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Science Briefing March 5, 2020

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Science Briefing March 5, 2020 Science Briefing March 5, 2020 Dr. Gabriela Gonzalez (Louisiana State Univ.) Women in Astronomy: Dr. Elizabeth Hays (GSFC) The Past Inspires the Future Dr. Farisa Morales (JPL) Facilitator: Dr. Quyen N. Hart (STScI) Outline of this Science Briefing 1. Dr. Gabriela Gonzalez (LIGO, Louisiana State University) Music of the Universe: Einstein’s gravitational waves 2. Dr. Elizabeth Hays (Goddard Space Flight Center) Gamma-ray Pulsars, Lighthouses in the Galaxy 3. Dr. Farisa Morales (NASA Jet Propulsion Laboratory) Formation of Planetary Systems 4. Q&A 5. Dr. Quyen Hart (Space Telescope Science Institute) [title] 6. Q&A 2 Music of the Universe: Einstein’s gravitational waves Gabriela González Louisiana State University Galina Sorokina [Image Credit: Henze/NASA] 3 Gravitational waves: a long history • Predicted by Einstein in 1916: “ripples in space time” • First observation announced in 2016 (100 years later!) • Signal “heard” by two LIGO observatories, from the dance and merger of two black holes. Phys. Rev. Lett. 116, 061102 (2016) 4 Interferometers to measure space(-time) • LIGO = Laser Interferometer Gravitational-wave Observatory Strain detected: 1 part in 1021 Interferometer is 4km long. Change in distance measured: 4/1000 of a proton diameter! Credit: Johan Jarnestad/ The Royal Swedish Academy of Sciences 5 LIGO detectors are not alone 6 More discoveries 2015 - 2017 Ten black hole mergers and… … a neutron star merger with fireworks that followed! NSF / LIGO / Sonoma State University / A. Simonnet7 More (public) music notes in 2019-20 gracedb.ligo.org Phone apps! 8 The next few years 9 And more instruments for different notes 10 The past inspires the future Einstein, 1904 Thorne, ca. 1970Weiss, ca. 1970 Gonzalez, Saulson, 1995 Choquet-BruhatDeWitt, -Morette, 1974 ca.1955 Weiss, Cordova, Reitze, Gonzalez, Thorne, 2016 11 More resources • Information : www.ligo.org (at many different levels, with links to documentaries, articles, books, activities, multimedia, student/teacher activities, LIGO magazine, ... )’ resourc es,…).ligo.org w.ligo.org • Images/Movies: https://www.ligo.caltech.edu/gallery • 1-hr public talk: https://insidetheperimeter.ca/music-of- the-universe-gabriela-gonzalez-public-lecture-webcast/ • Many TED, TEDx talks (search for LIGO TED) 12 Gamma-ray Pulsars, Lighthouses in the Galaxy Liz Hays Credit: NASA/Fermi/Cruz de Wilde Goddard Space Flight Center 13 What is a pulsar? • Pulsars pulse. Regularly repeating radio signals were co-discovered by Jocelyn Bell Burnell in 1967. • A pulsar is a rotating neutron star with a very strong magnetic field. • A star stops burning fuel and collapses into extremely dense, rapidly spinning ball of neutrons. • Small! Size of a large city, ~12 miles across. • Fast! A few times a second up to a few hundred times a second. • 1000s of pulsars have been found in our Galaxy using radio telescopes. 14 Pulsars are gamma-ray power houses The first seven gamma-ray pulsars and their pulse shapes at different wavelengths 15 Fermi maps the entire sky in gamma rays Credit: Fermi/LAT 16 Fermi has found more than 250 gamma-ray pulsars Credit: Fermi/LAT 17 Models predict gamma-ray emission from pulsars Alice Harding, NASA Goddard Space Flight Center • Scientists at NASA use supercomputers to trace the paths of particles caught in a pulsar’s electric and magnetic fields. Their fate in these models helps explain the observed gamma-ray emission. 18 Gamma rays reveal a different lighthouse The Fermi pulsars have changed the simple picture of a pulsar dramatically. gamma ray The gamma rays can come from a different part of the pulsars magnetic field and make a broad lighthouse beam. radio 19 Gamma-ray lighthouses in the sky Pulsars appear prominently in the informal gamma-ray constellations. The brightest steady source in the Fermi sky, the Vela pulsar, marks the beacon of Pharos, the lighthouse of Alexandria. The black widow spider represents a pulsar that is destroying a small companion star with its radiation. The radio telescope dish symbolizes close partnerships between gamma-ray and radio astronomy. Credit: NASA 20 Formation of Planetary Systems Farisa Y. Morales, PhD Exoplanet Observations Debris Disk Observations 21 Proto-planetary disks Planet perturbations of planetesimals Stars Form with Proto- Planet Perturbations Induce Formation of Rubble Bands Planetary Disks building Dust Production Planetesimals http://www.spitzer.caltech.edu/video- http://www.spitzer.caltech.edu/video- http://www.spitzer.caltech.edu/video- audio/730-ssc2004-22v2-The-Evolution-of-a- audio/749-ssc2005-10v1-Band-of-Rubble audio/724-ssc2004-17v2-Swirling-Rings-of- Planet-Forming-Disk Dust 22 Clues to Planetary System Architecture 23 Clues to Planetary System Architecture 24 Clues to Planetary System Architecture 25 Clues to Planetary System Architecture IRS MIPS 26 Clues to Planetary System Architecture IRS MIPS Figure 1 Morales et al. (2011) 27 Clues to Planetary System Architecture IRS MIPS Star Cold Model Warm Cold Warm Figure 1 Morales et al. (2011) 28 Two Belt Temperature • Dust production is clearly favored at the same characteristic Tdust horizon — across the large stellar spectral range (B8-K0) — slightly above the ice evaporation temperature for inner belts! • Note the relative void in Tdust ~ 100 K Figure 2 Morales et al. (2011) 29 Two Belt Temperature Median • Dust production is clearly ~190 K favored at the same characteristic Tdust horizon — across the large stellar spectral range (B8-K0) — slightly above the ice evaporation temperature for inner belts! • Note the relative void in Tdust ~ 100 K Figure 2 Morales et al. (2011) 30 Herschel Resolved Outer/Cold Rings! (PSF subtracted Mosaic) HD 107146 HD 166 HD 38206 HD 61005 HD 70313 N E HD 104860 HD 10939 HD 159492 HD 138965 HD 71722 HD 153053 HD 141378 HD 192425 HD 28355 HD 30422 Figure 1 Morales et al. (2016) 31 Water Ice Present in Kuiper-like Belts HD 166 (K0V) • ~456 Myr • 13.7pc • Mcold ≈ 0.009 MMoon 32 Rocky Particles in Terrestrial Planet Zones Stacked IRS Spectra Stellar Model Subtracted • The presence of rocky grains have been recently confirmed via a Stellar/Cold Subtracted Stellar/Cold/Large Warm Subtracted spectra stacking technique. Small grains a < aBOS 33 Planet Hunting—Ongoing Effort, Keck Figure 1: A mosaic of Palomar-PHARO and KeckII-NIRC2 NGS AO images of nine stars in our >5s candidates sample. The observations were obtained during our 2011A, 2012B, 2013A campaigns. Each image above results from the application of 34 the LOCI or KLIP algorithms, yielding contrast ratios up to 106. Candidate companions are indicated by white circles. Each star possesses dust debris as seen by Spitzer+Herschel and/or WISE. In all cases the warm dust is located inside the orbit of the candidate companion; in three cases, the candidates coincide with the inferred or resolved inner-edge of the outer cold dust location. Given the medium-to-large stellar proper motions for most candidate companions in our list, observations with Keck’s NIRC 2 over two to three years later will enable us to establish if they are gravitationally bound to the host stars. Angular Separations range from ~0.5 to 4.7 arcsec (~10 to 280 AU, median 95 AU). Figure 2 (below and right three panels): The HD 38206 HD 70313 HD 141328 FiSguErDe of1: Athe m osdusaitc eofxc Pesaslom fromar-P HHR8799ARO a nd(be Klowec)kII-N IRC2 NGS AO images of nine stars in our >5s candidates sample. The obsise rvacomtipaonsre dw ewreit hobt thosaineed of duri threnge ourof 201our 1Atar,ge 2012B,t 2013A campaigns. Each image above results from the application of 6 thestars LO CI(upper or KL-right).IP algori Keythm s,stellar yieldi ngparameters contrast ra tios up to 10 . Candidate companions are indicated by white circles. Each star possesses dust debris as seen by Spitzer+Herschel and/or WISE. In all cases the warm dust is located inside the orbit of compared in table (bottom-right). the candidate companion; in three cases, the candidates coincide with the inferred or resolved inner-edge of the outer cold dus t location. Given the medium-to-large stellar proper motions for most candidate companions in our list, observations with Ke ck’s NIRC 2 over two to three yeaHRrs l8799ater will enable us to establish if they are gravitationally bound to the host stars. Infrared Excess Angular Separations range from ~0.5Su to e t4.7 al., a2rc00s9e c (~10 to 280 AU, median 95 AU). Name Spec V D Age Touter Resolved Figure 2 (below and right three panels): The HDTyp 38206e (mag) HD(pc 70313) (M yrs) (KHD) 141328(" ) SED of the dust excess from HR8799 (below) HR8799 A5 5.95 39.4 30 45 1.8 is compared with those of three of our target HD 38206 A0 5.73 69.2 9 62 2.4 stars (upper-right). Key stellar parameters compared in table (bottom-right). HD 70313 A3 5.51 51.4 300 58 2.9 HD 141378 A5 6.42 49.2 150 59 2.4 HR 8799 Herschel Resolved sizes (bottom three rows; Morales et al., 2013). Infrared Excess Su et al., 2009 ! Name Spec V D Age Touter Resolved Type (mag) (pc) (Myrs) (K) (") HR8799 A5 5.95 39.4 30 45 1.8 HD 38206 A0 5.73 69.2 9 62 2.4 HD 70313 A3 5.51 51.4 300 58 2.9 HD 141378 A5 6.42 49.2 150 59 2.4 Herschel Resolved sizes (bottom three rows; Morales et al., 2013). ! Planet Hunting—Ongoing Effort, Palomar 35 Planet Hunting—Ongoing Effort, Palomar 36 Summary • Spitzer Space Telescope sees both warm and cold excess emission of debris around mature stars • Herschel Space Observatory confirmed the presence of cold-Kuiper belt like dust, measured the size of the outer cold belt, and revealed the presence of ice • Exopalent candidates have been identified using Keck and Palomar Observatories • For more info on Spitzer Space Telescope, its Legacy, images and animations • www.nasa.gov/spitzer • www.spitzer.caltech.edu 37 Inspiration • Cecilia Helena Payne-Gaposchkin was (1900-1979) was a British-born American astronomer and astrophysicist who proposed in her 1925 doctoral thesis that stars were composed primarily of hydrogen and helium.
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