Ultraviolet to near-infrared continuum flux distribution in the active binary RS canum venaticorum

1990 ◽  
Vol 169 (1-2) ◽  
pp. 233-236
Author(s):  
A. Gim�nez ◽  
V. Reglero ◽  
J. Fabregat
Keyword(s):  
Near Infrared ◽  
Flux Distribution ◽  
Infrared Continuum

scholarly journals On the Nature of the Binary Components of RX J0806.3+1527

2004 ◽  
Vol 194 ◽  
pp. 122-123
Author(s):  
K. Reinsch ◽  
V. Burwitz ◽  
R. Schwarz
Keyword(s):  
Main Sequence ◽  
Near Infrared ◽  
Flux Distribution ◽  
Galactic Disk ◽  
Modulation Amplitude ◽  
Direct Impact ◽  
Infrared Photometry ◽  
Short Period ◽  
Cyclotron Emission ◽  
Magnetic Nature

AbstractWe present imaging circular polarimetry and near-infrared photometry of the suspected ultra-short period while-dwarf binary RX J0806.3+1527 obtained with the ESO VLT and discuss the implications for a possible magnetic nature of the white dwarf accretor and the constraints derived for the nature of the donor star. Our V-filter data, show marginally significant circular polarization with a modulation amplitude of ≈ 0.5% typical for cyclotron emission from an accretion column in a magnetic field of order 10MG and not compatible with a direct-impact accretor model. The optical to near-infrared flux distribution is well described by a single blackbody with temperature kTbb = 35000 K and excludes a main-sequence stellar donor unless the binary is located several scale heights above the galactic disk population.

Visible to near-infrared continuum generation in a water-core photonic crystal fiber

2008 ◽  
Author(s):  
Alexandre Bozolan ◽  
Cristiano M. B. Cordeiro ◽  
Christiano J. S. de Matos ◽  
Eliane M. dos Santos ◽  
Carlos H. Brito Cruz ◽  
...  
Keyword(s):  
Photonic Crystal ◽  
Photonic Crystal Fiber ◽  
Near Infrared ◽  
Continuum Generation ◽  
Crystal Fiber ◽  
Infrared Continuum

scholarly journals Low Frequency Cutoffs in the Spectra of Radioquiet Quasars

1987 ◽  
Vol 121 ◽  
pp. 135-139
Author(s):  
R. Antonucci ◽  
R. Barvainis
Keyword(s):  
High Frequency ◽  
Near Infrared ◽  
Dust Emission ◽  
Low Frequency ◽  
Far Infrared ◽  
Low Energy Electrons ◽  
Order Of Magnitude ◽  
Infrared Continuum ◽  
Lower Cutoff ◽  
Rule Out

Radio-quiet and normal radio-loud quasars have very similar spectral properties in the ultraviolet, optical and near infrared regions, but their radio powers differ by several orders of magnitude. Somewhere between the near infrared and the radio their spectra must diverge dramatically.The IRAS survey detected 17 radio quiet quasars and luminous Seyfert 1's with −29. 5 ≤ Mv ≤ −21.6 (for Ho = 75). By coadding the survey data and using pointed observations, we have detections of most of these objects in all four IRAS passbands. The spectra are all rising with wavelength all the way to 100μ. We are measuring fluxes in the centimeter, millimeter, and, together with R Cutri, the near infrared and optical regions for each of these objects. Our goal is to constrain the location, shape, and spectral context of the low frequency cutoffs. Here we present the IRAS, millimeter and centimeter data. Measurements at the other wavelengths are still in progress.Although the spectra are rising steeply between 60μ and 100μ, we find that all of our objects are undetectable at 1.3 mm with the NRAO 12-m telescope. Our limits are typically an order of magnitude below the 100μ fluxes. (Ennis et al (1982) and Robson et al (1985) have already shown that the 1 mm fluxes of some radio quiet quasars must be below the extrapolation of the near infrared continuum.) Our objects are all extremely weak or undetected with the VLA at 2 cm and 1.3 cm, at levels typically three orders of magnitude below the 100μ fluxes. The sharpness of the required cutoffs allows us to rule out the hypothesis that the infrared is synchrotron radiation with the cutoff due to an absence of low energy electrons. The high frequency of the cutoffs makes free-free absorption implausible, but not impossible. It is possible that synchrotron self-absorption is suppressing the radio. There is circumstantial evidence that the far infrared is thermal dust emission. This would require a lower cutoff in the distribution of dust temperatures, which we think we can explain.

SPECTRO-INTERFEROMETRY OF THE Be STAR δ Sco: NEAR-INFRARED CONTINUUM AND GAS EMISSION REGION SIZES IN 2007

2010 ◽  
Vol 723 (1) ◽  
pp. 544-549 ◽  
Author(s):  
R. Millan-Gabet ◽  
J. D. Monnier ◽  
Y. Touhami ◽  
D. Gies ◽  
E. Hesselbach ◽  
...  
Keyword(s):  
Near Infrared ◽  
Emission Region ◽  
Gas Emission ◽  
Be Star ◽  
Infrared Continuum

The molecular interstellar medium and the near-infrared continuum of the barred liner NGC 6764

1991 ◽  
Vol 372 ◽  
pp. 67 ◽  
Author(s):  
A. Eckart ◽  
M. Cameron ◽  
J. M. Jackson ◽  
R. Genzel ◽  
A. I. Harris ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Near Infrared ◽  
Infrared Continuum

scholarly journals Radiative transfer simulations of multiphase AGN tori: thermal emission and polarisation

2014 ◽  
Vol 10 (S305) ◽  
pp. 377-380
Author(s):  
M. Baes ◽  
M. Stalevski ◽  
P. Camps ◽  
J. Fritz ◽  
L. Č. Popović
Keyword(s):  
Near Infrared ◽  
Thermal Emission ◽  
Spectral Energy Distribution ◽  
Galactic Nuclei ◽  
Spectral Energy ◽  
Central Engine ◽  
Hydrodynamical Simulations ◽  
Multi Phase ◽  
New Generation ◽  
Infrared Continuum

AbstractThe unification model of active galactic nuclei postulates an accreting supermassive black hole as the central engine, surrounded by a putative dusty torus. This dust absorbs the incoming radiation, re-emits it in the infrared and obscures our view of the central region at certain inclinations. We present a new set of AGN models, in which the torus is modelled as a 3D multiphase medium. These new models can explain the observed spectral energy distribution of AGNs over the entire infrared domain, including the observed silicate feature strength and the level of near-infrared continuum. A new generation of multi-phase models, based on hydrodynamical simulations, is being constructed. We will compute the polarisation structure of these physically motivated 3D torus models, and compare them to simpler smooth torus models and to the available observational data.

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