Catálogo de publicaciones - revistas
Título de Acceso Abierto
The Astrophysical Journal (ApJ)
Resumen/Descripción – provisto por la editorial en inglés
The Astrophysical Journal is an open access journal devoted to recent developments, discoveries, and theories in astronomy and astrophysics. Publications in ApJ constitute significant new research that is directly relevant to astrophysical applications, whether based on observational results or on theoretical insights or modeling.Palabras clave – provistas por la editorial
astronomy; astrophysics
Disponibilidad
| Institución detectada | Período | Navegá | Descargá | Solicitá |
|---|---|---|---|---|
| No detectada | desde jul. 1995 / hasta dic. 2023 | IOPScience |
Información
Tipo de recurso:
revistas
ISSN impreso
0004-637X
ISSN electrónico
1538-4357
Editor responsable
American Astronomical Society (AAS)
Idiomas de la publicación
- inglés
País de edición
Reino Unido
Información sobre licencias CC
Cobertura temática
Tabla de contenidos
Constraints on Optical Emission of FAST-detected FRB 20181130B with GWAC Synchronized Observations
L. P. Xin; H. L. Li; J. Wang
; X. H. Han; Y. L. Qiu; H. B. Cai; C. H. Niu; X. M. Lu; E. W. Liang; Z. G. Dai; X. G. Wang; X. Y. Wang; L. Huang; C. Wu; G. W. Li; Q. C. Feng; J. S. Deng; S. S. Sun; Y. G. Yang; J. Y. Wei
<jats:title>Abstract</jats:title> <jats:p>Multiwavelength simultaneous observations are essential to the constraints on the origin of fast radio bursts (FRBs). However, it is a significant observational challenge due to the nature of FRBs as transients with a radio millisecond duration, which occur randomly in the sky regardless of time and position. Here, we report the search for short-time fast optical bursts in the Ground-based Wide Angle Camera (GWAC) archived data associated with FRB 20181130B, which were detected by the Five-hundred-meter Aperture Spherical radio Telescope and recently reported. No new credible sources were detected in all single GWAC images with an exposure time of 10 s, including images with coverage of the expected arrival time in optical wavelength by taking the high dispersion measurements into account. Our results provide a limiting magnitude of 15.43 ± 0.04 mag in the <jats:italic>R</jats:italic> band, corresponding to a flux density of 1.66 Jy or 8.35 mag in AB system by assuming that the duration of the optical band is similar to that of the radio band of about 10 ms. This limiting magnitude makes the spectral index of <jats:italic>α</jats:italic> < 0.367 from optical to radio wavelength. The possible existence of longer-duration optical emission was also investigated with upper limits of 0.33 Jy (10.10 mag), 1.74 mJy (15.80 mag), and 0.16 mJy (18.39 mag) for the durations of 50 ms, 10 s, and 6060 s, respectively. This undetected scenario could be partially attributed to the shallow detection capability, as well as the high inferred distance of FRB 20181130B and the low fluence in radio wavelength. The future detectability of optical flashes associated with nearby and bright FRBs are also discussed in this paper.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 78
The Astrophysical Variance in Gaia–Radial Velocity Spectrometer Spectra
Rayna Rampalli; Melissa Ness; Shola Wylie
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 78
Dynamically Driven Inflow onto the Galactic Center and its Effect upon Molecular Clouds
H Perry Hatchfield; Mattia C. Sormani; Robin G. Tress; Cara Battersby; Rowan J. Smith; Simon C. O. Glover; Ralf S. Klessen
<jats:title>Abstract</jats:title> <jats:p>The Galactic bar plays a critical role in the evolution of the Milky Way’s Central Molecular Zone (CMZ), driving gas toward the Galactic Center via gas flows known as dust lanes. To explore the interaction between the CMZ and the dust lanes, we run hydrodynamic simulations in <jats:sc>arepo</jats:sc>, modeling the potential of the Milky Way’s bar in the absence of gas self-gravity and star formation physics, and we study the flows of mass using Monte Carlo tracer particles. We estimate the efficiency of the inflow via the dust lanes, finding that only about a third (30% ± 12%) of the dust lanes’ mass initially accretes onto the CMZ, while the rest overshoots and accretes later. Given observational estimates of the amount of gas within the Milky Way’s dust lanes, this suggests that the true total inflow rate onto the CMZ is 0.8 ± 0.6 <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> yr<jats:sup>−1</jats:sup>. Clouds in this simulated CMZ have sudden peaks in their average density near the apocenter, where they undergo violent collisions with inflowing material. While these clouds tend to counter-rotate due to shear, co-rotating clouds occasionally occur due to the injection of momentum from collisions with inflowing material (∼52% are strongly counter-rotating, and ∼7% are strongly co-rotating of the 44 cloud sample). We investigate the formation and evolution of these clouds, finding that they are fed by many discrete inflow events, providing a consistent source of gas to CMZ clouds even as they collapse and form stars.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 79
Differential Source Count for Gamma-Ray Bursts
Shreya Banerjee; David Eichler; Dafne Guetta
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 79
The Flare and Warp of the Young Stellar Disk Traced with LAMOST DR5 OB-type Stars
Yang Yu; Hai-Feng Wang; Wen-Yuan Cui; Lin-Lin Li; Chao Liu; Bo Zhang; Hao Tian; Zhen-Yan Huo; Jie Ju; Zhi-Cun Liu; Fang Wen; Shuai Feng
<jats:title>Abstract</jats:title> <jats:p>We present an analysis of the spatial density structure for the outer disk from 8–14 kpc with the LAMOST DR5 13,534 OB-type stars and observe similar flaring on the north and south sides of the disk, implying that the flaring structure is symmetrical about the Galactic plane, for which the scale height at different Galactocentric distances is from 0.14 to 0.5 kpc. By using the average slope to characterize the flaring strength, we find that the thickness of the OB stellar disk is similar but that flaring is slightly stronger compared to the thin disk as traced by red giant branch stars, possibly implying that secular evolution is not the main contributor to the flaring but rather perturbation scenarios such as interactions with passing dwarf galaxies could be possible. When comparing the scale height of the OB stellar disk on the north and south sides with the gas disk, the former one is slightly thicker than the latter one by ≈33 and 9 pc, meaning that one could tentatively use young OB-type stars to trace the gas properties. Meanwhile, we determine that the radial scale length of the young OB stellar disk is 1.17 ± 0.05 kpc, which is shorter than that of the gas disk, confirming that the gas disk is more extended than the stellar disk. What is more, by considering the midplane displacements (<jats:italic>Z</jats:italic> <jats:sub>0</jats:sub>) in our density model we find that almost all values of <jats:italic>Z</jats:italic> <jats:sub>0</jats:sub> are within 100 pc, with an increasing trend as Galactocentric distance increases.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 80
Searches for Continuous Gravitational Waves from Young Supernova Remnants in the Early Third Observing Run of Advanced LIGO and Virgo
R. Abbott; T. D. Abbott; S. Abraham; F. Acernese; K. Ackley; A. Adams; C. Adams; R. X. Adhikari; V. B. Adya; C. Affeldt; D. Agarwal; M. Agathos; K. Agatsuma; N. Aggarwal; O. D. Aguiar; L. Aiello; A. Ain; P. Ajith; T. Akutsu; K. M. Aleman; G. Allen; A. Allocca; P. A. Altin; A. Amato; S. Anand; A. Ananyeva; S. B. Anderson; W. G. Anderson; M. Ando; S. V. Angelova; S. Ansoldi; J. M. Antelis; S. Antier; S. Appert; Koya Arai; Koji Arai; Y. Arai; S. Araki; A. Araya; M. C. Araya; J. S. Areeda; M. Arène; N. Aritomi; N. Arnaud; S. M. Aronson; K. G. Arun; H. Asada; Y. Asali; G. Ashton; Y. Aso; S. M. Aston; P. Astone; F. Aubin; P. Aufmuth; K. AultONeal; C. Austin; S. Babak; F. Badaracco; M. K. M. Bader; S. Bae; Y. Bae; A. M. Baer; S. Bagnasco; Y. Bai; L. Baiotti; J. Baird; R. Bajpai; M. Ball; G. Ballardin; S. W. Ballmer; M. Bals; A. Balsamo; G. Baltus; S. Banagiri; D. Bankar; R. S. Bankar; J. C. Barayoga; C. Barbieri; B. C. Barish; D. Barker; P. Barneo; F. Barone; B. Barr; L. Barsotti; M. Barsuglia; D. Barta; J. Bartlett; M. A. Barton; I. Bartos; R. Bassiri; A. Basti; M. Bawaj; J. C. Bayley; A. C. Baylor; M. Bazzan; B. Bécsy; V. M. Bedakihale; M. Bejger; I. Belahcene; V. Benedetto; D. Beniwal; M. G. Benjamin; T. F. Bennett; J. D. Bentley; M. BenYaala; F. Bergamin; B. K. Berger; S. Bernuzzi; D. Bersanetti; A. Bertolini; J. Betzwieser; R. Bhandare; A. V. Bhandari; D. Bhattacharjee; S. Bhaumik; J. Bidler; I. A. Bilenko; G. Billingsley; R. Birney; O. Birnholtz; S. Biscans; M. Bischi; S. Biscoveanu; A. Bisht; B. Biswas; M. Bitossi; M.-A. Bizouard; J. K. Blackburn; J. Blackman; C. D. Blair; D. G. Blair; R. M. Blair; F. Bobba; N. Bode; M. Boer; G. Bogaert; M. Boldrini; F. Bondu; E. Bonilla; R. Bonnand; P. Booker; B. A. Boom; R. Bork; V. Boschi; N. Bose; S. Bose; V. Bossilkov; V. Boudart; Y. Bouffanais; A. Bozzi; C. Bradaschia; P. R. Brady; A. Bramley; A. Branch; M. Branchesi; J. E. Brau; M. Breschi; T. Briant; J. H. Briggs; A. Brillet; M. Brinkmann; P. Brockill; A. F. Brooks; J. Brooks; D. D. Brown; S. Brunett; G. Bruno; R. Bruntz; J. Bryant; A. Buikema; T. Bulik; H. J. Bulten; A. Buonanno; R. Buscicchio; D. Buskulic; R. L. Byer; L. Cadonati; M. Caesar; G. Cagnoli; C. Cahillane; H. W. Cain III; J. Calderón Bustillo; J. D. Callaghan; T. A. Callister; E. Calloni; J. B. Camp; M. Canepa; M. Cannavacciuolo; K. C. Cannon; H. Cao; J. Cao; Z. Cao; E. Capocasa; E. Capote; G. Carapella; F. Carbognani; J. B. Carlin; M. F. Carney; M. Carpinelli; G. Carullo; T. L. Carver; J. Casanueva Diaz; C. Casentini; G. Castaldi; S. Caudill; M. Cavaglià; F. Cavalier; R. Cavalieri; G. Cella; P. Cerdá-Durán; E. Cesarini; W. Chaibi; K. Chakravarti; B. Champion; C.-H. Chan; C. Chan; C. L. Chan; M. Chan; K. Chandra; P. Chanial; S. Chao; P. Charlton; E. A. Chase; E. Chassande-Mottin; D. Chatterjee; M. Chaturvedi; A. Chen; C. Chen; H. Y. Chen; J. Chen; K. Chen; X. Chen; Y.-B. Chen; Y.-R. Chen; Z. Chen; H. Cheng; C. K. Cheong; H. Y. Cheung; H. Y. Chia; F. Chiadini; C-Y. Chiang; R. Chierici; A. Chincarini; M. L. Chiofalo; A. Chiummo; G. Cho; H. S. Cho; S. Choate; R. K. Choudhary; S. Choudhary; N. Christensen; H. Chu; Q. Chu; Y-K. Chu; S. Chua; K. W. Chung; G. Ciani; P. Ciecielag; M. Cieślar; M. Cifaldi; A. A. Ciobanu; R. Ciolfi; F. Cipriano; A. Cirone; F. Clara; E. N. Clark; J. A. Clark; L. Clarke; P. Clearwater; S. Clesse; F. Cleva; E. Coccia; P.-F. Cohadon; D. E. Cohen; L. Cohen; M. Colleoni; C. G. Collette; M. Colpi; C. M. Compton; M. Constancio Jr.; L. Conti; S. J. Cooper; P. Corban; T. R. Corbitt; I. Cordero-Carrión; S. Corezzi; K. R. Corley; N. Cornish; D. Corre; A. Corsi; S. Cortese; C. A. Costa; R. Cotesta; M. W. Coughlin; S. B. Coughlin; J.-P. Coulon; S. T. Countryman; B. Cousins; P. Couvares; P. B. Covas; D. M. Coward; M. J. Cowart; D. C. Coyne; R. Coyne; J. D. E. Creighton; T. D. Creighton; A. W. Criswell; M. Croquette; S. G. Crowder; J. R. Cudell; T. J. Cullen; A. Cumming; R. Cummings; E. Cuoco; M. Curyło; T. Dal Canton; G. Dálya; A. Dana; L. M. DaneshgaranBajastani; B. D’Angelo; S. L. Danilishin; S. D’Antonio; K. Danzmann; C. Darsow-Fromm; A. Dasgupta; L. E. H. Datrier; V. Dattilo; I. Dave; M. Davier; G. S. Davies; D. Davis; E. J. Daw; R. Dean; D. DeBra; M. Deenadayalan; J. Degallaix; M. De Laurentis; S. Deléglise; V. Del Favero; F. De Lillo; N. De Lillo; W. Del Pozzo; L. M. DeMarchi; F. De Matteis; V. D’Emilio; N. Demos; T. Dent; A. Depasse; R. De Pietri; R. De Rosa; C. De Rossi; R. DeSalvo; R. De Simone; S. Dhurandhar; M. C. Díaz; M. Diaz-Ortiz Jr.; N. A. Didio; T. Dietrich; L. Di Fiore; C. Di Fronzo; C. Di Giorgio; F. Di Giovanni; T. Di Girolamo; A. Di Lieto; B. Ding; S. Di Pace; I. Di Palma; F. Di Renzo; A. K. Divakarla; A. Dmitriev; Z. Doctor; L. D’Onofrio; F. Donovan; K. L. Dooley; S. Doravari; I. Dorrington; M. Drago; J. C. Driggers; Y. Drori; Z. Du; J.-G. Ducoin; P. Dupej; O. Durante; D. D’Urso; P.-A. Duverne; S. E. Dwyer; P. J. Easter; M. Ebersold; G. Eddolls; B. Edelman; T. B. Edo; O. Edy; A. Effler; S. Eguchi; J. Eichholz; S. S. Eikenberry; M. Eisenmann; R. A. Eisenstein; A. Ejlli; Y. Enomoto; L. Errico; R. C. Essick; H. Estellés; D. Estevez; Z. Etienne; T. Etzel; M. Evans; T. M. Evans; B. E. Ewing; V. Fafone; H. Fair; S. Fairhurst; X. Fan; A. M. Farah; S. Farinon; B. Farr; W. M. Farr; N. W. Farrow; E. J. Fauchon-Jones; M. Favata; M. Fays; M. Fazio; J. Feicht; M. M. Fejer; F. Feng; E. Fenyvesi; D. L. Ferguson; A. Fernandez-Galiana; I. Ferrante; T. A. Ferreira; F. Fidecaro; P. Figura; I. Fiori; M. Fishbach; R. P. Fisher; R. Fittipaldi; V. Fiumara; R. Flaminio; E. Floden; E. Flynn; H. Fong; J. A. Font; B. Fornal; P. W. F. Forsyth; A. Franke; S. Frasca; F. Frasconi; C. Frederick; Z. Frei; A. Freise; R. Frey; P. Fritschel; V. V. Frolov; G. G. Fronzé; Y. Fujii; Y. Fujikawa; M. Fukunaga; M. Fukushima; P. Fulda; M. Fyffe; H. A. Gabbard; B. U. Gadre; S. M. Gaebel; J. R. Gair; J. Gais; S. Galaudage; R. Gamba; D. Ganapathy; A. Ganguly; D. Gao; S. G. Gaonkar; B. Garaventa; C. García-Núñez; C. García-Quirós; F. Garufi; B. Gateley; S. Gaudio; V. Gayathri; G. Ge; G. Gemme; A. Gennai; J. George; L. Gergely; P. Gewecke; S. Ghonge; Abhirup. Ghosh; Archisman Ghosh; Shaon Ghosh; Shrobana Ghosh; Sourath Ghosh; B. Giacomazzo; L. Giacoppo; J. A. Giaime; K. D. Giardina; D. R. Gibson; C. Gier; M. Giesler; P. Giri; F. Gissi; J. Glanzer; A. E. Gleckl; P. Godwin; E. Goetz; R. Goetz; N. Gohlke; B. Goncharov; G. González; A. Gopakumar; M. Gosselin; R. Gouaty; B. Grace; A. Grado; M. Granata; V. Granata; A. Grant; S. Gras; P. Grassia; C. Gray; R. Gray; G. Greco; A. C. Green; R. Green; A. M. Gretarsson; E. M. Gretarsson; D. Griffith; W. Griffiths; H. L. Griggs; G. Grignani; A. Grimaldi; E. Grimes; S. J. Grimm; H. Grote; S. Grunewald; P. Gruning; J. G. Guerrero; G. M. Guidi; A. R. Guimaraes; G. Guixé; H. K. Gulati; H.-K. Guo; Y. Guo; Anchal Gupta; Anuradha Gupta; P. Gupta; E. K. Gustafson; R. Gustafson; F. Guzman; S. Ha; L. Haegel; A. Hagiwara; S. Haino; O. Halim; E. D. Hall; E. Z. Hamilton; G. Hammond; W.-B. Han; M. Haney; J. Hanks; C. Hanna; M. D. Hannam; O. A. Hannuksela; H. Hansen; T. J. Hansen; J. Hanson; T. Harder; T. Hardwick; K. Haris; J. Harms; G. M. Harry; I. W. Harry; D. Hartwig; K. Hasegawa; B. Haskell; R. K. Hasskew; C.-J. Haster; K. Hattori; K. Haughian; H. Hayakawa; K. Hayama; F. J. Hayes; J. Healy; A. Heidmann; M. C. Heintze; J. Heinze; J. Heinzel; H. Heitmann; F. Hellman; P. Hello; A. F. Helmling-Cornell; G. Hemming; M. Hendry; I. S. Heng; E. Hennes; J. Hennig; M. H. Hennig; F. Hernandez Vivanco; M. Heurs; S. Hild; P. Hill; Y. Himemoto; A. S. Hines; Y. Hiranuma; N. Hirata; E. Hirose; S. Hochheim; D. Hofman; J. N. Hohmann; A. M. Holgado; N. A. Holland; I. J. Hollows; Z. J. Holmes; K. Holt; D. E. Holz; Z. Hong; P. Hopkins; J. Hough; E. J. Howell; C. G. Hoy; D. Hoyland; A. Hreibi; B-H. Hsieh; Y. Hsu; G-Z. Huang; H-Y. Huang; P. Huang; Y-C. Huang; Y.-J. Huang; Y.-W. Huang; M. T. Hübner; A. D. Huddart; E. A. Huerta; B. Hughey; D. C. Y. Hui; V. Hui; S. Husa; S. H. Huttner; R. Huxford; T. Huynh-Dinh; S. Ide; B. Idzkowski; A. Iess; B. Ikenoue; S. Imam; K. Inayoshi; H. Inchauspe; C. Ingram; Y. Inoue; G. Intini; K. Ioka; M. Isi; K. Isleif; K. Ito; Y. Itoh; B. R. Iyer; K. Izumi; V. JaberianHamedan; T. Jacqmin; S. J. Jadhav; S. P. Jadhav; A. L. James; A. Z. Jan; K. Jani; K. Janssens; N. N. Janthalur; P. Jaranowski; D. Jariwala; R. Jaume; A. C. Jenkins; C. Jeon; M. Jeunon; W. Jia; J. Jiang; H.-B. Jin; G. R. Johns; A. W. Jones; D. I. Jones; J. D. Jones; P. Jones; R. Jones; R. J. G. Jonker; L. Ju; K. Jung; P. Jung; J. Junker; K. Kaihotsu; T. Kajita; M. Kakizaki; C. V. Kalaghatgi; V. Kalogera; B. Kamai; M. Kamiizumi; N. Kanda; S. Kandhasamy; G. Kang; J. B. Kanner; Y. Kao; S. J. Kapadia; D. P. Kapasi; S. Karat; C. Karathanasis; S. Karki; R. Kashyap; M. Kasprzack; W. Kastaun; S. Katsanevas; E. Katsavounidis; W. Katzman; T. Kaur; K. Kawabe; K. Kawaguchi; N. Kawai; T. Kawasaki; F. Kéfélian; D. Keitel; J. S. Key; S. Khadka; F. Y. Khalili; I. Khan; S. Khan; E. A. Khazanov; N. Khetan; M. Khursheed; N. Kijbunchoo; C. Kim; J. C. Kim; J. Kim; K. Kim; W. S. Kim; Y.-M. Kim; C. Kimball; N. Kimura; P. J. King; M. Kinley-Hanlon; R. Kirchhoff; J. S. Kissel; N. Kita; H. Kitazawa; L. Kleybolte; S. Klimenko; A. M. Knee; T. D. Knowles; E. Knyazev; P. Koch; G. Koekoek; Y. Kojima; K. Kokeyama; S. Koley; P. Kolitsidou; M. Kolstein; K. Komori; V. Kondrashov; A. K. H. Kong; A. Kontos; N. Koper; M. Korobko; K. Kotake; M. Kovalam; D. B. Kozak; C. Kozakai; R. Kozu; V. Kringel; N. V. Krishnendu; A. Królak; G. Kuehn; F. Kuei; A. Kumar; P. Kumar; Rahul Kumar; Rakesh Kumar; J. Kume; K. Kuns; C. Kuo; H-S. Kuo; Y. Kuromiya; S. Kuroyanagi; K. Kusayanagi; K. Kwak; S. Kwang; D. Laghi; E. Lalande; T. L. Lam; A. Lamberts; M. Landry; B. B. Lane; R. N. Lang; J. Lange; B. Lantz; I. La Rosa; A. Lartaux-Vollard; P. D. Lasky; M. Laxen; A. Lazzarini; C. Lazzaro; P. Leaci; S. Leavey; Y. K. Lecoeuche; H. K. Lee; H. M. Lee; H. W. Lee; J. Lee; K. Lee; R. Lee; J. Lehmann; A. Lemaître; E. Leon; M. Leonardi; N. Leroy; N. Letendre; Y. Levin; J. N. Leviton; A. K. Y. Li; B. Li; J. Li; K. L. Li; T. G. F. Li; X. Li; C-Y. Lin; F-K. Lin; F-L. Lin; H. L. Lin; L. C.-C. Lin; F. Linde; S. D. Linker; J. N. Linley; T. B. Littenberg; G. C. Liu; J. Liu; K. Liu; X. Liu; M. Llorens-Monteagudo; R. K. L. Lo; A. Lockwood; M. L. Lollie; L. T. London; A. Longo; D. Lopez; M. Lorenzini; V. Loriette; M. Lormand; G. Losurdo; J. D. Lough; C. O. Lousto; G. Lovelace; H. Lück; D. Lumaca; A. P. Lundgren; L.-W. Luo; R. Macas; M. MacInnis; D. M. Macleod; I. A. O. MacMillan; A. Macquet; I. Magaña Hernandez; F. Magaña-Sandoval; C. Magazzù; R. M. Magee; R. Maggiore; E. Majorana; C. Makarem; I. Maksimovic; S. Maliakal; A. Malik; N. Man; V. Mandic; V. Mangano; J. L. Mango; G. L. Mansell; M. Manske; M. Mantovani; M. Mapelli; F. Marchesoni; M. Marchio; F. Marion; Z. Mark; S. Márka; Z. Márka; C. Markakis; A. S. Markosyan; A. Markowitz; E. Maros; A. Marquina; S. Marsat; F. Martelli; I. W. Martin; R. M. Martin; M. Martinez; V. Martinez; K. Martinovic; D. V. Martynov; E. J. Marx; H. Masalehdan; K. Mason; E. Massera; A. Masserot; T. J. Massinger; M. Masso-Reid; S. Mastrogiovanni; A. Matas; M. Mateu-Lucena; F. Matichard; M. Matiushechkina; N. Mavalvala; J. J. McCann; R. McCarthy; D. E. McClelland; P. McClincy; S. McCormick; L. McCuller; G. I. McGhee; S. C. McGuire; C. McIsaac; J. McIver; D. J. McManus; T. McRae; S. T. McWilliams; D. Meacher; M. Mehmet; A. K. Mehta; A. Melatos; D. A. Melchor; G. Mendell; A. Menendez-Vazquez; C. S. Menoni; R. A. Mercer; L. Mereni; K. Merfeld; E. L. Merilh; J. D. Merritt; M. Merzougui; S. Meshkov; C. Messenger; C. Messick; P. M. Meyers; F. Meylahn; A. Mhaske; A. Miani; H. Miao; I. Michaloliakos; C. Michel; Y. Michimura; H. Middleton; L. Milano; A. L. Miller; M. Millhouse; J. C. Mills; E. Milotti; M. C. Milovich-Goff; O. Minazzoli; Y. Minenkov; N. Mio; Ll. M. Mir; A. Mishkin; C. Mishra; T. Mishra; T. Mistry; S. Mitra; V. P. Mitrofanov; G. Mitselmakher; R. Mittleman; O. Miyakawa; A. Miyamoto; Y. Miyazaki; K. Miyo; S. Miyoki; Geoffrey Mo; K. Mogushi; S. R. P. Mohapatra; S. R. Mohite; I. Molina; M. Molina-Ruiz; M. Mondin; M. Montani; C. J. Moore; D. Moraru; F. Morawski; A. More; C. Moreno; G. Moreno; Y. Mori; S. Morisaki; Y. Moriwaki; B. Mours; C. M. Mow-Lowry; S. Mozzon; F. Muciaccia; Arunava Mukherjee; D. Mukherjee; Soma Mukherjee; Subroto Mukherjee; N. Mukund; A. Mullavey; J. Munch; E. A. Muñiz; P. G. Murray; R. Musenich; S. L. Nadji; K. Nagano; S. Nagano; A. Nagar; K. Nakamura; H. Nakano; M. Nakano; R. Nakashima; Y. Nakayama; I. Nardecchia; T. Narikawa; L. Naticchioni; B. Nayak; R. K. Nayak; R. Negishi; B. F. Neil; J. Neilson; G. Nelemans; T. J. N. Nelson; M. Nery; A. Neunzert; K. Y. Ng; S. W. S. Ng; C. Nguyen; P. Nguyen; T. Nguyen; L. Nguyen Quynh; W.-T. Ni; S. A. Nichols; A. Nishizawa; S. Nissanke; F. Nocera; M. Noh; M. Norman; C. North; S. Nozaki; L. K. Nuttall; J. Oberling; B. D. O’Brien; Y. Obuchi; J. O’Dell; W. Ogaki; G. Oganesyan; J. J. Oh; K. Oh; S. H. Oh; M. Ohashi; N. Ohishi; M. Ohkawa; F. Ohme; H. Ohta; M. A. Okada; Y. Okutani; K. Okutomi; C. Olivetto; K. Oohara; C. Ooi; R. Oram; B. O’Reilly; R. G. Ormiston; N. D. Ormsby; L. F. Ortega; R. O’Shaughnessy; E. O’Shea; S. Oshino; S. Ossokine; C. Osthelder; S. Otabe; D. J. Ottaway; H. Overmier; A. E. Pace; G. Pagano; M. A. Page; G. Pagliaroli; A. Pai; S. A. Pai; J. R. Palamos; O. Palashov; C. Palomba; K. Pan; P. K. Panda; H. Pang; P. T. H. Pang; C. Pankow; F. Pannarale; B. C. Pant; F. Paoletti; A. Paoli; A. Paolone; A. Parisi; J. Park; W. Parker; D. Pascucci; A. Pasqualetti; R. Passaquieti; D. Passuello; M. Patel; B. Patricelli; E. Payne; T. C. Pechsiri; M. Pedraza; M. Pegoraro; A. Pele; F. E. Peña Arellano; S. Penn; A. Perego; A. Pereira; T. Pereira; C. J. Perez; C. Périgois; A. Perreca; S. Perriès; J. Petermann; D. Petterson; H. P. Pfeiffer; K. A. Pham; K. S. Phukon; O. J. Piccinni; M. Pichot; M. Piendibene; F. Piergiovanni; L. Pierini; V. Pierro; G. Pillant; F. Pilo; L. Pinard; I. M. Pinto; B. J. Piotrzkowski; K. Piotrzkowski; M. Pirello; M. Pitkin; E. Placidi; W. Plastino; C. Pluchar; R. Poggiani; E. Polini; D. Y. T. Pong; S. Ponrathnam; P. Popolizio; E. K. Porter; J. Powell; M. Pracchia; T. Pradier; A. K. Prajapati; K. Prasai; R. Prasanna; G. Pratten; T. Prestegard; M. Principe; G. A. Prodi; L. Prokhorov; P. Prosposito; L. Prudenzi; A. Puecher; M. Punturo; F. Puosi; P. Puppo; M. Pürrer; H. Qi; V. Quetschke; P. J. Quinonez; R. Quitzow-James; F. J. Raab; G. Raaijmakers; H. Radkins; N. Radulesco; P. Raffai; S. X. Rail; S. Raja; C. Rajan; K. E. Ramirez; T. D. Ramirez; A. Ramos-Buades; J. Rana; P. Rapagnani; U. D. Rapol; B. Ratto; V. Raymond; N. Raza; M. Razzano; J. Read; L. A. Rees; T. Regimbau; L. Rei; S. Reid; D. H. Reitze; P. Relton; P. Rettegno; F. Ricci; C. J. Richardson; J. W. Richardson; L. Richardson; P. M. Ricker; G. Riemenschneider; K. Riles; M. Rizzo; N. A. Robertson; R. Robie; F. Robinet; A. Rocchi; J. A. Rocha; S. Rodriguez; R. D. Rodriguez-Soto; L. Rolland; J. G. Rollins; V. J. Roma; M. Romanelli; R. Romano; C. L. Romel; A. Romero; I. M. Romero-Shaw; J. H. Romie; C. A. Rose; D. Rosińska; S. G. Rosofsky; M. P. Ross; S. Rowan; S. J. Rowlinson; Santosh Roy; Soumen Roy; D. Rozza; P. Ruggi; K. Ryan; S. Sachdev; T. Sadecki; J. Sadiq; N. Sago; S. Saito; Y. Saito; K. Sakai; Y. Sakai; M. Sakellariadou; Y. Sakuno; O. S. Salafia; L. Salconi; M. Saleem; F. Salemi; A. Samajdar; E. J. Sanchez; J. H. Sanchez; L. E. Sanchez; N. Sanchis-Gual; J. R. Sanders; A. Sanuy; T. R. Saravanan; N. Sarin; B. Sassolas; H. Satari; B. S. Sathyaprakash; S. Sato; T. Sato; O. Sauter; R. L. Savage; V. Savant; T. Sawada; D. Sawant; H. L. Sawant; S. Sayah; D. Schaetzl; M. Scheel; J. Scheuer; A. Schindler-Tyka; P. Schmidt; R. Schnabel; M. Schneewind; R. M. S. Schofield; A. Schönbeck; B. W. Schulte; B. F. Schutz; E. Schwartz; J. Scott; S. M. Scott; M. Seglar-Arroyo; E. Seidel; T. Sekiguchi; Y. Sekiguchi; D. Sellers; A. S. Sengupta; N. Sennett; D. Sentenac; E. G. Seo; V. Sequino; A. Sergeev; Y. Setyawati; T. Shaffer; M. S. Shahriar; B. Shams; L. Shao; S. Sharifi; A. Sharma; P. Sharma; P. Shawhan; N. S. Shcheblanov; H. Shen; S. Shibagaki; M. Shikauchi; R. Shimizu; T. Shimoda; K. Shimode; R. Shink; H. Shinkai; T. Shishido; A. Shoda; D. H. Shoemaker; D. M. Shoemaker; K. Shukla; S. ShyamSundar; M. Sieniawska; D. Sigg; L. P. Singer; D. Singh; N. Singh; A. Singha; A. M. Sintes; V. Sipala; V. Skliris; B. J. J. Slagmolen; T. J. Slaven-Blair; J. Smetana; J. R. Smith; R. J. E. Smith; S. N. Somala; K. Somiya; E. J. Son; K. Soni; S. Soni; B. Sorazu; V. Sordini; F. Sorrentino; N. Sorrentino; H. Sotani; R. Soulard; T. Souradeep; E. Sowell; V. Spagnuolo; A. P. Spencer; M. Spera; A. K. Srivastava; V. Srivastava; K. Staats; C. Stachie; D. A. Steer; J. Steinlechner; S. Steinlechner; D. J. Stops; M. Stover; K. A. Strain; L. C. Strang; G. Stratta; A. Strunk; R. Sturani; A. L. Stuver; J. Südbeck; S. Sudhagar; V. Sudhir; R. Sugimoto; H. G. Suh; T. Z. Summerscales; H. Sun; L. Sun; S. Sunil; A. Sur; J. Suresh; P. J. Sutton; Takamasa Suzuki; Toshikazu Suzuki; B. L. Swinkels; M. J. Szczepańczyk; P. Szewczyk; M. Tacca; H. Tagoshi; S. C. Tait; H. Takahashi; R. Takahashi; A. Takamori; S. Takano; H. Takeda; M. Takeda; C. Talbot; H. Tanaka; Kazuyuki Tanaka; Kenta Tanaka; Taiki Tanaka; Takahiro Tanaka; A. J. Tanasijczuk; S. Tanioka; D. B. Tanner; D. Tao; A. Tapia; E. N. Tapia San Martin; E. N. Tapia San Martin; J. D. Tasson; S. Telada; R. Tenorio; L. Terkowski; M. Test; M. P. Thirugnanasambandam; M. Thomas; P. Thomas; J. E. Thompson; S. R. Thondapu; K. A. Thorne; E. Thrane; Shubhanshu Tiwari; Srishti Tiwari; V. Tiwari; K. Toland; A. E. Tolley; T. Tomaru; Y. Tomigami; T. Tomura; M. Tonelli; A. Torres-Forné; C. I. Torrie; I. Tosta e Melo; D. Töyrä; A. Trapananti; F. Travasso; G. Traylor; M. C. Tringali; A. Tripathee; L. Troiano; A. Trovato; L. Trozzo; R. J. Trudeau; D. S. Tsai; D. Tsai; K. W. Tsang; T. Tsang; J-S. Tsao; M. Tse; R. Tso; K. Tsubono; S. Tsuchida; L. Tsukada; D. Tsuna; T. Tsutsui; T. Tsuzuki; M. Turconi; D. Tuyenbayev; A. S. Ubhi; N. Uchikata; T. Uchiyama; R. P. Udall; A. Ueda; T. Uehara; K. Ueno; G. Ueshima; D. Ugolini; C. S. Unnikrishnan; F. Uraguchi; A. L. Urban; T. Ushiba; S. A. Usman; A. C. Utina; H. Vahlbruch; G. Vajente; A. Vajpeyi; G. Valdes; M. Valentini; V. Valsan; N. van Bakel; M. van Beuzekom; J. F. J. van den Brand; C. Van Den Broeck; D. C. Vander-Hyde; L. van der Schaaf; J. V. van Heijningen; J. Vanosky; M. H. P. M. van Putten; M. Vardaro; A. F. Vargas; V. Varma; M. Vasúth; A. Vecchio; G. Vedovato; J. Veitch; P. J. Veitch; K. Venkateswara; J. Venneberg; G. Venugopalan; D. Verkindt; Y. Verma; D. Veske; F. Vetrano; A. Viceré; A. D. Viets; V. Villa-Ortega; J.-Y. Vinet; S. Vitale; T. Vo; H. Vocca; E. R. G. von Reis; J. von Wrangel; C. Vorvick; S. P. Vyatchanin; L. E. Wade; M. Wade; K. J. Wagner; R. C. Walet; M. Walker; G. S. Wallace; L. Wallace; S. Walsh; J. Wang; J. Z. Wang; W. H. Wang; R. L. Ward; J. Warner; M. Was; T. Washimi; N. Y. Washington; J. Watchi; B. Weaver; L. Wei; M. Weinert; A. J. Weinstein; R. Weiss; C. M. Weller; F. Wellmann; L. Wen; P. Weßels; J. W. Westhouse; K. Wette; J. T. Whelan; D. D. White; B. F. Whiting; C. Whittle; D. Wilken; D. Williams; M. J. Williams; A. R. Williamson; J. L. Willis; B. Willke; D. J. Wilson; W. Winkler; C. C. Wipf; T. Wlodarczyk; G. Woan; J. Woehler; J. K. Wofford; I. C. F. Wong; C. Wu; D. S. Wu; H. Wu; S. Wu; D. M. Wysocki; L. Xiao; W-R. Xu; T. Yamada; H. Yamamoto; Kazuhiro Yamamoto; Kohei Yamamoto; T. Yamamoto; K. Yamashita; R. Yamazaki; F. W. Yang; L. Yang; Yang Yang; Yi Yang; Z. Yang; M. J. Yap; D. W. Yeeles; A. B. Yelikar; M. Ying; K. Yokogawa; J. Yokoyama; T. Yokozawa; A. Yoon; T. Yoshioka; Hang Yu; Haocun Yu; H. Yuzurihara; A. Zadrożny; M. Zanolin; S. Zeidler; T. Zelenova; J.-P. Zendri; M. Zevin; M. Zhan; H. Zhang; J. Zhang; L. Zhang; R. Zhang; T. Zhang; C. Zhao; G. Zhao; Yue Zhao; Yuhang Zhao; Z. Zhou; X. J. Zhu; Z.-H. Zhu; M. E. Zucker; J. Zweizig
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 80
Systematic Perturbations of the Thermodynamic Properties in Cool Cores of HIFLUGCS Galaxy Clusters
Shutaro Ueda; Keiichi Umetsu; FanLam Ng; Yuto Ichinohe; Tetsu Kitayama; Sandor M. Molnar
<jats:title>Abstract</jats:title> <jats:p>We present an ensemble X-ray analysis of systematic perturbations in the central hot gas properties for a sample of 28 nearby strong cool-core systems, selected from the HIghest X-ray FLUx Galaxy Cluster Sample (HIFLUGCS). We analyze their cool-core features observed with the Chandra X-ray Observatory. All individual systems in our sample exhibit at least a pair of positive and negative excess perturbations in the X-ray residual image after subtracting the global brightness profile. We extract and analyze X-ray spectra of the intracluster medium (ICM) in the detected perturbed regions. To investigate possible origins of the gas perturbations, we characterize thermodynamic properties of the ICM in the perturbed regions and characterize their correlations between positive and negative excess regions. The best-fit relations for temperature and entropy show a clear offset from the one-to-one relation, <jats:inline-formula> <jats:tex-math> <?CDATA ${T}_{\mathrm{neg}}/{T}_{\mathrm{pos}}={1.20}_{-0.03}^{+0.04}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>T</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>neg</mml:mi> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>T</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>pos</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.20</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.03</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.04</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjac1f16ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> and <jats:italic>K</jats:italic> <jats:sub>neg</jats:sub>/<jats:italic>K</jats:italic> <jats:sub>pos</jats:sub> = 1.43 ± 0.07, whereas the best-fit relation for pressure is found to be remarkably consistent with the one-to-one relation <jats:italic>P</jats:italic> <jats:sub>neg</jats:sub> = <jats:italic>P</jats:italic> <jats:sub>pos</jats:sub>, indicating that the ICM in the perturbed regions is in pressure equilibrium. These observed features in the HIFLUGCS sample are in agreement with the hypothesis that the gas perturbations in cool cores are generated by gas sloshing. We also analyze synthetic observations of perturbed cluster cores created from binary merger simulations, finding that the observed temperature ratio agrees with the simulations, <jats:italic>T</jats:italic> <jats:sub>neg</jats:sub>/<jats:italic>T</jats:italic> <jats:sub>pos</jats:sub> ∼ 1.3. We conclude that gas sloshing induced by infalling substructures plays a major role in producing the characteristic gas perturbations in cool cores. The ubiquitous presence of gas perturbations in cool cores may suggest a significant contribution of gas sloshing to suppressing runaway cooling of the ICM.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 81
The Young Stellar Population, Distance, and Cloud–Cloud Collision Induced Star Formation Scenario of the Trifid Nebula
Venu M. Kalari
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 81
On the Issue of the Origin of Type II Solar Radio Bursts
Gennady Chernov; Valery Fomichev
<jats:title>Abstract</jats:title> <jats:p>Type II solar radio bursts are among the most powerful events in the solar radio emission in the meter wavelength range. It is generally accepted that the agents generating type II radio bursts are magnetohydrodynamic shock waves. But the relationship between the shock waves and the other manifestations of the large-scale disturbances in the solar atmosphere (coronal mass ejections, Morton waves, EUW waves) remains unclear. To clarify a problem, it is important to determine the conditions of generation of type II radio bursts. Here, the model of the radio source is based on the generation of radio emission within the front of the collisionless shock wave where the Buneman instability of plasma waves is developed. In the frame of this model, the Alfvén magnetic Mach number must exceed the critical value, and there is a strict restriction on the perpendicularity of the front. The model allows us to obtain the information about the parameters of the shock waves and the parameters of the medium by the parameters of type II bursts. The estimates, obtained in this paper for several events with the band splitting of the fundamental and harmonic emission bands of the type II bursts, confirm the necessary conditions of the model. In this case the registration of type II radio bursts is an indication of the propagation of shock waves in the solar atmosphere, and the absence of type II radio bursts is not an indication of the absence of shock waves. Such a situation should be taken into account when investigating the relationship between type II radio bursts and other manifestations of solar activity.</jats:p>
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 82
The Solar Memory from Hours to Decades
Markus J. Aschwanden; Jay R. Johnson
Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.
Pp. 82