Overview and Reassessment of Noise Budget of Starshade Exoplanet Imaging
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100 Closest Stars Designation R.A
100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79, -
236. “Stelle E Costellazioni Del Cielo”
Progetto RaPHAEL (www.raphaelproject.com ) - Incontro nº 236 del 10/07/2005 - Colore Grigio verde 236. “Stelle e costellazioni del cielo” Una parte della natura umana è terrestre , ma un’altra parte è cosmica e stellare , volendo riscoprire la totalità della nostra vera natura è molto importante ritrovare la risonanza con le dimensioni trans-terrestri, facendo anche riemergere memorie di vite passate dove non avevamo un corpo umano e dove l’esistenza si svolgeva su altri continuum spazio-temporali. Abbiamo già visto come la Fantascienza sappia risvegliare questa risonanza (ved. incontro n° 212 ) e come ci permetta di concretizzare a livello mentale esperienze che qualcuno potrebbe aver difficoltà anche solo a concepire, adesso focalizziamo un attimo l’attenzione sull’incredibile fascino che ispirano le stelle ad ogni essere umano di animo sensibile... interiormente una parte di noi sa di originare dalle stelle ed è là che aspira a tornare! Una buona parte del nostro DNA origina da altri sistemi stellari, le leggende comparate delle varie tribù native americane raccontano che ben 12 razze galattiche hanno contribuito a creare il DNA dell’Homo sapiens. Ebbene noi suggeriamo di lasciarvi guidare dalla meditazione e dal ricordo immaginativo per recuperare i “circuiti” atemporali legati al piano cosmico , attraverso esercizi rilassati di rimpatrio energetico ed esperenziale (ed un respiro consapevole) molte esperienze possono riemergere… I nomi sotto riportati, con la posizione relativa rispetto alla costellazione di appartenenza (alfa= 1, -
Starshade Rendezvous Probe
Starshade Rendezvous Probe Starshade Rendezvous Probe Study Report Imaging and Spectra of Exoplanets Orbiting our Nearest Sunlike Star Neighbors with a Starshade in the 2020s February 2019 TEAM MEMBERS Principal Investigators Sara Seager, Massachusetts Institute of Technology N. Jeremy Kasdin, Princeton University Co-Investigators Jeff Booth, NASA Jet Propulsion Laboratory Matt Greenhouse, NASA Goddard Space Flight Center Doug Lisman, NASA Jet Propulsion Laboratory Bruce Macintosh, Stanford University Stuart Shaklan, NASA Jet Propulsion Laboratory Melissa Vess, NASA Goddard Space Flight Center Steve Warwick, Northrop Grumman Corporation David Webb, NASA Jet Propulsion Laboratory Study Team Andrew Romero-Wolf, NASA Jet Propulsion Laboratory John Ziemer, NASA Jet Propulsion Laboratory Andrew Gray, NASA Jet Propulsion Laboratory Michael Hughes, NASA Jet Propulsion Laboratory Greg Agnes, NASA Jet Propulsion Laboratory Jon Arenberg, Northrop Grumman Corporation Samuel (Case) Bradford, NASA Jet Propulsion Laboratory Michael Fong, NASA Jet Propulsion Laboratory Jennifer Gregory, NASA Jet Propulsion Laboratory Steve Matousek, NASA Jet Propulsion Laboratory Jonathan Murphy, NASA Jet Propulsion Laboratory Jason Rhodes, NASA Jet Propulsion Laboratory Dan Scharf, NASA Jet Propulsion Laboratory Phil Willems, NASA Jet Propulsion Laboratory Science Team Simone D'Amico, Stanford University John Debes, Space Telescope Science Institute Shawn Domagal-Goldman, NASA Goddard Space Flight Center Sergi Hildebrandt, NASA Jet Propulsion Laboratory Renyu Hu, NASA -
Data Release #3 Stuart Shaklan, Mario Damiano, Stefan Martin, Renyu Hu June 16, 2021
Starshade Exoplanet Data Challenge: Data Release #3 Stuart Shaklan, Mario Damiano, Stefan Martin, Renyu Hu June 16, 2021 © 2021 All rights reserved. Government sponsorship acknowledged. CL # 21-2781 Data provided • For RST: • Simulated spectra of scenes with the starshade blocking the target star. • Simulated spectra of the stars (starshade moved away from the scene). • Line spread and dispersion function with 1 nm, 5 mas resolution. • For HabEX: • Simulated IFS spectra of scenes with the starshade blocking the target star. • Simulated IFS spectra of the stars (starshade moved away from the scene). • Mapping arrays from lenslet positions to image plane positions with a wavelength resolution of 1 nm. RST Spectroscopy Modeling Methodology • Follows the same approach that GSFC (N. Zimmerman) took for CGI: • Use a ray trace model of the prisms and lenses. Map Image plane (x,y,lambda) to output plane (x’,y’,lambda). • But for speed, we use a 3rd order approximation to the distortion map, which has < 0.5 mas error. • Treat the slit as a simple field stop: ignore diffraction since the slit is wide compared to the PSF • Input image plane is computed with a 5 mas pixel pitch • Highly oversamples PSF • Highly oversampled compared to final CGI pixel pitch of 21.8 mas/pixel • Map from input to output with 5 mas resolution • Bin to 21.8 mas resolution using Matlab ‘imresize’ routine. • Absolute position of spectra in image plane are not tracked, but relative position of spectra in the simulations are all consistent with the scenes. Line Spread Function and Dispersion • The dispersion is calculated every nm, and on a 5 mas pixel grid (compared to 21.8 mas pixels in the camera). -
Exoplanet Detection Synergies Between Gaia and the WFIRST
Exoplanet detection synergies between Gaia and the WFIRST Coronagraph William Fanning1, Neil Zimmerman2, Michael McElwain2,3, Gabriel Grell4 1Embry-Riddle Aeronautical University, 2NASA Goddard, 3NASA Roman Technology Fellow, 4Harvard University Abstract Observability with the WFIRST CGI WFIRST (Wide-Field Infrared Survey Telescope) is a NASA mission designed to Below: Planet-star contrast related to angular separation. Planet-star contrast is study dark energy, exoplanets, and infrared astrophysics over a six-year period. the ratio of star brightness to planet brightness. The lower the ratio, the brighter the One of WFIRST’s instruments, the Coronagraph Instrument (CGI), will use star (in comparison to the planet). For example, the Sun-Earth contrast is 1e-10 at advanced technology to image exoplanets and characterize their atmospheres in 600nm. Gaia has a detection limit of α > 0.0684 mas, and G > 3. Gaia limits are reflected starlight. We used a Monte Carlo approach to model the population of applied here to show what planets can be observed by both WFIRST and Gaia. planets around nearby stars (distance < 20 pc), and then applied the detection limitations of Gaia and WFIRST CGI. The distribution model predicts that Gaia observations of bright, single stars will yield around 9 planets, 3 of which are accessible to WFIRST. Gaia Exoplanet Discoveries for WFIRST WFIRST’s Coronagraph Instrument is capable of directly imaging exoplanets by suppressing the starlight of the planets’ host stars. It can also characterize exoplanets through spectroscopy. There are already some targets that we know we want to look at; planets previously discovered by indirect detection methods such as the radial velocity technique. -
The Exo-S Probe Class Starshade Mission
The Exo-S probe class starshade mission The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Seager, Sara et al. “The Exo-S Probe Class Starshade Mission.” Ed. Stuart Shaklan. N.p., 2015. 96050W. © 2015 Society of Photo-Optical Instrumentation Engineers (SPIE) As Published http://dx.doi.org/10.1117/12.2190378 Publisher SPIE Version Final published version Citable link http://hdl.handle.net/1721.1/106349 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. Invited Paper The Exo-S Probe Class Starshade Mission Sara Seager*a, Margaret Turnbullb, William Sparksc, Mark Thomsond, Stuart B Shakland, Aki Robergee, Marc Kuchnere, N. Jeremy Kasdinf, Shawn Domagal-Goldmane, Webster Cashg, Keith Warfieldd, Doug Lismand, Dan Scharfd, David Webbd, Rachel Trabertd, Stefan Martind, Eric Cadyd, Cate Heneghand aMassachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA, USA 02139- 4307; bGlobal Science Institute, P.O. Box 252, Antigo, WI, USA 54409; cSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, USA 21218-2410; dJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA, USA 91109-8001; eGoddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD, USA 20771-2400; fPrinceton University, Department of Mechanical and Aerospace Engineering, Engineering Quadrangle, Olden Street, Princeton, NJ, USA 08544; gUniversity of Colorado, Center for Astrophysics and Space Astronomy, 389 UCB, Boulder, CO, USA 80309-0389 ABSTRACT Exo-S is a direct imaging space-based mission to discover and characterize exoplanets. -
The Detectability of Nightside City Lights on Exoplanets
Draft version September 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The Detectability of Nightside City Lights on Exoplanets Thomas G. Beatty1 1Department of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ 85721; [email protected] ABSTRACT Next-generation missions designed to detect biosignatures on exoplanets will also be capable of plac- ing constraints on the presence of technosignatures (evidence for technological life) on these same worlds. Here, I estimate the detectability of nightside city lights on habitable, Earth-like, exoplan- ets around nearby stars using direct-imaging observations from the proposed LUVOIR and HabEx observatories. I use data from the Soumi National Polar-orbiting Partnership satellite to determine the surface flux from city lights at the top of Earth's atmosphere, and the spectra of commercially available high-power lamps to model the spectral energy distribution of the city lights. I consider how the detectability scales with urbanization fraction: from Earth's value of 0.05%, up to the limiting case of an ecumenopolis { or planet-wide city. I then calculate the minimum detectable urbanization fraction using 300 hours of observing time for generic Earth-analogs around stars within 8 pc of the Sun, and for nearby known potentially habitable planets. Though Earth itself would not be detectable by LUVOIR or HabEx, planets around M-dwarfs close to the Sun would show detectable signals from city lights for urbanization levels of 0.4% to 3%, while city lights on planets around nearby Sun-like stars would be detectable at urbanization levels of & 10%. The known planet Proxima b is a particu- larly compelling target for LUVOIR A observations, which would be able to detect city lights twelve times that of Earth in 300 hours, an urbanization level that is expected to occur on Earth around the mid-22nd-century. -
Milestone Goto-Bino Series .Cdr
Kson MilestoneK Standard Alt/Az GOTO Mount INSTRUCTIONS CONTENT FOR KSON STANDARD ALT/AZ GOTO USER INTRODUCTION.................................................................................1 ACCESSORIES..................................................................................2 ASSEMBLY INSTRUCTIONS.............................................................3 FEATURES.........................................................................5 OPERATION MANUAL FOR SKYTOUCH CONTROLLER............... 6 KEY DESCRIPTION.................................................................................6 STATUS DESCRIPTION...........................................................................6 OPERATION PROCESS...........................................................................7 POWER ON......................................................................................7 WARNING........................................................................................7 ALIGNMENT STATUS........................................................................7 CHANGE THE DATE..................................................................7 CHANGE THE TIME...................................................................8 CHANGE THE SITE...................................................................8 ALIGNMENT.............................................................................9 NAVIGATION STATUS.....................................................................11 MENU STATUS................................................................................11 -
Editorial Satish Pande Kiran Ghadge ©
ISSN 2319-4361 (Indexed in Google Scholar) Volume 3 | Issue 3 | August - October 2014 Editorial Satish Pande Kiran Ghadge © Male White-bellied Minivet he low populations of Gyps vultures remain a cause forest departments with the participation of the local Tof concern. There is some evidence that the declining people and NGO’s. Many breeding sites of cliff nesting trend has now stabilized. To effectively promote vulture and tree nesting Gyps species are in private ownership conservation all present vulture breeding sites need to plots. The involvement of local communities is the be identifi ed urgently. These sites can then be prioritized pivot of vulture conservation. for protection and future conservation. Problems that Continued monitoring of such sites is possible such breeding sites may be facing can be identifi ed and with the active enthusiastic participation of sensitized appropriate measures can be taken by the respective local youth. Monitoring includes gathering data on Ela Journal / www.elafoundation.org / Vol. 3 Issue 3 / August - October 2014 | 1 EDITORIAL commencement of breeding, number of breeding pairs, activities are threatening natural habitats on an occupation of nests, incubation and hatching, food unprecedented scale. Small habitat pockets are the last availability, threats to nestlings, protection of nest trees resorts of several species. There are several other avian and provisioning of carcasses for feeding in case of species about which ornithological data on aspects food shortage. such as habitat preference, feeding and breeding Provisioning of food at vulture restaurants in the form ecology, population recruitment success and threats of dead and diclofenac-free carcasses can be done at the is not available. -
Scientific American
Medicine Climate Science Electronics How to Find the The Last Great Hacking the Best Treatments Global Warming Power Grid Winner of the 2011 National Magazine Award for General Excellence July 2011 ScientificAmerican.com PhysicsTHE IntellıgenceOF Evolution has packed 100 billion neurons into our three-pound brain. CAN WE GET ANY SMARTER? www.diako.ir© 2011 Scientific American www.diako.ir SCIENTIFIC AMERICAN_FP_ Hashim_23april11.indd 1 4/19/11 4:18 PM ON THE COVER Various lines of research suggest that most conceivable ways of improving brainpower would face fundamental limits similar to those that affect computer chips. Has evolution made us nearly as smart as the laws of physics will allow? Brain photographed by Adam Voorhes at the Department of Psychology, Institute for Neuroscience, University of Texas at Austin. Graphic element by 2FAKE. July 2011 Volume 305, Number 1 46 FEATURES ENGINEERING NEUROSCIENCE 46 Underground Railroad 20 The Limits of Intelligence A peek inside New York City’s subway line of the future. The laws of physics may prevent the human brain from By Anna Kuchment evolving into an ever more powerful thinking machine. BIOLOGY By Douglas Fox 48 Evolution of the Eye ASTROPHYSICS Scientists now have a clear view of how our notoriously complex eye came to be. By Trevor D. Lamb 28 The Periodic Table of the Cosmos CYBERSECURITY A simple diagram, which celebrates its centennial this 54 Hacking the Lights Out year, continues to serve as the most essential conceptual A powerful computer virus has taken out well-guarded tool in stellar astrophysics. By Ken Croswell industrial control systems. -
1455189355674.Pdf
THE STORYTeller’S THESAURUS FANTASY, HISTORY, AND HORROR JAMES M. WARD AND ANNE K. BROWN Cover by: Peter Bradley LEGAL PAGE: Every effort has been made not to make use of proprietary or copyrighted materi- al. Any mention of actual commercial products in this book does not constitute an endorsement. www.trolllord.com www.chenaultandgraypublishing.com Email:[email protected] Printed in U.S.A © 2013 Chenault & Gray Publishing, LLC. All Rights Reserved. Storyteller’s Thesaurus Trademark of Cheanult & Gray Publishing. All Rights Reserved. Chenault & Gray Publishing, Troll Lord Games logos are Trademark of Chenault & Gray Publishing. All Rights Reserved. TABLE OF CONTENTS THE STORYTeller’S THESAURUS 1 FANTASY, HISTORY, AND HORROR 1 JAMES M. WARD AND ANNE K. BROWN 1 INTRODUCTION 8 WHAT MAKES THIS BOOK DIFFERENT 8 THE STORYTeller’s RESPONSIBILITY: RESEARCH 9 WHAT THIS BOOK DOES NOT CONTAIN 9 A WHISPER OF ENCOURAGEMENT 10 CHAPTER 1: CHARACTER BUILDING 11 GENDER 11 AGE 11 PHYSICAL AttRIBUTES 11 SIZE AND BODY TYPE 11 FACIAL FEATURES 12 HAIR 13 SPECIES 13 PERSONALITY 14 PHOBIAS 15 OCCUPATIONS 17 ADVENTURERS 17 CIVILIANS 18 ORGANIZATIONS 21 CHAPTER 2: CLOTHING 22 STYLES OF DRESS 22 CLOTHING PIECES 22 CLOTHING CONSTRUCTION 24 CHAPTER 3: ARCHITECTURE AND PROPERTY 25 ARCHITECTURAL STYLES AND ELEMENTS 25 BUILDING MATERIALS 26 PROPERTY TYPES 26 SPECIALTY ANATOMY 29 CHAPTER 4: FURNISHINGS 30 CHAPTER 5: EQUIPMENT AND TOOLS 31 ADVENTurer’S GEAR 31 GENERAL EQUIPMENT AND TOOLS 31 2 THE STORYTeller’s Thesaurus KITCHEN EQUIPMENT 35 LINENS 36 MUSICAL INSTRUMENTS -
Extrasolar Planets and Their Host Stars
Kaspar von Braun & Tabetha S. Boyajian Extrasolar Planets and Their Host Stars July 25, 2017 arXiv:1707.07405v1 [astro-ph.EP] 24 Jul 2017 Springer Preface In astronomy or indeed any collaborative environment, it pays to figure out with whom one can work well. From existing projects or simply conversations, research ideas appear, are developed, take shape, sometimes take a detour into some un- expected directions, often need to be refocused, are sometimes divided up and/or distributed among collaborators, and are (hopefully) published. After a number of these cycles repeat, something bigger may be born, all of which one then tries to simultaneously fit into one’s head for what feels like a challenging amount of time. That was certainly the case a long time ago when writing a PhD dissertation. Since then, there have been postdoctoral fellowships and appointments, permanent and adjunct positions, and former, current, and future collaborators. And yet, con- versations spawn research ideas, which take many different turns and may divide up into a multitude of approaches or related or perhaps unrelated subjects. Again, one had better figure out with whom one likes to work. And again, in the process of writing this Brief, one needs create something bigger by focusing the relevant pieces of work into one (hopefully) coherent manuscript. It is an honor, a privi- lege, an amazing experience, and simply a lot of fun to be and have been working with all the people who have had an influence on our work and thereby on this book. To quote the late and great Jim Croce: ”If you dig it, do it.