Large-scale distributions of mid- and far-infrared emission from the center to the halo of M 82 revealed with AKARI

Kaneda, Hidehiro; Ishihara, Daisuke; Suzuki, Toyoaki; Ikeda, Norio; Onaka, Takashi; Yamagishi, Masao; Ohyama, Youichi; Wada, Takehiko; Yasuda, Akiko

doi:10.1051/0004-6361/200913769

Cited by 50 publications

(80 citation statements)

References 55 publications

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“…The reduced scaleheights in the southern part are a good argument for higher losses of cosmic rays towards the group centre. Kaneda et al (2010) detected a stronger radiation field only in the southeastern part of the galaxy, which favours higher inverse Compton losses in this area. However, this cannot explain the overall reduced extent of the southern halo and its reduced scaleheights.…”

Section: Scaleheights At λ22 CM and λ92 Cmmentioning

confidence: 83%

“…While the maps at 3 cm and 6 cm show only emission in the central disk and some extraplanar emission to the north and south of the very central region of M 82, the maps at 22 cm and 92 cm show the structure of the radio halo and the disk emission. Overall, the halo emission in the southern part seems to be less extended than in the northern part, but the whole halo emission correlates with the Hα-as well as the PAH + -morphology (Kaneda et al 2010). The most obvious difference between the northern and southern parts of the halo are two extensions accompanied by a suppression of emission in between them in the northern halo.…”

Section: Morphologymentioning

confidence: 83%

“…Using a value of S 60 = 630 Jy and S 100 = 529 Jy for the central 1 radius and S 60 = 1700 Jy and S 100 = 1840 Jy for a radius of 4 representing the whole galaxy (Kaneda et al 2010) leads to an energy density of U ph,c = 4.43 × 10 −11 erg cm −3 for the core and U ph,h = 5.57 × 10 −12 erg cm −3 for the halo.…”

Section: Cosmic Ray Electron Lossesmentioning

confidence: 99%

“…A detailed near-and mid-infrared spectroscopy by Förster Schreiber et al (2003) suggests two successive starburst periods about 10 and 5 Myr ago. This would explain the enrichment of the halo with ionised polycyclic aromatic hydrocarbons (PAH + ) observed by Kaneda et al (2010), which would otherwise have been destroyed by the starburst of the violent radiation. Additionally extended emission has been found ∼11 kpc to the north of the galaxy in Hα, X-rays, and UV (Devine & Bally 1999;Lehnert et al 1999;Hoopes et al 2005), which is spatially not connected to the main halo of M 82.…”

Section: Introductionmentioning

confidence: 99%

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M 82 – A radio continuum and polarisation study

Adebahr

Krause

Klein

et al. 2013

A&A

104

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Context. The potential role of magnetic fields and cosmic ray propagation for feedback processes in the early Universe can be probed by studies of local starburst counterparts with an equivalent star-formation rate. Aims. In order to study the cosmic ray propagation and determine the magnetic field strength and dominant loss processes in the nearby prototypical starbursting galaxy M 82, a multi-frequency analysis at four radio wavelengths is presented. Methods. Archival data from the Westerbork Synthesis Radio Telescope (WSRT) was reduced and a new calibration technique introduced to reach the high dynamic ranges needed for the complex source morphology. These data were combined with archival Very Large Array (VLA) data, yielding total power maps at λ3 cm, λ6 cm, λ22 cm, and λ92 cm. Results. The data show a confinement of the emission at wavelengths of λ3/λ6 cm to the core region and a largely extended halo reaching up to 4 kpc away from the galaxy midplane at wavelengths of λ22/λ92 cm up to a sensitivity limit of 90 µJy and 1.8 mJy respectively indicating different physical processes in the core and halo regions. The results are used to calculate the magnetic field strength to 98 µG in the core region and to 24 µG in the halo regions. From the observation of ionisation losses, the filling factor of the ionised medium could be estimated to 2%. This leads to a revised view of the magnetic field distribution in the core region and the propagation processes from the core into the halo regions. Conclusions. We find that the radio emission from the core region is dominated by very dense H -regions and supernova remnants, while the surrounding medium is filled with hot X-ray and neutral gas. Cosmic rays radiating at frequencies higher than 1.4 GHz suffer from high synchrotron and inverse Compton losses in the core region and are not able to reach the halo. Even the cosmic rays radiating at longer wavelengths are only able to build up the observed kpc-sized halo, when several starbursting periods are assumed where the far-infrared and radio luminosity vary by an order of magnitude. These findings, together with the strong correlation between Hα, ionised polycyclic aromatic hydrocarbons (PAH + ), and our radio continuum data, suggest a magnetic field which is frozen into the ionised medium and driven out of the galaxy kinematically.

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Section: Scaleheights At λ22 CM and λ92 Cmmentioning

confidence: 83%

Section: Morphologymentioning

confidence: 83%

Section: Cosmic Ray Electron Lossesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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M 82 – A radio continuum and polarisation study

Adebahr

Krause

Klein

et al. 2013

A&A

104

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“…Both FIR and UIR band emission has been detected in outflows or halo regions of several galaxies. Very extended UIR band emission has been detected in the outflow from M 82 (Engelbracht et al 2006;Kaneda et al 2010). The 3.3 μm UIR band emission associated with the outflow has been detected in NGC 253 (Tacconi-Garman et al 2005), in which emission further away from the galaxy has been detected in the FIR (Kaneda et al 2009b).…”

Section: Uir Bands In the Filamentmentioning

confidence: 95%

Detection of unidentified infrared bands in a Hαfilament in the dwarf galaxy NGC 1569 with AKARI

Onaka

Matsumoto

Sakon

et al. 2010

A&A

Self Cite

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Context. We report the detection of unidentified infrared (UIR) bands in a filamentary structure associated with Hα emission in the starburst dwarf galaxy NGC 1569 based on imaging and spectroscopic observations of the AKARI satellite. Aims. We investigate the processing and destruction of the UIR band carriers in an outflow from NGC 1569. Methods. We performed observations of NGC 1569 for 6 infrared bands (3.2, 4.1, 7, 11, 15, and 24 μm) with the infrared camera (IRC) onboard AKARI. Near-to mid-infrared (2−13 μm) spectroscopy of a Hα filament was also carried out with the IRC. Results. The extended structure associated with a Hα filament appears bright at 7 μm. Since the IRC 7 μm band (S7) efficiently traces the 6.2 and 7.7 μm UIR band emission, the IRC imaging observations suggest that the filament is bright at the UIR band emission. Follow-up spectroscopic observations with the IRC confirm the presence of 6.2, 7.7, and 11.3 μm emission in the filament. The filament spectrum exhibits strong 11.3 μm UIR band emission relative to the 7.7 μm band compared to the galaxy disk observed with the infrared spectrograph on Spitzer. The near-infrared spectrum also suggests the presence of excess continuum emission in 2.5−5 μm in the filament. Conclusions. The presence of the UIR bands associated with a Hα filament is found by AKARI/IRC observations. The Hα filament is thought to have been formed by the galactic outflow originating from the star-formation activity in the disk of NGC 1569. The destruction timescale of the UIR band carriers in the outflow is estimated to be much shorter (∼1.3 × 10 3 yr) than the timescale of the outflow (∼5.3 Myr). Thus it is unlikely that the band carriers survive the outflow environment. Alternatively, we suggest that the band carriers in the filaments may be produced by the fragmentation of large carbonaceous grains in shocks, which produce the Hα emission. The NIR excess continuum emission cannot be accounted for by free-free emission alone and a hot dust contribution may be needed, although the free-free emission intensity estimated from H i recombination lines has a large uncertainty.

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Charge‐exchange emission in the starburst galaxies M82 and NGC3256

Ranalli

2012

Astron Nachr

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Charge-exchange (CE) emission produces features which are detectable with the current X-ray instrumentation in the brightest near galaxies. We describe these aspects in the observed X-ray spectra of the star forming galaxies M82 and NGC 3256, from the Suzaku and XMM-Newton telescopes. Emission from both ions (O, C) and neutrals (Mg, Si) is recognised. We also describe how microcalorimeter instrumentation on future missions will improve CE observations.

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Large-scale distributions of mid- and far-infrared emission from the center to the halo of M 82 revealed with AKARI

Cited by 50 publications

References 55 publications

M 82 – A radio continuum and polarisation study

M 82 – A radio continuum and polarisation study

Detection of unidentified infrared bands in a Hαfilament in the dwarf galaxy NGC 1569 with AKARI

Charge‐exchange emission in the starburst galaxies M82 and NGC3256

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