An atlas of mid-infrared dust emission in spiral galaxies

Roussel, H.; Vigroux, L.; Bosma, A.; Sauvage, M.; Bonoli, C.; Gallais, P.; Hawarden, T. G.; Lequeux, J.; Madden, S.; Mazzei, P.

doi:10.1051/0004-6361:20010154

Cited by 55 publications

(101 citation statements)

References 40 publications

(53 reference statements)

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“…Bar driven inflow is another. ISOCAM studies of several samples of interacting, barred and collisional ring galaxies confirm this paradigm (Appleton et al 1999, Roussel et al 1999b, Wozniak et al 1999. The optical/UV data in the Antennae tell a fascinating story with evidence for a large age spread in star cluster populations.…”

Section: The Dark Side Of Star Formationmentioning

confidence: 92%

Extragalactic Results from the Infrared Space Observatory

Genzel

Césarsky

2000

Annu. Rev. Astron. Astrophys.

274

285

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More than a decade ago the IRAS satellite opened the realm of external galaxies for studies in the 10 to 100µm band and discovered emission from tens of thousands of normal and active galaxies.With the 1995-1998 mission of the Infrared Space Observatory 1 the next major steps in extragalactic infrared astronomy became possible: detailed imaging, spectroscopy and spectro-photometry of many galaxies detected by IRAS, as well as deep surveys in the mid-and far-IR. The spectroscopic data reveal a wealth of detail about the nature of the energy source(s) and about the physical conditions in galaxies. ISO's surveys for the first time explore the infrared emission of distant, high-redshift galaxies. ISO's main theme in extragalactic astronomy is the role of star formation in the activity and evolution of galaxies.

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Section: The Dark Side Of Star Formationmentioning

confidence: 92%

Extragalactic Results from the Infrared Space Observatory

Genzel

Césarsky

2000

Annu. Rev. Astron. Astrophys.

274

285

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“…Since the dust in the torus is certainly warmer than in the disk, this might also explain why the continuum emission is not more extended, as is the CO, in addition to the interferometer's filtering argument explained above. Midinfrared maps with ISO at 7 and 15 μm also show a high central concentration, but with low resolution (Roussel et al 2001). …”

Section: Dust Continuum Emissionmentioning

confidence: 95%

ALMA observations of feeding and feedback in nearby Seyfert galaxies: an AGN-driven outflow in NGC 1433

Combes

García‐Burillo

Casasola

et al. 2013

A&A

181

200

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We report ALMA observations of CO(3-2) emission in the Seyfert 2 galaxy NGC 1433 at the unprecedented spatial resolution of 0. 5 = 24 pc. Our aim is to probe active galactic nucleus (AGN) feeding and feedback phenomena through the morphology and dynamics of the gas inside the central kpc. The galaxy NGC 1433 is a strongly barred spiral with three resonant rings: one at the ultraharmonic resonance near corotation, and the others at the outer and inner Lindblad resonances (OLR and ILR). A nuclear bar of 400 pc radius is embedded in the large-scale primary bar. The CO map, which covers the whole nuclear region (nuclear bar and ring), reveals a nuclear gaseous spiral structure, inside the nuclear ring encircling the nuclear stellar bar. This gaseous spiral is well correlated with the dusty spiral seen in Hubble Space Telescope (HST) images. The nuclear spiral winds up in a pseudo-ring at ∼200 pc radius, which might correspond to the inner ILR. Continuum emission is detected at 0.87 mm only at the very centre, and its origin is more likely thermal dust emission than non-thermal emission from the AGN. It might correspond to the molecular torus expected to exist in this Seyfert 2 galaxy. The HCN(4-3) and HCO + (4-3) lines were observed simultaneously, but only upper limits are derived, with a ratio to the CO(3-2) line lower than 1/60 at 3σ, indicating a relatively low abundance of very dense gas. The kinematics of the gas over the nuclear disk reveal rather regular rotation only slightly perturbed by streaming motions due to the spiral; the primary and secondary bars are too closely aligned with the galaxy major or minor axis to leave a signature in the projected velocities. Near the nucleus, there is an intense high-velocity CO emission feature redshifted to 200 km s −1 (if located in the plane), with a blue-shifted counterpart, at 2 (100 pc) from the centre. While the CO spectra are quite narrow in the centre, this wide component is interpreted as an outflow involving a molecular mass of 3.6 × 10 6 M and a flow rate ∼7 M /yr. The flow could be in part driven by the central star formation, but is mainly boosted by the AGN through its radio jets.

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“…For observations where the object was quite extended (i.e. little background is present in the maps) the raw calibration flats were used (see Roussel et al 2001, for a more detailed description). After flat-fielding the images, the final map was constructed by projecting together all the individual images of the same configurations.…”

Section: Data Reductionmentioning

confidence: 99%

“…The photometric errors were calculated by taking into account the errors introduced by the photon noise, the readout noise, the memory effects as well as a 5% error due to flux density calibration uncertainties (ISOCAM handbook) and an additional 5% variation along each orbit (ISOCAM handbook). A more detailed description of the evaluation of the photometric errors is given in Roussel et al (2001). The total fluxes (integrated within the field of view of ISOCAM) for each galaxy are given in Table 2.…”

Section: The Datamentioning

confidence: 99%

“…7 we compare the F ν (6.7 µm)/F ν (15 µm) ratio with the F ν (12 µm)/F ν (25 µm) ratio for three samples of galaxies. The first sample (solid circles) is a sample of normal star-forming galaxies (Dale et al 2000), the second sample (open squares) is another sample (complementary to the first one) containing spiral galaxies (Roussel et al 2001) while the third sample (red triangles) consists of the sample of early-type galaxies presented in this work. A cross on the top left part of the diagram shows a typical error bar associated with the early-type galaxies.…”

Section: Colour-colour Diagramsmentioning

confidence: 99%

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

Xilouris

Madden

Galliano

et al. 2004

A&A

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Abstract. We present mid-infrared (MIR) maps for a sample of 18 early-type galaxies observed at 4.5, 6.7 and 15 µm with the ISOCAM instrument on board the ISO satellite with a 6 spatial resolution. We model the Spectral Energy Distribution (SED) of these galaxies using the stellar evolutionary synthesis model PÉGASE and we derive the MIR excess over the stellar component. We then explore the nature of this excess in terms of dust and Polycyclic Aromatic Hydrocarbon molecules (PAHs). We find that out of 18 galaxies, 10 show excess at 6.7 µm (due to the presence of PAH features) and 14 show excess at 15 µm (due to the presence of warm dust). In two galaxies, where a more complete wavelength coverage exists, an excess around 9.7 µm is seen (presumably due to silicate dust emission), while two other galaxies are totally devoid of dust. We also examine the morphology of the galaxies in these wavelengths by plotting the azimuthally averaged radial profiles as well as the MIR color profiles. We find that for the majority of the galaxies the 4.5 µm emission is well described by a de Vaucouleurs profile. The 6.7 µm and 15 µm emission is smoothly distributed throughout the galaxy while only a few galaxies show MIR emission which is more concentrated close to the center. Two dwarf galaxies in our sample show patchy distributions of the MIR emission while two other galaxies show edge-on disks. With color-color diagrams we delineate the regions occupied by late-type and early-type galaxies. Finally we show that the MIR excess found in strong radio galaxies like NGC 4486 (M87) can be explained by synchrotron emission.

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An atlas of mid-infrared dust emission in spiral galaxies

Cited by 55 publications

References 40 publications

Extragalactic Results from the Infrared Space Observatory

Extragalactic Results from the Infrared Space Observatory

ALMA observations of feeding and feedback in nearby Seyfert galaxies: an AGN-driven outflow in NGC 1433

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

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