SPM, a submillimeter photometer for PR0NAOS

Lamarre, J.-M.; Pajot, F.; Torre, J. P.; Guyot, G.; Bernard, J.-P.; Luca, A. De; Glard, M.; Mangin, J.; Peyturaux, R.; Puget, J.; Serra, G.; Boulanger, F.; Desert, X.; Ristorcelli, I.; Jegoudez, G.; Lagardère, H.; Leblanc, J.; Pons, R.; Recouvreur, G.; Barthélemy, Mathieu; Bourguignon, C.; Crussaire, J. P.; Dambier, G.; Delille, L.; Korczak, E.; Lepeltier, J. P.; Leriche, B.; Lizambert, C.; Narbonne, J.; Plaisant, C.; Reigner, J.; Renault, J. C.; Rioux, C.

doi:10.1016/1350-4495(94)90086-8

Cited by 19 publications

(8 citation statements)

References 12 publications

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“…A detailed multi-wavelength study of the starless core, TMC-1C, using multiple methods to determine the opacity index find that 1.7 ≤ β ≤ 2.7 with a most likely value near β = 2.2 (Schnee et al 2010). Another example is the PRONAOS (PROgramme NAtional d'Observations Submillimértiques; Lamarre et al 1994) balloon-borne experiment which finds that the opacity index has an inverse temperature dependence with β > 2 for T < 12.7 K (Dupac et al 2003). The lower bound of our opacity index overlaps with the PRONAOS opacity index curve (β = 1/(0.40 + 0.0079T ); Dupac 2009) for the typical T los found in our dust continuum models (see Figure 5).…”

Section: Power-law Index βmentioning

confidence: 99%

Observational Constraints on Submillimeter Dust Opacity

Shirley¹,

Huard²,

Pontoppidan³

et al. 2011

ApJ

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Infrared extinction maps and submillimeter dust continuum maps are powerful probes of the density structure in the envelope of star-forming cores. We make a direct comparison between infrared and submillimeter dust continuum observations of the low-mass Class 0 core, B335, to constrain the ratio of submillimeter to infrared opacity (κ smm /κ ir ) and the submillimeter opacity power-law index (κ ∝ λ −β ). Using the average value of theoretical dust opacity models at 2.2 µm, we constrain the dust opacity at 850 and 450 µm. Using new dust continuum models based upon the broken power-law density structure derived from interferometric observations of B335 and the infall model derived from molecular line observations of B335, we find that the opacity ratios are κ 850 κ 2.2 = (3.21 − 4.80) +0.44 −0.30 × 10 −4 and κ 450 κ 2.2 = (12.8 − 24.8) +2.4 −1.3 × 10 −4 with a submillimeter opacity power-law index of β smm = (2.18−2.58) +0.30−0.30 . The range of quoted values are determined from the uncertainty in the physical model for B335. For an average 2.2 µm opacity of 3800 ± 700 cm 2 g −1 , we find a dust opacity at 850 and 450 µm of κ 850 = (1.18 − 1.77) +0.36 −0.24 and κ 450 = (4.72 − 9.13) +1.9 −0.98 cm 2 g −1 of dust. These opacities are from (0.65 − 0.97)κ OH5 850 of the widely used theoretical opacities of Ossenkopf and Henning for coagulated ice grains with thin mantles at 850µm.

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Section: Power-law Index βmentioning

confidence: 99%

Observational Constraints on Submillimeter Dust Opacity

Shirley¹,

Huard²,

Pontoppidan³

et al. 2011

ApJ

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“…PRONAOS (PROgramme NAtional d'Observations Submillimétriques) is a French balloon-borne submillimeter experiment (Serra et al 2001;Ristorcelli et al 1998;Lamarre et al 1994). Four bolometers cooled at 0.3 K measure the submillimeter flux with sensitivity to low brightness gradients of about 4 MJy/sr in band 1 (200 µm) and 0.8 MJy/sr in band 4 (580 µm).…”

Section: Observationsmentioning

confidence: 99%

Inverse temperature dependence of the dust submillimeter spectral index

Dupac

Bernard

Boudet

et al. 2003

A&A

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259

349

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Abstract. We present a compilation of PRONAOS-based results concerning the temperature dependence of the dust submillimeter spectral index, including data from Galactic cirrus, star-forming regions, dust associated to a young stellar object, and a spiral galaxy. We observe large variations of the spectral index (from 0.8 to 2.4) in a wide range of temperatures (11 to 80 K). These spectral index variations follow a hyperbolic-shaped function of the temperature, high spectral indices (1.6-2.4) being observed in cold regions (11-20 K) while low indices (0.8-1.6) are observed in warm regions (35-80 K). Three distinct effects may play a role in this temperature dependence: one is that the grain sizes change in dense environments, another is that the chemical composition of the grains is not the same in different environments, a third one is that there is an intrinsic dependence of the dust spectral index on the temperature due to quantum processes. This last effect is backed up by laboratory measurements and could be the dominant one.

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“…PRONAOS was a French balloon-borne experiment designed to determine both the FIR dust emissivity spectral index and temperatures, by measuring the dust emission in four broad spectral bands centered at 200, 260, 360, and 580 µm (see Lamarre et al 1994;Serra et al 2002;Pajot et al 2006). The analysis of the PRONAOS observations toward several regions of the sky, ranging from diffuse molecular clouds to star forming regions such as Orion or M 17, have shown an anti-correlation between the dust temperature and the emissivity spectral index (see Dupac et al 2003a).…”

Section: Astronomical Evidencementioning

confidence: 99%

Far-infrared to millimeter astrophysical dust emission

Meny¹,

Gromov

Boudet³

et al. 2007

A&A

160

206

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Aims. We propose a new description of astronomical dust emission in the spectral region from the far-infrared to millimeter wavelengths. Methods. Unlike previous classical models, this description explicitly incorporates the effect of the disordered internal structure of amorphous dust grains. Our model is based on results from solid state physics used to interpret laboratory data. The model takes into account the effect of absorption by disordered charge distribution, as well as the effect of absorption by localized two level systems. Results. We review constraints on the various free parameters of the model from theory and laboratory experimental data. We show that, for realistic values of the free parameters, the shape of the emission spectrum will exhibit very broad structures whose shape will change in a non trivial way with the temperature of dust grains. The spectral shape also depends upon the parameters describing the internal structure of the grains. This opens new perspectives for identifying the nature of astronomical dust from the observed shape of the FIR/mm emission spectrum. A companion paper will provide an explicit comparison of the model with astronomical data.

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SPM, a submillimeter photometer for PR0NAOS

Cited by 19 publications

References 12 publications

Observational Constraints on Submillimeter Dust Opacity

Observational Constraints on Submillimeter Dust Opacity

Inverse temperature dependence of the dust submillimeter spectral index

Far-infrared to millimeter astrophysical dust emission

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