Goddard's Astrophysics Science Division Annual Report 2010 5B

Total Page:16

File Type:pdf, Size:1020Kb

Goddard's Astrophysics Science Division Annual Report 2010 5B The Astrophysics Science Division Annual Report 2010 Astrophysics Science Division The NASA/TM–2011–215870 Goddard’s Astrophysics Science Division Annual Report 2010 Joan Centrella and Francis Reddy, Editors Pat Tyler, Graphical Editor NASA/TM-2011-215870 NASA Goddard Space Flight Center Greenbelt, Maryland 20771 March 2011 7KH1$6$67,3URJUDP2IÀFH«LQ3URÀOH 6LQFHLWVIRXQGLQJ1$6$KDVEHHQGHGLFDWHGWRWKH &21)(5(1&(38%/,&$7,21&ROOHFWHG DGYDQFHPHQWRIDHURQDXWLFVDQGVSDFHVFLHQFH7KH SDSHUVIURPVFLHQWLÀFDQGWHFKQLFDOFRQIHUHQFHV 1$6$6FLHQWLÀFDQG7HFKQLFDO,QIRUPDWLRQ 67, V\PSRVLDVHPLQDUVRURWKHUPHHWLQJVVSRQVRUHG 3URJUDP2IÀFHSOD\VDNH\SDUWLQKHOSLQJ1$6$ RUFRVSRQVRUHGE\1$6$ PDLQWDLQWKLVLPSRUWDQWUROH 63(&,$/38%/,&$7,216FLHQWLÀFWHFKQLFDO 7KH1$6$67,3URJUDP2IÀFHLVRSHUDWHGE\ RUKLVWRULFDOLQIRUPDWLRQIURP1$6$SURJUDPV /DQJOH\5HVHDUFK&HQWHUWKHOHDGFHQWHUIRU SURMHFWVDQGPLVVLRQRIWHQFRQFHUQHGZLWKVXE 1$6$·VVFLHQWLÀFDQGWHFKQLFDOLQIRUPDWLRQ7KH MHFWVKDYLQJVXEVWDQWLDOSXEOLFLQWHUHVW 1$6$67,3URJUDP2IÀFHSURYLGHVDFFHVVWR WKH1$6$67,'DWDEDVHWKHODUJHVWFROOHFWLRQRI 7(&+1,&$/75$16/$7,21(QJOLVKODQJXDJH DHURQDXWLFDODQGVSDFHVFLHQFH67,LQWKHZRUOG WUDQVODWLRQVRIIRUHLJQVFLHQWLÀFDQGWHFKQLFDOPD 7KH3URJUDP2IÀFHLVDOVR1$6$·VLQVWLWXWLRQDO WHULDOSHUWLQHQWWR1$6$·VPLVVLRQ PHFKDQLVPIRUGLVVHPLQDWLQJWKHUHVXOWVRILWV UHVHDUFKDQGGHYHORSPHQWDFWLYLWLHV7KHVHUHVXOWV 6SHFLDOL]HGVHUYLFHVWKDWFRPSOHPHQWWKH67,3UR DUHSXEOLVKHGE\1$6$LQWKH1$6$67,5HSRUW JUDP2IÀFH·VGLYHUVHRIIHULQJVLQFOXGHFUHDWLQJ 6HULHVZKLFKLQFOXGHVWKHIROORZLQJUHSRUWW\SHV FXVWRPWKHVDXULEXLOGLQJFXVWRPL]HGGDWDEDVHV RUJDQL]LQJDQGSXEOLVKLQJUHVHDUFKUHVXOWVHYHQ 7(&+1,&$/38%/,&$7,215HSRUWVRI SURYLGLQJYLGHRV FRPSOHWHGUHVHDUFKRUDPDMRUVLJQLÀFDQWSKDVH RIUHVHDUFKWKDWSUHVHQWWKHUHVXOWVRI1$6$SUR )RUPRUHLQIRUPDWLRQDERXWWKH1$6$67,3URJUDP JUDPVDQGLQFOXGHH[WHQVLYHGDWDRUWKHRUHWLFDO 2IÀFHVHHWKHIROORZLQJ DQDO\VLV,QFOXGHVFRPSLODWLRQVRIVLJQLÀFDQW $FFHVVWKH1$6$67,3URJUDP+RPH3DJHDW VFLHQWLÀFDQGWHFKQLFDOGDWDDQGLQIRUPDWLRQ KWWSZZZVWLQDVDJRY67,KRPHSDJHKWPO GHHPHGWREHRIFRQWLQXLQJUHIHUHQFHYDOXH 1$6$·VFRXQWHUSDUWRISHHUUHYLHZHGIRUPDO (PDLO\RXUTXHVWLRQYLDWKH,QWHUQHWWR SURIHVVLRQDOSDSHUVEXWKDVOHVVVWULQJHQWOLPLWD KHOS#VWLQDVDJRY WLRQVRQPDQXVFULSWOHQJWKDQGH[WHQWRIJUDSKLF SUHVHQWDWLRQV )D[\RXUTXHVWLRQWRWKH1$6$$FFHVV+HOS'HVN DW 443 757-5803 7(&+1,&$/0(025$1'806FLHQWLÀF DQGWHFKQLFDOÀQGLQJVWKDWDUHSUHOLPLQDU\RURI 7HOHSKRQHWKH1$6$$FFHVV+HOS'HVNDW 443 VSHFLDOL]HGLQWHUHVWHJTXLFNUHOHDVHUHSRUWV 757-5802 ZRUNLQJSDSHUVDQGELEOLRJUDSKLHVWKDWFRQWDLQ :ULWHWR PLQLPDODQQRWDWLRQ'RHVQRWFRQWDLQH[WHQVLYH 1$6$$FFHVV+HOS'HVN DQDO\VLV 1$6$&HQWHUIRU$HUR6SDFH,QIRUPDWLRQ &2175$&7255(32576FLHQWLÀFDQGWHFKQL 71156WDQGDUG'ULYH FDOÀQGLQJVE\1$6$VSRQVRUHGFRQWUDFWRUVDQG +DQRYHU0' JUDQWHHV NASA/TM-2011-215870 Goddard’s Astrophysics Science Division Annual Report 2010 Joan Centrella NASA Goddard Space Flight Center, Greenbelt, Maryland Francis Reddy Syneren Technologies, Inc., Greenbelt, Maryland Pat Tyler, Graphical Editor Syneren Technologies, Inc., Greenbelt, Maryland National Aeronautics and Space Administration Goddard Space Flight Center Greenbelt, Maryland 20771 March 2011 Available from: NASA Center for AeroSpace Information National Technical Information Service 7115 Standard Drive 5285 Port Royal Road +DQRYHU0' 6SULQJ¿HOG9$ Astrophysics Science Division Annual Report 2010 Table of Contents +,-,: Y$!. *' R$/*$0 .....................................................................................................................................- N$0 F!1$) *' ASD .........................................................................................................................................2 A0!.3) ...........................................................................................................................................................4 R$)$!.15 H*65#*65() .................................................................................................................................-- E78#%.*'6 I Z0 -9, ! B#:$ C%;8!1( D0!.& G!#!7< .........................................................................-- T5$ D*)1%/$.< %& L<;!'-!#85!-$;*((*'6 G!#!7*$) ...........................................................................-- F$.;*: G!;;!-.!< F#!.$) &.%; S:.8.*)*'6 P#!1$) ............................................................................-+ U'3$.)(!'3*'6 (5$ E7(.!6!#!1(*1 G!;;!-R!< B!1=6.%:'3 ..........................................................-> T5$ E/%#:(*%' %& P#!'$(-F%.;*'6 D*)=) 0*(5 (5$ H$.)15$# S8!1$ O")$./!(%.< ........................-? C5!.6$ E715!'6$ X-.!< E;*))*%' *' (5$ H$#*%)85$.$ !'3 B$<%'3 ..............................................-@ T.%A!' A'!#%6) *' B*'!.< B#!1= H%#$ S<)($;) ................................................................................-4 M*##*)$1%'3 P:#)!. E1#*8)$): W$*65*'6 ! N$:(.%' S(!. ................................................................+- S:8$.'%/! S5%1= I'($.!1(*%')...........................................................................................................+> T5$ I''$. W%.=*'6) %& S(!.-&%.;*'6 G!#!7*$) !( (5$ E8%15 %& S(!. F%.;!(*%' ........................+? R$)$!.15 !'3 D$/$#%8;$'( ......................................................................................................................+@ S:"%."*(!# ............................................................................................................................................+@ S:8$. T.!')-I.%' G!#!1(*1 E#$;$'( R$1%.3$. (S:8$.-TIGER) ...............................................+@ C%);*1 R!< E'$.6$(*1) !'3 M!)) (CREAM) ...............................................................................+@ X-.!< Q:!'(:; C!#%.*;$($. (XQC) !'3 M*1.%-X ....................................................................+4 X-.!< A3/!'1$3 C%'1$8() T$)("$3 (XACT) ................................................................................2, P.*;%.3*!# I'&#!(*%' P%#!.*B!(*%' E78#%.$. ...........................................................................2+ B!##%%'-"%.'$ E78$.*;$'( 0*(5 ! S:8$.1%'3:1(*'6 S8$1(.%;$($. (BESS) ..........................22 G!;;!-R!< B:.)( P%#!.*;$($. ....................................................................................................2? C!#%.*;$(.*1 E#$1(.%' T$#$)1%8$ (CALET) ...............................................................................2C T5$ B!##%%' E78$.*;$'(!# T0*' T$#$)1%8$ &%. I'&.!.$3 I'($.&$.%;$(.< (BETTII) .............29 T$15'%#%6< D$/$#%8;$'( ..................................................................................................................>, L!"%.!(%.< A)(.%85<)*1) U)*'6 !' X-.!< M*1.%1!#%.*;$($. 0*(5 !' E#$1(.%' B$!; I%' T.!8 ...............................................................................................................>, X-.!< C!#%.*;$($. D$/$#%8;$'( .................................................................................................>- X-.!< M*..%. D$/$#%8;$'(: N:S(!. !'3 IXO ...........................................................................>2 F!.-I'&.!.$3 D$($1(%.) ...............................................................................................................>> MKID D$($1(%.) &%. S:";*##*;$($. A)(.%'%;< ......................................................................>C T$15'%#%6< D$/$#%8;$'( &%. S8!1$-"!)$3 I;!6*'6 I'($.&$.%;$($.) ....................................>@ T$15'%#%6< D$/$#%8;$'( &%. LISA ............................................................................................>9 T5.$$-D*;$')*%'!# T.!1= I;!6$. D$($1(%. &%. G!;;!-.!< !'3 N$:(.%' I;!6*'6 .............?- UV !'3 V*)*"#$ Z$.%-R$!3-N%*)$ I;!6*'6 D$($1(%. D$/$#%8;$'( ........................................?+ C3Z'T$ D$($1(%. D$/$#%8;$'( &%. H!.3 X-.!< C%3$3-M!)= D$($1(%.) ............................?2 P.%A$1() .......................................................................................................................................................?? I' O8$.!(*%' ........................................................................................................................................?C F$.;* G!;;!-.!< S8!1$ T$#$)1%8$ ...............................................................................................?C T5$ R%))* X-.!< T*;*'6 E78#%.$. (RXTE) ...................................................................................?4 XMM-N$0(%' G:$)( O")$./$. F!1*#*(< .....................................................................................C- S:B!=: (A)(.%-E+) .........................................................................................................................C+ H:""#$ S8!1$ T$#$)1%8$ ................................................................................................................C2 S0*&( ...............................................................................................................................................CC G!#!7< E/%#:(*%' E78#%.$. (GALEX) .........................................................................................C@ H*65 E'$.6< A)(.%85<)*1) S1*$'1$ A.15*/$ R$)$!.15 C$'($. (HEASARC) ...........................C4 T!"#$ %& C%'($'() * Astrophysics Science Division Annual Report 2010 WMAP S$/$'-Y$!. R$):#() ...........................................................................................................@+ I' D$/$#%8;$'( ...................................................................................................................................@? J!;$) W$"" S8!1$ T$#$)1%8$ ..........................................................................................................@?
Recommended publications
  • Ultraviolet Spectroscopy of Type Iib Supernovae: Diversity and the Impact of Circumstellar Material
    LJMU Research Online Ben-Ami, S, Hachinger, S, Gal-Yam, A, Mazzali, PA, Filippenko, AV, Horesh, A, Matheson, T, Modjaz, M, Sauer, DN, Silverman, JM, Smith, N and Yaron, O ULTRAVIOLET SPECTROSCOPY OF TYPE IIB SUPERNOVAE: DIVERSITY AND THE IMPACT OF CIRCUMSTELLAR MATERIAL http://researchonline.ljmu.ac.uk/id/eprint/2871/ Article Citation (please note it is advisable to refer to the publisher’s version if you intend to cite from this work) Ben-Ami, S, Hachinger, S, Gal-Yam, A, Mazzali, PA, Filippenko, AV, Horesh, A, Matheson, T, Modjaz, M, Sauer, DN, Silverman, JM, Smith, N and Yaron, O (2015) ULTRAVIOLET SPECTROSCOPY OF TYPE IIB SUPERNOVAE: DIVERSITY AND THE IMPACT OF CIRCUMSTELLAR MATERIAL. LJMU has developed LJMU Research Online for users to access the research output of the University more effectively. Copyright © and Moral Rights for the papers on this site are retained by the individual authors and/or other copyright owners. Users may download and/or print one copy of any article(s) in LJMU Research Online to facilitate their private study or for non-commercial research. You may not engage in further distribution of the material or use it for any profit-making activities or any commercial gain. The version presented here may differ from the published version or from the version of the record. Please see the repository URL above for details on accessing the published version and note that access may require a subscription. For more information please contact [email protected] http://researchonline.ljmu.ac.uk/ Ultraviolet Spectroscopy of Type IIb Supernovae: Diversity and the Impact of Circumstellar Material Sagi Ben-Ami1,2,3, Stephan Hachinger4,5, Avishay Gal-Yam2,6, Paolo A.
    [Show full text]
  • Information Summaries
    TIROS 8 12/21/63 Delta-22 TIROS-H (A-53) 17B S National Aeronautics and TIROS 9 1/22/65 Delta-28 TIROS-I (A-54) 17A S Space Administration TIROS Operational 2TIROS 10 7/1/65 Delta-32 OT-1 17B S John F. Kennedy Space Center 2ESSA 1 2/3/66 Delta-36 OT-3 (TOS) 17A S Information Summaries 2 2 ESSA 2 2/28/66 Delta-37 OT-2 (TOS) 17B S 2ESSA 3 10/2/66 2Delta-41 TOS-A 1SLC-2E S PMS 031 (KSC) OSO (Orbiting Solar Observatories) Lunar and Planetary 2ESSA 4 1/26/67 2Delta-45 TOS-B 1SLC-2E S June 1999 OSO 1 3/7/62 Delta-8 OSO-A (S-16) 17A S 2ESSA 5 4/20/67 2Delta-48 TOS-C 1SLC-2E S OSO 2 2/3/65 Delta-29 OSO-B2 (S-17) 17B S Mission Launch Launch Payload Launch 2ESSA 6 11/10/67 2Delta-54 TOS-D 1SLC-2E S OSO 8/25/65 Delta-33 OSO-C 17B U Name Date Vehicle Code Pad Results 2ESSA 7 8/16/68 2Delta-58 TOS-E 1SLC-2E S OSO 3 3/8/67 Delta-46 OSO-E1 17A S 2ESSA 8 12/15/68 2Delta-62 TOS-F 1SLC-2E S OSO 4 10/18/67 Delta-53 OSO-D 17B S PIONEER (Lunar) 2ESSA 9 2/26/69 2Delta-67 TOS-G 17B S OSO 5 1/22/69 Delta-64 OSO-F 17B S Pioneer 1 10/11/58 Thor-Able-1 –– 17A U Major NASA 2 1 OSO 6/PAC 8/9/69 Delta-72 OSO-G/PAC 17A S Pioneer 2 11/8/58 Thor-Able-2 –– 17A U IMPROVED TIROS OPERATIONAL 2 1 OSO 7/TETR 3 9/29/71 Delta-85 OSO-H/TETR-D 17A S Pioneer 3 12/6/58 Juno II AM-11 –– 5 U 3ITOS 1/OSCAR 5 1/23/70 2Delta-76 1TIROS-M/OSCAR 1SLC-2W S 2 OSO 8 6/21/75 Delta-112 OSO-1 17B S Pioneer 4 3/3/59 Juno II AM-14 –– 5 S 3NOAA 1 12/11/70 2Delta-81 ITOS-A 1SLC-2W S Launches Pioneer 11/26/59 Atlas-Able-1 –– 14 U 3ITOS 10/21/71 2Delta-86 ITOS-B 1SLC-2E U OGO (Orbiting Geophysical
    [Show full text]
  • NASA's Goddard Space Flight Center Laboratory for High Energy
    1 NASA’s Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, Maryland 20771 @S0002-7537~99!00301-7# This report covers the period from July 1, 1997 to June 30, Toshiaki Takeshima, Jane Turner, Ken Watanabe, Laura 1998. Whitlock, and Tahir Yaqoob. This Laboratory’s scientific research is directed toward The following investigators are University of Maryland experimental and theoretical research in the areas of X-ray, Scientists: Drs. Keith Arnaud, Manuel Bautista, Wan Chen, gamma-ray, and cosmic-ray astrophysics. The range of inter- Fred Finkbeiner, Keith Gendreau, Una Hwang, Michael Loe- ests of the scientists includes the Sun and the solar system, wenstein, Greg Madejski, F. Scott Porter, Ian Richardson, stellar objects, binary systems, neutron stars, black holes, the Caleb Scharf, Michael Stark, and Azita Valinia. interstellar medium, normal and active galaxies, galaxy clus- Visiting scientists from other institutions: Drs. Vadim ters, cosmic-ray particles, and the extragalactic background Arefiev ~IKI!, Hilary Cane ~U. Tasmania!, Peter Gonthier radiation. Scientists and engineers in the Laboratory also ~Hope College!, Thomas Hams ~U. Seigen!, Donald Kniffen serve the scientific community, including project support ~Hampden-Sydney College!, Benzion Kozlovsky ~U. Tel such as acting as project scientists and providing technical Aviv!, Richard Kroeger ~NRL!, Hideyo Kunieda ~Nagoya assistance to various space missions. Also at any one time, U.!, Eugene Loh ~U. Utah!, Masaki Mori ~Miyagi U.!, Rob- there are typically between twelve and eighteen graduate stu- ert Nemiroff ~Mich. Tech. U.!, Hagai Netzer ~U. Tel Aviv!, dents involved in Ph.D. research work in this Laboratory. Yasushi Ogasaka ~JSPS!, Lev Titarchuk ~George Mason U.!, Currently these are graduate students from Catholic U., Stan- Alan Tylka ~NRL!, Robert Warwick ~U.
    [Show full text]
  • The Progenitor of Supernova 2011Dh/Ptf11eon in Messier 51
    To Appear in ApJ Letters A Preprint typeset using LTEX style emulateapj v. 11/10/09 THE PROGENITOR OF SUPERNOVA 2011DH/PTF11EON IN MESSIER 51 Schuyler D. Van Dyk1, Weidong Li2, S. Bradley Cenko2, Mansi M. Kasliwal3, Assaf Horesh3, Eran O. Ofek3,4, Adam L. Kraus5,6, Jeffrey M. Silverman2, Iair Arcavi7, Alexei V. Filippenko2, Avishay Gal-Yam7, Robert M. Quimby3, Shrinivas R. Kulkarni3, Ofer Yaron7, and David Polishook7 To Appear in ApJ Letters ABSTRACT We have identified a luminous star at the position of supernova (SN) 2011dh/PTF11eon, in pre- SN archival, multi-band images of the nearby, nearly face-on galaxy Messier 51 (M51) obtained by the Hubble Space Telescope with the Advanced Camera for Surveys. This identification has been confirmed, to the highest available astrometric precision, using a Keck-II adaptive-optics image. The available early-time spectra and photometry indicate that the SN is a stripped-envelope, core-collapse Type IIb, with a more compact progenitor (radius ∼ 1011 cm) than was the case for the well-studied SN IIb 1993J. We infer that the extinction to SN 2011dh and its progenitor arises from a low Galactic foreground contribution, and that the SN environment is of roughly solar metallicity. The detected 0 object has absolute magnitude MV ≈ −7.7 and effective temperature ∼ 6000 K. The star’s radius, ∼ 1013 cm, is more extended than what has been inferred for the SN progenitor. We speculate that the detected star is either an unrelated star very near the position of the actual progenitor, or, more likely, the progenitor’s companion in a mass-transfer binary system.
    [Show full text]
  • Optical and Near-Infrared Observations of SN 2011Dh-The First 100 Days
    Astronomy & Astrophysics manuscript no. sn2011dh-astro-ph-v2 c ESO 2018 November 4, 2018 Optical and near-infrared observations of SN 2011dh - The first 100 days. M. Ergon1, J. Sollerman1, M. Fraser2, A. Pastorello3, S. Taubenberger4, N. Elias-Rosa5, M. Bersten6, A. Jerkstrand2, S. Benetti3, M.T. Botticella7, C. Fransson1, A. Harutyunyan8, R. Kotak2, S. Smartt2, S. Valenti3, F. Bufano9; 10, E. Cappellaro3, M. Fiaschi3, A. Howell11, E. Kankare12, L. Magill2; 13, S. Mattila12, J. Maund2, R. Naves14, P. Ochner3, J. Ruiz15, K. Smith2, L. Tomasella3, and M. Turatto3 1 The Oskar Klein Centre, Department of Astronomy, AlbaNova, Stockholm University, 106 91 Stockholm, Sweden 2 Astrophysics Research Center, School of Mathematics and Physics, Queens University Belfast, Belfast, BT7 1NN, UK 3 INAF, Osservatorio Astronomico di Padova, vicolo dell’Osservatorio n. 5, 35122 Padua, Italy 4 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany 5 Institut de Ciències de l’Espai (IEEC-CSIC), Facultat de Ciències, Campus UAB, E-08193 Bellaterra, Spain. 6 Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan 7 INAF-Osservatorio Astronomico di Capodimonte, Salita Moiariello, 16 80131 Napoli, Italy 8 Fundación Galileo Galilei-INAF, Telescopio Nazionale Galileo, Rambla José Ana Fernández Pérez 7, 38712 Breña Baja, TF - Spain 9 INAF, Osservatorio Astrofisico di Catania, Via Santa Sofia, I-95123, Catania, Italy 10 Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 252, Santiago, Chile 11 Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117 12 Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 13 Isaac Newton Group, Apartado 321, E-38700 Santa Cruz de La Palma, Spain 14 Observatorio Montcabrer, C Jaume Balmes 24, Cabrils, Spain 15 Observatorio de Cántabria, Ctra.
    [Show full text]
  • Prime Focus (09-10)
    Highlights of the September Sky. - - - 1st - - - Last Quarter Moon Prime Focus Dusk: Venus, Spica, and Mars nearly form a straight A Publication of the Kalamazoo Astronomical Society line less than 5º long. - - - 4th — 5th - - - September 2010 Dusk: Mars is just 2º upper right of Spica, which is about 4º right of Venus. - - - 8th - - - ThisThis MonthsMonths KAS EventsEvents New Moon - - - 10th - - - Dusk: Mars is above the Observing Session: Saturday, September 4 @ 8:00 pm thin crescent Moon. Jupiter & Open Clusters - Kalamazoo Nature Center - - - 11th - - - Dusk: Venus is 6º right of General Meeting: Friday, September 10 @ 7:00 pm the Moon. Kalamazoo Area Math & Science Center - See Page 8 for Details - - - 13th - - - PM: Antares is 4º left of the Waxing Gibbous Moon. Kiwanis Star Party: Saturday, September 11 @ 8:00 pm - - - 15th - - - Kiwanis Youth Conservation Area - See Page 7 for Details First Quarter Moon thth th Observing Session: Saturday, September 18 @ 8:00 pm - - - 17 — 19 - - - PM: Jupiter and Uranus Moon, Jupiter, Uranus & Neptune- Kalamazoo Nature Center are just 0.8º apart. - - - 19thth - - - AM: Mercury at greatest western elongation (18º). InsideInside thethe Newsletter.Newsletter. .. .. - - - 21st - - - PM: Jupiter and Uranus are both at opposition Perseid Potluck Picnic Report............. p. 2 - - - 22nd - - - Board Meeting Minutes......................... p. 2 PM: Jupiter (and Uranus) are about 6º below the Night Sky Volunteer Program............. p. 3 Moon. Autumnal Equinox Jack Horkheimer..................................... p. 4 (11:09 pm EDT) NASA Space Place.................................. p. 5 - - - 23rd - - - Full Moon September Night Sky............................. p. 6 - - - 27th - - - PM: Pleiades are about 2º KAS Officers & Announcements........ p. 7 left of the Moon. General Meeting Preview....................
    [Show full text]
  • Stellar Clusters in Dwarf Galaxies
    A&A 448, 471–478 (2006) Astronomy DOI: 10.1051/0004-6361:20052949 & c ESO 2006 Astrophysics Stellar clusters in dwarf galaxies L. Vanzi1 and M. Sauvage2 1 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile e-mail: [email protected] 2 CEA/DSM/DAPNIA/Service d’Astrophysique – UMR AIM, CE Saclay, 91191 Gif-sur-Yvette Cedex, France e-mail: [email protected] Received 28 February 2005 / Accepted 13 October 2005 ABSTRACT We present new observations in the Ks (2.2 µm) and L (3.7 µm) infrared bands of a sample of blue dwarf galaxies with the larger aim of studying the population of massive stellar clusters, the occurrence of dust-embedded stellar clusters, and their properties. All Ks images show a rich population of clusters, but only a small fraction of them is bright in L.MostL sources have radio counterparts. We derived the luminosity function in Ks for the galaxies IC 4661 and NGC 5408, finding both to be consistent with those of similar galaxies. We also compared the number of clusters and their luminosities with the star-formation rate of the host galaxies and found no compelling evidence of correlation. We conclude that young clusters and embedded clusters are a common feature of blue dwarf galaxies and possibly of galaxies in general, we suggest that their occurrence is due to purely statistical effects rather than a phenomenon related to specific physical conditions. In this sense we expect these objects to be abundant at high red-shift. Key words. galaxies: dwarf – galaxies: starburst – galaxies: star clusters 1.
    [Show full text]
  • Fundamental Properties of Core-Collapse Supernova and GRB Progenitors: Predicting the Look of Massive Stars Before Death
    A&A 558, A131 (2013) Astronomy DOI: 10.1051/0004-6361/201321906 & c ESO 2013 Astrophysics Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death Jose H. Groh1, Georges Meynet1, Cyril Georgy2, and Sylvia Ekström1 1 Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Astrophysics group, EPSAM, Keele University, Lennard-Jones Labs, ST5 5BG Keele, UK Received 16 May 2013 / Accepted 20 August 2013 ABSTRACT We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of Mini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with Mini = 9−20 M, we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the + following types of SN progenitors: WO1–3 (Mini ≥ 32 M), WN10–11 (25 < Mini < 32 M), LBV (20 ≤ Mini ≤ 25 M), G1 Ia (18 < Mini < 20 M), and RSGs (9 ≤ Mini ≤ 18 M). For non-rotating models, we found spectral types WO1–3 (Mini > 40 M), WN7–8 (25 < Mini ≤ 40 M), WN11h/LBV (20 < Mini ≤ 25 M), and RSGs (9 ≤ Mini ≤ 20 M).
    [Show full text]
  • Photographs Written Historical and Descriptive
    CAPE CANAVERAL AIR FORCE STATION, MISSILE ASSEMBLY HAER FL-8-B BUILDING AE HAER FL-8-B (John F. Kennedy Space Center, Hanger AE) Cape Canaveral Brevard County Florida PHOTOGRAPHS WRITTEN HISTORICAL AND DESCRIPTIVE DATA HISTORIC AMERICAN ENGINEERING RECORD SOUTHEAST REGIONAL OFFICE National Park Service U.S. Department of the Interior 100 Alabama St. NW Atlanta, GA 30303 HISTORIC AMERICAN ENGINEERING RECORD CAPE CANAVERAL AIR FORCE STATION, MISSILE ASSEMBLY BUILDING AE (Hangar AE) HAER NO. FL-8-B Location: Hangar Road, Cape Canaveral Air Force Station (CCAFS), Industrial Area, Brevard County, Florida. USGS Cape Canaveral, Florida, Quadrangle. Universal Transverse Mercator Coordinates: E 540610 N 3151547, Zone 17, NAD 1983. Date of Construction: 1959 Present Owner: National Aeronautics and Space Administration (NASA) Present Use: Home to NASA’s Launch Services Program (LSP) and the Launch Vehicle Data Center (LVDC). The LVDC allows engineers to monitor telemetry data during unmanned rocket launches. Significance: Missile Assembly Building AE, commonly called Hangar AE, is nationally significant as the telemetry station for NASA KSC’s unmanned Expendable Launch Vehicle (ELV) program. Since 1961, the building has been the principal facility for monitoring telemetry communications data during ELV launches and until 1995 it processed scientifically significant ELV satellite payloads. Still in operation, Hangar AE is essential to the continuing mission and success of NASA’s unmanned rocket launch program at KSC. It is eligible for listing on the National Register of Historic Places (NRHP) under Criterion A in the area of Space Exploration as Kennedy Space Center’s (KSC) original Mission Control Center for its program of unmanned launch missions and under Criterion C as a contributing resource in the CCAFS Industrial Area Historic District.
    [Show full text]
  • The Turbulent Tale of a Tiny Galaxy by Trudy Bell and Dr
    Space Place Partners’ Article August 2010 The Turbulent Tale of a Tiny Galaxy by Trudy Bell and Dr. Tony Phillips Next time you hike in the woods, pause at a babbling stream. Watch carefully how the water flows around rocks. After piling up in curved waves on the upstream side, like the bow wave in front of a motorboat, the water speeds around the rock, spilling into a riotous, turbulent wake downstream. Lightweight leaves or grass blades can get trapped in the wake, swirling round and round in little eddy currents that collect debris. Astronomers have found something similar happening in the turbulent wake of a tiny galaxy that is plunging into a cluster of 1,500 galaxies in the constellation Virgo. In this case, however, instead of collecting grass and leaves, eddy currents in the little galaxy’s tail seem to be gathering gaseous material to make new stars. “It’s a fascinating case of turbulence [rather than gravity] trapping the gas, allowing it to become dense enough to form stars,” says Janice A. Hester of the California Institute of Technology in Pasadena. The tell-tale galaxy, designated IC 3418, is only a hundredth the size of the Milky Way and hardly stands out in visible light images of the busy Virgo Cluster. Astronomers realized it was interesting, however, when they looked at it using NASA's Galaxy Evolution Explorer satellite. “Ultraviolet images from the Galaxy Evolution Explorer revealed a long tail filled with clusters of massive, young stars,” explains Hester. Galaxies with spectacular tails have been seen before.
    [Show full text]
  • The Possible Detection of a Binary Companion to a Type Ibn Supernova Progenitor J
    The Astrophysical Journal, 833:128 (6pp), 2016 December 20 doi:10.3847/1538-4357/833/2/128 © 2016. The American Astronomical Society. All rights reserved. THE POSSIBLE DETECTION OF A BINARY COMPANION TO A TYPE IBN SUPERNOVA PROGENITOR J. R. Maund1,7, A. Pastorello2, S. Mattila3,4, K. Itagaki5, and T. Boles6 1 Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK 2 INAF—Osservatorio Astronomico di Padova. Vicolo Osservatorio 5, I-35122, Padova, Italy 3 Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 4 Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland 5 Itagaki Astronomical Observatory, Teppo-cho, 990-2492 Yamagata, Japan 6 Coddenham Astronomical Observatory, Suffolk IP6 9QY, UK Received 2016 April 28; revised 2016 August 23; accepted 2016 September 20; published 2016 December 13 ABSTRACT We present late-time observations of the site of the Type Ibn supernova (SN) 2006jc, acquired with the Hubble Space Telescope Advanced Camera for Surveys. A faint blue source is recovered at the SN position, with brightness mFW435 =26.76 0.20, mFW555 =26.60 0.23 and mFW625 =26.32 0.19 mag, although there is no detection in a contemporaneous narrow-band Ha image. The spectral energy distribution of the late-time source is well-fit by a stellar-like spectrum (logTeff > 3.7 and log LL > 4), subject to only a small degree of reddening —consistent with that estimated for SN2006jc itself at early-times. The lack of further outbursts after the explosion of SN2006jc suggests that the precursor outburst originated from the progenitor.
    [Show full text]
  • OGLE-2014-SN-131: a Long-Rising Type Ibn Supernova from a Massive Progenitor E
    Astronomy & Astrophysics manuscript no. output c ESO 2017 March 8, 2017 OGLE-2014-SN-131: A long-rising Type Ibn supernova from a massive progenitor E. Karamehmetoglu1, F. Taddia1, J. Sollerman1, Ł. Wyrzykowski2, S. Schmidl3, M. Fraser4, C. Fremling1, J. Greiner5; 6, C. Inserra7, Z. Kostrzewa-Rutkowska2; 8; 9, K. Maguire7, S. Smartt7, M. Sullivan10, and D. R. Young7 1 Department of Astronomy, The Oskar Klein Centre, Stockholm University, AlbaNova, 10691 Stockholm, Sweden. e-mail: [email protected] 2 Warsaw University Astronomical Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland. 3 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany. 4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. 5 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany. 6 Excellence Cluster Universe, Technische Universität München, Boltzmannstrasse 2, 85748 Garching, Germany. 7 Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK. 8 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, the Netherlands. 9 Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, the Netherlands. 10 Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK. Received date / Accepted date ABSTRACT Context. Type Ibn supernovae (SNe Ibn) are thought to be the core-collapse explosions of massive stars whose ejecta interact with He-rich circumstellar material (CSM). Aims. We report the discovery of a SN Ibn, with the longest rise-time ever observed, OGLE-2014-SN-131. We discuss the potential powering mechanisms and the progenitor nature of this peculiar stripped-envelope (SE), circumstellar-interacting SN.
    [Show full text]