Skip to main content

The Factory and the Beehive. III. PTFEB132.707+19.810, A Low-mass Eclipsing Binary in Praesepe Observed by PTF and K2

Author(s): Kraus, Adam L; Douglas, Stephanie T; Mann, Andrew W; Agüeros, Marcel A; Law, Nicholas M; et al

To refer to this page use:
Full metadata record
DC FieldValueLanguage
dc.contributor.authorKraus, Adam L-
dc.contributor.authorDouglas, Stephanie T-
dc.contributor.authorMann, Andrew W-
dc.contributor.authorAgüeros, Marcel A-
dc.contributor.authorLaw, Nicholas M-
dc.contributor.authorCovey, Kevin R-
dc.contributor.authorFeiden, Gregory A-
dc.contributor.authorRizzuto, Aaron C-
dc.contributor.authorHoward, Andrew W-
dc.contributor.authorIsaacson, Howard-
dc.contributor.authorGaidos, Eric-
dc.contributor.authorTorres, Guillermo-
dc.contributor.authorBakos, Gaspar Aron-
dc.identifier.citationKraus, Adam L, Douglas, Stephanie T, Mann, Andrew W, Agüeros, Marcel A, Law, Nicholas M, Covey, Kevin R, Feiden, Gregory A, Rizzuto, Aaron C, Howard, Andrew W, Isaacson, Howard, Gaidos, Eric, Torres, Guillermo, Bakos, Gaspar. (2017). The Factory and the Beehive. III. PTFEB132.707+19.810, A Low-mass Eclipsing Binary in Praesepe Observed by PTF and K2. \apj, 845 (72 - 72. doi:10.3847/1538-4357/aa7e75en_US
dc.description.abstractTheoretical models of stars constitute the fundamental bedrock upon which much of astrophysics is built, but large swaths of model parameter space remain uncalibrated by observations. The best calibrators are eclipsing binaries in clusters, allowing measurement of masses, radii, luminosities, and temperatures for stars of known metallicity and age. We present the discovery and detailed characterization of PTFEB132.707+19.810, a P = 6.0 day eclipsing binary in the Praesepe cluster (τ ∼ 600–800 Myr; [Fe/H] = 0.14 ± 0.04). The system contains two late-type stars (SpTP = M3.5 ± 0.2; SpTS = M4.3 ± 0.7) with precise masses (Mp =  0.3953 0.0020 Me; Ms = 0.2098  0.0014 Me) and radii (Rp =  0.363 0.008 Re; Rs =  0.272 0.012 Re). Neither star meets the predictions of stellar evolutionary models. The primary has the expected radius but is cooler and less luminous, while the secondary has the expected luminosity but is cooler and substantially larger (by 20%). The system is not tidally locked or circularized. Exploiting a fortuitous 4:5 commensurability between Porb and Prot,prim, we demonstrate that fitting errors from the unknown spot configuration only change the inferred radii by 1%–2%. We also analyze subsets of data to test the robustness of radius measurements; the radius sum is more robust to systematic errors and preferable for model comparisons. We also test plausible changes in limb darkening and find corresponding uncertainties of ∼1%. Finally, we validate our pipeline using extant data for GU Boo, finding that our independent results match previous radii to within the mutual uncertainties (2%–3%). We therefore suggest that the substantial discrepancies are astrophysical; since they are larger than those for old field stars, they may be tied to the intermediate age of PTFEB132.707+19.810.en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.rightsFinal published version. This is an open access article.en_US
dc.titleThe Factory and the Beehive. III. PTFEB132.707+19.810, A Low-mass Eclipsing Binary in Praesepe Observed by PTF and K2en_US
dc.typeJournal Articleen_US

Files in This Item:
File Description SizeFormat 
Kraus_2017_ApJ_845_72.pdf2.38 MBAdobe PDFView/Download
apjaa7e75t1_mrt.txt19.15 kBTextView/Download
apjaa7e75t2_mrt.txt98.77 kBTextView/Download
apjaa7e75t4_mrt.txt5.38 kBTextView/Download

Items in OAR@Princeton are protected by copyright, with all rights reserved, unless otherwise indicated.