Digiorno-Like Object (DLO) in SETI

• Digiorno-Like Object (DLO) is a toy-model defining a stellar-powered pizza used in SETI to explore thermal equilibrium and orbital phenomena.
• The Flavor Zone concept specifies orbital distances where the DLO reaches optimal baking temperatures (375–425°F), illustrating precise radiative-cooking physics.
• Observational analyses conclude that DLOs are beyond current detection capabilities, serving as an extreme case for evaluating SETI technosignature limits.

A Digiorno-Like Object (DLO) is a toy-model “stellar-powered pizza” introduced in a SETI context to examine whether an advanced civilization could place flat, pizza-like food packages into orbit around a star and cook them directly with stellar irradiation. In that formulation, the associated Flavor Zone (FZ) is the regime for optimal cooking according to package directions: the range of orbital separations at which the DLO equilibrium temperature lies within the baking-instructions interval. The model was developed to study thermal equilibrium, orbital effects on cooking, and observational detectability, and its principal conclusion is that DLOs are not detectable with current technology (Pearce et al., 30 Mar 2026).

1. Definition, construction, and motivation

The DLO is defined as a flat disk of radius $R_p \approx 6$ in $\approx 0.127\ \mathrm{m}$, corresponding to a 12-inch pizza, with a surface composed of dough, tomato sauce, cheese, and toppings. The toy model assumes a uniform albedo $A \approx 0.06$, described as typical of cheddar cheese at near-IR wavelengths. The motivating premise is that a sufficiently advanced civilization could “skip the middle man” of converting starlight to electricity and then to oven heat, and instead use raw stellar flux for cooking directly in orbit. If such behavior were widespread, DLOs might produce observable photometric or spectroscopic anomalies (Pearce et al., 30 Mar 2026).

Within this framework, the DLO is not a planetary body, an artificial habitat, or an energy-harvesting megastructure in the usual SETI sense. It is a deliberately narrow toy model centered on food preparation by radiative heating. This suggests that the concept is intended less as a realistic engineering proposal than as a constrained probe of how detectability arguments behave when pushed to an extreme and highly specific techno-signature hypothesis.

2. Flavor Zone formalism

The Flavor Zone is defined as the range of orbital separations $r$ for which the DLO equilibrium temperature $T_p$ lies between $T_{\min}=463.7\ \mathrm{K}$ and $T_{\max}=491.5\ \mathrm{K}$, corresponding to $375$–$425\ ^\circ\mathrm{F}$. The thermal model begins from the incident, absorbed, and emitted powers:

$$P_{\mathrm{incident}} = L_* \cdot \frac{\pi R_p^2}{4\pi r^2},$$

$\approx 0.127\ \mathrm{m}$0

$\approx 0.127\ \mathrm{m}$1

At radiative equilibrium, $\approx 0.127\ \mathrm{m}$2, giving

$\approx 0.127\ \mathrm{m}$3

For a Sun-like star, substituting $\approx 0.127\ \mathrm{m}$4 yields

$\approx 0.127\ \mathrm{m}$5

Using a fiducial baking temperature of $\approx 0.127\ \mathrm{m}$6 ($\approx 0.127\ \mathrm{m}$7) gives $\approx 0.127\ \mathrm{m}$8. More generally, the inner and outer Flavor Zone boundaries for a Sun-like star are $\approx 0.127\ \mathrm{m}$9 and $A \approx 0.06$0 (Pearce et al., 30 Mar 2026).

The same analysis was extended to nearby stars using each star’s $A \approx 0.06$1, $A \approx 0.06$2, and $A \approx 0.06$3. In that comparison, cooler M-dwarfs have extremely tight FZs, $A \approx 0.06$4, while hot A stars such as Sirius A have FZs of order $A \approx 0.06$5–$A \approx 0.06$6 (Pearce et al., 30 Mar 2026). This suggests that the Flavor Zone is highly sensitive to stellar type and should be understood as a radiative-equilibrium construct tied to baking instructions rather than to any broader astrophysical habitability criterion.

3. Toy-model assumptions, cooking time, and orbital effects

The DLO is assumed to be a uniform, Lambertian flat disk of radius $A \approx 0.06$7 with wavelength-independent albedo $A \approx 0.06$8. Its orientation is held “cheese-on,” meaning face-on to the star, by hypothetical thrusters; an edge-on “crust-on” orientation would receive only $A \approx 0.06$9 of the flux. Thermal inertia, conduction within the pizza, and reradiation from toppings are neglected, so the model is pure radiative equilibrium (Pearce et al., 30 Mar 2026).

For cooking time, the toy model adopts the commercial recipe time $r$0–$r$1 at $r$2. A first-principles estimate is noted as possible in principle by integrating absorbed power until the cheese and crust reach glass-transition or melt temperature, but the operational scaling used is

$r$3

Accordingly, changes in orbital distance, albedo, or disk radius directly adjust cooking time through the factor $r$4 and $r$5 (Pearce et al., 30 Mar 2026).

For non-circular orbits, the instantaneous star–DLO distance varies as

$r$6

so the temperature varies as $r$7. In the Proxima Centauri case with release at the FZ midpoint, $r$8, all such orbits remain within the FZ for $r$9 around periastron even for $T_p$0 up to unity, but only orbits with $T_p$1 remain entirely within the FZ over the full $T_p$2 phase. Inclination $T_p$3 does not change cooking, but it does affect observability, including transit depth and reflected-light phase curves (Pearce et al., 30 Mar 2026). A plausible implication is that “successful cooking” in the toy model can be transiently achieved over portions of an orbit even when the orbit does not remain fully inside the Flavor Zone.

4. Observational signatures and detectability limits

Three observational channels were analyzed: transit photometry, direct imaging in thermal emission, and direct imaging in reflected light. In the transit case, a DLO with radius $T_p$4 around Proxima Centauri yields a transit depth $T_p$5. Simulations with planetplanet show flux dips $T_p$6, beyond present photometric precision, and simulated JWST F560W time-series also show no detectable transit. The required threshold is $T_p$7, whereas Kepler and TESS reach $T_p$8–$T_p$9 (Pearce et al., 30 Mar 2026).

For thermal direct imaging, assuming a $T_{\min}=463.7\ \mathrm{K}$0 blackbody, the DLO peaks near $T_{\min}=463.7\ \mathrm{K}$1. At Earth, for a DLO at $T_{\min}=463.7\ \mathrm{K}$2 from $T_{\min}=463.7\ \mathrm{K}$3 Cen A, the flux is $T_{\min}=463.7\ \mathrm{K}$4, compared with stellar flux $T_{\min}=463.7\ \mathrm{K}$5, implying a thermal contrast $T_{\min}=463.7\ \mathrm{K}$6, or about $T_{\min}=463.7\ \mathrm{K}$7 mag (Pearce et al., 30 Mar 2026).

For reflected light, the adopted phase-law model gives

$T_{\min}=463.7\ \mathrm{K}$8

with $T_{\min}=463.7\ \mathrm{K}$9. At full phase, $T_{\max}=491.5\ \mathrm{K}$0, about $T_{\max}=491.5\ \mathrm{K}$1 mag, for $T_{\max}=491.5\ \mathrm{K}$2 Cen A; at quadrature the DLO appears as a thin sliver with negligible reflected flux (Pearce et al., 30 Mar 2026).

The feasibility analysis is correspondingly negative. Transit searches would require $T_{\max}=491.5\ \mathrm{K}$3; direct imaging would require contrasts $T_{\max}=491.5\ \mathrm{K}$4 at separations $T_{\max}=491.5\ \mathrm{K}$5 for nearby cool stars; and even mid-IR nulling interferometry concepts such as LIFE or FKSI, which could in principle approach $T_{\max}=491.5\ \mathrm{K}$6–$T_{\max}=491.5\ \mathrm{K}$7 contrasts at $T_{\max}=491.5\ \mathrm{K}$8, remain $T_{\max}=491.5\ \mathrm{K}$9 orders of magnitude too shallow. The stated conclusion is categorical: no current or planned facility can detect DLOs in any realistic scenario, and the results determine that DLOs are not detectable with current technology nor should anyone ever try (Pearce et al., 30 Mar 2026).

5. Terminological ambiguity of the acronym “DLO”

A notable source of ambiguity is that the acronym “DLO” is already standard in robotics for “deformable linear object,” not Digiorno-Like Object. In that literature, DLOs are “cables, ropes, and wires,” or more generally elongated, highly deformable items such as “cable, rope, hose” whose length greatly exceeds cross-section (Lv et al., 19 Dec 2025); (Kicki et al., 2023).

The two usages are conceptually unrelated. In robotics, DLO research addresses state estimation, tracking, perception under occlusion, manipulation, planning, and control of flexible one-dimensional bodies (Lv et al., 19 Dec 2025). In the SETI usage, the DLO is a flat radiatively heated food package whose defining variables are stellar flux, equilibrium temperature, orbit, and observability (Pearce et al., 30 Mar 2026). This suggests that the Digiorno-Like Object should be treated as a field-specific reuse of an already overloaded acronym rather than as part of the established deformable-object literature.

6. SETI significance and interpretive role

The broader implication drawn from the DLO study is methodological rather than observational. The non-detectability of DLOs highlights the caution required when extrapolating Earth-centric technologies into SETI, even when the underlying physical scenario is internally consistent. The work underscores that a techno-signature may be conceivable in principle yet completely inaccessible in practice, and that detectability, rather than mere feasibility, should guide SETI strategy (Pearce et al., 30 Mar 2026).

The paper therefore places DLOs at the extreme end of speculative signature design. Future searches are recommended to focus on signatures closer to observational capabilities, including waste heat in the mid-IR at $375$0–$375$1 contrast and radio technosignatures, rather than speculative “stellar-cooked pizza.” It is also described as an illustrative “upper bound” on how exotic and contrived a civilization’s technology might be while still evading detection by factors of $375$2–$375$3 (Pearce et al., 30 Mar 2026). In that sense, the Digiorno-Like Object functions less as a candidate discovery class than as a limiting case for SETI reasoning about observability.