Dust and ionized gas association in E/S0 galaxies with dust lanes: clues to their origin

Finkelman, Ido; Brosch, Noah; Funes, Guillermo; Barway, Sudhanshu; Knyazev, A. Yu.; Vaïsänen, P.

doi:10.1111/j.1365-2966.2012.20710.x

Cited by 23 publications

(37 citation statements)

References 93 publications

(191 reference statements)

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“…Not surprisingly, by using optical images, we underestimated the dust mass for most of the sample ETGs, which is similar to what was found in previous studies (e.g. Patil et al 2007;Finkelman et al 2012;Kaviraj et al 2012;Viaene et al 2015). Fig.…”

Section: Dust Masssupporting

confidence: 90%

Cold gas and dust: Hunting spiral-like structures in early-type galaxies

Yıldız

Peletier

Duc

et al. 2020

A&A

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Context. Observations of neutral hydrogen (H I) and molecular gas show that 50% of all nearby early-type galaxies contain some cold gas. Molecular gas is always found in small gas discs in the central region of the galaxy, while neutral hydrogen is often distributed in a low-column density disc or ring typically extending well beyond the stellar body. Dust is frequently found in early-type galaxies as well. Aims. The goal of our study is to understand the link between dust and cold gas in nearby early-type galaxies as a function of H I content.Methods. We analyse deep optical g − r images obtained with the MegaCam camera at the Canada-France-Hawaii Telescope for a sample of 21 H I-rich and 41 H I-poor early-type galaxies.Results. We find that all H I-rich galaxies contain dust seen as absorption. Moreover, in 57 per cent of these H I-rich galaxies, the dust is distributed in a large-scale spiral pattern. Although the dust detection rate is relatively high in the H I-poor galaxies (∼59 per cent), most of these systems exhibit simpler dust morphologies without any evidence of spiral structures. We find that the H I-rich galaxies possess more complex dust morphology extending to almost two times larger radii than H I-poor objects. We measured the dust content of the galaxies from the optical colour excess and find that H I-rich galaxies contain six times more dust (in mass) than H I-poor ones. In order to maintain the dust structures in the galaxies, continuous gas accretion is needed, and the substantial H I gas reservoirs in the outer regions of early-type galaxies can satisfy this need for a long time. We find that there is a good correspondence between the observed masses of the gas and dust, and it is also clear that dust is present in regions further than 3 R eff . Conclusions. Our findings indicate an essential relation between the presence of cold gas and dust in early-type galaxies and offer a way to study the interstellar medium in more detail than what is possible with H I observations.

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Section: Dust Masssupporting

confidence: 90%

Cold gas and dust: Hunting spiral-like structures in early-type galaxies

Yıldız

Peletier

Duc

et al. 2020

A&A

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“…The extinction curve derived over optical-to-near-IR region of the electromagnetic spectrum for the dust occupied regions in Fornax A (NGC 1316) galaxy is shown in Figure 3. From this figure it is clear that the dust extinction curve plotted between the measured values of R λ = A λ E(B−V ) versus inverse of wavelength of their measurement varies linearly and follows closely the standard Galactic extinction law (Mathis et al, 1977); consistent with those derived for several other external galaxies (Goudfrooij et al, 1994;Sahu et al, 1996;Patil et al, 2001Patil et al, , 2002Patil et al, , 2003Patil et al, , 2007Patil et al, , 2009Dewangan et al, 1999;Finkelman et al, 2012;Vagshette et al, 2012a). Relatively smaller value of R λ in the case of NGC 1316 imply that, the dust grains responsible for the extinction of optical and near-IR light are smaller than the canonical grains in the Milky Way < a > < < a Gal >.…”

Section: Dust Extinctionsupporting

confidence: 84%

A multiwavelength view of the ISM in the merger remnant galaxy Fornax A

Deshmukh

Tate

Vagshette

et al. 2013

Res. Astron. Astrophys.

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We present multi-wavelength imagery of the merger remnant galaxy NGC 1316 with an objective to study the content of dust and its association with the other phases of the ISM. Color-index maps as well as extinction maps derived for this galaxy reveal an intricate and complex dust morphology in NGC 1316, i.e., in the inner part it exists in the form of a prominent lane while at about 6-7 kpc it apparently takes an arc-like pattern extended along the North-East direction. In addition to this, several other dust clumps and knots are also evident in this galaxy. Dust emission mapped using Spitzer data at 8 µm indicates even more complex morphological structures of the dust in NGC1316. The extinction curve derived over the optical to near-IR bands closely follows the standard Galactic curve suggesting similar properties of the dust grains. The dust content of NGC 1316 estimated from optical extinction is ∼ 2.13× 10 5 M ⊙ . This is a lower limit compared to that estimated using the IRAS flux densities ∼ 5.17× 10 6 M ⊙ and flux densities at 24µm, 70µm and 160 µm from MIPS ∼ 3.2× 10 7 M ⊙ . High resolution Chandra observations of this merger remnant system have provided with an unprecedented view of the complex nature of hot gas distribution in NGC 1316 which closely matches the morphology of ionized gas and to some extent with the dust also. X-ray color-color plot for the resolved sources within optical D 25 extent of NGC 1316 has enabled us to separate them in different classes.

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“…Another possibility, though, is the recent suggestion that accretion of dust that is embedded in a larger cold medium may be shielded from the harsh ISM resulting in a further significant increase in dust lifetimes (e.g. Clemens et al 2010;Dasyra et al 2012;Finkelman et al 2012). A full understanding of just how much longer dust may survive in such a scenario is beyond the scope of this work.…”

Section: Dispersion Dominated Galaxies Dust and Merger Ratesmentioning

confidence: 97%

“…Alternatively, the dust may result from internal processes such as cooling of hot halo gas (Fabian et al 1994;Bregman et al 2005;Lagos et al 2014) or production in asymptotic giant-branch (AGB) stars (Knapp 1985;Knapp et al 1992;Athey et al 2002;Matsuura et al 2009;Nanni et al 2013). Currently, there is no clear consensus regarding the internal versus external origins of dust in ETGs, and it is possible that both play some role with the balance between the two sources depending on the properties of individual galaxies (Rampazzo et al 2005;Cappellari et al 2011;Finkelman et al 2012).…”

mentioning

confidence: 99%

The SAMI Galaxy Survey: kinematics of dusty early-type galaxies

Bassett

Bekki

Cortese

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Recently, large samples of visually classified early-type galaxies (ETGs) containing dust have been identified using space-based infrared observations with the Herschel Space Telescope. The presence of large quantities of dust in massive ETGs is peculiar as X-ray halos of these galaxies are expected to destroy dust in ∼10 7 yr (or less). This has sparked a debate regarding the origin of the dust: is it internally produced by asymptotic giant branch (AGB) stars, or is it accreted externally through mergers? We examine the 2D stellar and ionised gas kinematics of dusty ETGs using IFS observations from the SAMI galaxy survey, and integrated star-formation rates, stellar masses, and dust masses from the GAMA survey. Only 8% (4/49) of visually-classified ETGs are kinematically consistent with being dispersion-supported systems. These "dispersion-dominated galaxies" exhibit discrepancies between stellar and ionised gas kinematics, either offsets in the kinematic position angle or large differences in the rotational velocity, and are outliers in star-formation rate at a fixed dust mass compared to normal star-forming galaxies. These properties are suggestive of recent merger activity. The remaining ∼90% of dusty ETGs have low velocity dispersions and/or large circular velocities, typical of "rotation-dominated galaxies". These results, along with the general evidence of published works on X-ray emission in ETGs, suggest that they are unlikely to host hot, X-ray gas consistent with their low M * when compared to dispersion-dominated galaxies. This means dust will be long lived and thus these galaxies do not require external scenarios for the origin of their dust content.

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Dust and ionized gas association in E/S0 galaxies with dust lanes: clues to their origin

Cited by 23 publications

References 93 publications

Cold gas and dust: Hunting spiral-like structures in early-type galaxies

Cold gas and dust: Hunting spiral-like structures in early-type galaxies

A multiwavelength view of the ISM in the merger remnant galaxy Fornax A

The SAMI Galaxy Survey: kinematics of dusty early-type galaxies

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