The opacity of spiral galaxy disks: IX. Dust and gas surface densities

Holwerda, Benne W.; Allen, R. J.; Blok, W. J. G. de; Bouchard, Antoine; González-Lópezlira, Rosa A.; Kruit, P.; Leroy, Adam K.

doi:10.1002/asna.201211713

Cited by 9 publications

(7 citation statements)

References 113 publications

(163 reference statements)

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“…The faceon optical depths found are typically smaller than one at optical wavelengths, indicating that the entire galaxy disc would be almost transparent when seen face-on. This result is somewhat in contradiction to the spiral disc transparency measurements using either the number of background galaxies (Holwerda et al 2005a(Holwerda et al , 2007b or overlapping galaxy pairs (Domingue et al 2000;Keel & White 2001a,b;Holwerda et al 2009Holwerda et al , 2013. These studies find that spiral arms are opaque and discs gradually become optically thick towards the galaxy's centre.…”

Section: Introductionmentioning

confidence: 56%

HERschelObservations of Edge-on Spirals (HEROES)

Verstappen

Fritz

Baes

et al. 2013

A&A

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Context. Edge-on spiral galaxies with prominent dust lanes provide us with an excellent opportunity to study the distribution and properties of the dust within them. The HEROES project was set up to observe a sample of seven large edge-on galaxies across various wavelengths for this investigation. Aims. Within this first paper, we present the Herschel observations and perform a qualitative and quantitative analysis on them, and we derive some global properties of the far infrared and submillimetre emission. Methods. We determine horizontal and vertical profiles from the Herschel observations of the galaxies in the sample and describe the morphology. Modified black-body fits to the global fluxes, measured using aperture photometry, result in dust temperatures and dust masses. The latter values are compared to those that are derived from radiative transfer models taken from the literature. Results. On the whole, our Herschel flux measurements agree well with archival values. We find that the exponential horizontal dust distribution model often used in the literature generally provides a good description of the observed horizontal profiles. Three out of the seven galaxies show signatures of extended vertical emission at 100 and 160 μm at the 5σ level, but in two of these it is probably due to deviations from an exactly edge-on orientation. Only for NGC 4013, a galaxy in which vertically extended dust has already been detected in optical images, we can detect vertically extended dust, and the derived scaleheight agrees with the value estimated through radiative transfer modelling. Our analysis hints at a correlation between the dust scaleheight and its degree of clumpiness, which we infer from the difference between the dust masses as calculated from modelling of optical data and from fitting the spectral energy distribution of Herschel datapoints.

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Section: Introductionmentioning

confidence: 56%

HERschelObservations of Edge-on Spirals (HEROES)

Verstappen

Fritz

Baes

et al. 2013

A&A

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“…Indeed, direct observations of galaxies have indicated that the intrinsic nature of dust in galaxies is highly variable, depending on multiple factors such as morphology and environment (see, e.g. , White et al 2000;Keel & White 2001;Holwerda 2005;Holwerda et al 2013a,b).…”

Section: Introductionmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): the galaxy stellar mass function to z = 0.1 from the r-band selected equatorial regions

Wright

Robotham

Driver

et al. 2017

Monthly Notices of the Royal Astronomical Society

110

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We derive the low redshift galaxy stellar mass function (GSMF), inclusive of dust corrections, for the equatorial Galaxy And Mass Assembly (GAMA) dataset covering 180 deg 2 . We construct the mass function using a density-corrected maximum volume method, using masses corrected for the impact of optically thick and thin dust. We explore the galactic bivariate brightness plane (M − µ), demonstrating that surface brightness effects do not systematically bias our mass function measurement above 10 7.5 M . The galaxy distribution in the M −µ-plane appears well bounded, indicating that no substantial population of massive but diffuse or highly compact galaxies are systematically missed due to the GAMA selection criteria. The GSMF is fit with a double Schechter function, with M = 10 10.78±0.01±0.20 M , φ 1 = (2.93 ± 0.40) × 10 −3 h 3 70 Mpc −3 , α 1 = −0.62 ± 0.03 ± 0.15, φ 2 = (0.63 ± 0.10) × 10 −3 h 3 70 Mpc −3 , and α 2 = −1.50±0.01±0.15. We find the equivalent faint end slope as previously estimated using the GAMA-I sample, although we find a higher value of M . Using the full GAMA-II sample, we are able to fit the mass function to masses as low as 10 7.5 M , and assess limits to 10 6.5 M . Combining GAMA-II with data from G10-COSMOS we are able to comment qualitatively on the shape of the GSMF down to masses as low as 10 6 M . Beyond the well known upturn seen in the GSMF at 10 9.5 the distribution appears to maintain a single power-law slope from 10 9 to 10 6.5 . We calculate the stellar mass density parameter given our best-estimate GSMF, finding Ω = 1.66 +0.24 −0.23 ± 0.97h −1 70 × 10 −3 , inclusive of random and systematic uncertainties.

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“…The face-on optical depths found are typically smaller than one at optical wavelengths, indicating that the entire galaxy disc would be almost transparent when seen face-on. This result is somewhat in contradiction to the spiral disc transparency measurements using either the number of background galaxies (Holwerda et al 2005a(Holwerda et al , 2007b or overlapping galaxy pairs (Domingue et al 2000;Keel & White 2001a,b;Holwerda et al 2009Holwerda et al , 2013. These studies find that spiral arms are opaque and discs gradually become optically thick towards the galaxy's centre.…”

Section: Introductionmentioning

confidence: 56%

HERschel Observations of Edge-on Spirals (HEROES). I: Far-infrared morphology and dust mass determination

Verstappen,

Fritz,

Baes

et al. 2013

Preprint

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Context. Edge-on spiral galaxies with prominent dust lanes provide us with an excellent opportunity to study the distribution and properties of the dust within them. The HEROES project was set up to observe a sample of seven large edge-on galaxies across various wavelengths for this investigation. Aims. Within this first paper, we present the Herschel observations and perform a qualitative and quantitative analysis on them, and we derive some global properties of the far infrared and submillimetre emission. Methods. We determine horizontal and vertical profiles from the Herschel observations of the galaxies in the sample and describe the morphology. Modified black-body fits to the global fluxes, measured using aperture photometry, result in dust temperatures and dust masses. The latter values are compared to those that are derived from radiative transfer models taken from the literature. Results. On the whole, our Herschel flux measurements agree well with archival values. We find that the exponential horizontal dust distribution model often used in the literature generally provides a good description of the observed horizontal profiles. Three out of the seven galaxies show signatures of extended vertical emission at 100 and 160 µm at the 5σ level, but in two of these it is probably due to deviations from an exactly edge-on orientation. Only for NGC 4013, a galaxy in which vertically extended dust has already been detected in optical images, we can detect vertically extended dust, and the derived scaleheight agrees with the value estimated through radiative transfer modelling. Our analysis hints at a correlation between the dust scaleheight and its degree of clumpiness, which we infer from the difference between the dust masses as calculated from modelling of optical data and from fitting the spectral energy distribution of Herschel datapoints.

show abstract

The opacity of spiral galaxy disks: IX. Dust and gas surface densities

Cited by 9 publications

References 113 publications

HERschelObservations of Edge-on Spirals (HEROES)

HERschelObservations of Edge-on Spirals (HEROES)

Galaxy And Mass Assembly (GAMA): the galaxy stellar mass function to z = 0.1 from the r-band selected equatorial regions

HERschel Observations of Edge-on Spirals (HEROES). I: Far-infrared morphology and dust mass determination

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