English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present high-spectral resolution M-band spectra from iSHELL on NASA'sInfrared Telescope Facility (IRTF) along the line of sight to the debris diskhost star HD 32297. We also present a Gemini Planet Imager (GPI) H-bandpolarimetric image of the HD 131488 debris disk. We search for fundamental COabsorption lines in the iSHELL spectra of HD 32297 but do not detect any. Weplace an upper limit on the CO column density of $\sim$6$\times10^{15}$cm$^{-2}$. By combining the column density upper limit, the CO mass measuredwith ALMA, and the geometrical properties of the disk, we estimate the scaleheight of the CO to be $\lesssim$ 2 au across the radial extent of the disk($\sim$80-120 au). We use the same method to estimate the CO scale height ofthree other edge-on, CO-rich debris disks that all have CO observed inabsorption with HST as well as in emission with ALMA: $\beta$ Pictoris, HD110058, and HD 131488. We compare our estimated CO scale heights of these foursystems to the millimeter dust scale heights and find that, under theassumption of hydrostatic equilibrium, there is a potential correlation betweenthe CO and millimeter dust scale heights. There are multiple factors thataffect the gas vertical structure such as turbulence, photodissociation withweak vertical mixing, as well as where the gas originates. One possibleexplanation for the potential correlation could be that the gas and dust are ofa similar secondary origin in these four systems.

Vertical Structure of Gas and Dust in Four Debris Disks