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Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born. -
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A&A 454, 527–536 (2006) Astronomy DOI: 10.1051/0004-6361:20053468 & c ESO 2006 Astrophysics A search for photometric variability of hydrogen-deficient planetary-nebula nuclei, J. M. González Pérez1,2, J.-E. Solheim2,3, and R. Kamben2 1 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Institut of Physics, University of Tromsø, 9037 Tromsø, Norway 3 Institut of Theoretical Astrophysics, University of Oslo, PO box 1029 Blindern, 0315 Oslo, Norway Received 18 May 2005 / Accepted 9 March 2006 ABSTRACT Aims. We searched for photometric variability in a sample of hot, hydrogen-deficient planetary nebula nuclei (PNNi) with “PG 1159” or “O VI” spectral type, most of them embedded in a bipolar or elliptical planetary nebula envelope (PNe). These characteristics may indicate the presence of a hidden close companion and an evolution affected by episodes of interaction between them. Methods. We obtained time-series photometry from a sample of 11 candidates using the Nordic Optical Telescope (NOT) with the Andalucía Faint Object Spectrograph and Camera (ALFOSC), modified with our own control software to be able to observe in a high- speed multi-windowing mode. The data were reduced on-line with the real time photometry (RTP) code, which allowed us to detect periodic variable stars with small amplitudes from CCD data in real time. We studied the properties of the observed modulation fre- quencies to investigate their nature. Results. We report the first detection of low-amplitude pulsations in the PNNi VV 47, NGC 6852, and Jn 1. In addition, we investi- gated the photometric variability of NGC 246. -
Planetary Nebulae
Planetary Nebulae A planetary nebula is a kind of emission nebula consisting of an expanding, glowing shell of ionized gas ejected from old red giant stars late in their lives. The term "planetary nebula" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years. The mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energizes the shell of nebulous gas around the central star, appearing as a bright colored planetary nebula at several discrete visible wavelengths. Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances. In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. -
Planetary Nebulae: Exposing the Top Polluters of the ISM
The Evolving ISM in the Milky Way & Nearby Galaxies Planetary Nebulae: Exposing the Top Polluters of the ISM Joseph L. Hora1, Massimo Marengo1, Howard A. Smith1, Luciano Cerrigone1, William B. Latter2 ABSTRACT The high mass loss rates of stars in their asymptotic giant branch (AGB) stage of evolution is one of the most important pathways for mass return from stars to the ISM. In the planetary nebulae (PNe) phase, the ejected material is illuminated and can be altered by the UV radiation from the central star. PNe therefore play a significant role in the ISM recycling process and in changing the environment around them. We show some highlights of the results of observations that have been carried out using the Spitzer instruments to study the gas and dust emission from PNe in the Milky Way and nearby galaxies. Spitzer is especially sensitive to the cool dust and molecules in the PNe shell and halos. We present new results from our program on Galactic PNe, including IRAC and IRS observations of NGC 6720 in the ring and halo of that nebula. Subject headings: galaxies: ISM | infrared: galaxies | infrared: ISM | ISM: dust, extinction | ISM: structure 1. Introduction A key link in the recycling of material to the Interstellar Medium (ISM) is the phase of stellar evolution from Asymptotic Giant Branch (AGB) to white dwarf star. When stars are on the AGB, they begin to lose mass at a prodigious rate. The stars on the AGB are relatively cool, and their atmospheres are a fertile environment for the formation of dust and molecules. -
The Perek-Kohoutek Catalogue of Planetary Nebulae
Perek- Right Catalog Other Declination Kohoutek ascension The Perek-Kohoutek number designation (2000.0) number (2000.0) Catalogue of 1 119+06.1 A 1 0h12.9m 69°11' 2 120+09.1 NGC 40 0h13.0m 72°32' Planetary Nebulae 3 118–08.1 Vy 1–1 0h18.7m 53°53' 4 119+00.1 BV 1 0h19.9m 62°59' Data is from Catalogue of Galactic Planetary 5 119–06.1 Hu 1–1 0h28.3m 55°58' Nebulae, updated version 2000, by L. Kohoutek, 6 120–05.1 Sh 2–176 0h31.8m 57°23' Hamburg-Berfedorf, 2001. 7 108–76.1 BOBN 1 0h37.2m –13°43' 8 121+03.1 We 1–1 0h38.9m 66°23' 9 121+00.1 BV 2 0h40.3m 62°51' 10 122–04.1 A 2 0h45.6m 57°57' 11 118–74.1 NGC 246 0h47.0m –11°53' 12 125–47.1 PHL 932 0h59.9m 15°44' 13 124–07.1 WeSb 1 1h00.9m 55°04' 14 124+02.1 KLSS 2–7 1h02.4m 65°46' 15 124+10.1 EL 0103+73 1h07.1m 73°33' 16 126+03.1 K 3–90 1h24.9m 65°39' 17 128–04.1 S 22 1h30.5m 58°24' 18 130–11.1 M 1–1 1h37.3m 50°28' 19 129–05.1 KLSS 2–8 1h40.1m 56°35' 20 130–10.1 NGC 650–1 1h42.4m 51°34' 21 129–02.1 We 2–5 1h42.6m 60°10' 22 131–05.1 BV 3 1h53.0m 56°25' 23 130+01.1 IC 1747 1h57.6m 63°20' 24 129+04.1 K 3–91 1h58.6m 66°34' 25 148–48.1 GR 0155+10 1h58.0m 10°57' 26 133–08.1 M 1–2 1h58.8m 52°54' 27 130+03.1 K 3–92 2h03.7m 64°57' 28 131+02.1 A 3 2h12.1m 64°09' 29 132+04.1 K 3–93 2h26.5m 65°47' 30 144–15.1 A 4 2h45.4m 42°34' 31 141–07.1 A 5 2h52.3m 50°36' 32 136+04.1 A 6 2h58.7m 64°30' 33 255–59.1 Lo 1 2h57.0m –44°10' 34 136+05.1 HEFE 1 3h03.8m 64°54' 35 138+02.1 IC 289 3h10.3m 61°19' 36 138+04.1 HtDe 2 3h11.0m 62°48' 37 147–09.1 HtWe 3 3h16.6m 46°54' 38 149–09.1 HtDe 3 3h27.2m 45°24' 39 220–53.1 NGC -
Unresolved H Enhancements at High Galactic Latitude In
The Astronomical Journal, 129:927–934, 2005 February # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. UNRESOLVED H ENHANCEMENTS AT HIGH GALACTIC LATITUDE IN THE WHAM SKY SURVEY MAPS R. J. Reynolds, V. Chaudhary, G. J. Madsen, and L. M. Haffner Department of Astronomy, University of Wisconsin, Madison, WI 53706 Receivved 2004 August 23; accepted 2004 October 27 ABSTRACT We have identified 85 regions of enhanced H emission at jbj > 10 subtending approximately 1 or less on the Wisconsin H Mapper (WHAM) sky survey. These high-latitude ‘‘WHAM point sources’’ have H fluxes of 10À11–10À9 ergs cmÀ2 sÀ1, radial velocities within about 70 km sÀ1 of the LSR, and line widths that range from less than 20 to about 80 km sÀ1 (FWHM). Twenty-nine of these enhancements are not identified with either cataloged nebulae or hot stars and appear to have kinematic properties that differ from those observed for planetary nebulae. Another 14 enhancements are near hot evolved low-mass stars that had no previously reported detections of associated nebulosity. The remainder of the enhancements are cataloged planetary nebulae and small, high-latitude H ii regions surrounding massive O and early B stars. Key words: catalogs — H ii regions — planetary nebulae: general — subdwarfs — white dwarfs 1. INTRODUCTION were then selected on the basis of whether the difference spectrum exhibited an emission feature that was significantly The Wisconsin H Mapper (WHAM) has provided the first greater than the scatter in the intensities of the nearest neighbors large-scale survey of the distribution and kinematics of ionized within the velocity range of the feature. -
Primary ID Alternate ID Nickname Con RA 2000 Dec-00 Mag Size Sbr CS Class S.A
Primary ID Alternate ID Nickname Con RA 2000 Dec-00 Mag Size SBr CS Class S.A. Ur. 2 Mill. U2000 PK Desig PN G Desig Henize ESO ARO NGC 40 Caldwell 2 Bowtie Nebula Cep 00h13m01.0s +72°31'19" 10.7 1.0' 19.3 11.6 3b+3 1 8 I-24 I-3 PK 120-9.1 PN G120.0+09.8 NGC 246 Caldwell 56 Skull nebula Cet 00h47m03.3s -11°52'19" 10.4 4.0' 22 11.8 3b 10 140 I-316 II-261 PK 118-74.1 PN G118.8-74.7 NGC 650 M 76 Little Dumbbell Per 01h42m19.9s +51°34'31" 10.1 2.7' 20.9 17.6 3+6 4 29 I-63 I-37 PN G130.9-10.5 IC 1747 Cas 01h57m35.9s +63°19'19" 12 13" 17.3 15.4 3b 1 17 I-34 I-17 PK 130-1.1 PN G130.2+01.3 Abell 4 Per 02h45m23.7s +42°33'05 16.7 22" 23 19.9 3b 4 43 I-100 I-62 PK 144-15.1 PN G144.3-15.5 IC 289 Cas 03h10m19.3s +61°19'01" 12 45" 20 13.3 4+2 1 28 I-45 I-18 PK 138-2.1 PN G138.8+02.8 NGC 1360 M 1-3 Comet Planetary For 03h33m14.6s -25°52'18" 9.4 6.0' 21.9 11.3 3 18 156 I-356 II-312 PN G220.3-53.9 ESO 482-7 IC 351 Per 03h47m33.1s +35°02'49" 11.9 8.0" 16.2 15.6 2a 4 60 I-118 I-95 PK 159-15.1 PN G159.0-15.1 IC 2003 Per 03h56m22.0s +33°52'31 12.6 11.0" 17.5 16.5 2 4 60 I-118 I-95 PK 161-14.1 PN G161.2-14.8 ARO 76 NGC 1501 Oyster Nebula Cam 04h06m59.2s +60°55'14" 12 56" 20.5 11.5 3 1 28 I-43 I-39 PK 144-6.1 PN G144.5+06.5 NGC 1514 Crystal Ball Nebula Tau 04h09m17.0s +30°46'33" 10.8 2.0' 20.9 9.5 3+2 5 60 I-139 I-95 PK 165-15.1 PN G165.5-15.2 NGC 1535 Cleopatra's Eye Eri 04h14m15.8s -12°44'22" 9.4 20" 15.6 15.9 4+2c 11 137 I-306 II-268 PK 206-40.1 PN G206.4-40.5 Sh 2-216 Sharpless 2-216 Per 04h45m00.0s +46°49'00 100' 3 5 42 I-75 I-65 PK 158-0.1 Jonckheere -
Index of First Authors
Cambridge University Press 978-0-521-51489-7 - Astronomical Applications of Astrometry: Ten Years of Exploitation of the Hipparcos Satellite Data Michael Perryman Index More information Index of first authors Aarseth, S. J. 286 Anderson, J. A. 119 Abad, C. 62, 279, 300, 310, 319, 526 Anderson, M. W. B. 130 Abadi, M. G. 527 Andrade, M. 125 Abbett, W. P. 345 Andrei,A.H.30, 60, 579 Abrahamyan, H. V. 228 Andronov, I. L. 170, 171 Abt, H. A. 34, 38, 107, 217, 219, 390, Andronova, A. A. 510 422, 447 Angione, R. J. 133 Acker, A. 454 Anglada Escude,´ G. 207 Adams, W. S. 354 Anguita, C. 255 Adelman-McCarthy, J. K. 74 Ankay, A. 447 Adelman, S. J. 160, 161, 167, 172, 186, 195, 235, 393, 427 Anosova, J. P. 309 Aerts, C. 184–188 Antonello, E. 125, 175, 176, 281, 285, 286 Agekyan, T. A. 303 Antoniucci, S. 358 Aguilar,L.A.279 Antonov, V. A. 584 Aitken, R. G. 97 Aoki, S. 14 Ak, S. 545 Appenzeller, I. 474 Akeson, R. L. 139 Applegate, J. H. 572 Alcaino, G. 547 Arellano Ferro, A. 173, 222 Alcala,´ J. M. 431 Arenou, F. 13, 61, 100, 106, 114, 115, 182, 208–211, 213, Alcobe,´ S. 526 298, 393, 470, 471, 594 Alcock, C. 173, 249, 452, 520 Arfken, G. 508 Alencar, S. H. P. 123, 419 Argus, D. F. 580 Alessi, B. S. 299 Argyle, R. W. 30, 57 Alexander, D. R. 344, 346, 349 Arias, E. F. 9, 69 Alksnis, A. 450 Arifyanto, M. I. 307, 526 Allard, F. -
The Caldwell Catalogue+Photos
The Caldwell Catalogue was compiled in 1995 by Sir Patrick Moore. He has said he started it for fun because he had some spare time after finishing writing up his latest observations of Mars. He looked at some nebulae, including the ones Charles Messier had not listed in his catalogue. Messier was only interested in listing those objects which he thought could be confused for the comets, he also only listed objects viewable from where he observed from in the Northern hemisphere. Moore's catalogue extends into the Southern hemisphere. Having completed it in a few hours, he sent it off to the Sky & Telescope magazine thinking it would amuse them. They published it in December 1995. Since then, the list has grown in popularity and use throughout the amateur astronomy community. Obviously Moore couldn't use 'M' as a prefix for the objects, so seeing as his surname is actually Caldwell-Moore he used C, and thus also known as the Caldwell catalogue. http://www.12dstring.me.uk/caldwelllistform.php Caldwell NGC Type Distance Apparent Picture Number Number Magnitude C1 NGC 188 Open Cluster 4.8 kly +8.1 C2 NGC 40 Planetary Nebula 3.5 kly +11.4 C3 NGC 4236 Galaxy 7000 kly +9.7 C4 NGC 7023 Open Cluster 1.4 kly +7.0 C5 NGC 0 Galaxy 13000 kly +9.2 C6 NGC 6543 Planetary Nebula 3 kly +8.1 C7 NGC 2403 Galaxy 14000 kly +8.4 C8 NGC 559 Open Cluster 3.7 kly +9.5 C9 NGC 0 Nebula 2.8 kly +0.0 C10 NGC 663 Open Cluster 7.2 kly +7.1 C11 NGC 7635 Nebula 7.1 kly +11.0 C12 NGC 6946 Galaxy 18000 kly +8.9 C13 NGC 457 Open Cluster 9 kly +6.4 C14 NGC 869 Open Cluster -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Astrobiology Math
National Aeronautics andSpace Administration Aeronautics National Astrobiology Math This collection of activities is based on a weekly series of space science problems intended for students looking for additional challenges in the math and physical science curriculum in grades 6 through 12. The problems were created to be authentic glimpses of modern science and engineering issues, often involving actual research data. The problems were designed to be one-pagers with a Teacher’s Guide and Answer Key as a second page. This compact form was deemed very popular by participating teachers. Astrobiology Math Mathematical Problems Featuring Astrobiology Applications Dr. Sten Odenwald NASA / ADNET Corp. [email protected] Astrobiology Math i http://spacemath.gsfc.nasa.gov Acknowledgments: We would like to thank Ms. Daniella Scalice for her boundless enthusiasm in the review and editing of this resource. Ms. Scalice is the Education and Public Outreach Coordinator for the NASA Astrobiology Institute (NAI) at the Ames Research Center in Moffett Field, California. We would also like to thank the team of educators and scientists at NAI who graciously read through the first draft of this book and made numerous suggestions for improving it and making it more generally useful to the astrobiology education community: Dr. Harold Geller (George Mason University), Dr. James Kratzer (Georgia Institute of Technology; Doyle Laboratory) and Ms. Suzi Taylor (Montana State University), For more weekly classroom activities about astronomy and space visit the Space Math@ NASA website, http://spacemath.gsfc.nasa.gov Image Credits: Front Cover: Collage created by Julie Fletcher (NAI), molecule image created by Jenny Mottar, NASA HQ. -
The N2K Consortium VI: Doppler Shifts Without Templates and Three
The N2K Consortium VI: Doppler Shifts Without Templates and Three New Short–Period Planets 1 John Asher Johnson2, Geoffrey W. Marcy2, Debra A. Fischer3, Gregory Laughlin4, R. Paul Butler5, Gregory W. Henry6, Jeff A. Valenti7, Eric B. Ford2, Steven S. Vogt4, Jason T. Wright2 [email protected] ABSTRACT We present a modification to the iodine cell Doppler technique that eliminates the need for an observed stellar template spectrum. For a given target star, we iterate toward a synthetic template spectrum beginning with an existing spec- trum of a similar star. We then perturb the shape of this first–guess template to match the program observation of the target star taken through an iodine cell. The elimination of a separate template observation saves valuable telescope time, a feature that is ideally suited for the quick–look strategy employed by the “Next 2000 Stars” (N2K) planet search program. Tests using Keck/HIRES spec- tra indicate that synthetic templates yield a short–term precision of3ms−1 and a long–term, run–to–run precision of 5 m s−1. We used this new Doppler tech- nique to discover three new planets: a 1.50 MJup planet in a 2.1375 d orbit around HD 86081; a 0.71 MJup planet in circular, 26.73 d orbit around HD 224693; and a Saturn–mass planet in an 18.179 d orbit around HD 33283. The remarkably short period of HD 86081b bridges the gap between the extremely short–period planets detected in the OGLE survey and the 16 Doppler–detected hot jupiters arXiv:astro-ph/0604348v2 22 May 2006 1Based on observations obtained at the W.