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

Matsushita, Satoki; Kawabe, Ryohei; Matsumoto, Hironori; Tsuru, Takeshi Go; Kohno, Kotaro; Morita, Koh-Ichiro; Okumura, Sachiko K.; Vila-Vilaro, Baltasar

doi:10.1086/317880

Cited by 75 publications

(101 citation statements)

References 31 publications

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“…3.2.4) are quite similar. A more recent study by Weiß et al (1999) discovered an additional CO feature in M 82 that is suggested to be a superbubble driven by a starburst in its center (Matsushita et al 2000), similar to the wildfire mode proposed by Alonso-Herrero et al (2001) for NGC 1614.…”

Section: Comparing Ngc 1614 With Galaxies With Nuclear Molecular Ringssupporting

confidence: 56%

The NGC 1614 interacting galaxy

König

Aalto

Müller

et al. 2013

A&A

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Minor mergers frequently occur between giant and gas-rich low-mass galaxies and can provide significant amounts of interstellar matter to refuel star formation and power active galactic nuclei (AGN) in the giant systems. Major starbursts and/or AGN result when fresh gas is transported and compressed in the central regions of the giant galaxy. This is the situation in the starburst minor merger NGC 1614, whose molecular medium we explore at half-arcsecond angular resolution through our observations of 12 CO (2−1) emission using the Submillimeter Array (SMA). We compare our 12 CO (2−1) maps with optical and Paα, Hubble Space Telescope and high angular resolution radio continuum images to study the relationships between dense molecular gas and the NGC 1614 starburst region. The most intense 12 CO emission occurs in a partial ring with ∼230 pc radius around the center of NGC 1614, with an extension to the northwest into the dust lane that contains diffuse molecular gas. We resolve ten giant molecular associations (GMAs) in the ring, which has an integrated molecular mass of ∼8 × 10 8 M . Our interferometric observations filter out a large part of the 12 CO (1−0) emission mapped at shorter spacings, indicating that most of the molecular gas is diffuse and that GMAs only exist near and within the circumnuclear ring. The molecular ring is uneven with most of the mass on the western side, which also contains GMAs extending into a pronounced tidal dust lane. The spatial and kinematic patterns in our data suggest that the northwest extension of the ring is a cosmic umbilical cord that is feeding molecular gas associated with the dust lane and tidal debris into the nuclear ring, which contains the bulk of the starburst activity. The astrophysical process for producing a ring structure for the final resting place of accreted gas in NGC 1614 is not fully understood, but the presence of numerous GMAs suggests an orbit-crowding or resonance phenomenon. There is some evidence that star formation is progressing radially outward within the ring, indicating that a self-triggering mechanism may also affect star formation processes. The net result of this merger therefore very likely increases the central concentration of stellar mass in the NGC 1614 remnant giant system.

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Section: Comparing Ngc 1614 With Galaxies With Nuclear Molecular Ringssupporting

confidence: 56%

The NGC 1614 interacting galaxy

König

Aalto

Müller

et al. 2013

A&A

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“…The HCN and HCO + data are in good agreement with previous measurements (e.g., Nguyen et al 1992). The gas disk in M82 is known to house two giant photodissociation regions (PDRs; e.g., García-Burillo et al 2002) and probably also a central massive black hole in formation (e.g., Matsushita et al 2000;Patruno et al 2006) and a superbubble emerging from a past SNE (e.g., Wei% et al 1999;Kronberg et al 1985). A different gas chemistry could hence be at play in the center than in the two PDRs.…”

Section: M82: Sb-dominated Galaxymentioning

confidence: 99%

A Multi‐Transition HCN and HCO⁺Study of 12 Nearby Active Galaxies: Active Galactic Nucleus versus Starburst Environments

Krips

Neri

García‐Burillo

et al. 2008

ApJ

249

377

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Recent studies have indicated that the HCN-to-CO(J ¼ 1Y0) and HCO + -to-HCN(J ¼ 1Y0) ratios are significantly different between galaxies with AGN (active galactic nucleus) and SB (starburst) signatures. In order to study the molecular gas properties in active galaxies and search for differences between AGN and SB environments, we observed the, and HCO + (J ¼ 3Y2) emission with the IRAM 30 m in the center of 12 nearby active galaxies which either exhibit nuclear SB and/or AGN signatures. Consistent with previous results, we find a significant difference of the HCN(, and HCO + -to-HCN intensity ratios between the sources dominated by an AGN and those with an additional or pure central SB: the HCN, HCO + , and HCO + -to-HCN intensity ratios tend to be higher in the galaxies of our sample with a central SB as opposed to the pure AGN cases, which show rather low intensity ratios. Based on an LVG analysis of these data, i.e., assuming purely collisional excitation, the (average) molecular gas densities in the SB-dominated sources of our sample seem to be systematically higher than in the AGN sources. The LVG analysis seems to further support systematically higher HCN and/or lower HCO + abundances as well as similar or higher gas temperatures in AGNs compared to the SB sources of our sample. In addition, we find that the HCN-to-CO ratios decrease with increasing rotational number J for the AGNs while they stay mostly constant for the SB sources.

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“…X-ray observations have revealed the presence of intermediatemass black holes with masses of 10 3 -10 6 M in M82 (Matsumoto et al 2001;Kaaret et al 2001), whose locations were found to coincide with the star clusters found by SUBARU observations (T. Harashima et al 2002, in preparation). In addition, a very energetic expanding molecular superbubble has been discovered (Matsushita et al 2000). These findings have created a lot of interest in the formation of black holes of various masses and the evolution of starburst galaxies (e.g., Ebisuzaki et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Peculiar Chemical Abundances in the Starburst Galaxy M82 and Hypernova Nucleosynthesis

Umeda

Nomoto

Tsuru

et al. 2002

ApJ

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X-ray observations have shown that the chemical abundance in the starburst galaxy M82 is quite rich in Si and S compared to oxygen. Such an abundance pattern cannot be explained with any combination of conventional Type I and II supernova yields. In addition, the energy-to-heavy-element mass ratio of the observed hot plasma is much higher than the value resulting from normal supernovae. We calculate abundances for explosive nucleosynthesis in core-collapse hypernovae and show that the abundance pattern and the large ratio between the energy and the heavy-element mass can be explained with hypernova nucleosynthesis. Such hypernova explosions are expected to occur for stars more massive than e20-25 M , and they likely dominate the starburst, because the time since the starburst in M82 is estimated to be as short as $10 6 -10 7 yr. We also investigate pair-instability supernovae ($150-300 M ) and conclude that the energy-to-heavy-element mass ratio in these supernovae is too small to explain the observation.

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

Cited by 75 publications

References 31 publications

The NGC 1614 interacting galaxy

The NGC 1614 interacting galaxy

A Multi‐Transition HCN and HCO⁺Study of 12 Nearby Active Galaxies: Active Galactic Nucleus versus Starburst Environments

Peculiar Chemical Abundances in the Starburst Galaxy M82 and Hypernova Nucleosynthesis

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

Cited by 75 publications

References 31 publications

The NGC 1614 interacting galaxy

The NGC 1614 interacting galaxy

A Multi‐Transition HCN and HCO+Study of 12 Nearby Active Galaxies: Active Galactic Nucleus versus Starburst Environments

Peculiar Chemical Abundances in the Starburst Galaxy M82 and Hypernova Nucleosynthesis

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A Multi‐Transition HCN and HCO⁺Study of 12 Nearby Active Galaxies: Active Galactic Nucleus versus Starburst Environments