High-resolution X-ray imaging of the Starburst Galaxy M82

Bregman, Joel N.; Schulman, Eric; Tomisaka, Kohji

doi:10.1086/175160

Cited by 70 publications

(76 citation statements)

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“…This implies that in X-ray observations, the value of f v, hot in the disk is not a reliable indicator for starburst. Instead the size of the halo in soft X-rays is strongly correlated with a starburst as can be seen from the size of the X-ray halos in recent XMM-Newton observations of NGC 253 (e.g., Pietsch et al 2001) and NGC 3079 (Breitschwerdt et al 2004), and also ROSAT observations of M 82 (e.g., Bregman et al 1995) and NGC 253 (Dahlem et al 1998;Pietsch et al 2000).…”

Section: Summary and Final Remarksmentioning

confidence: 94%

Volume filling factors of the ISM phases in star forming galaxies

Avillez¹,

Breitschwerdt²

2004

A&A

183

182

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Abstract. The role of matter circulation between the disk and halo in establishing the volume filling factors of the different ISM phases in the Galactic disk (|z| ≤ 250 pc) is investigated, using a modified version of the three-dimensional supernovadriven ISM model of Avillez (2000). We carried out adaptive mesh refinement simulations of the ISM with five supernova rates (in units of the Galactic value), σ/σ Gal = 1, 2, 4, 8 and 16 (corresponding to starburst conditions) using three finer level resolutions of 2.5, 1.25 and 0.625 pc, allowing us to understand how resolution would affect the volumes of gas phases in pressure equilibrium. We find that the volume filling factors of the different ISM phases depend sensitively on the existence of a duty cycle between the disk and halo acting as a pressure release valve for the hot (T > 10 5.5 K) phase in the disk. The amount of cold gas (defined as the gas with T < 10 3 K) picked up in the simulations varies from a value of 19% for σ/σ Gal = 1 to ∼5% for σ/σ Gal = 4 and ≤1% for higher SN rates. Background heating prevents the cold gas from immediate collapse and thus ensures the stability of the cold gas phase. The mean occupation fraction of the hot phase varies from about 17% for the Galactic SN rate to ∼28%, for σ/σ Gal = 4, and to 44% for σ/σ Gal = 16. Overall the filling factor of the hot gas does not increase much as we move towards higher SN rates, following a power law of f v, hot ∝ (σ/σ Gal ) 0.363 . Such a modest dependence on the SN rate is a consequence of the evacuation of the hot phase into the halo through the duty cycle. This leads to volume filling factors of the hot phase considerably smaller than those predicted in the three-phase model of McKee & Ostriker (1977) even in the absence of magnetic fields.

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Section: Summary and Final Remarksmentioning

confidence: 94%

Volume filling factors of the ISM phases in star forming galaxies

Avillez¹,

Breitschwerdt²

2004

A&A

183

182

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“…The nearby (3.25 Mpc; Sandage & Tammann 1975) irregular galaxy M82 (NGC 3034) has kiloparsec-scale bipolar outflows that can be seen by optical emission lines (e.g., Shopbell & Bland-Hawthorn 1998) and by X-ray (e.g., Bregman, Schulman, & Tomisaka 1995;see Fig. 1a).…”

Section: Introductionmentioning

confidence: 99%

Formation of a Massive Black Hole at the Center of the Superbubble in M82

Matsushita

Kawabe

Matsumoto

et al. 2000

The Astrophysical Journal

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We performed CO (1-0), CO (1-0), and HCN (1-0) interferometric observations of the central region 12 13 (about 450 pc in radius) of M82 with the Nobeyama Millimeter Array and have successfully imaged a molecular superbubble and spurs. The center of the superbubble is clearly shifted from the nucleus by 140 pc. This position is close to that of the massive black hole (BH) of տ460 M and the 2.2 mm secondary peak (a luminous , supergiant-dominated cluster), which strongly suggests that these objects may be related to the formation of the superbubble. Consideration of star formation in the cluster based on the infrared data indicates that (1) the energy release from supernovae can account for the kinetic energy of the superbubble, (2) the total mass of stellar-mass BHs available for building up the massive BH may be much higher than 460 M , and (3) it is possible to form , the middle-mass BH of 10 2 -10 3 M within the timescale of the superbubble. We suggest that the massive BH , was produced and is growing in the intense starburst region.

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“…At the same location hot gas emerges into the halo of M 82 (e.g. Shopbell & Bland-Hawthorn 1998;Bregman et al 1995) supporting the idea that the CO spurs indicate the walls of the superbubble.…”

Section: Co Morphology and Kinematicsmentioning

confidence: 57%

“…Bland & Tully 1988;McKeith et al 1995;Shopbell & Bland-Hawthorn 1998) and X-rays (e.g. Bregman et al 1995). The massive star formation (SF) is believed to be fueled by the large amount of molecular gas which is present in the centre of M 82.…”

Section: Introductionmentioning

confidence: 99%

The Effect of Violent Star Formation on the State of the Molecular Gas in M 82

Weiß

Neininger

Hüttemeister

et al. 2001

The Evolution of Galaxies

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Abstract. We present the results of a high angular resolution, multi-transition analysis of the molecular gas in M 82. The analysis is based on the two lowest transitions of 12 CO and the ground transition of the rare isotopes 13 CO and C 18 O measured with the PdBI, the BIMA array and the IRAM 30m telescope. In order to address the question of how the intrinsic molecular cloud properties are influenced by massive star formation we have carried out radiative transfer calculations based on the observed CO line ratios. The calculations suggest that the kinetic temperature of the molecular gas is high in regions with strong star formation and drops towards the outer molecular lobes with less ongoing star formation. The location of the highest kinetic temperature is coincident with that of the mid infrared (MIR) peaks which trace emission from hot dust. The hot gas is associated with low H 2 densities while the cold gas in the outer molecular lobes has high H 2 densities. We find that CO intensities do not trace H 2 column densities well. Most of the molecular gas is distributed in a double-lobed distribution which surrounds the starburst. A detailed analysis of the conversion factor from CO intensity to H 2 column density shows that X CO depends on the excitation conditions. We find X CO ∼ T −1 kin n(H 2 ) 1/2 , as expected for virialized clouds.

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High-resolution X-ray imaging of the Starburst Galaxy M82

Cited by 70 publications

References 0 publications

Volume filling factors of the ISM phases in star forming galaxies

Volume filling factors of the ISM phases in star forming galaxies

Formation of a Massive Black Hole at the Center of the Superbubble in M82

The Effect of Violent Star Formation on the State of the Molecular Gas in M 82

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