The Cold Debris Disk Surveys I. Host Star Properties

Abstract

We describe the dynamical, photometric, and spectroscopic data available for stars targeted by Spitzer and Herschel to search for cold circumstellar dust emission from debris disks, a collection that we name the Cold Debris Disk Surveys (CDDS). These data include Hipparcos and Gaia parallaxes, 0.4-1250 micron photometry, spectral types, effective temperatures, gravities, bolometric luminosities, visual extinctions, metallicities, lithium abundances, rotational periods, projected rotational velocities, the Ca~II HK and IR triplet activity indicators, and X-ray luminosities for 3675 stars. Within this sample, we investigate the frequency of stellar and planetary companions (including potential new proper motion companions); use the data to assign CDDS stars to the field or one of many moving groups, open clusters, or stellar associations; and investigate correlations between stellar activity indicators. In future papers, we plan to explore the magnitude and frequency of infrared excess emission as a function of host star properties; to search for new companions with Gaia; and to examine the evolution of infrared excesses with the ages of stars in clusters and the field.

Figures (21)

• Figure 1: Fraction of CDDS targets with photometric uncertainty $\delta m \lesssim$ 0.05 mag as a function of wavelength for BVI$_{\rm C}$ (purple), Gaia (light green), Pan-Starrs and SkyMapper griz (dark green), Tycho (light blue), and 2MASS (orange-red). The purple plus signs illustrate the fraction of stars with (i) $\rm B_T$ and B, (ii) $g$, $\rm V_T$, and V, (iii) $i$ and I, and (iv) 2MASS JHK plus other JHK data. The light green solid line indicates the fraction of CDDS stars with Gaia low resolution XP spectra. The fraction of targets with high quality optical and near-IR data ranges from $\sim$ 22% ( griz) to $\sim$ 70% (Tycho) to $\sim$ 80--90% (BVI$_{\rm C}$ and JHK) to close to 100% (Gaia).
• Figure 2: As in Fig. \ref{['fig: stats1']} for data from WISE (purple), Spitzer IRAC and MIPS (light blue), IRAS (dark green), Herschel PACS and SPIRE (gold), and submm--mm (red). The light blue symbols with a dark blue center indicate the fraction of CDDS stars with high quality synthetic photometry at 8--25 $\rm \,\mu {\rm m}$ from Spitzer IRS. The fraction of observed sources ranges from $\sim$ 1--2% at the longest wavelengths to $\sim$ 10--20% for Spitzer IRAC, Spitzer IRS, and IRAS 25 $\rm \,\mu {\rm m}$ to $\gtrsim$ 50% for W3, W4, and MIPS 24 $\rm \,\mu {\rm m}$ measurements. With a fraction observed of zero for 500 $\rm \,\mu {\rm m}$ SPIRE data with SNR $\ge$ 3, this point is not shown.
• Figure 3: Cumulative probability distribution of parallaxes for CDDS stars (blue curve) and stars in the Gaia 100 pc sample gaianearby2021 that lie close to the pecaut2013 main sequence (orange curve). The set of CDDS (Gaia) stars follows an $n \propto \pi^0$ ($n \propto \pi^{-2}$) volume density distribution, as indicated by the dashed (dotted) black curves.
• Figure 4: Frequency of BP--RP colors (lower x-axis labels) and main sequence spectral types pecaut2013 of stars in the CDDS sample (histogram) and main sequence stars in the Gaia 100 pc sample gaianearby2021. The frequency of Gaia stars has been normalized by a factor of 1/60. Relative to the Gaia sample of MS stars within 100 pc, the CDDS sample has many more AFGK stars and many fewer M-type and later stars.
• Figure 5: Summary of CDDS stars with companions. Each data point has some uncertainty or ambiguity, as described in the text, but is anticipated to be within a factor of a few of a true or well-determined value. Since each coordinate axis spans orders of magnitude, the broad characteristics of known non-single stars in the CDDS are well represented here.