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Arxiv:1612.03165V3 [Astro-Ph.HE] 12 Sep 2017 – 2 –
The second catalog of flaring gamma-ray sources from the Fermi All-sky Variability Analysis S. Abdollahi1, M. Ackermann2, M. Ajello3;4, A. Albert5, L. Baldini6, J. Ballet7, G. Barbiellini8;9, D. Bastieri10;11, J. Becerra Gonzalez12;13, R. Bellazzini14, E. Bissaldi15, R. D. Blandford16, E. D. Bloom16, R. Bonino17;18, E. Bottacini16, J. Bregeon19, P. Bruel20, R. Buehler2;21, S. Buson12;22, R. A. Cameron16, M. Caragiulo23;15, P. A. Caraveo24, E. Cavazzuti25, C. Cecchi26;27, A. Chekhtman28, C. C. Cheung29, G. Chiaro11, S. Ciprini25;26, J. Conrad30;31;32, D. Costantin11, F. Costanza15, S. Cutini25;26, F. D'Ammando33;34, F. de Palma15;35, A. Desai3, R. Desiante17;36, S. W. Digel16, N. Di Lalla6, M. Di Mauro16, L. Di Venere23;15, B. Donaggio10, P. S. Drell16, C. Favuzzi23;15, S. J. Fegan20, E. C. Ferrara12, W. B. Focke16, A. Franckowiak2, Y. Fukazawa1, S. Funk37, P. Fusco23;15, F. Gargano15, D. Gasparrini25;26, N. Giglietto23;15, M. Giomi2;59, F. Giordano23;15, M. Giroletti33, T. Glanzman16, D. Green13;12, I. A. Grenier7, J. E. Grove29, L. Guillemot38;39, S. Guiriec12;22, E. Hays12, D. Horan20, T. Jogler40, G. J´ohannesson41, A. S. Johnson16, D. Kocevski12;42, M. Kuss14, G. La Mura11, S. Larsson43;31, L. Latronico17, J. Li44, F. Longo8;9, F. Loparco23;15, M. N. Lovellette29, P. Lubrano26, J. D. Magill13, S. Maldera17, A. Manfreda6, M. Mayer2, M. N. Mazziotta15, P. F. Michelson16, W. Mitthumsiri45, T. Mizuno46, M. E. Monzani16, A. Morselli47, I. V. Moskalenko16, M. Negro17;18, E. Nuss19, T. Ohsugi46, N. Omodei16, M. Orienti33, E. -
Limits from the Hubble Space Telescope on a Point Source in SN 1987A
Limits from the Hubble Space Telescope on a Point Source in SN 1987A The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Graves, Genevieve J. M., Peter M. Challis, Roger A. Chevalier, Arlin Crotts, Alexei V. Filippenko, Claes Fransson, Peter Garnavich, et al. 2005. “Limits from the Hubble Space Telescopeon a Point Source in SN 1987A.” The Astrophysical Journal 629 (2): 944–59. https:// doi.org/10.1086/431422. Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:41399924 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Other Posted Material, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#LAA The Astrophysical Journal, 629:944–959, 2005 August 20 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. LIMITS FROM THE HUBBLE SPACE TELESCOPE ON A POINT SOURCE IN SN 1987A Genevieve J. M. Graves,1, 2 Peter M. Challis,2 Roger A. Chevalier,3 Arlin Crotts,4 Alexei V. Filippenko,5 Claes Fransson,6 Peter Garnavich,7 Robert P. Kirshner,2 Weidong Li,5 Peter Lundqvist,6 Richard McCray,8 Nino Panagia,9 Mark M. Phillips,10 Chun J. S. Pun,11,12 Brian P. Schmidt,13 George Sonneborn,11 Nicholas B. Suntzeff,14 Lifan Wang,15 and J. Craig Wheeler16 Received 2005 January 27; accepted 2005 April 26 ABSTRACT We observed supernova 1987A (SN 1987A) with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST ) in 1999 September and again with the Advanced Camera for Surveys (ACS) on the HST in 2003 November. -
A Dozen Colliding Wind X-Ray Binaries in the Star Cluster R 136 in the 30 Doradus Region
A dozen colliding wind X-ray binaries in the star cluster R 136 in the 30 Doradus region Simon F. Portegies Zwart?,DavidPooley,Walter,H.G.Lewin Massachusetts Institute of Technology, Cambridge, MA 02139, USA ? Hubble Fellow Subject headings: stars: early-type — tars: Wolf-Rayet — galaxies:) Magellanic Clouds — X-rays: stars — X-rays: binaries — globular clusters: individual (R136) –2– ABSTRACT We analyzed archival Chandra X-ray observations of the central portion of the 30 Doradus region in the Large Magellanic Cloud. The image contains 20 32 35 1 X-ray point sources with luminosities between 5 10 and 2 10 erg s− (0.2 × × — 3.5 keV). A dozen sources have bright WN Wolf-Rayet or spectral type O stars as optical counterparts. Nine of these are within 3:4 pc of R 136, the ∼ central star cluster of NGC 2070. We derive an empirical relation between the X-ray luminosity and the parameters for the stellar wind of the optical counterpart. The relation gives good agreement for known colliding wind binaries in the Milky Way Galaxy and for the identified X-ray sources in NGC 2070. We conclude that probably all identified X-ray sources in NGC 2070 are colliding wind binaries and that they are not associated with compact objects. This conclusion contradicts Wang (1995) who argued, using ROSAT data, that two earlier discovered X-ray sources are accreting black-hole binaries. Five early type stars in R 136 are not bright in X-rays, possibly indicating that they are either: single stars or have a low mass companion or a wide orbit. -
Kaluza-Klein Gravity, Concentrating on the General Rel- Ativity, Rather Than Particle Physics Side of the Subject
Kaluza-Klein Gravity J. M. Overduin Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, Victoria, British Columbia, Canada, V8W 3P6 and P. S. Wesson Department of Physics, University of Waterloo, Ontario, Canada N2L 3G1 and Gravity Probe-B, Hansen Physics Laboratories, Stanford University, Stanford, California, U.S.A. 94305 Abstract We review higher-dimensional unified theories from the general relativity, rather than the particle physics side. Three distinct approaches to the subject are identi- fied and contrasted: compactified, projective and noncompactified. We discuss the cosmological and astrophysical implications of extra dimensions, and conclude that none of the three approaches can be ruled out on observational grounds at the present time. arXiv:gr-qc/9805018v1 7 May 1998 Preprint submitted to Elsevier Preprint 3 February 2008 1 Introduction Kaluza’s [1] achievement was to show that five-dimensional general relativity contains both Einstein’s four-dimensional theory of gravity and Maxwell’s the- ory of electromagnetism. He however imposed a somewhat artificial restriction (the cylinder condition) on the coordinates, essentially barring the fifth one a priori from making a direct appearance in the laws of physics. Klein’s [2] con- tribution was to make this restriction less artificial by suggesting a plausible physical basis for it in compactification of the fifth dimension. This idea was enthusiastically received by unified-field theorists, and when the time came to include the strong and weak forces by extending Kaluza’s mechanism to higher dimensions, it was assumed that these too would be compact. This line of thinking has led through eleven-dimensional supergravity theories in the 1980s to the current favorite contenders for a possible “theory of everything,” ten-dimensional superstrings. -
Giant H II Regions in the Merging System NGC 3256: Are They the Birthplaces of Globular Clusters?
CORE Metadata, citation and similar papers at core.ac.uk Provided by CERN Document Server Paper I: To be submitted to A.J. Giant H II regions in the merging system NGC 3256: Are they the birthplaces of globular clusters? J. English University of Manitoba K.C. Freeman Research School of Astronomy and Astrophysics, The Australian National University ABSTRACT CCD images and spectra of ionized hydrogen in the merging system NGC3256 were acquired as part of a kinematic study to investigate the formation of globular clusters (GC) during the interactions and mergers of disk galaxies. This paper focuses on the proposition by Kennicutt & Chu (1988) that giant H II regions, with an Hα luminosity > 1:5 1040 erg s 1, are birthplaces of young populous clusters (YPC’s ). × − Although NGC 3256 has relatively few (7) giant H II complexes, compared to some other interacting systems, these regions are comparable in total flux to about 85 30- Doradus-like H II regions (30-Dor GHR’s). The bluest, massive YPC’s (Zepf et al. 1999) are located in the vicinity of observed 30-Dor GHR’s, contributing to the notion that some fraction of 30-Dor GHR’s do cradle massive YPC’s, as 30 Dor harbors R136. If interactions induce the formation of 30-Dor GHR’s, the observed luminosities indi- cate that almost 900 30-Dor GHR’s would form in NGC 3256 throughout its merger epoch. In order for 30-Dor GHR’s to be considered GC progenitors, this number must be consistent with the specific frequencies of globular clusters estimated for elliptical galaxies formed via mergers of spirals (Ashman & Zepf 1993). -
What Is Gravity Probe B? a Quest for Experimental Truth the GP-B Flight
What is Gravity Probe B? than Gravity Probe B. It’s just a star, a telescope, and a spinning sphere.” However, it took the exceptional collaboration of Stanford, Gravity Probe B (GP-B) is a NASA physics mission to experimentally MSFC, Lockheed Martin and a host of others more than four decades investigate Einstein’s 1916 general theory of relativity—his theory of gravity. to develop the ultra-precise gyroscopes and the other cutting- GP-B uses four spherical gyroscopes and a telescope, housed in a satellite edge technologies necessary to carry out this “simple” experiment. orbiting 642 km (400 mi) above the Earth, to measure, with unprecedented accuracy, two extraordinary effects predicted by the general theory of rela- The GP-B Flight Mission & Data Analysis tivity: 1) the geodetic effect—the amount by which the Earth warps the local spacetime in which it resides; and 2) the frame-dragging effect—the amount On April 20, 2004 at 9:57:24 AM PDT, a crowd of over 2,000 current and by which the rotating Earth drags its local spacetime around with it. GP-B former GP-B team members and supporters watched and cheered as the tests these two effects by precisely measuring the precession (displacement) GP-B spacecraft lifted off from Vandenberg Air Force Base. That emotionally angles of the spin axes of the four gyros over the course of a year and com- overwhelming day, culminating with the extraordinary live video of paring these experimental results with predictions from Einstein’s theory. the spacecraft separating from the second stage booster meant, as GP-B Program Manager Gaylord Green put it, “that 10,000 things went right.” A Quest for Experimental Truth Once in orbit, the spacecraft first underwent a four-month Initialization The idea of testing general relativity with orbiting gyroscopes was sug- and Orbit Checkout (IOC), in which all systems and instruments were gested independently by two physicists, George Pugh and Leonard Schiff, initialized, tested, and optimized for the data collection to follow. -
SEER for Hardware's Cost Model for Future Orbital Concepts (“FAR OUT”)
Presented at the 2008 SCEA-ISPA Joint Annual Conference and Training Workshop - www.iceaaonline.com SEER for Hardware’s Cost Model for Future Orbital Concepts (“FAR OUT”) Lee Fischman ISPA/SCEA Industry Hills 2008 Presented at the 2008 SCEA-ISPA Joint Annual Conference and Training Workshop - www.iceaaonline.com Introduction A model for predicting the cost of long term unmanned orbital spacecraft (Far Out) has been developed at the request of AFRL. Far Out has been integrated into SEER for Hardware. This presentation discusses the Far Out project and resulting model. © 2008 Galorath Incorporated Presented at the 2008 SCEA-ISPA Joint Annual Conference and Training Workshop - www.iceaaonline.com Goals • Estimate space satellites in any earth orbit. Deep space exploration missions may be considered as data is available, or may be an area for further research in Phase 3. • Estimate concepts to be launched 10-20 years into the future. • Cost missions ranging from exploratory to strategic, with a specific range decided based on estimating reliability. The most reliable estimates are likely to be in the middle of this range. • Estimates will include hardware, software, systems engineering, and production. • Handle either government or commercial missions, either “one-of-a-kind” or constellations. • Be used in a “top-down” manner using relatively less specific mission resumes, similar to those available from sources such as the Earth Observation Portal or Janes Space Directory. © 2008 Galorath Incorporated Presented at the 2008 SCEA-ISPA Joint Annual Conference and Training Workshop - www.iceaaonline.com Challenge: Technology Change Over Time Evolution in bus technologies Evolution in payload technologies and performance 1. -
The NTT Provides the Deepest Look Into Space 6
The NTT Provides the Deepest Look Into Space 6. A. PETERSON, Mount Stromlo Observatory,Australian National University, Canberra S. D'ODORICO, M. TARENGHI and E. J. WAMPLER, ESO The ESO New Technology Telescope r on La Silla has again proven its extraor- - dinary abilities. It has now produced the "deepest" view into the distant regions of the Universe ever obtained with ground- or space-based telescopes. Figure 1 : This picture is a reproduction of a I.1 x 1.1 arcmin portion of a composite im- age of forty-one 10-minute exposures in the V band of a field at high galactic latitude in the constellation of Sextans (R.A. loh 45'7 Decl. -0' 143. The individual images were obtained with the EMMI imager/spectrograph at the Nas- myth focus of the ESO 3.5-m New Technolo- gy Telescope using a 1000 x 1000 pixel Thomson CCD. This combination gave a full field of 7.6 x 7.6 arcmin and a pixel size of 0.44 arcsec. The average seeing during these exposures was 1.0 arcsec. The telescope was offset between the indi- vidual exposures so that the sky background could be used to flat-field the frame. This procedure also removed the effects of cos- mic rays and blemishes in the CCD. More than 97% of the objects seen in this sub- field are galaxies. For the brighter galax- ies, there is good agreement between the galaxy counts of Tyson (1988, Astron. J., 96, 1) and the NTT counts for the brighter galax- ies. -
Arxiv:0809.1275V2
How eccentric orbital solutions can hide planetary systems in 2:1 resonant orbits Guillem Anglada-Escud´e1, Mercedes L´opez-Morales1,2, John E. Chambers1 [email protected], [email protected], [email protected] ABSTRACT The Doppler technique measures the reflex radial motion of a star induced by the presence of companions and is the most successful method to detect ex- oplanets. If several planets are present, their signals will appear combined in the radial motion of the star, leading to potential misinterpretations of the data. Specifically, two planets in 2:1 resonant orbits can mimic the signal of a sin- gle planet in an eccentric orbit. We quantify the implications of this statistical degeneracy for a representative sample of the reported single exoplanets with available datasets, finding that 1) around 35% percent of the published eccentric one-planet solutions are statistically indistinguishible from planetary systems in 2:1 orbital resonance, 2) another 40% cannot be statistically distinguished from a circular orbital solution and 3) planets with masses comparable to Earth could be hidden in known orbital solutions of eccentric super-Earths and Neptune mass planets. Subject headings: Exoplanets – Orbital dynamics – Planet detection – Doppler method arXiv:0809.1275v2 [astro-ph] 25 Nov 2009 Introduction Most of the +300 exoplanets found to date have been discovered using the Doppler tech- nique, which measures the reflex motion of the host star induced by the planets (Mayor & Queloz 1995; Marcy & Butler 1996). The diverse characteristics of these exoplanets are somewhat surprising. Many of them are similar in mass to Jupiter, but orbit much closer to their 1Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Rd. -
A Review on Substellar Objects Below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs Or What?
geosciences Review A Review on Substellar Objects below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs or What? José A. Caballero Centro de Astrobiología (CSIC-INTA), ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Madrid, Spain; [email protected] Received: 23 August 2018; Accepted: 10 September 2018; Published: 28 September 2018 Abstract: “Free-floating, non-deuterium-burning, substellar objects” are isolated bodies of a few Jupiter masses found in very young open clusters and associations, nearby young moving groups, and in the immediate vicinity of the Sun. They are neither brown dwarfs nor planets. In this paper, their nomenclature, history of discovery, sites of detection, formation mechanisms, and future directions of research are reviewed. Most free-floating, non-deuterium-burning, substellar objects share the same formation mechanism as low-mass stars and brown dwarfs, but there are still a few caveats, such as the value of the opacity mass limit, the minimum mass at which an isolated body can form via turbulent fragmentation from a cloud. The least massive free-floating substellar objects found to date have masses of about 0.004 Msol, but current and future surveys should aim at breaking this record. For that, we may need LSST, Euclid and WFIRST. Keywords: planetary systems; stars: brown dwarfs; stars: low mass; galaxy: solar neighborhood; galaxy: open clusters and associations 1. Introduction I can’t answer why (I’m not a gangstar) But I can tell you how (I’m not a flam star) We were born upside-down (I’m a star’s star) Born the wrong way ’round (I’m not a white star) I’m a blackstar, I’m not a gangstar I’m a blackstar, I’m a blackstar I’m not a pornstar, I’m not a wandering star I’m a blackstar, I’m a blackstar Blackstar, F (2016), David Bowie The tenth star of George van Biesbroeck’s catalogue of high, common, proper motion companions, vB 10, was from the end of the Second World War to the early 1980s, and had an entry on the least massive star known [1–3]. -
The Messenger
THE MESSENGER No, 40 - June 1985 Radial Veloeities of Stars in Globular Clusters: a Look into CD Cen and 47 Tue M. Mayor and G. Meylan, Geneva Observatory, Switzerland Subjected to dynamical investigations since the beginning photometry of several clusters reveals a cusp in the luminosity of the century, globular clusters still provide astrophysicists function of the central region, which could be the first evidence with theoretical and observational problems, wh ich so far have for collapsed cores. only been partly solved. The development of photoelectric cross-corelation tech If for a long time the star density projected on the sky was niques for the determination of stellar radial velocities opened fairly weil represented by simple dynamical models, recent the door to kinematical investigations (Gunn and Griffin, 1979, N .~- .", '. '.'., .' 1 '&307 w E ,. 1~ S Fig. 1: Left: 47 Tue (NGC 104) from the Deep Blue Survey - SRC-(J). Right: Centre of 47 Tue from a near-infrared photometrie study of Lioyd Evans. The diameter ofthe large eirele eorresponds to the disk ofthe left photograph. The maximum ofthe rotation appears inside the eircle; the linear part of the rotation eurve (solid-body rotation) affeets only stars inside one areminute of the eentre. 1 Rlre J 250r;.' .;r2' -i4.:...__.....;6;.;.. .;rB. ,;.;10::....--. Tentative Time-table of Council Sessions (J lkm/5] and Committee Meetings in 1985 (.) Gen x =2. November 12 Scientific Technical Committee November 13-14 Finance Committee December 11 -12 Observing Programmes Committee December 16 Committee of Council December 17 Council 10. All meetings will take place at ESO in Garching. -
Cfa in the News ~ Week Ending 3 January 2010
Wolbach Library: CfA in the News ~ Week ending 3 January 2010 1. New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 2. 2009 in science and medicine, ROGER SCHLUETER, Belleville News Democrat (IL), Sunday, January 3, 2010 3. 'Science, celestial bodies have always inspired humankind', Staff Correspondent, Hindu (India), Tuesday, December 29, 2009 4. Why is Carpenter defending scientists?, The Morning Call, Morning Call (Allentown, PA), FIRST ed, pA25, Sunday, December 27, 2009 5. CORRECTIONS, OPINION BY RYAN FINLEY, ARIZONA DAILY STAR, Arizona Daily Star (AZ), FINAL ed, pA2, Saturday, December 19, 2009 6. We see a 'Super-Earth', TOM BEAL; TOM BEAL, ARIZONA DAILY STAR, Arizona Daily Star, (AZ), FINAL ed, pA1, Thursday, December 17, 2009 Record - 1 DIALOG(R) New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 TEXT: "In this paper we report on testing the 'rolen model' and 'opportunity-structure' hypotheses about the parents whom scientists mentioned as career influencers. According to the role-model hypothesis, the gender match between scientist and influencer is paramount (for example, women scientists would disproportionately often mention their mothers as career influencers)," scientists writing in the journal Social Studies of Science report (see also ). "According to the opportunity-structure hypothesis, the parent's educational level predicts his/her probability of being mentioned as a career influencer (that ism parents with higher educational levels would be more likely to be named). The examination of a sample of American scientists who had received prestigious postdoctoral fellowships resulted in rejecting the role-model hypothesis and corroborating the opportunity-structure hypothesis.