SOFIA: The Stratospheric Observatory for Infrared Astronomy

Stützki, J.

doi:10.1002/9783527619030.ch14

Cited by 9 publications

(8 citation statements)

References 16 publications

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“…The NASA and DLR de-velopment and operations costs, as well as the science observing time, are divided up in 80:20 proportions, respectively. SOFIA consists of a 2.7-m telescope developed by DLR that resides in a highly modified Boeing 747SP aircraft, enabling observations of a wide variety of astronomical objects at wavelengths from 0.3 µm to 1.6 mm (Stutzki 2006;Becklin et al 2007;Gehrz et al 2009). The SOFIA telescope design and its evolving instrument complement build upon the legacy of NASA's Kuiper Airborne Observatory (KAO), a 0.9 m infrared telescope that flew from 1974 to 1995 in a Lockheed C141 Starlifter aircraft (Gillespie 1981).…”

Section: Introductionmentioning

confidence: 99%

Early Science With Sofia, the Stratospheric Observatory for Infrared Astronomy

Young¹,

Becklin²,

Marcum³

et al. 2012

ApJ

256

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The Stratospheric Observatory for Infrared Astronomy (SOFIA) is an airborne observatory consisting of a specially modified Boeing 747SP with a 2.7-m telescope, flying at altitudes as high as 13.7 km (45,000 ft). Designed to observe at wavelengths from 0.3 µm to 1.6 mm, SOFIA operates above 99.8% of the water vapor that obscures much of the infrared and submillimeter. SOFIA has seven science instruments under development, including an occultation photometer, near-, mid-, and far-infrared cameras, infrared spectrometers, and heterodyne receivers. SOFIA, a joint project between NASA and the German Aerospace Center DLR, began initial science flights in 2010 December, and has conducted 30 science flights in the subsequent year. During this early science period three instruments have flown: the mid-infrared camera FORCAST, the heterodyne spectrometer GREAT, and the occultation photometer HIPO. This article provides an overview of the observatory and its early performance.

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Section: Introductionmentioning

confidence: 99%

Early Science With Sofia, the Stratospheric Observatory for Infrared Astronomy

Young¹,

Becklin²,

Marcum³

et al. 2012

ApJ

256

View full text Add to dashboard Cite

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“…The survivors evolve then under different destruction processes and are gradually eroded until diluted into the galactic field. Beech (1987); (2) Bazell & Desert (1988); (3) Dickman et al (1990); (4) Falgarone et al (1991); (5) Hetem & Lepine (1993); ( 6) Stutzki (1993); (7) Vogelaar & Wakker (1994); ( 8) Lee (2004); (9) Sánchez et al (2007a); (10) Lee et al (2008).…”

Section: Introductionmentioning

confidence: 99%

Internal Structure of Stellar Clusters: Geometry of Star Formation

Alfaro

Sánchez

2010

Proc. IAU

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Abstract. The study of the internal structure of star clusters provides important clues concerning their formation mechanism and dynamical evolution. There are both observational and numerical evidences indicating that open clusters evolve from an initial clumpy structure, presumably a direct consequence of the formation in a fractal medium, toward a centrally condensed state. This simple picture has, however, several drawbacks. There can be very young clusters exhibiting radial patterns maybe reflecting the early effect of gravity on primordial gas. There can be also very evolved clusters showing fractal patterns that either have survived through time or have been generated subsequently by some (unknown) mechanism. Additionally, the fractal structure of some open clusters is much clumpier than the average structure of the interstellar medium in the Milky Way, although in principle a very similar structure should be expected. Here we summarize and discuss observational and numerical results concerning this subject.

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“…Two routines which use this technique are gaussclumps originally developed by Stutzki & Güsten (1990) and clumpfind developed by Williams et al (1994). As Stutzki (1993) points out, these clump identification methods do not prove that the molecular cloud consists of clumps in a hierarchical structure, instead they provide a means to measure, in a more defined way, the parameters which characterise such an assumption.…”

Section: Introductionmentioning

confidence: 99%

The Bias of Molecular Clump Identification Programs: the Example of the Carina Molecular Clouds

Schneider

Brooks

2004

Publ. – Astron. Soc. Aust

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A large scale 12 CO J = 1 → 0 molecular line map of the Carina molecular cloud complex was obtained with the Mopra radio telescope in order to investigate its spatial and kinematic structure. The data show a complex velocity structure in two distinct cloud regions -the Northern and Southern Carina clouds. Two different clump identification methods (gaussclumps and clumpfind) were applied to the data. Though both algorithms find a similar clump mass spectral index (1.95 and 1.8, respectively), the properties of the clumps (mass, size, virial equilibrium) differ significantly. We discuss possible explanations for this discrepancy and question the validity of the Larson relations which could be an artifact of the limited spatial resolution and dynamic range of the observations.

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SOFIA: The Stratospheric Observatory for Infrared Astronomy

Cited by 9 publications

References 16 publications

Early Science With Sofia, the Stratospheric Observatory for Infrared Astronomy

Early Science With Sofia, the Stratospheric Observatory for Infrared Astronomy

Internal Structure of Stellar Clusters: Geometry of Star Formation

The Bias of Molecular Clump Identification Programs: the Example of the Carina Molecular Clouds

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