J/ApJ/760/12 LIGO/Virgo gravitational-wave (GW) bursts with GRBs (Abadie+, 2012)
Search for gravitational waves associated with gamma-ray bursts during LIGO
science run 6 and Virgo science runs 2 and 3.
Abadie J., Abbott B.P., Abbott R., Abbott T.D., Abernathy M., Accadia T.,
Acernese F., Adams C., Adhikari R.X., Affeldt C., Agathos M., Agatsuma K.,
Ajith P., Allen B., Ceron E.A., Amariutei D., Anderson S.B., Anderson W.G.,
Arai K., Arain M.A., Araya M.C., Aston S.M., Astone P., Atkinson D.,
Aufmuth P., Aulbert C., Aylott B.E., Babak S., Baker P., Ballardin G.,
Ballmer S., Barayoga J.C.B., Barker D., Barone F., Barr B., Barsotti L.,
Barsuglia M., Barton M.A., Bartos I., Bassiri R., Bastarrika M., Basti A.,
Batch J., Bauchrowitz J., Bauer TH.S., Bebronne M., Beck D., Behnke B.,
Bejger M., Beker M.G., Bell A.S., Belopolski I., Benacquista M.,
Berliner J.M., Bertolini A., Betzwieser J., Beveridge N., Beyersdorf P.T.,
Bilenko I.A., Billingsley G., Birch J., Biswas R., Bitossi M.,
Bizouard M.A., Black E., Blackburn J.K., Blackburn L., Blair D., Bland B.,
Blom M., Bock O., Bodiya T.P., Bogan C., Bondarescu R., Bondu F.,
Bonelli L., Bonnand R., Bork R., Born M., Boschi V., Bose S., Bosi L.,
Bouhou B., Braccini S., Bradaschia C., Brady P.R., Braginsky V.B.,
Branchesi M., Brau J.E., Breyer J., Briant T., Bridges D.O., Brillet A.,
Brinkmann M., Brisson V., Britzger M., Brooks A.F., Brown D.A., Bulik T.,
Bulten H.J., Buonanno A., Burguet-Castell J., Buskulic D., Buy C.,
Byer R.L., Cadonati L., Calloni E., Camp J.B., Campsie P., Cannizzo J.,
Cannon K., Canuel B., Cao J., Capano C.D., Carbognani F., Carbone L.,
Caride S., Caudill S., Cavaglia M., Cavalier F., Cavalieri R., Cella G.,
Cepeda C., Cesarini E., Chaibi O., Chalermsongsak T., Charlton P.,
Chassande-mottin E., Chelkowski S., Chen W., Chen X., Chen Y.,
Chincarini A., Chiummo A., Cho H.S., Chow J., Christensen N., Chua S.S.Y.,
Chung C.T.Y., Chung S., Ciani G., Clara F., Clark D.E., Clark J.,
Clayton J.H., Cleva F., Coccia E., Cohadon P.-F., Colacino C.N., Colas J.,
Colla A., Colombini M., Conte A., Conte R., Cook D., Corbitt T.R.,
Cordier M., Cornish N., Corsi A., Costa C.A., Coughlin M., Coulon J.-P.,
Couvares P., Coward D.M., Cowart M., Coyne D.C., Creighton J.D.E.,
Creighton T.D., Cruise A.M., Cumming A., Cunningham L., Cuoco E.,
Cutler R.M., Dahl K., Danilishin S.L., Dannenberg R., D'Antonio S.,
Danzmann K., Dattilo V., Daudert B., Daveloza H., Davier M., Daw E.J.,
Day R., Dayanga T., De Rosa R., Debra D., Debreczeni G., Degallaix J.,
Del Pozzo W., del Prete M., Dent T., Dergachev V., DeRosa R., DeSalvo R.,
Dhurandhar S., Di Fiore L., Di Lieto A., Di Palma I., Di Paolo Emilio M.,
Di Virgilio A., Diaz M., Dietz A., Donovan F., Dooley K.L., Drago M.,
Drever R.W.P., Driggers J.C., Du Z., Dumas J.-C., Dwyer S., Eberle T.,
Edgar M., Edwards M., Effler A., Ehrens P., Endroczi G., Engel R.,
Etzel T., Evans K., Evans M., Evans T., Factourovich M., Fafone V.,
Fairhurst S., Fan Y., Farr B.F., Fazi D., Fehrmann H., Feldbaum D.,
Feroz F., Ferrante I., Fidecaro F., Finn L.S., Fiori I., Fisher R.P.,
Flaminio R., Flanigan M., Foley S., Forsi E., Forte L.A., Fotopoulos N.,
Fournier J.-D., Franc J., Franco S., Frasca S., Frasconi F., Frede M.,
Frei M., Frei Z., Freise A., Frey R., Fricke T.T., Friedrich D.,
Fritschel P., Frolov V.V., Fujimoto M.-K., Fulda P.J., Fyffe M., Gair J.,
Galimberti M., Gammaitoni L., Garcia J., Garufi F., Gaspar M.E.,
Gehrels N., Gemme G., Geng R., Genin E., Gennai A., Gergely L.A., Ghosh S.,
Giaime J.A., Giampanis S., Giardina K.D., Giazotto A., Gil-casanova S.,
Gill C., Gleason J., Goetz E., Goggin L.M., Gonzalez G., Gorodetsky M.L.,
Gossler S., Gouaty R., Graef C., Graff P.B., Granata M., Grant A., Gras S.,
Gray C., Gray N., Greenhalgh R.J.S., Gretarsson A.M., Greverie C.,
Grosso R., Grote H., Grunewald S., Guidi G.M., Guido C., Gupta R.,
Gustafson E.K., Gustafson R., Ha T., Hallam J.M., Hammer D., Hammond G.,
Hanks J., Hanna C., Hanson J., Hardt A., Harms J., Harry G.M., Harry I.W.,
Harstad E.D., Hartman M.T., Haughian K., Hayama K., Hayau J.-F.,
Heefner J., Heidmann A., Heintze M.C., Heitmann H., Hello P., Hendry M.A.,
Heng I.S., Heptonstall A.W., Herrera V., Hewitson M., Hild S., Hoak D.,
Hodge K.A., Holt K., Holtrop M., Hong T., Hooper S., Hosken D.J., Hough J.,
Howell E.J., Hughey B., Husa S., Huttner S.H., Huynh-dinh T., Ingram D.R.,
Inta R., Isogai T., Ivanov A., Izumi K., Jacobson M., James E., Jang Y.J.,
Jaranowski P., Jesse E., Johnson W.W., Jones D.I., Jones G., Jones R.,
Jonker R.J.G., Ju L., Kalmus P., Kalogera V., Kandhasamy S., Kang G.,
Kanner J.B., Kasturi R., Katsavounidis E., Katzman W., Kaufer H.,
Kawabe K., Kawamura S., Kawazoe F., Kelley D., Kells W., Keppel D.G.,
Keresztes Z., Khalaidovski A., Khalili F.Y., Khazanov E.A., Kim B.K.,
Kim C., Kim H., Kim K., Kim N., Kim Y.M., King P.J., Kinzel D.L.,
Kissel J.S., Klimenko S., Kokeyama K., Kondrashov V., Koranda S.,
Korth W.Z., Kowalska I., Kozak D., Kranz O., Kringel V., Krishnamurthy S.,
Krishnan B., Krolak A., Kuehn G., Kumar P., Kumar R., Kwee P., Lam P.K.,
Landry M., Lantz B., Lastzka N., Lawrie C., Lazzarini A., Leaci P.,
Lee C.H., Lee H.K., Lee H.M., Leong J.R., Leonor I., Leroy N., Letendre N.,
Li J., Li T.G.F., Liguori N., Lindquist P.E., Liu Y., Liu Z.,
Lockerbie N.A., Lodhia D., Lorenzini M., Loriette V., Lormand M.,
Losurdo G., Lough J., Luan J., Lubinski M., Luck H., Lundgren A.P.,
Macdonald E., Machenschalk B., MacInnis M., Macleod D.M., Mageswaran M.,
Mailand K., Majorana E., Maksimovic I., Malvezzi V., Man N., Mandel I.,
Mandic V., Mantovani M., Marandi A., Marchesoni F., Marion F., Marka S.,
Marka Z., Markosyan A., Maros E., Marque J., Martelli F., Martin I.W.,
Martin R.M., Marx J.N., Mason K., Masserot A., Matichard F., Matone L.,
Matzner R.A., Mavalvala N., Mazzolo G., McCarthy R., McClelland D.E.,
McGuire S.C., McIntyre G., McIver J., McKechan D.J.A., McWilliams S.,
Meadors G.D., Mehmet M., Meier T., Melatos A., Melissinos A.C., Mendell G.,
Mercer R.A., Meshkov S., Messenger C., Meyer M.S., Miao H., Michel C.,
Milano L., Miller J., Minenkov Y., Mitrofanov V.P., Mitselmakher G.,
Mittleman R., Miyakawa O., Moe B., Mohan M., Mohanty S.D.,
Mohapatra S.R.P., Moraru D., Moreno G., Morgado N., Morgia A., Mori T.,
Morriss S.R., Mosca S., Mossavi K., Mours B., Mow-Lowry C.M., Mueller C.L.,
Mueller G., Mukherjee S., Mullavey A., Muller-Ebhardt H., Munch J.,
Murphy D., Murray P.G., Mytidis A., Nash T., Naticchioni L., Necula V.,
Nelson J., Neri I., Newton G., Nguyen T., Nishizawa A., Nitz A., Nocera F.,
Nolting D., Normandin M.E., Nuttall L., Ochsner E., O'dell J., Oelker E.,
Ogin G.H., Oh J.J., Oh S.H., O'reilly B., O'shaughnessy R., Osthelder C.,
Ott C.D., Ottaway D.J., Ottens R.S., Overmier H., Owen B.J., Page A.,
Palladino L., Palomba C., Pan Y., Pankow C., Paoletti F., Paoletti R.,
Papa M.A., Parisi M., Pasqualetti A., Passaquieti R., Passuello D.,
Patel P., Pedraza M., Peiris P., Pekowsky L., Penn S., Perreca A.,
Persichetti G., Phelps M., Pichot M., Pickenpack M., Piergiovanni F.,
Pietka M., Pinard L., Pinto I.M., Pitkin M., Pletsch H.J., Plissi M.V.,
Poggiani R., Pold J., Postiglione F., Prato M., Predoi V., Prestegard T.,
Price L.R., Prijatelj M., Principe M., Privitera S., Prix R., Prodi G.A.,
Prokhorov L.G., Puncken O., Punturo M., Puppo P., Quetschke V.,
Quitzow-James R., Raab F.J., Rabeling D.S., Racz I., Radkins H., Raffai P.,
Rakhmanov M., Rankins B., Rapagnani P., Raymond V., Re V., Redwine K.,
Reed C.M., Reed T., Regimbau T., Reid S., Reitze D.H., Ricci F., Riesen R.,
Riles K., Robertson N.A., Robinet F., Robinson C., Robinson E.L.,
Rocchi A., Roddy S., Rodriguez C., Rodruck M., Rolland L., Rollins J.G.,
Romano J.D., Romano R., Romie J.H., Rosinska D., Rover C., Rowan S.,
Rudiger A., Ruggi P., Ryan K., Sainathan P., Salemi F., Sammut L.,
Sandberg V., Sannibale V., Santamaria L., Santiago-Prieto I.,
Santostasi G., Sassolas B., Sathyaprakash B.S., Sato S., Saulson P.R.,
Savage R.L., Schilling R., Schnabel R., Schofield R.M.S., Schreiber E.,
Schulz B., Schutz B.F., Schwinberg P., Scott J., Scott S.M., Seifert F.,
Sellers D., Sentenac D., Sergeev A., Shaddock D.A., Shaltev M., Shapiro B.,
Shawhan P., Shoemaker D.H., Sibley A., Siemens X., Sigg D., Singer A.,
Singer L., Sintes A.M., Skelton G.R., Slagmolen B.J.J., Slutsky J.,
Smith J.R., Smith M.R., Smith R.J.E., Smith-Lefebvre N.D., Somiya K.,
Sorazu B., Soto J., Speirits F.C., Sperandio L., Stefszky M., Stein A.J.,
Stein L.C., Steinert E., Steinlechner J., Steinlechner S., Steplewski S.,
Stochino A., Stone R., Strain K.A., Strigin S.E., Stroeer A.S., Sturani R.,
Stuver A.L., Summerscales T.Z., Sung M., Susmithan S., Sutton P.J.,
Swinkels B., Tacca M., Taffarello L., Talukder D., Tanner D.B.,
Tarabrin S.P., Taylor J.R., Taylor R., ter Braack A.P.M., Thomas P.,
Thorne K.A., Thorne K.S., Thrane E., Thuring A., Tokmakov K.V.,
Tomlinson C., Toncelli A., Tonelli M., Torre O., Torres C., Torrie C.I.,
Tournefier E., Tucker E., Travasso F., Traylor G., Tseng K., Ugolini D.,
Vahlbruch H., Vajente G., van den Brand J.F.J., van den Broeck C.,
van der Putten S., van Veggel A.A., Vass S., Vasuth M., Vaulin R.,
Vavoulidis M., Vecchio A., Vedovato G., Veitch J., Veitch P.J.,
Veltkamp C., Verkindt D., Vetrano F., Vicere A., Villar A.E., Vinet J.-Y.,
Vitale S., Vocca H., Vorvick C., Vyatchanin S.P., Wade A., Wade L.,
Wade M., Waldman S.J., Wallace L., Wan Y., Wang M., Wang X., Wang Z.,
Wanner A., Ward R.L., Was M., Weinert M., Weinstein A.J., Weiss R., Wen L.,
Wessels P., West M., Westphal T., Wette K., Whelan J.T., Whitcomb S.E.,
White D.J., Whiting B.F., Wilkinson C., Willems P.A., Williams L.,
Williams R., Willke B., Winkelmann L., Winkler W., Wipf C.C., Wiseman A.G.,
Wittel H., Woan G., Wooley R., Worden J., Yakushin I., Yamamoto H.,
Yamamoto K., Yancey C.C., Yang H., Yeaton-Massey D., Yoshida S., Yu P.,
Yvert M., Zadrozny A., Zanolin M., Zendri J.-P., Zhang F., Zhang L.,
Zhang W., Zhao C., Zotov N., Zucker M.E., Zweizig J.,
(the Ligo Scientific Collaboration), (the Virgo Collaboration),
Briggs M.S., Connaughton V., Hurley K.C., Jenke P.A., von Kienlin A.,
Rau A., Zhang X.-L.
<Astrophys. J., 760, 12 (2012)>
=2012ApJ...760...12A 2012ApJ...760...12A (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays ; Interferometry
Keywords: binaries: close; gamma-ray burst: general; gravitational waves
Abstract:
We present the results of a search for gravitational waves associated
with 154 gamma-ray bursts (GRBs) that were detected by satellite-based
gamma-ray experiments in 2009-2010, during the sixth LIGO science run
and the second and third Virgo science runs. We perform two distinct
searches: a modeled search for coalescences of either two neutron
stars or a neutron star and black hole, and a search for generic,
unmodeled gravitational-wave bursts. We find no evidence for
gravitational-wave counterparts, either with any individual GRB in
this sample or with the population as a whole. For all GRBs we place
lower bounds on the distance to the progenitor, under the optimistic
assumption of a gravitational-wave emission energy of
10-2M☉c2 at 150Hz, with a median limit of 17Mpc. For
short-hard GRBs we place exclusion distances on binary neutron star
and neutron-star-black-hole progenitors, using astrophysically
motivated priors on the source parameters, with median values of 16Mpc
and 28Mpc, respectively. These distance limits, while significantly
larger than for a search that is not aided by GRB satellite
observations, are not large enough to expect a coincidence with a GRB.
However, projecting these exclusions to the sensitivities of Advanced
LIGO and Virgo, which should begin operation in 2015, we find that the
detection of gravitational waves associated with GRBs will become
quite possible.
Description:
The LIGO and Virgo detectors are kilometer-scale, power-recycled
Michelson interferometers with orthogonal Fabry-Perot arms. They are
designed to detect gravitational waves (GWs) with frequencies ranging
from ∼40Hz to several kHz, with maximum sensitivity near 150Hz. There
are two LIGO observatories: one located at Hanford, WA and the other
at Livingston, LA. The Hanford site houses two interferometers: one
with 4km arms (H1) and the other with 2km arms (H2). The Livingston
observatory has one 4km interferometer (L1). The Virgo detector (V1)
is in Cascina near Pisa, Italy.
The sixth LIGO science run was held from 2009 July 07 to 2010 October
20. The second Virgo science run was held from 2009 July 7 to 2010
January 8 with an improvement in sensitivity by roughly a factor of
two over Virgo's first science run. The third Virgo science run was
held from 2010 August 11 to October 20. The overall Virgo duty cycle
over these two science runs was 78% (See Figure 1).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 76 26 *Short GRB sample and search results
table2.dat 74 128 *Long GRB sample and search results
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Note on table1.dat and table2.dat: Information and limits on associated
gravitational wave (GW) emission for each of the analyzed GRBs that were
classified by us as short or long, respectively.
--------------------------------------------------------------------------------
See also:
VII/267 : Gravitational Wave Galaxy Catalogue (White+ 2011)
J/ApJS/199/18 : The Fermi GBM catalog (Paciesas+, 2012)
J/ApJ/715/1438 : Gravitational-wave bursts with GRBs (Abbott+, 2010)
J/ApJ/713/671 : Gravitational waves from pulsars (Abbott+, 2010)
http://gcn.gsfc.nasa.gov/ : The Gamma-ray Coordinates Network homepage
http://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html : Fermi GBM burst
catalog
Byte-by-byte Description of file: table[12].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- GRB GRB name (YYMMDDA or
YYMMDDNNN for the Fermi/GBM trigger ID) (1)
10 A1 --- f_GRB [Ds] GRB was assigned as short one (2)
12- 19 A8 "h:m:s" Time UTC trigger time
21- 22 I2 s Shift ? Time by which the trigger was shifted for
the coalescence search (only for table 1) (3)
24- 25 I2 h RAh Hour of right ascension (J2000) (4)
27- 28 I2 min RAm Minute of right ascension (J2000)
30- 31 I2 s RAs Second of right ascension (J2000)
33 A1 --- DE- Sign of declination (J2000) (4)
34- 35 I2 deg DEd Degree of declination (J2000) (4)
37- 38 I2 arcmin DEm Arcminute of declination (J2000)
40- 45 A6 --- Nw [H1H2L1V1 ] Gravitational wave detector network
used (5)
46- 48 A3 --- f_Nw [*dg, ] Observation peculiarity (6)
50- 53 F4.1 Mpc D150 [2.7/47.3]? Median exclusion distance for
the GW burst at 150Hz (7)
55- 58 F4.1 Mpc D300 [0.4/18.2]? Median exclusion distance for
the GW burst at 300Hz (7)
60- 63 F4.1 Mpc DNS-NS [2.1/37.1]? Median exclusion distance for
two neutron stars (NS-NS) (only for table1) (7)
65- 68 F4.1 Mpc DNS-BH [3.7/64.5]? median exclusion distance for
neutron star with a black hole (NS-BH)
(only for table 1) (7)
70- 76 A7 --- Det γ-ray detector(s) (8)
--------------------------------------------------------------------------------
Note (1): The GRB name in YYMMDD format or the Fermi/GBM trigger ID for GBM
triggers classified as a GRB without an available GRB name (see
http://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html and
Paciesas et al. 2012, Cat. J/ApJS/199/18)
Note (2): Both a "s" and a "D" indicate that, although the formal duration
of this GRB is longer than 4s ("D"), or unavailable ("s"), the GRB was
analyzed as a short GRB because of a prominent short spike at the
beginning of the light curve (see Section 4).
Note (3): The time in seconds by which the trigger was shifted for the
coalescence search following visual inspection of the light curve.
Note (4): The sky position used for the GW search.
Note (5): Detectors:
H1 = LIGO Hanford interferometer with 4km arms (WA)
H2 = LIGO Hanford interferometer with 2km arms (WA)
L1 = LIGO Livingston 4km interferometer (LA)
V1 = Virgo detector (Italy)
Note (6): Flag as follows:
* = when the shorter on-source window starting 120s before the trigger
is used for the GW burst search,
g = when the on-source window is extended to cover the GRB duration (T90>60s).
d = use of only H1L1 data for the burst search, because of data-quality
requirements.
Note (7): The result of the search: the 90% confidence lower limits on the
distance to the GRB for different waveform models. A standard siren
energy emission of EGW=10-2M☉c2 is assumed for the
circular sine-Gaussian GW burst models; these limits are not available
for four short GRBs which were not analyzed by GW burst search.
See section 7.1.
Note (8): The γ-ray detector that provided the sky location used for the
search: AGILE, BAT, GBM, IBIS, IPN or LAT.
For GRB 090802, IPN triangulation from Konus-WIND, INTEGRAL, and Fermi
was used to further constrain the sky position. The intersection of
the IPN and Fermi error regions was used to place search points using
the method described in Predoi & Hurley (2012JPhCS.363a2034P 2012JPhCS.363a2034P). For
this GRB, the quoted right ascension and declination correspond to the
center of the Fermi error region. For IPN localizations a complete
list of detectors can be found on the project trigger page,
http://www.ssl.berkeley.edu/ipn3/masterli.txt.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 17-Jul-2014