Spectral Irradiance Calibration in the Infrared. XI. Comparison of α Bootis and 1 Ceres with a Laboratory Standard

Witteborn, F. C.; Cohen, Martin; Bregman, J. D.; Wooden, D. H.; Heere, Karen R.; Shirley, Eric L.

doi:10.1086/300850

Cited by 15 publications

(12 citation statements)

References 9 publications

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“…Witteborn et al (1999) used the Kuiper Airborne Observatory to provide direct measurements of a single star, α Boo, which demonstrates the challenges of measuring the absolute flux of stars using observations through the atmosphere with the often complicated transfer to laboratory blackbodies.…”

Section: Airborne and Space-basedmentioning

confidence: 99%

Techniques and Review of Absolute Flux Calibration from the Ultraviolet to the Mid-Infrared

Bohlin¹,

Gordon²,

Tremblay³

2014

Publications of the Astronomical Society of the Pacific

182

176

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The measurement of precise absolute fluxes for stellar sources has been pursued with increased vigor since the discovery of the dark energy and the realization that its detailed understanding requires accurate spectral energy distributions (SEDs) of redshifted Ia supernovae in the rest frame. The flux distributions of spectrophotometric standard stars were initially derived from the comparison of stars to laboratory sources of known flux but are now mostly based on calculated model atmospheres. For example, pure hydrogen white dwarf (WD) models provide the basis for the HST CALSPEC archive of flux standards. The basic equations for quantitative spectrophotometry and photometry are explained in detail. Several historical lab based flux calibrations are reviewed; and the SEDs of stars in the major on-line astronomical databases are compared to the CALSPEC reference standard spectrophotometry. There is good evidence that relative fluxes from the visible to the near-IR wavelength of ∼2.5 µm are currently accurate to 1% for the primary reference standards; and new comparisons with lab flux standards show promise for improving that precision.

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Section: Airborne and Space-basedmentioning

confidence: 99%

Techniques and Review of Absolute Flux Calibration from the Ultraviolet to the Mid-Infrared

Bohlin¹,

Gordon²,

Tremblay³

2014

Publications of the Astronomical Society of the Pacific

182

176

View full text Add to dashboard Cite

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“…icy rich spots), which would remain undetected otherwise in disk-averaged studies of Ceres. A dusty regolith a few centimeters thick (Webster et al 1988), created by the impact of micrometeorites and possibly larger bodies, has been proposed (Witteborn et al 1999;Lim et al 2005) as a possible explanation for the shallow spectral signatures in the visible and near-infrared spectrum of Ceres and its small albedo constrast. But some small areas visible in our high-angular resolution images of Ceres could correspond to places on the surface where the regolith material has been cleared by "recent" endogenic or exogenic activity to expose more pristine material from the subsurface layers.…”

Section: Syntheticmentioning

confidence: 99%

Near-infrared mapping and physical properties of the dwarf-planet Ceres

Carry

Dumas

Fulchignoni

et al. 2007

A&A

104

115

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Aims. We study the physical characteristics (shape, dimensions, spin axis direction, albedo maps, mineralogy) of the dwarf-planet Ceres based on high angular-resolution near-infrared observations. Methods. We analyze adaptive optics J/H/K imaging observations of Ceres performed at Keck II Observatory in September 2002 with an equivalent spatial resolution of ∼50 km. The spectral behavior of the main geological features present on Ceres is compared with laboratory samples. Results. Ceres' shape can be described by an oblate spheroid (a = b = 479.7 ± 2.3 km, c = 444.4 ± 2.1 km) with EQJ2000.0 spin vector coordinates α 0 = 288• ± 5• and δ 0 = +66 • ± 5• . Ceres sidereal period is measured to be 9.074 10 +0.000 10 −0.000 14 h. We image surface features with diameters in the 50-180 km range and an albedo contrast of ∼6% with respect to the average Ceres albedo. The spectral behavior of the brightest regions on Ceres is consistent with phyllosilicates and carbonate compounds. Darker isolated regions could be related to the presence of frost.

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“…1 is significantly larger for 1B-1D (=0.015) than for 1A-1B and 1D-1E (being respectively 0.009 and 0.005). Due to the problems with memory effects in band 2 (4.08-12 µm), the factors of each sub-band of band 2 were determined by use of the corresponding spectral data of Cohen (Cohen et al 1992(Cohen et al , 1995(Cohen et al , 1996Witteborn et al 1999): for Vega and Sirius Cohen has constructed a calibrated model spectrum; a composite spectrum (i.e. various observed spectra have been spliced to each other using photometric data) is available for α Cen A, α Boo, γ Dra, α Tau, β And, α Cet, and β Peg; a template spectrum (i.e.…”

Section: Data Reductionmentioning

confidence: 99%

ISO-SWS calibration and the accurate modelling of cool-star atmospheres

Decin

Vandenbussche

Waelkens

et al. 2003

A&A

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Abstract. The fine calibration of the ISO-SWS detectors (Infrared Space Observatory -Short Wavelength Spectrometer) has proven to be a delicate problem. We therefore present a detailed spectroscopic study in the 2.38-12 µm wavelength range of a sample of 16 A0-M2 stars used for the calibration of ISO-SWS. By investigating the discrepancies between the ISO-SWS data of these sources, the theoretical predictions of their spectra, the high-resolution FTS-KP (Kitt Peak) spectrum of α Boo and the solar FTS-ATMOS (Atmospheric Trace Molecule Spectroscopy) spectrum, both calibration problems and problems in computing the theoretical models and the synthetic spectra are revealed. The underlying reasons for these problems are sought for and the impact on the further calibration of ISO-SWS and on the theoretical modelling is discussed extensively.

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Spectral Irradiance Calibration in the Infrared. XI. Comparison of α Bootis and 1 Ceres with a Laboratory Standard

Cited by 15 publications

References 9 publications

Techniques and Review of Absolute Flux Calibration from the Ultraviolet to the Mid-Infrared

Techniques and Review of Absolute Flux Calibration from the Ultraviolet to the Mid-Infrared

Near-infrared mapping and physical properties of the dwarf-planet Ceres

ISO-SWS calibration and the accurate modelling of cool-star atmospheres

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