Pauline Arriaga

Total Page：16

File Type：pdf, Size：1020Kb

Pauline Arriaga University of California - Los Angeles [email protected] Physics and Astronomy www.astro.ucla.edu/∼parriaga 475 Portola Plaza Phone: 619-851-7961 Los Angeles, CA 90095 OCRID: 0000-0001-6364-2834 Education University of California - Los Angeles Ph.D., Astrophysics, expected 2020 C. Phil. Astrophysics, 2018 M.A., Astrophysics, 2018 University of California - Berkeley B.A., Astronomy, Physics and Russian Literature, 2010 Research OSIRIS Imager I have worked on various aspects of the OSIRIS imager, primarily on the design of the Projects pupil masks and the H2-RG detector. I have extensively tested and helped update the control software for the detector. Debris Disk Modelling using Gemini Planet Imager Using primarily polarization data I have done extractions of geometry and phase curves of the HR4796A and HD32297 disks. I have further done dust modelling on the extracted phase curves. Python Karhunen-Loeve Image Processing I have contributed code to the public PyKLIP code base that allows for the forward modelling of disks. Upgrade of the 24-in UCLA Telescope and Solar Telescope I have recoded the control software in Java for a solar telescope to work with Galil motor controllers. I have additionally installed these motor controllers on both telescopes. I have also designed and fabricated parts for this installation. Analysis of the Eta Corvi disk using Herschel and Spitzer Using Herschel and Spitzer data I have done geometric and SED modelling of the Eta Corvi debris disk. Machine-Learned ASAS Classiﬁcation Catalogue Using semi-supervised machine-learned clustering algorithms and anomaly detection, I analyzed variable star phase curves. Languages English (native), Spanish (advanced), Russian (intermediate) and Skills IDL, Python, LATEX, C, Java, UNIX shell scripting Teaching University of California - Berkeley Course Instructor and Designer, IDL for astronomers, 2011-2012 Course Instructor and Designer, Python for astronomers, 2013-2014 Lab Assistant, Upper Division Optical Astronomy Lab, 2012 Lab Assistant, Introduction to Astronomy, 2013-2014 Teaching Assistant, Introduction to Astronomy, 2013-2014 Grader, Upper Division Classical Mechanics, 2013 Grader, Introduction to Astronomy, 2011-2012 University of California - Los Angeles Teaching Assistant, Upper Division Optical Astronomy Lab, 2014, 2015 Teaching Assistant, Upper Division Statistical Mechanics, 2015 Teaching Assistant, Upper Division Radiation and Fluid Mechanics, 2015 Teaching Assistant, Introduction to Astronomy - Life in the Universe, 2015 Major Full list of publications at https://orcid.org/0000-0001-6364-2834 Publications Awards and Teaching Assistant of the Year Fellowships UCLA Astronomy, 2014 Gluck Outreach Program Fellowship 2016, 2017.

Copy Link

Recommended publications

Linking Stars, Planets and Debris Through Herschel Observations of Radial Velocity Exoplanet Host Stars
Linking stars, planets and debris through Herschel observations of radial velocity exoplanet host stars Jonathan P. Marshall Universidad Autónoma de Madrid Introduction • Herschel observed 104 radial velocity exoplanet host stars, of which 30 also had detectable circumstellar discs (DEBRIS, DUNES, GT and SKARPS) • Given that we expect planets to form from the agglomeration of planetesimals, there should be some link between the two • Previous work with Spitzer identified no correlation between planets and debris (Moro-martin et al. 2007, Bryden et al. 2009) • Observational signatures of planets may be visible in the spatial distribution of dust discs around other stars Imaging exoplanets • We find exoplanets in systems with debris discs (Marois et al. 2008; Bonnefoy et al. 2011; Rameau et al. 2013) Multi-component discs • HIP 17439’s debris disc is potentially the result of two cold dust belts Ertel et al. 2014 Schueppler et al., subm. Dynamical interactions • e.g. Eta Corvi’s Spitzer IRS spectrum shows evidence for KBO material in inner system Matthews et al. 2010 Lisse et al. 2012 Perturbation • Stars hosting exoplanets with low orbital eccentricities show a weak tendency to have brighter discs • Planets with lower eorb are less disruptive to parent bodies in debris belts Maldonado et al. 2012 Eccentric discs • e.g. HIP 15371 • Asymmetric structure proposed to be the result of dynamical perturbation by a planetary companion . Similar evidence seen in other discs (in sub-mm) tends to be weak, potentially result of low s/n observation . Not necessarily a planet, as remnant gas could affect dust Faramaz et al. 2014 Coplanarity • Inclination of star, i*, and disc, id • Debris discs are generally seen to lie along the equatorial plane of the host star • Few exceptions, e.g.
[Show full text]
Telescope to Seek Dust Where Other Earths May Lie 22 January 2015, by Whitney Clavin
Telescope to seek dust where other Earths may lie 22 January 2015, by Whitney Clavin The new instrument, based at the Large Binocular Telescope Observatory at the top of Mount Graham in southeastern Arizona, will obtain the best infrared images yet of dust permeating a star's habitable zone, the region around the star where water—an essential ingredient for life as we know it—could pool on a planet. Earth sits comfortably within our sun's habitable zone, hence its glistening surface of oceans. Scientists want to take pictures of exo-Earths and break up their light into a rainbow of colors. This color information is displayed in plots, called The Large Binocular Telescope Interferometer (LBTI) spectra, which reveal chemical clues about whether instrument set its eyes on a dusty star system called Eta a planet could sustain life. But dust—which comes Corvi, depicted here in this artist's concept. Recent from colliding asteroids and evaporating collisions between comets and rocky bodies within the comets—can outshine the feeble light of a planet, star system are thought to have generated the surplus of making this task difficult. dust. Credit: Large Binocular Telescope Observatory "Imagine trying to view a firefly buzzing around a lighthouse in Canada from Los Angeles," said Denis Defrère of the University of Arizona, lead The NASA-funded Large Binocular Telescope author of the new study that appears in the Jan. 14 Interferometer, or LBTI, has completed its first issue of the Astrophysical Journal. "Now imagine study of dust in the "habitable zone" around a star, that fog is in the way.
[Show full text]
Debris Disks: the First 30 Years Where Will Herschel Take Us?
With thanks to M. Wyatt, P. Kalas, L. Churcher, G. Duchene, B. Sibthorpe, A. Roberge Debris Disks: the first 30 years Where will Herschel take us? Brenda Matthews Herzberg Institute of Astrophysics & University of Victoria Outline • Debris disk: definition and discovery • Incidence and evolution • Characterizing debris disks • Disks around low-mass stars (AU Mic) • Planetary connection • Herschel surveys “Debris” Disks • Debris disks are produced from the remnants of the planet formation process • Second generation dust is produced through collisional processes • The debris disk can include – Planetesimal population (though not directly observable) – Dust produced (detectable from optical centimetre) • Dust may lie in belts at various radii from the star Solar System Debris Disk Kuiper Belt Asteroid Belt Debris Disk Snapshot: Zodiacal Light Photo: Stefan Binnewies "The light at its brightest was considerably fainter than the brighter" portions of the milky way... The outline generally appeared of a " parabolic or probably elliptical form, and it would seem excentric" as regards the sun, and also inclined, though but slightly to the ecliptic."" "-- Captain Jacob 1859 Discovery: Vega Phenomenon IRAS ﬁnds excess around 20% of main sequence stars (Rhee et al. 2007) Backman & Paresce 1993" "The Big Three"" The discovery of excess emission from main sequence stars at IRAS wavelengths (Aumann et al. 1984). Circumstellar Dust Disks Smith & Terrile 1984 Beta Pic was the Rosetta Stone Debris Disk for 15 years >300 refereed papers Dust must be second generation •! Debris disks cannot be the remnants of the protoplanetary disks found around pre-main sequence stars (Backman & Paresce 1993): –! The stars are old (e.g., up to 100s of Myr, even Gyr) –! The dust is small (< 100 micron) (Harper et al.
[Show full text]
Disks in Nearby Planetary Systems with JWST and ALMA
Disks in Nearby Planetary Systems with JWST and ALMA Meredith A. MacGregor NSF Postdoctoral Fellow Carnegie Department of Terrestrial Magnetism 233rd AAS Meeting ExoPAG 19 January 6, 2019 MacGregor Circumstellar Disk Evolution molecular cloud 0 Myr main sequence star + planets (?) + debris disk (?) Star Formation > 10 Myr pre-main sequence star + protoplanetary disk Planet Formation 1-10 Myr MacGregor Debris Disks: Observables First extrasolar debris disk detected as “excess” infrared emission by IRAS (Aumann et al. 1984) SPHERE/VLT Herschel ALMA VLA Boccaletti et al (2015), Matthews et al. (2015), MacGregor et al. (2013), MacGregor et al. (2016a) Now, resolved at wavelengthsfrom from Herschel optical DUNES (scattered light) to millimeter and radio (thermal emission) MacGregor Planet-Disk Interactions Planets orbiting a star can gravitationally perturb an outer debris disk Expect to see a variety of structures: warps, clumps, eccentricities, central offsets, sharp edges, etc. Goal: Probe for wide separation planets using debris disk structure HD 15115 β Pictoris Kuiper Belt Asymmetry Warp Resonance Kalas et al. (2007) Lagrange et al. (2010) Jewitt et al. (2009) MacGregor Debris Disks Before ALMA Epsilon Eridani HD 95086 Tau Ceti Beta PictorisHR 4796A HD 107146 AU Mic Greaves+ (2014) Su+ (2015) Lawler+ (2014) Vandenbussche+ (2010) Koerner+ (1998) Hughes+ (2011) Matthews+ (2015) 49 Ceti HD 181327 HD 21997 Fomalhaut HD 10647 (q1 Eri) Eta Corvi HR 8799 Roberge+ (2013) Lebreton+ (2012) Moor+ (2015) Acke+ (2012) Liseau+ (2010) Lebreton+ (2016)
[Show full text]
Week 5: January 26-February 1, 2020
5# Ice & Stone 2020 Week 5: January 26-February 1, 2020 Presented by The Earthrise Institute About Ice And Stone 2020 It is my pleasure to welcome all educators, students, topics include: main-belt asteroids, near-Earth asteroids, and anybody else who might be interested, to Ice and “Great Comets,” spacecraft visits (both past and Stone 2020. This is an educational package I have put future), meteorites, and “small bodies” in popular together to cover the so-called “small bodies” of the literature and music. solar system, which in general means asteroids and comets, although this also includes the small moons of Throughout 2020 there will be various comets that are the various planets as well as meteors, meteorites, and visible in our skies and various asteroids passing by Earth interplanetary dust. Although these objects may be -- some of which are already known, some of which “small” compared to the planets of our solar system, will be discovered “in the act” -- and there will also be they are nevertheless of high interest and importance various asteroids of the main asteroid belt that are visible for several reasons, including: as well as “occultations” of stars by various asteroids visible from certain locations on Earth’s surface. Ice a) they are believed to be the “leftovers” from the and Stone 2020 will make note of these occasions and formation of the solar system, so studying them provides appearances as they take place. The “Comet Resource valuable insights into our origins, including Earth and of Center” at the Earthrise web site contains information life on Earth, including ourselves; about the brighter comets that are visible in the sky at any given time and, for those who are interested, I will b) we have learned that this process isn’t over yet, and also occasionally share information about the goings-on that there are still objects out there that can impact in my life as I observe these comets.
[Show full text]
Extrasolar Systems Shed Light on Our
NEWS FEATURE NEWS FEATURE Extrasolar systems shed light on our own Amazing as the discoveries of planets, comets, and asteroid belts around other stars are, it’s their potential to shed light on our Solar System’s origins that is exciting astronomers. Nadia Drake broader sense, we’re trying to understand Science Writer if our own world—and our own Solar Sys- tem—is ‘normal,’” says David Grinspoon, Chair of Astrobiology at the US Library of A planet smaller than Mercury circles a star astronomers can use the Solar System’s ar- Congress in Washington, DC, “or, in some 210 light-years away. Around another star, chitecture to predict the presence of un- extraordinary way, abnormal.” two planets live so close together that each seen objects in these systems, and use the periodically rises in the other’s sky. Other systems to learn more about the celestial Chasing Comets alien skies are home to two suns that rise events that gave birth to and shaped our One stellar system with a recently identified and set, casting double shadows over their Solar System. kinship to ours is that of Vega. This famil- double-sunned worlds. Planets so dense “We definitely learn more about the Solar iar star burns brightly in the northern sky, they might have diamond rinds, worlds System’s past and future by observing other where it forms a summertime triangle with whose year is shorter than an Earthday, oth- stellar systems,” says astronomer Kate Su stars Deneb and Altair. Just 25 light-years ers that orbit their star backward—the cos- of the University of Arizona, Tucson, AZ.
[Show full text]
Late Heavy Bombardment
Late Heavy Bombardment The Late Heavy Bombardment (abbreviated LHB and also known as the lunar cataclysm) is an event thought to have occurred approximately 4.1 to 3.8 billion years (Ga) ago,[1] at a time corresponding to the Neohadean and Eoarchean eras on Earth. During this interval, a disproportionately large number of asteroids are theorized to have collided with the early terrestrial planets in the inner Solar System, including Mercury, Venus, Earth, and Mars.[2] The Late Heavy Bombardment happened after the Earth and other rocky planets had formed and accreted most of their mass, but still quite early in Earth's history. Evidence for the LHB derives from lunar samples brought back by the Apollo astronauts. Isotopic dating of Moon rocks implies that most impact melts occurred in a rather narrow interval of time. Several hypotheses attempt to explain the apparent spike in the flux of impactors (i.e. asteroids and comets) in the inner Solar System, but no consensus yet exists. The Nice model, popular among planetary scientists, postulates that the giant planets underwent orbital Artist's impression of the Moon during the Late Heavy Bombardment (above) migration and in doing so, scattered objects in the asteroid and/or Kuiper belts and today (below). into eccentric orbits, and into the path of the terrestrial planets. Other researchers argue that the lunar sample data do not require a ataclysmicc cratering event near 3.9 Ga, and that the apparent clustering of impact-melt ages near this time is an artifact of sampling materials retrieved
[Show full text]
Astronomy Magazine 2020 Index
Astronomy Magazine 2020 Index SUBJECT A AAVSO (American Association of Variable Star Observers), Spectroscopic Database (AVSpec), 2:15 Abell 21 (Medusa Nebula), 2:56, 59 Abell 85 (galaxy), 4:11 Abell 2384 (galaxy cluster), 9:12 Abell 3574 (galaxy cluster), 6:73 active galactic nuclei (AGNs). See black holes Aerojet Rocketdyne, 9:7 airglow, 6:73 al-Amal spaceprobe, 11:9 Aldebaran (Alpha Tauri) (star), binocular observation of, 1:62 Alnasl (Gamma Sagittarii) (optical double star), 8:68 Alpha Canum Venaticorum (Cor Caroli) (star), 4:66 Alpha Centauri A (star), 7:34–35 Alpha Centauri B (star), 7:34–35 Alpha Centauri (star system), 7:34 Alpha Orionis. See Betelgeuse (Alpha Orionis) Alpha Scorpii (Antares) (star), 7:68, 10:11 Alpha Tauri (Aldebaran) (star), binocular observation of, 1:62 amateur astronomy AAVSO Spectroscopic Database (AVSpec), 2:15 beginner’s guides, 3:66, 12:58 brown dwarfs discovered by citizen scientists, 12:13 discovery and observation of exoplanets, 6:54–57 mindful observation, 11:14 Planetary Society awards, 5:13 satellite tracking, 2:62 women in astronomy clubs, 8:66, 9:64 Amateur Telescope Makers of Boston (ATMoB), 8:66 American Association of Variable Star Observers (AAVSO), Spectroscopic Database (AVSpec), 2:15 Andromeda Galaxy (M31) binocular observations of, 12:60 consumption of dwarf galaxies, 2:11 images of, 3:72, 6:31 satellite galaxies, 11:62 Antares (Alpha Scorpii) (star), 7:68, 10:11 Antennae galaxies (NGC 4038 and NGC 4039), 3:28 Apollo missions commemorative postage stamps, 11:54–55 extravehicular activity
[Show full text]
Ralph L. Mcnutt, Jr
Ralph L. McNutt, Jr. The John Hopkins University Applied Physics Laboratory, USA ISSI – BJ Forum: Session 1 Introduction and Exploration of Outer Overview Heliosphere and Interstellar 9:40 AM – 10:10 AM Medium - Beijing, China Thursday 7 November 2019 Introduction and Agenda • Context: The Current Effort • History: What Interstellar Probe Is • Science: The Compelling Case - Science Goal 1: Understand our Heliosphere as a Habitable Astrosphere - Science Goal 2: Understand Formation and Evolution of Planetary Systems - Science Goal 3: Uncover Early Galaxy and Star Formation • An Example Science Traceability Matrix • Example Instruments and Example Payload(s) • Where Could We Go: Target Map • Constraints and Trade-Offs • Mission Architecture Options and Engineering Requirements • “Deeper Dive” Tasks – Engineering Ramp Up • Final Thoughts 7 November 2019 ISSI-BJ Forum on EXPLORATION OF OUTER HELIOSPHERE AND NEARBY INTERSTELLAR MEDIUM 2 Study Team and Collaborators • R. L. McNutt, Jr (Study Principal Investigator) • P. C . B r a ndt (Study Project Scientist) • K. E. Mandt (Deputy Study Project Scientist) • M. V. Paul (Study Manager) • E. Provornikova (Working Group Lead – Heliosphere/Local Interstellar Medium) • C. Lisse (Working Group Lead – Circum-Solar Debris Disk/Astrophysics) • K. Runyon (Working Group Lead – Kuiper Belt Objects/Planetary) • A. Rymer (Working Group Lead - Exoplanetary Connections) And almost 200 professional scientists and engineers world-wide actively working in support for Interstellar Exploration 7 November 2019 ISSI-BJ
[Show full text]
Debris Disks with ALMA
Debris Disks with ALMA Jane Greaves University of St Andrews, Scotland (Scottish Universities Physics Alliance) origins of debris • debris is generated by collisions of comets or asteroids… – traces planetesimal belts > signpost to systems where planet formation got started – perturbations of dust disks indicate where distant giant planets are located – seen around main-sequence stars of any age Leinhardt & Richardson Bryden et al. 2006 submm imaging • optically thin dust in thermal equilibrium with the star – so for dust rings at tens of AU, far-infrared to submillimetre greybody emission • traces mass of debris: infer mass of comets • spectral slope > properties of grains – imaging shows scale of planetary system eta Corvi: Wyatt et al. 2005 submm 'rogues gallery' diversity • unexpectedly, great variety among disks – wide range of disk sizes: radii ~50 to 300 AU • Solar System's Kuiper Belt is at the small end – majority perturbed • requiring planets out to ~100 AU • explained by outwards migration via angular momentum exchange with planetesimal belt • no 'predictor' of whether a particular star will have debris – unclear whether seeing debris 'events' … or stars with steady state debris from very large numbers of comets > great diversity of planetary systems planetary interpretations • dust trapped in resonanances > clumps – map pointing to planet location Vega: Wyatt et al. 2003; Holland et al. 1998, 2003 wavelength dependence • balance of radiation pressure and gravity means dust of different sizes trapped differently – small particles feel more radiation force: so short- wavelength data show more blow-out • submm is ideal for imaging perturbations… brighter than millimetre, sensitive to large-ish well-trapped dust Wyatt 2005 • much better than optical scattering, which is sensitive to very small grains • e.g.
[Show full text]
Scottish Universities Physics Alliance Peer Reviewed Publications
Scottish Universities Physics Alliance Peer Reviewed Publications 2005 It was agreed by the Executive Committee of SUPA that a document should be produced each year listing articles published by SUPA staff in the previous calendar year. This is our first iteration and is intended to be used as a record in future discussions about SUPA. In order to produce this document, each university was asked to provide a list of academic staff in post in 2005, including anyone who took up a post part way through the year and any who may have left during 2005. Information was gathered from the Web of Science and staff were given the opportunity to check this information for accuracy. They were also invited to write a short paragraph on their current work to be included in the document. Anna Clements at the University of St Andrews has collected similar data and has provided short paragraphs on current research for some of the staff at St Andrews. In order to limit the number of publications appearing several times, any collaboration publications are listed under the collaboration title (at the end of the document) with a reference to the collaboration under the author’s entry. Before we start on the document for 2006, we need to revisit the process used this year. The document for 2005 was produced with time constraints and limited staff, issues that will not affect the 2006 document. There was a misjudgement made in the data presented in that the name of the author was removed from the list of co-authors, leaving the references incomplete.
[Show full text]
Qt6t24x5h2.Pdf
Lawrence Berkeley National Laboratory Recent Work Title Science Impacts of the SPHEREx All-Sky Optical to Near-Infrared Spectral Survey: Report of a Community Workshop Examining Extragalactic, Galactic, Stellar and Planetary Science Permalink https://escholarship.org/uc/item/6t24x5h2 Authors Doré, Olivier Werner, Michael W Ashby, Matt et al. Publication Date 2016-06-22 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Science Impacts of the SPHEREx All-Sky Optical to Near-Infrared Spectral Survey: Report of a Community Workshop Examining Extragalactic, Galactic, Stellar and Planetary Science Olivier Doré1;21, Michael W. Werner1;21, Matt Ashby26, Pancha Banerjee23, Nick Battaglia16, James Bauer1, Robert A. Benjamin34, Lindsey E. Bleem36;37, Jamie Bock21, Adwin Boogert2, Philip Bull1;21, Peter Capak8, Tzu-Ching Chang3, Jean Chiar38, Seth H. Cohen30, Asantha Cooray28, Brendan Crill1;21, Michael Cushing4, Roland de Putter21, Simon P. Driver32, Tim Eifler21, Chang Feng28, Simone Ferraro19, Douglas Finkbeiner31, B. Scott Gaudi18, Tom Greene5, Lynne Hillenbrand21, Peter A. Höflich6, Eric Hsiao6, Kevin Huffenberger6, Rolf A. Jansen30, Woong-Seob Jeong7, Bhavin Joshi30, Duho Kim30, Minjin Kim7, J.Davy Kirkpatrick8, Phil Korngut21, Elisabeth Krause9, Mariska Kriek25, Boris Leistedt10, Aigen Li40, Carey M. Lisse11, Phil Mauskopf30, Matt Mechtley30, Gary Melnick26, Joseph Mohr35;41, Jeremiah Murphy6, Abraham Neben13, David Neufeld24, Hien Nguyen1;21, Elena Pierpaoli23, Jeonghyun Pyo7, Jason Rhodes1;21,
[Show full text]