VizieR Online Data Catalog: TESS M-dwarf exoplanetary systems (Ballard, 2019)
Abstract
To generate a realistic synthetic sample of planetary systems, we take the following steps. We draw periods and radii for each mock planetary system from the empirical distribution of Dressing & Charbonneau (2015, J/ApJ/807/45). We then employ the distributions of Limbach & Turner (2015PNAS..112...20L) to assign eccentricity. We assign planetary masses with the relations of Zeng & Jacobsen (2017ApJ...837..164Z) for R<1.5 R{Earth} and Wolfgang et al. (2016, J/ApJ/825/19) for R>1.5 R{Earth}. Rogers (2015ApJ...801...41R) identified the cutoff between a majority of rocky planets and a majority of icy/gaseous planets at 1.5 R{Earth}, but these two relations also naturally overlap at 1.5 R{Earth}. We assess the stability of the system by ensuring that planets satisfy the criterion defined in Fabrycky et al. (2012, J/ApJ/790/146). For generating synthetic TESS planetary systems orbiting M dwarfs, we employ four different stellar masses corresponding to four different effective temperature ranges (from Boyajian et al. 2012, J/ApJ/757/112): 0.25 Mȯ (for stars 3200-3400 K), 0.41 Mȯ (for stars 3400-3600 K), 0.50 Mȯ (for stars 3600-3800 K), and 0.60 Mȯ (for stars 3800-4000 K). We then assign a Boolean TTV flag to each transiting planet. Finally, we calculate and record an independent density for each planet using only its mutual Hill spacing from neighboring planets.
(1 data file).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- June 2019
- DOI:
- 10.26093/cds/vizier.51570113
- Bibcode:
- 2019yCat..51570113B
- Keywords:
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- Stars: dwarfs;
- Stars: M-type;
- Exoplanets;
- Stars: distances;
- Effective temperatures;
- Stars: masses;
- Stars: diameters;
- Models