a subclass of grbs as possible ligo-2 gravitational-wave sources jay p. norris nasa/gsfc (1) the...
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A Subclass of GRBs as
Possible LIGO-2 Gravitational-Wave
Sources
Jay P. NorrisNASA/GSFC
(1) The prevalent belief structure:{Some, All?} GRBs associated with SNe.
(2) Demographics, attributes of possible subclass of nearby, ultra-low luminosity GRBs and their associates, nearby type Ib/c SNe.
(3) Predicted range of GW strains, detection rate for GRB subclass
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G
RB
98
04
25
S
N
19
98
bw
G
RB
03
03
29
S
N
20
03
dh
Only 20% of observed GRBs have associated redshifts:Some fraction of the remaining 80% may lie at higher
redshifts.
Obs’d SNzmax=1.77
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GRB-SN Belief Sparse Knowledge
Structure:
One very close ( 35 Mpc) ultra-low luminosity GRB, and one not so close ( 680 Mpc) subluminous GRB— Both manifest the presence of Type 1c SNe.
Constrained but open issue: The delay (in some cases)
TSN–TGRB<~ few days. Are the events simultaneous?
Detection of GW signal could depend on accurate knowledge of TSN or TGRB. Accurate TGRB is easy.
GW signal requires non-axisymmetric deformation (); Theoretical core collapses: ~ 10-4-10-2 to “unity”.
Is degree of non-axisymmetry related to GRB jet opening angle (via BH rotation)?
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Figure 2. The detailed classification of SNe requires not only the identificationof specific features in the early spectra, but also the analysis of the line profiles,luminosity and spectral evolutions. (Cappellero & Turrato: astro-ph/0012455)
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E. Pianastro-ph/9910236
Revised BeppoSAXerror box forGRB 980425
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Iwamoto et al.(1998):
Modeling yieldscore collapse for SN1998bw within +0.7/2 days of GRB 980425
22 days
40 days
12days
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Young, Baron & Branch (1995)
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GRB 011211, z = 2.14 Reeves et al., Nature, 2001, 416
Blue-shifted X-ray lines ( 0.09); assume: jet 20º, ne ~ 1015
cm-3
GRB ejecta runs into SN shell at R ~ 1015 cm TGRB - TSN ~ 4 days
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Matheson et al., GCN 2120; Stanek et al. (astro-ph/0304173)
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Are there T0_SN T0_GRB delays?
SN 1998bw light curve has evidence for upturn (end of “UV breakout” ?), which would place T0_SN ~ few days before T0_GRB. Modeling: T = -2,+0.7 days
X-ray afterglow spectral analysis (GRB 011211) suggests 4-day hiatus, SN to GRB.
? Type 1c SNe light curves not well studied, and are known to vary in “width” by at least a factor of ~ 3:
Cannot gauge T0_SN accurately by comparison with SN 1998bw, especially given GRB afterglow photometry at faint magnitudes.
[Theory: T ~ 10s - hrs — Woosley et al., collapsars
T ~ ??? — van Putten, BH-torus ]
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Core-collapse SN Explode Asymmetrically:
Images of 1987A (see S&T, Jan 2002, Wang & Wheeler)
Elemental asymmetries in (Wang et al. 2002)
SN remnants (1987A, Cas A)
Polarization in SNe: (Wang et al. 2001) Type 1a: <~ 0.3% Type II: ~ 1-2%, increasing with time Type 1b/c: ~ 3-7%
{GRB observed by RHESSI — Coburn & Boggs, Nature}
Some GRBs beamed into 4/[~500/2], (Frail et al. 2002)
SN Modeling — strong polar ejections
Pulsar space velocities
Some SNe are rapidly rotating at core-collapse, high T/W.
Non-axisymmetric (bar) instabilities possible, <~ unity.
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A Sub-Population of “Nearby” GRBs ?
BATSE subsample (~ 7%) of soft-spectrum GRBs. Defining characteristic: Very long pulses with long spectral lags (> 0.3 s).
*** Proportion increases to ~ 50% near BATSE threshold. ***
Additional Evidence for Nearby Spatial Distribution:
GRB980425/SN1998bw is canonical example, at 38
Mpc.
Log N—Log Fp has ~ -3/2 slope: cosmology
unimportant. Tendency towards Supergalactic Plane, similar to
SN Ib/c; long-lag GRB and nearby galaxy sky
distributions similar.
Implications: Detected sample, d <~ 100 Mpc. Ultra-
low luminosity (<~ 1048 ergs s-1). Rate: RGRB ~ ¼ RSN
Ib/c
*** Could be LIGO II sources: ~ 4 yr-1 within 50 Mpc
***
(see ApJ 2002, 579, 386)
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> 300 keV
: blue100-300 keV: green 50- 100 keV: yellow 25- 50 keV: red
“Typical” long-lag GRB, detected by BATSE.
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HETE-2 time profile for GRB 030329, 5-120 keV
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A Main Sequence “HR Diagram for Gamma-Ray Bursts”
L53 ≈ 1.1 (lag/0.01 s)-1.15
970228
000131
991216
030329Prediction:
Woosley & MacFadyen (1999), Ioka & Nakamura (2001), others predicted subclass of numerous, nearby GRBs: low luminosity, soft-spectrum, long-lag.Properties attributed to: (1) large jet opening angle & (2) low ~ 2-5.
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M. J. Hudson (1993)
7200 km/s100 Mpcz = 0.024
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Virgo
980425971208
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SNe Ib/Ic : 62 detected 1954-2001.75,
(> 2/3 since 1998.0)
With 85% at distances < 100 Mpc.
Only ~10% of “nearby” SNe are detected.
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RGRB (< 100 Mpc) ~ 30 yr-1 ~ ¼ RSNIb/c
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Fryer, Holz & Hughes
(2002);
Blondin, Mezzacappa & DeMarino (2003) :
Bar instabilities likely
( ~ unity).
Assuming 100 cycles,
f ~ 200-800 Hz,
source < 50 Mpc
h/Hz ~ 1.3 10-23
Expect ~ 4 long-lag
GRBs yr-1 (< 50
Mpc),
and we know when
they occur.
50 Mpc
680 Mpc
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Summary
Very good evidence that high-mass, highly energetic core-
collapse SNe are associated with GRBs — one nearby, a
few cosmologically distant examples of such associations.
Evidence indicates that these SNe and GRB events are
asymmetric ( high T/W). Are SN and GRB simultaneous?
Long-lag, soft-spectrum, apparently nearby, ultra low-
luminosity GRBs are numerous (~ 50%) near BATSE
threshold.
RGRB (<100 Mpc) ~ 30/yr ~ ¼ RSNIb/c.
A few yr-1 detectable by LIGO II.
Swift should see a larger fraction of “long-lag” GRBs than
BATSE.
Many chances to find the associated SNe and GW
signals !!!
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The End
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G.M. Harry et al.
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jet varies, view varies, view varies,
~ 2–20. outside jet cone. inside profiled jet.
Lmin
Lmax
Beaming Fraction Viewing angle Profiled jet
4 Ld ~ constant, Special Relativity: L() reflects ():
L-1. Lorentz contraction 30 < () < 1000
& Doppler boost (jet fastest on axis)
All three models realize broad observed, butnarrow actual Luminosity and Energy distributions.
v,max v,min
jet
L ~ const.across jet
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GRB “Pulse Paradigm”
GRBs : LGRBs : Lpeakpeak vs. vs. GRBs : LGRBs : Lpeakpeak vs. vs.
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GRBs : LGRBs : Lpeakpeak vs. vs. GRBs : LGRBs : Lpeakpeak vs. vs.
CCFLag
Time
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Possible Confirmation Approaches
(1) Untriggered BATSE bursts: For Fp < 0.25 ph cm-2
s-1 long-lag bursts predominate. But, larger localization errors; ID’ing as bona fide GRBs is problematic.
(2) ~ 400-500 additional triggered BATSE bursts.
(3) Cross-correlation of nearby matter distribution (d < 100 Mpc) and GRB positions (M. Hudson).
(4) Extrapolation of SNe light curves to T0,
comparison with GRB times and positions (J. Bonnell).
(5) Swift