Kepler Mission Scientist Dimitar Sasselov Discusses the Latest Discoveries of “Habitable” Earth-Like Planets
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Astronomy with Small Telescopes
Astronomy With Small Telescopes Bohdan Paczy´nski Princeton University Observatory, Princeton, NJ 08544 [email protected] ABSTRACT The All Sky Automated Survey (ASAS) is monitoring all sky to about 14 mag with a cadence of about 1 day; it has discovered about 105 variable stars, most of them new. The instrument used for the survey had aperture of 7 cm. A search for planetary transits has lead to the discovery of about a dozen confirmed planets, so called ’hot Jupiters’, providing the information of planetary masses and radii. Most discoveries were done with telescopes with aperture of 10 cm. We propose a search for optical transients covering all sky with a cadence of 10 - 30 minutes and the limit of 12 - 14 mag, with an instant verification of all candidate events. The search will be made with a large number of 10 cm instruments, and the verification will be done with 30 cm instruments. We also propose a system to be located at the L1 point of the Earth - Sun system to detect ’killer asteroids’. With a limiting magnitude of about 18 mag it could detect 10 m boulders several hours prior to their impact, provide warning against Tunguska-like events, as well as to provide news about spectacular but harmless more modest impacts. Subject headings: techniques: photometric — surveys — celestial mechanics — mete- oroids — stars: variable — gamma rays: bursts arXiv:astro-ph/0609161v3 7 Nov 2006 1. Introduction The goal of this paper is to point out that there are many tasks for which small and even very small telescopes are not only useful, but even indispensable. -
Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗
Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗ Mario Mateo1 e-mail: [email protected] Edward W. Olszewski2 e-mail: [email protected] Heather L. Morrison3 e-mail: [email protected] Received ; accepted ∗BasedonobservationsobtainedwiththeBlancoTelescopeatCTIO,whichisoperated by the National Optical Astronomy Observatory, under contract to AURA. 1Department of Astronomy, University of Michigan, 821 Dennison Bldg., Ann Arbor, MI 48109–1090 2Steward Observatory, 933 N. Cherry, University of Arizona, Tucson, AZ 85721-0065 3Cottrell Scholar of Research Corporation, and NSF Career Fellow; Department of Astronomy and Department of Physics, Case Western Reserve University, Cleveland OH 44106 –2– ABSTRACT We have obtained deep photometric data in 24 fields along the southeast extension of the major axis of the Sagittarius dwarf spheroidal (Sgr dSph) galaxy, and in four fields along the northwest extension. Using star counts at the expected position of the Sgr upper main-sequence within the resulting color-magnitude diagrams (CMDs), we unambiguously detect Sgr stars in the southeast over the range 10–34◦ from the galaxy’s center. If Sgr is symmetric, this implies a true major-axis diameter of at least 68◦, or nearly 30 kpc if all portions of Sgr are equally distant from the Sun. Star counts parallel to the galaxy’s minor-axis reveal that Sgr remains quite broad far from its center. This suggests that the outer portions of Sgr resemble a stream rather than an extension of the ellipsoidal inner regions of the galaxy. The inferred V-band surface brightness (SB) profile ranges from 27.3-30.5 mag arcsec−2 over this radial range and exhibits a change in slope ∼ 20◦ from the center of Sgr. -
Eliza Kempton (Formerly: Eliza Miller-Ricci) Grinnell College Department of Physics Grinnell, IA 50112 [email protected] (641) 269-9803
Eliza Kempton (Formerly: Eliza Miller-Ricci) Grinnell College Department of Physics Grinnell, IA 50112 [email protected] (641) 269-9803 EDUCATION Harvard University, Cambridge, MA – Ph.D. Astronomy – June 2009 Dissertation: Towards Detecting and Characterizing Earth-like Extrasolar Planets Advisors: Dimitar Sasselov & Sara Seager Middlebury College, Middlebury, VT – B.A. summa cum laude – May 2003 Major: Physics, Minors: Mathematics & French Senior Thesis: The Molecular Zeeman Effect and the G-Band: Stokes Polarimetry Modeling of Solar CH Lines (Advisors: Rich Wolfson & Han Uitenbroek) POSITIONS Assistant Professor of Physics – Grinnell College – August 2012 - present Sagan Postdoctoral Fellow – University of California, Santa Cruz – September 2009 - July 2012 RESEARCH INTERESTS Theoretical models of planetary atmospheres Detection and characterization of extrasolar planets Transiting extrasolar planets GRANTS, HONORS, AND AWARDS Research Corporation for Science Advancement – Cottrell Scholar Award ($100k grant) - 2016-2019 Grinnell College Harris Faculty Fellowship (yearlong sabbatical fellowship) - 2016/2017 Research Corporation for Science Advancement – Cottrell College Science Award ($40k grant plus $15k match from Grinnell College) - 2015-2017 Kavli Frontiers Fellow (National Academy of Sciences) - 2010, 2011, 2012 Eliza Kempton – CV Page !1 of 7! ADVANCE Junior Scientist Lecturer – University of Arizona - winter 2011 Sagan Postdoctoral Fellowship - 2009-2012 Harvard University Teaching Certificate of Distinction - 2006 Phi Beta -
Kepler Press
National Aeronautics and Space Administration PRESS KIT/FEBRUARY 2009 Kepler: NASA’s First Mission Capable of Finding Earth-Size Planets www.nasa.gov Media Contacts J.D. Harrington Policy/Program Management 202-358-5241 NASA Headquarters [email protected] Washington 202-262-7048 (cell) Michael Mewhinney Science 650-604-3937 NASA Ames Research Center [email protected] Moffett Field, Calif. 650-207-1323 (cell) Whitney Clavin Spacecraft/Project Management 818-354-4673 Jet Propulsion Laboratory [email protected] Pasadena, Calif. 818-458-9008 (cell) George Diller Launch Operations 321-867-2468 Kennedy Space Center, Fla. [email protected] 321-431-4908 (cell) Roz Brown Spacecraft 303-533-6059. Ball Aerospace & Technologies Corp. [email protected] Boulder, Colo. 720-581-3135 (cell) Mike Rein Delta II Launch Vehicle 321-730-5646 United Launch Alliance [email protected] Cape Canaveral Air Force Station, Fla. 321-693-6250 (cell) Contents Media Services Information .......................................................................................................................... 5 Quick Facts ................................................................................................................................................... 7 NASA’s Search for Habitable Planets ............................................................................................................ 8 Scientific Goals and Objectives ................................................................................................................. -
OGLE 2004-BLG-254: a K3 III Galactic Bulge Giant Spatially Resolved by A
Astronomy & Astrophysics manuscript no. 4414arti c ESO 2018 January 9, 2018 OGLE 2004–BLG–254: a K3 III Galactic Bulge Giant spatially resolved by a single microlens⋆ A. Cassan1,2,3, J.-P. Beaulieu1,3, P. Fouqu´e1,4, S. Brillant1,5, M. Dominik1,6, J. Greenhill1,7, D. Heyrovsk´y8, K. Horne1,6, U.G. Jørgensen1,9, D. Kubas1,5, H.C. Stempels6, C. Vinter1,9, M.D. Albrow1,12, D. Bennett1,13, J.A.R. Caldwell1,14,15, J.J. Calitz1,16, K. Cook1,17, C. Coutures1,18, D. Dominis1,19, J. Donatowicz1,20, K. Hill1,7, M. Hoffman1,16, S. Kane1,21, J.-B. Marquette1,3, R. Martin1,22, P. Meintjes1,16, J. Menzies1,23, V.R. Miller12, K.R. Pollard1,12, K.C. Sahu1,14, J. Wambsganss1,2, A. Williams1,22, A. Udalski10,11, M.K. Szyma´nski10,11, M. Kubiak10,11, G. Pietrzy´nski10,11,24, I. Soszy´nski10,11,24, K. Zebru´n˙ 10,11, O. Szewczyk10,11, and Ł. Wyrzykowski10,11,25 (Affiliations can be found after the references) Received ¡date¿ / Accepted ¡date¿ ABSTRACT Aims. We present an analysis of OGLE 2004–BLG–254, a high-magnification (A 60) and relatively short duration (tE 13.2 days) microlensing event in which the source star, a Bulge K-giant, has been spatially resolved◦ ≃ by a point-like lens. We seek to determine≃ the lens and source distance, and provide a measurement of the linear limb-darkening coefficients of the source star in the I and R bands. We discuss the derived values of the latter and compare them to the classical theoretical laws, and furthermore examine the cases of already published microlensed GK-giants limb-darkening measurements. -
Cycle 12 Abstract Catalog
Cycle 12 Abstract Catalog Generated April 04, 2003 ================================================================================ Proposal Category: GO Scientific Category: ISM AND CIRCUMSTELLAR MATTER ID: 9718 Title: SMC Extinction Curve Towards a Quiescent Molecular Cloud PI: Francois Boulanger PI Institution: Institut d'Astrophysique Spatiale The lack of 2175 A bump in the SMC extinction curve is interpreted as an absence of small carbon grains. ISO Mid-IR observations support this interpretation by showing that PAH features are absent in the spectra of SMC and LMC massive star forming regions. However, the only ISO observation of an SMC quiescent molecular cloud shows all PAH features, indicating a PAH abundance relative to large dust grains similar to that of Milky Way clouds. We identified a reddened B2III star associated with this cloud. We propose to observe it with STIS. This observation will provide the first measure of the extinction properties of SMC dust away from star forming regions. It will allow us to disentangle the effects of metallicity and massive stars on the SMC extinction curve and dust composition and to assess the relevance of the SMC bump-free extinction curve to low metallicity and/or starburst galaxies in general. ================================================================================ Proposal Category: GO Scientific Category: STELLAR POPULATIONS ID: 9719 Title: Search For Metallicity Spreads in M31 Globular Clusters PI: Terry Bridges PI Institution: Anglo-Australian Observatory Our recent deep HST photometry of the M31 halo globular cluster (GC) Mayall~II, also called G1, has revealed a red-giant branch with a clear spread that we attribute to an intrinsic metallicity dispersion of at least 0.4 dex in [Fe/H]. -
Extrasolar Planets Topics to Be Covered
3/25/2013 Extrasolar planets Astronomy 9601 1 Topics to be covered • 12.1 Physics and sizes • 12.2 Detecting extrasolar planets • 12.3 Observations of exoplanets • 12.4 Exoplanet statistics • 12.5 Planets and Life 2 What is a planet? What is a star? • The composition of Jupiter closely resembles that of the Sun: who’s to say that Jupiter is not simply a “failed star” rather than a planet? • The discovery of low-mass binary stars would be interesting, but (perhaps) not as exciting as discovering new “true” planets. • Is there a natural boundary between planets and stars? 3 1 3/25/2013 Planets and brown dwarfs • A star of mass less than 8% Luminosity “bump” due to short- of the Sun (80x Jupiter’s lived deuterium burning mass) will never grow hot Steady luminosity due to H burning enough in its core to fuse hydrogen • This is used as the boundary between true stars and very large gas planets • Object s b el ow thi s mass are called brown dwarfs • The boundary between BD and planet is more controversial – some argue it should be based on formation – other choose 0.013 solar masses=13 Mj as the boundary, as objects below this mass will never reach even deuterium fusion 4 Nelson et al., 1986, AJ, 311, 226 5 Pulsar planets • In 1992, Wolszczan and Frail announced the discovery of a multi‐ Artist’s conception of the planet planet planetary system around the orbiting pulsar PSR B1257+12 millisecond pulsar PSR 1257+12 (an earlier announcement had been retracted). -
1903Aj 23 . . . 22K 22 the Asteojsomic Al
22 THE ASTEOJSOMIC AL JOUENAL. Nos- 531-532 22K . Taking into account the smallness of the weights in- concerned. Through the use of these tables the positions . volved, the individual differences which make up the and motions of many stars not included in the present 23 groups in the preceding table agree^very well. catalogue can be brought into systematic harmony with it, and apparently without materially less accuracy for the in- dividual stars than could be reached by special compu- Tables of Systematic Correction for N2 and A. tations for these stars in conformity with the system of B. 1903AJ The results of the foregoing comparisons. have been This is especially true of the star-places computed by utilized to form tables of systematic corrections for ISr2, An, Dr. Auwers in the catalogues, Ai and As. As will be seen Ai and As. In right-ascension no distinction is necessary by reference to the catalogue the positions and motions of between the various catalogues published by Dr. Auwers, south polar stars taken from N2 agree better with the beginning with the Fundamental-G at alo g ; but in decli- results of this investigation than do those taken from As, nation the distinction between the northern, intermediate, which, in turn, are quoted from the Cape Catalogue for and southern catalogues must be preserved, so far as is 1890. SYSTEMATIC COBEECTIOEB : CEDEE OF DECLINATIONS. Eight-Ascensions ; Cokrections, ¿las and 100z//xtf. Declinations; Corrections, Æs and IOOzZ/x^. B — ISa B —A B —N2 B —An B —Ai âas 100 â[is âas 100 âgô âSs 100 -
The 2012 Transit of Venus
The 2012 Transit of Venus What is a Transit? Start Watching on June 5, 2012 at: A ‘transit’ occurs when one celestial body, such as a planet or Newfoundland (St. John’s) moon, passes in front of another from our perspective on Earth. 7:33 p.m. Atlantic (Halifax) 7:03 p.m. What Will Happen on June 5 ,2012? On June 5, 2012, Venus will cross the face of the Sun starting at the Eastern (Toronto) 6:04 p.m. times shown at right. This rare event has not happened since 2004 and will not happen again until 2117. The picture below shows a Central (Winnipeg) 5:05 p.m. time-lapse of the last transit of Venus in 2004, which is similar to how this year’s transit will look. Mountain (Calgary) 4:05 p.m. Pacific (Vancouver) 3:06 p.m. How to Use Your Transit Glasses Safely Time-lapse of the transit of the 2004 transit WARNING: Never look at the Sun with of Venus. The black circles are Venus at unprotected eyes! Permanent damage and even different times as it crosses the face of the blindness will result. If in doubt, consult: Sun (Credit: A. Cerezo, P. Alexandre, J. Merchán, and D. Marsán.) http://rasc.ca/transit-venus Home-made or improvised solar filters, such as smoked glass, exposed film, or CDs are not safe, as these provide no protection against harmful ultra-violet and infrared rays. It is safe to view the June 5th Transit of Venus, the 2012 May 20th Solar Eclipse and similar events through the Transit of Venus glasses. -
March 2020 OBSERVER
THE OBSERVER OF THE TWIN CITY AMATEUR ASTRONOMERS Volume 45, Number 3 March 2020 INSIDE THIS ISSUE: 1«Editor’s Choice: Image of the Month – NGC 7120 2«President’s Note 3«Calendar of Celestial Events – March 2020 3«New & Renewing Members/Dues Blues/E-Mail List 4«TCAA Calendar of Events for 2020 4«Report on the Annual Banquet & Business Meeting 5«Images of the 60th Anniversary Banquet 7«Message from NCRAL Chair Carl Wenning 7«AstroBits – News from Around the TCAA 8«March 2020 with Jeffrey L. Hunt 16«TCAA Image Gallery 17«Renewing Your TCAA Membership 18«Public Viewing Sessions for 2020 18«TCAA Active on Facebook 18«Did You Know? 19«TCAA Treasurer’s Report as of February 27, 2020 The TCAA is an affiliate of the Astronomical League as well as its EDITOR’S CHOICE: IMAGE OF THE MONTH – NGC 7120 North Central Region. For more information about the TCAA, be This image was taken by Tim Stone. Tim comments, “Here is a certain to visit the TCAA website at necklace (NGC 2185, 2183, and 2182) of beautiful star-forming regions tcaa.us/ with an incredible brooch (NGC 2170) hanging at the end. These objects, NGC 2170 in particular, show a later stage of star formation. Here enough powerful stars have formed and have driven off much of the hydrogen Visit Astroleague.org for additional nursery in which they formed. There is just a hint of the original hydrogen information about the League and its reservoir, to the left of 2170. We can already see what this new cluster numerous membership benefits, will look like in a few hundred thousand years. -
Transiting Extrasolar Planetary Candidates in the Galactic Bulge
1 To appear in NATURE, October 5, 2006 issue Transiting extrasolar planetary candidates in the Galactic bulge Kailash C. Sahu*, Stefano Casertano*, Howard E. Bond*, Jeff Valenti*, T. Ed Smith*, Dante Minniti¶, Manuela Zoccali¶, Mario Livio*, Nino Panagia*, Nikolai Piskunov#, Thomas M. Brown*, Timothy Brown†, Alvio Renzini‡, R. Michael Rich§, Will Clarkson*, Stephen Lubow* *Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 †High Altitude Observatory, 3450 Mitchell Lane, Boulder, CO 80307 ¶Universidad Catolica de Chile, Av. Vicuña Mackenna 4860, Santiago 22, Chile #Uppsala University, Box 515, S-751 20 Uppsala, SWEDEN ‡INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy §University of California at Los Angeles, Los Angeles, CA 90095-1562 More than 200 extrasolar planets have been discovered around relatively nearby stars, primarily through the Doppler line shifts owing to the reflex motions of their host stars, and more recently through transits of some planets across the face of the host stars. The detection of planets with the shortest known periods, 1.2 to 2.5 days, has mainly resulted from transit surveys which have generally targeted stars more massive than 0.75 M⊙, where M⊙ is the mass of the Sun. Here we report the results from a planetary transit search performed in a rich stellar field towards the Galactic bulge. We discovered 16 candidates with orbital periods between 0.4 and 4.2 days, five of which orbit stars of 0.44 to 0.75 M⊙. In two cases, radial-velocity measurements support the planetary nature of the companions. Five candidates have orbital periods below 1.0 day, constituting a new class of ultra-short-period planets (USPPs), which occur only around stars of less than 0.88 M⊙. -
December 1997
No. 90 – December 1997 T E L E S C O P E S A N D I N S T R U M E N T A T I O N A Deep Field with the Upgraded NTT S. D’ODORICO, ESO This colour deep image has been prepared from 4 deep images through the filters B, V, r and i obtained with the SUSI CCD imager at the ESO NTT. The image covers a 2.2 × 2.2 arcmin “emp- ty” field centred about 2 arcminutes south of the z = 4.7 QSO BR 1202- 0725. The four images result from the co-addition of dithered short integra- tions for a total of 52,800, 23,400, 23,400 and 16,200 seconds in the four bands, and the co-added images have average FWHMs of 0.84, 0.80, 0.80 and 0.68 arcsec respectively. The data were obtained for a scientif- ic programme approved for the ESO Period 58 and aimed at the study of the photometric redshift distribution of the faint galaxies and of gravitational lens- ing effects in the field. The P.I. of the proposal is Sandro D’Odorico and the Co-P.I. are J. Bergeron, H.M. Adorf, S. Charlot, D. Clements, S. Cristiani, L. da Costa, E. Egami, A. Fontana, B. Fort, L. Gautret, E. Giallongo, R. Gilmozzi, R.N. Hook, B. Leibundgut, Y. Mellier, P. Petitjean, A. Renzini, S. Savaglio, P. Shaver, S. Seitz and L. Yan. The pro- gramme was executed in service mode by the NTT team in February through April 1997 in photometric nights with seeing better than 1 arcsec.