ISOCAM view of the starburst galaxies M 82, NGC 253 and NGC 1808

Schreiber, N. M. Förster; Sauvage, M.; Charmandaris, V.; Laurent, O.; Gallais, P.; Mirabel, I. F.; Vigroux, L.

doi:10.1051/0004-6361:20021719

Cited by 64 publications

(21 citation statements)

References 84 publications

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“…Galaxies with a global color excess are all dominated by their central regions. This is a confirmation of predictions from hydrodynamical models (Athanassoula 1992;Friedli & Benz 1993), according to which a barred perturbation, through tidal torques and shocks, induces substantial mass transfer towards circumnuclear regions. We observe the consequences of these gas flows, i.e.…”

Section: Discussionsupporting

confidence: 84%

“…We find that the energy ratio F 12.75 /F 11.3 of circumnuclear regions decreases from 0.67 in NGC 1365 to 0.60 in NGC 613 and 5236, 0.52 in NGC 1097 and 0.47 in NGC 5194; in the averaged inner disks of NGC 1365, 5236 and 5194, where it is still measurable, it takes the approximate values 0.5, 0.45 and 0.4 . These figures are much lower than those observed in cores of starburst galaxies by Förster-Schreiber et al (2001), where it can reach 1.7, and argue for a generally small contribution of [NeII] to the spectra. Adopting as the intrinsic F 12.7 /F 11.3 UIB energy ratio the minimum value of F 12.75 /F 11.3 that we measure in our spectra, i.e.…”

Section: Nature Of the Mid-infrared Emitting Speciescontrasting

confidence: 62%

“…Some variation however exists. To compare the strength of the [NeII] line in our galaxies to that observed by Förster-Schreiber et al (2001) in the starburst galaxies M 82, NGC 253 and NGC 1808, we have measured in a similar way the flux of the blend F 12.75 above the pseudo-continuum drawn as a straight line between 12.31 and 13.23 µm, and the flux of the 11.3 µm UIB F 11.3 with its respective continuum level defined in the same way between 10.84 and 11.79 µm. We find that the energy ratio F 12.75 /F 11.3 of circumnuclear regions decreases from 0.67 in NGC 1365 to 0.60 in NGC 613 and 5236, 0.52 in NGC 1097 and 0.47 in NGC 5194; in the averaged inner disks of NGC 1365, 5236 and 5194, where it is still measurable, it takes the approximate values 0.5, 0.45 and 0.4 .…”

Section: Nature Of the Mid-infrared Emitting Speciesmentioning

confidence: 99%

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The impact of bars on the mid-infrared dust emission of spiral galaxies: global and circumnuclear properties

Roussel

Sauvage

Vigroux

et al. 2001

A&A

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Abstract.We study the mid-infrared properties of a sample of 69 nearby spiral galaxies, selected to avoid Seyfert activity contributing a significant fraction of the central energetics, or strong tidal interaction, and to have normal infrared luminosities. These observations were obtained with ISOCAM, which provides an angular resolution of the order of 10 (half-power diameter of the point spread function) and low-resolution spectro-imaging information. Between 5 and 18 µm, we mainly observe two dust phases, aromatic infrared bands and very small grains, both out of thermal equilibrium. On this sample, we show that the global F15/F7 colors of galaxies are very uniform, the only increase being found in early-type strongly barred galaxies, consistent with previous IRAS studies. The F15/F7 excesses are unambiguously due to galactic central regions where bar-induced starbursts occur. However, the existence of strongly barred early-type galaxies with normal circumnuclear colors indicates that the relationship between a distortion of the gravitational potential and a central starburst is not straightforward. As the physical processes at work in central regions are in principle identical in barred and unbarred galaxies, and since this is where the mid-infrared activity is mainly located, we investigate the mid-infrared circumnuclear properties of all the galaxies in our sample. We show how surface brightnesses and colors are related to both the available molecular gas content and the mean age of stellar populations contributing to dust heating. Therefore, the star formation history in galactic central regions can be constrained by their position in a color-surface brightness mid-infrared diagram.

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Section: Discussionsupporting

confidence: 84%

Section: Nature Of the Mid-infrared Emitting Speciescontrasting

confidence: 62%

Section: Nature Of the Mid-infrared Emitting Speciesmentioning

confidence: 99%

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The impact of bars on the mid-infrared dust emission of spiral galaxies: global and circumnuclear properties

Roussel

Sauvage

Vigroux

et al. 2001

A&A

Self Cite

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“…instrument. A number of early studies of local and z∼1 galaxies suggested that PAH emission correlates with total dust emission (e.g., Roussel et al 2001;Förster Schreiber et al 2003, 2004, though with some variations with metallicity, ionizing intensity, SFR surface density, and stellar population age (e.g., Normand et al 1995;Helou et al 2001;Alonso-Herrero et al 2004;Engelbracht et al 2005;Hogg et al 2005;Madden et al 2006;Draine et al 2007;Smith et al 2007;Galliano et al 2008;Hunt et al 2010;Sales et al 2010;Elbaz et al 2011;Magdis et al 2013;Seok et al 2014). Recently, Shivaei et al (2017) presented the first statistically significant trends showing lower ratios of the 7.7 μm to total IR luminosity, L 7.7 /L IR , with higher ionization intensity, lower gas-phase metallicity, and younger ages for galaxies at z∼2 from the MOSDEF survey .…”

Section: Discussionmentioning

confidence: 99%

The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies

Reddy

Oesch

Bouwens

et al. 2018

ApJ

206

293

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We use a newly assembled sample of 3545 star-forming galaxies with secure spectroscopic, grism, and photometric redshifts at z=1.5-2.5 to constrain the relationship between UV slope (β) and dust attenuation (L IR /L UV ≡IRX). Our sample significantly extends the range of L UV and β probed in previous UV-selected samples, including those as faint as M 1600 =−17.4 ( L 0.05 UV *  ) and −2.6β0.0. IRX is measured using stacks of deep Herschel data, and the results are compared with predictions of the IRX−β relation for different assumptions of the stellar population model and obscuration curve. We find that z=1.5-2.5 galaxies have an IRX −β relation that is consistent with the predictions for an SMC curve if we invoke subsolar-metallicity models currently favored for high-redshift galaxies, while the commonly assumed starburst curve overpredicts the IRX at a given β by a factor of 3. IRX is roughly constant with L UV for L UV 3×109 L e . Thus, the commonly observed trend of fainter galaxies having bluer β may simply reflect bluer intrinsic slopes for such galaxies, rather than lower obscurations. The IRX−β relation for young/low-mass galaxies at z2 implies a dust curve that is steeper than the SMC. The lower attenuations and higher ionizing photon output for low-metallicity stellar populations point to Lyman continuum production efficiencies, ξ ion , that may be elevated by a factor of ≈2 relative to the canonical value for L * galaxies, aiding in their ability to keep the universe ionized at z∼2.

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“…A number of studies have successfully decomposed low resolution mid-infrared spectra of galaxies into three components: A "PDR" component dominated by the aromatic emission features, an "H II" very small grain continuum steeply rising towards longer wavelengths and a hotter "AGN" dust continuum (Laurent et al 2000; see also Sturm et al 2000;Tran et al 2001;Förster Schreiber et al 2003). Dust obscuration can be important (Lutz et al 1998a;Tran et al 2001), with the additional complication of ice features (Spoon et al 2002).…”

Section: Star Formation: Aromatic Emission Featuresmentioning

confidence: 99%

ISO spectroscopy of star formation and active nuclei in the luminous infrared galaxy NGC 6240

Lutz¹,

Sturm²,

Genzel³

et al. 2003

A&A

105

121

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Abstract. We present Infrared Space Observatory mid-and far-infrared spectroscopy of the merging galaxy NGC 6240, an object presenting many aspects of importance for the role of star formation and AGN activity in [ultra]luminous infrared galaxies. The mid-infrared spectrum shows starburst indicators in the form of low excitation fine-structure line emission and aromatic "PAH" features. A strong high excitation [O IV] line is observed which most likely originates in the Narrow Line Region of an optically obscured AGN. NGC 6240 shows extremely powerful emission in the pure rotational lines of molecular hydrogen. We argue that this emission is mainly due to shocks in its turbulent central gas component and its starburst superwind. The total shock cooling in infrared emission lines accounts for ∼0.6% of the bolometric luminosity, mainly through rotational H 2 emission and the [O I] 63 µm line. We analyse several ways of estimating the luminosities of the starburst and the AGN in NGC 6240 and suggest that the contributions to its bolometric luminosity are most likely in the range 50-75% starburst and 25-50% AGN.

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ISOCAM view of the starburst galaxies M 82, NGC 253 and NGC 1808

Cited by 64 publications

References 84 publications

The impact of bars on the mid-infrared dust emission of spiral galaxies: global and circumnuclear properties

The impact of bars on the mid-infrared dust emission of spiral galaxies: global and circumnuclear properties

The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies

ISO spectroscopy of star formation and active nuclei in the luminous infrared galaxy NGC 6240

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