Interstellar matter in elliptical galaxies - III. Properties of dust extinction

Goudfrooij, Paul; Jong, T. de; Hansen, L.; Nørgaard-Nielsen, H. U.

doi:10.1093/mnras/271.4.833

Cited by 96 publications

(170 citation statements)

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“…About half the 3CR galaxies have some sort of dust feature, including irregular lanes, Ðlaments, and nuclear or large-scale disks above a threshold detection level of D3 ] 104 in dust. M _ That amount of dust is consistent with the amounts of dust found in nonactive elliptical galaxies by Goudfrooij et al (1994aGoudfrooij et al ( , 1994b and Tran et al (2001). As can be seen, therefore, these objects have dust masses 0.5È1 dex higher than those typical for elliptical galaxies and radio galaxy hosts, although nine of 46 3CR hosts are comparable to 1146]596, 4C 31.…”

Section: Discussionsupporting

confidence: 86%

“…As can be seen, all three of these galaxies have signiÐcant H I columns and dust masses typical of spiral galaxies. By comparison, elliptical galaxies typically have dust masses an order of magnitude lower (Goudfrooij et al 1994a(Goudfrooij et al , 1994b, although there are notable exceptions, including some large-scale FR II radio sources (de Ko † et al 2000 ;see also°6). In the legend of Figure 6 we note what the gray scales of each A B extinction map correspond to in terms of under the N H above assumptions.…”

Section: Obscuration Features and Distributionmentioning

confidence: 99%

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Host Galaxies, Obscuration, and Nuclear Structure of Three Nearby Compact Symmetric Objects

Perlman

Stocke

Conway

et al. 2001

The Astronomical Journal

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We present three-band Hubble Space T elescope imaging of three nearby (z ¹ 0.1) compact symmetric objects : 4C 31. 04, 1946]708, and 1146]596. These objects were chosen on the basis of proximity to Earth as well as H I 21 cm line absorption. The inner H-band isophotes of these galaxies are well Ðtted by Nuker models, typical of nearby elliptical galaxies. Each shows a signiÐcant Ñattening in the isophotal proÐle at radii as well as signiÐcant variations in ellipticity and P.A. However, as previous D0A .5, authors have noted, neither is uncommon for elliptical galaxies. All three objects show modest departures from Nuker law models at radii of 1È5 kpc. Each galaxy shows large well-distributed dust h 60 1 features, which are somewhat concentrated in the nuclear regions in features that resemble disks or tori. We Ðnd that the amount of dust in these galaxies is about 10 times higher than normal for elliptical galaxies and radio galaxy hosts. The major axes of the nuclear dust disks tend to be oriented roughly perpendicular to the radio axis. One galaxy, 4C 31.04, exhibits bright nuclear regions well aligned with the radio axis, while another, 1146]596, shows a signiÐcant near-IR excess resembling a stellar bar along its dust disk. The combination of outwardly normal isophotal proÐles with signiÐcant variations in P.A. and ellipticity is consistent with the host galaxies being relatively recent merger remnants and the mergers having occurred yr ago. Such a merger could have "" triggered ÏÏ the onset of the current Z108 active phase seen in these objects, but our data require a signiÐcant time delay between the merger event and the onset of nuclear activity. However, these data are also consistent with the hypothesis that the onset of nuclear activity in radio galaxies is due to relatively minor "" feeding ÏÏ events and/or the formation of "" bars within bars,ÏÏ events which would disturb the internal kinematics only slightly.

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Section: Discussionsupporting

confidence: 86%

Section: Obscuration Features and Distributionmentioning

confidence: 99%

Host Galaxies, Obscuration, and Nuclear Structure of Three Nearby Compact Symmetric Objects

Perlman

Stocke

Conway

et al. 2001

The Astronomical Journal

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“…The hot gas component dominates the ISM in E/S0 galaxies, and only comparatively small quantities are detected in the warm and cold phases (Bregman et al 1992). The derived masses of the warm ISM range from ∼10 3 to ∼10 6 M (Phillips et al 1986;Trinchieri & di Serego Alighieri 1991;Macchetto et al 1996;Goudfrooij et al 1994aGoudfrooij et al , 1994bGoudfrooij et al , 1994cGoudfrooij & de Jong 1995), orders of magnitude below the Xray emitting hot ISM and the stellar mass. Ionized gas is detected in 40-80% of early-type galaxies from their optical emission lines (Caldwell 1984;Phillips et al 1986;Macchetto et al 1996;Sarzi et al 2006Sarzi et al , 2009Yan et al 2006;Serra et al 2008).…”

Section: Introductionmentioning

confidence: 97%

“…Ionized gas is detected in 40-80% of early-type galaxies from their optical emission lines (Caldwell 1984;Phillips et al 1986;Macchetto et al 1996;Sarzi et al 2006Sarzi et al , 2009Yan et al 2006;Serra et al 2008). A&A 519, A40 (2010) The ionized gas is also usually morphologically associated with dust (Kim 1989;Goudfrooij et al 1994c).…”

Section: Introductionmentioning

confidence: 99%

Nearby early-type galaxies with ionized gas

Annibali

Bressan

Rampazzo

et al. 2010

A&A

121

162

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Aims. A significant fraction of early-type galaxies (ETGs) exhibit emission lines in their optical spectra. We attempt to identify the producing the emission mechanism and the ionized gas in ETGs, and its connection with the host galaxy evolution. Methods. We analyzed intermediate-resolution optical spectra of 65 ETGs, mostly located in low density environments and exhibiting spectros-copic diagnostic lines of ISM from which we had previously derived stellar population properties. To extract the emission lines from the galaxy spectra, we developed a new fitting procedure that accurately subtracts the underlying stellar continuum, and accounts for the uncertainties caused by the age-metallicity degeneracy. Results. Optical emission lines are detected in 89% of the sample. The incidence and strength of emission correlate with neither the E/S0 classification, nor the fast/slow rotator classification. By means of the classical [OIII]/Hβ versus [NII]/Hα diagnostic diagram, the nuclear galaxy activity is classified such that 72% of the galaxies with emission are LINERs, 9% are Seyferts, 12% are composite/transition objects, and 7% are non-classified. Seyferts have young luminostiy-weighted ages ( 5 Gyr), and appear, on average, significantly younger than LINERs and composites. Excluding the Seyferts from our sample, we find that the spread in the ([OIII], Hα, or [NII]) emission strength increases with the galaxy central velocity dispersion σ c . Furthermore, the [NII]/Hα ratio tends to increase with σ c . The [NII]/Hα ratio decreases with increasing galactocentric distance, indicative of either a decrease in the nebular metallicity, or a progressive "softening" of the ionizing spectrum. The average nebular oxygen abundance is slightly less than solar, and a comparison with the results obtained in Paper III from Lick indices shows that it is ≈0.2 dex lower than that of stars. Conclusions. The nuclear (r < r e /16) emission can be attributed to photoionization by PAGB stars alone only for ≈22% of the LINER/composite sample. On the other hand, we cannot exclude an important role of PAGB star photoionization at larger radii. For the major fraction of the sample, the nuclear emission is consistent with excitation caused by either a low-accretion rate AGN or fast shocks (200-500 km s −1 ) in a relatively gas poor environment (n 100 cm −3 ), or both. The derived [SII]6717/6731 ratios are consistent with the low gas densities required by the shock models. The derived nebular metallicities are indicative of either an external origin of the gas, or an overestimate of the oxygen yields by SN models.

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“…Another novel method of studying extragalactic dust extinction is through the study of early-type galaxies with resolved dust lanes (e.g. Goudfrooij et al 1994;Patil et al 2007;Finkelman et al 2008Finkelman et al , 2010. For those such galaxies with a relatively small dust covering factor, and a spatially smooth underlying stellar light distribution, the spectra of the underlying, dust-free galaxy can be measured with reasonable accuracy.…”

Section: Introductionmentioning

confidence: 99%

The dust extinction curves of gamma-ray burst host galaxies

Schady¹,

Dwelly²,

Page³

et al. 2011

A&A

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The composition and amount of interstellar dust within gamma-ray burst (GRB) host galaxies is of key importance when addressing selection effects in the GRB redshift distribution, and when studying the properties of their host galaxies. As well as the implications for GRB research, probing the dust within the high-z hosts of GRBs also contributes to our understanding of the conditions of the interstellar medium and star-formation in the distant Universe. Nevertheless, the physical properties of dust within GRB host galaxies continues to be a highly contended issue. In this paper we explore the mean extinction properties of dust within the host galaxies of a sample of 17 GRBs with total host galaxy visual extinction A V < 1 ( A V = 0.4), covering a redshift range z = 0.7−3.1. We find the average host extinction curve to have an ultraviolet slope comparable to that of the LMC, but with little evidence of a 2175 Å dust extinction feature as observed along Milky Way and LMC sightlines. We cannot at present rule out the presence of a 2175 Å feature, and both the standard SMC and LMC extinction curves also provide good fits to our data. However, we can reject an extinction curve that has a UV slope as flat as the mean Milky Way extinction curve, whilst also having a 2175 Å feature as prominent as seen in the mean Milky Way extinction curve. This is in contrast to the clear detection of a 2175 Å bump and the flatter extinction curves of some more heavily extinguished GRBs (A V > 1), which may be indicative of there being a dependence between dust abundance and the wavelength dependence of dust extinction, as has been previously speculated.

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Interstellar matter in elliptical galaxies - III. Properties of dust extinction

Cited by 96 publications

References 0 publications

Host Galaxies, Obscuration, and Nuclear Structure of Three Nearby Compact Symmetric Objects

Host Galaxies, Obscuration, and Nuclear Structure of Three Nearby Compact Symmetric Objects

Nearby early-type galaxies with ionized gas

The dust extinction curves of gamma-ray burst host galaxies

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