2012A&A...541A.148E


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.15CET22:54:16

2012A&A...541A.148E - Astronomy and Astrophysics, volume 541A, 148-148 (2012/5-1)

A peculiar class of debris disks from Herschel/DUNES. A steep fall off in the far infrared.

ERTEL S., WOLF S., MARSHALL J.P., EIROA C., AUGEREAU J.-C., KRIVOV A.V., LOEHNE T., ABSIL O., ARDILA D., AREVALO M., BAYO A., BRYDEN G., DEL BURGO C., GREAVES J., KENNEDY G., LEBRETON J., LISEAU R., MALDONADO J., MONTESINOS B., MORA A., PILBRATT G.L., SANZ-FORCADA J., STAPELFELDT K. and WHITE G.J.

Abstract (from CDS):

The existence of debris disks around old main sequence stars is usually explained by continuous replenishment of small dust grains through collisions from a reservoir of larger objects. We present photometric data of debris disks around HIP103389 (HD199260), HIP107350 (HNPeg, HD206860), and HIP114948 (HD219482), obtained in the context of our Herschel open time key program DUNES (DUst around NEarby Stars). We used Herschel/PACS to detect the thermal emission of the three debris disks with a 3σ sensitivity of a few mJy at 100µm and 160µm. In addition, we obtained Herschel/PACS photometric data at 70µm for HIP103389. These observations are complemented by a large variety of optical to far-infrared photometric data. Two different approaches are applied to reduce the Herschel data to investigate the impact of data reduction on the photometry. We fit analytical models to the available spectral energy distribution (SED) data using the fitting method of simulated thermal annealing as well as a classical grid search method. The SEDs of the three disks potentially exhibit an unusually steep decrease at wavelengths ≥70µm. We investigate the significance of the peculiar shape of these SEDs and the impact on models of the disks provided it is real. Using grain compositions that have been applied successfully for modeling of many other debris disks, our modeling reveals that such a steep decrease of the SEDs in the long wavelength regime is inconsistent with a power-law exponent of the grain size distribution -3.5 expected from a standard equilibrium collisional cascade. In contrast, a steep grain size distribution or, alternatively an upper grain size in the range of few tens of micrometers are implied. This suggests that a very distinct range of grain sizes would dominate the thermal emission of such disks. However, we demonstrate that the understanding of the data of faint sources obtained with Herschel is still incomplete and that the significance of our results depends on the version of the data reduction pipeline used. A new mechanism to produce the dust in the presented debris disks, deviations from the conditions required for a standard equilibrium collisional cascade (grain size exponent of -3.5), and/or significantly different dust properties would be necessary to explain the potentially steep SED shape of the three debris disks presented.

Abstract Copyright:

Journal keyword(s): circumstellar matter - stars: individual: HIP 103389 - infrared: planetary systems - stars: individual: HIP 107350 - infrared: stars - stars: individual: HIP 114948

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2586 0
2 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1602 1
3 HD 107146 PM* 12 19 06.5022221429 +16 32 53.870713669   7.61   6.7   G2V 212 0
4 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2096 0
5 HD 199260 PM* 20 56 47.3303687041 -26 17 46.969399809   6.20 5.70     F6V 95 0
6 HD 206860B BD* 21 44 28.47168 +14 46 07.7988           T2.5 77 0
7 HD 206860 BY* 21 44 31.3299733695 +14 46 18.982331039       6.16   G0V+ 440 1
8 HD 219482 PM* 23 16 57.6873978547 -62 00 04.318777045   6.146 5.647     F6V 99 0
9 NAME Castor Moving Group As* ~ ~           ~ 114 1
10 NAME Hercules-Lyra Moving Group MGr ~ ~           ~ 50 0
11 NAME Pleiades Moving Group MGr ~ ~           ~ 228 1

    Equat.    Gal    SGal    Ecl

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2019.11.15-22:54:16

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