The SMART Data Analysis Package for the Infrared Spectrograph on the<i>Spitzer Space Telescope</i>

Higdon, Sarah J.U.; Devost, D.; Higdon, James L.; Brandl, Bernhard R.; Houck, J. R.; Hall, Peter; Barry, D. J.; Charmandaris, V.; Smith, John David; Sloan, G. C.; Green, J.

doi:10.1086/425083

Cited by 434 publications

(417 citation statements)

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“…The rogue pixels were removed using the IRSCLEAN tool 3 , with the aggressive parameter equal to 0. Then the data were processed (full extraction, trimming, defringing and averaging over cycles) into a single spectrum per node position using SMART 4 (Higdon et al 2004). A similar procedure has been applied for LH off-source observations, and the obtained spectra have been subtracted from the on-source data for the corresponding node position, to cancel out the sky background.…”

Section: Mid-infrared Spectroscopymentioning

confidence: 99%

The chemical composition of TS 01, the most oxygen-deficient planetary nebula

Stasińska

Morisset

Tovmassian

et al. 2010

A&A

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The planetary nebula TS 01 (also called PN G 135.9+55.9 or SBS 1150+599A) with its record-holding low oxygen abundance and its double degenerate close binary core (period 3.9 h) is an exceptional object located in the Galactic halo. We have secured observational data in a complete wavelength range to pin down the abundances of half a dozen elements in the nebula. The abundances are obtained via detailed photoionization modelling which takes into account all the observational constraints (including geometry and aperture effects) using the pseudo-3D photoionization code Cloudy_3D. The spectral energy distribution of the ionizing radiation is taken from appropriate model atmospheres. Incidentally we find from the new observational constraints that both stellar components contribute to the ionization: the "cool" one provides the bulk of hydrogen ionization, while the "hot" one is responsible for the presence of the most highly charged ions, which explains why previous attempts to model the nebula experienced difficulties. The nebular abundances of C, N, O, and Ne are found to be 1/3.5, 1/4.2, 1/70, and 1/11 of the solar value respectively, with uncertainties of a factor 2. Thus the extreme O deficiency of this object is confirmed. The abundances of S and Ar are less than 1/30 of solar. The abundance of He relative to H is 0.089 ± 0.009. Standard models of stellar evolution and nucleosynthesis cannot explain the abundance pattern observed in the nebula. To obtain an extreme oxygen deficiency in a star whose progenitor has an initial mass of about 1 M requires an additional mixing process, which can be induced by stellar rotation and/or by the presence of the close companion. We have computed a stellar model with an initial mass of 1 M , appropriate metallicity, and initial rotation of 100 km s −1 , and find that rotation greatly improves the agreement between the predicted and observed abundances.

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Section: Mid-infrared Spectroscopymentioning

confidence: 99%

The chemical composition of TS 01, the most oxygen-deficient planetary nebula

Stasińska

Morisset

Tovmassian

et al. 2010

A&A

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“…The data were processed using the s15.3 version of the pipeline and using a script version of Smart (Higdon et al 2004). The reduction started from the droop images which are equivalent to the bcd images but lack stray-cross removal and flatfield.…”

Section: The Irs Infrared Spectrum Of Ngc 6210mentioning

confidence: 99%

Abundances in the planetary nebula NGC 6210

Pottasch¹,

Bernard─Salas

Roellig

2009

A&A

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The spectra of the planetary nebula NGC 6210 is reanalysed using spectral measurements made in the mid-infrared with the Spitzer Space Telescope and the Infrared Space Observatory. The aim is to determine the chemical composition of this object. We also make use of IUE and ground based spectra. Abundances determined from the mid-infrared lines, which are insensitive to electron temperature, are used as the basis for the determination of the composition, which is found to differ somewhat from earlier results. The abundances found, especially the low value of helium and oxygen, indicate that the central star was originally of rather low mass, probably ≤1 M . Abundances of phosphorus, iron, silicon, sodium, potassium and chlorine have been determined, some for the first time in this nebula. The electron temperature in this nebula is constant. The temperature, radius and luminosity of the central star is also discussed. It is shown that the luminosity is consistent with that predicted for a star of 0.9 M . But the predicted nebular age is inconsistent with the observed kinetic age.

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“…SMART package (Higdon et al 2004) and custom IDL routines, starting from the pipeline level of basic calibrated data (S18.18 products). The data reduction process involves removing bad pixels, subtracting background emission from the images, extracting the spectra, correcting for instrumental fringes, flux calibration and scaling of the modules, and trimming the order edges and rebinning.…”

Section: O B S E Rvat I O N S a N D Data R E D U C T I O Nmentioning

confidence: 99%

“…When necessary, we also used the routine irsclean_mask to flag additional bad pixels. We then co-added the cleaned images for each nod using a weighted average (see Higdon et al 2004).…”

Section: O B S E Rvat I O N S a N D Data R E D U C T I O Nmentioning

confidence: 99%