“IRAS” papers · AI for Research

We report on ASCA observations of two ultraluminous far-infrared galaxies, IRAS 15307+3252 and IRAS 20460+1925. An X-ray flux of 1.53 × 10−12 erg cm−2 s−1 in the 2–10 keV band was detected from IRAS 20460+1925. The continuous spectrum is well represented by a power law with a photon index of 1.99+0.18−0.15 and excess photoelectric absorption by a column of (2.6+0.29−0.32 × 1022 cm−2 in the rest frame. The spectrum also shows an iron K emission line with an equivalent width of 260+145−137 eV and a centroid energy of 6.36±0.08 keV in the rest frame. These spectral properties are consistent with those of Seyfert-2 galaxies, although the intrinsic 2–10 keV X-ray luminosity (corrected for absorption) of 1.20 × 1044 erg s−1 is high and close to that of quasars. No X-rays were detected from IRAS 15307+3252, and the upper limit to the X-ray flux is 7.2 × 10−14 erg cm−2 s−1 in the 2–10 keV band. However, the upper limit on the ratio of the X-ray flux to the far-infrared flux is not inconsistent with a source containing a highly obscured quasar.

Cited by 31Open access

ASCA Observations of Two Ultraluminous IRAS Galaxies: IRAS 15307+3252 and IRAS 20460+1925

小賀坂, 康志, 井上, 一, Brandt, William N. et al. · JAXA Repository (JAXA) · 1997

Cited by 0Open access

IRAS Asteroid Families

G. J. Veeder, J. G. Williams, E. F. Tedesco et al. · NASA Technical Reports Server (NASA) · 1991

The Infrared Astronomical Satellite (IRAS) sampled the entire asteroid population at wavelengths from 12 to 100 microns during its 1983 all sky survey. The IRAS Minor Planet Survey (IMPS) includes updated results for more recently numbered as well as other additional asteroids with reliable orbital elements. Albedos and diameters were derived from the observed thermal emission and assumed absolute visual magnitudes and then entered into the IMPS database at the Infrared Processing and Analysis Center (IPAC) for members of the Themis, Eos, Koronis and Maria asteroid families and compared with their visual colors. The IMPS results for the small (down to about 20 km) asteroids within these major families confirm trends previously noted for their larger members. Each of these dynamical families which are defined by their similar proper elements appears to have homogeneous physical properties.

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IRAS II Abschlussbericht

Tina Stäbler, Simon Hümbert, T. Stindl et al. · elib (German Aerospace Center) · 2020

Dieser interne Bericht enthält die Aktivitäten des IRAS II-Projekts aller Partner, die vom Projektbeginn am 1.12.2018 bis zum Projektende am 31.5.2020 stattfanden.

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The IRAS Survey

G. Neugebauer · Bulletin of the American Academy of Arts and Sciences · 1987

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Iras: a mystery

Douglas, Theo, Mrs. · The Journal of the Abraham Lincoln Association

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extragalactic IRAS sources

R. Fabbri, V. Natale · 1994

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Donde Tu Iras

Eduardo Alexander, Orq. Juan S. Garrido, Rafael Hernandez · Bulletin of Miscellaneous Information (Royal Gardens Kew) · 1946

Performer: Eduardo Alexander; Orq. Juan S. Garrido Writer: Rafael Hernandez Cancion. Digitized at 78 revolutions per minute. Four stylii were used to transfer this record. They are 3.5mil truncated eliptical, 2.3mil truncated conical, 2.8mil truncated conical, 3.3mil truncated conical. These were recorded flat and then also equalized with Turnover: 400.0, Rolloff: -12.0. The preferred versions suggested by an audio engineer at George Blood, L.P. have been copied to have the more friendly filenames. Matrix number: 4228-46 Catalog number: 2399 Other IDs from the record include: (4228-46)

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IRAS asteroid families

Williams, J. G., Matson, D. L., Tedesco, E. F. et al. · NASA Technical Reports Server (NASA)

The Infrared Astronomical Satellite (IRAS) sampled the entire asteroid population at wavelengths from 12 to 100 microns during its 1983 all sky survey. The IRAS Minor Planet Survey (IMPS) includes updated results for more recently numbered as well as other additional asteroids with reliable orbital elements. Albedos and diameters were derived from the observed thermal emission and assumed absolute visual magnitudes and then entered into the IMPS database at the Infrared Processing and Analysis Center (IPAC) for members of the Themis, Eos, Koronis and Maria asteroid families and compared with their visual colors. The IMPS results for the small (down to about 20 km) asteroids within these major families confirm trends previously noted for their larger members. Each of these dynamical families which are defined by their similar proper elements appears to have homogeneous physical properties.

Cited by 0Open access

IRAS Science Briefings

M. Mitchell Waldrop, Richard A. Kerr · Science · 1983

Cited by 2

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