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i, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, D. Svinkin

stitut für extraterrestrischePhysikfür stitut

Berkeley, CA 94720 CA Berkeley, Technical Institute of the Russian Academy of Sciences of Academy Russian the of Institute Technical

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Speaker y of Arizona, Lunar and Planetary Laboratory Lunar andPlanetary Arizona, of y

yamaoka@phys. [email protected] [email protected] [email protected] [email protected] [email protected] [email protected]

sit 1 Fuchinobe, Sagamihara, Kanagawa229 Sagamihara, Fuchinobe, 1

- sojuznaja84/32, Moscow 117997, Russian Federation - 1 mail: mail: mail: mail: mail: mail: mail: mail: mail: mail: mail: mail: mail: mail: [email protected] mail: 10 Copyright owned by the author(s) under the terms of the Creative Commons Attribution Commons of Creative terms the the under author(s) owned by the Copyright ------

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 K. Yamaoka K. University Gakuin Aoyama Mathematics, and Physics of Department 5 E E Rau A. Zhang, X. Kienlin, von A. Max Germany 85748 Garching, Giessenbachstrasse, E University of California, Santa Cruz 95064 CA, U.S.A. CA, 95064 Cruz Santa California, of University E Hajdas W. Institute Scherrer Paul Switzerland PSI, Villigen 5232 IoffePhysico Federation Russian 194021, Petersburg, St. E Smith M. D. I Cruz Santa and Physics of Department W. Boynton, C. Fellows, K. Harshman, R. Starr R. Harshman, K. Fellows, C. Boynton, W. Univer U.S.A. 85721, AZ Tucson, E Golenetski S. I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin Institutefor Space Research Prof E K. Hurley K. Laboratory Sciences Space Berkeley U.C. Way, Gauss 7 E The Interplanetary Network Database Network Interplanetary The

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0198, Japan 0198,

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- Hiroshima, Hiroshima 739 Hiroshima Hiroshima, a -

tokyo.ac.jp ku, Saitama ku,

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ku, Tokyo113 ku, -

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3, Los Alamos, NM 87545, U.S.A. NM 87545, Alamos, Los 3, nt Center for Astrophysics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Baltimore, Circle, Hilltop 1000 County, Baltimore Maryland, of University Astrophysics, for Center nt

S. Barthelmy, J. Cummings J. Barthelmy, S. Roma

Okubo, Sakura Okubo, - , - Universities Space Research Association, 10211 Wincopin Circle, Suite 500, Columbia, MD 21044 MD Columbia, 500, Suite Circle, Wincopin 10211 Association, Research Space Universities Makishima Cosmic Radiation Laboratory, The Institute of Physical and Chemical Research (RIKEN), Research Chemical and Physical of Institute The Laboratory, Radiation Cosmic Makishima Joi 3 cho, Kanazawa, cho, 920Ishikawa - [email protected] [email protected] [email protected] [email protected] [email protected] [email protected] D 21250 D 1 Hirosawa, Wako, Saitama 351 Saitama Wako, Hirosawa, 1 Also Also Also Also Emeritus Also -

5 2 3 4 2 M 1 Hongo, Bunkyo Hongo, 1 1 Kagamiyama, Higashi Kagamiyama, 1 1 Yoshinodai, Sagamihara, Kanagawa229 Sagamihara, Yoshinodai, 1 - - - mail: mail: mail: mail: mail: mail: mail: mail: [email protected] mail: mail: [email protected] mail: mail: mail: mail: mail: 3 3 1 . Makishima Copyright owned by the author(s) under the terms of the Creative Commons Attribution Commons of Creative terms the the under author(s) owned by the Copyright . Takahashi ------

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 INAF/IASF J. Goldsten Goldsten J. University Hopkins Johns Laboratory, Physics Applied U.S.A. MD20723, Laurel, E Feroci M. Monte, Del E. D. Palmer D. Laboratory National Alamos Los 166 Box P.O. E E Cline T. Center Flight Space Goddard NASA U.S.A. 20771, MD Greenbelt, 661, Code E Department of Physics, Kanazawa University Kanazawa Physics, of Department Kadoma E K Tokyo of University Physics, of Department 7 M. Tashiro,Y. Terada Tashiro,Y. M. University Saitama Physics, of Department Shimo 255 E Murakami T. M. Ohno, Y. Hanabata, Y. Fukazawa Y. Hanabata, Y. Ohno, M. University Hiroshima Physics, of Department 1 E T Instituteof Space and Astronautical Science (ISAS/JAXA) 3 E

PoS(GRB 2012)117

. sa.it http://pos.sis We describe We the describe localization data rrent IPN comprises 9

ray transients. - ShareAlike Licence. ShareAlike -

A . .A. S S NonCommercial . . - duration duration -

, roughly 100 of which are not localized by Swift or 35805, U 35805,

oma, Italy oma, able able on the IPN website. It comprises, among other things, a

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time monitor for short -

roma.inaf.it

- sky, full 40129 Bologna, Italy Bologna, 40129 -

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Bologna - Ray Bursts 2012 Conferen 2012 Bursts Ray [email protected] [email protected] [email protected] sa.grb@iasf - 11, 2012 11, - . It is an all

mail: mail: mail: mail: mail: mail: mail: Copyright owned by the author(s) under the terms of the Creative Commons Attribution Commons of Creative terms the the under author(s) owned by the Copyright - - - -

 Gamma Germany Munich, 7 May

GRB GRB bibliography, a comprehensive list of bursts from 1990 to the present, data. IPN and the of uses the of some describe also We Interplanetary Networks (IPNs) have been in use since the late 1970’s. The cu and detects about 325 GRBs/year Fermi IPN database, which is publicly avail NSSTC, 320 Sparkman Drive, Huntsville, AL AL Huntsville, Drive, Sparkman 320 NSSTC, E Meegan C. Association Research Space Universities U 35805, AL Huntsville, Drive, Sparkman 320 NSSTC, E INAF/IASF I 101, Gobetti Via E Briggs S. M. Connaughton, V. Huntsville in Alabama of University via Fosso del Cavaliere 100, 00133, R 00133, 100, Cavaliere Fossodel via E Marisaldi M.

PoS(GRB 2012)117

Hurley T N E s indicate the distant S , and that is what will be E R s P n - o i 6 s s 7 i 9 M R 1 , y A r S E a t E Y e N I n

L a l 4 E p

r M e I

t T n I t N he he only way to get arcminute GRB positions was by n O I a t , t S s i S I D it also has a present and a future M N the IPN has a long history, and over 30 spacecraft have P I But But .

. (figure 1)

i I t r y s eginning eginning (ca. 1975 A.D.) L f u 2 3 4 9 a 1 2 d 2 3 7 1 T X E R E P A S i O R O M - S e . Consequently,

e k m e b in this paper n 1 1 1 1 g A L A T S A z S s s z E r C i A s v E V R w I s s S a M n r o E o o o R e a a a i o a E S N s E O s P G z M S G i N E G W r r r r e S n b b l n F he he o y y A - H G u G N N s R e e e l R e t A D G H o e g g o s n p d I E S R b S n n n n E U U h h o o o u

p R H S T t O r r e e e e S G O In E n e P P p s P P N V V V V o S s B r I r m Introduction E K a

a o M M C M

Figure Figure 1. The timelines interplanetary of network some of since the interplanetary missions, while missions the black its lines are for which the missions which were closer have inception. to participated Earth. in the The red line

emphasized 1. triangulation participated in it IPNDatabase PoS(GRB 2012)117

- 2 (the

Earth Earth a full - Hurley

seconds; - m (INTEGRAL, . The IPN detects

. Integrating over

. “Full time” means RHESSI, , and and Suzaku, RHESSI, ffectively acts as 3 of the , i, and the IPN. The yearly measured by BAT the measured Swift in and it e

probability probability that two or more . The Venn diagram of figure

that . The IPN sensitivity as a function and other factors sky” means that there is no point in 3

- AGILE, Fermi, Fermi, AGILE,

150 keV range. The dashed line shows . The relation between the GRBs

blocking in orbit around Mercury, at a distance of 2 – -

. “All Figure Figure network closer to Earth. to closer network vity vity as a function of fluence. This is shown -

in orbit around Mars, at a distance of roughly 325 GRBs/year 5

ermi or Swift. or ermi . They are widely widely separated spacecraft will detect a burst; these observations can be used to triangulate the event. of of fluence. The sensitivity is expressed here as the efficiency, or probability of detecting a burst; the fluence is the 15 the probability that any two IPN spacecraft will detect a burst; spacecraft, if this will not result they in a triangulation are because both the separation is near too small. The line solid shows the

Figure Figure no planet about in an eccentric orbit with apogee 0.5 light latter rate slightly exceeds the former) about 100 bursts per year which are not F either observed by observed observed by Swift, Ferm rates are shown. The Swift bursts are those both within and outside the coded field of view of the BAT Odyssey, Odyssey, MESSENGER, MESSENGER, etects etects ray transients (mainly SGRs and GRBs) - essentially essentially NTEGRAL, NTEGRAL, I seconds; and omprises 9 spacecraft omprises -

light seconds. It is one of the best configurations that the IPN has ever had, since it - seconds from Earth; - to 700 light

0 . 00 sky monitor for gamma 3 3 - The of sensitivity the IPN is a primarily function of the GRB fluence and peak flux. To a

In this configuration, the IPN d Presently, the IPN c IPN the Presently, here here is no time when all the spacecraft are off The Current IPN Current The

much much lesser extent, it also depends on the burst duration peak fluxes and durations, we can derive the sensiti in figure the sky which is MESSENGER, and ) have ever invisible to all showsbetween relation detectedFermi,byburstsSwift,andIPN.the the the the missions. Indeed has not only two distant spacecraft, but also, a mini a also, but spacecraft, distant two only not has time, all that t Swift, Swift, in low Earth orbit; Wind, at 6 light roughly 260 to 126 IPNDatabase 1.1 PoS(GRB 2012)117

- r

ecraft ecraft Hurley of of thei

. It is composed The The user does not ). ). 5

The The region shaded in green . A small error box for GRB 4

(shaded in green)

has three main sections. The first is a a is first The sections. main three has is updated on a roughly monthly basis. Figure

The The first and third are sections updated semi 110808, 110808, formed by the intersection of IPN two annuli. box. error the defines

6

7000 GRB localizations from 1990 to the present. about ), ), or large, irregular areas (figure 4 h error box shapes, however, because programs are to available answer (ssl.berkeley.edu/ipn3/index.html)

y with over 11,000 titles published between 1972 and the present. The second

database database . The large, complex error box of GRB 110823

5

?” blocking. Figure Figure

The IPN IPN The - The localizations are expressed as small circles on the celestial sphere. They may intersect intersect may They sphere. celestial the on circles small as expressed are localizations The The Database of of a wide IPN annulus and an ecliptic latitude band. Parts of the localization are excluded by Earth need need to be concerned wit the frequently asked questions, namely, “did any GRBs occur during a given time period a with RA given and Dec, and if so, what were the areas consistent had which positions boxes error These These numbers are with steadily increasing time. second the while basis, daily roughly a on automatically to form neat, small polygons (figure GRB GRB bibliograph is a table of 25,000 events, mostly GRBs, SGRs, and flares, which occurred between 1990 and the present. The table observed contains them. The third is a their table of dates and times, and indicates which spac IPNDatabase 2. PoS(GRB 2012)117

. 2)

0ay, 0ay, L35 .

Virgo Virgo Hurley Ray Ray - , 201 (1,2)

(2012)

(3)

. 734

. ) energy photonenergy not not warrant rapid - ApJ positions

2010ah , 2012 ( Refining Refining Fermi GBM

LAT & IceCube & 1) 1)

13073 such as (5)

GCN Circ. GCN romNorthern Hemisphere Gamma ,

.

) vitational vitational radiation using LIGO and line IcSupernova Discovered by the Palomar -

7 2012 (

refining or confirming

consuming, and most bursts do . - 12AE41G. and 13070 . 357

. 76 Searching Searching for gra ng used for, are the following. (2008)

GBM trigger 353549464 (GRB 120316A?) : High : 120316A?) (GRB 353549464 trigger GBM (SN2010ah): A Broad GCN Circ GCN

. 3) (2012) , 674

The Search for Muon Neutrinos f Neutrinos Muon for Search The

741

ApJ

, ers ers of magnitude, or or are bei

IPNTriangulation of GRB 120316A ApJ Search for Gravitational Wave Bursts from Six Magnetars Six from WaveBursts Gravitational for Search

PTF 10bzf PTF , there is a need for it. Second, very few IPN localizations are announced in been been earching for neutrino emission using AMANDA using emission neutrino for earching

1dh, 1dh, and 2011fe

and when A. Corsi et al., al., et Corsi A. Abadie J. al., et al., et Achterberg A. W. Zheng and C. Akerlof , , Akerlof C. and Zheng W. al., et Hurley K. . And 4) s up. up. However, data are available for them. Users should feel free to consult the first

-

KH is grateful for IPN support under the following NASA grants: NNX07AR71G, Two things to keep in mind before starting any project with the data localization are first, The The IPN localization data are public, and may be used for any project. Some of projects Bursts with AMANDA with Bursts Transient Factory Transient emission in Fermi/LAT data in emission (4) the database is not fully populated. There are numerous gaps, which can be filled fairly

[3] [4] [5] [1] [2]

Acknowledgments Uses of the IPN Data

References 4. NNX and NNX12AD68G, NNX11AP96G, that easily if GCN Circulars. Doing so would be time follow advice. for author Searching Searching for GRBs consistent with optically detected Ib/c SNe, PTF10qts, 201 data 3. which they have positions by up to 4 ord IPNDatabase