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Infrared Excesses in stars with and without planets by Ra´ulFelipe Maldonado S´anchez Thesis submitted in partial fulfillment of the requirements for the degree of MASTER OF SCIENCE IN ASTROPHYSICS at the Instituto Nacional de Astrof´ısica, Optica´ y Electr´onica August 2015 Tonantzintla, Puebla Under the supervision of: Ph.D. Miguel Ch´avez Dagostino (INAOE) Ph.D. Emanuele Bertone (INAOE) c INAOE, 2015 The author hereby grants to INAOE permission to reproduce and to distribute publicly paper and electronic copies of this thesis document in whole or in part. To my family and friends iii Acknowledgments I would like to offer my special thanks to my advisors Ph.D. Miguel Ch´avez Dagostino and Ph.D. Emanuele Bertone for all their support, advice and patience since the be- ginning of the project until the successful conclusion of this work, for helping me to improve this thesis and sharing me the necessary knowledge to do this research work. My special thanks are extended to Ph.D. Olga Vega, Ph.D. Alicia Porras and Ph.D. Abraham Luna for being examiners of this thesis and giving me the advices and com- ments to improve this research work. I am particularly grateful with all my classmates and friends: Eric, Carlos, Leticia, Emanuel, Ana, Gisela and Alan. They have shown me the meaning of a true friendship. The let me know that the study and learning in a perfect work team is easier and much funnier. I hope we still be friends for a long time and even collaborate in future projects. I would like to express my very great appreciation to my colleague and friend Rodrigo Pineda, for his friendship and all his support through the master studies and during the development of this thesis, for encouraging me to continue in difficult times and showing me the importance of the study everyday. I also want to thank Msc. Fernando Cruz S´aenzde Miera for his help in the develop- ment of this work. I give my special thanks to my mom, sisters, brothers in law, nephews and nice, who are showing me their care and love everyday. The accomplishment of all my goals is because of their emotional support. I really appreciate the knowledge acquired from all the teachers in the master, for their teachings in the classroom. Finally, I thank CONACYT for the financial support in the master studies. v List of Figures 1.1 Spectral energy distributions of Vega, Fomalhaut, Eridani and β Pictoris.2 1.2 Diagram of the evolution of a typical circumstellar disk..........3 1.3 Spectral Energy Distribution of the Herbig Ae star AB Aurigae.....4 1.4 Two parameter debris disk model......................6 1.5 Spectral Energy Distributions of stars with prominent 22 µm excesses..9 1.6 Evolution of 24 µm excesses around Sun-like stars............ 11 1.7 β Pictoris coronagraphic images....................... 13 1.8 Dust emission around Eridani at a wavelength of 850 µm........ 13 2.1 WISE satellite in its mapping configuration................ 16 2.2 Fit photometry profile differences between AllWISE and WISE All-Sky 17 2.3 Comparison of a real and spurious detection in WISE images...... 22 2.4 Spectral type distributions of stars with and without planets....... 23 2.5 Distance distribution of stars with and without planets......... 24 2.6 V magnitude distributions of stars with and without planets...... 24 2.7 Metallicity distributions of stars with and without planets....... 25 3.1 Color vs spectral type of stars with and without planets samples.... 28 3.2 Color excess distribution of the stars with and without planets sample. 29 3.3 Comparison between ATLAS9 and NEXTGEN synthetic spectra.... 33 3.4 Comparison of synthetic spectra with same Teff , surface gravity but different metallicity.............................. 35 3.5 Johnson, 2MASS and WISE filter response curves............ 36 3.6 Best fit of the Synthetic Spectral Energy Distribution for the star HD108874 using ATLAS9 models........................... 37 2 3.7 χν distribution for the stars with and without planets.......... 37 3.8 WISE vs Tycho-2 B-V color-diagrams................... 41 4.1 Distribution of uncertainties in the flux ratio W4/W3 in dependence of W4 flux.................................... 47 4.2 Distribution of total uncertainties propagated in the different IR-detection methods.................................... 48 4.3 Excess significance distribution of stars with and without planets.... 49 vii 4.4 Comparison between W4 and W3 observed and synthetic photometry as a function of W4 flux for each star in the combined samples of stars with and without planets.......................... 50 4.5 Comparison between W4, W3 and W2 observed and synthetic photom- etry in dependence of W4 flux for each star in the combined samples of stars with and without planets....................... 51 4.6 Flux comparison of the WISE bands between the WISE catalogues avail- able in the literature............................. 53 4.7 Spectral energy distribution of HD 106906................. 55 4.8 Spectral energy distribution of V342Peg (HR 8799)............ 56 4.9 Spectral energy distribution of BD-10 3166................ 57 4.10 Spectral energy distribution of CD-301812................. 58 4.11 WISE W4 pixel intensity distribution of CD-301812........... 58 4.12 WISE W2, W3 and W4 images of CD-301812............... 59 4.13 Spectral energy distribution of HD107146................. 60 4.14 Spectral energy distribution of HD85301.................. 61 4.15 Spectral energy distribution of HD 136544................. 62 A.1 Empirically determined WISE vs. B-V photospheric color-color trends for all six WISE colors............................ 69 B.1 Spectral energy distributions of HD106906 & HR7899.......... 71 B.2 Spectral energy distributions of HD45184 & HD113337.......... 72 B.3 Spectral energy distributions of HD114729A & HR6907.......... 72 B.4 Spectral energy distributions of HD11506 & HD224693.......... 72 B.5 Spectral energy distributions of HD130322 & HD98649.......... 73 B.6 Spectral energy distributions of HD168443 & HD33643.......... 73 B.7 Spectral energy distribution of HD4113.................. 73 B.8 Spectral energy distributions of HD107146 & HD85301......... 74 B.9 Spectral energy distributions of HD60491 & HD125040.......... 74 B.10 Spectral energy distributions of AFLep & HD136544........... 75 B.11 Spectral energy distributions of HD29137 & HD34745.......... 75 B.12 Spectral energy distributions of HD8907 & LQHya............ 75 B.13 Spectral energy distributions of HD96418 & HR1981........... 76 B.14 Spectral energy distributions of HD205294 & HD44821.......... 76 B.15 Spectral energy distributions of HD85638 & HD209253.......... 76 List of Tables 3.1 Zero magnitude flux density for B, V, J, H, KS, W1, W2, W3, W4 bands. 30 3.2 Extinction law coefficients as a function of wavelength.......... 30 3.3 Color corrections............................... 32 3.4 Flux ratio comparison among the WISE bands in ATLAS9 synthetic spectra with different stellar parameters.................. 34 4.1 Number and percentage of IR excesses (E) in stars with and without planets.................................... 43 C.1 Stellar parameters of the sample of stars with planets........... 77 C.2 Stellar parameters of the sample of stars without planets......... 81 D.1 Observed fluxes for stars with planets................... 100 D.2 Observed fluxes for stars without planets.................. 106 ix Contents Acknowledgmentsv 1 Introduction1 1.1 Circumstellar Disks.............................1 1.1.1 Protoplanetary Disks........................4 1.1.2 Debris Disks.............................5 1.2 Observing Debris Disks at IR wavelengths................7 1.3 Mid-IR observations: Warm debris disks.................8 1.4 Planet interaction and disks........................ 12 1.5 Aims of this work.............................. 14 2 The sample selection 15 2.1 IR Surveys.................................. 15 2.1.1 Wide-field Infrared Survey Explorer (WISE)........... 15 2.1.2 Two Micron All Sky Survey (2MASS)............... 18 2.2 The sample................................. 19 2.2.1 Stars with planets.......................... 19 2.2.2 Stars without planets........................ 20 2.3 Optical and Infrared photometry..................... 21 2.3.1 Comparison of both samples.................... 22 3 Methodology 27 3.1 Correction for extinction and magnitude to flux conversion....... 27 3.2 Photosphere fitting and synthetic photometry.............. 32 3.3 Searching for Infrared Excesses....................... 38 3.3.1 Method 1 (This work)....................... 38 3.3.2 Method 2: Cruz-Saenz de Miera et al.(2014)........... 39 3.3.3 Method 3: Kennedy & Wyatt(2012)............... 39 3.3.4 Method 4: Morales et al.(2012).................. 40 3.3.5 Method 5: Patel et al.(2014)................... 40 4 Results 43 4.1 Comparing the two stellar samples.................... 44 xi 4.2 Comparison among the methods...................... 45 4.2.1 This work vs. Cruz-Saenz de Miera et al.(2014)......... 45 4.2.2 Kennedy & Wyatt(2012) vs. Morales et al.(2012)....... 45 4.2.3 Patel et al.(2014) vs. Morales et al.(2012)............ 46 4.3 Explaining differences among the methods................ 46 4.3.1 So, which is the best method?................... 51 4.4 Comparison between WISE data releases................. 52 4.5 Comments on some stars with planets................... 54 4.5.1 HD106906.............................. 54 4.5.2 V342Peg (HR 8799)........................ 55 4.5.3 BD-10 3166............................. 56 4.5.4 CD-301812 (WASP-79)....................... 57 4.6 Comments
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