Lithiation of N,N-dimethylmethallylamine

Fitt, John J.; Gschwend, Heinz W.

doi:10.1021/jo00329a046

Cited by 23 publications

(6 citation statements)

References 9 publications

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“…Helou, Soifer & Rowan-Robinson (1985) defined the parameter q as a logarithmic measure of the FIR/radio flux density ratio. For more general comparisons, theq FIR is defined aŝ (Fitt et al 1992), where α is the radio spectral index (S ν ∝ ν α ). The spectral index for the observed GMRT data is −0.79 ± 0.07.…”

Section: Global Radio Continuum Propertiesmentioning

confidence: 99%

“…The spectral index for the observed GMRT data is −0.79 ± 0.07. From the IRAS surveys (Fitt et al 1992) at 60 and 100 µm the flux densities of NGC 2997 are 32.28 and 85.14 Jy, respectively. Using the IRAS FIR flux density measurements and integrated flux densities measured with the GMRT, the derivedq FIR parameter is ∼2.19 ± 0.03, which is close to the median for spiral galaxies at 1.4 GHz, i.e.q FIR ≈ 2.30 with the rms scatter σq 0.2 (Helou, Soifer & Rowan-Robinson 1985;Condon & Broderick 1988;Condon, Frayer & Broderick 1991).…”

Section: Global Radio Continuum Propertiesmentioning

confidence: 99%

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GMRT observations of NGC 2997 and radio detection of the circumnuclear ring

Kodilkar

Kantharia

Ananthakrishnan

2011

Monthly Notices of the Royal Astronomical Society

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We present high‐resolution, high‐sensitivity radio continuum observations of the nearby spiral galaxy NGC 2997 at 332, 616 and 1272 MHz using the Giant Metrewave Radio Telescope (GMRT). The integrated spectrum of this galaxy has a spectral index of −0.92 (Sν ∝ να) and we place an upper limit to the thermal fraction at 1272 MHz of ∼ 10 per cent. Our multifrequency study shows a relatively flat spectrum source (α ∼ −0.6) at the centre of the galaxy. This leads to the radio detection of a circumnuclear ring in the high‐resolution map at 1272 MHz. We detect five hotspots in the ring, with an average star formation rate of ∼0.024 M⊙ yr−1, a median supernova (SN) rate of ∼0.001 yr−1 and luminosity of 1020 W Hz−1. We estimate an equipartition field in the central nuclear region of diameter ∼750 pc to be about G. We also report several interesting features along the spiral arms. In this paper, we present the low‐frequency radio continuum maps, the spectral index distribution, the circumnuclear ring and the derived physical properties.

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Section: Global Radio Continuum Propertiesmentioning

confidence: 99%

Section: Global Radio Continuum Propertiesmentioning

confidence: 99%

GMRT observations of NGC 2997 and radio detection of the circumnuclear ring

Kodilkar

Kantharia

Ananthakrishnan

2011

Monthly Notices of the Royal Astronomical Society

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“…However, this impression may be caused by a selection effect (see review by Soifer, Houck & Neugebauer 1987). Furthermore, high-resolution images of nearby spirals at 100 µm (Fitt et al 1992) show that the 100 µm emission generally is distributed disc-wide, whereas Burstein & Lebofsky need the 100 µm emission to be dominated by the nucleus to achieve large optical depth. Bothun & Rogers (1992) found from optical and 60 µm and 100 µm radial brightness profiles, that galaxy discs are optically thin at both optical and FIR wavelengths.…”

Section: Samplementioning

confidence: 99%

Compact radio cores in Seyfert galaxies

Roy¹,

Norris²,

Kesteven³

et al. 1994

ApJ

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We have observed a sample of 157 Seyfert galaxies with a 275 km baseline radio interferometer to search for compact, high brightness temperature radio emission from the active nucleus. We obtain the surprising result that compact radio cores are much more common in Seyfert 2 than in Seyfert 1 galaxies, which at first seems to be inconsistent with orientation unification schemes. We propose a model, involving optical depth effects in the narrow-line region, which can reconcile our result with the standard unified scheme.

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“…The radio -FIR correlation 1 also holds within starforming galaxies down to scales of below hundred parsec (e.g. Beck & Golla (1988); Bicay, Helou & Condon (1989); Fitt et al (1992); Xu et al (1992); Lu et al (1996); Hoernes, Berkhuijsen & Xu (1998); Hippelein et al (2003); Hughes et al (2006); Paladino et al (2006); Dumas et al (2011); Leverenz & Filipović (2012); Tabatabaei et al (2013b)). However, many authors (starting with Xu et al (1992)) found that the radio -FIR correlation within galaxies only becomes linear on starforming regions but is non-linear, usually with power-law exponent < 1, in other parts of a galaxy.…”

Section: Introductionmentioning

confidence: 98%

How cosmic ray electron propagation affects radio–far-infrared correlations in M 31 and M 33

Berkhuijsen

Beck

Tabatabaei

2013

Monthly Notices of the Royal Astronomical Society

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We investigate the effect of propagation of cosmic-ray electrons (CRE) on the nonthermal (synchrotron) -far-infrared correlations in M 31 and M 33. The thermal (TH) and nonthermal (NTH) emission components of the radio continuum emission at 1.4 GHz and one higher frequency are compared with dust emission from M 31 and M 33 using Spitzer data. In both galaxies the TH emission is linearly correlated with the emission from warm dust (24 µm, 70 µm), but the power laws of the NTH -FIR correlations have exponents b < 1 that increase with increasing frequency. Furthermore, the values of b for M 33 are significantly smaller (b ≃ 0.4) than those for M 31 (b ≃ 0.6). We interpret the differences in b as differences in the diffusion length of the CRE. We estimate the diffusion length in two ways: (1) by smoothing the NTH emission at the higher frequency until the correlation with NTH emission at 1.4 GHz has b = 1, and (2) by smoothing the TH emission until the correlation with the NTH emission at the same frequency has b = 1, assuming that the TH emission represents the source distribution of the CRE. Our smoothing experiments show that M 31 only has a thin NTH disk with a scale height of h = 0.3 − 0.4 kpc at 1.4 GHz, whereas M 33 has a similar thin disk as well as a thick disk with scale height h thick ≃ 2 kpc. In the thin disks, the (deprojected) diffusion length at 1.4 GHz is ≃ 1.5 kpc, yielding a diffusion coefficient of ≃ 2 10 28 cm 2 /s. The structure, strength and regularity of the magnetic field in a galaxy as well as the existence of a thick disk determine the diffusion of the CRE, and hence, the power-law exponent of the NTH -FIR correlations.

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Lithiation of N,N-dimethylmethallylamine

Cited by 23 publications

References 9 publications

GMRT observations of NGC 2997 and radio detection of the circumnuclear ring

GMRT observations of NGC 2997 and radio detection of the circumnuclear ring

Compact radio cores in Seyfert galaxies

How cosmic ray electron propagation affects radio–far-infrared correlations in M 31 and M 33

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