Molecular gas in high-luminosity IRAS galaxies

Sanders, D. B.; Scoville, N. Z.; Young, J. S.; Soifer, B. T.; Schloerb, F. P.; Rice, W.; Danielson, G. E.

doi:10.1086/184682

Cited by 143 publications

(124 citation statements)

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“…The corresponding total molecular hydrogen gas mass of Mrk 266 from the Nobeyama observations is thus M(H 2 ) = 7.0 × 10 9 M . Within the uncertainties, this is consistent with 206 Jy km s −1 measured with single-dish observations (Sanders et al 1986) and a corresponding estimate of M(H 2 ) = 2.5 × 10 9 M when adjusted to α = 1. If the CO to H 2 conversion factor appropriate for Mrk 266 is similar to GMCs in our Milky Way (α = 4±1; Radford et al 1991), the actual gas masses may be ∼4 times larger than the estimates computed here.…”

Section: The Integrated Emission From Co Nch and Hco +supporting

confidence: 90%

Investigation of Dual Active Nuclei, Outflows, Shock-Heated Gas, and Young Star Clusters in Markarian 266

Mazzarella

Iwasawa

Vavilkin

et al. 2012

The Astronomical Journal

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Results of observations with the Spitzer, Hubble, GALEX, Chandra, and XMM-Newton space telescopes are presented for the luminous infrared galaxy (LIRG) merger Markarian 266. The SW (Seyfert 2) and NE (LINER) nuclei reside in galaxies with Hubble types SBb (pec) and S0/a (pec), respectively. Both companions are more luminous than L * galaxies and they are inferred to each contain a ≈ 2.5 × 10 8 M black hole. Although the nuclei have an observed hard X-ray flux ratio of f X (NE)/f X (SW ) = 6.4, Mrk 266 SW is likely the primary source of a bright Fe Kα line detected from the system, consistent with the reflection-dominated X-ray spectrum of a heavily obscured active galactic nucleus (AGN). Optical knots embedded in an arc with aligned radio continuum radiation, combined with luminous H 2 line emission, provide evidence for a radiative bow shock in an AGN-driven outflow surrounding the NE nucleus. A soft X-ray emission feature modeled as shock-heated plasma with T ∼ 10 7 K is cospatial with radio continuum emission between the galaxies. Mid-infrared diagnostics provide mixed results, but overall suggest a composite system with roughly equal contributions of AGN and starburst radiation powering the bolometric luminosity. Approximately 120 star clusters have been detected, with most having estimated ages less than 50 Myr. Detection of 24 μm emission aligned with soft X-rays, radio continuum, and ionized gas emission extending ∼34 (20 kpc) north of the galaxies is interpreted as ∼2 × 10 7 M of dust entrained in an outflowing superwind. At optical wavelengths this Northern Loop region is resolved into a fragmented morphology indicative of Rayleigh-Taylor instabilities in an expanding shell of ionized gas. Mrk 266 demonstrates that the dust "blowout" phase can begin in a LIRG well before the galaxies fully coalesce during a subsequent ultraluminous infrared galaxy (ULIRG) phase, and rapid gas consumption in luminous dual AGNs with kiloparsec-scale separations early in the merger process may explain the paucity of detected binary QSOs (with parsec-scale orbital separations) in spectroscopic surveys. An evolutionary sequence is proposed representing a progression from dual to binary AGNs, accompanied by an increase in observed L x /L ir ratios by over two orders of magnitude.

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Section: The Integrated Emission From Co Nch and Hco +supporting

confidence: 90%

Investigation of Dual Active Nuclei, Outflows, Shock-Heated Gas, and Young Star Clusters in Markarian 266

Mazzarella

Iwasawa

Vavilkin

et al. 2012

The Astronomical Journal

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“…Even with a large potential of star forming fuel, the high star formation rates seen in DSFGs often implies short depletion timescales. Solomon & Sage (1988) provides a succinct summary of the depletion time, or rather L FIR /L CO , for local ULIRGs divided by morphological merger classes, given prior suggestions that mergers and interactions are responsible for elevated L FIR /L CO or lower τ depl over normal star-forming galaxies (Sanders & Mirabel, 1985;Sanders et al, 1986;Young et al, 1986). While they find non-interacting LIRGs have gas depletion timescales of ≈150 +20 −30 Myr, merging or merged galaxies have τ depl = 60 +30 −20 Myr and galaxies with tidal tails and bridges (e.g.…”

Section: Star Formation History and Dynamical Timementioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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“…It is well known (Sanders et al 1988, Sanders & Mirabel 1996, Solomon & Sage 1988) that the star formation efficiency of ULIRGS, which are mergers and closely interacting galaxies, is higher than that of normal spiral galaxies and there is a well-established trend whereby star formation efficiency increases with increasing FIR luminosity. Figure 8, which shows log(L FIR ) as a function of log(L ′ CO ) for normal spirals, LIRGs, ULIRGs, and EMGs, extends the trend above 10 13 L ⊙ .…”

Section: Molecular Gas Mass and Star Formation Efficiencymentioning

confidence: 99%

Molecular Gas at High Redshift

Solomon

Bout

2005

Annu. Rev. Astron. Astrophys.

850

1,013

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The Early Universe Molecular Emission Line Galaxies (EMGs) are a population of galaxies with only 36 examples that hold great promise for the study of galaxy formation and evolution at high redshift. The classification, luminosity of molecular line emission, molecular mass, far-infrared (FIR) luminosity, star formation efficiency, morphology, and dynamical mass of the currently known sample are presented and discussed. The star formation rates derived from the FIR luminosity range from about 300 to 5000 M⊙ year −1 and the molecular mass from 4 × 10 9 to 1 × 10 11 M⊙. At the lower end, these star formation rates, gas masses, and diameters are similar to those of local ultraluminous infrared galaxies, and represent starbursts in centrally concentrated disks, sometimes, but not always, associated with active galactic nuclei.

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Molecular gas in high-luminosity IRAS galaxies

Cited by 143 publications

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Investigation of Dual Active Nuclei, Outflows, Shock-Heated Gas, and Young Star Clusters in Markarian 266

Investigation of Dual Active Nuclei, Outflows, Shock-Heated Gas, and Young Star Clusters in Markarian 266

Dusty star-forming galaxies at high redshift

Molecular Gas at High Redshift

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