This work is supported by NASA Origins of Solar Systems through subcontract No. 1467483
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This work is supported by NASA Origins of Solar Systems through subcontract No. 1467483 How Common Are W3 and W4 Excesses in 75 pc ? • Asteroid belt/Zodiacal Light analogs: 4% • Kuiper Belt/Asteroid belt analogs: 96% In a) we trace the W2-W4 vs. B T -V T dependence for our sample of stars using a running mean to estimate the photospheric contribution to the WISE colors. We create a color SNR (Σ E ) from the color excess (E[W2-W4]). The distribution in b) was used to calculate the 99.5% confidence level (green line) above which stars were chosen as candidate debris disks. 1 Department of Physics and Astronomy at Stony Brook University 2 Department of Physics and Astronomy at The University of Western Ontario Empirically Finding Excesses at 12 µm and 22 µm a) b) We search for W3 (12µm) and W4 (22µm) excesses from exozodi or asteroid belts around ~15,000 Hipparcos stars within 75 pc by using short minus long wavelength WISE colors. Scan here to link to the paper for this work (Patel, Metchev, Heinze 2013, ApJS, 212,10 • 220 stars < 75 pc with excess at 12 µm or 22 µm • 111 New detections at any wavelength • 45% increase of 10-30µm excesses • 25% increase in 75 pc debris disk census The incidence rates we derive for 12 µm and 22 µm excesses exceed previous determinations from WISE by virtue of our precise photometric calibration. Our incidence rates for 12 µm excesses agree with the most sensitive results from Spitzer, while our incidence rates for 22 µm excesses are 1.5-3x less sensitive to Spitzer’s estimates. Finding Warm Debris Disks with WISE Around Bright Stars Rahul I. Patel 1 , Stanimir Metchev 1,2 , Aren Heinze 1 For the first time, we are able to detect small excesses even around bright solar neighborhood stars whose WISE fluxes are saturated. We do so by deriving and applying corrections to the fluxes of saturated stars in WISE.
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Finding Warm Debris Disks with WISE Around Bright Stars. Rahul I. Patel 1 , Stanimir Metchev 1,2 , Aren Heinze 1. Empirically Finding Excesses at 12 µm and 22 µ m. - PowerPoint PPT Presentation
Transcript of This work is supported by NASA Origins of Solar Systems through subcontract No. 1467483
This work is supported by NASA Origins of Solar Systems through subcontract No. 1467483
How Common Are W3 and W4 Excesses in 75 pc ? • Asteroid belt/Zodiacal Light
analogs: 4%• Kuiper Belt/Asteroid belt analogs: 96%
In a) we trace the W2-W4 vs. BT-VT dependence for our sample of stars using a running mean to estimate the photospheric contribution to the WISE colors. We create a color SNR (ΣE) from the color excess (E[W2-W4]). The distribution in b) was used to calculate the 99.5% confidence level (green line) above which stars were chosen as candidate debris disks.
1Department of Physics and Astronomy at Stony Brook University2Department of Physics and Astronomy at The University of Western Ontario
Empirically Finding Excesses at 12 µm and 22 µm
a) b)
We search for W3 (12µm) and W4 (22µm) excesses from exozodi or asteroid belts around ~15,000 Hipparcos stars within 75 pc by using short minus long wavelength WISE colors.
Scan here to link to the paper for this work (Patel, Metchev, Heinze 2013, ApJS, 212,10 (ArXiv:1403.3435)
• 220 stars < 75 pc with excess at 12 µm or 22 µm
• 111 New detections at any wavelength
• 45% increase of 10-30µm excesses
• 25% increase in 75 pc debris disk census
The incidence rates we derive for 12 µm and 22 µm excesses exceed previous determinations from WISE by virtue of our precise photometric calibration. Our incidence rates for 12 µm excesses agree with the most sensitive results from Spitzer, while our incidence rates for 22 µm excesses are 1.5-3x less sensitive to Spitzer’s estimates.
Finding Warm Debris Disks with WISE Around Bright StarsRahul I. Patel1, Stanimir
Metchev1,2, Aren Heinze1
For the first time, we are able to detect small excesses even around bright solar neighborhood stars whose WISE fluxes are saturated. We do so by deriving and applying corrections to the fluxes of saturated stars in WISE.
