Ultraviolet Extinction by Interstellar Dust in External Galaxies: M31

Bianchi, Luciana; Clayton, Geoffrey C.; Bohlin, R. C.; Hutchings, J. B.; Massey, Philip

doi:10.1086/177963

Cited by 102 publications

(103 citation statements)

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“…This finding is in accordance with the result of Bianchi et al (1996) who emphasized a low possibility for a weaker 2175 Å bump in M 31 extinction curve toward young blue stars in associations, infering R V > 4 as well. On the other hand, one has to point out the limited applicability of R 2490 value as an extinction law (R V ) indicator.…”

Section: Discussionsupporting

confidence: 93%

Initial mass function in the South-Western part of M 31

Veltchev

Nedialkov

Borisov

2004

A&A

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Abstract.We derive an average initial mass function (IMF) for 50 OB associations in the South-Western part of Andromeda galaxy, combining ultraviolet photometry of Hill et al. (1995, ApJ, 98, 595) and two datasets HST photometry with JHK s photometry from the 2MASS + I band photometry from Magnier et al. (1992, A&A, 96, 379). The mean extinctions within the associations were estimated in two independent ways and the stellar masses were determined by use of probabilistic techniques. The derived slope of the IMF Γ = −1.59 ± 0.09 is close to the universal Salpeter's law and to recent estimates for massive stars' IMF in the Galaxy and in the Magellanic Clouds.

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Section: Discussionsupporting

confidence: 93%

Initial mass function in the South-Western part of M 31

Veltchev

Nedialkov

Borisov

2004

A&A

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“…The 6.2 µm absorption feature in the Weingartner & Draine (2001a) grain models is due to PAHs. Bianchi et al (1996) present UV extinction curves toward selected bright stars in M31, finding an extinction law similar to the average Milky Way extinction curve, but with the 2175Å feature possibly somewhat weaker than in the Milky Way.…”

Section: Drainementioning

confidence: 68%

Interstellar Dust Grains

Draine

2003

Annu. Rev. Astron. Astrophys.

2,209

2,214

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This review surveys the observed properties of interstellar dust grains: the wavelength-dependent extinction of starlight, including absorption features, from UV to infrared; optical luminescence; infrared emission; microwave emission; optical, UV, and X-ray scattering by dust; and polarization of starlight and of infrared emission. The relationship between presolar grains in meteorites and the interstellar grain population is discussed. Candidate grain materials and abundance constraints are considered. A dust model consisting of amorphous silicate grains, graphite grains, and polycyclic aromatic hydrocarbons is compared with observed emission and scattering. Some issues concerning evolution of interstellar dust are discussed.

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“…While we did not try to apply these models to our data, we observe that at least the first two scenarios do not seem to be applicable to M31. Bianchi et al (1996) found that the M31 extinction curve is very similar to the average Galactic extinction law and a possible reduction in the 2175 Å bump is significant only at the 1σ level. Similar results were also reached in previous studies (e.g., Walterbos & Kennicutt 1988).…”

Section: Which Sources Are Responsible For the Dust Heating In M31?mentioning

confidence: 74%

Properties of M31

Montalto¹,

Seitz²,

Riffeser³

et al. 2009

A&A

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Aims. Observations acquired by the Spitzer Space Telescope and improvements to theoretical modeling of dust emission properties are used to discuss the distribution of dust and its characteristics in the closest neighbor spiral galaxy M31. These data are then used with GALEX FUV, NUV, and SDSS images to study the age dependence of the dust heating process. Methods. Spitzer IRAC/MIPS maps of M31 were matched together and compared to dust emission models allowing us to constrain the dust mass, the intensity of the mean radiation field, the abundance of polycyclic aromatic hydrocarbon (PAH) particles. The total infrared emission (TIR) was analyzed as a function of UV and optical colors and compared to predictions of models that consider age-dependent dust heating. Results. We demonstrate that cold-dust component emission dominates the infrared spectral energy distribution of M31. The mean intensity of the radiation field heating the dust is low (typically U < 2, where U = 1 is the value in the solar neighborhood). Because of a lack of submillimeter observations, the dust mass (M dust ) is only weakly constrained by the infrared spectrum, but we derived a lower limit of M dust 1.1 × 10 7 M with a best-fit model value of M dust = 7.6 × 10 7 M , in good agreement with expectations from CO and HI measurements. Across the spiral-ring structure of M31, we show that a fraction >3% of the total dust mass is in PAHs. UV and optical colors are correlated with the total infrared to far ultraviolet (TIR/FUV) ratios in ∼670 pc-sized regions over the disk of M31, although deviating from the relationship between infrared excess and ultraviolet spectral slope (referred as IRX-β relationship) for starburst galaxies. In particular, redder regions have lower values of the TIR/FUV ratio for a fixed color. Considering the predictions of models that account for the dust-heating age dependence, we found that in 83% of the regions analyzed across the 10 kpc ring, more than 50% of the energy absorbed by the dust is rediated at λ > 4000 Å and that dust in M31 appears mainly heated by populations a few Gyr old even across the star-forming ring. We also found that the attenuation varies radially peaking close to 10 kpc and decreases more rapidly with radius in the inner regions of M31 than in the outer regions in agreement with previous studies. We finally derived the attenuation map of M31 at 6 /px resolution (∼100 pc/px along the plane of M31). Conclusions.

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Ultraviolet Extinction by Interstellar Dust in External Galaxies: M31

Cited by 102 publications

References 0 publications

Initial mass function in the South-Western part of M 31

Initial mass function in the South-Western part of M 31

Interstellar Dust Grains

Properties of M31

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