CO Observations of the Spiral Galaxy IC 342

Wiklind, T.; Rydbeck, G.; Rydbeck, O. E. H.

doi:10.1007/978-94-009-4782-5_205

Cited by 19 publications

(31 citation statements)

References 3 publications

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“…The mean r 12 for the disk is 1:1 AE 0:2, significantly higher than the 0.66 mean value for the Galactic disk (Sakamoto et al 1995(Sakamoto et al , 1997. Wiklind et al (1990) also found high r 12 values in M83.…”

Section: Co Excitation In M83: Densities and Temperatures In The Molementioning

confidence: 63%

“…Wiklind et al (1990) found nuclear ratios of $1 with marginally higher resolution Swedish-ESO Submillimetre Telescope (SEST) observations. These ratios could imply T ex > 20 K, optically thick, molecular gas as suggested by Aalto (1994).…”

mentioning

confidence: 88%

“…M83 is a nearly face-on, gas-rich SBc spiral galaxy with a starburst nucleus (Rieke 1976;Bohlin et al 1983;Trinchieri, Fabbiano, & Paulumbo 1985;Turner, Ho, & Beck 1987;Telesco, Wolstencroft, & Done 1988;Turner & Ho 1994). It has a pronounced bar and thick spiral arms with welldefined dust lanes and vigorous star formation (Rumstay & Kaufman 1983;Handa et al 1990; Wiklind et al 1990; Tilanus & Allen 1993;Deutsch & Allen 1993;Rand, Lord, & Higdon 1999). The atomic hydrogen (H i) gas disk of M83 is over 1 in diameter (Huchtmeier & Bohnenstengel 1981).…”

Section: Introductionmentioning

confidence: 99%

“…Numerous studies have covered specific aspects of the CO in M83: arm and interarm molecular clouds in the southeastern portion of the optical disk (Wiklind et al 1990); molecular gas in the eastern arm Rand et al 1999); molecular gas at the bar-spiral arm transition ; the bar and nucleus (Handa et al 1990); the nucleus (Combes et al 1978;Petitpas & Wilson 1998). However, M83 has never been fully mapped in CO, perhaps because of its southerly location.…”

Section: Introductionmentioning

confidence: 99%

“…16b), r 12 is also 1:0 AE 0:2. Wiklind et al (1990) found ratios of $1 in the limited arm region contained in their SEST map. The implied T ex > 20 K for optically thick emission is much higher than expected for regions outside of the nucleus.…”

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confidence: 97%

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CO in the Disk of the Barred Spiral Galaxy M83: CO (1–0), CO (2–1), and Neutral Gas

Crosthwaite¹,

Turner²,

Buchholz³

et al. 2002

The Astronomical Journal

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We present '' on-the-fly '' maps of CO (1-0) and CO (2-1) in the barred spiral galaxy M83. The entire optical disk is filled with CO emission in both lines, including interarm regions. For a '' standard '' conversion factor the total molecular mass is 2:5 Â 10 9 M , 4% of the total dynamical mass. Molecular gas constitutes 80% of total gas mass within the inner 10 0 and 30% overall. CO (1-0) emission and 21 cm continuum emission are extremely well correlated spatially in regions where H 2 dominates the gas surface density. The spatial correlation between CO (1-0) and 100 lm emission is not as good. While the kinematics of the outer H i disk is severely nonaxisymmetrically perturbed, the kinematics of the CO disk and inner H i disk is well behaved and circular. The molecular disk appears to have a distinct hard edge at 5 0 . The hard edge is accompanied by a steep decline in the total gas surface density at that radius, although the H i does continue outward at a lower level. This edge is coincident with the onset of strong warping of the outer disk. The mean ratio of CO (2-1)/ CO (1-0) emission is $1, high by Galactic standards. Peaks in this ratio in interarm regions suggest that the CO emission is optically thin there, among other possibilities. Thus, M83 is unusual in that it has a relatively axisymmetric, almost entirely molecular, inner 10 0 gas disk surrounded by a warped, entirely atomic, outer gas disk. A sharp discontinuity separates the inner and outer gas disks. This kind of gas distribution is not seen in other late-type, gas-rich spirals.

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Section: Co Excitation In M83: Densities and Temperatures In The Molementioning

confidence: 63%

mentioning

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 97%

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CO in the Disk of the Barred Spiral Galaxy M83: CO (1–0), CO (2–1), and Neutral Gas

Crosthwaite¹,

Turner²,

Buchholz³

et al. 2002

The Astronomical Journal

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Chemical complexity in galaxies

Turner¹,

Meier²

2008

Science With the Atacama Large Millimeter Array

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ALMA will be able to detect a broad spectrum of molecular lines in galaxies. Current observations indicate that the molecular line emission from galaxies is remarkably variable, even on kpc scales. Imaging spectroscopy at resolutions of an arcsecond or better will reduce the chemical complexity by allowing regions of physical conditions to be defined and classified.A rich spectrum of molecular lines is available at millimeter and submillimeter wavelengths for the study of molecular clouds in galaxies. A recent single dish survey in the λ = 2 mm band of the starburst Sc galaxy NGC 253 revealed lines from 25 [1] of the over 35 molecular species detected to date in external galaxies (see contribution by S. Martín in this volume). Within the reach of ALMA will be thousands of transitions of over a hundred molecules, bringing a vast set of potential diagnostics of molecular gas and physical conditions within galaxies.

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TANGO I: Interstellar medium in nearby radio galaxies

Flaquer¹,

Léon²,

Combes³

et al. 2010

A&A

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Context. Powerful radio-AGN are hosted by massive elliptical galaxies that are usually very poor in molecular gas. Nevertheless, gas is needed at their very center to feed the nuclear activity. Aims. We study the molecular gas properties (i.e., mass, kinematics, distribution, origin) of these objects, and compare them with results for other known samples. Methods. At the IRAM-30m telescope, we performed a survey of the CO(1-0) and CO(2-1) emission from the most powerful radio galaxies of the Local Universe, selected only on the basis of their radio continuum fluxes. Results. The main result of our survey is that the molecular gas content of these galaxies is very low compared to spiral or FIR-selected galaxies. The median value of the molecular gas mass, including detections and upper limits, is 2.2 × 10 8 M . When separated into FR-I and FR-II types, a difference in their H 2 masses is found. The median value of FR-I galaxies is about 1.9 × 10 8 M and higher for FR-II galaxies, at about 4.5 × 10 8 M . Which is probably entirely because of a Malmquist bias. Our results contrast with those of previous surveys, whose targets were mainly selected by means of their FIR emission, implying that we measure higher observed masses of molecular gas. Moreover, the shape of CO spectra suggest that a central molecular gas disk exists in 30% of these radio galaxies, a lower rate than in other active galaxy samples. Conclusions. We find a low level of molecular gas in our sample of radio-selected AGNs, indicating that galaxies do not need much molecular gas to host an AGN. The presence of a molecular gas disk in some galaxies and the wide range of molecular gas masses may be indicative of different origins for the gas, which we can not exclude at present (e.g., minor/major mergers, stellar mass loss, or accretion).

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CO Observations of the Spiral Galaxy IC 342

Cited by 19 publications

References 3 publications

CO in the Disk of the Barred Spiral Galaxy M83: CO (1–0), CO (2–1), and Neutral Gas

CO in the Disk of the Barred Spiral Galaxy M83: CO (1–0), CO (2–1), and Neutral Gas

Chemical complexity in galaxies

TANGO I: Interstellar medium in nearby radio galaxies

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