Dust emission in early-type galaxies: The mid-infrared view

Xilouris, E. M.; Madden, S. C.; Galliano, F.; Vigroux, L.; Sauvage, M.

doi:10.1051/0004-6361:20034020

Cited by 85 publications

(111 citation statements)

References 51 publications

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“…The presence of dust in M 87 was also suggested by Xilouris et al (2004) by combining their ISO data at 4.5, 6.7, and 15 μm with IRAS data at 60 and 100 μm, using an aperture very similar to ours. Their estimate gives a smaller quantity of dust at a higher temperature.…”

Section: Dust Mass and Temperaturesupporting

confidence: 69%

TheHerschelVirgo Cluster Survey

Alighieri

Bianchi

Pappalardo

et al. 2013

A&A

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Aims. We study the dust content of a large optical input sample of 910 early-type galaxies (ETG) in the Virgo cluster, also extending to the dwarf ETG, and examine the results in relation to those on the other cold ISM components. Methods. We have searched for far-infrared emission in all galaxies in the input sample using the 250 μm image of the Herschel Virgo Cluster Survey (HeViCS). This image covers a large fraction of the cluster with an area of ∼55 square degrees. For the detected ETG we measured fluxes in five bands from 100 to 500 μm, and estimated the dust mass and temperature with modified black-body fits. Results. Dust is detected above the completeness limit of 25.4 mJy at 250 μm in 46 ETG, 43 of which are in the optically complete part of the input sample. In addition, dust is present at fainter levels in another six ETG. We detect dust in the four ETG with synchrotron emission, including M 87. Dust appears to be much more concentrated than stars and more luminous ETG have higher dust temperatures. Considering only the optically complete input sample and correcting for the contamination by background galaxies, dust detection rates down to the 25.4 mJy limit are 17% for ellipticals, about 40% for lenticulars (S0 + S0a), and around 3% for dwarf ETG. Dust mass does not correlate clearly with stellar mass and is often much greater than expected for a passive galaxy in a closedbox model. The dust-to-stars mass ratio anticorrelates with galaxy luminosity, and for some dwarf ETG reaches values as high as for dusty late-type galaxies. In the Virgo cluster slow rotators appear more likely to contain dust than fast ones. Comparing the dust results with those on Hi there are only eight ETG detected both in dust and in Hi in the HeViCS area; 39 have dust but only an upper limit on Hi, and eight have Hi but only an upper limit on dust. The locations of these galaxies in the cluster are different, with the dusty ETG concentrated in the densest regions, while the Hi rich ETG are at the periphery.

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Section: Dust Mass and Temperaturesupporting

confidence: 69%

TheHerschelVirgo Cluster Survey

Alighieri

Bianchi

Pappalardo

et al. 2013

A&A

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“…The large fraction of CO 2 in the solid state might be understood by considering that the sublimation temperature of solid CO 2 is 45-72 K while solid CO readily evaporates at dust temperatures above 20 K (van Dishoeck et al 1996); the thermal dust in NGC 1316 has a temperature of 30 K (Xilouris et al 2004), which is a typical dust temperature for elliptical galaxies (Goudfrooij & de Jong 1995;Temi et al 2004;Kaneda et al 2007a). Furthermore, CO 2 forms readily in laboratory ice analogs containing CO when subject to energetic processing such as ultraviolet irradiation or particle bombardment (e.g., d 'Hendecourt et al 1986;Sandford et al 1988), as expected from the past nuclear activity of NGC 1316.…”

Section: Resultsmentioning

confidence: 99%

“…At wavelengths shorter than 8 mm, spectra of elliptical galaxies are generally dominated by blackbody emission from low-mass asymptotic giant branch (AGB) stars with temperatures of 3000-5000 K (Athey et al 2002;Xilouris et al 2004). The ISO SWS revealed near-IR absorption features of molecular species such as CO, CO 2 , and H 2 O from the interstellar ice/gas in our Galaxy with different chemical compositions (e.g., de Graauw et al 1996).…”

Section: Introductionmentioning

confidence: 99%

Near- to Mid-Infrared Spectroscopy for the Giant Elliptical Galaxy NGC 1316 (Fornax A) with the AKARI Infrared Camera

Kaneda

Onaka

Sakon

2007

ApJ

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We present the near-to mid-infrared (∼2.5-13 mm) spectrum of the giant elliptical galaxy NGC 1316 (Fornax A) obtained with the Infrared Camera (IRC) on board AKARI. NGC 1316 is known to have a peculiar polycyclic aromatic hydrocarbon (PAH) emission spectrum with an unusually high ratio of the 11.3 mm to the 7.7 mm emission intensity through the Spitzer IRS observation. NGC 1316 is a 3 Gyr old merger remnant with a dormant nucleus that was rather active 0.1 Gyr ago; the relatively well-known evolutionary history makes the elliptical galaxy an ideal probe for studying long-term effects of past energetic events on the interstellar medium. We have found that there is no significant PAH emission feature at 3.3 mm while we have confirmed the peculiar PAH emission spectrum in the mid-infrared. We have detected a strong absorption feature at 4.3 mm, which may be attributed to solid-state CO 2 in grain mantles. We discuss physical implications for those unusual emission and absorption features.

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“…Table 1 lists the Herschel fluxes of M87, together with ISOCAM, IRAS, MIPS, and SCUBA data gathered from the literature (Xilouris et al 2004;Golombek et al 1988;Shi et al 2007;Haas et al 2004). The top panel in Fig.…”

Section: Discussionmentioning

confidence: 99%

“…After careful subtraction of a stellar emission template from the mid-infrared spectrum, these authors conclude that the nuclear spectrum can be fully accounted for by optically thin synchrotron emission and that there is little room for dust emission. On a larger scale, Xilouris et al (2004) present ISOCAM imaging of M87 and argue that the mid-infrared flux can be attributed to a single synchrotron emission component. Shi et al (2007) present Spitzer IRAC and MIPS imaging of M87 and find a slight excess in the FIR over a power-law interpolation.…”

Section: Present Ground-based Subarumentioning

confidence: 99%

TheHerschelVirgo Cluster Survey

Baes¹,

Clemens

Xilouris

et al. 2010

A&A

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The origin of the far-infrared emission from the nearby radio galaxy M87 remains a matter of debate. Some studies find evidence of a far-infrared excess due to thermal dust emission, whereas others propose that the far-infrared emission can be explained by synchrotron emission without the need for an additional dust emission component. We present Herschel PACS and SPIRE observations of M87, taken as part of the science demonstration phase observations of the Herschel Virgo Cluster Survey. We compare these data with a synchrotron model based on mid-infrared, far-infrared, submm and radio data from the literature to investigate the origin of the far-infrared emission. Both the integrated SED and the Herschel surface brightness maps are adequately explained by synchrotron emission. At odds with previous claims, we find no evidence of a diffuse dust component in M87, which is not unexpected in the harsh X-ray environment of this radio galaxy sitting at the core of the Virgo Cluster.

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Dust emission in early-type galaxies: The mid-infrared view

Cited by 85 publications

References 51 publications

TheHerschelVirgo Cluster Survey

TheHerschelVirgo Cluster Survey

Near- to Mid-Infrared Spectroscopy for the Giant Elliptical Galaxy NGC 1316 (Fornax A) with the AKARI Infrared Camera

TheHerschelVirgo Cluster Survey

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