Frequency of Debris Disks around Solar‐Type Stars: First Results from a<i>Spitzer</i>MIPS Survey

Bryden, G.; Beichman, Charles; Trilling, David E.; Rieke, G. H.; Holmes, Elizabeth; Lawler, Samantha; Stapelfeldt, K.; Werner, M. W.; Gautier, T. N.; Blaylock, Myra L.; Gordon, K. D.; Stansberry, J.; Su, K. Y. L.

doi:10.1086/498093

Cited by 253 publications

(499 citation statements)

References 65 publications

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“…Figure 11 summarizes the rates of IR excess detection in IRS spectral surveys and compares them with MIPS photometric results. For two wavelengths in each instrument, the distribution (Bryden et al 2006;Beichman et al 2006b;Trilling et al 2008). For IRS spectra, 203 stars with spectral types F0-M0 are observed from 10 through 32 μm (from this survey and the stars in Table 6).…”

Section: Limits On the Fractional Disk Luminositymentioning

confidence: 99%

“…Most of these data have already been published; for consistency, we have re-reduced all of them with a uniform set of analysis parameters. Our analysis is similar to that previously described in Beichman et al (2005a), Bryden et al (2006), andBeichman et al (2006b). At 24 μm, images are created from the raw data using software developed by the MIPS instrument team (Gordon et al 2005), with image flats chosen as a function of scan mirror position to correct for dust spots and with individual frames normalized to remove largescale gradients (Engelbracht et al 2007).…”

Section: Mips Photometrymentioning

confidence: 99%

“…For three systems that are marginally resolved at 70 μm (HD 10647, HD 38858, and HD 115617; see Section 5.2.3), the small aperture fails to capture all of the extended emission; for these three cases the MIPS fluxes listed in Table 5 are based on model fits to each disk (G. Bryden et al 2009, in preparation). While our procedure has changed little since Bryden et al (2006) was published, note that improvements in the instrument calibration since then have increased the overall 70 μm flux conversion by 4%, from 15.8 to 16.5 mJy/arcsec 2 /MIPS_70_unit (MIPS_70_unit is an internally defined standard based on the ratio of the measured signal to that from the stimulator flash signal (Gordon et al 2007). Overall, we find no qualitative disagreement between our results and those from earlier publications.…”

Section: Mips Photometrymentioning

confidence: 99%

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EXPLORATIONS BEYOND THE SNOW LINE:SPITZER/IRS SPECTRA OF DEBRIS DISKS AROUND SOLAR-TYPE STARS

Lawler

Beichman

Bryden

et al. 2009

ApJ

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We have observed 152 nearby solar-type stars with the Infrared Spectrometer (IRS) on the Spitzer Space Telescope. Including stars that met our criteria but were observed in other surveys, we get an overall success rate for finding excesses in the long-wavelength IRS band (30-34 μm) of 11.8% ± 2.4%. The success rate for excesses in the shortwavelength band (8.5-12 μm) is ∼1% including sources from other surveys. For stars with no excess at 8.5-12 μm, the IRS data set 3σ limits of around 1000 times the level of zodiacal emission present in our solar system, while at 30-34 μm data set limits of around 100 times the level of our solar system. Two stars (HD 40136 and HD 10647) show weak evidence for spectral features; the excess emission in the other systems is featureless. If the emitting material consists of large (10 μm) grains as implied by the lack of spectral features, we find that these grains are typically located at or beyond the snow line, ∼1-35 AU from the host stars, with an average distance of 14 ± 6 AU; however, smaller grains could be located at significantly greater distances from the host stars. These distances correspond to dust temperatures in the range ∼50-450 K. Several of the disks are well modeled by a single dust temperature, possibly indicative of a ring-like structure. However, a single dust temperature does not match the data for other disks in the sample, implying a distribution of temperatures within these disks. For most stars with excesses, we detect an excess at both IRS and Multiband Imaging Photometer for Spitzer (MIPS) wavelengths. Only three stars in this sample show a MIPS 70 μm excess with no IRS excess, implying that very cold dust is rare around solar-type stars.

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Section: Limits On the Fractional Disk Luminositymentioning

confidence: 99%

Section: Mips Photometrymentioning

confidence: 99%

Section: Mips Photometrymentioning

confidence: 99%

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EXPLORATIONS BEYOND THE SNOW LINE:SPITZER/IRS SPECTRA OF DEBRIS DISKS AROUND SOLAR-TYPE STARS

Lawler

Beichman

Bryden

et al. 2009

ApJ

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“…The double pair could be unbound and merely flying by (Reche et al 2009). Mamajek & Hillenbrand (2008); (23) Henry et al (1996); (24) Bryden et al (2006) and references therein; (25) Zuckerman & Webb (2000); (26) Merín et al (2004); (27) Valenti & Fischer (2005).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Kuiper belts around nearby stars

Nilsson

Liseau

Brandeker

et al. 2010

A&A

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Context. The existence of dusty debris disks around a large fraction of solar type main-sequence stars, inferred from excess far-IR and submillimetre emission compared to that expected from stellar photospheres, suggests that leftover planetesimal belts analogous to the asteroid-and comet reservoirs of the solar system are common. Aims. Sensitive submillimetre observations are essential to detect and characterise cold extended dust originating from collisions of small bodies in disks, belts, or rings at Kuiper-belt distances (30-50 AU or beyond). Measurements of the flux densities at these wavelengths will extend existing IR photometry and permit more detailed modelling of the Rayleigh-Jeans tail of the disks spectral energy distribution (SED), effectively constraining dust properties and disk extensions. By observing stars spanning from a few up to several hundred Myr, the evolution of debris disks during crucial phases of planet formation can be studied. Methods. We observed 22 exo-Kuiper-belt candidates at 870 μm, as part of a large programme with the LABOCA bolometer at the APEX telescope. Dust masses (or upper limits) were calculated from integrated 870 μm fluxes, and fits to the SED of detected sources revealed the fractional dust luminosities f dust , dust temperatures T dust , and power-law exponents β of the opacity law. Results. A total of 10 detections with at least 3σ significance were made, out of which five (HD 95086, HD 131835, HD 161868, HD 170773, and HD 207129) have previously never been detected at submillimetre wavelengths. Three additional sources are marginally detected with >2.5σ significance. The best-fit β parameters all lie between 0.1 and 0.8, in agreement with previous results indicating the presence of significantly larger grains than those in the ISM. From our relatively small sample we estimate f dust ∝ t −α , with α ∼ 0.8−2.0, and identify an evolution of the characteristic radial dust distance R dust that is consistent with the t 1/3 increase predicted from models of self-stirred collisions in debris disks.

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“…The occurrence rate of debris disks containing hot dust around Sun-like stars is very low, ∼2% (Bryden et al 2006a(Bryden et al , 2006bChen et al 2006). Recent work suggests that the hot dust around most mature Sun-like stars is transiently regeneratedsince it is found to be present in quantities far in excess of that expected to arise from sublimation of comets (Beichman et al 2005) or slow collisional grinding of asteroids left over from the era of planet formation .…”

Section: Introductionmentioning

confidence: 99%

CONSTRAINTS ON THE PRESENCE OF SiO GAS IN THE DEBRIS DISK OF HD 172555

Wilson

Nilsson

Chen

et al. 2016

ApJ

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We have carried out two sets of observations to quantify the properties of SiO gas in the unusual HD 172555 debris disk: (1) a search for the J=8-7 rotational transition from the vibrational ground state, carried out with the Atacama Pathfinder EXperiment (APEX) submillimeter telescope and heterodyne receiver at 863 μmand (2) a search at 8.3 μm for the P(17) ro-vibrational transition of gas phase SiO, carried out with the Very Large Telescope (VLT)/VISIR with a resolution, λ/Δλ, of 30,000. The APEX measurement resulted in a 3.3σ detection of an interstellar feature, but only an upper limit to emission at the radial velocity and line width expected from HD 172555. The VLT/VISIR result was also an upper limit. These were used to provide limits for the abundance of gas phase SiOfor a range of temperatures. The upper limit from our APEX detection, assuming an 8000 K primary star photospheric excitation, falls more than an order of magnitude below the self-shielding stability threshold derived by Johnson et al. (2012). Our results thus favor a solid-state origin for the 8.3 μm feature seen in the Spitzer IRS spectrum of the circumstellar excess emissionand the production of circumstellar O I and Si I by SiO UV photolysis. The implications of these estimates are explored in the framework of models of the HD 172555 circumstellar disk.

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Frequency of Debris Disks around Solar‐Type Stars: First Results from aSpitzerMIPS Survey

Cited by 253 publications

References 65 publications

EXPLORATIONS BEYOND THE SNOW LINE:SPITZER/IRS SPECTRA OF DEBRIS DISKS AROUND SOLAR-TYPE STARS

EXPLORATIONS BEYOND THE SNOW LINE:SPITZER/IRS SPECTRA OF DEBRIS DISKS AROUND SOLAR-TYPE STARS

Kuiper belts around nearby stars

CONSTRAINTS ON THE PRESENCE OF SiO GAS IN THE DEBRIS DISK OF HD 172555

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