The Solar Emission Intensity at 11

Saiedy, F.; Goody, R. M.

doi:10.1093/mnras/119.3.213

Cited by 26 publications

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“…(2.1)] at the three frequencies has been determined to better than 1% by Saiedy and Goody (1959) and Saiedy (1960a) and thus 8(v,p, 71 ) can be inferred.…”

Section: Methods I Observational Proceduresmentioning

confidence: 89%

“…The infrared spectrometer (see Saiedy and Goody, 1959), was a small double monochromator using a 7 X5 cm Merton replica grating having 1000 lines/cm and blazed for 10 .t in the first-order spectrum. Higher-order spectra of shorter wavelengths were eliminated by means of an indium antimonide filter with an antireflection coating of lead chloride.…”

Section: Methods I Observational Proceduresmentioning

confidence: 99%

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On the Atmospheric Infrared Continuum

1963

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were confirmed and extended to include the region 4 -12 p.Unexpectedly high absorption was observed in this latter region.(ii) These results inspired a reexamination of all available previous work, from which it was concluded that the extinction arises from two separate effects with different frequency and temperature dependence.They are i) a foreignbroadened component, roughly proportional to the foreign gas pressure and probably positively temperature dependent (0.5 to 1% per °C); and ii) a self-broadened component roughly proportional to partial vapour pressure and with a strong negative temperature dependence (2% per °C at 30°C).On the basis of several assumed line shapes, the accumulated wings of lines in the 50 la rotation band were computed at several points in the range 12 -40 p; the Lorentz shape gave a very good fit (1. 10%) to the foreign-broadened component, but none gave a satisfactory fit to the selfbroadened component. *The 15 11 CO2 band was found to give no detectable absorption (< 1% for 43 atm -cm of CO 2' the equivalent of 1.4 km of air at sea level) outside the range 12.7 to 17.8 11.The horizontal path experiment has already been reported in a joint paper with F. Saiedy and P. A. Sheppard, entitled 'On the Atmospheric Infrared Continuum', J.O.S.A. 51, 466 (1963); a copy is attached to this thesis.During this research a further paper, on the related topic of terrestrial heat balance, entitled 'Heat-balance measurements from an earth satellite -an analysis of possibilities' was published in Quart. J. Roy. Met. Soc., 87, 231 (1961); a copy is attached. 11.13 See Addendum for amended version. ,Chapter 1?1. IntroductionThe existence of a continuous absorption throughout the atmospheric infrared window between 8 and 13 microns has been knoinfor a long time, Elsasser (1938) probably being the first to draw attention to it. It has been observed many times since by all workers in the study of atmospheric radiation, both in transmission observations using the sun and artificial sources, and in emission studies from ground and space 2.iii) Since the advent of artificial earth satellites, several infrared emission experiments have been proposed, or in some cases already been carried out, to determine the earth's surface temperature distribution, cloud top height, ozone and carbon dioxide distribution, and temperature structure in the upper atmosphere.All of these, except possibly the last, require correction to some extent for the continuum.Much discussion has centred on the question of the origin of the continuum absorption; there is no doubt that it is largely due to wcter vapour, but the role of aerosol is less certain. That it is necessary to appeal to something other than water vapour appears to be due to the fact that measurements of continuum absorption by different workers do not seem to be consistent when compared on the basis of the existing picture of the water vapour continuum alone. Whilst it is not disputed that aerosol absorption in the 8 -13j. region can be significant under extremel...

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“…(2.1)] at the three frequencies has been determined to better than 1% by Saiedy and Goody (1959) and Saiedy (1960a) and thus 8(v,p, 71 ) can be inferred.…”

Section: Methods I Observational Proceduresmentioning

confidence: 89%

Section: Methods I Observational Proceduresmentioning

confidence: 99%

On the Atmospheric Infrared Continuum

1963

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“…It is concluded that the data out to 12 µm are of high quality. Specifically, Saiedy & Goody (1959) estimate that their measurement at 11.1 µm is accurate to 0.7%, standard error. Saiedy (1960) estimates the standard errors at 8.63 and 12.02 µm to be 0.9 and 1.8%, respectively.…”

Section: Measurements Of the Solar Sedmentioning

confidence: 96%

Absolute Physical Calibration in the Infrared

Rieke

Blaylock

Decin

et al. 2008

The Astronomical Journal

118

164

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We determine an absolute calibration for the Multiband Imaging Photometer for Spitzer 24 µm band and recommend adjustments to the published calibrations for Two Micron All Sky Survey (2MASS), Infrared Array Camera (IRAC), and IRAS photometry to put them on the same scale. We show that consistent results are obtained by basing the calibration on either an average A0V star spectral energy distribution (SED), or by using the absolutely calibrated SED of the Sun in comparison with solar-type stellar photometry (the solar analog method). After the rejection of a small number of stars with anomalous SEDs (or bad measurements), upper limits of ∼1.5% root mean square (rms) are placed on the intrinsic infrared (IR) SED variations in both A-dwarf and solar-type stars. These types of stars are therefore suitable as general-purpose standard stars in the IR. We provide absolutely calibrated SEDs for a standard zero magnitude A star and for the Sun to allow extending this work to any other IR photometric system. They allow the recommended calibration to be applied from 1 to 25 µm with an accuracy of ∼2%, and with even higher accuracy at specific wavelengths such as 2.2, 10.6, and 24 µm, near which there are direct measurements. However, we confirm earlier indications that Vega does not behave as a typical A0V star between the visible and the IR, making it problematic as the defining star for photometric systems. The integration of measurements of the Sun with those of solar-type stars also provides an accurate estimate of the solar SED from 1 through 30 µm, which we show agrees with theoretical models.

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“…These measurements are all quite old by now. The Saiedy and Goody (1959), Saiedy (1960) and Murcray, Murcray and Williams (1964) infrared measurements were referenced to standard sources and the Murcray, Murcray and Williams (1970) observations were obtained at balloon altitudes, above much of the atmosphere. Labs and Neckel also used the relative measurements of Pierce (1954) in the 1-2.5 µm regions to validate the shape of the model spectral energy distribution through the minimum in the solar atmospheric H − opacity.…”

Section: The Solar Analog Calibrationmentioning

confidence: 99%

Infrared irradiance calibration

Price

2004

Space Sci Rev

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Infrared astronomical measurements are calibrated against reference sources, usually primary standard stars that are, in turn, calibrated either by direct or indirect means. A direct calibration compares the star with a certified source, typically a blackbody. Indirect methods extrapolate a direct measurement of the flux at one wavelength to the flux at another. Historically, α Lyr (Vega) has been used as the primary standard as it is bright, easily accessible from the northern hemisphere, and is well calibrated in the visual. Until recently, the direct absolute infrared calibrations of α Lyr and those derived from the absolute solar flux scaled to the observed spectral energy distributions of solar type stars increasingly diverged with wavelength from those obtained using a model atmosphere to extrapolate the absolute visual flux of Vega into the infrared. The exception is the direct calibration by the 1996/97 Midcourse Space Experiment of the absolute fluxes for a number of the commonly used infrared standard stars, including Vega.In the mid-1980s, the Air Force Geophysics Laboratory began a program that led to the establishment of a network of stars with which to calibrate infrared space-based sensors. α Lyr and a CMa were adopted as the fundamental references and the absolute 1.2 to 35 µm infrared spectral energy distributions for the 616 secondary standard stars in the network were derived through spectral and photometric comparisons with the primary standards. The stars are also used for calibration at ground-based infrared observatories. For applications in which the network stars may not be bright enough, particularly at the longer infrared wavelengths, planets and the larger asteroids are used. Planets and asteroids move and rather sophisticated thermal modeling of the bodies is required to predict the disk-integrated brightness at a specific time with reasonable accuracy. The Infrared Space Observatory applied such a sophisticated 'thermo-physical' model to the largest asteroids to support calibration of the sensors to a claimed accuracy of within 5%. The AFRL program also created a spectral atlas of the brightest stars in the sky that, although they are variable, may be used for calibration if the large(r) attendant uncertainties are acceptable.

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The Solar Emission Intensity at 11

Cited by 26 publications

References 0 publications

On the Atmospheric Infrared Continuum

On the Atmospheric Infrared Continuum

Absolute Physical Calibration in the Infrared

Infrared irradiance calibration

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