A catalog of IRAS observations of large optical galaxies

Rice, W.; Lonsdale, C. J.; Soifer, B. T.; Neugebauer, G.; Koplan, E. L.; Lloyd, L. A.; Jong, T. de; Habing, H. J.

doi:10.1086/191283

Cited by 292 publications

(322 citation statements)

References 3 publications

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“…In this model, there is only a small mass of cool gas at higher densities (n H 2 = 10 4 cm −3 ). Given the star-burst nature of NGC 3628, model 5 appears physically more plausible, as is also suggested by the presence of warm dust in NGC 3628 (Rice et al 1988). In terms of beam-averaged quantities, the difference between the two models is slight.…”

Section: Ngc 3628mentioning

confidence: 82%

CI and CO in nearby galaxy centers

Israel¹

2009

A&A

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Aims. We study the physical properties and mass of molecular gas in the central regions of galaxies with active nuclei. Methods. Maps and measurements of the J = 1-0, J = 2-1, J = 3-2, J = 4-3 12 CO, the J = 1-0, J = 2-1 and J = 3-2 13 CO lines in the central arcminute squared of NGC 278, NGC 660, NGC 3628, NGC 4631, and NGC 4666, as well as 492 GHz [CI] maps in three of these are used to model the molecular gas. Results. All five objects contain bright CO emission in the central regions. Clear central concentrations were found in NGC 660, NGC 3628, and NGC 4666, but not in the weakest CO emitters NGC 278 and NGC 4631. In all cases, the observed lines could be modeled only with at least two distinct gas components. The physical condition of the molecular gas is found to differ from galaxy to galaxy. Relatively tenuous (density 100-1000 cm −3 ) and high kinetic temperature (100-150 K) gas occur in all galaxies, except perhaps NGC 3628, mixed with cooler (10-30 K) and denser (0.3−1.0 × 10 4 cm −3 ) gas. The CO-to-H 2 conversion factor X is typically an order of magnitude less than the "standard" value in the Solar Neighborhood in all galaxy centers. The molecular gas is constrained within radii between 0.6 and 1.5 kpc from the nuclei. Within these radii, H 2 masses are typically 0.6−1.5 × 10 8 M , which corresponds to no more than a few per cent of the dynamical mass in the same region.

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Section: Ngc 3628mentioning

confidence: 82%

CI and CO in nearby galaxy centers

Israel¹

2009

A&A

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“…Comparing the LFIR/µ for the SPT sources 11 , which lie in the range (1.1 − 21.9)µ −1 × 10 12 L , with the local starburst galaxy M82 (LFIR∼ (2.3 − 3.2) × 10 10 L , Rice et al 1988 andColbert et al 1999) show the significant difference in LFIR at high and low redshifts. Using this comparison and estimates of G0 for each SPT DSFG, we estimate approximate sizes of the PDRs populating the galaxies, following Stacey et al (2010).…”

Section: Sizes Of Pdrsmentioning

confidence: 95%

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Gullberg

Breuck

Vieira

et al. 2015

Monthly Notices of the Royal Astronomical Society

154

224

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We present [CII] observations of 20 strongly lensed dusty star forming galaxies at 2.1 < z < 5.7 using APEX and Herschel. The sources were selected on their 1.4 mm flux (S 1.4 mm > 20 mJy) from the South Pole Telescope survey, with far-infrared (FIR) luminosities determined from extensive photometric data. The [CII] line is robustly detected in 17 sources, all but one being spectrally resolved. Eleven out of 20 sources observed in [CII] also have low-J CO detections from ATCA. A comparison with midand high-J CO lines from ALMA reveals consistent [CII] and CO velocity profiles, suggesting that there is little differential lensing between these species. The [CII], low-J CO and FIR data allow us to constrain the properties of the interstellar medium. We find [CII] to CO(1-0) luminosity ratios in the SPT sample of 5200 ± 1800, with significantly less scatter than in other samples. This line ratio can be best described by a medium of [CII] and CO emitting gas with a higher [CII] than CO excitation temperature, high CO optical depth τ CO (1-0) 1, and low to moderate [CII] optical depth τ [CII] 1. The geometric structure of photodissociation regions allows for such conditions.

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“…not corrected for extinction) from the Third Reference Catalog of Bright Galaxies, (RC 3 -de Vaucouleurs et al 1991), we have used radio data obtained or collected by Loiseau et al (1987), Mountfort et al (1987), Alvarez et al (1987Alvarez et al ( , 1989, Klein et al (1989), Ye & Turtle (1991), and Haynes et al (1991). Infrared and submillimeter continuum data were taken from Schwering (1988), Rice et al (1988), Stanimirovic et al (2000), Aguirre et al (2003), Wilke et al (2004), Hughes et al (2006), Bolatto et al (2007), and Leroy et al (2007). The ultraviolet data of the LMC are those of Page & Carruthers (1981).…”

Section: Literature Datamentioning

confidence: 99%

Submillimeter to centimeter excess emission from the Magellanic Clouds

Israel¹,

Wall

Raban³

et al. 2010

A&A

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Aims. Our goal is to determine and study the global emission from the Magellanic Clouds over the full radio to ultraviolet spectral range. Methods. We have selected from the literature those flux densities that include the entire LMC and SMC respectively, and we have complemented these with maps extracted from the WMAP and COBE databases covering the missing 23−90 GHz (13-3.2 mm) and the poorly sampled 1.25-250 THz (240-1.25 μm) spectral ranges in order to reconstruct the global SEDs of the Magellanic Clouds over eight decades in frequency or wavelength. Results. A major result is the discovery of a pronounced excess of emission from the Magellanic Clouds at millimeter and submillimeter wavelengths. We also confirm global mid-infrared (12 μm) emission suppression, and determine accurate thermal radio fluxes and very low global extinctions for both LMC and SMC, the latter being the most extreme in all these respects. Conclusions. These and other dust properties such as the far-UV extinction curve appear to be correlated with (low) metallicity. Possible explanations are briefly considered. As long as the nature of the excess emission is unknown, the total dust masses and gas-to-dust ratios of the Magellanic Clouds cannot reliably be determined

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A catalog of IRAS observations of large optical galaxies

Cited by 292 publications

References 3 publications

CI and CO in nearby galaxy centers

CI and CO in nearby galaxy centers

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Submillimeter to centimeter excess emission from the Magellanic Clouds

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