Aperture synthesis of CO emission in extremely luminous infrared galaxies

Scoville, N. Z.; Sanders, D. B.; Sargent, A. I.; Soifer, B. T.; Tinney, C. G.

doi:10.1086/185543

Cited by 52 publications

(49 citation statements)

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“…While it is still possible that M H2 has been overestimated [25,26] a similarly tight correlation exists between L IR and L HCN , a s w ell as between SFE and L HCN =L CO [35], showing that the fraction of gas at very high densities (n > 10 5 cm 3 ) is greatly increased in ULIR systems. As these fractions are much higher than those found in normal spirals, this indicates that MSFR is intricately linked to the amount of gaseous dissipation [19,26,36].…”

Section: The Tails Of Two Mergersmentioning

confidence: 81%

“…Many studies have e v aluated the SFE in merging galaxies concluding that ULIR mergers are forming stars up to an order of magnitude more e ciently than normal spirals (see Figure 2 and [17]). While there is some question as to whether the Galactic conversion factor between CO and H 2 applies in merging galaxies [19,25,26], the expected variation leads to an overestimate of the molecular gas and therefore underestimates the actual SFEs. It therefore seems hard to escape the conclusion that massive stars are being formed at a higher rate for a given amount of cold gas than in quiescent systems, although the exact level of the enhancement is uncertain.…”

Section: Quantifying the Star Formation Activitymentioning

confidence: 99%

“…It can therefore be used as a measure of the massive star formation rate (MSFR; M > 5 M ) [18]. The IR luminous systems are both gas-rich and dusty [9,19,20], and most of their bolometric luminosity emerges in the far IR [9,17]. While there has been a long-standing debate over whether the most luminous systems are instead powered by an obscured AGN (see e.g.…”

Section: Introductionmentioning

confidence: 99%

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Mergers, interactions, and the fueling of starbursts

Hibbard¹

1997

AIP Conference Proceedings

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Abstract. The most active starbursts are found in galaxies with the highest IR luminosities, with peak star formation rates and e ciencies that are over an order of magnitude higher than in normal disk systems. These systems are almost exclusively on-going mergers. In this review I explore the conditions needed for interactions to experience such a phase by comparing two systems at similar stages of merging but quite di erent IR luminosities: NGC 4038/9 and Arp 299. These observations show that the most intense starbursts occur at the sites with the highest gas densities, which is a general result for IR luminous mergers. Observations and theory both suggest that the strength of the merger induced starburst depends on the internal structure of the progenitors, the amount and distribution of the gas, and the violence of the interaction. In particular, interactions involving progenitors with dense bulges, gas-rich disks, and/or a retrograde spin are expected to preferentially lead to large amounts of gaseous dissipation, although the interplay b e t w een these parameters is unknown. A major outstanding question is how the e ects of feedback alter these conclusions.

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Section: The Tails Of Two Mergersmentioning

confidence: 81%

Section: Quantifying the Star Formation Activitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Mergers, interactions, and the fueling of starbursts

Hibbard¹

1997

AIP Conference Proceedings

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“…(Sanders et al 1987) and CO contour (Scoville et al 1989). Right panel: HST B-band image and identified stellar clusters ('+') from Surace et al (1998).…”

Section: The Nuclear Starburst-agn Connection and Fate Of Uligsmentioning

confidence: 99%

Ultraluminous Infrared Galaxies

Sanders

Surace

Ishida

1999

Symp. - Int. Astron. Union

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Abstract. At luminosities above rv 1011 L 0 , infrared galaxies become the dominant population of extragalactic objects in the local Universe (z < 0.5), being more numerous than optically selected starburst and Seyfert galaxies, and QSOs at comparable bolometric luminosity. At the highest luminosities, ultraluminous infrared galaxies (ULIGs: Lir > 10 12 L 0 ) , outnumber optically selected QSOs by a factor of rv 1.5-2. All of the nearest ULIGs (z <0.1) appear to be advanced mergers that are powered by both a circumnuclear starburst and AGN, both of which are fueled by an enormous concentration of molecular gas (rv 10 10 M 0 ) that has been funneled into the merger nucleus. ULIGs may represent a primary stage in the formation of massive black holes and elliptical galaxy cores. The intense circumnuclear starburst that accompanies the ULIG phase may also represent a primary stage in the formation of globular clusters, and the metal enrichment of the intergalactic medium by gas and dust expelled from the nucleus due to the combined forces of supernova explosions and powerful stellar winds.

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“…Extensive surveys of CO rotation lines in low J transitions such as CO (1-0) at 2.6 mm and CO (2-1) at 1.3 mm have found very large amounts of molecular gas (up to a few times 10 10 M ) in the central kpc of (U)LIRGs (Scoville et al 1989;Sanders et al 1991). This gas, funneled into the nuclear region by the gravitational torque in a merger (Barnes & Hernquist 1996;Hopkins et al 2009), provides fuel for the nuclear starburst and/or AGN.…”

Section: Introductionmentioning

confidence: 99%

ALMA Explorations of Warm Dense Molecular Gas in Nearby LIRGs

Xu¹

2014

Proc. IAU

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Abstract. We present results of ALMA (Cycle-0) observations of the CO (6-5) line emission and the 435μm continuum of two nearby luminous infrared galaxies (LIRGs) NGC 34 (a major merger with an AGN) and NGC 1614 (a minor merger with a circum-nuclear starburst). Using receivers in the highest frequency ALMA band available (Band-9), these observations achieved the best angular resolutions (∼ 0 .25) for ALMA Cycle-0 observations and resolved for the first time distributions of warm dense molecular gas (n > 10 5 cm −3 , T > 100 K) in LIRGs with spatial resolutions better than 100 pc. Our ALMA data show a very tight correlation between the CO (6-5) line emission and the 435μm dust continuum emission, suggesting the warm dense molecular gas dominates the ISM in the central kpc of LIRGs, and gas heating and dust heating in the warm dense gas cores are strongly coupled. On the other hand, we saw very different spatial distributions and kinematic properties of warm dense gas in the two LIRGs, indicating that physical conditions in the ISM can be very different in different LIRGs.

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Aperture synthesis of CO emission in extremely luminous infrared galaxies

Cited by 52 publications

References 0 publications

Mergers, interactions, and the fueling of starbursts

Mergers, interactions, and the fueling of starbursts

Ultraluminous Infrared Galaxies

ALMA Explorations of Warm Dense Molecular Gas in Nearby LIRGs

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