature. T dust determined for the ISOPHOT sample, as well as for 6 quiescent galaxies observed with ISOPHOT by Alton et al (1998) consistently with Contursi et al (2001), seems to be independent of the UV radiation field as traced by the Hα + [NII]EW, of the metallicity or of the total luminosity. The average value is T dust = 20.8 ± 3.2 K, which we will assume also for galaxies without ISOPHOT measurements.…”

Section: An Alternative Methodssupporting

confidence: 58%

“…Unfortunately only integrated HI and dust masses are available for our spatially unresolved galaxies. It is however reasonable to assume that the cold dust is as extended as the optical disc (Alton et al 1998). The HI gas surface density is available only for a few galaxies in our sample from VLA observations (Cayatte et al 1994).…”

Section: An Alternative Methodsmentioning

confidence: 99%

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Molecular gas in normal late-type galaxies

Boselli

Lequeux²,

Gavazzi³

2002

A&A

219

390

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Abstract. We present 12 CO(J = 1-0) line observations of 22 low-luminosity spiral galaxies in the Virgo cluster. These data, together with 244 others available in the literature, allow us to build a large sample that we use to study the molecular gas properties of galaxies spanning a large range of morphological types and luminosities and belonging to different environments (clusters -field). The molecular gas content of the target galaxies is estimated using a luminosity-dependent X = N(H2)/I(CO) conversion factor that has been calibrated on a sample of nearby galaxies. X spans from ∼10 20 mol cm −2 (K km s −1 ) −1 in giant spirals to ∼10 21 mol cm −2 (K km s −1 ) −1 in dwarf irregulars. The value of the X conversion factor is found consistent with a value derived independently from dust masses estimated from FIR fluxes, with a metallicity-dependent dust to gas ratio. The relationships between X and the UV radiation field (as traced by the Hα + [NII]EW), the metallicity and the H band luminosity are analysed. We show that the molecular gas contained in molecular clouds or complexes is of the order of 15% of the total gas on average whatever the luminosity or the Hubble type of the galaxies. We discuss the relation between the star formation rate and the molecular gas content and estimate the average star formation efficiency of late-type galaxies.

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Section: An Alternative Methodssupporting

confidence: 58%

Section: An Alternative Methodsmentioning

confidence: 99%

Molecular gas in normal late-type galaxies

Boselli

Lequeux²,

Gavazzi³

2002

A&A

219

390

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“…According to Alton et al (1998), we interpret the steady increase in the surface brightness scale-length from 70 to 500 µm as the result of a cold-dust temperature gradient with galactocentric distance combined with a scale-length of the dust disk larger Notes. * Curve not fitted by an exponential fit within the selected range in radius; ** Profile not available.…”

Section: Discussion and Comparison With The Literaturementioning

confidence: 93%

“…With higher resolution Spitzer observations of 57 galaxies in the SINGS sample, Muñoz-Mateos et al (2009a) instead found that the distribution of the dust mass (derived from SED fits up to the longest available wavelength of 160 µm; FWHM = 38 ) has a similar scale-length to that measured for stellar emission at 3.6 µm. However, the result is not incompatible with that of Alton et al (1998), since near-IR (NIR) surface brightness profiles are steeper than in the optical.…”

Section: Introductionmentioning

confidence: 80%

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Casasola

Cassarà

Bianchi

et al. 2017

A&A

131

140

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Aims. The purpose of this work is the characterization of the radial distribution of dust, stars, gas, and star-formation rate (SFR) in a sub-sample of 18 face-on spiral galaxies extracted from the DustPedia sample. Methods. This study is performed by exploiting the multi-wavelength, from ultraviolet (UV) to sub-millimeter bands, DustPedia database, in addition to molecular ( 12 CO) and atomic (Hi) gas maps and metallicity abundance information available in the literature. We fitted the surface brightness profiles of the tracers of dust and stars, the mass surface density profiles of dust, stars, molecular gas, and total gas, and the SFR surface density profiles with an exponential curve and derived their scale-lengths. We also developed a method to solve for the CO-to-H 2 conversion factor (α CO ) per galaxy by using dust and gas mass profiles. Results. Although each galaxy has its own peculiar behaviour, we identified a common trend of the exponential scale-lengths vs. wavelength. On average, the scale-lengths normalized to the B-band 25 mag/arcsec 2 radius decrease from UV to 70 µm, from 0.4 to 0.2, and then increase back up to ∼0.3 at 500 microns. The main result is that, on average, the dust mass surface density scale-length is about 1.8 times the stellar one derived from IRAC data and the 3.6 µm surface brightness, and close to that in the UV. We found a mild dependence of the scale-lengths on the Hubble stage T: the scale-lengths of the Herschel bands and the 3.6 µm scale-length tend to increase from earlier to later types, the scale-length at 70 µm tends to be smaller than that at longer sub-mm wavelength with ratios between longer sub-mm wavelengths and 70 µm that decrease with increasing T. The scale-length ratio of SFR and stars shows a weak increasing trend towards later types. Our α CO determinations are in the range (0.3 − 9) M pc −2 (K km s −1 ) −1 , almost invariant by using a fixed dust-to-gas ratio mass (DGR) or a DGR depending on metallicity gradient.

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“…On the other hand, bright sources above 200 mJy with a red color could be dominated by very luminous galaxies such as Arp 220 at moderate redshifts. In addition, there may be a contribution from galaxies having very cold dust (Alton et al 1998;Haas et al 1998). The large errors associated with the flux calibration hampers further insight into the flux-color diagrams.…”

Section: Ir Colorsmentioning

confidence: 99%

ISO deep far-infrared survey in the “Lockman Hole”

Kawara

Matsuhara

Okuda

et al. 2004

A&A

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Abstract. We present the catalogs and source counts for the C 90 (reference wavelength of 90 µm) and C 160 (170 µm) bands, which were extracted from our analysis of an ISO deep far-infrared survey conducted as part of the Japan/UH ISO cosmology project. The total survey area is ∼0.9 deg 2 in two fields within the Lockman Hole. The analysis consists of source extraction using the IRAF DAOPHOT package and simulations carried out by adding artificial sources to the maps to estimate the detection rate, the flux bias, the positional accuracy, and the noise. The flux calibration was performed using the Sb galaxy UGC 06009 -the photometric error was estimated to be ∼50% at C 90 and ∼65% at C 160. The total noise estimated from the simulation is dominated by the confusion noise due to the high source density. The confusion noise is ∼20 mJy at C 90 and ∼35 mJy at C 160, which is much larger than the instrumental noise which is at the level of a few mJy or less. The catalogs were constructed by selecting 223 C 90 sources and 72 C 160 sources with a Signal to Noise Ratio (S NR) of three or greater. The distribution of the observed associations between C 90 and C 160 sources indicates that the 1σ positional errors are ∼20 and ∼35 at C 90 and C 160, respectively. The corrections for the detection rate and the flux bias are significant for sources fainter than 200 mJy at C 90 and 250 mJy at C 160. Most of the sources detected both at C 90 and C 160 have a F(C 160)/F(C 90) color redder than the Sb galaxy UGC 06009. Such a red color could result from reddening due to the flux bias or a K-correction brightening due to the effect of redshift. Red sources brighter than 200 mJy at C 160 may be very luminous galaxies like Arp 220 at moderate redshift. The source counts are derived by applying the corrections for the detection rate and flux bias. The resultant counts are quite consistent with the constraints derived from the fluctuation analysis performed in Paper II. The C 160 counts are also consistent with the results from the FIRBACK project. Our C 90 survey, which is 2-3 times deeper than those previously published, reveals an upturn in the count slope at around 200 mJy. While recent models give a reasonable fit to the C 160 counts, none of them are successful in accounting for the upturn in the C 90 counts. If the upturn is caused by ultraluminous IR galaxies, their redshifts would need to be at z ∼ 0.5, implying a major event in galaxy evolution at moderate redshift.

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The distribution of far-infrared emission from edge-on galaxies

Cited by 29 publications

References 18 publications

Molecular gas in normal late-type galaxies

Molecular gas in normal late-type galaxies

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

ISO deep far-infrared survey in the “Lockman Hole”

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