High-Resolution CO Observations of Luminous Infrared Galaxies

Bryant, P. M.; Scoville, N. Z.

doi:10.1086/300879

Cited by 207 publications

(277 citation statements)

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“…-a common finding of the ULIRG galaxy studies (Bryant & Scoville 1999). The nucleus of Arp 220 has a total molecular gas mass M H 2 ∼ 9 × 10 9 M within 300 pc (Scoville et al 1997;Downes & Solomon 1998;Sakamoto et al 1999;Tacconi et al 1999).…”

Section: Arp 220 -A Prototypical Ulirgmentioning

confidence: 87%

“…Millimetre-wave imaging provides a unique capability to probe such starburst nuclei in dusty LIRG/ULIRGs since the dust is optically thin at long wavelengths. Virtually all of the ULIRGs observed so far have massive concentrations of molecular gas in the central few kiloparsec (Scoville et al 1997;Downes & Solomon 1998;Bryant & Scoville 1999;Tacconi et al 1999).…”

Section: Arp 220 -A Prototypical Ulirgmentioning

confidence: 99%

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Evolution of star formation and gas

Scoville¹

2013

Secular Evolution of Galaxies

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In these lectures I review observations of star-forming molecular clouds in our Galaxy and nearby galaxies to develop a physical intuition for understanding star formation in the local and high-redshift Universe. A lot of this material is drawn from early work in the field since much of the work was done two decades ago and this background is not generally available in the present literature. I also attempt to synthesise our welldeveloped understanding of star formation in low-redshift galaxies with constraints from theory and observations at high redshift to develop an intuitive model for the evolution of galaxy mass and luminosity functions in the early Universe.The overall goal of this contribution is to provide students with background helpful for analysis of far-infrared (FIR) observations from Herschel and millimetre/submillimetre (mm/submm) imaging with ALMA (the Atacama Large Millimetre/submillimetre Array).These two instruments will revolutionise our understanding of the interstellar medium (ISM) and associated star formation and galaxy evolution, both locally and in the distant Universe. To facilitate interpreting the FIR spectra of Galactic star-forming regions and high-redshift sources, I develop a model for the dust heating and radiative transfer in order to elucidate the observed infrared (IR) emissions. I do this because I am not aware of a similar coherent discussion in the literature. Star-forming molecular cloudsHere, I provide an overview of the observations and physics of star-forming molecular clouds in the Galaxy and nearby normal galaxies. The motivation is to develop the intuitive background for analysis of observations at high 1 arXiv:1210.6990v2 [astro-ph.CO] 1 Nov 2012

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Section: Arp 220 -A Prototypical Ulirgmentioning

confidence: 87%

Section: Arp 220 -A Prototypical Ulirgmentioning

confidence: 99%

Evolution of star formation and gas

Scoville¹

2013

Secular Evolution of Galaxies

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“…If we assume a constant dust-to-gas ratio and rely on the SchmidtKennicutt law (Schmidt 1959;Kennicutt 1998), this implies denser star-forming gas in ULIRGs (as observed by e.g. Gao & Solomon 2004;Bryant & Scoville 1999;Iono et al 2009;Juneau et al 2009). These results are consistent with the scenario in Specific star formation rate averaged over the last 100 Myr, ψ S ; d) doubling timescale for the stellar mass, assuming the galaxies would continue forming stars at the present rate; e) dust mass, M d ; f) fraction of total dust luminosity contributed by the diffuse ISM, f μ ; g) temperature of warm dust in the birth cloud component, T BC W ; h) fraction of total dust luminosity contributed by warm dust in thermal equilibrium, ξ tot W ; i) temperature of cold dust in the diffuse ISM, T ISM C ; j) fraction of total dust luminosity contributed by cold dust in thermal equilibrium, ξ tot C .…”

Section: Comparison With Local Galaxies Of Infrared Luminositiesmentioning

confidence: 98%

Exploring the physical properties of local star-forming ULIRGs from the ultraviolet to the infrared

Cunha

Charmandaris

Díaz-Santos

et al. 2010

A&A

119

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We apply the da Cunha et al. (2008, MNRAS, 388, 1595 model of the spectral energy distribution (SEDs) of galaxies to a small pilot sample of purely star-forming ultra-luminous infrared galaxies (ULIRGs). We interpret the observed SEDs of 16 ULIRGs using this physically-motivated model that accounts for both the emission of stellar populations from the ultraviolet to the near-infrared and for the attenuation by dust in two components: an optically-thick starburst component and the diffuse ISM. The infrared emission is computed by assuming that all the energy absorbed by dust in these components is re-radiated at mid-and far-infrared wavelengths. This model allows us to derive statistically physical properties including star formation rates, stellar masses, the temperatures and masses of different dust components, and plausible star formation histories. We find that, although the ultraviolet-to-near-infrared emission represents only a small fraction of the total power radiated by ULIRGs, observations in this wavelength range are important for understanding the properties of the stellar populations and dust attenuation in the diffuse ISM of these galaxies. Furthermore, our analysis indicates that the use of mid-infrared spectroscopy from the infrared spectrograph on the Spitzer Space Telescope is crucial to obtain realistic estimates of the extinction to the central energy source, mainly via the depth of the 9.7-μm silicate feature, and thus accurately constrain the total energy balance. Our findings are consistent with the notion that, in the local Universe, the physical properties of ULIRGs are fundamentally different from those of galaxies with lower infrared luminosities and that local ULIRGs are the result of merger-induced starbursts. While these are well-established ideas, we demonstrate the usefulness of our SED modelling in deriving relevant physical parameters that provide clues to the star formation mode of galaxies.

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“…Different studies of the molecular and atomic gas towards IC 883 (Downes & Solomon 1998;Bryant & Scoville 1999;Clemens & Alexander 2004) provide evidence of the rotation of the disc from south-east towards north-west. This situation would imply that the putative jet is perpendicular to the rotation axis, and hence that no projection effect could explain the superposition of the jet on the disc.…”

Section: The Circumnuclear Regions Of Ic 883: a Jet Or A Disc?mentioning

confidence: 99%

e-MERLIN and VLBI observations of the luminous infrared galaxy IC 883: a nuclear starburst and an AGN candidate revealed

Romero-Cañizales

Pérez-Torres

Alberdi

et al. 2012

A&A

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Context. The high star formation rates of luminous infrared galaxies (LIRGs) make them ideal places for core-collapse supernova (CCSN) searches. Massive star formation can often be found in coexistence with an active galactic nucleus (AGN), contributing jointly to the energy source of LIRGs. At radio frequencies, where light is unaffected by dust extinction, it is possible to detect compact components within the innermost LIRG nuclear regions, such as SNe and SN remnants, as well as AGN buried deep in the LIRG nuclei. Aims. Our study of the LIRG IC 883 aims at: (i) investigating the parsec-scale radio structure of the (circum-)nuclear regions of IC 883; (ii) detecting at radio frequencies the two recently reported circumnuclear SNe 2010cu and 2011hi, which were discovered by near-IR (NIR) adaptive optics observations of IC 883; and (iii) further investigating the nature of SN 2011hi at NIR wavelengths. Methods. We used the electronic European very long baseline interferometry (VLBI) Network (e-EVN) at 5 GHz, and the electronic Multi-Element Remotely Linked Interferometer Network (e-MERLIN) at 6.9 GHz, to observe contemporaneously the LIRG IC 883 at high angular-resolution (from tens to hundreds of milliarcsec) and with high sensitivity (<70 μJy), complemented by archival VLBI data at 5 GHz and 8.4 GHz. We also used the Gemini North telescope to obtain late-time JHK photometry for SN 2011hi. Results. The circumnuclear regions traced by e-MERLIN at 6.9 GHz have an extension of ∼1 kpc, at a position angle of 130 • , and show a striking double-sided structure, which very likely corresponds to a warped rotating ring, in agreement with previous studies. Our e-EVN observations at 5 GHz and complementary archival VLBI data at 5 GHz and 8.4 GHz, reveal various milliarcsec compact components in the nucleus of IC 883. A single compact source, an AGN candidate, dominates the emission at both nuclear and circumnuclear scales, as imaged with the e-EVN and e-MERLIN, respectively. The other milliarcsec components are strongly indicative of ongoing nuclear CCSN activity. Our e-EVN observations also provided upper limits to the radio luminosity of the two SNe in IC 883 recently discovered at NIR wavelengths. We refine the classification of SN 2011hi as a Type IIP SN according to our latest epoch of Gemini North observations acquired in 2012, in agreement with a low-luminosity radio SN nature. We estimate a CCSN rate lower limit of 1.1 +1.3 −0.6 yr −1 for the entire galaxy, based on three nuclear radio SNe and the circumnuclear SNe 2010cu and 2011hi.

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High-Resolution CO Observations of Luminous Infrared Galaxies

Cited by 207 publications

References 93 publications

Evolution of star formation and gas

Evolution of star formation and gas

Exploring the physical properties of local star-forming ULIRGs from the ultraviolet to the infrared

e-MERLIN and VLBI observations of the luminous infrared galaxy IC 883: a nuclear starburst and an AGN candidate revealed

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