<i>ISO</i>LWS Spectroscopy of M82: A Unified Evolutionary Model

Colbert, James; Malkan, Matthew A.; Clegg, P. E.; Cox, P.; Fischer, J.; Lord, S. D.; Luhman, M. L.; Satyapal, S.; Smith, H. A.; Spinoglio, L.; Stacey, G. J.; Unger, S. J.

doi:10.1086/306711

Cited by 104 publications

(165 citation statements)

References 44 publications

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“…The dust mass in the total region is therefore considered to be lower limits to the real dust mass contained in this region. The ISO/LWS spectroscopy of the central ∼ 1 kpc region of M 82 shows that the SED over the wavelength range of 43−197 μm is well-fitted with a 48 K dust temperature and β = 1, giving a total infrared flux of 3.8 × 10 10 L (Colbert et al 1999). Our result shows overall consistency with the ISO result.…”

Section: Dust Mass and Luminositysupporting

confidence: 85%

“…High-sensitivity FIR observations from space are undoubtedly the most effective way to study the properties of faint extended emission from extraplanar dust, since dust emission typically peaks in the FIR, and low photon backgrounds in space enable us to detect faint diffuse emission. However, one serious problem is that the central starburst core is dazzlingly bright for space observations in the MIR and FIR, owing to tremendous star-forming activity in the central region of M 82 (Telesco & Harper 1980), and M 82 is the brightest galaxy in the MIR and FIR after the Magellanic Clouds on the sky (Colbert et al 1999). Then, instrumental effects caused by saturation in observing very bright sources severely hamper reliable detection of low-level FIR emission outside the disk.…”

Section: Introductionmentioning

confidence: 99%

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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

Kaneda¹,

Ishihara²,

Suzuki

et al. 2010

A&A

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Context. The edge-on starburst galaxy M 82 exhibits complicated distributions of gaseous materials in its halo, which include ionized superwinds driven by nuclear starbursts, neutral materials entrained by the superwinds, and large-scale neutral streamers probably caused by a past tidal interaction with M 81. Aims. We investigate detailed distributions of dust grains and polycyclic aromatic hydrocarbons (PAHs) around M 82 to understand their interplay with the gaseous components. Methods. We performed mid-(MIR) and far-infrared (FIR) observations of M 82 with the infrared camera (IRC) and far-infrared surveyor (FIS) onboard AKARI. Results. We obtained new MIR and FIR images of M 82, which reveal both faint extended emission in the halo and very bright emission in the center with signal dynamic ranges as broad as five orders of magnitude for the MIR and three for FIR, respectively. We detected MIR and FIR emission in the regions far away from the disk of the galaxy, reflecting the dust and PAHs in the halo of M 82. Conclusions. We find that the dust and PAHs are contained in both ionized and neutral gas components, implying that they have been expelled into the halo of M 82 by both starbursts and galaxy interaction. In particular, we obtain a tight correlation between the PAH and Hα emission, which provides evidence that the PAHs are well mixed in the ionized superwind gas and flowing out from the disk.

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Section: Dust Mass and Luminositysupporting

confidence: 85%

Section: Introductionmentioning

confidence: 99%

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

Kaneda¹,

Ishihara²,

Suzuki

et al. 2010

A&A

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“…Comparing the LFIR/µ for the SPT sources 11 , which lie in the range (1.1 − 21.9)µ −1 × 10 12 L , with the local starburst galaxy M82 (LFIR∼ (2.3 − 3.2) × 10 10 L , Rice et al 1988 andColbert et al 1999) show the significant difference in LFIR at high and low redshifts. Using this comparison and estimates of G0 for each SPT DSFG, we estimate approximate sizes of the PDRs populating the galaxies, following Stacey et al (2010).…”

Section: Sizes Of Pdrsmentioning

confidence: 93%

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Gullberg

Breuck

Vieira

et al. 2015

Monthly Notices of the Royal Astronomical Society

151

224

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We present [CII] observations of 20 strongly lensed dusty star forming galaxies at 2.1 < z < 5.7 using APEX and Herschel. The sources were selected on their 1.4 mm flux (S 1.4 mm > 20 mJy) from the South Pole Telescope survey, with far-infrared (FIR) luminosities determined from extensive photometric data. The [CII] line is robustly detected in 17 sources, all but one being spectrally resolved. Eleven out of 20 sources observed in [CII] also have low-J CO detections from ATCA. A comparison with midand high-J CO lines from ALMA reveals consistent [CII] and CO velocity profiles, suggesting that there is little differential lensing between these species. The [CII], low-J CO and FIR data allow us to constrain the properties of the interstellar medium. We find [CII] to CO(1-0) luminosity ratios in the SPT sample of 5200 ± 1800, with significantly less scatter than in other samples. This line ratio can be best described by a medium of [CII] and CO emitting gas with a higher [CII] than CO excitation temperature, high CO optical depth τ CO (1-0) 1, and low to moderate [CII] optical depth τ [CII] 1. The geometric structure of photodissociation regions allows for such conditions.

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“…Bradford et al 1999;Colbert et al 1999;Stacey et al 1999; C. C. Dudley et al, in preparation; J. Fischer et al, in preparation). Galaxies are identified by name according to the key in the figure.…”

Section: Sourcementioning

confidence: 99%

The [Cii] 158 Micron Line Deficit in Ultraluminous Infrared Galaxies Revisited

Luhman

Satyapal

Fischer

et al. 2003

ApJ

211

350

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We present a study of the [C ii] 157.74 lm fine-structure line in a sample of 15 ultraluminous infrared (IR) galaxies (IR luminosity L IR k10 12 L ; ULIRGs) using the Long Wavelength Spectrometer (LWS) on the Infrared Space Observatory (ISO). We confirm the observed order of magnitude deficit (compared to normal and starburst galaxies) in the strength of the [C ii] line relative to the far-infrared (FIR) dust continuum emission found in our initial report, but here with a sample that is twice as large. This result suggests that the deficit is a general phenomenon affecting 4 out of 5 ULIRGs. We present an analysis using observations of generally acknowledged photodissociation region (PDR) tracers ([C ii], [O i] 63 and 145 lm, and FIR continuum emission), which suggests that a high ultraviolet flux G 0 incident on a moderate density n PDR could explain the deficit. However, comparisons with other ULIRG observations, including CO (1-0), [C i] (1-0), and 6.2 lm polycyclic aromatic hydrocarbon (PAH) emission, suggest that high G 0 =n PDRs alone cannot produce a self-consistent solution that is compatible with all of the observations. We propose that non-PDR contributions to the FIR continuum can explain the apparent [C ii] deficiency. Here, unusually high G 0 and/ or n physical conditions in ULIRGs as compared to those in normal and starburst galaxies are not required to explain the [C ii] deficit. Dust-bounded photoionization regions, which generate much of the FIR emission but do not contribute significant [C ii] emission, offer one possible physical origin for this additional non-PDR component. Such environments may also contribute to the observed suppression of FIR fine-structure emission from ionized gas and PAHs, as well as the warmer FIR colors found in ULIRGs. The implications for observations at higher redshifts are also revisited.

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ISOLWS Spectroscopy of M82: A Unified Evolutionary Model

Cited by 104 publications

References 44 publications

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

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

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

The [Cii] 158 Micron Line Deficit in Ultraluminous Infrared Galaxies Revisited

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