Extreme Star Formation in the Interacting Galaxy Arp 299 (IC 694 + NGC 3690)

Alonso‐Herrero, A.; Rieke, G. H.; Rieke, M. J.; Scoville, N. Z.

doi:10.1086/308622

Cited by 121 publications

(223 citation statements)

References 60 publications

(94 reference statements)

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“…While the near-IR dominates the emission of the southern nucleus (designated B in the literature Gehrz et al 1983), the northwest component (designated C) has a comparable emission, and the northeast component (C ) is very faint at 2.2 µm. This near-IR faintness was discussed by Alonso-Herrero et al (2000), whose starburst models predict a persistence of the emission at 2 µm after their assumed Gaussian burst with a FWHM of 5 Myr. They concluded then that the star formation episode must have been shorter in C .…”

Section: Radio and Near-ir Comparisonmentioning

confidence: 81%

Star formation and AGN activity in a sample of local luminous infrared galaxies through multiwavelength characterization

Herrero-Illana

Pérez-Torres

Randriamanakoto

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Nuclear starbursts and AGN activity are the main heating processes in luminous infrared galaxies (LIRGs) and their relationship is fundamental to understand galaxy evolution. In this paper, we study the star-formation and AGN activity of a sample of 11 local LIRGs imaged with subarcsecond angular resolution at radio (8.4 GHz) and near-infrared (2.2 µm) wavelengths. This allows us to characterize the central kpc of these galaxies with a spatial resolution of 100 pc. In general, we find a good spatial correlation between the radio and the near-IR emission, although radio emission tends to be more concentrated in the nuclear regions. Additionally, we use an MCMC code to model their multi-wavelength spectral energy distribution (SED) using template libraries of starburst, AGN and spheroidal/cirrus models, determining the luminosity contribution of each component, and finding that all sources in our sample are starburst-dominated, except for NGC 6926 with an AGN contribution of 64%. Our sources show high star formation rates (40 to 167 M yr −1 ), supernova rates (0.4 to 2.0 SN yr −1 ), and similar starburst ages (13 to 29 Myr), except for the young starburst (9 Myr) in NGC 6926. A comparison of our derived star-forming parameters with estimates obtained from different IR and radio tracers shows an overall consistency among the different star formation tracers. AGN tracers based on mid-IR, high-ionization line ratios also show an overall agreement with our SED model fit estimates for the AGN. Finally, we use our wide-band VLA observations to determine pixel-by-pixel radio spectral indices for all galaxies in our sample, finding a typical median value (α −0.8) for synchrotron-powered LIRGs.

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Section: Radio and Near-ir Comparisonmentioning

confidence: 81%

Star formation and AGN activity in a sample of local luminous infrared galaxies through multiwavelength characterization

Herrero-Illana

Pérez-Torres

Randriamanakoto

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…These galaxies have K-band magnitudes in the range $12Y13.5. All of the LIRGs are nearby (v < 17; 000 km s À 1 ), and many have millimeter CO emission measurements (e.g., Sanders et al 1991), as well as NICMOS-2 images of their inner regions Alonso-Herrero et al 2000). Thus, we are able to choose galaxies with very compact nuclear a Kim et al (1995).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Dynamical Masses in Luminous Infrared Galaxies

Hinz

Rieke

2006

ApJ

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We have studied the dynamics and masses of a sample of 10 nearby luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs, respectively) using 2.3 m 12 CO-absorption line spectroscopy and near-infrared H-and K s -band imaging. By combining velocity dispersions derived from the spectroscopy, disk scale lengths obtained from the imaging, and a set of likely model density profiles, we calculate dynamical masses for each LIRG. For the majority of the sample, it is difficult to reconcile our mass estimates with the large amounts of gas derived from millimeter observations and from a standard conversion between 12 CO emission and H 2 mass. Our results imply that LIRGs do not have huge amounts of molecular gas (10 10 Y10 11 M ) at their centers and support previous indications that the standard conversion of 12 CO to H 2 probably overestimates the gas masses and cannot be used in these environments. This in turn suggests much more modest levels of extinction in the near-infrared for LIRGs than previously predicted (A V $ 10Y20 vs. A V $ 100Y1000). The lower gas mass estimates indicated by our observations imply that the star formation efficiency in these systems is very high and is triggered by cloud-cloud collisions, shocks, and winds rather than by gravitational instabilities in circumnuclear gas disks.

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“…Based on H i observations, Nordgren et al (1997) determined the systemic velocity of the system to be 3121 km s −1 , yielding a redshift of z = 0.010411. At a distance of 44.8 Mpc (linear scale: 217 pc/arcsec) (Fixsen et al 1996;Nordgren et al 1997, assum-ing H 0 = 73 km s −1 Mpc −1 ) the IR luminosity of the system is L IR ≈ 6.6 × 10 11 L ⊙ (Sanders et al 2003) of which Arp 299A contributes about 40 − 50% (Alonso-Herrero et al 2000;Charmandaris et al 2002). All three regions also exhibit bright molecular emission from hydrogen cyanide (HCN) J = 1 − 0 and carbon monoxide (CO) (Sargent & Scoville 1991;Aalto et al 1997).…”

Section: Introductionmentioning

confidence: 99%

Inflowing gas onto a compact obscured nucleus in Arp 299A

Falstad¹,

González-Alfonso²,

Aalto³

et al. 2017

A&A

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Aims. We probe the physical conditions in the core of Arp 299A and try to put constraints to the nature of its nuclear power source. − doublet at 119 µm is found redshifted by ∼175 km s −1 compared with other OH and H 2 O lines, suggesting a low excitation inflow. We find that at least two components are required in order to account for the excited molecular line spectrum. The inner component has a radius of 20 − 25 pc, a very high infrared surface brightness ( 3 × 10 13 L ⊙ kpc −2 ), warm dust (T d > 90 K), and a large H 2 column density (N H 2 > 10 24 cm −2 ). The modeling also indicates high nuclear H 2 O (1 − 5 × 10 −6 ) and OH (0.5 − 5 × 10 −5 ) abundances relative to H nuclei. The outer component is larger (50 − 100 pc) with slightly cooler dust (70 − 90 K) and molecular abundances that are about one order of magnitude lower. In addition to the two components that account for the excited OH and H 2 O lines, we require a much more extended inflowing component to account for the OH 2 Π 3/2 − 2 Π 3/2 5 2− doublet at 119 µm. Conclusions. The Compton-thick nature of the core makes it difficult to determine the nature of the buried power source, but the high surface brightness indicates that it is either an active galactic nucleus and/or a dense nuclear starburst. Our results are consistent with a composite source. The high OH/H 2 O ratio in the nucleus indicates that ion-neutral chemistry induced by X-rays or cosmic-rays is important. Finally we find a lower limit to the 16 O/ 18 O ratio of 400 in the nuclear region, possibly indicating that the nuclear starburst is in an early evolutionary stage, or that it is fed through a molecular inflow of, at most, solar metallicity.

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Extreme Star Formation in the Interacting Galaxy Arp 299 (IC 694 + NGC 3690)

Cited by 121 publications

References 60 publications

Star formation and AGN activity in a sample of local luminous infrared galaxies through multiwavelength characterization

Star formation and AGN activity in a sample of local luminous infrared galaxies through multiwavelength characterization

Dynamical Masses in Luminous Infrared Galaxies

Inflowing gas onto a compact obscured nucleus in Arp 299A

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