Infrared Techniques for Comet Observations

Hanner, M. S.; Tokunaga, A. T.

doi:10.1007/978-94-011-3378-4_3

Cited by 18 publications

(9 citation statements)

References 53 publications

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“…This has a nominal error of 1.45% and in general is within a few percent of other determinations in the near IR. Over the IRTF filter range the flux densities agree with the values given in Hanner & Tokunaga (1991) to within the errors. For the purpose of this paper we shall ignore the error in the Vega flux density and take the model as being a definition.…”

Section: The Total System Transmissionsupporting

confidence: 70%

“…However, it quickly became apparent that in general there is a lack of 10 and 20 µm data with known pass bands and a known zero points, particularly for the narrow band filters. For a summary of the current situation in 10 and 20 µm photometry see Hanner & Tokunaga (1991). It was therefore decided to set up new zero points for the IRTF filter set.…”

Section: Deriving the Apparent Magnitudesmentioning

confidence: 99%

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Infrared standards for ISO

Hammersley

Muizon

Kessler³

et al. 1998

Astron. Astrophys. Suppl. Ser.

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Abstract. We present N , 8.7 µm, 9.8 µm 12.5 µm and Q bolometry of 26 stars which were observed on the IRTF. These are primarily K giants which have been well measured at other wavelengths and are chosen to be single and non-variable. Hence the data presented provides a new homogeneous set of mid IR standards. As a test of part of the calibration strategy of ISO over this wavelength range, the zero points have been set using the Kurucz model grids (1993) to predict the mid IR magnitudes from near IR data. An analysis of the errors involved is presented and a comparison with more direct methods for the determination of the zero points suggest an possible error of 0.015 mags, although the source of this error is unclear as it is at the level of the uncertainty in the more direct methods. The effect of the SiO fundamental on the spectral energy distributions of K giants is discussed.

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Section: The Total System Transmissionsupporting

confidence: 70%

Section: Deriving the Apparent Magnitudesmentioning

confidence: 99%

Infrared standards for ISO

Hammersley

Muizon

Kessler³

et al. 1998

Astron. Astrophys. Suppl. Ser.

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show abstract

“…We have adopted a standard grain size distribution of a −3.5 between 0.005 and 0.05 μm (Sugerman et al 2006;Meikle et al 2007;Kotak et al 2009) and have tested two different concentrations, i.e., a dust model dominated by silicates (75% Si; 25% AC) and one dominated by amorphous carbon (75% AC; 25% Si). For each of these models, we used the optical grain constants of Hanner (1988) and Draine & Lee (1984), respectively.…”

Section: Radiative Transfer Modelingmentioning

confidence: 99%

SN 2007od: A TYPE IIP SUPERNOVA WITH CIRCUMSTELLAR INTERACTION

Andrews

Gallagher

Clayton

et al. 2010

ApJ

136

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SN 2007od exhibits characteristics that have rarely been seen in a Type IIP supernova (SN). Optical V-band photometry reveals a very steep brightness decline between the plateau and nebular phases of ∼4.5 mag, likely due to SN 2007od containing a low mass of 56 Ni. The optical spectra show an evolution from normal Type IIP with broad Hα emission, to a complex, four-component Hα emission profile exhibiting asymmetries caused by dust extinction after day 232. This is similar to the spectral evolution of the Type IIn SN 1998S, although no early-time narrow (∼200 km s −1 ) Hα component was present in SN 2007od. In both SNe, the intermediate-width Hα emission components are thought to arise in the interaction between the ejecta and its circumstellar medium (CSM). SN 2007od also shows a mid-infrared excess due to new dust. The evolution of the Hα profile and the presence of the mid-IR excess provide strong evidence that SN 2007od formed new dust before day 232. Late-time observations reveal a flattening of the visible light curve. This flattening is a strong indication of the presence of a light echo, which likely accounts for much of the broad, underlying Hα component seen at late times. We believe that the multi-peaked Hα emission is consistent with the interaction of the ejecta with a circumstellar ring or torus (for the inner components at ±1500 km s −1 ) and a single blob or cloud of circumstellar material out of the plane of the CSM ring (for the outer component at −5000 km s −1 ). The most probable location for the formation of new dust is in the cool dense shell created by the interaction between the expanding ejecta and its CSM. Monte Carlo radiative transfer modeling of the dust emission from SN 2007od implies that up to ∼4 × 10 −4 M of new dust has formed. This is similar to the amounts of dust formed in other core-collapse supernovae such as SNe 1999em, 2004et, and 2006jc.

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“…This locus thus encompasses typical photospheric temperatures of main-sequence stars. In Figures 2a and 2b we also include the colors of a Lyr (from data in Wamsteker 1981, Rieke, Lebofsky, & Low 1985, and/or Hanner & Tokunaga 1991. The comparison of infrared colors of a Lyr (the prototypical main-sequence star with an infrared excess ; Aumann et al 1984) with infrared colors of main-sequence photospheres and those measured for our sources allows us to detect excesses and understand their nature.…”

Section: Color-color Diagrams Of Isophot Iras Andmentioning

confidence: 99%

Infrared Space ObservatoryPhotometric Search of Main‐Sequence Stars for Vega‐Type Systems

Fajardo-Acosta

Stencel

Backman

et al. 1999

ApJ

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We obtained 3.6È20 km photometry of 38 bright [IRAS km) [ 0.7 Jy] main-sequence stars with F l (12 the Infrared Space Observatory (ISO). Observations were conducted with the ISOPHOT instrument, in the single-pointing photometry mode, through Ðlters at 3.6, 11.5, and 20.0 km. We searched for excess (Vega-type) emission from dust at temperatures K, located at D1È60 AU from the stars. We thus Z100 sampled dust at warm, terrestrial material temperatures and at cool (D100 K) temperatures of possible Kuiper BeltÈtype regions in these systems. We detected 20 km excesses from D14% of our sources, but we did not detect 11.5 km excesses from any of them. We present single-temperature blackbody models of the location and density of dust emission around 10 stars, two of them (29 Cyg and Gl 816) with excesses newly reported here. We make a thorough comparison of ISO and IRAS data on our target stars and propose a new calibration procedure for ISOPHOT staring measurements at 3.6, 11.5, and 20 km.

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Infrared Techniques for Comet Observations

Cited by 18 publications

References 53 publications

Infrared standards for ISO

Infrared standards for ISO

SN 2007od: A TYPE IIP SUPERNOVA WITH CIRCUMSTELLAR INTERACTION

Infrared Space ObservatoryPhotometric Search of Main‐Sequence Stars for Vega‐Type Systems

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