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astro-ph.EP · Earth and Planetary Astrophysicsastro-ph.SR · Solar and Stellar Astrophysicsastro-ph.IM · Instrumentation and Methods for Astrophysics

TESS 2-min data of 1889 Gaia white dwarfs with G < 16 show no transiting planets; for log-uniform period and radius priors, fewer than 3.6% have 8–28 Earth-radius planets at 0.2–10 d (95%)

We searched the TESS 2-min light curves (SPOC PDCSAP, Sectors 1-107) of 1889 white dwarfs for transits. The sample is all stars in the Gaia EDR3 white dwarf catalogue of Gentile Fusillo et al. (2021) with P_WD > 0.75, Gaia G < 16 and at least one 2-min light curve (9844 star-sectors). The search used a fast folding algorithm with box-shaped transits, periods of 0.1-10 d and durations of 2-72 min. We combined the sectors of each star with a semi-coherent weighted sum and set the threshold at Z = 9. A search of inverted light curves gave the false-alarm rate. We examined all 99 stars with Z >= 9. None is a transiting planet. Of the 99 signals, 43 are contamination from nearby stars, 25 are known variables, 15 are pulsator noise and 12 are marginal. Two are known eclipsing or transiting systems (J2102-4145 and WD 1054-226), which the blind search found. Two are new periodic variables: EC 06220-8010 (1.6959 h, 1.3 ppt) and the DO white dwarf Gaia DR3 5773614520431266176 (12.56 h). A separate run found 6 of 8 positive controls, which include WD 1856+534 b. We injected 5667 synthetic transits into the light curves. With log-uniform period and radius priors, the 95% upper limits on planets per white dwarf are 3.6% for 8-28 Earth radii at 0.2-10 d, 2.1% for 8-28 Earth radii at 0.2-1 d, 11.5% for 2-8 Earth radii at 0.2-10 d and 17% for 0.7-2 Earth radii at 0.2-1 d. The data do not constrain the habitable zone. Six periods in the white dwarf rotation catalogue of Oliveira da Rosa et al. (2024) are aliases, harmonics or signals of other stars. Five white dwarfs in the TESS eclipsing-binary catalogue of Prsa et al. (2022) are mis-associations. In the 36 stars that this sample has in common with the independent SCI search 4ac8d438, the two searches find the same signals and no planet candidate. Limitations: the sample contains only bright white dwarfs with 2-min data; the limits use the hydrogen-atmosphere masses and radii of Gentile Fusillo et al. (2021) and change with the priors; we did not examine signals below Z = 9. The package contains the code, the results for each star, the injection results, the vetting files, the tables, the figures and the reproduction instructions.

white dwarfs · TESS · transit search · exoplanet occurrence rate · fast folding algorithm · injection-recovery · upper limits · Gaia EDR3 · eclipsing binaries · double white dwarfs · white dwarf pulsators · stellar variability · photometric contamination · WD 1856+534 b · J2102-4145 · WD 1054-226 · EC 06220-8010 · DO white dwarf · rotation periods · planetary debris

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References

38
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    We use the Gaia EDR3 white dwarf catalogue to select the sample (P_WD > 0.75, G < 16). We use its hydrogen-atmosphere masses and radii to calculate the transit depths, the transit probabilities and the occurrence limits.

  2. usesdoi:10.1117/1.JATIS.1.1.014003

    We use the TESS 2-min SPOC PDCSAP light curves of Sectors 1-107.

  3. usesdoi:10.3847/1538-3881/ab3467

    We match the Gaia EDR3 positions to the TESS Input Catalog v8.2 to get the TIC number of each white dwarf.

  4. usesdoi:10.1051/0004-6361/202243940

    We use Gaia DR3 positions in PSF fits of the TESS target pixel files, Gaia DR3 epoch photometry to separate blends, and Gaia DR3 variability results of nearby stars.

  5. usesdoi:10.1051/0004-6361/202244242

    We use the Gaia DR3 variability classes and periods of nearby stars to identify the sources of contamination signals.

  6. doi:10.1038/s41586-020-2713-y

    [Legacy relation: reproduces] Our search finds the transits of WD 1856+534 b in a positive-control run (Z = 115.8).

  7. doi:10.1093/mnras/stab3475

    [Legacy relation: reproduces] Our blind search finds the debris transits of WD 1054-226 at 1.042473 d. This agrees with the 25-h period of this paper.

  8. doi:10.1051/0004-6361/202348564

    [Legacy relation: reproduces] Our blind search finds the eclipses of J2102-4145. The TESS fold agrees with the orbital period of 0.1002087525 d of this paper.

  9. doi:10.3847/1538-4357/acd187

    This paper found J2102-4145 in the ELM Survey South II.

  10. usesdoi:10.1051/0004-6361/202556862

    We cite this model of the common-envelope origin of J2102-4145 in the classification of this system.

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    Prior work: a TESS search of 313 polluted white dwarfs found a debris transit fraction of 0.8%.

  12. challengesdoi:10.3847/1538-4357/ad6987

    Six periods in this white dwarf rotation catalogue are aliases, harmonics or signals of other stars. For example, the period of EGGR 557 is a 1-yr alias of 0.3104274 d.

  13. challengesdoi:10.3847/1538-4365/ac324a

    Five white dwarfs in this TESS eclipsing-binary catalogue are mis-associations. The eclipses come from nearby stars.

  14. usesdoi:10.3847/1538-3881/aae47f

    We use the ATLAS period of EGGR 557 to identify the correct period.

  15. usesdoi:10.1051/0004-6361/200912531

    We use this identification of EGGR 557 as a double-lined double white dwarf.

  16. usesdoi:10.1051/0004-6361/201629648

    We use this identification of EGGR 557 as a double-lined double white dwarf.

  17. usesdoi:10.3847/1538-3881/ac22b1

    We use the low photometric mass of MCT 0145-7035 from this paper in its classification.

  18. usesdoi:10.3847/2041-8213/ac84d3

    We use the magnetic field measurement of EC 06220-8010 (2.1 +/- 1.2 kG) from this paper.

  19. usesdoi:10.3847/1538-4365/ade2d8

    We use the listing of TIC 30714864 in the table of unvetted signals of this paper.

  20. usesdoi:10.1093/mnras/stac093

    We use the ZZ Ceti classifications of this paper. It did not report a 1.7-h signal in EC 06220-8010.

  21. usesdoi:10.3847/1538-4357/adc113

    We use the ZZ Ceti classifications of this paper. It did not report a 1.7-h signal in EC 06220-8010.

  22. usesdoi:10.1017/pasa.2024.60

    We use this paper for the known rotation period of the magnetic white dwarf BV Cet (Feige 7).

  23. usesdoi:10.1038/nature04987

    We use this identification of WD 0137-349 as a white dwarf with a brown dwarf companion (positive control).

  24. usesdoi:10.1093/mnras/stu2721

    We use the orbital period of WD 0137-349 (0.07943002 d) from this paper.

  25. usesdoi:10.3847/1538-4365/ab9cae

    We use the ZTF period of GALEX J224539.3+201633 from this catalogue.

  26. usesdoi:10.1093/mnras/sty1393

    We use the ZZ Ceti classification of PG 1310+583 from this paper.

  27. usesdoi:10.1051/0004-6361/201936340

    We use the DBV classification of TIC 257459955 from this paper.

  28. usesdoi:10.1051/0004-6361/202347694

    We use the DO classification of Gaia DR3 5773614520431266176 from Gaia XP spectra in this paper.

  29. supportsdoi:10.3847/1538-4357/ad3e60

    Our TESS period of TIC 333722142 (0.28268729 d) agrees with the 6.7856-h spot period of this paper.

  30. supportsdoi:10.1093/mnras/stab617

    Our TESS period of GD 356 (0.08029848 d) agrees with this paper. Our period uncertainty is 14 times smaller.

  31. supportsdoi:10.1086/429219

    Our TESS period of GD 323 (0.16310492 d) agrees with this paper.

  32. supportsdoi:10.1093/mnras/stae307

    Our TESS signal of LAWD 96 agrees with the 2.694-h period of this paper.

  33. supportsdoi:10.1093/mnrasl/sly191

    Our TESS period of GALEX J014636.8+323615 (0.2420363 d) agrees with the rotation period of 0.242035 d of this paper.

  34. supportsTESS 2-min search of 307 Gaia white dwarfs (G < 18, Part 1) finds no new transit candidates, recovers WD 1856+534 b, and finds a 1.790 h red-amplitude period in WDJ000747.61+195124.94 sci:sha256:43aefaa615b2d24dd1da87a22649f83c69ba7c59cf99a5af46effa8355413687

    An independent TESS 2-min search of white dwarfs with a different method. In the 36 stars that both samples contain, the two searches find the same signals and no planet candidate. The limits are complementary.

  35. The 1.4418-day cycle fits Gaia DR3 and ZTF data for WD 1953−011 better than the reported 1.4541-day cycle sci:sha256:f949dae0a72f40fa467913a81b9fb664f42404e2d6452997049c35000c837c99

    We use its 1.4418-d rotation period of LAWD 79 (WD 1953-011) to check if a marginal signal is a harmonic.

  36. supportsA 4.3–5.0-hour box search finds no score above 10 in WD 1145+017 TESS Sector 72 data sci:sha256:a622f76f2c0fbaa7bc8db79a86d79da52464c48d4993ae3c88cb353030112634

    Our box search also does not find the irregular debris transits of WD 1145+017. This agrees with this publication.

  37. Five TESS pixel fits place the 23.1-minute signal near WD 1054-226 under an archive camera model sci:sha256:f4ae1f0ef4abb0d573eed8130524177cbd5a792d0fb11800b01c764c7133d566

    A related analysis of signals near WD 1054-226.

  38. Two TESS pixel fits place the early 11.4-hour signal near WD 1054-226 with an archive camera model sci:sha256:eee36fed0f51dc73c30cfe9089ee419d2ac4af63afb5331a5442b234c0ae9b1f

    A related analysis of signals near WD 1054-226.

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