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CALIFORNIA STATE UNIVERSITY, NORTHRIDGE Dust Temperature Distributions of Herschel Detected Debris Disk a Thesis Submitted in Pa CALIFORNIA STATE UNIVERSITY, NORTHRIDGE Dust Temperature Distributions of Herschel Detected Debris Disk A thesis submitted in partial fulfillment of the requirements For the degree of Master of Science in Physics By Jonathan Acuna May 2019 The thesis of Jonathan Michael Paul Acuna is approved: Dr Ana Cadavid Date Dr Farisa Morales Date Dr Damian Christian, Chair Date California State University, Northridge !ii Acknowledgments Thank you, Mom and Dad, for showing me the value of affordable living. Thank you, TA officemates, for a environment conducive to hard work. Thank you, Python Developers, for all the excellent libraries. Thank you, Department of Veteran Affairs, for funding my education and looking after my health. Thank you, REI, for for providing a small measure of stress relief during the hard times. Thank you, Rob, for being a good friend. Thank you, Farisa, for believing where others did not. Thank you, California State University, for providing everything needed for a Veteran to redefine the future. !iii Dedication To my nephew Anthony Echegoyen, who’s young fascination with science inspired me to work harder. !iv Table of Contents Signature page. ii Acknowledgements . iii Dedication . iv List of Figures . vi List of Tables. vii Abstract. viii Chapter 1: Introduction 1 1.1 Debris Disks. 1 1.2 Debris Disk History. 1 1.3 Instruments . 3 1.3.1 Spitzer/IRS . 4 1.3.2 Spitzer/MIPS. 4 1.3.3 Herschel/PACS. 5 1.3.4 Sky Surveys. 6 1.4 Viability of Black Body Fitting. 7 Chapter 2: Sample Selection 8 2.1 Selection process. 8 2.2 Removal steps. 8 2.3 Final Sample. 9 2.4 Data Origins. 9 Chapter 3: Data Reduction 11 3.1 Pipeline Description. 11 3.2 Pipeline steps. 12 3.2.1 Input . 12 3.2.2 Stitching and Saturation. 13 3.2.3 Fitting. 13 3.2.4 Plotting. 15 3.2.5 Data/Table Storage. 16 3.3 Pipeline Modules. 16 Chapter 4: Results of Fitting 17 4.1 Numerical break-down. 17 4.2 Single Belt Systems. 19 4.3 Double Belt Systems. 24 Chapter 5: Conclusion 28 References. 30 !v List of Figures 1.1 Image of planetary disks forming about the star HL Tau. The gaps between belts are good indicators for planets. Image Credit: ALMA(ESO/NAOJ/NRAO); C. Brogan, B. Saxton (NRAO/AUI/NSF). 2 1.2 Image of Fomalhaut system with known planet shown effecting debris disk. This shows a link between planets and belt structure. Credit: NASA, ESA, and P. Kalas (University of California, Berkeley and SETI Institute). 2 1.3 Image shows the different Bandpasses for the PACS instrument. Each filter has a range of sensitive wavelengths. Credit. PACS observers manual, ESA. 6 3.1 The first input is only the photometric measurements (a). Saturation limits are added (b) and any measurements above the saturation marks are excluded from the fitting. 15 4.1 Histogram showing distribution of debris disks. Number of disks vs temperatures of disks. There is a clear range for belt types. The Belts are overlaid and denoted by color. 17 4.2 Stellar Temperature vs. Spectral Type. There is a linear relation between temperature and spectral type with very low residuals. The double ring systems have a stellar temperature bias, in that they tend to predominantly occur (~94%) around stars at or above ~6000 K or early type stars in our sample. 18 4.3 Stellar Temperature vs. Age for 74 debris systems in our sample for which stellar age is known and for which dust temperatures were retrieved. 19 4.4 SEDs showing the photosphere in cyan, best-fit black body representing a single belt debris ring in red. All instrument measurements are shown by color with the points used for fitting shown in black. If the measurement is above the saturation limit of the instrument (horizontal line) than the measurement was not used to find the optimal temperature for the debris ring. The uncertainties for each measurement are shown as vertical pink lines. 22 4.5 SEDs for double-ring systems showing the photosphere in cyan, best-fit black body representing the inner warmer debris ring in red and the outer colder debris ring in blue. All instrument measurements are shown by color with the points used for fitting shown in black. If the measurement is above the saturation limit of the instrument (horizontal line) than the measurement was not used to find the optimal temperature for the debris ring. The uncertainties for each measurement are shown as vertical gray lines. 26 !vi List of Tables 4.1 This table shows the belt temperatures, star spectral type, star temperature and reduced chi squared values for all single belt systems. 21 4.2 This table shows the belt temperatures for inner and outer rings, star spectral type, star temperature and reduced chi squared values for all double ring systems. 25 !vii Abstract Dust Temperature Distributions of Herschel Detected Debris Disk By Jonathan Michael Paul Acuna Master of Science in Physics Using Herschel/PACS photometry, Spitzer/IRS spectroscopy, and complemented by near- and mid-infrared all-sky photometry from 2MASS and WISE, we develop a python pipeline to analyze the dust emission from a sample of 336 main sequence stars. The infrared data ranges in wavelength between 1.235 and 160 µm, and the sources were selected from the Herschel Heritage Debris Disk (H2D2) program. We model each source’s excess by using a blackbody curve represented by the Plank function. Spectral fitting with my pipeline identified 235 debris disk systems, 54 of which are best modeled using two distinct rings of dust, and the remaining 181 disks appear as single-belt sources. For single-ring systems, the temperatures range from ~28 to ~361 K, with a median value of 108 K. For those systems best fitted with two-belts, the inner rings range in temperature from ~103 to ~351 K, with a median temperature of 337 K. The outer/ cold rings have a median dust temperature of 65 K, and range between ~39 to 145 K. For those debris systems with Spitzer/IRS data, the warm dust components are well- !viii characterized and two-belt fits were common; however, if Spitzer/IRS data is not available, then the Herschel cold/dust detections typically resulted in a single-belt fit. This implies that identifying double belt systems relies heavily on detections between 5.2 and 38 µm. Finally, the temperature ranges found for the two-belt debris system are reminiscent of the temperatures of our own solar system’s asteroid and Kuiper belts, indicative of a common dust temperature horizon around main sequence stars. !ix Chapter 1 Introduction The purpose of this research is to analyze the photometric data of 376 stellar systems. All sources are members of the Herschel Heritage Debris Disk (H2D2) program. This is the first study to systematically analyze a sample of this size, testing for similarities and characteristics of systems with debris disks. The motivation for this type of study is that debris disks are signposts for planetary systems. This type of analysis could lead to a new detection method for planetary systems. 1.1 Debris Disks Circumstellar debris disks were first discovered in the 1980s by the Infrared Astronomical Satellite (IRAS). These disks are likely formed around Mature stars and can have their boundaries defined by shepherding planets. There is a disproportionate lifespan however between the dust in a debris disk and the parent star. The debris disks last only as long as there is a source feeding dust into them. Because of this the disks must have some type of replenishing mechanism, either from comets or asteroids. The disks can be used as indicators to identify properties of their parent systems. The disk architecture specifically has a lot of value when trying to understand a host system, like our own which has planet types separated by disks. 1.2 Debris Disk History It is thought that there is a link between the debris disk distributions and locations of nearby orbiting bodies. The prevailing theory is that the disks are composed of solid water and astro-sil particulates and maintain temperatures based on the amount of stellar !1 radiation they receive from their parent stars and the distance of the disks. These disks maintain an equilibrium temperature because the dust emits radiation at levels proportional to the ambient flux they absorb. Like all orbiting bodies the particulates in the debris disks orbit their parent stars in ellipses and can range in Figure 1.1. Image of planetary disks forming about the star HL Tau. The gaps between belts cross sectional radii by as much as a few are good indicators for planets. Image Credit: ALMA(ESO/NAOJ/NRAO); C. Brogan, B. astronomical units, see figure 1.1. The Saxton (NRAO/AUI/NSF) eccentricity of the disks could also be an indicator for the eccentricity of any nearby planets. Fomalhaut (figure 1.2) has a debris disk system with an observed orbiting body. Since their initial discovery, hundreds of debris disk rings have been confirmed. Initial work done with debris disks focused on stars with infrared excess, trying to relate belt properties to planetary system evolution phases. This early star work was done with a sample of nearby A type stars observed by the Spitzer/MIPS, first at 24 Figure 1.2. Image of Fomalhaut system with µm (Rieke et al. 2005) and later at 70 µm known planet shown effecting debris disk. This shows a link between planets and belt (Su et al. 2006). The early work showed structure.
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