144 research outputs found
Interventions to Safeguard System Effectiveness During Periods of Emergency Department Crowding
- Author
- Publication venue
- 'Wiley'
- Publication date
- 01/12/2011
- Field of study
This article summarizes the proceedings of a breakout session, “Interventions to Safeguard System Effectiveness,” at the 2011 Academic Emergency Medicine consensus conference, “Interventions to Assure Quality in the Crowded Emergency Department.” Key definitions fundamental to understanding the effectiveness of emergency care during periods of emergency department (ED) crowding are outlined. Next, a proposed research agenda to evaluate interventions directed at improving emergency care effectiveness is outlined, and the paper concludes with a prioritization of those interventions based on breakout session participant discussion and evaluation.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/89510/1/j.1553-2712.2011.01219.x.pd
First narrow-band search for continuous gravitational waves from known pulsars in advanced detector data
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- Tso R.
- Tsukada L.
- Tsuna D.
- Tuyenbayev D.
- Ueno K.
- Ugolini D.
- Unnikrishnan C. S.
- Urban A. L.
- Usman S. A.
- V
- Vahlbruch H.
- VAJENTE GABRIELE
- Valdes G.
- van Bakel N.
- van Beuzekom M.
- van den Br
- Van Den Broeck C.
- van der Schaaf L.
- van Heijningen J. V.
- van Veggel A. A.
- Vardaro M.
- Varma V.
- Vass S.
- Vasuth M.
- Vecchio A.
- Vedovato G.
- Veitch J.
- Veitch P. J.
- Venkateswara K.
- Venugopalan G.
- Verkindt D.
- Vetrano F.
- Vicere A.
- Viets A. D.
- Vinciguerra S.
- Vine D. J.
- Vinet J. -.Y.
- Virgo Collaboration
- Vitale S.
- Vo T.
- Vocca H.
- Vorvick C.
- Vyatchanin S. P.
- Wade A. R.
- Wade L. E.
- Wade M.
- Walet R.
- Walker M.
- Wallace L.
- Walsh S.
- Wang G.
- Wang H.
- Wang J. Z.
- Wang W. H.
- Wang Y. F.
- Ward R. L.
- Warner J.
- Was M.
- Watchi J.
- Weaver B.
- Wei L. -.W.
- Weinert M.
- Weinstein A. J.
- Weiss R.
- Wen L.
- Wessel E. K.
- Wessels P.
- Westerweck J.
- Westphal T.
- Wette K.
- Whelan J. T.
- Whiting B. F.
- Whittle C.
- Wilken D.
- Williams D.
- Williams R. D.
- Williamson A. R.
- Willis J. L.
- Willke B.
- Wimmer M. H.
- Winkler W.
- Wipf C. C.
- Wittel H.
- Woan G.
- Woehler J.
- Wofford J.
- Wong K. W. K.
- Worden J.
- Wright J. L.
- Wu D. S.
- Wysocki D. M.
- Xiao S.
- Yamamoto H.
- Yancey C. C.
- Yang L.
- Yap M. J.
- Yazback M.
- Yu Hang
- Yu Haocun
- Yvert M.
- Zadrozny A.
- Zanolin M.
- Zelenova T.
- Zendri J. -.P.
- Zertuche L. Magana
- Zevin M.
- Zhang L.
- Zhang M.
- Zhang T.
- Zhang Y. -.H.
- Zhao C.
- Zhou M.
- Zhou Z.
- Zhu S. J.
- Zhu X. J.
- Zucker M. E.
- Zweizig J.
- Publication venue
- American Physical Society
- Publication date
- 01/01/2017
- Field of study
Spinning neutron stars asymmetric with respect to their rotation axis are potential sources of
continuous gravitational waves for ground-based interferometric detectors. In the case of known pulsars a
fully coherent search, based on matched filtering, which uses the position and rotational parameters
obtained from electromagnetic observations, can be carried out. Matched filtering maximizes the signalto-
noise (SNR) ratio, but a large sensitivity loss is expected in case of even a very small mismatch
between the assumed and the true signal parameters. For this reason, narrow-band analysis methods have
been developed, allowing a fully coherent search for gravitational waves from known pulsars over a
fraction of a hertz and several spin-down values. In this paper we describe a narrow-band search of
11 pulsars using data from Advanced LIGO’s first observing run. Although we have found several initial
outliers, further studies show no significant evidence for the presence of a gravitational wave signal.
Finally, we have placed upper limits on the signal strain amplitude lower than the spin-down limit for 5 of
the 11 targets over the bands searched; in the case of J1813-1749 the spin-down limit has been beaten for
the first time. For an additional 3 targets, the median upper limit across the search bands is below the
spin-down limit. This is the most sensitive narrow-band search for continuous gravitational waves carried
out so far
3D-MRI rendering of the anatomical structures related to acupuncture points of the Dai mai, Yin qiao mai and Yang qiao mai meridians within the context of the WOMED concept of lateral tension: implications for musculoskeletal disease
- Author
- A Aquino
- A Campbell
- A Ellis
- A Nakagoshi
- A Vleeming
- Ansgar Rudisch
- B Kirschbaum
- C Lariviere
- C Profanter
- C Profanter
- C Profanter
- C Shi
- C Stecco
- CA Richardson
- Christian Kremser
- D Dressler
- D Guo
- DJ Theodorou
- DM Urquhart
- DM Urquhart
- E Fee
- E Peuker
- E Peuker
- E Peuker
- G Li
- G Maciocia
- G Maciocia
- H Kainz
- H Maas
- H Weiss
- Helga Moncayo
- HM Langevin
- J Hides
- J Ross
- J Shen
- K Itoh
- K Li
- M Gabriel
- M Loukas
- NM Rofsky
- OK Andersen
- OK Andersen
- P Deadman
- P Huijing
- PJ Barker
- PJ Barker
- PJ Barker
- PW Hodges
- R Moncayo
- R Moncayo
- R Prommegger
- RA Sweeney
- RA Sweeney
- Roy Moncayo
- S Robertson
- T Rasmussen
- T Renkawitz
- V Lo
- Publication venue
- BioMed Central
- Publication date
- 01/01/2007
- Field of study
BACKGROUND: A conceptual model of lateral muscular tension in patients presenting thyroid associated ophthalmopathy (TAO) has been recently described. Clinical improvement has been achieved by using acupuncture on points belonging to the so-called extraordinary meridians. The aim of this study was to characterize the anatomical structures related to these acupuncture points by means of 3D MRI image rendering relying on external markers. METHODS: The investigation was carried out the index case patient of the lateral tension model. A licensed medical acupuncture practitioner located the following acupuncture points: 1) Yin qiao mai meridian (medial ankle): Kidney 3, Kidney 6, the plantar Kidney 6 (Nan jing description); 2) Yang qiao mai meridian (lateral ankle): Bladder 62, Bladder 59, Bladder 61, and the plantar Bladder 62 (Nan jing description); 3) Dai mai meridian (wait): Liver 13, Gall bladder 26, Gall bladder 27, Gall bladder 28, and Gall bladder 29. The points were marked by taping a nitro-glycerin capsule on the skin. Imaging was done on a Siemens Magnetom Avanto MR scanner using an array head and body coil. Mainly T1-weighted imaging sequences, as routinely used for patient exams, were used to obtain multi-slice images. The image data were rendered in 3D modus using dedicated software (Leonardo, Siemens). RESULTS: Points of the Dai mai meridian – at the level of the waist – corresponded to the obliquus externus abdominis and the obliquus internus abdominis. Points of the Yin qiao mai meridian – at the medial side of the ankle – corresponded to tendinous structures of the flexor digitorum longus as well as to muscular structures of the abductor hallucis on the foot sole. Points of the Yang qiao mai meridian – at the lateral side of the ankle – corresponded to tendinous structures of the peroneus brevis, the peroneous longus, and the lateral surface of the calcaneus and close to the foot sole to the abductor digiti minimi. CONCLUSION: This non-invasive MRI investigation has revealed the anatomical relations of acupuncture points belonging to 3 of the so-called extraordinary meridians. We conclude that the clinically developed "WOMED concept of lateral tension" is related to tendino-muscular structures
Discovery of 4,6-disubstituted pyrimidines as potent inhibitors of the heat shock factor 1 (HSF1) stress pathway and CDK9.
- Author
- Publication venue
- 'Royal Society of Chemistry (RSC)'
- Publication date
- 01/01/2016
- Field of study
Heat shock factor 1 (HSF1) is a transcription factor that plays key roles in cancer, including providing a mechanism for cell survival under proteotoxic stress. Therefore, inhibition of the HSF1-stress pathway represents an exciting new opportunity in cancer treatment. We employed an unbiased phenotypic screen to discover inhibitors of the HSF1-stress pathway. Using this approach we identified an initial hit (1) based on a 4,6-pyrimidine scaffold (2.00 μM). Optimisation of cellular SAR led to an inhibitor with improved potency (25, 15 nM) in the HSF1 phenotypic assay. The 4,6-pyrimidine 25 was also shown to have high potency against the CDK9 enzyme (3 nM)
A gravitational-wave standard siren measurement of the Hubble constant
- Author
- Abbott
- Abbott
- Abbott
- Abbott
- Abdalla
- Acernese
- Ackley
- Adams
- Adams
- Addesso
- Adhikari
- Adya
- Affeldt
- Afrough
- Agarwal
- Agathos
- Agatsuma
- Aggarwal
- Aguiar
- Aiello
- Ain
- Ajith
- Alexander
- Allam
- Allen
- Allen
- Allocca
- Altin
- Amato
- Ananyeva
- Anderson
- Anderson
- Angelova
- Annis
- Antier
- Appert
- Arai
- Araya
- Arcavi Iair
- Areeda
- Arnaud
- Arun
- Ascenzi
- Ashton
- Ast
- Aston
- Astone
- Atallah
- Aufmuth
- Aulbert
- AultONeal
- Austin
- Avila-Alvarez
- Babak
- Bacon
- Bader
- Bae
- Baker
- Balanutsa
- Balbinot
- Baldaccini
- Ballardin
- Ballmer
- Banagiri
- Barayoga
- Barclay
- Barish
- Barker
- Barkett
- Barone
- Barr
- Barsotti
- Barsuglia
- Barta
- Bartlett
- Bartos
- Bassiri
- Basti
- Batch
- Bawaj
- Bayley
- Bazzan
- Bechtol
- Beer
- Bejger
- Belahcene
- Bell
- Benoit-Lévy
- Berger
- Berger
- Bergmann
- Bero
- Berry
- Bersanetti
- Bertin
- Bertolini
- Betzwieser
- Bhagwat
- Bhandare
- Bilenko
- Billingsley
- Billman
- Birch
- Birney
- Birnholtz
- Biscans
- Biscoveanu
- Bisht
- Bitossi
- Biwer
- Bizouard
- Blackburn
- Blackman
- Blair
- Blair
- Blair
- Blanchard
- Bloemen
- Bock
- Bode
- Boer
- Bogaert
- Bohe
- Bondu
- Bonilla
- Bonnand
- Boom
- Bork
- Boschi
- Bose
- Bossie
- Bouffanais
- Bozzi
- Bradaschia
- Brady
- Branchesi
- Brau
- Briant
- Bridle
- Brillet
- Brinkmann
- Brisson
- Brockill
- Broida
- Brooks
- Brooks
- Brout
- Brown
- Brown
- Brunett
- Buchanan
- Buckley
- Buckley-Geer
- Budnev
- Buikema
- Bulik
- Bulten
- Buonanno
- Burke
- Buskulic
- Butler
- Buy
- Byer
- Bécsy
- Cabero
- Cadonati
- Cagnoli
- Cahillane
- Calderón Bustillo
- Callister
- Calloni
- Camp
- Canepa
- Canizares
- Cannon
- Cano
- Cao
- Cao
- Capano
- Capocasa
- Carbognani
- Caride
- Carnero Rosell
- Carney
- Carrasco Kind
- Carretero
- Casanueva Diaz
- Casentini
- Castander
- Caudill
- Cavaglià
- Cavalier
- Cavalieri
- Cella
- Cepeda
- Cerdá-Durán
- Cerretani
- Cesarini
- Chamberlin
- Chan
- Chao
- Charlton
- Chase
- Chassande-Mottin
- Chatterjee
- Chatziioannou
- Cheeseboro
- Chen
- Chen
- Chen
- Cheng
- Chia
- Chincarini
- Chiummo
- Chmiel
- Cho
- Cho
- Chornock
- Chow
- Christensen
- Chu
- Chua
- Chua
- Chung
- Chung
- Ciani
- Ciolfi
- Cirelli
- Cirone
- Clara
- Clark
- Clearwater
- Cleva
- Cocchieri
- Coccia
- Cohadon
- Cohen
- Colla
- Collette
- Cominsky
- Constancio
- Conti
- Cook
- Cooper
- Copperwheat
- Corban
- Corbitt
- Cordero-Carrión
- Corley
- Cornish
- Corsi
- Cortese
- Costa
- Coughlin
- Coughlin
- Coulon
- Coulter
- Countryman
- Couvares
- Covas
- Cowan
- Coward
- Cowart
- Cowperthwaite
- Coyne
- Coyne
- Creighton
- Creighton
- Cripe
- Crowder
- Cullen
- Cumming
- Cunha
- Cunningham
- Cuoco
- D'Andrea
- D'Antonio
- Da Costa
- Da Silva Costa
- Dal Canton
- Danilishin
- Danzmann
- Dasgupta
- Datrier
- Dattilo
- Dave
- Davier
- Davis
- Davis
- Daw
- Day
- De Laurentis
- De Pietri
- De Rosa
- De Rossi
- De Ugarte-Postigo
- De Varona
- De
- DeBra
- Degallaix
- Del Pozzo
- Deléglise
- Demos
- Denker
- Dent
- DePoy
- Dergachev
- DeRosa
- Desai
- DeSalvo
- Devenson
- Dhurandhar
- Di Fiore
- Di Giovanni
- Di Girolamo
- Di Lieto
- Di Pace
- Di Palma
- Di Renzo
- Diehl
- Dietrich
- Doctor
- Dolique
- Donovan
- Dooley
- Doravari
- Dorrington
- Douglas
- Dovale Álvarez
- Downes
- Drago
- Dreissigacker
- Driggers
- Drlica-Wagner
- Drout
- Drout
- Du
- Ducrot
- Dupej
- Durret
- Dwyer
- Dálya
- Díaz
- Edo
- Edwards
- Effler
- Eftekhari
- Eggenstein
- Ehrens
- Eichholz
- Eikenberry
- Eisenstein
- Essick
- Estevez
- Estrada
- Etienne
- Etzel
- Evans
- Evans
- Evans
- Factourovich
- Fafone
- Fair
- Fairhurst
- Fan
- Farinon
- Farr
- Farr
- Fauchon-Jones
- Favata
- Fays
- Fee
- Fehrmann
- Feicht
- Fejer
- Fernandez
- Fernandez-Galiana
- Ferrante
- Ferreira
- Ferrini
- Fidecaro
- Finley
- Finstad
- Fiori
- Fiorucci
- Fishbach
- Fisher
- Fitz-Axen
- Flaminio
- Flaugher
- Fletcher
- Foley
- Fong
- Fong
- Font
- Forsyth
- Forsyth
- Fosalba
- Fournier
- Frasca
- Frasconi
- Frei
- Freise
- Frey
- Frey
- Frieman
- Fries
- Fritschel
- Frolov
- Fryer
- Fulda
- Fyffe
- Fynbo
- Gabbard
- Gadre
- Gaebel
- Gair
- Gammaitoni
- Ganija
- Gaonkar
- Garcia-Quiros
- García-Bellido
- Garufi
- Gateley
- Gaudio
- Gaur
- Gayathri
- Gaztanaga
- Gehrels
- Gemme
- Genin
- Gennai
- George
- George
- Gerdes
- Gergely
- Germain
- Ghonge
- Ghosh
- Ghosh Abhirup
- Ghosh Archisman
- Giaime
- Giannantonio
- Giardina
- Giazotto
- Gill
- Gill
- Glover
- Goetz
- Goetz
- Goldstein
- Gomes
- Goncharov
- Gonzalez Castro
- González
- González-Fernández
- Gopakumar
- Gorbovskoy
- Gorbunov
- Gorodetsky
- Gossan
- Gosselin
- Gouaty
- Grado
- Graef
- Granata
- Grant
- Gras
- Gray
- Greco
- Green
- Greiner
- Gress
- Gretarsson
- Groot
- Grote
- Gruen
- Gruendl
- Grunewald
- Gruning
- Guidi
- Guo
- Gupta
- Gupta
- Gushwa
- Gustafson
- Gustafson
- Gutierrez
- Haislip
- Halim
- Hall
- Hall
- Hamilton
- Hammond
- Haney
- Hanke
- Hanks
- Hanna
- Hanna
- Hannam
- Hannuksela
- Hanson
- Hardwick
- Harms
- Harry
- Harry
- Hart
- Hartley
- Hartley
- Haster
- Haughian
- Healy
- Heidmann
- Heintze
- Heitmann
- Hello
- Hemming
- Hendry
- Heng
- Hennig
- Heptonstall
- Herner
- Heurs
- Hild
- Hinderer
- Hjorth
- Hoak
- Hofman
- Holt
- Holz
- Honscheid
- Hopkins
- Horst
- Hosseinzadeh Griffin
- Hough
- Houston
- Howell
- Howell D. Andrew
- Hreibi
- Hu
- Huerta
- Huet
- Hughey
- Husa
- Huterer
- Huttner
- Huynh-Dinh
- Indik
- Inta
- Intini
- Irwin
- Isa
- Isac
- Isi
- Iyer
- Izumi
- Jacqmin
- Jain
- James
- Jani
- Jaranowski
- Jawahar
- Jeltema
- Jiménez-Forteza
- Johnson
- Johnson
- Jones
- Jones
- Jonker
- Ju
- Junker
- Kalaghatgi
- Kalogera
- Kamai
- Kandhasamy
- Kang
- Kanner
- Kapadia
- Karki
- Karvinen
- Kasen
- Kasen
- Kasprzack
- Katolik
- Katsavounidis
- Katzman
- Kaufer
- Kawabe
- Keitel
- Kemball
- Kennedy
- Kent
- Kent
- Kessler
- Key
- Khalili
- Khan
- Khan
- Khan
- Khazanov
- Kijbunchoo
- Kilpatrick
- Kim
- Kim
- Kim
- Kim
- Kim
- Kim Chunglee
- Kimbrell
- King
- King
- Kinley-Hanlon
- Kirchhoff
- Kissel
- Kleybolte
- Klimenko
- Knowles
- Koch
- Koehlenbeck
- Koley
- Kondrashov
- Kontos
- Kornilov
- Korobko
- Korth
- Kouprianov
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- Kozak
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- Kringel
- Krishnan
- Kron
- Krämer
- Królak
- Kuehn
- Kuehn
- Kuhlmann
- Kumar
- Kumar
- Kumar
- Kuo
- Kuropatkin
- Kutynia
- Kwang
- Kéfélian
- Lackey
- Lahav
- Lai
- Landry
- Lang
- Lange
- Lantz
- Lanza
- Lartaux-Vollard
- Lasky
- Laxen
- Lazzarini
- Lazzaro
- Leaci
- Leavey
- Lee
- Lee
- Lee
- Lee
- Lee
- Lehmann
- Lenon
- Leonardi
- Leroy
- Letendre
- Levan
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- Levin
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- Li
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- Linker
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- Littenberg
- Liu
- Liu
- Lo
- Lockerbie
- London
- Lopes
- Lord
- Lorenzini
- Loriette
- Lormand
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- Lough
- Lourenço
- Lousto
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- Ma
- Macas
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- MacInnis
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- Magaña Hernandez
- Magaña Zertuche
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- Magee
- Maia
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- Maksimovic
- Man
- Mandel
- Mandic
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- Mansell
- Manske
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- March
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- Marion
- Markakis
- Markosyan
- Markowitz
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- Marquina
- Marriner
- Marshall
- Martelli
- Martellini
- Martin
- Martin
- Martynov
- Mason
- Massera
- Masserot
- Massinger
- Masso-Reid
- Mastrogiovanni
- Matas
- Matheson
- Matichard
- Matone
- Mavalvala
- Mazumder
- McCarthy
- McClelland
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- McCuller
- McCully Curtis
- McGuire
- McIntyre
- McIver
- McMahon
- McManus
- McNeill
- McRae
- McWilliams
- Meacher
- Meadors
- Medina
- Mehmet
- Meidam
- Mejuto-Villa
- Melatos
- Mendell
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- Merilh
- Merzougui
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- Messenger
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- Metzger
- Meyers
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- Michel
- Middleton
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- Miller
- Miller
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- Millhouse
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- Minazzoli
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- Moffa
- Moggi
- Mogushi
- Mohan
- Mohapatra
- Montani
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- Moraru
- Moreno
- Morriss
- Mours
- Mow-Lowry
- Mueller
- Muir
- Muir
- Mukherjee
- Mukherjee
- Mukherjee Arunava
- Mukund
- Mullavey
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- Muratore
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- Muñoz
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- Márka
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- O'Brien
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- O'Reilly
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- Oberling
- Ogando
- Ogin
- Oh
- Oh
- Ohme
- Okada
- Oliver
- Oppermann
- Oram Richard J.
- Ormiston
- Ortega
- Osborne
- Ossokine
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- Overmier
- Owen
- Pace
- Page
- Page
- Pai
- Pai
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- Palamos
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- Palmese
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- Pan
- Pan Howard
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- Pang
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- Pant
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- Rolland
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- Rowan
- Rowlinson
- Ruggi
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- Rykoff
- Rüdiger
- Sachdev
- Sadecki
- Sadeghian
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- Sakellariadou
- Sako
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- Saleem
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- Sanchez
- Sanchez
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- Sandberg
- Sanders
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- Sathyaprakash
- Saulson
- Sauseda
- Sauter
- Savage
- Sawadsky
- Scarpine
- Schale
- Scheel
- Scheuer
- Schlegel
- Schmidt
- Schmidt
- Schnabel
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- Zucker
- Zweizig
- Publication venue
- Publication date
- 01/01/2017
- Field of study
On 17 August 2017, the Advanced LIGO 1 and Virgo 2 detectors observed the gravitational-wave event GW170817-a strong signal from the merger of a binary neutron-star system 3 . Less than two seconds after the merger, a γ-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO-Virgo-derived location of the gravitational-wave source 4-6 . This sky region was subsequently observed by optical astronomy facilities 7 , resulting in the identification 8-13 of an optical transient signal within about ten arcseconds of the galaxy NGC 4993. This detection of GW170817 in both gravitational waves and electromagnetic waves represents the first 'multi-messenger' astronomical observation. Such observations enable GW170817 to be used as a 'standard siren' 14-18 (meaning that the absolute distance to the source can be determined directly from the gravitational-wave measurements) to measure the Hubble constant. This quantity represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Here we report a measurement of the Hubble constant that combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using the electromagnetic data. In contrast to previous measurements, ours does not require the use of a cosmic 'distance ladder' 19 : the gravitational-wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be about 70 kilometres per second per megaparsec. This value is consistent with existing measurements 20,21 , while being completely independent of them. Additional standard siren measurements from future gravitationalwave sources will enable the Hubble constant to be constrained to high precision
First measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary–Black-hole Merger GW170814
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- Zelenova T
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- Zimmerman A
- Zucker M. E
- Zuntz J
- Zweizig J
- Publication venue
- 'American Astronomical Society'
- Publication date
- 01/01/2019
- Field of study
International audienceWe present a multi-messenger measurement of the Hubble constant H 0 using the binary–black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO)/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black hole merger. Our analysis results in , which is consistent with both SN Ia and cosmic microwave background measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20, 140] km s−1 Mpc−1, and it depends on the assumed prior range. If we take a broader prior of [10, 220] km s−1 Mpc−1, we find (57% of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on H 0
Multi-messenger observations of a binary neutron star merger
- Author
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- Aartsen MG
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- Milia Sabrina
- Miller AA
- Miller CJ
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- Monzani ME
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- Moore CJ
- Moore RW
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- Moreno E
- Moreno G
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- Morita K
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- Morlino G
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- Morris D
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- Morselli A
- Morselli A
- Moskalenko IV
- Moskvitin AS
- Mostaf M
- Motohara K
- Moulai M
- Moulin E
- Mours B
- Moussa A
- Mow-Lowry CM
- Mrka S
- Mrka Z
- Mueller AL
- Mueller AL
- Mueller BB
- Mueller G
- Mueller G
- Mueller MA
- Mueller S
- Muir AW
- Muir J
- Mukherjee Arunava
- Mukherjee D
- Mukherjee S
- Mukund N
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- Munch J
- Mundell CG
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- Muoz RR
- Murach T
- Murata KL
- Muratore M
- Murguia-Berthier A
- Murphy T
- Murray PG
- Mussa R
- Myers ST
- Nagai H
- Nagashima H
- Nagayama T
- Nahnhauer R
- Nakahira S
- Nakajima M
- Nakamura Y
- Nakaoka T
- Nakar E
- Nakarmi P
- Nakashima S
- Nakata F
- Nang Y
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- Natalucci L
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- Navarrini Alessandro
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- Negro M
- Neilsen E
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- Nynka M
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- Ohme F
- Ohsawa R
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- Ohta K
- Oikonomou F
- Ojha R
- Okada MA
- Okita H
- Oleynik Ph P
- Olinto A
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- Omodei N
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- Oozeer N
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- Ortu P
- Osborne JP
- Oslowski S
- Ossokine S
- Ostrowski M
- Ottaway DJ
- Ou G
- Overmier H
- Owen BJ
- Oya I
- Ozawa S
- Pacciani L
- Pace AE
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- Padilla N
- Padovani M
- Pagani C
- Page J
- Page KL
- Page MA
- Pai A
- Pai SA
- Pal-Singh A
- Palamos JR
- Palashov O
- Palatiello M
- Palatka M
- Palazzi E
- Palczewski T
- Paliya VS
- Palliyaguru N
- Palliyaguru NT
- Pallot D
- Pallotta J
- Palmas S
- Palmer DM
- Palmerio JT
- Palmese A
- Palomba C
- Pan Howard
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- Pandey SB
- Pandya H
- Paneque D
- Pang B
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- Pankow C
- Pannarale F
- Pant BC
- Panter M
- Paoletti F
- Paoletti F
- Paoli A
- Papa MA
- Papenbreer P
- Paragi Z
- Parente G
- Parida A
- Park IH
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- Pascucci D
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- Paul T
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- Paz-Chinchn F
- Pea-Rodriguez J
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- Pech M
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- Peiffer P
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- Pekowsky L
- Pelayo R
- Pele A
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- Penacchioni AV
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- Pepper JA
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- Perennes C
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- Perley DA
- Perlin M
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- Perri LM
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- Perrina C
- Perrodin D
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- Pescalli A
- Pesce-Rollins M
- Peters C
- Peters WM
- Petrera S
- Petrucci P-O
- Peyaud B
- Pfeiffer HP
- Phelps M
- Phlhofer G
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- Pian E
- Piano G
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- Piccinni OJ
- Pichot M
- Picozza P
- Piel Q
- Pieloth D
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- Pierog T
- Pierro V
- Pignata G
- Pike S
- Pilia M
- Pillant G
- Pimenta M
- Pinard L
- Pinat E
- Pinto IM
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- Piran T
- Piran T
- Piranomonte S
- Pirello M
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- Piron F
- Pirronello V
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- Pita S
- Pitkin M
- Pittori C
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- Podesta F
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- Podsiadlowski P
- Poe M
- Poggiani R
- Poh J
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- Pollmann A Obertacke
- Poolakkil S
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- Popolizio P
- Poppi S
- Porowski C
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- Powell J
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- Poznanski D
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- Prochaska JX
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- Prokhorov D
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- Puppo P
- Qi H
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- Qu JL
- Quataert E
- Quel EJ
- Querchfeld S
- Querel R
- Quetschke V
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- Quinn L
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- Quinones C
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- Quirrenbach A
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- Quitzow-James R
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- Rabeling DS
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- Racusin J
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- Rain S
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- Raja W
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- Rameez M
- Ramirez KE
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- Ramos-Buades A
- Ramos-Pollan R
- Rana J
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- Rapagnani P
- Rappoldi A
- RATIR RIMAS
- Rau A
- Rautenberg J
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- Ravignani D
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- Raymond V
- Razza A
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- Razzaque S
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- Rdiger A
- Rea IC
- Read J
- Rebolo R
- Regimbau T
- Rei L
- Reichart DE
- Reid S
- Reimann R
- Reimer A
- Reimer A
- Reimer O
- Reimer O
- Reitze DH
- Relethford B
- Relich M
- Ren W
- Ren Z
- Renaud M
- Renzi V
- Reposeur T
- Resconi E
- Resmi L
- Rest A
- Reva IV
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- Reyes SD
- Reynolds T
- Rho CD
- Rhode W
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- Ricci F
- Ricci R
- Ricciarini S
- Riccobene G
- Richman M
- Ricker PM
- Ridden-Harper R
- Ridky J
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- Rios-Lopez E
- Risse M
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- Rowell G
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- Saito S
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- Sakamaki A
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- Sakellariadou M
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- Salamida F
- Salazar H
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- Sarmiento-Cano C
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- Schieler H
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- Schneider A
- Schneider M
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- Schofield RMS
- Scholten O
- Schonbeck A
- Schoneberg S
- Schoorlemmer H
- Schovnek P
- Schreiber E
- Schroder FG
- Schroder S
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- Schulz A
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- Schulze S
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- Selsing J
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- Sergeev A
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- Serino M
- Serra G
- Serra-Ricart M
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- Settimo M
- Seunarine S
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- Siemens X
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- Steinlechner J
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- Suarez-Duran M
- Suchyta E
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- Tacca M
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- Tagliaferri G
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- Taiuti M
- Tajitsu A
- Takahashi I
- Takahashi J
- Takahashi M
- Takahashi T
- Takao Y
- Takayama M
- Talbot C
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- Tamura T
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- Tan Y
- Tanaka I
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- Tanimoto A
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- Tao C
- Tao L
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- Taracchini A
- Tarle G
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- Tasson JD
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- Ter Veen S
- Ter-Antonyan S
- Terai T
- Terliuk A
- Terreran G
- Terrier R
- Tesic G
- Testa V
- Tewari SV
- Thayer JB
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- Thene CC
- Thierry P
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- Thomas EG
- Thomas M
- Thomas P
- Thomas RC
- Thompson DJ
- Thorne KA
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- Thrane E
- Tibaldo L
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- Tibolla O
- Tilav S
- Timmermans C
- Tingay SJ
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- Tominaga N
- Tonelli M
- Tonnis C
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- Torii S
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- Torres-Flores S
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- Torrie CI
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- Travnicek P
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- Trinastic J
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- Tsvetkova AE
- Tucker BE
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- Turcati A
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- Turpin D
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- Tuyenbayev D
- Ty B
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- Ubertini P
- Uchiyama Y
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- Uemura M
- Ueno K
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- Ugolini D
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- Publication venue
- 'American Astronomical Society'
- Publication date
- 01/01/2017
- Field of study
On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40+8-8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Mo. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One- Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta
Search for gravitational waves from Scorpius X-1 in the second Advanced LIGO observing run with an improved hidden Markov model
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- Publication venue
- College Park, MD : American Physical Society
- Publication date
- 01/01/2019
- Field of study
We present results from a semicoherent search for continuous gravitational waves from the low-mass x-ray binary Scorpius X-1, using a hidden Markov model (HMM) to track spin wandering. This search improves on previous HMM-based searches of LIGO data by using an improved frequency domain matched filter, the J-statistic, and by analyzing data from Advanced LIGO's second observing run. In the frequency range searched, from 60 to 650 Hz, we find no evidence of gravitational radiation. At 194.6 Hz, the most sensitive search frequency, we report an upper limit on gravitational wave strain (at 95% confidence) of h095%=3.47×10-25 when marginalizing over source inclination angle. This is the most sensitive search for Scorpius X-1, to date, that is specifically designed to be robust in the presence of spin wandering. © 2019 American Physical Society
Search for Tensor, Vector, and Scalar Polarizations in the Stochastic Gravitational-Wave Background
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- Zhu X.J.
- Zucker M.E.
- Zweizig J.
- Publication venue
- College Park, MD : American Physical Society
- Publication date
- 01/01/2018
- Field of study
The detection of gravitational waves with Advanced LIGO and Advanced Virgo has enabled novel tests of general relativity, including direct study of the polarization of gravitational waves. While general relativity allows for only two tensor gravitational-wave polarizations, general metric theories can additionally predict two vector and two scalar polarizations. The polarization of gravitational waves is encoded in the spectral shape of the stochastic gravitational-wave background, formed by the superposition of cosmological and individually unresolved astrophysical sources. Using data recorded by Advanced LIGO during its first observing run, we search for a stochastic background of generically polarized gravitational waves. We find no evidence for a background of any polarization, and place the first direct bounds on the contributions of vector and scalar polarizations to the stochastic background. Under log-uniform priors for the energy in each polarization, we limit the energy densities of tensor, vector, and scalar modes at 95% credibility to Ω0T<5.58×10-8, Ω0V<6.35×10-8, and Ω0S<1.08×10-7 at a reference frequency f0=25 Hz. © 2018 American Physical Society
Erratum: “Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015–2017 LIGO Data” (2019, ApJ, 879, 10)
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- Yap M. J.
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- Yeeles D. W.
- Yu Hang
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- Yuen S. H. R.
- Zadrozny A.
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- Publication venue
- 'American Astronomical Society'
- Publication date
- 01/01/2019
- Field of study
Due to an error at the publisher, in the published article the number of pulsars presented in the paper is incorrect in multiple places throughout the text. Specifically, "222" pulsars should be "221." Additionally, the number of pulsars for which we have EM observations that fully overlap with O1 and O2 changes from "168" to "167." Elsewhere, in the machine-readable table of Table 1 and in Table 2, the row corresponding to pulsar J0952-0607 should be excised as well. Finally, in the caption for Table 2 the number of pulsars changes from "188" to "187.
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