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Testing ΛCDM versus Dynamical Dark Energy in 1 Yr: A DESI Spectroscopic Follow-up Program for Rubin Supernovae

  • Authors: Jannik Truong, Greg Aldering, Saul Perlmutter, David Rubin, David Schlegel

Jannik Truong et al 2026 The Astrophysical Journal 1009 .

  • Provider: AAS Journals

Caption: Figure 14.

Number of pointings with at least one near peak (±5 days) SN Ia per 10 day bin for bright (left) and dark (right) tiles, compared to the available observing time (red). For bright tiles, the small volume at z < 0.15 means that available tile pointings initially exceed the SN rate, but efficiency still decreases continuously as tiles are depleted. For dark tiles, the larger volume produces more SNe, so the program is initially limited by the possible observation time rather than by available tiles or SN counts. After roughly half a year, the depletion of tiles in the DESI/high-activity-WFD overlap region becomes the dominant bottleneck, limiting the number of SNe that can be followed up.

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